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Sample records for mock galaxy catalogues

  1. An algorithm to build mock galaxy catalogues using MICE simulations

    NASA Astrophysics Data System (ADS)

    Carretero, J.; Castander, F. J.; Gaztañaga, E.; Crocce, M.; Fosalba, P.

    2015-02-01

    We present a method to build mock galaxy catalogues starting from a halo catalogue that uses halo occupation distribution (HOD) recipes as well as the subhalo abundance matching (SHAM) technique. Combining both prescriptions we are able to push the absolute magnitude of the resulting catalogue to fainter luminosities than using just the SHAM technique and can interpret our results in terms of the HOD modelling. We optimize the method by populating with galaxies friends-of-friends dark matter haloes extracted from the Marenostrum Institut de Ciències de l'Espai dark matter simulations and comparing them to observational constraints. Our resulting mock galaxy catalogues manage to reproduce the observed local galaxy luminosity function and the colour-magnitude distribution as observed by the Sloan Digital Sky Survey. They also reproduce the observed galaxy clustering properties as a function of luminosity and colour. In order to achieve that, the algorithm also includes scatter in the halo mass-galaxy luminosity relation derived from direct SHAM and a modified Navarro-Frenk-White mass density profile to place satellite galaxies in their host dark matter haloes. Improving on general usage of the HOD that fits the clustering for given magnitude limited samples, our catalogues are constructed to fit observations at all luminosities considered and therefore for any luminosity subsample. Overall, our algorithm is an economic procedure of obtaining galaxy mock catalogues down to faint magnitudes that are necessary to understand and interpret galaxy surveys.

  2. Constructing mock catalogues for the REFLEX II galaxy cluster sample

    NASA Astrophysics Data System (ADS)

    Balaguera-Antolínez, A.; Sánchez, Ariel G.; Böhringer, H.; Collins, C.

    2012-09-01

    We describe the construction of a suite of galaxy cluster mock catalogues from N-body simulations, based on the properties of the new ROSAT-ESO Flux Limited X-Ray (REFLEX II) galaxy cluster catalogue. Our procedure is based on the measurements of the cluster abundance, and involves the calibration of the underlying scaling relation linking the mass of dark matter haloes to the cluster X-ray luminosity determined in the ROSAT energy band 0.1-2.4 keV. In order to reproduce the observed abundance in the luminosity range probed by the REFLEX II X-ray luminosity function [0.01 < LX/(1044 erg s-1 h-2) < 10], a mass-X-ray luminosity relation deviating from a simple power law is required. We discuss the dependence of the calibration of this scaling relation on the X-ray luminosity and the definition of halo masses and analyse the one- and two-point statistical properties of the mock catalogues. Our set of mock catalogues provides samples with self-calibrated scaling relations of galaxy clusters together with inherent properties of flux-limited surveys. This makes them a useful tool to explore different systematic effects and statistical methods involved in constraining both astrophysical and cosmological information from present and future galaxy cluster surveys.

  3. Fast and accurate mock catalogue generation for low-mass galaxies

    NASA Astrophysics Data System (ADS)

    Koda, Jun; Blake, Chris; Beutler, Florian; Kazin, Eyal; Marin, Felipe

    2016-06-01

    We present an accurate and fast framework for generating mock catalogues including low-mass haloes, based on an implementation of the COmoving Lagrangian Acceleration (COLA) technique. Multiple realisations of mock catalogues are crucial for analyses of large-scale structure, but conventional N-body simulations are too computationally expensive for the production of thousands of realizations. We show that COLA simulations can produce accurate mock catalogues with a moderate computation resource for low- to intermediate-mass galaxies in 1012 M⊙ haloes, both in real and redshift space. COLA simulations have accurate peculiar velocities, without systematic errors in the velocity power spectra for k ≤ 0.15 h Mpc-1, and with only 3-per cent error for k ≤ 0.2 h Mpc-1. We use COLA with 10 time steps and a Halo Occupation Distribution to produce 600 mock galaxy catalogues of the WiggleZ Dark Energy Survey. Our parallelized code for efficient generation of accurate halo catalogues is publicly available at github.com/junkoda/cola_halo.

  4. The REFLEX II Galaxy Cluster sample: mock catalogues and clustering analysis

    NASA Astrophysics Data System (ADS)

    Balaguera-Antolinez, Andres; Sanchez, Ariel G.; Bohringer, Hans

    2012-09-01

    We present results of the analysis of abundance and clustering from the new ROSAT-ESO Flux-Limited X-Ray (REFLEX) II galaxy cluster catalogue. To model the covariance matrix of the different statistics, we have created a set of 100 mock galaxy cluster catalogues built from a suite large volume LambdaCDM N-Body simulations (L-BASICC and calibrated with the X-ray luminosity function. We discuss the calibration scheme and some implications regarding the cluster scaling relations, particularly, the link between mass and luminosity. Similarly we show the behavior of the clustering signal as a function of the X-ray luminosity and some cosmological implications.

  5. Redshift weights for baryon acoustic oscillations: application to mock galaxy catalogues

    NASA Astrophysics Data System (ADS)

    Zhu, Fangzhou; Padmanabhan, Nikhil; White, Martin; Ross, Ashley J.; Zhao, Gongbo

    2016-09-01

    Large redshift surveys capable of measuring the baryon acoustic oscillation (BAO) signal have proven to be an effective way of measuring the distance-redshift relation in cosmology. Building off the work in Zhu et al., we develop a technique to directly constrain the distance-redshift relation from BAO measurements without splitting the sample into redshift bins. We apply the redshift weighting technique in Zhu et al. to the clustering of galaxies from 1000 Quick particle mesh (QPM) mock simulations after reconstruction and achieve a 0.75 per cent measurement of the angular diameter distance DA at z = 0.64 and the same precision for Hubble parameter H at z = 0.29. These QPM mock catalogues mimic the clustering and noise level of the Baryon Oscillation Spectroscopic Survey Data Release 12 (DR12). We compress the correlation functions in the redshift direction on to a set of weighted correlation functions. These estimators give unbiased DA and H measurements across the entire redshift range of the combined sample. We demonstrate the effectiveness of redshift weighting in improving the distance and Hubble parameter estimates. Instead of measuring at a single `effective' redshift as in traditional analyses, we report our DA and H measurements at all redshifts. The measured fractional error of DA ranges from 1.53 per cent at z = 0.2 to 0.75 per cent at z = 0.64. The fractional error of H ranges from 0.75 per cent at z = 0.29 to 2.45 per cent at z = 0.7. Our measurements are consistent with a Fisher forecast to within 10-20 per cent depending on the pivot redshift. We further show the results are robust against the choice of fiducial cosmologies, galaxy bias models, and redshift-space distortions streaming parameters.

  6. Lightcone mock catalogues from semi-analytic models of galaxy formation - I. Construction and application to the BzK colour selection

    NASA Astrophysics Data System (ADS)

    Merson, Alexander I.; Baugh, Carlton M.; Helly, John C.; Gonzalez-Perez, Violeta; Cole, Shaun; Bielby, Richard; Norberg, Peder; Frenk, Carlos S.; Benson, Andrew J.; Bower, Richard G.; Lacey, Cedric G.; Lagos, Claudia del P.

    2013-02-01

    We introduce a method for constructing end-to-end mock galaxy catalogues using a semi-analytical model of galaxy formation, applied to the halo merger trees extracted from a cosmological N-body simulation. The mocks that we construct are lightcone catalogues, in which a galaxy is placed according to the epoch at which it first enters the past lightcone of the observer, and incorporate the evolution of galaxy properties with cosmic time. We determine the position between the snapshot outputs at which a galaxy enters the observer's lightcone by interpolation. As an application, we consider the effectiveness of the BzK colour selection technique, which was designed to isolate galaxies in the redshift interval 1.4 < z < 2.5. The mock catalogue is in reasonable agreement with the observed number counts of all BzK galaxies, as well as with the observed counts of the subsample of BzKs that are star-forming galaxies. We predict that over 75 per cent of the model galaxies with KAB ≤ 23, and 1.4 < z < 2.5, are selected by the BzK technique. Interloper galaxies, outside the intended redshift range, are predicted to dominate bright samples of BzK galaxies (i.e. with KAB ≤ 21). Fainter K-band cuts are necessary to reduce the predicted interloper fraction. We also show that shallow B-band photometry can lead to confusion in classifying BzK galaxies as being star forming or passively evolving. Overall, we conclude that the BzK colour selection technique is capable of providing a sample of galaxies that is representative of the 1.4 < z < 2.5 galaxy population.

  7. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release

    NASA Astrophysics Data System (ADS)

    Kitaura, Francisco-Shu; Rodríguez-Torres, Sergio; Chuang, Chia-Hsun; Zhao, Cheng; Prada, Francisco; Gil-Marín, Héctor; Guo, Hong; Yepes, Gustavo; Klypin, Anatoly; Scóccola, Claudia G.; Tinker, Jeremy; McBride, Cameron; Reid, Beth; Sánchez, Ariel G.; Salazar-Albornoz, Salvador; Grieb, Jan Niklas; Vargas-Magana, Mariana; Cuesta, Antonio J.; Neyrinck, Mark; Beutler, Florian; Comparat, Johan; Percival, Will J.; Ross, Ashley

    2016-03-01

    We reproduce the galaxy clustering catalogue from the SDSS-III Baryon Oscillation Spectroscopic Survey Final Data Release (BOSS DR11&DR12) with high fidelity on all relevant scales in order to allow a robust analysis of baryon acoustic oscillations and redshift space distortions. We have generated (6000) 12 288 MultiDark PATCHY BOSS (DR11) DR12 light cones corresponding to an effective volume of ˜192 000 [h-1 Gpc]3 (the largest ever simulated volume), including cosmic evolution in the redshift range from 0.15 to 0.75. The mocks have been calibrated using a reference galaxy catalogue based on the halo abundance matching modelling of the BOSS DR11&DR12 galaxy clustering data and on the data themselves. The production follows three steps. First, we apply the PATCHY code to generate a dark matter field and an object distribution including non-linear stochastic galaxy bias. Secondly, we run the halo/stellar distribution reconstruction HADRON code to assign masses to the various objects. This step uses the mass distribution as a function of local density and non-local indicators (i.e. tidal field tensor eigenvalues and relative halo exclusion separation for massive objects) from the reference simulation applied to the corresponding patchy dark matter and galaxy distribution. Finally, we apply the SUGAR code to build the light cones. The resulting MultiDarkPATCHY mock light cones reproduce the number density, selection function, survey geometry, and in general within 1σ, for arbitrary stellar mass bins, the power spectrum up to k = 0.3 h Mpc-1, the two-point correlation functions down to a few Mpc scales, and the three-point statistics of the BOSS DR11&DR12 galaxy samples.

  8. Creating mock catalogues of stellar haloes from cosmological simulations

    NASA Astrophysics Data System (ADS)

    Lowing, Ben; Wang, Wenting; Cooper, Andrew; Kennedy, Rachel; Helly, John; Cole, Shaun; Frenk, Carlos

    2015-01-01

    We present a new technique for creating mock catalogues of the individual stars that make up the accreted component of stellar haloes in cosmological simulations and show how the catalogues can be used to test and interpret observational data. The catalogues are constructed from a combination of methods. A semi-analytic galaxy formation model is used to calculate the star formation history in haloes in an N-body simulation and dark matter particles are tagged with this stellar mass. The tags are converted into individual stars using a stellar population synthesis model to obtain the number density and evolutionary stage of the stars, together with a phase-space sampling method that distributes the stars while ensuring that the phase-space structure of the original N-body simulation is maintained. A set of catalogues based on the Λ cold dark matter Aquarius simulations of Milky Way mass haloes have been created and made publicly available on a website. Two example applications are discussed that demonstrate the power and flexibility of the mock catalogues. We show how the rich stellar substructure that survives in the stellar halo precludes a simple measurement of its density profile and demonstrate explicitly how pencil-beam surveys can return almost any value for the slope of the profile. We also show that localized variations in the abundance of particular types of stars, a signature of differences in the composition of stellar populations, allow streams to be easily identified.

  9. Minimization of biases in galaxy peculiar velocity catalogues

    NASA Astrophysics Data System (ADS)

    Sorce, Jenny G.

    2015-07-01

    Galaxy distances and derived radial peculiar velocity catalogues constitute valuable data sets to study the dynamics of the Local Universe. However, such catalogues suffer from biases whose effects increase with the distance. Malmquist biases and lognormal error distribution affect the catalogues. Velocity fields of the Local Universe reconstructed with these catalogues present a spurious overall infall on to the Local Volume if they are not corrected for biases. Such an infall is observed in the reconstructed velocity field obtained when applying the Bayesian Wiener-Filter technique to the raw second radial peculiar velocity catalogue of the Cosmicflows project. In this paper, an iterative method to reduce spurious non-Gaussianities in the radial peculiar velocity distribution, to retroactively derive overall better distance estimates resulting in a minimization of the effects of biases, is presented. This method is tested with mock catalogues. To control the cosmic variance, mocks are built out of different cosmological constrained simulations which resemble the Local Universe. To realistically reproduce the effects of biases, the mocks are constructed to be lookalikes of the second data release of the Cosmicflows project, with respect to the size, distribution of data and distribution of errors. Using a suite of mock catalogues, the outcome of the correction is verified to be affected neither by the added error realization, nor by the data point selection, nor by the constrained simulation. Results are similar for the different tested mocks. After correction, the general infall is satisfactorily suppressed. The method allows us to obtain catalogues which together with the Wiener-Filter technique give reconstructions approximating non-biased velocity fields at 100-150 km s-1 (2-3 h-1 Mpc in terms of linear displacement), the linear theory threshold.

  10. HALOGEN: a tool for fast generation of mock halo catalogues

    NASA Astrophysics Data System (ADS)

    Avila, Santiago; Murray, Steven G.; Knebe, Alexander; Power, Chris; Robotham, Aaron S. G.; Garcia-Bellido, Juan

    2015-06-01

    We present a simple method of generating approximate synthetic halo catalogues: HALOGEN. This method uses a combination of second-order Lagrangian Perturbation Theory (2LPT) in order to generate the large-scale matter distribution, analytical mass functions to generate halo masses, and a single-parameter stochastic model for halo bias to position haloes. HALOGEN represents a simplification of similar recently published methods. Our method is constrained to recover the two-point function at intermediate (10 h-1 Mpc < r < 50 h-1 Mpc) scales, which we show is successful to within 2 per cent. Larger scales (˜100 h-1 Mpc) are reproduced to within 15 per cent. We compare several other statistics (e.g. power spectrum, point distribution function, redshift space distortions) with results from N-body simulations to determine the validity of our method for different purposes. One of the benefits of HALOGEN is its flexibility, and we demonstrate this by showing how it can be adapted to varying cosmologies and simulation specifications. A driving motivation for the development of such approximate schemes is the need to compute covariance matrices and study the systematic errors for large galaxy surveys, which requires thousands of simulated realizations. We discuss the applicability of our method in this context, and conclude that it is well suited to mass production of appropriate halo catalogues. The code is publicly available at https://github.com/savila/halogen.

  11. Galaxy simulations: Kinematics and mock observations

    NASA Astrophysics Data System (ADS)

    Moody, Christopher E.

    2013-08-01

    There are six topics to my thesis, which are: (1) slow rotator production in varied simulation schemes and kinematically decoupled cores and twists in those simulations, (2) the change in number of clumps in radiation pressure and no-radiation pressure simulations, (3) Sunrise experiments and failures including UVJ color-color dust experiments and UVbeta slopes, (4) the Sunrise image pipeline and algorithms. Cosmological simulations of have typically produced too many stars at early times. We find that the additional radiation pressure (RP) feedback suppresses star formation globally by a factor of ~ 3. Despite this reduction, the simulation still overproduces stars by a factor of ~ 2 with respect to the predictions provided by abundance matching methods. In simulations with RP the number of clumps falls dramatically. However, only clumps with masses Mclump/Mdisk ≤ 8% are impacted by the inclusion of RP, and clump counts above this range are comparable. Above this mass, the difference between and RP and no-RP contrast ratios diminishes. If we restrict our selection to galaxies hosting at least a single clump above this mass range then clump numbers, contrast ratios, survival fractions and total clump masses show little discrepancy between RP and no-RP simulations. By creating mock Hubble Space Telescope observations we find that the number of clumps is slightly reduced in simulations with RP. We demonstrate that clumps found in any single gas, stellar, or mock observation image are not necessarily clumps found in another map, and that there are few clumps common to multiple maps. New kinematic observations from ATLAS3D have highlighted the need to understand the evolutionary mechanism leading to a spectrum of fast-rotator and slow-rotators in early-type galaxies. We address the formation of slow and fast rotators through a series of controlled, comprehensive hydrodynamic simulations sampling idealized galaxy merger formation scenarios constructed from model

  12. Testing cosmology with a catalogue of voids in the BOSS galaxy surveys

    NASA Astrophysics Data System (ADS)

    Nadathur, Seshadri

    2016-09-01

    We present a public catalogue of voids in the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 11 LOWZ and CMASS galaxy surveys. This catalogue contains information on the location, sizes, densities, shapes and bounding surfaces of 8956 independent, disjoint voids, making it the largest public void catalogue to date. Voids are identified using a version of the ZOBOV algorithm, the operation of which has been calibrated though tests on mock galaxy populations in N-body simulations, as well as on a suite of 4096 mock catalogues which fully reproduce the galaxy clustering, survey masks and selection functions. Based on this, we estimate a false positive detection rate of 3 per cent. Comparison with mock catalogues limits deviations of the void size distribution from that predicted in the ΛCDM model to be less than 6 per cent for voids with effective radius 8 < Rv < 60 h-1Mpc and in the redshift range 0.15 < z < 0.7. This could tightly constrain modified gravity scenarios and models with a varying equation of state, but we identify systematic biases which must be accounted for to reduce the theoretical uncertainty in the predictions for these models to the current level of precision attained from the data. We also examine the distribution of void densities and identify a deficit of the deepest voids relative to ΛCDM expectations, which is significant at more than the 3σ equivalent level. We discuss possible explanations for this discrepancy but at present its cause remains unknown.

  13. The Theoretical Astrophysical Observatory: Cloud-based Mock Galaxy Catalogs

    NASA Astrophysics Data System (ADS)

    Bernyk, Maksym; Croton, Darren J.; Tonini, Chiara; Hodkinson, Luke; Hassan, Amr H.; Garel, Thibault; Duffy, Alan R.; Mutch, Simon J.; Poole, Gregory B.; Hegarty, Sarah

    2016-03-01

    We introduce the Theoretical Astrophysical Observatory (TAO), an online virtual laboratory that houses mock observations of galaxy survey data. Such mocks have become an integral part of the modern analysis pipeline. However, building them requires expert knowledge of galaxy modeling and simulation techniques, significant investment in software development, and access to high performance computing. These requirements make it difficult for a small research team or individual to quickly build a mock catalog suited to their needs. To address this TAO offers access to multiple cosmological simulations and semi-analytic galaxy formation models from an intuitive and clean web interface. Results can be funnelled through science modules and sent to a dedicated supercomputer for further processing and manipulation. These modules include the ability to (1) construct custom observer light cones from the simulation data cubes; (2) generate the stellar emission from star formation histories, apply dust extinction, and compute absolute and/or apparent magnitudes; and (3) produce mock images of the sky. All of TAO’s features can be accessed without any programming requirements. The modular nature of TAO opens it up for further expansion in the future.

  14. The EAGLE simulations of galaxy formation: Public release of halo and galaxy catalogues

    NASA Astrophysics Data System (ADS)

    McAlpine, S.; Helly, J. C.; Schaller, M.; Trayford, J. W.; Qu, Y.; Furlong, M.; Bower, R. G.; Crain, R. A.; Schaye, J.; Theuns, T.; Dalla Vecchia, C.; Frenk, C. S.; McCarthy, I. G.; Jenkins, A.; Rosas-Guevara, Y.; White, S. D. M.; Baes, M.; Camps, P.; Lemson, G.

    2016-04-01

    We present the public data release of halo and galaxy catalogues extracted from the EAGLE suite of cosmological hydrodynamical simulations of galaxy formation. These simulations were performed with an enhanced version of the GADGET code that includes a modified hydrodynamics solver, time-step limiter and subgrid treatments of baryonic physics, such as stellar mass loss, element-by-element radiative cooling, star formation and feedback from star formation and black hole accretion. The simulation suite includes runs performed in volumes ranging from 25 to 100 comoving megaparsecs per side, with numerical resolution chosen to marginally resolve the Jeans mass of the gas at the star formation threshold. The free parameters of the subgrid models for feedback are calibrated to the redshift z = 0 galaxy stellar mass function, galaxy sizes and black hole mass-stellar mass relation. The simulations have been shown to match a wide range of observations for present-day and higher-redshift galaxies. The raw particle data have been used to link galaxies across redshifts by creating merger trees. The indexing of the tree produces a simple way to connect a galaxy at one redshift to its progenitors at higher redshift and to identify its descendants at lower redshift. In this paper we present a relational database which we are making available for general use. A large number of properties of haloes and galaxies and their merger trees are stored in the database, including stellar masses, star formation rates, metallicities, photometric measurements and mock gri images. Complex queries can be created to explore the evolution of more than 105 galaxies, examples of which are provided in the Appendix. The relatively good and broad agreement of the simulations with a wide range of observational datasets makes the database an ideal resource for the analysis of model galaxies through time, and for connecting and interpreting observational datasets.

  15. Maximum likelihood random galaxy catalogues and luminosity function estimation

    NASA Astrophysics Data System (ADS)

    Cole, Shaun

    2011-09-01

    We present a new algorithm to generate a random (unclustered) version of an magnitude limited observational galaxy redshift catalogue. It takes into account both galaxy evolution and the perturbing effects of large-scale structure. The key to the algorithm is a maximum likelihood (ML) method for jointly estimating both the luminosity function (LF) and the overdensity as a function of redshift. The random catalogue algorithm then works by cloning each galaxy in the original catalogue, with the number of clones determined by the ML solution. Each of these cloned galaxies is then assigned a random redshift uniformly distributed over the accessible survey volume, taking account of the survey magnitude limit(s) and, optionally, both luminosity and number density evolution. The resulting random catalogues, which can be employed in traditional estimates of galaxy clustering, make fuller use of the information available in the original catalogue and hence are superior to simply fitting a functional form to the observed redshift distribution. They are particularly well suited to studies of the dependence of galaxy clustering on galaxy properties as each galaxy in the random catalogue has the same list of attributes as measured for the galaxies in the genuine catalogue. The derivation of the joint overdensity and LF estimator reveals the limit in which the ML estimate reduces to the standard 1/Vmax LF estimate, namely when one makes the prior assumption that the are no fluctuations in the radial overdensity. The new ML estimator can be viewed as a generalization of the 1/Vmax estimate in which Vmax is replaced by a density corrected Vdc, max.

  16. Mocking the ECO and RESOLVE Surveys: Probing the Environmental Dependencies of Galaxy Properties

    NASA Astrophysics Data System (ADS)

    Berlind, Andreas A.; Florez, Jonathan; Calderon, Victor; Sinha, Manodeep; Moffett, Amanda J.; Eckert, Kathleen D.; Kannappan, Sheila; Stark, David; Baker, Ashley; RESOLVE Team

    2016-01-01

    We present mock catalogs for the RESOLVE survey and the associated Environmental COntext (ECO) catalog. The mock catalogs are constructed by populating dark matter halos in cosmological N-body simulations with galaxies using prescriptions that yield the same joint distributions of galaxy properties and overall clustering strength as seen in the ECO catalog. Specifically, we use a combination of Halo Occupation Distribution (HOD), Conditional Luminosity Function (CLF), and abundance matching techniques to connect mock galaxies to halos and we adopt different assumptions of how observable properties correlate with the properties of the underlying halos. We use the resulting mock catalogs to assess systematic errors in environmental metrics, such as errors in the inferred masses of galaxy groups that are due to group over-merging or fragmentation. We also use the mock catalogs to compare to an interesting trend that we find for galaxies that live in the 10% lowest density environments in ECO and RESOLVE. In the observations, we find that, at fixed stellar or baryonic mass, these galaxies in low density regions are bluer, more star forming, and more gas rich than galaxies residing in higher density environments. Some mock-making prescriptions are more successful than others in matching this observed trend, highlighting the power of mock catalogs to connect observations to the underlying relationships between galaxies and their dark matter halos. The RESOLVE survey is supported by NSF grant AST-0955368.

  17. Galaxy triplets in Sloan Digital Sky Survey Data Release 7 - I. Catalogue

    NASA Astrophysics Data System (ADS)

    O'Mill, Ana Laura; Duplancic, Fernanda; García Lambas, Diego; Valotto, Carlos; Sodré, Laerte

    2012-04-01

    We present a new catalogue of galaxy triplets derived from the Sloan Digital Sky Survey (SDSS) Data Release 7. The identification of systems was performed considering galaxies brighter than Mr=-20.5 and imposing constraints over the projected distances, radial velocity differences of neighbouring galaxies and isolation. To improve the identification of triplets, we employed a data pixelization scheme, which allows us to handle large amounts of data as in the SDSS photometric survey. Using spectroscopic and photometric data in the redshift range 0.01 ≤z≤ 0.40, we obtain 5901 triplet candidates. We have used a mock catalogue to analyse the completeness and contamination of our methods. The results show a high level of completeness (˜80 per cent) and low contamination (˜5 per cent). By using photometric and spectroscopic data, we have also addressed the effects of fibre collisions in the spectroscopic sample. We have defined an isolation criterion considering the distance of the triplet brightest galaxy to the closest neighbour cluster, to describe a global environment, as well as the galaxies within a fixed aperture, around the triplet brightest galaxy, to measure the local environment. The final catalogue comprises 1092 isolated triplets of galaxies in the redshift range 0.01 ≤z≤ 0.40. Our results show that photometric redshifts provide very useful information, allowing us to complete the sample of nearby systems whose detection is affected by fibre collisions, as well as extending the detection of triplets to large distances, where spectroscopic redshifts are not available.

  18. IMPROVED MOCK GALAXY CATALOGS FOR THE DEEP2 GALAXY REDSHIFT SURVEY FROM SUBHALO ABUNDANCE AND ENVIRONMENT MATCHING

    SciTech Connect

    Gerke, Brian F.; Wechsler, Risa H.; Behroozi, Peter S.; Yan, Renbin; Coil, Alison L.

    2013-09-15

    We develop empirical methods for modeling the galaxy population and populating cosmological N-body simulations with mock galaxies according to the observed properties of galaxies in survey data. We use these techniques to produce a new set of mock catalogs for the DEEP2 Galaxy Redshift Survey based on the output of the high-resolution Bolshoi simulation, as well as two other simulations with different cosmological parameters, all of which we release for public use. The mock-catalog creation technique uses subhalo abundance matching to assign galaxy luminosities to simulated dark-matter halos. It then adds color information to the resulting mock galaxies in a manner that depends on the local galaxy density, in order to reproduce the measured color-environment relation in the data. In the course of constructing the catalogs, we test various models for including scatter in the relation between halo mass and galaxy luminosity, within the abundance-matching framework. We find that there is no constant-scatter model that can simultaneously reproduce both the luminosity function and the autocorrelation function of DEEP2. This result has implications for galaxy-formation theory, and it restricts the range of contexts in which the mock catalogs can be usefully applied. Nevertheless, careful comparisons show that our new mock catalogs accurately reproduce a wide range of the other properties of the DEEP2 catalog, suggesting that they can be used to gain a detailed understanding of various selection effects in DEEP2.

  19. Optimal Weights For Measuring Redshift Space Distortions in Multi-tracer Galaxy Catalogues

    NASA Astrophysics Data System (ADS)

    Pearson, David W.; Samushia, Lado; Gagrani, Praful

    2016-08-01

    Since the volume accessible to galaxy surveys is fundamentally limited, it is extremely important to analyse available data in the most optimal fashion. One way of enhancing the cosmological information extracted from the clustering of galaxies is by weighting the galaxy field. The most widely used weighting schemes assign weights to galaxies based on the average local density in the region (FKP weights) and their bias with respect to the dark matter field (PVP weights). They are designed to minimize the fractional variance of the galaxy power-spectrum. We demonstrate that the currently used bias dependent weighting scheme can be further optimized for specific cosmological parameters. We develop a procedure for computing the optimal weights and test them against mock catalogues for which the values of all fitting parameters, as well as the input power-spectrum are known. We show that by applying these weights to the joint power-spectrum of Emission Line Galaxies and Luminous Red Galaxies from the Dark Energy Spectroscopic Instrument survey, the variance in the measured growth rate parameter can be reduced by as much as 36 per cent.

  20. The SuperCOSMOS all-sky galaxy catalogue

    NASA Astrophysics Data System (ADS)

    Peacock, J. A.; Hambly, N. C.; Bilicki, M.; MacGillivray, H. T.; Miller, L.; Read, M. A.; Tritton, S. B.

    2016-10-01

    We describe the construction of an all-sky galaxy catalogue, using SuperCOSMOS scans of Schmidt photographic plates from the UK Schmidt Telescope and Second Palomar Observatory Sky Survey. The photographic photometry is calibrated using Sloan Digital Sky Survey data, with results that are linear to 2 per cent or better. All-sky photometric uniformity is achieved by matching plate overlaps and also by requiring homogeneity in optical-to-2MASS colours, yielding zero-points that are uniform to 0.03 mag or better. The typical AB depths achieved are BJ < 21, RF < 19.5 and IN < 18.5, with little difference between hemispheres. In practice, the IN plates are shallower than the BJ and RF plates, so for most purposes we advocate the use of a catalogue selected in these two latter bands. At high Galactic latitudes, this catalogue is approximately 90 per cent complete with 5 per cent stellar contamination; we quantify how the quality degrades towards the Galactic plane. At low latitudes, there are many spurious galaxy candidates resulting from stellar blends: these approximately match the surface density of true galaxies at |b| = 30°. Above this latitude, the catalogue limited in BJ and RF contains in total about 20 million galaxy candidates, of which 75 per cent are real. This contamination can be removed, and the sky coverage extended, by matching with additional data sets. This SuperCOSMOS catalogue has been matched with 2MASS and with WISE, yielding quasi-all-sky samples of respectively 1.5 million and 18.5 million galaxies, to median redshifts of 0.08 and 0.20. This legacy data set thus continues to offer a valuable resource for large-angle cosmological investigations.

  1. The MICE Grand Challenge light-cone simulation - III. Galaxy lensing mocks from all-sky lensing maps

    NASA Astrophysics Data System (ADS)

    Fosalba, P.; Gaztañaga, E.; Castander, F. J.; Crocce, M.

    2015-02-01

    In Paper I of this series, we presented a new N-body light-cone simulation from the MICE Collaboration, the MICE Grand Challenge (MICE-GC), containing about 70 billion dark-matter particles in a (3 h-1 Gpc)3 comoving volume, from which we built halo and galaxy catalogues using a Halo Occupation Distribution and Halo Abundance Matching technique, as presented in the companion Paper II. Given its large volume and fine mass resolution, the MICE-GC simulation also allows an accurate modelling of the lensing observables from upcoming wide and deep galaxy surveys. In the last paper of this series (Paper III), we describe the construction of all-sky lensing maps, following the `Onion Universe' approach, and discuss their properties in the light-cone up to z = 1.4 with sub-arcminute spatial resolution. By comparing the convergence power spectrum in the MICE-GC to lower mass-resolution (i.e. particle mass ˜1011 h-1 M⊙) simulations, we find that resolution effects are at the 5 per cent level for multipoles ℓ ˜ 103 and 20 per cent for ℓ ˜ 104. Resolution effects have a much lower impact on our simulation, as shown by comparing the MICE-GC to recent numerical fits by Takahashi. We use the all-sky lensing maps to model galaxy lensing properties, such as the convergence, shear, and lensed magnitudes and positions, and validate them thoroughly using galaxy shear auto and cross-correlations in harmonic and configuration space. Our results show that the galaxy lensing mocks here presented can be used to accurately model lensing observables down to arcminute scales. Accompanying this series of papers, we make a first public data release of the MICE-GC galaxy mock, the MICECAT v1.0, through a dedicated web-portal for the MICE simulations, http://cosmohub.pic.es, to help developing and exploiting the new generation of astronomical surveys.

  2. VizieR Online Data Catalog: Galaxies in the Tycho-2 catalogue (Metz+, 2004)

    NASA Astrophysics Data System (ADS)

    Metz, M.; Geffert, M.

    2004-01-01

    We have identified galaxies in the Tycho-2 Catalogue (Cat. ) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. ) and the Tycho-2 positions of the galaxies. (1 data file).

  3. Galaxy And Mass Assembly (GAMA) blended spectra catalogue: strong galaxy-galaxy lens and occulting galaxy pair candidates

    NASA Astrophysics Data System (ADS)

    Holwerda, B. W.; Baldry, I. K.; Alpaslan, M.; Bauer, A.; Bland-Hawthorn, J.; Brough, S.; Brown, M. J. I.; Cluver, M. E.; Conselice, C.; Driver, S. P.; Hopkins, A. M.; Jones, D. H.; López-Sánchez, Á. R.; Loveday, J.; Meyer, M. J.; Moffett, A.

    2015-06-01

    We present the catalogue of blended galaxy spectra from the Galaxy And Mass Assembly (GAMA) survey. These are cases where light from two galaxies are significantly detected in a single GAMA fibre. Galaxy pairs identified from their blended spectrum fall into two principal classes: they are either strong lenses, a passive galaxy lensing an emission-line galaxy; or occulting galaxies, serendipitous overlaps of two galaxies, of any type. Blended spectra can thus be used to reliably identify strong lenses for follow-up observations (high-resolution imaging) and occulting pairs, especially those that are a late-type partly obscuring an early-type galaxy which are of interest for the study of dust content of spiral and irregular galaxies. The GAMA survey setup and its AUTOZ automated redshift determination were used to identify candidate blended galaxy spectra from the cross-correlation peaks. We identify 280 blended spectra with a minimum velocity separation of 600 km s-1, of which 104 are lens pair candidates, 71 emission-line-passive pairs, 78 are pairs of emission-line galaxies and 27 are pairs of galaxies with passive spectra. We have visually inspected the candidates in the Sloan Digital Sky Survey (SDSS) and Kilo Degree Survey (KiDS) images. Many blended objects are ellipticals with blue fuzz (Ef in our classification). These latter `Ef' classifications are candidates for possible strong lenses, massive ellipticals with an emission-line galaxy in one or more lensed images. The GAMA lens and occulting galaxy candidate samples are similar in size to those identified in the entire SDSS. This blended spectrum sample stands as a testament of the power of this highly complete, second-largest spectroscopic survey in existence and offers the possibility to expand e.g. strong gravitational lens surveys.

  4. An extensive catalogue of early-type galaxies in the nearby Universe

    NASA Astrophysics Data System (ADS)

    Dabringhausen, J.; Fellhauer, M.

    2016-08-01

    We present a catalogue of 1715 early-type galaxies from the literature, spanning the luminosity range from faint dwarf spheroidal galaxies to giant elliptical galaxies. The aim of this catalogue is to be one of the most comprehensive and publicly available collections of data on early-type galaxies. The emphasis in this catalogue lies on dwarf elliptical galaxies, for which some samples with detailed data have been published recently. For almost all of the early-type galaxies included in it, this catalogue contains data on their locations, distances, redshifts, half-light radii, the masses of their stellar populations and apparent magnitudes in various passbands. Data on metallicity and various colours are available for a majority of the galaxies presented here. The data on magnitudes, colours, metallicities and masses of the stellar populations are supplemented with entries that are based on fits to data from simple stellar population models and existing data from observations. Also, some simple transformations have been applied to the data on magnitudes, colours and metallicities in this catalogue, in order to increase the homogeneity of these data. Estimates on the Sérsic profiles, internal velocity dispersions, maximum rotational velocities, dynamical masses and ages are listed for several hundreds of the galaxies in this catalogue. Finally, each quantity listed in this catalogue is accompanied with information on its source, so that users of this catalogue can easily exclude data that they do not consider as reliable enough for their purposes.

  5. Apples to apples A2 - I. Realistic galaxy simulated catalogues and photometric redshift predictions for next-generation surveys

    NASA Astrophysics Data System (ADS)

    Ascaso, B.; Mei, S.; Benítez, N.

    2015-11-01

    We present new mock catalogues for two of the largest Stage IV next-generation surveys in the optical and infrared: Large Synoptic Sky Telescope (LSST) and Euclid, based on an N-body simulation+semi-analytical cone with a posterior modification with PHOTREAL. This technique modifies the original photometry by using an empirical library of spectral templates to make it more realistic. The reliability of the catalogues is confirmed by comparing the obtained colour-magnitude relation, the luminosity and mass function and the angular correlation function with those of real data. Consistent comparisons between the expected photometric redshifts for different surveys are also provided. Very deep near-infrared surveys such as Euclid will provide very good performance (Δz/(1 + z) ˜ 0.025-0.053) down to H ˜ 24 AB mag and up to z ˜ 3 depending on the optical observations available from the ground, whereas extremely deep optical surveys such as LSST will obtain an overall lower photometric redshift resolution (Δz/(1 + z) ˜ 0.045) down to i ˜ 27.5 AB mag, being considerably improved (Δz/(1 + z) ˜ 0.035) if we restrict the sample down to i ˜ 24 AB mag. Those numbers can be substantially upgraded by selecting a subsample of galaxies with the best quality photometric redshifts. We finally discuss the impact that these surveys will have for the community in terms of photometric redshift legacy. This is the first of a series of papers where we set a framework for comparability between mock catalogues and observations with a particular focus on cluster surveys. The Euclid and LSST mocks are made publicly available.

  6. Catalogue of far-infrared loops in the Galaxy

    NASA Astrophysics Data System (ADS)

    Könyves, V.; Kiss, Cs.; Moór, A.; Kiss, Z. T.; Tóth, L. V.

    2007-03-01

    Aims:An all-sky survey of loop- and arc-like intensity enhancements has been performed to investigate the large-scale structure of the diffuse far-infrared emission. Methods: We used maps made of 60 and 100 μm processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs, or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. Results: We identified 462 far-infrared loops, analysed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of fin ≈ 30% and fout ≈ 5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power-law size luminosity function β = 1.37 for low Galactic latitudes in the outer Milky Way. Conclusions: .Deviations in the celestial distribution of far-infrared loops clearly indicate that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power-law indices of size luminosity distributions suggest that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes, while it is governed by supersonic turbulence above the Galactic plane. Appendices B-D are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/463/1227

  7. Star-galaxy separation strategies for WISE-2MASS all-sky infrared galaxy catalogues

    NASA Astrophysics Data System (ADS)

    Kovács, András; Szapudi, István

    2015-04-01

    We combine photometric information of the Wide-Field Infrared Survey Explorer (WISE) and Two Micron All Sky Survey (2MASS) all-sky infrared data bases, and demonstrate how to produce clean and complete galaxy catalogues for future analyses. Adding 2MASS colours to WISE photometry improves star-galaxy separation efficiency substantially at the expense of losing a small fraction of the galaxies. We find that 93 per cent of the WISE objects within W1 < 15.2 mag have a 2MASS match, and that a class of supervised machine learning algorithms, support vector machines (SVM), are efficient classifiers of objects in our multicolour data set. We constructed a training set from the Sloan Digital Sky Survey PhotoObj table with known star-galaxy separation, and determined redshift distribution of our sample from the Galaxy and Mass Assembly spectroscopic survey. Varying the combination of photometric parameters input into our algorithm we show that W1WISE - J2MASS is a simple and effective star-galaxy separator, capable of producing results comparable to the multidimensional SVM classification. We present a detailed description of our star-galaxy separation methods, and characterize the robustness of our tools in terms of contamination, completeness, and accuracy. We explore systematics of the full sky WISE-2MASS galaxy map, such as contamination from moon glow. We show that the homogeneity of the full sky galaxy map is improved by an additional J2MASS < 16.5 mag flux limit. The all-sky galaxy catalogue we present in this paper covers 21 200 deg2 with dusty regions masked out, and has an estimated stellar contamination of 1.2 per cent and completeness of 70.1 per cent among 2.4 million galaxies with zmed ≈ 0.14. WISE-2MASS galaxy maps with well controlled stellar contamination will be useful for spatial statistical analyses, including cross-correlations with other cosmological random fields, such as the cosmic microwave background. The same techniques also yield a

  8. Measuring the neutrino mass from future wide galaxy cluster catalogues

    SciTech Connect

    Carbone, Carmelita; Moscardini, Lauro; Cimatti, Andrea; Fedeli, Cosimo E-mail: cosimo.fedeli@astro.ufl.edu E-mail: a.cimatti@unibo.it

    2012-03-01

    We present forecast errors on a wide range of cosmological parameters obtained from a photometric cluster catalogue of a future wide-field Euclid-like survey. We focus in particular on the total neutrino mass as constrained by a combination of the galaxy cluster number counts and correlation function. For the latter we consider only the shape information and the Baryon Acoustic Oscillations (BAO), while marginalising over the spectral amplitude and the redshift space distortions. In addition to the cosmological parameters of the standard ΛCDM+ν model we also consider a non-vanishing curvature, and two parameters describing a redshift evolution for the dark energy equation of state. For completeness, we also marginalise over a set of ''nuisance'' parameters, representing the uncertainties on the cluster mass determination. We find that combining cluster counts with power spectrum information greatly improves the constraining power of each probe taken individually, with errors on cosmological parameters being reduced by up to an order of magnitude. In particular, the best improvements are for the parameters defining the dynamical evolution of dark energy, where cluster counts break degeneracies. Moreover, the resulting error on neutrino mass is at the level of σ(M{sub ν}) ∼ 0.9 eV, comparable with that derived from present Lyα forest measurements and Cosmic Microwave background (CMB) data in the framework of a non-flat Universe. Further adopting Planck priors and reducing the number of free parameters to a ΛCDM+ν cosmology allows to place constraints on the total neutrino mass of σ(M{sub ν}) ∼ 0.08 eV, close to the lower bound enforced by neutrino oscillation experiments. Finally, in the optimistic case where uncertainties in the calibration of the mass-observable relation were so small to be neglected, the combination of Planck priors with cluster counts and power spectrum would constrain the total neutrino mass down to σ(M{sub ν}) ∼ 0.034 eV, i

  9. MegaZ-LRG: a photometric redshift catalogue of one million SDSS luminous red galaxies

    NASA Astrophysics Data System (ADS)

    Collister, Adrian; Lahav, Ofer; Blake, Chris; Cannon, Russell; Croom, Scott; Drinkwater, Michael; Edge, Alastair; Eisenstein, Daniel; Loveday, Jon; Nichol, Robert; Pimbblet, Kevin; de Propris, Roberto; Roseboom, Isaac; Ross, Nic; Schneider, Donald P.; Shanks, Tom; Wake, David

    2007-02-01

    We describe the construction of MegaZ-LRG, a photometric redshift catalogue of over one million luminous red galaxies (LRGs) in the redshift range 0.4 < z < 0.7 with limiting magnitude i < 20. The catalogue is selected from the imaging data of the Sloan Digital Sky Survey (SDSS) Data Release 4. The 2dF-SDSS LRG and Quasar (2SLAQ) spectroscopic redshift catalogue of 13000 intermediate-redshift LRGs provides a photometric redshift training set, allowing use of ANNz, a neural network-based photometric-redshift estimator. The rms photometric redshift accuracy obtained for an evaluation set selected from the 2SLAQ sample is σz = 0.049 averaged over all galaxies, and σz = 0.040 for a brighter subsample (i < 19.0). The catalogue is expected to contain ~5 per cent stellar contamination. The ANNz code is used to compute a refined star/galaxy probability based on a range of photometric parameters; this allows the contamination fraction to be reduced to 2 per cent with negligible loss of genuine galaxies. The MegaZ-LRG catalogue is publicly available on the World Wide Web from http://www.2slaq.info.

  10. Populating dark matter haloes with galaxies: comparing the 2dFGRS with mock galaxy redshift surveys

    NASA Astrophysics Data System (ADS)

    Yang, Xiaohu; Mo, H. J.; Jing, Y. P.; van den Bosch, Frank C.; Chu, YaoQuan

    2004-06-01

    In two recent papers, we developed a powerful technique to link the distribution of galaxies to that of dark matter haloes by considering halo occupation numbers as a function of galaxy luminosity and type. In this paper we use these distribution functions to populate dark matter haloes in high-resolution N-body simulations of the standard ΛCDM cosmology with Ωm= 0.3, ΩΛ= 0.7 and σ8= 0.9. Stacking simulation boxes of 100 h-1 Mpc and 300 h-1 Mpc with 5123 particles each we construct mock galaxy redshift surveys out to a redshift of z= 0.2 with a numerical resolution that guarantees completeness down to 0.01L*. We use these mock surveys to investigate various clustering statistics. The predicted two-dimensional correlation function ξ(rp, π) reveals clear signatures of redshift space distortions. The projected correlation functions for galaxies with different luminosities and types, derived from ξ(rp, π), match the observations well on scales larger than ~3 h-1 Mpc. On smaller scales, however, the model overpredicts the clustering power by about a factor two. Modelling the `finger-of-God' effect on small scales reveals that the standard ΛCDM model predicts pairwise velocity dispersions (PVD) that are ~400 km s-1 too high at projected pair separations of ~1 h-1 Mpc. A strong velocity bias in massive haloes, with bvel≡σgal/σdm~ 0.6 (where σgal and σdm are the velocity dispersions of galaxies and dark matter particles, respectively) can reduce the predicted PVD to the observed level, but does not help to resolve the overprediction of clustering power on small scales. Consistent results can be obtained within the standard ΛCDM model only when the average mass-to-light ratio of clusters is of the order of 1000 (M/L)solar in the B-band. Alternatively, as we show by a simple approximation, a ΛCDM model with σ8~= 0.75 may also reproduce the observational results. We discuss our results in light of the recent WMAP results and the constraints on σ8 obtained

  11. The MCXC: a meta-catalogue of x-ray detected clusters of galaxies

    NASA Astrophysics Data System (ADS)

    Piffaretti, R.; Arnaud, M.; Pratt, G. W.; Pointecouteau, E.; Melin, J.-B.

    2011-10-01

    We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4 keV band luminosity L500, total mass M500, and radius R500. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is available in electronic format for maximum usefulness in X-ray, SZ, and other multiwavelength studies. The catalog is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/534/A109

  12. The Millennium Galaxy Catalogue: the space density and surface-brightness distribution(s) of galaxies

    NASA Astrophysics Data System (ADS)

    Driver, S. P.; Liske, J.; Cross, N. J. G.; De Propris, R.; Allen, P. D.

    2005-06-01

    We recover the joint and individual space density and surface-brightness distribution(s) of galaxies from the Millennium Galaxy Catalogue (MGC). The MGC is a local survey spanning 30.9 deg2 and probing approximately 1-2 mag arcsec-2 deeper than either the Two-Degree Field Galaxy Redshift Survey (2dFGRS) or the Sloan Digital Sky Survey (SDSS). The MGC contains 10095 galaxies to BMGC < 20 mag with 96 per cent spectroscopic completeness. For each galaxy we derive individual K-corrections and seeing-corrected sizes. We implement a joint luminosity-surface-brightness step-wise maximum-likelihood method to recover the bivariate brightness distribution (BBD) inclusive of most selection effects. Integrating the BBD over surface brightness we recover the following Schechter function parameters: φ*= (0.0177 +/- 0.0015)h3Mpc-3, M*BMGC- 5 log h= (-19.60 +/- 0.04) mag and α=-1.13 +/- 0.02. Compared to the 2dFGRS we find a consistent M* value but a slightly flatter faint-end slope and a higher normalization, resulting in a final luminosity density jbJ= (1.99 +/- 0.17) × 108hLsolarMpc-3- marginally higher than, but consistent with, the earlier 2dFGRS, ESP, and SDSS z= 0.1 results. The MGC is inconsistent with the SDSS z= 0.0 result (+3σ) if one adopts the derived SDSS evolution. The MGC surface-brightness distribution is a well-bounded Gaussian at the M* point with φ*= (3.5 +/- 0.1) × 10-2h3Mpc-3, μe*= (21.90 +/- 0.01) mag arcsec-2 and σln Re= 0.35 +/- 0.01. The characteristic surface brightness for luminous systems is invariant to MBMGC- 5 log h~-19 mag faintwards of which it moves to lower surface brightness. The surface-brightness distribution also broadens (σln Re~ 0.5 - 0.7) towards lower luminosities. The luminosity dependence of σln Re provides a new constraint for both the theoretical development and numerical simulations, which typically predict a mass-independent σlnRe~ 0.56 +/- 0.04. Higher resolution (FWHM << 1 arcsec) and deeper (μlim>> 26 mag arcsec-2 in

  13. The MICE Grand Challenge lightcone simulation - II. Halo and galaxy catalogues

    NASA Astrophysics Data System (ADS)

    Crocce, M.; Castander, F. J.; Gaztañaga, E.; Fosalba, P.; Carretero, J.

    2015-10-01

    This is the second in a series of three papers in which we present an end-to-end simulation from the MICE collaboration, the MICE Grand Challenge (MICE-GC) run. The N-body contains about 70 billion dark-matter particles in a (3 h-1 Gpc)3 comoving volume spanning five orders of magnitude in dynamical range. Here, we introduce the halo and galaxy catalogues built upon it, both in a wide (5000 deg2) and deep (z < 1.4) lightcone and in several comoving snapshots. Haloes were resolved down to few 1011 h-1 M⊙. This allowed us to model galaxies down to absolute magnitude Mr < -18.9. We used a new hybrid halo occupation distribution and abundance matching technique for galaxy assignment. The catalogue includes the spectral energy distributions of all galaxies. We describe a variety of halo and galaxy clustering applications. We discuss how mass resolution effects can bias the large-scale two-pt clustering amplitude of poorly resolved haloes at the ≲5 per cent level, and their three-pt correlation function. We find a characteristic scale-dependent bias of ≲6 per cent across the BAO feature for haloes well above M⋆ ˜ 1012 h-1 M⊙ and for luminous red galaxy like galaxies. For haloes well below M⋆ the scale dependence at 100 h-1 Mpc is ≲2 per cent. Lastly, we discuss the validity of the large-scale Kaiser limit across redshift and departures from it towards non-linear scales. We make the current version of the lightcone halo and galaxy catalogue (MICECATv1.0) publicly available through a dedicated web portal to help develop and exploit the new generation of astronomical surveys.

  14. Catalogues of isolated galaxies, isolated pairs, and isolated triplets in the local Universe

    NASA Astrophysics Data System (ADS)

    Argudo-Fernández, M.; Verley, S.; Bergond, G.; Duarte Puertas, S.; Ramos Carmona, E.; Sabater, J.; Fernández Lorenzo, M.; Espada, D.; Sulentic, J.; Ruiz, J. E.; Leon, S.

    2015-06-01

    Context. The construction of catalogues of galaxies and the a posteriori study of galaxy properties in relation to their environment have been hampered by scarce redshift information. The new 3-dimensional (3D) surveys permit small, faint, physically bound satellites to be distinguished from a background-projected galaxy population, giving a more comprehensive 3D picture of the surroundings. Aims: We aim to provide representative samples of isolated galaxies, isolated pairs, and isolated triplets for testing galaxy evolution and secular processes in low density regions of the local Universe, as well as to characterise their local and large-scale environments. Methods: We used spectroscopic data from the tenth data release of the Sloan Digital Sky Survey (SDSS-DR10) to automatically and homogeneously compile catalogues of 3702 isolated galaxies, 1240 isolated pairs, and 315 isolated triplets in the local Universe (z ≤ 0.080). To quantify the effects of their local and large-scale environments, we computed the projected density and the tidal strength for the brightest galaxy in each sample. Results: We find evidence of isolated pairs and isolated triplets that are physically bound at projected separations up to d ≤ 450 kpc with radial velocity difference Δν ≤ 160 km s-1, where the effect of the companion typically accounts for more than 98% of the total tidal strength affecting the central galaxy. For galaxies in the catalogues, we provide their positions, redshifts, and degrees of relation with their physical and large-scale environments. The catalogues are publicly available to the scientific community. Conclusions: For isolated galaxies, isolated pairs, and isolated triplets, there is no difference in their degree of interaction with the large-scale structure (up to 5 Mpc), which may suggest that they have a common origin in their formation and evolution. We find that most of them belong to the outer parts of filaments, walls, and clusters, and generally

  15. CoMaLit - III. Literature catalogues of weak lensing clusters of galaxies (LC2)

    NASA Astrophysics Data System (ADS)

    Sereno, Mauro

    2015-07-01

    The measurement of the mass of clusters of galaxies is crucial for their use in cosmology and astrophysics. Masses can be efficiently determined with weak lensing (WL) analyses. I compiled literature catalogues of WL clusters (LC2). Cluster identifiers, coordinates, and redshifts have been standardized. WL masses were reported to over-densities of 2500, 500, 200, and to the virial one in the reference ΛCDM model. Duplicate entries were carefully handled. I produced three catalogues: LC2-single, with 485 unique groups and clusters analysed with the single-halo model; LC2-substructure, listing substructures in complex systems; LC2-all, listing all the 822 WL masses found in the literature. The catalogues and future updates are publicly available at http://pico.bo.astro.it/˜sereno/CoMaLit/LC2/.

  16. X-ray morphological study of galaxy cluster catalogues

    NASA Astrophysics Data System (ADS)

    Democles, Jessica; Pierre, Marguerite; Arnaud, Monique

    2016-07-01

    Context : The intra-cluster medium distribution as probed by X-ray morphology based analysis gives good indication of the system dynamical state. In the race for the determination of precise scaling relations and understanding their scatter, the dynamical state offers valuable information. Method : We develop the analysis of the centroid-shift so that it can be applied to characterize galaxy cluster surveys such as the XXL survey or high redshift cluster samples. We use it together with the surface brightness concentration parameter and the offset between X-ray peak and brightest cluster galaxy in the context of the XXL bright cluster sample (Pacaud et al 2015) and a set of high redshift massive clusters detected by Planck and SPT and observed by both XMM-Newton and Chandra observatories. Results : Using the wide redshift coverage of the XXL sample, we see no trend between the dynamical state of the systems with the redshift.

  17. Redshift Distributions of Galaxies in the DES Science Verification Shear Catalogue and Implications for Weak Lensing

    SciTech Connect

    Bonnett, C.

    2015-07-21

    We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model- or machine learning-based photometric redshift methods { annz2, bpz calibrated against BCC-U fig simulations, skynet, and tpz { are analysed. For training, calibration, and testing of these methods, we also construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evalu-ated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-zs. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72 ±0.01 over the range 0:3 < z < 1:3, we construct three tomographic bins with means of z = {0.45; 0.67,1.00g}. These bins each have systematic uncertainties δz ≲ 0.05 in the mean of the fiducial skynet photo-z n(z). We propagate the errors in the redshift distributions through to their impact on cosmological parameters estimated with cosmic shear, and find that they cause shifts in the value of σ8 of approx. 3%. This shift is within the one sigma statistical errors on σ8 for the DES SV shear catalog. We also found that further study of the potential impact of systematic differences on the critical surface density, Σcrit, contained levels of bias safely less than the statistical power of DES SV data. We recommend a final Gaussian prior for the photo-z bias in the mean of n(z) of width 0:05 for each of the three tomographic bins, and show that this is a sufficient bias model for the corresponding cosmology analysis.

  18. A sample of X-ray emitting normal galaxies from the BMW-HRI Catalogue

    NASA Astrophysics Data System (ADS)

    Tajer, M.; Trinchieri, G.; Wolter, A.; Campana, S.; Moretti, A.; Tagliaferri, G.

    2005-06-01

    We obtained a sample of 143 normal galaxies with X-ray luminosity in the range 1038{-}1043 erg s-1 from the cross-correlation of the ROSAT HRI Brera Multi-scale Wavelet (BMW-HRI) Catalogue with the Lyon-Meudon Extragalactic Database (LEDA). We find that the average X-ray properties of this sample are in good agreement with those of other samples of galaxies in the literature. We selected a complete flux limited serendipitous sample of 32 galaxies from which we derived the log N-log S distribution of normal galaxies in the flux range 1.1{-} 110 × 10-14 erg cm-2 s-1. The resulting distribution is consistent with the Euclidean -1.5 slope. Comparisons with other samples, such as the Extended Medium Sensitivity Survey, the ROSAT All Sky Survey, the XMM-Newton/2dF survey, and the Chandra Deep Field Survey indicate that the log N -log S distribution of normal galaxies is consistent with a Euclidean slope over a flux range of about 6 decades.

  19. A catalogue of photometric redshifts for the SDSS-DR9 galaxies

    NASA Astrophysics Data System (ADS)

    Brescia, M.; Cavuoti, S.; Longo, G.; De Stefano, V.

    2014-08-01

    Context. Accurate photometric redshifts for large samples of galaxies are among the main products of modern multiband digital surveys. Over the last decade, the Sloan Digital Sky Survey (SDSS) has become a sort of benchmark against which to test the various methods. Aims: We present an application of a new method to the estimation of photometric redshifts for the galaxies in the SDSS Data Release 9 (SDSS-DR9). Photometric redshifts for more than 143 million galaxies were produced. Methods: The Multi Layer Perceptron with Quasi Newton Algorithm (MLPQNA) model, provided within the framework of the DAta Mining and Exploration Web Application REsource (DAMEWARE), is an interpolative method derived from machine learning models. Results: The obtained redshifts have an overall uncertainty of σ = 0.023 with a very small average bias of ~3 × 10-5, and a fraction of catastrophic outliers (|Δz| > 2σ) of ~5%. This result is slightly better than what was already available in the literature in terms of the smaller fraction of catastrophic outliers as well. The produced catalogue, composed by 58 tables is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/568/A126

  20. NIR Tully-Fisher in the Zone of Avoidance - III. Deep NIR catalogue of the HIZOA galaxies

    NASA Astrophysics Data System (ADS)

    Said, Khaled; Kraan-Korteweg, Renée C.; Jarrett, T. H.; Staveley-Smith, Lister; Williams, Wendy L.

    2016-11-01

    We present a deep near-infrared (NIR; J, H, and Ks bands) photometric catalogue of sources from the Parkes H I Zone of Avoidance (HIZOA) survey, which forms the basis for an investigation of the matter distribution in the Zone of Avoidance. Observations were conducted between 2006 and 2013 using the Infrared Survey Facility (IRSF), a 1.4-m telescope situated at the South African Astronomical Observatory site in Sutherland. The images cover all 1108 HIZOA detections and yield 915 galaxies. An additional 105 bright 2MASS galaxies in the southern ZOA were imaged with the IRSF, resulting in 129 galaxies. The average Ks-band seeing and sky background for the survey are 1.38 arcsec and 20.1 mag, respectively. The detection rate as a function of stellar density and dust extinction is found to depend mainly on the H I mass of the H I detected galaxies, which in principal correlates with the NIR brightness of the spiral galaxies. The measured isophotal magnitudes are of sufficient accuracy (errors ˜0.02 mag) to be used in a Tully-Fisher analysis. In the final NIR catalogue, 285 galaxies have both IRSF and 2MASS photometry (180 HIZOA plus 105 bright 2MASX galaxies). The Ks-band isophotal magnitudes presented in this paper agree, within the uncertainties, with those reported in the 2MASX catalogue. Another 30 galaxies, from the HIZOA northern extension, are also covered by UKIDSS Galactic Plane Survey (GPS) images, which are one magnitude deeper than our IRSF images. A modified version of our photometry pipeline was used to derive the photometric parameters of these UKIDSS galaxies. Good agreement was found between the respective Ks-band isophotal magnitudes. These comparisons confirm the robustness of the isophotal parameters and demonstrate that the IRSF images do not suffer from foreground contamination, after star removal, nor underestimate the isophotal fluxes of ZoA galaxies.

  1. VizieR Online Data Catalog: MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)

    NASA Astrophysics Data System (ADS)

    Piffaretti, R.; Arnaud, M.; Pratt, G. W.; Pointecouteau, E.; Melin, J.-B.

    2011-09-01

    We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L500, total mass M500, and radius R500. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. (1 data file).

  2. SDSS-III Baryon Oscillation Spectroscopic Survey data release 12: Galaxy target selection and large-scale structure catalogues

    DOE PAGES

    Reid, Beth; Ho, Shirley; Padmanabhan, Nikhil; Percival, Will J.; Tinker, Jeremy; Tojeiro, Rito; White, Marin; Daniel J. Einstein; Maraston, Claudia; Ross, Ashley J.; et al

    2015-11-17

    The Baryon Oscillation Spectroscopic Survey (BOSS), part of the Sloan Digital Sky Survey (SDSS) III project, has provided the largest survey of galaxy redshifts available to date, in terms of both the number of galaxy redshifts measured by a single survey, and the effective cosmological volume covered. Key to analysing the clustering of these data to provide cosmological measurements is understanding the detailed properties of this sample. Potential issues include variations in the target catalogue caused by changes either in the targeting algorithm or properties of the data used, the pattern of spectroscopic observations, the spatial distribution of targets formore » which redshifts were not obtained, and variations in the target sky density due to observational systematics. We document here the target selection algorithms used to create the galaxy samples that comprise BOSS. We also present the algorithms used to create large-scale structure catalogues for the final Data Release (DR12) samples and the associated random catalogues that quantify the survey mask. The algorithms are an evolution of those used by the BOSS team to construct catalogues from earlier data, and have been designed to accurately quantify the galaxy sample. Furthermore, the code used, designated mksample, is released with this paper.« less

  3. SDSS-III Baryon Oscillation Spectroscopic Survey data release 12: Galaxy target selection and large-scale structure catalogues

    SciTech Connect

    Reid, Beth; Ho, Shirley; Padmanabhan, Nikhil; Percival, Will J.; Tinker, Jeremy; Tojeiro, Rito; White, Marin; Daniel J. Einstein; Maraston, Claudia; Ross, Ashley J.; Sanchez, Ariel G.; Schlegel, David; Sheldon, Erin; Strauss, Michael A.; Thomas, Daniel; Wake, David; Beutler, Florian; Bizyaev, Dmitry; Bolton, Adam S.; Brownstein, Joel R.; Chuang, Chia -Hsun; Dawson, Kyle; Harding, Paul; Kitaura, Francisco -Shu; Leauthaud, Alexie; Masters, Karen; McBride, Cameron K.; More, Surhud; Olmstead, Matthew D.; Oravetz, Daniel; Nuza, Sebastian E.; Pan, Kaike; Parejko, John; Pforr, Janine; Prada, Francisco; Rodriguez-Torres, Sergio; Salazar-Albornoz, Salvador; Samushia, Lado; Schneider, Donald P.; Scoccola, Claudia G.; Simmons, Audrey; Vargas-Magana, Mariana

    2015-11-17

    The Baryon Oscillation Spectroscopic Survey (BOSS), part of the Sloan Digital Sky Survey (SDSS) III project, has provided the largest survey of galaxy redshifts available to date, in terms of both the number of galaxy redshifts measured by a single survey, and the effective cosmological volume covered. Key to analysing the clustering of these data to provide cosmological measurements is understanding the detailed properties of this sample. Potential issues include variations in the target catalogue caused by changes either in the targeting algorithm or properties of the data used, the pattern of spectroscopic observations, the spatial distribution of targets for which redshifts were not obtained, and variations in the target sky density due to observational systematics. We document here the target selection algorithms used to create the galaxy samples that comprise BOSS. We also present the algorithms used to create large-scale structure catalogues for the final Data Release (DR12) samples and the associated random catalogues that quantify the survey mask. The algorithms are an evolution of those used by the BOSS team to construct catalogues from earlier data, and have been designed to accurately quantify the galaxy sample. Furthermore, the code used, designated mksample, is released with this paper.

  4. SDSS-III Baryon Oscillation Spectroscopic Survey Data Release 12: galaxy target selection and large-scale structure catalogues

    NASA Astrophysics Data System (ADS)

    Reid, Beth; Ho, Shirley; Padmanabhan, Nikhil; Percival, Will J.; Tinker, Jeremy; Tojeiro, Rita; White, Martin; Eisenstein, Daniel J.; Maraston, Claudia; Ross, Ashley J.; Sánchez, Ariel G.; Schlegel, David; Sheldon, Erin; Strauss, Michael A.; Thomas, Daniel; Wake, David; Beutler, Florian; Bizyaev, Dmitry; Bolton, Adam S.; Brownstein, Joel R.; Chuang, Chia-Hsun; Dawson, Kyle; Harding, Paul; Kitaura, Francisco-Shu; Leauthaud, Alexie; Masters, Karen; McBride, Cameron K.; More, Surhud; Olmstead, Matthew D.; Oravetz, Daniel; Nuza, Sebastián E.; Pan, Kaike; Parejko, John; Pforr, Janine; Prada, Francisco; Rodríguez-Torres, Sergio; Salazar-Albornoz, Salvador; Samushia, Lado; Schneider, Donald P.; Scóccola, Claudia G.; Simmons, Audrey; Vargas-Magana, Mariana

    2016-01-01

    The Baryon Oscillation Spectroscopic Survey (BOSS), part of the Sloan Digital Sky Survey (SDSS) III project, has provided the largest survey of galaxy redshifts available to date, in terms of both the number of galaxy redshifts measured by a single survey, and the effective cosmological volume covered. Key to analysing the clustering of these data to provide cosmological measurements is understanding the detailed properties of this sample. Potential issues include variations in the target catalogue caused by changes either in the targeting algorithm or properties of the data used, the pattern of spectroscopic observations, the spatial distribution of targets for which redshifts were not obtained, and variations in the target sky density due to observational systematics. We document here the target selection algorithms used to create the galaxy samples that comprise BOSS. We also present the algorithms used to create large-scale structure catalogues for the final Data Release (DR12) samples and the associated random catalogues that quantify the survey mask. The algorithms are an evolution of those used by the BOSS team to construct catalogues from earlier data, and have been designed to accurately quantify the galaxy sample. The code used, designated MKSAMPLE, is released with this paper.

  5. Documentation for the machine-readable version of the Morphological Catalogue of Galaxies (MCG) of Vorontsov-Velyaminov et al, 1962-1968

    NASA Technical Reports Server (NTRS)

    Warren, W. H., Jr.

    1982-01-01

    Modifications, corrections, and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies.' In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalogue resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.

  6. The 3XMM/SDSS Stripe 82 Galaxy Cluster Survey. I. Cluster catalogue and discovery of two merging cluster candidates

    NASA Astrophysics Data System (ADS)

    Takey, A.; Durret, F.; Mahmoud, E.; Ali, G. B.

    2016-10-01

    We present a galaxy cluster survey based on XMM-Newton observations that are located in Stripe 82 of the Sloan Digital Sky Survey (SDSS). The survey covers an area of 11.25 deg2. The X-ray cluster candidates were selected as serendipitously extended detected sources from the third XMM-Newton serendipitous source catalogue (3XMM-DR5). A cross-correlation of the candidate list that comprises 94 objects with recently published X-ray and optically selected cluster catalogues provided optical confirmations and redshift estimates for about half of the candidate sample. We present a catalogue of X-ray cluster candidates previously known in X-ray and/or optical bands from the matched catalogues or NED. The catalogue consists of 54 systems with redshift measurements in the range of 0.05-1.19 with a median of 0.36. Of these, 45 clusters have spectroscopic confirmations as stated in the matched catalogues. We spectroscopically confirmed another 6 clusters from the available spectroscopic redshifts in the SDSS-DR12. The cluster catalogue includes 17 newly X-ray discovered clusters, while the remainder were detected in previous XMM-Newton and/or ROSAT cluster surveys. Based on the available redshifts and fluxes given in the 3XMM-DR5 catalogue, we estimated the X-ray luminosities and masses for the cluster sample. We also present the list of the remaining X-ray cluster candidates (40 objects) that have no redshift information yet in the literature. Of these candidates, 25 sources are considered as distant cluster candidates beyond a redshift of 0.6. We also searched for galaxy cluster mergers in our cluster sample and found two strong candidates for newly discovered cluster mergers at redshifts of 0.11 and 0.26. The X-ray and optical properties of these systems are presented. Tables A.1, C.1, and C.2 are also available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/594/A32

  7. Redshift distributions of galaxies in the Dark Energy Survey Science Verification shear catalogue and implications for weak lensing

    NASA Astrophysics Data System (ADS)

    Bonnett, C.; Troxel, M. A.; Hartley, W.; Amara, A.; Leistedt, B.; Becker, M. R.; Bernstein, G. M.; Bridle, S. L.; Bruderer, C.; Busha, M. T.; Carrasco Kind, M.; Childress, M. J.; Castander, F. J.; Chang, C.; Crocce, M.; Davis, T. M.; Eifler, T. F.; Frieman, J.; Gangkofner, C.; Gaztanaga, E.; Glazebrook, K.; Gruen, D.; Kacprzak, T.; King, A.; Kwan, J.; Lahav, O.; Lewis, G.; Lidman, C.; Lin, H.; MacCrann, N.; Miquel, R.; O'Neill, C. R.; Palmese, A.; Peiris, H. V.; Refregier, A.; Rozo, E.; Rykoff, E. S.; Sadeh, I.; Sánchez, C.; Sheldon, E.; Uddin, S.; Wechsler, R. H.; Zuntz, J.; Abbott, T.; Abdalla, F. B.; Allam, S.; Armstrong, R.; Banerji, M.; Bauer, A. H.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Carnero Rosell, A.; Carretero, J.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; DePoy, D. L.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Doel, P.; Fausti Neto, A.; Fernandez, E.; Flaugher, B.; Fosalba, P.; Gerdes, D. W.; Gruendl, R. A.; Honscheid, K.; Jain, B.; James, D. J.; Jarvis, M.; Kim, A. G.; Kuehn, K.; Kuropatkin, N.; Li, T. S.; Lima, M.; Maia, M. A. G.; March, M.; Marshall, J. L.; Martini, P.; Melchior, P.; Miller, C. J.; Neilsen, E.; Nichol, R. C.; Nord, B.; Ogando, R.; Plazas, A. A.; Reil, K.; Romer, A. K.; Roodman, A.; Sako, M.; Sanchez, E.; Santiago, B.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thaler, J.; Thomas, D.; Vikram, V.; Walker, A. R.; Dark Energy Survey Collaboration

    2016-08-01

    We present photometric redshift estimates for galaxies used in the weak lensing analysis of the Dark Energy Survey Science Verification (DES SV) data. Four model- or machine learning-based photometric redshift methods—annz2, bpz calibrated against BCC-Ufig simulations, skynet, and tpz—are analyzed. For training, calibration, and testing of these methods, we construct a catalogue of spectroscopically confirmed galaxies matched against DES SV data. The performance of the methods is evaluated against the matched spectroscopic catalogue, focusing on metrics relevant for weak lensing analyses, with additional validation against COSMOS photo-z 's. From the galaxies in the DES SV shear catalogue, which have mean redshift 0.72 ±0.01 over the range 0.3 catalogue. We further study the potential impact of systematic differences on the critical surface density, Σcrit , finding levels of bias safely less than the statistical power of DES SV data. We recommend a final Gaussian prior for the photo-z bias in the mean of n (z ) of width 0.05 for each of the three tomographic bins, and show that this is a sufficient bias model for the corresponding cosmology analysis.

  8. Strong bimodality in the host halo mass of central galaxies from galaxy-galaxy lensing

    NASA Astrophysics Data System (ADS)

    Mandelbaum, Rachel; Wang, Wenting; Zu, Ying; White, Simon; Henriques, Bruno; More, Surhud

    2016-04-01

    We use galaxy-galaxy lensing to study the dark matter haloes surrounding a sample of locally brightest galaxies (LBGs) selected from the Sloan Digital Sky Survey. We measure mean halo mass as a function of the stellar mass and colour of the central galaxy. Mock catalogues constructed from semi-analytic galaxy formation simulations demonstrate that most LBGs are the central objects of their haloes, greatly reducing interpretation uncertainties due to satellite contributions to the lensing signal. Over the full stellar mass range, 10.3 < log [M*/M⊙] < 11.6, we find that passive central galaxies have haloes that are at least twice as massive as those of star-forming objects of the same stellar mass. The significance of this effect exceeds 3σ for log [M*/M⊙] > 10.7. Tests using the mock catalogues and on the data themselves clarify the effects of LBG selection and show that it cannot artificially induce a systematic dependence of halo mass on LBG colour. The bimodality in halo mass at fixed stellar mass is reproduced by the astrophysical model underlying our mock catalogue, but the sign of the effect is inconsistent with recent, nearly parameter-free age-matching models. The sign and magnitude of the effect can, however, be reproduced by halo occupation distribution models with a simple (few-parameter) prescription for type dependence.

  9. Catalogue of the morphological features in the Spitzer Survey of Stellar Structure in Galaxies (S4G)

    NASA Astrophysics Data System (ADS)

    Herrera-Endoqui, M.; Díaz-García, S.; Laurikainen, E.; Salo, H.

    2015-10-01

    Context. A catalogue of the features for the complete Spitzer Survey of Stellar Structure in Galaxies (S4G), including 2352 nearby galaxies, is presented. The measurements are made using 3.6 μm images, largely tracing the old stellar population; at this wavelength the effects of dust are also minimal. The measured features are the sizes, ellipticities, and orientations of bars, rings, ringlenses, and lenses. Measured in a similar manner are also barlenses (lens-like structures embedded in the bars), which are not lenses in the usual sense, being rather the more face-on counterparts of the boxy/peanut structures in the edge-on view. In addition, pitch angles of spiral arm segments are measured for those galaxies where they can be reliably traced. More than one pitch angle may appear for a single galaxy. All measurements are made in a human-supervised manner so that attention is paid to each galaxy. Aims: We create a catalogue of morphological features in the complete S4G. Methods: We used isophotal analysis, unsharp masking, and fitting ellipses to measured structures. Results: We find that the sizes of the inner rings and lenses normalized to barlength correlate with the galaxy mass: the normalized sizes increase toward the less massive galaxies; it has been suggested that this is related to the larger dark matter content in the bar region in these systems. Bars in the low mass galaxies are also less concentrated, likely to be connected to the mass cut-off in the appearance of the nuclear rings and lenses. We also show observational evidence that barlenses indeed form part of the bar, and that a large fraction of the inner lenses in the non-barred galaxies could be former barlenses in which the thin outer bar component has dissolved. Full Tables 2 and 3 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/582/A86

  10. The Planck Catalogue of High-z source candidates : A laboratory for high-z star forming galaxies

    NASA Astrophysics Data System (ADS)

    Montier, Ludovic

    2015-08-01

    The Planck satellite has provided the first FIR/submm all-sky survey with a sensitivity allowing us to identify the rarest, most luminous high-z dusty star-forming sources on the sky. It opens a new window on these extreme star-forming systems at redshift above 1.5, providing a powerful laboratory to study the mechanisms of galaxy evolution and enrichment in the frame of the large scale structure growth.I will describe how the Planck catalogue of high-z source candidates (PHz, Planck 2015 in prep.) has been built and charcaterized over 25% of the sky by selecting the brightest red submm sources at a 5' resolution. Follow-up observations with Herschel/SPIRE over 228 Planck candidates have shown that 93% of these candidates are actually overdensities of red sources with SEDs peaking at 350um (Planck Int. results. XXVII 2014). Complementarily to this population of objects, 12 Planck high-z candidates have been identified as strongly lensed star forming galaxies at redshift lying between 2.2 and 3.6 (Canameras et al 2015 subm.), with flux densities larger than 400 mJy up to 1 Jy at 350um, and strong magnification factors. These Planck lensed star-forming galaxies are the rarest brightest lensed in the submm range, providing a unique opportunity to extend the exploration of the star-forming system in this range of mass and redshift.I will detail further a specific analysis performed on a proto-cluster candidate, PHz G95.5-61.6, identified as a double structure at z=1.7 and z=2.03, using an extensive follow-up program (Flores-Cacho et al 2015 subm.). This is the first Planck proto-cluster candidate with spectroscopic confirmation, which opens a new field of statistical analysis about the evolution of dusty star-forming galaxies in such accreting structures.I will finally discuss how the PHz catalogue may help to answer some of the fundamental questions like: At what cosmic epoch did massive galaxy clusters form most of their stars? Is star formation more or less vigorous

  11. A catalogue of 2D photometric decompositions in the SDSS-DR7 spectroscopic main galaxy sample: preferred models and systematics

    NASA Astrophysics Data System (ADS)

    Meert, Alan; Vikram, Vinu; Bernardi, Mariangela

    2015-02-01

    We present a catalogue of 2D, point spread function-corrected de Vacouleurs, Sérsic, de Vacouleurs+Exponential, and Sérsic+Exponential fits of ˜7 × 105 spectroscopically selected galaxies drawn from the Sloan Digital Sky Survey (SDSS) Data Release 7. Fits are performed for the SDSS r band utilizing the fitting routine GALFIT and analysis pipeline PYMORPH. We compare these fits to prior catalogues. Fits are analysed using a physically motivated flagging system. The flags suggest that more than 90 per cent of two-component fits can be used for analysis. We show that the fits follow the expected behaviour for early and late galaxy types. The catalogues provide a robust set of structural and photometric parameters for future galaxy studies. We show that some biases remain in the measurements, e.g. the presence of bars significantly affect the bulge measurements although the bulge ellipticity may be used to separate barred and non-barred galaxies, and about 15 per cent of bulges of two-component fits are also affected by resolution. The catalogues are available in electronic format. We also provide an interface for generating postage stamp images of the 2D model and residual as well as the 1D profile. These images can be generated for a user-uploaded list of galaxies on demand.

