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Sample records for lyman series profiles

  1. Interpreting the convergence of Lyman series absorption lines

    NASA Technical Reports Server (NTRS)

    Jenkins, Edward B.

    1990-01-01

    Spectra of quasars at high z often show absorption at the Lyman limit from intervening gas systems at intermediate z having N(H) approx. greater than 10(exp 7) cm(-2). In some circumstances, N(H) can be determined by measuring the strength of the Lyman limit absorption or the damping wings of Lyman - alpha. With a spectrum taken at low wavelength resolution, say, lambda/delta lambda approx. 10(exp 3), it is usually not possible to distinguish individual Lyman series lines near the limit, yet one can still discern how rapidly the average intensity drops off as the limit is approached from the long wavelength side. The purpose here is to point out the information which is available from measurements of this series convergence.

  2. Lyman alpha solar spectral irradiance line profile observations and models

    NASA Astrophysics Data System (ADS)

    Snow, Martin; Machol, Janet; Quemerais, Eric; Curdt, Werner; Kretschmar, Matthieu; Haberreiter, Margit

    2016-04-01

    Solar lyman alpha solar spectral irradiance measurements are available on a daily basis, but only the 1-nm integrated flux is typically published. The International Space Science Institute (ISSI) in Bern, Switzerland has sponsored a team to make higher spectral resolution data available to the community. Using a combination of SORCE/SOLSTICE and SOHO/SUMER observations plus empirical and semi-empirical modeling, we will produce a dataset of the line profile. Our poster will describe progress towards this goal.

  3. O2 density and temperature profiles retrieving from direct solar Lyman-alpha radiation measurements

    NASA Astrophysics Data System (ADS)

    Guineva, V.; Witt, G.; Gumbel, J.; Khaplanov, M.; Werner, R.; Hedin, J.; Neichev, S.; Kirov, B.; Bankov, L.; Gramatikov, P.; Tashev, V.; Popov, M.; Hauglund, K.; Hansen, G.; Ilstad, J.; Wold, H.

    2009-12-01

    The resonance transition 2P-2S of the atomic hydrogen (Lyman-alpha emission) is the strongest and most conspicuous feature in the solar EUV spectrum. The Lyman-alpha radiation transfer depends on the resonance scattering from the hydrogen atoms in the atmosphere and on the O2 absorption. Since the Lyman-alpha extinction in the atmosphere is a measure for the column density of the oxygen molecules, the atmospheric O2 density and temperature profiles can be calculated thereof. A detector of solar Lyman-alpha radiation was manufactured in the Stara Zagora Department of the Solar-Terrestrial Influences Laboratory (STIL). Its basic part is an ionization camera, filled in with NO. A 60 V power supply is applied to the chamber. The produced photoelectric current from the sensor is fed to a two-channel amplifier, providing analog signal. The characteristics of the Lyman-alpha detector were studied. It passed successfully all tests and the results showed that the so-designed instrument could be used in rocket experiments to measure the Lymanalpha flux. From the measurements of the detector, the Lyman-alpha vertical profile can be obtained. Programs are created to compute the O2 density, atmospheric power and temperature profiles based on Lymanalpha data. The detector design appertained to ASLAF project (Attenuation of the Solar Lyman-Alpha Flux), a scientific cooperation between STIL—Bul.Acad.Sci., Stara Zagora Department and the Atmospheric Physics Group at the Department of Meteorology (MISU), Stockholm University, Sweden. The joint project was part of the rocket experiment HotPay I, in the ALOMAR eARI Project, EU’s 6th Framework Programme, Andøya Rocket Range, Andenes, Norway. The project is partly financed by the Bulgarian Ministry of Science and Education.

  4. A Study of the Lyman-α Line Profile in DBA White Dwarfs

    NASA Astrophysics Data System (ADS)

    Genest-Beaulieu, C.; Bergeron, P.

    2017-03-01

    The hydrogen abundances in DBA white dwarfs determined from optical or UV spectra have been reported to differ significantly in some studies. We revisit this problem using our own model atmospheres and synthetic spectra, and present a theoretical investigation of the Lyman-α line profile as a function of effective temperature and hydrogen abundance. We identify one possible solution to this discrepancy and show considerable improvement from a detailed analysis of optical and UV spectra of DBA stars.

  5. The intrinsic H I Lyman-alpha line profiles of late-type stars

    NASA Technical Reports Server (NTRS)

    Neff, J. E.; Landsman, W. B.; Bookbinder, J. A.; Linsky, J. L.

    1990-01-01

    The Lyman-alpha line of neutral hydrogen is probably the most important cooling channel for chromospheric plasma in late-type stars, yet it is also the least studied major line in the far ultraviolet. The scattering of much of the stellar Lyman-alpha flux by interstellar hydrogen, coupled with the geocoronal emission foreground, seriously complicates the analysis of the Lyman-alpha spectra. The influence of the local interstellar medium on the observed profiles was circumvented by observing stars with radial velocities sufficiently high to Doppler shift the center of the stellar emission line out of the interstellar absorption core. There are several stars that have high radial velocities by virtue of their presence in close binary systems. High resolution IUE (International Ultraviolet Explorer) spectra of Ly alpha line of two such eclipsing binary stars, AR Lac and TY Pyx, are obtained, at each orbital quadrature phase, when the projected orbital velocity is a maximum. By combining the spectra from opposite quadratures it is possible to piece together the entire stellar emission profiles. The third star in this study, delta Lep, is a single star with a high space velocity.

  6. DA white dwarf effective temperatures determined from IUE Lyman-alpha profiles

    NASA Technical Reports Server (NTRS)

    Holberg, J. B.; Basile, J.; Wesemael, F.

    1986-01-01

    The Lyman-alpha profiles of 12 DA white dwarfs have been obtained with the International Ultraviolet Explorer Satellite. Analysis of these profiles provides an improved, uniform, and relatively bias-free measure of effective temperature for these stars over the range 20,000-60,000 K. Simultaneous estimates of surface gravity yield a mean gravity of log g = 7.96 for the entire sample, with the hottest stars tending to have the lowest gravities. A significant exception to this trend occurs in the case of the gravitation of HZ 43. An important by-product of this work has been the determination of a correction to IUE fluxes over the 1150-1350 A range.

  7. Theoretical profiles of Lyman-alpha satellites and application to synthetic spectra of DA white dwarfs

    NASA Technical Reports Server (NTRS)

    Allard, N. F.; Koester, D.

    1992-01-01

    We present new theoretical calculations for the red wing of the Lyman-alpha profile. Close collisions with neutral and ionized hydrogen lead to the formation of the pseudomolecules H-H and H-H(+) with the appearance of satellite features near 1600 and 1400 A. The calculations include multiperturber effects, which are responsible for the formation of H3 and H3 with features near 1950 and 2600 A. The theoretical absorption profiles are included in stellar atmosphere codes and used to predict synthetic spectra for DA white dwarfs of intermediate temperatures (20,000 to 8000 K). These new calculations offer a unique opportunity to determine accurate effective temperatures and surface gravities for the variable ZZ Ceti stars.

  8. Kinetic-Energy Distribution of D(2p) Atoms from Analysis of the D Lyman-Alpha Line Profile

    NASA Technical Reports Server (NTRS)

    Ciocca, M.; Ajello, Joseph M.; Liu, Xianming; Maki, Justin

    1997-01-01

    The kinetic-energy distribution of D(2p) atoms resulting from electron-impact dissociation of D2 has been measured. A high-resolution vacuum ultraviolet spectrometer was employed for the first measurement of the D Lyman-alpha (D L(alpha)) emission line profiles at 20- and 100-eV excitation energies. Analysis of the deconvoluted line profile of D L(alpha) at 100 eV reveals the existence of a narrow line central peak of 29+/-2 mA full width at half maximum and a broad pedestal wing structure about 190 mA wide. The wings of the line can be used to determine the fast atom distribution. The wings of D L(alpha) arise from dissociative excitation of a series of doubly excited states that cross the Franck-Condon region between 23 and 40 eV. The fast atom distribution at 100-eV electron impact energy spans the energy range from 1 to 10 eV with a peak value near 6 eV. Slow D(2p) atoms characterized by a distribution function with peak energy near 100 meV produce the central peak profile, which is nearly independent of the impact energy. The deconvoluted line profiles of the central peak at 20 eV for dissociative excitation of D2 and H2 are fitted with an analytical function for use in calibration of space flight instrumentation equipped with a D/H absorption cell. The kinetic-energy and line profile results are compared to similar measurements for H2. The absolute cross sections for the line center (slow atoms) and wings (fast atoms) and total emission line profile were measured from threshold to 400 eV. Analytical model coefficients are given for the energy dependence of the measured slow atom cross section.

  9. Kinetic-Energy Distribution of D(2p) Atoms from Analysis of the D Lyman-Alpha Line Profile

    NASA Technical Reports Server (NTRS)

    Ciocca, M.; Ajello, Joseph M.; Liu, Xianming; Maki, Justin

    1997-01-01

    The kinetic-energy distribution of D(2p) atoms resulting from electron-impact dissociation of D2 has been measured. A high-resolution vacuum ultraviolet spectrometer was employed for the first measurement of the D Lyman-alpha (D L(alpha)) emission line profiles at 20- and 100-eV excitation energies. Analysis of the deconvoluted line profile of D L(alpha) at 100 eV reveals the existence of a narrow line central peak of 29+/-2 mA full width at half maximum and a broad pedestal wing structure about 190 mA wide. The wings of the line can be used to determine the fast atom distribution. The wings of D L(alpha) arise from dissociative excitation of a series of doubly excited states that cross the Franck-Condon region between 23 and 40 eV. The fast atom distribution at 100-eV electron impact energy spans the energy range from 1 to 10 eV with a peak value near 6 eV. Slow D(2p) atoms characterized by a distribution function with peak energy near 100 meV produce the central peak profile, which is nearly independent of the impact energy. The deconvoluted line profiles of the central peak at 20 eV for dissociative excitation of D2 and H2 are fitted with an analytical function for use in calibration of space flight instrumentation equipped with a D/H absorption cell. The kinetic-energy and line profile results are compared to similar measurements for H2. The absolute cross sections for the line center (slow atoms) and wings (fast atoms) and total emission line profile were measured from threshold to 400 eV. Analytical model coefficients are given for the energy dependence of the measured slow atom cross section.

  10. The Ly(alpha) Line Profiles of Ultraluminous Infrared Galaxies: Fast Winds and Lyman Continuum Leakage

    NASA Technical Reports Server (NTRS)

    Martin, Crystal L.; Dijkstra, Mark; Henry, Alaina L.; Soto, Kurt T.; Danforth, Charles W.; Wong, Joseph

    2015-01-01

    We present new Hubble Space Telescope Cosmic Origins Spectrograph far-ultraviolet (far-UV) spectroscopy and Keck Echellete optical spectroscopy of 11 ultraluminous infrared galaxies (ULIRGs), a rare population of local galaxies experiencing massive gas inflows, extreme starbursts, and prominent outflows. We detect Ly(alpha) emission from eight ULIRGs and the companion to IRAS09583+4714. In contrast to the P Cygni profiles often seen in galaxy spectra, the Ly(alpha) profiles exhibit prominent, blueshifted emission out to Doppler shifts exceeding -1000 km/s in three H II-dominated and two AGN-dominated ULIRGs. To better understand the role of resonance scattering in shaping the Ly(alpha) line profiles, we directly compare them to non-resonant emission lines in optical spectra. We find that the line wings are already present in the intrinsic nebular spectra, and scattering merely enhances the wings relative to the line core. The Ly(alpha) attenuation (as measured in the COS aperture) ranges from that of the far-UV continuum to over 100 times more. A simple radiative transfer model suggests the Ly(alpha) photons escape through cavities which have low column densities of neutral hydrogen and become optically thin to the Lyman continuum in the most advanced mergers. We show that the properties of the highly blueshifted line wings on the Ly(alpha) and optical emission-line profiles are consistent with emission from clumps of gas condensing out of a fast, hot wind. The luminosity of the Ly(alpha) emission increases nonlinearly with the ULIRG bolometric luminosity and represents about 0.1-1% of the radiative cooling from the hot winds in the H II-dominated ULIRGs.

  11. THE Lyα LINE PROFILES OF ULTRALUMINOUS INFRARED GALAXIES: FAST WINDS AND LYMAN CONTINUUM LEAKAGE

    SciTech Connect

    Martin, Crystal L.; Wong, Joseph; Dijkstra, Mark; Henry, Alaina; Soto, Kurt T.; Danforth, Charles W.

    2015-04-10

    We present new Hubble Space Telescope Cosmic Origins Spectrograph far-ultraviolet (far-UV) spectroscopy and Keck Echellete optical spectroscopy of 11 ultraluminous infrared galaxies (ULIRGs), a rare population of local galaxies experiencing massive gas inflows, extreme starbursts, and prominent outflows. We detect Lyα emission from eight ULIRGs and the companion to IRAS09583+4714. In contrast to the P Cygni profiles often seen in galaxy spectra, the Lyα profiles exhibit prominent, blueshifted emission out to Doppler shifts exceeding −1000 km s{sup −1} in three H ii-dominated and two AGN-dominated ULIRGs. To better understand the role of resonance scattering in shaping the Lyα line profiles, we directly compare them to non-resonant emission lines in optical spectra. We find that the line wings are already present in the intrinsic nebular spectra, and scattering merely enhances the wings relative to the line core. The Lyα attenuation (as measured in the COS aperture) ranges from that of the far-UV continuum to over 100 times more. A simple radiative transfer model suggests the Lyα photons escape through cavities which have low column densities of neutral hydrogen and become optically thin to the Lyman continuum in the most advanced mergers. We show that the properties of the highly blueshifted line wings on the Lyα and optical emission-line profiles are consistent with emission from clumps of gas condensing out of a fast, hot wind. The luminosity of the Lyα emission increases nonlinearly with the ULIRG bolometric luminosity and represents about 0.1–1% of the radiative cooling from the hot winds in the H ii-dominated ULIRGs.

  12. The Ly(alpha) Line Profiles of Ultraluminous Infrared Galaxies: Fast Winds and Lyman Continuum Leakage

    NASA Technical Reports Server (NTRS)

    Martin, Crystal L.; Dijkstra, Mark; Henry, Alaina L.; Soto, Kurt T.; Danforth, Charles W.; Wong, Joseph

    2015-01-01

    We present new Hubble Space Telescope Cosmic Origins Spectrograph far-ultraviolet (far-UV) spectroscopy and Keck Echellete optical spectroscopy of 11 ultraluminous infrared galaxies (ULIRGs), a rare population of local galaxies experiencing massive gas inflows, extreme starbursts, and prominent outflows. We detect Ly(alpha) emission from eight ULIRGs and the companion to IRAS09583+4714. In contrast to the P Cygni profiles often seen in galaxy spectra, the Ly(alpha) profiles exhibit prominent, blueshifted emission out to Doppler shifts exceeding -1000 km/s in three H II-dominated and two AGN-dominated ULIRGs. To better understand the role of resonance scattering in shaping the Ly(alpha) line profiles, we directly compare them to non-resonant emission lines in optical spectra. We find that the line wings are already present in the intrinsic nebular spectra, and scattering merely enhances the wings relative to the line core. The Ly(alpha) attenuation (as measured in the COS aperture) ranges from that of the far-UV continuum to over 100 times more. A simple radiative transfer model suggests the Ly(alpha) photons escape through cavities which have low column densities of neutral hydrogen and become optically thin to the Lyman continuum in the most advanced mergers. We show that the properties of the highly blueshifted line wings on the Ly(alpha) and optical emission-line profiles are consistent with emission from clumps of gas condensing out of a fast, hot wind. The luminosity of the Ly(alpha) emission increases nonlinearly with the ULIRG bolometric luminosity and represents about 0.1-1% of the radiative cooling from the hot winds in the H II-dominated ULIRGs.

  13. Doppler line profiles measurement of the Jovian Lyman Alpha emission with OAO-C

    NASA Technical Reports Server (NTRS)

    Barker, E. S.; Cochran, W. D.; Smith, H. J.

    1982-01-01

    Observation of Jupiter made with the high resolution ultraviolet spectrometer of the Orbiting Astronomical Observatory copernicus in April and May, 1980, yield a Jovian Lyman alpha emission intensity of 7 + or 2.5 RR. This indicates a decrease by about a factor of two since the Voyager ultraviolet spectrometer measurements, nearly a year earlier. An unusually high column abundance of hydrogen atoms above the methane homopause at the Voyager epoch is indicated. Since the auroral charged particle bombardment of molecular hydrogen is expected to contribute significantly to the global population of the hydrogen atoms, it is suggested that at the time of the Voyager Jupiter encounter unusually high auroral activity existed, perhaps d to the high concentration of the Io plasma torus. The temporal variation of the Saturn lyman alpha emission, when contrasted with the Jovian data, reveals that the auroral processes are not nearly as important in determining the Saturn Lyman alpha intensity in the nonauroral region.

  14. Observations of the Lyman series forest towards the redshift 7.1 quasar ULAS J1120+0641

    NASA Astrophysics Data System (ADS)

    Barnett, R.; Warren, S. J.; Becker, G. D.; Mortlock, D. J.; Hewett, P. C.; McMahon, R. G.; Simpson, C.; Venemans, B. P.

    2017-05-01

    We present a 30 h integration Very Large Telescope X-shooter spectrum of the Lyman series forest towards the z = 7.084 quasar ULAS J1120+0641. The only detected transmission at S/N > 5 is confined to seven narrow spikes in the Lyα forest, over the redshift range 5.858 Lyman series forest may have been detected. There is a Gunn-Peterson (GP) trough in the Lyα forest from z = 6.122 all the way to the quasar near zone at z = 7.04. The trough, of comoving length 240 h-1 Mpc, is over twice as long as the next longest known GP trough. We combine the spectroscopic and photometric results to constrain the evolution of the Lyα effective optical depth (τGPeff) with redshift, extending a similar analysis by Simpson et al. We find τGPeff ∝ (1 + z)ξ where ξ = 11.2+ 0.4-0.6, for z > 5.5. The data nevertheless provide only a weak limit on the volume-weighted intergalactic medium (IGM) hydrogen neutral fraction at z 6.5, xH i > 10-4, similar to limits at redshift z 6 from less distant quasars. The new observations cannot extend measurements of the neutral fraction of the IGM to higher values because absorption in the Lyα forest is already saturated near z 6. For higher neutral fractions, other methods such as measuring the red damping wing of the IGM will be required.

  15. Modelling of the hydrogen Lyman lines during solar flares

    NASA Astrophysics Data System (ADS)

    Brown, Stephen Alistair; Fletcher, Lyndsay; Labrosse, Nicolas

    2017-08-01

    The hydrogen Lyman series and continuum are both observed with high cadence and spectral resolution by the EVE instrument on NASA’s solar dynamics observatory. The Lyman lines, some of which will also be observed by the SPICE spectrometer on Solar Orbiter, can provide useful information about the dynamics of the solar chromosphere during a flare, where most of the event’s energy is deposited. In Brown et al (2016), we measured line shifts in the Lyman lines using the EVE instrument and calculated corresponding plasma flow speeds of around 30 kilometres per second. However, the observed signs of these shifts varied. We have also modelled Lyman line profiles output from the radiative hydrodynamic code RADYN (Carlsson & Stein 1997, Allred et al 2015) and the radiative transfer code RH (Uitenbroek 2001) and present our initial findings. We show that the dynamics of the plasma are reflected in complex features in the true line profile, but that the detection of a line shift in a particular direction from EVE observations may not be indicative of the true plasma flow, particularly when these model profiles are passed through the EVE instrumental response. We present several cases of atmospheric responses for differing amounts of energy input, and outline interesting features in the Lyman line profiles which are thought to be linked to the response of the dynamic atmosphere.

  16. A New SBUV Ozone Profile Time Series

    NASA Technical Reports Server (NTRS)

    McPeters, Richard

    2011-01-01

    Under NASA's MEaSUREs program for creating long term multi-instrument data sets, our group at Goddard has re-processed ozone profile data from a series of SBUV instruments. We have processed data from the Nimbus 7 SBUV instrument (1979-1990) and data from SBUV/2 instruments on NOAA-9 (1985-1998), NOAA-11 (1989-1995), NOAA-16 (2001-2010), NOAA-17 (2002-2010), and NOAA-18 (2005-2010). This reprocessing uses the version 8 ozone profile algorithm but now uses the Brion, Daumont, and Malicet (BMD) ozone cross sections instead of the Bass and Paur cross sections. The new cross sections have much better resolution, and extended wavelength range, and a more consistent temperature dependence. The re-processing also uses an improved cloud height climatology based on the Raman cloud retrievals of OMI. Finally, the instrument-to-instrument calibration is set using matched scenes so that ozone diurnal variation in the upper stratosphere does not alias into the ozone trands. Where there is no instrument overlap, SAGE and MLS are used to estimate calibration offsets. Preliminary analysis shows a more coherent time series as a function of altitude. The net effect on profile total column ozone is on average an absolute reduction of about one percent. Comparisons with ground-based systems are significantly better at high latitudes.

  17. On the Role of the State in the Governing of Higher Education: A Bibliography of Lyman A. Glenny. Public Administration Series: Bibliography P-929.

    ERIC Educational Resources Information Center

    Quay, Richard H.

    A bibliography of materials authored or coauthored by Lyman A. Glenny from 1951 through 1981 on the role of the state in the governance of higher education is presented. Topics include the following: quality and accountability and statewide review procedures; the role of the state in the governance of higher education; response to stress at 10…

  18. Kinetic Energy Distribution of D(2p) Atoms From Analysis of the D Lyman-a Line Profile

    NASA Technical Reports Server (NTRS)

    Ciocca, Marco; Ajello, Joseph M.; Liu, Xianming; Maki, Justin

    1997-01-01

    The absolute cross sections of the line center (slow atoms) and wings (fast atoms) and total emission line profile were measured from threshold to 400 eV. Analytical model coeffiecients are given for the energy dependence of the measured slow atom cross section.

  19. Kinetic Energy Distribution of D(2p) Atoms From Analysis of the D Lyman-a Line Profile

    NASA Technical Reports Server (NTRS)

    Ciocca, Marco; Ajello, Joseph M.; Liu, Xianming; Maki, Justin

    1997-01-01

    The absolute cross sections of the line center (slow atoms) and wings (fast atoms) and total emission line profile were measured from threshold to 400 eV. Analytical model coeffiecients are given for the energy dependence of the measured slow atom cross section.

  20. Venus Lyman-Alpha a Morphological and Radiative Transfer Analysis

    NASA Astrophysics Data System (ADS)

    Colwell, William Bradford

    The Venus Lyman-α corona is caused by resonance scattering of the solar 1215.67A Lyman-α line by hydrogen atoms in the Venus upper atmosphere. The atmospheric atomic hydrogen content is probed remotely via Lyman-α observations. On 10 February 1990 the Galileo spacecraft flew by Venus, obtaining a series of Venus scans with the Ultraviolet Spectrometer Experiment. The Pioneer Venus Orbiter Ultraviolet Spectrometer obtained Venus Lyman-α images approximately weekly throughout its 14-year mission (1978-1992), spanning the 11-year solar cycle. I analyze the data using a two-dimensional non-isothermal complete-frequency-redistribution multiple scattering code modified from the LYAB code provided by James Bishop for the Earth corona. I employ the VTS3 neutral thermosphere model (Hedin et al., J. Geophys. Res., 88, 73, 1983), and calculate diffusive profiles for the vertical distribution of atomic hydrogen, characterized by hydrogen number density n0 and vertical flux φ0 at the exobase (Paxton et al., J. Geophys. Res., 193, 1766, 1988). The flux parameter controls the hydrogen amount in the lower thermosphere and the exobase density controls the amount in the upper thermosphere and exosphere. I determine the parameter values which best fit the data for selected segments of the sunlit disk, taking advantage of the almost linear relationship between the PV Langmuir probe photoelectron current and measured solar Lyman-α output. I find an equatorial minimum of hydrogen and evidence for a polar hood of enhanced hydrogen abundance. The pre-dawn bulge enhancement near the dawn terminator extends to high latitudes (>60o). All features examined persist throughout solar cycle and increase in hydrogen abundance with solar activity. The parameters I determine agree with the work of Paxton et al. and with densities derived from in situ measurement by Brinton et al. (Geophys. Res. Ler., 7, 865, 1980). Both parameters increase with solar activity and there is evidence suggesting

  1. Hydrogen Lyman Alpha Spectral Line Profiles in Coronal Holes from 1.5 - 6.5 Solar Radii

    NASA Astrophysics Data System (ADS)

    Suleiman, R. M.; Kohl, J. L.; Cranmer, S. R.

    2007-12-01

    UVCS has made detailed measurements of H I Lyα spectral line profiles in a polar coronal hole at projected heliocentric heights from 3.5 to 6.5 R\\odot during 1998 January 5 -- 11. Similar polar coronal hole measurements were made during 1998 June 16 -- 21. Earlier UVCS observations obtained at 1.5 to 2.5 R\\odot are used for comparison. In addition, new measurements are being made for the current phase of the solar cycle. From these measurements we derive 1/e half widths of coronal velocity distributions at the observed heights. The velocity distribution includes all motions contributing to the Doppler shifts along the line of sight (LOS). We also measure absolute intensities that can be used to derive outflow speeds via a Doppler dimming analysis. At large heights in coronal holes, the outflowing coronal plasma becomes nearly collisionless and the ionization balance is believed to become frozen. H I Lyα profile measurements characterize the neutral hydrogen velocity distribution, which at lower heights can also be used to describe the proton distribution. However, in the regions above 3~R\\odot, the H0 velocity distribution may not be the same as that for the protons because the characteristic time for charge transfer between H0 and protons becomes longer than the time it takes for the plasma to flow through a density scale height. Hence, the H0 velocity distribution may not be directly affected by transverse wave motion or wave damping. An indication of an adiabatic radial decrease in the neutral hydrogen temperature would indicate a decoupling of the protons and neutral hydrogen, and also indicate the absence of mechanisms that would heat the neutrals. We will compare the observations with the predictions of a theoretical model of the combined electron, proton and neutral hydrogen plasma. Such a comparison could lead to an improved knowledge of the proton heating at these large heights. This work is supported by the National Aeronautics and Space

  2. Rocket borne solar eclipse experiment to measure the temperature structure of the solar corona via lyman-. cap alpha. line profile observations

    SciTech Connect

    Argo, H.V.

    1981-01-01

    A rocket borne experiment to measure the temperature structure of the inner solar corona via the doppler broadening of the resonance hydrogen Lyman-..cap alpha.. (lambda1216A) radiation scattered by ambient neutral hydrogen atoms was attempted during the 16 Feb 1980 solar eclipse. Two Nike-Black Brant V sounding rockets carrying instrumented payloads were launched into the path of the advancing eclipse umbra from the San Marco satellite launch platform 3 miles off the east coast of Kenya.

  3. D/H in Lyman Limit absorbers with simple velocity structure

    NASA Astrophysics Data System (ADS)

    Webb, John

    2001-07-01

    The deuterium abundance in QSO absorbers provides a direct measurement of the baryonic density of the Universe. We will use STIS to obtain new high resolution data of two carefully selected, intermediate redshift absorption systems. Existing FOS data constrain the velocity structure of these systems and show that the high neutral hydrogen column densities are high enough detect deuterium in the new higher resolution observations we propose here. Markarian 132, z{abs} = 1.7306: The FOS G270 spectrum covers the whole Lyman series from Ly-beta down to the limit. Voigt profile fitting to the whole series reveals two strong components but the system is dominated by a cloud with logN{HI} = 18.3 +/- 0.1 which lies at the blue edge of the complex. The velocity spread within this component is b{eff} < 50 km/s. Ton 34, z{abs} = 1.6077: This is a grey Lyman limit system. The Ly-alpha profile looks fairly narrow. Fitting Voigt profiles to the whole series gives logN{HI} = 17.4 +/- 0.1 and b{eff} < 39 km/s so this system may be a single component system.

  4. Modeling Solar Lyman Alpha Irradiance

    NASA Technical Reports Server (NTRS)

    Pap, J.; Hudson, H. S.; Rottman, G. J.; Willson, R. C.; Donnelly, R. F.; London, J.

    1990-01-01

    Solar Lyman alpha irradiance is estimated from various solar indices using linear regression analyses. Models developed with multiple linear regression analysis, including daily values and 81-day running means of solar indices, predict reasonably well both the short- and long-term variations observed in Lyman alpha. It is shown that the full disk equivalent width of the He line at 1083 nm offers the best proxy for Lyman alpha, and that the total irradiance corrected for sunspot effect also has a high correlation with Lyman alpha.

  5. Computational Method for the Systematic Identification of Analog Series and Key Compounds Representing Series and Their Biological Activity Profiles.

    PubMed

    Stumpfe, Dagmar; Dimova, Dilyana; Bajorath, Jürgen

    2016-08-25

    A computational methodology is introduced for detecting all unique series of analogs in large compound data sets, regardless of chemical relationships between analogs. No prior knowledge of core structures or R-groups is required, which are automatically determined. The approach is based upon the generation of retrosynthetic matched molecular pairs and analog networks from which distinct series are isolated. The methodology was applied to systematically extract more than 17 000 distinct series from the ChEMBL database. For comparison, analog series were also isolated from screening compounds and drugs. Known biological activities were mapped to series from ChEMBL, and in more than 13 000 of these series, key compounds were identified that represented substitution sites of all analogs within a series and its complete activity profile. The analog series, key compounds, and activity profiles are made freely available as a resource for medicinal chemistry applications.

  6. Damped Lyman-α Systems

    NASA Astrophysics Data System (ADS)

    Petitjean, P.; Ledoux, C.

    Recently, Prochaska & Wolfe (1997) have used Keck spectra of 17 DLA absorbers to investigate the kinematics of the neutral gas using unsaturated low excitation transitions such as Si iiλ 1808. They show that the absorption profiles are inconsistent with models of galactic haloes with random motions, spherically infalling gas and slowly rotating hot disks. The CDM model (Kauffmann 1996) is rejected as it produces disks with rotation velocities too small to account for the large observed velocity broadening of the absorption lines. Models of thick disks (h ~0.3 R, where h is the vertical scale and R the radius) with large rotational velocity (v 225kms-1) can reproduce the data. By combining new data on five damped systems with information gathered in the literature, we study the kinematics of the low and high-ionization phases in a sample of 26 damped Lyman-α systems in the redshift range 1.17 - 4.38. We show that the broader the line the more asymmetric, as expected in case rotation dominates the line broadening. However this correlation does not hold for velocities larger than 150 km/s indicating that evidence for rotational motions if any is restricted to velocity broadenings Δ V < 150kms-1. The systems with Δ V > 200kms-1 are peculiar with kinematics consistent with random motions. They show sub-systems as those expected if the objects are in the process of merging.

  7. FUSE/Lyman grant

    NASA Technical Reports Server (NTRS)

    Hurwitz, M.; Bowyer, S.

    1986-01-01

    A variety of options for a short wavelength spectrometer for the Lyman telescope has been studied, and the optimum configuration for this instrument identified. In this spectrometer option study it is assumed (consistent with performance goals outlined by the project) that the instrument, whose prime spectral domain is 900-12000A, will incorporate a grazing incidence telescope which will maintain good collecting efficiency down to 100A. In particular it is assumed that the telescope will have an effective focal length of 10 meters, an image quality of 1.5", and will provide a diverging f/10 beam. Designs compatible with this telescope are analyzed, and it is determined that a two-element grazing incidence spectrometer using as its first optic an ellipsoid to re-focus the beam and a varied line-space plane diffraction grating to disperse the light is the best overall design. This spectrometer could be fed by a small pick-off mirror located just behind the prime focus of the telescope and would clear the light path when not in use. A test of the diffraction efficiency of a low blaze angle grating is undertaken, which is the only technical uncertainty in the spectrometer design.

  8. Rufus A. Lyman: pharmacy's lamplighter.

    PubMed

    Worthen, Dennis B

    2009-08-28

    Rufus Ashley Lyman, a physician, was one of the most prominent leaders in US pharmacy education during the first half of the 20th century. He remains the only individual to be the founding dean at colleges of pharmacy at 2 state universities. His role in the creation and sustenance of the American Journal of Pharmaceutical Education provided a platform for a national community and a sounding board for faculty members and others interested in professional education. His efforts to increase pharmacy educational standards were instrumental in the abandonment of the 2-year graduate in pharmacy (PhG) degree and the universal acceptance of the 4-year bachelor of science (BS) degree. Lyman's simple approach and fierce championship of his beliefs led to his recognition as a lamplighter for the profession.Curt P. Wimmer, chair of the New York Branch of the American Pharmaceutical Association (now the American Pharmacists Association (APhA), introduced the 1947 Remington Honor Medalist, Rufus Ashley Lyman. Wimmer mentioned that Lyman worked as a lamplighter in Omaha, Nebraska, during medical school. Continuing the lamplighter analogy, Wimmer cited Lyman's work as a pharmacy educator and editor: "in the councils of your colleagues, your lamp became a torch emitting red hot sparks that often burnt and seared and scorched -- but always made for progress."1 This description provides an evocative image of one of the most prominent pharmacy educators and leaders of the first half of the 20th century.

  9. Rufus A. Lyman: Pharmacy's Lamplighter

    PubMed Central

    2009-01-01

    Rufus Ashley Lyman, a physician, was one of the most prominent leaders in US pharmacy education during the first half of the 20th century. He remains the only individual to be the founding dean at colleges of pharmacy at 2 state universities. His role in the creation and sustenance of the American Journal of Pharmaceutical Education provided a platform for a national community and a sounding board for faculty members and others interested in professional education. His efforts to increase pharmacy educational standards were instrumental in the abandonment of the 2-year graduate in pharmacy (PhG) degree and the universal acceptance of the 4-year bachelor of science (BS) degree. Lyman's simple approach and fierce championship of his beliefs led to his recognition as a lamplighter for the profession. Curt P. Wimmer, chair of the New York Branch of the American Pharmaceutical Association (now the American Pharmacists Association (APhA), introduced the 1947 Remington Honor Medalist, Rufus Ashley Lyman. Wimmer mentioned that Lyman worked as a lamplighter in Omaha, Nebraska, during medical school. Continuing the lamplighter analogy, Wimmer cited Lyman's work as a pharmacy educator and editor: “in the councils of your colleagues, your lamp became a torch emitting red hot sparks that often burnt and seared and scorched—but always made for progress.”1 This description provides an evocative image of one of the most prominent pharmacy educators and leaders of the first half of the 20th century. PMID:19777099

  10. Interplanetary Lyman-beta emissions

    NASA Technical Reports Server (NTRS)

    Paresce, F.

    1973-01-01

    Derivation of the intensity of the diffuse hydrogen Lyman-beta glow at 1025 A which is due to resonance scattering of the solar H I 1025 A line by interstellar and interplanetary hydrogen. Two sources of neutral hydrogen are considered: the local interstellar medium interacting with the solar system, and the dust deionization of the H(+) component of the solar wind. It is shown that if the dust geometrical factor is less than or equal to five quintillionths per cm, observations of backscattered Lyman-beta radiation will provide a unique determination of the density and temperature of the local interstellar medium.

  11. Analytic Lyman-alpha wing diagnostics and the chromospheric excitation balance in cool dwarfs

    NASA Technical Reports Server (NTRS)

    Gayley, K. G.

    1994-01-01

    I show that the Lyman alpha wings of cool dwarfs can be understood in terms of a very simple model, based on a simplified representation of the chromospheric hydrogen excitation balance and approximate analytic wing diagnostics in partial redistribution. Much of the complexity of the radiation transfer in the partially coherent and steeply temperature-sensitive Lyman alpha line is circumvented by this technique. The result is an expedient scheme for inverting the Lyman alpha wing profile to determine the characteristic free electron density and its gradient in the middle chromosphere. This represents an important new diagnostic for constraining chromospheric models and their radiative losses. I apply this diagnostic to the Lyman alpha wing profiles of the Sun and AU Mic and show that current instrumentation, most notably the Goddard High Resolution Spectrograph (GHRS) on the Hubble Space Telescope, is capable of providing the necessary data.

  12. Profiling and Utilizing Learning Style. NASSP Learning Style Series.

    ERIC Educational Resources Information Center

    Keefe, James W., Ed.

    In 1986, the National Association of Secondary School Principals, with the assistance of a national task force, published the NASSP Learning Style Profile (LSP) for diagnosis of the cognitive styles, perceptual response tendencies, and instructional preferences of middle level and senior high school students. This monograph offers a short course…

  13. Lyman-Alpha Observations of High Radial Velocity Stars

    NASA Astrophysics Data System (ADS)

    Bookbinder, Jay

    1990-12-01

    H I LYMAN -ALPHA (LY-A) IS ONE OF THE MOST IMPORTANT LINES EMITTED BY PLASMA IN THE TEMPERATURE RANGE OF 7000 TO 10 TO THE FIFTH POWER K IN LATE-TYPE STARS. IT IS A MAJOR COMPONENT OF THE TOTAL RADIATIVE LOSS RATE, AND IT PLAYS A CRUCIAL ROLE IN DETERMINING THE ATMOSPHERIC STRUCTURE AND IN FLUORESCING OTHER UV LINES. YET IT IS ALSO THE LEAST STUDIED MAJOR LINE IN THE FAR UV, BECAUSE MOST OF THE LINE FLUX IS ABSORBED BY THE ISM ALONG THE LINE OF SIGHT AND BECAUSE IT IS STRONGLY COMTAMINATED BY THE GEOCORONAL BACKGROUND. A KNOWLEDGE OF THE Ly-A PROFILE IS ALSO IMPORTANT FOR STUDIES OF DEUTERIUM IN THE INTERSTELLAR MEDIUM. BY OBSERVING HIGH RADIAL VELOCITY STARS WE WILL OBTAIN FOR THE FIRST TIME HIGH RESOLUTION SPECTRA OF THE CORE OF A STELLAR H I LYMAN-A EMISSION LINE PROFILE.

  14. Rocket Measurements of the Direct Solar Lyman-alpha Radiation Penetrating in the Atmosphere

    NASA Astrophysics Data System (ADS)

    Guineva, V. H.; Witt, G.; Gumbel, J.; Khaplanov, M.; Tashev, V. L.

    2006-03-01

    The resonance transition 2P-2S of the atomic hydrogen (Lyman-alpha emission) is the strongest and most conspicuous feature in the solar EUV spectrum. The Lyman-alpha radiation transfer depends on the resonance scattering from the hydrogen atoms in the atmosphere and on the O2 absorption. Since the Lyman-alpha extinction in the atmosphere is a measure for the column density of the oxygen molecules, the atmospheric temperature profile can be calculated thereof. Rocket measurements of the direct Lyman-alpha radiation vertical profile in the summer mesosphere and thermosphere (up to 120 km), at high latitudes will be carried out in June 2006. The Lyman-alpha flux will be registered by a detector of solar Lyman-alpha radiation, manufactured in the Stara Zagora Department of the Solar-Terrestrial Influences Laboratory (STIL BAS). Its basic part is an ionization camera, filled in with NO. The scientific data analysis will include raw data reduction, radiative transfer simulations, temperature retrieval as well as co-analysis with other parameters, measured near the polar summer mesopause. This project is a scientific cooperation between STIL-BAS, Stara Zagora Department and the Atmospheric Physics Group at the Department of Meteorology (MISU), Stockholm University, Sweden. The joint project is part from the rocket experiment HotPay I, in the ALOMAR eARI Project, EU's 6th Framework Programme, Andoya Rocket Range, Andenes, Norway.

  15. Lyman-α spectral properties of five newly discovered Lyman continuum emitters

    NASA Astrophysics Data System (ADS)

    Verhamme, A.; Orlitová, I.; Schaerer, D.; Izotov, Y.; Worseck, G.; Thuan, T. X.; Guseva, N.

    2017-01-01

    Aims: We have recently reported the discovery of five low redshift Lyman continuum (LyC) emitters (LCEs) with absolute escape fractions fescLyC that range from 6 to 13%, higher than previously found and that more than double the number of low redshift LCEs. We use these observations to test theoretical predictions about a link between the characteristics of the Lyman-alpha (Lyα) line from galaxies and the escape of ionizing photons. Methods: We analyse the Lyα spectra of eight LCEs of the local Universe observed with the Cosmic Origins Spectrograph onboard the Hubble Space Telescope (our five leakers and three galaxies from the litterature), and compare their strengths and shapes to the theoretical criteria and comparison samples of local galaxies: the Lyman Alpha Reference Survey, Lyman-break analogs, Green Peas, and the high-redshift strong LyC leaker Ion2. Results: Our LCEs are found to be strong Lyα emitters, with high equivalent widths, EW(Lyα) > 70 Å, and large Lyα escape fractions, fescLyα> 20%. The Lyα profiles are all double-peaked with a small peak separation, in agreement with our theoretical expectations. They also have no underlying absorption at the Lyα position. All these characteristics are very different from the Lyα properties of typical star-forming galaxies of the local Universe. A subset of the comparison samples (2-3 Green Pea galaxies) share these extreme values, indicating that they could also be leaking. We also find a strong correlation between the star formation rate surface density and the escape fraction of ionizing photons, indicating that the compactness of star-forming regions plays a role in shaping low column density paths in the interstellar medium of LCEs. Conclusions: The Lyα properties of LCEs are peculiar: Lyα can be used as a reliable tracer of LyC escape from galaxies, complementing other indirect diagnostics proposed in the literature.

  16. Lyman-Alpha aurora

    SciTech Connect

    Durrance, S.T.; Clarke, J.T.

    1984-10-01

    The existence of intense and variable H Ly a emission from Uranus is demonstrated utilizing the monochromatic imaging capabilities of the International Ultraviolet Explorer satellite. A series of 14 observations, using the IUE short wavelength spectrograph in low dispersion and covering the period from 3 March 1982 through 2 September 1983, shows the disk averaged Ly a brightness of Uranus to vary between 690 and 2230 Rayleighs. Model calculations indicates that 400 R of this emission can be attributed to resonant scattering of solar Ly a radiation. An upper limit of 100 R is obtained for the Raman scattering of solar Ly a by H2 (1280 A). This implies that 300 R is contributed to the planetary Ly a emission by Rayleigh scattering. In addition to being unexpectedly strong, the Uranian Ly a emission has been observed to vary by a factor of two in one 24 hr period and by about 50% in one 5 hr period.

  17. Identifying arsenic trioxide (ATO) functions in leukemia cells by using time series gene expression profiles.

    PubMed

    Yang, Hong; Lin, Shan; Cui, Jingru

    2014-02-10

    Arsenic trioxide (ATO) is presently the most active single agent in the treatment of acute promyelocytic leukemia (APL). In order to explore the molecular mechanism of ATO in leukemia cells with time series, we adopted bioinformatics strategy to analyze expression changing patterns and changes in transcription regulation modules of time series genes filtered from Gene Expression Omnibus database (GSE24946). We totally screened out 1847 time series genes for subsequent analysis. The KEGG (Kyoto encyclopedia of genes and genomes) pathways enrichment analysis of these genes showed that oxidative phosphorylation and ribosome were the top 2 significantly enriched pathways. STEM software was employed to compare changing patterns of gene expression with assigned 50 expression patterns. We screened out 7 significantly enriched patterns and 4 tendency charts of time series genes. The result of Gene Ontology showed that functions of times series genes mainly distributed in profiles 41, 40, 39 and 38. Seven genes with positive regulation of cell adhesion function were enriched in profile 40, and presented the same first increased model then decreased model as profile 40. The transcription module analysis showed that they mainly involved in oxidative phosphorylation pathway and ribosome pathway. Overall, our data summarized the gene expression changes in ATO treated K562-r cell lines with time and suggested that time series genes mainly regulated cell adhesive. Furthermore, our result may provide theoretical basis of molecular biology in treating acute promyelocytic leukemia. Copyright © 2013 Elsevier B.V. All rights reserved.

  18. Lyman Alpha Galaxies at High Redshift

    NASA Astrophysics Data System (ADS)

    Rhoads, J. E.; Malhotra, S.; Dawson, S.; Dey, A.; Jannuzi, B. T.; Spinrad, H.; Stern, D.; Wang, J. X.; Xu, C.; Brown, M. J. I.; Landes, E.

    2004-05-01

    Because strong Lyman alpha emission is expected from young star forming galaxies at high redshift, it offers an efficient tool for identifying these galaxies. The Large Area Lyman Alpha survey is one of the first and largest successful searches for Lyman alpha emitting galaxies at high redshift. In the LALA Bootes field (which lies within the NOAO Deep Wide-Field Survey's Bootes field) we have obtained deep narrowband images covering 1/3 square degree in each of eight filters, sampling redshifts z=4.5, 5.7, and 6.5. We focus here on the higher redshift windows, where we have confirmed a luminous Lyman alpha emitting galaxy at z=6.535 and several others in the z=5.7 window. We discuss the physical properties of these objects, including their contribution to star formation rates and metal production. We also discuss the implications of Lyman alpha galaxy observations at z=6.5 for reionization.

  19. The AGN Fraction in Lyman Alpha Galaxies

    NASA Astrophysics Data System (ADS)

    Wang, Junxian; Rhoads, J.; Malhotra, S.

    2007-05-01

    A large fraction of high redshift Lyman-alpha emitters selected through narrow band imaging technique show rest frame equivalent widths (EWs) above 200\\AA. This is beyond the maximum EW expected for normal stellar population. The high EWs can be produced by younger stellar populations, dust, or by type 2 AGNs. We review recent observational progresses on the AGN fraction in high redshift Lyman-alpha searches, including radio, X-ray, and optical spectroscopic observations. Specifically, we show that an upper limit of 5% of the AGN fraction has been obtained based on deep Chandra images. We also present deep IMACS multi-slit spectroscopic observations of 200 candidate z 4.5 Lyman-alpha emitting galaxies selected in the Large Area Lyman Alpha (LALA) narrow band imaging survey Cetus field. This consitutes the largest ever sample of high redshift Lyman-alpha emitters with spectroscopic follow-up.

  20. Biography Today: Sports Series. Profiles of People of Interest to Young Readers, Volume 4.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This book is the fourth in a series of biographies on today's sports figures designed for students age 9 years and older. It contains alphabetically arranged sketches of the sports figures. Each entry provides at least one picture of the individual profiled. Bold faced rubrics lead the reader to information on birth, youth, early memories,…

  1. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 4.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This is the fourth volume of the "Biography Today Author Series." Each volume contains alphabetically arranged sketches. Each entry provides at least one picture of the individual profiled with additional information about the birth, youth, early memories, education, first jobs, marriage and family, career highlights, memorable experiences,…

  2. Biography Today: Profiles of People of Interest to Young Readers. Sports Series, Volume 9.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This ninth volume of the "Biography Today Sports" series is intended to appeal to young readers in a format they can enjoy reading and readily understand. Each alphabetically-arranged sketch provides at least one picture of the individual profiled, and bold-faced rubrics lead the reader to information on birth, youth, early memories,…

  3. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 12.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This special subject volume, "Biography Today Author Series," Volume 12, was designed to appeal to young readers in a format they can enjoy reading and readily understand. Each volume contains alphabetically arranged sketches; each entry provides at least one photograph of the individual profiled, and bold-faced rubrics lead the reader…

  4. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 3.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This is the third volume of the "Biography Today Author Series." Each volume contains alphabetically arranged sketches. Each entry provides at least one picture of the individual profiled with additional information about the birth, youth, early memories, education, first jobs, marriage and family, career highlights, memorable experiences,…

  5. Biography Today: Profiles of People of Interest to Young Readers. Scientists & Inventors Series, Volume 5.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This book, a special volume focusing on computer-related scientists and inventors, provides 12 biographical profiles of interest to readers ages 9 and above. The Biography Today series was created to appeal to young readers in a format they can enjoy reading and readily understand. Each entry provides at least one picture of the individual…

  6. Biography Today: Sports Series. Profiles of People of Interest to Young Readers. Volume 3, 1999.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This third volume is part of a series of biographies that profile individuals of interest to young people over the age of 9 years. The entries in this volume include Joe Dumars, basketball; Jim Harbaugh, football; Dominik Hasek, hockey; Michelle Kwan, figure skating; Rebecca Lobo, basketball; Greg Maddux, baseball; Fatuma Roba, marathon running;…

  7. Weighing the Low-Redshift Lyman-alpha Forest

    NASA Technical Reports Server (NTRS)

    Shull, Mike

    2005-01-01

    In 2003-2004, our FUSE research group prepared several major surveys of the amount of baryonic matter in the intergalactic medium (IGM), using the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite. These surveys include measurements of the Lyman-alpha absorption line of neutral hydrogen (H I), the far-ultraviolet (1032,1038 Angstrom) doublet of highly ionized oxygen ( O VI), the higher Lyman-series lines (Ly-beta, Ly-gamma, etc) of H I, and the 977 Angstrom line of c III. As an overview, our FUSE spectroscopic studies, taken together with data from the Hubble Space Telescope, show that approximately 30% of the normal matter is contained in intergalactic hydrogen gas clouds (the Lyman-alpha forest). Another 5-10% resides in hotter gas at temperatures of 10(exp 5) to 10(exp 6) K, visible in 0 VI and C III absorption. Along with the matter attributed to galaxies, we have now accounted for approximately HALF of all the baryonic matter in the universe. Where is the other half? That matter my exist in even hotter gas, invisible through the ultraviolet absorption lines, but perhaps detectable through X-ray absorption lines of more highly ionized oxygen and neon.

  8. Lyman Alpha Spicule Observatory (LASO)

    NASA Astrophysics Data System (ADS)

    Chamberlin, P. C.; Allred, J. C.; Airapetian, V.; Gong, Q.; Mcintosh, S. W.; De Pontieu, B.; Fontenla, J. M.

    2011-12-01

    The Lyman Alpha Spicule Observatory (LASO) sounding rocket will observe small-scale eruptive events called "Rapid Blue-shifted Events" (RBEs) [Rouppe van der Voort et al., 2009], the on-disk equivalent of Type-II spicules, and extend observations that explore their role in the solar coronal heating problem [De Pontieu et al., 2011]. LASO utilizes a new and novel optical design to simultaneously observe two spatial dimensions at 4.2" spatial resolution (2.1" pixels) over a 2'x2' field of view with high spectral resolution of 66mÅ (33mÅ pixels) across a broad 20Å spectral window. This spectral window contains three strong chromospheric and transition region emissions and is centered on the strong Hydrogen Lyman-α emission at 1216Å. This instrument makes it possible to obtain new data crucial to the physical understanding of these phenomena and their role in the overall energy and momentum balance from the upper chromosphere to lower corona. LASO was submitted March 2011 in response to the ROSES SHP-LCAS call.

  9. Lyman Alpha Spicule Observatory (LASO)

    NASA Astrophysics Data System (ADS)

    Chamberlin, Phillip C.; Allred, J.; Airapetian, V.; Gong, Q.; Fontenla, J.; McIntosh, S.; de Pontieu, B.

    2011-05-01

    The Lyman Alpha Spicule Observatory (LASO) sounding rocket will observe small-scale eruptive events called "Rapid Blue-shifted Events” (RBEs), the on-disk equivalent of Type-II spicules, and extend observations that explore their role in the solar coronal heating problem. LASO utilizes a new and novel optical design to simultaneously observe two spatial dimensions at 4.2" spatial resolution (2.1” pixels) over a 2'x2' field of view with high spectral resolution of 66mÅ (33mÅ pixels) across a broad 20Å spectral window. This spectral window contains three strong chromospheric and transition region emissions and is centered on the strong Hydrogen Lyman-α emission at 1216Å. This instrument makes it possible to obtain new data crucial to the physical understanding of these phenomena and their role in the overall energy and momentum balance from the upper chromosphere to lower corona. LASO was submitted March 2011 in response to the ROSES SHP-LCAS call.

  10. Lyman Alpha Spicule Observatory (LASO)

    NASA Technical Reports Server (NTRS)

    Chamberlin, Phillip C.

    2011-01-01

    The Lyman Alpha Spicule Observatory (LASO) sounding rocket will observe smallscale eruptive events called "Rapid Blue-shifted Events" (RBEs) [Rouppe van der Voort et al., 2009], the on-disk equivalent of Type-II spicules, and extend observations that explore their role in the solar coronal heating problem [De Pontieu et al., 2011]. LASO utilizes a new and novel optical design to simultaneously observe two spatial dimensions at 4.2" spatial resolution (2.1" pixels) over a 2'x2' field of view with high spectral resolution of 66mAngstroms (33mAngstroms pixels) across a broad 20Angstrom spectral window. This spectral window contains three strong chromospheric and transition region emissions and is centered on the strong Hydrogen Lyman-a emission at 1216Angstroms. This instrument makes it possible to obtain new data crucial to the physical understanding of these phenomena and their role in the overall energy and momentum balance from the upper chromosphere to lower corona. LASO was submitted March 2011 in response to the ROSES SHP-LCAS call.

  11. Lyman Alpha Emitters and Galaxy Formation Scenarios

    NASA Astrophysics Data System (ADS)

    Malhotra, S.; Kovac, K.; Somerville, R.; Moustakas, L.; Rhoads, J. E.

    2002-12-01

    The Large Area Lyman Alpha (LALA) survey has successfully identified the population of young Lyman-alpha emitting galaxies predicted about 35 years ago. High equivalent widths of the Lyman-alpha line in these sources suggest that they are a very young (age < 107 years), metal poor, population of stars at redshifts 4.5 and 5.7, making them very interesting objects to study in the context of galaxy formation scenarios. We have begun to do exactly this using the correlation function of LALA galaxies. While the strong correlation function indicates massive halos, the volume density of Lyman-alpha sources and the faint continuum levels indicate low-mass stellar systems. This discrepancy can be resolved by postulating multiple emitters in a single halo.

  12. Results of the mission profile life test. [for J-series mercury ion engines

    NASA Technical Reports Server (NTRS)

    Bechtel, R. T.; Trump, G. E.; James, E. L.

    1982-01-01

    Seven J series 30-cm diameter thrusters have been tested in segments of up to 5,070 hr, for 14,541 hr in the Mission Profile Life Test facility. Test results have indicated the basic thruster design to be consistent with the lifetime goal of 15,000 hr at 2-A beam. The only areas of concern identified which appear to require additional verification testing involve contamination of mercury propellant isolators, which may be due to facility constituents, and the ability of specially covered surfaces to contain sputtered material and prevent flake formation. The ability of the SCR, series resonant inverter power processor to operate the J series thruster and autonomous computer control of the thruster/processor system were demonstrated.

  13. Results of the mission profile life test. [for J-series mercury ion engines

    NASA Technical Reports Server (NTRS)

    Bechtel, R. T.; Trump, G. E.; James, E. L.

    1982-01-01

    Seven J series 30-cm diameter thrusters have been tested in segments of up to 5,070 hr, for 14,541 hr in the Mission Profile Life Test facility. Test results have indicated the basic thruster design to be consistent with the lifetime goal of 15,000 hr at 2-A beam. The only areas of concern identified which appear to require additional verification testing involve contamination of mercury propellant isolators, which may be due to facility constituents, and the ability of specially covered surfaces to contain sputtered material and prevent flake formation. The ability of the SCR, series resonant inverter power processor to operate the J series thruster and autonomous computer control of the thruster/processor system were demonstrated.

  14. Investigation of a Related Series of Turbine-Blade Profiles in Cascade

    NASA Technical Reports Server (NTRS)

    Dunavant, James C.; Erwin, John R.

    1953-01-01

    An application of airfoil design methods was used to design series of related turbine-blade profiles to satisfy the conditions of inlet flow angle and turning angle encountered in the usual range of turbine operation. A series of blade profiles applicable to most turbine blading requirements and a secondary series with particular reference to impulse conditions were designed. Five blade sections from these series ranging in mean-line turning angles from 63 deg. to 120 deg. were tested in low-speed cascade tunnels. From low-speed test results optimum blade angles of attack were selected at each test condition. The induced angle and the deviation angle of the flow were determined from the low-speed data. If these angles are known for the solidity and inlet angle of an application, the necessary camber is specified. A method of predicting high-speed pressure distributions from low-speed cascade test results is presented to extend the usefulness of the low-speed data. Sample high-speed tests of two of the five blade sections were made at Mach numbers up to the critical value. The results indicated satisfactory flow conditions in all of the blade passages tested.

  15. HETDEX: Evolution of Lyman Alpha Emitters

    NASA Astrophysics Data System (ADS)

    Blanc, Guillermo A.; Gebhardt, K.; Hill, G. J.; Gronwall, C.; Ciardullo, R.; Finkelstein, S.; Gawiser, E.; HETDEX Collaboration

    2012-01-01

    The Hobby Eberly Telescope Dark Energy Experiment (HETDEX) will produce a sample of 800,000 Lyman Alpha Emitters (LAEs) over the 1.9Lyman Alpha photon escape fraction. Our results show a strong evolution in the Lyman Alpha escape fraction with redshift, most likely associated with the buildup of dust in the ISM. Dust is shown to be the main parameter setting the escape of Lyman Alpha photons. The observed relation between E(B-V) and the escape fraction indicates that radiative transfer effects in LAEs promote the escape of Lyman Alpha photons, but only up to the point of them suffering similar amounts of extinction as continuum photons. Enhancement of the Lyman Alpha EW (e.g. due to the presence of a clumpy medium) seems not to be a common process in these objects. We also discuss the potential of the full HETDEX sample to study the evolution of LAE properties.

  16. Lyman-α blobs: polarization arising from cold accretion

    NASA Astrophysics Data System (ADS)

    Trebitsch, Maxime; Verhamme, Anne; Blaizot, Jérémy; Rosdahl, Joakim

    2016-10-01

    Lyman-α nebulae are typically found in massive environments at high redshift (z ≳ 2). The origin of their Lyman-α (Lyα) emission remains debated. Recent polarimetric observations showed that at least some Lyα sources are polarized. This is often interpreted as proof that the photons are centrally produced and contradicts the scenario in which the Lyα emission is the cooling radiation emitted by gas that is heated during the accretion onto the halo. We suggest that this cooling radiation scenario is compatible with the polarimetric observations. To test this idea, we post-processed a radiative hydrodynamics simulation of a blob with the MCLya Monte Carlo transfer code. We computed radial profiles for the surface brightness and the degree of polarization and compared them to existing observations. We found that computed and observed profiles both are consistent with a significant contribution of the extragalactic gas to the Lyα emission. Most of the photons are centrally emitted and are subsequently scattered inside the filament, which produces the observed high level of polarization. We argue that the contribution of the extragalactic gas to the Lyα emission does not prevent polarization. On the contrary, we find that pure galactic emission causes the polarization profile to be too steep to be consistent with observations.

  17. Simultaneous measurements of the hydrogen airglow emissions of Lyman alpha, Lyman beta, and Balmer alpha.

    NASA Technical Reports Server (NTRS)

    Weller, C. S.; Meier, R. R.; Tinsley, B. A.

    1971-01-01

    Comparison of Lyman-alpha, 740- to 1050-A, and Balmer-alpha airglow measurements made at 134 deg solar-zenith angle on Oct. 13, 1969, with resonance-scattering models of solar radiation. Model comparison with Lyman-alpha data fixes the hydrogen column abundance over 215 km to 2 x 10 to the 13th per cu cm within a factor of 2. Differences between the Lyman-alpha model and data indicate a polar-equatorial departure from spherical symmetry in the hydrogen distribution. A Lyman-beta model based on the hydrogen distribution found to fit the Lyman-alpha data fits the spatial variation of the 740- to 1050-A data well from 100 to 130 km, but it does not fit the data well at higher altitudes; thus the presence of more rapidly absorbed shorter-wavelength radiation is indicated. This same resonance-scattering model yields Balmer-alpha intensities that result in good spatial agreement with the Balmer-alpha measurements, but a fivefold increase in the measured solar line center Lyman-beta flux is required (as required for the Lyman-beta measurement). The intensity ratio of Lyman-beta and Balmer-alpha at night is found to be a simple measure of the hydrogen optical depth if measurements with good accuracy can be made in the visible and ultraviolet spectrum.

  18. GALEX NUV Lyman break galaxies

    NASA Astrophysics Data System (ADS)

    Williger, G. M.; Haberzettl, L.; Lehnert, M. D.; Nesvadba, N. P. H.; Valls-Gabaud, D.

    2010-12-01

    Lyman Break Galaxies (LBGs) have been the benchmarks against which other samples of high redshift galaxies have been compared for the last 2 decades. They are unique in that no other selection mechanism allows us to study galaxies selected in a consistent manner over redshifts 0.5≲ z≲ 7. An important remaining gap is the redshift range z˜1.5-2.5, which includes NUV-band dropouts. We searched for LBGs at this epoch using very sensitive multi-wavelength data from the FUV to mid-IR in the GOODS-S. We combined the dropout technique with color selection to identify star-forming galaxies at 1.5≲ z≲ 2.5. We find only a small overlap with the BM/BX selection method (Adelberger et al. 2004), and our sample of ˜ 200 z˜ 2 LBG candidates includes a significant number of relatively redder LBGs. By comparing our results to other selection methods for star-forming galaxies at z˜2 (BM/BX, BzK), we can show that the use of true dropout selection results in a cleaner, more efficient sample of LBG candidates. Our selected z˜ 2 LBG candidates are more consistent with LBG samples at z≤ 3 than BM/BX and BzK galaxies, despite our sample including relatively younger, lower mass systems.

  19. The Re-Analysis of Ozone Profile Data from a 41-Year Series of SBUV Instruments

    NASA Technical Reports Server (NTRS)

    Kramarova, Natalya; Frith, Stacey; Bhartia, Pawan K.; McPeters, Richard; Labow, Gordon; Taylor, Steven; Fisher, Bradford

    2012-01-01

    In this study we present the validation of ozone profiles from a number of Solar Back Scattered Ultra Violet (SBUV) and SBUV/2 instruments that were recently reprocessed using an updated (Version 8.6) algorithm. The SBUV dataset provides the longest available record of global ozone profiles, spanning a 41-year period from 1970 to 2011 (except a 5-year gap in the 1970s) and includes ozone profile records obtained from the Nimbus-4 BUV and Nimbus-7 SBUV instruments, and a series of SBUV(/2) instruments launched on NOAA operational satellites (NOAA 09, 11, 14, 16, 17, 18, 19). Although modifications in instrument design were made in the evolution from the BUV instrument to the modern SBUV(/2) model, the basic principles of the measurement technique and retrieval algorithm remain the same. The long term SBUV data record allows us to create a consistent, calibrated dataset of ozone profiles that can be used for climate studies and trend analyses. In particular, we focus on estimating the various sources of error in the SBUV profile ozone retrievals using independent observations and analysis of the algorithm itself. For the first time we include in the metadata a quantitative estimate of the smoothing error, defined as the error due to profile variability that the SBUV observing system cannot inherently measure. The magnitude of the smoothing error varies with altitude, latitude, season and solar zenith angle. Between 10 and 1 hPa the smoothing errors for the SBUV monthly zonal mean retrievals are of the order of 1 %, but start to increase above and below this layer. The largest smoothing errors, as large as 15-20%, were detected in in the troposphere. The SBUV averaging kernels, provided with the ozone profiles in version 8.6, help to eliminate the smoothing effect when comparing the SBUV profiles with high vertical resolution measurements, and make it convenient to use the SBUV ozone profiles for data assimilation and model validation purposes. The smoothing error can

  20. Lyman-alpha imagery of Comet Kohoutek

    NASA Technical Reports Server (NTRS)

    Carruthers, G. R.; Opal, C. B.; Page, T. L.; Meier, R. R.; Prinz, D. K.

    1974-01-01

    Electrographic imagery of Comet Kohoutek in the 1100-1500 A wavelength range was obtained from a sounding rocket on Jan. 8, 1974, and from the Skylab space station on 13 occasions between Nov. 26, 1973 and Feb. 2, 1974. These images are predominantly due to Lyman-alpha (1216 A) emission from the hydrogen coma of the comet. The rocket pictures have been calibrated for absolute sensitivity and a hydrogen production rate has been determined. However, the Skylab camera suffered degradation of its sensitivity during the mission, and its absolute sensitivity for each observation can only be estimated by comparison of the comet images with those taken by the rocket camera, with imagery of the geocoronal Lyman-alpha glow, of the moon in reflected Lyman-alpha, and of ultraviolet-bright stars. The rocket and geocoronal comparisons are used to derive a preliminary, qualitative history of the development of the cometary hydrogen coma and the associated hydrogen production rate.

  1. Time series modeling of live-cell shape dynamics for image-based phenotypic profiling.

    PubMed

    Gordonov, Simon; Hwang, Mun Kyung; Wells, Alan; Gertler, Frank B; Lauffenburger, Douglas A; Bathe, Mark

    2016-01-01

    Live-cell imaging can be used to capture spatio-temporal aspects of cellular responses that are not accessible to fixed-cell imaging. As the use of live-cell imaging continues to increase, new computational procedures are needed to characterize and classify the temporal dynamics of individual cells. For this purpose, here we present the general experimental-computational framework SAPHIRE (Stochastic Annotation of Phenotypic Individual-cell Responses) to characterize phenotypic cellular responses from time series imaging datasets. Hidden Markov modeling is used to infer and annotate morphological state and state-switching properties from image-derived cell shape measurements. Time series modeling is performed on each cell individually, making the approach broadly useful for analyzing asynchronous cell populations. Two-color fluorescent cells simultaneously expressing actin and nuclear reporters enabled us to profile temporal changes in cell shape following pharmacological inhibition of cytoskeleton-regulatory signaling pathways. Results are compared with existing approaches conventionally applied to fixed-cell imaging datasets, and indicate that time series modeling captures heterogeneous dynamic cellular responses that can improve drug classification and offer additional important insight into mechanisms of drug action. The software is available at http://saphire-hcs.org.

  2. HETDEX: Diffuse Lyman-Alpha Emission

    NASA Astrophysics Data System (ADS)

    Tuttle, Sarah E.; Finkelstein, S.; Gebhardt, K.; HETDEX Collaboration

    2012-01-01

    The intermediate redshift universe probed by HETDEX, 1.8 < z < 3.0, holds a great deal of information about star formation and the evolution of galaxies. Although simulations reveal a regime active with gas accretion and feeding of galaxies via filaments, observational evidence for this accretion from the Intergalactic Medium (IGM) at any redshift has been very limited. Here we use data from VIRUS-P across several well-characterized fields to put limits on diffuse emission of Lyman-Alpha at the outskirts of galaxies. This work is done in preparation for a similar program with the full HETDEX sample of Lyman-Alpha Emitters (LAEs).

  3. Initial neuropsychological profile of a series of 20 patients with logopenic variant of primary progressive aphasia.

    PubMed

    Magnin, Eloi; Chopard, Gilles; Ferreira, Sabrina; Sylvestre, Geraldine; Dariel, Elfried; Ryff, Ilham; Mertz, Catherine; Lamidieu, Charlie; Hidalgo, Julie; Tio, Gregory; Haffen, Sophie; Galmiche, Jean; Moulin, Thierry; Vandel, Pierre; Rumbach, Lucien

    2013-01-01

    Logopenic variant of primary progressive aphasia (LPPA) is classically considered as an isolated language disorder, but verbal short-term memory deficit induces difficulties in neuropsychological tests that are not intended to evaluate language. The aim of this study is to describe the initial symptoms and neuropsychological profiles of LPPA. A retrospective study was conducted with a series of 20 consecutive patients diagnosed with LPPA. Clinical, neuroimaging, neuropsychological, and linguistic examinations are reported. The first neuropsychological examinations (mean time between neuropsychological assessment and diagnosis: 11 months) were then compared to 20 patients with mild cognitive impairment (MCI) and 20 patients with Alzheimer's disease (AD) matched by age, gender, and education level. A recent onset or aggravation of anxiety disorders was frequently reported. An unusual neuropsychological profile, different from that of AD or MCI, was observed: dissociation between verbal and visual memory performances, poor encoding performances on verbal memory tests, and preserved orientation to time, difficulties with mental calculation and fluency tasks. Biparetal abnormality and left hippocampal diaschisis was frequently observed. Asymptomatic dopaminergic depletion was observed in four patients. Our study identifies that de novo or recently worsening anxiety and specific neuropsychological profiles call for screening for LPPA, including a linguistic examination. Sometimes, there may be a continuum between LPPA and corticobasal syndrome.

  4. Dissecting the Lyman α emission halo of LAB1

    NASA Astrophysics Data System (ADS)

    Weijmans, Anne-Marie; Bower, Richard G.; Geach, James E.; Swinbank, A. Mark; Wilman, R. J.; de Zeeuw, P. T.; Morris, Simon L.

    2010-03-01

    We report observations of Lyman alpha blob 1 (LAB1) in the SSA 22 protocluster region (z = 3.09) with the integral-field spectrograph SAURON. We increased the signal-to-noise ratio in the spectra by more than a factor of 3 compared to our previous observations. This allows us to probe the structure of the LAB system in detail, examining its structure in the spatial and wavelength dimensions. We find that the emission from the system comes largely from five distinct blobs. Two of the emission regions are associated with Lyman break galaxies, while a third appears to be associated with a heavily obscured submillimeter galaxy. The fourth and fifth components do not appear to be associated with any galaxy despite the deep imaging that is available in this field. If we interpret wavelength shifts in the line centroid as velocity structure in the underlying gas, many of these emission systems show evidence of velocity shear. It remains difficult to distinguish between an underlying rotation of the gas and an outflow driven by the central object. We have examined all of the line profiles for evidence of strong absorption features. While several systems are better fitted by the inclusion of a weak absorption component, we do not see evidence for a large-scale coherent absorption feature such as that seen in LAB2.

  5. Shedding Lyman Alpha Light on Cosmological Reionization

    NASA Astrophysics Data System (ADS)

    Rhoads, James E.; Malhotra, Sangeeta; Ammons, S. Mark; Dressler, Alan; Gonzalez, Alicia; Finkelstein, Steven; Hibon, Pascale; Jiang, Tianxing; Lee, Janice; Mobasher, Bahram; Monson, Andy; Persson, S. Eric; Probst, Ronald; Swaters, Rob; Tilvi, Vithal S.; Veilleux, Sylvain; Wang, Junxian; Zabludoff, Ann; Zheng, Zhenya

    2015-08-01

    Lyman alpha photons are a powerful tool for studying reionization. They interact strongly with neutral hydrogen, so that neutral intergalactic gas acts to hide Lyman alpha light from our instruments. I will discuss two ongoing narrowband surveys to study the Epoch of Reionization. The Deep And Wide Narrowband (DAWN) survey is a 40 night NOAO survey program to look for Lyman alpha emission at redshift 7.7, using the NEWFIRM camera on the 4m Mayall Telescope at Kitt Peak National Observatory. The First Light And Reionization Experiment (FLARE) is pursuing a corresponding survey at redshift 8.8, using the FourStar camera on the Magellan telescope. Both surveys are motivated by the application of Lyman alpha lines to the study of reionization. Reionization marked the first global impact that gravitationally bound objects (stars and/or black holes) had on the universe around them, and also the last time that most hydrogen atoms did anything noteworthy. I will present results from both the DAWN and FLARE surveys, which have identified candidate galaxies near redshifts 7.7 and 8.8 in multiple fields.

  6. Experimental investigation of uranium-series isotope mobility in a basaltic weathering profile

    NASA Astrophysics Data System (ADS)

    Dosseto, Anthony; Menozzi, Davide; Kinsley, Leslie

    2015-04-01

    The measurement of uranium (U)-series isotopes in regolith can be used to determine the formation rate of weathering profiles. This approach aims at following how the U-series isotope composition of primary minerals (i.e. those derived from the parent material) vary during the development of the weathering profile. Nevertheless, regolith samples are a complex mixture of primary minerals, secondary minerals that are the residue of primary mineral weathering, secondary minerals that precipitate from pore water, minerals derived from atmospheric deposition and organic matter. In this study, firstly we aim at isolating primary minerals and the secondary minerals derived from them, by evaluating a sequential extraction procedure designed to eliminate carbonates, Fe-Mn oxides and organic matter. Secondly, we investigate the behaviour of U-series isotopes during primary mineral dissolution by applying a mild HF/HCl etching solution to the residues of the sequential extraction. These experiments were performed on bedrock, saprolite and soil derived from a basaltic weathering profile in south-eastern Australia. Results show that up to 50% of U is removed during sequential extraction, suggesting that (i) there is a large pool of labile U in the bedrock and (ii) secondary phases and organic matter account for a large fraction of the U budget in bulk saprolite and soil. Sequential extraction has little impact on the (234U/238U) activity ratio of bedrock and saprolite, whilst it shows a decrease in soil. This suggests that the pool of U removed from bedrock and saprolite has a (234U/238U) similar to that of primary minerals; but in the soil, the U removed (mostly from organic matter) is enriched in 234U. This is expected as organic matter uptakes U from pore solutions, which are generally enriched in 234U. During HF/HCl etching, the (234U/238U) of bedrock and saprolite is greater than 1. Sheng and Kuroda [1] previously proposed that (234U/238U) >1 in rocks could be explained by

  7. HETDEX: Developing the HET's Second Generation Low Resolution Spectrograph for Probing Lyman-alpha Emitting Galaxies

    NASA Astrophysics Data System (ADS)

    Chonis, Taylor S.; Hill, G. J.; Lee, H.; Tuttle, S. E.; Vattiat, B. L.; Gebhardt, K.; Finkelstein, S. L.; Adams, J. J.; HETDEX Collaboration

    2012-01-01

    HETDEX will map the power spectrum of 0.8 million blindly discovered Lyman-alpha Emitting Galaxies (LAE) using a revolutionary new array of massively replicated fiber-fed spectrographs dubbed the Visible Integral-Field Replicable Unit Spectrograph (VIRUS). In the era of the Hobby-Eberly Telescope wide-field upgrade and VIRUS, the current Low Resolution Spectrograph (LRS) must be replaced with a fiber instrument. We discuss the development of the second generation LRS (LRS2), which is a multi-channel instrument based on the VIRUS design. In its current design phase, it is fed by a 287 fiber microlens coupled integral field unit that covers 7” x 12” with 0.62” resolution. The instrument covers 3720 Å to 4700 Å at R ≈ 1900 and 4600 Å to 7000 Å at R ≈1200. With the purpose of making the instrument ideal for follow-up observations of LAE in the HETDEX survey, we discuss the science drivers for selecting the instrument's spectral resolution. We test the utility of the instrument and pilot a future study with LRS2 by presenting R ≈ 2000 spectra taken with the VIRUS prototype spectrograph (VIRUS-P) in a high-resolution mode at the McDonald Observatory Harlan J. Smith 2.7 m telescope. These LAE were originally discovered in the HETDEX Pilot Survey and their Lyman-alpha line profiles are constrained by near-infrared observations of rest-frame optical emission lines that set the systemic redshift of the galaxies. We discuss the velocity offsets of the Lyman-alpha line from the systemic line center and compare the line profiles to theoretical predictions and to similar observations for Lyman-break galaxies. Our observations provide an example of how LRS2 can be used to probe Lyman-alpha emission in 2 < z < 3 star forming galaxies.

  8. The impact of Lyman-alpha trapping on the massive black hole seed formation

    NASA Astrophysics Data System (ADS)

    Ge, Qi

    2015-01-01

    Supermassive black holes with masses up to a few billion solar masses have been observed when the universe was only one billion years old. One viable seeding mechanism for these black holes is the direct gaseous collapse into a massive black hole on the order of 104 - 106solar masses. This process can only occur when atomic hydrogen line cooling is efficient and fragmentation is suppressed during the collapse, thus requiring metal-line and molecular hydrogen cooling to be insignificant. As the cloud collapses to high densities, neutral hydrogen becomes optically thick to Lyman-alpha radiation, limiting the effectiveness of radiative cooling. We improve on previous methods of treating the optically thick regime, such as an effective equation of state, by formulating an approximate method to calculate the local trapping of Lyman-alpha radiation, which considers both non-coherence scattering and line cooling from the Lyman series. Here we explore its effect on massive black hole formation in cosmological simulations with the adaptive mesh refinement code Enzo. We show that Lyman-alpha trapping can further suppress fragmentation and affect the local thermodynamical state of the central collapsing gas cloud. By including this process at high densities, we expect that our results will provide more accurate conditions and accretion rates, leading to the formation of a supermassive star or quasistar.

  9. Restframe Optical Properties of Lyman Break Galaxies

    NASA Astrophysics Data System (ADS)

    Shapley, A. E.; Steidel, C. C.; Adelberger, K. L.; Pettini, M.; Dickinson, M. E.; Giavalisco, M.

    2000-12-01

    We review recent results from near-IR studies of z ~ 3 galaxies that have been selected by their broadband optical colors using the Lyman Break technique. Specifically, we discuss the use of near-IR imaging at J and Ks, in combination with previously obtained optical photometry, to untangle the degenerate effects of dust extinction and age on galaxy spectral energy distributions. We use the observed optical-to-infrared colors for a subsample of galaxies from our extensive high-redshift survey to constrain both the amount of dust and the ages of the observed stellar populations. Thus, we hope to learn about distribution of ages, unextincted star-formation rates, and formed stellar masses of these high-redshift galaxies. We also make use of the restframe UV luminosity function of Lyman Break galaxies, in combination with the distribution of restframe UV-to-optical colors (measured with the R-Ks color at z ~ 3), to determine the restframe optical luminosity function of Lyman Break galaxies. Finally, we describe new efforts, using near-infrared spectroscopy, to study familiar restframe optical nebular emission lines redshifted to 1.5 - 2.5 μm in z ~ 3 galaxies. The properties of these emission features should indicate the range of dynamical masses and metallicities of high redshift star-forming galaxies. We also hope to use the velocity offsets measured between restframe optical nebular lines, Lyman-α , and restframe-UV interstellar metal lines, to characterize the starburst-induced outflows present in Lyman Break galaxies, how they depend on other galaxy properties, and what their impact is on the surrounding intergalactic medium.

  10. Observation of a Lyman-alpha flare with PROBA2/LYRA

    NASA Astrophysics Data System (ADS)

    Wauters, Laurence; Dominique, Marie; Dammasch, Ingolf; Kretzschmar, Matthieu

    2017-08-01

    Lyman-alpha (121.6 nm) is an optical thick line mostly formed in the chromosphere. Although one of the strongest lines of the solar spectrum, there are very few reports of solar flare signatures in Lyman-alpha and the few observations available differ significantly in shape, time duration and amplitude. Consequently, the fraction of non-thermal energy deposited during solar flares in this wavelength is still subject to discussion. The LYRA experiment is a radiometer on board the PROBA2 spacecraft launched in 2009. LYRA is composed of three identical units (one nominal, two backups), which each includes four distinct broadband channels, among which one covering Lyman-alpha. Despite the fact that the LYRA Lyman-alpha signal has degraded quickly at the beginning of the mission in the nominal channel, it observed about ten flares. Additionally, one more flare was observed in one of the backup channels. In this talk, we will analyse this particular flare profile and compare it to other instruments including Goes-15, EVE/MEGS-P, LYRA Zirconium channel.

  11. A Sounding Rocket Experiment for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP)

    NASA Technical Reports Server (NTRS)

    Kubo, M.; Kano, R.; Kobayashi, K.; Ishikawa, R.; Bando, T.; Narukage, N.; Katsukawa, Y.; Ishikawa, S.; Suematsu, Y.; Hara, H.; Tsuneta, S.; Shimizu, T.; Sakao, T.; Ichimoto, K.; Winebarger, A.; Cirtain, J.; De Pontieu, B.; Casini, R.; Auchere, F.; Trujillo, Bueno J.; Manso, Sainz R.; Ramos, Asensio A.; Stepan, J.; Belluzi, L.; Carlsson, M.

    2014-01-01

    A sounding-rocket experiment called the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is presently under development to measure the linear polarization profiles caused by scattering processes and the Hanle effect in the hydrogen Lyman-alpha line (121.567nm). Accurate measurements of the linear polarization signals caused by scattering processes and the Hanle effect are essential to explore the strength and structures of weak magnetic fields. The primary target of future solar telescopes is to measure the weak magnetic field in outer solar atmospheres (from the chromosphere to the corona through the transition region). The hydrogen Lyman-alpha-line is one of the best lines for the diagnostics of magnetic fields in the outer solar atmospheres. CLASP is to be launched in 2015, and will provide, for the first time, the observations required for magnetic field measurements in the upper chromosphere and transition region. CLASP is designed to have a polarimetric sensitivity of 0.1% and a spectral resolution of 0.01nm for the Lyman-alpha line. CLASP will measure two orthogonal polarizations simultaneously for about 5-minute flight. Now the integration of flight mirrors and structures is in progress. In addition to our strategy to realize such a high-precision spectro-polarimetry in the UV, we will present a progress report on our pre-launch evaluation of optical and polarimetric performances of CLASP.

  12. Changes in weight loss and lipid profiles after a dietary purification program: a prospective case series

    PubMed Central

    Callahan, Erica

    2013-01-01

    Objective The purpose of this case series was to describe immediate changes to weight and lipid profiles after a 21-day Standard Process whole food supplement and dietary modification program. Methods Changes in weight and lipid profiles were measured for 7 participants (6 men and 1 woman) participating in a 21-day program. The dietary modifications throughout the Standard Process program were consumption of (1) unlimited fresh or frozen vegetables and fruits and preferably twice as many vegetables as fruits, (2) ½ to 1 cup of cooked lentils or brown rice each day, (3) 4 to 7 teaspoons of cold pressed oils per day, and (4) at least 64 oz of water a day. After day 10 of the program, participants were allowed to consume 1 to 2 servings of baked, broiled, or braised poultry or fish per day. Participants consumed a whey protein–based shake as meal replacement 2 times per day. Nutritional supplementation included a cleanse product on days 1 to 7, soluble fiber supplementation including oat bran concentrate and apple pectin on all days, and “green food” supplementation on days 8 to 21. Results Weight loss ranged between 5.2 (2.4 kg) and 19.9 lb (9.0 kg) (average, 11.7 lb; 5.3 kg). Total cholesterol levels decreased with ranges between 11 and 77 mg/dL, and low-density lipoprotein cholesterol levels decreased in a range between 7 and 67 mg/dL. Conclusion After participating in a dietary program, the 7 participants demonstrated short-term weight loss and improvements in their lipid profiles. PMID:23997722

  13. Changes in weight loss and lipid profiles after a dietary purification program: a prospective case series.

    PubMed

    Callahan, Erica

    2013-03-01

    The purpose of this case series was to describe immediate changes to weight and lipid profiles after a 21-day Standard Process whole food supplement and dietary modification program. Changes in weight and lipid profiles were measured for 7 participants (6 men and 1 woman) participating in a 21-day program. The dietary modifications throughout the Standard Process program were consumption of (1) unlimited fresh or frozen vegetables and fruits and preferably twice as many vegetables as fruits, (2) ½ to 1 cup of cooked lentils or brown rice each day, (3) 4 to 7 teaspoons of cold pressed oils per day, and (4) at least 64 oz of water a day. After day 10 of the program, participants were allowed to consume 1 to 2 servings of baked, broiled, or braised poultry or fish per day. Participants consumed a whey protein-based shake as meal replacement 2 times per day. Nutritional supplementation included a cleanse product on days 1 to 7, soluble fiber supplementation including oat bran concentrate and apple pectin on all days, and "green food" supplementation on days 8 to 21. Weight loss ranged between 5.2 (2.4 kg) and 19.9 lb (9.0 kg) (average, 11.7 lb; 5.3 kg). Total cholesterol levels decreased with ranges between 11 and 77 mg/dL, and low-density lipoprotein cholesterol levels decreased in a range between 7 and 67 mg/dL. After participating in a dietary program, the 7 participants demonstrated short-term weight loss and improvements in their lipid profiles.

  14. Asperger Syndrome in India: Findings from a Case-Series with Respect to Clinical Profile and Comorbidity

    PubMed Central

    Sreedaran, Priya; Ashok, M. V.

    2015-01-01

    Asperger syndrome (AS) is an autism spectrum disorder with a high rate of psychiatric comorbidity. We describe the clinical profile and psychiatric comorbidity in a series of affected individuals referred to an Indian general hospital psychiatry setting. Gilliam Asperger's disorder scale was used to evaluate the clinical characteristics while Mini-International Neuropsychiatric Interview (MINI)-KID and MINI-PLUS were used to assess psychiatric comorbidity. The profile of subjects with AS in our case-series appears similar to that published elsewhere with high rates of psychiatric comorbidity. Mental health professionals should evaluate for psychiatric comorbidity in individuals with autism spectrum disorders. PMID:25969609

  15. Asperger syndrome in India: findings from a case-series with respect to clinical profile and comorbidity.

    PubMed

    Sreedaran, Priya; Ashok, M V

    2015-01-01

    Asperger syndrome (AS) is an autism spectrum disorder with a high rate of psychiatric comorbidity. We describe the clinical profile and psychiatric comorbidity in a series of affected individuals referred to an Indian general hospital psychiatry setting. Gilliam Asperger's disorder scale was used to evaluate the clinical characteristics while Mini-International Neuropsychiatric Interview (MINI)-KID and MINI-PLUS were used to assess psychiatric comorbidity. The profile of subjects with AS in our case-series appears similar to that published elsewhere with high rates of psychiatric comorbidity. Mental health professionals should evaluate for psychiatric comorbidity in individuals with autism spectrum disorders.

  16. Io's Atmosphere Silhouetted in Transit by Jupiter Lyman-alpha

    NASA Astrophysics Data System (ADS)

    Retherford, Kurt

    2014-10-01

    Io's active volcanos both directly establish local gas plumes and indirectly establish a more global sublimation atmosphere, through plume deposited sulfur dioxide frost patches. Despite decades of study and recent observational advances the very basic question about the relative role of each of these sources is unresolved. The correlation between volcanic activity variability and Io's dramatic influence on numerous time-variable phenomenon in the Jupiter system cannot be causally linked until this answer is in hand. Our experienced team has developed a novel approach to use STIS in a new way to obtain global radial profiles of SO2 scale height distributions above both plume and sublimation dominated regions. We exploit the bright Lyman-alpha dayglow of Jupiter as a background illumination source together with the strongly absorptive nature of SO2 at 121.6 nm to image Io's atmosphere in silhouette with unprecedented detail during transit events. Our program provides the following key information for SO2: 1) First high-altitude (>400 km) radial measurements of tangential column densities and scale heights; 2) First clear measurement of sublimation densities at polar locations; 3) Volcanic densities for large and mid-sized plumes (possibly new ones); 4) Globally distributed limb profiles allowing strong distinctions between plume and sublimation dominated locations; 5) Repeated imaging on a few day and a few week timescales for improved plume variability constraints; and 6) Lyman-alpha reflectance imaging at Io central lon. ~180 deg, filling a gap in previous coverage. These new information are critical to breaking through an impasse in our understanding of Io's atmosphere.

  17. The Lyman α signature of the first galaxies

    NASA Astrophysics Data System (ADS)

    Smith, Aaron; Safranek-Shrader, Chalence; Bromm, Volker; Milosavljević, Miloš

    2015-06-01

    We present the Cosmic Lyman α Transfer code, a massively parallel Monte Carlo radiative transfer code, to simulate Lyman α (Lyα) resonant scattering through neutral hydrogen as a probe of the first galaxies. We explore the interaction of centrally produced Lyα radiation with the host galactic environment. Lyα photons emitted from the luminous starburst region escape with characteristic features in the line profile depending on the density distribution, ionization structure, and bulk velocity fields. For example, anisotropic ionization exhibits a tall peak close to line centre with a skewed tail that drops off gradually. Idealized models of first galaxies explore the effect of mass, anisotropic H II regions, and radiation pressure driven winds on Lyα observables. We employ mesh refinement to resolve critical structures. We also post-process an ab initio cosmological simulation and examine images captured at various distances within the 1 Mpc3 comoving volume. Finally, we discuss the emergent spectra and surface brightness profiles of these objects in the context of high-z observations. The first galaxies will likely be observed through the red damping wing of the Lyα line. Observations will be biased towards galaxies with an intrinsic red peak located far from line centre that reside in extensive H II super bubbles, which allows Hubble flow to sufficiently redshift photons away from line centre and facilitate transmission through the intergalactic medium. Even with gravitational lensing to boost the luminosity this preliminary work indicates that Lyα emission from stellar clusters within haloes of Mvir < 109 M⊙ is generally too faint to be detected by the James Webb Space Telescope.

  18. Seeing Galaxies Through the Forest: Spectral Stacking of Damped Lyman Alpha Systems

    NASA Astrophysics Data System (ADS)

    Yen, Steffi; Jorgenson, R.; Murphy, M.

    2013-01-01

    Damped Lyman alpha Systems (DLAs) are the highest column density (N(HI) >= 2x10^20 cm^-2) neutral gas absorbers detected in the sightlines to distant quasars. DLAs dominate the neutral gas mass content of the Universe from z=[0,5], suggesting that they are the reservoirs of neutral gas for star formation across cosmic time. However, the nature of DLAs is not fully understood because they are detected in absorption against the light of background quasars. The resulting spectra contain absorption from the Lyman alpha forest, a series of smaller neutral hydrogen lines, essentially filaments of neutral gas in the IGM. At high redshifts (z >= 2), the forest becomes quite thick, making it difficult to distinguish intervening forest lines from metal lines of the DLA. By employing the technique of spectral stacking, we essentially subtract the incoherent Lyman alpha forest lines, enabling us to measure metal lines that typically fall in the forest region, such as O VI, N V, and molecular hydrogen. In addition, the increased signal-to-noise ratio in the DLA stack allows us to search for the presence of weak metal lines and/or Lyman alpha emission not typically seen in a single DLA spectrum. We will present the results obtained from our stack of 97 high-resolution (FWHM ~ 8 km/s) VLT/UVES spectra. Initial analysis of the stack shows a possible detection of Lyman alpha emission in the DLA trough. We will combine this VLT/UVES stack with a previously created stack of ~110 Keck/HIRES spectra to create the highest signal-to-noise ratio, high-resolution DLA spectral stack. Analysis of this final stack will shed new light on our understanding of the role of DLAs in galaxy formation and evolution. This work was conducted by a Research Experience for Undergraduates (REU) position at the University of Hawai'i's Institute for Astronomy and funded by the NSF.

  19. The Lyman-alpha line in various solar features. I - Observations

    NASA Technical Reports Server (NTRS)

    Fontenla, J.; Reichmann, E. J.; Tandberg-Hanssen, E.

    1988-01-01

    Lyman-alpha line observations of the solar atmosphere obtained by the SMM ultraviolet spectrometer and polarimeter are presented. High spectral and spatial resolution data and broadband spectroheliograms show that, on the disk, the central reversal of the line is highly variable in depth and is frequently shifted, leading to asymmetric profiles. It is suggested that a dynamic layer overlying the limb may be responsible for distorting the background profile of the line and producing the observed asymmetric profiles. Narrow and extended prominences reaching velocities of several hundred km/sec are also noted.

  20. Lyman Alpha Photochemistry in the Solar Nebula

    NASA Technical Reports Server (NTRS)

    Fegley, Bruce, Jr.

    1997-01-01

    The purpose of the project "Lyman Alpha Photochemistry in the Solar Nebula" was to model photochemistry in the primitive solar nebula and the early solar systems. As part of the modeling, it was necessary to model the composition of the gas and dust accreted by the solar nebula. This final report contains a list of publications where the results of this project have been published.

  1. Relativistic effects in Lyman-α forest

    SciTech Connect

    Iršič, Vid; Dio, Enea Di; Viel, Matteo E-mail: enea.didio@oats.inaf.it

    2016-02-01

    We present the calculation of the Lyman-alpha (Lyman-α) transmitted flux fluctuations with full relativistic corrections to the first order. Even though several studies exist on relativistic effects in galaxy clustering, this is the first study to extend the formalism to a different tracer of underlying matter at unique redshift range (z=2−5). Furthermore, we show a comprehensive application of our calculations to the Quasar-Lyman-α cross-correlation function. Our results indicate that the signal of relativistic effects are sizeable at Baryonic Acoustic Oscillation (BAO) scale mainly due to the large differences in density bias factors of our tracers. We construct an observable, the anti-symmetric part of the cross-correlation function, that is dominated by the relativistic signal and offers a new way to measure the relativistic terms at relatively small scales. The analysis shows that relativistic effects are important when considering cross-correlations between tracers with very different biases, and should be included in the data analysis of the current and future surveys. Moreover, the idea presented in this paper is highly complementary to other techniques and observables trying to isolate the effect of the relativistic corrections and thus test the validity of the theory of gravity beyond the Newtonian regime.

  2. Population Profiles; A Series of 14 Units, Plus Extras, for the Study of Demography. Numbers 8 and 9.

    ERIC Educational Resources Information Center

    Lee, Everett S.; Bouvier, Leon F.

    "Growth and Future of Cities" and "The Nation's Minorities" are units eight and nine, respectively from the fourteen-units series Population Profiles. The former initiates its consideration of our urban future with two divergent points of view on population distribution. Those views are brought into perspective by an historical investigation of…

  3. Population Profiles; A Series of 14 Units, Plus Extras, for the Study of Demography. Numbers 8 and 9.

    ERIC Educational Resources Information Center

    Lee, Everett S.; Bouvier, Leon F.

    "Growth and Future of Cities" and "The Nation's Minorities" are units eight and nine, respectively from the fourteen-units series Population Profiles. The former initiates its consideration of our urban future with two divergent points of view on population distribution. Those views are brought into perspective by an historical investigation of…

  4. Pluto's Extended Atmosphere: New Horizons Alice Lyman-α Imaging

    NASA Astrophysics Data System (ADS)

    Retherford, Kurt D.; Gladstone, G. Randall; Stern, S. Alan; Weaver, Harold A.; Young, Leslie A.; Ennico, Kimberly A.; Olkin, Cathy B.; Cheng, Andy F.; Greathouse, Thomas K.; Hinson, David P.; Kammer, Joshua A.; Linscott, Ivan R.; Parker, Alex H.; Parker, Joel Wm.; Pryor, Wayne R.; Schindhelm, Eric; Singer, Kelsi N.; Steffl, Andrew J.; Strobel, Darrell F.; Summers, Michael E.; Tsang, Constantine C. C.; Tyler, G. Len; Versteeg, Maarten H.; Woods, William W.; Cunningham, Nathaniel J.; Curdt, Werner

    2015-11-01

    Pluto's upper atmosphere is expected to extend several planetary radii, proportionally more so than for any planet in our solar system. Atomic hydrogen is readily produced at lower altitudes due to photolysis of methane and transported upward to become an important constituent. The Interplanetary Medium (IPM) provides a natural light source with which to study Pluto's atomic hydrogen atmosphere. While direct solar Lyman-α emissions dominate the signal at 121.6 nm at classical solar system distances, the contribution of diffuse illumination by IPM Lyman-α sky-glow is roughly on par at Pluto (Gladstone et al., Icarus, 2015). Hydrogen atoms in Pluto's upper atmosphere scatter these bright Lyα emission lines, and detailed simulations of the radiative transfer for these photons indicate that Pluto would appear dark against the IPM Lyα background. The Pluto-Alice UV imaging spectrograph on New Horizons conducted several observations of Pluto during the encounter to search for airglow emissions, characterize its UV reflectance spectra, and to measure the radial distribution of IPM Lyα near the disk. Our early results suggest that these model predictions for the darkening of IPM Lyα with decreasing altitude being measureable by Pluto-Alice were correct. We'll report our progress toward extracting H and CH4 density profiles in Pluto's upper atmosphere through comparisons of these data with detailed radiative transfer modeling. These New Horizons findings will have important implications for determining the extent of Pluto's atmosphere and related constraints to high-altitude vertical temperature structure and atmospheric escape.This work was supported by NASA's New Horizons project.

  5. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 1.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.

    The serialized reference work "Biography Today" is initiating a "Subject Series" that in five separate volumes will encompass: authors, artists, scientists, and inventors, sports figures, and world leaders. This is the first volume in the "Author Series." There will be no duplication between the regular series and the special subject volumes. This…

  6. Partial Redistribution in the H Lyman Lines of Late-type Stars.

    NASA Astrophysics Data System (ADS)

    Sim, S. A.

    2003-10-01

    The effects of partial redistribution (PRD) in the formation of the hydrogen Lyman α and β lines are discussed with reference to simple atmospheric models of several late-type stars at different evolutionary stages. Radiative transfer calculations have been carried out using Carlsson's MULTI code which has been modified to include PRD by Hubeny & Lites. It is demonstrated that there is a rapid escalation in the importance of PRD in stars with surface gravity lower than the Sun, and that line profiles predicted using PRD are in significantly better agreement with observations than are those calculated assuming complete redistribution (CRD). The effects of PRD in H Lyman α on calculations of ion{Fe}{2} fluorescent spectra are examined, and it is found that there are significant, systematic differences between fluorescent spectra calculated using a PRD rather than CRD treatment of the pumping line.

  7. A Sounding Rocket Experiment for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP)

    NASA Astrophysics Data System (ADS)

    Kubo, M.; Kano, R.; Kobayashi, K.; Bando, T.; Narukage, N.; Ishikawa, R.; Tsuneta, S.; Katsukawa, Y.; Ishikawa, S.; Suematsu, Y.; Hara, H.; Shimizu, T.; Sakao, T.; Ichimoto, K.; Goto, M.; Holloway, T.; Winebarger, A.; Cirtain, J.; De Pontieu, B.; Casini, R.; Auchère, F.; Trujillo Bueno, J.; Manso Sainz, R.; Belluzzi, L.; Asensio Ramos, A.; Štěpán, J.; Carlsson, M.

    2014-10-01

    A sounding-rocket experiment called the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is presently under development to measure the linear polarization profiles in the hydrogen Lyman-alpha (Lyα) line at 121.567 nm. CLASP is a vacuum-UV (VUV) spectropolarimeter to aim for first detection of the linear polarizations caused by scattering processes and the Hanle effect in the Lyα line with high accuracy (0.1%). This is a fist step for exploration of magnetic fields in the upper chromosphere and transition region of the Sun. Accurate measurements of the linear polarization signals caused by scattering processes and the Hanle effect in strong UV lines like Lyα are essential to explore with future solar telescopes the strength and structures of the magnetic field in the upper chromosphere and transition region of the Sun. The CLASP proposal has been accepted by NASA in 2012, and the flight is planned in 2015.

  8. Soil formation rates determined from Uranium-series isotope disequilibria in soil profiles from the southeastern Australian highlands

    NASA Astrophysics Data System (ADS)

    Suresh, P. O.; Dosseto, A.; Hesse, P. P.; Handley, H. K.

    2013-10-01

    The sustainability of soil resources is determined by the balance between the rates of production and removal of soils. Samples from four weathering profiles at Frogs Hollow in the upper catchment area of the Murrumbidgee River (southeastern Australia) were analyzed for their uranium-series (U-series) isotopic composition to estimate soil production rates. Sequential leaching was conducted on sample aliquots to assess how U-series nuclides are distributed between primary and secondary minerals. Soil is increasingly weathered from bottom to top which is evident from the decrease in (234U/238U) ratios and increase in relative quartz content with decreasing soil depth. One soil profile shows little variation in mineralogy and U-series geochemistry with depth, explained by the occurrence of already extensively weathered saprolite, so that further weathering has minimal effect on mineralogy and geochemistry. Al2O3 is mobilized from these soils, and hence a silicon-based weathering index treating Al2O3 as mobile is introduced, which increases with decreasing soil depth, in all profiles. Leached and unleached aliquots show similar mineralogy with slight variation in relative concentrations, whereas the elemental and isotopic composition of uranium and thorium show notable differences between leached and unleached samples. Unleached samples show systematic variations in uranium-series isotopic compositions with depth compared to leached samples. This is most likely explained by the mobilization of U and Th from the samples during leaching. Soil residence times are calculated by modeling U-series activity ratios for each profile separately. Inferred timescales vary up to 30 kyr for unleached aliquots from profile F1 to up to 12 kyr for both leached and unleached aliquots from profile F2. Muscovite content shows a linear relationship with U-series derived soil residence times. This relationship provides an alternative method to estimate residence timescales for profiles with

  9. Doppler speeds of the hydrogen Lyman lines in solar flares from EVE

    NASA Astrophysics Data System (ADS)

    Brown, Stephen A.; Fletcher, Lyndsay; Labrosse, Nicolas

    2016-11-01

    Aims: The hydrogen Lyman lines provide important diagnostic information about the dynamics of the chromosphere, but there have been few systematic studies of their variability during flares. We investigate Doppler shifts in these lines in several flares, and use these to calculate plasma speeds. Methods: We use spectral data from the Multiple EUV Grating Spectrograph B (MEGS-B) detector of the Extreme-Ultraviolet Variability Experiment (EVE) instrument on the Solar Dynamics Observatory. MEGS-B obtains full-disk spectra of the Sun at a resolution of 0.1 nm in the range 37-105 nm, which we analyse using three independent methods. The first method performs Gaussian fits to the lines, and compares the quiet-Sun centroids with the flaring ones to obtain the Doppler shifts. The second method uses cross-correlation to detect wavelength shifts between the quiet-Sun and flaring line profiles. The final method calculates the "center-of-mass" of the line profile, and compares the quiet-Sun and flaring centroids to obtain the shift. Results: In a study of 6 flares we find strong signatures of both upflow and downflow in the Lyman lines, with speeds measured in Sun-as-a-Star data of around 10 km s-1, and speeds in the flare excess signal of around 30 km s-1. Conclusions: All events showing upflows in Lyman lines are associated with some kind of eruption or coronal flow in imaging data, which may be responsible for the net blueshifts. Events showing downflows in the Lyman lines may be associated with loop contraction or faint downflows, but it is likely that chromospheric condensation flows are also contributing.

  10. Lyman alpha SMM/UVSP absolute calibration and geocoronal correction

    NASA Technical Reports Server (NTRS)

    Fontenla, Juan M.; Reichmann, Edwin J.

    1987-01-01

    Lyman alpha observations from the Ultraviolet Spectrometer Polarimeter (UVSP) instrument of the Solar Maximum Mission (SMM) spacecraft were analyzed and provide instrumental calibration details. Specific values of the instrument quantum efficiency, Lyman alpha absolute intensity, and correction for geocoronal absorption are presented.