  12. Population gradients in the Sloan Digital Sky Survey Galaxy Catalogue: the role of merging

    NASA Astrophysics Data System (ADS)

    Tortora, C.; Napolitano, N. R.

    2012-04-01

    We investigate the role of the environment on the colour and stellar population gradients in a local sample of ˜3500 central and ˜1150 satellite Sloan Digital Sky Survey (SDSS) early-type galaxies. The environment is parametrized in terms of the number of satellite galaxies, Ngal, in each group. For central galaxies, we find that both optical colour and mass-to-light (M/L) ratio gradients are shallower in central galaxies residing in denser environments (higher Ngal). This trend is driven by metallicity gradients, while age gradients appear to be less dependent on the environment and to have a larger scatter. On the other hand, satellites do not show any differences in terms of the environment. The same results are found if galaxies are classified by central age, and both central and satellite galaxies have shallower gradients if they are older and steeper gradients if younger, satellites being independent of ages. In central galaxies, we show that the observed trends can be explained with the occurrence of dry mergings, which are more numerous in denser environments and producing shallower colour gradients because of more uniform metallicity distributions due to the mixing of stellar populations, while no final clues about merging occurrence can be obtained for satellites. Finally, we discuss all systematics on stellar population fitting and their impact on the final results.

  13. Luminosity dependence of the spatial and velocity distributions of galaxies: semi-analytic models versus the Sloan Digital Sky Survey

    NASA Astrophysics Data System (ADS)

    Li, Cheng; Jing, Y. P.; Kauffmann, Guinevere; Börner, Gerhard; Kang, Xi; Wang, Lan

    2007-04-01

    By comparing semi-analytic galaxy catalogues with data from the Sloan Digital Sky Survey (SDSS), we show that current galaxy formation models reproduce qualitatively the dependence of galaxy clustering and pairwise peculiar velocities on luminosity, but some subtle discrepancies with the data still remain. The comparisons are carried out by constructing a large set of mock galaxy redshift surveys that have the same selection function as the SDSS Data Release Four (DR4). The mock surveys are based on two sets of semi-analytic catalogues presented by Croton et al. and Kang et al. From the mock catalogues, we measure the redshift-space projected two-point correlation function wp(rp), the power spectrum P(k) and the pairwise velocity dispersion (PVD) in Fourier space σ12(k) and in configuration space σ12(rp), for galaxies in different luminosity intervals. We then compare these theoretical predictions with the measurements derived from the SDSS DR4. On large scales and for galaxies brighter than L*, both sets of mock catalogues agree well with the data. For fainter galaxies, however, both models predict stronger clustering and higher pairwise velocities than observed. We demonstrate that this problem can be resolved if the fraction of faint satellite galaxies in massive haloes is reduced by ~30 per cent compared to the model predictions. A direct look into the model galaxy catalogues reveals that a significant fraction (15 per cent) of faint galaxies (-18 < M0.1r - 5 log10h < -17) reside in haloes with Mvir > 1013 Msolar, and this population is predominantly red in colour. These faint red galaxies are responsible for the high PVD values of low-luminosity galaxies on small scales.

  14. VizieR Online Data Catalog: Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)

    NASA Astrophysics Data System (ADS)

    Konyves, V.; Kiss, Cs.; Moor, A.; Kiss, Z. T.; Toth, L. V.

    2006-11-01

    An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of fin~30% and fout~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane. (4 data files).

  15. ICE-COLA: towards fast and accurate synthetic galaxy catalogues optimizing a quasi-N-body method

    NASA Astrophysics Data System (ADS)

    Izard, Albert; Crocce, Martin; Fosalba, Pablo

    2016-07-01

    Next generation galaxy surveys demand the development of massive ensembles of galaxy mocks to model the observables and their covariances, what is computationally prohibitive using N-body simulations. COmoving Lagrangian Acceleration (COLA) is a novel method designed to make this feasible by following an approximate dynamics but with up to three orders of magnitude speed-ups when compared to an exact N-body. In this paper, we investigate the optimization of the code parameters in the compromise between computational cost and recovered accuracy in observables such as two-point clustering and halo abundance. We benchmark those observables with a state-of-the-art N-body run, the MICE Grand Challenge simulation. We find that using 40 time-steps linearly spaced since zi ˜ 20, and a force mesh resolution three times finer than that of the number of particles, yields a matter power spectrum within 1 per cent for k ≲ 1 h Mpc-1 and a halo mass function within 5 per cent of those in the N-body. In turn, the halo bias is accurate within 2 per cent for k ≲ 0.7 h Mpc-1 whereas, in redshift space, the halo monopole and quadrupole are within 4 per cent for k ≲ 0.4 h Mpc-1. These results hold for a broad range in redshift (0 < z < 1) and for all halo mass bins investigated (M > 1012.5 h-1 M⊙). To bring accuracy in clustering to one per cent level we study various methods that re-calibrate halo masses and/or velocities. We thus propose an optimized choice of COLA code parameters as a powerful tool to optimally exploit future galaxy surveys.

  16. HerMES: a search for high-redshift dusty galaxies in the HerMES Large Mode Survey - catalogue, number counts and early results

    NASA Astrophysics Data System (ADS)

    Asboth, V.; Conley, A.; Sayers, J.; Béthermin, M.; Chapman, S. C.; Clements, D. L.; Cooray, A.; Dannerbauer, H.; Farrah, D.; Glenn, J.; Golwala, S. R.; Halpern, M.; Ibar, E.; Ivison, R. J.; Maloney, P. R.; Marques-Chaves, R.; Martinez-Navajas, P. I.; Oliver, S. J.; Pérez-Fournon, I.; Riechers, D. A.; Rowan-Robinson, M.; Scott, Douglas; Siegel, S. R.; Vieira, J. D.; Viero, M.; Wang, L.; Wardlow, J.; Wheeler, J.

    2016-10-01

    Selecting sources with rising flux densities towards longer wavelengths from Herschel/Spectral and Photometric Imaging Receiver (SPIRE) maps is an efficient way to produce a catalogue rich in high-redshift (z > 4) dusty star-forming galaxies. The effectiveness of this approach has already been confirmed by spectroscopic follow-up observations, but the previously available catalogues made this way are limited by small survey areas. Here we apply a map-based search method to 274 deg2 of the Herschel Multi-tiered Extragalactic Survey (HerMES) Large Mode Survey and create a catalogue of 477 objects with SPIRE flux densities S500 > S350 > S250 and a 5σ cut-off S500 > 52 mJy. From this catalogue we determine that the total number of these `red' sources is at least an order of magnitude higher than predicted by galaxy evolution models. These results are in agreement with previous findings in smaller HerMES fields; however, due to our significantly larger sample size we are also able to investigate the shape of the red source counts for the first time. We have obtained spectroscopic redshift measurements for two of our sources using the Atacama Large Millimeter/submillimeter Array. The redshifts z = 5.1 and 3.8 confirm that with our selection method we can indeed find high-redshift dusty star-forming galaxies.

  17. NIHAO X: reconciling the local galaxy velocity function with cold dark matter via mock H i observations

    NASA Astrophysics Data System (ADS)

    Macciò, Andrea V.; Udrescu, Silviu M.; Dutton, Aaron A.; Obreja, Aura; Wang, Liang; Stinson, Greg R.; Kang, Xi

    2016-11-01

    We introduce project NIHAO (Numerical Investigation of a Hundred Astrophysical Objects), a set of 100 cosmological zoom-in hydrodynamical simulations performed using the gasoline code, with an improved implementation of the SPH algorithm. The haloes in our study range from dwarf to Milky Way masses, and represent an unbiased sampling of merger histories, concentrations and spin parameters. The particle masses and force softenings are chosen to resolve the mass profile to below 1% of the virial radius at all masses, ensuring that galaxy half-light radii are well resolved. Using the same treatment of star formation and stellar feedback for every object, the simulated galaxies reproduce the observed inefficiency of galaxy formation across cosmic time as expressed through the stellar mass vs halo mass relation, and the star formation rate vs stellar mass relation. We thus conclude that stellar feedback is the chief piece of physics required to limit the efficiency of star formation in galaxies less massive than the Milky Way.

  18. The VIMOS-VLT deep survey: the group catalogue

    NASA Astrophysics Data System (ADS)

    Cucciati, O.; Marinoni, C.; Iovino, A.; Bardelli, S.; Adami, C.; Mazure, A.; Scodeggio, M.; Maccagni, D.; Temporin, S.; Zucca, E.; De Lucia, G.; Blaizot, J.; Garilli, B.; Meneux, B.; Zamorani, G.; Le Fèvre, O.; Cappi, A.; Guzzo, L.; Bottini, D.; Le Brun, V.; Tresse, L.; Vettolani, G.; Zanichelli, A.; Arnouts, S.; Bolzonella, M.; Charlot, S.; Ciliegi, P.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Ilbert, O.; Lamareille, F.; McCracken, H. J.; Marano, B.; Merighi, R.; Paltani, S.; Pellò, R.; Pollo, A.; Pozzetti, L.; Vergani, D.; Pérez-Montero, E.

    2010-09-01

    Aims: We present a homogeneous and complete catalogue of optical galaxy groups identified in the purely flux-limited (17.5 ≤ IAB ≤ 24.0) VIMOS-VLT deep redshift Survey (VVDS). Methods: We use mock catalogues extracted from the Millennium Simulation, to correct for potential systematics that might affect the overall distribution as well as the individual properties of the identified systems. Simulated samples allow us to forecast the number and properties of groups that can be potentially found in a survey with VVDS-like selection functions. We use them to correct for the expected incompleteness and, to asses in addition, how well galaxy redshifts trace the line-of-sight velocity dispersion of the underlying mass overdensity. In particular, on these mock catalogues we train the adopted group-finding technique i.e., the Voronoi-Delaunay Method (VDM). The goal is to fine-tune its free parameters, recover in a robust and unbiased way the redshift and velocity dispersion distributions of groups (n(z) and n(σ), respectively), and maximize, at the same time, the level of completeness and purity of the group catalogue. Results: We identify 318 VVDS groups with at least 2 members in the range 0.2 ≤ z ≤ 1.0, among which 144 (/30) with at least 3 (/5) members. The sample has an overall completeness of ~60% and a purity of ~50%. Nearly 45% of the groups with at least 3 members are still recovered if we run the algorithm with a particular parameter set that maximizes the purity (~75%) of the resulting catalogue. We use the group sample to explore the redshift evolution of the fraction fb of blue galaxies (U-B ≤ 1) in the redshift range 0.2 ≤ z ≤ 1. We find that the fraction of blue galaxies is significantly lower in groups than in the global population (i.e. in the whole ensemble of galaxies irrespective of their environment). Both of these quantities increase with redshift, the fraction of blue galaxies in groups exhibiting a marginally significant steeper

  19. On the evolution of the star formation rate function of massive galaxies: constraints at 0.4 < z < 1.8 from the GOODS-MUSIC catalogue

    NASA Astrophysics Data System (ADS)

    Fontanot, Fabio; Cristiani, Stefano; Santini, Paola; Fontana, Adriano; Grazian, Andrea; Somerville, Rachel S.

    2012-03-01

    We study the evolution of the star formation rate function (SFRF) of massive (M★ > 1010 M⊙) galaxies over the 0.4 < z < 1.8 redshift range and its implications for our understanding of the physical processes responsible for galaxy evolution. We use multiwavelength observations included in the Great Observatories Origins Deep Survey-Multiwavelength Southern Infrared Catalog (GOODS-MUSIC) catalogue, which provides a suitable coverage of the spectral region from 0.3 to 24 ?m and either spectroscopic or photometric redshifts for each object. Individual SFRs have been obtained by combining ultraviolet and 24-?m observations, when the latter were available. For all other sources a 'spectral energy distribution (SED) fitting' SFR estimate has been considered. We then define a stellar mass limited sample, complete in the M★ > 1010 M⊙ range and determine the SFRF using the 1/Vmax algorithm. We thus define simulated galaxy catalogues based on the predictions of three different state-of-the-art semi-analytical models (SAMs) of galaxy formation and evolution, and compare them with the observed SFRF. We show that the theoretical SFRFs are well described by a double power law functional form and its redshift evolution is approximated with high accuracy by a pure evolution of the typical SFR (SFR★). We find good agreement between model predictions and the high-SFR end of the SFRF, when the observational errors on the SFR are taken into account. However, the observational SFRF is characterized by a double-peaked structure, which is absent in its theoretical counterparts. At z > 1.0 the observed SFRF shows a relevant density evolution, which is not reproduced by SAMs, due to the well-known overprediction of intermediate-mass galaxies at z˜ 2. SAMs are thus able to reproduce the most intense SFR events observed in the GOODS-MUSIC sample and their redshift distribution. At the same time, the agreement at the low-SFR end is poor: all models overpredict the space density of

  20. Catalogue of HI PArameters (CHIPA)

    NASA Astrophysics Data System (ADS)

    Saponara, J.; Benaglia, P.; Koribalski, B.; Andruchow, I.

    2015-08-01

    The catalogue of HI parameters of galaxies HI (CHIPA) is the natural continuation of the compilation by M.C. Martin in 1998. CHIPA provides the most important parameters of nearby galaxies derived from observations of the neutral Hydrogen line. The catalogue contains information of 1400 galaxies across the sky and different morphological types. Parameters like the optical diameter of the galaxy, the blue magnitude, the distance, morphological type, HI extension are listed among others. Maps of the HI distribution, velocity and velocity dispersion can also be display for some cases. The main objective of this catalogue is to facilitate the bibliographic queries, through searching in a database accessible from the internet that will be available in 2015 (the website is under construction). The database was built using the open source `` mysql (SQL, Structured Query Language, management system relational database) '', while the website was built with ''HTML (Hypertext Markup Language)'' and ''PHP (Hypertext Preprocessor)''.

  1. Mock Trials for Children.

    ERIC Educational Resources Information Center

    Hickey, M. Gail

    1990-01-01

    Demonstrates how role-playing in a mock trial situation allows children to view critically both sides of an issue and introduce them to trial procedure. Offers pre-trial activities, ways to teach students to see both sides of a situation, themes for mock trials, and supporting resources. (GG)

  2. Building a better understanding of the massive high-redshift BOSS CMASS galaxies as tools for cosmology

    NASA Astrophysics Data System (ADS)

    Favole, Ginevra; McBride, Cameron K.; Eisenstein, Daniel J.; Prada, Francisco; Swanson, Molly E.; Chuang, Chia-Hsun; Schneider, Donald P.

    2016-10-01

    We explore the massive bluer star-forming population of the Sloan Digital Sky Survey (SDSS) III/BOSS CMASS DR11 galaxies at z > 0.55 to quantify their differences, in terms of redshift-space distortions and large-scale bias, with respect to the luminous red galaxy sample. We perform a qualitative analysis to understand the significance of these differences and whether we can model and reproduce them in mock catalogues. Specifically, we measure galaxy clustering in CMASS on small and intermediate scales (0.1 ≲ r ≲ 50 h-1 Mpc) by computing the two-point correlation function - both projected and redshift-space - of these galaxies, and a new statistic, Σ(π), able to separate the coherent and dispersed redshift-space distortion contributions and the large-scale bias. We interpret our clustering measurements by adopting a Halo Occupation Distribution (HOD) scheme that maps them on to high-resolution N-body cosmological simulations to produce suitable mock galaxy catalogues. The traditional HOD prescription can be applied to the red and the blue samples, independently, but this approach is unphysical since it allows the same mock galaxies to be either red or blue. To overcome this ambiguity, we modify the standard formulation and infer the red and the blue models by splitting the full mock catalogue into two complementary and non-overlapping submocks. This separation is performed by constraining the HOD with the observed CMASS red and blue galaxy fractions and produces reliable and accurate models.

  3. The Mock Research Paper

    ERIC Educational Resources Information Center

    Clark, Carlton

    2008-01-01

    The mock research paper combines creative writing with academic writing and, in the process, breaks down that binary. This article describes a writing assignment that offers an introduction to the college research paper genre. This assignment helps students focus on crafting an argument and learning genre conventions while postponing until the…

  4. Bibliography of Mock Trial Materials.

    ERIC Educational Resources Information Center

    National Inst. for Citizen Education in the Law, Washington, DC.

    This catalog lists general articles on mock trials, information for arranging mock trial competitions, mock trial problem sets, and video tapes. The problem sets contain introductory material, applicable law, statements of facts, witness statements, and documents. The cases include issues in family, consumer, criminal, and immigration law. Several…

  5. The same with less: the cosmic web of warm versus cold dark matter dwarf galaxies

    NASA Astrophysics Data System (ADS)

    Reed, Darren S.; Schneider, Aurel; Smith, Robert E.; Potter, Doug; Stadel, Joachim; Moore, Ben

    2015-08-01

    We explore fundamental properties of the distribution of low-mass dark matter haloes within the cosmic web using warm dark matter (WDM) and cold dark matter (CDM) cosmological simulations. Using self-abundance-matched mock galaxy catalogues, we show that the distribution of dwarf galaxies in a WDM universe, wherein low-mass halo formation is heavily suppressed, is nearly indistinguishable to that of a CDM universe whose low-mass haloes are not seen because galaxy formation is suppressed below some threshold halo mass. However, if the scatter between dwarf galaxy luminosity and halo properties is large enough, low-mass CDM haloes would sometimes host relatively bright galaxies thereby populating CDM voids with the occasional isolated galaxy and reducing the numbers of completely empty voids. Otherwise, without high mass to light scatter, all mock galaxy clustering statistics that we consider - the auto-correlation function, the numbers and radial profiles of satellites, the numbers of isolated galaxies, and the probability distribution function of small voids - are nearly identical in CDM and WDM. WDM voids are neither larger nor emptier than CDM voids, when constructed from abundance-matched halo catalogues. It is thus a challenge to determine whether the CDM problem of the overabundance of small haloes with respect to the number density of observed dwarf galaxies has a cosmological solution or an astrophysical solution. However, some clues about the dark matter particle and the scatter between the properties of dwarf galaxies and their dark matter halo hosts might be found in the cosmic web of galaxies in future surveys of the local volume.

  6. Understanding the nature of luminous red galaxies (LRGs): connecting LRGs to central and satellite subhaloes

    NASA Astrophysics Data System (ADS)

    Masaki, Shogo; Hikage, Chiaki; Takada, Masahiro; Spergel, David N.; Sugiyama, Naoshi

    2013-08-01

    We develop a novel abundance matching method to construct a mock catalogue of luminous red galaxies (LRGs) in the Sloan Digital Sky Survey (SDSS), using catalogues of haloes and subhaloes in N-body simulations for a Λ-dominated cold dark matter model. Motivated by observations suggesting that LRGs are passively evolving, massive early-type galaxies with a typical age ≳5 Gyr, we assume that simulated haloes at z = 2 (z2-halo) are progenitors for LRG-host subhaloes observed today, and we label the most tightly bound particles in each progenitor z2-halo as LRG `stars'. We then identify the subhaloes containing these stars to z = 0.3 (SDSS redshift) in descending order of the masses of z2-haloes until the comoving number density of the matched subhaloes becomes comparable to the measured number density of SDSS LRGs, bar{n}_LRG=10^{-4} h^3 Mpc^{-3}. Once the above prescription is determined, our only free parameter is the number density of haloes identified at z = 2 and this parameter is fixed to match the observed number density at z = 0.3. By tracing subsequent merging and assembly histories of each progenitor z2-halo, we can directly compute, from the mock catalogue, the distributions of central and satellite LRGs and their internal motions in each host halo at z = 0.3. While the SDSS LRGs are galaxies selected by the magnitude and colour cuts from the SDSS images and are not necessarily a stellar-mass-selected sample, our mock catalogue reproduces a host of SDSS measurements: the halo occupation distribution for central and satellite LRGs, the projected autocorrelation function of LRGs, the cross-correlation of LRGs with shapes of background galaxies (LRG-galaxy weak lensing) and the non-linear redshift-space distortion effect, the Finger-of-God effect, in the angle-averaged redshift-space power spectrum. The mock catalogue generated based on our method can be used for removing or calibrating systematic errors in the cosmological interpretation of LRG clustering

  7. Ramanujan's mock theta functions.

    PubMed

    Griffin, Michael; Ono, Ken; Rolen, Larry

    2013-04-01

    In his famous deathbed letter, Ramanujan introduced the notion of a mock theta function, and he offered some alleged examples. Recent work by Zwegers [Zwegers S (2001) Contemp Math 291:268-277 and Zwegers S (2002) PhD thesis (Univ of Utrecht, Utrecht, The Netherlands)] has elucidated the theory encompassing these examples. They are holomorphic parts of special harmonic weak Maass forms. Despite this understanding, little attention has been given to Ramanujan's original definition. Here, we prove that Ramanujan's examples do indeed satisfy his original definition. PMID:23536292

  8. Catalogues of planetary nebulae.

    NASA Astrophysics Data System (ADS)

    Acker, A.

    Firstly, the general requirements concerning catalogues are studied for planetary nebulae, in particular concerning the objects to be included in a catalogue of PN, their denominations, followed by reflexions about the afterlife and comuterized versions of a catalogue. Then, the basic elements constituting a catalogue of PN are analyzed, and the available data are looked at each time.

  9. An 80 Mpc Filament of Galaxies at Redshift z=2.38

    NASA Technical Reports Server (NTRS)

    Woodgate, B.; Palunas, P.; Francis, P.; Williger, G.; Teplitz, H.

    2004-01-01

    We present the detection of 34 Lyman-alpha emission-line galaxy candidates in a 80 x 80 x 60 co-moving Mpc region surrounding the known z=2.38 galaxy cluster J2143-4423. We have confirmed 15 of these candidates in followup spectroscopy with 2dF at the AAT. The peak space density is a factor of 4 greater than that found by field samples at similar redshifts. The distribution of these galaxy candidates contains several 5-10 Mpc scale voids. We compare our observations with mock catalogs derived from the VIRGO consortium Lambda-CDM N-body simulations. Fewer than 1\\% of the mock catalogues contains voids as large as we observe. Our observations thus tentatively suggest that the galaxy distribution at redshift 2.38 contains larger voids than predicted by current models. The distribution of galaxies suggests a filament or cross-section of a great wall at least 80 x 10 Mpc in transverse extent. Three of the candidate galaxies and one previously discovered galaxy have the large luminosities and extended morphologies of "Lyman-alpha blobs". X-ray properties and physical characteristics of those blobs will be discussed in an accompanying poster by Williger et al.

  10. GLACE survey: OSIRIS/GTC tuneable filter Hα imaging of the rich galaxy cluster ZwCl 0024.0+1652 at z = 0.395. I. Survey presentation, TF data reduction techniques, and catalogue

    NASA Astrophysics Data System (ADS)

    Sánchez-Portal, M.; Pintos-Castro, I.; Pérez-Martínez, R.; Cepa, , J.; Pérez García, A. M.; Domínguez-Sánchez, H.; Bongiovanni, A.; Serra, A. L.; Alfaro, E.; Altieri, B.; Aragón-Salamanca, A.; Balkowski, C.; Biviano, A.; Bremer, M.; Castander, F.; Castañeda, H.; Castro-Rodríguez, N.; Chies-Santos, A. L.; Coia, D.; Diaferio, A.; Duc, P. A.; Ederoclite, A.; Geach, J.; González-Serrano, I.; Haines, C. P.; McBreen, B.; Metcalfe, L.; Oteo, I.; Pérez-Fournón, I.; Poggianti, B.; Polednikova, J.; Ramón-Pérez, M.; Rodríguez-Espinosa, J. M.; Santos, J. S.; Smail, I.; Smith, G. P.; Temporin, S.; Valtchanov, I.

    2015-06-01

    The cores of clusters at 0 ≲ z ≲ 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type galaxies. Clusters grow through the accretion of galaxies and groups from the surrounding field, which implies that galaxy properties, notably the star formation ability, are altered as they fall into overdense regions. The critical issues for understanding this evolution are how the truncation of star formation is connected to the morphological transformation and what physical mechanism is responsible for these changes. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a thorough study of the variations in galaxy properties (star formation, AGN activity, and morphology) as a function of environment in a representative and well-studied sample of clusters. To address these questions, the GLACE survey is making a deep panoramic survey of emission line galaxies (ELG), mapping a set of optical lines ([O ii], [O iii], Hβ andHα/[N ii] when possible) in several galaxy clusters at z ~ 0.40, 0.63, and 0.86. Using the tunable filters (TF) of the OSIRIS instrument at the 10.4 m GTC telescope, the GLACE survey applies the technique of TF tomography: for each line, a set of images are taken through the OSIRIS TF, each image tuned at a different wavelength (equally spaced), to cover a rest frame velocity range of several thousand km s-1 centred on the mean cluster redshift, and scanned for the full TF field of view of an 8 arcmin diameter. Here we present the first results of the GLACE project, targeting the Hα/[N ii] lines in the intermediate-redshift cluster ZwCl 0024.0+1652 at z = 0.395. Two pointings have been performed that cover ~2 × rvir. We discuss the specific techniques devised to process the TF tomography observations in order to generate the catalogue of cluster Hα emitters, which contains more than 200 sources down to a star formation rate (SFR) ≲1 M⊙/yr. An ancillary broadband catalogue is constructed

  11. Galaxies

    SciTech Connect

    Not Available

    1981-01-01

    Normal galaxies, radio galaxies, and Seyfert galaxies are considered. The large magellanic cloud and the great galaxy in Andromedia are highlighted. Quasars and BL lacertae objects are also discussed and a review of the spectral observations of all of these galaxies and celestial objects is presented.

  12. Synthetic data products for future H I galaxy surveys: a tool for characterizing source confusion in spectral line stacking experiments

    NASA Astrophysics Data System (ADS)

    Elson, E. C.; Blyth, S. L.; Baker, A. J.

    2016-08-01

    Much of our current understanding of neutral, atomic gas in galaxies comes from radio observations of the nearby Universe. Until the next generation of instruments allow us to push to much higher redshifts, we must rely mostly upon theoretical models of galaxy formation to provide us with key insights into the likely cosmic evolution of H I in the Universe, and its links to molecular clouds and star formation. In this work, we present a new set of methods to convert mock galaxy catalogues into synthetic data cubes containing model galaxies with realistic spatial and spectral H I distributions over large cosmological volumes. Such synthetic data products can be used to guide observing and data handling/analysis strategies for forthcoming H I galaxy surveys. As a demonstration of the potential use of our simulated products we use them to conduct several mock H I stacking experiments for both low and high-redshift galaxy samples. The stacked spectra can be accurately decomposed into contributions from target and non-target galaxies, revealing in all co-added spectra large fractions of contaminant mass due to source confusion. Our results are consistent with similar estimates extrapolated from z = 0 observational data. The amount of confused mass in a stacked spectrum grows almost linearly with the size of the observational beam, suggesting potential overestimates of Ω _{H I} by some recent H I stacking experiments. Our simulations will allow the study of subtle redshift-dependent effects in future stacking analyses.

  13. Formation, evolution and properties of isolated field elliptical galaxies

    NASA Astrophysics Data System (ADS)

    Niemi, Sami-Matias; Heinämäki, Pekka; Nurmi, Pasi; Saar, Enn

    2010-06-01

    We study the properties, evolution and formation mechanisms of isolated field elliptical (IfE) galaxies. We create a `mock' catalogue of IfE galaxies from the Millennium Simulation Galaxy Catalogue, and trace their merging histories. The formation, identity and assembly redshifts of simulated isolated and non-isolated elliptical galaxies are studied and compared. Observational and numerical data are used to compare age, mass and the colour-magnitude relation. Our results, based on simulation data, show that almost 7 per cent of all elliptical galaxies brighter than -19mag in B band can be classified as IfE galaxies. Results also show that isolated elliptical galaxies have a rather flat luminosity function; a number density of ~3 × 10-6h3Mpc-3mag-1, throughout their B-band magnitudes. IfE galaxies show bluer colours than non-isolated elliptical galaxies and they appear younger, in a statistical sense, according to their mass-weighted age. IfE galaxies also form and assemble at lower redshifts compared to non-isolated elliptical galaxies. About 46 per cent of IfE galaxies have undergone at least one major merging event in their formation history, while the same fraction is only ~33 per cent for non-isolated ellipticals. Almost all (~98 per cent) isolated elliptical galaxies show merging activity during their evolution, pointing towards the importance of mergers in the formation of IfE galaxies. The mean time of the last major merging is at z ~ 0.6 or 6Gyr ago for isolated ellipticals, while non-isolated ellipticals experience their last major merging significantly earlier at z ~ 1.1 or 8Gyr ago. After inspecting merger trees of simulated IfE galaxies, we conclude that three different, yet typical, formation mechanisms can be identified: solitude, coupling and cannibalism. Our results also predict a previously unobserved population of blue, dim and light galaxies that fulfil observational criteria to be classified as IfE galaxies. This separate population comprises

  14. Users and Union Catalogues

    ERIC Educational Resources Information Center

    Hartley, R. J.; Booth, Helen

    2006-01-01

    Union catalogues have had an important place in libraries for many years. Their use has been little investigated. Recent interest in the relative merits of physical and virtual union catalogues and a recent collaborative project between a physical and several virtual union catalogues in the United Kingdom led to the opportunity to study how users…

  15. Cosmic web reconstruction through density ridges: catalogue

    NASA Astrophysics Data System (ADS)

    Chen, Yen-Chi; Ho, Shirley; Brinkmann, Jon; Freeman, Peter E.; Genovese, Christopher R.; Schneider, Donald P.; Wasserman, Larry

    2016-10-01

    We construct a catalogue for filaments using a novel approach called SCMS (subspace constrained mean shift). SCMS is a gradient-based method that detects filaments through density ridges (smooth curves tracing high-density regions). A great advantage of SCMS is its uncertainty measure, which allows an evaluation of the errors for the detected filaments. To detect filaments, we use data from the Sloan Digital Sky Survey, which consist of three galaxy samples: the NYU main galaxy sample (MGS), the LOWZ sample and the CMASS sample. Each of the three data set covers different redshift regions so that the combined sample allows detection of filaments up to z = 0.7. Our filament catalogue consists of a sequence of two-dimensional filament maps at different redshifts that provide several useful statistics on the evolution cosmic web. To construct the maps, we select spectroscopically confirmed galaxies within 0.050 < z < 0.700 and partition them into 130 bins. For each bin, we ignore the redshift, treating the galaxy observations as a 2-D data and detect filaments using SCMS. The filament catalogue consists of 130 individual 2-D filament maps, and each map comprises points on the detected filaments that describe the filamentary structures at a particular redshift. We also apply our filament catalogue to investigate galaxy luminosity and its relation with distance to filament. Using a volume-limited sample, we find strong evidence (6.1σ-12.3σ) that galaxies close to filaments are generally brighter than those at significant distance from filaments.

  16. Have baryonic acoustic oscillations in the galaxy distribution really been measured?

    NASA Astrophysics Data System (ADS)

    Cabré, Anna; Gaztañaga, Enrique

    2011-03-01

    Recent publications claim that there is no convincing evidence for measurements of the baryonic acoustic oscillation (BAO) feature in galaxy samples using either monopole or radial information. Different claims seem contradictory: data are either not consistent with the BAO model or data are consistent with both the BAO model and featureless models without BAO. We investigate this point with a set of 216 realistic mock galaxy catalogues extracted from MICE 7680, one of the largest volume dark matter simulation run to date, with a volume of 1300 cubical gigaparsecs. Our mocks cover similar volume, densities and bias as the real galaxies and provide 216 realizations of the lambda or ω=-1 cold dark matter (ωCDM) BAO model. We find that only 20 per cent of the mocks show a statistically significant (3σ) preference for the true (input) ωCDM BAO model as compared to a featureless (non-physical) model without BAO. Thus the volume of current galaxy samples is not yet large enough to claim that the BAO feature has been detected. Does this mean that we cannot locate the BAO position? Using a simple (non-optimal) algorithm we show that in 50 per cent (100 per cent) of the mocks, we can find the BAO position within 5 per cent (20 per cent) of the true value. These two findings are not in contradiction: the former is about model selection and the later is about parameter fitting within a model. We conclude that current monopole and radial BAO measurements can be used as standard rulers if we assume ωCDM type of models.

  17. Fresno County Mock Trial Competition.

    ERIC Educational Resources Information Center

    Fresno City Unified School District, CA.

    THE FOLLOWING IS THE FULL TEXT OF THIS DOCUMENT: The Fresno County Office of Education and the Fresno Unified School District hosted the Mock Trial Competition. The state competition is sponsored by the Constitutional Rights Foundation, with cosponsorship from the California State Bar Association and the California Young Lawyer's Association. This…

  18. Mock Trials and Critical Thinking.

    ERIC Educational Resources Information Center

    Karraker, Meg Wilkes

    1993-01-01

    One college teacher's use of mock trials in sociology instruction is described. Students are assigned roles as petitioner, respondent, attorneys, judge, courtroom staff, witnesses, reporters, and jurors. Pretrial investigations provide experience in information-gathering and critical thinking. Posttrial debriefing reveals others' thinking…

  19. Galaxy bias from the Dark Energy Survey Science Verification data: Combining galaxy density maps and weak lensing maps

    DOE PAGES

    Chang, C.; Pujol, A.; Gaztañaga, E.; Amara, A.; Réfrégier, A.; Bacon, D.; Becker, M. R.; Bonnett, C.; Carretero, J.; Castander, F. J.; et al

    2016-04-15

    We measure the redshift evolution of galaxy bias for a magnitude-limited galaxy sample by combining the galaxy density maps and weak lensing shear maps for a ~116 deg2 area of the Dark Energy Survey (DES) Science Verification (SV) data. This method was first developed in Amara et al. and later re-examined in a companion paper with rigorous simulation tests and analytical treatment of tomographic measurements. In this work we apply this method to the DES SV data and measure the galaxy bias for a i < 22.5 galaxy sample. We find the galaxy bias and 1σ error bars in fourmore » photometric redshift bins to be 1.12 ± 0.19 (z = 0.2–0.4), 0.97 ± 0.15 (z = 0.4–0.6), 1.38 ± 0.39 (z = 0.6–0.8), and 1.45 ± 0.56 (z = 0.8–1.0). These measurements are consistent at the 2σ level with measurements on the same data set using galaxy clustering and cross-correlation of galaxies with cosmic microwave background lensing, with most of the redshift bins consistent within the 1σ error bars. In addition, our method provides the only σ8 independent constraint among the three. We forward model the main observational effects using mock galaxy catalogues by including shape noise, photo-z errors, and masking effects. We show that our bias measurement from the data is consistent with that expected from simulations. With the forthcoming full DES data set, we expect this method to provide additional constraints on the galaxy bias measurement from more traditional methods. Moreover, in the process of our measurement, we build up a 3D mass map that allows further exploration of the dark matter distribution and its relation to galaxy evolution.« less

  20. Galaxy bias from the Dark Energy Survey Science Verification data: combining galaxy density maps and weak lensing maps

    NASA Astrophysics Data System (ADS)

    Chang, C.; Pujol, A.; Gaztañaga, E.; Amara, A.; Réfrégier, A.; Bacon, D.; Becker, M. R.; Bonnett, C.; Carretero, J.; Castander, F. J.; Crocce, M.; Fosalba, P.; Giannantonio, T.; Hartley, W.; Jarvis, M.; Kacprzak, T.; Ross, A. J.; Sheldon, E.; Troxel, M. A.; Vikram, V.; Zuntz, J.; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Annis, J.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Rosell, A. Carnero; Kind, M. Carrasco; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Doel, P.; Eifler, T. F.; Estrada, J.; Evrard, A. E.; Flaugher, B.; Frieman, J.; Goldstein, D. A.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Honscheid, K.; Jain, B.; James, D. J.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lima, M.; Marshall, J. L.; Martini, P.; Melchior, P.; Miller, C. J.; Miquel, R.; Mohr, J. J.; Nichol, R. C.; Nord, B.; Ogando, R.; Plazas, A. A.; Reil, K.; Romer, A. K.; Roodman, A.; Rykoff, E. S.; Sanchez, E.; Scarpine, V.; Schubnell, M.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Walker, A. R.

    2016-07-01

    We measure the redshift evolution of galaxy bias for a magnitude-limited galaxy sample by combining the galaxy density maps and weak lensing shear maps for a ˜116 deg2 area of the Dark Energy Survey (DES) Science Verification (SV) data. This method was first developed in Amara et al. and later re-examined in a companion paper with rigorous simulation tests and analytical treatment of tomographic measurements. In this work we apply this method to the DES SV data and measure the galaxy bias for a i < 22.5 galaxy sample. We find the galaxy bias and 1σ error bars in four photometric redshift bins to be 1.12 ± 0.19 (z = 0.2-0.4), 0.97 ± 0.15 (z = 0.4-0.6), 1.38 ± 0.39 (z = 0.6-0.8), and 1.45 ± 0.56 (z = 0.8-1.0). These measurements are consistent at the 2σ level with measurements on the same data set using galaxy clustering and cross-correlation of galaxies with cosmic microwave background lensing, with most of the redshift bins consistent within the 1σ error bars. In addition, our method provides the only σ8 independent constraint among the three. We forward model the main observational effects using mock galaxy catalogues by including shape noise, photo-z errors, and masking effects. We show that our bias measurement from the data is consistent with that expected from simulations. With the forthcoming full DES data set, we expect this method to provide additional constraints on the galaxy bias measurement from more traditional methods. Furthermore, in the process of our measurement, we build up a 3D mass map that allows further exploration of the dark matter distribution and its relation to galaxy evolution.

  1. The REFLEX II galaxy cluster survey: power spectrum analysis

    NASA Astrophysics Data System (ADS)

    Balaguera-Antolínez, A.; Sánchez, Ariel G.; Böhringer, H.; Collins, C.; Guzzo, L.; Phleps, S.

    2011-05-01

    We present the power spectrum of galaxy clusters measured from the new ROSAT-ESO Flux-Limited X-Ray (REFLEX II) galaxy cluster catalogue. This new sample extends the flux limit of the original REFLEX catalogue to 1.8 × 10-12 erg s-1 cm-2, yielding a total of 911 clusters with ≥94 per cent completeness in redshift follow-up. The analysis of the data is improved by creating a set of 100 REFLEX II-catalogue-like mock galaxy cluster catalogues built from a suite of large-volume Λ cold dark matter (ΛCDM) N-body simulations (L-BASICC II). The measured power spectrum is in agreement with the predictions from a ΛCDM cosmological model. The measurements show the expected increase in the amplitude of the power spectrum with increasing X-ray luminosity. On large scales, we show that the shape of the measured power spectrum is compatible with a scale-independent bias and provide a model for the amplitude that allows us to connect our measurements with a cosmological model. By implementing a luminosity-dependent power-spectrum estimator, we observe that the power spectrum measured from the REFLEX II sample is weakly affected by flux-selection effects. The shape of the measured power spectrum is compatible with a featureless power spectrum on scales k > 0.01 h Mpc-1 and hence no statistically significant signal of baryonic acoustic oscillations can be detected. We show that the measured REFLEX II power spectrum displays signatures of non-linear evolution.

  2. The Herschel Point Source Catalogue

    NASA Astrophysics Data System (ADS)

    Marton, Gabor; Schulz, Bernhard; Altieri, Bruno; Calzoletti, Luca; Kiss, Csaba; Lim, Tanya; Lu, Nanyao; Paladini, Roberta; Papageorgiou, Andreas; Pearson, Chris; Rector, John; Shupe, David; Valtchanov, Ivan; Verebélyi, Erika; Xu, Kevin

    2015-08-01

    The Herschel Space Observatory was the fourth cornerstone mission in the European Space Agency (ESA) science programme with excellent broad band imaging capabilities in the submillimetre and far-infrared part of the spectrum. Although the spacecraft finished its observations in 2013, it left a large legacy dataset that is far from having been fully scrutinized and still has potential for new scientific discoveries. This is specifically true for the photometric observations of the PACS and SPIRE instruments that scanned >10% of the sky at 70, 100, 160, 250, 350 and 500 microns. Some source catalogs have already been produced by individual observing programs, but there are many observations that would never be analyzed for their full source content. To maximize the science return of the SPIRE and PACS data sets, our international team of instrument experts is in the process of building the Herschel Point Source Catalog (HPSC) from all scan map observations. Our homogeneous source extraction enables a systematic and unbiased comparison of sensitivity across the different Herschel fields that single programs will generally not be able to provide. The extracted point sources will contain individual YSOs of our Galaxy, unresolved YSO clusters in resolved nearby galaxies and unresolved galaxies of the local and distant Universe that are related to star formation. Such a huge dataset will help scientists better understand the evolution from interstellar clouds to individual stars. Furthermore the analysis of stellar clusters and the star formation on galactic scales will add more details to the understanding of star formation laws through time.We present our findings on comparison of different source detection and photometric tools. First results of the extractions are shown along with the description of our pipelines and catalogue entries. We also provide an additional science product, the structure noise map, that is used for the quality assessment of the catalogue in

  3. Algorithm for the direct reconstruction of the dark matter correlation function from weak lensing and galaxy clustering

    SciTech Connect

    Baldauf, Tobias; Smith, Robert E.; Seljak, Uros; Mandelbaum, Rachel

    2010-03-15

    The clustering of matter on cosmological scales is an essential probe for studying the physical origin and composition of our Universe. To date, most of the direct studies have focused on shear-shear weak lensing correlations, but it is also possible to extract the dark matter clustering by combining galaxy-clustering and galaxy-galaxy-lensing measurements. In order to extract the required information, one must relate the observable galaxy distribution to the underlying dark matter distribution. In this study we develop in detail a method that can constrain the dark matter correlation function from galaxy clustering and galaxy-galaxy-lensing measurements, by focusing on the correlation coefficient between the galaxy and matter overdensity fields. Our goal is to develop an estimator that maximally correlates the two. To generate a mock galaxy catalogue for testing purposes, we use the halo occupation distribution approach applied to a large ensemble of N-body simulations to model preexisting SDSS luminous red galaxy sample observations. Using this mock catalogue, we show that a direct comparison between the excess surface mass density measured by lensing and its corresponding galaxy clustering quantity is not optimal. We develop a new statistic that suppresses the small-scale contributions to these observations and show that this new statistic leads to a cross-correlation coefficient that is within a few percent of unity down to 5h{sup -1} Mpc. Furthermore, the residual incoherence between the galaxy and matter fields can be explained using a theoretical model for scale-dependent galaxy bias, giving us a final estimator that is unbiased to within 1%, so that we can reconstruct the dark matter clustering power spectrum at this accuracy up to k{approx}1h Mpc{sup -1}. We also perform a comprehensive study of other physical effects that can affect the analysis, such as redshift space distortions and differences in radial windows between galaxy clustering and weak

  4. On Ramanujan's definition of mock theta function.

    PubMed

    Rhoades, Robert C

    2013-05-01

    In his famous "deathbed" letter, Ramanujan "defined" the notion of a mock theta function and offered some examples of functions he believed satisfied his definition. Very recently, Griffin et al. established for the first time that Ramanujan's mock theta functions actually satisfy his own definition. On the other hand, Zwegers' 2002 doctoral thesis [Zwegers S (2002) Mock theta functions. PhD thesis (Univ Utrecht, Utrecht, The Netherlands)] showed that all of Ramanujan's examples are holomorphic parts of harmonic Maass forms. This has led to an alternate definition of a mock theta function. This paper shows that Ramanujan's definition of mock theta function is not equivalent to the modern definition. PMID:23625007

  5. Behavior of Neutral Hydrogen in the NGC 877/6 Galaxy Group

    NASA Astrophysics Data System (ADS)

    Manning Hall, Porter; Minchin, Robert F.; Taylor, Rhys

    2015-01-01

    We observed a 5 square degree area centered on -02:17:31, 14:32:00 at 21-cm as part of the Arecibo Galaxy Environment Survey (AGES) with the NGC 877/6 galaxy group at a velocity of 4000 km/s as the primary target. Our observations covered the redshift range -5,000 < cz < 20,000 km/s allowing for a large volume in front and behind the complex to be analyzed. The NGC 877/6 group contains 8 galaxies inside a common HI envelope with a total neutral hydrogen mass of LogMHI = 10.73. HI is detected outside of the optically-identified galaxies and there are a number of tidal features within the complex. These include AGC 749170, a possible tidal remnant identified by ALFALFA and whose detection we confirm here. Another, smaller group associated with UGC 1742 (LogMHI = 9.95; cz = 6900 km/s) was identified as showing signs of galaxy interaction as well as the possibility of a tidal formation not catalogued in NED as a galaxy. Of the 44 HI sources identified in the data cube, 12 (27%) were not previously recorded in the NED database as galaxies. We will continue our analysis with data from the Mock spectrometers which will extend the redshift range to 45000 km/s.

  6. A catalogue of AKARI FIS BSC extragalactic objects

    NASA Astrophysics Data System (ADS)

    Marton, Gabor; Toth, L. Viktor; Gyorgy Balazs, Lajos

    2015-08-01

    We combined photometric data of about 70 thousand point sources from the AKARI Far-Infrared Surveyor Bright Source Catalogue with AllWISE catalogue data to identify galaxies. We used Quadratic Discriminant Analysis (QDA) to classify our sources. The classification was based on a 6D parameter space that contained AKARI [F65/F90], [F90/F140], [F140/F160] and WISE W1-W2 colours along with WISE W1 magnitudes and AKARI [F140] flux values. Sources were classified into 3 main objects types: YSO candidates, evolved stars and galaxies. The training samples were SIMBAD entries of the input point sources wherever an associated SIMBAD object was found within a 30 arcsecond search radius. The QDA resulted more than 5000 AKARI galaxy candidate sources. The selection was tested cross-correlating our AKARI extragalactic catalogue with the Revised IRAS-FSC Redshift Catalogue (RIFSCz). A very good match was found. A further classification attempt was also made to differentiate between extragalactic subtypes using Support Vector Machines (SVMs). The results of the various methods showed that we can confidently separate cirrus dominated objects (type 1 of RIFSCz). Some of our “galaxy candidate” sources are associated with 2MASS extended objects, and listed in the NASA Extragalactic Database so far without clear proofs of their extragalactic nature. Examples will be presented in our poster. Finally other AKARI extragalactic catalogues will be also compared to our statistical selection.

  7. Color and magnitude dependence of galaxy clustering

    NASA Astrophysics Data System (ADS)

    Müller, Volker

    2016-10-01

    A quantitative study of the clustering properties of galaxies in the cosmic web as a function of absolute magnitude and colour is presented using the SDSS Data Release 7 galaxy redshift survey. We compare our results with mock galaxy samples obtained with four different semi-analytical models of galaxy formation imposed on the merger trees of the Millenium simulation.

  8. Measuring galaxy environment with the synergy of future photometric and spectroscopic surveys

    NASA Astrophysics Data System (ADS)

    Cucciati, O.; Marulli, F.; Cimatti, A.; Merson, A. I.; Norberg, P.; Pozzetti, L.; Baugh, C. M.; Branchini, E.

    2016-10-01

    We exploit the synergy between low-resolution spectroscopy and photometric redshifts to study environmental effects on galaxy evolution in slitless spectroscopic surveys from space. As a test case, we consider the future Euclid Deep survey (˜40 deg2), which combines a slitless spectroscopic survey limited at Hα flux ≥5 × 10-17 erg cm-2 s-1 and a photometric survey limited in H band (H ≤ 26). We use Euclid-like galaxy mock catalogues, in which we anchor the photometric redshifts to the 3D galaxy distribution of the available spectroscopic redshifts. We then estimate the local density contrast by counting objects in cylindrical cells with radius from 1 to 10 h-1Mpc, over the redshift range 0.9 < z < 1.8. We compare this density field with the one computed in a mock catalogue with the same depth as the Euclid Deep survey (H = 26) but without redshift measurement errors. We find that our method successfully separates high- from low-density environments (the last from the first quintile of the density distribution), with higher efficiency at low redshift and large cells: the fraction of low-density regions mistaken by high-density peaks is <1 per cent for all scales and redshifts explored, but for scales of 1 h-1Mpc for which is a few per cent. These results show that we can efficiently study environment in photometric samples if spectroscopic information is available for a smaller sample of objects that sparsely samples the same volume. We demonstrate that these studies are possible in the Euclid Deep survey, i.e. in a redshift range in which environmental effects are different from those observed in the local Universe, hence providing new constraints for galaxy evolution models.

  9. Efficient reconstruction of linear baryon acoustic oscillations in galaxy surveys

    NASA Astrophysics Data System (ADS)

    Burden, A.; Percival, W. J.; Manera, M.; Cuesta, Antonio J.; Vargas Magana, Mariana; Ho, Shirley

    2014-12-01

    Reconstructing an estimate of linear baryon acoustic oscillations (BAO) from an evolved galaxy field has become a standard technique in recent analyses. By partially removing non-linear damping caused by bulk motions, the real-space BAO peak in the correlation function is sharpened, and oscillations in the power spectrum are visible to smaller scales. In turn these lead to stronger measurements of the BAO scale. Future surveys are being designed assuming that this improvement has been applied, and this technique is therefore of critical importance for future BAO measurements. A number of reconstruction techniques are available, but the most widely used is a simple algorithm that decorrelates large-scale and small-scale modes approximately removing the bulk-flow displacements by moving the overdensity field. We consider the practical implementation of this algorithm, looking at the efficiency of reconstruction as a function of the assumptions made for the bulk-flow scale, the shot-noise level in a random catalogue used to quantify the mask and the method used to estimate the bulk-flow shifts. We also examine the efficiency of reconstruction against external factors including galaxy density, volume and edge effects, and consider their impact for future surveys. Throughout we make use of the mocks catalogues created for the Baryon Oscillation Spectroscopic Survey (BOSS) Date Release 11 samples covering 0.43 < z < 0.7 (CMASS) and 0.15 < z < 0.43 (LOWZ), to empirically test these changes.

  10. Quantifying correlations between galaxy emission lines and stellar continua

    NASA Astrophysics Data System (ADS)

    Beck, Róbert; Dobos, László; Yip, Ching-Wa; Szalay, Alexander S.; Csabai, István

    2016-03-01

    We analyse the correlations between continuum properties and emission line equivalent widths of star-forming and active galaxies from the Sloan Digital Sky Survey. Since upcoming large sky surveys will make broad-band observations only, including strong emission lines into theoretical modelling of spectra will be essential to estimate physical properties of photometric galaxies. We show that emission line equivalent widths can be fairly well reconstructed from the stellar continuum using local multiple linear regression in the continuum principal component analysis (PCA) space. Line reconstruction is good for star-forming galaxies and reasonable for galaxies with active nuclei. We propose a practical method to combine stellar population synthesis models with empirical modelling of emission lines. The technique will help generate more accurate model spectra and mock catalogues of galaxies to fit observations of the new surveys. More accurate modelling of emission lines is also expected to improve template-based photometric redshift estimation methods. We also show that, by combining PCA coefficients from the pure continuum and the emission lines, automatic distinction between hosts of weak active galactic nuclei (AGNs) and quiescent star-forming galaxies can be made. The classification method is based on a training set consisting of high-confidence starburst galaxies and AGNs, and allows for the similar separation of active and star-forming galaxies as the empirical curve found by Kauffmann et al. We demonstrate the use of three important machine learning algorithms in the paper: k-nearest neighbour finding, k-means clustering and support vector machines.

  11. Intensity mapping cross-correlations: connecting the largest scales to galaxy evolution

    NASA Astrophysics Data System (ADS)

    Wolz, L.; Tonini, C.; Blake, C.; Wyithe, J. S. B.

    2016-05-01

    Intensity mapping of the neutral hydrogen (H I) is a new observational tool to efficiently map the large-scale structure over wide redshift ranges. The cross-correlation of intensity maps with galaxy surveys is a robust measure of the cosmological power spectrum and the H I content of galaxies which diminishes systematics caused by instrumental effects and foreground removal. We examine the cross-correlation signature at redshift 0.9 using a semi-analytical galaxy formation model in order to model the H I gas of galaxies as well as their optical magnitudes. We determine the scale-dependent clustering of the cross-correlation power for different types of galaxies determined by their colours, which act as a proxy for their star formation activity. We find that the cross-correlation coefficient with H I density for red quiescent galaxies falls off more quickly on smaller scales k > 0.2 h Mpc-1 than for blue star-forming galaxies. Additionally, we create a mock catalogue of highly star-forming galaxies to mimic the WiggleZ Dark Energy Survey, and use this to predict existing and future measurements using data from the Green Bank telescope and Parkes telescope. We find that the cross-power of highly star-forming galaxies shows a higher clustering on small scales than any other galaxy type and that this significantly alters the power spectrum shape on scales k > 0.2 h Mpc-1. We show that the cross-correlation coefficient is not negligible when interpreting the cosmological cross-power spectrum and additionally contains information about the H I content of the optically selected galaxies.

  12. Galaxy-galaxy(-galaxy) lensing as a sensitive probe of galaxy evolution

    NASA Astrophysics Data System (ADS)

    Saghiha, H.; Hilbert, S.; Schneider, P.; Simon, P.

    2012-11-01

    Context. The gravitational lensing effect provides various ways to study the mass environment of galaxies. Aims: We investigate how galaxy-galaxy(-galaxy) lensing can be used to test models of galaxy formation and evolution. Methods: We consider two semi-analytic galaxy formation models based on the Millennium Run N-body simulation: the Durham model by Bower et al. (2006, MNRAS, 370, 645) and the Garching model by Guo et al. (2011, MNRAS, 413, 101). We generate mock lensing observations for the two models, and then employ Fast Fourier Transform methods to compute second- and third-order aperture statistics in the simulated fields for various galaxy samples. Results: We find that both models predict qualitatively similar aperture signals, but there are large quantitative differences. The Durham model predicts larger amplitudes in general. In both models, red galaxies exhibit stronger aperture signals than blue galaxies. Using these aperture measurements and assuming a linear deterministic bias model, we measure relative bias ratios of red and blue galaxy samples. We find that a linear deterministic bias is insufficient to describe the relative clustering of model galaxies below ten arcmin angular scales. Dividing galaxies into luminosity bins, the aperture signals decrease with decreasing luminosity for brighter galaxies, but increase again for fainter galaxies. This increase is likely an artifact due to too many faint satellite galaxies in massive group and cluster halos predicted by the models. Conclusions: Our study shows that galaxy-galaxy(-galaxy) lensing is a sensitive probe of galaxy evolution.

  13. Catalogue of Icelandic Volcanoes

    NASA Astrophysics Data System (ADS)

    Ilyinskaya, Evgenia; Larsen, Gudrun; Gudmundsson, Magnus T.; Vogfjord, Kristin; Pagneux, Emmanuel; Oddsson, Bjorn; Barsotti, Sara; Karlsdottir, Sigrun

    2016-04-01

    The Catalogue of Icelandic Volcanoes is a newly developed open-access web resource in English intended to serve as an official source of information about active volcanoes in Iceland and their characteristics. The Catalogue forms a part of an integrated volcanic risk assessment project in Iceland GOSVÁ (commenced in 2012), as well as being part of the effort of FUTUREVOLC (2012-2016) on establishing an Icelandic volcano supersite. Volcanic activity in Iceland occurs on volcanic systems that usually comprise a central volcano and fissure swarm. Over 30 systems have been active during the Holocene (the time since the end of the last glaciation - approximately the last 11,500 years). In the last 50 years, over 20 eruptions have occurred in Iceland displaying very varied activity in terms of eruption styles, eruptive environments, eruptive products and the distribution lava and tephra. Although basaltic eruptions are most common, the majority of eruptions are explosive, not the least due to magma-water interaction in ice-covered volcanoes. Extensive research has taken place on Icelandic volcanism, and the results reported in numerous scientific papers and other publications. In 2010, the International Civil Aviation Organisation (ICAO) funded a 3 year project to collate the current state of knowledge and create a comprehensive catalogue readily available to decision makers, stakeholders and the general public. The work on the Catalogue began in 2011, and was then further supported by the Icelandic government and the EU through the FP7 project FUTUREVOLC. The Catalogue of Icelandic Volcanoes is a collaboration of the Icelandic Meteorological Office (the state volcano observatory), the Institute of Earth Sciences at the University of Iceland, and the Civil Protection Department of the National Commissioner of the Iceland Police, with contributions from a large number of specialists in Iceland and elsewhere. The Catalogue is built up of chapters with texts and various

  14. Youth at Risk: Mock Disposition Hearing.

    ERIC Educational Resources Information Center

    Taylor, Elenor

    1988-01-01

    Presents materials necessary for conducting a mock disposition hearing in which students learn how courts deal with wayward and neglected juveniles. Intended to illustrate the problems that courts face in dealing with minors, the materials include activity instructions and a mock probation report to be used in the simulation. (GEA)

  15. Marine Science Film Catalogue.

    ERIC Educational Resources Information Center

    Chapman, Frank L.

    Forty-eight motion picture films and filmstrips in the field of marine science are catalogued in this booklet. Following the alphabetical index, one page is devoted to each film indicating its type, producer, recommended grade level, running time, and presence of color and/or sound. A summary of film content, possible uses, and outstanding…

  16. Standard Asteroid Photometric Catalogue

    NASA Astrophysics Data System (ADS)

    Piironen, J.; Lagerkvist, C.-I.; Torppa, J.; Kaasalainen, M.; Warner, B.

    2001-12-01

    The Asteroid Photometric Catalogue (APC) is now in its fifth update with over 8600 lightcurves of more than 1000 asteroids in the database. The APC also has references of over one thousand lightcurves not in digital format. The catalogue has been published by Uppsala University Observatory and is distributed by request (contact: classe@astro.uu.se). The new update also includes a list of known asteroid rotational periods and a CD-ROM containing all the existing digital data in the APC. The total number of observed lightcurves is growing rapidly, not the least because of the new state-of-the-art equipment and growing interest among amateur astronomers. The photometric database is now so large that the present format must be altered to facilitate a user-friendly on-line service for the down- and uploading of data. We are proposing (and have started to construct) a new Internet-based Standard Asteroid Photometric Catalogue (SAPC). The website is planned to open during the first half of the year 2002. In addition to the data files, the site would contain the index and guide to the catalogue, a web-form for reporting observations, and some general observing guidelines (e.g., on filters, timing, etc.). There would also be a list of asteroids for which more observations are needed, together with recommended observing periods. This would be accompanied by an up-to-date collection of physical asteroid models based on photometric data, as well as links to observer network pages and other sites that work in collaboration with the catalogue project. Our aim is to develop this site into a global standard service used by everyone involved in asteroid photometry.

  17. VizieR Online Data Catalog: The ENACS Catalogue. V. (Katgert+ 1998)

    NASA Astrophysics Data System (ADS)

    Katgert, P.; Mazure, A.; den Hartog, R.; Adami, C.; Biviano, A.; Perea, J.

    1998-04-01

    Table enacs presents the full ENACS catalogue: i.e. redshifts and photometry of 5634 galaxies in the directions of 107 rich Southern cluster candidates from the ACO catalogue. Table 2 of this paper lists additional redshifts from the literature for 33 galaxies contained within the Optopus areas of 4 clusters observed in the ENACS. Table 5 of this paper lists the centre of the Optopus plates and the dates of the Optopus observations (3 data files).

  18. Catalogue of Icelandic volcanoes

    NASA Astrophysics Data System (ADS)

    Ilyinskaya, Evgenia; Larsen, Gudrun; Vogfjörd, Kristin; Tumi Gudmundsson, Magnus; Jonsson, Trausti; Oddsson, Björn; Reynisson, Vidir; Barsotti, Sara; Karlsdottir, Sigrun

    2015-04-01

    Volcanic activity in Iceland occurs on volcanic systems that usually comprise a central volcano and fissure swarm. Over 30 systems have been active during the Holocene. In the last 100 years, over 30 eruptions have occurred displaying very varied activity in terms of eruption styles, eruptive environments, eruptive products and their distribution. Although basaltic eruptions are most common, the majority of eruptions are explosive, not the least due to magma-water interaction in ice-covered volcanoes. Extensive research has taken place on Icelandic volcanism, and the results reported in scientific papers and other publications. In 2010, the International Civil Aviation Organisation funded a 3 year project to collate the current state of knowledge and create a comprehensive catalogue readily available to decision makers, stakeholders and the general public. The work on the Catalogue began in 2011, and was then further supported by the Icelandic government and the EU. The Catalogue forms a part of an integrated volcanic risk assessment project in Iceland (commenced in 2012), and the EU FP7 project FUTUREVOLC (2012-2016), establishing an Icelandic volcano Supersite. The Catalogue is a collaborative effort between the Icelandic Meteorological Office (the state volcano observatory), the Institute of Earth Sciences at the University of Iceland, and the Icelandic Civil Protection, with contributions from a large number of specialists in Iceland and elsewhere. The catalogue is scheduled for opening in the first half of 2015 and once completed, it will be an official publication intended to serve as an accurate and up to date source of information about active volcanoes in Iceland and their characteristics. The Catalogue is an open web resource in English and is composed of individual chapters on each of the volcanic systems. The chapters include information on the geology and structure of the volcano; the eruption history, pattern and products; the known precursory signals

  19. Merged infrared catalogue

    NASA Technical Reports Server (NTRS)

    Schmitz, M.; Brown, L. W.; Mead, J. M.; Nagy, T. A.

    1978-01-01

    A compilation of equatorial coordinates, spectral types, magnitudes, and fluxes from five catalogues of infrared observations is presented. This first edition of the Merged Infrared Catalogue contains 11,201 oservations from the Two-Micron Sky Survey, Observations of Infrared Radiation from Cool Stars, the Air Force Geophysics Laboratory four Color Infrared Sky Survey and its Supplemental Catalog, and from Catalog of 10 micron Celestial Objects (HALL). This compilation is a by-product of a computerized infrared data base under development at Goddard Space Flight Center; the objective is to maintain a complete and current record of all infrared observations from 1 micron m to 1000 micron m of nonsolar system objects. These observations are being placed into a standardized system.

  20. Technology Catalogue. First edition

    SciTech Connect

    Not Available

    1994-02-01

    The Department of Energy`s Office of Environmental Restoration and Waste Management (EM) is responsible for remediating its contaminated sites and managing its waste inventory in a safe and efficient manner. EM`s Office of Technology Development (OTD) supports applied research and demonstration efforts to develop and transfer innovative, cost-effective technologies to its site clean-up and waste management programs within EM`s Office of Environmental Restoration and Office of Waste Management. The purpose of the Technology Catalogue is to provide performance data on OTD-developed technologies to scientists and engineers assessing and recommending technical solutions within the Department`s clean-up and waste management programs, as well as to industry, other federal and state agencies, and the academic community. OTD`s applied research and demonstration activities are conducted in programs referred to as Integrated Demonstrations (IDs) and Integrated Programs (IPs). The IDs test and evaluate.systems, consisting of coupled technologies, at specific sites to address generic problems, such as the sensing, treatment, and disposal of buried waste containers. The IPs support applied research activities in specific applications areas, such as in situ remediation, efficient separations processes, and site characterization. The Technology Catalogue is a means for communicating the status. of the development of these innovative technologies. The FY93 Technology Catalogue features technologies successfully demonstrated in the field through IDs and sufficiently mature to be used in the near-term. Technologies from the following IDs are featured in the FY93 Technology Catalogue: Buried Waste ID (Idaho National Engineering Laboratory, Idaho); Mixed Waste Landfill ID (Sandia National Laboratories, New Mexico); Underground Storage Tank ID (Hanford, Washington); Volatile organic compound (VOC) Arid ID (Richland, Washington); and VOC Non-Arid ID (Savannah River Site, South Carolina).

  1. Fingers-of-God effect of infalling satellite galaxies

    NASA Astrophysics Data System (ADS)

    Hikage, Chiaki; Yamamoto, Kazuhiro

    2016-01-01

    Non-linear redshift-space distortion known as the Fingers-of-God (FoG) effect is a major systematic uncertainty in redshift-space distortion studies conducted to test gravity models. The FoG effect has been usually attributed to the random motion of galaxies inside their clusters. When the internal galaxy motion is not well virialized, however, the coherent infalling motion towards the cluster centre generates the FoG effect. Here, we derive an analytical model of the satellite velocity distribution due to the infall motion combined with the random motion. We show that the velocity distribution becomes far from Maxwellian when the infalling motion is dominant. We use simulated subhalo catalogues to find that the contribution of infall motion is important to massive subhaloes and that the velocity distribution has a top-hat like shape as expected from our analytic model. We also study the FoG effect due to infall motion on the redshift-space power spectrum. Using simulated mock samples of luminous red galaxies constructed from haloes and massive subhaloes in N-body simulations, we show that the redshift-space power spectra can differ from expectations when the infall motion is ignored.

  2. Searchable solar feature catalogues

    NASA Astrophysics Data System (ADS)

    Zharkova, V. V.; Aboudarham, J.; Zharkov, S.; Ipson, S. S.; Benkhalil, A. K.; Fuller, N.

    The searchable Solar Feature Catalogues (SFCs) are developed from digitized solar images using automated pattern recognition techniques. The techniques were applied for the detection of sunspots, active regions, filaments and line-of-sight magnetic neutral lines in automatically standardized full disk solar images in Ca II K1, Ca II K3 and Ha lines taken at the Paris-Meudon Observatory and white light images and magnetograms from SOHO/MDI. The results of the automated recognition were verified with manual synoptic maps and available statistical data that revealed good detection accuracy. Based on the recognized parameters, a structured database of Solar Feature Catalogues was built on a MySQL server for every feature and published with various pre-designed search pages on the Bradford University web site http://www.cyber.brad.ac.uk/egso/SFC/. The SFCs with nine year coverage (1996-2004) is to be used for deeper investigation of the feature classification and solar activity forecast.

  3. The DES Science Verification weak lensing shear catalogues

    NASA Astrophysics Data System (ADS)

    Jarvis, M.; Sheldon, E.; Zuntz, J.; Kacprzak, T.; Bridle, S. L.; Amara, A.; Armstrong, R.; Becker, M. R.; Bernstein, G. M.; Bonnett, C.; Chang, C.; Das, R.; Dietrich, J. P.; Drlica-Wagner, A.; Eifler, T. F.; Gangkofner, C.; Gruen, D.; Hirsch, M.; Huff, E. M.; Jain, B.; Kent, S.; Kirk, D.; MacCrann, N.; Melchior, P.; Plazas, A. A.; Refregier, A.; Rowe, B.; Rykoff, E. S.; Samuroff, S.; Sánchez, C.; Suchyta, E.; Troxel, M. A.; Vikram, V.; Abbott, T.; Abdalla, F. B.; Allam, S.; Annis, J.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Castander, F. J.; Clampitt, J.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; DePoy, D. L.; Desai, S.; Diehl, H. T.; Doel, P.; Fausti Neto, A.; Flaugher, B.; Fosalba, P.; Frieman, J.; Gaztanaga, E.; Gerdes, D. W.; Gruendl, R. A.; Gutierrez, G.; Honscheid, K.; James, D. J.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lima, M.; March, M.; Martini, P.; Miquel, R.; Mohr, J. J.; Neilsen, E.; Nord, B.; Ogando, R.; Reil, K.; Romer, A. K.; Roodman, A.; Sako, M.; Sanchez, E.; Scarpine, V.; Schubnell, M.; Sevilla-Noarbe, I.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Swanson, M. E. C.; Tarle, G.; Thaler, J.; Thomas, D.; Walker, A. R.; Wechsler, R. H.

    2016-08-01

    We present weak lensing shear catalogues for 139 square degrees of data taken during the Science Verification (SV) time for the new Dark Energy Camera (DECam) being used for the Dark Energy Survey (DES). We describe our object selection, point spread function estimation and shear measurement procedures using two independent shear pipelines, IM3SHAPE and NGMIX, which produce catalogues of 2.12 million and 3.44 million galaxies, respectively. We detail a set of null tests for the shear measurements and find that they pass the requirements for systematic errors at the level necessary for weak lensing science applications using the SV data. We also discuss some of the planned algorithmic improvements that will be necessary to produce sufficiently accurate shear catalogues for the full 5-yr DES, which is expected to cover 5000 square degrees.

  4. Technology catalogue. Second edition

    SciTech Connect

    1995-04-01

    The Department of Energy`s (DOE`s) Office of Environmental Management (EM) is responsible for remediating DOE contaminated sites and managing the DOE waste inventory in a safe and efficient manner. EM`s Office of Technology Development (OTD) supports applied research and demonstration efforts to develop and transfer innovative, cost-effective technologies to its site clean-up and waste-management programs within EM. The purpose of the Technology Catalogue is to: (a) provide performance data on OTD-developed technologies to scientists and engineers responsible for preparing Remedial Investigation/Feasibility Studies (RI/FSs) and other compliance documents for the DOE`s clean-up and waste-management programs; and (b) identify partnering and commercialization opportunities with industry, other federal and state agencies, and the academic community.

  5. Modelling and interpreting spectral energy distributions of galaxies with BEAGLE

    NASA Astrophysics Data System (ADS)

    Chevallard, Jacopo; Charlot, Stéphane

    2016-10-01

    We present a new-generation tool to model and interpret spectral energy distributions (SEDs) of galaxies, which incorporates in a consistent way the production of radiation and its transfer through the interstellar and intergalactic media. This flexible tool, named BEAGLE (for BayEsian Analysis of GaLaxy sEds), allows one to build mock galaxy catalogues as well as to interpret any combination of photometric and spectroscopic galaxy observations in terms of physical parameters. The current version of the tool includes versatile modelling of the emission from stars and photoionized gas, attenuation by dust and accounting for different instrumental effects, such as spectroscopic flux calibration and line spread function. We show a first application of the BEAGLE tool to the interpretation of broad-band SEDs of a published sample of ˜ 10^4 galaxies at redshifts 0.1 ≲ z ≲ 8. We find that the constraints derived on photometric redshifts using this multipurpose tool are comparable to those obtained using public, dedicated photometric-redshift codes and quantify this result in a rigorous statistical way. We also show how the post-processing of BEAGLE output data with the PYTHON extension PYP-BEAGLE allows the characterization of systematic deviations between models and observations, in particular through posterior predictive checks. The modular design of the BEAGLE tool allows easy extensions to incorporate, for example, the absorption by neutral galactic and circumgalactic gas, and the emission from an active galactic nucleus, dust and shock-ionized gas. Information about public releases of the BEAGLE tool will be maintained on http://www.jacopochevallard.org/beagle.

  6. Extragalactic distance scale derived from ''sosie'' galaxies. I. Distances of 167 galaxies which are sosies of 14 nearby galaxies

    SciTech Connect

    Bottinelli; Gouguenheim, L.; Paturel, G.; de Vaucouleurs, G.

    1985-11-01

    The method of ''sosie'' galaxies is applied to a large sample of galaxies extracted from the BGP catalog of H I line data and the Second Reference Catalogue of Bright Galaxies. The ''sosies'' of 14 calibrating galaxies (primary calibrators and galaxies in the nearest groups) are defined as those having the same parameters, either (1) morphological type T, axis ratio R, and maximum rotation velocity V/sub M/ or (2) T, R, and luminosity index ..lambda../sub c/.

  7. Detection of satellite remnants in the Galactic halo with Gaia- III. Detection limits for ultrafaint dwarf galaxies

    NASA Astrophysics Data System (ADS)

    Antoja, T.; Mateu, C.; Aguilar, L.; Figueras, F.; Antiche, E.; Hernández-Pérez, F.; Brown, A. G. A.; Valenzuela, O.; Aparicio, A.; Hidalgo, S.; Velázquez, H.

    2015-10-01

    We present a method to identify ultrafaint dwarf galaxies (UFDGs) candidates in the halo of the Milky Way using the future Gaia catalogue and we explore its detection limits and completeness. The method is based on the Wavelet Transform and searches for overdensities in the combined space of sky coordinates and proper motions, using kinematics in the search for the first time. We test the method with a Gaia mock catalogue that has the Gaia Universe Model Snapshot as a background, and use a library of around 30 000 UFDGs simulated as Plummer spheres with a single stellar population. For the UFDGs, we use a wide range of structural and orbital parameters that go beyond the range spanned by real systems, where some UFDGs may remain undetected. We characterize the detection limits as function of the number of observable stars by Gaia in the UFDGs with respect to that of the background and their apparent sizes in the sky and proper motion planes. We find that the addition of proper motions in the search improves considerably the detections compared to a photometric survey at the same magnitude limit. Our experiments suggest that Gaia will be able to detect UFDGs that are similar to some of the known UFDGs even if the limit of Gaia is around 2 mag brighter than that of SDSS, with the advantage of having a full-sky catalogue. We also see that Gaia could even find some UFDGs that have lower surface brightness than the SDSS limit.

  8. X-ray selected stars in HRC and BHRC catalogues

    NASA Astrophysics Data System (ADS)

    Mickaelian, A. M.; Paronyan, G. M.

    2014-12-01

    A joint HRC/BHRC Catalogue has been created based on merging of Hamburg ROSAT Catalogue (HRC) and Byurakan Hamburg ROSAT Catalogue (BHRC). Both have been made by optical identifications of X-ray sources based on low-dispersion spectra of the Hamburg Quasar Survey (HQS) using ROSAT Catalogues. As a result, the largest sample of 8132 (5341+2791) optically identified X-ray sources was created having count rate (CR) of photons ≤ 0.04 ct/s in the area with galactic latitudes |b|≤ 20° and declinations d≤ 0°.There are 4253 AGN, 492 galaxies, 1800 stars and 1587 unknown objects in the sample. All stars have been found in GSC 2.3.2, as well as most of them are in GALEX, USNO-B1.0, 2MASS and WISE catalogues. In addition, 1429 are in SDSS DR9 and 204 have SDSS spectra. For these stars we have carried out spectral classification and along with the bright stars, many new cataclysmic variables (CV), white dwarfs (WD) and late-type stars (K-M and C) have been revealed. For all stars, statistical studies of their multiwavelength properties have been made. An attempt to find a connection between the radiation fluxes in different bands for different types of sources, and identify their characteristics was made as well.