  11. Betty Kessler Lyman and the Indiana Federal Children's Theatre.

    ERIC Educational Resources Information Center

    Webb, Dorothy

    1995-01-01

    States that the special place that the Mickey Mouse Theater and its leader, Betty Lyman, occupy in the history of the Federal Theater project can best be understood in the economic and political context of the Depression. Concludes that there is little evidence to suggest Lyman's group contributed to the growth of children's theater in Indiana.…

  12. Variations in solar Lyman alpha irradiance on short time scales

    NASA Technical Reports Server (NTRS)

    Pap, J. M.

    1992-01-01

    Variations in solar UV irradiance at Lyman alpha are studied on short time scales (from days to months) after removing the long-term changes over the solar cycle. The SME/Lyman alpha irradiance is estimated from various solar indices using linear regression analysis. In order to study the nonlinear effects, Lyman alpha irradiance is modeled with a 5th-degree polynomial as well. It is shown that the full-disk equivalent width of the He line at 1083 nm, which is used as a proxy for the plages and active network, can best reproduce the changes observed in Lyman alpha. Approximately 72 percent of the solar-activity-related changes in Lyman alpha irradiance arise from plages and the network. The network contribution is estimated by the correlation analysis to be about 19 percent. It is shown that significant variability remains in Lyman alpha irradiance, with periods around 300, 27, and 13.5d, which is not explained by the solar activity indices. It is shown that the nonlinear effects cannot account for a significant part of the unexplained variation in Lyman alpha irradiance. Therefore, additional events (e.g., large-scale motions and/or a systematic difference in the area and intensity of the plages and network observed in the lines of Ca-K, He 1083, and Lyman alpha) may explain the discrepancies found between the observed and estimated irradiance values.

  13. On the Lack of Correlation Between Mg II 2796, 2803 Angstrom and Lyman alpha Emission in Lensed Star-Forming Galaxies

    NASA Technical Reports Server (NTRS)

    Rigby, Jane Rebecca; Bayliss, M. B.; Gladders, M. D.; Sharon, K.; Wuyts, E.; Dahle, H.

    2014-01-01

    We examine the Mg II 2796, 2803 Angstrom, Lyman alpha, and nebular line emission in five bright star-forming galaxies at 1.66 less than z less than 1.91 that have been gravitationally lensed by foreground galaxy clusters. All five galaxies show prominent Mg II emission and absorption in a P Cygni profile. We find no correlation between the equivalent widths of Mg II and Lyman alpha emission. The Mg II emission has a broader range of velocities than do the nebular emission line profiles; the Mg II emission is redshifted with respect to systemic by 100 to 200 km s(exp-1). When present, Lyman alpha is even more redshifted. The reddest components of Mg II and Lyman alpha emission have tails to 500-600 km s(exp-1), implying a strong outflow. The lack of correlation in the Mg II and Lyman alpha equivalent widths, the differing velocity profiles, and the high ratios of Mg II to nebular line fluxes together suggest that the bulk of Mg II emission does not ultimately arise as nebular line emission, but may instead be reprocessed stellar continuum emission.

  14. 238U, 232Th profiling and U-series isotope analysis of fossil teeth by laser ablation-ICPMS

    NASA Astrophysics Data System (ADS)

    Eggins, Stephen; Grün, Rainer; Pike, Alistair W. G.; Shelley, Michael; Taylor, Lois

    2003-05-01

    U and Th concentration profiles in fossil hominid and faunal teeth have been measured by laser ablation ICPMS. These profiles record diverse modes of U and Th uptake, particularly within enamel, that can be broadly related to the state of sample preservation. Observed U profiles are in general inconsistent with existing diffusion-adsorption models developed for U-uptake in bone and teeth. Where the models appear applicable, calculated diffusion rates are several orders of magnitude smaller than previous estimates. Laser ablation ICPMS offers a means of rapidly characterizing U and Th distributions in the enamel and dentine components of teeth as a precursor to ESR and U-series dating. In particular, it should allow the identification of teeth (and also bone) samples that have simple U-uptake histories and are amenable to precise dating by time-consuming and expensive Th-U and Pa-U TIMS techniques. We also demonstrated the use of laser ablation ICPMS to measure U-series isotopes in dentine and enamel samples with relatively high U concentrations (>20 ppm). These results, obtained using a quadrupole ICPMS, illustrate significant promise for in situ U-series isotope analysis, particularly when combined with the greater sensitivity and multi-collection capabilities of new sector ICPMS instrumentation. The latter may permit precise isotope ratio measurements on samples containing only a few ppm of U.

  15. Finding high-redshift voids using Lyman α forest tomography

    NASA Astrophysics Data System (ADS)

    Stark, Casey W.; Font-Ribera, Andreu; White, Martin; Lee, Khee-Gan

    2015-11-01

    We present a new method of finding cosmic voids using tomographic maps of Lyα forest flux. We identify cosmological voids with radii of 2-12 h-1 Mpc in a large N-body simulation at z = 2.5, and characterize the signal of the high-redshift voids in density and Lyα forest flux. The void properties are similar to what has been found at lower redshifts, but they are smaller and have steeper radial density profiles. Similarly to what has been found for low-redshift voids, the radial velocity profiles have little scatter and agree very well with the linear theory prediction. We run the same void finder on an ideal Lyα flux field and tomographic reconstructions at various spatial samplings. We compare the tomographic map void catalogues to the density void catalogue and find good agreement even with modest-sized voids (r > 6 h-1 Mpc). Using our simple void-finding method, the configuration of the ongoing COSMOS Lyman Alpha Mapping And Tomography Observations (CLAMATO) survey covering 1 deg2 would provide a sample of about 100 high-redshift voids. We also provide void-finding forecasts for larger area surveys, and discuss how these void samples can be used to test modified gravity models, study high-redshift void galaxies, and to make an Alcock-Paczynski measurement. To aid future work in this area, we provide public access to our simulation products, catalogues, and sample tomographic flux maps.

  16. Characterizing Lyman Alpha Scattering in Nearby Galaxies

    NASA Astrophysics Data System (ADS)

    Bridge, Joanna; Hayes, Matthew; Melinder, Jens; Östlin, Göran; Gronwall, Caryl

    2017-01-01

    The hydrogen emission line of Lyman alpha (Lyα) has long been recognized as key to studying high redshift star-forming galaxies. However, due to the resonance of the emission line, the path that a Lyα photon takes from emission to eventual escape from the galaxy is essentially a mystery. This scattering poses a problem for using Lyα as a key emission feature of galaxies because it results in Lyα not being observed in all star-forming galaxies, and, in galaxies where it is observed, the place where the photon is originally emitted and where it is observed are two very different things. We discuss here how the Lyman-Alpha Reference Sample (LARS) provides a unique sample of 14 nearby (0.02 < z < 0.2) galaxies in which we investigate the role of scattering, both on the global scale of the galaxies and down to scales of ~ 50 parsecs using Hubble Space Telescope imaging. We compare the Lyα/Hα ratios with those expected from pure dust attenuation models, finding that in some cases significant positive departures are found on small scales, consistent with geometrical effects being important on sizes comparable to the HII regions. We then develop a simple scattering model in which we are able to estimate the average path length a Lyα photon travels with respect to non-resonant radiation, and quantifiy the excess dust optical depth to which Lyα radiation may be susceptible.

  17. A Possible Solution to the Lyman/Balmer Line Problem in Hot DA White Dwarfs

    NASA Astrophysics Data System (ADS)

    Preval, Simon P.; Barstow, Martin A.; Badnell, Nigel R.; Holberg, Jay B.; Hubeny, Ivan

    2015-06-01

    Arguably, the best method for determining the effective temperature (Teff) and surface gravity (log g) of a DA white dwarf is by fitting the Hydrogen Lyman and Balmer absorption features. However, as has been shown for white dwarfs with Teff>50,000K, the calculated value from the Lyman and Balmer lines are discrepant, which worsens with increasing temperature. Many different solutions have been suggested, ranging from the input physics used to calculate the models, to interstellar reddening. We will focus on the former, and consider three variables. The first is the atomic data used, namely the number of transitions included in line blanketing treatments and the photoionization cross sections. The second is the stark broadening treatment used to synthesise the Lyman and Balmer line profiles, namely the calculations performed by Lemke (1997) and Tremblay & Bergeron (2009). Finally, the third is the atmospheric content. The model grids are calculated with a pure H composition, and a metal polluted composition using the abundances of Preval et al. (2013). We present the preliminary results of our analysis, whereby we have determined the Teff for a small selection of white dwarfs. We plan to extend our analysis by allowing metallicity to vary in future model grids.

  18. Reconnaissance of the TRAPPIST-1 exoplanet system in the Lyman-α line

    NASA Astrophysics Data System (ADS)

    Bourrier, V.; Ehrenreich, D.; Wheatley, P. J.; Bolmont, E.; Gillon, M.; de Wit, J.; Burgasser, A. J.; Jehin, E.; Queloz, D.; Triaud, A. H. M. J.

    2017-03-01

    The TRAPPIST-1 system offers the opportunity to characterize terrestrial, potentially habitable planets orbiting a nearby ultracool dwarf star. We performed a four-orbit reconnaissance with the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope to study the stellar emission at Lyman-α, to assess the presence of hydrogen exospheres around the two inner planets, and to determine their UV irradiation. We detect the Lyman-α line of TRAPPIST-1, making it the coldest exoplanet host star for which this line has been measured. We reconstruct the intrinsic line profile, showing that it lacks broad wings and is much fainter than expected from the stellar X-ray emission. TRAPPIST-1 has a similar X-ray emission as Proxima Cen but a much lower Ly-α emission. This suggests that TRAPPIST-1 chromosphere is only moderately active compared to its transition region and corona. We estimated the atmospheric mass loss rates for all planets, and found that despite a moderate extreme UV emission the total XUV irradiation could be strong enough to strip the atmospheres of the inner planets in a few billions years. We detect marginal flux decreases at the times of TRAPPIST-1b and c transits, which might originate from stellar activity, but could also hint at the presence of extended hydrogen exospheres. Understanding the origin of these Lyman-α variations will be crucial in assessing the atmospheric stability and potential habitability of the TRAPPIST-1 planets.

  19. Late Rectal Toxicity on RTOG 94-06: Analysis Using a Mixture Lyman Model

    SciTech Connect

    Tucker, Susan L.; Dong Lei; Bosch, Walter R.; Michalski, Jeff; Winter, Kathryn; Mohan, Radhe; Purdy, James A.; Kuban, Deborah; Lee, Andrew K.; Cheung, M. Rex; Thames, Howard D.; Cox, James D.

    2010-11-15

    Purpose: To estimate the parameters of the Lyman normal-tissue complication probability model using censored time-to-event data for Grade {>=}2 late rectal toxicity among patients treated on Radiation Therapy Oncology Group 94-06, a dose-escalation trial designed to determine the maximum tolerated dose for three-dimensional conformal radiotherapy of prostate cancer. Methods and Materials: The Lyman normal-tissue complication probability model was fitted to data from 1,010 of the 1,084 patients accrued on Radiation Therapy Oncology Group 94-06 using an approach that accounts for censored observations. Separate fits were obtained using dose-volume histograms for whole rectum and dose-wall histograms for rectal wall. Results: With a median follow-up of 7.2 years, the crude incidence of Grade {>=}2 late rectal toxicity was 15% (n = 148). The parameters of the Lyman model fitted to dose-volume histograms data, with 95% profile-likelihood confidence intervals, were TD{sub 50} = 79.1 Gy (75.3 Gy, 84.3 Gy), m = 0.146 (0.107, 0.225), and n = 0.077 (0.041, 0.156). The fit based on dose-wall histogram data was not significantly different. Patients with cardiovascular disease had a significantly higher incidence of late rectal toxicity (p = 0.015), corresponding to a dose-modifying factor of 5.3%. No significant association with late rectal toxicity was found for diabetes, hypertension, rectal volume, rectal length, neoadjuvant hormone therapy, or prescribed dose per fraction (1.8 Gy vs. 2 Gy). Conclusions: These results, based on a large cohort of patients from a multi-institutional trial, are expected to be widely representative of the ability of the Lyman model to describe the long-term risk of Grade {>=}2 late rectal toxicity after three-dimensional conformal radiotherapy of prostate cancer.

  20. H Lyman alpha transport in the heliosphere based on an expansion into scattering hierarchies.

    NASA Astrophysics Data System (ADS)

    Scherer, H.; Fahr, H. J.

    1996-05-01

    The radiation transport equation for solar HI-Lyman Alpha line photons in the interplanetary medium is solved by an expansion of the luminosity function into scattering orders. The solution introduces the exact redistribution function which takes into account the local thermodynamical conditions of the scattering agent, like temperature, density and bulk velocity of the neutral interplanetary hydrogen. Also the actually observed solar HI-Lyman Alpha emission profile will be taken into account. With the simplifying assumption of a constant temperature and bulk velocity of the hydrogen it is then possible to numerically solve the radiation transport equation with an adaptive Gauss-Legendre integration for photons of the first and the second scattering order. The result of this calculation astonishingly enough gives a less satisfying fit of experimental Lyman-Alpha data (like those by Pioneer-10, Voyager 1/2) than that obtained with optically thin approximations which, however, also clearly fail to describe the data satisfactorily well at large solar distances. As we can show here results from multiscattering calculations are fairly sensitive to local variations of the temperature and the bulk velocity of the interstellar hydrogen. If the latter are properly taken into account, fits of the data can be much improved. Though a fully satisfying fit as we show, can only be achieved with improved hydrogen models. Our results also imply that photons of the second and of higher scattering orders only play a minor role and in most cases can even be neglected. According to these experiences in multiscattering calculations we have developed a first order multiscattering code that takes account of the spatial variations in the temperature and bulk velocity of interplanetary hydrogen given by the recent model by Osterbart & Fahr. With these calculations we can give satisfactorily good fits both of upwind and downwind heliospheric Lyman-α glow data as well.

  1. Origin of the Lyman excess in early-type stars

    NASA Astrophysics Data System (ADS)

    Cesaroni, R.; Sánchez-Monge, Á.; Beltrán, M. T.; Molinari, S.; Olmi, L.; Treviño-Morales, S. P.

    2016-04-01

    Context. Ionized regions around early-type stars are believed to be well-known objects, but until recently, our knowledge of the relation between the free-free radio emission and the IR emission has been observationally hindered by the limited angular resolution in the far-IR. The advent of Herschel has now made it possible to obtain a more precise comparison between the two regimes, and it has been found that about a third of the young H ii regions emit more Lyman continuum photons than expected, thus presenting a Lyman excess. Aims: With the present study we wish to distinguish between two scenarios that have been proposed to explain the existence of the Lyman excess: (i) underestimation of the bolometric luminosity, or (ii) additional emission of Lyman-continuum photons from an accretion shock. Methods: We observed an outflow (SiO) and an infall (HCO+) tracer toward a complete sample of 200 H ii regions, 67 of which present the Lyman excess. Our goal was to search for any systematic difference between sources with Lyman excess and those without. Results: While the outflow tracer does not reveal any significant difference between the two subsamples of H ii regions, the infall tracer indicates that the Lyman-excess sources are more associated with infall signposts than the other objects. Conclusions: Our findings indicate that the most plausible explanation for the Lyman excess is that in addition to the Lyman continuum emission from the early-type star, UV photons are emitted from accretion shocks in the stellar neighborhood. This result suggests that high-mass stars and/or stellar clusters containing young massive stars may continue to accrete for a long time, even after the development of a compact H ii region. Based on observations carried out with the IRAM 30 m Telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).

  2. Influence of non-adiabatic temperature variations on line profile variations of slowly rotating beta Cephei stars and SPBs. II. Simulations of line profile time series

    NASA Astrophysics Data System (ADS)

    De Ridder, J.; Dupret, M.-A.; Neuforge, C.; Aerts, C.

    2002-04-01

    We investigate to what extent non-adiabatic temperature variations at the surface of slowly rotating non-radially pulsating beta Cephei stars and slowly pulsating B stars affect silicon line profile variations. We use the non-adiabatic amplitudes of the effective temperature and gravity variation presented in Dupret et al. (\\cite{Dupret02}), together with a Kurucz intensity grid, to compute time series of line profile variations. Our simulations point out that the line shapes do not change significantly due to temperature variations. We find equivalent width variations of at most two percent of the mean equivalent width. We confront our results with observational equivalent width variations and with photometrically obtained effective temperature variations. Based on observations obtained with the Swiss photometric telescope and with the ESO/CAT telescope, at La Silla in Chile.

  3. Epileptic Electroencephalography Profile Associates with Attention Problems in Children with Fragile X Syndrome: Review and Case Series

    PubMed Central

    Cowley, Benjamin; Kirjanen, Svetlana; Partanen, Juhani; Castrén, Maija L.

    2016-01-01

    Fragile X syndrome (FXS) is the most common cause of inherited intellectual disability and a variant of autism spectrum disorder (ASD). The FXS population is quite heterogeneous with respect to comorbidities, which implies the need for a personalized medicine approach, relying on biomarkers or endophenotypes to guide treatment. There is evidence that quantitative electroencephalography (EEG) endophenotype-guided treatments can support increased clinical benefit by considering the patient's neurophysiological profile. We describe a case series of 11 children diagnosed with FXS, aged one to 14 years, mean 4.6 years. Case data are based on longitudinal clinically-observed reports by attending physicians for comorbid symptoms including awake and asleep EEG profiles. We tabulate the comorbid EEG symptoms in this case series, and relate them to the literature on EEG endophenotypes and associated treatment options. The two most common endophenotypes in the data were diffuse slow oscillations and epileptiform EEG, which have been associated with attention and epilepsy respectively. This observation agrees with reported prevalence of comorbid behavioral symptoms for FXS. In this sample of FXS children, attention problems were found in 37% (4 of 11), and epileptic seizures in 45% (5 of 11). Attention problems were found to associate with the epilepsy endophenotype. From the synthesis of this case series and literature review, we argue that the evidence-based personalized treatment approach, exemplified by neurofeedback, could benefit FXS children by focusing on observable, specific characteristics of comorbid disease symptoms. PMID:27462212

  4. Epileptic Electroencephalography Profile Associates with Attention Problems in Children with Fragile X Syndrome: Review and Case Series.

    PubMed

    Cowley, Benjamin; Kirjanen, Svetlana; Partanen, Juhani; Castrén, Maija L

    2016-01-01

    Fragile X syndrome (FXS) is the most common cause of inherited intellectual disability and a variant of autism spectrum disorder (ASD). The FXS population is quite heterogeneous with respect to comorbidities, which implies the need for a personalized medicine approach, relying on biomarkers or endophenotypes to guide treatment. There is evidence that quantitative electroencephalography (EEG) endophenotype-guided treatments can support increased clinical benefit by considering the patient's neurophysiological profile. We describe a case series of 11 children diagnosed with FXS, aged one to 14 years, mean 4.6 years. Case data are based on longitudinal clinically-observed reports by attending physicians for comorbid symptoms including awake and asleep EEG profiles. We tabulate the comorbid EEG symptoms in this case series, and relate them to the literature on EEG endophenotypes and associated treatment options. The two most common endophenotypes in the data were diffuse slow oscillations and epileptiform EEG, which have been associated with attention and epilepsy respectively. This observation agrees with reported prevalence of comorbid behavioral symptoms for FXS. In this sample of FXS children, attention problems were found in 37% (4 of 11), and epileptic seizures in 45% (5 of 11). Attention problems were found to associate with the epilepsy endophenotype. From the synthesis of this case series and literature review, we argue that the evidence-based personalized treatment approach, exemplified by neurofeedback, could benefit FXS children by focusing on observable, specific characteristics of comorbid disease symptoms.

  5. Lyman alpha emissions in the outer heliosphere

    NASA Technical Reports Server (NTRS)

    Quemerais, E.; Lallement, R.; Bertaux, J. L.; Sandel, B. R.

    1995-01-01

    Since 1993, the Ultraviolet Spectrometers aboard both Voyager 1 and 2, were used to study the Ly-alpha glow pattern backscattered by neutral hydrogen atoms at great distance from the sun. When compared to a radiative transfer calculation for an unperturbed interstellar hydrogen flow into the solar system, the data present an excess of intensity seen in the direction of the incoming interstellar wind. An absolute estimate of this Lyman alpha intensity yields 10 to 15 Rayleighs for each spacecraft. We discuss the possibility that this excess is caused by a gradient of hydrogen at large distance from the Sun due to the filtration of interstellar hydrogen when crossing the heliopause. Comparisons with results from the Baranov-Malama model of neutral-plasma coupling at the heliopause are presented. The data yield a range of possible values for the hydrogen gradient which may be used to infer the location of the heliopause.

  6. Lyman Spitzer: Astronomer, Physicist, Engineer, and Mountaineer

    NASA Astrophysics Data System (ADS)

    Morton, D. C.

    2006-12-01

    NASA's naming of the Spitzer Space Telescope after Lyman Spitzer was a most appropriate choice, recognizing an outstanding scientist who also contributed extensively to space astronomy. As an astronomer he was a leading authority in the physics of both the interstellar medium and stellar dynamics, wrote textbooks for both fields, and guided many research students. As a physicist he conceived the Stellarator for magnetic confinement, managed a laboratory for controlled fusion, and wrote a textbook on plasma physics. As an engineer he led the development of the payload for the successful Copernicus satellite, which fulfilled his 1946 proposal for an extraterrestrial observatory. His mountaineering included first ascents on Baffin Island and in the Canadian Rockies as well as the summit of the challenging Mt Waddington in the Coast Range.

  7. Lyman Spitzer, Jr. (1914-1997)

    NASA Astrophysics Data System (ADS)

    Field, George B.

    1998-03-01

    Lyman Spitzer, Jr., the Bruce Medalist of the Astronomical Society of the Pacific for 1973, died on 1997 March 31. An intrepid leader, he founded the Princeton Plasma Physics Laboratory and was Principal Investigator on NASA's Copernicus Orbiting Astronomical Observatory. He established the theoretical foundations for the modern study of the interstellar medium and contributed to the theory of evolution of stellar clusters. His 1955 monograph, The Physics of Fully Ionized Gases (2d ed., 1962), his Diffuse Matter in Space (1968), and his Physical Processes in the Interstellar Medium (1978) all became the standard references in their fields. The success of the Hubble Space Telescope is due in large part to his foresight and leadership in pursuing this project. An avid rock climber, Spitzer ascended many peaks around the world. His scientific achievements enriched astronomy for decades to come.

  8. EUVL mask inspection at Hydrogen Lyman Alpha

    NASA Astrophysics Data System (ADS)

    Jota, Thiago S.; Milster, Tom D.

    2012-11-01

    Mask inspection is an outstanding challenge for Extreme Ultra-Violet Lithography (EUVL). The purpose of this investigation is to compare imaging characteristics of ArF and KrF inspection sources to imaging characteristics using a source at the Lyman-alpha line of Hydrogen at 121.6nm (HLA). HLA provides a raw resolution improvement of 37% to ArF and 51% to KrF, based on proportional wavelength scaling. The HLA wavelength is in an atmospheric transmission window, so a vacuum environment is not required. Our comparison uses rigorous vector imaging techniques to simulate partially coherent illumination schemes and reasonably accurate mask material properties and dimensions. Contrast is evaluated for representative spatial frequencies. Imaging and detection of defects are also considered with NILS and MEEF. The goal is high throughput inspection with maximum resolution, contrast, and sensitivity.

  9. Lyman Alpha Galaxies and Galaxy Formation Scenarios

    NASA Astrophysics Data System (ADS)

    Rhoads, James; Malhotra, Sangeeta

    2005-08-01

    The Large Area Lyman Alpha survey has successfully identified the population of young Lyα emitting galaxies predicted over 35 years ago. High equivalent widths of Lyα in these sources suggest that they are a very young (age < 10^7 years), metal poor, population of stars, making them very interesting objects for understanding galaxy formation. With two nights of Magellan+IMACS time, we will obtain spectroscopic confirmation of 150-200 secure LALA sources at redshift z=4.5. Followup of a similar number of fainter Lyα candidates will characterize the completeness and weed out foreground emission line galaxies. The excellent match between wide-field capabilities of IMACS and the LALA survey makes this the most complete confirmation and characterization of the high redshift Lyα population yet. With our spectroscopic sample, we will: (1) Search for AGN among our sample- a few should be found if the AGN fraction is comparable to that in Lyman break galaxies. (2) Produce a high S/N coadded spectrum, where we will look for (a) HeII (1640Å) emission, which is an indicator of Pop III stars; and (b) ISM absorption lines, whose velocity offset relative to the Lyα emission is an indicator of galactic winds in these early starbursts. (3) Obtain a clean measurement of spatial correlations among Lyα galaxies, and thereby derive the halo mass, occupancy number, and duty cycle of Lyα galaxies, to see how they fit into the bigger picture of galaxy formation.

  10. The Advancement President and the Academy: Profiles in Institutional Leadership. Series on Higher Education.

    ERIC Educational Resources Information Center

    Murphy, Mary Kay, Ed.

    This book presents 15 essays concerning the growing importance of institutional advancement experience to winning and successfully conducting a college or university presidency. This is a series of essays by successful university CEOs who achieved their positions from an advancement background and who clearly understand the importance of…

  11. The Advancement President and the Academy: Profiles in Institutional Leadership. Series on Higher Education.

    ERIC Educational Resources Information Center

    Murphy, Mary Kay, Ed.

    This book presents 15 essays concerning the growing importance of institutional advancement experience to winning and successfully conducting a college or university presidency. This is a series of essays by successful university CEOs who achieved their positions from an advancement background and who clearly understand the importance of…

  12. Lyman-{alpha} transfer in primordial hydrogen recombination

    SciTech Connect

    Hirata, Christopher M.; Forbes, John

    2009-07-15

    Cosmological constraints from the cosmic microwave background (CMB) anisotropies rely on accurate theoretical calculations of the cosmic recombination history. Recent work has emphasized the importance of radiative transfer calculations due to the high optical depth in the H i Lyman lines. Transfer in the Ly{alpha} line is dominated by true emission and absorption, Hubble expansion, and resonant scattering. Resonant scattering causes photons to diffuse in frequency due to random kicks from the thermal velocities of hydrogen atoms, and also to drift toward lower frequencies due to energy loss via atomic recoil. Past analyses of Ly{alpha} transfer during the recombination era have either considered a subset of these processes, ignored time dependence, or incorrectly assumed identical emission and absorption profiles. We present here a fully time-dependent radiative transfer calculation of the Ly{alpha} line including all of these processes, and compare it to previous results that ignored the resonant scattering. We find a faster recombination due to recoil enhancement of the Ly{alpha} escape rate, leading to a reduction in the free electron density of 0.45% at z=900. This results in an increase in the small-scale CMB power spectrum that is negligible for the current data but will be a 0.9{sigma} correction for Planck. We discuss the reasons why we find a smaller correction than some other recent computations.

  13. Mapping forest height, foliage height profiles and disturbance characteristics with time series of gap-filled Landsat and ALI imagery

    NASA Astrophysics Data System (ADS)

    Helmer, E.; Ruzycki, T. S.; Wunderle, J. M.; Kwit, C.; Ewert, D. N.; Voggesser, S. M.; Brandeis, T. J.

    2011-12-01

    We mapped tropical dry forest height (RMSE = 0.9 m, R2 = 0.84, range 0.6-7 m) and foliage height profiles with a time series of gap-filled Landsat and Advanced Land Imager (ALI) imagery for the island of Eleuthera, The Bahamas. We also mapped disturbance type and age with decision tree classification of the image time series. Having mapped these variables in the context of studies of wintering habitat of an endangered Nearctic-Neotropical migrant bird, the Kirtland's Warbler (Dendroica kirtlandii), we then illustrated relationships between forest vertical structure, disturbance type and counts of forage species important to the Kirtland's Warbler. The ALI imagery and the Landsat time series were both critical to the result for forest height, which the strong relationship of forest height with disturbance type and age facilitated. Also unique to this study was that seven of the eight image time steps were cloud-gap-filled images: mosaics of the clear parts of several cloudy scenes, in which cloud gaps in a reference scene for each time step are filled with image data from alternate scenes. We created each cloud-cleared image, including a virtually seamless ALI image mosaic, with regression tree normalization of the image data that filled cloud gaps. We also illustrated how viewing time series imagery as red-green-blue composites of tasseled cap wetness (RGB wetness composites) aids reference data collection for classifying tropical forest disturbance type and age.

  14. Analysis on atmospheric pressure, temperature, and wind speed profiles during total solar eclipse 9 March 2016 using time series clustering

    NASA Astrophysics Data System (ADS)

    Septem Riza, Lala; Wihardi, Yaya; Nurdin, Enjang Ali; Dwi Ardi, Nanang; Puji Asmoro, Cahyo; Wijaya, Agus Fany Chandra; Aria Utama, Judhistira; Bayu Dani Nandiyanto, Asep

    2016-11-01

    Air temperature, pressure, and wind speed measurements on the surface taken during the Total Solar Eclipse (TSE) of March 9, 2016, are made. They were taken in Terentang Beach, Bangka Island, Indonesia. In this paper, we propose to analyze them by using time series clustering. The following steps are conducted: data collecting, splitting, smoothing, distance calculation, and clustering. The final results show cluster memberships of the three parameters on 3 time frames: one day before, the TSE day, and one day after. After doing some simulations, it can be seen that the profiles of temperature and pressure on the TSE day are on the same cluster while the wind-speed profile on the TSE day is the same as on the one day after.

  15. Biography Today. Profiles of People of Interest to Young Readers. Artists Series. Vol. 1, 1996.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This issue of "Biography Today" features 18 short biographies about artists in a format young readers can enjoy and understand. Each entry provides at least one picture of the individual profiled, and bold-faced rubrics lead the reader to information on birth, youth, early memories, education, first jobs, marriage and family, career highlights,…

  16. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 13.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This special subject volume on "Authors" was especially created to appeal to young readers in a format they can enjoy reading and readily understand. Each volume contains alphabetically arranged sketches. Each entry provides at least one picture of the individual profiled, and bold-faced rubrics lead the reader to information on birth,…

  17. Biography Today: Scientists & Inventors Series. Profiles of People of Interest to Young Readers. Vol. 1, 1996.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This issue of "Biography Today" looks at scientists and inventors and is created to appeal to young readers in a format they can and enjoy and easily understand. Each entry provides at least one picture of the individual profiled, and bold-faced rubrics lead the reader to information on birth, youth, early memories, education, first jobs, marriage…

  18. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 6.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This book provides biographical profiles of 11 authors of interest to readers ages 9 and above and was created to appeal to young readers in a format they can enjoy reading and readily understand. Biographies were prepared after extensive research, and each volume contains a cumulative index, a general index, a place of birth index, and a birthday…

  19. Student Characteristics as Compared to the Community Profile. Research Report Series. Volume XIV, No. 3.

    ERIC Educational Resources Information Center

    Lucas, John A.

    In fall 1984, a study was conducted in Illinois at William Rainey Harper College (WRHC) to provide a student profile for general information purposes, to gather data not available on the college's automated student data file, and to analyze WRHC's marketing outreach. Surveys were mailed to random samples of 500 degree credit students and 300…

  20. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 9.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This book presents biographical profiles of 10 authors of interest to readers ages 9 and above and was created to appeal to young readers in a format they can enjoy and readily understand. Biographies were prepared after extensive research, and each volume contains a cumulative index, a general index, a place of birth index, and a birthday index.…

  1. Biography Today: Profiles of People of Interest to Young Readers. Sports Series, Volume 8.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This volume provides biographies on sports figures. Each entry offers at least one picture of the individual profiled, and bold-faced rubrics lead to information on birth, youth, early memories, education, first jobs, marriage and family, career highlights, memorable experiences, hobbies, and honors and awards. Each entry ends with a list of…

  2. Biography Today: Profiles of People of Interest to Young Readers. Scientists & Inventors Series.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    2002-01-01

    This volume on "Scientists and Inventors" was created to appeal to young readers in a format they can enjoy reading and can readily understand. Each volume contains alphabetically arranged sketches of outstanding people. Each entry provides at least one picture of the individual profiled, and bold-faced rubrics lead the reader to…

  3. Occupational Competency Profile for Health Occupations Education Program: Health Agency Assessment. Information Series: Report No. 10.

    ERIC Educational Resources Information Center

    Walters, Norma J.

    This assessment instrument is intended to provide health occupations teachers and state departments of education with information needed to revise and improve the curriculum used in training prospective health occupations teachers and in updating certification requirements for practicing health care professionals. The profile lists the…

  4. Biography Today: Profiles of People of Interest to Young Readers. Sports Series, Volume 7.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This volume provides biographies on sports figures. Each entry offers at least one picture of the individual profiled, and bold-faced rubrics lead to information on birth, youth, early memories, education, first jobs, marriage and family, career highlights, memorable experiences, hobbies, and honors and awards. Each entry ends with a list of…

  5. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 14.

    ERIC Educational Resources Information Center

    Abbey, Cherie D., Ed.

    This special subject volume of biographies of authors was created to appeal to young readers in a format they can enjoy reading and readily understand. Each entry provides at least one picture of the individual profiled, and bold-faced rubrics lead the reader to information on birth, youth, early memories, education, first jobs, marriage and…

  6. Occupational Competency Profile for Health Occupations Education Program: Health Agency Assessment. Information Series: Report No. 10.

    ERIC Educational Resources Information Center

    Walters, Norma J.

    This assessment instrument is intended to provide health occupations teachers and state departments of education with information needed to revise and improve the curriculum used in training prospective health occupations teachers and in updating certification requirements for practicing health care professionals. The profile lists the…

  7. Profiles of STEM Students: Persisters, Joiners, Changers and Departers. ACT Research Report Series 2017-3

    ERIC Educational Resources Information Center

    Westrick, Paul

    2017-01-01

    This study is an extension of two previous studies that provided profiles of persisting STEM majors overall (regardless of academic performance) and persisting STEM majors who earned semester GPAs of 3.0 or higher (Westrick, 2016, 2017). Using data from 25 four-year institutions, this study compared the mean ACT assessment scores, HSGPAs, and ACT…

  8. Biography Today: Profiles of People of Interest to Young Readers. Author Series, Volume 5.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    As with the regular issues of "Biography Today," this special subject volume on "Authors" was created to appeal to young readers in a format they can enjoy reading and readily understand. Each volume contains alphabetically-arranged sketches. Each entry in the volume provides at least one picture of the individual profiled, and…

  9. Gravitational lensing and the Lyman-alpha forest

    NASA Technical Reports Server (NTRS)

    Ikeuchi, Satoru; Turner, Edwin L.

    1991-01-01

    Possible connections between the inhomogeneities responsible for the Lyman-alpha forest in quasar spectra and gravitational lensing effects are investigated. For most models of the Lyman-alpha forest, no significant lensing is expected. For some versions of the CDM model-based minihalo hypothesis, gravitational lensings on scales less than abour 0.1 arcsec would occur with a frequency approaching that with which ordinary galaxies cause arcsecond scale lensing.

  10. Cytotoxicity Profiles for a Series of Triorganophosphinegold(I) Dithiocarbamates and Triorganophosphinegold(I) Xanthates

    PubMed Central

    de Vos, Dick; Ho, Soo Yei

    2004-01-01

    A series of triorganophosphinegold(1) dithiocarbamate (R3PAuS2CNR'2) and xanthate (R3PAuS2COR') complexes have been prepared and characterised spectroscopically. Based on crystallographic evidence, the molecules feature linear gold(1) geometries defined by sulphur and phosphorus donors. The complexes, along with a series of known anti-cancer agents, have been screened against a panel of seven human cancer cell lines. Uniformly, the dithiocarbamate derivatives are more active than their xanthate counterparts, with the most active complex being Et3PAu(S2CNEt2), and are more active than cisplatin in all cell lines screened but, not as potent as taxol. PMID:18365074

  11. A series of recommended tests when validating probabilistic DNA profile interpretation software.

    PubMed

    Bright, Jo-Anne; Evett, Ian W; Taylor, Duncan; Curran, James M; Buckleton, John

    2015-01-01

    There has been a recent push from many jurisdictions for the standardisation of forensic DNA interpretation methods. Current research is moving from threshold-based interpretation strategies towards continuous interpretation strategies. However laboratory uptake of software employing probabilistic models is slow. Some of this reluctance could be due to the perceived intimidating calculations to replicate the software answers and the lack of formal internal validation requirements for interpretation software. In this paper we describe a set of experiments which may be used to internally validate in part probabilistic interpretation software. These experiments included both single source and mixed profiles calculated with and without dropout and drop-in and studies to determine the reproducibility of the software with replicate analyses. We do this by way of example using three software packages: STRmix™, LRmix, and Lab Retriever. We outline and demonstrate the profile examples where the expected answer may be calculated and provide all calculations.

  12. Time-series observations of phytoplankton productivity in the western North Pacific by an underwater profiling buoy system

    NASA Astrophysics Data System (ADS)

    Fujiki, T.; Honda, M. C.; Matsumoto, K.; Kawakami, H.; Wakita, M.; Saino, T.; Marine Biogeochemical Cycle Research Team

    2010-12-01

    An understanding of the variability in phytoplankton primary productivity provides a basic knowledge of the ecosystem structure and carbon cycle in the ocean. Primary productivity in the world’s oceans has been measured mostly by the radiocarbon tracer or oxygen evolution methods. These methods require bottle incubations for periods ranging from hours to 1 day. This methodological limitation makes it difficult to measure primary productivity in situ with high temporal and spatial resolution. In particular, ship-based studies of the open ocean have been limited in their ability to conduct time-series observations for understanding variability in primary productivity. To overcome these problems, we developed an underwater profiling buoy system incorporating a fast repetition rate fluorometer which enables real-time high-frequency measurements of primary productivity, and started time-series observations in the western North Pacific as part of the environmental biogeochemical cycle research program in JAMSTEC. Here, we show the results of observations in the western North Pacific by the underwater profiling buoy system.

  13. Lyman continuum galaxies: Observed Lyman continuum flux measurements at z ~ 3-4 and mechanisms behind the escape

    NASA Astrophysics Data System (ADS)

    Cooke, Jeff; Ryan-Weber, Emma; Garel, Thibault; Gonzalo Diaz, C.

    2016-06-01

    Measuring the surviving Lyman continuum (LyC) flux and inferred ionizing photon escape fraction (f_esc) of Lyman break galaxies has proved challenging, in part due to the historical selection criteria based on a Lyman continuum break. A few galaxies, largely serendipitous, have been detected with measurable LyC flux but have colors inconsistent with Lyman break galaxy expectations for their specific redshifts. I will discuss our physically motivated technique that provides an accurate measure of the average f_esc for the z ~ 3 Lyman break galaxy population that has also identified a population of galaxies, termed Lyman continuum galaxies (LCGs) with high expected levels of surviving LyC flux. I will present the results of our program that uses 30-band photometry, HST imaging, and deep medium-band IR imaging from the ZFOURGE survey to select z ~ 3-4 LCGs. We obtained very deep Keck spectroscopy that has confirmed the LCG population and has directly measured the predicted level of LyC flux. In addition, our program has obtained deep Keck infrared spectroscopy to calibrate restframe optical nebular emission-line models used to predict the LyC escape fraction, with the aim to measure the f_esc of galaxies at the Epoch of Reionization where direct LyC flux detection is not possible.

  14. Variability of the Lyman alpha flux with solar activity

    SciTech Connect

    Lean, J.L.; Skumanich, A.

    1983-07-01

    A three-component model of the solar chromosphere, developed from ground based observations of the Ca II K chromospheric emission, is used to calculate the variability of the Lyman alpha flux between 1969 and 1980. The Lyman alpha flux at solar minimum is required in the model and is taken as 2.32 x 10/sup 11/ photons/cm/sup 2//s. This value occurred during 1975 as well as in 1976 near the commencement of solar cycle 21. The model predicts that the Lyman alpha flux increases to as much as 5 x 10/sup 11/ photons/cm/sup 2//s at the maximum of the solar cycle. The ratio of the average fluxes for December 1979 (cycle maximum) and July 1976 (cycle minimum) is 1.9. During solar maximum the 27-day solar rotation is shown to cause the Lyman alpha flux to vary by as much as 40% or as little as 5%. The model also shows that the Lyman alpha flux varies over intermediate time periods of 2 to 3 years, as well as over the 11-year sunspot cycle. We conclude that, unlike the sunspot number and the 10.7-cm radio flux, the Lyman alpha flux had a variability that was approximately the same during each of the past three cycles. Lyman alpha fluxes calculated by the model are consistent with measurements of the Lyman alpha flux made by 11 of a total of 14 rocket experiments conducted during the period 1969--1980. The model explains satisfactorily the absolute magnitude, long-term trends, and the cycle variability seen in the Lyman alpha irradiances by the OSO 5 satellite experiment. The 27-day variability observed by the AE-E satellite experiment is well reproduced. However, the magntidue of the AE-E 1 Lyman alpha irradiances are higher than the model calculations by between 40% and 80%. We suggest that the assumed calibration of the AE-E irradiances is in error.

  15. Physical Properties of Lyman-alpha Forest and Damped Lyman-alpha Systems

    NASA Astrophysics Data System (ADS)

    Kulkarni, V. P.; Fall, S. M.

    1995-12-01

    We present a review of our results regarding various physical properties of quasar absorption line systems, in particular, the Lyman-alpha forest and the damped Lyman-alpha systems. We made the first detection of the quasar proximity effect at low redshifts, using HST Key Project data on the Ly-alpha forest for z < 1. This allowed the first empirical estimate of the intensity of the ionizing UV background at < z > ~ 0.5 and showed evidence for evolution of the ionizing UV background with redshift. We have also studied the implications of non-thermal motions inside Ly-alpha forest clouds for the statistics of these clouds. We showed that the distributions in H I column densities f(N) for systems with saturated Ly-alpha lines and the extent (and sign) of N-sigma correlations could differ from previous estimates, if the clouds possessed non-Maxwellian velocity distributions. We also present results of a study of the chemical properties of several damped Lyman-alpha systems, based on published high-sensitivity observations. In particular, we examine the total (gas + solid phase) metallicity and the dust content of these systems. Results will also be presented of an analysis of an 18 km s(-1) resolution spectrum of the Ly-alpha forest of the z = 2.1 quasar Q1331+170, performed in collaboration with Dr. D. G. York, Dr. D. E. Welty (U. Chicago), Dr. R. F. Green, Dr. K. Huang (NOAO) and Dr. J. Bechtold (U. Arizona). One of the main results is some evidence for small-scale clustering among the Ly-alpha forest clouds.

  16. Cryptogenic organizing pneumonia: clinical profile in a series of 34 admitted patients in a hospital in India.

    PubMed

    Sen, T; Udwadia, Z F

    2008-04-01

    Cryptogenic Organizing Pneumonia (COP) is a relatively rare disorder which is gratifying to treat due to its prompt steroid responsiveness. There have been only 2 case reports on COP from India but no large series entity reported from this country. The medical records of all patients with biopsy (histopathology) proven COP admitted in a tertiary care hospital in Mumbai (2000-2005) were retrospectively analyzed. We looked at clinical and radiographic profiles, initial diagnosis and treatment, lag period to starting definitive therapy and steroid responsiveness. When compared to other series of patients with COP, our series showed several similarities and some differences. Distinctive features were the striking female preponderance and the utility of transbronchial biopsies in establishing the diagnosis. Long delays in diagnosis with patients mislabeled as tuberculosis or pneumonia, lead to delays in starting steroids resulting in 21% of our patients continuing to deteriorate. This comprehensive review of COP, the first of its kind from India, reveals its varied clinical and radiographic spectrum. A high index of suspicion will lead to prompt steroid therapy which will result in better patient outcome.

  17. A Systematic Approach to Time-series Metabolite Profiling and RNA-seq Analysis of Chinese Hamster Ovary Cell Culture.

    PubMed

    Hsu, Han-Hsiu; Araki, Michihiro; Mochizuki, Masao; Hori, Yoshimi; Murata, Masahiro; Kahar, Prihardi; Yoshida, Takanobu; Hasunuma, Tomohisa; Kondo, Akihiko

    2017-03-02

    Chinese hamster ovary (CHO) cells are the primary host used for biopharmaceutical protein production. The engineering of CHO cells to produce higher amounts of biopharmaceuticals has been highly dependent on empirical approaches, but recent high-throughput "omics" methods are changing the situation in a rational manner. Omics data analyses using gene expression or metabolite profiling make it possible to identify key genes and metabolites in antibody production. Systematic omics approaches using different types of time-series data are expected to further enhance understanding of cellular behaviours and molecular networks for rational design of CHO cells. This study developed a systematic method for obtaining and analysing time-dependent intracellular and extracellular metabolite profiles, RNA-seq data (enzymatic mRNA levels) and cell counts from CHO cell cultures to capture an overall view of the CHO central metabolic pathway (CMP). We then calculated correlation coefficients among all the profiles and visualised the whole CMP by heatmap analysis and metabolic pathway mapping, to classify genes and metabolites together. This approach provides an efficient platform to identify key genes and metabolites in CHO cell culture.

  18. A Systematic Approach to Time-series Metabolite Profiling and RNA-seq Analysis of Chinese Hamster Ovary Cell Culture

    PubMed Central

    Hsu, Han-Hsiu; Araki, Michihiro; Mochizuki, Masao; Hori, Yoshimi; Murata, Masahiro; Kahar, Prihardi; Yoshida, Takanobu; Hasunuma, Tomohisa; Kondo, Akihiko

    2017-01-01

    Chinese hamster ovary (CHO) cells are the primary host used for biopharmaceutical protein production. The engineering of CHO cells to produce higher amounts of biopharmaceuticals has been highly dependent on empirical approaches, but recent high-throughput “omics” methods are changing the situation in a rational manner. Omics data analyses using gene expression or metabolite profiling make it possible to identify key genes and metabolites in antibody production. Systematic omics approaches using different types of time-series data are expected to further enhance understanding of cellular behaviours and molecular networks for rational design of CHO cells. This study developed a systematic method for obtaining and analysing time-dependent intracellular and extracellular metabolite profiles, RNA-seq data (enzymatic mRNA levels) and cell counts from CHO cell cultures to capture an overall view of the CHO central metabolic pathway (CMP). We then calculated correlation coefficients among all the profiles and visualised the whole CMP by heatmap analysis and metabolic pathway mapping, to classify genes and metabolites together. This approach provides an efficient platform to identify key genes and metabolites in CHO cell culture. PMID:28252038

  19. [Profile Orifice Shapers. A valid instrument also for the root canal preparation of short teeth: proposal for a series modification].

    PubMed

    Marsico, E M; Rao Genovese, F

    2002-10-01

    The several endodontic instruments, currently used for the canal preparation with the crown-down technique, simplified only in part root canal therapy, but increased the costs. The authors examined the Profile Orefice Shapers Series, planned only for the preparation of the coronal third, and carried out a comparative analysis with other endodontic instruments currently available. Eighty-seven teeth with a 19 mm work lenght were selected for this study. Endodontic treatment was performed using exclusively Profile Orefice Shapers under constant irrigation with 2.5% sodium hypoclorite to clean and shape the canal and System B and Obtura II to obturate the root canal system. Postoperative films show an adequate root canal shaping and a complete apical seal. Endodontic therapy was simplified (only 5 instruments to obtain a good canal shaping); clinical time and costs were decreased. The authors obtained a good shaping and apical seal using the Profile Orefice Shapers in short teeth. The quality of the root canal therapy obtainable with these instruments is confirmed by radiographs. Some modifications are suggested: increase of instruments working length, introduction of 3 extra intermediate instruments and restriction of working part diameter (1 mm) and operative procedures that lead to obtain an excellent and complete use of these instruments.

  20. Dynamic Agricultural Land Unit Profile Database Generation using Landsat Time Series Images

    NASA Astrophysics Data System (ADS)

    Torres-Rua, A. F.; McKee, M.

    2012-12-01

    government efforts for a given occurrence at the land unit level, and affecting the potential economic trade-off level in the area. In this study a framework is proposed to create and continuously update a land unit profile database using historical Landsat satellite imagery records. An experimental test is implemented for the agricultural lands in Central Utah. This location was selected because of their success in increasing the efficiency of water use and control along the entire irrigation system. A set of crop health metrics from the literature (NDVI, LAI, NDWI) is calculated and evaluated to measure crop response to farm management for its evaluation in time. The resulting land unit profile database is then tested to determine land unit profile groups based on land unit management characteristics. Comparison with essential inputs (water availability and climate conditions) and crop type (outputs) on a year basis is provided.

  1. Coastal environmental profile of South Jahore, Malaysia. Technical pub. series 6

    SciTech Connect

    Not Available

    1991-01-01

    Malaysia's South Johore region has undergone rapid development recently, seriously damaging its ecologically sensitive and important coastal resources. The report profiles the area's coastal environment and identies major environmental problems, as well as chief obstacles to sustainable development. Chapter 2 describes South Johore's physical environment, physiography, climate, and geology. Chapters 3-7 cover in detail the area's natural resource endowment; coastal ecosystems; population and socioeconomics; land use; and fisheries and aquaculture. Chapter 8 focuses on economic sectors other than aquaculture, including agriculture, forestry, livestock, shipping, industry, and transportation, while Chapter 9 covers tourism and its potential impact on South Johore's ecology. Chapter 10 reviews the major types of environmental degradation in the region, including various types of coastal pollution, forest destruction, and coastal erosion. The laws, regulations, and institutions that govern environmental management are covered in Chapter 11. Chapter 12 concludes the report with an overview of the chief constraints to effective environmental management.

  2. Lyman Alpha Blobs: Seeds of Galaxy Groups

    NASA Astrophysics Data System (ADS)

    Hall, Agnar; Prescott, Moire

    2017-01-01

    Recently, evidence has been mounting that giant Lyman alpha (Lya) nebulae, or "blobs," at high redshift are coincident with regions of galaxy overdensity and likely the progenitors of galaxy groups. These Lya blobs are rare structures found at roughly 1 < z < 6 which have typical diameters of ~100 kpc and Lya luminosities of ~10^42 to 10^44 erg s^-1. Using Hubble Space Telescope (HST) imaging, we explore the environments of three systematically-selected blobs at 1.5 < z < 2.5. Comparing the total surface density of galaxies in a region centered on the blob to the average surface density of galaxies in the field, we find that all three blobs exhibit significant overdensity (up to a factor of 5-10). After narrowing down which galaxies are most likely to be associated with each Lya blob, we confirm that the raw overdensities are enhanced and find evidence of a luminosity gap in at least one of the three systems studied. These results suggest that Lya blobs offer new insight into the early phases of galaxy group and cluster formation.

  3. Obituary: Lyman Francis Kells, 1917-2004

    NASA Astrophysics Data System (ADS)

    Hockey, Thomas

    2007-12-01

    Lyman Francis Kells was born in Seattle, Washington, on 19 May 1917. He earned a 1938 BS in Chemistry from the University of Washington. He received a PhD. in 1944, also from the University of Washington. Kells held research positions at the Carbide and Carbon Chemicals Corporation of New York, New York, from 1944 through 1946; the Standard Oil Development Company of New Jersey, from 1946 through 1948; and Allied Chemical Corporation of Morristown, New Jersey, from 1951 through 1961. His wartime work involved the separation of Uranium isotopes by gaseous diffusion, based on a method developed in part by Harold Urey. Kells was on the faculty of Hunter College 1948-1949, an Assistant Professor at Iona College 1949-1951, a Special Lecturer at Newark College of Engineering in 1961, an Assistant Professor of Chemistry at East Tennessee State University 1962-1964, and a Professor of Chemistry at Westmar College 1964-1974. He died on 4 November 2004 in Seattle, Washington. Kells was a member of the American Association for the Advancement of Science, the American Chemical Society, the Astronomical Society of the Pacific, and the New York Academy of Science, as well as this Society. He was a Unitarian. Kells is survived by his daughters Leila Stefani Newcomb and Christina V. Cohen.

  4. The Lyman far ultraviolet spectroscopic explorer

    NASA Astrophysics Data System (ADS)

    Moos, Warren

    The Lyman Far UltravioletSpectroscopic Explorer mission will obtain high resolution spectra (R~30,000) in the 912 to 1200 Å region with sufficient sensitivity to study faint sources throughout the galaxy and at large extragalactic distances. This spectral region provides unique tools for solving problems in cosmology (e.g. deuterium), galactic structure and evolution (e.g. O VI and H2), stellar evolution (e.g. O VI), and planetary science (e.g. H2). The transmission of the glancing incidence telescope will enable extension of the spectral coverage with moderate resolution down to 100 Å. The Phase A instrument design consists of a 70 cm Wolter type II telescope feeding either near normal incidence gratings on the Rowland circle for the longer wavelengths or glancing incidence EUV gratings for coverage down to 100 Å. In 1989, NASA selected the mission for Phase B study. Both Canada and the United Kingdom are participating in the definition and development of the mission.

  5. Magnetic Turbulence and Line Broadening in Simulations of Lyman-Alpha Absorption

    NASA Astrophysics Data System (ADS)

    Gurvich, Alex; Burkhart, Blakesley K.; Bird, Simeon

    2016-01-01

    We use the Illustris cosmological AREPO simulations to study the effects of gas turbulence and magnetic fields on measurements from the Lyman-Alpha forest. We generate simulated Lyman-Alpha spectra and plot the distributions of Column Density (CDD) and Doppler Width (b) both by adhering to the canonical method of fitting Voigt profiles to absorption lines and by directly measuring the column density and equivalent widths from snapshot data .We investigate the effects of additional unresolved gas turbulence in Illustris by adding an additional broadening term to the line profiles to mimic turbulent broadening. When we do this, we find a measurable effect in the CDD and an offset in the mean of the b distribution corresponding to the additional turbulence. We also compare different MHD runs in AREPO we find that the CDD can measurably differentiate between magnetic seed field at redshifts as low as z=0.1, but we do not find that the b distribution is affected at a detectable level. Our work suggests that the effects of turbulence and magnetic fields from z=2-0.1 can potentially be measured with these diagnostics. This work was supported in part by the NSF REU and DoD ASSURE programs under NSF grant no. 1262851 and by the Smithsonian Institution.

  6. Faint Lyman Alpha Emitters And Lyman Break Galaxies In The A2744 Field.

    NASA Astrophysics Data System (ADS)

    de la Vieuville, Geoffroy

    2017-06-01

    We present in this work the results obtained on the characterization of the sources of reionization behind the lensing cluster A2744. Taking advantage of the combined very deep observations of the MUSE-IFU (GTO program) and Hubble (Frontiers Field program), we are able to blindly spectroscopically select a large sample of Lyman-Alpha Emitters (LAEs) ( 3 < z < 6.7 ) and apply photometric criteria to select a population of Lyman-Break Galaxies (LBGs)( z 3 - 8 )in the MUSE FOV. Thanks to the capabilities of MUSE and the lensing effect, our LAE sample is typically 10-100 times fainter (39 < Log(L) < 42.5 ) than in blank field surveys, allowing us to set reliable constraints on the faint end of the LAE luminosity functions. Our recent work on the LAE luminosity function shows that this population could possibly play a predominant role in the reionization of the universe. The relative contribution of the different star forming galaxies (LAE and LBG) remains highly uncertain. As the two populations are selected in the exact same volume of universe, this work allows us to discuss the intersection of those two populations as well as the evolution of their contribution to reionization with redshift.

  7. 13 years time series of stratospheric and mesospheric ozone profiles measured by the NDACC microwave radiometer SOMORA over Switzerland: comparison to radiosonde and MLS/AURA satellite ozone profiles.

    NASA Astrophysics Data System (ADS)

    Maillard Barras, Eliane; Haefele, Alexander; Ruffieux, Dominique; Kämpfer, Niklaus

    2014-05-01

    The microwave radiometer SOMORA measures ozone volume mixing ratio in the stratosphere and lower mesosphere since January 2000 with a time resolution of 30 min. The ozone vertical distribution is calculated from the measurement of the rotational emission line of ozone at 142.17 GHz. Ozone profiles are retrieved using ARTS/Qpack, a general environment for radiative transfer simulation and retrieval of ozone profiles based on the optimal estimation method (OEM) of Rodgers. SOMORA is an instrument of the NDACC.The measurement time series has been influenced by the upgrade from an acousto optical spectrometer (AOS) setup to a digital FFT spectrometer setup in 2010. The ozone profiles dataset measured by the AOS (2000-2010) and FFT spectrometer (since 2010) is then homogenized using one year parallel measurements by adding an altitude dependent offset to the AOS ozone profiles. The ozone profiles measured by AOS show a slightly better vertical resolution above 55 km than the ozone profiles measured by FFT due to the higher spectral resolution.The homogenized 13 years SOMORA time series has been validated against Payerne radiosonde (RS) ozone profiles, GROMOS microwave radiometer ozone profiles of Bern, another NDACC instrument, and MLS/AURA satellite simultaneous ozones profiles, and the results will be shown. For the whole period of respective common measurements, SOMORA ozone profiles are within 5% of Payerne RS, 15% of GROMOS and 10% of MLS ozone profiles.

  8. First Results from the Large Area Lyman Alpha Survey

    NASA Astrophysics Data System (ADS)

    Rhoads, J. E.; Malhotra, S.; Dey, A.; Stern, D.; Spinrad, H.; Jannuzi, B. T.

    1999-12-01

    Young galaxies undergoing their first burst of star formation are expected to have strong Lyman-α emission, due to low metallicity and dust content. However, studies to date have found comparatively small samples of such objects. We have embarked on a major project to obtain a statistically useful sample of several hundred Lyman-α emitters at z 4.5 (the Large Area Lyman Alpha, or LALA, survey). We are using the 8k x 8k CCD Mosaic camera at the Kitt Peak National Observatory 4m Mayall telescope. To date, we have surveyed a total volume of 1.3 x 106 comoving Mpc^3 (H_0 =70, \\Omega_m =0.2, \\Lambda=0) to 5 \\sigma flux limits of (1.8 to 2.6) \\times 10^{-17} erg/cm^2 /s. We are finding an emission line object density of 9 deg-2 Angstroms-1 with narrowband flux between 2.6 and 5.2 x 10-17 erg/cm2/ s at wavelength \\lambda \\simeq 6640 Angstroms. Our first spectroscopic followup with the Keck 10m telescope implies that \\sim 1/3 to 1/2 of these are z\\approx 4.5 Lyman-\\alpha emitters, and that the density of Lyman-\\alpha emitters in this restricted flux range is \\sim 4000 deg^{-2} (unit z)^{-1}, or \\sim 9\\times 10^{-4} Mpc^{-3}$ for our assumed cosmology.

  9. The Characteristic Dimension of Lyman-Alpha Forest Clouds Toward Q0957+561

    NASA Technical Reports Server (NTRS)

    Dolan, J. F.; Michalitsianos, A. G.; Hill, R. J.; Nguyen, Q. T.; Fisher, Richard (Technical Monitor)

    2000-01-01

    Far-ultraviolet spectra of the gravitational lens components Q0957+561 A and B were obtained with the Hubble Space Telescope Faint Object Spectrograph to investigate the characteristic dimension of Lyman-alpha forest clouds in the direction of the quasar. If one makes the usual assumption that the absorbing structures are spherical clouds with a single radius, that radius can be found analytically from the ratio of Lyman-alpha lines in only one line of sight to the number in both. A simple power series approximation to this solution, accurate everywhere to better than 1%, will be presented. Absorption lines in Q0957+561 having equivalent width greater than 0.3 A in the observer's frame not previously identified as interstellar lines, metal lines, or higher order Lyman lines were taken to be Ly-alpha forest lines. The existence of each line in this consistently selected set was then verified by its presence in two archival FOS spectra with approximately 1.5 times higher signal to noise than our spectra. Ly-alpha forest lines appear at 41 distinct wavelengths in the spectra of the two images. One absorption line in the spectrum of image A has no counterpart in the spectrum of image B, and one line in image B has no counterpart in image A. Based on the separation of the lines of sight over the redshift range searched for Ly-alpha forest lines, the density of the absorbing clouds in the direction of Q0957+561 must change significantly over a radius R = 160 (+120, -70) h (sup -1) (sub 50) kpc (H (sub 0) 50 h (sub 50) km s (sup -1) kpc (sup -1), q (sub 0) = 1/2). The 95% confidence interval on R extends from (50 950) h (sup -1) (sub 50) kpc.

  10. Headache attributed to airplane travel ('airplane headache'): clinical profile based on a large case series.

    PubMed

    Mainardi, F; Lisotto, C; Maggioni, F; Zanchin, G

    2012-06-01

    The 'headache attributed to airplane travel', also named 'airplane headache' (AH), is a recently described headache disorder that appears exclusively in relation to airplane flights, in particular during the landing phase. Based on the stereotypical nature of the attacks in all reported cases, we proposed provisional diagnostic criteria for AH in a previously published paper. Up to now 37 cases have been described in the literature. After our paper was disseminated via the Internet, we received several email messages from subjects around the world who had experienced such a peculiar headache. Their cooperation, by completing a structured questionnaire and allowing the direct observation of three subjects, enabled us to carry out a study on a total of 75 patients suffering from AH. Our survey confirmed the stereotypical nature of the attacks, in particular with regard to the short duration of the pain (lasting less than 30 minutes in up to 95% of the cases), the clear relationship with the landing phase, the unilateral pain, the male preponderance, and the absence of accompanying signs and/or symptoms. It is conceivable to consider barotrauma as one of the main mechanisms involved in the pathophysiology of AH. The observation that the pain appears inconstantly in the majority of cases, without any evident disorder affecting the paranasal sinuses, could be consistent with a multimodal pathogenesis underlying this condition, possibly resulting in the interaction between anatomic, environmental and temporary concurrent factors. This is by far the largest AH case series ever reported in the literature. The diagnostic criteria that we previously proposed proved to be valid when applied to a large number of patients suffering from this condition. We support its recognition as a new form of headache, to be included in the forthcoming update of the International Headache Society Classification, within '10. Headache attributed to disorder of homoeostasis'. Its formal

  11. Green Peas and diagnostics for Lyman continuum leaking in star-forming dwarf galaxies

    NASA Astrophysics Data System (ADS)

    Thuan, Trinh

    2014-10-01

    One of the key questions in observational cosmology is the identification of the sources responsible for cosmic reionization. The general consensus is that a population of faint low-mass galaxies must be responsible for the bulk of the ionizing photons. However, attempts at identifying individual galaxies showing Lyman continuum (LyC) leakage have so far not been successful, both at high and low redshifts. We propose here to observe directly the LyC of five so-called "Green Pea" (GP) galaxies. GPs share many of the properties of the Lyman Break galaxies at high z (compactness, low mass, low metallicity, high specific star formation rate, gas-rich and clumpy morphology) and may constitute local examples of the long sought-after LyC leaking galaxies. The five GPs have been identified by searching the Sloan Data Release 10 spectral data base of 2 million spectra for non-AGN emission-line objects that meet the following criteria: high [OIII]5007/[OII]3727 ratios, large GALEX FUV fluxes, and redshifted enough (z~0.3) so that the LyC is shifted into the sensitive spectral range of COS. Our unique GP sample will allow us to combine for the first time four fundamental tests for LyC leaking in galaxies and validate their usefulness as LyC leaking indicators : 1) direct measurements of the LyC; 2) high [OIII]/[OII] ratios; 3) characteristics of the Lyman alpha line profile; and 4) residual intensities in the low-ionization ISM absorption UV lines.

  12. Doppler speeds of the hydrogen Lyman lines in solar flares from EVE

    NASA Astrophysics Data System (ADS)

    Brown, Stephen

    2016-10-01

    The hydrogen Lyman lines provide important diagnostic information about the dynamics of the chromosphere, but until recently there have been few systematic studies of their variability during flares. We investigate Doppler shifts in these lines in several flares, and use these to calculate plasma speeds. We use spectral data from the Multiple EUV Grating Spectrograph B (MEGS-B) detector on board the Extreme-Ultraviolet Variability Experiment (EVE) instrument on the Solar Dynamics Observatory. MEGS-B obtains full-disk spectra of the Sun at a resolution of 0.1nm in the range 37-105nm, which we analyse using three independent methods. The first method performs Gaussian fits to the lines, and compares the quiet-Sun centroids with the flaring ones to obtain the Doppler shifts. The second method uses cross-correlation to detect wavelength shifts between the quiet-Sun and flaring line profiles. The final method calculates the “center-of-mass" of the line profile, and compares the quiet-Sun and flaring centroids to obtain the shift. In a study of 6 flares we find signatures of both upflow and downflow in the Lyman lines, with speeds of around 10 km s^‑1 in the line profiles that have not undergone pre-flare subtraction, and speeds in the flare-excess profiles of around 30 km s^‑1 . We include analysis of AIA images of these events in order to understand potential contributions from material ejections, and find that not all upflows can be explained by ejecta. We discuss current and future attempts at modelling these line profiles.

  13. 75 FR 53323 - Certificate of Alternative Compliance for the Offshore Supply Vessel LYMAN MARTIN

    Federal Register 2010, 2011, 2012, 2013, 2014

    2010-08-31

    ... SECURITY Coast Guard Certificate of Alternative Compliance for the Offshore Supply Vessel LYMAN MARTIN... Alternative Compliance was issued for the offshore supply vessel LYMAN MARTIN as required by 33 U.S.C. 1605(c... LYMAN MARTIN, O.N. 11227085. The horizontal distance between the forward and aft masthead lights may...

  14. Lyman Alpha Galaxies and Galaxy Formation Scenarios

    NASA Astrophysics Data System (ADS)

    Malhotra, Sangeeta; Rhoads, James; Dey, Arjun; Jannuzi, Buell

    2003-02-01

    The Large Area Lyman Alpha survey has successfully identified the population of young Lyα emitting galaxies predicted over 30 years ago. High equivalent widths of Lyα line in these sources suggest that they are a very young (age < 10^7 years), metal poor, population of stars at redshifts 4.5, 5.7 and 6.6, making them very interesting objects to study in the context of galaxy formation scenarios. We have begun to do exactly this using the correlation function of LALA galaxies, with fairly puzzling results. Before this leads to more complications in theoretical galaxy formation scenarios, we would like to put the observational results on a firm footing. In order to do that we ask for one night of Keck/Deimos time for spectroscopic confirmation of 50 secure LALA sources at z=4.5, and a similar number of fainter sources, in order to (1) characterize the completeness of this survey, and (2) weed out foreground emission line galaxies which affect the small scale correlation function. The excellent match between wide-field capabilities of DEIMOS and the LALA survey will allow the most complete confirmation and characterization of the high redshift Lyα population yet in terms of photometric sample reliability, while our planned spectra of foreground emission line galaxies will lead to a characterization of emission line selected star-forming galaxies at 0.25 < z < 1.5. We will use our spectroscopic sample to obtain a clean measurement of the small scale correlations among Lyα galaxies (which are clearly seen in our photometric sample). This will let us understand the halo mass, occupancy number, and duty cycle of these objects, and hence better how Lyα sources fit into the bigger picture of galaxy formation.

  15. Gas Accretion via Lyman Limit Systems

    NASA Astrophysics Data System (ADS)

    Lehner, Nicolas

    In cosmological simulations, a large fraction of the partial Lyman limit systems (pLLSs; 16 log N HI < 17 . 2 16\\lesssim \\log N_{\\text{HI}} < 17.2 ) and LLSs (17. 2 ≤ logN HI < 19) probes large-scale flows in and out of galaxies through their circumgalactic medium (CGM). The overall low metallicity of the cold gaseous streams feeding galaxies seen in these simulations is the key to differentiating them from metal rich gas that is either outflowing or being recycled. In recent years, several groups have empirically determined an entirely new wealth of information on the pLLSs and LLSs over a wide range of redshifts. A major focus of the recent research has been to empirically determine the metallicity distribution of the gas probed by pLLSs and LLSs in sizable and representative samples at both low (z < 1) and high (z > 2) redshifts. Here I discuss unambiguous evidence for metal-poor gas at all z probed by the pLLSs and LLSs. At z < 1, all the pLLSs and LLSs so far studied are located in the CGM of galaxies with projected distances \\lesssim 100-200 kpc. Regardless of the exact origin of the low-metallicity pLLSs/LLSs, there is a significant mass of cool, dense, low-metallicity gas in the CGM that may be available as fuel for continuing star formation in galaxies over cosmic time. As such, the metal-poor pLLSs and LLSs are currently among the best observational evidence of cold, metal-poor gas accretion onto galaxies.

  16. Simulating the time series of a selected gene expression profile in an agent-based tumor model

    NASA Astrophysics Data System (ADS)

    Mansury, Yuri; Deisboeck, Thomas S.

    2004-09-01

    To elucidate the role of environmental conditions in molecular-level dynamics and to study their impact on macroscopic brain tumor growth patterns, the expression of the genes Tenascin C and PCNA in a 2D agent-based model for the migratory trait is calibrated using experimental data from the literature, while the expression of these genes for the proliferative trait is obtained as the model output. Numerical results confirm that the gene expression of Tenascin C is indeed consistently higher in the migratory glioma cell phenotype and show that the expression of PCNA is consistently higher among proliferating tumor cells. Intriguingly, the time series of the tumor cells’ gene expression exhibit a sudden change in behavior during the invasion of the tumor into a nutrient-abundant region, showing a robust positive correlation between the expression of Tenascin C and the tumor’s diameter, yet a strong negative correlation between the expression of PCNA and the diameter. These molecular-level dynamics correspond to the emergence of a structural asymmetry in the form of a bulging tumor rim in the nutrient-abundant region. The simulated time series thus supports the critical role of the migratory cell phenotype during both the tumor system’s overall macroscopic expansion and the evolvement of regional growth patterns, particularly in the later stages. Furthermore, detrended fluctuation analysis (DFA) suggests that for prediction purposes, the simulated gene expression profiles of Tenascin C and PCNA that were determined separately for the migrating and proliferating phenotypes exhibit lesser predictability than those of the phenotypic mixture combining all viable tumor cells typically found in clinical biopsies. Finally, partitioning the tumor into distinct geographic regions of interest (ROI) reveals that the gene expression profile of tumor cells in the quadrant close to the nutrient-abundant region is representative for the entire tumor whereas the expression

  17. Stellar lyman alpha emission and the local interstellar medium

    NASA Technical Reports Server (NTRS)

    Simon, Theodore

    1992-01-01

    Under the auspices of this ADP program, a systematic study was made of IUE archival images in order to extract spectra of the Lyman alpha region and to measure the stellar Lyman alpha flux for as many late-type stars as possible. The Lyman alpha resonance line is a powerful cooling channel for the hot chromospheres of solar-type stars, but has not been studied before in any systematic fashion across the H-R diagram. A major deterrent which has limited the use of Lyman alpha in the study of stellar chromospheres is the contamination of this spectral feature caused by the scattering of solar Lyman alpha photons in the Earth's exosphere. This scattered light is monochromatically imaged through the entrance slot of the IUE telescope and is superposed onto the stellar spectrum. In all but the shortest exposures with IUE, this 'geocoronal emission' overwhelms the stellar flux and makes it impossible to directly measure the strength of the stellar chromospheric feature. The IUESIPS processing contains no provision for correcting standard G.O. output products for this contamination. The first task was to develop a scheme for removing the geocoronal flux, specifically from low-dispersion spectra taken with the Short-Wavelength Camera of IUE. The strategy adopted was to fit a 'sky model' to the spatially-resolved geocoronal emission observed through the large science aperture of the telescope, using the spectral orders on either side of the central ones where the stellar emission is concentrated. The model emission was then subtracted from the observed image, leaving behind the corrected stellar Lyman alpha emission. The details of this fitting procedure are described. Having devised a successful method for removing the unwanted geocoronal emission, the correction procedure was applied to 366 archival images which, from inspection of the photowrites in the IUE browse file, seemed especially promising. In this survey, Lyman alpha emission were eventually detected in the

  18. Influence of dense quantum plasmas on fine-structure splitting of Lyman doublets of hydrogenic systems

    NASA Astrophysics Data System (ADS)

    De, Madhab; Ray, Debasis

    2015-05-01

    Relativistic calculations are performed to study the effects of oscillatory quantum plasma screening on the fine-structure splitting between the components of Lyman-α and β line doublets of atomic hydrogen and hydrgen-like argon ion within dense quantum plasmas, where the effective two-body (electron-nucleus) interaction is modeled by the Shukla-Eliasson oscillatory exponential cosine screened-Coulomb potential. The numerical solutions of the radial Dirac equation for the quantum plasma-embedded atomic systems reveal that the oscillatory quantum screening effect suppresses the doublet (energy) splitting substantially and the suppression becomes more prominent at large quantum wave number kq. In the absence of the oscillatory cosine screening term, much larger amount of suppression is noticed at larger values of kq, and the corresponding results represent the screening effect of an exponential screened-Coulomb two-body interaction. The Z4 scaling of the Lyman doublet splitting in low-Z hydrogen isoelectronic series of ions in free space is violated in dense quantum plasma environments. The relativistic data for the doublet splitting in the zero screening (kq = 0) case are in very good agreement with the NIST reference data, with slight discrepancies (˜0.2%) arising from the neglect of the quantum electrodynamic effects.

  19. Influence of dense quantum plasmas on fine-structure splitting of Lyman doublets of hydrogenic systems

    SciTech Connect

    De, Madhab Ray, Debasis

    2015-05-15

    Relativistic calculations are performed to study the effects of oscillatory quantum plasma screening on the fine-structure splitting between the components of Lyman-α and β line doublets of atomic hydrogen and hydrgen-like argon ion within dense quantum plasmas, where the effective two-body (electron–nucleus) interaction is modeled by the Shukla–Eliasson oscillatory exponential cosine screened-Coulomb potential. The numerical solutions of the radial Dirac equation for the quantum plasma-embedded atomic systems reveal that the oscillatory quantum screening effect suppresses the doublet (energy) splitting substantially and the suppression becomes more prominent at large quantum wave number k{sub q}. In the absence of the oscillatory cosine screening term, much larger amount of suppression is noticed at larger values of k{sub q}, and the corresponding results represent the screening effect of an exponential screened-Coulomb two-body interaction. The Z{sup 4} scaling of the Lyman doublet splitting in low-Z hydrogen isoelectronic series of ions in free space is violated in dense quantum plasma environments. The relativistic data for the doublet splitting in the zero screening (k{sub q} = 0) case are in very good agreement with the NIST reference data, with slight discrepancies (∼0.2%) arising from the neglect of the quantum electrodynamic effects.

  20. Performance Characterization of the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) CCD Cameras

    NASA Technical Reports Server (NTRS)

    Joiner, Reyann; Kobayashi, Ken; Winebarger, Amy; Champey, Patrick

    2014-01-01

    The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a sounding rocket instrument which is currently being developed by NASA's Marshall Space Flight Center (MSFC) and the National Astronomical Observatory of Japan (NAOJ). The goal of this instrument is to observe and detect the Hanle effect in the scattered Lyman-Alpha UV (121.6nm) light emitted by the Sun's Chromosphere to make measurements of the magnetic field in this region. In order to make accurate measurements of this effect, the performance characteristics of the three on-board charge-coupled devices (CCDs) must meet certain requirements. These characteristics include: quantum efficiency, gain, dark current, noise, and linearity. Each of these must meet predetermined requirements in order to achieve satisfactory performance for the mission. The cameras must be able to operate with a gain of no greater than 2 e(-)/DN, a noise level less than 25e(-), a dark current level which is less than 10e(-)/pixel/s, and a residual nonlinearity of less than 1%. Determining these characteristics involves performing a series of tests with each of the cameras in a high vacuum environment. Here we present the methods and results of each of these performance tests for the CLASP flight cameras.

  1. Performance Characterization of the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) CCD Cameras

    NASA Technical Reports Server (NTRS)

    Joiner, Reyann; Kobayashi, Ken; Winebarger, Amy; Champey, Patrick

    2014-01-01

    The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a sounding rocket instrument currently being developed by NASA's Marshall Space Flight Center (MSFC), the National Astronomical Observatory of Japan (NAOJ), and other partners. The goal of this instrument is to observe and detect the Hanle effect in the scattered Lyman-Alpha UV (121.6nm) light emitted by the Sun's chromosphere. The polarized spectrum imaged by the CCD cameras will capture information about the local magnetic field, allowing for measurements of magnetic strength and structure. In order to make accurate measurements of this effect, the performance characteristics of the three on- board charge-coupled devices (CCDs) must meet certain requirements. These characteristics include: quantum efficiency, gain, dark current, read noise, and linearity. Each of these must meet predetermined requirements in order to achieve satisfactory performance for the mission. The cameras must be able to operate with a gain of 2.0+/- 0.5 e--/DN, a read noise level less than 25e-, a dark current level which is less than 10e-/pixel/s, and a residual non- linearity of less than 1%. Determining these characteristics involves performing a series of tests with each of the cameras in a high vacuum environment. Here we present the methods and results of each of these performance tests for the CLASP flight cameras.

  2. THE LYMAN ALPHA REFERENCE SAMPLE: EXTENDED LYMAN ALPHA HALOS PRODUCED AT LOW DUST CONTENT

    SciTech Connect

    Hayes, Matthew; Oestlin, Goeran; Duval, Florent; Guaita, Lucia; Melinder, Jens; Sandberg, Andreas; Schaerer, Daniel; Verhamme, Anne; Orlitova, Ivana; Mas-Hesse, J. Miguel; Oti-Floranes, Hector; Adamo, Angela; Atek, Hakim; Cannon, John M.; Herenz, E. Christian; Kunth, Daniel; Laursen, Peter

    2013-03-10

    We report on new imaging observations of the Lyman alpha emission line (Ly{alpha}), performed with the Hubble Space Telescope, that comprise the backbone of the Lyman alpha Reference Sample. We present images of 14 starburst galaxies at redshifts 0.028 < z < 0.18 in continuum-subtracted Ly{alpha}, H{alpha}, and the far ultraviolet continuum. We show that Ly{alpha} is emitted on scales that systematically exceed those of the massive stellar population and recombination nebulae: as measured by the Petrosian 20% radius, R{sub P20}, Ly{alpha} radii are larger than those of H{alpha} by factors ranging from 1 to 3.6, with an average of 2.4. The average ratio of Ly{alpha}-to-FUV radii is 2.9. This suggests that much of the Ly{alpha} light is pushed to large radii by resonance scattering. Defining the Relative Petrosian Extension of Ly{alpha} compared to H{alpha}, {xi}{sub Ly{alpha}} = R {sup Ly{alpha}}{sub P20}/R {sup H{alpha}}{sub P20}, we find {xi}{sub Ly{alpha}} to be uncorrelated with total Ly{alpha} luminosity. However, {xi}{sub Ly{alpha}} is strongly correlated with quantities that scale with dust content, in the sense that a low dust abundance is a necessary requirement (although not the only one) in order to spread Ly{alpha} photons throughout the interstellar medium and drive a large extended Ly{alpha} halo.

  3. Profiles.

    ERIC Educational Resources Information Center

    Macintosh, Henry G.

    An introduction to profiles is presented with examples provided to permit an overall appraisal of the potential of profiles, of the principles upon which they might be based, and of the problems that will have to be overcome if their potential is to be realized in practice. The larger scale examples of profiles discussed are the Scottish Pupil…

  4. The measurement of O2 number density by absorption of Lyman alpha

    NASA Technical Reports Server (NTRS)

    Smith, L. G.; Miller, K. L.

    1974-01-01

    Measurements of O2 number density obtained from rocket observations of the absorption profile of solar Lyman alpha (1216 A) have been compared with values derived from nearly simultaneous measurements of atmospheric density from other rocket techniques: grenades, falling sphere, and Pitot tube. All launches were from Wallops Island, Virginia. The atmospheric density derived from the absorption spectroscopy data is found to be about 20% less than that from the other techniques when a constant value of the absorption cross section of 1.0 times 10 to the minus 20th sq cm is used. The agreement is worse when the cross section is allowed to vary across the width of the solar line. The data in the altitude range 70-90 km are interpreted as showing that the effective value of the absorption cross section at Lyman alpha for O2 at 200 K and negligible pressure is about 0.8 times 10 to the minus 20th sq cm.

  5. Comparing Local Starbursts to High-Redshift Galaxies: A Search for Lyman-Break Analogs

    NASA Technical Reports Server (NTRS)

    Petty, Sara M.; de Mello, Duila F.; Gallagher III, John S.; Gardner, Jonathan; Lotz, Jennifer M.; Mountain, C. Matt; Smith, Linda J.

    2008-01-01

    We compare the restframe far-ultraviolet (FUV) morphologies of 8 nearby interacting and starburst galaxies (Arp 269, M 82, Mrk 08, NGC 0520, NGC 1068, NGC 3079, NGC 3310, NGC 7673) with 54 galaxies at z approx.1.5 and 46 galaxies at z approx.4 in the Great Observatories Origins Deep Survey (GOODS) images taken with the Advanced Camera for Surveys onboard the Hubble Space Telescope. We calculate the Gini coefficient (G), the second order moment of 20% of the brightest pixels (M20), and the S ersic index (n). We find that 20% (11/54) of z approx.1.5 and 37% (17/46) of z approx.4 galaxies are bulge-like, using G and M20. We also find approx.70% of the z approx.1.5 and z approx.4 galaxies have exponential disks with n > 0.8. The 2D profile combined with the nonparametric methods provides more detail, concerning the nature of disturbed systems, such as merger and post-merger types. We also provide qualitative descriptions of each galaxy system and at each redshift. We conclude that Mrk 08, NGC 3079, and NGC 7673 have similar morphologies as the starburst FUV restframe galaxies and Lyman-break galaxies at z approx.1.5 and 4, and determine that they are Lyman-break analogs.

  6. MEL-N16: A Series of Novel Endomorphin Analogs with Good Analgesic Activity and a Favorable Side Effect Profile.

    PubMed

    Liu, Xin; Zhao, Long; Wang, Yuan; Zhou, Jingjing; Wang, Dan; Zhang, Yixin; Zhang, Xianghui; Wang, Zhaojuan; Yang, Dongxu; Mou, Lingyun; Wang, Rui

    2017-08-10

    Opioid peptides are neuromodulators that bind to opioid receptors and reduce pain sensitivity. Endomorphins are among the most active endogenous opioid peptides, and they have good affinity and selectivity toward the μ opioid receptor. However, their clinical usage is hindered by their inability to cross the blood-brain barrier and their poor in vivo activity after peripheral injection. In order to overcome these defects, we have designed and synthesized a series of novel endomorphin analogs with multiple site modifications. Radioligand binding, cAMP accumulation, and β-arrestin-2 recruitment assays were employed to determine the activity of synthesized endomorphin analogs toward opioid receptors. The blood-brain barrier permeability and antinociceptive effect of these analogs were determined in several rodent models of acute and persistent pain. In addition, the side effects of the analogs were examined. The radioligand binding assay and functional activity examination indicated that the MEL-N16 series of compounds were more active agonists against μ opioid receptor than were the parent peptides. Notably, the analogs displayed biased downstream signaling toward G-protein pathways over β-arrestin-2 recruitment. The analogs showed highly potent antinociceptive effects in the tested nociceptive models. In comparison with endomorphins, the synthesized analogs were better able to penetrate the blood-brain barrier and exerted their pain regulatory activity in the central nervous system after peripheral injection. These analogs also have lower tendency to cause side effects than morphine does at similar or equal antinociceptive doses. The MEL-N16 compounds have highly potent and efficacious analgesic effects in various pain models with a favorable side effect profile.

  7. Joint Lyman α emitters - quasars reionization constraints

    NASA Astrophysics Data System (ADS)

    Baek, S.; Ferrara, A.; Semelin, B.

    2012-06-01

    We present a novel method to investigate c reionization, using joint spectral information on high-redshift Lyman α emitters (LAEs) and quasi-stellar objects (QSOs). Although LAEs have been proposed as reionization probes, their use is hampered by the fact their Lyα line is damped not only by intergalactic H I but also internally by dust. Our method allows us to overcome such degeneracy. First, we carefully calibrate a reionization simulation with QSO absorption line experiments. Then we identify LAEs (? and equivalent width >20 Å) in two simulation boxes at z= 5.7 and 6.6 and we build synthetic images/spectra of a prototypical LAE. The surface brightness maps show the presence of a scattering halo extending up to 150 kpc from the galaxye. For each LAE we then select a small box of (10 h-1 Mpc)3 around it and derive the optical depth τ along three viewing axes. At redshift 5.7, we find that the Lyα transmissivity ?, almost independent of the halo mass. This constancy arises from the conspiracy of two effects: (i) the intrinsic Lyα line width and (ii) the infall peculiar velocity. At higher redshift, z= 6.6, where ? the transmissivity is instead largely set by the local H I abundance and ? consequently increases with halo mass, Mh, from 0.15 to 0.3. Although outflows are present, they are efficiently pressure confined by infall in a small region around the LAE; hence they only marginally affect transmissivity. Finally, we cast line of sight originating from background QSOs passing through foreground LAEs at different impact parameters, and compute the quasar transmissivity (?). At small impact parameters, d < 1 cMpc, a positive correlation between ? and Mh is found at z= 5.7, which tends to become less pronounced (i.e. flatter) at larger distances. Quantitatively, a roughly 10× increase (from 5 × 10-3 to 6 × 10-2) of ? is observed in the range log Mh= (10.4-11.6). This correlation becomes even stronger at z= 6.6. By cross-correlating ? and ?, we can obtain a

  8. Enhanced direct collapse due to Lyman α feedback

    NASA Astrophysics Data System (ADS)

    Johnson, Jarrett L.; Dijkstra, Mark

    2017-05-01

    We assess the impact of trapped Lyman α cooling radiation on the formation of direct collapse black holes (DCBHs). We apply a one-zone chemical and thermal evolution model, accounting for the photodetachment of H- ions, precursors to the key coolant H2, by Lyman α photons produced during the collapse of a cloud of primordial gas in an atomic cooling halo at high redshift. We find that photodetachment of H- by trapped Lyman α photons may lower the level of the H2-dissociating background radiation field required for DCBH formation substantially, dropping the critical flux by up to a factor of a few. This translates into a potentially large increase in the expected number density of DCBHs in the early Universe, and supports the view that DCBHs may be the seeds for the BHs residing in the centers of a significant fraction of galaxies today. We find that detachment of H- by Lyman α has the strongest impact on the critical flux for the relatively high background radiation temperatures expected to characterize the emission from young, hot stars in the early Universe. This lends support to the DCBH origin of the highest redshift quasars.

  9. Fiscal Profiles, 2006: "The Fourteenth in a Periodic Series of Factsheets about the Financing of California Higher Education." California Postsecondary Education Commission Report 06-13

    ERIC Educational Resources Information Center

    California Postsecondary Education Commission, 2006

    2006-01-01

    Fiscal Profiles, 2006 is the fourteenth in a series of periodic reports by the California Postsecondary Education Commission of statistical information on the financing of the State's public higher education institutions. It also includes selected financial and enrollment information on public elementary and secondary education and on California's…

  10. Profiles.

    ERIC Educational Resources Information Center

    School Arts, 1979

    1979-01-01

    Profiles seven Black, Native American, and Chicano artists and art teachers: Hale A. Woodruff, Allan Houser, Luis Jimenez, Betrand D. Phillips, James E. Pate, I, and Fernando Navarro. This article is part of a theme issue on multicultural art. (SJL)

  11. Profiles.

    ERIC Educational Resources Information Center

    School Arts, 1979

    1979-01-01

    Profiles seven Black, Native American, and Chicano artists and art teachers: Hale A. Woodruff, Allan Houser, Luis Jimenez, Betrand D. Phillips, James E. Pate, I, and Fernando Navarro. This article is part of a theme issue on multicultural art. (SJL)

  12. Damped Lyman-α Absorbers bias: measurement and evolution

    NASA Astrophysics Data System (ADS)

    Pérez-Rafòls, I.; Miralda-Escudé, J.; Font-Ribera, A.

    2017-03-01

    We present an update on the measurement of the Damped Lyman-α Absorbers (DLAs) bias from the cross-correlation of DLA and the Lyman-α forest. We also use an upgraded method to deal with the broadband function problems. In our analysis, we use of the final Data Release of BOSS. We find the bias of the DLA to be b_d = 1.90 plusmn;0.11. With the improved statistics, we explore the evolution of the DLA bias with column density and redshift. We find no clear evidence of any evolution in neither of them. This means that the dark matter halos hosting the DLA are essentially the same independently of the properties of the DLA.

  13. Lyman Continuum Emission Search at z 1 Using GALEX Imaging

    NASA Astrophysics Data System (ADS)

    Friedman, Peter G.; Small, T. A.; Deharveng, J. M.; Milliard, B.

    2007-12-01

    We present the status and results of a search for Lyman continuum emission from galaxies at z 1. We use GALEX data in the Extended Groth Strip. Our method is to stack FUV image flux at locations of DEEP2 redshift catalog galaxies in the redshift range 1 < z < 1.5. In this range, the GALEX FUV band (1350-1800 A) is sensitive only to rest wavelengths below 912 A. We normalize FUV flux to NUV flux and calculate the Lyman continuum emission escape fraction by fitting SED models to broad-band fluxes from ground-based surveys of the same galaxies. GALEX is a NASA Small Explorer mission with contributions from France and South Korea. This work uses data from the AEGIS collaboration, which is supported by grants from the National Science Foundation, NASA, and the Keck Observatory.

  14. GALEX Imaging Search for Lyman Continuum Emission at z 1

    NASA Astrophysics Data System (ADS)

    Friedman, Peter G.; Small, T. A.; Deharveng, J. M.; Milliard, B.

    2009-01-01

    We present the status and results of a search for Lyman continuum emission from galaxies at z 1. We use GALEX data in the Extended Groth Strip. Our method is to stack FUV image flux at locations of DEEP2 redshift catalog galaxies in the redshift range 1 < z < 1.5. In this range, the GALEX FUV band (1350-1800 A) is sensitive only to rest wavelengths below 912 A. We normalize FUV flux to NUV flux and calculate the Lyman continuum emission escape fraction by fitting SED models to broad-band fluxes from ground-based surveys of the same galaxies. GALEX is a NASA Small Explorer mission with contributions from France and South Korea. This work uses data from the AEGIS collaboration, which is supported by grants from the National Science Foundation, NASA, and the Keck Observatory.

  15. GALEX Imaging Search for Lyman Continuum Emission at z 1

    NASA Astrophysics Data System (ADS)

    Friedman, Peter G.; Small, T. A.; Deharveng, J. M.; Milliard, B.

    2010-01-01

    We present the status and results of a search for Lyman continuum emission from galaxies at z 1. We use GALEX data in the Extended Groth Strip. Our method is to stack FUV image flux at locations of DEEP2 redshift catalog galaxies in the redshift range 1 < z < 1.5. In this range, the GALEX FUV band (1350-1800 A) is sensitive only to rest wavelengths below 912 A. We normalize FUV flux to NUV flux and calculate the Lyman continuum emission escape fraction by fitting SED models to broad-band fluxes from ground-based surveys of the same galaxies. GALEX is a NASA Small Explorer mission with contributions from France and South Korea. This work uses data from the AEGIS collaboration, which is supported by grants from the National Science Foundation, NASA, and the Keck Observatory.

  16. The First IRS Spectrum of a Lyman Break Galaxy

    NASA Astrophysics Data System (ADS)

    Siana, Brian; Colbert, James; Frayer, David; Teplitz, Harry

    2006-05-01

    A significant portion of the star-formation in the high redshift universe resides in the ultraviolet-luminous Lyman Break Galaxies (LBGs). Although they are UV bright, the bulk of their luminosities are emitted in the far-infrared (FIR). Unlike the population of luminous infrared galaxies (LIRGs and ULIRGs), LBGs are typically too faint in the MIR to for Spitzer spectroscopy. We propose deep IRS spectroscopy of the lensed Lyman-Break Galaxy (LBG) MS1512-cB58. The factor of ~30 magnification provides the only opportunity to obtain a MIR spectrum of a typical (L*) LBG. We will measure the strength of the PAH features, allowing a comparison with Lbol as measured from longer wavelength photometry. We will also fit the shape of the warm dust (VSG) continuum and compare it to expectations from the IRAC-to-MIPS70 SED.

  17. New interpretations of extraterrestrial Lyman-alpha observations.

    NASA Technical Reports Server (NTRS)

    Blum, P. W.; Fahr, H. J.

    1972-01-01

    The solar Lyman-alpha radiation pressure affects the orbits and the velocities of the interstellar particles entering the solar system. This leads to enhanced particle losses in the heliosphere, since particles spend a longer time crossing it. This causes a stronger decrease of the density with decreasing distances from the sun than had been calculated without accounting for the radiation pressure. Furthermore, the emission pattern of the solar Lyman-alpha radiation is anisotropic and rotates with the sun in a 27-day period. This causes a temporal change in the location of the intensity extrema. At the same time it produces hydrogen density anisotropies with extrema deviating in their directions from those which had been calculated without consideration of the radiation pressure.

  18. Lyman alpha initiated winds in late-type stars

    NASA Technical Reports Server (NTRS)

    Haisch, B. M.; Linsky, J. L.; Vanderhucht, K. A.

    1979-01-01

    The IUE survey of late-type stars revealed a sharp division in the HR diagram between stars with solar type spectra (chromosphere and transition region lines) and those with non-solar type spectra (only chromosphere lines). Models of both hot coronae and cool wind flows were calculated using stellar model chromospheres as starting points for stellar wind calculations in order to investigate the possibility of having a supersonic transition locus in the HR diagram dividing hot coronae from cool winds. From these models, it is concluded that the Lyman alpha flux may play an important role in determining the location of a stellar wind critical point. The interaction of Lyman alpha radiation pressure with Alfven waves in producing strong, low temperature stellar winds in the star Arcturus is examined.

  19. Lyman-alpha observations of Comet West /1975n/

    NASA Technical Reports Server (NTRS)

    Opal, C. B.; Carruthers, G. R.

    1977-01-01

    The rate of hydrogen production of Comet West is studied through rocket observation of solar Lyman-alpha radiation resonantly scattered by the escaping hydrogen atoms. Two sets of Lyman-alpha exposure sequences are used to obtain computer-smoothed brightness contour (isophote) maps covering a density range of 100:1. A simple radial outflow model is applied to the contour maps to determine the rate of hydrogen production (3.2 by 10 to the 30th power atoms/sec.) Discrepancies between the observed shape of the outer isophotes and predicted models may be explained by optical depth effects, or by the presence of small pieces of the comet's nucleus distributed along the orbit. Hydrogen, carbon, and oxygen production for Comet West and Comet Kohoutek are compared; differences may be accounted for by variations in the composition or evolution of the two comets.

  20. Bio-optical profile data report: Joint Global Ocean Flux Study, Hawaii Ocean Time-Series, HOT-3, R/V Moana Wave, 6-10 January 1989

    NASA Technical Reports Server (NTRS)

    Collins, Donald J.; Rhea, W. Joseph; Tran, An Van

    1990-01-01

    Time-series measurements of the incident surface downwelling irradiance and vertical profiles of the Bio-optical properties of the ocean have been measured during the third cruise of the Hawaii Ocean Time-Series to the ALOHA site, 22 degrees 56.4 minutes N, 157 degrees 54.6 minutes W, north of the island of Oahu, Hawaii, during the period January 6 to 10, 1989. A summary of these data is presented to permit investigators an overview of the data collected. The data are available in digital form for scientific investigators.

  1. Broadband distortion modeling in Lyman-α forest BAO fitting

    NASA Astrophysics Data System (ADS)

    Blomqvist, Michael; Kirkby, David; Bautista, Julian E.; Arinyo-i-Prats, Andreu; Busca, Nicolás G.; Miralda-Escudé, Jordi; Slosar, Anže; Font-Ribera, Andreu; Margala, Daniel; Schneider, Donald P.; Vazquez, Jose A.

    2015-11-01

    In recent years, the Lyman-α absorption observed in the spectra of high-redshift quasars has been used as a tracer of large-scale structure by means of the three-dimensional Lyman-α forest auto-correlation function at redshift zsimeq 2.3, but the need to fit the quasar continuum in every absorption spectrum introduces a broadband distortion that is difficult to correct and causes a systematic error for measuring any broadband properties. We describe a k-space model for this broadband distortion based on a multiplicative correction to the power spectrum of the transmitted flux fraction that suppresses power on scales corresponding to the typical length of a Lyman-α forest spectrum. Implementing the distortion model in fits for the baryon acoustic oscillation (BAO) peak position in the Lyman-α forest auto-correlation, we find that the fitting method recovers the input values of the linear bias parameter bF and the redshift-space distortion parameter βF for mock data sets with a systematic error of less than 0.5%. Applied to the auto-correlation measured for BOSS Data Release 11, our method improves on the previous treatment of broadband distortions in BAO fitting by providing a better fit to the data using fewer parameters and reducing the statistical errors on βF and the combination bF(1+βF) by more than a factor of seven. The measured values at redshift z=2.3 are βF=1.39+0.11 +0.24 +0.38-0.10 -0.19 -0.28 and bF(1+βF)=-0.374+0.007 +0.013 +0.020-0.007 -0.014 -0.022 (1σ, 2σ and 3σ statistical errors). Our fitting software and the input files needed to reproduce our main results are publicly available.

  2. Computer assisted performance tests of the Lyman Alpha Coronagraph

    NASA Technical Reports Server (NTRS)

    Parkinson, W. H.; Kohl, J. L.

    1979-01-01

    Preflight calibration and performance tests of the Lyman Alpha Coronagraph rocket instrument in the laboratory, with the experiment in its flight configuration and illumination levels near those expected during flight were successfully carried out using a pulse code modulation telemetry system simulator interfaced in real time to a PDP 11/10 computer system. Post acquisition data reduction programs developed and implemented on the same computer system aided in the interpretation of test and calibration data.

  3. The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP)

    NASA Technical Reports Server (NTRS)

    Ishikawa, Shin-nosuke; Kano, R.; Kobayashi, K.; Bando, T.; Narukage, N..; Ishikawa, R.; Kubo, M.; Katsukawa, Y.; Suematsu, Y.; Hara, H.; hide

    2014-01-01

    To Understand energy release process in the Sun including solar flares, it is essentially important to measure the magnetic field of the atmosphere of the Sun. Magnetic field measurement of the upper layers (upper chromosphere and above) was technically difficult and not well investigated yet. Upper chromosphere and transition region magnetic field measurement by Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) sounding rocket to be launched in 2015. The proposal is already selected and developments of the flight components are going.

  4. Photoelectron Emission and Lyman Alpha Measurements by the CHAMPS Rockets

    NASA Astrophysics Data System (ADS)

    Sternovsky, Z.; Robertson, S. H.; Dickson, S.; Gausa, M. A.; Friedrich, M.; Horanyi, M.

    2012-12-01

    The daytime CHAMPS (CHarge And mass of Meteoritic smoke ParticleS) sounding rocket carried a suit of instruments for the monitoring of photoemission current and Lyman alpha flux as a function of altitude. The results show that photoemission is significant down to 60-75 km altitude, depending on the photo-emitting surface. Lyman alpha was detected to about 65 km altitude. The daytime CHAMPS rocket launched on 13 October 13:50 UT from the Andøya Rocket Range, Norway. The CHAMPS instruments detected layers of particles, probably of meteoric origin, charged both positive and negative in the 63-93 km altitude range. The CHAMPS payloads were also designed to characterize the plasma environment and thus also carried Faraday rotation antennas and electron and ion probes. Solar UV plays an important role in charge balance for both the rocket body and meteoric smoke particles. Photoelectron emission was monitored by a set of three detectors consisting of an emitting surface (Platinum, Aluminum and Zirconium) biased at -10 V and placed behind a fine grid. The Al and Zr surfaces produced similar signals with photoemission measureable above 75 km altitude. The Pt surface emitted photoelectrons even below 60 km altitude. The different behavior of Pt can possibly be due to exposure to atomic oxygen, though further analysis is necessary. The solar Lyman alpha radiation was measured by a UV photodiode placed behind a pair or filters to reduce the contribution to the signal from visible light. Lyman alpha was detected down to 65 km altitude, which confirms that photo-detachment and photoelectric charging needs to be considered for the charge balance of particle layers in the mesosphere region. All instruments were calibrated at the facilities of the Laboratory for Atmospheric and Space Physics at the University of Colorado.

  5. Observation of Lyman-alpha emission in interplanetary space

    NASA Technical Reports Server (NTRS)

    Bertaux, J. L.; Blamont, J. E.

    1972-01-01

    The extraterrestrial Lyman-alpha emission was mapped by the OGO 5 satellite, when it was outside the geocorona. Three maps, obtained at different periods of the year, are presented and analyzed. The results suggest that at least half of the emission takes place in the solar system, and give strong support to the theory that in its motion toward the apex, the sun crosses neutral atomic hydrogen of interstellar origin, giving rise to an apparent interstellar wind.

  6. A LYMAN BREAK GALAXY IN THE EPOCH OF REIONIZATION FROM HUBBLE SPACE TELESCOPE GRISM SPECTROSCOPY

    SciTech Connect

    Rhoads, James E.; Malhotra, Sangeeta; Cohen, Seth; Zheng Zhenya; Stern, Daniel; Dickinson, Mark; Pirzkal, Norbert; Grogin, Norman; Koekemoer, Anton; Peth, Michael A.; Spinrad, Hyron; Reddy, Naveen; Hathi, Nimish; Budavari, Tamas; Ferreras, Ignacio; Gardner, Jonathan P.; Gronwall, Caryl; Haiman, Zoltan; Kuemmel, Martin; Meurer, Gerhardt; and others

    2013-08-10

    We present observations of a luminous galaxy at z = 6.573-the end of the reionization epoch-which has been spectroscopically confirmed twice. The first spectroscopic confirmation comes from slitless Hubble Space Telescope Advanced Camera for Surveys grism spectra from the PEARS survey (Probing Evolution And Reionization Spectroscopically), which show a dramatic continuum break in the spectrum at rest frame 1216 A. The second confirmation is done with Keck + DEIMOS. The continuum is not clearly detected with ground-based spectra, but high wavelength resolution enables the Ly{alpha} emission line profile to be determined. We compare the line profile to composite line profiles at z = 4.5. The Ly{alpha} line profile shows no signature of a damping wing attenuation, confirming that the intergalactic gas is ionized at z = 6.57. Spectra of Lyman breaks at yet higher redshifts will be possible using comparably deep observations with IR-sensitive grisms, even at redshifts where Ly{alpha} is too attenuated by the neutral intergalactic medium to be detectable using traditional spectroscopy from the ground.