  9. A FIRST LOOK AT CREATING MOCK CATALOGS WITH MACHINE LEARNING TECHNIQUES

    SciTech Connect

    Xu Xiaoying; Ho, Shirley; Trac, Hy; Schneider, Jeff; Ntampaka, Michelle; Poczos, Barnabas

    2013-08-01

    We investigate machine learning (ML) techniques for predicting the number of galaxies (N{sub gal}) that occupy a halo, given the halo's properties. These types of mappings are crucial for constructing the mock galaxy catalogs necessary for analyses of large-scale structure. The ML techniques proposed here distinguish themselves from traditional halo occupation distribution (HOD) modeling as they do not assume a prescribed relationship between halo properties and N{sub gal}. In addition, our ML approaches are only dependent on parent halo properties (like HOD methods), which are advantageous over subhalo-based approaches as identifying subhalos correctly is difficult. We test two algorithms: support vector machines (SVM) and k-nearest-neighbor (kNN) regression. We take galaxies and halos from the Millennium simulation and predict N{sub gal} by training our algorithms on the following six halo properties: number of particles, M{sub 200}, {sigma}{sub v}, v{sub max}, half-mass radius, and spin. For Millennium, our predicted N{sub gal} values have a mean-squared error (MSE) of {approx}0.16 for both SVM and kNN. Our predictions match the overall distribution of halos reasonably well and the galaxy correlation function at large scales to {approx}5%-10%. In addition, we demonstrate a feature selection algorithm to isolate the halo parameters that are most predictive, a useful technique for understanding the mapping between halo properties and N{sub gal}. Lastly, we investigate these ML-based approaches in making mock catalogs for different galaxy subpopulations (e.g., blue, red, high M{sub star}, low M{sub star}). Given its non-parametric nature as well as its powerful predictive and feature selection capabilities, ML offers an interesting alternative for creating mock catalogs.

  10. Functional Mock-up Unit Export of EnergyPlus

    SciTech Connect

    2012-08-01

    The Functional Mock-up Unit Export of EnergyPlus is a software package that allows EnergyPlus to be exported as a Functional Mock-up Unit. This allows other software tools to run EnergyPlus as part of a larger simulation. To do so, the outside software needs to implement the Functional Mock-up interface standard (http://www.modelisar.com/), and be able to import Functional Mock-up Units for co-simulation.

  11. The PASTEL catalogue: 2016 version

    NASA Astrophysics Data System (ADS)

    Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent

    2016-06-01

    The bibliographical compilation of stellar atmospheric parameters (Teff, log g, [Fe/H]) relying on high-resolution, high signal-to-noise spectroscopy started in the eighties with the so-called [Fe/H] catalogue, and was continued in 2010 with the PASTEL catalogue, which also includes determinations of Teff alone, based on various methods. Here we present an update of the PASTEL catalogue. The main journals and the CDS database have been surveyed to find relevant publications presenting new determinations of atmospheric parameters. As of February 2016, PASTEL includes 64 082 determinations of either Teff or (Teff, log g, [Fe/H]) for 31 401 stars, corresponding to 1142 bibliographical references. Some 11 197 stars have a determination of the three parameters (Teff, log g, [Fe/H]) with a high-quality spectroscopic metallicity. The PASTEL catalogue is available in electronic form at the CDS (http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/pastel).

  12. Connecting massive galaxies to dark matter haloes in BOSS - I. Is galaxy colour a stochastic process in high-mass haloes?

    NASA Astrophysics Data System (ADS)

    Saito, Shun; Leauthaud, Alexie; Hearin, Andrew P.; Bundy, Kevin; Zentner, Andrew R.; Behroozi, Peter S.; Reid, Beth A.; Sinha, Manodeep; Coupon, Jean; Tinker, Jeremy L.; White, Martin; Schneider, Donald P.

    2016-08-01

    We use subhalo abundance matching (SHAM) to model the stellar mass function (SMF) and clustering of the Baryon Oscillation Spectroscopic Survey (BOSS) `CMASS' sample at z ˜ 0.5. We introduce a novel method which accounts for the stellar mass incompleteness of CMASS as a function of redshift, and produce CMASS mock catalogues which include selection effects, reproduce the overall SMF, the projected two-point correlation function wp, the CMASS dn/dz, and are made publicly available. We study the effects of assembly bias above collapse mass in the context of `age matching' and show that these effects are markedly different compared to the ones explored by Hearin et al. at lower stellar masses. We construct two models, one in which galaxy colour is stochastic (`AbM' model) as well as a model which contains assembly bias effects (`AgM' model). By confronting the redshift dependent clustering of CMASS with the predictions from our model, we argue that that galaxy colours are not a stochastic process in high-mass haloes. Our results suggest that the colours of galaxies in high-mass haloes are determined by other halo properties besides halo peak velocity and that assembly bias effects play an important role in determining the clustering properties of this sample.

  13. Efficient construction of mock catalogs for baryon acoustic oscillation surveys

    NASA Astrophysics Data System (ADS)

    Sunayama, Tomomi; Padmanabhan, Nikhil; Heitmann, Katrin; Habib, Salman; Rangel, Esteban

    2016-05-01

    Precision measurements of the large scale structure of the Universe require large numbers of high fidelity mock catalogs to accurately assess, and account for, the presence of systematic effects. We introduce and test a scheme for generating mock catalogs rapidly using suitably derated N-body simulations. Our aim is to reproduce the large scale structure and the gross properties of dark matter halos with high accuracy, while sacrificing the details of the halo's internal structure. By adjusting global and local time-steps in an N-body code, we demonstrate that we recover halo masses to better than 0.5% and the power spectrum to better than 1% both in real and redshift space for k=1hMpc-1, while requiring a factor of 4 less CPU time. We also calibrate the redshift spacing of outputs required to generate simulated light cones. We find that outputs separated by Δ z=0.05 allow us to interpolate particle positions and velocities to reproduce the real and redshift space power spectra to better than 1% (out to k=1hMpc-1). We apply these ideas to generate a suite of simulations spanning a range of cosmologies, motivated by the Baryon Oscillation Spectroscopic Survey (BOSS) but broadly applicable to future large scale structure surveys including eBOSS and DESI. As an initial demonstration of the utility of such simulations, we calibrate the shift in the baryonic acoustic oscillation peak position as a function of galaxy bias with higher precision than has been possible so far. This paper also serves to document the simulations, which we make publicly available.

  14. Efficient construction of mock catalogs for baryon acoustic oscillation surveys

    NASA Astrophysics Data System (ADS)

    Sunayama, Tomomi; Padmanabhan, Nikhil; Heitmann, Katrin; Habib, Salman; Rangel, Esteban

    2016-05-01

    Precision measurements of the large scale structure of the Universe require large numbers of high fidelity mock catalogs to accurately assess, and account for, the presence of systematic effects. We introduce and test a scheme for generating mock catalogs rapidly using suitably derated N-body simulations. Our aim is to reproduce the large scale structure and the gross properties of dark matter halos with high accuracy, while sacrificing the details of the halo's internal structure. By adjusting global and local time-steps in an N-body code, we demonstrate that we recover halo masses to better than 0.5% and the power spectrum to better than 1% both in real and redshift space for k=1hMpc‑1, while requiring a factor of 4 less CPU time. We also calibrate the redshift spacing of outputs required to generate simulated light cones. We find that outputs separated by Δ z=0.05 allow us to interpolate particle positions and velocities to reproduce the real and redshift space power spectra to better than 1% (out to k=1hMpc‑1). We apply these ideas to generate a suite of simulations spanning a range of cosmologies, motivated by the Baryon Oscillation Spectroscopic Survey (BOSS) but broadly applicable to future large scale structure surveys including eBOSS and DESI. As an initial demonstration of the utility of such simulations, we calibrate the shift in the baryonic acoustic oscillation peak position as a function of galaxy bias with higher precision than has been possible so far. This paper also serves to document the simulations, which we make publicly available.

  15. Catalogue of Texas spiders

    PubMed Central

    Dean, David Allen

    2016-01-01

    Abstract This catalogue lists 1,084 species of spiders (three identified to genus only) in 311 genera from 53 families currently recorded from Texas and is based on the “Bibliography of Texas Spiders” published by Bea Vogel in 1970. The online list of species can be found at http://pecanspiders.tamu.edu/spidersoftexas.htm. Many taxonomic revisions have since been published, particularly in the families Araneidae, Gnaphosidae and Leptonetidae. Many genera in other families have been revised. The Anyphaenidae, Ctenidae, Hahniidae, Nesticidae, Sicariidae and Tetragnathidae were also revised. Several families have been added and others split up. Several genera of Corinnidae were transferred to Phrurolithidae and Trachelidae. Two genera from Miturgidae were transferred to Eutichuridae. Zoridae was synonymized under Miturgidae. A single species formerly in Amaurobiidae is now in the Family Amphinectidae. Some trapdoor spiders in the family Ctenizidae have been transferred to Euctenizidae. Gertsch and Mulaik started a list of Texas spiders in 1940. In a letter from Willis J. Gertsch dated October 20, 1982, he stated “Years ago a first listing of the Texas fauna was published by me based largely on Stanley Mulaik material, but it had to be abandoned because of other tasks.” This paper is a compendium of the spiders of Texas with distribution, habitat, collecting method and other data available from revisions and collections. This includes many records and unpublished data (including data from three unpublished studies). One of these studies included 16,000 adult spiders belonging to 177 species in 29 families. All specimens in that study were measured and results are in the appendix. Hidalgo County has 340 species recorded with Brazos County at 323 and Travis County at 314 species. These reflect the amount of collecting in the area. PMID:27103878

  16. Catalogue of Texas spiders.

    PubMed

    Dean, David Allen

    2016-01-01

    This catalogue lists 1,084 species of spiders (three identified to genus only) in 311 genera from 53 families currently recorded from Texas and is based on the "Bibliography of Texas Spiders" published by Bea Vogel in 1970. The online list of species can be found at http://pecanspiders.tamu.edu/spidersoftexas.htm. Many taxonomic revisions have since been published, particularly in the families Araneidae, Gnaphosidae and Leptonetidae. Many genera in other families have been revised. The Anyphaenidae, Ctenidae, Hahniidae, Nesticidae, Sicariidae and Tetragnathidae were also revised. Several families have been added and others split up. Several genera of Corinnidae were transferred to Phrurolithidae and Trachelidae. Two genera from Miturgidae were transferred to Eutichuridae. Zoridae was synonymized under Miturgidae. A single species formerly in Amaurobiidae is now in the Family Amphinectidae. Some trapdoor spiders in the family Ctenizidae have been transferred to Euctenizidae. Gertsch and Mulaik started a list of Texas spiders in 1940. In a letter from Willis J. Gertsch dated October 20, 1982, he stated "Years ago a first listing of the Texas fauna was published by me based largely on Stanley Mulaik material, but it had to be abandoned because of other tasks." This paper is a compendium of the spiders of Texas with distribution, habitat, collecting method and other data available from revisions and collections. This includes many records and unpublished data (including data from three unpublished studies). One of these studies included 16,000 adult spiders belonging to 177 species in 29 families. All specimens in that study were measured and results are in the appendix. Hidalgo County has 340 species recorded with Brazos County at 323 and Travis County at 314 species. These reflect the amount of collecting in the area. PMID:27103878

  17. Luminosity function for galaxy clusters

    NASA Astrophysics Data System (ADS)

    Bajan, K.; Biernacka, M.; Flin, P.; Godłowski, W.; Panko, E.; Popiela, J.

    2016-10-01

    We constructed and studied the luminosity function of 6188 galaxyclusters. This was performed by counting brightness of galaxiesbelonging to clusters in the PF catalogue, taking galaxy data fromMRSS. Our result shows that the investigated structures arecharacterized by a luminosity function different from that ofoptical galaxies and radiogalaxies (Machalski & Godłowski2000). The implications of this result for theoriesof galaxy formation are briefly discussed.

  18. Remnant radio galaxies in the LOFAR Lockman Hole

    NASA Astrophysics Data System (ADS)

    Brienza, Marisa; Godfrey, Leith; Morganti, Raffaella

    2016-08-01

    I will present recent 150-MHz deep observations performed with the Low-frequency Array (LOFAR) of the well-known extragalactic region of the Lockman Hole. Thanks to its high sensitivity and resolution this data allows us to perform new studies of the radio loud AGN population at low radio frequencies. In particular, we conducted a systematic search of remnant radio galaxies, which represent the final "dying" phase of the radio galaxy evolution, when the jets have switched off. This class of sources is best to investigate the life-cycle of radio loud AGN as well as to quantify the role of radio AGN feedback. Indeed, the modelling of their radio spectrum provides constraints on the time-scales of activity and quiescence of the radio source and on its energy output. For a long time there have been claims that deep low-frequency surveys would have enhanced the detection of this class of sources, which are usually rare in flux limited samples.With our search, we thus intend to provide good statistics on the detection and properties of remnant radio galaxies. To avoid selection biases towards any specific class of objects we used both morphological and spectral selection criteria. To do this we combined the LOFAR data with publicly available surveys at other frequencies as well as dedicated deep observations. We find that the fraction of candidate remnant sources is < 6-8% of the entire radio source population and is dominated by steep spectrum sources. To better understand the observed fraction we developed mock catalogues of the radio sky population based on radio galaxy evolution models. These models are used to constrain the main mechanisms contributing to the source luminosity evolution i.e. adiabatic expansion, radiative losses, as well as to make predictions on their fraction in flux limited samples.

  19. Measures of galaxy environment - I. What is 'environment'?

    NASA Astrophysics Data System (ADS)

    Muldrew, Stuart I.; Croton, Darren J.; Skibba, Ramin A.; Pearce, Frazer R.; Ann, Hong Bae; Baldry, Ivan K.; Brough, Sarah; Choi, Yun-Young; Conselice, Christopher J.; Cowan, Nicolas B.; Gallazzi, Anna; Gray, Meghan E.; Grützbauch, Ruth; Li, I.-Hui; Park, Changbom; Pilipenko, Sergey V.; Podgorzec, Bret J.; Robotham, Aaron S. G.; Wilman, David J.; Yang, Xiaohu; Zhang, Youcai; Zibetti, Stefano

    2012-01-01

    The influence of a galaxy's environment on its evolution has been studied and compared extensively in the literature, although differing techniques are often used to define environment. Most methods fall into two broad groups: those that use nearest neighbours to probe the underlying density field and those that use fixed apertures. The differences between the two inhibit a clean comparison between analyses and leave open the possibility that, even with the same data, different properties are actually being measured. In this work, we apply 20 published environment definitions to a common mock galaxy catalogue constrained to look like the local Universe. We find that nearest-neighbour-based measures best probe the internal densities of high-mass haloes, while at low masses the interhalo separation dominates and acts to smooth out local density variations. The resulting correlation also shows that nearest-neighbour galaxy environment is largely independent of dark matter halo mass. Conversely, aperture-based methods that probe superhalo scales accurately identify high-density regions corresponding to high-mass haloes. Both methods show how galaxies in dense environments tend to be redder, with the exception of the largest apertures, but these are the strongest at recovering the background dark matter environment. We also warn against using photometric redshifts to define environment in all but the densest regions. When considering environment, there are two regimes: the 'local environment' internal to a halo best measured with nearest neighbour and 'large-scale environment' external to a halo best measured with apertures. This leads to the conclusion that there is no universal environment measure and the most suitable method depends on the scale being probed.

  20. Machine learning etudes in astrophysics: selection functions for mock cluster catalogs

    SciTech Connect

    Hajian, Amir; Alvarez, Marcelo A.; Bond, J. Richard E-mail: malvarez@cita.utoronto.ca

    2015-01-01

    Making mock simulated catalogs is an important component of astrophysical data analysis. Selection criteria for observed astronomical objects are often too complicated to be derived from first principles. However the existence of an observed group of objects is a well-suited problem for machine learning classification. In this paper we use one-class classifiers to learn the properties of an observed catalog of clusters of galaxies from ROSAT and to pick clusters from mock simulations that resemble the observed ROSAT catalog. We show how this method can be used to study the cross-correlations of thermal Sunya'ev-Zeldovich signals with number density maps of X-ray selected cluster catalogs. The method reduces the bias due to hand-tuning the selection function and is readily scalable to large catalogs with a high-dimensional space of astrophysical features.

  1. CMB-galaxy correlation in Unified Dark Matter scalar field cosmologies

    SciTech Connect

    Bertacca, Daniele; Bartolo, Nicola; Matarrese, Sabino; Raccanelli, Alvise; Piattella, Oliver F.; Pietrobon, Davide; Giannantonio, Tommaso E-mail: alvise.raccanelli@port.ac.uk E-mail: davide.pietrobon@jpl.nasa.gov E-mail: sabino.matarrese@pd.infn.it

    2011-03-01

    We present an analysis of the cross-correlation between the CMB and the large-scale structure (LSS) of the Universe in Unified Dark Matter (UDM) scalar field cosmologies. We work out the predicted cross-correlation function in UDM models, which depends on the speed of sound of the unified component, and compare it with observations from six galaxy catalogues (NVSS, HEAO, 2MASS, and SDSS main galaxies, luminous red galaxies, and quasars). We sample the value of the speed of sound and perform a likelihood analysis, finding that the UDM model is as likely as the ΛCDM, and is compatible with observations for a range of values of c{sub ∞} (the value of the sound speed at late times) on which structure formation depends. In particular, we obtain an upper bound of c{sub ∞}{sup 2} ≤ 0.009 at 95% confidence level, meaning that the ΛCDM model, for which c{sub ∞}{sup 2} = 0, is a good fit to the data, while the posterior probability distribution peaks at the value c{sub ∞}{sup 2} = 10{sup −4} . Finally, we study the time dependence of the deviation from ΛCDM via a tomographic analysis using a mock redshift distribution and we find that the largest deviation is for low-redshift sources, suggesting that future low-z surveys will be best suited to constrain UDM models.

  2. Computing the three-point correlation function of galaxies in O(N^2) time

    NASA Astrophysics Data System (ADS)

    Slepian, Zachary; Eisenstein, Daniel J.

    2015-12-01

    We present an algorithm that computes the multipole coefficients of the galaxy three-point correlation function (3PCF) without explicitly considering triplets of galaxies. Rather, centring on each galaxy in the survey, it expands the radially binned density field in spherical harmonics and combines these to form the multipoles without ever requiring the relative angle between a pair about the central. This approach scales with number and number density in the same way as the two-point correlation function, allowing run-times that are comparable, and 500 times faster than a naive triplet count. It is exact in angle and easily handles edge correction. We demonstrate the algorithm on the LasDamas SDSS-DR7 mock catalogues, computing an edge corrected 3PCF out to 90 Mpc h-1 in under an hour on modest computing resources. We expect this algorithm will render it possible to obtain the large-scale 3PCF for upcoming surveys such as Euclid, Large Synoptic Survey Telescope (LSST), and Dark Energy Spectroscopic Instrument.

  3. The XMM Cluster Survey: The Halo Occupation Number of BOSS galaxies in X-ray clusters

    NASA Astrophysics Data System (ADS)

    Mehrtens, Nicola; Romer, A. Kathy; Nichol, Robert C.; Collins, Chris A.; Sahlén, Martin; Rooney, Philip J.; Mayers, Julian A.; Bermeo-Hernandez, A.; Bristow, Martyn; Capozzi, Diego; Christodoulou, L.; Comparat, Johan; Hilton, Matt; Hoyle, Ben; Kay, Scott T.; Liddle, Andrew R.; Mann, Robert G.; Masters, Karen; Miller, Christopher J.; Parejko, John K.; Prada, Francisco; Ross, Ashley J.; Schneider, Donald P.; Stott, John P.; Streblyanska, Alina; Viana, Pedro T. P.; White, Martin; Wilcox, Harry; Zehavi, Idit

    2016-08-01

    We present a direct measurement of the mean halo occupation distribution (HOD) of galaxies taken from the eleventh data release (DR11) of the Sloan Digital Sky Survey-III Baryon Acoustic Oscillation Survey (BOSS). The HOD of BOSS low-redshift (LOWZ: 0.2 < z < 0.4) and Constant-Mass (CMASS: 0.43 < z < 0.7) galaxies is inferred via their association with the dark-matter halos of 174 X-ray-selected galaxy clusters drawn from the XMM Cluster Survey (XCS). Halo masses are determined for each galaxy cluster based on X-ray temperature measurements, and range between log10(M180/M⊙) = 13 - 15. Our directly-measured HODs are consistent with the HOD-model fits inferred via the galaxy-clustering analyses of Parejko et al. (2013) for the BOSS LOWZ sample and White et al. (2011) for the BOSS CMASS sample. Under the simplifying assumption that the other parameters that describe the HOD hold the values measured by these authors, we have determined a best-fit alpha-index of 0.91±0.08 and 1.27^{+0.03}_{-0.04} for the CMASS and LOWZ HOD, respectively. These alpha-index values are consistent with those measured by White et al. (2011) and Parejko et al. (2013). In summary, our study provides independent support for the HOD-models assumed during the development of the BOSS mock-galaxy catalogues that have subsequently been used to derive BOSS cosmological constraints.

  4. An accurate tool for the fast generation of dark matter halo catalogues

    NASA Astrophysics Data System (ADS)

    Monaco, P.; Sefusatti, E.; Borgani, S.; Crocce, M.; Fosalba, P.; Sheth, R. K.; Theuns, T.

    2013-08-01

    We present a new parallel implementation of the PINpointing Orbit Crossing-Collapsed HIerarchical Objects (PINOCCHIO) algorithm, a quick tool, based on Lagrangian Perturbation Theory, for the hierarchical build-up of dark matter (DM) haloes in cosmological volumes. To assess its ability to predict halo correlations on large scales, we compare its results with those of an N-body simulation of a 3 h-1 Gpc box sampled with 20483 particles taken from the MICE suite, matching the same seeds for the initial conditions. Thanks to the Fastest Fourier Transforms in the West (FFTW) libraries and to the relatively simple design, the code shows very good scaling properties. The CPU time required by PINOCCHIO is a tiny fraction (˜1/2000) of that required by the MICE simulation. Varying some of PINOCCHIO numerical parameters allows one to produce a universal mass function that lies in the range allowed by published fits, although it underestimates the MICE mass function of Friends-of-Friends (FoF) haloes in the high-mass tail. We compare the matter-halo and the halo-halo power spectra with those of the MICE simulation and find that these two-point statistics are well recovered on large scales. In particular, when catalogues are matched in number density, agreement within 10 per cent is achieved for the halo power spectrum. At scales k > 0.1 h Mpc-1, the inaccuracy of the Zel'dovich approximation in locating halo positions causes an underestimate of the power spectrum that can be modelled as a Gaussian factor with a damping scale of d = 3 h-1 Mpc at z = 0, decreasing at higher redshift. Finally, a remarkable match is obtained for the reduced halo bispectrum, showing a good description of non-linear halo bias. Our results demonstrate the potential of PINOCCHIO as an accurate and flexible tool for generating large ensembles of mock galaxy surveys, with interesting applications for the analysis of large galaxy redshift surveys.

  5. Galaxy shapes and alignments in the MassiveBlack-II hydrodynamic and dark matter-only simulations

    NASA Astrophysics Data System (ADS)

    Tenneti, Ananth; Mandelbaum, Rachel; Di Matteo, Tiziana; Kiessling, Alina; Khandai, Nishikanta

    2015-10-01

    We compare the shapes and intrinsic alignments of galaxies in the MassiveBlack-II (MBII) cosmological hydrodynamic simulation to those in an identical dark matter-only (DMO) simulation. Understanding the impact of baryonic physics on galaxy shapes should prove useful for creating mock galaxy catalogues based on DMO simulations that mimic intrinsic alignments in hydrodynamic simulations. The dark matter subhaloes are typically rounder in MBII, and the shapes of stellar matter in low-mass galaxies are more misaligned with the shapes of dark matter of the corresponding subhaloes in the DMO simulation. At z = 0.06, the fractional difference in the mean misalignment angle between MBII and DMO simulations varies from ˜28to12 per cent in the mass range 1010.8-6.0 × 1014 h-1 M⊙. We study the dark matter halo shapes and alignments as a function of radius, and find that while galaxies in MBII are more aligned with the inner parts of their dark matter subhaloes, there is no radial trend in their alignments with the corresponding subhalo in the DMO simulation. This result highlights the importance of baryonic physics in determining galaxy alignments with inner parts of their halo. Finally, we find that the stellar-dark matter misalignment suppresses the ellipticity-direction (ED) correlation of galaxies in comparison to that of dark matter haloes. In the projected shape-density correlation (wδ +), higher mean ellipticities of the stellar component reduce this effect, but differences of the order of 30-40 per cent remain on scales >1 Mpc.

  6. Planck intermediate results. XI. The gas content of dark matter halos: the Sunyaev-Zeldovich-stellar mass relation for locally brightest galaxies

    NASA Astrophysics Data System (ADS)

    Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Barrena, R.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Bernard, J.-P.; Bersanelli, M.; Bikmaev, I.; Bock, J. J.; Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bourdin, H.; Burenin, R.; Burigana, C.; Butler, R. C.; Cabella, P.; Chamballu, A.; Chary, R.-R.; Chiang, L.-Y.; Chon, G.; Christensen, P. R.; Clements, D. L.; Colafrancesco, S.; Colombi, S.; Colombo, L. P. L.; Comis, B.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Démoclès, J.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, T. R.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leonardi, R.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Luzzi, G.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marleau, F.; Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Pajot, F.; Paoletti, D.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Spencer, L.; Starck, J.-L.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Valenziano, L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wang, W.; Welikala, N.; Weller, J.; White, S. D. M.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.

    2013-09-01

    We present the scaling relation between Sunyaev-Zeldovich (SZ) signal and stellar mass for almost 260,000 locally brightest galaxies (LBGs) selected from the Sloan Digital Sky Survey (SDSS). These are predominantly the central galaxies of their dark matter halos. We calibrate the stellar-to-halo mass conversion using realistic mock catalogues based on the Millennium Simulation. Applying a multi-frequency matched filter to the Planck data for each LBG, and averaging the results in bins of stellar mass, we measure the mean SZ signal down to M∗ ~ 2 × 1011 M⊙, with a clear indication of signal at even lower stellar mass. We derive the scaling relation between SZ signal and halo mass by assigning halo properties from our mock catalogues to the real LBGs and simulating the Planck observation process. This relation shows no evidence for deviation from a power law over a halo mass range extending from rich clusters down to M500 ~ 2 × 1013 M⊙, and there is a clear indication of signal down to M500 ~ 4 × 1012 M⊙. Planck's SZdetections in such low-mass halos imply that about a quarter of all baryons have now been seen in the form of hot halo gas, and that this gas must be less concentrated than the dark matter in such halos in order to remain consistent with X-ray observations. At the high-mass end, the measured SZ signal is 20% lower than found from observations of X-ray clusters, a difference consistent with the magnitude of Malmquist bias effects that were previously estimated for the X-ray sample.

  7. Catalogue of Australian Cynipoidea (Hymenoptera)

    Technology Transfer Automated Retrieval System (TEKTRAN)

    A catalogue of all families, subfamilies, genera, and species of Cynipoidea present in Australia is presented here. The Australian cynipoid fauna is very poorly known, with 37 genera cited: one each for Austrocynipidae, Ibaliidae, Liopteridae, two for Cynipidae, and 32 for Figitidae. The first Austr...

  8. Catalogue of representative meteor spectra

    NASA Astrophysics Data System (ADS)

    Vojáček, V.; Borovička, J.; Koten, P.; Spurný, P.; Štork, R.

    2016-01-01

    We present a library of low-resolution meteor spectra that includes sporadic meteors, members of minor meteor showers, and major meteor showers. These meteors are in the magnitude range from +2 to ‑3, corresponding to meteoroid sizes from 1 mm to10 mm. This catalogue is available online at the CDS for those interested in video meteor spectra.

  9. Catalogue of representative meteor spectra

    NASA Astrophysics Data System (ADS)

    Vojáček, V.; Borovička, J.; Koten, P.; Spurný, P.; Štork, R.

    2016-01-01

    We present a library of low-resolution meteor spectra that includes sporadic meteors, members of minor meteor showers, and major meteor showers. These meteors are in the magnitude range from +2 to -3, corresponding to meteoroid sizes from 1 mm to10 mm. This catalogue is available online at the CDS for those interested in video meteor spectra.

  10. Astronomical Catalogues - Definition Elements and Afterlife

    NASA Astrophysics Data System (ADS)

    Jaschek, C.

    1984-09-01

    Based on a look at the different meanings of the term catalogue (or catalog), a definition is proposed. In an analysis of the main elements, a number of requirements that catalogues should satisfy are pointed out. A section is devoted to problems connected with computer-readable versions of printed catalogues.

  11. Using Galaxy Winds to Constrain Galaxy Evolution

    NASA Astrophysics Data System (ADS)

    Churchill, Christopher W.; Klypin, A.; Ceverino, D.; Kacprzak, G.; Klimek, E.

    2010-01-01

    Analysis of mock quasar spectra of metal absorption lines in the proximity of formed galaxies in cosmological simulation is a highly promising for understanding the role of galaxies in IGM physics, or IGM physics in the role of galaxy formation in context of the cosmic web. Such analysis using neutral hydrogen in the cosmic web has literally revolutionized our understanding of the Lyman alpha forest. We are undertaking a wholesale approach to use powerful Lambda-CDM simulations to interpret absorption line data from redshift 1-3 starbursting galaxies e.g. Lyman break galaxies, etc) The data with which direct quantitative comparison is made are from the DEEP survey (Weiner et al.) and the collective work of Steidel et al. and collaborators. The simulations are performed using the Eulerian Gasdynamics plus N-body Adaptive Refinement Tree (ART) code, which has gas cell resolutions of 20-50 pc. Physical processes implemented in the code include realistic radiative cooling, star formation, metal enrichment and thermal feedback due to type II and type Ia supernovae. We quantitatively compare the spatial and kinematic distribution of HI, MgII, CIV, and OVI of absorption lines over a range of impact parameters for various simulated galaxies as a function of redshift, and discuss key insights for interpreting the underlying temperature, density, and ionization structure of the halo/cosmic-web interface, and the influence of galaxies on its chemical enrichment.

  12. Mock gravity and the cosmic structure

    SciTech Connect

    Hogan, C.J.

    1989-05-01

    The process of generating large-scale cosmic structure from the radiation-pressure or 'mock gravity' instability is studied with particular emphasis on the implications of the Berkeley-Nagoya rocket data for the submillimeter background. The linear theory of perturbations in an absorbing medium embedded in an expanding universe of radiation sources is presented. The instability sets up collapse velocities in linear perturbation theory which far exceed those from gravitational instability, so growth continues even after the instability switches off. Perturbation due to this effect is analyzed and related to the growth of large-scale cosmic structures at recent times; large-scale structure is shown to evolve very little from 1 + z about 5 to the present. Nonlinear small-scale effects of the instability are analyzed; it is shown that radiation pressure would compress gas into small, dense pressure-confined clouds with tau much greater than one. 32 refs.

  13. How to Plan and Conduct a Mock Trial: Civil Trial.

    ERIC Educational Resources Information Center

    Missouri State Bar Association, Jefferson City.

    This document contains resources and suggested steps to help secondary teachers organize and conduct a mock trial. Although written specifically for use in Missouri, the document can easily be used and adapted by teachers in other states. The authors believe that a mock trial is a valuable learning experience in many ways. It may be used to help…

  14. How type of excuse defense, mock juror age, and defendant age affect mock jurors' decisions.

    PubMed

    Higgins, Pamela L; Heath, Wendy P; Grannemann, Bruce D

    2007-08-01

    The authors investigated the effects of mock juror age (younger vs. older), defendant age (22 vs. 65), and type of excuse defense used by defendants (a highly self-inflicted condition, Cocaine Dependency Disorder, vs. a less self-inflicted condition, Posttraumatic Stress Disorder) on mock juror decisions. Ninety-six younger and 96 older adults read a scenario and answered a questionnaire. Results indicated that the defendant using the highly self-inflicted excuse was more likely to receive a guilty verdict and a longer sentence than was the defendant using the less self-inflicted excuse. Older jurors were more certain of their verdicts and saw the defendant as more responsible for his condition than did younger jurors. Defendant age did not affect juror decisions. In addition, excuse type and juror age affected the jurors' perceptions of the victim's responsibility for the attack. The authors discuss the potential influence of juror age on perceptions of defendant responsibility.

  15. VizieR Online Data Catalog: Galaxies and Clusters of Galaxies (CGCG) (Zwicky, 1968)

    NASA Astrophysics Data System (ADS)

    Zwicky, F.; et al.

    1995-10-01

    This document describes a machine-readable version of a portion of the "Catalogue of Galaxies and Clusters of Galaxies" (Zwicky, et al.). The published catalogue covers 560 Palomar Sky Survey fields, and for each field it lists both individual galaxies and clusters of galaxies. Its limiting magnitude for galaxies is approximately +15.5 apparent photographic magnitude. The present machine-readable version includes only the individual galaxies. It consists of two files, the first of which lists the galaxies (data file) and the second of which enumerates the fields covered (headers file). Note: the abbreviation ADC used in this document refers to the Astronomical Data Center, NASA/Goddard Space Flight Center. (2 data files).

  16. The Planck Catalogue of High-z source candidates

    NASA Astrophysics Data System (ADS)

    Montier, Ludovic

    2015-08-01

    The Planck satellite has provided the first FIR/submm all-sky survey with a sensitivity allowing us to identify the rarest, most luminous high-z dusty star-forming sources on the sky. It opens a new window on these extreme star-forming systems at redshift above 1.5, providing a powerful laboratory to study the mechanisms of galaxy evolution and enrichment in the frame of the large scale structure growth.I will describe how the Planck catalogue of high-z source candidates (PHz, Planck 2015 in prep.) has been built and charcaterized over 25% of the sky by selecting the brightest red submm sources at a 5' resolution. Follow-up observations with Herschel/SPIRE over 228 Planck candidates have shown that 93% of these candidates are actually overdensities of red sources with SEDs peaking at 350um (Planck Int. results. XXVII 2014). Complementarily to this population of objects, 12 Planck high-z candidates have been identified as strongly lensed star forming galaxies at redshift lying between 2.2 and 3.6 (Canameras et al 2015 subm.), with flux densities larger than 400 mJy up to 1 Jy at 350um, and strong magnification factors. These Planck lensed star-forming galaxies are the rarest brightest lensed in the submm range, providing a unique opportunity to extend the exploration of the star-forming system in this range of mass and redshift.I will detail further a specific analysis performed on a proto-cluster candidate, PHz G95.5-61.6, identified as a double structure at z=1.7 and z=2.03, using an extensive follow-up program (Flores-Cacho et al 2015 subm.). This is the first Planck proto-cluster candidate with spectroscopic confirmation, which opens a new field of statistical analysis about the evolution of dusty star-forming galaxies in such accreting structures.I will finally discuss how the PHz catalogue may help to answer some of the fundamental questions like: At what cosmic epoch did massive galaxy clusters form most of their stars? Is star formation more or less vigorous

  17. Comparison of Zero Zone Catalogues of the Fon Program Based on the Kyiv and Kitab Observations

    NASA Astrophysics Data System (ADS)

    Andruk, V. M.; Relke, H.; Protsyuk, Yu. I.; Muminov, M. M.; Ehgamberdiev, Sh. A.; Yuldoshev, Q. X.; Golovnia, V. V.

    The two new catalogues for the zero zone of the FON project were created after the processing of two different collections of digitized photographic plates. The photographic plates were received at the DAZ and DWA telescopes of the Kitab observatory of the Republic of Uzbekistan (KO UAS) and of the Main astronomical observatory in Kyiv (MAO NASU) in the number of 90 and 120 plates, respectively. The digitization of these photographic plates in the frame of the Ukrainian Virtual Observatory project was performed by means of the Epson Expression 10000XL scanner with the scanning resolution of 1200 dpi. The coordinates of stars and galaxies for the both catalogues are determined in the system of the Tycho2 catalogue. The stellar magnitudes of all objects are done in B-magnitudes of the photoelectric standard system. The difference between the calculated and the reference positions is equal σαδ = ±0.06-0.07". The internal accuracy of the both catalogues for all objects is σαδ = ±0.20", σB = ±0.18m and σ αδ = ±0.27", σ B = ±0.17m, respectively. We present the comparison of these both catalogues with each other and with the Tycho2, UCAC4 as well as PPMX catalogues and discuss the results.

  18. Radio loud far-infrared galaxies

    NASA Technical Reports Server (NTRS)

    Dey, Arjun; Vanbreugel, Wil; Shields, Joseph C.

    1990-01-01

    The first results are presented of a multiwavelength study of Infrared Astronomy Satellite (IRAS) galaxies with excess radio emission. The sample was selected by cross correlating the IRAS Faint Source Survey, and the Point Source Catalogue with the Texas radio survey. Recent optical (imaging and spectroscopic) and radio (VLA) observations are discussed. These observations will be used to investigate possible connections between radio galaxy activity, star formation and galaxy interactions.

  19. An implementation of geospatial semantic catalogue service

    NASA Astrophysics Data System (ADS)

    Chen, Xu; Zhu, Xinyan; Du, Daosheng; Liu, Tingting

    2008-12-01

    Along with the development of earth observation technology, large amounts of geospatial information are accessible. There are also a lot of geospatial data and services which are shared on the Internet. However they vary in formats and are stored at various organizations leading to problems of data discovery, data interoperability and usability. The Open Geospatial Consortium (OGC) has developed standard service called catalogue in order to overcome this problem. The goal of a geospatial catalogue is to support a wide range of users in discovering relevant geographic data and services from heterogeneous and distributed repositories. But in most of geospatial catalogue services, the search functionality is limited to the direct match of keywords from metadata, the OGC catalogues may not return useful results as the used keywords often do not match with the meta-information stored in the catalogues. In this paper, we propose a geospatial semantic catalogue services that aims at overcoming this limitation.

  20. The Solar Stormwatch CME catalogue.

    NASA Astrophysics Data System (ADS)

    Barnard, Luke

    2015-04-01

    Since the launch of the twin STEREO satellites in late 2006, the Heliospheric Imagers have been used, with good results, in tracking transients of solar origin, such as Coronal Mass Ejections (CMEs), out through the inner heliosphere. A frequently used approach is to build a "J-Map", in which multiple elongation profiles along a constant position angle are stacked in time, building an image in which radially propagating transients form curved tracks in the J-Map. From this the time-elongation profile of a solar transient can be manually identified. This is a time consuming and laborious process, and the results are subjective, depending on the skill and expertise of the investigator. With the Heliospheric Imager data it is possible to follow CMEs from the outer limits of the solar corona all the way to 1AU. Solar Stormwatch is a citizen science project that employs the power of thousands of volunteers to both identify and track CMEs in the Heliospheric Imager data. The CMEs identified by Solar Stormwatch are tracked many times by multiple users and this allows the calculation of consensus time-elongation profiles for each event and also provides an estimate of the error in the consensus profile. Therefore this system does not suffer from the potential subjectivity of individual researchers identifying and tracking CMEs. In this sense, the Solar Stormwatch system can be thought of as providing a middle ground between manually identified CME catalogues, such as the CDAW list, and CME catalogues generated through fully automated algorithms, such as CACtus and ARTEMIS etc. We provide a summary of the reduction of the Solar Stormwatch data into a catalogue of CMEs observed by STEREO-A and STEREO-B through the deep minimum of solar cycle 23 and review some key statistical properties of these CMEs. Through some case studies of the propagation of CMEs out into the inner heliosphere we argue that the Solar Stormwatch CME catalogue, which publishes the time

  1. Identification of stars in a J1744.0 star catalogue Yixiangkaocheng

    NASA Astrophysics Data System (ADS)

    Ahn, S.-H.

    2012-05-01

    The stars in the Chinese star catalogue, Yixiangkaocheng, which were edited by the Jesuit astronomer Kögler in AD 1744 and published in AD 1756, are identified with their counterparts in the Hipparcos catalogue. The equinox of the catalogue is confirmed to be J1744.0. By considering the precession of equinox, proper motions and nutation, the star closest to the location of each star in Yixiangkaocheng, having a proper magnitude, is selected as the corresponding identified star. I identified 2848 stars and 13 nebulosities out of 3083 objects in Yixiangkaocheng, and so the identification rate reached 92.80 per cent. I find that the magnitude classification system in Yixiangkaocheng agrees with the modern magnitude system. The catalogue includes dim stars, whose visual magnitudes are larger than 7, but most of these stars have Flamsteed designations. I find that the stars whose declination is lower than -30° have relatively larger offsets and different systematic behaviour from other stars. This indicates that there might be two different sources of stars in Yixiangkaocheng. In particular, I find that μ1 Sco and γ1 Sgr approximately mark the boundary between two different source catalogues. The observer's location, as estimated from these facts, agrees with the latitude of Greenwich where Flamsteed made his observations. The positional offsets between the Yixiangkaocheng stars and the Hipparcos stars are 0.6 arcmin, which implies that the source catalogue of stars with δ > -30° must have come from telescopic observations. Nebulosities in Yixiangkaocheng are identified with a few double stars, o Cet (the variable star, Mira), the Andromeda galaxy, ω Cen and NGC6231. These entities are associated with listings in Halley's Catalogue of the Southern Stars of AD 1679 as well as Flamsteed's catalogue of AD 1690.

  2. Solar Feature Catalogues In Egso

    NASA Astrophysics Data System (ADS)

    Zharkova, V. V.; Aboudarham, J.; Zharkov, S.; Ipson, S. S.; Benkhalil, A. K.; Fuller, N.

    2005-05-01

    The Solar Feature Catalogues (SFCs) are created from digitized solar images using automated pattern recognition techniques developed in the European Grid of Solar Observation (EGSO) project. The techniques were applied for detection of sunspots, active regions and filaments in the automatically standardized full-disk solar images in Caii K1, Caii K3 and Hα taken at the Meudon Observatory and white-light images and magnetograms from SOHO/MDI. The results of automated recognition are verified with the manual synoptic maps and available statistical data from other observatories that revealed high detection accuracy. A structured database of the Solar Feature Catalogues is built on the MySQL server for every feature from their recognized parameters and cross-referenced to the original observations. The SFCs are published on the Bradford University web site http://www.cyber.brad.ac.uk/egso/SFC/ with the pre-designed web pages for a search by time, size and location. The SFCs with 9 year coverage (1996 2004) provide any possible information that can be extracted from full disk digital solar images. Thus information can be used for deeper investigation of the feature origin and association with other features for their automated classification and solar activity forecast.

  3. Detail of mock balconies at northeast corner; camera facing west. ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    Detail of mock balconies at northeast corner; camera facing west. - Mare Island Naval Shipyard, Hospital Wards, Cedar Avenue, eat side between Fourteenth Avenue & Cossey Street, Vallejo, Solano County, CA

  4. Boeing CST-100 Mock-Up Undergoes Airbag Stabilization Test

    NASA Video Gallery

    The Boeing Company's mock-up CST-100 spacecraft was put through water landing development tests Oct. 1-5, 2012, at Bigelow Aerospace's headquarters outside of Las Vegas. Engineers with Bigelow have...

  5. VizieR Online Data Catalog: Nearby early-type galaxies catalog (Dabringhausen+, 2016)

    NASA Astrophysics Data System (ADS)

    Dabringhausen, J.; Fellhauer, M.

    2016-06-01

    We present a catalogue of 1715 early-type galaxies from the literature, spanning the luminosity range from faint dwarf spheroidal galaxies to giant elliptical galaxies. The aim of this catalogue is to be one of the most comprehensive and publicly available collections of data on early-type galaxies. The emphasis in this catalogue lies on dwarf elliptical galaxies, for which some samples with detailed data have been published recently. For almost all of the early-type galaxies included in it, this catalogue contains data on their locations, distances, redshifts, half-light radii, the masses of their stellar populations and apparent magnitudes in various passbands. Data on metallicity and various colours are available for a majority of the galaxies presented here. The data on magnitudes, colours, metallicities and masses of the stellar populations is supplemented with entries that are based on fits to data from simple stellar population models and existing data from observations. Also, some simple transformations have been applied to the data on magnitudes, colours and metallicities in this catalog, in order to increase the homogeneity of this data. Estimates on the Sersic profiles, internal velocity dispersions, maximum rotational velocities, dynamical masses and ages are listed for several hundreds of the galaxies in this catalogue. Finally, each quantity listed in this catalogue is accompanied with information on its source, so that users of this catalogue can easily exclude data that they do not consider as reliable enough for their purposes. (10 data files).

  6. ESO Catalogue Facility Design and Performance

    NASA Astrophysics Data System (ADS)

    Moins, C.; Retzlaff, J.; Arnaboldi, M.; Zampieri, S.; Delmotte, N.; Forchí, V.; Klein Gebbinck, M.; Lockhart, J.; Micol, A.; Vera Sequeiros, I.; Bierwirth, T.; Peron, M.; Romaniello, M.; Suchar, D.

    2013-10-01

    The ESO Phase 3 Catalogue Facility provides investigators with the possibility to ingest catalogues resulting from ESO public surveys and large programs and to query and download their content according to positional and non-positional criteria. It relies on a chain of tools that covers the complete workflow from submission to validation and ingestion into the ESO archive and catalogue repository and a web application to browse and query catalogues. This repository consists of two components. One is a Sybase ASE relational database where catalogue meta-data are stored. The second one is a Sybase IQ data warehouse where the content of each catalogue is ingested in a specific table that returns all records matching a user's query. Spatial indexing has been implemented in Sybase IQ to speed up positional queries and relies on the Spherical Geometry Toolkit from the Johns Hopkins University which implements the Hierarchical Triangular Mesh (HTM) algorithm. It is based on a recursive decomposition of the celestial sphere in spherical triangles and the assignment of an index to each of them. It has been complemented with the use of optimized indexes on the non-positional columns that are likely to be frequently used as query constraints. First tests performed on catalogues such as 2MASS have confirmed that this approach provides a very good level of performance and a smooth user experience that are likely to facilitate the scientific exploitation of catalogues.

  7. Submillimeter, millimeter, and microwave spectral line catalogue

    NASA Technical Reports Server (NTRS)

    Poynter, R. L.; Pickett, H. M.

    1984-01-01

    This report describes a computer accessible catalogue of submillimeter, millimeter, and microwave spectral lines in the frequency range between 0 and 10000 GHz (i.e., wavelengths longer than 30 micrometers). The catalogue can be used as a planning guide or as an aid in the identification and analysis of observed spectral lines. The information listed for each spectral line includes the frequency and its estimated error, the intensity, lower state energy, and quantum number assignment. The catalogue has been constructed using theoretical least squares fits of published spectral lines to accepted molecular models. The associated predictions and their estimated errors are based upon the resultant fitted parameters and their covariances. Future versions of this catalogue will add more atoms and molecules and update the present listings (151 species) as new data appear. The catalogue is available from the authors as a magnetic tape recorded in card images and as a set of microfiche records.

  8. An analysis of the first three catalogues of southern star clusters and nebulae

    NASA Astrophysics Data System (ADS)

    Cozens, Glendyn John

    2008-06-01

    of the Lacaille and Herschel catalogues. In order to identify and compare the catalogues, positions given for an object by each astronomer were precessed to J2000.0 coordinates. These modern positions for an object could then be plotted onto modern photographic star atlases and digital images of the sky, to determine the accuracy of the original positions. Analysis of the three non-stellar catalogues included the determination of the radial distance of each object from its "correct" position and diagrams of both difference in Right Ascension and difference in Declination against Right Ascension and Declination, in order to identify any trends. Each catalogue contained some copy or printing errors, but these were omitted from the statistical calculations performed. The results for the three catalogues, from the astrometric perspective, showed that the Herschel catalogue contained the most accurate positions, followed closely by the Lacaille catalogue with no obvious or systematic trends in their inaccuracies. In contrast, the Dunlop catalogue showed some clear trends in the positional inaccuracies which, regardless of mitigating circumstances, to some extent warranted John Herschel's criticism. Finally an examination of the completeness of each catalogue was undertaken to determine the thoroughness of each astronomer. Firstly the effective aperture and theoretical magnitude limit for each telescope was calculated. Next the non-stellar objects were grouped into five types, open clusters, globular clusters, diffuse nebulae, planetary nebulae and galaxies, and a single working magnitude limit was found for each catalogue. A number of indicators were used to determine the working magnitude limit. The number of faint objects of each type which were seen, and the number of bright objects which were missed by the three astronomers, was assessed. In both the Dunlop and Herschel catalogues galaxies gave the best indicator of the working magnitude limit. Globular clusters

  9. VizieR Online Data Catalog: HI supershells catalogue (Suad+, 2014)

    NASA Astrophysics Data System (ADS)

    Suad, L. A.; Caiafa, C. F.; Arnal, E. M.; Cichowolski, S.

    2014-02-01

    The HI supershells catalogue was carried out making use of the Leiden-Argentine-Bonn (LAB) HI survey in the outer part of the Galaxy. The identification of the supershell candidates was made using a combination of two techniques: a visual inspection one plus an automatic searching algorithm. A total of 566 supershell candidates were identified. Most of them (347) are located in the second galactic quadrant, while 219 were found in the third one. (1 data file).

  10. Gas in void galaxies

    NASA Astrophysics Data System (ADS)

    Kreckel, Kathryn Joyce

    . We find that the void galaxies are ! generally gas rich, low luminosity, blue disk galaxies, but identify three as early type galaxies. The void galaxy optical and H I properties are not unusual for their luminosity and morphology. The small scale clustering in the void is similar to that in higher density regions, and we identify 18 H I rich neighboring galaxies in the voids. Two of these are systems of three galaxies linearly aligned and joined by a H I bridge, suggestive of filamentary formation within the void. We find no population of H I rich low luminosity galaxies within the observed voids that are not close companions of the targeted sample. Finally, to put these observations in a theoretical context, we analyze a (120 h^-1 Mpc)^3 adaptive mesh refinement hydrodynamic simulation that contains a high resolution subvolume centered on a ~30 Mpc diameter void. We construct mock observations with ~1 kpc resolution of the stellar and gas properties of these systems which reproduce the range of colors and luminosities observed in the SDSS for nearby galaxies, however we find no strong trends with density. We also make predictions for a significant population of low luminosity (M_r = -14) dwarf galaxies that is preferentially located in low density regions and specifically in the void center.

  11. Measurements of H(z) and DA(z) from the two-dimensional two-point correlation function of Sloan Digital Sky Survey luminous red galaxies

    NASA Astrophysics Data System (ADS)

    Chuang, Chia-Hsun; Wang, Yun

    2012-10-01

    We present a method for measuring the Hubble parameter, H(z), and angular diameter distance, DA(z), from the two-dimensional two-point correlation function and validate it using LasDamas mock galaxy catalogues. Applying our method to the sample of luminous red galaxies from the Sloan Digital Sky Survey Data Release 7, we measure H(z=0.35)≡H(0.35)=82.1-4.9+4.8 km s-1 Mpc -1 and DA(z=0.35)≡DA(0.35)=1048-58+60 Mpc without assuming a dark energy model or a flat universe. We find that the derived measurements of H(0.35) rs(zd)/c and DA(0.35)/rs(zd) [where rs(zd) is the sound horizon at the drag epoch] are nearly uncorrelated, have tighter constraints and are more robust with respect to possible systematic effects. Our galaxy clustering measurements of {H(0.35) rs(zd)/c,DA(0.35)/rs(zd)}={0.0434±0.0018,6.60±0.26} (with the correlation coefficient r = 0.0604) can be used to combine with cosmic microwave background and any other cosmological data sets to constrain dark energy. Our results represent the first measurements of H(z) and DA(z) (or H(z) rs(zd)/c and DA(0.35)/rs(zd)) from galaxy clustering data. Our work has significant implications for future surveys in establishing the feasibility of measuring both H(z) and DA(z) from galaxy clustering data.

  12. Submillimeter, millimeter, and microwave spectral line catalogue

    NASA Technical Reports Server (NTRS)

    Poynter, R. L.; Pickett, H. M.

    1980-01-01

    A computer accessible catalogue of submillimeter, millimeter, and microwave spectral lines in the frequency range between O and 3000 GHz (such as; wavelengths longer than 100 m) is discussed. The catalogue was used as a planning guide and as an aid in the identification and analysis of observed spectral lines. The information listed for each spectral line includes the frequency and its estimated error, the intensity, lower state energy, and quantum number assignment. The catalogue was constructed by using theoretical least squares fits of published spectral lines to accepted molecular models. The associated predictions and their estimated errors are based upon the resultant fitted parameters and their covariances.

  13. VizieR Online Data Catalog: The Southern SHARC catalogue (Burke+, 2003)

    NASA Astrophysics Data System (ADS)

    Burke, D. J.; Collins, C. A.; Sharples, R. M.; Romer, A. K.; Nichol, R. C.

    2003-06-01

    The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg2 and is selected from long (greater than 10ks) ROSAT exposures with a declination <+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x1035W and 4x1037W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H0 set to 50km/s/Mpc. (5 data files).

  14. Mouse genetics: Catalogue and scissors

    PubMed Central

    Sung, Young Hoon; Baek, In-Jeoung; Seong, Je Kyung; Kim, Jin-Soo; Lee, Han-Woong

    2012-01-01

    Phenotypic analysis of gene-specific knockout (KO) mice has revolutionized our understanding of in vivo gene functions. As the use of mouse embryonic stem (ES) cells is inevitable for conventional gene targeting, the generation of knockout mice remains a very time-consuming and expensive process. To accelerate the large-scale production and phenotype analyses of KO mice, international efforts have organized global consortia such as the International Knockout Mouse Consortium (IKMC) and International Mouse Phenotype Consortium (IMPC), and they are persistently expanding the KO mouse catalogue that is publicly available for the researches studying specific genes of interests in vivo. However, new technologies, adopting zinc-finger nucleases (ZFNs) or Transcription Activator-Like Effector (TALE) Nucleases (TALENs) to edit the mouse genome, are now emerging as valuable and effective shortcuts alternative for the conventional gene targeting using ES cells. Here, we introduce the recent achievement of IKMC, and evaluate the significance of ZFN/TALEN technology in mouse genetics. [BMB Reports 2012; 45(12): 686-692] PMID:23261053

  15. THE DEEP2 GALAXY REDSHIFT SURVEY: THE VORONOI-DELAUNAY METHOD CATALOG OF GALAXY GROUPS

    SciTech Connect

    Gerke, Brian F.; Newman, Jeffrey A.; Davis, Marc; Coil, Alison L.; Cooper, Michael C.; Dutton, Aaron A.; Faber, S. M.; Guhathakurta, Puragra; Koo, David C.; Phillips, Andrew C.; Noeske, Kai; Rosario, David J.; Weiner, Benjamin J.; Willmer, Christopher N. A.; Yan, Renbin

    2012-05-20

    We present a public catalog of galaxy groups constructed from the spectroscopic sample of galaxies in the fourth data release from the Deep Extragalactic Evolutionary Probe 2 (DEEP2) Galaxy Redshift Survey, including the Extended Groth Strip (EGS). The catalog contains 1165 groups with two or more members in the EGS over the redshift range 0 < z < 1.5 and 1295 groups at z > 0.6 in the rest of DEEP2. Twenty-five percent of EGS galaxies and fourteen percent of high-z DEEP2 galaxies are assigned to galaxy groups. The groups were detected using the Voronoi-Delaunay method (VDM) after it has been optimized on mock DEEP2 catalogs following similar methods to those employed in Gerke et al. In the optimization effort, we have taken particular care to ensure that the mock catalogs resemble the data as closely as possible, and we have fine-tuned our methods separately on mocks constructed for the EGS and the rest of DEEP2. We have also probed the effect of the assumed cosmology on our inferred group-finding efficiency by performing our optimization on three different mock catalogs with different background cosmologies, finding large differences in the group-finding success we can achieve for these different mocks. Using the mock catalog whose background cosmology is most consistent with current data, we estimate that the DEEP2 group catalog is 72% complete and 61% pure (74% and 67% for the EGS) and that the group finder correctly classifies 70% of galaxies that truly belong to groups, with an additional 46% of interloper galaxies contaminating the catalog (66% and 43% for the EGS). We also confirm that the VDM catalog reconstructs the abundance of galaxy groups with velocity dispersions above {approx}300 km s{sup -1} to an accuracy better than the sample variance, and this successful reconstruction is not strongly dependent on cosmology. This makes the DEEP2 group catalog a promising probe of the growth of cosmic structure that can potentially be used for cosmological tests.

  16. Cosmology with void-galaxy correlations.

    PubMed

    Hamaus, Nico; Wandelt, Benjamin D; Sutter, P M; Lavaux, Guilhem; Warren, Michael S

    2014-01-31

    Galaxy bias, the unknown relationship between the clustering of galaxies and the underlying dark matter density field is a major hurdle for cosmological inference from large-scale structure. While traditional analyses focus on the absolute clustering amplitude of high-density regions mapped out by galaxy surveys, we propose a relative measurement that compares those to the underdense regions, cosmic voids. On the basis of realistic mock catalogs we demonstrate that cross correlating galaxies and voids opens up the possibility to calibrate galaxy bias and to define a static ruler thanks to the observable geometric nature of voids. We illustrate how the clustering of voids is related to mass compensation and show that volume-exclusion significantly reduces the degree of stochasticity in their spatial distribution. Extracting the spherically averaged distribution of galaxies inside voids from their cross correlations reveals a remarkable concordance with the mass-density profile of voids.

  17. Galaxy 'Hunting' Made Easy

    NASA Astrophysics Data System (ADS)

    2007-09-01

    Galaxies found under the Glare of Cosmic Flashlights Astronomers using ESO's Very Large Telescope have discovered in a single pass about a dozen otherwise invisible galaxies halfway across the Universe. The discovery, based on a technique that exploits a first-class instrument, represents a major breakthrough in the field of galaxy 'hunting'. ESO PR Photo 40a/07 ESO PR Photo 40a/07 Newly Found Galaxies (SINFONI/VLT) The team of astronomers led by Nicolas Bouché have used quasars to find these galaxies. Quasars are very distant objects of extreme brilliance, which are used as cosmic beacons that reveal galaxies lying between the quasar and us. The galaxy's presence is revealed by a 'dip' in the spectrum of the quasar - caused by the absorption of light at a specific wavelength. The team used huge catalogues of quasars, the so-called SDSS and 2QZ catalogues, to select quasars with dips. The next step was then to observe the patches of the sky around these quasars in search for the foreground galaxies from the time the Universe was about 6 billion years old, almost half of its current age. "The difficulty in actually spotting and seeing these galaxies stems from the fact that the glare of the quasar is too strong compared to the dim light of the galaxy," says Bouché. This is where observations taken with SINFONI on ESO's VLT made the difference. SINFONI is an infrared 'integral field spectrometer' that simultaneously delivers very sharp images and highly resolved colour information (spectra) of an object on the sky. ESO PR Photo 32e/07 ESO PR Photo 40b/07 Chasing 'Hidden' Galaxies (Artist's Impression) With this special technique, which untangles the light of the galaxy from the quasar light, the team detected 14 galaxies out of the 20 pre-selected quasar patches of sky, a hefty 70% success rate. "This high detection rate alone is a very exciting result," says Bouché. "But, these are not just ordinary galaxies: they are most notable ones, actively forming a lot of

  18. Magnitude systems in old star catalogues

    NASA Astrophysics Data System (ADS)

    Fujiwara, Tomoko; Yamaoka, Hitoshi

    2005-06-01

    The current system of stellar magnitudes originally introduced by Hipparchus was strictly defined by Norman Pogson in 1856. He based his system on Ptolemy's star catalogue, the Almagest, recorded in about AD137, and defined the magnitude-intensity relationship on a logarithmic scale. Stellar magnitudes observed with the naked eye recorded in seven old star catalogues were analyzed in order to examine the visual magnitude systems. Although psychophysicists have proposed that human visual sensitivity follows a power-law scale, it is shown here that the degree of agreement is far better for a logarithmic scale than for a power-law scale. It is also found that light ratios in each star catalogue are nearly equal to 2.512, if the brightest (1st magnitude) and the faintest (6th magnitude and dimmer) stars are excluded from the study. This means that the visual magnitudes in the old star catalogues agree fully with Pogson's logarithmic scale.

  19. FRBCAT: The Fast Radio Burst Catalogue

    NASA Astrophysics Data System (ADS)

    Petroff, E.; Barr, E. D.; Jameson, A.; Keane, E. F.; Bailes, M.; Kramer, M.; Morello, V.; Tabbara, D.; van Straten, W.

    2016-09-01

    Here, we present a catalogue of known Fast Radio Burst sources in the form of an online catalogue, FRBCAT. The catalogue includes information about the instrumentation used for the observations for each detected burst, the measured quantities from each observation, and model-dependent quantities derived from observed quantities. To aid in consistent comparisons of burst properties such as width and signal-to-noise ratios, we have re-processed all the bursts for which we have access to the raw data, with software which we make available. The originally derived properties are also listed for comparison. The catalogue is hosted online as a Mysql database which can also be downloaded in tabular or plain text format for off-line use. This database will be maintained for use by the community for studies of the Fast Radio Burst population as it grows.

  20. Submillimeter, millimeter, and microwave spectral line catalogue

    NASA Technical Reports Server (NTRS)

    Poynter, R. L.; Pickett, H. M.

    1981-01-01

    A computer accessible catalogue of submillimeter, millimeter and microwave spectral lines in the frequency range between 0 and 3000 GHZ (i.e., wavelengths longer than 100 mu m) is presented which can be used a planning guide or as an aid in the identification and analysis of observed spectral lines. The information listed for each spectral line includes the frequency and its estimated error, the intensity, lower state energy, and quantum number assignment. The catalogue was constructed by using theoretical least squares fits of published spectral lines to accepted molecular models. The associated predictions and their estimated errors are based upon the resultant fitted parameters and their covariances. Future versions of this catalogue will add more atoms and molecules and update the present listings (133 species) as new data appear. The catalogue is available as a magnetic tape recorded in card images and as a set of microfiche records.

  1. The History of Ptolemy's Star Catalogue

    NASA Astrophysics Data System (ADS)

    Graßhoff, Gerd

    Table of contents

    Contents: Introduction.- The Stars of the Almagest.- Accusations.- The Rehabilitation of Ptolemy.- The Analysis of the Star Catalogue.- Structures in Ptolemy's Star Catalogue.- Theory and Observation.- Appendix A.- Stars and Constellations.- Identifications.- Appendix B.- Transformation Formulae.- Column Headings.- Appendix C.- Column Headings.- Literature.- Index.

  2. The Environmental Dependence of the Galaxy Luminosity Function in the ECO Survey

    NASA Astrophysics Data System (ADS)

    Andrews, Hayley; Andreas A. Berlind, Victor Calderon, Kathleen D. Eckert, Sheila J. Kannappan, Amanda J. Moffett, David V. Stark

    2016-01-01

    We study the environmental dependence of the galaxy luminosity function in the ECO survey and compare it with models that associate galaxies with dark matter halos. Specifically, we quantify the environment of each galaxy in the ECO survey using an Nth nearest neighbor distance metric, and we measure how the galaxy luminosity distribution varies from low density to high density environments. As expected, we find that luminous galaxies preferentially populate high density regions, while low luminosity galaxies preferentially populate lower density environments. We investigate whether this trend can be explained simply by the correlation of galaxy luminosity and dark matter halo mass combined with the environmental dependence of the halo mass function. In other words, we test the hypothesis that the luminosity of a galaxy depends solely on the mass of its dark matter halo and does not exhibit a residual dependence on the halo's larger environment. To test this hypothesis, we first construct mock ECO catalogs by populating dark matter halos in an N-body simulation with galaxies using a model that preserves the overall clustering strength of the galaxy population. We then assign luminosities to the mock galaxies using physically motivated models that connect luminosity to halo mass and are constrained to match the global ECO luminosity function. Finally, we impose the radial and angular selection functions of the ECO survey and repeat our environmental analysis on the mock catalogs. Though our mock catalog luminosity functions display similar qualitative trends as those from the ECO data, the trends are not in agreement quantitatively. Our results thus suggest that the simple models used to build the mocks are incomplete and that galaxy luminosity is possibly correlated with the larger scale density field.

  3. Understanding Pretrial Publicity: Predecisional Distortion of Evidence by Mock Jurors

    ERIC Educational Resources Information Center

    Hope, Lorraine; Memon, Amina; McGeorge, Peter

    2004-01-01

    Prejudicial pretrial publicity (PTP) constitutes a serious source of juror bias. The current study examined differences in predecisional distortion for mock jurors exposed to negative PTP (N-PTP) versus nonexposed control participants. According to work by K. A. Carlson and J. E. Russo (2001), predecisional distortion occurs when jurors bias new…

  4. Utilization of the Mock Event for Classroom Demonstration Purposes.

    ERIC Educational Resources Information Center

    Van Dusen, Virgil

    1998-01-01

    A mock event was introduced into a required pharmacy law course to provide real-life application of a realistic legal event. The aim was to create student interest in and understanding of legal principles through student participation in a dramatized deposition by a plaintiff's attorney. Students enjoyed the exercise and suggested it be continued…

  5. The Implementation of Mock Negotiations in Teaching International Business Management.

    ERIC Educational Resources Information Center

    Raffield, Barney T., III

    Mock negotiations are used as part of an undergraduate course in international business management at Lebanon Valley College (Pennsylvania) in order to introduce students to the process of negotiating for advantage in foreign countries and to emphasize the importance of an individual nation's customs, culture, and ways of transacting business in…

  6. The Seventh Generation: A Mock Hearing. Teaching Strategy.

    ERIC Educational Resources Information Center

    Mertz, Gayle

    1993-01-01

    Presents a classroom activity that features a mock hearing on environmental issues before an international court. Asserts that international cooperation is necessary if the world is to avert environmental disaster. Provides role descriptions for the witnesses and step-by-step instructional procedures. (CFR)

  7. A Mock U.N. Game: Teaching Global Awareness.

    ERIC Educational Resources Information Center

    Regenbogen, Joe

    1988-01-01

    Describes a classroom simulation that has students role play membership in the United Nations. Students are assigned countries and through research and debate learn that country's position on international issues. The culminating activity has students participate in a mock United Nations Assembly vote. Argues that this method encourages students…

  8. Thermal Pollution: Background Material for a Mock Trial

    ERIC Educational Resources Information Center

    Armstrong, David G.

    1977-01-01

    Secondary teachers can involve students in a mock trial based on a 1975 New Jersey Superior Court case involving "thermal pollution." Article provides teachers' instructions; background data for plaintiff, defense, and witnesses; debriefing questions; and capstone activity. Available from: Law in American Society Foundation, 33 North LaSalle…

  9. Mock Trial: A Window to Free Speech Rights and Abilities

    ERIC Educational Resources Information Center

    Schwartz, Sherry

    2010-01-01

    This article provides some strategies to alleviate the current tensions between personal responsibility and freedom of speech rights in the public school classroom. The article advocates the necessity of making sure students understand the points and implications of the first amendment by providing a mock trial unit concerning free speech rights.…

  10. Hamilton Jeffers and the Double Star Catalogues

    NASA Astrophysics Data System (ADS)

    Tenn, Joseph S.

    2013-01-01

    Astronomers have long tracked double stars in efforts to find those that are gravitationally-bound binaries and then to determine their orbits. Court reporter and amateur astronomer Shelburne Wesley Burnham (1838-1921) published a massive double star catalogue containing more than 13,000 systems in 1906. The next keeper of the double stars was Lick Observatory astronomer Robert Grant Aitken (1864-1951), who produced a much larger catalogue in 1932. Aitken maintained and expanded Burnham’s records of observations on handwritten file cards, eventually turning them over to Lick Observatory astrometrist Hamilton Moore Jeffers (1893-1976). Jeffers further expanded the collection and put all the observations on punched cards. With the aid of Frances M. "Rete" Greeby (1921-2002), he made two catalogues: an Index Catalogue with basic data about each star, and a complete catalogue of observations, with one observation per punched card. He enlisted Willem van den Bos of Johannesburg to add southern stars, and they published the Index Catalogue of Visual Double Stars, 1961.0. As Jeffers approached retirement he became greatly concerned about the disposition of the catalogues. He wanted to be replaced by another "double star man," but Lick Director Albert E. Whitford (1905-2002) had the new 120-inch reflector, the world’s second largest telescope, and he wanted to pursue modern astrophysics instead. Jeffers was vociferously opposed to turning over the card files to another institution, and especially against their coming under the control of Kaj Strand of the U.S. Naval Observatory. In the end the USNO got the files and has maintained the records ever since, first under Charles Worley (1935-1997), and, since 1997, under Brian Mason. Now called the Washington Double Star Catalog (WDS), it is completely online and currently contains more than 1,000,000 measures of more than 100,000 pairs.

  11. New Generation of Catalogues for the New Generation of Users: A Comparison of Six Library Catalogues

    ERIC Educational Resources Information Center

    Mercun, Tanja; Zumer, Maja

    2008-01-01

    Purpose: The purpose of this paper is to describe some of the problems and issues faced by online library catalogues. It aims to establish how libraries have undertaken the mission of developing the next generation catalogues and how they compare to new tools such as Amazon. Design/methodology/approach: An expert study was carried out in January…

  12. Star formation rates in isolated galaxies selected from the Two-Micron All-Sky Survey

    NASA Astrophysics Data System (ADS)

    Melnyk, O.; Karachentseva, V.; Karachentsev, I.

    2015-08-01

    We have considered the star formation properties of 1616 isolated galaxies from the 2MASS XSC (Extended Source Catalog) selected sample (2MIG) with the far-ultraviolet GALEX magnitudes. This sample was then compared with corresponding properties of isolated galaxies from the Local Orphan Galaxies (LOG) catalogue and paired galaxies. We found that different selection algorithms define different populations of isolated galaxies. The population of the LOG catalogue, selected from non-clustered galaxies in the Local Supercluster volume, mostly consists of low-mass spiral and late-type galaxies. The specific star formation rate (SSFR) upper limit in isolated and paired galaxies does not exceed the value of ˜dex(-9.4). This is probably common for galaxies of differing activity and environment (at least at z < 0.06). The fractions of quenched galaxies are nearly twice as high in the paired galaxy sample as in the 2MIG isolated galaxy sample. From the behaviour of (S)SFR versus M* relations we deduced that the characteristic value influencing evolutionary processes is the galaxy mass. However, the environmental influence is notable: paired massive galaxies with logM* > 11.5 have higher (S)SFR than isolated galaxies. Our results suggest that the environment helps to trigger the star formation in the highest mass galaxies. We found that the fraction of AGN in the paired sample is only a little higher than in our isolated galaxy sample. We assume that AGN phenomenon is probably defined by secular galaxy evolution.

  13. A Revised Earthquake Catalogue for South Iceland

    NASA Astrophysics Data System (ADS)

    Panzera, Francesco; Zechar, J. Douglas; Vogfjörd, Kristín S.; Eberhard, David A. J.

    2016-01-01

    In 1991, a new seismic monitoring network named SIL was started in Iceland with a digital seismic system and automatic operation. The system is equipped with software that reports the automatic location and magnitude of earthquakes, usually within 1-2 min of their occurrence. Normally, automatic locations are manually checked and re-estimated with corrected phase picks, but locations are subject to random errors and systematic biases. In this article, we consider the quality of the catalogue and produce a revised catalogue for South Iceland, the area with the highest seismic risk in Iceland. We explore the effects of filtering events using some common recommendations based on network geometry and station spacing and, as an alternative, filtering based on a multivariate analysis that identifies outliers in the hypocentre error distribution. We identify and remove quarry blasts, and we re-estimate the magnitude of many events. This revised catalogue which we consider to be filtered, cleaned, and corrected should be valuable for building future seismicity models and for assessing seismic hazard and risk. We present a comparative seismicity analysis using the original and revised catalogues: we report characteristics of South Iceland seismicity in terms of b value and magnitude of completeness. Our work demonstrates the importance of carefully checking an earthquake catalogue before proceeding with seismicity analysis.

  14. The Adopted Morphological Types of 247 Rich PF Galaxy Clusters

    NASA Astrophysics Data System (ADS)

    Panko, Elena; Bajan, Katarzyna; Flin, Piotr; Gotsulyak, Alla

    2016-10-01

    Morphological types were determined for 247 rich galaxy clusters from the PF Catalogue of Galaxy Clusters and Groups. The adopted types are based on classical morphological schemes and consider concentration to the cluster center, the signs of preferential direction or plane in the cluster, and the positions of the brightest galaxies. It is shown that both concentration and preferential plane are significant and independent morphological criteria.

  15. A pseudo-spectrum analysis of galaxy-galaxy lensing

    NASA Astrophysics Data System (ADS)

    Hikage, Chiaki; Oguri, Masamune

    2016-10-01

    We present the application of the pseudo-spectrum method to galaxy-galaxy lensing. We derive explicit expressions for the pseudo-spectrum analysis of the galaxy-shear cross-spectrum, which is the Fourier space counterpart of the stacked galaxy-galaxy lensing profile. The pseudo-spectrum method corrects observational issues such as the survey geometry, masks of bright stars and their spikes, and inhomogeneous noise, which distort the spectrum and also mix the E-mode and the B-mode signals. Using ray-tracing simulations in N-body simulations including realistic masks, we confirm that the pseudo-spectrum method successfully recovers the input galaxy-shear cross-spectrum. We also show that the galaxy-shear cross-spectrum has an excess covariance relative to the Gaussian covariance at small scales (k ≳ 1h Mpc-1) where the shot noise is dominated in the Gaussian approximation. We find that the excess is consistent with the expectation from the halo sample variance (HSV), which originates from the matter fluctuations at scales larger than the survey area. We apply the pseudo-spectrum method to the observational data of Canada-France-Hawaii Telescope Lensing survey shear catalogue and three different spectroscopic samples of Sloan Digital Sky Survey Luminous Red Galaxy, and Baryon Oscillation Spectroscopic Survey CMASS and LOWZ galaxies. The galaxy-shear cross-spectra are significantly detected at the level of 7-10σ using the analytic covariance with the HSV contribution included. We also confirm that the observed spectra are consistent with the halo model predictions with the halo occupation distribution parameters estimated from previous work. This work demonstrates the viability of galaxy-galaxy lensing analysis in the Fourier space.

  16. Using Controversial Mock Trials in "Psychology and Law" Courses: Suggestions from Participants.

    ERIC Educational Resources Information Center

    Werth, James L., Jr.; Harvey, James; McNamara, Rebecca; Svoboda, Andrea; Gulbrandson, Raina; Hendren, Jennifer; Greedy, Tiffany; Leybold, Christie

    2002-01-01

    Describes a mock trial focused on Jack Kevorkian and an euthanasia case that was included in a psychology and law course. Discusses the course format, provides the reactions to the mock trial by students and consultants, and includes suggestions for improving the mock trial. (CMK)

  17. Galaxy and mass assembly (GAMA): projected galaxy clustering

    NASA Astrophysics Data System (ADS)

    Farrow, D. J.; Cole, Shaun; Norberg, Peder; Metcalfe, N.; Baldry, I.; Bland-Hawthorn, Joss; Brown, Michael J. I.; Hopkins, A. M.; Lacey, Cedric G.; Liske, J.; Loveday, Jon; Palamara, David P.; Robotham, A. S. G.; Sridhar, Srivatsan

    2015-12-01

    We measure the projected two-point correlation function of galaxies in the 180 deg2 equatorial regions of the GAMA II survey, for four different redshift slices between z = 0.0 and 0.5. To do this, we further develop the Cole method of producing suitable random catalogues for the calculation of correlation functions. We find that more r-band luminous, more massive and redder galaxies are more clustered. We also find that red galaxies have stronger clustering on scales less than ˜3 h-1 Mpc. We compare to two different versions of the GALFORM galaxy formation model, Lacey et al. (in preparation) and Gonzalez-Perez et al., and find that the models reproduce the trend of stronger clustering for more massive galaxies. However, the models underpredict the clustering of blue galaxies, can incorrectly predict the correlation function on small scales and underpredict the clustering in our sample of galaxies with {˜ } 3 Lr^*. We suggest possible avenues to explore to improve these clustering predictions. The measurements presented in this paper can be used to test other galaxy formation models, and we make the measurements available online to facilitate this.

  18. A 2 epoch proper motion catalogue from the UKIDSS Large Area Survey

    NASA Astrophysics Data System (ADS)

    Smith, Leigh; Lucas, Phil; Burningham, Ben; Jones, Hugh; Pinfield, David; Smart, Ricky; Andrei, Alexandre

    2013-04-01

    The UKIDSS Large Area Survey (LAS) began in 2005, with the start of the UKIDSS program as a 7 year effort to survey roughly 4000 square degrees at high galactic latitudes in Y, J, H and K bands. The survey also included a significant quantity of 2-epoch J band observations, with epoch baselines ranging from 2 to 7 years. We present a proper motion catalogue for the 1500 square degrees of the 2 epoch LAS data, which includes some 800,000 sources with motions detected above the 5σ level. We developed a bespoke proper motion pipeline which applies a source-unique second order polynomial transformation to UKIDSS array coordinates of each source to counter potential local non-uniformity in the focal plane. Our catalogue agrees well with the proper motion data supplied in the current WFCAM Science Archive (WSA) DR9 catalogue where there is overlap, and in various optical catalogues, but it benefits from some improvements. One improvement is that we provide absolute proper motions, using LAS galaxies for the relative to absolute correction. Also, by using unique, local, 2nd order polynomial tranformations, as opposed to the linear transformations in the WSA, we correct better for any local distortions in the focal plane, not including the radial distortion that is removed by their pipeline.

  19. The extragalactic distance scale derived from 'sosie' galaxies. I - Distances of 167 galaxies which are sosies of 14 nearby galaxies

    NASA Astrophysics Data System (ADS)

    Bottinelli, L.; Gouguenheim, L.; Paturel, G.; de Vaucouleurs, G.

    1985-11-01

    The method of "sosie" galaxies is applied to a large sample of galaxies extracted from the BGP catalog of H I line data and the Second Reference Catalogue of Bright Galaxies. The "sosies" of 14 calibrating galaxies (primary calibrators and galaxies in the nearest groups) are defined as those having the same parameters, either (1) morphological type T, axis ratio R, and maximum rotation velocity VM or (2) T, R, and luminosity index Λc. These two sets provide respectively for 127 and 72 galaxies (28 are in common) distance moduli directly derived from apparent magnitudes and/or diameters. The distances obtained here are compared with various other determinations; the agreement is generally good.

  20. Radio emission in peculiar galaxies

    NASA Technical Reports Server (NTRS)

    Demellorabaca, Dulia F.; Abraham, Zulema

    1990-01-01

    During the last decades a number of surveys of peculiar galaxies have been carried out and accurate positions become available. Since peculiarities are a possible evidence of radio emission (Wright, 1974; Sulentic, 1976; Stocke et al., 1978), the authors selected a sample of 24 peculiar galaxies with optical jet-like features or extensions in different optical catalogues, mainly the Catalogue of Southern Peculiar Galaxies and Associations (Arp and Madore, 1987) and the ESO/Uppsala Survey of the ESO(B) Atlas (Lauberts, 1982) for observation at the radio continuum frequency of 22 GHz. The sample is listed in a table. Sol (1987) studied this sample and concluded that the majority of the jet-like features seem to admit an explanation in terms of interactive galaxies with bridges and/or tails due to tidal effects. Only in a few cases do the jets seem to be possibly linked to some nuclear activity of the host galaxy. The observations were made with the 13.7m-radome enclosed Itapetinga Radiotelescope (HPBW of 4.3 arcmin), in Brazil. The receiver was a 1 GHz d.s.b. super-heterodine mixer operated in total-power mode, with a system temperature of approximately 800 K. The observational technique consisted in scans in right ascention, centralized in the optical position of the galaxy. The amplitude of one scan was 43 arcmin, and its duration time was 20 seconds. The integration time was at least 2 hours (12 ten-minute observations) and the sensibility limit adopted was an antenna temperature greater than 3 times the r.m.s. error of the baseline determination. Virgo A was used as the calibrator source. Three galaxies were detected for the first time as radio sources and four other known galaxies at low frequencies had their flux densities measured at 22 GHz. The results for these sources are presented.

  1. Hipparcos to deliver its final results catalogue soon

    NASA Astrophysics Data System (ADS)

    1995-10-01

    them, almost 30 years ago, to propose carrying out these observations from the relatively benign environment of space. Hipparcos is, by present standards, a medium-sized satellite, with a 30 cm telescope sensing simply ordinary light. But it has been described as the most imaginative in the short history of space astronomy. This foresight has been amply repaid. In the long history of stargazing it ranks with the surveys by Hipparchus the Greek in the 2nd Century BC and by Tichy Brahe the Dane in the 16th Century AD, both of which transformed human perceptions of the Universe. Positions derived from the Hipparcos satellite are better than a millionth of a degree, and newly a thousand times more accurate than star positions routinely determined from he ground. This accuracy makes it possible to measure directly the distances to the stars. While it took 250 years between astronomers first setting out on the exacting task of measuring the distance to a star, and a stellar distance being measured for the first time, ESA's Hipparcos mission has revolutionised this long, painstaking, and fundamental task by measuring accurate distances and movements of more than one hundred thousand. The measurement concept involved he satellite triangulating its way between he stars all wound the sky, building up a celestial map in much the same way as land surveyors use triangulation between hill-tops to measure distances accurately. Only the angles involved are much smaller : the accuracy that has been achieved with the Hipparcos Catalogue is such that he two edges of a coin, viewed from he other side of the Atlantic Ocean, could be distinguished. The results from Hipparcos will deliver scientists with long-awaited details of our place in he Milky Way Galaxy. Most of he stars visible to the naked eye are, to a large extent, companions of the Sun, in a great orbital march around the centre of the Galaxy, a journey so long that it takes individual stars 250 million years to complete, in

  2. Radio Galaxies.

    ERIC Educational Resources Information Center

    Downes, Ann

    1986-01-01

    Provides background information on radio galaxies. Topic areas addressed include: what produces the radio emission; radio telescopes; locating radio galaxies; how distances to radio galaxies are found; physics of radio galaxies; computer simulations of radio galaxies; and the evolution of radio galaxies with cosmic time. (JN)

  3. Extended Source/Galaxy All Sky 2

    NASA Technical Reports Server (NTRS)

    2003-01-01

    This panoramic view encompasses the entire sky and reveals the distribution of galaxies beyond the Milky Way galaxy, which astronomers call extended sources, as observed by Two Micron All-Sky Survey. The image is assembled from a database of over 1.6 million galaxies listed in the survey's All-Sky Survey Extended Source Catalog,; more than half of the galaxies have never before been catalogued. The colors represent how the many galaxies appear at three distinct wavelengths of infrared light (blue at 1.2 microns, green at 1.6 microns, and red at 2.2 microns). Quite evident are the many galactic clusters and superclusters, as well as some streamers composing the large-scale structure of the nearby universe. The blue overlay represents the very close and bright stars from our own Milky Way galaxy. In this projection, the bluish Milky Way lies predominantly toward the upper middle and edges of the image.

  4. Mock Nuclear Processing Facility-Safeguards Training Requirements

    SciTech Connect

    Gibbs, Philip; Hasty, Tim; Johns, Rissell; Baum, Gregory

    2014-08-31

    This document outlines specific training requirements in the topical areas of Material Control and Accounting (MC&A) and Physical Protection(PP) which are to be used as technical input for designing a mock Integrated Security Facility (ISF) at Sandia National Laboratories (SNL). The overall project objective for these requirements is to enhance the ability to deliver training on Material Protection Control and Accounting (MC&A) concepts regarding hazardous material such as irradiated materials with respect to bulk processing facilities.

  5. The one-point PDF of the initial conditions of our local Universe from the IRAS PSC redshift catalogue

    NASA Astrophysics Data System (ADS)

    Monaco, P.; Efstathiou, G.; Maddox, S. J.; Branchini, E.; Frenk, C. S.; McMahon, R. G.; Oliver, S. J.; Rowan-Robinson, M.; Saunders, W.; Sutherland, W. J.; Tadros, H.; White, S. D. M.

    2000-11-01

    The algorithm ztrace of Monaco & Efstathiou is applied to the IRAS PSCz catalogue to reconstruct the initial conditions of our local Universe with a resolution down to ~5h-1Mpc. The one-point probability distribution function (PDF) of the reconstructed initial conditions is consistent with the assumptions that: (i) IRAS galaxies trace mass on scales of ~5h-1Mpc and (ii) the statistics of the primordial density fluctuations are Gaussian. We use simulated PSCz catalogues, constructed from N-body simulations with Gaussian initial conditions, to show that local non-linear bias can cause the recovered initial PDF (assuming no bias) to be non-Gaussian. However, for plausible bias models, the distortions of the recovered PDF would be difficult to detect using the volume finely sampled by the PSCz catalogue. So, for Gaussian initial conditions, a range of bias models remain compatible with our PSCz reconstruction results.

  6. Next generation sequencing data of a defined microbial mock community

    PubMed Central

    Singer, Esther; Andreopoulos, Bill; Bowers, Robert M.; Lee, Janey; Deshpande, Shweta; Chiniquy, Jennifer; Ciobanu, Doina; Klenk, Hans-Peter; Zane, Matthew; Daum, Christopher; Clum, Alicia; Cheng, Jan-Fang; Copeland, Alex; Woyke, Tanja

    2016-01-01

    Generating sequence data of a defined community composed of organisms with complete reference genomes is indispensable for the benchmarking of new genome sequence analysis methods, including assembly and binning tools. Moreover the validation of new sequencing library protocols and platforms to assess critical components such as sequencing errors and biases relies on such datasets. We here report the next generation metagenomic sequence data of a defined mock community (Mock Bacteria ARchaea Community; MBARC-26), composed of 23 bacterial and 3 archaeal strains with finished genomes. These strains span 10 phyla and 14 classes, a range of GC contents, genome sizes, repeat content and encompass a diverse abundance profile. Short read Illumina and long-read PacBio SMRT sequences of this mock community are described. These data represent a valuable resource for the scientific community, enabling extensive benchmarking and comparative evaluation of bioinformatics tools without the need to simulate data. As such, these data can aid in improving our current sequence data analysis toolkit and spur interest in the development of new tools. PMID:27673566

  7. Thermal hydraulic modeling of the mock fuel facility

    NASA Astrophysics Data System (ADS)

    Gardner, Jacob

    The major focus of this thesis was to make improved three dimensional models of the Mock Fuel Facility. Three distinct experiment types run with the Mock Fuel Facility (MFF) were the main focus of this thesis. Two of the experiments were modeled and an in-depth analysis of the model results was performed to gain a better understanding of the Mock Fuel Facility. For the third experiment the process of creating a model was begun. There were multiple purposes for the work completed in this thesis. The work was done partially to gain a greater understanding of the UMass Lowell Research Reactor (UMLRR). There is minimal instrumentation within the UMLRR to measure localized temperatures within the UMLRR. It is hoped that the work done in this thesis will provide a basis for future modeling work which will give insight into the temperature profiles within the UMLRR. This work is also being done to gain insight into the capabilities of the COMSOL multiphysics modelling software and evaluate its potential for future modelling work. Finally this work is also being done for its potential as an educational tool. The MFF and COMSOL have potential to be used for experimental lab work by students to learn about computer modeling and validation.

  8. A Coupled THMC model of FEBEX mock-up test

    SciTech Connect

    Zheng, Liange; Samper, Javier

    2008-09-15

    FEBEX (Full-scale Engineered Barrier EXperiment) is a demonstration and research project for the engineered barrier system (EBS) of a radioactive waste repository in granite. It includes two full-scale heating and hydration tests: the in situ test performed at Grimsel (Switzerland) and a mock-up test operating at CIEMAT facilities in Madrid (Spain). The mock-up test provides valuable insight on thermal, hydrodynamic, mechanical and chemical (THMC) behavior of EBS because its hydration is controlled better than that of in situ test in which the buffer is saturated with water from the surrounding granitic rock. Here we present a coupled THMC model of the mock-up test which accounts for thermal and chemical osmosis and bentonite swelling with a state-surface approach. The THMC model reproduces measured temperature and cumulative water inflow data. It fits also relative humidity data at the outer part of the buffer, but underestimates relative humidities near the heater. Dilution due to hydration and evaporation near the heater are the main processes controlling the concentration of conservative species while surface complexation, mineral dissolution/precipitation and cation exchanges affect significantly reactive species as well. Results of sensitivity analyses to chemical processes show that pH is mostly controlled by surface complexation while dissolved cations concentrations are controlled by cation exchange reactions.

  9. Massive relic galaxies prefer dense environments

    NASA Astrophysics Data System (ADS)

    Peralta de Arriba, Luis; Quilis, Vicent; Trujillo, Ignacio; Cebrián, María; Balcells, Marc

    2016-09-01

    We study the preferred environments of z ˜ 0 massive relic galaxies (M⋆ ≳ 1010 M⊙ galaxies with little or no growth from star formation or mergers since z ˜ 2). Significantly, we carry out our analysis on both a large cosmological simulation and an observed galaxy catalogue. Working on the Millennium I-WMAP7 simulation we show that the fraction of today massive objects which have grown less than 10 per cent in mass since z ˜ 2 is ˜0.04 per cent for the whole massive galaxy population with M⋆ > 1010 M⊙. This fraction rises to ˜0.18 per cent in galaxy clusters, confirming that clusters help massive galaxies remain unaltered. Simulations also show that massive relic galaxies tend to be closer to cluster centres than other massive galaxies. Using the New York University Value-Added Galaxy Catalogue, and defining relics as M⋆ ≳ 1010 M⊙ early-type galaxies with colours compatible with single-stellar population ages older than 10 Gyr, and which occupy the bottom 5-percentile in the stellar mass-size distribution, we find 1.11 ± 0.05 per cent of relics among massive galaxies. This fraction rises to 2.4 ± 0.4 per cent in high-density environments. Our findings point in the same direction as the works by Poggianti et al. and Stringer et al. Our results may reflect the fact that the cores of the clusters are created very early on, hence the centres host the first cluster members. Near the centres, high-velocity dispersions and harassment help cluster core members avoid the growth of an accreted stellar envelope via mergers, while a hot intracluster medium prevents cold gas from reaching the galaxies, inhibiting star formation.

  10. Radio loud far-infrared galaxies

    SciTech Connect

    Dey, A; Shields, J.C. . Dept. of Astronomy); Van Breugel, W.J.M. )

    1990-03-01

    We present the first results of a multiwavelength study of IRAS galaxies with excess radio emission. The sample was selected by cross-correlating the IRAS Faint Source Survey (for {vert bar}b{vert bar} {ge} 50{degree}) and the Point Source Catalogue (for 10{degree} < {vert bar}b{vert bar} < 50{degree}) with the Texas radio survey. Recent optical (imaging and spectroscopic) and radio (VLA) observations are discussed. These observations will be used to investigate possible connections between radio galaxy activity, star formation and galaxy interactions. 15 refs., 3 figs.

  11. Ultraviolet to infrared emission of z > 1 galaxies: Can we derive reliable star formation rates and stellar masses?

    NASA Astrophysics Data System (ADS)

    Buat, V.; Heinis, S.; Boquien, M.; Burgarella, D.; Charmandaris, V.; Boissier, S.; Boselli, A.; Le Borgne, D.; Morrison, G.

    2014-01-01

    Aims: Our knowledge of the cosmic mass assembly relies on measurements of star formation rates (SFRs) and stellar masses (Mstar), of galaxies as a function of redshift. These parameters must be estimated in a consistent way with a good knowledge of systematics before studying their correlation and the variation of the specific SFR. Constraining these fundamental properties of galaxies across the Universe is of utmost importance if we want to understand galaxy formation and evolution. Methods: We seek to derive SFRs and stellar masses in distant galaxies and to quantify the main uncertainties affecting their measurement. We explore the impact of the assumptions made in their derivation with standard calibrations or through a fitting process, as well as the impact of the available data, focusing on the role of infrared emission originating from dust. Results: We build a sample of galaxies with z > 1, all observed from the ultraviolet to the infrared in their rest frame. The data are fitted with the code CIGALE, which is also used to build and analyse a catalogue of mock galaxies. Models with different star formation histories are introduced: an exponentially decreasing or increasing SFR and a more complex one coupling a decreasing SFR with a younger burst of constant star formation. We define different sets of data, with or without a good sampling of the ultraviolet range, near-infrared, and thermal infrared data. Variations of the metallicity are also investigated. The impact of these different cases on the determination of stellar mass and SFR are analysed. Conclusions: Exponentially decreasing models with a redshift formation of the stellar population zf ≃ 8 cannot fit the data correctly. All the other models fit the data correctly at the price of unrealistically young ages when the age of the single stellar population is taken to be a free parameter, especially for the exponentially decreasing models. The best fits are obtained with two stellar populations. As

  12. Crustal Dynamics Project: Catalogue of site information

    NASA Technical Reports Server (NTRS)

    1985-01-01

    This document represents a catalogue of site information for the Crustal Dynamics Project. It contains information and descriptions of those sites used by the Project as observing stations for making the precise geodetic measurements useful for studies of the Earth's crustal movements and deformation.

  13. Observing the Origins of Galaxy Structure in the Illustris Simulation

    NASA Astrophysics Data System (ADS)

    Snyder, Greg

    2014-10-01

    Many processes affect the appearance of galaxies, and it has recently become possible to predict how these processes set internal galaxy structure in significant populations. Such calculations are poised to clarify the physics of star formation quenching, the cosmological formation of bulges and disks, and the observability of galaxy mergers. To advance these goals, we propose to build and analyze a very large set of mock HST images based on the Illustris Project. This accurate continuous-volume hydrodynamical simulation formed thousands of structurally diverse Milky Way-mass galaxies in {106.5 Mpc}^3 with detail comparable to the resolution of HST at many cosmic times. We will mock-observe 41,000 model galaxies at 0 < z < 5 in broadband filters used by ACS, WFC3, and JWST/NIRCAM, and measure automated morphology diagnostics from each image. This will constitute a timely and effective tool to advance two key goals of observational cosmology with HST: linking the building blocks of galaxies across cosmic time, and understanding the implications of galaxy morphology and structure. It will allow us to study the emergence of the Hubble Sequence, estimate merger rates and consequences, and interpret star formation patterns in distant galaxies. Therefore this model dataset is ideally suited to enhance results from HST Treasury and Archival Legacy surveys, the Ultra Deep Fields, and Frontier Fields. To increase the science return, we will publicly release our model images and morphology catalogs, providing a tool that can directly link physical mechanisms to high redshift galaxy data.

  14. The PASTEL catalogue of stellar parameters

    NASA Astrophysics Data System (ADS)

    Soubiran, C.; Le Campion, J.-F.; Cayrel de Strobel, G.; Caillo, A.

    2010-06-01

    Aims: The PASTEL catalogue is an update of the [Fe/H] catalogue, published in 1997 and 2001. It is a bibliographical compilation of stellar atmospheric parameters providing (T_eff, log g, [Fe/H]) determinations obtained from the analysis of high resolution, high signal-to-noise spectra, carried out with model atmospheres. PASTEL also provides determinations of the one parameter T_eff based on various methods. It is aimed in the future to provide also homogenized atmospheric parameters and elemental abundances, radial and rotational velocities. A web interface has been created to query the catalogue on elaborated criteria. PASTEL is also distributed through the CDS database and VizieR. Methods: To make it as complete as possible, the main journals have been surveyed, as well as the CDS database, to find relevant publications. The catalogue is regularly updated with new determinations found in the literature. Results: As of Febuary 2010, PASTEL includes 30151 determinations of either T_eff or (T_eff, log g, [Fe/H]) for 16 649 different stars corresponding to 865 bibliographical references. Nearly 6000 stars have a determination of the three parameters (T_eff, log g, [Fe/H]) with a high quality spectroscopic metallicity. The catalogue can be queried through a dedicated web interface at http://pastel.obs.u-bordeaux1.fr/. It is also available in electronic form at the Centre de Données Stellaires in Strasbourg (http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/pastel), at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/515/A111

  15. X-rays beware: the deepest Chandra catalogue of point sources in M31

    NASA Astrophysics Data System (ADS)

    Vulic, N.; Gallagher, S. C.; Barmby, P.

    2016-10-01

    This study represents the most sensitive Chandra X-ray point source catalogue of M31. Using 133 publicly available Chandra ACIS-I/S observations totalling ˜1 Ms, we detected 795 X-ray sources in the bulge, north-east, and south-west fields of M31, covering an area of ≈0.6 deg2, to a limiting unabsorbed 0.5-8.0 keV luminosity of ˜1034 erg s-1. In the inner bulge, where exposure is approximately constant, X-ray fluxes represent average values because they were determined from many observations over a long period of time. Similarly, our catalogue is more complete in the bulge fields since monitoring allowed more transient sources to be detected. The catalogue was cross-correlated with a previous XMM-Newton catalogue of M31's D25 isophote consisting of 1948 X-ray sources, with only 979 within the field of view of our survey. We found 387 (49 per cent) of our Chandra sources (352 or 44 per cent unique sources) matched to within 5 arcsec of 352 XMM-Newton sources. Combining this result with matching done to previous Chandra X-ray sources we detected 259. new sources in our catalogue. We created X-ray luminosity functions (XLFs) in the soft (0.5-2.0 keV) and hard (2.0-8.0 keV) bands that are the most sensitive for any large galaxy based on our detection limits. Completeness-corrected XLFs show a break around ≈1.3 × 1037 erg s-1, consistent with previous work. As in past surveys, we find that the bulge XLFs are flatter than the disc, indicating a lack of bright high-mass X-ray binaries in the disc and an aging population of low-mass X-ray binaries in the bulge.

  16. Unusual flux-distance relationship for pulsars suggested by analysis of the Australia national telescopy facility pulsar catalogue

    SciTech Connect

    Singleton, John; Perez, M R; Singleton, J; Ardavan, H; Ardavan, A

    2009-01-01

    We analyze pulsar fluxes at 1400 MHz (S(1400)) and distances d taken from the Australia National Telescope Facility (ATNF) Pulsar Catalogue. Under the assumption that pulsar populations in different parts of the Galaxy are similar, we find that either (a) pulsar fluxes diminish with distance according to a non-standard power law (we suggest S(1400){proportional_to} 1/d rather than {proportional_to} 1/d{sup 2}) or (b) that there are very significant (i.e. order of magnitude) errors in the distance estimates quoted in the ATNF Catalogue. The former conclusion (a) supports a recent model for pulsar emission that has also successfully explained the frequency spectrum of the Crab pulsar over 16 orders of magnitude of frequency, whilst alternative (b) would necessitate a radical re-evaluation of both the dispersion method for estimating pulsar distances and current ideas about the distribution of pulsars within our Galaxy.

  17. A Comparative Study of the Guo Shoujing Star Catalogue and the Ulugh Beg Star Catalogue

    NASA Astrophysics Data System (ADS)

    Sun, Xiaochun; Yang, Fan; Zhao, Yongheng

    2015-08-01

    The Chinese Star Catalogue by Guo Shoujing (1231-1316) contained equatorial coordinates of 678 stars, more than doubled the number of stars in previous Chinese star catalogues. In the period 1420-1437, using astronomical instruments at Samarkand Observatory, Ulugh Beg (1394-1449) made independent observations and determined star positions of 1018 stars. An analysis of two star catalogues will show the observational techniques behind them and their accuracies. Both astronomers tried to increase accuracy of measurement by enlarging the astronomical instruments. The Chinese catalogue gives equatorial coordinates of stars. The coordinates were directly read off the armillary sphere, which was mounted equatorially mounted. Sun Xiaochun (1996) suggested that the data of the existent Guo Shoujing catalogue was actually observed around 1380, at the beginning of the Ming dynasty. The Ulugh Beg catalogue gives ecliptic coordinates of stars. Does this mean they were directly measured using an ecliptic instrument? Using Fourier analysis we discover a 3 arc minute systematic error in the declinations, which are derived from the ecliptic coordinates, suggesting the data might be first measured equatorially and then converted to ecliptic coordinates, following Ptolemaic tradition. The 3 arc minute systematic error was caused by the misalignment of the instrument's pole and celestial north pole. And the Our comparative study might throw some light on transmission of astronomical knowledge and techniques between China and Central Asia in medieval times.

  18. 32 CFR 575.6 - Catalogue, United States Military Academy.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 32 National Defense 3 2014-07-01 2014-07-01 false Catalogue, United States Military Academy. 575.6... ADMISSION TO THE UNITED STATES MILITARY ACADEMY § 575.6 Catalogue, United States Military Academy. The latest edition of the catalogue, United States Military Academy, contains additional...

  19. 32 CFR 575.6 - Catalogue, United States Military Academy.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 32 National Defense 3 2013-07-01 2013-07-01 false Catalogue, United States Military Academy. 575.6... ADMISSION TO THE UNITED STATES MILITARY ACADEMY § 575.6 Catalogue, United States Military Academy. The latest edition of the catalogue, United States Military Academy, contains additional...

  20. 32 CFR 575.6 - Catalogue, United States Military Academy.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 32 National Defense 3 2011-07-01 2009-07-01 true Catalogue, United States Military Academy. 575.6... ADMISSION TO THE UNITED STATES MILITARY ACADEMY § 575.6 Catalogue, United States Military Academy. The latest edition of the catalogue, United States Military Academy, contains additional...

  1. 32 CFR 575.6 - Catalogue, United States Military Academy.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 32 National Defense 3 2012-07-01 2009-07-01 true Catalogue, United States Military Academy. 575.6... ADMISSION TO THE UNITED STATES MILITARY ACADEMY § 575.6 Catalogue, United States Military Academy. The latest edition of the catalogue, United States Military Academy, contains additional...

  2. 32 CFR 575.6 - Catalogue, United States Military Academy.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 32 National Defense 3 2010-07-01 2010-07-01 true Catalogue, United States Military Academy. 575.6... ADMISSION TO THE UNITED STATES MILITARY ACADEMY § 575.6 Catalogue, United States Military Academy. The latest edition of the catalogue, United States Military Academy, contains additional...

  3. Inferring Host Dark Matter Halo Masses of Individual Galaxies from Neighboring Galaxy Counts

    NASA Astrophysics Data System (ADS)

    Oguri, Masamune; Lin, Yen-Ting

    2015-03-01

    How well can we infer host dark matter halo masses of individual galaxies? Based on the halo occupation distribution framework, we analytically compute the number of neighboring galaxies within a cylinder of some redshift interval and radius in transverse comoving distance. The result is used to derive the conditional probability distribution function (PDF) of the host halo mass of a galaxy, given the neighboring galaxy counts. We compare our analytic results with those obtained using a realistic mock galaxy catalog, finding reasonable agreements. We find the optimal cylinder radius to be ∼ 0.5-1 {{h}-1} Mpc for the inference of halo masses. The PDF is generally broad, and sometimes has two peaks at low- and high-mass regimes because of the effect of chance projection along the line of sight. Potential applications and extensions of the new theoretical framework developed herein are also discussed.

  4. Seismic Catalogue and Seismic Network in Haiti

    NASA Astrophysics Data System (ADS)

    Belizaire, D.; Benito, B.; Carreño, E.; Meneses, C.; Huerfano, V.; Polanco, E.; McCormack, D.

    2013-05-01

    The destructive earthquake occurred on January 10, 2010 in Haiti, highlighted the lack of preparedness of the country to address seismic phenomena. At the moment of the earthquake, there was no seismic network operating in the country, and only a partial control of the past seismicity was possible, due to the absence of a national catalogue. After the 2010 earthquake, some advances began towards the installation of a national network and the elaboration of a seismic catalogue providing the necessary input for seismic Hazard Studies. This paper presents the state of the works carried out covering both aspects. First, a seismic catalogue has been built, compiling data of historical and instrumental events occurred in the Hispaniola Island and surroundings, in the frame of the SISMO-HAITI project, supported by the Technical University of Madrid (UPM) and Developed in cooperation with the Observatoire National de l'Environnement et de la Vulnérabilité of Haiti (ONEV). Data from different agencies all over the world were gathered, being relevant the role of the Dominican Republic and Puerto Rico seismological services which provides local data of their national networks. Almost 30000 events recorded in the area from 1551 till 2011 were compiled in a first catalogue, among them 7700 events with Mw ranges between 4.0 and 8.3. Since different magnitude scale were given by the different agencies (Ms, mb, MD, ML), this first catalogue was affected by important heterogeneity in the size parameter. Then it was homogenized to moment magnitude Mw using the empirical equations developed by Bonzoni et al (2011) for the eastern Caribbean. At present, this is the most exhaustive catalogue of the country, although it is difficult to assess its degree of completeness. Regarding the seismic network, 3 stations were installed just after the 2010 earthquake by the Canadian Government. The data were sent by telemetry thought the Canadian System CARINA. In 2012, the Spanish IGN together

  5. Platelet Function During Hypothermia in Experimental Mock Circulation.

    PubMed

    Van Poucke, Sven; Stevens, Kris; Kicken, Cécile; Simons, Antoine; Marcus, Abraham; Lancé, Marcus

    2016-03-01

    Alterations in platelet function are a common finding in surgical procedures involving cardiopulmonary bypass and hypothermia. Although the combined impact of hypothermia and artificial circulation on platelets has been studied before, the ultimate strategy to safely minimize the risk for bleeding and thrombosis is yet unknown. The aim of this study was to evaluate the use of a mock circulation loop to study the impact of hypothermia for platelet-related hemostatic changes. Venous blood was collected from healthy adult humans (n = 3). Closed mock circulation loops were assembled, each consisting of a centrifugal pump, an oxygenator with integrated heat exchanger, and a hardshell venous reservoir. The experiment started with the mock circulation temperature set at 37°C (T0 [0 h]). Cooling was then initiated at T1 (+2 h), where temperature was adjusted from 37°C to 32°C. Hypothermia was maintained from T2 (+4 h) to T3 (+28 h). From that point in time, rewarming from 32°C to 37°C was initiated with similar speed as cooling. From time point T4 (+30 h), normothermia (37°C) was maintained until the experiment ended at T5 (+32 h). Blood samples were analyzed in standard hematological tests: light transmission aggregometry (LTA) (arachidonic acid [AA], adenosine diphosphate [ADP], collagen [COL], thrombin-receptor-activating-peptide-14 [TRAP]), multiple electrode aggregometry (MEA) (AA, ADP, COL, TRAP), and rotational thromboelastometry (ROTEM) (EXTEM, FIBTEM, PLTEM). Hemoglobin, hematocrit, and platelet count decrease more substantially during temperature drop (37-32°C) than during hypothermia maintenance. Hb and Hct continue to follow this trend during active rewarming (32-37°C). PC increase from the moment active rewarming was initiated. None of the values return to the initial values. LTA values demonstrate a similar decrease in aggregation after stimulation with the platelet agonists between the start of the mock circulation and the start of cooling. Except

  6. RECONSTRUCTING THE INITIAL DENSITY FIELD OF THE LOCAL UNIVERSE: METHODS AND TESTS WITH MOCK CATALOGS

    SciTech Connect

    Wang Huiyuan; Mo, H. J.; Yang Xiaohu; Van den Bosch, Frank C.

    2013-07-20

    Our research objective in this paper is to reconstruct an initial linear density field, which follows the multivariate Gaussian distribution with variances given by the linear power spectrum of the current cold dark matter model and evolves through gravitational instabilities to the present-day density field in the local universe. For this purpose, we develop a Hamiltonian Markov Chain Monte Carlo method to obtain the linear density field from a posterior probability function that consists of two components: a prior of a Gaussian density field with a given linear spectrum and a likelihood term that is given by the current density field. The present-day density field can be reconstructed from galaxy groups using the method developed in Wang et al. Using a realistic mock Sloan Digital Sky Survey DR7, obtained by populating dark matter halos in the Millennium simulation (MS) with galaxies, we show that our method can effectively and accurately recover both the amplitudes and phases of the initial, linear density field. To examine the accuracy of our method, we use N-body simulations to evolve these reconstructed initial conditions to the present day. The resimulated density field thus obtained accurately matches the original density field of the MS in the density range 0.3{approx}<{rho}/ {rho}-bar {approx}<20 without any significant bias. In particular, the Fourier phases of the resimulated density fields are tightly correlated with those of the original simulation down to a scale corresponding to a wavenumber of {approx}1 h Mpc{sup -1}, much smaller than the translinear scale, which corresponds to a wavenumber of {approx}0.15 h Mpc{sup -1}.

  7. Galaxy Group Properties in Observations and Simulations

    NASA Astrophysics Data System (ADS)

    Nurmi, Pasi

    2016-10-01

    In this project, we compare different properties of galaxy groups in cosmological N-body simulations and SDSS galaxy group catalogs. In the first part of the project (Nurmi et al. 2013) we compared the basic properties of the groups like the luminosity functions, group richness and velocity dispersion distributions and studied how good is the agreement between the mock group catalog and the SDSS group catalog. Here we continue the earlier study and use updated galaxy group catalog (SDSS DR10) and new simulation data (Guo et al. 2013). We reanalyse earlier group properties and include new properties in the analysis like group environment, star formation rates and group masses. Our analysis show that there are clear differences between the simulated and observed properties of galaxy groups, especially for small groups with a few members. Also, the high luminosities are clearly overestimated in the simulations compared with the SDSS group data.

  8. Implementation of Mock Competency Skill Assessments to Improve Student Outcomes.

    PubMed

    Payne, Camille; Ziegler, M Penny; Baughman, Diana M; Jones, Jackie

    2015-01-01

    A primary responsibility for nurse educators is to provide students with theoretical knowledge and clinical skills for professional nursing. In this study, laboratory faculty developed a creative pedagogical strategy to reduce nursing student stress during assessment of skill performance. Mock competencies were structured so that students participated in peer-to-peer evaluations in simulated competency assessments. The purpose of this study was to determine whether this pedagogical strategy had an impact on first-round pass rates for skills competency assessments. PMID:25950797

  9. Neutron spectrum from the little boy mock-up

    SciTech Connect

    Robba, A.A.

    1986-01-01

    Most of the human exposure data used for setting radiation protection guidelines have been obtained by following the survivors of the nuclear explosions at Hiroshima and Nagasaki. Proper evaluation of these data requires estimates of the radiation exposure received by those survivors. Until now neutron dose estimates have relied primarily on calculations as no measurements of the leakage neutron flux or neutron spectrum were available. We have measured the high-energy leakage neutron spectrum from a mock-up of the Little Boy device operating at delayed critical. The measurements are compared with Monte Carlo calculations of the leakage neutron spectrum.

  10. Quantum modular forms, mock modular forms, and partial theta functions

    NASA Astrophysics Data System (ADS)

    Kimport, Susanna

    Defined by Zagier in 2010, quantum modular forms have been the subject of an explosion of recent research. Many of these results are aimed at discovering examples of these functions, which are defined on the rational numbers and have "nice" modularity properties. Though the subject is in its early stages, numerous results (including Zagier's original examples) show these objects naturally arising from many areas of mathematics as limits of other modular-like functions. One such family of examples is due to Folsom, Ono, and Rhoades, who connected these new objects to partial theta functions (introduced by Rogers in 1917) and mock modular forms (about which there is a rich theory, whose origins date back to Ramanujan in 1920). In this thesis, we build off of the work of Folsom, Ono, and Rhoades by providing an infinite family of quantum modular forms of arbitrary positive half-integral weight. Further, this family of quantum modular forms "glues" mock modular forms to partial theta functions and is constructed from a so-called "universal" mock theta function by extending a method of Eichler and Zagier (originally defined for holomorphic Jacobi forms) into a non-holomorphic setting. In addition to the infinite family, we explore the weight 1/2 and 3/2 functions in more depth. For both of these weights, we are able to explicitly write down the quantum modular form, as well as the corresponding "errors to modularity," which can be shown to be Mordell integrals of specific theta functions and, as a consequence, are real-analytic functions. Finally, we turn our attention to the partial theta functions associated with these low weight examples. Berndt and Kim provide asymptotic expansions for a certain class of partial theta functions as q approaches 1 radially within the unit disk. Here, we extend this work to not only obtain asymptotic expansions for this class of functions as q approaches any root of unity, but also for a certain class of derivatives of these functions

  11. Representations of affine superalgebras and mock theta functions. III

    NASA Astrophysics Data System (ADS)

    Kac, V. G.; Wakimoto, M.

    2016-08-01

    We study modular invariance of normalized supercharacters of tame integrable modules over an affine Lie superalgebra, associated to an arbitrary basic Lie superalgebra g. For this we develop a several step modification process of multivariable mock theta functions, where at each step a Zwegers' type 'modifier' is used. We show that the span of the resulting modified normalized supercharacters is \\operatorname{SL}_2( Z)-invariant, with the transformation matrix equal, in the case the Killing form on g is non-degenerate, to that for the basic defect 0 subalgebra g^! of g, orthogonal to a maximal isotropic set of roots of g.

  12. The stellar kinematics of corotating spiral arms in Gaia mock observations

    NASA Astrophysics Data System (ADS)

    Hunt, Jason A. S.; Kawata, Daisuke; Grand, Robert J. J.; Minchev, Ivan; Pasetto, Stefano; Cropper, Mark

    2015-06-01

    We have observed an N-body/smoothed particle hydrodynamics simulation of a Milky Way-like barred spiral galaxy. We present a simple method that samples N-body model particles into mock Gaia stellar observations and takes into account stellar populations, dust extinction and Gaia's science performance estimates. We examine the kinematics of stars with V ≤ 16 mag around a nearby spiral arm at a similar position to the Perseus arm at three lines of sight in the disc plane; (l, b) = (90, 0), (120, 0) and (150, 0) deg. We find that the structure of the peculiar kinematics around the corotating spiral arm, which is found in Kawata et al. (2014b), is still visible in the observational data expected to be produced by Gaia, despite the dust extinction and expected observational errors of Gaia. These observable kinematic signatures will enable testing whether the Perseus arm of the Milky Way is similar to the corotating spiral arms commonly seen in N-body simulations.

  13. Seachable Solar Feature Catalogues in EGSO

    NASA Astrophysics Data System (ADS)

    Zharkova, V. V.; Aboudarham, J.; Zharkov, S. I.; Ipson, S. S.; Benkhalil, A. K.; Fuller, N.

    2004-12-01

    The searchable Solar Feature Catalogues (SFC) developed using automated pattern recognition techniques from digitized solar images are presented. The techniques were applied for detection of sunspots, active regions, filaments and line-on-sight magnetic neutral lines in the automatically standardized full disk solar images in Ca II K1, Ca II K3 and Ha taken at the Meudon Observatory and white light images and magnetograms from SOHO/MDI. The results of automated recognition were verified with the manual synoptic maps and available statistical data that revealed good detection accuracy. Based on the recognized parameters a structured database of the Solar Feature Catalogues was built on a mysql server for every feature and published with various pre-designed search pages on the Bradford University web site. The SFCs with 10 year coverage (1996-2005) is to be used for deeper investigation of the solar activity, activity feature classification and forecast.

  14. Grid Enabled Geospatial Catalogue Web Service

    NASA Technical Reports Server (NTRS)

    Chen, Ai-Jun; Di, Li-Ping; Wei, Ya-Xing; Liu, Yang; Bui, Yu-Qi; Hu, Chau-Min; Mehrotra, Piyush

    2004-01-01

    Geospatial Catalogue Web Service is a vital service for sharing and interoperating volumes of distributed heterogeneous geospatial resources, such as data, services, applications, and their replicas over the web. Based on the Grid technology and the Open Geospatial Consortium (0GC) s Catalogue Service - Web Information Model, this paper proposes a new information model for Geospatial Catalogue Web Service, named as GCWS which can securely provides Grid-based publishing, managing and querying geospatial data and services, and the transparent access to the replica data and related services under the Grid environment. This information model integrates the information model of the Grid Replica Location Service (RLS)/Monitoring & Discovery Service (MDS) with the information model of OGC Catalogue Service (CSW), and refers to the geospatial data metadata standards from IS0 19115, FGDC and NASA EOS Core System and service metadata standards from IS0 191 19 to extend itself for expressing geospatial resources. Using GCWS, any valid geospatial user, who belongs to an authorized Virtual Organization (VO), can securely publish and manage geospatial resources, especially query on-demand data in the virtual community and get back it through the data-related services which provide functions such as subsetting, reformatting, reprojection etc. This work facilitates the geospatial resources sharing and interoperating under the Grid environment, and implements geospatial resources Grid enabled and Grid technologies geospatial enabled. It 2!so makes researcher to focus on science, 2nd not cn issues with computing ability, data locztic, processir,g and management. GCWS also is a key component for workflow-based virtual geospatial data producing.

  15. New Statistical Perspective to Link Void Distributions with Galaxy Clusters

    NASA Astrophysics Data System (ADS)

    Russell, Esra; Pycke, Jean-Renaud

    2016-07-01

    Voids dominate the total observed volume of the large scale structure and they are very sensitive to their environments which can strongly affect their shape as well their distributions. Therefore the void size distribution functions may play an important role to understand the dynamical processes affecting the structure formation of the Universe Here, using cosmic void data sets of Sutter et al. (2012) generated by galaxy mock catalogs which are tuned to three SDSS main samples, we obtain the size distribution of voids as a three parameter redshift independent log-normal void probability function. We find that the shape of the three parameter void distribution from the mock data samples is strikingly similar to the galaxy log-normal mass distribution obtained from numerical studies. This similarity of void size and galaxy mass distributions may possibly indicate evidence of large scale nonlinear mechanisms affecting both voids and galaxies, such as large scale accretion and tidal effects. Taking into account that all voids we study are generated by galaxy mock catalogs and they show hierarchical structures at different levels, it may be possible that the same nonlinear mechanisms of mass distribution affect the void size distribution.

  16. Remapping simulated halo catalogues in redshift space

    NASA Astrophysics Data System (ADS)

    Mead, A. J.; Peacock, J. A.

    2014-12-01

    We discuss the extension to redshift space of a rescaling algorithm, designed to alter the effective cosmology of a pre-existing simulated particle distribution or catalogue of dark matter haloes. The rescaling approach was initially developed by Angulo & White and was adapted and applied to halo catalogues in real space in our previous work. This algorithm requires no information other than the initial and target cosmological parameters, and it contains no tuned parameters. It is shown here that the rescaling method also works well in redshift space, and that the rescaled simulations can reproduce the growth rate of cosmological density fluctuations appropriate for the target cosmology. Even when rescaling a grossly non-standard model with Λ = 0 and zero baryons, the redshift-space power spectrum of standard Λ cold dark matter can be reproduced to about 5 per cent error for k < 0.2 h Mpc-1. The ratio of quadrupole-to-monopole power spectra remains correct to the same tolerance up to k = 1 h Mpc-1, provided that the input halo catalogue contains measured internal velocity dispersions.

  17. An Astrostatistical Approach to Distant Galaxy Morphology

    NASA Astrophysics Data System (ADS)

    Lotz, Jennifer

    2012-10-01

    A galaxy's morphology is an important tracer of its recent assembly history and correlates strongly with other fundamental properties such as star-formation history, kinematics, and black hole mass. Our current approaches do not fully exploit the wealth of structural information available in the deep HST images, nor do they reliably classify rare but important populations such as galaxy mergers and unstable disks at z > 1. As a result, the connections between galaxy assembly, star formation, and morphological transformation via mergers, disk instabilities, and bulge formation remain unsolved problems.Our primary goals for this Legacy Archival program are {1} to derive a rigorous statistical methodology for quantifying and classifying distant galaxy structures; {2} to apply these new astrostatistical algorithms to galaxies at 0 < z < 2.5 in the major HST extragalactic legacy fields and measure the structural evolution; {3} to measure and classify mock HST images of hydrodynamical cosmological simulations of galaxies at 0 < z < 2.5, and test these against our measurements of the real universe.This program will produce several much-needed Legacy products. With these algorithms, we will produce and publicly release high quality catalogs of optical/near-IR quantitative morphology and classifications for the HST extragalactic legacy fields. We will also provide similar catalogs for mock HST images of state-of-the-art cosmological simulations of galaxy assembly and structural evolution. Finally, we will publicly release the software for calculating our new morphology statistics and running the new galaxy classification algorithms to encourage broad use by the community.

  18. The star catalogue of Hevelius. Machine-readable version and comparison with the modern Hipparcos Catalogue

    NASA Astrophysics Data System (ADS)

    Verbunt, F.; van Gent, R. H.

    2010-06-01

    The catalogue by Johannes Hevelius with the positions and magnitudes of 1564 entries was published by his wife Elisabeth Koopman in 1690. We provide a machine-readable version of the catalogue, and briefly discuss its accuracy on the basis of comparison with data from the modern Hipparcos Catalogue. We compare our results with an earlier analysis by Rybka (1984), finding good overall agreement. The magnitudes given by Hevelius correlate well with modern values. The accuracy of his position measurements is similar to that of Brahe, with σ = 2´ for longitudes and latitudes, but with more errors >5´ than expected for a Gaussian distribution. The position accuracy decreases slowly with magnitude. The fraction of stars with position errors larger than a degree is 1.5%, rather smaller than the fraction of 5% in the star catalogue of Brahe. Star catalogue of Hevelius is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A29

  19. Determining the bivariate brightness distribution of galaxies.

    NASA Astrophysics Data System (ADS)

    Boyce, P. J.; Phillipps, S.

    1995-04-01

    In this paper we describe a set of criteria which we propose a sample of galaxies must satisfy if it is to be useful for determining the bivariate brightness distribution (BBD) of galaxies in luminosity and surface brightness and we consider the prospects for deriving such a sample. First, we note that determinations of the galaxy luminosity function can be seriously in error if surface brightness (visibility) selection effects are ignored. We suggest that a determination of the BBD is a more physically useful aim. A straightforward way to obtain the BBD would be to determine a luminosity function in a set of narrow surface brightness bins. We propose a set of criteria which the sample of galaxies in each surface brightness bin must satisfy if it is to be reliably used in such a determination. Each sample should be restricted to a well defined range in morphological type, the measured isophotal size and magnitude and the surface brightness of each galaxy should be corrected to a common galactic inclination, all galaxies should have measured redshifts and the sample should be complete to a known isophotal size and/or magnitude. We then describe a rigorous method for selecting samples which satisfy these criteria from existing catalogues of galaxies. We apply this method to the ESO-LV catalogue and find that from the intial sample of 11000 galaxies with a disk component we can only find 5 subsamples in half-magnitude wide surface brightness bins which satisfy our proposed criteria. The largest derived subsample contains only 27 galaxies, far too few to determine a luminosity function at its surface brightness. We suggest that had our proposed criteria been applied to the samples used in previous determinations of the BBD or the galaxy luminosity function then sample sizes would have been greatly reduced. For this reason, we suggest that the conclusions of previous work should be treated with caution.

  20. Hubble Space Telescope mock-up in use in the MDF

    NASA Technical Reports Server (NTRS)

    1986-01-01

    View of helium filled mock-up of the Hubble Space Telescope in use in the Manipulator Development Facility (MDF) in bldg 9A. The mock-up is being maneuvered into a mock-up of the Shuttle payload bay on the end of the remote manipulator system (RMS) arm. The Space Shuttle full fuselage trainer is seen in the background, to the left. To the right is another simulation of the Hubble Telescope.

  1. Introducing GRACE Follow-On mock data challenge project

    NASA Astrophysics Data System (ADS)

    Darbeheshti, Neda; Naeimi, Majid; Hewitson, Martin; Heinzel, Gerhard; Flury, Jakob

    2016-04-01

    GRACE Follow-On satellites will be launched in 2017. Equipped with the additional Laser Ranging Instrument (LRI) sensor, GRACE Follow-On is expected to reach even better spatial and temporal resolution for the Earth's gravity field. GRACE Follow-On mock data challenge project is part of the geo-Q project at Leibniz Universität Hannover and plans several runs of data challenges for GRACE Follow-On. The challenges are coordinated from simple gravity field recovery in 2015 to more advanced forms when LRI noise model will be added in 2016 challenge. The aim of these challenges is to engage different research centers around the world to test their methods for gravity field recovery from simulated data which will lead to develop data analysis tools and capabilities for GRACE follow-On data. In this contribution we introduce the mock data challenge project for GRACE and GRACE Follow-On. The highlights and objectives of the challenges will be given, with the details about the webpage and data exchange for the participants.

  2. VizieR Online Data Catalog: Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)

    NASA Astrophysics Data System (ADS)

    Misgeld, I.; Mieske, S.; Hilker, M.

    2008-07-01

    The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein & Zabludoff (2003ApJ...591..764C). (1 data file).

  3. Lyman-α emitters in the context of hierarchical galaxy formation: predictions for VLT/MUSE surveys

    NASA Astrophysics Data System (ADS)

    Garel, T.; Guiderdoni, B.; Blaizot, J.

    2016-02-01

    The VLT/Multi Unit Spectrograph Explorer (MUSE) integral-field spectrograph can detect Lyα emitters (LAE) in the redshift range 2.8 ≲ z ≲ 6.7 in a homogeneous way. Ongoing MUSE surveys will notably probe faint Lyα sources that are usually missed by current narrow-band surveys. We provide quantitative predictions for a typical wedding-cake observing strategy with MUSE based on mock catalogues generated with a semi-analytic model of galaxy formation coupled to numerical Lyα radiation transfer models in gas outflows. We expect ≈1500 bright LAEs (FLyα ≳ 10-17 erg s-1 cm-2) in a typical shallow field (SF) survey carried over ≈100 arcmin2 , and ≈2000 sources as faint as 10-18 erg s-1 cm-2 in a medium-deep field (MDF) survey over 10 arcmin2 . In a typical deep field (DF) survey of 1 arcmin2 , we predict that ≈500 extremely faint LAEs (FLyα ≳ 4 × 10-19 erg s-1 cm-2) will be found. Our results suggest that faint Lyα sources contribute significantly to the cosmic Lyα luminosity and SFR budget. While the host haloes of bright LAEs at z ≈ 3 and 6 have descendants with median masses of 2 × 1012 and 5 × 1013 M⊙, respectively, the faintest sources detectable by MUSE at these redshifts are predicted to reside in haloes which evolve into typical sub-L* and L* galaxy haloes at z = 0. We expect typical DF and MDF surveys to uncover the building blocks of Milky Way-like objects, even probing the bulk of the stellar mass content of LAEs located in their progenitor haloes at z ≈ 3.

  4. The BMW (Brera-Multiscale-Wavelet) Catalogue of Serendipitous X-Ray Sources

    NASA Astrophysics Data System (ADS)

    Lazzati, Davide; Campana, Sergio; Covino, Stefano; Israel, Gian L.; Guzzo, Luigi; Mignani, Roberto; Moretti, Alberto; Panzera, Maria R.; Tagliaferri, Gianpiero

    In collaboration with the Observatories of Palermo and Rome and the SAX-SDC we are constructing a multi-site interactive archive system featuring specific analysis tools. In this context we developed a detection algorithm based on the Wavelet Transform (WT) and performed a systematic analysis of all ROSATHRI public data (˜3100 observations +1000 to come). The WT is specifically suitable to detect and characterize extended sources while properly detecting point sources in very crowded fields. Moreover, the good angular resolution of HRI images allows the source extension and position to be accurately determined. This effort has produced the BMW (Brera Multiscale Wavelet) catalogue, with more than 19,000 sources detected at the ˜4.2σ level. For each source detection we have information on the X-ray flux and extension, allowing for instance to select complete samples of extended X-ray sources such as candidate clusters of galaxies or SNR's. Details about the detection algorithm and the catalogue can be found in Lazzati et al. 1999 and Campana et al. 1999. Here we shall present an overview of first results from several undergoing projects which make use of the BMW catalogue.

  5. Galaxy Zoo: morphologies derived from visual inspection of galaxies from the Sloan Digital Sky Survey

    NASA Astrophysics Data System (ADS)

    Lintott, Chris J.; Schawinski, Kevin; Slosar, Anže; Land, Kate; Bamford, Steven; Thomas, Daniel; Raddick, M. Jordan; Nichol, Robert C.; Szalay, Alex; Andreescu, Dan; Murray, Phil; Vandenberg, Jan

    2008-09-01

    In order to understand the formation and subsequent evolution of galaxies one must first distinguish between the two main morphological classes of massive systems: spirals and early-type systems. This paper introduces a project, Galaxy Zoo, which provides visual morphological classifications for nearly one million galaxies, extracted from the Sloan Digital Sky Survey (SDSS). This achievement was made possible by inviting the general public to visually inspect and classify these galaxies via the internet. The project has obtained more than 4 × 107 individual classifications made by ~105 participants. We discuss the motivation and strategy for this project, and detail how the classifications were performed and processed. We find that Galaxy Zoo results are consistent with those for subsets of SDSS galaxies classified by professional astronomers, thus demonstrating that our data provide a robust morphological catalogue. Obtaining morphologies by direct visual inspection avoids introducing biases associated with proxies for morphology such as colour, concentration or structural parameters. In addition, this catalogue can be used to directly compare SDSS morphologies with older data sets. The colour-magnitude diagrams for each morphological class are shown, and we illustrate how these distributions differ from those inferred using colour alone as a proxy for morphology. This publication has been made possible by the participation of more than 100000 volunteers in the Galaxy Zoo project. Their contributions are individually acknowledged at http://www.galaxyzoo.org/Volunteers.aspx E-mail: cjl@astro.ox.ac.uk (CJL); kevins@astro.ox.ac.uk (KS)

  6. New Pulkovo combined catalogues of the radio source positions.

    NASA Astrophysics Data System (ADS)

    Sokolova, Yulia; Malkin, Zinovy

    2012-08-01

    Catalogues of radio source positions (RSC) obtained from Very Long Baseline Interferometry (VLBI) observations serve as the realizations of the IAU International Celestial Reference System (ICRS) since 1998. With increasing of the volume and improving the accuracy of VLBI observations with time, development of advanced methods of the RSC construction is a topical problem to realize the full potential of VLBI technology. This task becomes more and more important nowadays in view of expected during coming years realization of the VLBI2010 network and highly accurate GAIA catalogue of optical positions of extragalactic objects. One of the commonly used methods of improving the accuracy of the source position catalogues is construction of a combined catalogue. In this paper, we present new Pulkovo combined catalogues PUL(2012)C01 and PUL(2012)C02 which have been constructed mainly following the strategy developed by Sokolova & Malkin (2007, A&A, 474, 665). Besides using more data, several developments were realized such as improved method of determination of the optimal number of the expansion terms, more careful investigation of the stochastic errors of input catalogues, improved weighting scheme, additional test of the quality of the individuals and combined RSC, etc. The PUL(2012)C01 catalogue is aimed at stochastic improvement of the ICRF2, the PUL(2012)C02 catalogue is constructed in the independent system. Results of comparison of our combined catalogues with individual catalogues and ICRF2 are presented.

  7. The Far-Infrared Properties of the Most Isolated Galaxies

    NASA Astrophysics Data System (ADS)

    Lisenfeld, U.; Verdes-Montenegro, L.; Sulentic, J.; Leon, S.; Espada, D.; Bergond, G.; García, E.; Sabater, J.; Santander-Vela, J. D.; Verley, S.

    2007-05-01

    A long-standing question in galaxy evolution involves the role of nature (self-regulation) vs. nurture (environment) on the observed properties (and evolution) of galaxies. A collaboration centreed at the Instituto de Astrofisica de Andalucia (Granada, Spain) is trying to address this question by producing a observational database for a sample of 1050 isolated galaxies from the catalogue of Karachentseva (1973) with the overarching goal being the generation of a "zero-point" sample against which effects of environment on galaxies can be assessed. The AMIGA (Analysis of the Interstellar Medium of Isolated Galaxies) database (see www.iaa.es/AMIGA.html) will include optical, IR and radio line and continuum measures. The galaxies in the sample represent the most isolated galaxies in the local universe. In the present contribution, we will present the project, as well as the results of an analysis of the far-infrared (FIR) and molecular gas properties of this sample.

  8. Void galaxy properties depending on void filament straightness

    NASA Astrophysics Data System (ADS)

    Shim, Junsup; Lee, Jounghun; Hoyle, Fiona

    2015-08-01

    We investigate the properties of galaxies belonging to the filaments in cosmic void regions, using the void catalogue constructed by Pan et al. (2012) from the SDSS DR7. To identify galaxy filaments within a void, voids with 30 or more galaxies are selected as a sample. We identify 3172 filaments in 1055 voids by applying the filament finding algorithm utilizing minimal spanning tree (MST) which is an unique linear pattern into which connects all the galaxies in a void. We study the correlations between galaxy properties and the specific size of filament which quantifies the degree of the filament straightness. For example, the average magnitude and the magnitude of the faintest galaxy in filament decrease as the straightness of the filament increases. We also find that the correlations become stronger in rich filaments with many member galaxies than in poor ones. We discuss a physical explanation to our findings and their cosmological implications.

  9. Photometric redshift requirements for lens galaxies in galaxy-galaxy lensing analyses

    NASA Astrophysics Data System (ADS)

    Nakajima, R.; Mandelbaum, R.; Seljak, U.; Cohn, J. D.; Reyes, R.; Cool, R.

    2012-03-01

    Weak gravitational lensing is a valuable probe of galaxy formation and cosmology. Here we quantify the effects of using photometric redshifts (photo-z) in galaxy-galaxy lensing, for both sources and lenses, both for the immediate goal of using galaxies with photo-z as lenses in the Sloan Digital Sky Survey (SDSS) and as a demonstration of methodology for large, upcoming weak lensing surveys that will by necessity be dominated by lens samples with photo-z. We calculate the bias in the lensing mass calibration as well as consequences for absolute magnitude (i.e. k-corrections) and stellar mass estimates for a large sample of SDSS Data Release 8 (DR8) galaxies. The redshifts are obtained with the template-based photo-z code ZEBRA on the SDSS DR8 ugriz photometry. We assemble and characterize the calibration samples (˜9000 spectroscopic redshifts from four surveys) to obtain photometric redshift errors and lensing biases corresponding to our full SDSS DR8 lens and source catalogues. Our tests of the calibration sample also highlight the impact of observing conditions in the imaging survey when the spectroscopic calibration covers a small fraction of its footprint; atypical imaging conditions in calibration fields can lead to incorrect conclusions regarding the photo-z of the full survey. For the SDSS DR8 catalogue, we find σΔz/(1+z)= 0.096 and 0.113 for the lens and source catalogues, with flux limits of r= 21 and 21.8, respectively. The photo-z bias and scatter is a function of photo-z and template types, which we exploit to apply photo-z quality cuts. By using photo-z rather than spectroscopy for lenses, dim blue galaxies and L* galaxies up to z˜ 0.4 can be used as lenses, thus expanding into unexplored areas of parameter space. We also explore the systematic uncertainty in the lensing signal calibration when using source photo-z, and both lens and source photo-z; given the size of existing training samples, we can constrain the lensing signal calibration (and

  10. The infrared database of extragalactic observables from Spitzer - I. The redshift catalogue

    NASA Astrophysics Data System (ADS)

    Hernán-Caballero, Antonio; Spoon, Henrik W. W.; Lebouteiller, Vianney; Rupke, David S. N.; Barry, Donald P.

    2016-01-01

    This is the first of a series of papers on the Infrared Database of Extragalactic Observables from Spitzer (IDEOS). In this work, we describe the identification of optical counterparts of the infrared sources detected in Spitzer Infrared Spectrograph (IRS) observations, and the acquisition and validation of redshifts. The IDEOS sample includes all the spectra from the Cornell Atlas of Spitzer/IRS Sources (CASSIS) of galaxies beyond the Local Group. Optical counterparts were identified from correlation of the extraction coordinates with the NASA Extragalactic Database (NED). To confirm the optical association and validate NED redshifts, we measure redshifts with unprecedented accuracy on the IRS spectra (σ(Δz/(1+z)) ˜ 0.0011) by using an improved version of the maximum combined pseudo-likelihood method (MCPL). We perform a multistage verification of redshifts that considers alternate NED redshifts, the MCPL redshift, and visual inspection of the IRS spectrum. The statistics is as follows: the IDEOS sample contains 3361 galaxies at redshift 0 < z < 6.42 (mean: 0.48, median: 0.14). We confirm the default NED redshift for 2429 sources and identify 124 with incorrect NED redshifts. We obtain IRS-based redshifts for 568 IDEOS sources without optical spectroscopic redshifts, including 228 with no previous redshift measurements. We provide the entire IDEOS redshift catalogue in machine-readable formats. The catalogue condenses our compilation and verification effort, and includes our final evaluation on the most likely redshift for each source, its origin, and reliability estimates.

  11. Planck 2015 results. XXVII. The second Planck catalogue of Sunyaev-Zeldovich sources

    NASA Astrophysics Data System (ADS)

    Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Barrena, R.; Bartlett, J. G.; Bartolo, N.; Battaner, E.; Battye, R.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Böhringer, H.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J.-F.; Carvalho, P.; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R.-R.; Chiang, H. C.; Chon, G.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Comis, B.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Dahle, H.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Désert, F.-X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Eisenhardt, P. R. M.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Fergusson, J.; Feroz, F.; Ferragamo, A.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Grainge, K. J. B.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jin, T.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maggio, G.; Maino, D.; Mak, D. S. Y.; Mandolesi, N.; Mangilli, A.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; McGehee, P.; Mei, S.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nastasi, A.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Olamaie, M.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrott, Y. C.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rozo, E.; Rubiño-Martín, J. A.; Rumsey, C.; Rusholme, B.; Rykoff, E. S.; Sandri, M.; Santos, D.; Saunders, R. D. E.; Savelainen, M.; Savini, G.; Schammel, M. P.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Shimwell, T. W.; Spencer, L. D.; Stanford, S. A.; Stern, D.; Stolyarov, V.; Stompor, R.; Streblyanska, A.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tramonte, D.; Tristram, M.; Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; White, S. D. M.; Wright, E. L.; Yvon, D.; Zacchei, A.; Zonca, A.

    2016-09-01

    We present the all-sky Planck catalogue of Sunyaev-Zeldovich (SZ) sources detected from the 29 month full-mission data. The catalogue (PSZ2) is the largest SZ-selected sample of galaxy clusters yet produced and the deepest systematic all-sky surveyof galaxy clusters. It contains 1653 detections, of which 1203 are confirmed clusters with identified counterparts in external data sets, and is the first SZ-selected cluster survey containing >103 confirmed clusters. We present a detailed analysis of the survey selection function in terms of its completeness and statistical reliability, placing a lower limit of 83% on the purity. Using simulations, we find that the estimates of the SZ strength parameter Y5R500are robust to pressure-profile variation and beam systematics, but accurate conversion to Y500 requires the use of prior information on the cluster extent. We describe the multi-wavelength search for counterparts in ancillary data, which makes use of radio, microwave, infra-red, optical, and X-ray data sets, and which places emphasis on the robustness of the counterpart match. We discuss the physical properties of the new sample and identify a population of low-redshift X-ray under-luminous clusters revealed by SZ selection. These objects appear in optical and SZ surveys with consistent properties for their mass, but are almost absent from ROSAT X-ray selected samples.

  12. Deep 3-GHz observations of the Lockman Hole North with the Very Large Array - II. Catalogue and μJy source properties

    NASA Astrophysics Data System (ADS)

    Vernstrom, T.; Scott, Douglas; Wall, J. V.; Condon, J. J.; Cotton, W. D.; Kellermann, K. I.; Perley, R. A.

    2016-11-01

    This is the second of two papers describing the observations and source catalogues derived from sensitive 3-GHz images of the Lockman Hole North using the Karl G. Jansky Very Large Array (VLA). We describe the reduction and cataloguing process, which yielded an image with 8 arcsec resolution and instrumental noise of σn = 1.01 μJy beam-1 rms (before primary-beam corrections) and a catalogue of 558 sources detected above 5σn. We include details of how we estimate source spectral indices across the 2-GHz VLA bandwidth, finding a median index of -0.76 ± 0.04. Stacking of source spectra reveals a flattening of spectral index with decreasing flux density. We present a source count derived from the catalogue. We show a traditional count estimate compared with a completely independent estimate made via a P(D) confusion analysis, and find very good agreement. Cross-matches of the catalogue with X-ray, optical, infrared, radio, and redshift catalogues are also presented. The X-ray, optical and infrared data, as well as active galactic nuclei (AGN) selection criteria allow us to classify 10 per cent as radio-loud AGN, 28 per cent as radio-quiet AGN, and 58 per cent as star-forming galaxies, with only 4 per cent unclassified.

  13. The Planck Catalogue of Galactic Cold Clumps : Looking at the early stages of star-formation

    NASA Astrophysics Data System (ADS)

    Montier, Ludovic

    2015-08-01

    The Planck satellite has provided an unprecedented view of the submm sky, allowing us to search for the dust emission of Galactic cold sources. Combining Planck-HFI all-sky maps in the high frequency channels with the IRAS map at 100um, we built the Planck catalogue of Galactic Cold Clumps (PGCC, Planck 2015 results XXVIII 2015), counting 13188 sources distributed over the whole sky, and following mainly the Galactic structures at low and intermediate latitudes. This is the first all-sky catalogue of Galactic cold sources obtained with a single instrument at this resolution and sensitivity, which opens a new window on star-formation processes in our Galaxy.I will briefly describe the colour detection method used to extract the Galactic cold sources, i.e., the Cold Core Colour Detection Tool (CoCoCoDeT, Montier et al. 2010), and its application to the Planck data. I will discuss the statistical distribution of the properties of the PGCC sources (in terms of dust temperature, distance, mass, density and luminosity), which illustrates that the PGCC catalogue spans a large variety of environments and objects, from molecular clouds to cold cores, and covers various stages of evolution. The Planck catalogue is a very powerful tool to study the formation and the evolution of prestellar objects and star-forming regions.I will finally present an overview of the Herschel Key Program Galactic Cold Cores (PI. M.Juvela), which allowed us to follow-up about 350 Planck Galactic Cold Clumps, in various stages of evolution and environments. With this program, the nature and the composition of the 5' Planck sources have been revealed at a sub-arcmin resolution, showing very different configurations, such as starless cold cores or multiple Young Stellar objects still embedded in their cold envelope.

  14. The morphological types of galaxies in the Local Supercluster

    NASA Astrophysics Data System (ADS)

    Bajan, K.; Flin, P.; Godłowski, W.

    2016-10-01

    On the basis of the Hyper - Leda Catalogue HyperLeda 8293 galaxies with heliocentric radial velocities below 2500 km s-1 were selected; 4570 had known morphological types (4366 had calculated b/a ratio). We checked the frequency of the distribution of various types in the LSC, finding spirals and irregulars most numerous, in accordance with expectations. The axial ratio of galaxy diameters of various types was studied, and the dependence of this parameter on the morphological type was noted.

  15. The outer halo globular cluster system of M31 - I. The final PAndAS catalogue

    NASA Astrophysics Data System (ADS)

    Huxor, A. P.; Mackey, A. D.; Ferguson, A. M. N.; Irwin, M. J.; Martin, N. F.; Tanvir, N. R.; Veljanoski, J.; McConnachie, A.; Fishlock, C. K.; Ibata, R.; Lewis, G. F.

    2014-08-01

    We report the discovery of 59 globular clusters (GCs) and two candidate GCs in a search of the halo of M31, primarily via visual inspection of Canada-France-Hawaii Telescope/MegaCam imagery from the Pan-Andromeda Archaeological Survey (PAndAS). The superior quality of these data also allows us to check the classification of remote objects in the Revised Bologna Catalogue (RBC), plus a subset of GC candidates drawn from Sloan Digital Sky Survey (SDSS) imaging. We identify three additional new GCs from the RBC, and confirm the GC nature of 11 SDSS objects (8 of which appear independently in our remote halo catalogue); the remaining 188 candidates across both lists are either foreground stars or background galaxies. Our new catalogue represents the first uniform census of GCs across the M31 halo - we find clusters to the limit of the PAndAS survey area at projected radii of up to Rproj ˜ 150 kpc. Tests using artificial clusters reveal that detection incompleteness cuts in at luminosities below MV = -6.0; our 50 per cent completeness limit is MV ≈ -4.1. We construct a uniform set of PAndAS photometric measurements for all known GCs outside Rproj = 25 kpc, and any new GCs within this radius. With these data, we update results from Huxor et al., investigating the luminosity function (LF), colours and effective radii of M31 GCs with a particular focus on the remote halo. We find that the GCLF is clearly bimodal in the outer halo (Rproj > 30 kpc), with the secondary peak at MV ˜ -5.5. We argue that the GCs in this peak have most likely been accreted along with their host dwarf galaxies. Notwithstanding, we also find, as in previous surveys, a substantial number of GCs with above-average luminosity in the outer M31 halo - a population with no clear counterpart in the Milky Way.

  16. The BMW-Chandra Serendipitous Source Catalogue

    NASA Astrophysics Data System (ADS)

    Romano, P.; Campana, S.; Mignani, R. P.; Moretti, A.; Panzera, M. R.; Tagliaferri, G.

    We present the BMW-Chandra Source Catalogue drawn from all Chandra ACIS-I pointed observations with an exposure time in excess of 10 ks public as of March 2003 (136 observations). Using the wavelet detection algorithm developed by \\citep{Lazzatiea99} and \\citep{Campanaea99}, which can characterize point-like as well as extended sources, we identified 21325 sources which were visually inspected and verified. Among them, 16758 are not associated with the targets of the pointings and are considered certain; they have a 0.5-10 keV absorption corrected flux distribution median of ˜ 7 × 10-15 erg cm-2 s-1. The catalogue consists of source positions, count rates, extensions and relative errors in three energy bands (total, 0.5-7 keV; soft, 0.5-2 keV; and hard band, 2-7 keV), as well as the additional information drawn from the headers of the original files. We also extracted source counts in four additional energy bands, (0.5-1.0 keV, 1.0-2.0 keV, 2.0-4.0 keV and 4.0-7.0 keV). We compute the sky coverage in the soft and hard bands. The complete catalogue provides a sky coverage in the soft band (0.5-2 keV, S/N =3) of ˜ 8 deg2 at a limiting flux of ˜ 10-13 erg cm-2 s-1, and ˜ 2 deg2 at a limiting flux of ˜ 10-15 erg cm-2 s-1. http://www.merate.mi.astro.it/~xanadu/BMC/bmc_home.html

  17. Associations Between the Ancient Star Catalogues

    NASA Astrophysics Data System (ADS)

    Duke, Dennis W.

    2002-07-01

    There are just two substantial sources of star coordinates preserved for us from antiquity: the star catalogue of Ptolemy's Almagest, and the rising, setting, and culmination phenomena, along with some star declinations and right ascensions, from Hipparchus' Commentary to Aratus. Given the controversy associated with the idea that Ptolemy's catalogue is, in whole or in substantial part, a copy of an earlier but now lost catalogue of Hipparchus, it is of interest to try to establish clear and significant associations, or the lack thereof, between the two sets of ancient star data. There have been two complementary efforts to clarify the possible associations. Vogt used the phenomena and declinations to reconstruct the ecliptical coordinates of some 122 stars in Hipparchus' Commentary that also appear in the Almagest catalogue. Vogt's conclusion was that since his reconstructed coordinates and the Almagest coordinates were, in general, different, Ptolemy did not obtain his data from Hipparchus. Vogt did notice five stars with very similar errors and concluded that Ptolemy probably did copy those from Hipparchus. More recently, however, Grasshoff has pointed out that there are several reasons to doubt Vogt's conclusion. Further, Grasshoff worked in the opposite direction, using the Almagest coordinates to compute the Hipparchan phenomena, and concluded, for two reasons, that the Almagest data and the Commentary data share a common origin. First, there are a number of stars that share large common errors, and it is highly unlikely that these agreements could be coincidental. Second, the correlation coefficients between the various error sets are typically large and statistically significant, and this also suggests a common origin of the two data sets. However, Grasshoff provided no analysis of the correlations to support this second conclusion. In this paper I will (1) analyze the correlations between the errors of the phenomena and the predictions of these phenomena

  18. Mock jurors' perceptions of facial hair on criminal offenders.

    PubMed

    Conti, Richard P; Conti, Melanie A

    2004-06-01

    Two studies were conducted to measure whether mock jurors would stereotype criminal offenders as having facial hair. In Study 1, participants were asked which photograph belonged to a defendant in a rape case and which photograph belonged to a plaintiff in a head-injury case after they were "accidentally" dropped. The photographs were similar in appearance except one had facial hair. 78% of 63 participants (or 49) identified the photograph with facial hair as being involved in the rape case. In Study 2, 371 participants were asked to sketch the face of a criminal offender. 82% of the sketches (or 249) contained some form of facial hair. Results are consistent with the hypothesis that criminal defendants are perceived as having facial hair.

  19. The Mock LISA Data Challenges: History, Status, Prospects

    NASA Technical Reports Server (NTRS)

    Vallisneri, Michele; Babak, Stas; Baker, John; Benacquista, Matt; Cornish, Neil; Crowder, Jeff; Cutler, Curt; Larson, Shane; Littenberg, Tyson; Porter, Edward; Vecchio, Alberto

    2007-01-01

    This slide presentation reviews the importance for the Mock LISA Data Challenges (MLDC). Laser Interferometer Space Antenna (LISA) is a gravitational wave (GW) observatory that will return data such that data analysis is integral to the measurement concept. Further rationale of the MLDC are to kickstart the development of a LISA data-analysis computational infrastructure, and to encourage, track, and compare progress in LISA data-analysis development in the open community. The MLDCs is a coordinated, voluntary effort in GW community, that will periodically issue datasets with synthetic noise and GW signals from sources of undisclosed parameters; increasing difficulty. The challenge participants return parameter estimates and descriptions of search methods. Some of the challenges and the resultant entries are reviewed. The aim is to show that LISA data analysis is possible, and to develop new techniques, using multiple international teams for the development of LISA core analysis tools

  20. Advanced smile diagnostics using CAD/CAM mock-ups.

    PubMed

    Sancho-Puchades, Manuel; Fehmer, Vincent; Hämmerle, Christoph; Sailer, Irena

    2015-01-01

    Diagnostics are essential for predictable restorative dentistry. Both patient and clinician must agree on a treatment goal before the final restorations are delivered to avoid future disappointments. However, fully understanding the patient's desires is difficult. A useful tool to overcome this problem is the diagnostic wax-up and mock-up. A potential treatment outcome is modeled in wax prior to treatment and transferred into the patient's mouth using silicon indexes and autopolymerizing resin to obtain the patient's approval. Yet, this time-consuming procedure only produces a single version of the possible treatment outcome, which can be unsatisfactory for both the patient and the restorative team. Contemporary digital technologies may provide advantageous features to aid in this diagnostic treatment step. This article reviews opportunities digital technologies offer in the diagnostic phase, and presents clinical cases to illustrate the procedures.

  1. Engineering and manufacturing of ITER first mirror mock-ups

    SciTech Connect

    Joanny, M.; Travere, J. M.; Salasca, S.; Corre, Y.; Marot, L.; Thellier, C.; Gallay, G.; Cammarata, C.; Passier, B.; Ferme, J. J.

    2010-10-15

    Most of the ITER optical diagnostics aiming at viewing and monitoring plasma facing components will use in-vessel metallic mirrors. These mirrors will be exposed to a severe plasma environment and lead to an important tradeoff on their design and manufacturing. As a consequence, investigations are carried out on diagnostic mirrors toward the development of optimal and reliable solutions. The goals are to assess the manufacturing feasibility of the mirror coatings, evaluate the manufacturing capability and associated performances for the mirrors cooling and polishing, and finally determine the costs and delivery time of the first prototypes with a diameter of 200 and 500 mm. Three kinds of ITER candidate mock-ups are being designed and manufactured: rhodium films on stainless steel substrate, molybdenum on TZM substrate, and silver films on stainless steel substrate. The status of the project is presented in this paper.

  2. Solving a Mock Arsenic-Poisoning Case Using Atomic Spectroscopy

    NASA Astrophysics Data System (ADS)

    Tarr, Matthew A.

    2001-01-01

    A new upper-level undergraduate atomic spectroscopy laboratory procedure has been developed that presents a realistic problem to students and asks them to assist in solving it. Students are given arsenic-laced soda samples from a mock crime scene. From these samples, they are to gather evidence to help prosecute a murder suspect. The samples are analyzed by inductively coupled plasma atomic emission spectroscopy or by atomic absorbance spectroscopy to determine the content of specific metal impurities. By statistical comparison of the samples' composition, the students determine if the soda samples can be linked to arsenic found in the suspect's home. As much as possible, the procedures and interpretations are developed by the students. Particular emphasis is placed on evaluating the limitations and capabilities of the analytical method with respect to the demands of the problem.