  7. Making damped Lyman-α systems in semi-analytic models

    NASA Astrophysics Data System (ADS)

    Maller, Ariyeh H.; Somerville, Rachel S.; Prochaska, Jason X.; Primack, Joel R.

    1999-04-01

    The velocity profiles of weak metal absorption lines can be used to observationally probe the kinematic state of gas in damped Lyman-α systems. Prochaska and Wolfe [5] have argued that the flat distribution of velocity widths (Δv) combined with the asymmetric line profiles indicate that the DLAS are disks with large rotation velocities (~200 km/s). An alternative explanation has been proposed by Haehnelt, Steinmetz, and Rauch (HSR) [2], in which the observed large velocity widths and asymmetric profiles can be produced by lines of sight passing through two or more clumps each having relatively small internal velocity dispersions. We investigate the plausibility of this scenario in the context of semi-analytic models based on hierarchical merging trees and including simple treatments of gas dynamics, star formation, supernova feedback, and chemical evolution. We find that all the observed properties of the metal-line systems including the distribution of Δv and the asymmetric profiles, can be reproduced by lines of sight passing through sub-clumps that are bound within larger virialized dark matter halos. In order to produce enough multiple hits, we find that the cold gas must be considerably more extended than the optical radius of the proto-galaxies, perhaps even beyond the tidal radius of the sub-halo. This could occur due to tidal stripping or supernova-driven outflows.

  8. Dynamical and Stellar Masses of Lyman-alpha Galaxies

    NASA Astrophysics Data System (ADS)

    Rhoads, James E.; Malhotra, S.; McLinden, E.; Richardson, M. L.; Finkelstein, S. L.; Tilvi, V. S.

    2012-01-01

    We have observed strong nebular lines of [OIII] and H alpha for Lyman-alpha galaxies at z=2-3.1 using Keck+NIRSPEC, LBT+LUCIFER, and Gemini+NIFS. [OIII] 5007 is strong enough to dominate the 2 micron K band fluxes of these galaxies, and leads to an overestimate of the stellar mass of the galaxy by an order of magnitude. After correcting for the observed [OIII] lines, we infer low masses and young ages for these galaxies. We also use the physical widths of the rest-optical lines, combined with spatial sizes from HST imaging, to obtain direct dynamical mass estimates of Lyman alpha galaxies (which cannot be done using the resonantly scattered Lyman alpha line). Finally, we combine our stellar mass estimates and line widths to place these galaxies on the baryonic Tully-Fisher relation. We find that the stellar masses required to reproduce the observed light are lower than one would expect based on the galaxies' line widths. The stellar mass densities of these galaxies are comparable to those of elliptical galaxies today. We gratefully acknowledge support from NSF grant NSF-AST-0808165.

  9. The Lyman-alpha Imager onboard Solar Polar Orbit Telescope

    NASA Astrophysics Data System (ADS)

    Li, Baoquan; Li, Haitao; Zhou, Sizhong; Jiang, Bo

    2013-12-01

    Solar Polar ORbit Telescope (SPORT) was originally proposed in 2004 by the National Space Science Center, Chinese Academy of Sciences, which is currently being under background engineering study phase in China. SPORT will carry a suite of remote-sensing and in-situ instruments to observe coronal mass ejections (CMEs), solar high-latitude magnetism, and the fast solar wind from a polar orbit around the Sun. The Lyman-alpha Imager (LMI) is one of the key remotesensing instruments onboard SPORT with 45arcmin FOV, 2000mm effective focal length and 1.4arcsec/pixel spatial resolution . The size of LMI is φ150×1000mm, and the weight is less than10kg, including the 7kg telescope tube and 3kg electronic box. There are three 121.6nm filters used in the LMI optical path, so the 98% spectral purity image of 121.6nm can be achieved. The 121.6nm solar Lyman-alpha line is produced in the chromosphere and very sensitive to plasma temperature, plasma velocity and magnetism variation in the chromosphere. Solar Lyman-alpha disk image is an ideal tracker for corona magnetism variation.

  10. Analysis of solar Lyman alpha radiation in the heliosphere

    NASA Astrophysics Data System (ADS)

    Fayock, B.; Zank, G. P.; Heerikhuisen, J.

    2013-06-01

    Various NASA spacecraft have measured ultraviolet radiation in the heliosphere at different locations over time. Much of this data corresponds to back-scattered Lyman-alpha radiation from neutral hydrogen, particularly in the context of planetary atmospheric measurements and inferred solar activity. Less attention has been devoted to using this data in the context of large-scale heliospheric simulations with complex global models. A 3D Monte Carlo simulation has been developed for analysis of Lyman-alpha scattering using global heliospheric models developed within CSPAR as a background. The simulation tracks individual photons in a sun-centered spherical coordinate system with a radial limit of 1000 AU while retaining statistics for each cell within the grid space, which is defined by the global input data. Two of the statistics collected are the number of scatters and the total distance traveled by photons within a cell. Those photons directed towards the sun provide a measure of backscatter intensity that can be compared to antisolar observations of Lyman-alpha photons by spacecraft. Preliminary results reveal a similar trend of intensity between simulation in the upwind direction and reduced Voyager data, suggesting an accurate portrayal of neutral hydrogen in the heliosphere.

  11. 100 Most Popular Business Leaders for Young Adults: Biographical Sketches and Professional Paths. Profiles and Pathways Series.

    ERIC Educational Resources Information Center

    Logan, Rochelle; Halverstadt, Julie

    This book, which is intended as a reference for teenagers and educators, profiles the lives and professional paths of the 100 most popular business leaders for young adults. Those profiled were selected for a number of reasons, including the following: their names are recognizable; they are associated with businesses and industries that are…

  12. 100 Most Popular Business Leaders for Young Adults: Biographical Sketches and Professional Paths. Profiles and Pathways Series.

    ERIC Educational Resources Information Center

    Logan, Rochelle; Halverstadt, Julie

    This book, which is intended as a reference for teenagers and educators, profiles the lives and professional paths of the 100 most popular business leaders for young adults. Those profiled were selected for a number of reasons, including the following: their names are recognizable; they are associated with businesses and industries that are…

  13. School Renewal and Non-Instructional Time for Teachers: Profiles From the National Network for Educational Renewal. Professional Practice Series.

    ERIC Educational Resources Information Center

    Vaughns, A. J.

    This paper provides a basic description of the methods used to make available non-instructional time and presents profiles of seven schools in the Network for Educational Renewal (NER). Each profile describes the school's unique background, approach to providing non-instructional time for teachers, and lessons learned. Some strategies identified…

  14. The Lyman alpha forest of the high-z quasar 0000-263

    NASA Technical Reports Server (NTRS)

    Penprase, Bryan; Gilmozzi, Roberto; Bowen, David; Madau, Piero

    1993-01-01

    Medium-resolution (delta(v) = 45 km/s) optical spectra of the bright, high-redshift (z = 4.1) quasar 0000-263 taken at the ESO 3.5-m NTT telescope were analyzed to determine the distribution of column densities, velocities and line widths of the Lyman-alpha forest absorption components. The values of NH, b, and z were determined by fitting Voigt profiles to the lines, and convolving with a Gaussian instrumental response function. Over 350 components with log N(sub H) greater than 13.2 were identified. An analysis of the dependence of the number of components with z reveals that the number evolution of components obeys the power law dN/dz varies as (1+z)(sup gamma), where gamma = 0.5 +/- 0.4 for the sample of 182 lines with log N(sub H) greater than 14.0. The distribution of component strengths is found to obey f(N(sub H)) varies as N(sub h)(sup -beta), where beta = -1.55 for components with log(N(sub H)) is greater than 14.7, and beta = -0.68 for the components with log(N(sub H)) greater than 13.5. A distinct break in the f(N(sub H)) histogram is also observed, at log(N(sub H)) is approximately 14.7. The results are briefly considered in the context of theoretical models of quasar Lyman alpha clouds and their evolution.

  15. The first detection of [OIII] emission from high-redshift damped Lyman-α galaxies

    NASA Astrophysics Data System (ADS)

    Weatherley, S. J.; Warren, S. J.; Møller, P.; Fall, S. M.; Fynbo, J. U.; Croom, S. M.

    2005-04-01

    We present the detection of [OIII] emission lines from the galaxies responsible for two high-redshift z > 1.75 damped Lyman-α (DLA) absorption lines. We find two sources of [OIII] emission corresponding to the z= 1.92 DLA absorber towards the quasar Q2206-1958, and we also detect [OIII] emission from the galaxy responsible for the z= 3.10 DLA absorber towards the quasar 2233.9+1381. These are the first detections of rest-frame optical emission lines from high-redshift DLA galaxies. Unlike the Lyα line, the [OIII] line provides a measure of the systemic velocity of the galaxy. We compare the [OIII] redshifts with the velocity profile of the low-ionization metal lines in these two absorbers, with the goal of distinguishing between the model of Prochaska and Wolfe of DLA absorbers as large rapidly rotating cold thick discs, and the standard hierarchical cold dark matter model of structure formation, in which DLAs arise in protogalactic fragments. We find some discrepancies with the predictions of the former model. Furthermore, the image of the DLA galaxy towards Q2206-1958 shows a complex disturbed morphology, which is more in accord with the hierarchical picture. We use the properties of the rest-frame optical emission lines to further explore the question posed by Møller et al.: are high-redshift DLA galaxies Lyman-break galaxies (LBGs) selected by gas cross-section? The measured velocity dispersions of the DLA galaxies are in agreement with this picture, while the data on the [OIII] luminosities and the velocity differences between the Lyα and [OIII] lines are inconclusive, as there are insufficient LBG measurements overlapping in luminosity. Finally, we estimate the star formation rates in these two DLA galaxies, using a variety of diagnostics, and include a discussion of the extent to which the [OIII] line is useful for this purpose.

  16. Time series analysis of ground-based microwave measurements at K- and V-bands to detect temporal changes in water vapor and temperature profiles

    NASA Astrophysics Data System (ADS)

    Panda, Sibananda; Sahoo, Swaroop; Pandithurai, Govindan

    2017-01-01

    Ground-based microwave measurements performed at water vapor and oxygen absorption line frequencies are widely used for remote sensing of tropospheric water vapor density and temperature profiles, respectively. Recent work has shown that Bayesian optimal estimation can be used for improving accuracy of radiometer retrieved water vapor and temperature profiles. This paper focuses on using Bayesian optimal estimation along with time series of independent frequency measurements at K- and V-bands. The measurements are used along with statistically significant but short background data sets to retrieve and sense temporal variations and gradients in water vapor and temperature profiles. To study this capability, the Indian Institute of Tropical Meteorology (IITM) deployed a microwave radiometer at Mahabubnagar, Telangana, during August 2011 as part of the Integrated Ground Campaign during the Cloud Aerosol Interaction and Precipitation Enhancement Experiment (CAIPEEX-IGOC). In this study, temperature profiles for the first time have been estimated using short but statistically significant background information so as to improve the accuracy of the retrieved profiles as well as to be able to detect gradients. Estimated water vapor and temperature profiles are compared with those taken from the reanalysis data updated by the Earth System Research Laboratory, National Oceanic and Atmospheric Administration (NOAA), to determine the range of possible errors. Similarly, root mean square errors are evaluated for a month for water vapor and temperature profiles to estimate the accuracy of the retrievals. It is found that water vapor and temperature profiles can be estimated with an acceptable accuracy by using a background information data set compiled over a period of 1 month.

  17. Lyman alpha radiation in external galaxies

    NASA Technical Reports Server (NTRS)

    Neufeld, David A.; Mckee, Christopher F.

    1990-01-01

    The Ly alpha line of atomic hydrogen is often a luminous component of the radiation emitted by distant galaxies. Except for those galaxies which have a substantial central source of non-stellar ionizing radiation, most of the Ly alpha radiation emitted by galaxies is generated within regions of the interstellar medium which are photoionized by starlight. Conversely, much of the energy radiated by photoionized regions is carried by the Ly alpha line. Only hot, massive stars are capable of ionizing hydrogen in the interstellar medium which surrounds them, and because such stars are necessarily short-lived, Ly alpha emission traces regions of active star formation. Researchers argue that the strength of the Ly alpha emission observed from external galaxies may be used to estimate quantitatively the dust content of the emitting region, while the Ly alpha line profile is sensitive to the presence of shock waves. Interstellar dust particles and shock waves are intimately associated with the process of star formation in two senses. First, both dust particles and shock waves owe their existence to stellar activity; second, they may both serve as agents which facilitate the formation of stars, shocks by triggering gravitational instabilities in the interstellar gas that they compress, and dust by shielding star-forming molecular clouds from the ionizing and dissociative effects of external UV radiation. By using Ly alpha observations as a probe of the dust content in diffuse gas at high redshift, we might hope to learn about the earliest epochs of star formation.

  18. Measurement of precipitation induced FUV emission and Geocoronal Lyman Alpha from the IMI mission

    NASA Technical Reports Server (NTRS)

    Mende, Stephen B.; Fuselier, S. A.; Rairden, R. L.

    1995-01-01

    This final report describes the activities of the Lockheed Martin Palo Alto Research Laboratory in studying the measurement of ion and electron precipitation induced Far Ultra-Violet (FUV) emissions and Geocoronal Lyman Alpha for the NASA Inner Magnetospheric Imager (IMI) mission. this study examined promising techniques that may allow combining several FUV instruments that would separately measure proton aurora, electron aurora, and geocoronal Lyman alpha into a single instrument operated on a spinning spacecraft. The study consisted of two parts. First, the geocoronal Lyman alpha, proton aurora, and electron aurora emissions were modeled to determine instrument requirements. Second, several promising techniques were investigated to determine if they were suitable for use in an IMI-type mission. Among the techniques investigated were the Hydrogen gas cell for eliminating cold geocoronal Lyman alpha emissions, and a coded aperture spectrometer with sufficient resolution to separate Doppler shifted Lyman alpha components.

  19. The Lyman β forest as a cosmic thermometer

    SciTech Connect

    Iršič, Vid; Viel, Matteo E-mail: viel@oats.inaf.it

    2014-12-01

    We present a comprehensive analysis of high resolution hydrodynamic simulations in terms of Lyman α and Lyman β one dimensional flux power spectra P{sub αα} and P{sub ββ}). In particular, we focus on the behaviour that the flux auto-power spectra and cross-power spectra P{sub αβ}) display when the intergalactic medium (IGM) thermal history is changed in a range of values that bracket a reference model, while cosmological parameters are kept fixed to best fit the cosmic microwave background data. We present empirical fits that describe at the sub-percent level the dependence of the power spectra on the thermal parameters. At the largest scales, the power spectra show a constant bias between each other that is set by the parameters describing the IGM thermal state. The cross-power spectrum has an oscillatory pattern and crosses zero at a scale which depends on T{sub 0}, the IGM temperature at the mean density, for reasonable values of the power-law index γ of the IGM temperature-density relation T=T{sub 0}(1+δ){sup γ-1}). By performing a Fisher matrix analysis, we find that the power spectrum P{sub ββ} is more sensitive to the thermal history than P{sub αα} alone, due to the fact that it probes denser regions than Lyman α. When we combine the power and cross spectra the constraints on γ can be improved by a factor ∼ 4, while the constraints on T{sub 0} improve by a factor of ∼ 2. We address the role of signal-to-noise and resolution by mocking realistic observations and we conclude that the framework presented in this work can significantly improve the knowledge of the IGM thermal state, which will in turn guarantee better constraints on IGM-derived cosmological parameters.

  20. The Lyman alpha reference sample. VI. Lyman alpha escape from the edge-on disk galaxy Mrk 1486

    NASA Astrophysics Data System (ADS)

    Duval, Florent; Östlin, Göran; Hayes, Matthew; Zackrisson, Erik; Verhamme, Anne; Orlitova, Ivana; Adamo, Angela; Guaita, Lucia; Melinder, Jens; Cannon, John M.; Laursen, Peter; Rivera-Thorsen, Thoger; Herenz, E. Christian; Gruyters, Pieter; Mas-Hesse, J. Miguel; Kunth, Daniel; Sandberg, Andreas; Schaerer, Daniel; Månsson, Tore

    2016-03-01

    Context. Recent numerical simulations suggest that the strength of the Lyman alpha (Lyα) line of star-forming disk galaxies strongly depends on the inclination at which they are observed: from edge-on to face-on, we expect to see a change from a strongly attenuated Lyα line to a strong Lyα emission line. Aims: We aim to understand how a strong Lyα emission line is able to escape from the low-redshift highly inclined (edge-on) disk galaxy Mrk 1486 (z ~ 0.0338). To our knowledge, this work is the first observational study of Lyα transport inside an edge-on disk galaxy. Methods: Using a large set of HST imaging and spectroscopic data, we investigated the interstellar medium (ISM) structure and the dominant source of Lyα radiation inside Mrk 1486. Moreover, using a 3D Monte Carlo Lyα radiation transfer code, we studied the radiative transfer of Lyα and UV continuum photons inside a 3D geometry of neutral hydrogen (HI) and dust that models the ISM structure at the galaxy center. Our numerical simulations predicted the Lyα line profile that we then compared to the one observed in the HST/COS spectrum of Mrk 1486. Results: While a pronounced Lyα absorption line emerges from the disk of Mrk 1486, very extended Lyα structures are observed at large radii from the galaxy center: a large Lyα-halo and two very bright Lyα regions located slightly above and below the disk plane. The analysis of IFU Hα spectroscopic data of Mrk 1486 indicates the presence of two bipolar outflowing halos of HI gas at the same location as these two bright Lyα regions. Comparing different diagnostic diagrams (such as [OIII]5007/Hβ versus [OI]6300/Hα) to photo- and shock-ionization models, we find that the Lyα production of Mrk 1486 is dominated by photoionization inside the galaxy disk. From this perspective, our numerical simulations succeed in reproducing the strength and shape of the observed Lyα emission line of Mrk 1486 by assuming a scenario in which the Lyα photons are

  1. Broadband distortion modeling in Lyman-α forest BAO fitting

    SciTech Connect

    Blomqvist, Michael; Kirkby, David; Margala, Daniel E-mail: dkirkby@uci.edu; and others

    2015-11-01

    In recent years, the Lyman-α absorption observed in the spectra of high-redshift quasars has been used as a tracer of large-scale structure by means of the three-dimensional Lyman-α forest auto-correlation function at redshift z≅ 2.3, but the need to fit the quasar continuum in every absorption spectrum introduces a broadband distortion that is difficult to correct and causes a systematic error for measuring any broadband properties. We describe a k-space model for this broadband distortion based on a multiplicative correction to the power spectrum of the transmitted flux fraction that suppresses power on scales corresponding to the typical length of a Lyman-α forest spectrum. Implementing the distortion model in fits for the baryon acoustic oscillation (BAO) peak position in the Lyman-α forest auto-correlation, we find that the fitting method recovers the input values of the linear bias parameter b{sub F} and the redshift-space distortion parameter β{sub F} for mock data sets with a systematic error of less than 0.5%. Applied to the auto-correlation measured for BOSS Data Release 11, our method improves on the previous treatment of broadband distortions in BAO fitting by providing a better fit to the data using fewer parameters and reducing the statistical errors on β{sub F} and the combination b{sub F}(1+β{sub F}) by more than a factor of seven. The measured values at redshift z=2.3 are β{sub F}=1.39{sup +0.11 +0.24 +0.38}{sub −0.10 −0.19 −0.28} and b{sub F}(1+β{sub F})=−0.374{sup +0.007 +0.013 +0.020}{sub −0.007 −0.014 −0.022} (1σ, 2σ and 3σ statistical errors). Our fitting software and the input files needed to reproduce our main results are publicly available.

  2. Broadband distortion modeling in Lyman-α forest BAO fitting

    SciTech Connect

    Blomqvist, Michael; Kirkby, David; Bautista, Julian E.; Arinyo-i-Prats, Andreu; Busca, Nicolás G.; Miralda-Escudé, Jordi; Slosar, Anže; Font-Ribera, Andreu; Margala, Daniel; Schneider, Donald P.; Vazquez, Jose A.

    2015-11-23

    Recently, the Lyman-α absorption observed in the spectra of high-redshift quasars has been used as a tracer of large-scale structure by means of the three-dimensional Lyman-α forest auto-correlation function at redshift z≃ 2.3, but the need to fit the quasar continuum in every absorption spectrum introduces a broadband distortion that is difficult to correct and causes a systematic error for measuring any broadband properties. Here, we describe a k-space model for this broadband distortion based on a multiplicative correction to the power spectrum of the transmitted flux fraction that suppresses power on scales corresponding to the typical length of a Lyman-α forest spectrum. In implementing the distortion model in fits for the baryon acoustic oscillation (BAO) peak position in the Lyman-α forest auto-correlation, we find that the fitting method recovers the input values of the linear bias parameter bF and the redshift-space distortion parameter βF for mock data sets with a systematic error of less than 0.5%. Applied to the auto-correlation measured for BOSS Data Release 11, our method improves on the previous treatment of broadband distortions in BAO fitting by providing a better fit to the data using fewer parameters and reducing the statistical errors on βF and the combination bF(1+βF) by more than a factor of seven. The measured values at redshift z=2.3 are βF=1.39+0.11 +0.24 +0.38-0.10 -0.19 -0.28 and bF(1+βF)=-0.374+0.007 +0.013 +0.020-0.007 -0.014 -0.022 (1σ, 2σ and 3σ statistical errors). Our fitting software and the input files needed to reproduce our main results are publicly available.

  3. Broadband distortion modeling in Lyman-α forest BAO fitting

    DOE PAGES

    Blomqvist, Michael; Kirkby, David; Bautista, Julian E.; ...

    2015-11-23

    Recently, the Lyman-α absorption observed in the spectra of high-redshift quasars has been used as a tracer of large-scale structure by means of the three-dimensional Lyman-α forest auto-correlation function at redshift z≃ 2.3, but the need to fit the quasar continuum in every absorption spectrum introduces a broadband distortion that is difficult to correct and causes a systematic error for measuring any broadband properties. Here, we describe a k-space model for this broadband distortion based on a multiplicative correction to the power spectrum of the transmitted flux fraction that suppresses power on scales corresponding to the typical length of amore » Lyman-α forest spectrum. In implementing the distortion model in fits for the baryon acoustic oscillation (BAO) peak position in the Lyman-α forest auto-correlation, we find that the fitting method recovers the input values of the linear bias parameter bF and the redshift-space distortion parameter βF for mock data sets with a systematic error of less than 0.5%. Applied to the auto-correlation measured for BOSS Data Release 11, our method improves on the previous treatment of broadband distortions in BAO fitting by providing a better fit to the data using fewer parameters and reducing the statistical errors on βF and the combination bF(1+βF) by more than a factor of seven. The measured values at redshift z=2.3 are βF=1.39+0.11 +0.24 +0.38-0.10 -0.19 -0.28 and bF(1+βF)=-0.374+0.007 +0.013 +0.020-0.007 -0.014 -0.022 (1σ, 2σ and 3σ statistical errors). Our fitting software and the input files needed to reproduce our main results are publicly available.« less

  4. Lyman-alpha radiation hydrodynamics of galactic winds before cosmic reionization

    NASA Astrophysics Data System (ADS)

    Smith, Aaron; Bromm, Volker; Loeb, Abraham

    2017-01-01

    Radiation from the first stars and galaxies initiated the dramatic phase transition marking an end to the cosmic dark ages. The emission and absorption signatures from the Lyman-alpha transition of neutral hydrogen have been indispensable in extending the observational frontier for high-redshift galaxies into the epoch of reionization. Lyman-alpha radiative transfer provides clues about the processes leading to Lyman-alpha escape from individual galaxies and the subsequent transmission through the intergalactic medium. Cosmological simulations incorporating Lyman-alpha radiative transfer enhance our understanding of fundamental physics by supplying the inferred spectra and feedback on the gas. We discuss the dynamical impact of Lyman-alpha radiation pressure on galaxy formation throughout cosmic reionization with the first fully coupled Lyman-alpha radiation-hydrodynamics simulations. We self-consistently follow the chemistry, cooling, self-gravity, and ionizing radiation in protogalaxies and find that Lyman-alpha radiation pressure turns out to be dynamically important in several spherically symmetric simulations. As a case in point we apply our model to the COSMOS redshift 7 (CR7) galaxy at z = 6.6, which exhibits a +160 km/s velocity offset between the Lyman-alpha and HeII line peaks. We find that a massive black hole with a nonthermal Compton-thick spectrum is able to reproduce the observed Lyman-alpha signatures as a result of higher photon trapping and longer potential lifetime. We conclude with a general discussion of Lyman-alpha radiation in the first galaxies by considering simulations that cover the expected range of halo and source properties.

  5. On the Transient Correlation Structure of Water Vapor and Carbon Dioxide Time Series Over Low-Profile Vegetation

    NASA Astrophysics Data System (ADS)

    Scanlon, T. M.; Sahu, P.

    2007-12-01

    Much work has previously centered on temperature and water vapor similarity as a result of its application to the flux-variance method. Less attention, however, has been paid to similarity between carbon dioxide and water vapor. In this study, we analyze water vapor and carbon dioxide time series to infer causes of departure from correlation coefficients of +/-1. Photosynthesis and transpiration, both stomatal processes, have identical sources and sinks. Therefore, under hypothetical conditions in which carbon and water fluxes are comprised of only these two components, the effects of entrainment (which operates at a large scale) and differences in molecular diffusivities between water vapor and carbon dioxide (which operates at a small scale) can cause degradation in the correlation between the two time series. Under more realistic conditions in which the non- stomatal processes of respiration and bare evaporation are active, additional degradation is imparted upon the correlation. The correlation structure between water vapor and carbon dioxide time series is analyzed using high- frequency data collected over an early-growth corn field on the Eastern Shore of Virginia. We contrast the correlations observed following a long dry-down period with those observed shortly after a significant rainfall, when both bare soil evaporation and respiration fluxes became enhanced. Wavelet analysis is applied to the time series to distinguish between the effects of small-scale vs. large-scale process on the degradation of the correlation.

  6. Bioinformatics analysis of time-series genes profiling to explore key genes affected by age in fracture healing.

    PubMed

    Wang, Wei; Shen, Hao; Xie, Jingjing; Zhou, Qiang; Chen, Yu; Lu, Hua

    2014-06-01

    The present study was aimed to explore possible key genes and bioprocess affected by age during fracture healing. GSE589, GSE592 and GSE1371 were downloaded from gene expression omnibus database. The time-series genes of three age levels rats were firstly identified with hclust function in R. Then functional and pathway enrichment analysis for selected time-series genes were performed. Finally, the VennDiagram package of R language was used to screen overlapping n time-series genes. The expression changes of time-series genes in the rats of three age levels were classified into two types: one was higher expressed at 0 day, decreased at 3 day to 2 week, and increased from 4 to 6 week; the other was the opposite. Functional and pathways enrichment analysis showed that 12 time-series genes of adult and old rats were significantly involved in ECM-receptor interaction pathway. The expression changes of 11 genes were consistent with time axis, 10 genes were up-regulated at 3 days after fracture, and increased slowly in 6 week, while Itga2b was down-regulated. The functions of 106 overlapping genes were all associated with growth and development of bone after fracture. The key genes in ECM-receptor interaction pathway including Spp1, Ibsp, Tnn and Col3a1 have been reported to be related to fracture in literatures. The difference during fracture healing in three age levels rats is mainly related to age. The Spp1, Ibsp, Tnn and Col3a1 are possible potential age-related genes and ECM-receptor interaction pathway is the potential age-related process during fracture healing.

  7. Development and validation of software to process radio occultation data: From time series of frequency residuals to vertical profiles of atmospheric and ionospheric properties

    NASA Astrophysics Data System (ADS)

    Moore, L.; Withers, P.; Cahoy, K.; Beerer, I.; Hu, R.; Kennedy, K.; Kingsbury, R.; Webber, M.

    2012-12-01

    For most planetary science instruments, expertise in data processing is widely distributed across the planetary science community. This is not the case for radio occultation observations, which provide vertical profiles of atmospheric and ionospheric properties from measurements of the frequency of radio signals. Increasing the population of radio occultation processing experts will have positive consequences for this field. Here we report the latest results from a project to develop and disseminate capabilities to process radio occultation data. We describe how to obtain vertical profiles of atmospheric and ionospheric properties from time series of frequency residuals, emphasizing issues important for practical implementation that are not obvious in published work. Our methods have been demonstrated successfully on data from a Mars Global Surveyor occultation at Mars. Small differences exist between our results and those archived by the Mars Global Surveyor team, indicating that our techniques, though promising, have not yet been perfected.

  8. Biography Today: Profiles of People of Interest to Young Readers. World Leaders Series: Modern African Leaders. Volume 2.

    ERIC Educational Resources Information Center

    Harris, Laurie Lanzen, Ed.; Abbey, Cherie D., Ed.

    This book provides biographical profiles of 16 leaders of modern Africa of interest to readers ages 9 and above and was created to appeal to young readers in a format they can enjoy reading and easily understand. Biographies were prepared after extensive research, and this volume contains a name index, a general index, a place of birth index, and…

  9. Profiles in Online Learning: A Series on Leadership--Tom Layton: Judo and the Art of Technology Innovation.

    ERIC Educational Resources Information Center

    Danielson, Larry

    1998-01-01

    Profiles a high school technology teacher and creator of CyberSchool, a distance learning program of the Eugene (Oregon) School District. Discusses Tom Layton's education, early work experience, establishment of a high school English-as-a-Second-Language (ESL) program, integration of computers into the classroom, reputation as a technology leader,…

  10. Occupational Competency Profile for Health Occupations Education Program: Teacher Self-Assessment. Information Series: Report No. 11.

    ERIC Educational Resources Information Center

    Walters, Norma J.

    This assessment instrument is intended to assist teachers in evaluating the relevance of the competencies included in the health occupations education curriculum they are teaching and in assessing their own continuing education needs. The profile lists the competencies required of persons working at the following sites: hospital departments…

  11. Profiles in Online Learning: A Series on Leadership--Tom Layton: Judo and the Art of Technology Innovation.

    ERIC Educational Resources Information Center

    Danielson, Larry

    1998-01-01

    Profiles a high school technology teacher and creator of CyberSchool, a distance learning program of the Eugene (Oregon) School District. Discusses Tom Layton's education, early work experience, establishment of a high school English-as-a-Second-Language (ESL) program, integration of computers into the classroom, reputation as a technology leader,…

  12. Biography Today: Profiles of People of Interest to Young Readers. World Leaders Series: Environmental Leaders 2. Volume 3.

    ERIC Educational Resources Information Center

    Hillstrom, Kevin, Ed.; Hillstrom, Laurie, Ed.

    This book provides biographical profiles of 11 environmental leaders of interest to readers ages 9 and above and was created to appeal to young readers in a format they can enjoy reading and readily understand. Biographies were prepared after extensive research, and each volume contains a cumulative index, a general index, a place of birth index,…

  13. Profiles of Students Completing Teacher Education Programs at MSU: Fall, 1983 through Spring, 1986. Program Evaluation Series No. 20.

    ERIC Educational Resources Information Center

    Freeman, Donald J.; Kalaian, Sima A.

    The program evaluation design at Michigan State University (MSU) includes three surveys (entry-level, exit-level, and follow-up) that trace the progress of teacher candidates from program entry through their initial years of teaching. This report provides a comprehensive profile of students completing teacher preparation programs at MSU from fall,…

  14. Occupational Competency Profile for Health Occupations Education Program: Teacher Self-Assessment. Information Series: Report No. 11.

    ERIC Educational Resources Information Center

    Walters, Norma J.

    This assessment instrument is intended to assist teachers in evaluating the relevance of the competencies included in the health occupations education curriculum they are teaching and in assessing their own continuing education needs. The profile lists the competencies required of persons working at the following sites: hospital departments…

  15. Student Characteristics as Compared to the Community Profile, Fall, 1985. [Research Report Series], Volume XV, No. 11.

    ERIC Educational Resources Information Center

    Lucas, John A.

    In fall 1985, a study was conducted at William Rainey Harper College (WRHC) to provide a student profile for general information purposes, to gather data not available on the college's automated data file, and to analyze WRHC's marketing outreach. Surveys were mailed to random samples of 500 credit degree students and 300 continuing education…

  16. Optical alignment of the Chromospheric Lyman-Alpha Spectro-Polarimeter using sophisticated methods to minimize activities under vacuum

    NASA Astrophysics Data System (ADS)

    Giono, G.; Katsukawa, Y.; Ishikawa, R.; Narukage, N.; Kano, R.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.; Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J.

    2016-07-01

    The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a sounding-rocket instrument developed at the National Astronomical Observatory of Japan (NAOJ) as a part of an international collaboration. The instrument main scientific goal is to achieve polarization measurement of the Lyman-α line at 121.56 nm emitted from the solar upper-chromosphere and transition region with an unprecedented 0.1% accuracy. The optics are composed of a Cassegrain telescope coated with a "cold mirror" coating optimized for UV reflection and a dual-channel spectrograph allowing for simultaneous observation of the two orthogonal states of polarization. Although the polarization sensitivity is the most important aspect of the instrument, the spatial and spectral resolutions of the instrument are also crucial to observe the chromospheric features and resolve the Ly-α profiles. A precise alignment of the optics is required to ensure the resolutions, but experiments under vacuum conditions are needed since Ly-α is absorbed by air, making the alignment experiments difficult. To bypass this issue, we developed methods to align the telescope and the spectrograph separately in visible light. We explain these methods and present the results for the optical alignment of the CLASP telescope and spectrograph. We then discuss the combined performances of both parts to derive the expected resolutions of the instrument, and compare them with the flight observations performed on September 3rd 2015.

  17. Lyman-alpha forests cool warm dark matter

    NASA Astrophysics Data System (ADS)

    Baur, Julien; Palanque-Delabrouille, Nathalie; Yèche, Christophe; Magneville, Christophe; Viel, Matteo

    2016-08-01

    The free-streaming of keV-scale particles impacts structure growth on scales that are probed by the Lyman-alpha forest of distant quasars. Using an unprecedentedly large sample of medium-resolution QSO spectra from the ninth data release of SDSS, along with a state-of-the-art set of hydrodynamical simulations to model the Lyman-alpha forest in the non-linear regime, we issue one of the tightest bounds to date, from Ly-α data alone, on pure dark matter particles: mX>4.09 keV (95% CL) for early decoupled thermal relics such as a hypothetical gravitino, and correspondingly ms>24.4 keV (95% CL) for a non-resonantly produced right-handed neutrino. This limit depends on the value on ns, and Planck measures a higher value of ns than SDSS-III/BOSS. Our bounds thus change slightly when Ly-α data are combined with CMB data from Planck 2016. The limits shift to mX>2.96 keV (95% CL) and ms>16.0 keV (95% CL). Thanks to SDSS-III data featuring smaller uncertainties and covering a larger redshift range than SDSS-I data, our bounds confirm the most stringent results established by previous works and are further at odds with a purely non-resonantly produced sterile neutrino as dark matter.

  18. What Drives the Differential Evolution of Lyman Break Galaxies?

    NASA Astrophysics Data System (ADS)

    Sawicki, Marcin; Thompson, David

    2005-06-01

    Analysis of the luminosity function of Lyman Break Galaxies in our deep, wide Keck Deep Fields survey robustly shows that the evolution of the LBG population is differential with luminosity from z~4 to z~3. Two of the possible mechanisms driving this evolution relate to (1) changes in the properties of dust and (2) changes in the duration of starbursting episodes in sub-L* LBGs. We will use archival Spitzer IRAC, HST, and ground-based imaging of GOODS and the HDFs to compare the spectral energy distributions of LBGs as a function of redshift and luminosity and search for related differences in reddening and starburst age. Finding such differences will not only identify the processes responsible for the evolution of the luminosity function but will thereby also point us towards the underlying physical mechanisms that control how galaxies form and evolve at high redshift. The non-detection of such differences will mean that the responsible mechanism lies elsewhere and will give impetus to other lines of attacking the problem. We have experience in analyzing the spectral energy distributions of Lyman Break Galaxies and request salary and other support to allow us to extend our techniques to higher redshifts, larger samples, and fainter objects with no spectroscopic redshifts that we need to help understand the observed evolution of the luminosity function. Significantly, our analysis will compare LBG subsamples in a differential and hence very robust way and thus will help us understand how galaxies are assembled at high redshift.

  19. Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP)

    NASA Technical Reports Server (NTRS)

    Kano, Ryohei; Bando, Takamasa; Narukage, Noriyuki; Ishikawa, Ryoko; Kubo, Masahito; Katsukawa, Yukio; Ishikawa, Shin-­nosuke; Hara, Hirohisa; Suematsu, Yoshinori; Giono, Gabriel; Shimizu, Toshifumi; Sakao, Taro; Ichimoto, Kiyoshi; Goto, Motoshi; Winebarger, amy; Kobayashi, Ken; Trujullo Bueno, Javier; Auchere, Frederic

    2015-01-01

    Chromosphere, the transition layer of the sun is a region to switch to the magnetic pressure dominated from plasma pressure dominated, simultaneous observation of the detailed magnetic field measurement and plasma of dynamic phenomenon here is what is the frontier of the next solar physics. As This is a challenge that has just mentioned, even the next solar observation satellite plan SOLAR-C, in the experiments we had used a NASA sounding rocket for the first time in the SOLAR-C plan, will address the chromosphere-transition layer magnetic field measurement there. It is, is a Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) plan, the linear polarization of Lyman ?? emission lines chromosphere-transition layer shoots (121.6nm) were detected in 0.1 percent of high accuracy, a new technique called Hanre effect I get the magnetic field information of chromosphere-transition layer. In Japan, the US and Europe joint observation in November 2012 as a rocket experiment is adopted to NASA this plan that full-scale start-up, start from assembly work is 2014 spring flight observation device, currently, it is where the alignment of the optical elements have been implemented. After this, it is planned to continue with the performance evaluation towards the observation implementation of summer 2015. In addition to once again explain the contents of the plan In this presentation, we report an overview of the entire development and preparation current status.

  20. The Balmer Lines of He ii in the Blue Wing of the Hydrogen Lyman α Line Observed in a Quiescent Prominence

    NASA Astrophysics Data System (ADS)

    Vial, J.-C.; Eurin, G.; Curdt, W.

    2015-02-01

    We revisit the prominence observations in the Lyman α line of Curdt et al. ( Astron. Astrophys. 511, L4, 2010) and focus on the bump in the blue wing of the line, which we identify with He ii Balmer lines. We determine the transition candidates, derive an upper limit for the width of the profile and an associated non-thermal velocity close to 0 km s-1, with the assumption that the kinetic temperature is equal to the formation temperature. We compare the total intensity with the corresponding H Lyman α intensity and find a ratio much lower than that measured by Ebadi, Vial, and Ajabshirizadeh ( Solar Phys. 257, 91, 2009) in other Lyman lines. We confirm this result with observations performed by Schwartz et al. (private communication, 2014), we discuss a possible interpretation, and suggest that this issue needs to be addressed closely in future observations.

  1. A coronagraphic absorbing cloud reveals the narrow-line region and extended Lyman α emission of QSO J0823+0529

    NASA Astrophysics Data System (ADS)

    Fathivavsari, H.; Petitjean, P.; Noterdaeme, P.; Pâris, I.; Finley, H.; López, S.; Srianand, R.; Sánchez, P.

    2015-11-01

    We report long-slit spectroscopic observations of the quasar SDSS J082303.22+052907.6 (z_{C IV}} ˜ 3.1875), whose broad-line region (BLR) is partly eclipsed by a strong damped Lyman α (DLA; logN(H I) = 21.7) cloud. This allows us to study the narrow-line region (NLR) of the quasar and the Lyman α emission from the host galaxy. Using CLOUDY models that explain the presence of strong N V and P V absorption together with the detection of Si II* and O I** absorption in the DLA, we show that the density and the distance of the cloud to the quasar are in the ranges 180 < nH < 710 cm-3 and 580 > r0 > 230 pc, respectively. Sizes of the neutral (˜2-9pc) and highly ionized phases (˜3-80pc) are consistent with the partial coverage of the C IV BLR by the C IV absorption from the DLA (covering factor of ˜0.85). We show that the residuals are consistent with emission from the NLR with C IV/Lyman α ratios varying from 0 to 0.29 through the profile. Remarkably, we detect extended Lyman α emission up to 25 kpc to the north and west directions and 15 kpc to the south and east. We interpret the emission as the superposition of strong emission in the plane of the galaxy up to 10 kpc with emission in a wind of projected velocity ˜500 km s-1 which is seen up to 25 kpc. The low metallicity of the DLA (0.27 solar) argues for at least part of this gas being infalling towards the active galactic nucleus and possibly being located where accretion from cold streams ends up.

  2. Esthetic Considerations for Reconstructing Implant Emergence Profile Using Titanium and Zirconia Custom Implant Abutments: Fifty Case Series Report.

    PubMed

    Kutkut, Ahmad; Abu-Hammad, Osama; Mitchell, Richard

    2015-10-01

    Titanium and zirconia custom implant abutments are now commonly used for esthetic implant dentistry. Custom implant abutments allow the clinician to improve an implant's emergence profile, to customize cervical margins in accordance with the anatomy of the natural root, and to compensate for poor implant angulation. All of these are essential for optimum esthetic outcomes. Computer-aided design/computer-aided machining (CAD/CAM) technology allows the clinician to design custom implant abutment configurations and create natural-looking superstructures that are in harmony with the adjacent dentition and soft tissue. The CAD/CAM technique provides precise fit, reduces the cost of the procedure, and eliminates dimensional inaccuracies inherent in the conventional waxing and casting technique. The aim of this report is to describe a simplified technique for reconstructing emergence profiles during implant restoration using milled titanium and zirconia custom implant abutments. The results of 50 consecutive cases are reported.

  3. [OIII] Emission and Gas Kinematics in a Lyman-alpha Blob at z ~ 3.1

    NASA Astrophysics Data System (ADS)

    McLinden, Emily; Rhoads, J. E.; Malhotra, S.; Hibon, P.; Tilvi, V.

    2013-01-01

    We present spectroscopic measurements of the [OIII] emission line from two subregions of strong Lyman-alpha emission in a radio-quiet Lyman-alpha blob (LAB). The blob under study is LAB1 at z ~ 3.1 first reported, by Steidel et al (2000). The [OIII] detections are from the two Lyman break galaxies embedded in the blob halo. We made our [OIII] measurements with LUCIFER on the 8.4m Large Binocular Telescope and NIRSPEC on 10m Keck Telescope. Comparing the redshift of the [OIII] to Lyman-alpha redshifts allows us to take a step towards understanding the kinematics of the gas in the blob. Using both LUCIFER and NIRSPEC we consistently find velocity offsets between the [OIII] and Lyman-alpha redshifts consistent with 0 km/s in both subregions studied (ranging from -43.88 ± 69.01 -- 36.58 ± 63.85 km/s). We discuss the possible implications of this result, as it could downplay the role of winds and outflows in powering the Lyman-alpha emission in this LAB, since a velocity offset between nebular emission lines and Lyman-alpha are often interpreted as evidence of large-scale outflows.

  4. Decaying neutrinos and the abundance of He I in Lyman limit systems and Lyman-Alpha clouds

    NASA Astrophysics Data System (ADS)

    Sciama, D. W.

    1994-02-01

    In this Letter we show that photons from decaying intergalactic neutrinos could explain an anomaly recently found by Reimers & Vogel in the abundance of He I in three high-redshift Lyman limit systems of the Quasi Stellar Object (QSO) HS 1700+6416. Their data and analysis yield He I column densities approximately 5 times greater than given by their model calculations. They conclude that the effective hydrogen ionizing flux is about eight times greater than the helium ionizing flux. Such a steep spectrum is not expected for the integrated radiation from QSOs but would arise naturally in the decaying neutrino theory, whose decay photons can ionize hydrogen but not helium. Similar considerations show that the decaying neutrino theory is compatible with the upper limits found by Reimers & Vogel for the column density of He I in three Lyman alpha clouds along the line of sight to HS 1700+6416. Both these conclusions depend on the absence of significant intergalactic absorption of photons capable of ionizing He II. This assumption can be tested by searching for a He II Gunn-Peterson absorption trough in the spectra of suitable QSOs.

  5. Prospects for constraining neutrino mass using Planck and Lyman-{alpha} forest data

    SciTech Connect

    Gratton, Steven; Lewis, Antony; Efstathiou, George

    2008-04-15

    In this paper we investigate how well Planck and Lyman-{alpha} forest data will be able to constrain the sum of the neutrino masses, and thus, in conjunction with flavor oscillation experiments, be able to determine the absolute masses of the neutrinos. It seems possible that Planck, together with a Lyman-{alpha} survey, will be able to put pressure on an inverted hierarchial model for the neutrino masses. However, even for optimistic assumptions of the precision of future Lyman-{alpha} data sets, it will not be possible to confirm a minimal-mass normal hierarchy.

  6. Two Lensed Lyman-α Emitting Galaxies at z~ 5

    NASA Astrophysics Data System (ADS)

    Bayliss, Matthew B.; Wuyts, Eva; Sharon, Keren; Gladders, Michael D.; Hennawi, Joseph F.; Koester, Benjamin P.; Dahle, Håkon

    2010-09-01

    We present observations of two strongly lensed z ~ 5 Lyman-α emitting galaxies that were discovered in the Sloan Giant Arcs Survey (SGAS). We identify the two sources as SGAS J091541+382655 at z = 5.200 and SGAS J134331+415455 at z = 4.994. We measure their AB magnitudes at (i, z) = (23.34 ± 0.09, 23.29 ± 0.13) mag and (i, z) = (23.78 ± 0.18, 24.24+0.18 -0.16) mag and the rest-frame equivalent widths of the Lyman-α emission at 25.3 ± 4.1 Å and 135.6 ± 20.3 Å for SGAS J091541+382655 and SGAS J134331+415455, respectively. Each source is strongly lensed by a massive galaxy cluster in the foreground, and the magnifications due to gravitational lensing are recovered from strong lens modeling of the foreground lensing potentials. We use the magnification to calculate the intrinsic, unlensed Lyman-α and UV continuum luminosities for both sources, as well as the implied star formation rates. We find SGAS J091541+382655 and SGAS J134341+415455 to be galaxies with (L Ly-α, L UV) <= (0.6 L* Ly-α, 2 L*UV) and (L Ly-α, L UV) = (0.5 L* Ly-α, 0.9 L*UV), respectively. Comparison of the spectral energy distributions of both sources against stellar population models produces estimates of the mass in young stars in each galaxy; we report an upper limit of M stars <= 7.9+3.7 -2.5 × 107 M sun h -1 0.7 for SGAS J091531+382655 and a range of viable masses for SGAS J134331+415455 of 2 × 108 M sun h -1 0.7< M stars < 6 × 109 M sun h -1 0.7. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnología e Innovaci

  7. Iron profiles and speciation of the upper water column at the Bermuda Atlantic Time-series Study site: a model based sensitivity study

    NASA Astrophysics Data System (ADS)

    Weber, L.; Völker, C.; Oschlies, A.; Burchard, H.

    2007-08-01

    A one-dimensional model of the biogeochemistry and speciation of iron is coupled with the General Ocean Turbulence Model (GOTM) and a NPZD-type ecosystem model. The model is able to simulate the temporal patterns and vertical profiles of dissolved iron (dFe) in the upper ocean at the Bermuda Atlantic Time-series Study site reasonably well. Subsurface model profiles strongly depend on the parameter values chosen for the loss processes for iron, colloidal aggregation and scavenging onto particles. Estimates for these parameters based on observations in particle-rich waters result in depletion of dFe. A high stability constant of iron-binding organic ligands is required to reproduce the observed degree of organic complexation below the mixed layer. The scavenging residence time for iron in the model is shortest in spring and summer, because of the larger abundance of particles, and increases with depth towards values on the order of a hundred years. A solubility of atmospherically deposited iron higher than 2% lead to dFe concentrations incompatible with observations. Despite neglecting ultraviolet radiation, the model produces diurnal variations and mean vertical profiles of H2O2 and iron species that are in good agreement with observations.

  8. Iron profiles and speciation of the upper water column at the Bermuda Atlantic time-series Study site: a model based sensitivity study

    NASA Astrophysics Data System (ADS)

    Weber, L.; Völker, C.; Oschlies, A.; Burchard, H.

    2007-03-01

    A one-dimensional model of the biogeochemistry and speciation of iron is coupled with the General Ocean Turbulence Model (GOTM) and a NPZD-type ecosystem model. The model is able to simulate the temporal patterns and vertical profiles of dissolved iron (dFe) in the upper ocean at the Bermuda Atlantic Time-series Study site reasonably well. Subsurface model profiles strongly depend on the parameter values chosen for the loss processes for iron, colloidal aggregation and scavenging onto particles. Current estimates for these parameters result in depletion of dFe. A high stability constant of iron-binding organic ligands is required to reproduce the observed degree of organic complexation below the mixed layer. A solubility of atmospherically deposited iron higher than 2% lead to dFe concentrations incompatible with observations. Despite neglecting ultraviolet radiation, the model produces diurnal variations and mean vertical profiles of H2O2 and iron species that are in good agreement with observations.

  9. Long-term series of tropospheric water vapour amounts and HDO/H2O ratio profiles above Jungfraujoch.

    NASA Astrophysics Data System (ADS)

    Lejeune, B.; Mahieu, E.; Schneider, M.; Hase, F.; Servais, C.; Demoulin, P.

    2012-04-01

    Water vapour is a crucial climate variable involved in many processes which widely determine the energy budget of our planet. In particular, water vapour is the dominant greenhouse gas in the Earth's atmosphere and its radiative forcing is maximum in the middle and upper troposphere. Because of the extremely high variability of water vapour concentration in time and space, it is challenging for the available relevant measurement techniques to provide a consistent data set useful for trend analyses and climate studies. Schneider et al. (2006a) showed that ground-based Fourier Transform Infrared (FTIR) spectroscopy, performed from mountain observatories, allows for the detection of H2O variabilities up to the tropopause. Furthermore, the FTIR measurements allow the retrieval of HDO amounts and therefore the monitoring of HDO/H2O ratio profiles whose variations act as markers for the source and history of the atmospheric water vapour. In the framework of the MUSICA European project (Multi-platform remote Sensing of Isotopologues for investigating the Cycle of Atmospheric water, http://www.imk-asf.kit.edu/english/musica.php), a new approach has been developed and optimized by M. Schneider and F. Hase, using the PROFFIT algorithm, to consistently retrieve tropospheric water vapour profiles from high-resolution ground-based infrared solar spectra and so taking benefit from available long-term data sets of ground-based observations. The retrieval of the water isotopologues is performed on a logarithmic scale from 14 micro-windows located in the 2600-3100 cm-1 region. Other important features of this new retrieval strategy are: a speed dependant Voigt line shape model, a joint temperature profile retrieval and an interspecies constraint for the HDO/H2O profiles. In this contribution, we will combine the quality of the MUSICA strategy and of our observations, which are recorded on a regular basis with FTIR spectrometers, under clear-sky conditions, at the NDACC site

  10. Optical design of Lyman/FUSE. [Far UV Spectroscopic Explorer

    NASA Technical Reports Server (NTRS)

    Content, D. A.; Davila, P. M.; Osantowski, J. F.; Saha, T. T.; Wilson, M. E.

    1990-01-01

    The optical system for the proposed Lyman/Far UV Spectroscopic Explorer (FUSE) orbiting observatory is described and illustrated with drawings and graphs of predicted performance. The system comprises (1) an FUV channel based on a 1.84-m-diameter Rowland circle spectrograph with five high-density modified ellipsiodal near-normal-incidence gratings and an array of four MAMA detectors; (2) an EUV channel with ellipsoidal mirror, planar varied-line-space grating, microchannel-plate array, and wedge-and-strip anode detector; (3) a 70-cm Wolter II glancing-incidence telescope; and (4) a CCD-detector fine-error sensor to provide accurate pointing (within 200 marcsec rms). The resolving powers of the spectrographs are 30,000 in the FUV and 300-600 (wavelength-dependent) in the EUV.

  11. Equilibrium slab models of Lyman-alpha clouds

    NASA Technical Reports Server (NTRS)

    Charlton, Jane C.; Salpeter, Edwin E.; Hogan, Craig J.

    1993-01-01

    Solutions for the equilibrium configuration of a slab with ionizing radiation incident equally from both sides are explored. Radiation effects (photoionization, Ly-alpha photon trapping, and mock gravity) as well as external pressure and self gravity (with and without dark matter) are included. The general formalism is applied to structure growth on small scales at very high z due to mock gravity on dust. Emphasis is placed on the application of slab models at z of less than 5, particularly those that may correspond to Ly-alpha forest, Lyman limit, and damped Ly-alpha systems. The regime with a dominant outward force contributed by trapping of Ly-alpha photons is discussed. General expressions are given for the equilibrium, including dark matter, assuming various relationships between the density of the dark matter halo and the total gas column density.

  12. Stellar Lyman-alpha emission and the local interstellar medium

    NASA Technical Reports Server (NTRS)

    Landsman, Wayne; Simon, Theodore

    1991-01-01

    The UV spectra now available in the IUE archives have been systematically searched for the presence of Lyman-alpha emission in late-type stars. The results provide the first survey of the behavior of the Ly-alpha emission line across most of the cool half of the H-R diagram. The normalized Ly-alpha emission flux is strongest in the chromospherically active RS CVn stars and in the dMe stars. The range of normalized flux values is much smaller among F-type stars than in stars of later spectral type. A dropoff appears in the flux levels of stars at B-V less than 0.30 mag. The measurements are used to search for evidence of possible high column density clouds in the local ISM. The cloud previously identified toward Alpha Oph may be seen in the reduced flux observed toward Beta Oph.

  13. Spacelab Lyman Alpha-White Light Coronagraph Program

    NASA Astrophysics Data System (ADS)

    Kohl, J. L.

    1986-06-01

    The Spacelab Lyman Alpha Coronagraph (SLAC) of the Smithsonian Astrophysical Observatory (SAO) and the White Light Coronagraph (WLC) to be provided by the High Altitude Observatory (HAO) are two separate coronagraphs which would be operated in a joint fashion during Spacelab missions to be flown by the Space Shuttle. The two instruments would be used to perform joint observations of solar coronal structures from 1.2 to 8.0 solar radii from sun-center in vacuum ultraviolet and visible radiations. Temperatures, densities, and flow velocities throughout the solar wing acceleration region of the inner solar corona were measured. The Phase I Definition activity resulted in the successful definition and preliminary design of the experiment/instrumentation subsystem and associated software, ground support equipment and interfaces to the extended required to accurately estimate the scope of the investigation and prepare an Investigational Development Plan; the performance of the necessary functional, operations, and safety analyses necessary to complete the Experiment Requirements document.

  14. Type II Quasars among Z>4 Strong Lyman Alpha Sources

    NASA Astrophysics Data System (ADS)

    Malhotra, Sangeeta

    2002-09-01

    Strong Lyman-alpha emission is expected both from primordial galaxies and from the type II quasars required to explain the hard x-ray background. We have identified ~300 Ly-alpha sources at redshifts 4.5 and 5.7. About 60% of these show rest equivalent widths >200 Angstrom, which requires active nuclei, or extreme populations of massive stars. Our Ly-alpha survey (LALA) is a unique resource for determining the space density of type II quasars at high z efficiently. The large fields of ACIS and LALA will allow us to observe 60 ly-alpha emitters, including the brightest narrow line Ly-alpha emitter with EW=660. This will have implications for composition of the X-ray background, background radiation at other wavelengths, and structure formation (stars vs black holes) in the early universe.

  15. Spacelab Lyman Alpha-White Light Coronagraph Program

    NASA Technical Reports Server (NTRS)

    Kohl, J. L.

    1986-01-01

    The Spacelab Lyman Alpha Coronagraph (SLAC) of the Smithsonian Astrophysical Observatory (SAO) and the White Light Coronagraph (WLC) to be provided by the High Altitude Observatory (HAO) are two separate coronagraphs which would be operated in a joint fashion during Spacelab missions to be flown by the Space Shuttle. The two instruments would be used to perform joint observations of solar coronal structures from 1.2 to 8.0 solar radii from sun-center in vacuum ultraviolet and visible radiations. Temperatures, densities, and flow velocities throughout the solar wing acceleration region of the inner solar corona were measured. The Phase I Definition activity resulted in the successful definition and preliminary design of the experiment/instrumentation subsystem and associated software, ground support equipment and interfaces to the extended required to accurately estimate the scope of the investigation and prepare an Investigational Development Plan; the performance of the necessary functional, operations, and safety analyses necessary to complete the Experiment Requirements document.

  16. Optical design of Lyman/FUSE. [Far UV Spectroscopic Explorer

    NASA Technical Reports Server (NTRS)

    Content, D. A.; Davila, P. M.; Osantowski, J. F.; Saha, T. T.; Wilson, M. E.

    1990-01-01

    The optical system for the proposed Lyman/Far UV Spectroscopic Explorer (FUSE) orbiting observatory is described and illustrated with drawings and graphs of predicted performance. The system comprises (1) an FUV channel based on a 1.84-m-diameter Rowland circle spectrograph with five high-density modified ellipsiodal near-normal-incidence gratings and an array of four MAMA detectors; (2) an EUV channel with ellipsoidal mirror, planar varied-line-space grating, microchannel-plate array, and wedge-and-strip anode detector; (3) a 70-cm Wolter II glancing-incidence telescope; and (4) a CCD-detector fine-error sensor to provide accurate pointing (within 200 marcsec rms). The resolving powers of the spectrographs are 30,000 in the FUV and 300-600 (wavelength-dependent) in the EUV.

  17. A model for the disc Lyman alpha emission of Uranus

    NASA Technical Reports Server (NTRS)

    Ben Jaffel, L.; Prange, R.; Emerich, C.; Vidal-Madjar, A.; Mcconnell, J. C.

    1991-01-01

    A new efficient radiative transfer algorithm for nonhomogeneous model atmospheres has been applied to the Uranian atmosphere. The contribution of the scatter solar Lyman-alpha to the Uranain emission is of the order of 300 R, and the Rayleigh contribution may reach 450 R for small values of the eddy diffusion coefficient (EDC). The total solar contribution may then reach about 750 R for a solar flux of 2.5 x 10 to the 11th photons/sq cm/s/A. A level of up to 400 R is confirmed in some directions for the interstellar wind contribution. The values of the atmospheric EDC necessary to mimic the observations are 50-100 sq cm/s. A small additional source located on the dayside Uranian atmosphere seems necessary correctly to fit the shape of the limb to limb intensity variation, especially near the limbs. Its contribution to the emergent intensity would range from 100 to 500 R.

  18. Towards physics responsible for large-scale Lyman-α forest bias parameters

    SciTech Connect

    Agnieszka M. Cieplak; Slosar, Anze

    2016-03-08

    Using a series of carefully constructed numerical experiments based on hydrodynamic cosmological SPH simulations, we attempt to build an intuition for the relevant physics behind the large scale density (bδ) and velocity gradient (bη) biases of the Lyman-α forest. Starting with the fluctuating Gunn-Peterson approximation applied to the smoothed total density field in real-space, and progressing through redshift-space with no thermal broadening, redshift-space with thermal broadening and hydrodynamically simulated baryon fields, we investigate how approximations found in the literature fare. We find that Seljak's 2012 analytical formulae for these bias parameters work surprisingly well in the limit of no thermal broadening and linear redshift-space distortions. We also show that his bη formula is exact in the limit of no thermal broadening. Since introduction of thermal broadening significantly affects its value, we speculate that a combination of large-scale measurements of bη and the small scale flux PDF might be a sensitive probe of the thermal state of the IGM. Lastly, we find that large-scale biases derived from the smoothed total matter field are within 10–20% to those based on hydrodynamical quantities, in line with other measurements in the literature.

  19. Towards physics responsible for large-scale Lyman-α forest bias parameters

    NASA Astrophysics Data System (ADS)

    Cieplak, Agnieszka M.; Slosar, Anže

    2016-03-01

    Using a series of carefully constructed numerical experiments based on hydrodynamic cosmological SPH simulations, we attempt to build an intuition for the relevant physics behind the large scale density (bδ) and velocity gradient (bη) biases of the Lyman-α forest. Starting with the fluctuating Gunn-Peterson approximation applied to the smoothed total density field in real-space, and progressing through redshift-space with no thermal broadening, redshift-space with thermal broadening and hydrodynamically simulated baryon fields, we investigate how approximations found in the literature fare. We find that Seljak's 2012 analytical formulae for these bias parameters work surprisingly well in the limit of no thermal broadening and linear redshift-space distortions. We also show that his bη formula is exact in the limit of no thermal broadening. Since introduction of thermal broadening significantly affects its value, we speculate that a combination of large-scale measurements of bη and the small scale flux PDF might be a sensitive probe of the thermal state of the IGM. We find that large-scale biases derived from the smoothed total matter field are within 10-20% to those based on hydrodynamical quantities, in line with other measurements in the literature.

  20. Towards physics responsible for large-scale Lyman-α forest bias parameters

    DOE PAGES

    Agnieszka M. Cieplak; Slosar, Anze

    2016-03-08

    Using a series of carefully constructed numerical experiments based on hydrodynamic cosmological SPH simulations, we attempt to build an intuition for the relevant physics behind the large scale density (bδ) and velocity gradient (bη) biases of the Lyman-α forest. Starting with the fluctuating Gunn-Peterson approximation applied to the smoothed total density field in real-space, and progressing through redshift-space with no thermal broadening, redshift-space with thermal broadening and hydrodynamically simulated baryon fields, we investigate how approximations found in the literature fare. We find that Seljak's 2012 analytical formulae for these bias parameters work surprisingly well in the limit of no thermalmore » broadening and linear redshift-space distortions. We also show that his bη formula is exact in the limit of no thermal broadening. Since introduction of thermal broadening significantly affects its value, we speculate that a combination of large-scale measurements of bη and the small scale flux PDF might be a sensitive probe of the thermal state of the IGM. Lastly, we find that large-scale biases derived from the smoothed total matter field are within 10–20% to those based on hydrodynamical quantities, in line with other measurements in the literature.« less

  1. Discovery of Ubiquitous Fast-Propagating Intensity Disturbances by the Chromospheric Lyman Alpha Spectropolarimeter (CLASP)

    NASA Astrophysics Data System (ADS)

    Kubo, M.; Katsukawa, Y.; Suematsu, Y.; Kano, R.; Bando, T.; Narukage, N.; Ishikawa, R.; Hara, H.; Giono, G.; Tsuneta, S.; Ishikawa, S.; Shimizu, T.; Sakao, T.; Winebarger, A.; Kobayashi, K.; Cirtain, J.; Champey, P.; Auchère, F.; Trujillo Bueno, J.; Asensio Ramos, A.; Štěpán, J.; Belluzzi, L.; Manso Sainz, R.; De Pontieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R.; Goto, M.

    2016-12-01

    High-cadence observations by the slit-jaw (SJ) optics system of the sounding rocket experiment known as the Chromospheric Lyman Alpha Spectropolarimeter (CLASP) reveal ubiquitous intensity disturbances that recurrently propagate in either the chromosphere or the transition region or both at a speed much higher than the speed of sound. The CLASP/SJ instrument provides a time series of two-dimensional images taken with broadband filters centered on the Lyα line at a 0.6 s cadence. The multiple fast-propagating intensity disturbances appear in the quiet Sun and in an active region, and they are clearly detected in at least 20 areas in a field of view of 527″ × 527″ during the 5 minute observing time. The apparent speeds of the intensity disturbances range from 150 to 350 km s-1, and they are comparable to the local Alfvén speed in the transition region. The intensity disturbances tend to propagate along bright elongated structures away from areas with strong photospheric magnetic fields. This suggests that the observed fast-propagating intensity disturbances are related to the magnetic canopy structures. The maximum distance traveled by the intensity disturbances is about 10″, and the widths are a few arcseconds, which are almost determined by a pixel size of 1.″03. The timescale of each intensity pulse is shorter than 30 s. One possible explanation for the fast-propagating intensity disturbances observed by CLASP is magnetohydrodynamic fast-mode waves.

  2. Towards physics responsible for large-scale Lyman-α forest bias parameters

    SciTech Connect

    Cieplak, Agnieszka M.; Slosar, Anže E-mail: anze@bnl.gov

    2016-03-01

    Using a series of carefully constructed numerical experiments based on hydrodynamic cosmological SPH simulations, we attempt to build an intuition for the relevant physics behind the large scale density (b{sub δ}) and velocity gradient (b{sub η}) biases of the Lyman-α forest. Starting with the fluctuating Gunn-Peterson approximation applied to the smoothed total density field in real-space, and progressing through redshift-space with no thermal broadening, redshift-space with thermal broadening and hydrodynamically simulated baryon fields, we investigate how approximations found in the literature fare. We find that Seljak's 2012 analytical formulae for these bias parameters work surprisingly well in the limit of no thermal broadening and linear redshift-space distortions. We also show that his b{sub η} formula is exact in the limit of no thermal broadening. Since introduction of thermal broadening significantly affects its value, we speculate that a combination of large-scale measurements of b{sub η} and the small scale flux PDF might be a sensitive probe of the thermal state of the IGM. We find that large-scale biases derived from the smoothed total matter field are within 10–20% to those based on hydrodynamical quantities, in line with other measurements in the literature.

  3. Discovery of Ubiquitous Fast Propagating Intensity Disturbances by the Chromospheric Lyman Alpha Spectropolarimeter (CLASP)

    NASA Technical Reports Server (NTRS)

    Kubo, M.; Katsukawa, Y.; Suematsu, Y.; Kano, R.; Bando, T.; Narukage, N.; Ishikawa, R.; Hara, H.; Giono, G.; Tsuneta, S.; hide

    2016-01-01

    High cadence observations by the slit-jaw (SJ) optics system of the sounding rocket experiment known as the Chromospheric Lyman Alpha SpectroPolarimeter (CLASP) reveal ubiquitous intensity disturbances that recurrently propagate in one or both of the chromosphere or transition region at a speed much higher than the sound speed. The CLASP/SJ instrument provides a time series of 2D images taken with broadband filters centered on the Ly(alpha) line at a 0.6 s cadence. The fast propagating intensity disturbances are detected in the quiet Sun and in an active region, and at least 20 events are clearly detected in the field of view of 527'' x 527'' during the 5-minute observing time. The apparent speeds of the intensity disturbances range from 150 to 350 km/s, and they are comparable to the local Alfven speed in the transition region. The intensity disturbances tend to propagate along bright elongated structures away from areas with strong photospheric magnetic fields. This suggests that the observed propagating intensity disturbances are related to the magnetic canopy structures. The maximum distance traveled by the intensity disturbances is of about 10'', and the widths are a few arcseconds, which is almost determined by the pixel size of 1.''03. The timescale of each intensity pulse is shorter than 30 s. One possible explanation of the fast propagating intensity disturbances observed by CLASP is magneto-hydrodynamic fast mode waves.

  4. The Lyman alpha reference sample. II. Hubble space telescope imaging results, integrated properties, and trends

    SciTech Connect

    Hayes, Matthew; Östlin, Göran; Duval, Florent; Sandberg, Andreas; Guaita, Lucia; Melinder, Jens; Rivera-Thorsen, Thøger; Adamo, Angela; Schaerer, Daniel; Verhamme, Anne; Orlitová, Ivana; Mas-Hesse, J. Miguel; Otí-Floranes, Héctor; Cannon, John M.; Pardy, Stephen; Atek, Hakim; Kunth, Daniel; Laursen, Peter; Herenz, E. Christian

    2014-02-10

    We report new results regarding the Lyα output of galaxies, derived from the Lyman Alpha Reference Sample, and focused on Hubble Space Telescope imaging. For 14 galaxies we present intensity images in Lyα, Hα, and UV, and maps of Hα/Hβ, Lyα equivalent width (EW), and Lyα/Hα. We present Lyα and UV radial light profiles and show they are well-fitted by Sérsic profiles, but Lyα profiles show indices systematically lower than those of the UV (n ≈ 1-2 instead of ≳ 4). This reveals a general lack of the central concentration in Lyα that is ubiquitous in the UV. Photometric growth curves increase more slowly for Lyα than the far ultraviolet, showing that small apertures may underestimate the EW. For most galaxies, however, flux and EW curves flatten by radii ≈10 kpc, suggesting that if placed at high-z only a few of our galaxies would suffer from large flux losses. We compute global properties of the sample in large apertures, and show total Lyα luminosities to be independent of all other quantities. Normalized Lyα throughput, however, shows significant correlations: escape is found to be higher in galaxies of lower star formation rate, dust content, mass, and nebular quantities that suggest harder ionizing continuum and lower metallicity. Six galaxies would be selected as high-z Lyα emitters, based upon their luminosity and EW. We discuss the results in the context of high-z Lyα and UV samples. A few galaxies have EWs above 50 Å, and one shows f{sub esc}{sup Lyα} of 80%; such objects have not previously been reported at low-z.

  5. Star formation rate and metallicity of damped Lyman α absorbers in cosmological smoothed particle hydrodynamics simulations

    NASA Astrophysics Data System (ADS)

    Nagamine, K.; Springel, V.; Hernquist, L.

    2004-02-01

    We study the distribution of the star formation rate (SFR) and metallicity of damped Lyman α absorbers (DLAs) in the redshift range z= 0-4.5 using cosmological smoothed particle hydrodynamics (SPH) simulations of the Λ cold dark matter model. Our simulations include standard radiative cooling and heating with a uniform ultraviolet background, star formation, supernova (SN) feedback, as well as a phenomenological model for feedback by galactic winds. The latter allows us to examine, in particular, the effect of galactic outflows on the distribution of the SFR and metallicity of DLAs. We employ a `conservative entropy' formulation of SPH which alleviates numerical overcooling effects that affected earlier simulations. In addition, we utilize a series of simulations of varying box-size and particle number to investigate the impact of numerical resolution on our results. We find that there is a positive correlation between the projected stellar mass density and the neutral hydrogen column density (NHI) of DLAs for high NHI systems, and that there is a good correspondence in the spatial distribution of stars and DLAs in the simulations. The evolution of typical star-to-gas mass ratios in DLAs can be characterized by an increase from approximately 2 at z= 4.5 to 3 at z= 3, to 10 at z= 1 and finally to 20 at z= 0. We also find that the projected SFR density in DLAs follows the Kennicutt law well at all redshifts, and the simulated values are consistent with the recent observational estimates of this quantity by Wolfe, Prochaska & Gawiser. The rate of evolution in the mean metallicity of simulated DLAs as a function of redshift is mild, and is consistent with the rate estimated from observations. The predicted metallicity of DLAs is generally subsolar in our simulations, and there is a significant scatter in the distribution of DLA metallicity for a given NHI. However, we find that the median metallicity of simulated DLAs is close to that of Lyman-break galaxies, and is

  6. Stellar Populations and Radiative Transfer of Lyman Alpha Galaxies

    NASA Astrophysics Data System (ADS)

    Finkelstein, Steven L.; Rhoads, J. E.; Malhotra, S.; Pirzkal, N.; Wang, J.; Grogin, N.

    2007-05-01

    From stellar population modeling of z 4.5 Lyman alpha emitting galaxies (LAEs), we find that they are in general a young (t 10 Myr), low mass (M 108 MSun) subset of galaxies. We detected 22 LAE candidates in two or more broadband filters (g', r', i' and z') in the Large Area Lyman Alpha (LALA) survey Cetus Field with the MMT. These objects had calculated rest-frame equivalent widths (EWs) ranging from 5-800 Å. By comparing broad and narrow-band colors of these galaxies to stellar population models, we determined their ages and stellar masses. The highest EW objects were found to have an average age of 4 Myr, consistent with ongoing star formation. The lowest EW objects showed an age of 40 - 200 Myr, consistent with the expectation that larger numbers of old stars are causing low EWs. We found masses ranging from 2 x 107 MSun for the youngest objects in the sample to 2 x 109 MSun for the oldest. While young stellar populations are the generally accepted cause of the large Lyα EW in these objects, it is possible that dust effects could produce large EWs in older populations. This could occur if the ISM were sufficiently clumpy such that the continuum photons would suffer attenuation, while the Lyα photons would be resonantly scattered by the clumps, eventually escaping. We investigate this radiative transfer scenario with our second sample, which consists of six LAE candidates in the GOODS CDF-S, selected at z 4.5 with Hα narrow-band imaging obtained at CTIO. We will present results of stellar population studies of these objects, constraining their rest-frame UV with HST and their rest-frame optical with Spitzer.

  7. The Lyman-α Forest As a Cosmological Probe

    NASA Astrophysics Data System (ADS)

    Viel, M.

    2006-09-01

    The Lyman-α forest consists of the absorptions produced by intervening neutral hydrogen along lines of sight to distant quasars. About 80% percent of the baryons at z>2 are believed to reside in the filamentary structures probed by the absorptions. These intergalactic structures trace the underlying dark matter density field at scales and redshifts which cannot be probed by any other observable. After describing the essential physical aspects and a brief historical introduction, I will describe the first analytical models of the Lyman-α forest in the framework of cold dark matter scenarios. Then, I will focus on possible ways of extracting cosmological parameters from a set of observed quasar spectra, by running a grid of cosmological hydro-dynamical simulations. In particular, I will recover the linear dark matter power spectrum at z>2 and at scales of ˜1-40 comoving Mpc. I will address the significance of the results obtained especially when combined with the larger scales measurement of the power spectrum made by WMAP, giving constraints on the power spectrum amplitude, spectral index and its running. I will critically compare all the results obtained with those of the SDSS collaboration, based on a set of more than 3000 quasars at low resolution. Several physical aspects, which could affect the constraints on cosmological parameters, will be briefly discussed: feedback effects in the form of galactic winds, metal enrichment, the thermal state of the intergalactic medium and the amplitude and nature of the ultraviolet background. Finally, I will address further improvements that could be achieved in the next few years in this field both under the observational and the theoretical sides. In particular, the perspectives of measuring the cosmic expansion using absorption lines.

  8. Do Lyman-alpha photons escape from star-forming galaxies through dust holes?

    NASA Astrophysics Data System (ADS)

    France, Kevin; Wofford, A.; Leitherer, C.; Fleming, B.; McCandliss, S. R.; Nell, N.

    2014-01-01

    H I Lyman-alpha (LyA) is commonly used as a signpost for the entire galaxy at redshifts z>2, and yet spatially and kinematically resolved views of the local conditions within galaxies that determine the integrated properties of this line are scarce. We obtained Hubble Space Telescope (HST) images in continuum-subtracted LyA, H-alpha, H-beta, and far-UV continuum of three low-inclination spiral star-forming galaxies located at redshifts z=0.02, 0.03, and 0.05. This was accomplished using the UVIS and SBC channels of the Wide Field Camera 3 (WFC3) and the Advanced Camera for Surveys (ACS), respectively. Previous HST spectroscopy obtained by our team with the Cosmic Origins Spectrograph (COS) showed that the galaxies display different integrated LyA profiles within their central few kiloparsecs, i.e., pure absorption, single emission, and double emission, which are representative of what is observed between redshifts 0-3. This data is useful for establishing the relative importance of starburst phase, dust content, and gas kinematics in determining the LyA escape. We present preliminary results that combine our spectroscopic and imaging observations.

  9. On the selection of damped Lyman α systems using Mg II absorption at 2 < zabs < 4

    NASA Astrophysics Data System (ADS)

    Berg, T. A. M.; Ellison, S. L.; Prochaska, J. X.; Sánchez-Ramírez, R.; Lopez, S.; D'Odorico, V.; Becker, G.; Christensen, L.; Cupani, G.; Denney, K.; Worseck, G.

    2017-01-01

    The XQ-100 survey provides optical and near-infrared coverage of 36 blindly selected, intervening damped Lyman α systems (DLAs) at 2 < zabs < 4, simultaneously covering the Mg II doublet at λλ2796, 2803Å, and the Ly α transition. Using the XQ-100 DLA sample, we investigate the completeness of selecting DLA absorbers based on their Mg II rest-frame equivalent width (W0^{2796}) at these redshifts. Of the 29 DLAs with clean Mg II profiles, we find that six (20 per cent of DLAs) have W0^{2796} < 0.6 Å. The DLA incidence rate of W0^{2796} < 0.6 Å absorbers is a factor of ˜5 higher than what is seen in z ˜ 1 samples, indicating a potential evolution in the Mg II properties of DLAs with redshift. All of the W0^{2796} < 0.6 Å DLAs have low metallicities (-2.5 < [M/H] < -1.7), small velocity widths (v90 < 50 km s-1), and tend to have relatively low N(H I). We demonstrate that the exclusion of these low W0^{2796} DLAs results in a higher mean N(H I) which in turn leads to an ˜7 per cent increase in the cosmological gas density of H I of DLAs at 2 < zabs < 4; and that this exclusion has a minimal effect on the H I-weighted mean metallicity.

  10. Spectroscopic Confirmation of Two Lyman Break Galaxies at Redshift Beyond 7

    NASA Astrophysics Data System (ADS)

    Vanzella, E.; Pentericci, L.; Fontana, A.; Grazian, A.; Castellano, M.; Boutsia, K.; Cristiani, S.; Dickinson, M.; Gallozzi, S.; Giallongo, E.; Giavalisco, M.; Maiolino, R.; Moorwood, A.; Paris, D.; Santini, P.

    2011-04-01

    We report the spectroscopic confirmation of two Lyman break galaxies at redshift >7. The galaxies were observed as part of an ultra-deep spectroscopic campaign with FORS2 at the ESO/VLT for the confirmation of z ~= 7 "z-band dropout" candidates selected from our VLT/Hawk-I imaging survey. Both galaxies show a prominent emission line at 9735 Å and 9858 Å, respectively: the lines have fluxes of ~(1.6-1.2) × 10-17 erg s-1 cm-2 and exhibit a sharp decline on the blue side and a tail on the red side. The asymmetry is quantitatively comparable to the observed asymmetry in z ~ 6 Lyα lines, where absorption by neutral hydrogen in the intergalactic medium (IGM) truncates the blue side of the emission-line profile. We carefully evaluate the possibility that the galaxies are instead at lower redshift and we are observing either [O II], [O III], or Hα emission: however from the spectroscopic and the photometric data we conclude that there are no other plausible identifications, except for Lyα at redshift >7, implying that these are two of the most robust redshift determination for galaxies in the reionization epoch. Based on their redshifts and broadband photometry, we derive limits on the star formation rate and on the ultraviolet spectral slopes of the two galaxies. We argue that these two galaxies alone are unlikely to have ionized the IGM in their surroundings.

  11. Solid-state continuous Lyman-alpha source for laser-cooling of antihydrogen

    SciTech Connect

    Walz, Jochen; Beyer, Thomas; Kolbe, Daniel; Markert, Frank; Muellers, Andreas; Scheid, Martin

    2008-08-08

    Cooling antihydrogen atoms is important for future experiments both to test the fundamental CPT symmetry by high-resolution laser spectroscopy and also to measure the gravitational acceleration of antimatter. Laser-cooling of antihydrogen can be done on the strong 1 S-2 P transition at the wavelength of Lyman-alpha (121.6 nm). Ongoing work to set up a solid-state continuous-wave laser source at Lyman-alpha is described.

  12. Mapping High-Velocity H-alpha and Lyman-alpha Emission from Supernova 1987A

    NASA Technical Reports Server (NTRS)

    France, Kevin; McCray, Richard; Fransson, Claes; Larsson, Josefin; Frank, Kari A.; Burrows, David N.; Challis, Peter; Kirshner, Robert P.; Chevalier, Roger A.; Garnavich, Peter; Heng, Kevin; Lawrence, Stephen S.; Lundqvist, Peter; Smith, Nathan; Sonneborn, George

    2015-01-01

    We present new Hubble Space Telescope images of high-velocity H-alpha and Lyman-alpha emission in the outer debris of SN 1987A. The H-alpha images are dominated by emission from hydrogen atoms crossing the reverse shock. For the first time we observe emission from the reverse shock surface well above and below the equatorial ring, suggesting a bipolar or conical structure perpendicular to the ring plane. Using the H-alpha imaging, we measure the mass flux of hydrogen atoms crossing the reverse shock front, in the velocity intervals (-7,500 < V(sub obs) < -2,800 km/s) and (1,000 < V(sub obs) < 7,500 km/s), ?M(sub H) = 1.2 × 10(exp -3) M/ y. We also present the first Lyman-alpha imaging of the whole remnant and new Chandra X-ray observations. Comparing the spatial distribution of the Lyman-alpha and X-ray emission, we observe that the majority of the high-velocity Lyman-alpha emission originates interior to the equatorial ring. The observed Lyman-alpha/H-alpha photon ratio, R(L-alpha/H-alpha) approx. = 17, is significantly higher than the theoretically predicted ratio of approx. = 5 for neutral atoms crossing the reverse shock front. We attribute this excess to Lyman-alpha emission produced by X-ray heating of the outer debris. The spatial orientation of the Lyman-alpha and X-ray emission suggests that X-ray heating of the outer debris is the dominant Lyman-alpha production mechanism in SN 1987A at this phase in its evolution.

  13. The impact of different physical processes on the statistics of Lyman-limit and damped Lyman α absorbers

    NASA Astrophysics Data System (ADS)

    Altay, Gabriel; Theuns, Tom; Schaye, Joop; Booth, C. M.; Dalla Vecchia, Claudio

    2013-12-01

    We compute the z = 3 neutral hydrogen column density distribution function f(NHI) for 19 simulations drawn from the Overwhelmingly Large Simulations project using a post-processing correction for self-shielding calculated with full radiative transfer of the ionizing background radiation. We investigate how different physical processes and parameters affect the abundance of Lyman-limit systems (LLSs) and damped Lyman α absorbers including: (i) metal-line cooling; (ii) the efficiency of feedback from supernovae and active galactic nuclei; (iii) the effective equation of state for the interstellar medium; (iv) cosmological parameters; (v) the assumed star formation law and (vi) the timing of hydrogen reionization. We find that the normalization and slope, D = d log _{10} f /d log _{10} N_{H I}, of f(NHI) in the LLS regime are robust to changes in these physical processes. Among physically plausible models, f(NHI) varies by less than 0.2 dex and D varies by less than 0.18 for LLSs. This is primarily due to the fact that these uncertain physical processes mostly affect star-forming gas which contributes less than 10 per cent to f(NHI) in the LLS column density range. At higher column densities, variations in f(NHI) become larger (approximately 0.5 dex at f(NHI) = 1022 cm-2 and 1.0 dex at f(NHI) = 1022 cm-2) and molecular hydrogen formation also becomes important. Many of these changes can be explained in the context of self-regulated star formation in which the amount of star-forming gas in a galaxy will adjust such that outflows driven by feedback balance inflows due to accretion. Tools to reproduce all figures in this work can be found at the following url: https://bitbucket.org/galtay/hi-cddf-owls-1

  14. Neutrino signatures on the high-transmission regions of the Lyman α forest

    NASA Astrophysics Data System (ADS)

    Villaescusa-Navarro, F.; Vogelsberger, M.; Viel, M.; Loeb, A.

    2013-06-01

    We quantify the impact of massive neutrinos on the statistics of low-density regions in the intergalactic medium as probed by the Lyman α forest at redshifts z = 2.2-4. Based on mock but realistic quasar (QSO) spectra extracted from hydrodynamic simulations with cold dark matter, baryons and neutrinos, we find that the probability distribution of weak Lyman α absorption features, as sampled by Lyman α flux regions at high transmissivity, is strongly affected by the presence of massive neutrinos. We show that systematic errors affecting the Lyman α forest reduce but do not erase the neutrino signal. Using the Fisher matrix formalism, we conclude that the sum of the neutrino masses can be measured, using the method proposed in this paper, with a precision smaller than 0.4 eV using a catalogue of 200 high-resolution (signal-to-noise ratio ˜100) QSO spectra. This number reduces to 0.27 eV by making use of reasonable priors in the other parameters that also affect the statistics of the high-transitivity regions of the Lyman α forest. The constraints obtained with this method can be combined with independent bounds from the cosmic microwave background, large-scale structures and measurements of the matter power spectrum from the Lyman α forest to produce tighter upper limits on the sum of the masses of the neutrinos.

  15. Discovery of a very Lyman-α-luminous quasar at z = 6.62

    NASA Astrophysics Data System (ADS)

    Koptelova, Ekaterina; Hwang, Chorng-Yuan; Yu, Po-Chieh; Chen, Wen-Ping; Guo, Jhen-Kuei

    2017-02-01

    Distant luminous quasars provide important information on the growth of the first supermassive black holes, their host galaxies and the epoch of reionization. The identification of quasars is usually performed through detection of their Lyman-α line redshifted to 0.9 microns at z > 6.5. Here, we report the discovery of a very Lyman-α luminous quasar, PSO J006.1240 + 39.2219 at redshift z = 6.618, selected based on its red colour and multi-epoch detection of the Lyman-α emission in a single near-infrared band. The Lyman-α line luminosity of PSO J006.1240 + 39.2219 is unusually high and estimated to be 0.8 × 1012 Solar luminosities (about 3% of the total quasar luminosity). The Lyman-α emission of PSO J006.1240 + 39.2219 shows fast variability on timescales of days in the quasar rest frame, which has never been detected in any of the known high-redshift quasars. The high luminosity of the Lyman-α line, its narrow width and fast variability resemble properties of local Narrow-Line Seyfert 1 galaxies which suggests that the quasar is likely at the active phase of the black hole growth accreting close or even beyond the Eddington limit.

  16. First detection of cosmic microwave background lensing and Lyman-α forest bispectrum

    NASA Astrophysics Data System (ADS)

    Doux, Cyrille; Schaan, Emmanuel; Aubourg, Eric; Ganga, Ken; Lee, Khee-Gan; Spergel, David N.; Tréguer, Julien

    2016-11-01

    We present the first detection of a correlation between the Lyman-α forest and cosmic microwave background gravitational lensing. For each Lyman-α forest in SDSS-III/BOSS DR12, we correlate the one-dimensional power spectrum with the cosmic microwave background lensing convergence on the same line of sight from Planck. This measurement constitutes a position-dependent power spectrum, or a squeezed bispectrum, and quantifies the nonlinear response of the Lyman-α forest power spectrum to a large-scale overdensity. The signal is measured at 5 σ and is consistent with the expectation of the standard Λ CDM cosmological model. We measure the linear bias of the Lyman-α forest with respect to the dark matter distribution and constrain a combination of nonlinear terms including the nonlinear bias. This new observable provides a consistency check for the Lyman-α forest as a large-scale structure probe and tests our understanding of the relation between intergalactic gas and dark matter. In the future, it could be used to test hydrodynamical simulations and calibrate the relation between the Lyman-α forest and dark matter.

  17. Discovery of a very Lyman-α-luminous quasar at z = 6.62.

    PubMed

    Koptelova, Ekaterina; Hwang, Chorng-Yuan; Yu, Po-Chieh; Chen, Wen-Ping; Guo, Jhen-Kuei

    2017-02-02

    Distant luminous quasars provide important information on the growth of the first supermassive black holes, their host galaxies and the epoch of reionization. The identification of quasars is usually performed through detection of their Lyman-α line redshifted to 0.9 microns at z > 6.5. Here, we report the discovery of a very Lyman-α luminous quasar, PSO J006.1240 + 39.2219 at redshift z = 6.618, selected based on its red colour and multi-epoch detection of the Lyman-α emission in a single near-infrared band. The Lyman-α line luminosity of PSO J006.1240 + 39.2219 is unusually high and estimated to be 0.8 × 10(12) Solar luminosities (about 3% of the total quasar luminosity). The Lyman-α emission of PSO J006.1240 + 39.2219 shows fast variability on timescales of days in the quasar rest frame, which has never been detected in any of the known high-redshift quasars. The high luminosity of the Lyman-α line, its narrow width and fast variability resemble properties of local Narrow-Line Seyfert 1 galaxies which suggests that the quasar is likely at the active phase of the black hole growth accreting close or even beyond the Eddington limit.

  18. Discovery of a very Lyman-α-luminous quasar at z = 6.62

    PubMed Central

    Koptelova, Ekaterina; Hwang, Chorng-Yuan; Yu, Po-Chieh; Chen, Wen-Ping; Guo, Jhen-Kuei

    2017-01-01

    Distant luminous quasars provide important information on the growth of the first supermassive black holes, their host galaxies and the epoch of reionization. The identification of quasars is usually performed through detection of their Lyman-α line redshifted to 0.9 microns at z > 6.5. Here, we report the discovery of a very Lyman-α luminous quasar, PSO J006.1240 + 39.2219 at redshift z = 6.618, selected based on its red colour and multi-epoch detection of the Lyman-α emission in a single near-infrared band. The Lyman-α line luminosity of PSO J006.1240 + 39.2219 is unusually high and estimated to be 0.8 × 1012 Solar luminosities (about 3% of the total quasar luminosity). The Lyman-α emission of PSO J006.1240 + 39.2219 shows fast variability on timescales of days in the quasar rest frame, which has never been detected in any of the known high-redshift quasars. The high luminosity of the Lyman-α line, its narrow width and fast variability resemble properties of local Narrow-Line Seyfert 1 galaxies which suggests that the quasar is likely at the active phase of the black hole growth accreting close or even beyond the Eddington limit. PMID:28150701

  19. Copernicus measurement of the Jovian Lyman-alpha emission and its aeronomical significance

    NASA Technical Reports Server (NTRS)

    Atreya, S. K.; Kerr, R. B.; Upson, W. L., II; Festou, M. C.; Donahue, T. M.; Barker, E. S.; Cochran, W. D.; Bertaux, J. L.

    1982-01-01

    It is pointed out that the intensity of the Lyman-alpha emission is a good indicator of the principal aeronomical processes on the major planets. The high-resolution ultraviolet spectrometer aboard the Orbiting Astronomical Observatory Copernicus was used in 1980 April and May to detect the Jovian Lyman-alpha emission by spectroscopically discriminating it from other Doppler shifted Lyman-alpha emissions such as those of the geocorona, and the interplanetary medium. Taking into consideration the reported emission data, it appears that an unusually large energy input due to the particle precipitation in the auroral region must have been responsible for the large observed Lyman-alpha intensity during the Voyager encounter. At most other times, the observed Jovian Lyman-alpha intensity can be explained, within the range of statistical uncertainty, by a model that takes into consideration the solar EUV flux, the solar Lyman-alpha flux, the high exospheric temperature, and the eddy diffusion coefficient without energy input from the auroral sources.

  20. An extreme O III emitter at z=3.2: a low metallicity Lyman continuum source

    NASA Astrophysics Data System (ADS)

    de Barros, S.; Vanzella, E.

    2015-12-01

    We investigate the physical properties of a Lyman continuum emitter candidate at z=3.212 with photometric coverage from U to MIPS 24μm band and VIMOS/VLT and MOSFIRE/Keck spectroscopy. Investigation of the UV spectrum confirms a direct spectroscopic detection of the Lyman continuum emission with S/N>5. Non-zero Lyα flux at the systemic redshift and high Lyman-α escape fraction suggest a low HI column density. The weak C and Si low-ionization absorption lines are also consistent with a low covering fraction along the line of sight. The O IIIdoub+Hβ equivalent width is one of the largest reported for a galaxy at z>3 (EW(O IIIdoub+Hβ)} ≃q 1600Å, rest-frame; 6700Å observed-frame) and the NIR spectrum shows that this is mainly due to an extremely strong [OIII] emission. The large observed O III/O II ratio (>10) and high ionization parameter are consistent with prediction from photoionization models in case of a density-bounded nebula scenario. This source is currently the first high-z example of a Lyman continuum emitter exhibiting indirect and direct evidences of a Lyman continuum leakage and having physical properties consistent with theoretical expectation from Lyman continuum emission from a density-bounded nebula.

  1. Time series gene expression profiling and temporal regulatory pathway analysis of BMP6 induced osteoblast differentiation and mineralization.

    PubMed

    Luo, Weijun; Friedman, Michael S; Hankenson, Kurt D; Woolf, Peter J

    2011-05-23

    BMP6 mediated osteoblast differentiation plays a key role in skeletal development and bone disease. Unfortunately, the signaling pathways regulated by BMP6 are largely uncharacterized due to both a lack of data and the complexity of the response. To better characterize the signaling pathways responsive to BMP6, we conducted a time series microarray study to track BMP6 induced osteoblast differentiation and mineralization. These temporal data were analyzed using a customized gene set analysis approach to identify temporally coherent sets of genes that act downstream of BMP6. Our analysis identified BMP6 regulation of previously reported pathways, such as the TGF-beta pathway. We also identified previously unknown connections between BMP6 and pathways such as Notch signaling and the MYB and BAF57 regulatory modules. In addition, we identify a super-network of pathways that are sequentially activated following BMP6 induction. In this work, we carried out a microarray-based temporal regulatory pathway analysis of BMP6 induced osteoblast differentiation and mineralization using GAGE method. This novel temporal analysis is more informative and powerful than the classical static pathway analysis in that: (1) it captures the interconnections between signaling pathways or functional modules and demonstrates the even higher level organization of molecular biological systems; (2) it describes the temporal perturbation patterns of each pathway or module and their dynamic roles in osteoblast differentiation. The same set of experimental and computational strategies employed in our work could be useful for studying other complex biological processes. © 2011 Luo et al; licensee BioMed Central Ltd.

  2. Novel gene targets detected by genomic profiling in a consecutive series of 126 adults with acute lymphoblastic leukemia.

    PubMed

    Safavi, Setareh; Hansson, Markus; Karlsson, Karin; Biloglav, Andrea; Johansson, Bertil; Paulsson, Kajsa

    2015-01-01

    In contrast to acute lymphoblastic leukemia in children, adult cases of this disease are associated with a very poor prognosis. In order to ascertain whether the frequencies and patterns of submicroscopic changes, identifiable with single nucleotide polymorphism array analysis, differ between childhood and adult acute lymphoblastic leukemia, we performed single nucleotide polymorphism array analyses of 126 adult cases, the largest series to date, including 18 paired diagnostic and relapse samples. Apart from identifying characteristic microdeletions of the CDKN2A, EBF1, ETV6, IKZF1, PAX5 and RB1 genes, the present study uncovered novel, focal deletions of the BCAT1, BTLA, NR3C1, PIK3AP1 and SERP2 genes in 2-6% of the adult cases. IKZF1 deletions were associated with B-cell precursor acute lymphoblastic leukemia (P=0.036), BCR-ABL1-positive acute lymphoblastic leukemia (P<0.001), and higher white blood cell counts (P=0.005). In addition, recurrent deletions of RASSF3 and TOX were seen in relapse samples. Comparing paired diagnostic/relapse samples revealed identical changes at diagnosis and relapse in 27%, clonal evolution in 22%, and relapses evolving from ancestral clones in 50%, akin to what has previously been reported in pediatric acute lymphoblastic leukemia and indicating that the mechanisms of relapse may be similar in adult and childhood cases. These findings provide novel insights into the leukemogenesis of adult acute lymphoblastic leukemia, showing similarities to childhood disease in the pattern of deletions and the clonal relationship between diagnostic and relapse samples, but with the adult cases harboring additional aberrations that have not been described in pediatric acute lymphoblastic leukemia.

  3. Physical properties and small-scale structure of the Lyman-alpha forest: Inversion of the HE 1122-1628 UVES spectrum

    NASA Astrophysics Data System (ADS)

    Rollinde, E.; Petitjean, P.; Pichon, C.

    2001-09-01

    We study the physical properties of the Lyman-alpha forest by applying the inversion method described by Pichon et al. (\\cite{Pichon01}) to the high resolution and high S/N ratio spectrum of the zem=2.40 quasar HE 1122-1628 obtained during Science Verification of UVES at the VLT. We compare the column densities obtained with the new fitting procedure with those derived using standard Voigt profile methods. The agreement is good and gives confidence in the new description of the Lyman-alpha forest as a continuous field as derived from our method. We show that the observed number density of lines with log N > 13 and 14 is, respectively, 50 and 250 per unit redshift at z ~ 2. We study the physical state of the gas, neglecting peculiar velocities, assuming a relation between the overdensity and the temperature, T={/line T}(rho (x)/{bar rho })2beta . There is an intrinsic degeneracy between the parameters beta and {/line T}. We demonstrate that, at a fixed beta , the temperature at mean density, {/line T}, can be uniquely extracted, however. While applying the method to HE 1122-1628, we conclude that for 0.2 < beta < 0.3, 6000 < {/line T} < 15 000 K at z ~ 2. We investigate the small-scale structure of strong absorption lines using the information derived from the Lyman-beta , Lyman-gamma and C iv profiles. Introducing the Lyman-beta line in the fit allows us to reconstruct the density field up to rho /{bar rho } ~ 10 instead of 5 for the Lyman-alpha line only. The neutral hydrogen density is of the order of ~ 2x 10-9 cm-3 and the C IV/H I ratio varies from about 0.001 to 0.01 within the complexes of total column density N(H I) ~ 1015 cm-2. Such numbers are expected for photo-ionized gas of density nH ~ 10-4 cm-3 and [C/H] ~ -2.5. There may be small velocity shifts ( ~ 10 km s-1) between the peaks in the C iv and H I density profiles. Although the statistics is small, it seems that C IV/H I and nHI are anti-correlated. This could be a consequence of the high

  4. The Lyman alpha reference sample. III. Properties of the neutral ISM from GBT and VLA observations

    SciTech Connect

    Pardy, Stephen A.; Cannon, John M.; Melinder, Jens E-mail: jcannon@macalester.edu; and others

    2014-10-20

    We present new H I imaging and spectroscopy of the 14 UV-selected star-forming galaxies in the Lyman Alpha Reference Sample (LARS), aimed for a detailed study of the processes governing the production, propagation, and escape of Lyα photons. New H I spectroscopy, obtained with the 100 m Green Bank Telescope (GBT), robustly detects the H I spectral line in 11 of the 14 observed LARS galaxies (although the profiles of two of the galaxies are likely confused by other sources within the GBT beam); the three highest redshift galaxies are not detected at our current sensitivity limits. The GBT profiles are used to derive fundamental H I line properties of the LARS galaxies. We also present new pilot H I spectral line imaging of five of the LARS galaxies obtained with the Karl G. Jansky Very Large Array (VLA). This imaging localizes the H I gas and provides a measurement of the total H I mass in each galaxy. In one system, LARS 03 (UGC 8335 or Arp 238), VLA observations reveal an enormous tidal structure that extends over 160 kpc from the main interacting systems and that contains >10{sup 9} M {sub ☉} of H I. We compare various H I properties with global Lyα quantities derived from Hubble Space Telescope measurements. The measurements of the Lyα escape fraction are coupled with the new direct measurements of H I mass and significantly disturbed H I velocities. Our robustly detected sample reveals tentative correlations between the total H I mass and linewidth, and key Lyα tracers. Further, on global scales, these data support a complex coupling between Lyα propagation and the H I properties of the surrounding medium.

  5. Development of Flight Slit-Jaw Optics for Chromospheric Lyman-Alpha SpectroPolarimeter

    NASA Technical Reports Server (NTRS)

    Kubo, Masahito; Suematsu, Yoshinori; Kano, Ryohei; Bando, Takamasa; Hara, Hirohisa; Narukage, Noriyuki; Katsukawa, Yukio; Ishikawa, Ryoko; Ishikawa, Shin-nosuke; Kobiki, Toshihiko; hide

    2015-01-01

    In sounding rocket experiment CLASP, I have placed a slit a mirror-finished around the focal point of the telescope. The light reflected by the mirror surface surrounding the slit is then imaged in Slit-jaw optical system, to obtain the a-ray Lyman secondary image. This image, not only to use the real-time image in rocket flight rocket oriented direction selection, and also used as a scientific data showing the spatial structure of the Lyman alpha emission line intensity distribution and solar chromosphere around the observation area of the polarimetric spectroscope. Slit-jaw optical system is a two off-axis mirror unit part including a parabolic mirror and folding mirror, Lyman alpha transmission filter, the optical system magnification 1x consisting camera. The camera is supplied from the United States, and the other was carried out fabrication and testing in all the Japanese side. Slit-jaw optical system, it is difficult to access the structure, it is necessary to install the low place clearance. Therefore, influence the optical performance, the fine adjustment is necessary optical elements are collectively in the form of the mirror unit. On the other hand, due to the alignment of the solar sensor in the US launch site, must be removed once the Lyman alpha transmission filter holder including a filter has a different part from the mirror unit. In order to make the structure simple, stray light measures Aru to concentrate around Lyman alpha transmission filter. To overcome the difficulties of performing optical alignment in Lyman alpha wavelength absorbed by the atmosphere, it was planned 'following four steps in order to reduce standing time alignment me. 1. is measured in advance refractive index at Lyman alpha wavelength of Lyman alpha transmission filter (121.567nm), to prepare a visible light Firuwo having the same optical path length in the visible light (630nm).2. The mirror structure CLASP before mounting unit standing, dummy slit and camera standing

  6. Development of Flight Slit-Jaw Optics for Chromospheric Lyman-Alpha SpectroPolarimeter

    NASA Technical Reports Server (NTRS)

    Kubo, Masahito; Suematsu, Yoshinori; Kano, Ryohei; Bando, Takamasa; Hara, Hirohisa; Narukage, Noriyuki; Katsukawa, Yukio; Ishikawa, Ryoko; Ishikawa, Shin-nosuke; Kobiki, Toshihiko; hide

    2015-01-01

    In sounding rocket experiment CLASP, I have placed a slit a mirror-finished around the focal point of the telescope. The light reflected by the mirror surface surrounding the slit is then imaged in Slit-jaw optical system, to obtain the alpha-ray Lyman secondary image. This image, not only to use the real-time image in rocket flight rocket oriented direction selection, and also used as a scientific data showing the spatial structure of the Lyman alpha emission line intensity distribution and solar chromosphere around the observation area of the polarimetric spectroscope. Slit-jaw optical system is a two off-axis mirror unit part including a parabolic mirror and folding mirror, Lyman alpha transmission filter, the optical system magnification 1x consisting camera. The camera is supplied from the United States, and the other was carried out fabrication and testing in all the Japanese side. Slit-jaw optical system, it is difficult to access the structure, it is necessary to install the low place clearance. Therefore, influence the optical performance, the fine adjustment is necessary optical elements are collectively in the form of the mirror unit. On the other hand, due to the alignment of the solar sensor in the US launch site, must be removed once the Lyman alpha transmission filter holder including a filter has a different part from the mirror unit. In order to make the structure simple, stray light measures Aru to concentrate around Lyman alpha transmission filter. To overcome the difficulties of performing optical alignment in Lyman alpha wavelength absorbed by the atmosphere, it was planned following four steps in order to reduce standing time alignment me. 1: is measured in advance refractive index at Lyman alpha wavelength of Lyman alpha transmission filter (121.567nm), to prepare a visible light Firuwo having the same optical path length in the visible light (630nm). 2: The mirror structure CLASP before mounting unit standing, dummy slit and camera standing

  7. Jovian Equatorial H Lyman-alpha and the Ionosphere

    NASA Astrophysics Data System (ADS)

    Ballester, Gilda E.