  3. Engineering and manufacturing of ITER first mirror mock-ups.

    PubMed

    Joanny, M; Travère, J M; Salasca, S; Corre, Y; Marot, L; Thellier, C; Gallay, G; Cammarata, C; Passier, B; Fermé, J J

    2010-10-01

    Most of the ITER optical diagnostics aiming at viewing and monitoring plasma facing components will use in-vessel metallic mirrors. These mirrors will be exposed to a severe plasma environment and lead to an important tradeoff on their design and manufacturing. As a consequence, investigations are carried out on diagnostic mirrors toward the development of optimal and reliable solutions. The goals are to assess the manufacturing feasibility of the mirror coatings, evaluate the manufacturing capability and associated performances for the mirrors cooling and polishing, and finally determine the costs and delivery time of the first prototypes with a diameter of 200 and 500 mm. Three kinds of ITER candidate mock-ups are being designed and manufactured: rhodium films on stainless steel substrate, molybdenum on TZM substrate, and silver films on stainless steel substrate. The status of the project is presented in this paper.

  4. Mock LISA data challenge for the Galactic white dwarf binaries

    SciTech Connect

    Blaut, Arkadiusz; Babak, Stanislav; Krolak, Andrzej

    2010-03-15

    We present data analysis methods used in the detection and estimation of parameters of gravitational-wave signals from the white dwarf binaries in the mock LISA data challenge. Our main focus is on the analysis of challenge 3.1, where the gravitational-wave signals from more than 6x10{sup 7} Galactic binaries were added to the simulated Gaussian instrumental noise. The majority of the signals at low frequencies are not resolved individually. The confusion between the signals is strongly reduced at frequencies above 5 mHz. Our basic data analysis procedure is the maximum likelihood detection method. We filter the data through the template bank at the first step of the search, then we refine parameters using the Nelder-Mead algorithm, we remove the strongest signal found and we repeat the procedure. We detect reliably and estimate parameters accurately of more than ten thousand signals from white dwarf binaries.

  5. Broad Absorption Line Quasar catalogues with Supervised Neural Networks

    SciTech Connect

    Scaringi, Simone; Knigge, Christian; Cottis, Christopher E.; Goad, Michael R.

    2008-12-05

    We have applied a Learning Vector Quantization (LVQ) algorithm to SDSS DR5 quasar spectra in order to create a large catalogue of broad absorption line quasars (BALQSOs). We first discuss the problems with BALQSO catalogues constructed using the conventional balnicity and/or absorption indices (BI and AI), and then describe the supervised LVQ network we have trained to recognise BALQSOs. The resulting BALQSO catalogue should be substantially more robust and complete than BI-or AI-based ones.

  6. Extending the ISC-GEM Global Earthquake Instrumental Catalogue

    NASA Astrophysics Data System (ADS)

    Di Giacomo, Domenico; Engdhal, Bob; Storchak, Dmitry; Villaseñor, Antonio; Harris, James

    2015-04-01

    After a 27-month project funded by the GEM Foundation (www.globalquakemodel.org), in January 2013 we released the ISC-GEM Global Instrumental Earthquake Catalogue (1900 2009) (www.isc.ac.uk/iscgem/index.php) as a special product to use for seismic hazard studies. The new catalogue was necessary as improved seismic hazard studies necessitate that earthquake catalogues are homogeneous (to the largest extent possible) over time in their fundamental parameters, such as location and magnitude. Due to time and resource limitation, the ISC-GEM catalogue (1900-2009) included earthquakes selected according to the following time-variable cut-off magnitudes: Ms=7.5 for earthquakes occurring before 1918; Ms=6.25 between 1918 and 1963; and Ms=5.5 from 1964 onwards. Because of the importance of having a reliable seismic input for seismic hazard studies, funding from GEM and two commercial companies in the US and UK allowed us to start working on the extension of the ISC-GEM catalogue both for earthquakes that occurred beyond 2009 and for earthquakes listed in the International Seismological Summary (ISS) which fell below the cut-off magnitude of 6.25. This extension is part of a four-year program that aims at including in the ISC-GEM catalogue large global earthquakes that occurred before the beginning of the ISC Bulletin in 1964. In this contribution we present the updated ISC GEM catalogue, which will include over 1000 more earthquakes that occurred in 2010 2011 and several hundreds more between 1950 and 1959. The catalogue extension between 1935 and 1949 is currently underway. The extension of the ISC-GEM catalogue will also be helpful for regional cross border seismic hazard studies as the ISC-GEM catalogue should be used as basis for cross-checking the consistency in location and magnitude of those earthquakes listed both in the ISC GEM global catalogue and regional catalogues.

  7. Astrometric Star Catalogues as Combination of Hipparcos/Tycho Catalogues with Ground-Based Observations

    NASA Astrophysics Data System (ADS)

    Vondrak, J.

    The successful ESA mission Hipparcos provided very precise parallaxes, positions and proper motions of many stars in optical wavelength. Therefore, it is a primary representation of International Celestial Reference System in this wavelength. However, the shortness of the mission (less than four years) causes some problems with proper motions of the stars that are double or multiple. Therefore, a combination of the positions measured by Hipparcos satellite with ground-based observations with much longer history provides a better reference frame that is more stable in time. Several examples of such combinations are presented (ACT, TYCHO-2, FK6, GC+HIP, TYC2+HIP, ARIHIP) and briefly described. The stress is put on the most recent Earth Orientation Catalogue (EOC) that uses about 4.4 million optical observations of latitude/universal time variations (made during the twentieth century at 33 observatories in Earth orientation programmes), in combination with some of the above mentioned combined catalogues. The second version of the new catalogue EOC-2 contains 4418 objects, and the precision of their proper motions is far better than that of Hipparcos Catalogue.

  8. "The Midnight Judges Ride Again": Marbury v. Madison. Mock Trial Prepared for Classroom Use.

    ERIC Educational Resources Information Center

    Price, Mary A.

    The goal of this mock trial is to dramatize the Federalists' struggle to strengthen their control over the judicial branch of the U.S. government after losing the Presidency and Congress in the 1800 election. This mock trial reveals the personalities of key historical figures, such as Jefferson, Madison, and Marshall and distinguishes how they…

  9. Introducing Preservice Teachers to Issues Surrounding Evolution and Creationism via a Mock Trial.

    ERIC Educational Resources Information Center

    Helgeson, Lars J.; Hoover, John; Sheehan, James

    2002-01-01

    Describes cooperation between social studies and science education professors to introduce preservice teachers to the evolution versus creationism debate via a mock trial. Uses a hypothetical situation in which a 6th grade teacher was fired for not balancing evolution and creationism in his teaching. Reports that the mock trial slightly increased…

  10. Citizenship Education in Michigan Schools: A Mock Election and Political Awareness Resource Guide. Secondary Level.

    ERIC Educational Resources Information Center

    Michigan State Board of Education, Lansing.

    An eight-chapter resource guide helps high school students become actively involved in the presidential election process. Chapter 1 contains directions for student participation in the 1984 Michigan statewide mock election; these directions are easily adaptable to other state and local mock election projects. Included are sample voter application…

  11. Employing a Mock Trial in a Criminology Course: An Applied Learning Experience.

    ERIC Educational Resources Information Center

    Shepelak, Norma J.

    1996-01-01

    Recounts a criminology class exercise that consisted of staging a mock trial using the murders from Truman Capote's "In Cold Blood" as source material. Students research the case and role play various lawyers, jury members, and witnesses. Identifies and discusses four educational objectives attainable through the staging of mock trials. (MJP)

  12. Mock Trials versus Management or Litigation-Driven Models of Business Law Instruction

    ERIC Educational Resources Information Center

    Gershuny, Pamela; McAllister, Charles; Rainey, Carolyn

    2012-01-01

    This study was designed to gain a greater understanding of the learning outcomes associated with the mock trial as an active teaching method. Participating in a product liability mock trial presents students with the complex interplay of administrative regulations and common law. As in real life, the harsh constraints of time pressures, less than…

  13. Statement of Facts for 1994 City-Wide Mock Trial Competitions. Scott Walker v. Tanya Brewster.

    ERIC Educational Resources Information Center

    National Inst. for Citizen Education in the Law, Washington, DC.

    Prepared by the District of Columbia Street Law Project for its 23rd annual city-wide mock trial competition, this instructional handout provides the material for a mock civil trial over an accidental shooting. Thirteen-year-old T. J. Walker, Scott Walker's son from a previous marriage, visited the home of 5-year-old Jesse Walker with a pistol…

  14. The Rhetoric of Mock Trial Debate: Using Logos, Pathos and Ethos in Undergraduate Competition

    ERIC Educational Resources Information Center

    Walker, Felicia R.

    2005-01-01

    While engaging in learning about roles of evidence, rules of procedure and case law, undergraduate mock trial students must also learn how to effectively communicate their evidence to the fact-finder. In mock trial, as in real courtroom trials in the United States legal system, communication skills and the ability to persuade are essential. This…

  15. The Palermo Swift-BAT hard X-ray catalogue. III. Results after 54 months of sky survey

    NASA Astrophysics Data System (ADS)

    Cusumano, G.; La Parola, V.; Segreto, A.; Ferrigno, C.; Maselli, A.; Sbarufatti, B.; Romano, P.; Chincarini, G.; Giommi, P.; Masetti, N.; Moretti, A.; Parisi, P.; Tagliaferri, G.

    2010-12-01

    Aims: We present the Second Palermo Swift-BAT hard X-ray catalogue obtained by analysing data acquired in the first 54 months of the Swift mission. Methods: Using our software dedicated to the analysis of data from coded mask telescopes, we analysed the BAT survey data in three energy bands (15-30 keV, 15-70 keV, 15-150 keV), obtaining a list of 1256 detections above a significance threshold of 4.8 standard deviations. The identification of the source counterparts is pursued using two strategies: the analysis of field observations of soft X-ray instruments and cross-correlation of our catalogue with source databases. Results: The survey covers 50% of the sky to a 15-150 keV flux limit of 1.0×10-11 erg cm-2 s-1 and 9.2×10-12 erg cm-2 s-1 for |b| < 10° and |b| > 10°, respectively. The Second Palermo Swift-BAT hard X-ray catalogue includes 1079 (~86%) hard X-ray sources with an associated counterpart (26 with a double association and 2 with a triple association) and 177 BAT excesses (~14%) that still lack a counterpart. The distribution of the BAT sources among the different object classes consists of ~19% Galactic sources, ~57% extragalactic sources, and ~10% sources with a counterpart at softer energies whose nature has not yet been determined. About half of the BAT associated sources lack a counterpart in the ROSAT catalogues. This suggests that either moderate or strong absorption may be preventing their detection in the ROSAT energy band. The comparison of our BAT catalogue with the Fermi Large Area Telescope First Source Catalogue identifies 59 BAT/Fermi correspondences: 48 blazars, 3 Seyfert galaxies, 1 interacting galaxy, 3 high mass X-ray binaries, and 4 pulsars/supernova remnants. This small number of correspondences indicates that different populations make the sky shine in these two different energy bands. Catalogue is also available in electronic firm at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc

  16. Discussion for the systematic differences of GC and SAOC catalogues.

    NASA Astrophysics Data System (ADS)

    Lu, Peizhen; Xu, Tongqi

    With the calculation method of Bien et al. describing systematic differences, the systematic differences of the GC and SAOC catalogues relating to the FK5 catalogue were calculated. The results were compared with that of the GC through the FK4 catalogue as a reference catalogue. It shows if there are more common stars, the results of two methods are coincident in the main. The systematic differences of SAOC and those of AGK3 and Perth70 were also compared. The results are consistent except in the range near the celestial pole.

  17. A new catalogue of eclipsing binary stars with eccentric orbits

    NASA Astrophysics Data System (ADS)

    Bulut, I.; Demircan, O.

    2007-06-01

    A new catalogue of eclipsing binary stars with eccentric orbits is presented. The catalogue lists the physical parameters (including apsidal motion parameters) of 124 eclipsing binaries with eccentric orbits. In addition, the catalogue also contains a list of 150 candidate systems, about which not much is known at present. Full version of the catalogue is available online (see the Supplementary Material section at the end of this paper) and in electronic form at the CDS via http://cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/MNRAS/(vol)/ (page) E-mail: ibulut@comu.edu.tr

  18. Catalogues of variable stars from Parenago to the present day

    NASA Astrophysics Data System (ADS)

    Samus, N. N.

    2006-04-01

    After World War II, the International Astronomical Union made Soviet astronomers responsible for variable-star catalogues. This work has been continued ever since the first edition of the General Catalogue of Variable Stars compiled by the team headed by P.P. Parenago and B.V. Kukarkin and published in 1948. Currently, the catalogue work is a joint project of the Institute of Astronomy (Russian Academy of Sciences) and the Sternberg Astronomical Institute (Moscow University). This paper is a brief review of recent trends in the field of variable-star catalogues. Problems as well as new prospects related to modern large-scale automatic photometric sky surveys are discussed.

  19. Characterization of flaws in a tube bundle mock-up for reliability studies

    SciTech Connect

    Kupperman, D.S.; Bakhtiari, S.

    1997-02-01

    As part of an assessment of in-service inspection of steam generator tubes, the authors will assemble a steam generator mock-up for round robin studies and use as a test bed in evaluating emerging technologies. Progress is reported on the characterization of flaws that will be part of the mock-up. Eddy current and ultrasonic techniques are being evaluated as a means to characterize the flaws in the mock-up tubes before final assembly. Twenty Inconel 600 tubes with laboratory-grown cracks, typical of those to be used in the mock-up, were provided by Pacific Northwest National Laboratory for laboratory testing. After the tubes were inspected with eddy current and ultrasonic techniques, they were destructively analyzed to establish the actual depths, lengths, and profiles of the cracks. The analysis of the results will allow the best techniques to be used for characterizing the flaws in the mock-up tubes.

  20. Photometric stellar catalogue for TV meteor astronomy

    NASA Astrophysics Data System (ADS)

    Leonov, V. A.; Bagrov, A. V.

    2016-01-01

    Photometry for ordinary astrophysics was carefully developed for its own purposes. As stars radiation is very similar to the blackbody radiation, astronomers measure star illumination in wide or narrow calibrated spectral bands. This is enough for star photometry with precise accuracy and for measuring their light flux in these bands in energetic units. Meteors are moving objects and do not allow collection of more photons then they emit. So meteor observers use the whole spectral band that can be covered by sensitivity of their light sensors. This is why measurements of stellar magnitudes of background stars by these sensors are not the same as catalogued star brightness in standard photometric spectral bands. Here we present a special photometric catalogue of 93 bright non-variable stars of the northern hemisphere, that can be used by meteor observers of standard background whose brightness are calculated in energetic units as well as in non-systematic stellar magnitudes in spectral wavelength of the WATEC 902 sensitivity.

  1. Pan-European catalogue of flood events

    NASA Astrophysics Data System (ADS)

    Parajka, Juraj; Mangini, Walter; Viglione, Alberto; Hundecha, Yeshewatesfa; Ceola, Serena

    2016-04-01

    There have been numerous extreme flood events observed in Europe in the past years. One of the way to improve our understanding about causing flood generation mechanisms is to analyse spatial and temporal variability of a large number of flood events. The aim of this study is to present a pan-European catalogue of flood events developed within the SWITCH-ON EU Project. The flood events are identified from daily discharge observations at 1315 stations listed in Global Runoff Data Centre database. The average length of discharge time-series for selected stations is 54 years. For each event, basin boundary and additional hydrological and weather characteristics are extracted. Hydrological characteristics are extracted from the pan-European HYPE model simulations. Precipitation, together with the corresponding proportions of rainfall and snowfall, snowmelt, and evapotranspiration are computed as total amounts between the event start date and event peak date. Soil moisture, soil moisture deficit, and basin accumulated snow water equivalent are computed for the event start date. Weather characteristics are derived from the weather circulation pattern catalogue developed within COST 733 Project. The results are generated in an open data access and tools framework which allows reproduction and extension of results to other regions. More information about the analysis and project are available at: http://www.water-switch-on.eu/lab.html.

  2. HELCATS - Heliospheric Cataloguing, Analysis and Techniques Service

    NASA Astrophysics Data System (ADS)

    Barnes, D.; Harrison, R. A.; Davies, J. A.; Byrne, J.; Perry, C. H.; Moestl, C.; Rouillard, A. P.; Bothmer, V.; Rodriguez, L.; Eastwood, J. P.; Kilpua, E.; Odstrcil, D.; Gallagher, P.

    2015-12-01

    Understanding the evolution of the solar wind is fundamental to advancing our knowledge of energy and mass transport in the Solar System, making it crucial to space weather and its prediction. The advent of truly wide-angle heliospheric imaging has revolutionised the study of both transient (CMEs) and background (IRs) solar wind plasma structures, by enabling their direct and continuous observation out to 1 AU and beyond. The EU-funded FP7 HELCATS project combines European expertise in heliospheric imaging, built up in particular through lead involvement in NASA's STEREO mission, with expertise in solar and coronal imaging as well as in-situ and radio measurements of solar wind phenomena, in a programme of work that will enable a much wider exploitation and understanding of heliospheric imaging observations. The HELCATS project endeavors to catalogue transient and background solar wind structures imaged by STEREO/HI throughout the duration of the mission. This catalogue will include estimates of their kinematic properties using a variety of established and more speculative approaches, which are to be evaluated through comparisons with solar source and in-situ measurements. The potential for driving numerical models from these kinematic properties is to be assessed, as is their complementarity to radio observations, specifically Type II bursts and interplanetary scintillation. This presentation provides an overview of the HELCATS project and its progress in first 18 months of operations.

  3. Radio luminosity function of brightest cluster galaxies

    NASA Astrophysics Data System (ADS)

    Yuan, Z. S.; Han, J. L.; Wen, Z. L.

    2016-08-01

    By cross-matching the currently largest optical catalogue of galaxy clusters and the NVSS radio survey data base, we obtain a large complete sample of brightest cluster galaxies (BCGs) in the redshift range of 0.05 < z ≤ 0.45, which have radio emission and redshift information. We confirm that more powerful radio BCGs tend to be these optically very bright galaxies located in more relaxed clusters. We derived the radio luminosity functions of the largest sample of radio BCGs, and find that the functions depend on the optical luminosity of BCGs and the dynamic state of galaxy clusters. However, the radio luminosity function does not show significant evolution with redshift.

  4. Brightest Cluster Galaxies and Dry Mergers

    NASA Astrophysics Data System (ADS)

    Deng, Z. G.; Liu, F. S.; Xia, X. Y.; Mao, S.

    2008-01-01

    Photometric properties of the early type Brightest Cluster Galaxies (BCGs) has been investigated for a sample of 85 BCGs with redshifts less than 0.1 selected from the C4 cluster catalogue. The results are compared to those obtained from a sample of elliptical galaxies chosen with similar apparent magnitude and redshift ranges. We find that BCGs have steeper size-luminosity (R~Lα) and Faber-Jackson (L~σβ) relations than the bulk of early type galaxies. The differences in the scaling relations suggest that the dynamical structure and formation route of BCGs may be different from the bulk of early type galaxies, in particular dry (dissipationless) mergers may play a more important role in their formation.

  5. The ASTRODEEP Frontier Fields catalogues. I. Multiwavelength photometry of Abell-2744 and MACS-J0416

    NASA Astrophysics Data System (ADS)

    Merlin, E.; Amorín, R.; Castellano, M.; Fontana, A.; Buitrago, F.; Dunlop, J. S.; Elbaz, D.; Boucaud, A.; Bourne, N.; Boutsia, K.; Brammer, G.; Bruce, V. A.; Capak, P.; Cappelluti, N.; Ciesla, L.; Comastri, A.; Cullen, F.; Derriere, S.; Faber, S. M.; Ferguson, H. C.; Giallongo, E.; Grazian, A.; Lotz, J.; Michałowski, M. J.; Paris, D.; Pentericci, L.; Pilo, S.; Santini, P.; Schreiber, C.; Shu, X.; Wang, T.

    2016-05-01

    Context. The Frontier Fields survey is a pioneering observational program aimed at collecting photometric data, both from space (Hubble Space Telescope and Spitzer Space Telescope) and from ground-based facilities (VLT Hawk-I), for six deep fields pointing at clusters of galaxies and six nearby deep parallel fields, in a wide range of passbands. The analysis of these data is a natural outcome of the Astrodeep project, an EU collaboration aimed at developing methods and tools for extragalactic photometry and creating valuable public photometric catalogues. Aims: We produce multiwavelength photometric catalogues (from B to 4.5 μm) for the first two of the Frontier Fields, Abell-2744 and MACS-J0416 (plus their parallel fields). Methods: To detect faint sources even in the central regions of the clusters, we develop a robust and repeatable procedure that uses the public codes Galapagos and Galfit to model and remove most of the light contribution from both the brightest cluster members, and the intra-cluster light. We perform the detection on the processed HST H160 image to obtain a pure H-selected sample, which is the primary catalogue that we publish. We also add a sample of sources which are undetected in the H160 image but appear on a stacked infrared image. Photometry on the other HST bands is obtained using SExtractor, again on processed images after the procedure for foreground light removal. Photometry on the Hawk-I and IRAC bands is obtained using our PSF-matching deconfusion code t-phot. A similar procedure, but without the need for the foreground light removal, is adopted for the Parallel fields. Results: The procedure of foreground light subtraction allows for the detection and the photometric measurements of ~2500 sources per field. We deliver and release complete photometric H-detected catalogues, with the addition of the complementary sample of infrared-detected sources. All objects have multiwavelength coverage including B to H HST bands, plus K

  6. Automatic Detection of Galaxy Groups by Probabilistic Hough Transform

    NASA Astrophysics Data System (ADS)

    Ibrahem, R. T.; Tino, P.; Pearson, R. J.; Ponman, T. J.; Babul, A.

    2015-12-01

    Galaxy groups play a significant role in explaining the evolution of the universe. Given the amounts of available survey data, automated discovery of galaxy groups is of utmost interest. We introduce a novel methodology, based on probabilistic Hough transform, for finding galaxy groups embedded in a rich background. The model takes advantage of a typical signature pattern of galaxy groups known as "fingers-of-God". It also allows us to include prior astrophysical knowledge as an inherent part of the method. The proposed method is first tested in large scale controlled experiments with 2-D patterns and then verified on 3-D realistic mock data (comparing with the well-known friends-of-friends method used in astrophysics). The experiments suggest that our methodology is a promising new candidate for galaxy group finders developed within a machine learning framework.

  7. Modern Special Collections Cataloguing: A University of London Case Study

    ERIC Educational Resources Information Center

    Attar, K. E.

    2013-01-01

    Recent years have seen a growing emphasis on modern special collections (in themselves no new phenomenon), with a dichotomy between guidance for detailed cataloguing in "Descriptive Cataloging of Rare Materials (Books)" (DCRM(B), 2007) and the value of clearing cataloguing backlogs expeditiously. This article describes the De la Mare Family…

  8. VizieR Online Data Catalog: MHO Catalogue (Davis+, 2010)

    NASA Astrophysics Data System (ADS)

    Davis, C. J.; Gell, R.; Khanzadyan, T.; Smith, M. D.; Jenness, T.

    2010-02-01

    The catalogue contains almost 1000 objects and covers regions on the sky loosely based on the constellations and associated Giant Molecular Clouds (Perseus, Orion A, Orion B, Taurus, etc.); full details are given in the paper. Note also that this catalogue is being maintained (and updated) at a dedicated, search-able website: http://www.jach.hawaii.edu/UKIRT/MHCat/ (2 data files).

  9. The VIPERS Multi-Lambda Survey. I. UV and near-IR observations, multi-colour catalogues, and photometric redshifts

    NASA Astrophysics Data System (ADS)

    Moutard, T.; Arnouts, S.; Ilbert, O.; Coupon, J.; Hudelot, P.; Vibert, D.; Comte, V.; Conseil, S.; Davidzon, I.; Guzzo, L.; Llebaria, A.; Martin, C.; McCracken, H. J.; Milliard, B.; Morrison, G.; Schiminovich, D.; Treyer, M.; Van Werbaeke, L.

    2016-05-01

    We present observations collected in the CFHTLS-VIPERS region in the ultraviolet with the GALEX satellite (far- and near-ultraviolet channels) and in the near-infrared with the CFHT/WIRCam camera (Ks band) over an area of 22 and 27 deg2, respectively. The depth of the photometry was optimised to measure the physical properties (e.g., star formation rate, stellar masses) of all the galaxies in the VIPERS spectroscopic survey. The large volume explored by VIPERS will enable a unique investigation of the relationship between the galaxy properties and their environment (density field and cosmic web) at high redshift (0.5 ≤ z ≤ 1.2). In this paper, we present the observations, the data reductions, and the build-up of the multi-colour catalogues. The CFHTLS-T0007 (gri-χ2) images are used as reference to detect and measure the Ks-band photometry, while the T0007 u∗-selected sources are used as priors to perform the GALEX photometry based on a dedicated software (EMphot). Our final sample reaches NUVAB ~ 25 (at 5σ) and KAB ~ 22 (at 3σ). The large spectroscopic sample (~51 000 spectroscopic redshifts) allows us to highlight the robustness of our star/galaxy separation and the reliability of our photometric redshifts with a typical accuracy of σz ≤ 0.04 and a fraction of catastrophic failures η ≤ 2% down to i ~ 23. We present various tests on the Ks-band completeness and photometric redshift accuracy by comparing our results with existing overlapping deep photometric catalogues. Finally, we discuss the BzK sample of passive and active galaxies at high redshift and the evolution of galaxy morphology in the (NUV-r) vs. (r-Ks) diagram at low redshift (z ≤ 0.25) based on the high image quality of the CFHTLS. The catalogue is available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/590/A102The images, catalogues, and photometric redshifts for 1.5 million sources (down to NUV

  10. Value of Hipparcos Catalogue shown by planet assessments

    NASA Astrophysics Data System (ADS)

    1996-08-01

    now have privileged use of the data for nearly a year, before the release of the catalogues to the world-wide astronomical community in April 1997. The new precision in star-fixing promises an extraordinary harvest of new results, on subjects ranging from asteroids to cosmology. A vivid picture of the stars in motion in our corner of the Milky Way Galaxy is one expected outcome. Hipparcos has more than doubled the number of known variable stars, and has discovered many thousands of new double or multiple star systems. Striding the light-years by parallax The study of stars with candidate planets is a dramatic example of Hipparcos's new determinations of the distances of stars by the parallax principle. Many other discoveries will flow from it. Parallax is an unfamiliar name for a familiar concept, akin to stereoscopic vision. People judge distances in nearby scenes from the difference in direction of the two eyes when focused on an object. Military rangefinders use the same principle, with more widely separated optics. Astronomers adapt the Earth's orbit to make a huge rangefinder. At opposite seasons, the Earth is on opposite sides of the Sun, at vantage points 300 million kilometres apart. As a result, the bearings of stars change a little. Nearby stars shift more than very distant stars, and astronomers can measure their distances by trigonometry. Until now, unavoidable inaccuracies in observing the directions of stars from the ground have meant that the distances of only the closest stars can be measured directly by parallax, out to about 100 light-years. Even at short ranges the margin of uncertainty is often wide. Long chains of inference and observation extend the distance scale to much farther objects, including galaxies millions or billions of light-years away. From the resulting estimates, astronomers try to calculate the age of the Universe and arrive at conclusions about its origin and evolution. The foundation for these reckonings has been decidedly shaky

  11. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations in Fourier-space

    DOE PAGES

    Beutler, Florian; Seo, Hee -Jong; Ross, Ashley J.; McDonald, Patrick; Saito, Shun; Bolton, Adam S.; Joel R. Brownstein; Chuang, Chia -Hsun; Cuesta, Antonio J.; Eisenstein, Daniel J.; et al

    2016-07-13

    Here, we analyse the Baryon Acoustic Oscillation (BAO) signal of the final Baryon Oscillation Spectroscopic Survey (BOSS) data release (DR12). Our analysis is performed in Fourier-space, using the power spectrum monopole and quadrupole. The dataset includes 1 198 006 galaxies over the redshift range 0.2 < z < 0.75. We divide this dataset into three (overlapping) redshift bins with the effective redshifts zeff = 0.38, 0.51 and 0.61. We demonstrate the reliability of our analysis pipeline using N-body simulations as well as 1000 MultiDark-Patchy mock catalogues, which mimic the BOSS-DR12 target selection. We apply density eld reconstruction to enhance themore » BAO signal-to-noise ratio. By including the power spectrum quadrupole we can sep-arate the line-of-sight and angular modes, which allows us to constrain the angular diameter distance DA(z) and the Hubble parameter H ( z ) separately. We obtain two independent 1 : 6% and 1 : 5% constraints on DA(z) and 2.9% and 2.3% constraints on H(z) for the low (zeff = 0.38) and high (zeff = 0.61) redshift bin, respectively. We obtain two independent 1% and 0.9% constraints on the angular averaged distance DV(z), when ignoring the Alcock-Paczynski e ect. The detection significance of the BAO signal is of the order of 8σ (post-reconstruction) for each of the three redshift bins. Our results are in good agreement with the Planck prediction within CDM. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. (2016) to produce the final cosmological constraints from BOSS.« less

  12. The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations in Fourier-space

    NASA Astrophysics Data System (ADS)

    Beutler, Florian; Seo, Hee-Jong; Ross, Ashley J.; McDonald, Patrick; Saito, Shun; Bolton, Adam S.; Brownstein, Joel R.; Chuang, Chia-Hsun; Cuesta, Antonio J.; Eisenstein, Daniel J.; Font-Ribera, Andreu; Grieb, Jan Niklas; Hand, Nick; Kitaura, Francisco-Shu; Modi, Chirag; Nichol, Robert C.; Percival, Will J.; Prada, Francisco; Rodriguez-Torres, Sergio; Roe, Natalie A.; Ross, Nicholas P.; Salazar-Albornoz, Salvador; Sánchez, Ariel G.; Schneider, Donald P.; Slosar, Anže; Tinker, Jeremy; Tojeiro, Rita; Vargas-Magaña, Mariana; Vazquez, Jose A.

    2016-09-01

    We analyse the Baryon Acoustic Oscillation (BAO) signal of the final Baryon Oscillation Spectroscopic Survey (BOSS) data release (DR12). Our analysis is performed in Fourier-space, using the power spectrum monopole and quadrupole. The dataset includes 1 198 006 galaxies over the redshift range 0.2 < z < 0.75. We divide this dataset into three (overlapping) redshift bins with the effective redshifts zeff = 0.38, 0.51 and 0.61. We demonstrate the reliability of our analysis pipeline using N-body simulations as well as ˜1000 MultiDark-Patchy mock catalogues, which mimic the BOSS-DR12 target selection. We apply density field reconstruction to enhance the BAO signal-to-noise ratio. By including the power spectrum quadrupole we can separate the line-of-sight and angular modes, which allows us to constrain the angular diameter distance DA(z) and the Hubble parameter H(z) separately. We obtain two independent 1.6% and 1.5% constraints on DA(z) and 2.9% and 2.3% constraints on H(z) for the low (zeff = 0.38) and high (zeff = 0.61) redshift bin, respectively. We obtain two independent 1% and 0.9% constraints on the angular averaged distance DV(z), when ignoring the Alcock-Paczynski effect. The detection significance of the BAO signal is of the order of 8σ (post-reconstruction) for each of the three redshift bins. Our results are in good agreement with the Planck prediction within ΛCDM. This paper is part of a set that analyses the final galaxy clustering dataset from BOSS. The measurements and likelihoods presented here are combined with others in Alam et al. (2016) to produce the final cosmological constraints from BOSS.

  13. Properties of an H I-selected galaxy sample

    NASA Technical Reports Server (NTRS)

    Szomoru, Arpad; Guhathakurta, Puragra; Van Gorkom, Jacqueline H.; Knapen, Johan H.; Weinberg, David H.; Fruchter, Andrew S.

    1994-01-01

    We analyze the properties of a sample of galaxies identified in a 21cm, H I-line survey of selected areas in the Perseus-Pisces supercluster and its foreground void. Twelve fields were observed in the supercluster, five of them (target fields) centered on optically bright galaxies, and the other seven (blank fields) selected to contain no bright galaxies within 45 min. of their centers. We detected nine previously uncatalogued, gas-rich galaxies, six of them in the target fields. We also detected H I from seven previously catalogued galaxies in these fields. Observations in the void covered the same volume as the 12 supercluster fields at the same H I-mass sensitivity, but no objects were detected. Combining out H I data with optical broadband and H alpha imaging, we conclude that the properties of H I-selected galaxies do not differ substantially from those of late-type galaxies found in optical surveys. In particular, the galaxies in our sample do not appear to be unusually faint for their H I mass, or for their circular velocity. We find tentative evidence for a connection between optical surface brightness and degree of isolation, in the sense that low surface brightness galaxies tend to be more isolated. The previously catalogued, optically bright galaxies in our survey volume dominate the total H I mass density and cross section; the uncatalogued galaxies contribute only approximately 19 percent of the mass and approximately 12 percent of the cross section. Thus, existing estimates of the density and cross section of neutral hydrogen, most of which are based on optically selected galaxy samples, are probably accurate. Such estimates can be used to compare the nearby universe to the high-redshift universe probed by quasar absorption lines.

  14. Thin slice expert testimony and mock trial deliberations.

    PubMed

    Parrott, Caroline Titcomb; Brodsky, Stanley L; Wilson, Jennifer Kelly

    2015-01-01

    This study examined impressions of expert witness testimony in a not guilty by reason of insanity defense on two outcomes: witness's credibility and verdict. Borrowing in part from the "thin slice" methodology, we assessed outcomes in a 2 (deliberating vs. non-deliberating jurors) × 3 (length of videotaped testimony) between-subjects design. In 30 mock juries, 188 participants viewed the testimony by a forensic psychologist; then half of the juries deliberated. Thinner slices of the testimony were defined by the lower (30s long) and upper (5 min long) temporal bounds in the literature. The third, fuller testimony condition was 10 min long and served as the accuracy marker for the shorter sliced exposures. We aimed to explore potential consequences to jurors relying on impressions of the expert, and his or her opinion, and to test that effect post deliberation. Accounting for deliberation, brief impressions of expert credibility generally exerted a similar influence on credibility to fuller considerations. The essential finding was that a two-way interaction emerged from time slice and deliberation on verdict for jurors in the 30s condition. Overall, predictive accuracy was found in the 5 min slice, yet accuracy was not supported in the predictions based on the shortest slice. Individually-formed impressions are not likely to translate to the verdict ballot post-deliberation. Instead, brief impressions are likely to be heavily influenced by deliberation. Implications for understanding how impression-based testimony evaluations translate from the jury box to the deliberation room are discussed.

  15. Apex high-altitude research sailplane mock-up

    NASA Technical Reports Server (NTRS)

    1995-01-01

    This photo shows a mock-up of the Apex high-altitude research sailplane intended to be carried aloft by a balloon. The Apex High-Altitude Flight Experiment is expected to explore the aerodynamics of controlled flight at very high altitudes near 100,000 feet. The Apex will be hoisted aloft tail-first from Dryden by a large high-altitude balloon and released at about 110,000-feet altitude. As it gradually descends, its instrumentation will collect aerodynamic data. The remotely-piloted, semi-autonomous Apex will combine a modified ASC sailplane fuselage design with a new wing designed at the Massachusetts Institute of Technology. The wing will have a special airfoil designed for high subsonic speeds at extreme altitudes. A device extending behind the right wing is a 'wake rake,' which will measure aerodynamic drag behind a test section of the wing, while a rocket pack mounted beneath the fuselage will assist the Apex in transitioning to horizontal flight. Research flights were expected to begin in mid-1998, but a series of technical problems delayed them. In the spring of 1999, Apex entered mothball status. This continued for a year, and in the spring of 2000 NASA selected Apex as part of phase 1 of the Revolutionary Concepts effort.

  16. A simple, economical, and effective portable paediatric mock circulatory system.

    PubMed

    Vandenberghe, S; Shu, F; Arnold, D K; Antaki, J F

    2011-07-01

    Ventricular assist devices (VADs) and total artificial hearts have been in development for the last 50 years. Since their inception, simulators of the circulation with different degrees of complexity have been produced to test these devices in vitro. Currently, a new path has been taken with the extensive efforts to develop paediatric VADs, which require totally different design constraints. This paper presents the manufacturing details of an economical simulator of the systemic paediatric circulation. This simulator allows the insertion of a paediatric VAD, includes a pumping ventricle, and is adjustable within the paediatric range. Rather than focusing on complexity and physiological simulation, this simulator is designed to be simple and practical for rapid device testing. The simulator was instrumented with medical sensors and data were acquired under different conditions with and without the new PediaFlowTM paediatric VAD. The VAD was run at different impeller speeds while simulator settings such as vascular resistance and stroke volume were varied. The hydraulic performance of the VAD under pulsatile conditions could be characterized and the magnetic suspension could be tested via manipulations such as cannula clamping. This compact mock loop has proven to be valuable throughout the PediaFlow development process and has the advantage that it is uncomplicated and can be manufactured cheaply. It can be produced by several research groups and the results of different VADs can then be compared easily.

  17. A hybrid mock circulation loop for a total artificial heart.

    PubMed

    Nestler, Frank; Bradley, Andrew P; Wilson, Stephen J; Timms, Daniel L; Frazier, O Howard; Cohn, William E

    2014-09-01

    Rotary blood pumps are emerging as a viable technology for total artificial hearts, and the development of physiological control algorithms is accelerated with new evaluation environments. In this article, we present a novel hybrid mock circulation loop (HMCL) designed specifically for evaluation of rotary total artificial hearts (rTAH). The rTAH is operated in the physical domain while all vasculature elements are embedded in the numerical domain, thus combining the strengths of both approaches: fast and easy exchange of the vasculature model together with improved controllability of the pump. Parameters, such as vascular resistance, compliance, and blood volume, can be varied dynamically in silico during operation. A hydraulic-numeric interface creates a real-time feedback loop between the physical and numerical domains. The HMCL uses computer-controlled resistance valves as actuators, thereby reducing the size and number of hydraulic elements. Experimental results demonstrate a stable interaction over a wide operational range and a high degree of flexibility. Therefore, we demonstrate that the newly created design environment can play an integral part in the hydraulic design, control development, and durability testing of rTAHs. PMID:25234760

  18. Effects of neuroimaging evidence on mock juror decision making.

    PubMed

    Greene, Edith; Cahill, Brian S

    2012-01-01

    During the penalty phase of capital trials, defendants may introduce mitigating evidence that argues for a punishment "less than death." In the past few years, a novel form of mitigating evidence-brain scans made possible by technological advances in neuroscience-has been proffered by defendants to support claims that brain abnormalities reduce their culpability. This exploratory study assessed the impact of neuroscience evidence on mock jurors' sentencing recommendations and impressions of a capital defendant. Using actual case facts, we manipulated diagnostic evidence presented by the defense (psychosis diagnosis; diagnosis and neuropsychological test results; or diagnosis, test results, and neuroimages) and future dangerousness evidence presented by the prosecution (low or high risk). Recommendations for death sentences were affected by the neuropsychological and neuroimaging evidence: defendants deemed at high risk for future dangerousness were less likely to be sentenced to death when jurors had this evidence than when they did not. Neuropsychological and neuroimaging evidence also had mitigating effects on impressions of the defendant. We describe study limitations and pose questions for further research.

  19. Effects of neuroimaging evidence on mock juror decision making.

    PubMed

    Greene, Edith; Cahill, Brian S

    2012-01-01

    During the penalty phase of capital trials, defendants may introduce mitigating evidence that argues for a punishment "less than death." In the past few years, a novel form of mitigating evidence-brain scans made possible by technological advances in neuroscience-has been proffered by defendants to support claims that brain abnormalities reduce their culpability. This exploratory study assessed the impact of neuroscience evidence on mock jurors' sentencing recommendations and impressions of a capital defendant. Using actual case facts, we manipulated diagnostic evidence presented by the defense (psychosis diagnosis; diagnosis and neuropsychological test results; or diagnosis, test results, and neuroimages) and future dangerousness evidence presented by the prosecution (low or high risk). Recommendations for death sentences were affected by the neuropsychological and neuroimaging evidence: defendants deemed at high risk for future dangerousness were less likely to be sentenced to death when jurors had this evidence than when they did not. Neuropsychological and neuroimaging evidence also had mitigating effects on impressions of the defendant. We describe study limitations and pose questions for further research. PMID:22213023

  20. D3-instantons, mock theta series and twistors

    NASA Astrophysics Data System (ADS)

    Alexandrov, Sergei; Manschot, Jan; Pioline, Boris

    2013-04-01

    The D-instanton corrected hypermultiplet moduli space of type II string theory compactified on a Calabi-Yau threefold is known in the type IIA picture to be determined in terms of the generalized Donaldson-Thomas invariants, through a twistorial construction. At the same time, in the mirror type IIB picture, and in the limit where only D3-D1-D(-1)-instanton corrections are retained, it should carry an isometric action of the S-duality group SL(2, {Z} ). We prove that this is the case in the one-instanton approximation, by constructing a holomorphic action of SL(2, {Z} ) on the linearized twistor space. Using the modular invariance of the D4-D2-D0 black hole partition function, we show that the standard Darboux coordinates in twistor space have modular anomalies controlled by period integrals of a Siegel-Narain theta series, which can be canceled by a contact transformation generated by a holomorphic mock theta series.

  1. Commentary: Perception of remorse by mock jurors in a capital murder trial.

    PubMed

    Batista, Leonardo M; Myers, Wade

    2012-01-01

    The study by Corwin et al. adds to the emerging but limited data on the impact of defendant remorse on sentencing decisions. The authors studied verbal and nonverbal expressions of defendant remorse and whether they were perceived as remorseful by mock jurors. They found that incongruent verbal and nonverbal behavior, as well as mock jurors' willingness to approach emotional situations, resulted in more lenient sentences for defendants. An overarching and as yet unanswered validity concern regarding this line of research in general is whether the use of undergraduate mock jurors reliably models real jurors in actual courtroom settings.

  2. Gaussian covariance matrices for anisotropic galaxy clustering measurements

    NASA Astrophysics Data System (ADS)

    Grieb, Jan Niklas; Sánchez, Ariel G.; Salazar-Albornoz, Salvador; Dalla Vecchia, Claudio

    2016-04-01

    Measurements of the redshift-space galaxy clustering have been a prolific source of cosmological information in recent years. Accurate covariance estimates are an essential step for the validation of galaxy clustering models of the redshift-space two-point statistics. Usually, only a limited set of accurate N-body simulations is available. Thus, assessing the data covariance is not possible or only leads to a noisy estimate. Further, relying on simulated realizations of the survey data means that tests of the cosmology dependence of the covariance are expensive. With these points in mind, this work presents a simple theoretical model for the linear covariance of anisotropic galaxy clustering observations with synthetic catalogues. Considering the Legendre moments (`multipoles') of the two-point statistics and projections into wide bins of the line-of-sight parameter (`clustering wedges'), we describe the modelling of the covariance for these anisotropic clustering measurements for galaxy samples with a trivial geometry in the case of a Gaussian approximation of the clustering likelihood. As main result of this paper, we give the explicit formulae for Fourier and configuration space covariance matrices. To validate our model, we create synthetic halo occupation distribution galaxy catalogues by populating the haloes of an ensemble of large-volume N-body simulations. Using linear and non-linear input power spectra, we find very good agreement between the model predictions and the measurements on the synthetic catalogues in the quasi-linear regime.

  3. Star formation in quasar and active galaxy environments

    NASA Astrophysics Data System (ADS)

    Coldwell, Georgina V.; Lambas, Diego G.

    2003-09-01

    We use the 2dF public 100 K data release of galaxies and samples of quasars and active galaxies taken from the Véron-Cetty and Véron catalogue to study the nature of galaxies in the surroundings of active objects with redshifts in the range 0.1 < z < 0.2. We explore the distribution of neighbour 2dF galaxy spectral types, η, at different projected distances from the quasars and active galaxies with radial velocity difference ΔV= 500 km s-1. For comparison, we perform a similar analysis on the environment of typical galaxies in the 2dF catalogue, a sample of bright early-type galaxies, i.e. η < -1.4 and MbJ < -21, and also on a sample of 2dF galaxy groups. We find a higher relative fraction of emission-line galaxies, i.e. with 2dF spectral type indices η >3.5, in the vicinity of quasars and active galaxies compared to that in the neighbourhood of typical galaxies, bright early types and groups. This effect extends up to projected distance rp~ 1 h-1 Mpc for active galaxies and rp~ 3 h-1 Mpc for quasars. We also find a tendency for companion galaxies of quasars to be brighter than the neighbours of active galaxies within rp~ 3 h-1 Mpc. We estimate average star-formation rates for objects at different distances from quasars, active galaxies, galaxies and groups. We find a significantly higher star-formation activity within ~2.0 h-1 Mpc from quasars with respect to typical galaxies, which reinforces the idea that star formation is enhanced in the neighbourhood of quasars. Our tests with the group environment provide evidence against quasars being associated with groups. Also, our analysis of the neighbours of bright early types shows that although these galaxies are typical hosts of quasars, their companion galaxies are significantly different in terms of the star-formation activity.

  4. Catalogue of Meteor Showers and Storms in Korean History

    NASA Astrophysics Data System (ADS)

    Ahn, Sang-Hyeon

    2004-03-01

    We present a more complete and accurate catalogue of astronomical records for meteor showers and meteor storms appeared in primary official Korean history books, such as Samguk-sagi, Koryo-sa, Seungjeongwon-ilgi, and Choson-Wangjo-Sillok. So far the catalogue made by Imoto and Hasegawa in 1958 has been widely used in the international astronomical society. The catalogue is based on a report by Sekiguchi in 1917 that is mainly based on secondary history books. We observed that the catalogue has a number of errors in either dates or sources of the records. We have thoroughly checked the primary official history books, instead of the secondary ones, in order to make a corrected and extended catalogue. The catalogue contains 25 records of meteor storms, four records of intense meteor-showers, and five records of usual showers in Korean history. We also find that some of those records seem to correspond to some presently active meteor showers such as the Leonids, the Perseids, and the ¥ç-Aquarids-Orionids pair. However, a large number of those records do not correspond to such present showers. This catalogue we obtained can be useful for various astrophysical studies in the future.

  5. Grid computing enhances standards-compatible geospatial catalogue service

    NASA Astrophysics Data System (ADS)

    Chen, Aijun; Di, Liping; Bai, Yuqi; Wei, Yaxing; Liu, Yang

    2010-04-01

    A catalogue service facilitates sharing, discovery, retrieval, management of, and access to large volumes of distributed geospatial resources, for example data, services, applications, and their replicas on the Internet. Grid computing provides an infrastructure for effective use of computing, storage, and other resources available online. The Open Geospatial Consortium has proposed a catalogue service specification and a series of profiles for promoting the interoperability of geospatial resources. By referring to the profile of the catalogue service for Web, an innovative information model of a catalogue service is proposed to offer Grid-enabled registry, management, retrieval of and access to geospatial resources and their replicas. This information model extends the e-business registry information model by adopting several geospatial data and service metadata standards—the International Organization for Standardization (ISO)'s 19115/19119 standards and the US Federal Geographic Data Committee (FGDC) and US National Aeronautics and Space Administration (NASA) metadata standards for describing and indexing geospatial resources. In order to select the optimal geospatial resources and their replicas managed by the Grid, the Grid data management service and information service from the Globus Toolkits are closely integrated with the extended catalogue information model. Based on this new model, a catalogue service is implemented first as a Web service. Then, the catalogue service is further developed as a Grid service conforming to Grid service specifications. The catalogue service can be deployed in both the Web and Grid environments and accessed by standard Web services or authorized Grid services, respectively. The catalogue service has been implemented at the George Mason University/Center for Spatial Information Science and Systems (GMU/CSISS), managing more than 17 TB of geospatial data and geospatial Grid services. This service makes it easy to share and

  6. Can neutrino decay-driven mock gravity save hot dark matter?

    NASA Technical Reports Server (NTRS)

    Splinter, Randall J.; Melott, Adrian L.

    1992-01-01

    The radiative decay of a 30 eV neutrino with a lifetime of order 10 exp 23-24 s has recently been shown to yield a satisfactory explanation of a wide range of problems in astrophysics. In this paper, it is investigated whether the photon flux generated by the radiative decay of a massive neutrino is capable of generating sufficient radiation pressure to cause a 'mock gravitational' collapse of primordial hydrogen clouds. It is shown that when using neutral hydrogen as a source of opacity for mock gravity the time scale for mock gravitational collapse is significantly larger than the expansion time scale. Thus, the model fails as a source of galactic seed perturbations. Furthermore, it is argued that nonlinear feedback mechanisms will be unable to increase the collapse rate of the cloud under mock gravity.

  7. The Laniakea supercluster of galaxies.

    PubMed

    Tully, R Brent; Courtois, Hélène; Hoffman, Yehuda; Pomarède, Daniel

    2014-09-01

    Galaxies congregate in clusters and along filaments, and are missing from large regions referred to as voids. These structures are seen in maps derived from spectroscopic surveys that reveal networks of structure that are interconnected with no clear boundaries. Extended regions with a high concentration of galaxies are called 'superclusters', although this term is not precise. There is, however, another way to analyse the structure. If the distance to each galaxy from Earth is directly measured, then the peculiar velocity can be derived from the subtraction of the mean cosmic expansion, the product of distance times the Hubble constant, from observed velocity. The peculiar velocity is the line-of-sight departure from the cosmic expansion and arises from gravitational perturbations; a map of peculiar velocities can be translated into a map of the distribution of matter. Here we report a map of structure made using a catalogue of peculiar velocities. We find locations where peculiar velocity flows diverge, as water does at watershed divides, and we trace the surface of divergent points that surrounds us. Within the volume enclosed by this surface, the motions of galaxies are inward after removal of the mean cosmic expansion and long range flows. We define a supercluster to be the volume within such a surface, and so we are defining the extent of our home supercluster, which we call Laniakea.

  8. The Laniakea supercluster of galaxies.

    PubMed

    Tully, R Brent; Courtois, Hélène; Hoffman, Yehuda; Pomarède, Daniel

    2014-09-01

    Galaxies congregate in clusters and along filaments, and are missing from large regions referred to as voids. These structures are seen in maps derived from spectroscopic surveys that reveal networks of structure that are interconnected with no clear boundaries. Extended regions with a high concentration of galaxies are called 'superclusters', although this term is not precise. There is, however, another way to analyse the structure. If the distance to each galaxy from Earth is directly measured, then the peculiar velocity can be derived from the subtraction of the mean cosmic expansion, the product of distance times the Hubble constant, from observed velocity. The peculiar velocity is the line-of-sight departure from the cosmic expansion and arises from gravitational perturbations; a map of peculiar velocities can be translated into a map of the distribution of matter. Here we report a map of structure made using a catalogue of peculiar velocities. We find locations where peculiar velocity flows diverge, as water does at watershed divides, and we trace the surface of divergent points that surrounds us. Within the volume enclosed by this surface, the motions of galaxies are inward after removal of the mean cosmic expansion and long range flows. We define a supercluster to be the volume within such a surface, and so we are defining the extent of our home supercluster, which we call Laniakea. PMID:25186900

  9. The Laniakea supercluster of galaxies

    NASA Astrophysics Data System (ADS)

    Tully, R. Brent; Courtois, Hélène; Hoffman, Yehuda; Pomarède, Daniel

    2014-09-01

    Galaxies congregate in clusters and along filaments, and are missing from large regions referred to as voids. These structures are seen in maps derived from spectroscopic surveys that reveal networks of structure that are interconnected with no clear boundaries. Extended regions with a high concentration of galaxies are called `superclusters', although this term is not precise. There is, however, another way to analyse the structure. If the distance to each galaxy from Earth is directly measured, then the peculiar velocity can be derived from the subtraction of the mean cosmic expansion, the product of distance times the Hubble constant, from observed velocity. The peculiar velocity is the line-of-sight departure from the cosmic expansion and arises from gravitational perturbations; a map of peculiar velocities can be translated into a map of the distribution of matter. Here we report a map of structure made using a catalogue of peculiar velocities. We find locations where peculiar velocity flows diverge, as water does at watershed divides, and we trace the surface of divergent points that surrounds us. Within the volume enclosed by this surface, the motions of galaxies are inward after removal of the mean cosmic expansion and long range flows. We define a supercluster to be the volume within such a surface, and so we are defining the extent of our home supercluster, which we call Laniakea.

  10. Extended Source/Galaxy All Sky 1

    NASA Technical Reports Server (NTRS)

    2003-01-01

    This panoramic view of the entire sky reveals the distribution of galaxies beyond our Milky Way galaxy, which astronomers call extended sources, as observed by Two Micron All-Sky Survey. The image is constructed from a database of over 1.6 million galaxies listed in the survey's Extended Source Catalog; more than half of the galaxies have never before been catalogued. The image is a representation of the relative brightnesses of these million-plus galaxies, all observed at a wavelength of 2.2 microns.

    The brightest and nearest galaxies are represented in blue, and the faintest, most distant ones are in red. This color scheme gives insights into the three dimensional large-scale structure of the nearby universe with the brightest, closest clusters and superclusters showing up as the blue and bluish-white features. The dark band in this image shows the area of the sky where our Milky Way galaxy blocks our view of distant objects, which, in this projection, lies predominantly along the edges of the image.

  11. Photometric Properties of Galaxies in Poor Clusters

    NASA Astrophysics Data System (ADS)

    Sharma, M.; Prabhu, T.

    We study several statistical properties of galaxies in four poor clusters of galaxies using optical photometry. We select these poor clusters as luminous, extended X-ray sources identified with poor galaxy systems in the EMSS catalogue of clusters of galaxies. The clusters are at moderate redshifts (0.08galaxy populations are clearly evolved, as traced by the tightness of their color--magnitude relations and accordance of the latter with those of the Virgo Cluster. The fraction of blue galaxies is similar to those of low-redshift richness 0 clusters and higher than those of richer clusters at similar redshifts. The luminosity functions (LFs) of the individual clusters are not significantly different from each other. Using these, we construct composite LFs in B, V , and R bands (to MV=-18). The faint-end of these LFs are flat, like the V-band LF of other (e.g., MKW/AWM) poor clusters, but steeper than the field LF in the R-band. In terms of the statistical properties of their member galaxies, poor clusters appear to be lower-mass extensions of their rich counterparts.

  12. The Herschel-ATLAS data release 1 - I. Maps, catalogues and number counts

    NASA Astrophysics Data System (ADS)

    Valiante, E.; Smith, M. W. L.; Eales, S.; Maddox, S. J.; Ibar, E.; Hopwood, R.; Dunne, L.; Cigan, P. J.; Dye, S.; Pascale, E.; Rigby, E. E.; Bourne, N.; Furlanetto, C.; Ivison, R. J.

    2016-11-01

    We present the first major data release of the largest single key-project in area carried out in open time with the Herschel Space Observatory. The Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) is a survey of 600 deg2 in five photometric bands - 100, 160, 250, 350 and 500 μm - with the Photoconductor Array Camera and Spectrometer and Spectral and Photometric Imaging Receiver (SPIRE) cameras. In this paper and the companion Paper II, we present the survey of three fields on the celestial equator, covering a total area of 161.6 deg2 and previously observed in the Galaxy and Mass Assembly (GAMA) spectroscopic survey. This paper describes the Herschel images and catalogues of the sources detected on the SPIRE 250 μm images. The 1σ noise for source detection, including both confusion and instrumental noise, is 7.4, 9.4 and 10.2 mJy at 250, 350 and 500 μm. Our catalogue includes 120 230 sources in total, with 113 995, 46 209 and 11 011 sources detected at >4σ at 250, 350 and 500 μm. The catalogue contains detections at >3σ at 100 and 160 μm for 4650 and 5685 sources, and the typical noise at these wavelengths is 44 and 49 mJy. We include estimates of the completeness of the survey and of the effects of flux bias and also describe a novel method for determining the true source counts. The H-ATLAS source counts are very similar to the source counts from the deeper HerMES survey at 250 and 350 μm, with a small difference at 500 μm. Appendix A provides a quick start in using the released data sets, including instructions and cautions on how to use them.

  13. Moderate Velocity Ball Impact of a Mock High-Explosive

    SciTech Connect

    Furmanski, Jevan; Rae, Philip; Clements, Bradford E.

    2012-06-05

    Modeling of thermal and mechanical events in high-explosive materials is complicated by the composite nature of the material, which experiences viscoelastic and plastic deformations and sustains damage in the form of microcracks that can dominate its overall behavior. A mechanical event of interest is projectile interaction with the material, which leads to extreme local deformation and adiabatic heating, which can potentially lead to adverse outcomes in an energetic material. Simulations of such an event predicted large local temperature rises near the path of a spherical projectile, but these were experimentally unconfirmed and hence potentially non-physical. This work concerns the experimental verification of local temperatures both at the surface and in the wake of a spherical projectile penetrating a mock (unreactive) high-explosive at {approx}700 m/s. Fast response thermocouples were embedded radially in a mid-plane of a cylindrical target, which was bonded around the thermocouples with epoxy and recorded by an oscilloscope through a low-pass filter with a bandwidth of 500 Hz. A peak temperature rise of 70 K was measured both at the equator of the projectile and in its wake, in good agreement with the temperature predicted in the minimally distorted elements at those locations by a finite element model in ABAQUS employing the ViscoSCRAM constitutive model. Further work is needed to elucidate the extreme temperature rises in material undergoing crushing or fragmentation, which is difficult to predict with meshed finite element methods due to element distortion, and also challenging to quantify experimentally.

  14. Thin slice expert testimony and mock trial deliberations.

    PubMed

    Parrott, Caroline Titcomb; Brodsky, Stanley L; Wilson, Jennifer Kelly

    2015-01-01

    This study examined impressions of expert witness testimony in a not guilty by reason of insanity defense on two outcomes: witness's credibility and verdict. Borrowing in part from the "thin slice" methodology, we assessed outcomes in a 2 (deliberating vs. non-deliberating jurors) × 3 (length of videotaped testimony) between-subjects design. In 30 mock juries, 188 participants viewed the testimony by a forensic psychologist; then half of the juries deliberated. Thinner slices of the testimony were defined by the lower (30s long) and upper (5 min long) temporal bounds in the literature. The third, fuller testimony condition was 10 min long and served as the accuracy marker for the shorter sliced exposures. We aimed to explore potential consequences to jurors relying on impressions of the expert, and his or her opinion, and to test that effect post deliberation. Accounting for deliberation, brief impressions of expert credibility generally exerted a similar influence on credibility to fuller considerations. The essential finding was that a two-way interaction emerged from time slice and deliberation on verdict for jurors in the 30s condition. Overall, predictive accuracy was found in the 5 min slice, yet accuracy was not supported in the predictions based on the shortest slice. Individually-formed impressions are not likely to translate to the verdict ballot post-deliberation. Instead, brief impressions are likely to be heavily influenced by deliberation. Implications for understanding how impression-based testimony evaluations translate from the jury box to the deliberation room are discussed. PMID:26346686

  15. The ASTRODEEP Frontier Fields catalogues. II. Photometric redshifts and rest frame properties in Abell-2744 and MACS-J0416

    NASA Astrophysics Data System (ADS)

    Castellano, M.; Amorín, R.; Merlin, E.; Fontana, A.; McLure, R. J.; Mármol-Queraltó, E.; Mortlock, A.; Parsa, S.; Dunlop, J. S.; Elbaz, D.; Balestra, I.; Boucaud, A.; Bourne, N.; Boutsia, K.; Brammer, G.; Bruce, V. A.; Buitrago, F.; Capak, P.; Cappelluti, N.; Ciesla, L.; Comastri, A.; Cullen, F.; Derriere, S.; Faber, S. M.; Giallongo, E.; Grazian, A.; Grillo, C.; Mercurio, A.; Michałowski, M. J.; Nonino, M.; Paris, D.; Pentericci, L.; Pilo, S.; Rosati, P.; Santini, P.; Schreiber, C.; Shu, X.; Wang, T.

    2016-05-01

    Aims: We present the first public release of photometric redshifts, galaxy rest frame properties and associated magnification values in the cluster and parallel pointings of the first two Frontier Fields, Abell-2744 and MACS-J0416. The released catalogues aim to provide a reference for future investigations of extragalactic populations in these legacy fields: from lensed high-redshift galaxies to cluster members themselves. Methods: We exploit a multiwavelength catalogue, ranging from Hubble Space Telescope (HST) to ground-based K and Spitzer IRAC, which is specifically designed to enable detection and measurement of accurate fluxes in crowded cluster regions. The multiband information is used to derive photometric redshifts and physical properties of sources detected either in the H-band image alone, or from a stack of four WFC3 bands. To minimize systematics, median photometric redshifts are assembled from six different approaches to photo-z estimates. Their reliability is assessed through a comparison with available spectroscopic samples. State-of-the-art lensing models are used to derive magnification values on an object-by-object basis by taking into account sources positions and redshifts. Results: We show that photometric redshifts reach a remarkable ~3-5% accuracy. After accounting for magnification, the H-band number counts are found to be in agreement at bright magnitudes with number counts from the CANDELS fields, while extending the presently available samples to galaxies that, intrinsically, are as faint as H ~ 32-33, thanks to strong gravitational lensing. The Frontier Fields allow the galaxy stellar mass distribution to be probed, depending on magnification, at 0.5-1.5 dex lower masses with respect to extragalactic wide fields, including sources at Mstar ~ 107-108 M⊙ at z > 5. Similarly, they allow the detection of objects with intrinsic star formation rates (SFRs) >1 dex lower than in the CANDELS fields reaching 0.1-1 M⊙/yr at z ~ 6-10. The

  16. VizieR Online Data Catalog: XMMOMCDFS catalogue (Antonucci+, 2015)

    NASA Astrophysics Data System (ADS)

    Antonucci, M.; Talavera, A.; Vagnetti, F.; Trevese, D.; Comastri, A.; Paolillo, M.; Ranalli, P.; Vignali, C.

    2014-11-01

    We present the catalogue of the Optical Monitor observations performed by XMM-Newton in the Chandra Deep Field South during the XMM-CDFS Deep Survey (Comastri et al. 2011A&A...526L...9C). The main catalogue provides photometric measurements for 1129 CDFS sources from individual observations and/or from the stacked images, and includes optical/UV/X-ray photometric and spectroscopic information from other surveys. The supplementary catalogue contains 44 alternative XMM-OM identifications for 38 EIS/COMBO-17 sources. (2 data files).

  17. SIMULATED VOID GALAXIES IN THE STANDARD COLD DARK MATTER MODEL

    SciTech Connect

    Kreckel, Kathryn; Ryan Joung, M.; Cen Renyue

    2011-07-10

    We analyze a (120 h{sup -1} Mpc){sup 3} adaptive mesh refinement hydrodynamic simulation that contains a higher resolution 31 x 31 x 35 h{sup -3} Mpc subvolume centered on a {approx}30 Mpc diameter void. Our detailed {approx}1 kpc resolution allows us to identify 1300 galaxies within this void to a limiting halo mass of {approx}10{sup 10} M{sub sun}. Nearly 1000 galaxies are found to be in underdense regions, with 300 galaxies residing in regions less than half the mean density of the simulation volume. We construct mock observations of the stellar and gas properties of these systems and reproduce the range of colors and luminosities observed in the Sloan Digital Sky Survey for nearby (z < 0.03) galaxies. We find no trends with density for the most luminous (M{sub r} < -18) galaxies, however our dwarf void galaxies (M{sub r} > -16), though they are less reliably resolved, typically appear bluer, with higher rates of star formation and specific star formation and lower mean stellar ages than galaxies in average density environments. We find a significant population of low-luminosity (M{sub r} {approx} -14) dwarf galaxies that is preferentially located in low-density regions and specifically in the void center. This population may help to reduce, but not remove, the discrepancy between the predicted and observed number of void galaxies.

  18. LOFAR 150-MHz observations of the Boötes field: catalogue and source counts

    NASA Astrophysics Data System (ADS)

    Williams, W. L.; van Weeren, R. J.; Röttgering, H. J. A.; Best, P.; Dijkema, T. J.; de Gasperin, F.; Hardcastle, M. J.; Heald, G.; Prandoni, I.; Sabater, J.; Shimwell, T. W.; Tasse, C.; van Bemmel, I. M.; Brüggen, M.; Brunetti, G.; Conway, J. E.; Enßlin, T.; Engels, D.; Falcke, H.; Ferrari, C.; Haverkorn, M.; Jackson, N.; Jarvis, M. J.; Kapińska, A. D.; Mahony, E. K.; Miley, G. K.; Morabito, L. K.; Morganti, R.; Orrú, E.; Retana-Montenegro, E.; Sridhar, S. S.; Toribio, M. C.; White, G. J.; Wise, M. W.; Zwart, J. T. L.

    2016-08-01

    We present the first wide area (19 deg2), deep (≈120-150 μJy beam-1), high-resolution (5.6 × 7.4 arcsec) LOFAR High Band Antenna image of the Boötes field made at 130-169 MHz. This image is at least an order of magnitude deeper and 3-5 times higher in angular resolution than previously achieved for this field at low frequencies. The observations and data reduction, which includes full direction-dependent calibration, are described here. We present a radio source catalogue containing 6 276 sources detected over an area of 19 deg2, with a peak flux density threshold of 5σ. As the first thorough test of the facet calibration strategy, introduced by van Weeren et al., we investigate the flux and positional accuracy of the catalogue. We present differential source counts that reach an order of magnitude deeper in flux density than previously achieved at these low frequencies, and show flattening at 150-MHz flux densities below 10 mJy associated with the rise of the low flux density star-forming galaxies and radio-quiet AGN.

  19. Toward a molecular catalogue of synapses.

    PubMed

    Grant, Seth G N

    2007-10-01

    1906 was a landmark year in the history of the study of the nervous system, most notably for the first 'neuroscience' Nobel prize given to the anatomists Ramon Y Cajal and Camillo Golgi. 1906 is less well known for another event, also of great significance for neuroscience, namely the publication of Charles Sherrington's book 'The Integrative Action of the Nervous system'. It was Cajal and Golgi who debated the anatomical evidence for the synapse and it was Sherrington who laid its foundation in electrophysiological function. In tribute to these pioneers in synaptic biology, this article will address the issue of synapse diversity from the molecular point of view. In particular I will reflect upon efforts to obtain a complete molecular characterisation of the synapse and the unexpectedly high degree of molecular complexity found within it. A case will be made for developing approaches that can be used to generate a general catalogue of synapse types based on molecular markers, which should have wide application.

  20. Soft X-ray properties of a spectroscopically selected sample of interacting and isolated Seyfert galaxies

    NASA Astrophysics Data System (ADS)

    Pfefferkorn, F.; Boller, Th.; Rafanelli, P.

    2001-03-01

    We present a catalogue of ROSAT detected sources in the sample of spectroscopically selected Seyfert 1 and Seyfert 2 galaxies of Rafanelli et al. (\\cite{Rafanelli95}). The catalogue contains 102 Seyfert 1 and 36 Seyfert 2 galaxies. The identification is based on X-ray contour maps overlaid on optical images taken from the Digitized Sky Survey. We have derived the basic spectral and timing properties of the X-ray detected Seyfert galaxies. For Seyfert 1 galaxies a strong correlation between photon index and X-ray luminosity is detected. We confirm the presence of generally steeper X-ray continua in narrow-line Seyfert 1 galaxies (NLS1s) compared to broad-line Seyfert 1 galaxies. Seyfert 2 galaxies show photon indices similar to those of NLS1s. Whereas a tendency for an increasing X-ray luminosity with increasing interaction strength is found for Seyfert 1 galaxies, such a correlation is not found for Seyfert 2 galaxies. For Seyfert 1 galaxies we found also a strong correlation for increasing far-infrared luminosity with increasing interaction strength. Both NLS1s and Seyfert 2 galaxies show the highest values of far-infrared luminosity compared to Seyfert 1 galaxies, suggesting that NLS1s and Seyfert 2 galaxies host strong (circumnuclear) star formation. For variable Seyfert galaxies we present the X-ray light curves obtained from the ROSAT All-Sky Survey and from ROSAT PSPC and HRI pointed observations. Besides the expected strong short- and long-term X-ray variability in Seyfert 1 galaxies, we find indications for X-ray flux variations in Seyfert 2 galaxies. All overlays can be retrieved via CDS anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)} or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/368/797

  1. Searching for Galaxy Clusters in the VST-KiDS Survey

    NASA Astrophysics Data System (ADS)

    Radovich, M.; Puddu, E.; Bellagamba, F.; Moscardini, L.; Roncarelli, M.; Getman, F.; Grado, A.

    We present the methods and first results of the search for galaxy clusters in the Kilo Degree Survey (KiDS). The adopted algorithm and the criterium for selecting the member galaxies are illustrated. Here we report the preliminary results obtained over a small area (7 deg2), and the comparison of our cluster candidates with those found in the RedMapper and SZ Planck catalogues; the analysis to a larger area (148 deg2) is currently in progress. By the KiDS cluster search, we expect to increase the completeness of the clusters catalogue to z = 0.6-0.7 compared to RedMapper.

  2. A Catalogue of XMM-Newton BL Lacs

    NASA Astrophysics Data System (ADS)

    Racero, E.; De la Calle, I.; Rouco Escorial, A.

    2015-05-01

    A catalogue of XMM-Newton BL Lac is presented based on a cross-correlation with the 1374 BL Lac objects listed in the 13th edition of the Veron-Cetty and Veron (2010) catalogue. X-ray counterparts were searched for in the field of view of more than 10000 pointed observations available in the XMM-Newton Archive (XSA) that were public before June 2012. The cross-correlation yielded around 250 XMM-Newton observations, which correspond to 162 different sources. X-ray data from the three EPIC cameras and Optical Monitor data were uniformly analyzed using the latest XMM-Newton Science Analysis System (SAS) version. The catalogue collects X-ray spectral properties, including flux variability, of the sample in the 0.2--10 KeV energy band. All the catalogue products will be made publicly available to the scientific community.

  3. Philosophy and updating of the asteroid photometric catalogue

    NASA Technical Reports Server (NTRS)

    Magnusson, Per; Barucci, M. Antonietta; Capria, M. T.; Dahlgren, Mats; Fulchignoni, Marcello; Lagerkvist, C. I.

    1992-01-01

    The Asteroid Photometric Catalogue now contains photometric lightcurves for 584 asteroids. We discuss some of the guiding principles behind it. This concerns both observers who offer input to it and users of the product.

  4. Official 1997 Mock Trial Materials for the Twenty-Fifth Annual District of Columbia Public Schools Mock Trail Program: Ricki Jones, Plaintiff v. Metro City, Defendant.

    ERIC Educational Resources Information Center

    Henderson, Kamina A.; Roe, Richard L.

    This packet of materials contains law-related materials for students to conduct a mock trial. In this case a faulty water system, containing the parasite Pindia, contributed to the death of an AIDS patient. Statements from the plaintiff, a representative of the Metro City Water Department, health officials, and others are presented. New releases,…

  5. The Criteria for Morphological Classification of PF Galaxy Clusters

    NASA Astrophysics Data System (ADS)

    Panko, E. A.

    The morphological types of galaxy clusters resulting from their out ward appearance is physically related to the clusters and their member galaxies. Presented here is an adopted system of morphological types of galaxy clusters based on the Zwicky, Boutz&Morgan, Rood&Sastry, and L'opez-Cruz systems. The adopted types are suitable for automated classification of galaxy clusters from The Catalogue of Galaxy Clusters and Groups (Panko& Flin 2006). Numerical criteria describing 6 main types were distinguished: Concentrated C, Intermediate I, Open O, Line L, Flat F, and cD. The types correspond to the base divisions from regular to irregular clusters, but also note the presence of preferential direction orplane in each cluster.

  6. Mock communities highlight the diversity of host-associated eukaryotes.

    PubMed

    Wegener Parfrey, Laura

    2015-09-01

    Host-associated microbes are ubiquitous. Every multicellular eukaryote, and even many unicellular eukaryotes (protists), hosts a diverse community of microbes. High-throughput sequencing (HTS) tools have illuminated the vast diversity of host-associated microbes and shown that they have widespread influence on host biology, ecology and evolution (McFall-Ngai et al. ). Bacteria receive most of the attention, but protists are also important components of microbial communities associated with humans (Parfrey et al. ) and other hosts. As HTS tools are increasingly used to study eukaryotes, the presence of numerous and diverse host-associated eukaryotes is emerging as a common theme across ecosystems. Indeed, HTS studies demonstrate that host-associated lineages account for between 2 and 12% of overall eukaryotic sequences detected in soil, marine and freshwater data sets, with much higher relative abundances observed in some samples (Ramirez et al. ; Simon et al. ; de Vargas et al. ). Previous studies in soil detected large numbers of predominantly parasitic lineages such as Apicomplexa, but did not delve into their origin [e.g. (Ramirez et al. )]. In this issue of Molecular Ecology, Geisen et al. () use mock communities to show that many of the eukaryotic organisms detected by environmental sequencing in soils are potentially associated with animal hosts rather than free-living. By isolating the host-associated fraction of soil microbial communities, Geisen and colleagues help explain the surprisingly high diversity of parasitic eukaryotic lineages often detected in soil/terrestrial studies using high-throughput sequencing (HTS) and reinforce the ubiquity of these host-associated microbes. It is clear that we can no longer assume that organisms detected in bulk environmental sequencing are free-living, but instead need to design studies that specifically enumerate the diversity and function of host-associated eukaryotes. Doing so will allow the field to

  7. Mock communities highlight the diversity of host-associated eukaryotes.

    PubMed

    Wegener Parfrey, Laura

    2015-09-01

    Host-associated microbes are ubiquitous. Every multicellular eukaryote, and even many unicellular eukaryotes (protists), hosts a diverse community of microbes. High-throughput sequencing (HTS) tools have illuminated the vast diversity of host-associated microbes and shown that they have widespread influence on host biology, ecology and evolution (McFall-Ngai et al. ). Bacteria receive most of the attention, but protists are also important components of microbial communities associated with humans (Parfrey et al. ) and other hosts. As HTS tools are increasingly used to study eukaryotes, the presence of numerous and diverse host-associated eukaryotes is emerging as a common theme across ecosystems. Indeed, HTS studies demonstrate that host-associated lineages account for between 2 and 12% of overall eukaryotic sequences detected in soil, marine and freshwater data sets, with much higher relative abundances observed in some samples (Ramirez et al. ; Simon et al. ; de Vargas et al. ). Previous studies in soil detected large numbers of predominantly parasitic lineages such as Apicomplexa, but did not delve into their origin [e.g. (Ramirez et al. )]. In this issue of Molecular Ecology, Geisen et al. () use mock communities to show that many of the eukaryotic organisms detected by environmental sequencing in soils are potentially associated with animal hosts rather than free-living. By isolating the host-associated fraction of soil microbial communities, Geisen and colleagues help explain the surprisingly high diversity of parasitic eukaryotic lineages often detected in soil/terrestrial studies using high-throughput sequencing (HTS) and reinforce the ubiquity of these host-associated microbes. It is clear that we can no longer assume that organisms detected in bulk environmental sequencing are free-living, but instead need to design studies that specifically enumerate the diversity and function of host-associated eukaryotes. Doing so will allow the field to

  8. HELCATS - Heliospheric Cataloguing, Analysis and Techniques Service

    NASA Astrophysics Data System (ADS)

    Harrison, Richard; Davies, Jackie; Perry, Chris; Moestl, Christian; Rouillard, Alexis; Bothmer, Volker; Rodriguez, Luciano; Eastwood, Jonathan; Kilpua, Emilia; Gallagher, Peter

    2016-04-01

    Understanding the evolution of the solar wind is fundamental to advancing our knowledge of energy and mass transport in the solar system, rendering it crucial to space weather and its prediction. The advent of truly wide-angle heliospheric imaging has revolutionised the study of both transient (CMEs) and background (SIRs/CIRs) solar wind plasma structures, by enabling their direct and continuous observation out to 1 AU and beyond. The EU-funded FP7 HELCATS project combines European expertise in heliospheric imaging, built up in particular through lead involvement in NASA's STEREO mission, with expertise in solar and coronal imaging as well as in-situ and radio measurements of solar wind phenomena, in a programme of work that will enable a much wider exploitation and understanding of heliospheric imaging observations. With HELCATS, we are (1.) cataloguing transient and background solar wind structures imaged in the heliosphere by STEREO/HI, since launch in late October 2006 to date, including estimates of their kinematic properties based on a variety of established techniques and more speculative, approaches; (2.) evaluating these kinematic properties, and thereby the validity of these techniques, through comparison with solar source observations and in-situ measurements made at multiple points throughout the heliosphere; (3.) appraising the potential for initialising advanced numerical models based on these kinematic properties; (4.) assessing the complementarity of radio observations (in particular of Type II radio bursts and interplanetary scintillation) in combination with heliospheric imagery. We will, in this presentation, provide an overview of progress from the first 18 months of the HELCATS project.