    An excess of H Ly alpha emission has been a persistent feature in Jupiter's equatorial upper atmosphere since its discovery in 1978. This Ly alpha 'bulge' was found by high-resolution IUE observations to be due to broadening of the Jovian line increasing the resonant scattering of the solar Ly alpha, rather than from a local enhancement in the H density. The line broadening implies that the H column at the bulge is disturbed by a localized, non-thermal process, and two mechanisms have been proposed to explain this: one by the generation of turbulence from strong thermospheric winds or jets meeting at the bulge region and originating in the active Jovian auroral zones, the other involving a superthermal population of H atoms produced by a process analogous to the equatorial anomaly and tropical arcs on the Earth. Some line broadening was also observed in the off-bulge region while modelling of the usual bulge profile does not predict this behavior, but these observations may have been performed at a time of an unusually large extension of the bulge. We propose to make a series of high-dispersion observations (of improved S/N) for a detailed longitudinal study of the line profile which would be of benefit independently of the particular bulge conditions (to be determined with low-dispersion exposures). In addition, new insight will be gained with simultaneous ground-based observations of the newly discovered global ionospheric H3+ emissions. These emissions are diagnostic of the ionospheric temperature and ion density, and have already shown very particular characteristics in the H Ly alpha bulge region. Coordinated observations of the whole longitudinal range should therefore set new constraints on the mechanisms operating in the Jovian equatorial upper atmosphere.

  8. The Lyman alpha reference sample. VII. Spatially resolved Hα kinematics

    NASA Astrophysics Data System (ADS)

    Herenz, Edmund Christian; Gruyters, Pieter; Orlitova, Ivana; Hayes, Matthew; Östlin, Göran; Cannon, John M.; Roth, Martin M.; Bik, Arjan; Pardy, Stephen; Otí-Floranes, Héctor; Mas-Hesse, J. Miguel; Adamo, Angela; Atek, Hakim; Duval, Florent; Guaita, Lucia; Kunth, Daniel; Laursen, Peter; Melinder, Jens; Puschnig, Johannes; Rivera-Thorsen, Thøger E.; Schaerer, Daniel; Verhamme, Anne

    2016-03-01

    We present integral field spectroscopic observations with the Potsdam Multi-Aperture Spectrophotometer of all 14 galaxies in the z ~ 0.1 Lyman Alpha Reference Sample (LARS). We produce 2D line-of-sight velocity maps and velocity dispersion maps from the Balmer α (Hα) emission in our data cubes. These maps trace the spectral and spatial properties of the LARS galaxies' intrinsic Lyα radiation field. We show our kinematic maps that are spatially registered onto the Hubble Space Telescope Hα and Lyman α (Lyα) images. We can conjecture a causal connection between spatially resolved Hα kinematics and Lyα photometry for individual galaxies, however, no general trend can be established for the whole sample. Furthermore, we compute the intrinsic velocity dispersion σ0, the shearing velocity vshear, and the vshear/σ0 ratio from our kinematic maps. In general LARS galaxies are characterised by high intrinsic velocity dispersions (54 km s-1 median) and low shearing velocities (65 km s-1 median). The vshear/σ0 values range from 0.5 to 3.2 with an average of 1.5. It is noteworthy that five galaxies of the sample are dispersion-dominated systems with vshear/σ0< 1, and are thus kinematically similar to turbulent star-forming galaxies seen at high redshift. When linking our kinematical statistics to the global LARS Lyα properties, we find that dispersion-dominated systems show higher Lyα equivalent widths and higher Lyα escape fractions than systems with vshear/σ0> 1. Our result indicates that turbulence in actively star-forming systems is causally connected to interstellar medium conditions that favour an escape of Lyα radiation. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).The reduced data cubes (FITS files) are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130

  9. First Simultaneous Detection of Lyman-alpha Emission and Lyman Break from a Galaxy at Redshift 7.51 from Faint Infrared Grism Survey (FIGS)

    NASA Astrophysics Data System (ADS)

    Tilvi, Vithal; Pirzkal, Norbert; Malhotra, Sangeeta; Finkelstein, Steven L.; Rhoads, James E.; Windhorst, Rogier A.; Grogin, Norman A.; Koekemoer, Anton M.; Zakamska, Nadia L.; Ryan, Russell E.; Christensen, Lise; Hathi, Nimish P.; Pharo, John; Joshi, Bhavin; Yang, Huan; Gronwall, Caryl; Cimatti, Andrea; Walsh, J.; O'Connell, Robert W.; Straughn, Amber; Östlin, Göran; Rothberg, Barry; Livermore, Rachael C.; Hibon, Pascale; Gardner, Jonathan P.; FIGS Team

    2017-01-01

    Galaxies at high-redshifts provide a powerful tool to probe cosmic dawn, and therefore it is crucial to reliably identify these galaxies. Here, we present an unambiguous and first simultaneous detection of a Lyman-alpha line and a Lyman break from a galaxy (FIGS_GN1_1292) at z=7.51, observed in the Faint Infrared Grism Survey (FIGS: PI Mlahotra). FIGS is currently the most sensitive G102 grism survey, with 160-orbit depth equally distributed in four different fields in GOODS-N and GOODS-S. FIGS_GN1_1292 is detected independently in multiple position angles, and has a Lyman-alpha line flux of 1.06e-17 erg/s/cm^2, nearly a factor of four higher than in the archival MOSFIRE spectroscopic observations. This higher flux in the grism data is consistent with other recent observations implying that ground-based near-infrared spectroscopy may underestimate the total emission line fluxes, and if confirmed, can have strong implications for reionization studies that are based on ground-based Lyman-alpha measurements. The successful detection of continuum in such a high-redshift galaxy demonstrates the sensitivity of the FIGS survey, and the capability of grism spectroscopy to study the epoch of reionization using upcoming missions like the Wide Field Infrared Survey Telescope (WFIRST).

  10. A Spectroscopic Redshift Measurement for a Luminous Lyman Break Galaxy at z = 7.730 Using Keck/MOSFIRE

    NASA Astrophysics Data System (ADS)

    Oesch, P. A.; van Dokkum, P. G.; Illingworth, G. D.; Bouwens, R. J.; Momcheva, I.; Holden, B.; Roberts-Borsani, G. W.; Smit, R.; Franx, M.; Labbé, I.; González, V.; Magee, D.

    2015-05-01

    We present a spectroscopic redshift measurement of a very bright Lyman break galaxy at z=7.7302+/- 0.0006 using the Keck/Multi-Object Spectrometer for Infra-Red Exploration. The source was pre-selected photometrically in the EGS field as a robust z ˜ 8 candidate with H = 25.0 mag based on optical non-detections and a very red Spitzer/IRAC [3.6]-[4.5] broad-band color driven by high equivalent width [O iii]+Hβ line emission. The Lyα line is reliably detected at 6.1σ and shows an asymmetric profile as expected for a galaxy embedded in a relatively neutral intergalactic medium near the Planck peak of cosmic reionization. The line has a rest-frame equivalent width of E{{W}0}=21+/- 4 Å and is extended with {{V}FWHM}=360-70+90 km s-1. The source is perhaps the brightest and most massive z ˜ 8 Lyman break galaxy in the full CANDELS and BoRG/HIPPIES surveys, having already assembled {{10}9.9+/- 0.2} {{M}⊙ } of stars at only 650 Myr after the Big Bang. The spectroscopic redshift measurement sets a new redshift record for galaxies. This enables reliable constraints on the stellar mass, star formation rate, and formation epoch, as well as combined [O iii]+Hβ line equivalent widths. The redshift confirms that the IRAC [4.5] photometry is very likely dominated by line emission with EW0([O iii]+Hβ) = 720-150+180 Å. This detection thus adds to the evidence that extreme rest-frame optical emission lines are a ubiquitous feature of early galaxies promising very efficient spectroscopic follow-up in the future with infrared spectroscopy using the James Webb Space Telescope and, later, ELTs.

  11. Sub-Lyman-alpha observations of supernova remnants

    NASA Technical Reports Server (NTRS)

    Long, K. S.

    1993-01-01

    The first map of O VI lambda 1035 emission of the Cygnus Loop has now been obtained with Voyager. The first good spectra of the sub-Lyman-alpha region in the Cygnus Loop and in the Large Magellanic Cloud (LMC) remnant N49 have been obtained with the Hopkins Ultraviolet Telescope. The lines detected below 1200 A include S VI lambda lambda 933,945, C III lambda 977, N III lambda 991, and O VI lambda lambda 1032,1038. The O VI luminosities of the Cygnus Loop and of N49 exceed their soft X-ray luminosities. There is O VI emission at the primary shock front in the Cygnus Loop and from the bright optical filaments. The HUT spectra of the Cygnus Loop can be interpreted in terms of shocks with velocities of 170-190 km/s; the differences between the two spectra are due to the time since the beginning of the shock-cloud encounter.

  12. Sub-Lyman-alpha observations of supernova remnants

    NASA Technical Reports Server (NTRS)

    Long, K. S.

    1993-01-01

    The first map of O VI lambda 1035 emission of the Cygnus Loop has now been obtained with Voyager. The first good spectra of the sub-Lyman-alpha region in the Cygnus Loop and in the Large Magellanic Cloud (LMC) remnant N49 have been obtained with the Hopkins Ultraviolet Telescope. The lines detected below 1200 A include S VI lambda lambda 933,945, C III lambda 977, N III lambda 991, and O VI lambda lambda 1032,1038. The O VI luminosities of the Cygnus Loop and of N49 exceed their soft X-ray luminosities. There is O VI emission at the primary shock front in the Cygnus Loop and from the bright optical filaments. The HUT spectra of the Cygnus Loop can be interpreted in terms of shocks with velocities of 170-190 km/s; the differences between the two spectra are due to the time since the beginning of the shock-cloud encounter.

  13. Lyman continuum leaking AGN in the SSA22 field

    NASA Astrophysics Data System (ADS)

    Micheva, Genoveva; Iwata, Ikuru; Inoue, Akio K.

    2017-02-01

    Subaru/SuprimeCam narrow-band photometry of the SSA22 field reveals the presence of four Lyman continuum (LyC) candidates among a sample of 14 active galactic nuclei (AGNs). Two show offsets and likely have stellar LyCin nature or are foreground contaminants. The remaining two LyC candidates are type I AGN. We argue that the average LyC escape fraction of high-redshift, low-luminosity AGN is not likely to be unity, as often assumed in the literature. From direct measurement we obtain the average LyC-to-UV flux density ratio and ionizing emissivity for a number of AGN classes and find it at least a factor of 2 lower than values obtained assuming fesc = 1. Comparing to recent Ly α forest measurements, AGNs at redshift z ˜ 3 make up at most ˜12 per cent and as little as ˜5 per cent of the total ionizing budget. Our results suggest that AGNs are unlikely to dominate the ionization budget of the Universe at high redshifts.

  14. Haro 11: Where is the Lyman Continuum Source?

    NASA Astrophysics Data System (ADS)

    Keenan, Ryan P.; Oey, M. S.; Jaskot, Anne; James, Bethan

    2017-01-01

    Haro 11 is the best known source of Lyman continuum (LyC) emission in the local universe and is thought to be an analog of the early galaxies that drove cosmic reionization. The source of LyC emission within Haro 11 has not yet been identified, since the LyC detection is unresolved. To map the optically thin regions in this galaxy, we apply our technique of ionization parameter mapping, which uses continuum-subtracted, HST WFC3 and ACS narrowband images of [O III] and [O II] emission to construct ratio maps. These allow us to identify regions of the galaxy that are likely to be optically thin. Due to the importance of continuum subtraction for this technique, we also develop a new method for scaling the continuum images based on the mode of the pixel distribution. We find that a region extending from Haro 11 Knot A appears to be optically thin. Other regions of the galaxy have also been suggested as potential LyC sources, based on the presence of a ULX (Knot B) and Ly-alpha emission (Knot C). Our work now adds Knot A as a third candidate LyC source in this complex merger system. (This work was supported by NASA grant HST-GO-13702)

  15. Dust properties of Lyman-break galaxies in cosmological simulations

    NASA Astrophysics Data System (ADS)

    Yajima, Hidenobu; Nagamine, Kentaro; Thompson, Robert; Choi, Jun-Hwan

    2014-04-01

    Recent observations have indicated the existence of dust in high-redshift galaxies, however, the dust properties in them are still unknown. Here we present theoretical constraints on dust properties in Lyman-break galaxies (LBGs) at z = 3 by post-processing a cosmological smoothed particle hydrodynamics simulation with radiative transfer calculations. We calculate the dust extinction in 2800 dark matter haloes using the metallicity information of individual gas particles in our simulation. We use only bright galaxies with rest-frame ultraviolet (UV) magnitude M1700 < -20 mag, and study the dust size, dust-to-metal mass ratio, and dust composition. From the comparison of calculated colour excess between B and V band [i.e. E(B - V)] and the observations, we constrain the typical dust size, and show that the best-fitting dust grain size is ˜ 0.05 μm, which is consistent with the results of theoretical dust models for Type II supernova. Our simulation with the dust extinction effect can naturally reproduce the observed rest-frame UV luminosity function of LBGs at z = 3 without assuming an ad hoc constant extinction value. In addition, in order to reproduce the observed mean E(B - V), we find that the dust-to-metal mass ratio needs to be similar to that of the local galaxies, and that the graphite dust is dominant or at least occupy half of dust mass.

  16. Lyman-Werner UV escape fractions from primordial haloes

    NASA Astrophysics Data System (ADS)

    Schauer, Anna T. P.; Whalen, Daniel J.; Glover, Simon C. O.; Klessen, Ralf S.

    2015-12-01

    Population III (Pop III) stars can regulate star formation in the primordial Universe in several ways. They can ionize nearby haloes, and even if their ionizing photons are trapped by their own haloes, their Lyman-Werner (LW) photons can still escape and destroy H2 in other haloes, preventing them from cooling and forming stars. LW escape fractions are thus a key parameter in cosmological simulations of early reionization and star formation but have not yet been parametrized for realistic haloes by halo or stellar mass. To do so, we perform radiation hydrodynamical simulations of LW UV escape from 9-120 M⊙ Pop III stars in 105-107 M⊙ haloes with ZEUS-MP. We find that photons in the LW lines (i.e. those responsible for destroying H2 in nearby systems) have escape fractions ranging from 0 to 85 per cent. No LW photons escape the most massive halo in our sample, even from the most massive star. Escape fractions for photons elsewhere in the 11.18-13.6 eV energy range, which can be redshifted into the LW lines at cosmological distances, are generally much higher, being above 60 per cent for all but the least massive stars in the most massive haloes. We find that shielding of H2 by neutral hydrogen, which has been neglected in most studies to date, produces escape fractions that are up to a factor of 3 smaller than those predicted by H2 self-shielding alone.

  17. DUST OBSCURATION IN LYMAN BREAK GALAXIES AT z {approx} 4

    SciTech Connect

    Ho, I-Ting; Wang, Wei-Hao; Morrison, Glenn E.; Miller, Neal A. E-mail: itho@asiaa.sinica.edu.t

    2010-10-20

    Measuring star formation rates (SFRs) in high-z galaxies with their rest-frame ultraviolet (UV) continuum can be uncertain because of dust obscuration. Prior studies had used the submillimeter emission at 850 {mu}m to determine the intrinsic SFRs of rest-frame UV-selected galaxies, but the results suffered from the low sensitivity and poor resolution ({approx}15''). Here, we use ultradeep Very Large Array 1.4 GHz images with {approx}1''-2'' resolutions to measure the intrinsic SFRs. We perform stacking analyses in the radio images centered on {approx}3500 Lyman break galaxies (LBGs) at z {approx} 4 in the Great Observatories Origins Deep Survey-North and South fields selected with Hubble Space Telescope/Advanced Camera for Surveys data. The stacked radio flux is very low, 0.08 {+-} 0.15 {mu}Jy, implying a mean SFR of 6 {+-} 11 M{sub sun} yr{sup -1}. This is comparable to the uncorrected mean UV SFRs of {approx}5 M{sub sun} yr{sup -1}, implying that the z {approx} 4 LBGs have little dust extinction. The low SFR and dust extinction support the previous results that z {approx} 4 LBGs are in general not submillimeter galaxies. We further show that there is no statistically significant excess of dust-hidden star-forming components within {approx}22 kpc from the LBGs.

  18. Where have all the Lyman-alpha blobs gone?

    NASA Astrophysics Data System (ADS)

    Keel, William

    Lyman alpha emission blobs, up to 100 kpc in size and 10^44 ergs/sec in line luminosity, populate cosmic structures at z>2. Their nature and relation to galaxies and active nuclei remain uncertain from existing data, as does their evolution with cosmic time. Cooling flows of pristine material entering galaxies for the first time, photoionization by (often hidden) AGN, and unusually powerful starburst winds have been suggested to account for these objects. Recent results seem to favor the wind picture, which requires extremely powerful and brief starbursts and perhaps unusually dense surrounding media as well. The GALEX slitless grism mode offers a uniquely powerful way to search for similar objects in windows near z=0.3 and z=0.9. We therefore propose observations of regions of known large-scale density enhancements at z=0.9, where available evidence shows that cluster environments are still very active. Given the sensitivity of the instrument and low background levels, the results would either measure or very strongly limit the evolution of these clouds, and improve our picture of how they relate to the other kinds of objects we can see in the early Universe.

  19. On the Nature of Lyman-α Emitters

    NASA Astrophysics Data System (ADS)

    Wang, Junxian; Malhotra, Sangeeta; Rhoads, James; Brown, Michael; Heckman, Timothy; Norman, Colin

    2003-05-01

    More than half of the approximately 360 Lyman-α emitters found by the LALA survey show rest equivalent widths (EWs) larger than 200 Å, which is the maximum EW expected for normal stellar population. The high EWs can be reproduced by stellar populations with high proportions of young, massive stars, or by type 2 AGNs, which are supposed to be detectable in X-ray by deep Chandra images. An 180 ks Chandra ACIS exposure was obtained to study the X-ray properties of these emitters. However, none of the 49 sources imaged was significantly detected (over 2σ level) in X-ray. These sources cannot be detected in the stacked X-ray image either, which has an effective Chandra exposure time of 6.5 million seconds. The 3σ upper limit of the average X-ray flux is 7.9 × 10-17 erg.cm-2.s-1 in the 0.5 - 10.0 keV band, which is much fainter than the type 2 quasars discovered by Chandra so far. Optical spectra also show no AGN signatures.

  20. Coupling the emission of ionizing radiation and Lyman alpha

    NASA Astrophysics Data System (ADS)

    Hayes, Matthew

    2013-10-01

    The class of objects that reionized intergalactic hydrogen remains an observational and theoretical problem that is in contention for being the most prominent puzzle piece in contemporary astrophysics. The current consensus - determined almost entirely by ruling out bright active galaxies - is that the process was possibly begun and almost certainly finished by faint, lower-mass galaxies forming their early generations of stars. Recent observations of z 3 galaxies may even have identified the analog populations.However understanding how the emitted ionizing power of galaxies is causally related to their {robustly determined} physical properties is not a study that can be performed at high-z: neither the spatial information nor the standard multi-wavelength diagnostics are available. Moreover, on a case-by-case basis, the intervening IGM absorption is impossible to determine. These considerations have spawned a number of detailed studies with UV space telescopes, the synthesis of which however is that a characteristic population of Lyman continuum {LyC} emitting objects has not yet been identified. We show in this proposal that we have identified a characteristic trait in galaxy spectra that is highly indicative of LyC emission, by combining {a} high-z phenomenological studies, {b} new high-resolution UV spectra of local galaxies, and {c} sophisticated models of radiation transport. Believing that we have determined the signature, we propose to test the new hypothesis with deep spectroscopic observations with HST/COS under the Cycle 21 UV initiative.

  1. SIZING UP Ly{alpha} AND LYMAN BREAK GALAXIES

    SciTech Connect

    Malhotra, Sangeeta; Rhoads, James E.; McLinden, Emily; Finkelstein, Steven L.; Hathi, Nimish; Nilsson, Kim; Pirzkal, Norbert

    2012-05-10

    We measure the sizes for a sample of 174 Ly{alpha}-selected galaxies with broadband imaging with the Hubble Space Telescope. Over the redshift range 2.25 < z < 6, Ly{alpha}-selected galaxies have a characteristic, constant, small size in rest-frame ultraviolet (UV) light. Coupled with a characteristic star formation intensity (i.e., UV luminosity per unit area), this can explain their non-evolving ultraviolet continuum luminosity function. This is in contrast to Lyman break galaxies (LBGs) over the same redshift range, which have been previously shown to increase in linear size as H(z){sup -1}. The compact physical size seems to be a critical determining factor in whether a galaxy will show Ly{alpha} emission or not. The L{sub *} of LBGs and its evolution with redshift can be derived from a simple model where the star formation intensity has an upper limit set by feedback processes, independent of redshift. The increase in L{sub *} of LBGs is mainly driven by the increase in linear size over redshifts for z = 2-7. Since Ly{alpha} galaxies do not grow in linear size, they do not show an increase in L{sub *}.

  2. Clinico-radiological profile and outcome of dengue patients with central nervous system manifestations: A case series in an Eastern India tertiary care hospital

    PubMed Central

    Pal, Souren; Sen, Kaushik; Biswas, Nirendra Mohan; Ghosal, Anirban; Rousan Jaman, S. K.; Yashavantha Kumar, K. Y.

    2016-01-01

    Background and Objective: Dengue, an acute viral disease, transmitted by Aedes mosquitoes, has a variable clinical spectrum ranging from asymptomatic infection to life-threatening dengue hemorrhagic fever and dengue shock syndrome. However, neurological complications, in general, are unusual but have been observed more frequently in the recent past, and some studies highlighted varied neurological complications during the course of illness. Although dengue is classically considered a nonneurotropic virus, there is increasing evidence for dengue viral neurotropism. In this study, we have evaluated clinico-radiological profile and outcome of nine serologically confirmed dengue patients having varied manifestations of central nervous system (CNS) involvement. Materials and Methods: All the consecutive patients presented with neurological complications with positive serology for dengue infection (IgM positivity) in Department of Medicine, in a tertiary care hospital in Eastern India from August 2013 to October 2014 were included in the study. These patients were subjected to a detailed clinical evaluation, laboratory assessment including complete hemogram, coagulation profile, liver function test, serum electrolytes, and routine CSF (Cerebrospinal Fluid) study with the exclusion of other common neuroinvasive pathogens. Results: Out of 9 patients with neurological complications associated with confirmed dengue infection, 2 (22%) patients had dengue encephalopathy, 5 (56%) patients have dengue encephalitis, 1 (11%) patient had dengue meningitis, and 1 (11%) patient had postdengue immune-mediated CNS involvement. Conclusion: This case series reaffirms the occurrence of varied CNS manifestations in dengue virus infection and underlines the importance of inclusion of dengue in the differential diagnosis of acute encephalitis syndrome. PMID:26933357

  3. Design and Fabrication of the All-Reflecting H-Lyman alpha Coronagraph/Polarimeter

    NASA Technical Reports Server (NTRS)

    Hoover, Richard B.; Johnson, R. Barry; Fineschi, Silvano; Walker, Arthur B. C., Jr.; Baker, Phillip C.; Zukic , Muamer; Kim, Jongmin

    1993-01-01

    We have designed, analyzed, and are now fabricating an All-Reflecting H-Lyman alpha Coronagraph/Polarimeter for solar research. This new instrument operates in a narrow bandpass centered at lambda 1215.7 A-the neutral hydrogen Lyman alpha (Ly-alpha) line. It is shorter and faster than the telescope which produced solar Ly-alpha images as a part of the MSSTA payload that was launched on May 13, 1991. The Ly-alpha line is produced and linearly polarized in the solar corona by resonance scattering, and the presence of a magnetic field modifies this polarization according to the Hanle effect. The Lyman alpha Coronagraph/Polarimeter instrument has been designed to measure coronal magnetic fields by interpreting, via the Hanle effect, the measured linear polarization of the coronal Ly-alpha line. Ultrasmooth mirrors, polarizers, and filters are being flow-polished for this instrument from CVD silicon carbide substrates. These optical components will be coated using advanced induced transmission and absorption thin film multilayer coatings, to optimize the reflectivity and polarization properties at 1215.7 A. We describe some of the solar imaging results obtained with the MSSTA Lyman alpha coronagraph. We also discuss the optical design parameters and fabrication plans for the All-Reflecting H-Lyman alpha Coronagraph/Polarimeter.

  4. Imaging of the Field of 4C41.17 Below the Lyman Limit

    NASA Technical Reports Server (NTRS)

    Lacy, Mark; Rawlings, Steve

    1997-01-01

    Imaging of zeta greater than or equal to 3.4 radio galaxy fields below the Lyman continuum wavelength allows companion galaxies to be identified on the basis of red colors across the wavelength of redshifted Ly(alpha) and very red colors across the redshifted Lyman continuum. These arise due to a combination of absorption by intervening Ly(alpha) forest and Lyman-limit systems, and intrinsic Lyman-limit breaks in the galaxy spectral energy distribution caused by an Hi screen or breaks in stellar spectra. As a pilot study, we have imaged the field of the zeta = 3.8 radio galaxy 4C41.17 in U, V and R with the Auxiliary Port of the WHT. We find a number of potential companion galaxies, which require confirmation via spectroscopy or narrow-band imaging. The Lyman-limit in the spectrum of the radio galaxy itself and its implications for the origin of the UV flux is also discussed.

  5. Weathering and denudation rates determined by the combined analysis of Uranium series nuclides and in situ Beryllium in a weathering profile (Vosges massif, Strengbach catchment, France)

    NASA Astrophysics Data System (ADS)

    Ackerer, Julien; Chabaux, François; Van der Woerd, Jerome; Pelt, Eric; Kali, Elise; Pierret, Marie Claire; Viville, Daniel; Wyns, Robert; Negrel, Philippe

    2015-04-01

    The determination of soil sustainability is a major issue for societies. It is crucial to estimate the soil formation and denudation rates to evaluate the landscapes stability and their response to natural or anthropological forcings. In this work, we propose to combine the analysis of Uranium-Thorium-Radium isotopes with the cosmogenic in situ Beryllium in a weathering profile located in the Strengbach catchment to estimate both production rate of regolith and denudation rate of soil and to establish a soil mass balance at millennial timescales. The weathering profile is located on the summit of the watershed and extending from the top soil to the granitic fractured bedrock at 2 m depth. Whole rock data shows different trends of variation of major and trace element concentrations and also of U-Th-Ra disequilibria in the upper part of the regolith (0-80 cm) and the deeper part of the fractured saprolith and/or bedrock (100cm-200cm). Modeling of the U-Th-Ra data in this deeper part of the profile, using a particle swarm optimization model dedicated to isotopic ratios leads to a regolith production rate at the summit of the watershed of 35 ± 9 T/km²/year. In addition, a numerical optimization for nonlinear inverse problem has been performed to estimate the regolith residence time and the mean denudation rate at the summit from the Beryllium data. The results show that the regolith residence time is about 14 000 years and the mean denudation rate is 32 ± 8 T/km²/year. The consistency between the regolith production rate and the soil denudation rate suggests therefore that in such a temperate context, the long-term mass balance of soil developed on granitic bedrock would be close to a steady state. The data also highlights that the determination of a weathering production rate from analysis of Uranium series nuclides in whole rock samples cannot be easily obtained by analyzing only surficial soil samples, and requires the analysis of the deeper fractured saprolith

  6. Zero-P: a new zero-profile cage-plate device for single and multilevel ACDF. A single institution series with four years maximum follow-up and review of the literature on zero-profile devices.

    PubMed

    Barbagallo, Giuseppe M V; Romano, Dario; Certo, Francesco; Milone, Pietro; Albanese, Vincenzo

    2013-11-01

    To analyze the prospectively collected data in a series of patients treated with single- or multilevel ACDF with a stand-alone, zero-profile device, focusing on clinico-radiological outcome, complications and technical hints, and to review the literature on such new devices. Eighty-five patients harboring symptomatic DDD underwent ACDF with the Zero-P cage-plate: 29 at 1-level and 56 at 2-4 levels (total 162 devices). In the multilevel group, 9 patients received a combination of Zero-P and stand-alone cages (hybrid implants). This study focuses on 32 patients with follow-up ranging from 20 to 48 months. NDI, SF-36 and arm pain VAS scores were registered preoperatively and at follow-up visits. Dysphagia was assessed using the Bazaz score. Imaging included X-rays, CT and MRI, also to assess the presence of vertebral body fractures in multilevel cases. Paired Student t test was used for statistical analysis. SF-36 and NDI showed a statistically significant improvement (p < 0.01) and mean arm pain VAS score decreased from 79 to 41. X-rays and CT demonstrated, respectively, a 94.5 % and a 92 % fusion rate. Three patients complained of moderate and two of mild transient dysphagia (15.5 %). No device-related complications occurred and no fractures, secondary to four screws insertion in one vertebral body (i.e., swiss cheese effect), were detected in multilevel cases. In patients with extensive anterior osteophytes only a "focal spondylectomy" was required. The Zero-P device is safe and efficient, even in multilevel cases. Dysphagia is minimal, extensive anterior osteophytectomy is unnecessary and technical hints may ease the surgical workflow. This is the largest series, with the longest follow-up, reported.

  7. Detection of high Lyman continuum leakage from four low-redshift compact star-forming galaxies

    NASA Astrophysics Data System (ADS)

    Izotov, Y. I.; Schaerer, D.; Thuan, T. X.; Worseck, G.; Guseva, N. G.; Orlitová, I.; Verhamme, A.

    2016-10-01

    Following our first detection reported in Izotov et al., we present the detection of Lyman continuum (LyC) radiation of four other compact star-forming galaxies observed with the Cosmic Origins Spectrograph (COS) onboard the Hubble Space Telescope. These galaxies, at redshifts of z ˜ 0.3, are characterized by high emission-line flux ratios [O III] λ5007/[O II] λ3727 ≳ 5. The escape fractions of the LyC radiation fesc(LyC) in these galaxies are in the range of ˜6-13 per cent, the highest values found so far in low-redshift star-forming galaxies. Narrow double-peaked Ly α emission lines are detected in the spectra of all four galaxies, compatible with predictions for LyC leakers. We find escape fractions of Ly α, fesc(Ly α) ˜ 20-40 per cent, among the highest known for Ly α emitting galaxies. Surface brightness profiles produced from the COS acquisition images reveal bright star-forming regions in the centre and exponential discs in the outskirts with disc scalelengths α in the range ˜0.6-1.4 kpc. Our galaxies are characterized by low metallicity, ˜1/8-1/5 solar, low stellar mass ˜(0.2-4) × 109 M⊙, high star formation rates, SFR ˜ 14-36 M⊙ yr-1, and high SFR densities, Σ ˜ 2-35 M⊙ yr-1 kpc-2. These properties are comparable to those of high-redshift star-forming galaxies. Finally, our observations, combined with our first detection reported in Izotov et al., reveal that a selection for compact star-forming galaxies showing high [O III] λ5007/[O II] λ3727 ratios appears to pick up very efficiently sources with escaping LyC radiation: all five of our selected galaxies are LyC leakers.

  8. The high-ion content and kinematics of low-redshift Lyman limit systems

    SciTech Connect

    Fox, Andrew J.; Tumlinson, Jason; Bordoloi, Rongmon; Lehner, Nicolas; Howk, J. Christopher; Tripp, Todd M.; Katz, Neal; Prochaska, J. Xavier; Werk, Jessica K.; Oppenheimer, Benjamin D.; Davé, Romeel

    2013-12-01

    We study the high-ion content and kinematics of the circumgalactic medium around low-redshift galaxies using a sample of 23 Lyman limit systems (LLSs) at 0.08 < z < 0.93 observed with the Cosmic Origins Spectrograph on board the Hubble Space Telescope. In Lehner et al., we recently showed that low-z LLSs have a bimodal metallicity distribution. Here we extend that analysis to search for differences between the high-ion and kinematic properties of the metal-poor and metal-rich branches. We find that metal-rich LLSs tend to show higher O VI columns and broader O VI profiles than metal-poor LLSs. The total H I line width (Δv {sub 90} statistic) in LLSs is not correlated with metallicity, indicating that the H I kinematics alone cannot be used to distinguish inflow from outflow and gas recycling. Among the 17 LLSs with O VI detections, all but two show evidence of kinematic sub-structure, in the form of O VI-H I centroid offsets, multiple components, or both. Using various scenarios for how the metallicities in the high-ion and low-ion phases of each LLS compare, we constrain the ionized hydrogen column in the O VI phase to lie in the range log N(H II) ∼ 17.6-20. The O VI phase of LLSs is a substantial baryon reservoir, with M(high-ion) ∼ 10{sup 8.5-10.9} (r/150 kpc){sup 2} M {sub ☉}, similar to the mass in the low-ion phase. Accounting for the O VI phase approximately doubles the contribution of low-z LLSs to the cosmic baryon budget.

  9. Do Lyman-alpha photons escape from star-forming galaxies through dust-holes?

    NASA Astrophysics Data System (ADS)

    Wofford, Aida

    2012-10-01

    The hydrogen Lyman-alpha line is arguably the most important signature of galaxies undergoing their first violent burst of star formation. Although Lya photons are easily destroyed by dust, candidate Lya emitters have been detected at z>5. Thus the line can potentially be used to probe galaxy formation and evolution, as long as the astrophysical processes that regulate the escape of Lya photons from star-forming galaxies are well understood.We request 15 orbits for imaging in Lya and the FUV continuum with ACS/SBC, and in the H-beta/H-alpha ratio {proxy for dust extinction} with WFC3/UVIS, a sample of isolated non-AGN face-on spirals for which our team previously obtained and analyzed COS FUV spectroscopy of the central regions. Each target shows a different Lya profile, i.e., pure absorption, P-Cygni like, and multiple-emission. From the COS data, we already know the starburst phase and H I gas velocity. The images would greatly increase the impact of our spectroscopic study by enabling us to 1} conclusively determine if Lya photons escape through dust-holes, 2} assess the relative importance of dust extinction, ISM kinematics, and starburst phase in regulating the Lya escape, 3} clarify what we can really learn from the Lya equivalent width, and 4} provide constraints on the dust extinction to Lya 3D radiative transfer models. Ultimately this program will inform our understanding of the Lya escape at high redshift by providing spatially resolved views of the local conditions within star-forming galaxies that favor escape.

  10. The Lyman break analogue Haro 11: spatially resolved chemodynamics with VLT FLAMES

    NASA Astrophysics Data System (ADS)

    James, B. L.; Tsamis, Y. G.; Walsh, J. R.; Barlow, M. J.; Westmoquette, M. S.

    2013-04-01

    Using VLT/Fibre Large Array Multi Element Spectrograph (FLAMES) optical integral field unit observations, we present the first spatially resolved spectroscopic study of the well-known blue compact galaxy Haro 11, thought to be a local analogue to high-redshift Lyman break galaxies. Haro 11 displays complex emission line profiles, consisting of narrow (full width at half-maximum, FWHM ≲ 200 km s-1) and broad (FWHM ˜ 200-300 km s-1) components. We identify three distinct emission knots kinematically connected to one another. A chemodynamical analysis is presented, revealing that spatially resolved ionic and elemental abundances do not agree with those derived from integrated spectra across the galaxy. We conclude that this is almost certainly due to the surface brightness weighting of electron temperature in integrated spectra, leading to higher derived abundances. We find that the eastern knot has a low gas density, but a higher temperature (by ˜4000 K) and consequently an oxygen abundance ˜0.4 dex lower than the neighbouring regions. A region of enhanced N/O is found specifically in Knot C, confirming previous studies that found anomalously high N/O ratios in this system. Maps of the Wolf-Rayet (WR) feature at 4686 Å reveal large WR populations (˜900-1500 stars) in Knots A and B. The lack of WR stars in Knot C combined with an age of ˜7.4 Myr suggests that a recently completed WR phase may be responsible for the observed N/O excess. Conversely, the absence of N-enriched gas and strong WR emission in Knots A and B suggests that we are observing these regions at an epoch where stellar ejecta has yet to cool and mix with the interstellar medium.

  11. CAN THE LYMAN CONTINUUM LEAKED OUT OF H II REGIONS EXPLAIN DIFFUSE IONIZED GAS?

    SciTech Connect

    Seon, Kwang-Il

    2009-09-20

    We present an attempt to explain the diffuse Halpha emission of a face-on galaxy M 51 with the 'standard' photoionization model, in which the Lyman continuum (Lyc) escaping from H II regions propagates large distances into the diffuse interstellar medium (ISM). The diffuse Halpha emission of M 51 is analyzed using thin slab models and exponential disk models in the context of the 'on-the-spot' approximation. The scale height of the ionized gas needed to explain the diffuse Halpha emission with the scenario is found to be of the order of {approx}1-2 kpc, consistent with those of our Galaxy and edge-on galaxies. The model also provides a vertical profile, when the galaxy is viewed edge-on, consisting of two-exponential components. However, it is found that an incredibly low absorption coefficient of kappa{sub 0} {approx} 0.4-0.8 kpc{sup -1} at the galactic plane, or, equivalently, an effective cross section as low as sigma{sub eff} {approx} 10{sup -5} of the photoionization cross section at 912 A is required to allow the stellar Lyc photons to travel through the H I disk. Such a low absorption coefficient is out of accord with the properties of the ISM. Furthermore, we found that even the model that has the diffuse ionized gas (DIG) phase only and no H I gas phase shows highly concentrated Halpha emissions around H II regions, and can account for only {approx}<26% of the Halpha luminosity of the DIG. This result places a strong constraint on the ionizing source of the DIG. We also report that the Halpha intensity distribution functions not only of the DIG, but also of H II regions in M 51, appear to be lognormal.

  12. Monitoring vegetation recovery in fire-affected areas using temporal profiles of spectral signal from time series MODIS and LANDSAT satellite images

    NASA Astrophysics Data System (ADS)

    Georgopoulou, Danai; Koutsias, Nikos

    2015-04-01

    Vegetation phenology is an important element of vegetation characteristics that can be useful in vegetation monitoring especially when satellite remote sensing observations are used. In that sense temporal profiles extracted from spectral signal of time series MODIS and LANDSAT satellite images can be used to characterize vegetation phenology and thus to be helpful for monitoring vegetation recovery in fire-affected areas. The aim of this study is to explore the vegetation recovery pattern of the catastrophic wildfires that occurred in Peloponnisos, southern Greece, in 2007. These fires caused the loss of 67 lives and were recognized as the most extreme natural disaster in the country's recent history. Satellite remote sensing data from MODIS and LANDSAT satellites in the period from 2000 to 2014 were acquired and processed to extract the temporal profiles of the spectral signal for selected areas within the fire-affected areas. This dataset and time period analyzed together with the time that these fires occurred gave the opportunity to create temporal profiles seven years before and seven years after the fire. The different scale of the data used gave us the chance to understand how vegetation phenology and therefore the recovery patterns are influenced by the spatial resolution of the satellite data used. Different metrics linked to key phenological events have been created and used to assess vegetation recovery in the fire-affected areas. Our analysis was focused in the main land cover types that were mostly affected by the 2007 wildland fires. Based on CORINE land-cover maps these were agricultural lands highly interspersed with large areas of natural vegetation followed by sclerophyllous vegetation, transitional woodland shrubs, complex cultivation patterns and olive groves. Apart of the use of the original spectral data we estimated and used vegetation indices commonly found in vegetation studies as well as in burned area mapping studies. In this study we

  13. HST/STIS Spectroscopy of the Local Lyman-Alpha Forest

    NASA Technical Reports Server (NTRS)

    Heap, Sara R.; Dave, R. A.; Weymann, R.; Williger, G.; Jenkins, E.; Tripp, T.; Fisher, Richard R. (Technical Monitor)

    2001-01-01

    The Space Telescope Imaging Spectrograph (STIS) aboard the Hubble Space Telescope has brought a new era in studying the low-redshift Lyman-alpha Forest. The advantages of STIS over previous HST spectrographs include:(l) a high spectral resolution (7 km/s) comparable to Keck/HIRES spectra of the high-redshift Lyman-alpha forest; (2) a high observing efficiency brought about by an imaging detector able to span the full fares wavelength range (1150-1700 A, or equivalently, z=0.0-0.4) in a single exposure. The STIS Investigation Definition Team is therefore conducting an observational program to determine the properties of the low-redshift intergalactic medium as manifested by the Lyman-alpha forest. The team has made observations of the quasars: 3C 273, 3C 351, and PKS 0405. We shall present results based on the sightline to 3C 273, the brightest of these sources.

  14. Self-regulating galaxy formation. I - H II disk and Lyman-alpha pressure

    NASA Technical Reports Server (NTRS)

    Cox, D. P.

    1985-01-01

    The nascent interstellar medium and star formation model are incorporated into a scenario for the formation epoch of spiral galaxies. The structure, star formation time scale, and luminosity of a self-gravitating isothermal disk are evaluated as functions of the disk surface density. The importance of radiation pressure, particularly that of Lyman-alpha, in maintaining an inflated disk and halting infall is discussed. The Lyman-alpha pressure also supports a considerable halo of material in the vicinity of the disk. A first-order infall scenario and the time-dependent properties of the system it constructs are presented. Disk properties are evaluated at the epoch at which further material is supportable against infall by Lyman-alpha pressure. The two-dimensional family of disk galaxies whose scales and surface density are expressible in terms of fundamental constants and which arise from the three parameter sets of perturbations in the Hubble flow are determined.

  15. Continuous-wave Lyman-alpha generation with solid-state lasers.

    PubMed

    Scheid, Martin; Kolbe, Daniel; Markert, Frank; Hänsch, Theodor W; Walz, Jochen

    2009-07-06

    A coherent continuous-wave Lyman-alpha source based on four-wave sum-frequency mixing in mercury vapor has been realized with solid-state lasers. The third-order nonlinear susceptibility is enhanced by the 6(1)S - 7(1)S two-photon resonance and the near 6(1)S-6(3)P one-photon resonance. The phase matching curve for this four-wave mixing scheme is observed for the first time. In addition we investigate the two-photon enhancement of the Lyman-alpha yield and observe that the maxima of Lyman-alpha generation are shifted compared to the two-photon resonances of the different isotopes.

  16. Variability of Lyman-alpha and the ultraviolet continuum of 3C 446

    NASA Technical Reports Server (NTRS)

    Bregman, J. N.; Glassgold, A. E.; Huggins, P. J.; Kinney, A. L.

    1986-01-01

    IUE observations have been conducted over the 1230-3175 A range for the violently variable quasar 3C 446, beginning in June 1980, at intervals of 1.2, 2.2, 0.5, and 0.4 yr. Strong absorption of the continuum was found below 1830 A, probably corresponding to a Lyman edge at z of 1.00 + or - 0.01. The absence of Mg II 2798 A absorption implies that the column density is in the lower end of the range, unless the gas is metal-poor. The Lyman-alpha emission line was detected in five spectra; relative to the number of ionizing protons, the line strengths are the same as in normal quasars, and line equivalent widths are small due to the continuum's rise redward of 912 A, which is much steeper than in normal quasars. The Lyman-alpha line and the nearby continuum vary so as to maintain constant equivalent width.

  17. Building a Lyman-α detector for measurement of recycling rates in LTX

    NASA Astrophysics Data System (ADS)

    Yoo, Jongsoo; Kaita, Robert; Majeski, Richard; Foley, Jill; Merino, Enrique

    2007-11-01

    The measurement of the particle recycling rate is essential for understanding the performance improvements of lithium PFC devices like CDX-U and LTX. Recycling is usually measured by using atomic H-α (Balmer-α) emission, but the signal can be difficult to interpret because H-α has a high reflectivity for many wall materials including lithium. In contrast, Lyman-α is known to have a low reflectivity at a lithium wall. To measure recycling rates for LTX, a Lyman- α detector with a photodiode and a directly deposited 117-131nm pass-band filter has been developed. The detector has been tested with collisional beam excitations with a background of hydrogen gas. Based on known inelastic collision cross sections of a hydrogen beam, the relative intensity of Lyman- α collisionally induced fluorescence (CIF) to H-α CIF has been calculated. By comparing the theoretical ratio with the measured one, the detector can be calibrated.

  18. Bright z ~ 3 Lyman break galaxies in deep wide field surveys

    NASA Astrophysics Data System (ADS)

    Bian, Fuyan

    In my thesis I investigate the luminous z ˜ 3 Lyman break galaxies in deep wide field surveys. In the first part of the thesis, I use the LBT/LUCIFER to observe a lensed high-redshift star-forming galaxy (J0900+2234) at z = 2.03. With the high S/N near-IR spectroscopic observations, I reveal the detailed physical properties of this high-redshift galaxy, including SFR, metallicity, dust extinction, dynamical mass, and electron number density. In the second part of the thesis, I select a large sample of LBGs at z ˜ 3 from our new LBT Bootes field survey, and study the bright end luminosity function (LF), stellar mass function (SMF) and clustering properties of bright LBGs (1L* < L < 2.5L*). Together with other LF and SMF measurements, the evolution of LF and SMF can be well described by continuously rising star formation history model. Using the clustering measurements in this work and other works, a tight relation between the average host galaxy halo mass and the galaxy star formation rate is found, which can be interpreted as arising from cold flow accretion. The relation also suggests that the cosmic star formation efficiency is about 5%-20% of the total cold flow mass. This cosmic star formation efficiency does not evolve with redshift (from z ˜ 5 to z ˜ 3), hosting dark matter halo mass (1011 -- 1013 M⊙ ), or galaxy luminosity (from 0.3L* to 3L* ). In the third and fourth parts, with the spectroscopic follow-up observations of the bright LBGs, I establish a sample of spectroscopically-confirmed ultraluminous LBGs (ULBGs) in NOAO Boo¨tes field. With this new ULBG sample, the rest-frame UV LF of LBG at M1700A = -23.0 was measured for the first time. I find that the ULBGs have larger outflow velocity, broader Lyalpha emission and ISM absorption line profiles, and more prominent C IV P-Cygni profile. This profile may imply a top-heavy IMF in these ULBGs. The ULBGs have larger stellar mass and SFR, but smaller dust extinction than the typical L* LBGs at z ˜ 2

  19. The life and scientific contributions of Lyman J. Briggs

    USGS Publications Warehouse

    Landa, Edward R.; Nimmo, John R.

    2003-01-01

    Lyman J. Briggs (1874-1963), an early twentieth century physicist at the U. S. Department of Agriculture (USDA), made many significant contributions to our understanding of soil-water and plant-water interactions. He began his career at the Bureau of Soils (BOS) in 1896. At age 23, Briggs published (1897) a description of the roles of surface tension and gravity in determining the state of static soilmoisture. Concepts he presented remain central to this subject more than 100 yr later. With J. W. McLane, Briggs developed the "moisture equivalent" concept (a precursor to the idea of field capacity) and a centrifuge apparatus for measuring it. Briggs left the BOS at the end of 1905, under pressure from Milton Whitney, and moved to the Bureau of Plant Industry. Briggs' multi-state experiments with H. L. Shantz on water-use efficiencies showed that in a climate like that of the Great Plains, plants use water more productively in the cooler north than in the warmer south. In 1920, he moved from the USDA to the National Bureau of Standards (NBS), rising to Director in 1933. Among his other contributions to the American scientific community was his leadership, beginning in 1939, of a top secret committee that evolved into the Manhattan Project to develop an atomic bomb during World War II. A life-long baseball fan, Briggs at age 84, studied the speed, spin, and deflection of the curve ball, aided by manager Cookie Lavagetto and the pitching staff of the Washington Senators; he published these findings in a paper in the American Journal of Physics in 1959.

  20. THE SIZE-LUMINOSITY DISTRIBUTIONS OF LYMAN-BREAK GALAXIES

    NASA Astrophysics Data System (ADS)

    Huang, Kuang-Han; CANDELS Collaboration

    2014-01-01

    Lyman-break galaxies (LBGs) comprise the largest sample of star-forming galaxies at z>3 and are crucial to our understanding of galaxy formation and evolution. Their luminosity functions allow us to calculate the cosmic star formation history, and their sizes also provide valuable information about the angular momentum content of the galaxies and dark matter halos. However, due to surface brightness dimming effects, galaxies at high redshifts are especially susceptible to selection effects; it is important to understand the selection effects before we can draw conclusions from the statistics of LBG properties. In this work we will investigate the size--luminosity distribution of LBGs between 3 and 6 with careful modeling of selection effects and measurement errors of size and magnitude. Our modeling is more careful than previous studies because it is performed in the two-dimensional size--magnitude space. The results of this work show that (1) the effective radii of star-forming galaxies likely evolve as H(z)^{-2/3} at a fixed luminosity, (2) the widths of the LBG size distribution are larger than expected from the spin parameter distribution of dark matter halos, and (3) the size--luminosity relation slopes of LBGs are similar to those for late-type disk galaxies in the local universe. These results favor the disk formation theory put forward by Fall & Efstathiou (1980) if the majority of LBGs are disks, but more observational evidence is needed to confirm the kinematical structure of LBGs as well as to explain the widths of the size distribution.

  1. Equilibrium Slab Models of Lyman-Alpha Clouds

    NASA Technical Reports Server (NTRS)

    Charlton, Jane C.; Salpeter, Edwin E.; Hogan, Craig J.