  9. The Compiled Catalogue of Photoelectric UBVR Stellar Magnitudes in the TYCHO2 System

    NASA Astrophysics Data System (ADS)

    Relke, E.; Protsyuk, Yu. I.; Andruk, V. M.

    In order to calibrate the images of astronomical photographic plates from the archive of UkrVO was created the compiled catalogue of photoelectric UBVR stellar magnitudes. It is based on: the Kornilov catalogue of 13586 WBVR stellar magnitudes (Kornilov at al., 1991), the Mermilliod catalogue of 68540 UBV stellar magnitudes (Mermilliod, 1991) and the Andruk catalogue of 1141 UBVR stellar magnitudes (Andruk at al.,1995). All original coordinates have the different epoch and equinox. We performed the cross reference of stars from these three catalogues with the Tycho2, UCAC4 and XPM catalogues and created a new photometric catalogue on the epoch and equinox of J2000.0.

  10. Mass Modelling of dwarf Spheroidal Galaxies

    NASA Astrophysics Data System (ADS)

    Klimentowski, Jarosław; Łokas, Ewa L.; Kazantzidis, Stelios; Prada, Francisco; Mayer, Lucio; Mamon, Gary A.

    2008-05-01

    We study the origin and properties of unbound stars in the kinematic samples of dwarf spheroidal galaxies. For this purpose we have run a high resolution N-body simulation of a two-component dwarf galaxy orbiting in a Milky Way potential. We create mock kinematic data sets by observing the dwarf in different directions. When the dwarf is observed along the tidal tails the kinematic samples are strongly contaminated by unbound stars from the tails. However, most of the unbound stars can be removed by the method of interloper rejection proposed by den Hartog & Katgert. We model the velocity dispersion profiles of the cleaned-up kinematic samples using solutions of the Jeans equation. We show that even for such a strongly stripped dwarf the Jeans analysis, when applied to cleaned samples, allows us to reproduce the mass and mass-to-light ratio of the dwarf with accuracy typically better than 25%.

  11. The star catalogues of Ptolemaios and Ulugh Beg. Machine-readable versions and comparison with the modern Hipparcos Catalogue

    NASA Astrophysics Data System (ADS)

    Verbunt, F.; van Gent, R. H.

    2012-08-01

    In late antiquity and throughout the middle ages, the positions of stars on the celestial sphere were obtained from the star catalogue of Ptolemaios. A catalogue based on new measurements appeared in 1437, with positions by Ulugh Beg, and magnitudes from the 10th-century astronomer al-Sufi. We provide machine-readable versions of these two star catalogues, based on the editions by Toomer (1998, Ptolemy's Almagest, 2nd edn.) and Knobel (1917, Ulugh Beg's catalogue of stars), and determine their accuracies by comparison with the modern Hipparcos Catalogue. The magnitudes in the catalogues correlate well with modern visual magnitudes; the indication "faint" by Ptolemaios is found to correspond to his magnitudes 5 and 6. Gaussian fits to the error distributions in longitude/latitude give widths σ ≃ 27'/23' in the range |Δλ,Δβ| < 50' for Ptolemaios and σ ≃ 22'/18' in Ulugh Beg. Fits to the range |Δλ,Δβ| < 100' gives 10-15% larger widths, showing that the error distributions are broader than Gaussians. The fraction of stars with positions wrong by more than 150' is about 2% for Ptolemaios and 0.1% in Ulugh Beg; the numbers of unidentified stars are 1 in Ptolemaios and 3 in Ulugh Beg. These numbers testify to the excellent quality of both star catalogues (as edited by Toomer and Knobel). Machine-readable catalogues are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/544/A31

  12. Optical-to-virial velocity ratios of local disc galaxies from combined kinematics and galaxy-galaxy lensing

    NASA Astrophysics Data System (ADS)

    Reyes, R.; Mandelbaum, R.; Gunn, J. E.; Nakajima, R.; Seljak, U.; Hirata, C. M.

    2012-10-01

    In this paper, we measure the optical-to-virial velocity ratios Vopt/V200c of disc galaxies in the Sloan Digital Sky Survey (SDSS) at a mean redshift of = 0.07 and with stellar masses 109 < M* < 1011 M⊙. Vopt/V200c, the ratio of the circular velocity measured at the optical radius of the disc (˜10 kpc) to that at the virial radius of the dark matter halo (˜150 kpc), is a powerful observational constraint on disc galaxy formation. It links galaxies to their dark matter haloes dynamically and constrains the total mass profile of disc galaxies over an order of magnitude in length scale. For this measurement, we combine Vopt derived from the Tully-Fisher relation (TFR) from Reyes et al. with V200c derived from halo masses measured with galaxy-galaxy lensing. In anticipation of this combination, we use similarly selected galaxy samples for both the TFR and lensing analysis. For three M* bins with lensing-weighted mean stellar masses of 0.6, 2.7 and 6.5 × 1010 M⊙, we find halo-to-stellar mass ratios M200c/M* = 41, 23 and 26, with 1σ statistical uncertainties of around 0.1 dex, and Vopt/V200c = 1.27 ± 0.08, 1.39 ± 0.06 and 1.27 ± 0.08 (1σ), respectively. Our results suggest that the dark matter and baryonic contributions to the mass within the optical radius are comparable, if the dark matter halo profile has not been significantly modified by baryons. The results obtained in this work will serve as inputs to and constraints on disc galaxy formation models, which will be explored in future work. Finally, we note that this paper presents a new and improved galaxy shape catalogue for weak lensing that covers the full SDSS Data Release 7 footprint.

  13. VizieR Online Data Catalog: The XMM-Newton 2nd Incremental Source Catalogue (2XMMi) (XMM-SSC, 2008)

    NASA Astrophysics Data System (ADS)

    Xmm-Newton Survey Science Centre, Consortium

    2008-09-01

    The 2XMMi catalogue is the fourth publicly released XMM X-ray source catalogue produced by the XMM Survey Science Centre (SSC) consortium, following the 1XMM (Cat. IX/37, released in April 2003), 2XMMp (July 2006) and 2XMM (Cat. IX/39, August 2007) catalogues: 2XMMp was a preliminary version of 2XMM. 2XMMi is an incremental version of the 2XMM catalogue. The 2XMMi catalogue is about 17% larger than the 2XMM catalogue, which it supersedes, due to the 1-year longer baseline of observations included (it is about 8 times larger than the 1XMM catalogue). As such, it is the largest X-ray source catalogue ever produced, containing more than twice as many discrete sources as either the ROSAT survey or pointed catalogues. 2XMMi complements deeper Chandra and XMM-Newton small area surveys, probing a large sky area at the flux limit where the bulk of the objects that contribute to the X-ray background lie. The 2XMMi catalogue provides a rich resource for generating large, well-defined samples for specific studies, utilizing the fact that X-ray selection is a highly efficient (arguably the most efficient) way of selecting certain types of object, notably active galaxies (AGN), clusters of galaxies, interacting compact binaries and active stellar coronae. The large sky area covered by the serendipitous survey, or equivalently the large size of the catalogue, also means that 2XMMi is a superb resource for exploring the variety of the X-ray source population and identifying rare source types. The production of the 2XMMi catalogue has been undertaken by the XMM-Newton SSC consortium in fulfilment of one of its major responsibilities within the XMM-Newton project. The catalogue production process has been designed to exploit fully the capabilities of the XMM-Newton EPIC cameras and to ensure the integrity and quality of the resultant catalogue through rigorous screening of the data. The predecessor 2XMM catalogue was made from a subset of public observations emerging from a re

  14. VizieR Online Data Catalog: The XMM-Newton 2nd Incremental Source Catalogue (2XMMi) (XMM-SSC, 2008)

    NASA Astrophysics Data System (ADS)

    Xmm-Newton Survey Science Centre, Consortium

    2007-09-01

    The 2XMMi catalogue is the fourth publicly released XMM X-ray source catalogue produced by the XMM Survey Science Centre (SSC) consortium, following the 1XMM (Cat. IX/37, released in April 2003), 2XMMp (July 2006) and 2XMM (Cat. IX/39, August 2007) catalogues: 2XMMp was a preliminary version of 2XMM. 2XMMi is an incremental version of the 2XMM catalogue. The 2XMMi catalogue is about 17% larger than the 2XMM catalogue, which it supersedes, due to the 1-year longer baseline of observations included (it is about 8 times larger than the 1XMM catalogue). As such, it is the largest X-ray source catalogue ever produced, containing more than twice as many discrete sources as either the ROSAT survey or pointed catalogues. 2XMMi complements deeper Chandra and XMM-Newton small area surveys, probing a large sky area at the flux limit where the bulk of the objects that contribute to the X-ray background lie. The 2XMMi catalogue provides a rich resource for generating large, well-defined samples for specific studies, utilizing the fact that X-ray selection is a highly efficient (arguably the most efficient) way of selecting certain types of object, notably active galaxies (AGN), clusters of galaxies, interacting compact binaries and active stellar coronae. The large sky area covered by the serendipitous survey, or equivalently the large size of the catalogue, also means that 2XMMi is a superb resource for exploring the variety of the X-ray source population and identifying rare source types. The production of the 2XMMi catalogue has been undertaken by the XMM-Newton SSC consortium in fulfilment of one of its major responsibilities within the XMM-Newton project. The catalogue production process has been designed to exploit fully the capabilities of the XMM-Newton EPIC cameras and to ensure the integrity and quality of the resultant catalogue through rigorous screening of the data. The predecessor 2XMM catalogue was made from a subset of public observations emerging from a re

  15. Percolation galaxy groups and clusters in the sdss redshift survey: identification, catalogs, and the multiplicity function

    SciTech Connect

    Berlind, Andreas A.; Frieman, Joshua A.; Weinberg, David H.; Blanton, Michael R.; Warren, Michael S.; Abazajian, Kevork; Scranton, Ryan; Hogg, David W.; Scoccimarro, Roman; Bahcall, Neta A.; Brinkmann, J.; Gott, J.Richard, III; Kleinman, S.J.; Krzesinski, J.; Lee, Brian C.; Miller, Christopher J.; Nitta, Atsuko; Schneider, Donald P.; Tucker, Douglas L.; Zehavi, Idit; /CCPP, New York /Chicago U., Astron. Astrophys. Ctr. /Ohio State U., Dept. Astron. /Los Alamos /Pittsburgh U. /Princeton U. /Subaru Telescope /Apache Point Observ. /Mt. Suhora Observ., Cracow /LBL, Berkeley /Cerro-Tololo InterAmerican Obs. /Penn State U., Astron. Astrophys. /Fermilab /Arizona U., Astron. Dept. - Steward Observ. /Case Western Reserve U.

    2006-01-01

    We identify galaxy groups and clusters in volume-limited samples of the SDSS redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with ten or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than {approx}1%; a halo completeness of more than {approx}97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is {approx}20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1 square degrees on the sky. We correct for incompleteness caused by fiber collisions and survey edges, and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.

  16. Constraints on radio source clustering towards galaxy clusters: application for cm-wavelength simulations of blind sky surveys

    NASA Astrophysics Data System (ADS)

    Lew, Bartosz

    2016-10-01

    We derive constraints on radio source clustering towards Planck-selected galaxy clusters using the NVSS point source catalog. The constraint can be used for making a more realistic Sunyaev-Zeldovich effect (SZE) mocks, calculating predictions of detectable clusters count and for quantifying source confusion in radio surveys.

  17. GALAXY CLUSTERING TOPOLOGY IN THE SLOAN DIGITAL SKY SURVEY MAIN GALAXY SAMPLE: A TEST FOR GALAXY FORMATION MODELS

    SciTech Connect

    Choi, Yun-Young; Kim, Juhan; Kim, Sungsoo S.; Park, Changbom; Gott, J. Richard; Weinberg, David H.; Vogeley, Michael S.

    2010-09-15

    We measure the topology of the main galaxy distribution using the Seventh Data Release of the Sloan Digital Sky Survey, examining the dependence of galaxy clustering topology on galaxy properties. The observational results are used to test galaxy formation models. A volume-limited sample defined by M{sub r} < -20.19 enables us to measure the genus curve with an amplitude of G = 378 at 6 h {sup -1} Mpc smoothing scale, with 4.8% uncertainty including all systematics and cosmic variance. The clustering topology over the smoothing length interval from 6 to 10 h {sup -1} Mpc reveals a mild scale dependence for the shift ({Delta}{nu}) and void abundance (A{sub V}) parameters of the genus curve. We find substantial bias in the topology of galaxy clustering with respect to the predicted topology of the matter distribution, which varies with luminosity, morphology, color, and the smoothing scale of the density field. The distribution of relatively brighter galaxies shows a greater prevalence of isolated clusters and more percolated voids. Even though early (late)-type galaxies show topology similar to that of red (blue) galaxies, the morphology dependence of topology is not identical to the color dependence. In particular, the void abundance parameter A{sub V} depends on morphology more strongly than on color. We test five galaxy assignment schemes applied to cosmological N-body simulations of a {Lambda}CDM universe to generate mock galaxies: the halo-galaxy one-to-one correspondence model, the halo occupation distribution model, and three implementations of semi-analytic models (SAMs). None of the models reproduces all aspects of the observed clustering topology; the deviations vary from one model to another but include statistically significant discrepancies in the abundance of isolated voids or isolated clusters and the amplitude and overall shift of the genus curve. SAM predictions of the topology color dependence are usually correct in sign but incorrect in magnitude

  18. The alignment between satellites and central galaxies: theory versus observations

    NASA Astrophysics Data System (ADS)

    Kang, X.; van den Bosch, Frank C.; Yang, Xiaohu; Mao, Shude; Mo, H. J.; Li, Cheng; Jing, Y. P.

    2007-07-01

    Recent studies have shown that the distribution of satellite galaxies is preferentially aligned with the major axis of their central galaxy. The strength of this alignment has been found to depend strongly on the colours of the satellite and central galaxies, and only weakly on the mass of the halo in which the galaxies reside. In this paper we study whether these alignment signals, and their dependence on galaxy and halo properties, can be reproduced in a hierarchical structure formation model of a ΛCDM concordance cosmology. To that extent we use a large N-body simulation which we populate with galaxies following a semi-analytical model for galaxy formation. We find that if the orientation of the central galaxy is perfectly aligned with that of its dark matter halo, then the predicted central-satellite alignment signal is much stronger than observed. If, however, the minor axis of a central galaxy is perfectly aligned with the angular momentum vector of its dark matter halo, we can accurately reproduce the observed alignment strength as a function of halo mass and galaxy colour. Although this suggests that the orientation of central galaxies is governed by the angular momentum of their dark matter haloes, we emphasize that any other scenario in which the minor axes of central galaxy and halo are misaligned by ~40° (on average) will match the data equally well. Finally, we show that dependence of the alignment strength on the colour of the central galaxy is most likely an artefact due to interlopers in the group catalogue. The dependence on the colour of the satellite galaxies, on the other hand, is real and owes to the fact that red satellites are associated with subhaloes that were more massive at their time of accretion.

  19. An imaging and spectroscopic study of the planetary nebulae in NGC 5128 (Centaurus A). Planetary nebulae catalogues

    NASA Astrophysics Data System (ADS)

    Walsh, J. R.; Rejkuba, M.; Walton, N. A.

    2015-02-01

    Context. Planetary nebulae (PNe) are excellent tracers of the common low mass stars through their strong and narrow emission lines. The velocities of large numbers of PNe are excellent tracers of galaxy kinematics. NGC 5128, the nearest large early-type galaxy, offers the possibility to gather a large sample. Aims: Imaging and spectroscopic observations of PNe in NGC 5128 were obtained to find and measure their velocities. Combined with literature data, a large sample of high quality kinematic probes is assembled for dynamical studies. Methods: NTT imaging was obtained in 15 fields in NGC 5128 across 1° with EMMI and [O III] and off-band filters. Newly detected sources, combined with literature PN, were used as input for FLAMES multi-fibre spectroscopy in MEDUSA mode. Spectra of the 4600-5100 Å region were analysed and velocities measured based on [O III]4959, 5007 Å and often Hβ. Results: The chief results are catalogues of 1118 PN candidates and 1267 spectroscopically confirmed PNe in NGC 5128. The catalogue of PN candidates contains 1060 PNe discovered with NTT EMMI imaging and 58 from literature surveys. The spectroscopic PN catalogue has FLAMES radial velocity and emission line measurements for 1135 PNe, of which 486 are new. Another 132 PN radial velocities are available from the literature. For 629 PNe observed with FLAMES, Hβ was measured in addition to [O III]. Nine targets show double-lined or more complex profiles, and their possible origin is discussed. FLAMES spectra of 48 globular clusters were also targetted: 11 had emission lines detected (two with multiple components), but only 3 are PNe likely to belong to the host globular. Conclusions: The total of 1267 confirmed PNe in NGC 5128 with radial velocity measurements (1135 with small velocity errors) is the largest collection of individual kinematic probes in an early-type galaxy. This PN dataset, as well as the catalogue of PN candidates, are valuable resources for detailed investigation of NGC

  20. Conformity Between LR0 Mock-Ups and Vvers Npp Rpv Neutron Flux Attenuation

    NASA Astrophysics Data System (ADS)

    Belousov, Sergey; Ilieva, Krassimira; Kirilova, Desislava

    2009-08-01

    The conformity of the mock-up results and those for reactor pressure vessel (RPV) of nuclear power plants (NPP) has been evaluated in order to qualify if the mock-ups data could be used for benchmark's purpose only, or/and for simulating of the NPP irradiation conditions. Neutron transport through the vessel has been calculated by the three-dimensional discrete ordinate code TORT with problem oriented multigroup energy neutron cross-section library BGL. Neutron flux/fluence and spectrum shape represented by normalized group neutron fluxes in the multigroup energy structure, for neutrons with energy above 0.5 MeV, have been used for conformity analysis. It has been demonstrated that the relative difference of the attenuation factor as well as the group neutron fluxes did not exceed 10% at all considered positions for VVER-440. For VVER-1000, it has been obtained the same consistency, except for the location behind the RPV. The neutron flux attenuation behind the RPV is 18% higher than the mock-up attenuation. It has been shown that this difference arises from the dissimilarity of the biological shielding. The obtained results have demonstrated that the VVERs' mock-ups are appropriate for simulating the NPP irradiation conditions. The mock-up results for VVER-1000 have to be applied more carefully i.e. taking into account the existing peculiarity of the biological shielding and RPV attenuation azimuthal dependence.

  1. A prototype catalogue: DOE National Laboratory technologies for infrastructure modernization

    SciTech Connect

    Currie, J.W.; Wilfert, G.L.; March, F.

    1990-01-01

    The purpose of this report is to provide the Office of Technology Assessment (OTA) with information about selected technologies under development in the Department of Energy (DOE) through its National Laboratory System and its Program Office operations. The technologies selected are those that have the potential to improve the performance of the nation's public works infrastructure. The product is a relational database that we refer to as a prototype catalogue of technologies.'' The catalogue contains over 100 entries of DOE-supported technologies having potential application to infrastructure-related problems. The work involved conceptualizing an approach, developing a framework for organizing technology information, and collecting samples of readily available data to be put into a prototype catalogue. In developing the catalogue, our objectives were to demonstrate the concept and provide readily available information to OTA. As such, the catalogue represents a preliminary product. The existing database is not exhaustive and likely represents only a fraction of relevant technologies developed by DOE. In addition, the taxonomy we used to classify technologies is based on the judgment of project staff and has received minimal review by individuals who have been involved in the development and testing of the technologies. Finally, end users will likely identify framework changes and additions that will strengthen the catalogue approach. The framework for the catalogue includes four components: a description of the technology, along with potential uses and other pertinent information; identification of the source of the descriptive information; identification of a person or group knowledgeable about the technology; and a classification of the described technology in terms of its type, application, life-cycle use, function, and readiness.

  2. The AKARI Far-Infrared Bright Source Catalogue

    NASA Astrophysics Data System (ADS)

    Yamamura, Issei

    The AKARI Far-Infrared Bright Source Catalogue is now available to the world-wide astro-nomical community. The catalogue contains about 0.4 million infrared sources detected and measured at four far-infrared wavelengths bands centered at 65, 90, 140, 160 µm. It shall be used as one of the standard resources in the modern astronomical researches. AKARI, the first Japanese infrared astronomical satellite, was launched in February 2006, and carried out an all-sky survey during its 16 months cryogenic mission lifetime. AKARI is equipped with a 68.5 cm cooled telescope and two instruments, the Infrared Camera (IRC; 1.8-26.5 µm) and the Far-Infrared Surveyor (FIS; 50-180 µm). The All-Sky Survey was made in two bands (9 and 18 µm) by the IRC and in four wavelengths by the FIS. The FIR survey covered more than 94 per cent of the entire sky with more than two independent scans. The first public release of the point source catalogue is made in March 2010. The catalogue is intended to provide a source list of uniform detection limit over the entire sky (in fact the limit is different in the Galactic Plane regions). It includes about 0.4 million sources. The detection limit at the most sensitive band, 90 µm, is about 0.6 Jy. The flux uncertainty is 20-40 per cent, depending on the band. The position information is as accurate as about 5 arcsec, enabling us to carry out a precise identification using other catalogues. The Mid-Infrared Point Source Catalogue is also released at the same time. With the higher spatial resolution and better sensitivity, the AKARI catalogues shall be used as the standard infrared source list in various fields in astronomy. The catalogue provides a good opportunity for follow-up observations with Herschel, Plank, SOFIA, ALMA, and other ongoing and future facilities. AKARI is a JAXA project with the participation of ESA. The Far-Infrared Bright Source Catalogue is the product of collaborations between the institutes in Japan, Korea, UK, and the

  3. Identifying and relating biological concepts in the Catalogue of Life

    PubMed Central

    2011-01-01

    Background In this paper we describe our experience of adding globally unique identifiers to the Species 2000 and ITIS Catalogue of Life, an on-line index of organisms which is intended, ultimately, to cover all the world's known species. The scientific species names held in the Catalogue are names that already play an extensive role as terms in the organisation of information about living organisms in bioinformatics and other domains, but the effectiveness of their use is hindered by variation in individuals' opinions and understanding of these terms; indeed, in some cases more than one name will have been used to refer to the same organism. This means that it is desirable to be able to give unique labels to each of these differing concepts within the catalogue and to be able to determine which concepts are being used in other systems, in order that they can be associated with the concepts in the catalogue. Not only is this needed, but it is also necessary to know the relationships between alternative concepts that scientists might have employed, as these determine what can be inferred when data associated with related concepts is being processed. A further complication is that the catalogue itself is evolving as scientific opinion changes due to an increasing understanding of life. Results We describe how we are using Life Science Identifiers (LSIDs) as globally unique identifiers in the Catalogue of Life, explaining how the mapping to species concepts is performed, how concepts are associated with specific editions of the catalogue, and how the Taxon Concept Schema has been adopted in order to express information about concepts and their relationships. We explore the implications of using globally unique identifiers in order to refer to abstract concepts such as species, which incorporate at least a measure of subjectivity in their definition, in contrast with the more traditional use of such identifiers to refer to more tangible entities, events, documents

  4. THE EVOLUTION OF THE NUMBER DENSITY OF COMPACT GALAXIES

    SciTech Connect

    Poggianti, B. M.; Calvi, R.; Renzini, A.; Moretti, A.; D'Onofrio, M.; Valentinuzzi, T.; Fritz, J.

    2013-11-10

    We compare the number density of compact (small size) massive galaxies at low and high redshift using our Padova Millennium Galaxy and Group Catalogue (PM2GC) at z = 0.03-0.11 and the CANDELS results from Barro et al. at z = 1-2. The number density of local compact galaxies with luminosity weighted (LW) ages compatible with being already passive at high redshift is compared with the density of compact passive galaxies observed at high-z. Our results place an upper limit of a factor ∼2 on the evolution of the number density and are inconsistent with a significant size evolution for most of the compact galaxies observed at high-z. Instead, the evolution may be significant (up to a factor five) for the most extreme, ultracompact galaxies. Considering all compact galaxies, regardless of LW age and star formation activity, a minority of local compact galaxies (≤1/3) might have formed at z < 1. Finally, we show that the secular decrease of the galaxy stellar mass due to simple stellar evolution may in some cases be a non-negligible factor in the context of the evolution of the mass-size relation, and we caution that passive evolution in mass should be taken into account when comparing samples at different redshifts.

  5. Oxygen abundances in low surface-brightness galaxies

    NASA Technical Reports Server (NTRS)

    Roennback, Jari

    1993-01-01

    Recent theories predict that some protogalaxies, in low-density environments of the field, are contracting and interacting so slowly that global star formation can be delayed until today. These systems should be gas rich and have low surface-brightness. Blue compact galaxies (BCG's) and other compact HII region galaxies currently experiencing a burst of star formation are good candidates of truly young galaxies (in the sense that global star formation recently has been initiated). If they really are young, they ought to have a recent phase when their brightness was much lower than in the bursting phase. No claims of observations of such proto-BCG's exist. Observations of galaxies in their juvenile phases would undoubtedly be of great interest, e.g. the determination of the primordial helium abundance would improve. A proper place to search for young nearby galaxies could be among blue low surface-brightness galaxies (BLSBG's) in the local field. The study of low surface-brightness galaxies (LSBG's) as a group began relatively recently. They are galaxies with extraordinary properties both as individuals and as a group. A few years ago we started an optical study of a sample of BLSBG's selected from the ESO/Uppsala catalogue. Results of spectroscopic observations obtained on a subsample - 8 galaxies - of our selection are reported. The HII region oxygen chemical abundances and its relation to the blue absolute magnitude and surface-brightness is investigated.

  6. Intrinsic alignment of simulated galaxies in the cosmic web: implications for weak lensing surveys

    NASA Astrophysics Data System (ADS)

    Codis, S.; Gavazzi, R.; Dubois, Y.; Pichon, C.; Benabed, K.; Desjacques, V.; Pogosyan, D.; Devriendt, J.; Slyz, A.

    2015-04-01

    The intrinsic alignment of galaxy shapes (by means of their angular momentum) and their cross-correlation with the surrounding dark matter tidal field are investigated using the 160 000, z = 1.2 synthetic galaxies extracted from the high-resolution cosmological hydrodynamical simulation HORIZON-AGN. One- and two-point statistics of the spin of the stellar component are measured as a function of mass and colour. For the low-mass galaxies, this spin is locally aligned with the tidal field `filamentary' direction while, for the high-mass galaxies, it is perpendicular to both filaments and walls. The bluest galaxies of our synthetic catalogue are more strongly correlated with the surrounding tidal field than the reddest galaxies, and this correlation extends up to ˜10 h- 1 Mpc comoving distance. We also report a correlation of the projected ellipticities of blue, intermediate-mass galaxies on a similar scale at a level of 10-4 which could be a concern for cosmic shear measurements. We do not report any measurable intrinsic alignments of the reddest galaxies of our sample. This work is a first step towards the use of very realistic catalogue of synthetic galaxies to evaluate the contamination of weak lensing measurement by the intrinsic galactic alignments.

  7. H-ATLAS: the far-infrared properties of galaxies in and around the Coma cluster

    NASA Astrophysics Data System (ADS)

    Fuller, C.; Davies, J. I.; Smith, M. W. L.; Valiante, E.; Eales, S.; Bourne, N.; Dunne, L.; Dye, S.; Furlanetto, C.; Ibar, E.; Ivison, R.; Maddox, S.; Sansom, A.; Michałowski, M. J.; Davis, T.

    2016-05-01

    We describe a far-infrared survey of the Coma cluster and the galaxy filament it resides within. Our survey covers an area of ˜150 deg2 observed by Herschel H-ATLAS (Herschel Astrophysical Terahertz Large Area Survey) in five bands at 100, 160, 250, 350 and 500 μm. The SDSS spectroscopic survey (mr ≤ 17.8) is used to define an area (within the virial radius) and redshift selected (4268 < v < 9700 km s-1) sample of 744 Coma cluster galaxies - the Coma Cluster Catalogue. For comparison, we also define a sample of 951 galaxies in the connecting filament - the Coma Filament Catalogue. The optical positions and parameters are used to define appropriate apertures to measure each galaxy's far-infrared emission. We have detected 99 of 744 (13 per cent) and 422 of 951 (44 per cent) of the cluster and filament galaxies in the SPIRE 250 μm band. We consider the relative detection rates of galaxies of different morphological types finding that it is only the S0/Sa population that shows clear differences between the cluster and filament. We find no differences between the dust masses and temperatures of cluster and filament galaxies with the exception of early-type galaxy dust temperatures, which are significantly hotter in the cluster than in the filament (X-ray heating?). From a chemical evolution model, we find no evidence for different evolutionary processes (gas loss or infall) between galaxies in the cluster and filament.

  8. Les galaxies

    NASA Astrophysics Data System (ADS)

    Combes, Francoise

    2016-08-01

    Considerable progress has been made on galaxy formation and evolution in recent years, and new issues. The old Hubble classification according to the tuning fork of spirals, lenticulars and ellipticals, is still useful but has given place to the red sequence, the blue cloud and the green valley, showing a real bimodality of types between star forming galaxies (blue) and quenched ones (red). Large surveys have shown that stellar mass and environment density are the two main factors of the evolution from blue to red sequences. Evolution is followed directly with redshift through a look-back time of more than 12 billion years. The most distant galaxy at z=11. has already a stellar mass of a billion suns. In an apparent anti-hierarchical scenario, the most massive galaxies form stars early on, while essentially dwarf galaxies are actively star-formers now. This downsizing feature also applies to the growth of super-massive black holes at the heart of each bulgy galaxy. The feedback from active nuclei is essential to explain the distribution of mass in galaxies, and in particular to explain why the fraction of baryonic matter is so low, lower by more than a factor 5 than the baryonic fraction of the Universe. New instruments just entering in operation, like MUSE and ALMA, provide a new and rich data flow, which is developed in this series of articles.

  9. The XXL Survey. II. The bright cluster sample: catalogue and luminosity function

    NASA Astrophysics Data System (ADS)

    Pacaud, F.; Clerc, N.; Giles, P. A.; Adami, C.; Sadibekova, T.; Pierre, M.; Maughan, B. J.; Lieu, M.; Le Fèvre, J. P.; Alis, S.; Altieri, B.; Ardila, F.; Baldry, I.; Benoist, C.; Birkinshaw, M.; Chiappetti, L.; Démoclès, J.; Eckert, D.; Evrard, A. E.; Faccioli, L.; Gastaldello, F.; Guennou, L.; Horellou, C.; Iovino, A.; Koulouridis, E.; Le Brun, V.; Lidman, C.; Liske, J.; Maurogordato, S.; Menanteau, F.; Owers, M.; Poggianti, B.; Pomarède, D.; Pompei, E.; Ponman, T. J.; Rapetti, D.; Reiprich, T. H.; Smith, G. P.; Tuffs, R.; Valageas, P.; Valtchanov, I.; Willis, J. P.; Ziparo, F.

    2016-06-01

    Context. The XXL Survey is the largest survey carried out by the XMM-Newton satellite and covers a total area of 50 square degrees distributed over two fields. It primarily aims at investigating the large-scale structures of the Universe using the distribution of galaxy clusters and active galactic nuclei as tracers of the matter distribution. The survey will ultimately uncover several hundreds of galaxy clusters out to a redshift of ~2 at a sensitivity of ~10-14 erg s-1 cm-2 in the [0.5-2] keV band. Aims: This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3 × 10-14 erg s-1 cm-2 on the source flux within a 1' aperture. Methods: The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. Results: The bright cluster sample consists of systems with masses between M500 = 7 × 1013 and 3 × 1014 M⊙, mostly located between z = 0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of σ8 and/or ΩM appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z ~ 1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters. Based on

  10. Catalogue of knowledge and skills for sleep medicine.

    PubMed

    Penzel, Thomas; Pevernagie, Dirk; Dogas, Zoran; Grote, Ludger; de Lacy, Simone; Rodenbeck, Andrea; Bassetti, Claudio; Berg, Søren; Cirignotta, Fabio; d'Ortho, Marie-Pia; Garcia-Borreguero, Diego; Levy, Patrick; Nobili, Lino; Paiva, Teresa; Peigneux, Philippe; Pollmächer, Thomas; Riemann, Dieter; Skene, Debra J; Zucconi, Marco; Espie, Colin

    2014-04-01

    Sleep medicine is evolving globally into a medical subspeciality in its own right, and in parallel, behavioural sleep medicine and sleep technology are expanding rapidly. Educational programmes are being implemented at different levels in many European countries. However, these programmes would benefit from a common, interdisciplinary curriculum. This 'catalogue of knowledge and skills' for sleep medicine is proposed, therefore, as a template for developing more standardized curricula across Europe. The Board and The Sleep Medicine Committee of the European Sleep Research Society (ESRS) have compiled the catalogue based on textbooks, standard of practice publications, systematic reviews and professional experience, validated subsequently by an online survey completed by 110 delegates specialized in sleep medicine from different European countries. The catalogue comprises 10 chapters covering physiology, pathology, diagnostic and treatment procedures to societal and organizational aspects of sleep medicine. Required levels of knowledge and skills are defined, as is a proposed workload of 60 points according to the European Credit Transfer System (ECTS). The catalogue is intended to be a basis for sleep medicine education, for sleep medicine courses and for sleep medicine examinations, serving not only physicians with a medical speciality degree, but also PhD and MSc health professionals such as clinical psychologists and scientists, technologists and nurses, all of whom may be involved professionally in sleep medicine. In the future, the catalogue will be revised in accordance with advances in the field of sleep medicine.

  11. Mock-up Test of Remote Controlled Dismantling Apparatus for Large-sized Vessels

    SciTech Connect

    Kimura, M.; Myodo, M.; Okane, S.; Miyajima, K.

    2002-02-26

    The remote dismantling apparatus, which is equipped with multi-units for functioning of washing, cutting, collection of cut pieces and so on, has been constructed to dismantle the large-sized vessels in the JAERI's Reprocessing Test Facility (JRTF). The apparatus has five-axis movement capability and its operation is performed remotely. The mock-up tests were performed to evaluate the applicability of the apparatus to actual dismantling activities by using the mock-ups of LV-3 and LV-5 in the facility. It was confirmed that each unit was satisfactory functioned by remote operation. Efficient procedure for dismantling the large-sized vessel was studied and various data were obtained from the mock-up tests. This apparatus was found to be applicable for the actual dismantling activity in JRTF.

  12. An Innovative Approach to Pharmacy Law Education Utilizing a Mock Board of Pharmacy Meeting

    PubMed Central

    Bess, D. Todd; Taylor, Jade; Schwab, Carol A.; Wang, Junling; Carter, Jason A.

    2016-01-01

    A thorough understanding of pharmacy law by students is important in the molding of future pharmacy practitioners but a standardized template for the best way to educate students in this area has not been created. A mock Board of Pharmacy meeting was designed and incorporated into the Pharmacy Law course to meet the ACPE accreditation standards at the University of Tennessee College of Pharmacy. Students acted as Board of Pharmacy members and utilized technology to decide outcomes of cases and requests addressed in a typical 2 day Tennessee Board of Pharmacy meeting. The actual responses to those cases, as well as similar cases and requests addressed over a 5 year period, were revealed to students after they made motions on mock scenarios. Student participation in this interactive learning experience resulted in good understanding of the rules and regulations of pharmacy practice and the consequences associated with violating regulations. Such mock Board of Pharmacy meeting is recommended for future pharmacy law education. PMID:27347433

  13. Thermo-mechanical tests of a CFC divertor mock-up

    NASA Astrophysics Data System (ADS)

    Cardella, A.; Akiba, M.; Duwe, R.; Di Pietro, E.; Suzuki, S.; Satoh, K.; Reheis, N.

    1994-04-01

    Thermo-mechanical tests have been performed on a divertor mock-up consisting of a metallic tube armoured with five carbon fibre composite tiles. The tube is inserted inside the tiles and brazed with TiCuSil braze (monoblock concept). The tube material is TZM, a molybdenum alloy, and the armour material is SEP CARB N112, a high conductivity carbon-carbon composite. Using special surface preparation consisting of laser drilling, small (˜- 500 μm) holes in the composite have been made to increase the surface wetted by the braze and the resistance. The mock-up has been tested at the JAERI 400 kW electron beam test facility JEBIS. The aim of the test was to assess the performance of the mock-up in screening and thermal fatigue tests with particular attention to the behaviour of the armour to heat sink joint.

  14. Optical coherence tomography layer thickness characterization of a mock artery during angioplasty balloon deployment

    NASA Astrophysics Data System (ADS)

    Azarnoush, Hamed; Vergnole, Sébastien; Boulet, Benoît; Lamouche, Guy

    2011-03-01

    Optical coherence tomography (OCT) is used to study the deformation of a mock artery in an angioplasty simulation setup. An OCT probe integrated in a balloon catheter provides intraluminal real-time images during balloon inflation. Swept-source OCT is used for imaging. A 4 mm semi-compliant polyurethane balloon is used for experiments. The balloon is inflated inside a custom-built multi-layer artery phantom. The phantom has three layers to mock artery layers, namely, intima, media and adventitia. Semi-automatic segmentation of phantom layers is performed to provide a detailed assessment of the phantom deformation at various inflation pressures. Characterization of luminal diameter and thickness of different layers of the mock artery is provided for various inflation pressures.

  15. Thermal Damage on LX-04 Mock Material and Gas Permeability Assessment

    SciTech Connect

    Hsu, P C; Dehaven, M; McClelland, M; Maienschein, J

    2004-11-15

    RM-04-BR, a mock material for the plastic-bonded HMX-based explosive LX-04, is characterized after being thermally damaged at 140 C and 190 C. We measured the following material properties before and after the thermal experiments: sample volume, density, sound speed, and gas permeability in the material. Thermal treatment of the mock material leads to de-coloring and insignificant weight loss. Sample expanded, resulting in density reductions of 1.0% to 2.5% at 140 C and 190 C, respectively. Permeability in the mock samples was found to increase from 10{sup -15} to 10{sup -16} m{sup 2}, as the porosity increased. The permeability measurements are well represented by the Blake-Kozeny equation for laminar flow through porous media. The results are similar to the gas permeability in PBX-9501 obtained by other researchers.

  16. Galaxy Zoo 1: data release of morphological classifications for nearly 900 000 galaxies

    SciTech Connect

    Linott, C.; Slosar, A.; Lintott, C.; Schawinski, K.; Bamford, S.; Slosar, A.; Land, K.; Thomas, D.; Edmondson, E.; Masters, K.; Nichol, R.C.; Raddick, M.J.; Szalay, A.; Andreescu, D.; Murray, P.; Vandenberg, J.

    2011-01-01

    Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900,000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org.

  17. The XXL survey: first results on clusters of galaxy

    NASA Astrophysics Data System (ADS)

    Pacaud, Florian

    2016-07-01

    With a total geometric area of 50deg2, XXL is the largest contiguous survey undertaken by the XMM-Newton satellite. The final survey catalogues are expected to contain ~25000 AGNs down to a flux limit of 3e-15 erg/s/cm2 and ~500 groups and clusters of galaxies up to a redshift of z~1.5. The first results of the survey focus on a sub-sample of the 100 brightest galaxy clusters and have recently been released to the public. In this contribution, I will first describe the sample and the modeling of its selection function. Then, I will discuss some of the most significant early scientific results based on the catalogue, namely the measured scaling relations, the baryon budget of XXL groups, the detection of superstructures and the cosmological implications of the sample.

  18. The Thousand-Ruby Galaxy

    NASA Astrophysics Data System (ADS)

    2008-09-01

    ESO's Wide Field Imager has captured the intricate swirls of the spiral galaxy Messier 83, a smaller look-alike of our own Milky Way. Shining with the light of billions of stars and the ruby red glow of hydrogen gas, it is a beautiful example of a barred spiral galaxy, whose shape has led to it being nicknamed the Southern Pinwheel. Messier 83, M83 ESO PR Photo 25/08 Spiral Galaxy Messier 83 This dramatic image of the galaxy Messier 83 was captured by the Wide Field Imager at ESO's La Silla Observatory, located high in the dry desert mountains of the Chilean Atacama Desert. Messier 83 lies roughly 15 million light-years away towards the huge southern constellation of Hydra (the sea serpent). It stretches over 40 000 light-years, making it roughly 2.5 times smaller than our own Milky Way. However, in some respects, Messier 83 is quite similar to our own galaxy. Both the Milky Way and Messier 83 possess a bar across their galactic nucleus, the dense spherical conglomeration of stars seen at the centre of the galaxies. This very detailed image shows the spiral arms of Messier 83 adorned by countless bright flourishes of ruby red light. These are in fact huge clouds of glowing hydrogen gas. Ultraviolet radiation from newly born, massive stars is ionising the gas in these clouds, causing the great regions of hydrogen to glow red. These star forming regions are contrasted dramatically in this image against the ethereal glow of older yellow stars near the galaxy's central hub. The image also shows the delicate tracery of dark and winding dust streams weaving throughout the arms of the galaxy. Messier 83 was discovered by the French astronomer Nicolas Louis de Lacaille in the mid 18th century. Decades later it was listed in the famous catalogue of deep sky objects compiled by another French astronomer and famous comet hunter, Charles Messier. Recent observations of this enigmatic galaxy in ultraviolet light and radio waves have shown that even its outer desolate regions

  19. Study of the star catalogue (epoch AD 1396.0) recorded in ancient Korean astronomical almanac

    NASA Astrophysics Data System (ADS)

    Jeon, Junhyeok; Lee, Yong Bok; Lee, Yong-Sam

    2015-11-01

    The study of old star catalogues provides important astrometric data. Most of the researches based on the old star catalogues were manuscript published in Europe and from Arabic/Islam. However, the old star catalogues published in East Asia did not get attention. Therefore, among the East Asian star catalogues we focus on a particular catalogue recorded in a Korean almanac. Its catalogue contains 277 stars that are positioned in a region within 10° of the ecliptic plane. The stars in the catalogue were identified using the modern Hipparcos catalogue. We identified 274 among 277 stars, which is a rate of 98.9 per cent. The catalogue records the epoch of the stars' positions as AD 1396.0. However, by using all of the identified stars we found that the initial epoch of the catalogue is AD 1363.1 ± 3.2. In conclusion, the star catalogue was compiled and edited from various older star catalogues. We assume a correlation with the Almagest by Ptolemaios. This study presents newly analysed results from the historically important astronomical data discovered in East Asia. Therefore, this star catalogue will become important data for comparison with the star catalogues published in Europe and from Arabic/Islam.

  20. X-15 mock-up with test pilot Milt Thompson

    NASA Technical Reports Server (NTRS)

    1993-01-01

    NASA research pilot Milt Thompson is seen here with the mock-up of X-15 #3 that was later installed at the NASA Dryden Flight Research Center, Edwards, California. Milton 0. Thompson was a research pilot, Chief Engineer and Director of Research Projects during a long career at the NASA Dryden Flight Research Center. Thompson was hired as an engineer at the flight research facility on 19 March 1956, when it was still under the auspices of NACA. He became a research pilot on 25 May 1958. Thompson was one of the 12 NASA, Air Force, and Navy pilots to fly the X-15 rocket-powered research aircraft between 1959 and 1968. He began flying X-15s on 29 October 1963. He flew the aircraft 14 times during the following two years, reaching a maximum speed of 3723 mph (Mach 5.42) and a peak altitude of 214,100 feet on separate flights. (On a different flight, he reached a Mach number of 5.48 but his mph was only 3712.) Thompson concluded his active flying career in 1968, becoming Director of Research Projects. In 1975 he was appointed Chief Engineer and retained the position until his death on 8 August 1993. The X-15 was a rocket powered aircraft 50 ft long with a wingspan of 22 ft. It was a missile-shaped vehicle with an unusual wedge-shaped vertical tail, thin stubby wings, and unique side fairings that extended along the side of the fuselage. The X-15 weighed about 14,000 lb empty and approximately 34,000 lb at launch. The XLR-99 rocket engine, manufactured by Thiokol Chemical Corp., was pilot controlled and was capable of developing 57,000 lb of thrust. North American Aviation built three X-15 aircraft for the program. The X-15 research aircraft was developed to provide in-flight information and data on aerodynamics, structures, flight controls, and the physiological aspects of high-speed, high-altitude flight. A follow on program used the aircraft as a testbed to carry various scientific experiments beyond the Earth's atmosphere on a repeated basis. For flight in the dense

  1. X-15 mock-up with test pilot Milt Thompson

    NASA Technical Reports Server (NTRS)

    1993-01-01

    NASA research pilot Milt Thompson stands next to a mock-up of X-15 number 3 that was later installed at the NASA Dryden Flight Research Center, Edwards, California. Milton 0. Thompson was a research pilot, Chief Engineer and Director of Research Projects during a long career at the NASA Dryden Flight Research Center. Thompson was hired as an engineer at the flight research facility on 19 March 1956, when it was still under the auspices of NACA. He became a research pilot on 25 May 1958. Thompson was one of the 12 NASA, Air Force, and Navy pilots to fly the X-15 rocket-powered research aircraft between 1959 and 1968. He began flying X-15s on 29 October 1963. He flew the aircraft 14 times during the following two years, reaching a maximum speed of 3723 mph (Mach 5.42) and a peak altitude of 214,100 feet on separate flights. Thompson concluded his active flying career in 1968, becoming Director of Research Projects. In 1975 he was appointed Chief Engineer and retained the position until his death on 8 August 1993. The X-15 was a rocket-powered aircraft 50 ft long with a wingspan of 22 ft. It was a missile-shaped vehicle with an unusual wedge-shaped vertical tail, thin stubby wings, and unique side fairings that extended along the side of the fuselage. The X-15 weighed about 14,000 lb empty and approximately 34,000 lb at launch. The XLR-99 rocket engine, manufactured by Thiokol Chemical Corp., was pilot controlled and was capable of developing 57,000 lb of thrust. North American Aviation built three X-15 aircraft for the program. The X-15 research aircraft was developed to provide in-flight information and data on aerodynamics, structures, flight controls, and the physiological aspects of high-speed, high-altitude flight. A follow-on program used the aircraft as a testbed to carry various scientific experiments beyond the Earth's atmosphere on a repeated basis. For flight in the dense air of the usable atmosphere, the X-15 used conventional aerodynamic controls such as

  2. Reassessing the BATSE Catalogue of Terrestrial Gamma-ray Flashes

    NASA Astrophysics Data System (ADS)

    Sleinkofer, A. M.; Briggs, M. S.; Connaughton, V.

    2015-12-01

    Since Terrestrial Gamma-ray Flashes (TGFs) were discovered by the Burst and Transient Source Experiment (BATSE) on NASA's Compton Gamma-ray Observatory (CGRO) in the 1990s, other observations have increased our knowledge of TGFs. This improved understanding includes characteristics such as the distributions of geographic locations, pulse durations, pulse shapes, and pulse multiplicities. Using this post-BATSE knowledge, we reassessed the BATSE TGF catalogue(http://gammaray.nsstc.nasa.gov/batse/tgf/). Some BATSE triggers have features that can easily identify the trigger as a TGF, while others display different features that are unusual for TGFs. The BATSE triggers of the TGF catalogue were classified into five categories: TGFs, Terrestrial Electron Beams (TEBs), unusual TGFs, uncertain due to insufficient data, and TEB candidates. The triggers with unusual features will be further investigated. A table of our classifications and comments will be added to the online catalogue.

  3. Second ROSAT all-sky survey (2RXS) source catalogue

    NASA Astrophysics Data System (ADS)

    Boller, Th.; Freyberg, M. J.; Trümper, J.; Haberl, F.; Voges, W.; Nandra, K.

    2016-04-01

    Aims: We present the second ROSAT all-sky survey source catalogue, hereafter referred to as the 2RXS catalogue. This is the second publicly released ROSAT catalogue of point-like sources obtained from the ROSAT all-sky survey (RASS) observations performed with the position-sensitive proportional counter (PSPC) between June 1990 and August 1991, and is an extended and revised version of the bright and faint source catalogues. Methods: We used the latest version of the RASS processing to produce overlapping X-ray images of 6.4° × 6.4° sky regions. To create a source catalogue, a likelihood-based detection algorithm was applied to these, which accounts for the variable point-spread function (PSF) across the PSPC field of view. Improvements in the background determination compared to 1RXS were also implemented. X-ray control images showing the source and background extraction regions were generated, which were visually inspected. Simulations were performed to assess the spurious source content of the 2RXS catalogue. X-ray spectra and light curves were extracted for the 2RXS sources, with spectral and variability parameters derived from these products. Results: We obtained about 135 000 X-ray detections in the 0.1-2.4 keV energy band down to a likelihood threshold of 6.5, as adopted in the 1RXS faint source catalogue. Our simulations show that the expected spurious content of the catalogue is a strong function of detection likelihood, and the full catalogue is expected to contain about 30% spurious detections. A more conservative likelihood threshold of 9, on the other hand, yields about 71 000 detections with a 5% spurious fraction. We recommend thresholds appropriate to the scientific application. X-ray images and overlaid X-ray contour lines provide an additional user product to evaluate the detections visually, and we performed our own visual inspections to flag uncertain detections. Intra-day variability in the X-ray light curves was quantified based on the

  4. Euclid Star Catalogue Management for the Fine Guidance Sensor

    NASA Astrophysics Data System (ADS)

    2015-09-01

    The Fine Guidance Sensor is a key element of the AOCS subsystem for the Euclid spacecraft in order to achieve the required absolute pointing accuracy and pointing stability of the telescope Line of Sight. The Fine Guidance Sensor is able to give measure of the relative attitude with respect to the first attitude acquired and the measure of the absolute attitude with respect to the inertial reference frame through the use of an on-board Star Catalogue. The presence of at least 3 star-like objects per FoV is needed to compute the attitude; considering the small FGS FoV (0.1x0.1deg) the Star Catalogue shall be complete up to visual magnitude 19 to allow the correct coverage. The paper describes the implementation of the catalogue in the FGS design and the management of the big amount of data on ground, between ground and spacecraft, and on-board.

  5. Three editions of the star catalogue of Tycho Brahe. Machine-readable versions and comparison with the modern Hipparcos Catalogue

    NASA Astrophysics Data System (ADS)

    Verbunt, F.; van Gent, R. H.

    2010-06-01

    Tycho Brahe completed his catalogue with the positions and magnitudes of 1004 fixed stars in 1598. This catalogue circulated in manuscript form. Brahe edited a shorter version with 777 stars, printed in 1602, and Kepler edited the full catalogue of 1004 stars, printed in 1627. We provide machine-readable versions of the three versions of the catalogue, describe the differences between them and briefly discuss their accuracy on the basis of comparison with modern data from the Hipparcos Catalogue. We also compare our results with earlier analyses by Dreyer (1916, Tychonis Brahe Dani Scripta Astronomica, Vol. II) and Rawlins (1993, DIO, 3, 1), finding good overall agreement. The magnitudes given by Brahe correlate well with modern values, his longitudes and latitudes have error distributions with widths of 2´, with excess numbers of stars with larger errors (as compared to Gaussian distributions), in particular for the faintest stars. Errors in positions larger than ≃10´, which comprise about 15% of the entries, are likely due to computing or copying errors. The full tables KeplerE and Variants (see Table 4) and the table with the latin descriptions of the stars are available in electronic form only at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A28

  6. The DEEP2 Galaxy Redshift Survey: The Voronoi-Delaunay Method Catalog of Galaxy Groups

    SciTech Connect

    Gerke, Brian F.; Newman, Jeffrey A.; Davis, Marc; Marinoni, Christian; Yan, Renbin; Coil, Alison L.; Conroy, Charlie; Cooper, Michael C.; Faber, S.M.; Finkbeiner, Douglas P.; Guhathakurta, Puragra; Kaiser, Nick; Koo, David C.; Phillips, Andrew C.; Weiner, Benjamin J.; /Maryland U.

    2012-02-14

    We use the first 25% of the DEEP2 Galaxy Redshift Survey spectroscopic data to identify groups and clusters of galaxies in redshift space. The data set contains 8370 galaxies with confirmed redshifts in the range 0.7 {<=} z {<=} 1.4, over one square degree on the sky. Groups are identified using an algorithm (the Voronoi-Delaunay Method) that has been shown to accurately reproduce the statistics of groups in simulated DEEP2-like samples. We optimize this algorithm for the DEEP2 survey by applying it to realistic mock galaxy catalogs and assessing the results using a stringent set of criteria for measuring group-finding success, which we develop and describe in detail here. We find in particular that the group-finder can successfully identify {approx}78% of real groups and that {approx}79% of the galaxies that are true members of groups can be identified as such. Conversely, we estimate that {approx}55% of the groups we find can be definitively identified with real groups and that {approx}46% of the galaxies we place into groups are interloper field galaxies. Most importantly, we find that it is possible to measure the distribution of groups in redshift and velocity dispersion, n({sigma}, z), to an accuracy limited by cosmic variance, for dispersions greater than 350 km s{sup -1}. We anticipate that such measurements will allow strong constraints to be placed on the equation of state of the dark energy in the future. Finally, we present the first DEEP2 group catalog, which assigns 32% of the galaxies to 899 distinct groups with two or more members, 153 of which have velocity dispersions above 350 km s{sup -1}. We provide locations, redshifts and properties for this high-dispersion subsample. This catalog represents the largest sample to date of spectroscopically detected groups at z {approx} 1.

  7. Gamma-ray detected radio galaxies

    NASA Astrophysics Data System (ADS)

    Beckmann, Volker; Soldi, Simona; De Jong, Sandra; Kretschmer, Karsten; Savchenko, Volodymyr

    2016-07-01

    So far 15 radio galaxies have been detected in the gamma-ray domain by CGRO/EGRET and Fermi/LAT, with a few detections also in the VHE range. We search for distinguishing parameters and estimate the total number of gamma-ray emitting radio galaxies that are potentially detectable by Fermi/LAT. We use Fermi/LAT data in comparison with X-ray and hard X-ray data in order to constrain basic parameters such as the total power of the inverse Compton branch and the position of its peak. We search for possible correlations between the radio, UV, X-ray, and gamma-ray domain and derive the number counts distribution. We then compare their properties with those of the radio galaxies in the 3CRR and SMS4 catalogues. The data show no correlation between the peak of the inverse Compton emission and its luminosity. For the gamma-ray detected radio galaxies the luminosities in the various bands are correlated, except for the UV band, but there is no indication of a correlation of peak frequency or luminosity with the spectral slopes in the X-ray or gamma-ray band. The comparison with other bright radio galaxies shows that the gamma-ray detected objects are among those that have the largest X-ray but rather moderate radio fluxes. Their UV and X-ray luminosities are similar, but gamma-ray detected radio galaxies are predominantly of type FR-I, while the 3CRR sample contains mainly FR-II objects. The number counts of the so far gamma-ray detected radio galaxies shows a very shallow slope, indicating that potentially a fraction of radio galaxies has been missed so far or has not been identified as such, although the predicted number of 22 ± 7 is consistent with the observed 15 objects.

  8. Supervoids in the WISE-2MASS catalogue imprinting cold spots in the cosmic microwave background

    NASA Astrophysics Data System (ADS)

    Finelli, F.; García-Bellido, J.; Kovács, A.; Paci, F.; Szapudi, I.

    2016-01-01

    The Cold Spot (CS) is a clear feature in the cosmic microwave background (CMB); it could be of primordial origin, or caused by a intervening structure along the line of sight. We identified a large projected underdensity in the recently constructed WISE-2MASS all-sky infrared galaxy catalogue aligned with the CS direction at (l, b) ≈ (209°, -57°). It has an angular size of tens of degrees, and shows a ˜20 per cent galaxy underdensity in the centre. Moreover, we find another large underdensity in the projected WISE-2MASS galaxy map at (l, b) ≈ (101°, 46°) (hereafter Draco supervoid), also aligned with a CMB decrement, although less significant than that of the CS direction. Motivated by these findings, we develop spherically symmetric Lemaitre-Tolman-Bondi (LTB) compensated void models to explain the observed CMB decrements with these two underdensities, or `supervoids'. Within our perturbative treatment of the LTB voids, we find that the integrated Sachs-Wolfe and Riess-Sciama effects due to the Draco supervoid can account for the CMB decrement observed in the same direction. On the contrary, the extremely deep CMB decrement in the CS direction is more difficult to explain by the presence of the CS supervoid only. Nevertheless, the probability of a random alignment between the CS and the corresponding supervoid is disfavoured, and thus its contribution as a secondary anisotropy cannot be neglected. We comment on how the approximations used in this paper, in particular the assumption of spherical symmetry, could change quantitatively our conclusions and might provide a better explanation for the CMB CS.

  9. Towards a Next-Generation Catalogue Cross-Match Service

    NASA Astrophysics Data System (ADS)

    Pineau, F.; Boch, T.; Derriere, S.; Arches Consortium

    2015-09-01

    We have been developing in the past several catalogue cross-match tools. On one hand the CDS XMatch service (Pineau et al. 2011), able to perform basic but very efficient cross-matches, scalable to the largest catalogues on a single regular server. On the other hand, as part of the European project ARCHES1, we have been developing a generic and flexible tool which performs potentially complex multi-catalogue cross-matches and which computes probabilities of association based on a novel statistical framework. Although the two approaches have been managed so far as different tracks, the need for next generation cross-match services dealing with both efficiency and complexity is becoming pressing with forthcoming projects which will produce huge high quality catalogues. We are addressing this challenge which is both theoretical and technical. In ARCHES we generalize to N catalogues the candidate selection criteria - based on the chi-square distribution - described in Pineau et al. (2011). We formulate and test a number of Bayesian hypothesis which necessarily increases dramatically with the number of catalogues. To assign a probability to each hypotheses, we rely on estimated priors which account for local densities of sources. We validated our developments by comparing the theoretical curves we derived with the results of Monte-Carlo simulations. The current prototype is able to take into account heterogeneous positional errors, object extension and proper motion. The technical complexity is managed by OO programming design patterns and SQL-like functionalities. Large tasks are split into smaller independent pieces for scalability. Performances are achieved resorting to multi-threading, sequential reads and several tree data-structures. In addition to kd-trees, we account for heterogeneous positional errors and object's extension using M-trees. Proper-motions are supported using a modified M-tree we developed, inspired from Time Parametrized R-trees (TPR

  10. Radio emission from dusty galaxies observed by AKARI

    NASA Astrophysics Data System (ADS)

    Pepiak, A.; Pollo, A.; Takeuchi, T. T.; Solarz, A.; Jurusik, W.

    2014-10-01

    We probe radio-infrared correlation for two samples of extragalactic sources from the local Universe from the AKARI All-Sky Catalogue. The first, smaller sample (1053 objects) was constructed by the cross-correlation of the AKARI/FIS All-Sky Survey Bright Source Catalogue, the AKARI IRC All-Sky Survey Point Source Catalogue and the NRAO VLA Sky Survey, i.e. it consists of sources detected in the mid- and far-infrared by AKARI, and at the 1.4 GHz radio frequency by NRAO. The second, larger sample (13,324 objects) was constructed by the cross-correlation of only the AKARI/FIS All-Sky Survey Bright Source Catalogue and the NRAO VLA Sky Survey, i.e. it consists of sources detected in the far-infrared and radio, without a condition to be detected in the mid-infrared. Additionally, all objects in both samples were identified as galaxies in the NED and/or SIMBAD databases, and a part of them is known to host active galactic nuclei (AGNs). For the present analysis, we have restricted our samples only to sources with known redshift z. In this paper, we analyse the far-infrared-radio correlation for both of these samples. We compare the ratio of infrared and radio emission from normal star-forming dusty galaxies and AGNs in both samples. For the smaller sample we obtained =2.14 for AGNs and =2.27 for normal galaxies, while for the larger sample =2.15 for AGNs and =2.22 for normal galaxies. An average value of the slope in both samples is ~2.2, which is consistent with the previous measurements from the literature.

  11. Official 1996 Mock Trial Materials for the Twenty-Fourth Annual District of Columbia Public Schools Mock Trial Program. Kyle Wilkins, Plaintiff, v. New Columbia County School District, Defendant.

    ERIC Educational Resources Information Center

    Ashbrook, Alexandra M.

    This guide contains the 1996 mock trial materials for the District of Columbia mock trial program. The trial focuses on a high school student who died of a heart attack attributed to the use of steroids. The plaintiff, the student's father, alleges that the school, its principal, and track coach were negligent in the death because they failed to…

  12. Selecting background galaxies in weak-lensing analysis of galaxy clusters

    NASA Astrophysics Data System (ADS)

    Formicola, I.; Radovich, M.; Meneghetti, M.; Mazzotta, P.; Grado, A.; Giocoli, C.

    2016-05-01

    In this paper, we present a new method to select the faint, background galaxies used to derive the mass of galaxy clusters by weak lensing. The method is based on the simultaneous analysis of the shear signal, that should be consistent with zero for the foreground, unlensed galaxies, and of the colours of the galaxies: photometric data from the COSMic evOlution Survey are used to train the colour selection. In order to validate this methodology, we test it against a set of state-of-the-art image simulations of mock galaxy clusters in different redshift [0.23-0.45] and mass [0.5-1.55 × 1015 M⊙] ranges, mimicking medium-deep multicolour imaging observations [e.g. Subaru, Large Binocular Telescope]. The performance of our method in terms of contamination by unlensed sources is comparable to a selection based on photometric redshifts, which however requires a good spectral coverage and is thus much more observationally demanding. The application of our method to simulations gives an average ratio between estimated and true masses of ˜0.98 ± 0.09. As a further test, we finally apply our method to real data, and compare our results with other weak-lensing mass estimates in the literature: for this purpose, we choose the cluster Abell 2219 (z = 0.228), for which multiband (BVRi) data are publicly available.

  13. The Million Optical - Radio/X-ray Associations (MORX) Catalogue

    NASA Astrophysics Data System (ADS)

    Flesch, Eric W.

    2016-10-01

    This automated catalogue combines all the largest published optical, radio, and X-ray sky catalogues to find probable radio/X-ray associations to optical objects, plus double radio lobes, using uniform processing against all input data. The total count is 1 002 855 optical objects so presented. Each object is displayed with J2000 astrometry, optical and radio/X-ray identifiers, red and blue photometry, and calculated probabilities and optical field solutions of the associations. This is the third and final edition of this method.

  14. The Brera Multi-scale Wavelet ROSAT HRI source catalogue

    NASA Astrophysics Data System (ADS)

    Panzera, M. R.; Campana, S.; Covino, S.; Lazzati, D.; Mignani, R. P.; Moretti, A.; Tagliaferri, G.

    2003-02-01

    We present the Brera Multi-scale Wavelet ROSAT HRI source catalogue (BMW-HRI) derived from all ROSAT HRI pointed observations with exposure times longer than 100 s available in the ROSAT public archives. The data were analyzed automatically using a wavelet detection algorithm suited to the detection and characterization of both point-like and extended sources. This algorithm is able to detect and disentangle sources in very crowded fields and/or in the presence of extended or bright sources. Images have been also visually inspected after the analysis to ensure verification. The final catalogue, derived from 4303 observations, consists of 29 089 sources detected with a detection probability of >=4.2 sigma . For each source, the primary catalogue entries provide name, position, count rate, flux and extension along with the relative errors. In addition, results of cross-correlations with existing catalogues at different wavelengths (FIRST, IRAS, 2MASS and GSC2) are also reported. Some information is available on the web via the DIANA Interface. As an external check, we compared our catalogue with the previously available ROSHRICAT catalogue (both in its short and long versions) and we were able to recover, for the short version, ~ 90% of the entries. We computed the sky coverage of the entire HRI data set by means of simulations. The complete BMW-HRI catalogue provides a sky coverage of 732 deg2 down to a limiting flux of ~ 10-12 erg s-1 cm-2 and of 10 deg2 down to ~ 10-14 erg s-1 cm-2. We were able to compute the cosmological log(N)-log(S) distribution down to a flux of =~ 1.2 x 10-14 erg s-1 cm-2. The catalogue is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/399/351

  15. SPECTRAL IMAGING OF GALAXY CLUSTERS WITH PLANCK

    SciTech Connect

    Bourdin, H.; Mazzotta, P.; Rasia, E.

    2015-12-20

    The Sunyaev–Zeldovich (SZ) effect is a promising tool for detecting the presence of hot gas out to the galaxy cluster peripheries. We developed a spectral imaging algorithm dedicated to the SZ observations of nearby galaxy clusters with Planck, with the aim of revealing gas density anisotropies related to the filamentary accretion of materials, or pressure discontinuities induced by the propagation of shock fronts. To optimize an unavoidable trade-off between angular resolution and precision of the SZ flux measurements, the algorithm performs a multi-scale analysis of the SZ maps as well as of other extended components, such as the cosmic microwave background (CMB) anisotropies and the Galactic thermal dust. The demixing of the SZ signal is tackled through kernel-weighted likelihood maximizations. The CMB anisotropies are further analyzed through a wavelet analysis, while the Galactic foregrounds and SZ maps are analyzed via a curvelet analysis that best preserves their anisotropic details. The algorithm performance has been tested against mock observations of galaxy clusters obtained by simulating the Planck High Frequency Instrument and by pointing at a few characteristic positions in the sky. These tests suggest that Planck should easily allow us to detect filaments in the cluster peripheries and detect large-scale shocks in colliding galaxy clusters that feature favorable geometry.

  16. Measuring neutrino masses with a future galaxy survey

    SciTech Connect

    Hamann, Jan; Hannestad, Steen; Wong, Yvonne Y.Y. E-mail: sth@phys.au.dk

    2012-11-01

    We perform a detailed forecast on how well a EUCLID-like photometric galaxy and cosmic shear survey will be able to constrain the absolute neutrino mass scale. Adopting conservative assumptions about the survey specifications and assuming complete ignorance of the galaxy bias, we estimate that the minimum mass sum of Σm{sub ν} ≅ 0.06 eV in the normal hierarchy can be detected at 1.5σ to 2.5σ significance, depending on the model complexity, using a combination of galaxy and cosmic shear power spectrum measurements in conjunction with CMB temperature and polarisation observations from PLANCK. With better knowledge of the galaxy bias, the significance of the detection could potentially reach 5.4σ. Interestingly, neither PLANCK+shear nor PLANCK+galaxy alone can achieve this level of sensitivity; it is the combined effect of galaxy and cosmic shear power spectrum measurements that breaks the persistent degeneracies between the neutrino mass, the physical matter density, and the Hubble parameter. Notwithstanding this remarkable sensitivity to Σm{sub ν}, EUCLID-like shear and galaxy data will not be sensitive to the exact mass spectrum of the neutrino sector; no significant bias ( < 1σ) in the parameter estimation is induced by fitting inaccurate models of the neutrino mass splittings to the mock data, nor does the goodness-of-fit of these models suffer any significant degradation relative to the true one (Δχ{sub eff}{sup 2} < 1)

  17. Hipparcos to deliver its final results catalogue soon

    NASA Astrophysics Data System (ADS)

    1995-10-01

    them, almost 30 years ago, to propose carrying out these observations from the relatively benign environment of space. Hipparcos is, by present standards, a medium-sized satellite, with a 30 cm telescope sensing simply ordinary light. But it has been described as the most imaginative in the short history of space astronomy. This foresight has been amply repaid. In the long history of stargazing it ranks with the surveys by Hipparchus the Greek in the 2nd Century BC and by Tichy Brahe the Dane in the 16th Century AD, both of which transformed human perceptions of the Universe. Positions derived from the Hipparcos satellite are better than a millionth of a degree, and newly a thousand times more accurate than star positions routinely determined from he ground. This accuracy makes it possible to measure directly the distances to the stars. While it took 250 years between astronomers first setting out on the exacting task of measuring the distance to a star, and a stellar distance being measured for the first time, ESA's Hipparcos mission has revolutionised this long, painstaking, and fundamental task by measuring accurate distances and movements of more than one hundred thousand. The measurement concept involved he satellite triangulating its way between he stars all wound the sky, building up a celestial map in much the same way as land surveyors use triangulation between hill-tops to measure distances accurately. Only the angles involved are much smaller : the accuracy that has been achieved with the Hipparcos Catalogue is such that he two edges of a coin, viewed from he other side of the Atlantic Ocean, could be distinguished. The results from Hipparcos will deliver scientists with long-awaited details of our place in he Milky Way Galaxy. Most of he stars visible to the naked eye are, to a large extent, companions of the Sun, in a great orbital march around the centre of the Galaxy, a journey so long that it takes individual stars 250 million years to complete, in

  18. Galaxy Zoo: reproducing galaxy morphologies via machine learning

    NASA Astrophysics Data System (ADS)

    Banerji, Manda; Lahav, Ofer; Lintott, Chris J.; Abdalla, Filipe B.; Schawinski, Kevin; Bamford, Steven P.; Andreescu, Dan; Murray, Phil; Raddick, M. Jordan; Slosar, Anze; Szalay, Alex; Thomas, Daniel; Vandenberg, Jan

    2010-07-01

    We present morphological classifications obtained using machine learning for objects in the Sloan Digital Sky Survey DR6 that have been classified by Galaxy Zoo into three classes, namely early types, spirals and point sources/artefacts. An artificial neural network is trained on a subset of objects classified by the human eye, and we test whether the machine-learning algorithm can reproduce the human classifications for the rest of the sample. We find that the success of the neural network in matching the human classifications depends crucially on the set of input parameters chosen for the machine-learning algorithm. The colours and parameters associated with profile fitting are reasonable in separating the objects into three classes. However, these results are considerably improved when adding adaptive shape parameters as well as concentration and texture. The adaptive moments, concentration and texture parameters alone cannot distinguish between early type galaxies and the point sources/artefacts. Using a set of 12 parameters, the neural network is able to reproduce the human classifications to better than 90 per cent for all three morphological classes. We find that using a training set that is incomplete in magnitude does not degrade our results given our particular choice of the input parameters to the network. We conclude that it is promising to use machine-learning algorithms to perform morphological classification for the next generation of wide-field imaging surveys and that the Galaxy Zoo catalogue provides an invaluable training set for such purposes. This publication has been made possible by the participation of more than 100000 volunteers in the Galaxy Zoo project. Their contributions are individually acknowledged at http://www.galaxyzoo.org/Volunteers.aspx. E-mail: mbanerji@ast.cam.ac.uk ‡ Einstein Fellow.

  19. Galaxy clusters as probes for cosmology and dark matter

    NASA Astrophysics Data System (ADS)

    Battistelli, Elia S.; Burigana, Carlo; de Bernardis, Paolo; Kirillov, Alexander A.; Neto, Gastao B. Lima; Masi, Silvia; Norgaard-Nielsen, Hans U.; Ostermann, Peter; Roman, Matthieu; Rosati, Piero; Rossetti, Mariachiara

    2016-07-01

    In recent years, significant progress has been made in building new galaxy clusters samples, at low and high redshifts, from wide-area surveys, particularly exploiting the Sunyaev-Zel’dovich (SZ) effect. A large effort is underway to identify and characterize these new systems with optical/NIR and X-ray facilities, thus opening new avenues to constraint cosmological models using structure growth and geometrical tests. A census of galaxy clusters sets constraints on reionization mechanisms and epochs, which need to be reconciled with recent limits on the reionization optical depth from cosmic microwave background (CMB) experiments. Future advances in SZ effect measurements will include the possibility to (unambiguously) measure directly the kinematic SZ effect, to build an even larger catalogue of galaxy clusters able to study the high redshift universe, and to make (spatially-)resolved galaxy cluster maps with even spectral capability to (spectrally-)resolve the relativistic corrections of the SZ effect.

  20. Study of the Lynx-Cancer void galaxies. - V. The extremely isolated galaxy UGC 4722

    NASA Astrophysics Data System (ADS)

    Chengalur, J. N.; Pustilnik, S. A.; Makarov, D. I.; Perepelitsyna, Y. A.; Safonova, E. S.; Karachentsev, I. D.

    2015-04-01

    We present a detailed study of the extremely isolated Sdm galaxy UGC 4722 (MB = -17.4) located in the nearby Lynx-Cancer void. UGC 4722 is a member of the Catalogue of Isolated Galaxies, and has also been identified as one of the most isolated galaxies in the Local Supercluster. Optical images of the galaxy however show that it has a peculiar morphology with an elongated ˜14 kpc-long plume. New observations with the Russian 6-m telescope (BTA) and the Giant Metrewave Radio Telescope (GMRT) of the ionized and neutral gas in UGC 4722 reveal the second component responsible for the disturbed morphology of the system. This is a small, almost completely destroyed, very gas-rich dwarf (MB = -15.2, M(H I)/LB ˜ 4.3) We estimate the oxygen abundance for both galaxies to be 12 + log (O/H) ˜ 7.5-7.6 which is two to three times lower than what is expected from the luminosity-metallicity relation for similar galaxies in denser environments. The ugr colours of the plume derived from Sloan Digital Sky Survey (SDSS) images are consistent with a simple stellar population with a post starburst age of 0.45-0.5 Gyr. This system hence appears to be the first known case of a minor merger with a prominent tidal feature consisting of a young stellar population.

  1. MCMC Analysis of biases in the interpretation of disk galaxy kinematics

    NASA Astrophysics Data System (ADS)

    Aquino-Ortíz, E.; Valenzuela, O.; Cano-Díaz, M.; Sánchez-Sánchez, S. F.; Hernández-Toledo, H.

    2016-06-01

    The new generation of galaxy surveys like SAMI, CALIFA and MaNGA opens up the possibility of studying simultaneously properties of galaxies such as spiral arms, bars, disk geometry and orientation, stellar and gas mass distribution, 2D kinematics, etc. The previous task involves exploring a complicated multi-dimensional parameter space. Puglielli et al. (2010) introduced Bayesian statistics and MCMC (Monte Carlo Markov Chain) techniques to construct dynamical models of spiral galaxies. In our study we used synthetic velocity fields that include non-circular motions and assume different disk orientations in order to produce mock observations. We apply popular reconstruction techniques in order to estimate the geometrical disk parameters, systemic velocities, rotation curve shape and maximum circular velocity which are crucial to construct the scaling relations. We conclude that a detailed analysis of kinematics in galaxies using MCMC technique will be reflected in accurate estimations of galaxy properties and more robust scalings relations, otherwise physical conclusions may be importantly biased.

  2. State of Oklahoma v. Tracy Smith. 1999-2000 Oklahoma High School Mock Trial Program.

    ERIC Educational Resources Information Center

    Stucky, Melanie; Eberle, April; Cale, Stephen

    This mock trial curriculum is intended to help high school students learn about the law and the legal system. The curriculum is divided into the following sections: Statement of the Case, Stipulations, Legal Authorities, Witness Statements/Narrative Report (Prosecution Witnesses; Defense Witnesses), and Exhibits (Statement of Miranda Rights; Front…

  3. Seeing is Believing: Video Mock-Ups to Evaluate and Demonstrate Multimedia Designs

    ERIC Educational Resources Information Center

    Fadde, Peter J.

    2007-01-01

    A video mock-up is a "design story", described by Patrick Parrish in a recent "TechTrends" article as "imagining the journey of a learner's experience in engaging with a finished design". A design story allows designers to show their design vision to others and to observe features and benefits of the program as a learner would experience it. The…

  4. Effects of Detail in Eyewitness Testimony on Decisions by Mock Jurors.

    ERIC Educational Resources Information Center

    Heath, Wendy P.; Grannemann, Bruce D.; Sawa, Stephanie E.; Hodge, Kristine M.

    1997-01-01

    Investigated the effects of the presence and typicality of detail in a witness' testimony on mock juror judgments. Results indicate that the presence of detail affected the ratings of witnesses. Atypical or typical detail provided by one witness, with no detail provided by the opposing witness, enhanced assessments of the former. (RJM)

  5. The Florida High School Mock Trial Competition Case Materials, 1997. State of Florida v. Lee Appleman.

    ERIC Educational Resources Information Center

    Florida Law Related Education Association, Tallahassee.

    This material provides students with information to prepare for a mock trial. The defendant in this case has been accused of the crime of driving under the influence of alcoholic beverages causing severe bodily injury. Case materials include stipulated facts, jury instructions, depositions, and other related materials. (EH)

  6. Mock and National Examinations Correlations in a Health Information Associate Degree Program

    ERIC Educational Resources Information Center

    Jenkins, Neisa R.

    2013-01-01

    Students enrolled in associate degree programs face social and personal challenges that can affect their learning and assessment skills. Social and personal challenges such as unemployment rates, race, age, and gender may affect their employability. The purpose of this quantitative correlational study was to examine the mock and national…

  7. "Francine, Kerplunk, and the Golden Nugget" -- Conducting Mock Trials and Debates in the Classroom.

    ERIC Educational Resources Information Center

    Beck, Charles R.

    1999-01-01

    Describes the process for creating a mock trial based on the fable "Francine, Kerplunk, and the Golden Nugget." Explains that during the jury deliberations the jurors utilize chart structures to assess the credibility of the witness' testimony and the attorney's arguments. Maintains that chart structures can also be adapted to classroom debates.…

  8. Mechanical Characterization of the Iter Mock-Up Insulation after Reactor Irradiation

    NASA Astrophysics Data System (ADS)

    Prokopec, R.; Humer, K.; Fillunger, H.; Maix, R. K.; Weber, H. W.

    2010-04-01

    The ITER mock-up project was launched in order to demonstrate the feasibility of an industrial impregnation process using the new cyanate ester/epoxy blend. The mock-up simulates the TF winding pack cross section by a stainless steel structure with the same dimensions as the TF winding pack at a length of 1 m. It consists of 7 plates simulating the double pancakes, each of them is wrapped with glass fiber/Kapton sandwich tapes. After stacking the 7 plates, additional insulation layers are wrapped to simulate the ground insulation. This paper presents the results of the mechanical quality tests on the mock-up pancake insulation. Tensile and short beam shear specimens were cut from the plates extracted from the mock-up and tested at 77 K using a servo-hydraulic material testing device. All tests were repeated after reactor irradiation to a fast neutron fluence of 1×1022 m-2 (E>0.1 MeV). In order to simulate the pulsed operation of ITER, tension-tension fatigue measurements were performed in the load controlled mode. Initial results show a high mechanical strength as expected from the high number of thin glass fiber layers, and an excellent homogeneity of the material.

  9. MECHANICAL CHARACTERIZATION OF THE ITER MOCK-UP INSULATION AFTER REACTOR IRRADIATION

    SciTech Connect

    Prokopec, R.; Humer, K.; Fillunger, H.; Maix, R. K.; Weber, H. W.

    2010-04-08

    The ITER mock-up project was launched in order to demonstrate the feasibility of an industrial impregnation process using the new cyanate ester/epoxy blend. The mock-up simulates the TF winding pack cross section by a stainless steel structure with the same dimensions as the TF winding pack at a length of 1 m. It consists of 7 plates simulating the double pancakes, each of them is wrapped with glass fiber/Kapton sandwich tapes. After stacking the 7 plates, additional insulation layers are wrapped to simulate the ground insulation. This paper presents the results of the mechanical quality tests on the mock-up pancake insulation. Tensile and short beam shear specimens were cut from the plates extracted from the mock-up and tested at 77 K using a servo-hydraulic material testing device. All tests were repeated after reactor irradiation to a fast neutron fluence of 1x10{sup 22} m{sup -2}(E>0.1 MeV). In order to simulate the pulsed operation of ITER, tension-tension fatigue measurements were performed in the load controlled mode. Initial results show a high mechanical strength as expected from the high number of thin glass fiber layers, and an excellent homogeneity of the material.

  10. Speaking with (Dis)respect: A Study of Reactions to Mock Spanish

    ERIC Educational Resources Information Center

    Callahan, Laura

    2010-01-01

    This paper reports on an investigation into the reactions of 147 participants of various ethnicities to a language practice in the USA that has been characterized as Mock Spanish, a special register in which Spanish words or phrases are used to evoke humor by indexing an often unflattering image of Spanish speakers. Research questions include…

  11. The Trial of Napoleon: A Case Study for Using Mock Trials.

    ERIC Educational Resources Information Center

    MacKay, Charles

    2000-01-01

    Describes a course entitled "The Trial of Napoleon Bonaparte" that focuses on a fictitious mock trial of Napoleon Bonaparte to answer the question: did Napoleon pervert or preserve the gain of the French Revolution? Discusses the strengths and weaknesses of the course. (CMK)

  12. Town vs. gown: a direct comparison of community residents and student mock jurors.

    PubMed

    Hosch, Harmon M; Culhane, Scott E; Tubb, V Anne; Granillo, Edgar A

    2011-01-01

    The use of students as mock jurors in the majority of legal psychology studies on jury behavior has been criticized (e.g., Bray & Kerr, 1979; Diamond, 1997). This study examined the degree to which student mock jurors' decisions were generalizable to those of real jurors. The participants of the study included 297 jury-eligible university students and 297 volunteers from the venire in the same community as that in which the students resided. All participants viewed one of six versions of a videotaped criminal trial. The defendant testified in English or in Spanish. In addition, the race of defendant was varied. Three bilingual individuals served as defendants with one appearing to be of northern European origin, one of Latino background, and one of African origin. Dependent variables included verdict and, for those who found the defendant guilty, the number of years to which he should be sentenced, and whether he should be fined. Student mock jurors differed reliably from their community counterparts on several demographic characteristics. However, the two groups had mixed results in relation to decision-making tasks. There was no difference in individual verdict preferences, but the students' sentence recommendations were more punitive. These results are interpreted in the context of the generalizability of mock juror studies.

  13. Bling My Research! A Mock Grant Panel Activity Illustrating the Importance of Basic Research

    ERIC Educational Resources Information Center

    Leander, Celeste A.; Whitton, Jeannette

    2010-01-01

    First-year university students have misconceptions about the source and dynamics of publicly funded research money. We designed an activity in which students take part in a mock grant panel. The results indicated a strong tendency toward student funding of applied medical research at the expense of basic research. Exposure to a few examples of…

  14. Millimeter wave experiment of ITER equatorial EC launcher mock-up

    SciTech Connect

    Takahashi, K.; Oda, Y.; Kajiwara, K.; Kobayashi, N.; Isozaki, M.; Sakamoto, K.; Omori, T.; Henderson, M.

    2014-02-12

    The full-scale mock-up of the equatorial launcher was fabricated in basis of the baseline design to investigate the mm-wave propagation properties of the launcher, the manufacturability, the cooling line management, how to assemble the components and so on. The mock-up consists of one of three mm-wave transmission sets and one of eight waveguide lines can deliver the mm-wave power. The mock-up was connected to the ITER compatible transmission line and the 170GHz gyrotron and the high power experiment was carried out. The measured radiation pattern of the beam at the location of 2.5m away from the EL mock-up shows the successful steering capability of 20°∼40°. It was also revealed that the radiated profile at both steering and fixed focusing mirror agreed with the calculation. The result also suggests that some unwanted modes are included in the radiated beam. Transmission of 0.5MW-0.4sec and of 0.12MW-50sec were also demonstrated.

  15. Using mock trials to teach students forensic core competencies in marriage and family therapy.

    PubMed

    Miller, John K; Linville, Deanna; Todahl, Jeff; Metcalfe, Joe

    2009-10-01

    This article provides a description of a university-based project that used mock trials to train both practicum-level marriage and family therapy and law students in forensic work, and a qualitative investigation of student experiences with the training. The content of the training focused on American Association for Marriage and Family Therapy (AAMFT) core competencies that relate specifically to the legal aspects of therapy. This article describes the didactic training the students received to prepare for the mock trials, the structure and protocol of the mock trials themselves, and the specific AAMFT core competencies addressed in the project. The results of an analysis of focus group interviews with participating law school (n = 15) and marriage and family therapy (n = 19) students are presented as well as the results of a 36-item Knowledge, Skills, and Comfort Level Questionnaire completed by participating marriage and family therapy students. Participants discussed the value of the training with regard to preparation for mock trial procedures, preparation for testimony, importance of documentation, and cross-discipline collaboration issues. The article concludes with a discussion of how this type of training may be used in developing students' skills with regard to forensic and legal core competencies, and future research directions.

  16. The Mock Trial: A Dynamic Exercise for Thinking Critically about Management Theories, Topics, and Practices

    ERIC Educational Resources Information Center

    Farmer, Kevin; Meisel, Steven I.; Seltzer, Joe; Kane, Kathleen

    2013-01-01

    The Mock Trial is an experiential exercise adapted from a law school process that encourages students to think critically about theories, topics, and the practice of management in an innovative classroom experience. Playing the role of attorneys and witnesses, learners ask questions and challenge assumptions by playing roles in a trial with…

  17. Order of Verdict Consideration and Decision Rule Effects on Mock Jury Decision Making.

    ERIC Educational Resources Information Center

    Olaye, Imafidon M.

    A study investigated the effects of order verdict consideration and decision rule on jury verdicts. After reading the summary of an actual trial, 240 mock jurors drawn from undergraduate communications classes were randomly assigned to six-member juries. Jury assignments were made under two verdict orders (ascending and descending order of…

  18. Statement of Facts for 1977 City-Wide Mock Trial Competitions. Walker Thomas v. Sam Nomad.

    ERIC Educational Resources Information Center

    National Inst. for Citizen Education in the Law, Washington, DC.

    Prepared by the District of Columbia Street Law Project for its annual city-wide mock trial competition, this instructional handout provides material for a civil case over an automobile accident. Walker Thomas is suing Sam Nomad for damages that resulted from a collision, for which both parties blame the other. The handout clarifies the laws and…

  19. Data-Based Active Learning in the Principles of Macroeconomics Course: A Mock FOMC Meeting

    ERIC Educational Resources Information Center

    Whiting, Cathleen

    2006-01-01

    The author presents an active-learning exercise for the introductory macroeconomics class in which students participate in a mock Federal Open Market Committee (FOMC) meeting. Preparation involves data gathering and writing both a research report and a policy recommendation. An FOMC meeting is simulated in which students give their policy…

  20. Using Mock Trials to Teach Students Forensic Core Competencies in Marriage and Family Therapy

    ERIC Educational Resources Information Center

    Miller, John K.; Linville, Deanna; Todahl, Jeff; Metcalfe, Joe

    2009-01-01

    This article provides a description of a university-based project that used mock trials to train both practicum-level marriage and family therapy and law students in forensic work, and a qualitative investigation of student experiences with the training. The content of the training focused on American Association for Marriage and Family Therapy…

  1. NUV signatures of environment driven galaxy quenching in SDSS groups

    NASA Astrophysics Data System (ADS)

    Crossett, Jacob P.; Pimbblet, Kevin A.; Jones, D. Heath; Brown, Michael J. I.; Stott, John P.

    2016-09-01

    We have investigated the effect of group environment on residual star formation in galaxies, using GALEX NUV galaxy photometry with the SDSS group catalogue of Yang et al. (2007). We compared the (NUV - r) colours of grouped and non-grouped galaxies, and find a significant increase in the fraction of red sequence galaxies with blue (NUV - r) colours outside of groups. When comparing galaxies in mass matched samples of satellite (non-central), and non-grouped galaxies, we found a >4σ difference in the distribution of (NUV - r) colours, and an (NUV - r) blue fraction >3σ higher outside groups. A comparison of satellite and non-grouped samples has found the NUV fraction is a factor of ˜2 lower for satellite galaxies between 1010.5M⊙ and 1010.7M⊙, showing that higher mass galaxies are more able to form stars when not influenced by a group potential. There was a higher (NUV - r) blue fraction of galaxies with lower Sérsic indices (n < 3) outside of groups, not seen in the satellite sample. We have used stellar population models of Bruzual & Charlot (2003) with multiple burst, or exponentially declining star formation histories to find that many of the (NUV - r) blue non-grouped galaxies can be explained by a slow (˜2 Gyr) decay of star formation, compared to the satellite galaxies. We suggest that taken together, the difference in (NUV - r) colours between samples can be explained by a population of secularly evolving, non-grouped galaxies, where star formation declines slowly. This slow channel is less prevalent in group environments where more rapid quenching can occur.

  2. The fate of high-redshift massive compact galaxies

    NASA Astrophysics Data System (ADS)

    de la Rosa, Ignacio G.; La Barbera, Francesco; Ferreras, Ignacio; Sánchez Almeida, Jorge; Dalla Vecchia, Claudio; Martínez-Valpuesta, Inma; Stringer, Martin

    2016-04-01

    Massive high-redshift quiescent compact galaxies (nicknamed red nuggets) have been traditionally connected to present-day elliptical galaxies, often overlooking the relationships that they may have with other galaxy types. We use large bulge-disc decomposition catalogues based on the Sloan Digital Sky Survey to check the hypothesis that red nuggets have survived as compact cores embedded inside the haloes or discs of present-day massive galaxies. In this study, we designate a compact core as the bulge component that satisfies a prescribed compactness criterion. Photometric and dynamic mass-size and mass-density relations are used to show that, in the inner regions of galaxies at z ˜ 0.1, there are abundant compact cores matching the peculiar properties of the red nuggets, an abundance comparable to that of red nuggets at z ˜ 1.5. Furthermore, the morphology distribution of the present-day galaxies hosting compact cores is used to demonstrate that, in addition to the standard channel connecting red nuggets with elliptical galaxies, a comparable fraction of red nuggets might have ended up embedded in discs. This result generalizes the inside-out formation scenario; present-day massive galaxies can begin as dense spheroidal cores (red nuggets), around which either a spheroidal halo or a disc is formed later.

  3. Eighteenth Century Short Title Catalogue on CD-ROM.

    ERIC Educational Resources Information Center

    Richey, Debora J.

    The Eighteenth Century Short Title Catalogue (ESTC) on compact disc provides access to nearly 300,000 printed materials from Britain and the British colonies from 1701 to 1800. The file contains a wide variety of materials (laws, almanacs, posters, catalogs, directories, verses, monographs, advertisements, and flyers) in all languages, and covers…

  4. Modelling and Implementation of Catalogue Cards Using FreeMarker

    ERIC Educational Resources Information Center

    Radjenovic, Jelen; Milosavljevic, Branko; Surla, Dusan

    2009-01-01

    Purpose: The purpose of this paper is to report on a study involving the specification (using Unified Modelling Language (UML) 2.0) of information requirements and implementation of the software components for generating catalogue cards. The implementation in a Java environment is developed using the FreeMarker software.…

  5. Restful Implementation of Catalogue Service for Geospatial Data Provenance

    NASA Astrophysics Data System (ADS)

    Jiang, L. C.; Yue, P.; Lu, X. C.

    2013-10-01

    Provenance, also known as lineage, is important in understanding the derivation history of data products. Geospatial data provenance helps data consumers to evaluate the quality and reliability of geospatial data. In a service-oriented environment, where data are often consumed or produced by distributed services, provenance could be managed by following the same service-oriented paradigm. The Open Geospatial Consortium (OGC) Catalogue Service for the Web (CSW) is used for the registration and query of geospatial data provenance by extending ebXML Registry Information Model (ebRIM). Recent advance of the REpresentational State Transfer (REST) paradigm has shown great promise for the easy integration of distributed resources. RESTful Web Service aims to provide a standard way for Web clients to communicate with servers based on REST principles. The existing approach for provenance catalogue service could be improved by adopting the RESTful design. This paper presents the design and implementation of a catalogue service for geospatial data provenance following RESTful architecture style. A middleware named REST Converter is added on the top of the legacy catalogue service to support a RESTful style interface. The REST Converter is composed of a resource request dispatcher and six resource handlers. A prototype service is developed to demonstrate the applicability of the approach.

  6. Catalogue of the Lichenized and Lichenicolous Fungi of Montenegro

    PubMed Central

    Knežević, Branka; Mayrhofer, Helmut

    2011-01-01

    Summary The catalogue is based on a comprehensive evaluation of 169 published sources. The lichen mycota as currently known from Montenegro includes 681 species (with eight subspecies, nine varieties and one form) of lichenized fungi, 12 species of lichenicolous fungi, and nine non-lichenized fungi traditionally included in lichenological literature. PMID:21423858

  7. A reference gene catalogue of the pig gut microbiome.

    PubMed

    Xiao, Liang; Estellé, Jordi; Kiilerich, Pia; Ramayo-Caldas, Yuliaxis; Xia, Zhongkui; Feng, Qiang; Liang, Suisha; Pedersen, Anni Øyan; Kjeldsen, Niels Jørgen; Liu, Chuan; Maguin, Emmanuelle; Doré, Joël; Pons, Nicolas; Le Chatelier, Emmanuelle; Prifti, Edi; Li, Junhua; Jia, Huijue; Liu, Xin; Xu, Xun; Ehrlich, Stanislav D; Madsen, Lise; Kristiansen, Karsten; Rogel-Gaillard, Claire; Wang, Jun

    2016-09-19

    The pig is a major species for livestock production and is also extensively used as the preferred model species for analyses of a wide range of human physiological functions and diseases(1). The importance of the gut microbiota in complementing the physiology and genome of the host is now well recognized(2). Knowledge of the functional interplay between the gut microbiota and host physiology in humans has been advanced by the human gut reference catalogue(3,4). Thus, establishment of a comprehensive pig gut microbiome gene reference catalogue constitutes a logical continuation of the recently published pig genome(5). By deep metagenome sequencing of faecal DNA from 287 pigs, we identified 7.7 million non-redundant genes representing 719 metagenomic species. Of the functional pathways found in the human catalogue, 96% are present in the pig catalogue, supporting the potential use of pigs for biomedical research. We show that sex, age and host genetics are likely to influence the pig gut microbiome. Analysis of the prevalence of antibiotic resistance genes demonstrated the effect of eliminating antibiotics from animal diets and thereby reducing the risk of spreading antibiotic resistance associated with farming systems.

  8. A reference gene catalogue of the pig gut microbiome.

    PubMed

    Xiao, Liang; Estellé, Jordi; Kiilerich, Pia; Ramayo-Caldas, Yuliaxis; Xia, Zhongkui; Feng, Qiang; Liang, Suisha; Pedersen, Anni Øyan; Kjeldsen, Niels Jørgen; Liu, Chuan; Maguin, Emmanuelle; Doré, Joël; Pons, Nicolas; Le Chatelier, Emmanuelle; Prifti, Edi; Li, Junhua; Jia, Huijue; Liu, Xin; Xu, Xun; Ehrlich, Stanislav D; Madsen, Lise; Kristiansen, Karsten; Rogel-Gaillard, Claire; Wang, Jun

    2016-01-01

    The pig is a major species for livestock production and is also extensively used as the preferred model species for analyses of a wide range of human physiological functions and diseases(1). The importance of the gut microbiota in complementing the physiology and genome of the host is now well recognized(2). Knowledge of the functional interplay between the gut microbiota and host physiology in humans has been advanced by the human gut reference catalogue(3,4). Thus, establishment of a comprehensive pig gut microbiome gene reference catalogue constitutes a logical continuation of the recently published pig genome(5). By deep metagenome sequencing of faecal DNA from 287 pigs, we identified 7.7 million non-redundant genes representing 719 metagenomic species. Of the functional pathways found in the human catalogue, 96% are present in the pig catalogue, supporting the potential use of pigs for biomedical research. We show that sex, age and host genetics are likely to influence the pig gut microbiome. Analysis of the prevalence of antibiotic resistance genes demonstrated the effect of eliminating antibiotics from animal diets and thereby reducing the risk of spreading antibiotic resistance associated with farming systems. PMID:27643971

  9. VizieR Online Data Catalog: MEXSAS catalogue (Vagnetti+, 2016)

    NASA Astrophysics Data System (ADS)

    Vagnetti, F.; Middei, R.; Antonucci, M.; Paolillo, M.; Serafinelli, R.

    2016-08-01

    We present the catalog of the Multi-Epoch XMM Serendipitous AGN Sample (MEXSAS), extracted from the fifth release of the XMM-Newton Serendipitous Source Catalogue (XMMSSC-DR5) and cross-matched with the Sloan Digital Sky Survey Quasar catalogs DR7Q and DR12Q. It contains 2700 repeatedly observed AGN, with corrected excess variance information. (1 data file).

  10. The BMW-Chandra survey. Serendipitous Source Catalogue

    NASA Astrophysics Data System (ADS)

    Romano, P.; Mignani, R. P.; Campana, S.; Moretti, A.; Panzera, M. R.; Tagliaferri, G.; Mottini, M.

    2009-07-01

    We present the BMW-Chandra source catalogue derived from Chandra ACIS-I observations (exposure time > 10ks) public as of March 2003 by using a wavelet detection algorithm (Lazzati et al. 1999; Campana et al. 1999). The catalogue contains a total of 21325 sources, 16758 of which are serendipitous. Our sky coverage in the soft band (0.5-2keV, S/N=3) is ~ 8 deg2 for FX ≥ 10-13 erg cm-2 s-1, and ~ 2 deg2 for FX ≥ 10-15 erg cm-2 s-1. The catalogue contains information on positions, count rates (and errors) in three energy bands (total, 0.5-7keV; soft, 0.5-2keV; and hard, 2-7keV), and in four additional energy bands, SB1 (0.5-1keV), SB2 (1-2keV), HB1 (2-4keV), and HB2 (4-7keV), as well as information on the source extension, and cross-matches with the FIRST, IRAS, 2MASS, and GSC-2 catalogues.

  11. 12. Photocopy of photograph (from Catalogue of Drugs, Chemicals, Proprietary ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    12. Photocopy of photograph (from Catalogue of Drugs, Chemicals, Proprietary Medicines, Pharmaceutical Preparations, Druggists' Sundries, Etc. Portland, ME: Cook, Everett, and Pennell, 1896.) ca. 1896, photographer unknown 'MAIN OFFICE AND COUNTING ROOM' - Woodman Building, 140 Middle Street, Portland, Cumberland County, ME

  12. 11. Photocopy of photograph (from Catalogue of Drugs, Chemicals, Proprietary ...

    Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

    11. Photocopy of photograph (from Catalogue of Drugs, Chemicals, Proprietary Medicines, Pharmaceutical Preparations, Druggists' Sundries, Etc. Portland, ME: Cook, Everett, and Pennell, 1896.) ca. 1896, photographer unknown 'SECTION OF MAIN FLOOR AND ORDER DEPARTMENT' - Woodman Building, 140 Middle Street, Portland, Cumberland County, ME

  13. An empirical model to form and evolve galaxies in dark matter halos

    NASA Astrophysics Data System (ADS)

    Li, Shi-Jie; Zhang, You-Cai; Yang, Xiao-Hu; Wang, Hui-Yuan; Tweed, Dylan; Liu, Cheng-Ze; Yang, Lei; Shi, Feng; Lu, Yi; Luo, Wen-Tao; Wei, Jian-Wen

    2016-08-01

    Based on the star formation histories of galaxies in halos with different masses, we develop an empirical model to grow galaxies in dark matter halos. This model has very few ingredients, any of which can be associated with observational data and thus be efficiently assessed. By applying this model to a very high resolution cosmological N-body simulation, we predict a number of galaxy properties that are a very good match to relevant observational data. Namely, for both centrals and satellites, the galaxy stellar mass functions up to redshift z ≃ 4 and the conditional stellar mass functions in the local universe are in good agreement with observations. In addition, the two point correlation function is well predicted in the different stellar mass ranges explored by our model. Furthermore, after applying stellar population synthesis models to our stellar composition as a function of redshift, we find that the luminosity functions in the 0.1 u, 0.1 g, 0.1 r, 0.1 i and 0.1 z bands agree quite well with the SDSS observational results down to an absolute magnitude at about -17.0. The SDSS conditional luminosity function itself is predicted well. Finally, the cold gas is derived from the star formation rate to predict the HI gas mass within each mock galaxy. We find a remarkably good match to observed HI-to-stellar mass ratios. These features ensure that such galaxy/gas catalogs can be used to generate reliable mock redshift surveys.

  14. An empirical model to form and evolve galaxies in dark matter halos

    NASA Astrophysics Data System (ADS)

    Li, Shi-Jie; Zhang, You-Cai; Yang, Xiao-Hu; Wang, Hui-Yuan; Tweed, Dylan; Liu, Cheng-Ze; Yang, Lei; Shi, Feng; Lu, Yi; Luo, Wen-Tao; Wei, Jian-Wen

    2016-08-01

    Based on the star formation histories of galaxies in halos with different masses, we develop an empirical model to grow galaxies in dark matter halos. This model has very few ingredients, any of which can be associated with observational data and thus be efficiently assessed. By applying this model to a very high resolution cosmological N-body simulation, we predict a number of galaxy properties that are a very good match to relevant observational data. Namely, for both centrals and satellites, the galaxy stellar mass functions up to redshift z ≃ 4 and the conditional stellar mass functions in the local universe are in good agreement with observations. In addition, the two point correlation function is well predicted in the different stellar mass ranges explored by our model. Furthermore, after applying stellar population synthesis models to our stellar composition as a function of redshift, we find that the luminosity functions in the 0.1 u, 0.1 g, 0.1 r, 0.1 i and 0.1 z bands agree quite well with the SDSS observational results down to an absolute magnitude at about ‑17.0. The SDSS conditional luminosity function itself is predicted well. Finally, the cold gas is derived from the star formation rate to predict the HI gas mass within each mock galaxy. We find a remarkably good match to observed HI-to-stellar mass ratios. These features ensure that such galaxy/gas catalogs can be used to generate reliable mock redshift surveys.

  15. Catalogues of hot white dwarfs in the Milky Way from GALEX's ultraviolet sky surveys: constraining stellar evolution

    NASA Astrophysics Data System (ADS)

    Bianchi, Luciana; Efremova, Boryana; Herald, James; Girardi, Léo; Zabot, Alexandre; Marigo, Paola; Martin, Christopher

    2011-03-01

    We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786 Å) and near-UV (NUV; 1771-2831 Å) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ˜19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ˜22.6/22.7 mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV≤ 0.5 mag, over 21 435/1579 deg2. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors ≤0.3 mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV - NUV < -0.13; this colour cut corresponds to stellar Teff hotter than ˜18 000 K (the exact value varying with gravity). An additional colour cut of NUV-r > 0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r < 0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an

  16. The Royal Society Catalogue as an Index to Nineteenth Century American Science

    ERIC Educational Resources Information Center

    Elliott, Clark A.

    1970-01-01

    The Royal Society Catalogue of Scientific Papers is investigated in terms of its coverage of American science journals and American scientists. The journals indexed by the catalogue are compared to other standard lists of journals from the nineteenth century. (Author)

  17. Galaxy Clusters

    NASA Astrophysics Data System (ADS)

    Miller, Christopher J. Miller

    2012-03-01

    There are many examples of clustering in astronomy. Stars in our own galaxy are often seen as being gravitationally bound into tight globular or open clusters. The Solar System's Trojan asteroids cluster at the gravitational Langrangian in front of Jupiter’s orbit. On the largest of scales, we find gravitationally bound clusters of galaxies, the Virgo cluster (in the constellation of Virgo at a distance of ˜50 million light years) being a prime nearby example. The Virgo cluster subtends an angle of nearly 8◦ on the sky and is known to contain over a thousand member galaxies. Galaxy clusters play an important role in our understanding of theUniverse. Clusters exist at peaks in the three-dimensional large-scale matter density field. Their sky (2D) locations are easy to detect in astronomical imaging data and their mean galaxy redshifts (redshift is related to the third spatial dimension: distance) are often better (spectroscopically) and cheaper (photometrically) when compared with the entire galaxy population in large sky surveys. Photometric redshift (z) [Photometric techniques use the broad band filter magnitudes of a galaxy to estimate the redshift. Spectroscopic techniques use the galaxy spectra and emission/absorption line features to measure the redshift] determinations of galaxies within clusters are accurate to better than delta_z = 0.05 [7] and when studied as a cluster population, the central galaxies form a line in color-magnitude space (called the the E/S0 ridgeline and visible in Figure 16.3) that contains galaxies with similar stellar populations [15]. The shape of this E/S0 ridgeline enables astronomers to measure the cluster redshift to within delta_z = 0.01 [23]. The most accurate cluster redshift determinations come from spectroscopy of the member galaxies, where only a fraction of the members need to be spectroscopically observed [25,42] to get an accurate redshift to the whole system. If light traces mass in the Universe, then the locations

  18. A Cluster and a Sea of Galaxies

    NASA Astrophysics Data System (ADS)

    2010-05-01

    A new wide-field image released today by ESO displays many thousands of distant galaxies, and more particularly a large group belonging to the massive galaxy cluster known as Abell 315. As crowded as it may appear, this assembly of galaxies is only the proverbial "tip of the iceberg", as Abell 315 - like most galaxy clusters - is dominated by dark matter. The huge mass of this cluster deflects light from background galaxies, distorting their observed shapes slightly. When looking at the sky with the unaided eye, we mostly only see stars within our Milky Way galaxy and some of its closest neighbours. More distant galaxies are just too faint to be perceived by the human eye, but if we could see them, they would literally cover the sky. This new image released by ESO is both a wide-field and long-exposure one, and reveals thousands of galaxies crowding an area on the sky roughly as large as the full Moon. These galaxies span a vast range of distances from us. Some are relatively close, as it is possible to distinguish their spiral arms or elliptical halos, especially in the upper part of the image. The more distant appear just like the faintest of blobs - their light has travelled through the Universe for eight billion years or more before reaching Earth. Beginning in the centre of the image and extending below and to the left, a concentration of about a hundred yellowish galaxies identifies a massive galaxy cluster, designated with the number 315 in the catalogue compiled by the American astronomer George Abell in 1958 [1]. The cluster is located between the faint, red and blue galaxies and the Earth, about two billion light-years away from us. It lies in the constellation of Cetus (the Whale). Galaxy clusters are some of the largest structures in the Universe held together by gravity. But there is more in these structures than the many galaxies we can see. Galaxies in these giants contribute to only ten percent of the mass, with hot gas in between galaxies

  19. A Galaxy for Science and Research

    NASA Astrophysics Data System (ADS)

    2007-11-01

    During his visit to ESO's Very Large Telescope at Paranal, the European Commissioner for Science and Research, Janez Potočnik, participated in an observing sequence and took images of a beautiful spiral galaxy. ESO PR Photo 43/07 ESO PR Photo 49/07 Twisted Spiral Galaxy NGC 134 The visit took place on 27 October and the Commissioner observed with one of the FORS instruments on Antu, the first 8.2-m Unit Telescope of the VLT. "Two hours bus ride from the nearest town, Antofagasta, in the middle of nowhere and at 2 600 m altitude, rises a state of the art astronomical observatory at which scientists from across Europe venture to exploit some of the most advanced technologies and sophisticated techniques available within astronomy. One of the facilities is the VLT, the Very Large Telescope, with which, together with the other telescopes, scientists can study objects at the far edge of the Universe," wrote Potočnik on his blog. Known until now as a simple number in a catalogue, NGC 134, the 'Island in the Universe' that was observed by the Commissioner is replete with remarkable attributes, and the VLT has clapped its eyes on them. Just like our own Galaxy, NGC 134 is a barred spiral with its spiral arms loosely wrapped around a bright, bar-shaped central region. One feature that stands out is its warped disc. While a galaxy's disc is often pictured as a flat structure of gas and stars surrounding the galaxy's centre, a warped disc is a structure that, when viewed sideways, resembles a bent record album left out too long in the burning Sun. Warps are actually not atypical. More than half of the spiral galaxies do show warps one way or another, and our own Milky Way also has a small warp. Many theories exist to explain warps. One possibility is that warps are the aftermath of interactions or collisions between galaxies. These can also produce tails of material being pulled out from the galaxy. The VLT image reveals that NGC 134 also appears to have a tail of gas

  20. A deep optical/near-infrared catalogue of Serpens

    NASA Astrophysics Data System (ADS)

    Spezzi, L.; Merín, B.; Oliveira, I.; van Dishoeck, E. F.; Brown, J. M.

    2010-04-01

    We present a deep optical/near-infrared imaging survey of the Serpens molecular cloud. This survey constitutes the complementary optical data to the Spitzer “Core To Disk” (c2d) Legacy survey in this cloud. The survey was conducted using the wide field camera at the Isaac Newton Telescope. About 0.96 square degrees were imaged in the R and Z filters, covering the entire region where most of the young stellar objects identified by the c2d survey are located. The 26 524 point-like sources were detected in both R and Z bands down to R ≈ 24.5 mag and Z ≈ 23 mag with a signal-to-noise ratio better than 3. The 95% completeness limit of our catalogue corresponds to 0.04 M⊙ for members of the Serpens star-forming region (age 2 Myr and distance 260 pc) in the absence of extinction. Adopting the typical extinction of the observed area (AV ≈ 7 mag), we estimate a 95% completeness level down to M ≈ 0.1 M_⊙. The astrometric accuracy of our catalogue is 0.4 arcsec with respect to the 2MASS catalogue. Our final catalogue contains J2000 celestial coordinates, magnitudes in the R and Z bands calibrated to the SDSS photometric system and, where possible, JHKS magnitudes from 2MASS for sources in 0.96 square degrees in the direction of Serpens. This data product has already been used within the frame of the c2d Spitzer Legacy Project analysis in Serpens to study the star/disk formation and evolution in this cloud. Here we use it to obtain new indications of the disk-less population in Serpens. Catalogue (in VizieR) is only available in electronic form at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr/viz-bin/Cat

  1. Accurate and efficient halo-based galaxy clustering modelling with simulations

    NASA Astrophysics Data System (ADS)

    Zheng, Zheng; Guo, Hong

    2016-06-01

    Small- and intermediate-scale galaxy clustering can be used to establish the galaxy-halo connection to study galaxy formation and evolution and to tighten constraints on cosmological parameters. With the increasing precision of galaxy clustering measurements from ongoing and forthcoming large galaxy surveys, accurate models are required to interpret the data and extract relevant information. We introduce a method based on high-resolution N-body simulations to accurately and efficiently model the galaxy two-point correlation functions (2PCFs) in projected and redshift spaces. The basic idea is to tabulate all information of haloes in the simulations necessary for computing the galaxy 2PCFs within the framework of halo occupation distribution or conditional luminosity function. It is equivalent to populating galaxies to dark matter haloes and using the mock 2PCF measurements as the model predictions. Besides the accurate 2PCF calculations, the method is also fast and therefore enables an efficient exploration of the parameter space. As an example of the method, we decompose the redshift-space galaxy 2PCF into different components based on the type of galaxy pairs and show the redshift-space distortion effect in each component. The generalizations and limitations of the method are discussed.

  2. The XMM-Newton survey of the Small Magellanic Cloud: The X-ray point-source catalogue

    NASA Astrophysics Data System (ADS)

    Sturm, R.; Haberl, F.; Pietsch, W.; Ballet, J.; Hatzidimitriou, D.; Buckley, D. A. H.; Coe, M.; Ehle, M.; Filipović, M. D.; La Palombara, N.; Tiengo, A.

    2013-10-01

    Context. Local-Group galaxies provide access to samples of X-ray source populations of whole galaxies. The XMM-Newton survey of the Small Magellanic Cloud (SMC) completely covers the bar and eastern wing with a 5.6 deg2 area in the (0.2-12.0) keV band. Aims: To characterise the X-ray sources in the SMC field, we created a catalogue of point sources and sources with moderate extent. Sources with high extent (≥40'') have been presented in a companion paper. Methods: We searched for point sources in the EPIC images using sliding-box and maximum-likelihood techniques and classified the sources using hardness ratios, X-ray variability, and their multi-wavelength properties. Results: The catalogue comprises 3053 unique X-ray sources with a median position uncertainty of 1.3'' down to a flux limit for point sources of ~10-14 erg cm-2 s-1 in the (0.2-4.5) keV band, corresponding to 5 × 1033 erg s-1 for sources in the SMC. We discuss statistical properties, like the spatial distribution, X-ray colour diagrams, luminosity functions, and time variability. We identified 49 SMC high-mass X-ray binaries (HMXB), four super-soft X-ray sources (SSS), 34 foreground stars, and 72 active galactic nuclei (AGN) behind the SMC. In addition, we found candidates for SMC HMXBs (45) and faint SSSs (8) as well as AGN (2092) and galaxy clusters (13). Conclusions: We present the most up-to-date catalogue of the X-ray source population in the SMC field. In particular, the known population of X-ray binaries is greatly increased. We find that the bright-end slope of the luminosity function of Be/X-ray binaries significantly deviates from the expected universal high-mass X-ray binary luminosity function. Based on observations obtained with XMM-Newton an ESA science mission with instruments and contributions directly funded by ESA Member States and NASACatalogue is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc

  3. Group-galaxy correlations in redshift space as a probe of the growth of structure

    NASA Astrophysics Data System (ADS)

    Mohammad, F. G.; de la Torre, S.; Bianchi, D.; Guzzo, L.; Peacock, J. A.

    2016-05-01

    We investigate the use of the cross-correlation between galaxies and galaxy groups to measure redshift-space distortions (RSD) and thus probe the growth rate of cosmological structure. This is compared to the classical approach based on using galaxy auto-correlation. We make use of realistic simulated galaxy catalogues that have been constructed by populating simulated dark matter haloes with galaxies through halo occupation prescriptions. We adapt the classical RSD dispersion model to the case of the group-galaxy cross-correlation function and estimate the RSD parameter β by fitting both the full anisotropic correlation function ξs(rp, π) and its multipole moments. In addition, we define a modified version of the latter statistics by truncating the multipole moments to exclude strongly non-linear distortions at small transverse scales. We fit these three observable quantities in our set of simulated galaxy catalogues and estimate statistical and systematic errors on β for the case of galaxy-galaxy, group-group, and group-galaxy correlation functions. When ignoring off-diagonal elements of the covariance matrix in the fitting, the truncated multipole moments of the group-galaxy cross-correlation function provide the most accurate estimate, with systematic errors below 3 per cent when fitting transverse scales larger than 10 h-1 Mpc. Including the full data covariance enlarges statistical errors but keep unchanged the level of systematic error. Although statistical errors are generally larger for groups, the use of group-galaxy cross-correlation can potentially allow the reduction of systematics while using simple linear or dispersion models.

  4. The nature of voids - II. Tracing underdensities with biased galaxies

    NASA Astrophysics Data System (ADS)

    Nadathur, S.; Hotchkiss, S.

    2015-11-01

    We study how the properties of cosmic voids depend on those of the tracer galaxy populations in which they are identified. We use a suite of halo occupation distribution mocks in a simulation, identify voids in these populations using the ZOBOV void finder and measure their abundances, sizes, tracer densities and dark matter content. To separate the effects of bias from those of sampling density, we do the same for voids traced by randomly downsampled subsets of the simulation dark matter particles. At the same sampling density, galaxy bias reduces the total number of voids by ˜50 per cent and can dramatically change their size distribution. The matter content of voids in biased and unbiased tracers also differs. Deducing void properties from simulation therefore requires the use of realistic galaxy mocks. We discuss how the void observables can be related to their matter content. In particular we consider the compensation of the total mass deficit in voids and find that the distinction between over- and undercompensated voids is not a function of void size alone, as has previously been suggested. However, we find a simple linear relationship between the average density of tracers in the void and the total mass compensation on much larger scales. The existence of this linear relationship holds independent of the bias and sampling density of the tracers. This provides a universal tool to classify void environments and will be important for the use of voids in observational cosmology.

  5. Whirlpool Galaxy

    NASA Technical Reports Server (NTRS)

    1999-01-01

    Scientists are seeing unprecedented detail of the spiral arms and dust clouds in the nearby Whirlpool galaxy, thanks to a new Hubble Space Telescope image, available at http://www.jpl.nasa.gov/pictures/wfpc/wfpc.html. The image uses data collected January 15 and 24, 1995, and July 21, 1999, by Hubble's Wide Field and Planetary Camera 2, designed and built by JPL. Using the image, a research group led by Dr. Nick Scoville of the California Institute of Technology, Pasadena, clearly defined the structure of the galaxy's cold dust clouds and hot hydrogen, and they linked star clusters within the galaxy to their parent dust clouds.

    The Whirlpool galaxy is one of the most photogenic galaxies. This celestial beauty is easily seen and photographed with smaller telescopes and studied extensively from large ground- and space-based observatories. The new composite image shows visible starlight and light from the emission of glowing hydrogen, which is associated with the most luminous young stars in the spiral arms.

    The galaxy is having a close encounter with a nearby companion galaxy, NGC 5195, just off the upper edge of the image. The companion's gravitational pull is triggering star formation in the main galaxy, lit up by numerous clusters of young and energetic stars in brilliant detail. Luminous clusters are highlighted in red by their associated emission from glowing hydrogen gas.

    This image was composed by the Hubble Heritage Team from Hubble archive data and was superimposed onto data taken by Dr. Travis Rector of the National Optical Astronomy Observatory at the .9-meter (35-inch) telescope at the National Science Foundation's Kitt Peak National Observatory, Tucson, Ariz. Scoville's team includes M. Polletta of the University of Geneva, Switzerland; S. Ewald and S. Stolovy of Caltech; and R. Thompson and M. Rieke of the University of Arizona, Tucson.

    The Space Telescope Science Institute, Baltimore, Md., manages space operations for the Hubble Space

  6. VizieR Online Data Catalog: Richness of galaxy clusters (Oguri, 2014)

    NASA Astrophysics Data System (ADS)

    Oguri, M.

    2015-04-01

    We apply our cluster finding algorithm CAMIRA to imaging data of SDSS DR8 (Aihara et al., 2011ApJS..193...29A). The input galaxy catalogue includes model magnitudes (MODEL_MAG) and their errors for SDSS ugriz-band. We exclude galaxies with any of the following flags; SATURATED, SATURCENTER, BRIGHT, and DEBLENDEDAS_MOVING. We only use galaxies with extinction-corrected i-band magnitude brighter than 21.0 and its error smaller than 0.2. (1 data file).

  7. VizieR Online Data Catalog: Ultraviolet Excess Galaxies (Mitchell+ 1982)

    NASA Astrophysics Data System (ADS)

    Mitchell, K. J.; Brotzman, L. E.; Warnock, A.; Usher, P. D.

    2015-05-01

    The catalog contains a list of 412 faint galaxies selected for their apparent ultraviolet excess. The galaxies were selected from a 3-color (UBV) plate taken with the Palomar 48-inch Schmidt telescope. The 14-inch-square plates cover an area of 30 square degrees centered on Kapteyn Selected Area 28. The catalog includes running numbers, coordinates, color codes, magnitude codes, morphologies, diameters, and notes. The catalogued galaxies were selected by eye from the Palomar Schmidt 3-color (UBV) plate PS24771, centered on Kapteyn Selexted Area 28 and taken by Usher under conditions of good seeing and transparency. (1 data file).

  8. Far infrared structure of spiral galaxies from the IRAS CPC images

    NASA Technical Reports Server (NTRS)

    Wainscoat, Richard J.; Chokshi, Arati; Doyle, Laurance R.

    1989-01-01

    Significant extended far infrared (50 micron and 100 micron) structure was found for five face-on spiral galaxies (NGC2403, M51, M83, NGC6946, and IC342) from fourteen galaxies searched in the Infrared Astronomy Satellite (IRAS) chopped photometric channel (CPC) catalogue. Images were initially processed to remove instrumental and background artifacts, the isophotal centroids of each image determined, and multiple images of each galaxy (for each wavelength) superimposed and averaged to improve signal-to-noise. Calibration of these images was performed using IRAS survey array data. Infrared isophotes were then superimposed on optical (blue) images so that direct structural comparisons could be made.

  9. Virtual Instrumentation to study galaxies

    NASA Astrophysics Data System (ADS)

    Prugniel, Ph.; Chilingarian, I.; Flores, H.; Guibert, J.; Haigron, R.; Jégouzo, I.; Royer, F.; Tajahmady, F.; Theureau, G.; Vétois, J.

    2004-12-01

    The MIGALE project builds and maintains databases and analysis tools to help studies of the evolution of galaxies between z=1 and z=0. At z=0 MIGALE offers the whole-sky multiparametric HyperLeda database and the new HIgi database (see this G. Theureau and J.-M. Martin, this conference) dedicated to HI observations. At larger distances we are developing the Disgal database discussed by H. Flores and M. Puech at this conference. MIGALE is also operating the Giraffe Archive (F. Royer, this conference) containing the reduced spectra produced by the VLT spectrograph Giraffe. These systems provide altogether a very fine multi-wavelength and multiparametric description of galaxies. The data collected and distributed are either compilations or original surveys, catalogues or pixels (spectra and images). These services offer several facilities for processing and analysing the data (on-line pipeline). This constellation of services share a common software (Pleinpot) providing some general low-level layers (access to database and to FITS data), some specialized astronomical recipes (like models to study stellar populations) and the Virtual Observatory interface required for inter-operability with other projects.

  10. Galaxy And Mass Assembly (GAMA): galaxy radial alignments in GAMA groups

    NASA Astrophysics Data System (ADS)

    Schneider, Michael D.; Cole, Shaun; Frenk, Carlos S.; Kelvin, Lee; Mandelbaum, Rachel; Norberg, Peder; Bland-Hawthorn, Joss; Brough, Sarah; Driver, Simon; Hopkins, Andrew; Liske, Jochen; Loveday, Jon; Robotham, Aaron

    2013-08-01

    We constrain the distributions of projected radial alignment angles of satellite galaxy shapes within the Galaxy And Mass Assembly survey group catalogue. We identify the galaxy groups using spectroscopic redshifts and measure galaxy projected ellipticities from Sloan Digital Sky Survey imaging. With a sample of 3850 groups with 13 655 satellite galaxies with high quality shape measurements, we find a less than 2σ signal of radial alignments in the mean projected ellipticity components and the projected position angle when using galaxy shape estimates optimized for weak lensing measurements. Our radial alignment measurement increases to greater than 3σ significance relative to the expectation for no alignments if we use 2D Sérsic model fits to define galaxy orientations. Our weak measurement of radial alignments is in conflict with predictions from dark-matter N-body simulations, which we interpret as evidence for large misalignments of baryons and dark matter in group and cluster satellites. Within our uncertainties, that are dominated by our small sample size, we find only weak and marginally significant trends of the radial alignment angle distributions on projected distance from the group centre, host halo mass, and redshift that could be consistent with a tidal torquing mechanism for radial alignments. Using our lensing optimized shape estimators, we estimate that intrinsic alignments of galaxy group members may contribute a systematic error to the mean differential projected surface mass density of groups inferred from weak lensing observations by -1 ± 20 per cent at scales around 300 h-1 kpc from the group centre assuming a photometric redshift rms error of 10 per cent, and given our group sample with median redshift of 0.17 and median virial masses ˜1013 h-1 M⊙.

  11. Modeling the Galaxy Three-Point Correlation Function

    SciTech Connect

    Marin, Felipe; Wechsler, Risa; Frieman, Joshua A.; Nichol, Robert; /Portsmouth U., ICG

    2007-06-05

    We present new theoretical predictions for the galaxy three-point correlation function (3PCF) using high-resolution dissipationless cosmological simulations of a flat Lambda CDM Universe which resolve galaxy-size halos and subhalos. We create realistic mock galaxy catalogs by assigning luminosities and colors to dark matter halos and subhalos, and we measure the reduced 3PCF as a function of luminosity and color in both real and redshift space. As galaxy luminosity and color are varied, we find small differences in the amplitude and shape dependence of the reduced 3PCF, at a level qualitatively consistent with recent measurements from the SDSS and 2dFGRS. We confirm that discrepancies between previous 3PCF measurements can be explained in part by differences in binning choices. We explore the degree to which a simple local bias model can fit the simulated 3PCF. The agreement between the model predictions and galaxy 3PCF measurements lends further credence to the straightforward association of galaxies with CDM halos and subhalos.

  12. The color-indices of early-type galaxies with core collapse supernovae

    NASA Astrophysics Data System (ADS)

    Polyakova, G. D.

    We performed least-squares fits to determine the transformation equations of the color-indices (u-g), (g-r) (SDSS photometric catalog, Release 8, 2011); (NUV-B) (GALEX ultra-violet Atlas of nearby galaxies, Gil de Paz et al, 2007); (B-Ve), (U-Be) (General photometry of galaxies, Prugniel et al, 1998) to the photometric system of catalogue RC3 (U-B)T and (B-V)T. We determined the color - indices (U-B)Tc and (B-V)Tc for the 20 galaxies with SNe of types Ibc and II. The 17 of these galaxies are seen to fall in red sequence galaxies of color- magnitude diagram for 872 of the RC3 early-type galaxies with known (U-B)T0 colors. The blue galaxies are NGC 4691, NGC 838 and NGC 7803 - the galaxies with active galaxy nuclei (AGN). The 12 host galaxies are peculiar and 13 - are members of group of galaxies.

  13. "Galaxy," Defined

    NASA Astrophysics Data System (ADS)

    Willman, B.; Strader, J.

    2012-09-01

    A growing number of low luminosity and low surface brightness astronomical objects challenge traditional notions of both galaxies and star clusters. To address this challenge, we propose a definition of galaxy that does not depend on a cold dark matter model of the universe: a galaxy is a gravitationally bound collection of stars whose properties cannot be explained by a combination of baryons and Newton's laws of gravity. After exploring several possible observational diagnostics of this definition, we critically examine the classification of ultra-faint dwarfs, globular clusters, ultra-compact dwarfs, and tidal dwarfs. While kinematic studies provide an effective diagnostic of the definition in many regimes, they can be less useful for compact or very faint systems. To explore the utility of using the [Fe/H] spread as a complementary diagnostic, we use published spectroscopic [Fe/H] measurements of 16 Milky Way dwarfs and 24 globular clusters to uniformly calculate their [Fe/H] spreads and associated uncertainties. Our principal results are (1) no known, old star cluster less luminous than MV = -10 has a significant (gsim0.1 dex) spread in its iron abundance; (2) known ultra-faint dwarf galaxies can be unambiguously classified with a combination of kinematic and [Fe/H] observations; (3) the observed [Fe/H] spreads in massive (gsim 106 M ⊙) globular clusters do not necessarily imply that they are the stripped nuclei of dwarfs, nor a need for dark matter; and (4) if ultra-compact dwarf galaxies reside in dark matter halos akin to those of ultra-faint dwarfs of the same half-light radii, then they will show no clear dynamical signature of dark matter. We suggest several measurements that may assist the future classification of massive globular clusters, ultra-compact dwarfs, and ultra-faint galaxies. Our galaxy definition is designed to be independent of the details of current observations and models, while our proposed diagnostics can be refined or replaced as

  14. The same with less: The cosmic web of warm versus cold dark matter dwarf galaxies

    NASA Astrophysics Data System (ADS)

    Reed, Darren; Schneider, Aurel; Smith, Robert E.; Stadel, Joachim; Moore, Ben

    2015-01-01

    We explore fundamental properties of the distribution of low mass dark matter halos within the cosmic web using warm dark matter (WDM) and cold dark matter (CDM) cosmological simulations. Using self abundance-matched mock galaxy catalogs, we show that the distribution of dwarf galaxies in a WDM universe wherein low mass halo formation is heavily suppressed, is nearly indistinguishable to that of a CDM universe whose low mass halos are not seen because galaxy formation is suppressed below some threshold halo mass. However, if the scatter between dwarf galaxy luminosity and halo properties is large enough, low mass CDM halos would sometimes host relatively bright galaxies thereby populating CDM voids with the occasional isolated galaxyand reducing the numbers of completely empty voids. Otherwise, without high mass to light scatter, all mock galaxy clustering statistics that we consider-the auto-correlation function, the numbers and radial profiles of satellites, the numbers of isolated galaxies, and the PDF of small voids-are nearly identical in CDM and WDM. WDM voids are neither larger nor emptier than CDM voids, when constructed from abundance- matched halo catalogs. It is thus a challenge to determine whether the CDM problem of the over-abundance of small halos with respect to the number density of observed dwarf galaxies has a cosmological solution or an astrophysical solution. However, some clues about the dark matter particle and the scatter between the properties of dwarfgalaxies and their dark matter halo hosts might be found in the cosmic web of galaxies in future surveys of the local volume.

  15. A PARAMETERIZED GALAXY CATALOG SIMULATOR FOR TESTING CLUSTER FINDING, MASS ESTIMATION, AND PHOTOMETRIC REDSHIFT ESTIMATION IN OPTICAL AND NEAR-INFRARED SURVEYS

    SciTech Connect

    Song, Jeeseon; Mohr, Joseph J.; Barkhouse, Wayne A.; Rude, Cody; Warren, Michael S.; Dolag, Klaus

    2012-03-01

    We present a galaxy catalog simulator that converts N-body simulations with halo and subhalo catalogs into mock, multiband photometric catalogs. The simulator assigns galaxy properties to each subhalo in a way that reproduces the observed cluster galaxy halo occupation distribution, the radial and mass-dependent variation in fractions of blue galaxies, the luminosity functions in the cluster and the field, and the color-magnitude relation in clusters. Moreover, the evolution of these parameters is tuned to match existing observational constraints. Parameterizing an ensemble of cluster galaxy properties enables us to create mock catalogs with variations in those properties, which in turn allows us to quantify the sensitivity of cluster finding to current observational uncertainties in these properties. Field galaxies are sampled from existing multiband photometric surveys of similar depth. We present an application of the catalog simulator to characterize the selection function and contamination of a galaxy cluster finder that utilizes the cluster red sequence together with galaxy clustering on the sky. We estimate systematic uncertainties in the selection to be at the {<=}15% level with current observational constraints on cluster galaxy populations and their evolution. We find the contamination in this cluster finder to be {approx}35% to redshift z {approx} 0.6. In addition, we use the mock galaxy catalogs to test the optical mass indicator B{sub gc} and a red-sequence redshift estimator. We measure the intrinsic scatter of the B{sub gc}-mass relation to be approximately log normal with {sigma}{sub log10M}{approx}0.25 and we demonstrate photometric redshift accuracies for massive clusters at the {approx}3% level out to z {approx} 0.7.

  16. Photometric Properties of Face-on Isolated Spiral Galaxies

    NASA Astrophysics Data System (ADS)

    Bahr, Alexander; Epstein, P.; Durbala, A.

    2011-05-01

    We want to quantify the relative role of nature versus nurture in defining the observed properties of galaxies. In simpler terms we would like to disentangle the ``genetic'’ and the environmental influences in shaping the morphology of galaxies. In order to do that one needs to firstly define a zero-order baseline, i.e., a sample of galaxies that have been minimally perturbed by neighbors in the last few billion years of their existence. Such a sample has been produced and refined in different stages in the context of the AMIGA international project (www.iaa.es/AMIGA.html). The recent catalogue ``The All-Sky Catalog of Isolated Galaxies Selected from 2MASS'’ (Karachentseva, V. E. et al. 2010) allows us to complete and enrich the initial sample constructed within AMIGA with new objects, thus enhancing the statistical relevance of our study. Our focus is to define a subset of isolated disk spiral galaxies. We constrain the sample selection by: 1) orientation, restricting to almost face-on galaxies and 2) availability of good photometric images in SDSS. The goal is to ``dissect'’ (decompose) these galaxies in major components (disk, bulge, bars, etc.) and to study the properties of the components in a statistical context. Having a reasonable representation of all morphological types, we aim to test the bimodality of bulges and bars. We present a progress report of our work.

  17. Cataloguing Rules for Books and other Media in Primary and Secondary Schools. A Simplified Version of Anglo-American Cataloguing Rules, Together with Rules for Cataloguing Non-book Materials. Fifth (Expanded) Edition.

    ERIC Educational Resources Information Center

    Furlong, Norman, Comp.; Platt, Peter, Comp.

    The School Library Association (London, England) presents a brief and simplified version of the 1967 "Anglo-American Cataloguing Rules" along with cataloging rules for non-book materials based on the "Non-book Materials: Cataloguing Rules" of 1973. The 33 rules are briefly stated, and short examples are given for main entries, titles, imprint,…

  18. Extragalatic zoo. I. [New galaxies

    SciTech Connect

    Schorn, R.A.

    1988-01-01

    The characteristics of various types of extragalactic objects are described. Consideration is given to cD galaxies, D galaxies, N galaxies, Markarian galaxies, liners, starburst galaxies, and megamasers. Emphasis is also placed on the isolated extragalatic H I region; the isolated extragalatic H II region; primeval galaxies or photogalaxies; peculiar galaxies; Arp galaxies; interacting galaxies; ring galaxies; and polar-ring galaxies. Diagrams of these objects are provided.

  19. LoCuSS: Exploring the selection of faint blue background galaxies for cluster weak-lensing

    NASA Astrophysics Data System (ADS)

    Ziparo, Felicia; Smith, Graham P.; Okabe, Nobuhiro; Haines, Chris P.; Pereira, Maria J.; Egami, Eiichi

    2016-10-01

    Cosmological constraints from galaxy clusters rely on accurate measurements of the mass and internal structure of clusters. An important source of systematic uncertainty in cluster mass and structure measurements is the secure selection of background galaxies that are gravitationally lensed by clusters. This issue has been shown to be particular severe for faint blue galaxies. We therefore explore the selection of faint blue background galaxies, by reference to photometric redshift catalogues derived from the COSMOS survey and our own observations of massive galaxy clusters at z ≃ 0.2. We show that methods relying on photometric redshifts of galaxies in/behind clusters based on observations through five filters, and on deep 30-band COSMOS photometric redshifts are both inadequate to safely identify faint blue background galaxies with the same 1 per cent contamination level that we have achieved with red galaxies. This is due to the small number of filters used by the former, and absence of massive galaxy clusters at redshifts of interest in the latter. Nevertheless, our least contaminated blue galaxy sample yields stacked weak-lensing results consistent with our previously published results based on red galaxies, and we show that the stacked clustercentric number density profile of these faint blue galaxies is consistent with expectations from consideration of the lens magnification signal of the clusters. Indeed, the observed number density of blue background galaxies changes by ˜10 - 30 per cent across the radial range over which other surveys assume it to be flat.

  20. Automatic approach to solve the morphological galaxy classification problem using the sparse representation technique and dictionary learning

    NASA Astrophysics Data System (ADS)

    Diaz-Hernandez, R.; Ortiz-Esquivel, A.; Peregrina-Barreto, H.; Altamirano-Robles, L.; Gonzalez-Bernal, J.

    2016-06-01

    The observation of celestial objects in the sky is a practice that helps astronomers to understand the way in which the Universe is structured. However, due to the large number of observed objects with modern telescopes, the analysis of these by hand is a difficult task. An important part in galaxy research is the morphological structure classification based on the Hubble sequence. In this research, we present an approach to solve the morphological galaxy classification problem in an automatic way by using the Sparse Representation technique and dictionary learning with K-SVD. For the tests in this work, we use a database of galaxies extracted from the Principal Galaxy Catalog (PGC) and the APM Equatorial Catalogue of Galaxies obtaining a total of 2403 useful galaxies. In order to represent each galaxy frame, we propose to calculate a set of 20 features such as Hu's invariant moments, galaxy nucleus eccentricity, gabor galaxy ratio and some other features commonly used in galaxy classification. A stage of feature relevance analysis was performed using Relief-f in order to determine which are the best parameters for the classification tests using 2, 3, 4, 5, 6 and 7 galaxy classes making signal vectors of different length values with the most important features. For the classification task, we use a 20-random cross-validation technique to evaluate classification accuracy with all signal sets achieving a score of 82.27 % for 2 galaxy classes and up to 44.27 % for 7 galaxy classes.

  1. Amiba and Galaxy Cluster Survey via Thermal Sunyaev-Zel Effects

    NASA Astrophysics Data System (ADS)

    Chiueh, Tzihong

    2003-03-01

    Array for Microwave Background Anisotropy (AMiBA) is a 19-element, platform-mounted interferometry telescope operating at 90 GHz. With a 10' field of view and 2' angular resolution, the designed sensitivity of AMiBA for real-space imaging of galaxy clusters via the Sunyaev-Zel'dovich effect can achieve 150μ {K {K {√ {sec} } ; {√ {sec } }} . I present our preliminary tests for the quality of AMiBA cluster images via mosaic mock observations on the simulated sky produced by cosmological N-body/SPH simulations. I also discuss the issue of confusion caused by the synchrotron and dust emission from galaxies residing in clusters.

  2. The global warming of group satellite galaxies

    NASA Astrophysics Data System (ADS)

    Yozin, C.; Bekki, K.

    2016-08-01

    Recent studies adopting λRe, a proxy for specific angular momentum, have highlighted how early-type galaxies (ETGs) are composed of two kinematical classes for which distinct formation mechanisms can be inferred. With upcoming surveys expected to obtain λRe from a broad range of environments (e.g. SAMI, MaNGA), we investigate in this numerical study how the λRe-ɛe distribution of fast-rotating dwarf satellite galaxies reflects their evolutionary state. By combining N-body/SPH simulations of progenitor disc galaxies (stellar mass ≃109 M⊙), their cosmologically-motivated sub-halo infall history and a characteristic group orbit/potential, we demonstrate the evolution of a satellite ETG population driven by tidal interactions (e.g. harassment). As a general result, these satellites remain intrinsically fast-rotating oblate stellar systems since their infall as early as z = 2; mis-identifications as slow rotators often arise due to a bar/spiral lifecycle which plays an integral role in their evolution. Despite the idealistic nature of its construction, our mock λRe-ɛe distribution at z < 0.1 reproduces its observational counterpart from the ATLAS3D/SAURON projects. We predict therefore how the observed λRe-ɛe distribution of a group evolves according to these ensemble tidal interactions.

  3. Wax-up and mock-up. A guide for anterior periodontal and restorative treatments.

    PubMed

    Gurrea, Jon; Bruguera, August

    2014-01-01

    When starting a case, having the end result in mind is the basis in any kind of treatment, even more so in those where the anterior teeth morphology, size and proportion will be changed. Here is where a good treatment plan based on a diagnostic wax-up that is tried in with a mock-up and approved by the patient becomes crucial. This case report exemplifies how transferring the information from the diagnostic wax up to the patient's mouth is of help not only to the restorative dentist and the laboratory technician, but also to the surgeon when performing the crown lengthening. This treatment plan cannot be seen as a sequence of isolated procedures but as a single workflow. The wax-up/mock-up binomial is a guide even for the periodontist in a novel approach to surgical crown lengthening.

  4. Comparison of polygraph data obtained from individuals involved in mock crimes and actual criminal investigations.

    PubMed

    Pollina, Dean A; Dollins, Andrew B; Senter, Stuart M; Krapohl, Donald J; Ryan, Andrew H

    2004-12-01

    In a preliminary attempt to determine the generalizability of data from laboratory mock-crime studies, the authors examined the similarities and differences among the cardiovascular, electrodermal, and respiration responses of deceptive and nondeceptive individuals elicited to crime-relevant and crime-irrelevant questions. Participants in the laboratory group were randomly assigned to nondeceptive (n = 28) or deceptive (n = 27) treatment groups, and a mock-crime scenario was used. The field participants were confirmed nondeceptive (n = 28) or deceptive (n = 39) criminal suspects who underwent polygraph examinations between 1993 and 1997. The results indicated that there were salient differences between field and similarly obtained laboratory polygraph response measures. However, accuracy of laboratory participants' classifications using logistic regression analysis was not significantly different from field participants' classification accuracy.

  5. [Pandemic influenza vaccines. Concepts, European mock-up licenses, and acceptance criteria].

    PubMed

    Pfleiderer, M

    2010-12-01

    The concept of identifying appropriate scientific and regulatory principles to ensure rapid availability of pandemic influenza vaccines when needed were already developed starting in the year 2003. These principles allowed licensing of three so-called mock-up vaccines far ahead of any real presenting pandemic event. Those licenses (Marketing Authorizations) were immediately adapted to the novel H1N1 strain shortly after its identification in April 2009 ensuring that as early as September 2009 large parts of the German as well as of the EU population had access to licensed products which had undergone sufficient evaluation before first use in humans. In contrast, for pandemic vaccine concepts without a previously licensed mock-up version it generally took twice as much time to accumulate data supporting the granting of a Marketing Authorization. This article describes in detail the translation of concepts of producing, testing, and licensing of pandemic influenza vaccines into practice under real conditions. PMID:21161474

  6. System Tests on Full Scale VEGA Launcher Mock-Up at the European Spaceport

    NASA Astrophysics Data System (ADS)

    Leofanti, Jose Luis; Fotino, Domenico; Bianchini, Angelo; Scaccia, Aldo

    2012-07-01

    Between the end of 2010 and the first half of 2011, a full scale mock-up of the VEGA launcher was assembled at Kourou spaceport in the frame of the so- called “Combined Tests”. Beyond the verification of the interfaces with the ground segment, this mock-up was used to perform dry runs of the flight time-line up lift off in both night and day conditions and, during these dry runs, several system tests in representative environmental conditions were carried out. This paper gives an overview on all the tests performed mainly in terms of test sequence, test setup preparation and main results. Attention is focused on the final countdown dry-run were thermal, inertial system alignment, ground operations and structural dynamic tests have been performed contemporarily following the operational plan.

  7. Advanced Spacesuit Portable Life Support System Packaging Concept Mock-Up Design & Development

    NASA Technical Reports Server (NTRS)

    O''Connell, Mary K.; Slade, Howard G.; Stinson, Richard G.

    1998-01-01

    A concentrated development effort was begun at NASA Johnson Space Center to create an advanced Portable Life Support System (PLSS) packaging concept. Ease of maintenance, technological flexibility, low weight, and minimal volume are targeted in the design of future micro-gravity and planetary PLSS configurations. Three main design concepts emerged from conceptual design techniques and were carried forth into detailed design, then full scale mock-up creation. "Foam", "Motherboard", and "LEGOtm" packaging design concepts are described in detail. Results of the evaluation process targeted maintenance, robustness, mass properties, and flexibility as key aspects to a new PLSS packaging configuration. The various design tools used to evolve concepts into high fidelity mock ups revealed that no single tool was all encompassing, several combinations were complimentary, the devil is in the details, and, despite efforts, many lessons were learned only after working with hardware.

  8. [Catalogues of therapeutic nursing activities in neurological early rehabilitation].

    PubMed

    Lautenschläger, S; Wallesch, C W

    2015-02-01

    Under the German DRG-system, hospital-based rehabilitation of still critically ill patients becomes increasingly important. The code for early neurological rehabilitation in the DRG-system's (Diagnosis Related Groups) list of operations and procedures requires an average daily therapeutic intensity of 300 min, part of which is being contributed by therapeutic nursing. As therapeutic aspects are integrated in other nursing activities, it is difficult to separate its time consumption. This problem is pragmatically resolved by catalogues of therapeutic nursing activities which assign plausible amounts of therapeutic minutes to each activity. The 4 catalogues that are used most often are described and compared. Nursing science has not focused yet on therapeutic nursing. PMID:25317957

  9. Chamber catalogues of optical and fluorescent signatures distinguish bioaerosol classes

    NASA Astrophysics Data System (ADS)

    Hernandez, Mark; Perring, Anne E.; McCabe, Kevin; Kok, Greg; Granger, Gary; Baumgardner, Darrel

    2016-07-01

    Rapid bioaerosol characterization has immediate applications in the military, environmental and public health sectors. Recent technological advances have facilitated single-particle detection of fluorescent aerosol in near real time; this leverages controlled ultraviolet exposures with single or multiple wavelengths, followed by the characterization of associated fluorescence. This type of ultraviolet induced fluorescence has been used to detect airborne microorganisms and their fragments in laboratory studies, and it has been extended to field studies that implicate bioaerosol to compose a substantial fraction of supermicron atmospheric particles. To enhance the information yield that new-generation fluorescence instruments can provide, we report the compilation of a referential aerobiological catalogue including more than 50 pure cultures of common airborne bacteria, fungi and pollens, recovered at water activity equilibrium in a mesoscale chamber (1 m3). This catalogue juxtaposes intrinsic optical properties and select bandwidths of fluorescence emissions, which manifest to clearly distinguish between major classes of airborne microbes and pollens.

  10. An annotated catalogue of the Iranian Alysiinae (Hymenoptera: Braconidae).

    PubMed

    Gadallah, Neveen S; Ghahari, Hassan; Peris-Felipo, Francisco Javier; Fischer, Maximilian

    2015-06-19

    In the present study, a catalogue of the Iranian Alysiinae (Hymenoptera: Braconidae) is given. It is based on a detailed study of all available published data. In total 78 species from 15 genera including Alloea Haliday, 1833 (1 species), Angelovia Zaykov, 1980 (1 species), Aphaereta Foerster, 1862 (2 species), Aspilota Foerster, 1862 (2 species), Chorebus Haliday, 1833 (42 species), Coelinidea Viereck, 1913 (2 species), Coloneura Foerster, 1862 (1 species), Dacnusa Haliday, 1833 (10 species), Dinotrema Foerster, 1862 (5 species), Idiasta Foerster, 1862 (1 species), Orthostigma Ratzeburg, 1844 (3 species), Phaenocarpa Foerster, 1862 (1 species), Protodacnusa Griffiths, 1964 (2 species), Pseudopezomachus Mantero, 1905 (2 species), and Synaldis Foerster, 1862 (3 species) are reported in this catalogue. Two species are new records for Iran: Coelinidea elegans (Curtis, 1829) and Dacnusa (Pachysema) aterrima Thomson, 1895. Also, a faunistic list with distribution data and host records is provided.

  11. Catalogue of snout mites (Acariformes: Bdellidae) of the world.

    PubMed

    Hernandes, Fabio A; Skvarla, Michael J; Fisher, J Ray; Dowling, Ashley P G; Ochoa, Ronald; Ueckermann, Edward A; Bauchan, Gary R

    2016-01-01

    Bdellidae (Trombidiformes: Prostigmata) are moderate to large sized predatory mites that inhabit soil, leaves, leaf litter, and intertidal rocks. They are readily recognized by an elongated, snout-like gnathosoma and by elbowed pedipalps bearing two (one in Monotrichobdella Baker & Balock) long terminal setae. Despite being among the first mites ever described, with species described by Carl Linnaeus, the knowledge about bdellids has never been compiled into a taxonomic catalogue. Here we present a catalogue listing 278 valid species; for each species we include distribution information, taxonomic literature, and type depository institutions. The genus Rigibdella Tseng, 1978 is considered a junior synonym of Cyta von Heyden, 1826, and Bdellodes Oudemans, 1937 is considered a junior synonym of Odontoscirus Tohr, 1913. Illustrated keys to subfamilies and genera are presented, as well as keys to species of each genus. PMID:27615820

  12. Crashing galaxies, cosmic fireworks

    SciTech Connect

    Keel, W.C.

    1989-01-01

    The study of binary systems is reviewed. The history of the study of interacting galaxies, the behavior of gas in binary systems, studies to identify the processes that occur when galaxies interact, and the relationship of Seyfert galaxies and quasars to binary systems are discussed. The development of an atlas of peculiar galaxies (Arp, 1966) and methods for modeling galaxy interactions are examined.

  13. Soft tissue waxup and mock-up as key factors in a treatment plan: case presentation.

    PubMed

    Viana, Pedro Couto; Correia, André; Neves, Manuel; Kovacs, Zsolt; Neugbauer, Rudiger

    2012-01-01

    Rehabilitation of edentulous spaces in esthetic areas is a challenge to the clinician due to the loss of soft tissues. In these clinical situations, it would be desirable to evaluate and predict the gingival architecture to recover in the oral rehabilitation. To fulfill this need, the diagnostic wax should anticipate the final rehabilitation with the integration of hard and soft tissue. Thus, it is essential to produce a diagnostic waxup that integrates these two components that are simultaneously seeking to recreate the harmony of white and pink esthetic. This diagnostic waxup will be the basis for the creation of the provisional prosthesis and a soft tissue mock-up. After placing the provisional prosthesis in the mouth, the soft tissue mock-up can be applied to assess its esthetic impact at facial and intraoral level. Dentist and patient should objectively assess the appearance of the final result. After approval of this rehabilitation concept, the virtual surgical planning can be performed and the surgical guide can be designed, allowing the treatment to take place. This protocol allows the development of a rigorous treatment plan based on the integration of teeth and gingiva component. The waxup and the soft tissue mock-up play a significant role, since they allow an earlier evaluation of the esthetic result, better prosthetic and surgical planning, and it allows us to anticipate the need for gingiva-colored ceramics use. The authors present a clinical case report of the importance of the wax-up and soft tissue mock-up in the treatment plan.

  14. Clinically based diagnostic wax-up for optimal esthetics: the diagnostic mock-up.

    PubMed

    Simon, Harel; Magne, Pascal

    2008-05-01

    A diagnostic wax-up can enhance the predictability of treatment by modeling the desired result in wax prior to treatment. It is critical to correlate the wax-up to the patient to avoid a result that appears optimal on the casts but does not correspond to the patient's smile. This article reviews the applications and techniques for clinically based diagnostic wax-up, and focuses on the diagnostic mock-up philosophy as a means to obtain predictable esthetics and function.

  15. Irradiation capabilities of LR-0 reactor with VVER-1000 Mock-Up core.

    PubMed

    Košťál, Michal; Rypar, Vojtěch; Svadlenková, Marie; Cvachovec, František; Jánský, Bohumil; Milčák, Ján

    2013-12-01

    Even low power reactors, such as zero power reactors, are sufficient for semiconductor radiation hardness effect investigation. This reflects the fact that fluxes necessary for affecting semiconductor electrical resistance are much lower than fluxes necessary to affect material parameters. The paper aims to describe the irradiation possibilities of the LR-0 reactor with a special core arrangement corresponding to VVER-1000 dosimetry Mock-Up.

  16. Using a Mock Trial Method to Enhance Effectiveness of Teaching Evidence-Based Practice in Nursing.

    PubMed

    White, Cindy T

    2015-01-01

    Traditional teaching methodologies may deter adult learning because of passive the exchange of knowledge. Teaching to the "evidence" substantiating best practice requires a systematic approach to transfer knowledge into clinical inquiry. A mock trial simulated role-play activity was selected to show the value of learning through active engagement. The nurse "defendant" was challenged to substantiate practice based on the evidence. Seminar participants (the jury) scrutinized testimony through deliberation before delivering the final verdict. PMID:26580469

  17. The Distribution of separations of DMSA Hipparcos Catalogue

    NASA Astrophysics Data System (ADS)

    Ling, J. F.; Magdalena, P.; Prieto, C.

    2004-08-01

    We have constructed volume-limited samples of wide binaries in the Hipparcos Catalogue Double and Multiple Systems Annex (DMSA, Section C), out to distances of 100 pc and 200 pc. We study the distribution of linear separations for these samples of binaries. We find that they closely follow Öpik's distribution in the interval of separations between about 10 and 800 AU (for the 100 pc sample), and between 15 and 1400 AU (for the 200 pc sample)

  18. Annotated catalogue of Australian weevils  (Coleoptera: Curculionoidea).

    PubMed

    Pullen, Kimberi R; Jennings, Debbie; Oberprieler, Rolf G

    2014-01-01

    This catalogue presents the first-ever complete inventory of all described taxa of Australian weevils, including both valid and invalid names. The geographical scope spans mainland Australia and its continental islands as well as the subantarctic Heard and McDonald Islands, the Pacific Lord Howe and Norfolk Islands and the Indian-Ocean Christmas Island. 4111 species in 832 genera (including one extinct species and one fossil) are recognised as occurring in this territory, distributed over seven families, 20 subfamilies and 94 tribes. The families and subfamilies are arranged in a currently accepted phylogenetic sequence but the tribes, genera and species in alphabetical order. Introductory chapters outline the discovery and composition of the Australian weevil fauna, the burden of synonymy, the format and conventions of the catalogue and the taxonomic and nomenclatural changes proposed. Sixteen new genera and six new species are described, two new names and 25 new generic and 72 new species synonymies and 189 new combinations are proposed and 46 type species designations are effected. The records of 356 taxa are annotated to justify or explain various taxonomic and nomenclatural acts and issues, covering descriptions of new taxa, new synonymies and generic combinations, artificial taxon concepts, changes in classification and a number of nomenclatural matters. The catalogue of the taxa present in Australia is followed by a list of 19 species incorrectly recorded from Australia or introduced as biocontrol agents but not established, and by one species inquirenda. All these records are also annotated. Two appendices list the 102 species introduced into Australia, both accidental and deliberate (as weed control agents). A bibliography with full references of all original descriptions and pertinent other citations from the literature is provided, and an index to all names concludes the catalogue.

  19. Deep observations of the Super-CLASS supercluster at 325 MHz with the GMRT: the low-frequency source catalogue

    NASA Astrophysics Data System (ADS)

    Riseley, C. J.; Scaife, A. M. M.; Hales, C. A.; Harrison, I.; Birkinshaw, M.; Battye, R. A.; Beswick, R. J.; Brown, M. L.; Casey, C. M.; Chapman, S. C.; Demetroullas, C.; Hung, C.-L.; Jackson, N. J.; Muxlow, T.; Watson, B.

    2016-10-01

    We present the results of 325 MHz Giant Metrewave Radio Telescope observations of a supercluster field, known to contain five Abell clusters at redshift z ˜ 0.2. We achieve a nominal sensitivity of 34 μJy beam-1 towards the phase centre. We compile a catalogue of 3257 sources with flux densities in the range 183 μ {Jy}-1.5 {Jy} within the entire ˜6.5 deg2 field of view. Subsequently, we use available survey data at other frequencies to derive the spectral index distribution for a sub-sample of these sources, recovering two distinct populations - a dominant population which exhibit spectral index trends typical of steep-spectrum synchrotron emission, and a smaller population of sources with typically flat or rising spectra. We identify a number of sources with ultrasteep spectra or rising spectra for further analysis, finding two candidate high-redshift radio galaxies and three gigahertz-peaked-spectrum radio sources. Finally, we derive the Euclidean-normalized differential source counts using the catalogue compiled in this work, for sources with flux densities in excess of 223 μJy. Our differential source counts are consistent with both previous observations at this frequency and models of the low-frequency source population. These represent the deepest source counts yet derived at 325 MHz. Our source counts exhibit the well-known flattening at mJy flux densities, consistent with an emerging population of star-forming galaxies; we also find marginal evidence of a downturn at flux densities below 308 μJy, a feature so far only seen at 1.4 GHz.

  20. THROES: A Catalogue of Herschel Observations of Evolved Stars

    NASA Astrophysics Data System (ADS)

    Ramos-Medina, J.; Sánchez-Contreras, C.; García-Lario, P.; Rodrigo, C.

    2015-12-01

    We are building a catalogue of fully-reprocessed observations of all evolved stars observed with Herschel (THROES). In a first stage, we focus on observations performed with the PACS instrument in its full range spectroscopy mode. Once finished, the catalogue will offer all reduced data for each observation, as well as, complementary information from other observatories. As a first step, we concentrate our efforts on two main activities: 1) the reprocessing and data-reduction of more than 200 individual sources, observed by Herschel/PACS in the 55-210 micron range, available in the Herschel Science Archive (HSA); 2) The creation of an initial catalogue, accesible via web and the Virtual Observatory (VO), with all the information relative to PACS observations and the classification of the sources. Our ultimate goal will be to carry out a comprehensive and systematic study of the far infrared properties of low-and intermediate-mass (1-8 FX1) evolved stars using these data. These objects cover the whole range of possible evolutionary stages in this short-lived phase of stellar evolution, from AGB phase to the PN stage, displaying a wide variety of chemical and physical properties.

  1. NASA space geodesy program: Catalogue of site information

    NASA Technical Reports Server (NTRS)

    Bryant, M. A.; Noll, C. E.

    1993-01-01

    This is the first edition of the NASA Space Geodesy Program: Catalogue of Site Information. This catalogue supersedes all previous versions of the Crustal Dynamics Project: Catalogue of Site Information, last published in May 1989. This document is prepared under the direction of the Space Geodesy and Altimetry Projects Office (SGAPO), Code 920.1, Goddard Space Flight Center. SGAPO has assumed the responsibilities of the Crustal Dynamics Project, which officially ended December 31, 1991. The catalog contains information on all NASA supported sites as well as sites from cooperating international partners. This catalog is designed to provde descriptions and occupation histories of high-accuracy geodetic measuring sites employing space-related techniques. The emphasis of the catalog has been in the past, and continues to be with this edition, station information for facilities and remote locations utilizing the Satellite Laser Ranging (SLR), Lunar Laser Ranging (LLR), and Very Long Baseline Interferometry (VLBI) techniques. With the proliferation of high-quality Global Positioning System (GPS) receivers and Doppler Orbitography and Radiopositioning Integrated by Satellite (DORIS) transponders, many co-located at established SLR and VLBI observatories, the requirement for accurate station and localized survey information for an ever broadening base of scientists and engineers has been recognized. It is our objective to provide accurate station information to scientific groups interested in these facilities.

  2. Dynamic Characterization of Mock Explosive Material Using Reverse Taylor Impact Experiments

    SciTech Connect

    Ferranti, L; Gagliardi, F J; Cunningham, B J; Vandersall, K S

    2010-03-25

    The motivation for the current study is to evaluate the dynamic loading response of an inert mock explosive material used to replicate the physical and mechanical properties of LX-17-1 and PBX 9502 insensitive high explosives. The evaluation of dynamic material parameters is needed for predicting the deformation behavior including the onset of failure and intensity of fragmentation resulting from high velocity impact events. These parameters are necessary for developing and validating physically based material constitutive models that will characterize the safety and performance of energetic materials. The preliminary study uses a reverse Taylor impact configuration that was designed to measure the dynamic behavior of the explosive mock up to and including associated fragmentation. A stationary rod-shaped specimen was impacted using a compressed-gas gun by accelerating a rigid steel anvil attached to a sabot. The impact test employed high-speed imaging and velocity interferometry diagnostics for capturing the transient deformation of the sample at discrete times. Once established as a viable experimental technique with mock explosives, future studies will examine the dynamic response of insensitive high explosives and propellants.

  3. Differences in expert witness knowledge: do mock jurors notice and does it matter?

    PubMed

    Parrott, Caroline T; Neal, Tess M S; Wilson, Jennifer K; Brodsky, Stanley L

    2015-03-01

    The knowledge of experts presumably affects their credibility and the degree to which the trier of fact agrees with them. However, specific effects of demonstrated knowledge are largely unknown. In this experiment, we manipulated a forensic expert's level of knowledge in a mock-trial paradigm. We tested the influence of low versus high expert knowledge on mock juror perceptions of expert credibility, on agreement with the expert, and on sentencing. We also tested expert gender as a potential moderator. Knowledge effects were statistically significant; however, these differences carried little practical utility in predicting mock jurors' ultimate decisions. Contrary to the hypotheses that high knowledge would yield increased credibility and agreement, knowledge manipulations influenced only perceived expert likeability. The low-knowledge expert was perceived as more likeable than the high-knowledge counterpart, a paradoxical finding. No significant differences across expert gender were found. Implications for conceptualizing expert witness knowledge and credibility and their potential effects on juror decision-making are discussed.

  4. Differences in expert witness knowledge: do mock jurors notice and does it matter?

    PubMed

    Parrott, Caroline T; Neal, Tess M S; Wilson, Jennifer K; Brodsky, Stanley L

    2015-03-01

    The knowledge of experts presumably affects their credibility and the degree to which the trier of fact agrees with them. However, specific effects of demonstrated knowledge are largely unknown. In this experiment, we manipulated a forensic expert's level of knowledge in a mock-trial paradigm. We tested the influence of low versus high expert knowledge on mock juror perceptions of expert credibility, on agreement with the expert, and on sentencing. We also tested expert gender as a potential moderator. Knowledge effects were statistically significant; however, these differences carried little practical utility in predicting mock jurors' ultimate decisions. Contrary to the hypotheses that high knowledge would yield increased credibility and agreement, knowledge manipulations influenced only perceived expert likeability. The low-knowledge expert was perceived as more likeable than the high-knowledge counterpart, a paradoxical finding. No significant differences across expert gender were found. Implications for conceptualizing expert witness knowledge and credibility and their potential effects on juror decision-making are discussed. PMID:25770282

  5. VizieR Online Data Catalog: New Numerical Galaxy Catalog (nu2GC) (Makiya+,

    NASA Astrophysics Data System (ADS)

    Makiya, R.; Enoki, M.; Ishiyama, T.; Kobayashi, M. A. R.; Nagashima, M.; Okamoto, T.; Okoshi, K.; Oogi, T.; Shirakata, H.

    2016-10-01

    The mock galaxy catalog calculated by the nu2-GC model descri the paper. File light-cone_nu2gc-H2.dat contains the galaxies having B-band apparent magnitude brighter than 28 [AB mag] and located at the redshift range 0mock galaxy catalogs, catalognu2gc-Lz**.dat, that contain the simulated galaxies in the 1.123 (Gpc/h)3 size box at redshift z = 0.0, 0.48, 1.01, 1.97, 2.95, 6.97. For each simulated galaxy, redshift, comoving distance, stellar mass, gas mass, black hole mass, star formation rate, metallicity, and magnitude in B-, V-, SDSS-rp and 2MASS-Ks bands are given. Terms of Use : When you write papers using these catalogs, we would be very grateful if you could refer the following two papers: Ishiyama et al., 2015PASJ...67...61I, Makiya et al., 2016PASJ...68...25M. (7 data files).

  6. Galaxy formation.

    PubMed

    Peebles, P J

    1998-01-01

    It is argued that within the standard Big Bang cosmological model the bulk of the mass of the luminous parts of the large galaxies likely had been assembled by redshift z approximately 10. Galaxy assembly this early would be difficult to fit in the widely discussed adiabatic cold dark matter model for structure formation, but it could agree with an isocurvature version in which the cold dark matter is the remnant of a massive scalar field frozen (or squeezed) from quantum fluctuations during inflation. The squeezed field fluctuations would be Gaussian with zero mean, and the distribution of the field mass therefore would be the square of a random Gaussian process. This offers a possibly interesting new direction for the numerical exploration of models for cosmic structure formation.

  7. Galaxy formation

    PubMed Central

    Peebles, P. J. E.

    1998-01-01

    It is argued that within the standard Big Bang cosmological model the bulk of the mass of the luminous parts of the large galaxies likely had been assembled by redshift z ∼ 10. Galaxy assembly this early would be difficult to fit in the widely discussed adiabatic cold dark matter model for structure formation, but it could agree with an isocurvature version in which the cold dark matter is the remnant of a massive scalar field frozen (or squeezed) from quantum fluctuations during inflation. The squeezed field fluctuations would be Gaussian with zero mean, and the distribution of the field mass therefore would be the square of a random Gaussian process. This offers a possibly interesting new direction for the numerical exploration of models for cosmic structure formation. PMID:9419326

  8. Shaping galaxy evolution with galaxy structure

    NASA Astrophysics Data System (ADS)

    Cheung, Edmond

    A fundamental pursuit of astronomy is to understand galaxy evolution. The enormous scales and complex physics involved in this endeavor guarantees a never-ending journey that has enamored both astronomers and laymen alike. But despite the difficulty of this task, astronomers have still attempted to further this goal. Among of these astronomers is Edwin Hubble. His work, which includes the famous Hubble sequence, has immeasurably influenced our understanding of galaxy evolution. In this thesis, we present three works that continues Hubble's line of study by using galaxy structure to learn about galaxy evolution. First, we examine the dependence of galaxy quiescence on inner galactic structure with the AEGIS/ DEEP2 survey at 0.5In this thesis, we present three works that continues Hubble's line of study by using galaxy structure to learn about galaxy evolution. First, we examine the dependence of galaxy quiescence on inner galactic structure with the AEGIS/ DEEP2 survey at 0.5galaxies from quiescent galaxies. Our method indicates that the inner stellar mass is the most correlated parameter of quenching, implying that the process that quenches galaxies must also buildup their inner structure. Second, we explore the relationship between galactic bars and their host galaxies with Galaxy Zoo 2 at z˜0. The correlations of bar properties and galaxy properties are consistent with simulations of bar formation and evolution, indicating that bars affect their host galaxies. Finally, we investigate whether bars can drive supermassive black hole growth with data from Chandra and Galaxy Zoo: Hubble at 0.2galaxies to a matched sample of inactive, control galaxies shows that there is no statistically significant excess of bars in active hosts. Our result shows that bars are not the primary fueling mechanism of supermassive black hole

  9. On the quantitative measurement of fracture toughness in high explosive and mock materials

    SciTech Connect

    Liu, Cheng; Cady, Carl M; Rae, Philip J; Lovato, Manuel L

    2010-01-01

    Two approaches in measuring the fracture toughness of heterogeneous high explosives and their mocks are explored in this investigation. One is the global measurement according to the ASTM E 1820-06 standard, which is primarily developed for metallic materials to obtain quantitative measurement of parameters such as the stress intensity factor, the J-integral, and the crack-tip opening displacement (CTOD). The second approach is based on local measurements using digital image correlation (DIC). Detailed results and comparisons of the two strategies will be presented for the Mock 900-21, a mechanical simulant of the PBX 9501 high explosive. Cracking is the most dominant mechanical failure mechanism in high explosives (HE) and a key parameter for describing and predicting crack initiation and extension is the fracture toughness. Quantitative measurement of such material property poses challenges, and this is mainly because that the material is highly heterogeneous with a very complicated microstructure and the contrast of the mechanical properties of the constituents is also remarkably high. In this investigation, we explore two strategies in measuring the fracture toughness of heterogeneous high explosives and their mocks. The first approach is based on the global measurement according to the ASTM E 1820-06 standard, which is primarily developed for metallic materials to obtain quantitative measurement of parameters such as the stress intensity factor, the J-integral, and the crack-tip opening displacement (CTOD). However, there are difficulties in applying the ASTM standard on energetic solids that include identifying the moment of crack initiation and pinpointing exact crack length at each instant of time. The second approach is based on local measurements. We developed a technique for quantitatively identifying the location and extent of macroscopic cracks in heterogeneous high explosive and mock material. By combining such a technique with the displacement field

  10. Northern dwarf and low surface brightness galaxies. IV - The large-scale space distribution

    NASA Technical Reports Server (NTRS)

    Thuan, Trinh X.; Alimi, Jean-Michel; Gott, J. Richard, III; Schneider, Stephen E.

    1991-01-01

    Results are reported from a statistical analysis of published observational data on a sample of 860 northern dwarf and low-surface-brightness (D/LSB) galaxies with delta = 0 deg or greater and b between -40 and 40 deg, selected from the Uppsala General Catalogue of Galaxies (Nilson et al., 1973). The results are presented in extensive redshift/space maps, histograms, graphs and tables and characterized in detail. It is shown that the distribution of D/LSB galaxies closely resembles that of bright galaxies, apparently ruling out biased-star-formation models predicting a uniform distribution of D/LSBs. Although bright galaxies outside clusters are somewhat more clustered than the H I-rich D/LSBs, the latters' pairwise peculiar velocity (460 + or - 50 km/sec) is similar to that of the former.

  11. Dwarf spheroidal galaxies: Keystones of galaxy evolution

    NASA Technical Reports Server (NTRS)

    Gallagher, John S., III; Wyse, Rosemary F. G.

    1994-01-01

    Dwarf spheroidal galaxies are the most insignificant extragalactic stellar systems in terms of their visibility, but potentially very significant in terms of their role in the formation and evolution of much more luminous galaxies. We discuss the present observational data and their implications for theories of the formation and evolution of both dwarf and giant galaxies. The putative dark-matter content of these low-surface-brightness systems is of particular interest, as is their chemical evolution. Surveys for new dwarf spheroidals hidden behind the stars of our Galaxy and those which are not bound to giant galaxies may give new clues as to the origins of this unique class of galaxy.

  12. The initial conditions for stellar protocluster formation. III. The Herschel counterparts of the Spitzer Dark Cloud catalogue

    NASA Astrophysics Data System (ADS)

    Peretto, N.; Lenfestey, C.; Fuller, G. A.; Traficante, A.; Molinari, S.; Thompson, M. A.; Ward-Thompson, D.

    2016-05-01

    Context. Galactic plane surveys of pristine molecular clouds are key for establishing a Galactic-scale view of star formation. For this reason, an unbiased sample of infrared dark clouds in the 10° < | l | < 65°, | b | < 1° region of the Galactic plane was built using Spitzer 8 μm extinction. However, intrinsic fluctuations in the mid-infrared background can be misinterpreted as foreground clouds. Aims: The main goal of this study is to disentangle real clouds in the Spitzer Dark Cloud (SDC) catalogue from artefacts due to fluctuations in the mid-infrared background. Methods: We constructed H2 column density maps at ~18″ resolution using the 160 μm and 250 μm data from the Herschel Galactic plane survey Hi-GAL. We also developed an automated detection scheme that confirms the existence of a SDC through its association with a peak on these Herschel column density maps. Detection simulations, along with visual inspection of a small sub-sample of SDCs, have been performed to get more insight into the limitations of our automated identification scheme. Results: Our analysis shows that 76( ± 19)% of the catalogued SDCs are real. This fraction drops to 55( ± 12)% for clouds with angular diameters larger than ~1 arcmin. The contamination of the PF09 catalogue by large spurious sources reflects the large uncertainties associated to the construction of the 8 μm background emission, a key stage in identiying SDCs. A comparison of the Herschel confirmed SDC sample with the BGPS and ATLASGAL samples shows that SDCs probe a unique range of cloud properties, reaching down to more compact and lower column density clouds than any of these two (sub-)millimetre Galactic plane surveys. Conclusions: Even though about half of the large SDCs are spurious sources, the vast majority of the catalogued SDCs do have a Herschel counterpart. The Herschel-confirmed sample of SDCs offers a unique opportunity to study the earliest stages of both low- and high-mass star formation across

  13. Galaxies at High Redshift

    NASA Astrophysics Data System (ADS)

    Pérez-Fournon, I.; Balcells, M.; Moreno-Insertis, F.; Sánchez, F.

    2010-08-01

    Participants; Group photograph; Preface; Acknowledgements; 1. Galaxy formation and evolution: recent progress R. Ellis; 2. Galaxies at high redshift M. Dickinson; 3. High-redshift galaxies: the far-infrared and sub-millimeter view A. Franceschini; 4. Quasar absorption lines J. Bechtold; 5. Stellar population synthesis models at low and high redshift G. Bruzual A.; 6. Elliptical galaxies K. C. Freeman; 7. Disk galaxies K. C. Freeman; 8. Dark matter in disk galaxies K. C. Freeman.

  14. In Vitro Matured Oocytes Are More Susceptible than In Vivo Matured Oocytes to Mock ICSI Induced Functional and Genetic Changes

    PubMed Central

    Salian, Sujit Raj; Singh, Vikram Jeet; Kalthur, Guruprasad; Adiga, Satish Kumar

    2015-01-01

    Background Concerns regarding the safety of ICSI have been intensified recently due to increased risk of birth defects in ICSI born children. Although fertilization rate is significantly higher in ICSI cycles, studies have failed to demonstrate the benefits of ICSI in improving the pregnancy rate. Poor technical skill, and suboptimal in vitro conditions may account for the ICSI results however, there is no report on the effects of oocyte manipulations on the ICSI outcome. Objective The present study elucidates the influence of mock ICSI on the functional and genetic integrity of the mouse oocytes. Methods Reactive Oxygen Species (ROS) level, mitochondrial status, and phosphorylation of H2AX were assessed in the in vivo matured and IVM oocytes subjected to mock ICSI. Results A significant increase in ROS level was observed in both in vivo matured and IVM oocytes subjected to mock ICSI (P<0.05-0.001) whereas unique mitochondrial distribution pattern was found only in IVM oocytes (P<0.01-0.001). Importantly, differential H2AX phosphorylation was observed in both in vivo matured and IVM oocytes subjected to mock ICSI (P <0.001). Conclusion The data from this study suggests that mock ICSI can alter genetic and functional integrity in oocytes and IVM oocytes are more vulnerable to mock ICSI induced changes. PMID:25786120

  15. The WSRT ZoA Perseus-Pisces filament wide-field H I imaging survey - I. H I catalogue and atlas

    NASA Astrophysics Data System (ADS)

    Ramatsoku, M.; Verheijen, M. A. W.; Kraan-Korteweg, R. C.; Józsa, G. I. G.; Schröder, A. C.; Jarrett, T. H.; Elson, E. C.; van Driel, W.; de Blok, W. J. G.; Henning, P. A.

    2016-07-01

    We present results of a blind 21cm H I-line imaging survey of a galaxy overdensity located behind the Milky Way at ℓ, b ≈ 160°, 0.5°. The overdensity corresponds to a zone-of-avoidance crossing of the Perseus-Pisces Supercluster filament. Although it is known that this filament contains an X-ray galaxy cluster (3C 129) hosting two strong radio galaxies, little is known about galaxies associated with this potentially rich cluster because of the high Galactic dust extinction. We mapped a sky area of ˜9.6 deg2 using the Westerbork Synthesis Radio Telescope in a hexagonal mosaic of 35 pointings observed for 12 h each, in the radial velocity range cz = 2400-16 600 km s-1. The survey has a sensitivity of 0.36 mJy beam-1 rms at a velocity resolution of 16.5 km s-1. We detected 211 galaxies, 62 per cent of which have a near-infrared counterpart in the UKIDSS Galactic Plane Survey. We present a catalogue of the H I properties and an H I atlas containing total intensity maps, position-velocity diagrams, global H I profiles and UKIDSS counterpart images. For the resolved galaxies we also present H I velocity fields and radial H I surface density profiles. A brief analysis of the structures outlined by these galaxies finds that 87 of them lie at the distance of the Perseus-Pisces Supercluster (cz ˜ 4000-8000 km s-1) and seem to form part of the 3C 129 cluster. Further 72 detections trace an overdensity at a velocity of cz ≈ 10 000 km s-1 and seem to coincide with a structure predicted from mass density reconstructions in the first 2MASS Redshift Survey.

  16. Evolution of galaxy structure using visual morphologies in CANDELS and Hydro-ART simulations

    NASA Astrophysics Data System (ADS)

    Mozena, Mark W.

    2013-08-01

    present in the simulations with our observations, we are able to probe the model's ability to create realistic galaxy populations. The first chapter of this thesis focuses on visually classifying and studying galaxy populations at z~2 and how they change with redshift for a given mass. The second chapter focuses on applying our techniques to Hydro-ART simulations at z~2 and comparing these mock 'observed' simulations with our real WFC3 HST observations. Both of these chapters closely resemble manuscripts in the process of being submitted for independent publication.

  17. Diverse structural evolution at z > 1 in cosmologically simulated galaxies

    NASA Astrophysics Data System (ADS)

    Snyder, Gregory F.; Lotz, Jennifer; Moody, Christopher; Peth, Michael; Freeman, Peter; Ceverino, Daniel; Primack, Joel; Dekel, Avishai

    2015-08-01

    From mock Hubble Space Telescope images, we quantify non-parametric statistics of galaxy morphology, thereby predicting the emergence of relationships among stellar mass, star formation, and observed rest-frame optical structure at 1 < z < 3. We measure automated diagnostics of galaxy morphology in cosmological simulations of the formation of 22 central galaxies with 9.3 < log10M*/M⊙ < 10.7. These high-spatial-resolution zoom-in calculations enable accurate modelling of the rest-frame UV and optical morphology. Even with small numbers of galaxies, we find that structural evolution is neither universal nor monotonic: galaxy interactions can trigger either bulge or disc formation, and optically bulge-dominated galaxies at this mass may not remain so forever. Simulated galaxies with M* > 1010M⊙ contain relatively more disc-dominated light profiles than those with lower mass, reflecting significant disc brightening in some haloes at 1 < z < 2. By this epoch, simulated galaxies with specific star formation rates below 10- 9.7 yr- 1 are more likely than normal star-formers to have a broader mix of structural types, especially at M* > 1010 M⊙. We analyse a cosmological major merger at z ˜ 1.5 and find that the newly proposed Multimode-Intensity-Deviation (MID) morphology diagnostics trace later merger stages while Gini-M20 trace earlier ones. MID is sensitive also to clumpy star-forming discs. The observability time of typical MID-enhanced events in our simulation sample is <100 Myr. A larger sample of cosmological assembly histories may be required to calibrate such diagnostics in the face of their sensitivity to viewing angle, segmentation algorithm, and various phenomena such as clumpy star formation and minor mergers.

  18. A Cluster and a Sea of Galaxies

    NASA Astrophysics Data System (ADS)

    2010-05-01

    A new wide-field image released today by ESO displays many thousands of distant galaxies, and more particularly a large group belonging to the massive galaxy cluster known as Abell 315. As crowded as it may appear, this assembly of galaxies is only the proverbial "tip of the iceberg", as Abell 315 - like most galaxy clusters - is dominated by dark matter. The huge mass of this cluster deflects light from background galaxies, distorting their observed shapes slightly. When looking at the sky with the unaided eye, we mostly only see stars within our Milky Way galaxy and some of its closest neighbours. More distant galaxies are just too faint to be perceived by the human eye, but if we could see them, they would literally cover the sky. This new image released by ESO is both a wide-field and long-exposure one, and reveals thousands of galaxies crowding an area on the sky roughly as large as the full Moon. These galaxies span a vast range of distances from us. Some are relatively close, as it is possible to distinguish their spiral arms or elliptical halos, especially in the upper part of the image. The more distant appear just like the faintest of blobs - their light has travelled through the Universe for eight billion years or more before reaching Earth. Beginning in the centre of the image and extending below and to the left, a concentration of about a hundred yellowish galaxies identifies a massive galaxy cluster, designated with the number 315 in the catalogue compiled by the American astronomer George Abell in 1958 [1]. The cluster is located between the faint, red and blue galaxies and the Earth, about two billion light-years away from us. It lies in the constellation of Cetus (the Whale). Galaxy clusters are some of the largest structures in the Universe held together by gravity. But there is more in these structures than the many galaxies we can see. Galaxies in these giants contribute to only ten percent of the mass, with hot gas in between galaxies

  19. On the dust content of galaxy clusters

    NASA Astrophysics Data System (ADS)

    Gutiérrez, C. M.; López-Corredoira, M.

    2014-11-01

    Context. Most of the contribution to dust emission in clusters of galaxies comes from late-type galaxies. However, several ejection processes of material from these galaxies could introduce dust in the intracluster media. Even a relatively low abundance of this dust could act as an efficient cooling agent and have a relevant role in the evolution of clusters. Aims: We present a study to estimate the dust content in galaxy clusters. Methods: This was done by using one the most complete existing catalogues of galaxy clusters based on Sloan Digital Sky Survey (SDSS) data and following two methods: the first one compares the colours of samples of galaxies in the background of clusters with those of galaxies in the field. Using this method, we have explored clustercentric distances up to 6 Mpc; this covers at least 2 × R200 for all the clusters in the sample. The galaxies used in this first method were selected from the SDSS-DR9, among those having reliable photometry and accurate estimation of photometric redshifts. Using the colours of background galaxies, we analyzed several regions at galactic latitudes | b | > 20° and >50°. The results are largely independent of the galactic cut applied. At | b | > 20°, the sample contains 56 985 clusters in the redshift range 0.05 galaxies. The second method computes the contribution of dust in clusters of galaxies to the far infrared sky. That is estimated indirectly by measuring the effect of clusters in the E(B - V) extinction map. Results: Using the first method, we did not find any dependence with clustercentric distance in the colours of background galaxies. As representative of the whole results, the surface integral of the excess of colour g - i in three rings centred in the clusters and with radius 0-1, 0-2, and 0-3 Mpc is -3.7 ± 3.5, + 3.2 ± 6.8, and -4.5 ± 10.1 milimag Mpc2, respectively. This allows us to constrain the mass of dust in the intracluster media

  20. The circumgalactic medium of high-redshift galaxies

    NASA Astrophysics Data System (ADS)

    Pallottini, A.; Gallerani, S.; Ferrara, A.

    2014-10-01

    We study the properties of the circumgalactic medium (CGM) of high-z galaxies in the metal enrichment simulations presented in Pallottini et al. At z = 4, we find that the simulated CGM gas density profiles are self-similar, once scaled with the virial radius of the parent dark matter halo. We also find a simple analytical expression relating the neutral hydrogen equivalent width (EWH I) of CGM absorbers as a function of the line-of-sight impact parameter (b). We test our predictions against mock spectra extracted from the simulations and show that the model reproduces the EWH I(b) profile extracted from the synthetic spectra analysis. When compared with available data, our CGM model nicely predicts the observed EWH I(b) in z ≲ 2 galaxies, and supports the idea that the CGM profile does not evolve with redshift.

  1. Watching a Cannibal Galaxy Dine

    NASA Astrophysics Data System (ADS)

    2009-11-01

    A new technique using near-infrared images, obtained with ESO's 3.58-metre New Technology Telescope (NTT), allows astronomers to see through the opaque dust lanes of the giant cannibal galaxy Centaurus A, unveiling its "last meal" in unprecedented detail - a smaller spiral galaxy, currently twisted and warped. This amazing image also shows thousands of star clusters, strewn like glittering gems, churning inside Centaurus A. Centaurus A (NGC 5128) is the nearest giant, elliptical galaxy, at a distance of about 11 million light-years. One of the most studied objects in the southern sky, by 1847 the unique appearance of this galaxy had already caught the attention of the famous British astronomer John Herschel, who catalogued the southern skies and made a comprehensive list of nebulae. Herschel could not know, however, that this beautiful and spectacular appearance is due to an opaque dust lane that covers the central part of the galaxy. This dust is thought to be the remains of a cosmic merger between a giant elliptical galaxy and a smaller spiral galaxy full of dust. Between 200 and 700 million years ago, this galaxy is indeed believed to have consumed a smaller spiral, gas-rich galaxy - the contents of which appear to be churning inside Centaurus A's core, likely triggering new generations of stars. First glimpses of the "leftovers" of this meal were obtained thanks to observations with the ESA Infrared Space Observatory , which revealed a 16 500 light-year-wide structure, very similar to that of a small barred galaxy. More recently, NASA's Spitzer Space Telescope resolved this structure into a parallelogram, which can be explained as the remnant of a gas-rich spiral galaxy falling into an elliptical galaxy and becoming twisted and warped in the process. Galaxy merging is the most common mechanism to explain the formation of such giant elliptical galaxies. The new SOFI images, obtained with the 3.58-metre New Technology Telescope at ESO's La Silla Observatory

  2. Galaxies Collide to Create Hot, Huge Galaxy

    NASA Technical Reports Server (NTRS)

    2009-01-01

    This image of a pair of colliding galaxies called NGC 6240 shows them in a rare, short-lived phase of their evolution just before they merge into a single, larger galaxy. The prolonged, violent collision has drastically altered the appearance of both galaxies and created huge amounts of heat turning NGC 6240 into an 'infrared luminous' active galaxy.

    A rich variety of active galaxies, with different shapes, luminosities and radiation profiles exist. These galaxies may be related astronomers have suspected that they may represent an evolutionary sequence. By catching different galaxies in different stages of merging, a story emerges as one type of active galaxy changes into another. NGC 6240 provides an important 'missing link' in this process.

    This image was created from combined data from the infrared array camera of NASA's Spitzer Space Telescope at 3.6 and 8.0 microns (red) and visible light from NASA's Hubble Space Telescope (green and blue).

  3. A UNIFIED EMPIRICAL MODEL FOR INFRARED GALAXY COUNTS BASED ON THE OBSERVED PHYSICAL EVOLUTION OF DISTANT GALAXIES

    SciTech Connect

    Bethermin, Matthieu; Daddi, Emanuele; Sargent, Mark T.; Elbaz, David; Mullaney, James; Pannella, Maurilio; Hezaveh, Yashar; Le Borgne, Damien; Buat, Veronique; Charmandaris, Vassilis; Lagache, Guilaine; Scott, Douglas

    2012-10-01

    We reproduce the mid-infrared to radio galaxy counts with a new empirical model based on our current understanding of the evolution of main-sequence (MS) and starburst (SB) galaxies. We rely on a simple spectral energy distribution (SED) library based on Herschel observations: a single SED for the MS and another one for SB, getting warmer with redshift. Our model is able to reproduce recent measurements of galaxy counts performed with Herschel, including counts per redshift slice. This agreement demonstrates the power of our 2-Star-Formation Modes (2SFM) decomposition in describing the statistical properties of infrared sources and their evolution with cosmic time. We discuss the relative contribution of MS and SB galaxies to the number counts at various wavelengths and flux densities. We also show that MS galaxies are responsible for a bump in the 1.4 GHz radio counts around 50 {mu}Jy. Material of the model (predictions, SED library, mock catalogs, etc.) is available online.

  4. Joint constraints on galaxy bias and σ8 through the N-pdf of the galaxy number density

    NASA Astrophysics Data System (ADS)

    Arnalte-Mur, Pablo; Vielva, Patricio; Martínez, Vicent J.; Sanz, José L.; Saar, Enn; Paredes, Silvestre

    2016-03-01

    We present a full description of the N-probability density function of the galaxy number density fluctuations. This N-pdf is given in terms, on the one hand, of the cold dark matter correlations and, on the other hand, of the galaxy bias parameter. The method relies on the assumption commonly adopted that the dark matter density fluctuations follow a local non-linear transformation of the initial energy density perturbations. The N-pdf of the galaxy number density fluctuations allows for an optimal estimation of the bias parameter (e.g., via maximum-likelihood estimation, or Bayesian inference if there exists any a priori information on the bias parameter), and of those parameters defining the dark matter correlations, in particular its amplitude (σ8). It also provides the proper framework to perform model selection between two competitive hypotheses. The parameters estimation capabilities of the N-pdf are proved by SDSS-like simulations (both, ideal log-normal simulations and mocks obtained from Las Damas simulations), showing that our estimator is unbiased. We apply our formalism to the 7th release of the SDSS main sample (for a volume-limited subset with absolute magnitudes Mr <= -20). We obtain hat b = 1.193 ± 0.074 and σ̂8 = 0.862 ± 0.080, for galaxy number density fluctuations in cells of the size of 30h-1Mpc. Different model selection criteria show that galaxy biasing is clearly favoured.

  5. Galaxy NGC 55

    NASA Technical Reports Server (NTRS)

    2003-01-01

    This image of the nearby edge-on spiral galaxy NGC 55 was taken by Galaxy Evolution Explorer on September 14, 2003, during 2 orbits. This galaxy lies 5.4 million light years from our Milky Way galaxy and is a member of the 'local group' of galaxies that also includes the Andromeda galaxy (M31), the Magellanic clouds, and 40 other galaxies. The spiral disk of NGC 55 is inclined to our line of sight by approximately 80 degrees and so this galaxy looks cigar-shaped. This picture is a combination of Galaxy Evolution Explorer images taken with the far ultraviolet (colored blue) and near ultraviolet detectors, (colored red). The bright blue regions in this image are areas of active star formation detected in the ultraviolet by Galaxy Evolution Explorer. The red stars in this image are foreground stars in our own Milky Way galaxy.

  6. Hierarchical Bayesian inference of galaxy redshift distributions from photometric surveys

    NASA Astrophysics Data System (ADS)

    Leistedt, Boris; Mortlock, Daniel J.; Peiris, Hiranya V.

    2016-08-01

    Accurately characterizing the redshift distributions of galaxies is essential for analysing deep photometric surveys and testing cosmological models. We present a technique to simultaneously infer redshift distributions and individual redshifts from photometric galaxy catalogues. Our model constructs a piecewise constant representation (effectively a histogram) of the distribution of galaxy types and redshifts, the parameters of which are efficiently inferred from noisy photometric flux measurements. This approach can be seen as a generalization of template-fitting photometric redshift methods and relies on a library of spectral templates to relate the photometric fluxes of individual galaxies to their redshifts. We illustrate this technique on simulated galaxy survey data, and demonstrate that it delivers correct posterior distributions on the underlying type and redshift distributions, as well as on the individual types and redshifts of galaxies. We show that even with uninformative priors, large photometric errors and parameter degeneracies, the redshift and type distributions can be recovered robustly thanks to the hierarchical nature of the model, which is not possible with common photometric redshift estimation techniques. As a result, redshift uncertainties can be fully propagated in cosmological analyses for the first time, fulfilling an essential requirement for the current and future generations of surveys.

  7. Dwarf Galaxies in the Antlia Cluster: First Results

    NASA Astrophysics Data System (ADS)

    Smith Castelli, A. V.; Bassino, L. P.; Cellone, S. A.; Richtler, T.; Dirsch, B.; Infante, L.; Aruta, C.; Gómez, M.

    The Antlia cluster (l = 273°, b = 19°) is the third nearest galaxy cluster (d = 35 Mpc) after Virgo and Fornax. In spite of its proximity, it has been poorly investigated. Its population is dominated by early type galaxies, with dwarf ellipticals being the most abundant galaxy type [1]. Here we present the first results of a project aimed to study the galaxy population of the Antlia cluster. Our results correspond to the identification and classification of dwarf galaxies in the central cluster region, extending the list of \\cite{FS90} (FS90 catalogue), a photographic survey that is complete only up to B_T ≃ 18 mag (M_B ≃ -14.7 mag at the Antlia cluster distance). The final aim of our project is to study the luminosity function, morphology and structural parameters of dwarf galaxies in the Antlia cluster with a more complete sample. We also intend to investigate the kinematics of the cluster (50 spectra have been already obtained).

  8. An accurate and self-consistent chemical abundance catalogue for the APOGEE/Kepler sample

    NASA Astrophysics Data System (ADS)

    Hawkins, K.; Masseron, T.; Jofré, P.; Gilmore, G.; Elsworth, Y.; Hekker, S.

    2016-10-01

    Context. The APOGEE survey has obtained high-resolution infrared spectra of more than 100 000 stars. Deriving chemical abundances patterns of these stars is paramount to piecing together the structure of the Milky Way. While the derived chemical abundances have been shown to be precise for most stars, some calibration problems have been reported, in particular for more metal-poor stars. Aims: In this paper, we aim to (1) re-determine the chemical abundances of the APOGEE+Kepler stellar sample (APOKASC) with an independent procedure, line list and line selection, and high-quality surface gravity information from asteroseismology; and (2) extend the abundance catalogue by including abundances that are not currently reported in the most recent APOGEE release (DR12). Methods: We fixed the Teff and log g to those determined using spectrophotometric and asteroseismic techniques, respectively. We made use of the Brussels Automatic Stellar Parameter (BACCHUS) code to derive the metallicity and broadening parameters for the APOKASC sample. In addition, we derived differential abundances with respect to Arcturus. Results: We have validated the BACCHUS code on APOGEE data using several well-known stars, and stars from open and globular clusters. We also provide the abundances of C, N, O, Mg, Ca, Si, Ti, S, Al, Na, Ni, Mn, Fe, K, and V for every star and line, and show the impact of line selection on the final abundances. Improvements have been made for some elements (e.g. Ti, Si, V). Additionally, we measure new abundance ratios not found in the current APOGEE release including P, Cu, Rb, and Yb, which are only upper limits at this time, as well as Co and Cr which are promising. Conclusions: In this paper, we present an independent analysis of the APOKASC sample and provide abundances of up to 21 elements. This catalogue can be used not only to study chemical abundance patterns of the Galaxy but also to train data driven spectral approaches which can improve the abundance

  9. Decreased specific star formation rates in AGN host galaxies

    NASA Astrophysics Data System (ADS)

    Shimizu, T. Taro; Mushotzky, Richard F.; Meléndez, Marcio; Koss, Michael; Rosario, David J.

    2015-09-01

    We investigate the location of an ultra-hard X-ray selected sample of active galactic nuclei (AGN) from the Swift Burst Alert Telescope (BAT) catalogue with respect to the main sequence (MS) of star-forming galaxies using Herschel-based measurements of the star formation rate (SFR) and M*'s from Sloan Digital Sky Survey photometry where the AGN contribution has been carefully removed. We construct the MS with galaxies from the Herschel Reference Survey and Herschel Stripe 82 Survey using the exact same methods to measure the SFR and M* as the Swift/BAT AGN. We find that a large fraction of the Swift/BAT AGN lie below the MS indicating decreased specific SFR (sSFR) compared to non-AGN galaxies. The Swift/BAT AGN are then compared to a high-mass galaxy sample (CO Legacy Database for GALEX Arecibo SDSS Survey, COLD GASS), where we find a similarity between the AGN in COLD GASS and the Swift/BAT AGN. Both samples of AGN lie firmly between star-forming galaxies on the MS and quiescent galaxies far below the MS. However, we find no relationship between the X-ray luminosity and distance from the MS. While the morphological distribution of the BAT AGN is more similar to star-forming galaxies, the sSFR of each morphology is more similar to the COLD GASS AGN. The merger fraction in the BAT AGN is much higher than the COLD GASS AGN and star-forming galaxies and is related to distance from the MS. These results support a model in which bright AGN tend to be in high-mass star-forming galaxies in the process of quenching which eventually starves the supermassive black hole itself.

  10. Evaluation of the content coverage of SNOMED-CT to represent ICNP Version 1 catalogues.

    PubMed

    Park, Hyeoun-Ae; Lundberg, Cynthia B; Coenen, Amy; Konicek, Debra J

    2009-01-01

    To evaluate the ability of SNOMED-CT (Systematized Nomenclature of Medicine Clinical Terms) to represent ICNP (International Classification for Nursing Practice) nursing diagnosis and intervention catalogue concepts. We selected the 194 nursing diagnosis and 139 nursing intervention catalogue statements from ICNP Version 1.0. From June 2007 through December 2007, the first author mapped the ICNP catalogue concepts to SNOMED-CT using Apelon's TermWorks and CLUE browser 5.0. The second and fourth authors from SNOMED Terminology Solutions and the third author from ICN validated the mapping result. SNOMED-CT covered 172 concepts of 194 nursing diagnosis and 136 concepts of 139 nursing intervention catalogue concepts. SNOMED-CT can represent most (92.5%) of the ICNP nursing diagnosis and intervention catalogue concepts. Improvements to synonymy and adding missing concepts would lead to greater coverage of nursing diagnosis and intervention catalogue concepts.

  11. Astrophysical Aspects of the Contents of the Input Catalogue

    NASA Astrophysics Data System (ADS)

    Egret, D.; Gómez, E.

    1985-08-01

    The authors illustrate some aspects of the astrophysical contents of the HIPPARCOS Input Catalogue through the comparison of the complete merged file L3 with the file L3/SIM obtained as a result from the first simulation. The following astrophysical topics are considered: the upper part of the HR diagram; the red nearby stars; the distance scale; some problems of galactic structure; old population stars; binary stars with known orbit. The analysis shows, besides a general satisfactory percentage of inclusion for most important programs, an important limitation affecting the faintest red stars, good candidate for parallaxes, but penalized by the observing strategy.

  12. SphinX catalogue of small flares and brightenings

    NASA Astrophysics Data System (ADS)

    Gryciuk, Magdalena; Sylwester, Janusz; Gburek, Szymon; Siarkowski, Marek; Mrozek, Tomasz; Kepa, Anna

    The Solar Photometer in X-rays (SphinX) was designed to measure soft X-ray solar emission in the energy range between 1 keV and 15 keV. The instrument operated from February until November 2009 aboard CORONAS-Photon satellite, during the phase of extraordinary low minimum of solar activity. Thanks to its very high sensitivity SphinX was able to record large number of tiny flares and brightenings. A catalogue of events observed by SphinX will be presented. Results of statistical analysis of events’ characteristics will be discussed.

  13. Catalogue of geoidal variations for simple seafloor topographic features

    NASA Technical Reports Server (NTRS)

    Bowin, C.

    1975-01-01

    A catalogue is presented of theoretical geoidal variations for three types of structural features common to the earth's surface: seamounts, submarine ridges, and submarine trenches. These structures were simulated by simple geometric shapes modeled in three-dimensions. A computer program calculated the potential and gravitational variations over the models. Profile plots of geoidal variations and free-air gravity anomalies are presented over cross-sections of the structures. A ready reference information set is provided for comparison with satellite altimeter data for ocean areas.

  14. The Splatalogue (Spectral Line Catalogue) and Calibase (Calibration Source Database)

    NASA Astrophysics Data System (ADS)

    Markwick-Kemper, Andrew J.; Remijan, A. J.; Fomalont, E.

    2006-06-01

    The next generation of powerful millimeter/submillimeter observatories (ALMA, Herschel) require extensive resources to help identify spectral line transitions and suitable calibration sources. We describe the compilation of a spectral line catalogue and calibration source database. The Calibase is an extensible repository of measurements of radio and submm calibration sources, building on the SMA, PTCS, VLA and VLBA lists. The Splatalogue is a comprehensive transition-resolved compilation of observed, measured and calculated spectral lines. Extending the JPL and CDMS lists, and updating the Lovas/NIST list of observed astrophysical transitions, it adds atomic and recombination lines, template spectra, and is completely VO-compliant, queryable under the IVOA SLAP standard.

  15. ExoData: Open Exoplanet Catalogue exploration and analysis tool

    NASA Astrophysics Data System (ADS)

    Varley, Ryan

    2015-12-01

    ExoData is a python interface for accessing and exploring the Open Exoplanet Catalogue. It allows searching of planets (including alternate names) and easy navigation of hierarchy, parses spectral types and fills in missing parameters based on programmable specifications, and provides easy reference of planet parameters such as GJ1214b.ra, GJ1214b.T, and GJ1214b.R. It calculates values such as transit duration, can easily rescale units, and can be used as an input catalog for large scale simulation and analysis of planets.

  16. A Statistical Approach to Galaxy Cluster Gas Inhomogeneity: Chandra Observations of Nearby Galaxy Clusters

    NASA Astrophysics Data System (ADS)

    Reese, Erik D.; Kawahara, H.; Kitayama, T.; Sasaki, S.; Suto, Y.

    2009-01-01

    Motivated by cosmological hydrodynamic simulations, the intracluster medium (ICM) inhomogeneity of galaxy clusters is modeled statistically with a lognormal model for density inhomogeneity. Through mock observations of synthetic clusters the relationship between density inhomogeneities and that of the X-ray surface brightness has been developed. This enables one to infer the statistical properties of the fluctuations of the underlying three-dimensional density distribution of real galaxy clusters from X-ray observations. We explore inhomogeneity in the intracluster medium by applying the above methodology to Chandra observations of a sample of nearby galaxy clusters. We also consider extensions of the model, including Poissonian effects and compare this hybrid lognormal-Poisson model to the nearby cluster Chandra data. EDR gratefully acknowledges support from JSPS (Japan Society for the Promotion of Science) Postdoctoral Fellowhip for Foreign Researchers award P07030. HK is supported by Grands-in-Aid for JSPS of Science Fellows. This work is also supported by Grant-in-Aid for Scientific research of Japanese Ministry of Education, Culture, Sports, Science and Technology (Nos. 20.10466, 19.07030, 16340053, 20340041, and 20540235) and by JSPS Core-to-Core Program "International Research Network for Dark Energy".

  17. VizieR Online Data Catalog: Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)

    NASA Astrophysics Data System (ADS)

    Cucciati, O.; Marinoni, C.; Iovino, A.; Bardelli, S.; Adami, C.; Mazure, A.; Scodeggio, M.; Maccagni, D.; Temporin, S.; Zucca, E.; de, Lucia G.; Blaizot, J.; Garilli, B.; Meneux, B.; Zamorani, G.; Le Fevre, O.; Cappi, A.; Guzzo, L.; Bottini, D.; Le Brun, V.; Tresse, L.; Vettolani, G.; Zanichelli, A.; Arnouts, S.; Bolzonella, M.; Charlot, S.; Ciliegi, P.; Contini, T.; Foucaud, S.; Franzetti, P.; Gavignaud, I.; Ilbert, O.; Lamareille, F.; McCracken, H. J.; Marano, B.; Merighi, R.; Paltani, S.; Pella, R.; Pollo, A.; Pozzetti, L.; Vergani, D.; Perez-Montero, E.

    2010-08-01

    We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg2^) by means of the VDM algorithm, in the range 0.2<=z<=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement). (2 data files).

  18. The Atacama Cosmology Telescope: Dusty Star-Forming Galaxies and Active Galactic Nuclei in the Southern Survey

    NASA Technical Reports Server (NTRS)

    Marsden, Danica; Gralla, Megan; Marriage, Tobias A.; Switzer, Eric R.; Partridge, Bruce; Massardi, Marcella; Morales, Gustavo; Addison, Graeme; Bond, J. Richard; Crighton, Devin; Das, Sudeep; Devlin, Mark; Dunner, Rolando; Hajian, Amir; Hilton, Matt; Hincks, Adam; Hughes, John P.; Irwin, Kent; Kosowsky, Arthur; Menanteau, Felipe; Moodley, Kavilan; Niemack, Michael; Page, Lyman; Reese, Erik D.; Schmitt, Benjamin; Sehgal, Neelima; Sievers, Johnathan; Staggs, Suzanne; Swetz, Daniel; Thornton, Robert; Wollack, Edward

    2014-01-01

    We present a catalogue of 191 extragalactic sources detected by the Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern survey. Flux densities span 14 -1700 mJy, and we use source spectral indices derived using ACT-only data to divide our sources into two subpopulations: 167 radio galaxies powered by central active galactic nuclei (AGN) and 24 dusty star-forming galaxies (DSFGs). We cross-identify 97 per cent of our sources (166 of the AGN and 19 of the DSFGs) with those in currently available catalogues. When combined with flux densities from the Australia Telescope 20 GHz survey and follow-up observations with the Australia Telescope Compact Array, the synchrotron-dominated population is seen to exhibit a steepening of the slope of the spectral energy distribution from 20 to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated source population has a median spectral index, A(sub 148-218), of 3.7 (+0.62 or -0.86), and includes both local galaxies and sources with redshift around 6. Dusty sources with no counterpart in existing catalogues likely belong to a recently discovered subpopulation of DSFGs lensed by foreground galaxies or galaxy groups.

  19. The Atacama Cosmology Telescope: Dusty Star-Forming Galaxies and Active Galactic Nuclei in the Southern Survey

    NASA Technical Reports Server (NTRS)

    Marsden, Danica; Gralla, Megan; Marriage, Tobias A.; Switzer, Eric R.; Partridge, Bruce; Massardi, Marcella; Morales, Gustavo; Addison, Graeme; Bond, J. Richard; Crichton, Devin; Das, Sudeep; Devlin, Mark; Dunner, Rolando; Hajian, Amir; Hilton, Matt; Hincks, Adam; Hughes, John P.; Irwin, Kent; Kosowsky, Arthur; Menanteau, Felipe; Moodley, Kavilan; Niemack, Michael; Page, Lyman; Reese, Erik D.; Wollack, Edward

    2014-01-01

    We present a catalogue of 191 extragalactic sources detected by the Atacama Cosmology Telescope (ACT) at 148 and/or 218 GHz in the 2008 Southern survey. Flux densities span 14 - 1700 mJy, and we use source spectral indices derived using ACT-only data to divide our sources into two subpopulations: 167 radio galaxies powered by central active galactic nuclei (AGN) and 24 dusty star-forming galaxies (DSFGs). We cross-identify 97 per cent of our sources (166 of the AGN and 19 of the DSFGs) with those in currently available catalogues. When combined with flux densities from the Australia Telescope 20 GHz survey and follow-up observations with the Australia Telescope Compact Array, the synchrotron-dominated population is seen to exhibit a steepening of the slope of the spectral energy distribution from 20 to 148 GHz, with the trend continuing to 218 GHz. The ACT dust-dominated source population has a median spectral index, alpha(sub 148-218), of 3.7 +0.62/-0.86), and includes both local galaxies and sources with redshift around 6. Dusty sources with no counterpart in existing catalogues likely belong to a recently discovered subpopulation of DSFGs lensed by foreground galaxies or galaxy groups.

  20. VizieR Online Data Catalog: The PASTEL catalogue (Soubiran+, 2016-)

    NASA Astrophysics Data System (ADS)

    Soubiran, C.; Le Campion, J.-F.; Brouillet, N.; Chemin, L.

    2016-03-01

    PASTEL is a bibliographical catalogue compiling determinations of stellar atmospheric parameters. It provides (Teff, logg, [Fe/H]) determinations obtained from detailed analyses of high resolution, high signal to noise spectra, carried out with the help of model atmospheres. It also provides effective temperatures Teff from various methods. PASTEL is regularly updated. The catalogue supersedes the two previous versions of the [Fe/H] catalogue (Cayrel de Strobel et al., 1997 [Cat. III/200], 2001 [Cat. III/221]). (1 data file).

  1. VizieR Online Data Catalog: The PASTEL catalogue (Soubiran+, 2010-)

    NASA Astrophysics Data System (ADS)

    Soubiran, C.; Le Campion, J.-F.; Cayrel de Strobel, G.; Caillo, A.

    2010-01-01

    PASTEL is a bibliographical catalogue compiling determinations of stellar atmospheric parameters. It provides (Teff, logg, [Fe/H]) determinations obtained from detailed analyses of high resolution, high signal to noise spectra, carried out with the help of model atmospheres. It also provides effective temperatures Teff from various methods. PASTEL is regularly updated. The catalogue supersedes the two previous versions of the [Fe/H] catalogue (Cayrel de Strobel et al., 1997 [Cat. III/200], 2001 [Cat. III/221]). (1 data file).

  2. Byzantine medical manuscripts: towards a new catalogue, with a specimen for an annotated checklist of manuscripts based on an index of Diels' Catalogue.

    PubMed

    Touwaide, Alain

    2009-01-01

    Greek manuscripts containing medical texts were inventoried at the beginning of the 20th century by a team of philologists under the direction of Hermann Diels. The resulting catalogue, however useful it was when new and still is today, needs to be updated not only because some manuscripts have been destroyed, certain collections and single items have changed location, new shelfmark systems have been sometimes adopted and cataloguing has made substantial progress, but also because in Diels' time the concept of ancient medicine was limited, the method used in compiling data was not standardized and, in a time of manual recording and handling of information, mistakes could not be avoided. The present article is an introduction to a new catalogue of Greek medical manuscripts. In the first part, it surveys the history of the heuristic and cataloguing of Greek medical manuscripts from the 16th century forward; in the second part, it highlights the problems in Diels' catalogue and describes the genesis and methods of the new catalogue, together with the plan for its completion; and in the third part, it provides a sample of such a new catalogue, with a list of the Greek medical manuscripts in the libraries of the United Kingdom and Ireland. PMID:20349553

  3. The Mock LISA Data Challenge Round 3: New and Improved Sources

    NASA Technical Reports Server (NTRS)

    Baker, John

    2008-01-01

    The Mock LISA Data Challenges are a program to demonstrate and encourage the development of data-analysis capabilities for LISA. Each round of challenges consists of several data sets containing simulated instrument noise and gravitational waves from sources of undisclosed parameters. Participants are asked to analyze the data sets and report the maximum information they can infer about the source parameters. The challenges are being released in rounds of increasing complexity and realism. Challenge 3. currently in progress, brings new source classes, now including cosmic-string cusps and primordial stochastic backgrounds, and more realistic signal models for supermassive black-hole inspirals and galactic double white dwarf binaries.

  4. Friends-of-friends galaxy group finder with membership refinement. Application to the local Universe

    NASA Astrophysics Data System (ADS)

    Tempel, E.; Kipper, R.; Tamm, A.; Gramann, M.; Einasto, M.; Sepp, T.; Tuvikene, T.

    2016-04-01

    Context. Groups form the most abundant class of galaxy systems. They act as the principal drivers of galaxy evolution and can be used as tracers of the large-scale structure and the underlying cosmology. However, the detection of galaxy groups from galaxy redshift survey data is hampered by several observational limitations. Aims: We improve the widely used friends-of-friends (FoF) group finding algorithm with membership refinement procedures and apply the method to a combined dataset of galaxies in the local Universe. A major aim of the refinement is to detect subgroups within the FoF groups, enabling a more reliable suppression of the fingers-of-God effect. Methods: The FoF algorithm is often suspected of leaving subsystems of groups and clusters undetected. We used a galaxy sample built of the 2MRS, CF2, and 2M++ survey data comprising nearly 80 000 galaxies within the local volume of 430 Mpc radius to detect FoF groups. We conducted a multimodality check on the detected groups in search for subgroups. We furthermore refined group membership using the group virial radius and escape velocity to expose unbound galaxies. We used the virial theorem to estimate group masses. Results: The analysis results in a catalogue of 6282 galaxy groups in the 2MRS sample with two or more members, together with their mass estimates. About half of the initial FoF groups with ten or more members were split into smaller systems with the multimodality check. An interesting comparison to our detected groups is provided by another group catalogue that is based on similar data but a completely different methodology. Two thirds of the groups are identical or very similar. Differences mostly concern the smallest and largest of these other groups, the former sometimes missing and the latter being divided into subsystems in our catalogue. The catalogues are available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc

  5. Galaxy groups

    SciTech Connect

    Brent Tully, R.

    2015-02-01

    Galaxy groups can be characterized by the radius of decoupling from cosmic expansion, the radius of the caustic of second turnaround, and the velocity dispersion of galaxies within this latter radius. These parameters can be a challenge to measure, especially for small groups with few members. In this study, results are gathered pertaining to particularly well-studied groups over four decades in group mass. Scaling relations anticipated from theory are demonstrated and coefficients of the relationships are specified. There is an update of the relationship between light and mass for groups, confirming that groups with mass of a few times 10{sup 12}M{sub ⊙} are the most lit up while groups with more and less mass are darker. It is demonstrated that there is an interesting one-to-one correlation between the number of dwarf satellites in a group and the group mass. There is the suggestion that small variations in the slope of the luminosity function in groups are caused by the degree of depletion of intermediate luminosity systems rather than variations in the number per unit mass of dwarfs. Finally, returning to the characteristic radii of groups, the ratio of first to second turnaround depends on the dark matter and dark energy content of the universe and a crude estimate can be made from the current observations of Ω{sub matter}∼0.15 in a flat topology, with a 68% probability of being less than 0.44.

  6. Evaluation of the completeness and accuracy of an earthquake catalogue based on hydroacoustic monitoring

    NASA Astrophysics Data System (ADS)

    Willemann, R. J.

    2002-12-01

    NOAA's Pacific Marine Environment Laboratory (PMEL) produces a catalogue of Pacific Ocean earthquakes based on hydroacoustic monitoring from April 1996. The International Seismological Centre (ISC) worked without referring to the PMEL catalogue for earthquakes through April 2000, so the ISC and PMEL catalogues are independent until then. The PMEL catalogue includes many more intraplate and mid-ocean ridge earthquakes; more than 20 times as many earthquakes as the ISC catalogue in some areas. In some areas ISC earthquakes are nearly a strict subset PMEL earthquakes, but elsewhere many ISC earthquakes are not in the PMEL catalogue. Along the Pacific-Antarctic Plate Boundary (45°-70°S, 110°-180°W), for example, the PMEL catalogue misses out many ISC earthquakes, including a few MW(Harvard)>5 crustal earthquakes. Near the Cocos Ridge (2°-7°N, 81°-88°E) for many of the earthquakes in each catalogue, there is no corresponding earthquake in the other. Among earthquakes that are in both catalogues, location differences may be much greater than the formal location uncertainties. But formal errors are known to underestimate true location errors, so studying the seismic arrival time residuals with respect to the hydroacoucoustic origins and hydroacoustic arrival times residuals with respect to the seismic origins provides a more rigorous evaluation of the intrinsic differences between these two monitoring technologies.

  7. Lorentzian’ analysis of the accuracy of modern catalogues of stellar positions

    NASA Astrophysics Data System (ADS)

    Varaksina, N. Y.; Nefedyev, Y. A.; Churkin, K. O.; Zabbarova, R. R.; Demin, S. A.

    2015-12-01

    There is a new approach for the estimation of the position accuracy and proper motions of the stars in astrometric catalogues by comparison of the stars' positions in the researched and Hipparcos catalogues in different periods, but under a standard equinox. To verify this method was carried out the analysis of the star positions and proper motions UCAC2, PPM, ACRS, Tycho-2, ACT, TRC, FON and Tycho catalogues. As a result of this study was obtained that the accuracy of positions and proper motions of the stars in Tycho-2 and UCAC2 catalogues are approximately equal. The results of the comparison are represented graphically.

  8. The origin of galaxies and clusters of galaxies.

    PubMed

    Peebles, P J

    1984-06-29

    Debate on how galaxies and clusters of galaxies formed has reached an interesting stage at which one can find arguments for quite different scenarios. The galaxy distribution has a complex "frothy" character that could be the fossil of a network of protoclusters or pancakes that produced galaxies. However, there are galaxies like our own that seem never to have been in a protocluster but are physically similar to the galaxies in dense clusters. Some clues to be assessed in resolving this dilemma are the possible existence of galaxy filaments, the relative ages of galaxies and clusters of galaxies, and the continuity between cluster and field galaxies and between galaxies and clusters of galaxies.

  9. The distribution of early- and late-type galaxies in the Coma cluster

    NASA Technical Reports Server (NTRS)

    Doi, M.; Fukugita, M.; Okamura, S.; Turner, E. L.

    1995-01-01

    The spatial distribution and the morohology-density relation of Coma cluster galaxies are studied using a new homogeneous photmetric sample of 450 galaxies down to B = 16.0 mag with quantitative morphology classification. The sample covers a wide area (10 deg X 10 deg), extending well beyond the Coma cluster. Morphological classifications into early- (E+SO) and late-(S) type galaxies are made by an automated algorithm using simple photometric parameters, with which the misclassification rate is expected to be approximately 10% with respect to early and late types given in the Third Reference Catalogue of Bright Galaxies. The flattened distribution of Coma cluster galaxies, as noted in previous studies, is most conspicuously seen if the early-type galaxies are selected. Early-type galaxies are distributed in a thick filament extended from the NE to the WSW direction that delineates a part of large-scale structure. Spiral galaxies show a distribution with a modest density gradient toward the cluster center; at least bright spiral galaxies are present close to the center of the Coma cluster. We also examine the morphology-density relation for the Coma cluster including its surrounding regions.

  10. Creation of Large Catalogues by Using of Virtual Observatories

    NASA Astrophysics Data System (ADS)

    Protsyuk, Yu. I.; Kovalchuk, O. M.

    We developed an application program tosearch images in the registers and databases of Virtual Observatories and to download them to local computer. The program has the ability to process XML file in VO Table format to generate links to images, as well as to work directly with the astronomical servers. To improve the efficiency for downloading of large number of images, we used multi-threaded mode. The program runs under the Windows operating system. Using the program in 2014 year, we found and downloaded more than 145 thousand of images of open clusters, having total volume of about 300 GB. Total download time was about 7 days. To process the downloaded images, we created and configured a complex of 10 virtual machines on two PCs for parallel image processing by using Astrometrica program. Total processing time was about 14 days. An application program was also created to analyse the obtained results, which were used to create four catalogues of stellar coordinates at the average epoch of 1953 to 1998. The total number of stars in the catalogues is more than 35 million. The standard error is 0.04" to 0.07", and the average number of observations is 4 to 6. The catalogs are used to improve proper motions of stars in and around of open clusters.

  11. Architectural Historical Heritage: a Tridimensional Multilayers Cataloguing Method

    NASA Astrophysics Data System (ADS)

    Calisi, D.; Tommasetti, A.; Topputo, R.

    2011-09-01

    In the Future the digital filing system will be the method for storing and cataloguing heritages, private assets and arts collections. Today this elaborate process is confined only to the library, painting or parietal heritage. What is missing is a digitalized acquisition of the architectural heritage, which is described at multiple levels of representation. Taking a critical look at the urban setting until you reach the single buildings in their complexity, there is a clear need to establish an open and up-to-date system in order to communicate the different degrees of interaction with the architectural elements that must be preserved and accessed to like a work of art. The breakdown and cataloguing at tridimensional levels affects the different scales of the representation of the city at the stage of stimulating and interactive fruition for those users interested in historical and cognitive research and at the stage of active and project implementation well. The hierarchy of layers of data storage city based should be lived and experienced on a superficial stage as a simple user of the knowledge offered by the digital language of animation and interactivity. It may be the case of a tourist or a citizen who is eager to deepen his awareness of a building, a neighbourhood together with its layering of history and architectural value. This article proposes the development of a database that will be used and extended from time to time with new information related to surveys, projects and restorations of the existing.

  12. A photometric catalogue of southern emission-line stars

    NASA Astrophysics Data System (ADS)

    de Winter, D.; van den Ancker, M. E.; Maira, A.; Thé, P. S.; Djie, H. R. E. Tjin A.; Redondo, I.; Eiroa, C.; Molster, F. J.

    2001-12-01

    We present a catalogue of previously unpublished optical and infrared photometry for a sample of 162 emission-line objects and shell stars visible from the southern hemisphere. The data were obtained between 1978 and 1997 in the Walraven (WULBV), Johnson/Cousins (UBV(RI)c) and ESO and SAAO near-infrared (JHKLM) photometric systems. Most of the observed objects are Herbig Ae/Be (HAeBe) stars or HAeBe candidates appearing in the list of HAeBe candidates of Thé et al. (1994), although several B[e] stars, LBVs and T Tauri stars are also included in our sample. For many of the stars the data presented here are the first photo-electric measurements in the literature. The resulting catalogue consists of 1809 photometric measurements. Optical variability was detected in 66 out of the 116 sources that were observed more than once. 15 out of the 50 stars observed multiple times in the infrared showed variability at 2.2 mu m (K band). Based on observations collected at the European Southern Observatory, La Silla, Chile and on observations collected at the South African Astronomical Observatory. Tables 2-4 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http:/ /cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/380/609

  13. eGenomics: Cataloguing Our Complete Genome Collection III

    PubMed Central

    Field, Dawn; Garrity, George; Gray, Tanya; Selengut, Jeremy; Sterk, Peter; Thomson, Nick; Tatusova, Tatiana; Cochrane, Guy; Glöckner, Frank Oliver; Kottmann, Renzo; Lister, Allyson L.; Tateno, Yoshio; Vaughan, Robert

    2007-01-01

    This meeting report summarizes the proceedings of the “eGenomics: Cataloguing our Complete Genome Collection III” workshop held September 11–13, 2006, at the National Institute for Environmental eScience (NIEeS), Cambridge, United Kingdom. This 3rd workshop of the Genomic Standards Consortium was divided into two parts. The first half of the three-day workshop was dedicated to reviewing the genomic diversity of our current and future genome and metagenome collection, and exploring linkages to a series of existing projects through formal presentations. The second half was dedicated to strategic discussions. Outcomes of the workshop include a revised “Minimum Information about a Genome Sequence” (MIGS) specification (v1.1), consensus on a variety of features to be added to the Genome Catalogue (GCat), agreement by several researchers to adopt MIGS for imminent genome publications, and an agreement by the EBI and NCBI to input their genome collections into GCat for the purpose of quantifying the amount of optional data already available (e.g., for geographic location coordinates) and working towards a single, global list of all public genomes and metagenomes.

  14. The influence of local environment on the emergence of AGN activity in galaxies

    NASA Astrophysics Data System (ADS)

    Martínez, M. A.; Del Olmo, A.; Perea, J.; Coziol, R.; Focardi, P.

    2011-11-01

    We have carried out a spectroscopic study to determine the frequency and nature of the nuclear activity found in compact groups. With this aim we chose two samples, one selected from the Hickson Compact Groups Catalogue and another one from the Updated Zwicky Catalogue of Compact Groups. With the analysis of 1056 galaxies we found that more than 71% present some kind of emission, most of them, being low luminosity AGN (L_{Hα}=10^{39} erg s^{-1}). From these we only detect broad components in 16 which means a remarkable deficiency of broad line AGNs as compared to narrow lineAGNs, despite the high frequency of active galaxies encountered ingeneral in these groups.

  15. Low Strain Rate Compression Measurements of PBX 9501, PBXN-9, and Mock 9501

    NASA Astrophysics Data System (ADS)

    Idar, D. J.; Peterson, P. D.; Scott, P. D.; Funk, D. J.

    1997-07-01

    Low strain rate (10-3 to 10-1 1/s) compression measurements have been obtained on three different composite materials: PBX 9501, PBXN-9, and a sugar mock of PBX 9501. These measurements expand on earlier efforts to identify the behavior of PBX 9501 and sugar mocks at different rates, aspect ratios (L/d) and temperatures. PBX 9501 samples at three different L/d's were strained at the same rate to evalute the effect of aspect ration on stress-strain parameters. Extensometer and strain gage data obtained with these measurements were also compared for precision. PBXN-9 data were obtained at two different L/d's, two different temperatures, an at three different rates. The PBXN-9 data exhibit similar trends to other energetic materials data, i.e. 1) increased ultimate compressive strength and modulus of elasticity with either an increase in strain rate, or decrease in temperature, and 2) small changes in the strain at maximum stress with changes in temperature or strain rate. A comparison of the PBXN-9 data to the PBX 9501 data shows that both begin to fail at comparable strains. However, PBXN-9 is considerably weaker in terms of the ultimate compressive strength.

  16. Low strain rate compression measurements of PBXN-9, PBX 9501, and mock 9501

    SciTech Connect

    Idar, D.J.; Scott, P.D.; Funk, D.J.; Peterson, P.D.

    1998-07-01

    Low strain rate (10{sup {minus}3} to 10{sup {minus}1}s{sup {minus}1}) compression measurements have been obtained on three different composite materials: PBXN-9, PBX 9501, and a 9501 sugar mock. These measurements expand on earlier efforts to identify the behavior of PBX 9501 and sugar mocks at different rates, sample aspect ratios (L/d) and temperatures. PBX 9501 samples at three different L/d{close_quote}s were strained at the same strain rate to evaluate L/d effects on the stress-strain parameters. PBXN-9 data were obtained at two different L/d{close_quote}s, two different temperatures, and at three different rates. The PBXN-9 data exhibit similar trends to other energetic materials data, i.e. 1)increased ultimate compressive strength and modulus of elasticity with either an increase in strain rate, or decrease in temperature, and 2)small increases in the strain at maximum stress with decreases in temperature or strain rate. A comparison of the PBXN-9 data to the PBX 9501 data shows that both begin to fail at comparable strains, however the PBXN-9 data is considerably weaker in terms of the ultimate compressive strength. {copyright} {ital 1998 American Institute of Physics.}

  17. Low strain rate compression measurements of PBX 9501, PBXN-9, and MOCK 9501

    SciTech Connect

    Idar, D.J.; Peterson, P.D.; Scott, P.D.; Funk, D.J.

    1997-07-01

    Low strain rate (10{sup -3} to 10{sup -1} 1/s) compression measurements have been obtained on three different composite materials: PBX 9501, PBXN-9, and a sugar mock of PBX 9501. These measurements expand on earlier efforts to identify the behavior of PBX 9501 and sugar mocks at different rates, aspect ratios (L/d) and temperatures. PBX 9501 samples at three different L/d`s were strained at the same rate to evaluate Lid effects on the stress strain parameters. Extensometer and strain gage data obtained with these measurements were also compared for precision. PBXN-9 data were obtained at two different L/ds, two different temperatures, and at three different rates. The PBXN-9 data exhibit similar trends to other energetic materials data, i.e. 1) increased ultimate compressive strength and modulus of elasticity with either an increase in strain rate, or decrease in temperature, and 2) small changes in the strain at maximum stress with changes in temperature or strain rate. A comparison of the PBXN-9 data to the PBX 9501 data shows that both begin to fail at comparable strains, however the PBXN- 9 data is considerably weaker in terms of the ultimate compressive strength.

  18. Low strain rate compression measurements of PBXN-9, PBX 9501, and mock 9501

    NASA Astrophysics Data System (ADS)

    Idar, D. J.; Peterson, P. D.; Scott, P. D.; Funk, D. J.

    1998-07-01

    Low strain rate (10-3 to 10-1 s-1) compression measurements have been obtained on three different composite materials: PBXN-9, PBX 9501, and a 9501 sugar mock. These measurements expand on earlier efforts to identify the behavior of PBX 9501 and sugar mocks at different rates, sample aspect ratios (L/d) and temperatures. PBX 9501 samples at three different L/d's were strained at the same strain rate to evaluate L/d effects on the stress-strain parameters. PBXN-9 data were obtained at two different L/d's, two different temperatures, and at three different rates. The PBXN-9 data exhibit similar trends to other energetic materials data, i.e. 1)increased ultimate compressive strength and modulus of elasticity with either an increase in strain rate, or decrease in temperature, and 2)small increases in the strain at maximum stress with decreases in temperature or strain rate. A comparison of the PBXN-9 data to the PBX 9501 data shows that both begin to fail at comparable strains, however the PBXN-9 data is considerably weaker in terms of the ultimate compressive strength.

  19. Haemodynamic modeling of the cardiovascular system using mock circulation loops to test cardiovascular devices.

    PubMed

    Timms, Daniel L; Gregory, Shaun D; Stevens, Michael C; Fraser, John F

    2011-01-01

    Comprehensive testing and evaluation of cardiovascular device function and performance is required prior to clinical implementation. Initial proof of concept investigations are conducted within in-vitro mock circulation loops, before proof of principle is demonstrated via in-vivo animal testing. To facilitate the rapid transition of cardiovascular devices through this development period, a testing apparatus was developed that closely models the natural human cardiovascular system haemodynamics. This mock circulation system accurately replicates cardiac function, coupled to systemic and pulmonary circulations. The physiological response produced by a number of clinical cardiovascular conditions can be actively controlled by variable parameters such as vascular resistance, arterial/venous compliance, ventricle contractility, heart rate, and heart /vascular volumes, while anatomical variations such as valve regurgitation and septal defects can be included. Auto-regulation of these parameters was attempted to reproduce the Frank-Starling mechanism, baroreceptor reflex, skeletal muscle pump, and postural changes. Steady state validation of loop performance was achieved by replicating the progression of a patient's clinical haemodynamics from heart failure, through VAD support, to heart transplantation. The system has been used to evaluate pulsatile and non-pulsatile ventricular assist devices, counter pulsation devices, non-invasive cardiac output monitors and cardiovascular stents. The interaction of these devices with the cardiovascular system was also investigated with regards to physiological control strategies and cannula placement. The system is a valuable tool for the accelerated progression of cardiovascular device development.

  20. Damage & fracture of high-explosive mock subject to cyclic loading

    SciTech Connect

    Liu, Cheng; Rae, Philip J; Cady, Carl M; Lovato, Manuel L

    2011-01-11

    We use four-point bend specimen with a single shallow edge notch to study the fracture process in Mock 900-21, a PBX 9501 high explosive simulant mock. Subject to monotonic loading we determine quantitatively the threshold load for macroscopic crack initiation from the notch tip. The four-point bend specimen is then subject to cyclic loading in such a way that during the first cycle, the applied force approaches but does not exceed the threshold load determined from the monotonic loading test and in the subsequent cycles, the overall maximum deformation is maintained to be equal to that of the first cycle. It is expected and is also confirmed that no macroscopic damage and cracking occur during the first cycle. However, we observe that sizable macroscopic crack is generated and enlarged during the subsequent cycles, even though the applied force never exceeds the threshold load. Details of the process of damage fonnation, accumulation, and crack extension are presented and the mechanical mechanism responsible for such failure process is postulated and discussed.