    1993-01-01

    We model the L(sub y(alpha)) clouds as slabs of hydrogen with an ionizing extragalactic radiation field incident from both sides. In general, the equilibrium configuration of a slab at redshift z approx. less than 5 is determined by a balance of the gas pressure, gravity (including the effects of a dark matter halo), and the pressure exerted by the inter-galactic medium, P(sub ext). These models have been used to make predictions of the number of slabs as a function of the neutral hydrogen column density, N(sub H). A break in the curve is predicted at the transition between regimes where gravity and pressure are the dominant confining forces, with a less rapid decrease at larger N(sub H). The transition from optically thin to optically thick slabs leads to a gap in the distribution, whose location is governed largely by the spectrum of ionizing radiation. There are certain parallels between lines of sight through the outer HI disk of spiral galaxy with increasing radius, and the progression from damped, to Lyman limit, to forest clouds. We discuss briefly the possibility that at least some of the observed low z forest clouds may be a separate population, associated with galaxies, as suggested by the observations of Bahcall et al. This population could dominate the forest at present if the dark matter attached to galaxies should lead to gravity confinement for this disk population, while the isolated clouds remain pressure confined. The formalism developed in this paper will allow a more detailed study. We also discuss a more general parameter study of the equilibrium configuration of slabs, including mock gravity and L(sub y(alpha)) photon trapping.

  2. Haro 11: Where is the Lyman Continuum Source?

    NASA Astrophysics Data System (ADS)

    Keenan, Ryan P.; Oey, M. S.; Jaskot, Anne E.; James, Bethan L.

    2017-10-01

    Identifying the mechanism by which high-energy Lyman continuum (LyC) photons escaped from early galaxies is one of the most pressing questions in cosmic evolution. Haro 11 is the best known local LyC-leaking galaxy, providing an important opportunity to test our understanding of LyC escape. The observed LyC emission in this galaxy presumably originates from one of the three bright, photoionizing knots known as A, B, and C. It is known that Knot C has strong Lyα emission, and Knot B hosts an unusually bright ultraluminous X-ray source, which may be a low-luminosity active galactic nucleus. To clarify the LyC source, we carry out ionization-parameter mapping (IPM) by obtaining narrow-band imaging from the Hubble Space Telescope WFC3 and ACS cameras to construct spatially resolved ratio maps of [O iii]/[O ii] emission from the galaxy. IPM traces the ionization structure of the interstellar medium and allows us to identify optically thin regions. To optimize the continuum subtraction, we introduce a new method for determining the best continuum scale factor derived from the mode of the continuum-subtracted, image flux distribution. We find no conclusive evidence of LyC escape from Knots B or C, but instead we identify a high-ionization region extending over at least 1 kpc from Knot A. This knot shows evidence of an extremely young age (≲1 Myr), perhaps containing very massive stars (>100 M ⊙). It is weak in Lyα, so if it is confirmed as the LyC source, our results imply that LyC emission may be independent of Lyα emission.

  3. HETDEX: The Physical Properties of Lyman-alpha Emitters

    NASA Astrophysics Data System (ADS)

    Gronwall, Caryl; Blanc, G.; Ciardullo, R.; Finkelstein, S.; Gawiser, E.; Gebhardt, K.; HETDEX Collaboration

    2012-01-01

    Beginning in Fall 2012, the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) will map out 300 square degrees via a blind integral-field spectroscopic survey which will detect 800,000 Lyman-alpha emitters (LAEs) at 1.9 < z < 3.5. The goal of HETDEX is to explore the expansion history of the universe via the LAE power spectrum, but these emission-line sources are also important probes of galaxy evolution. LAEs are observed "in the act" of formation with low mass, little dust, very young ages, and a two-dimensional clustering scale-length that implies that they are the progenitors of today's Milky Way type galaxies. The unprecedented size of the HETDEX survey will allow us to explore the 3-D clustering of these objects and to measure their halo masses as a function of redshift. We will also be able to explore the physical properties of LAEs over a wide range of environments, and study how their luminosity functions, equivalent width distributions, and star formation rates change with galaxy density and redshift. In preparation for HETDEX, we undertook a 3 year pilot survey to test the feasibility of the experiment and design an optimal observing strategy. These observations were performed with a proto-type HETDEX spectrograph (VIRUS-P) on the McDonald 2.7-m telescope, and covered Ly-alpha in the redshift range 1.9 < z < 3.8. This survey discovered 104 Ly-alpha emitting galaxies in 169 sq. arcmin of sky, and reached objects with Ly-alpha line luminosities as faint as 3 x 1042 ergs/s. We will present the Ly-alpha luminosity function, equivalent width distributions, and star formation rates measured for this sample and discuss the implications of the pilot survey results for HETDEX.

  4. Lyman-Werner escape fractions from the first galaxies

    NASA Astrophysics Data System (ADS)

    Schauer, Anna T. P.; Agarwal, Bhaskar; Glover, Simon C. O.; Klessen, Ralf S.; Latif, Muhammad A.; Mas-Ribas, Lluís; Rydberg, Claes-Erik; Whalen, Daniel J.; Zackrisson, Erik

    2017-05-01

    Direct collapse black holes forming in pristine, atomically cooling haloes at z ≈ 10-20 may act as the seeds of supermassive black holes (BHs) at high redshifts. In order to create a massive BH seed, the host halo needs to be prevented from forming stars. H2 therefore needs to be irradiated by a large flux of Lyman-Werner (LW) UV photons in order to suppress H2 cooling. A key uncertainty in this scenario is the escape fraction of LW radiation from first galaxies, which is the dominant source of UV photons at this epoch. To better constrain this escape fraction, we have performed radiation-hydrodynamical simulations of the growth of H ii regions and their associated photodissociation regions in the first galaxies using the zeus-mp code. We find that the LW escape fraction crucially depends on the propagation of the ionization front (I-front). For an R-type I-front overrunning the halo, the LW escape fraction is always larger than 95 per cent. If the halo recombines later from the outside-in, due to a softened and weakened spectrum, the LW escape fraction in the rest frame of the halo (the near-field) drops to zero. A detailed and careful analysis is required to analyse slowly moving, D-type I-fronts, where the escape fraction depends on the microphysics and can be as small as 3 per cent in the near-field and 61 per cent in the far-field or as large as 100 per cent in both the near-field and the far-field.

  5. How Lyman alpha bites/beats the dust

    NASA Astrophysics Data System (ADS)

    Hayes, Matthew

    2014-10-01

    The bulk of high redshift star formation occurs in IR-bright objects. At similar epochs the de facto spectroscopic tracer of galaxies is the Lyman-alpha line, which is used almost ubiquitously with a diverse range of applications in galaxy evolution. Ly-alpha is also very sensitive to dust absorption, however, and a challenging emergent result of recent years is that an overwhelming fraction of IR-bright galaxies are also luminous Ly-alpha emitters. How is this possible given the mammoth dust contents? We will take advantage of the unique capabilities of HST and the Cycle 22 UV initiative to find out.Ly-alpha observations are infamously difficult to interpret because of the resonant nature of the transition. This has motivated detailed studies of nearby galaxies with space-based platforms, that have aided in unleashing the power of Ly-alpha for high-z studies. Only HST provides the UV access and resolution to do this, and hundreds of orbits have been devoted to studying UV-selected galaxies. Yet the UV reveals a small fraction of high-z star formation and no study has ever imaged the IR-bright systems in Ly-alpha. The proposed ACS observations will do this in five Ultraluminous Infrared Galaxies (ULIRGs), sampling spatial scales of just 50 pc. We will test sophisticated new models of Ly-alpha escape, study morphologies in comparison to the stars and nebular gas, measure global Ly-alpha quantities for the first time, and probe the relevant structures in the ISM in minute detail. We will finally push nearby Ly-alpha studies to the highest possible bolometric luminosities.

  6. The Nature of High Equivalent Width Lyman-α Galaxies

    NASA Astrophysics Data System (ADS)

    Finkelstein, S. L.; Rhoads, J. E.; Malhotra, S.; Pirzkal, N.; Wang, J.

    2005-12-01

    We present new results on the nature of the high equivalent width Lyα lines seen in high-redshift galaxies. These galaxies were identified on the basis of their large equivalent width Lyα emission, beyond the maximum expected for normal stellar populations. To be produced, this strong Lyα emission requires a strong ionizing continuum. Previous X-ray images and optical spectra show that this emission is not powered by active galactic nuclei. The optical colors of these galaxies provide a diagnostic of the stellar populations. The large equivalent widths seen in the Lyα line in these galaxies could be produced via star formation if the stellar photospheres are hotter than normal, which might be expected for star formation in low metallicity galaxies. They could also result from a top-heavy initial mass function. Both of these scenarios might be expected in primitive galaxies. To investigate these galaxies, we have computed stellar population models using the stellar population synthesis code created by Bruzual and Charlot (2003). We will use these models to predict the equivalent width distribution of the Lyα line in these high-redshift galaxies. We will also be able to derive estimates of stellar masses and stellar population ages, and be able to determine if these systems are indeed young and relatively primitive. Furthermore, we are obtaining new deep broadband imaging data on high-redshift galaxies taken from the Large Area Lyman Alpha (LALA) survey. These observations will yield better equivalent width measurements and continuum colors than previous data has allowed. We will compare these colors with the expectations for hot stars. We will also be able to constrain the star-formation rate using the UV continuum light from these galaxies, which will provide a valuable comparison with star-formation rates derived from the Lyα luminosity alone.

  7. First Results from the Large-Area Lyman Alpha Survey

    NASA Astrophysics Data System (ADS)

    Rhoads, James E.; Malhotra, Sangeeta; Dey, Arjun; Stern, Daniel; Spinrad, Hyron; Jannuzi, Buell T.

    2000-12-01

    We report on a new survey for z~4.5 Lyα sources, the Large-Area Lyman Alpha (LALA) survey. Our survey achieves an unprecedented combination of volume and sensitivity by using narrowband filters on the new 81922 pixel CCD Mosaic camera at the 4 m Mayall telescope of Kitt Peak National Observatory. Well-detected sources with flux and equivalent width matching previously known high-redshift Lyα galaxies (i.e., observed equivalent width EW>80 Å 2.6×10-17 ergs cm-2 s-1

  8. Lyman α radiation hydrodynamics of galactic winds before cosmic reionization

    NASA Astrophysics Data System (ADS)

    Smith, Aaron; Bromm, Volker; Loeb, Abraham

    2017-01-01

    The dynamical impact of Lyman α (Lyα) radiation pressure on galaxy formation depends on the rate and duration of momentum transfer between Lyα photons and neutral hydrogen gas. Although photon trapping has the potential to multiply the effective force, ionizing radiation from stellar sources may relieve the Lyα pressure before appreciably affecting the kinematics of the host galaxy or efficiently coupling Lyα photons to the outflow. We present self-consistent Lyα radiation-hydrodynamics simulations of high-z galaxy environments by coupling the Cosmic Lyα Transfer code (COLT) with spherically symmetric Lagrangian frame hydrodynamics. The accurate but computationally expensive Monte Carlo radiative transfer calculations are feasible under the one-dimensional approximation. The initial starburst drives an expanding shell of gas from the centre and in certain cases, Lyα feedback significantly enhances the shell velocity. Radiative feedback alone is capable of ejecting baryons into the intergalactic medium (IGM) for protogalaxies with a virial mass of Mvir ≲ 108 M⊙. We compare the Lyα signatures of Population III stars with 105 K blackbody emission to that of direct collapse black holes with a non-thermal Compton-thick spectrum and find substantial differences if the Lyα spectra are shaped by gas pushed by Lyα radiation-driven winds. For both sources, the flux emerging from the galaxy is reprocessed by the IGM such that the observed Lyα luminosity is reduced significantly and the time-averaged velocity offset of the Lyα peak is shifted redward.

  9. A Spectroscopic Search for Leaking Lyman Continuum at Zeta Approximately 0.7

    NASA Technical Reports Server (NTRS)

    Bridge, Carrie R.; Teplitz, Harry I.; Siana, Brian; Scarlata, Claudia; Rudie, Gwen C.; Colbert, James; Ferguson, Henry C.; Brown, Thomas M.; Conselice, Christopher J.; Armus, Lee; hide

    2010-01-01

    We present the results of rest-frame, UV slitless spectroscopic observations of a sample of 32 z approx. 0.7 Lyman Break Galaxy (LBG) analogs in the COSMOS field. The spectroscopic search was performed with the Solar Blind Channel (SBC) on HST. While we find no direct detections of the Lyman Continuum we achieve individual limits (3sigma) of the observed non-ionizing UV to Lyman continuum flux density ratios, f(sub nu)(1500A)/f(sub nu)(830A) of 20 to 204 (median of 73.5) and 378.7 for the stack. Assuming an intrinsic Lyman Break of 3.4 and an optical depth of Lyman continuum photons along the line of sight to the galaxy of 85% we report an upper limit for the relative escape fraction in individual galaxies of 0.02 - 0.19 and a stacked 3sigma upper limit of 0.01. We find no indication of a relative escape fraction near unity as seen in some LBGs at z approx. 3. Our UV spectra achieve the deepest limits to date at any redshift on the escape fraction in individual sources. The contrast between these z approx. 0.7 low escape fraction LBG analogs with z approx. 3 LBGs suggests that either the processes conducive to high f(sub esc) are not being selected for in the z less than or approx.1 samples or the average escape fraction is decreasing from z approx. 3 to z approx. 1. We discuss possible mechanisms which could affect the escape of Lyman continuum photons

  10. The Lyman-continuum photon production efficiency in the high-redshift Universe

    NASA Astrophysics Data System (ADS)

    Wilkins, Stephen M.; Feng, Yu; Di-Matteo, Tiziana; Croft, Rupert; Stanway, Elizabeth R.; Bouwens, Rychard J.; Thomas, Peter

    2016-05-01

    The Lyman-continuum photon production efficiency (ξion) is a critical ingredient for inferring the number of photons available to reionize the intergalactic medium. To estimate the theoretical production efficiency in the high-redshift Universe we couple the BlueTides cosmological hydrodynamical simulation with a range of stellar population synthesis models. We find Lyman-continuum photon production efficiencies of log10(ξion/erg-1 Hz) ≈ 25.1-25.5 depending on the choice of stellar population synthesis model. These results are broadly consistent with recent observational constraints at high-redshift though favour a model incorporating the effects of binary evolution.

  11. Large Equivalent Width Galaxies from Large Area Lyman-Alpha Survey

    NASA Astrophysics Data System (ADS)

    Malhotra, S.; Rhoads, J.; Dey, A.; Jannuzi, B.; Stern, D.; Spinrad, H.

    2001-05-01

    We find many candidate z=4.5 Lyman-alpha emitting galaxies in our LALA (Large Area Lyman Alpha) survey. More than half of these sources have rest frame equivalent widths greater than 200 Angstroms, which is the largest equivalent width expected for a standard stellar initial mass function (IMF). Either these sources are type II quasars or galaxies with an IMF dominated by massive stars. From Chandra Deep Field X-ray source counts, we estimate that only 10-20% of the LALA sources can be type II quasars. This then indicates that some galaxies at high redshifts had top heavy IMFs.

  12. Differential smoothing of time-series measurements to identify disturbances in performance and quantify animal response characteristics: An example using milk yield profiles in dairy cows.

    PubMed

    Codrea, M C; Højsgaard, S; Friggens, N C

    2011-10-01

    Recent advances in on-farm technology now provide us with multiple time-series of reliably measured indicators of animal performance and status at the level of the individual. This paper presents a smoothing approach for extracting biologically meaningful features from such time series using bovine milk yield data as an example. The main goal of this study was to illustrate how the method can be used to detect production deviations, extract quantifiable features of the deviation profiles, and thus provide means to examine hypotheses concerning the nature of the deviations. The effectiveness of the method was assessed with complete lactation curves from 47 Holstein cows. Within their lactations, the cows were each subjected to 1 nutritional challenge for a period of 4 d (their standard diet: a maize silage-based total mixed ration was diluted with 60% wheat straw), which provoked a decline in the milk yield in all cows. The challenge was imposed between the same calendar days for all cows. Thus, the cows were at different stages of lactation: early (n = 14), mid (n = 15), and late (n = 18). Each milk-yield curve was decomposed into components that capture the short-term deviations of the cow such as the response to the nutritional challenge and describe the phenotypic potential yield function of that cow throughout its lactation. The difference between the 2 components gives a measure of the milk loss. In all, 480 deviations were detected from the complete lactations of 47 cows. The milk loss provoked by the feeding challenge (n = 47) was significantly related to the milk yield immediately before the challenge (r = 0.86, P < 0.01). The correlation between the rate of recovery and milk loss was (r = 0.94, P < 0.01). Further, there was no significant slope (P > 0.1) to the relationship between the ratio (rate of recovery/milk loss) and days from calving, indicating that the force of recovery was unaffected by stage of lactation. These results suggest that differential

  13. UV Spectral Variability and the Lyman-Alpha Forest in the Lensed Quasar Q0957+561

    NASA Technical Reports Server (NTRS)

    Dolan, J. F.; Michalitsianos, A. G.; Nguyen, Q. T.; Hill, R. J.

    1999-01-01

    Far-ultraviolet spectra of the gravitational lens components Q0957+561 A and B were obtained with the Hubble Space Telescope Faint Object Spectrograph (FOS) at five equally spaced epochs, one every two weeks. We confirm the flux variability of the quasar's Lyman-alpha and O VI lambda 1037 emission lines reported in IUE (International Ultraviolet Explorer) spectra. The fluxes in these lines vary on a time scale of weeks in the local rest frame (LRF), independently of each other and of the surrounding continuum. The individual spectra of each image were co-added to investigate the properties of the Lyman-alpha forest along the two lines of sight to the quasar. Absorption lines having equivalent width W (sub lambda) greater than or equal to 0.3 Angstroms in the LRF not previously identified as interstellar lines, metal lines, or higher order Lyman lines were taken to be LY-alpha forest lines. The existence of each line in this consistently selected set was then verified by its presence in two archival FOS spectra with approx. 1.5 times higher signal to noise than our co-added spectra. Ly-alpha forest lines with W (sub lambda) greater than or equal to 0.3 Angstroms appear at 42 distinct wavelengths in the spectra of the two images. Two absorption lines in the spectrum of image A have no counterpart at that wavelength in the spectrum of image B, and two lines in image B have no counterpart in image A. Based on the separation of the lines of sight at the redshift of the absorption lines appearing in only one spectrum, the density of the absorbing clouds in the direction of Q0957+561 must change significantly over a distance of 79 (+34, -26) h (sub 50) (sup -1) kpc in the simplified model where the absorbers are treated as spherical clouds and the characteristic dimension is the radius. (We adopt H (sub 0)= 50 h (sub 50) km s (sup -1) kpc (sup -1), q (sub 0) = 1/2, and LAMBDA = 0 throughout the paper.) The two limits define the 68% confidence interval on the

  14. In situ measurement of water vapor in the stratosphere with a cryogenically cooled Lyman-alpha hygrometer

    NASA Technical Reports Server (NTRS)

    Schwab, J. J.; Weinstock, E. M.; Nee, J. B.; Anderson, J. G.

    1990-01-01

    In situ measurements of water vapor in the stratosphere with a new instrument are reported. The instrument has been designed to observe daytime water vapor from a multiinstrument balloon gondola that simultaneously measures free radicals such as OH, HO2, and O3 in the stratosphere up to 40 km. Lyman-alpha photofragment fluorescence is used to measure water molecules in a flowing sample of ambient air. A brief description of the instrument is given, followed by the results of the first four balloon flights. The measured mixing ratio for this flight varies from 3.0-5.5 ppmv over the altitude range of 17-34 km. Adjustments in the cooling protocol for the flights of July 6, 1988, July 28, and August 25, 1989, result in a much higher signal-to-noise ratio. Profiles from these three flights are similar to, but somewhat higher, than the 1987 profile. Implications of measurements are discussed, as are the issues of short- and long-term variability of stratospheric water vapor.

  15. The Primordial Deuterium Abundance of the Most Metal-poor Damped Lyman-α System

    NASA Astrophysics Data System (ADS)

    Cooke, Ryan J.; Pettini, Max; Nollett, Kenneth M.; Jorgenson, Regina

    2016-10-01

    We report the discovery and analysis of the most metal-poor damped Lyα (DLA) system currently known, which also displays the Lyman series absorption lines of neutral deuterium. The average [O/H] abundance of this system is [O/H] = -2.804 ± 0.015, which includes an absorption component with [O/H] = -3.07 ± 0.03. Despite the unfortunate blending of many weak D i absorption lines, we report a precise measurement of the deuterium abundance of this system. Using the six highest-quality and self-consistently analyzed measures of D/H in DLAs, we report tentative evidence for a subtle decrease of D/H with increasing metallicity. This trend must be confirmed with future high-precision D/H measurements spanning a range of metallicity. A weighted mean of these six independent measures provides our best estimate of the primordial abundance of deuterium, 105 (D/H)P = 2.547 ± 0.033 ({{log}}10 {{{(D/H)}}}{{P}}=-4.5940+/- 0.0056). We perform a series of detailed Monte Carlo calculations of Big Bang nucleosynthesis (BBN) that incorporate the latest determinations of several key nuclear reaction cross-sections, and propagate their associated uncertainty. Combining our measurement of (D/H)P with these BBN calculations yields an estimate of the cosmic baryon density, 100 ΩB,0 h 2(BBN) = 2.156 ± 0.020, if we adopt the most recent theoretical determination of the d{(p,γ )}3{He} reaction rate. This measure of ΩB,0 h 2 differs by ˜2.3σ from the Standard Model value estimated from the Planck observations of the cosmic microwave background. Using instead a d{(p,γ )}3{He} reaction rate that is based on the best available experimental cross-section data, we estimate 100 ΩB,0 h 2(BBN) = 2.260 ± 0.034, which is in somewhat better agreement with the Planck value. Forthcoming measurements of the crucial d{(p,γ )}3{He} cross-section may shed further light on this discrepancy. Based on observations collected at the European Organisation for Astronomical Research in the Southern

  16. Stationary Inverted Balmer and Lyman populations for a CW HI water-plasma laser

    NASA Astrophysics Data System (ADS)

    Mills, Randell L.

    2002-10-01

    Stationary inverted H Balmer and Lyman populations were observed from a low pressure water-vapor microwave discharge plasma. The ionization and population of excited atomic hydrogen levels was attributed to energy provided by a catalytic resonance energy transfer between hydrogen atoms and molecular oxygen formed in the water plasma. The catalysis mechanism was supported by the observation of O^2+ and H Balmer line broadening of 55 eV compared to 1 eV for hydrogen alone. The high hydrogen atom temperature with a relatively low electron temperature, Te = 2 eV, exhibited characteristics of cold recombining plasmas. These conditions of a water plasma favored an inverted population in the lower levels. Thus, the catalysis of atomic hydrogen may pump a cw HI laser. From our results, laser oscillations are may be possible from (i) n = 3, n = 4, n = 5, n = 6, n = 7, and n = 8 to n = 2, (ii) n = 4, n = 5, n = 6, and n = 7 to n = 3 and (iii) n = 5 and n = 6 to n = 4. Lines of the Balmer series of n = 5, and n = 6 to n = 2 and the Paschen series of n = 5 to n = 3 were of particular importance because of the potential to design blue and 1.3 micron infrared lasers, respectively, which are ideal for many communications and microelectronics applications. At a microwave input power of 9W/cm^3, a collisional radiative model showed that the hydrogen excited state population distribution was consistent with an n = 1arrow5,6 pumping power of an unprecedented 200W/cm^3. High power hydrogen gas lasers are anticipated at wavelengths, over a broad spectral range from far infrared to violet which may be miniaturized to micron dimensions. Such a hydrogen laser represents the first new atomic gas laser in over a decade, and it may prove to be the most efficient, versatile, and useful of all. A further application is the direct generation of electrical power using photovoltaic conversion of the spontaneous or stimulated water vapor plasma emission.

  17. Lyman-α forest constraints on decaying dark matter

    NASA Astrophysics Data System (ADS)

    Wang, Mei-Yu; Croft, Rupert A. C.; Peter, Annika H. G.; Zentner, Andrew R.; Purcell, Chris W.

    2013-12-01

    We present an analysis of high-resolution N-body simulations of decaying dark matter cosmologies focusing on the statistical properties of the transmitted Lyman-α (Lyα) forest flux in the high-redshift intergalactic medium (IGM). In this type of model a dark matter particle decays into a slightly less massive stable dark matter daughter particle and a comparably light particle. The small mass splitting provides a nonrelativistic kick velocity Vk=cΔM/M to the daughter particle resulting in free-streaming and subsequent damping of small-scale density fluctuations. Current Lyα forest power spectrum measurements probe comoving scales up to ˜2-3h-1Mpc at redshifts z˜2-4, providing one of the most robust ways to probe cosmological density fluctuations on relatively small scales. The suppression of structure growth due to the free-streaming of dark matter daughter particles also has a significant impact on the neutral hydrogen cloud distribution, which traces the underlying dark matter distribution well at high redshift. We exploit Lyα forest power spectrum measurements to constrain the amount of free-streaming of dark matter in such models and thereby place limits on decaying dark matter based only on the dynamics of cosmological perturbations without any assumptions about the interactions of the decay products. We use a suite of dark-matter-only simulations together with the fluctuating Gunn-Peterson approximation to derive the Lyα flux distribution. We argue that this approach should be sufficient for our main purpose, which is to demonstrate the power of the Lyα forest to constrain decaying dark matter models. We find that Sloan Digital Sky Survey 1D Lyα forest power spectrum data place a lifetime-dependent upper limit Vk≲30-70km/s for decay lifetimes ≲10Gyr. This is the most stringent model-independent bound on invisible dark matter decays with small mass splittings. For larger mass splittings (large Vk), Lyα forest data restrict the dark matter

  18. Lyman Alpha Emitting Galaxies in the Nearby Universe

    NASA Astrophysics Data System (ADS)

    Hayes, Matthew

    2015-07-01

    The Lyman alpha emission line (Lyα) of neutral hydrogen (Hi) is intrinsically the brightest emission feature in the spectrum of astrophysical nebulae, making it a very attractive observational feature with which to survey galaxies. Moreover as an ultraviolet resonance line, Lyα possesses several unique characteristics that make it useful to study the properties of the interstellar medium and ionising stellar population at all cosmic epochs. In this review, I present a summary of Lyα observations of galaxies in the nearby universe. By ultraviolet continuum selection, at the magnitudes reachable with current facilities, only ≈ 5% of the local galaxy population shows a Lyα equivalent width (W Lyα) that exceeds 20 Å. This fraction increases dramatically at higher redshifts, but only in the local universe can we study galaxies in detail and assemble unprecedented multi-wavelength datasets. I discuss many local Lyα observations, showing that when galaxies show net Lyα emission, they ubiquitously also produce large-scale halos of scattered Lyα, that dominate the integrated luminosity. Concerning global measurements, we discuss how W Lyα and the Lyα escape fraction (f Lyα esc) are higher (W Lyα ≳ 20 Å and f Lyα esc ≳ 10%) in galaxies that represent the less massive and younger end of the distribution for local objects. This is connected with various properties, such that Lyα-emitting galaxies have lower metal abundances (median value of 12 + log(O/H) ~ 8.1) and dust reddening. However, the presence of galactic outflows/winds is also vital to Doppler shift the Lyα line out of resonance with the atomic gas, and high W Lyα is found only among galaxies with winds faster than ~ 50 km s-1. The empirical evidence is then assembled into a coherent picture, and the requirement for star-formation-driven feedback is discussed in the context of an evolutionary sequence where the interstellar medium is accelerated and/or subject to hydrodynamical instabilities

  19. Dust biasing of damped Lyman alpha systems: a Bayesian analysis

    NASA Astrophysics Data System (ADS)

    Pontzen, Andrew; Pettini, Max

    2009-02-01

    If damped Lyman alpha systems (DLAs) contain even modest amounts of dust, the ultraviolet luminosity of the background quasar can be severely diminished. When the spectrum is redshifted, this leads to a bias in optical surveys for DLAs. Previous estimates of the magnitude of this effect are in some tension; in particular, the distribution of DLAs in the (NHI, Z) (i.e. column density-metallicity) plane has led to claims that we may be missing a considerable fraction of metal-rich, high column density DLAs, whereas radio surveys do not unveil a substantial population of otherwise hidden systems. Motivated by this tension, we perform a Bayesian parameter estimation analysis of a simple dust obscuration model. We include radio and optical observations of DLAs in our overall likelihood analysis and show that these do not, in fact, constitute conflicting constraints. Our model gives statistical limits on the biasing effects of dust, predicting that only 7 per cent of DLAs are missing from optical samples due to dust obscuration; at 2σ confidence, this figure takes a maximum value of 17 per cent. This contrasts with recent claims that DLA incidence rates are underestimated by 30-50 per cent. Optical measures of the mean metallicities of DLAs are found to underestimate the true value by just 0.1dex (or at most 0.4dex,2σ confidence limit), in agreement with the radio survey results of Akerman et al. As an independent test, we use our model to make a rough prediction for dust reddening of the background quasar. We find a mean reddening in the DLA rest frame of log10 ~= -2.4 +/- 0.6, consistent with direct analysis of the Sloan Digital Sky Survey (SDSS) quasar population by Vladilo et al., log10 = -2.2 +/- 0.1. The quantity most affected by dust biasing is the total cosmic density of metals in DLAs, ΩZ,DLA, which is underestimated in optical surveys by a factor of approximately 2.

  20. The Evolution of Lyman Limit Absorption Systems to Redshift Six

    NASA Astrophysics Data System (ADS)

    Songaila, Antoinette; Cowie, Lennox L.

    2010-10-01

    We have measured the redshift evolution of the density of Lyman limit systems (LLSs) in the intergalactic medium over the redshift range 0 < z < 6. We have used two new quasar samples to (1) improve coverage at z ~ 1, with GALEX grism spectrograph observations of 50 quasars with 0.8 < z em < 1.3, and (2) extend coverage to z ~ 6, with Keck ESI spectra of 25 quasars with 4.17 < z em < 5.99. Using these samples together with published data, we find that the number density of LLS per unit redshift, n(z), can be well fit by a simple evolution of the form n(z) = n 3.5[(1 + z)/4.5]γ with n 3.5 = 2.80 ± 0.33 and γ = 1.94+0.36 -0.32 for the entire range 0 < z < 6. We have also reanalyzed the evolution of damped Lyα systems (DLAs) in the redshift range 4 < z < 5 using our high-redshift quasar sample. We find a total of 17 DLAs and sub-DLAs, which we have analyzed in combination with published data. The DLAs with log H I column density {>} 20.3 show the same redshift evolution as the LLS. When combined with previous results, our DLA sample is also consistent with a constant ΩDLA = 9 × 10-4 from z = 2 to z = 5. We have used the LLS number density evolution to compute the evolution in the mean free path (mfp) of ionizing photons. We find a smooth evolution to z ~ 6, very similar in shape to that of Madau et al. but about a factor of two higher. Recent theoretical models roughly match to the z < 6 data but diverge from the measured power law at z>6 in different ways, cautioning against extrapolating the fit to the mfp outside the measured redshift range. Based in part on data obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts.

  1. The nature of proximate damped Lyman α systems

    NASA Astrophysics Data System (ADS)

    Ellison, Sara L.; Prochaska, J. Xavier; Hennawi, Joseph; Lopez, Sebastian; Usher, Christopher; Wolfe, Arthur M.; Russell, David M.; Benn, Chris R.

    2010-08-01

    We present high-resolution echelle spectra of seven proximate damped Lyman α (PDLA) systems. The relative velocity separation of each PDLA from the background quasar is Δ V < 3000 km s-1. Combining our sample with a further nine PDLAs from the literature we compare the chemical properties of the proximate systems with a control sample of intervening DLAs. The PDLAs are usually excluded from statistical studies of absorption-selected galaxies and this sample constitutes the first systematic study of their chemical and ionization properties. Taken at face value, the sample of 16 PDLAs exhibits a wide range of metallicities, ranging from Z ~ 1/3 to ~ 1/1000 Zsolar, including the DLA with the lowest N(SiII)/N(HI) yet reported in the literature. However, some of these abundances may require ionization corrections. We find several pieces of evidence that indicate enhanced ionization and the presence of a hard ionizing spectrum in PDLAs which lead to properties that contrast with the intervening DLAs, particularly when the N(HI) is low. The abundances of Zn, Si and S in PDLAs with log N(HI) > 21, where ionization corrections are minimized, are systematically higher than the intervening population by a factor of around 3. We also find possible evidence for a higher fraction of NV absorbers amongst the PDLAs, although the statistics are still modest. 6/7 of our echelle sample show high ionization species (SiIV, CIV, OVI or NV) offset by >100 km s-1 from the main low ion absorption. We analyse fine-structure transitions of CII* and SiII* to constrain the PDLA distance from the quasi-stellar object (QSO). Lower limits range from tens of kpc to >160 kpc for the most stringent limit. We conclude that (at least some) PDLAs do exhibit different characteristics relative to the intervening population out to 3000 kms-1 (and possibly beyond). None the less, the PDLAs appear distinct from lower column density associated systems, and the inferred QSO-absorber separations mean they

  2. SWAN: A Study of Solar Wind Anisotropies on SOHO with Lyman Alpha Sky Mapping

    NASA Astrophysics Data System (ADS)

    Bertaux, J. L.; Kyrölä, E.; Quémerais, E.; Pellinen, R.; Lallement, R.; Schmidt, W.; Berthé, M.; Dimarellis, E.; Goutail, J. P.; Taulemesse, C.; Bernard, C.; Leppelmeier, G.; Summanen, T.; Hannula, H.; Huomo, H.; Kehlä, V.; Korpela, S.; Leppälä, K.; Strömmer, E.; Torsti, J.; Viherkanto, K.; Hochedez, J. F.; Chretiennot, G.; Peyroux, R.; Holzer, T.

    1995-12-01

    On board the SOHO spacecraft poised at L1 Lagrange point, the SWAN instrument is mainly devoted to the measurement of large scale structures of the solar wind, and in particular the distribution with heliographic latitude of the solar wind mass flux. This is obtained from an intensity map of the sky Lymanα emission, which reflects the shape of the ionization cavity carved in the flow of interstellar H atoms by the solar wind. The methodology, inversion procedure and related complications are described. The subject of latitude variation of the solar wind is shortly reviewed: earlier Lymanα results from Prognoz in 1976 are confirmed by Ulysses. The importance of the actual value of the solar wind mass flux for the equation of dynamics in a polar coronal hole is stressed. The instrument is composed of one electronic unit commanding two identical Sensor Units, each of them allowing to map a full hemisphere with a resolution of 1°, thanks to a two-mirrors periscope system. The design is described in some details, and the rationale for choice between several variants are discussed. A hydrogen absorption cell is used to measure the shape of the interplanetary Lymanα line and other Lyman α emissions. Other types of observations are also discussed : the geocorona, comets (old and new), the solar corona, and a possible signature of the heliopause. The connexion with some other SOHO instruments, in particular LASCO, UVCS, SUMER, is briefly discussed.

  3. Precise Determination of the Lyman-1 Transition Energy in Hydrogen-like Gold Ions with Microcalorimeters

    NASA Astrophysics Data System (ADS)

    Kraft-Bermuth, S.; Andrianov, V.; Bleile, A.; Echler, A.; Egelhof, P.; Grabitz, P.; Kilbourne, C.; Kiselev, O.; McCammon, D.; Scholz, P.

    2014-09-01

    The precise determination of the transition energy of the Lyman-1 line in hydrogen-like heavy ions provides a sensitive test of quantum electrodynamics in very strong Coulomb fields. We report the determination of the Lyman-1 transition energy of gold ions (Au) with microcalorimeters at the experimental storage ring at GSI. X-rays produced by the interaction of 125 MeV/u Au ions with an internal argon gas-jet target were detected. The detector array consisted of 14 pixels with silicon thermistors and Sn absorbers, for which an energy resolution of 50 eV for an X-ray energy of 59.5 keV was obtained in the laboratory. The Lyman-1 transition energy was determined for each pixel in the laboratory frame, then transformed into the emitter frame and averaged. A Dy-159 source was used for energy calibration. The absolute positions of the detector pixels, which are needed for an accurate correction of the Doppler shift, were determined by topographic measurements and by scanning a collimated Am-241 source across the cryostat window. The energy of the Lyman-1 line in the emitter frame is eV, in good agreement with theoretical predictions. The systematic error is dominated by the uncertainty in the position of the cryostat relative to the interaction region of beam and target.

  4. A comment on the measurement of atmospheric density by absorption of Lyman-alpha.

    NASA Technical Reports Server (NTRS)

    Smith, L. G.; Miller, K. L.

    1973-01-01

    It is shown that the absorption cross section for molecular oxygen at Lyman alpha is about 0.8 times 10 to the minus twentieth power sq cm. It is pointed out that, for application of absorption spectroscopy to the measurement of molecular oxygen density in the atmosphere, no correction for the variation of cross section with wavelength is necessary.

  5. Baryon Acoustic Oscillations in Lyman Alpha Forest - Quasar Cross-Correlations

    NASA Astrophysics Data System (ADS)

    Ho, Shirley; Aubourg, E.; Bailey, S. J.; Bautista, J.; Beutler, F.; Bizyaev, D.; Blomqvist, M.; Bolton, A. S.; Brewington, H.; Brinkmann, J. V.; Brownstein, J.; Busca, N. G.; Carithers, W.; Croft, R. A.; Dawson, K. S.; Delubac, T.; Ebelke, G.; Eisenstein, D.; Feng, Y.; Font-Ribera, A.; Hogg, D. W.; Kinemuchi, K.; Kirkby, D.; Le Goff, J.; Lee, K.; Malanushenko, E.; Malanushenko, V.; Marchante, M.; Margela, D.; Miralda-Escudé, J.; Muna, D.; Myers, A. D.; Nichol, R.; Oravetz, D.; Palanque-Delabrouille, N.; Pan, K.; Noterdaeme, P.; O'Connel, R.; Paris, I.; Petitjean, P.; Pieri, M.; Rollinde, E.; Ross, N.; Rossi, G.; Schlegel, D. J.; Schneider, D. P.; Simmons, A.; Slosar, A.; Viel, M.; Weinberg, D. H.; Xu, X.; Yeche, C.; York, D. G.

    2014-01-01

    We investigate the signal of BAO in the cross-correlations between SDSS III-BOSS DR10 and DR11 quasars and Lyman Alpha Forest. We present two independent analyses that follow slightly different methodologies. In one, we fit the BAO using DR10 data only following multipole methods described in Xu et al. 2012 adapting to the fact that Lyman-Alpha forest is negatively biased, while in the other analyses, we analyze DR11 data following methodologies in Font-Ribera et al., 2012 and Kirkby et al. 2013. In the two analyses, we use different treatments of the Lyman Alpha Forest, different fitting methodologies and found consistent cosmological results. The expected signal-to-noise is weaker than the Lyman-Alpha Forest auto-correlations, however this will be a test of principle of finding BAO in cross-correlations, where systematics can be more easily mitigated. This method also applies to future surveys with medium/dense coverage of multiple tracers in similar redshift range, such as SDSS IV, DESI, WFIRST and EUCLID.

  6. Properties of nearby interstellar hydrogen deduced from Lyman-alpha sky background measurements

    NASA Technical Reports Server (NTRS)

    Thomas, G. E.

    1972-01-01

    For a sufficiently rapid relative motion of the solar system and the nearby interstellar gas, neutral atoms may be expected to penetrate the heliosphere before becoming ionized. Recent satellite measurements of the Lyman alpha emission above the geocorona indicate such an interstellar wind of neutral hydrogen emerging from the direction of Sagittarius and reaching to within a few astronomical units of the sun. A detailed model of the scattering of solar Lyman alpha from the spatial distribution of neutral hydrogen in interplanetary space is presented. This asymmetric distribution is established by solar wind and solar ultraviolet ionization processes along the trajectories of the incoming hydrogen atoms. The values of the interstellar density, the relative velocity, and the gas temperature are adjusted to agree with the Lyman alpha measurements. The results may be interpreted in terms of two models, the cold model and the hot model of the interstellar gas, depending on whether galactic Lyman alpha emission is present at its maximum allowable value or negligibly small.

  7. The Crafoord Prize 1985 in Astronomy to Professor Lyman Spitzer Jr.

    NASA Astrophysics Data System (ADS)

    Gahm, G.

    The Royal Swedish Academy of Sciences has awarded the Crafoord Prize 1985 of 135000 US$ to Professor Lyman Spitzer Jr., Princeton, U.S.A., for his "Fundamental pioneering studies of practically every aspect of the interstellar medium, culminating in the results obtained using the Copernicus satellite".

  8. Lyman-α imaging of the SO2 distribution on Io

    NASA Astrophysics Data System (ADS)

    Feldman, Paul D.; Strobel, Darrell F.; Moos, H. Warren; Retherford, Kurt D.; Wolven, Brian C.; McGrath, Melissa A.; Roesler, Fred L.; Woodward, R. Carey; Oliversen, Ronald J.; Ballester, Gilda E.

    2000-06-01

    Imaging spectroscopy of Io in the ultraviolet (1160-1720 Å) was carried out with the Space Telescope Imaging Spectrograph on HST on three dates in October 1997 and August 1998. Among the initial results was the observation of concentrated regions of Hi Lyman-α flux near the poles of Io that exhibited a morphology and temporal variability different from those of the atomic oxygen and sulfur emission regions seen near the equatorial limbs. We examine the suggestion that the primary source of Lyman-α emission is surface reflected solar radiation that penetrates the thin polar atmosphere, but is strongly absorbed by the thicker SO2 atmosphere near Io's equator. Spectral and spatial analyses lead to derived SO2 column densities that are in good agreement with those derived from earlier HST observations of Io's albedo in the 2000-2300 Å wavelength range. The Lyman-α images clearly illustrate features of Io's atmosphere that have been deduced from previous observations and theoretical modeling: a non-uniformity with respect to the sub-solar point dominated by a freezing out of the SO2 near the poles and variation with both longitude and time due to the variability of the sources of the atmospheric gas. Lyman-α imaging is demonstrated to be an extremely powerful and direct way to globally map the dynamic atmosphere of Io.

  9. A Search for z>6.5 Lyman-alpha Emitting Galaxies with WISP

    NASA Astrophysics Data System (ADS)

    Bagley, Micaela B.; Scarlata, Claudia; Dai, Yu Sophia; Rafelski, Marc; Baronchelli, Ivano; Colbert, James W.; Dominguez, Alberto; Hathi, Nimish P.; Henry, Alaina L.; Malkan, Matthew Arnold; Martin, Crystal L.; Mehta, Vihang; Pahl, Anthony; Ross, Nathaniel; Rutkowski, Michael J.; Teplitz, Harry I.; WISP Team

    2016-01-01

    The observed number density of Lyman-alpha emitting galaxies at z>6 provides an important probe of the reionization history of the universe. Because Lyman-alpha photons are very sensitive to the presence of neutral hydrogen, the evolution of the galaxy number density above redshift 6 can be used as a measurement on the progress of reionization. However, the Lyman-alpha luminosity function is currently poorly constrained at high-z. We present the results of a systematic search for Lyman-alpha emitters (LAEs) at redshifts of ~6.5 to 7.5 using the HST WFC3 Infrared Spectroscopic Parallels (WISP) survey. WISP's uncorrelated fields are well-suited to the study of bright LAEs, minimizing the effects of clustering introduced by a patchy reionization. From the 30 deepest WISP fields, we compile a sample of single-line emitters, confirm redshifts with broadband colors, and identify LAE candidates that have "dropped out" (are undetected at the 1 sigma level) of the WFC3 UVIS filters. By combining our results with other z~7 studies, we determine whether the number density of LAEs evolves past z~6.5.

  10. Transverse Structure in the Lyman Alpha Forest and a Program to Measure the Cosmological Constant

    NASA Astrophysics Data System (ADS)

    Crotts, Arlin

    2001-07-01

    We propose to combine archival UV HST spectra of close QSO pairs with a large sample of similar optical spectra in order to determine the clustering strength of intergalactic H I absorption {the Lyman Alpha forest} with the intent of constraining hydrodynamic/gravitational models of structure formation in the early Universe. Furthermore, this dataset will allow a comparison of radial versus transverse clustering for weak overdensities in the Universe. Since radial versus transverse size for objects co-expanding with the Hubble flow is an excellent measure of the cosmological constant Lambda, and since the Lyman Alpha forest is relatively weakly clustered, the shape of its clustering function in radial versus transverse dimensions is an excellent prospect for uncovering the value of Lambda. We would like to fully analyze the close QSO pairs in the archive, including several that remain unpublished after many years, and combine these with high quality optical spectra extending blueward to atmospheric cutoff in order to provide study of Lyman Alpha forest structure that is as free as possible of systematic errors due to interloping metal lines. Such a study might not only determine Lambda, but lead to an independent, new measure of the density of normal matter Omega_baryon, the strength of ionizing radiation flux in the early Universe, and better constraints on other cosmological parameters open to study after testing numerical models of the Lyman Alpha forest can be trusted.

  11. A Lyman-alpha tunable acousto-optic filter for detecting superthermal flare protons

    NASA Technical Reports Server (NTRS)

    Mickey, Donald L.

    1994-01-01

    The goal of this project was to develop and characterize a narrow-band, tunable filter for use near the Lyman-alpha line of hydrogen at 121.6 nm. Such a filter could form the critical component of an instrument to observe asymmetries in the solar Lyman-alpha line, caused by energetic protons accelerated during the impulsive phase of solar flares. Characteristic charge-exchange nonthermal emission at Lyman alpha should be produced when sub-MeV protons are injected into the chromosphere, but no instrument suitable for their detection has been developed. Such an instrument would require a narrow-band (less than 0.01 nm) tunable filter with aperture and throughput consistent with imaging a solar active region at 0.1 second intervals. The development of acousto-optic tunable filters (AOTF) suitable for use as compact, simple tunable filters for astronomical work suggested an investigation into the use of an AOTF at Lyman-alpha.

  12. A two-component model of variations of Lyman-alpha emission with solar-activity level

    NASA Astrophysics Data System (ADS)

    Katiushina, V. V.; Krasinets, M. V.; Nusinov, A. A.; Bart, Ch. A.; Rottman, G. J.

    1991-02-01

    The relationship between the intensity of solar UV radiation in the Lyman-alpha line and the 10.7-cm emission is analyzed on the basis of SME data for 1982-1988. It is shown that the closest correlation between these parameters corresponds to the hypothesis that the Lyman-alpha radiation is a superposition of two components: background and upwelling from active regions. It is pointed out that various characteristics of Lyman-alpha variations in an activity cycle can be explained with the two-component model.

  13. Lunar Reconnaissance Orbiter (LRO) Lyman Alpha Mapping Project (LAMP) Maps of the Permanently Shaded Regions (PSR) at the Lunar Poles

    NASA Astrophysics Data System (ADS)

    Rojas, Paul; Retherford, Kurt; Gladstone, Randall; Stern, Alan; Egan, Anthony; Miles, Paul; Parker, Joel; Kaufmann, David; Horvath, David; Greathouse, Thomas; Versteeg, Maartem; Steffl, Andrew; Mukherjee, Joey; Davis, Michael; Slater, David; Bayless, Amanda; Feldmann, Paul; Hurley, Dana; Pryor, Wayne; Hendrix, Amanda

    2013-04-01

    The Lyman Alpha Mapping Project (LAMP) instrument on-board LRO is a UV spectrograph covering the spectral range of 57-196 nm. We present Lyman-alpha and far-UV albedo maps of the north and south poles. These maps indicate that the coldest, permanently shadowed regions (PSR) in deep polar craters have significantly lower Lyman-alpha albedo than the surrounding regions, which is best explained by a high surface porosity there - possibly related to the accumulation of volatile frosts.

  14. Io's SO2 Atmosphere Viewed in Silhouette by Jupiter Lyman

    NASA Astrophysics Data System (ADS)

    Retherford, Kurt D.; Roth, Lorenz; Feaga, Lori M.; Becker, Tracy M.; Tsang, Constantine; Jessup, Kandis-Lea; Grava, Cesare

    2016-10-01

    We report a new technique for mapping Io's SO2 vapor distribution. Hubble's Space Telescope Imaging Spectrograph (STIS) instrument observed Io during four Jupiter transit events to obtain medium resolution far-UV spectral images near the Lyman-α wavelength of 121.6 nm. Jupiter's bright Lyman-α dayglow provides a background light source for opacity measurements, much like during a stellar occultation or transiting exoplanet event. Peaks in the photoabsorption cross-sections for sulfur dioxide occur near 122 nm, with resulting absorptions raising the altitude where a tangential line of sight opacity of tau=1 is detected up to resolvable distances above the disk. This method of measuring column densities along lines of sight above the limb complements Lyman-α reflectance imaging and other methods for measuring Io's SO2 gas. For example, interpretation of Io's surface reflected components at far-UV wavelengths is complicated by SO2 frost features being correlated with regions of known volcanic outgassing activity, while Jupiter's Lyman-α dayglow provides a more spatially uniform background light source. Initial examination of these near-terminator limb observations with STIS confirms the findings from previous Lyman-α disk reflectance imaging using STIS's G140L mode (e.g., Feldman et al., GRL, 2000; Feaga et al. 2009) that Io's polar SO2 density is roughly an order of magnitude lower than found at the equator. As Strobel & Wolven (2001) described it, Io appears to wear its dayside atmosphere as "a belt" around the equator. We describe detailed simulations, now underway, that incorporate the STIS point spread function and consideration of additional attenuation by atmospheric hydrogen atoms, which are produced by charge exchange reactions between magnetospheric protons and Io's atmosphere.

  15. Mapping tropical dry forest height, foliage height profiles and disturbance type and age with a time series of cloud-cleared Landsat and ALI image mosaics to characterize avian habitat

    Treesearch

    E.H. Helmer; Thomas S. Ruzycki; Jr. Joseph M. Wunderle; Shannon Vogesser; Bonnie Ruefenacht; Charles Kwit; Thomas J. Brandeis; David N. Ewert

    2010-01-01

    Remote sensing of forest vertical structure is possible with lidar data, but lidar is not widely available. Here we map tropical dry forest height (RMSE=0.9 m, R2=0.84, range 0.6–7 m), and we map foliage height profiles, with a time series of Landsat and Advanced Land Imager (ALI) imagery on the island of Eleuthera, The Bahamas, substituting time for vertical canopy...

  16. A Statistical Profile of the Entering Class at Broome Community College, Fall 1983: Student Characteristics, Needs and Goals. Working Paper Series No. 1-85.

    ERIC Educational Resources Information Center

    Romano, Richard M., Comp.

    Broome Community College (BCC) is developing a series of questionnaires to assess the impact of college on its students, and to measure the college's role, if any, in promoting social mobility. The first study in this series focused on the backgrounds, needs, and goals of students who entered BCC during June, July, and August of 1983. Students who…

  17. The ESO UVES advanced data products quasar sample - VI. Sub-damped Lyman α metallicity measurements and the circumgalactic medium

    NASA Astrophysics Data System (ADS)

    Quiret, S.; Péroux, C.; Zafar, T.; Kulkarni, V. P.; Jenkins, E. B.; Milliard, B.; Rahmani, H.; Popping, A.; Rao, S. M.; Turnshek, D. A.; Monier, E. M.

    2016-06-01

    The circumgalactic medium (CGM) can be probed through the analysis of absorbing systems in the line of sight to bright background quasars. We present measurements of the metallicity of a new sample of 15 sub-damped Lyman α absorbers (sub-DLAs, defined as absorbers with 19.0 < log N(H I) < 20.3) with redshift 0.584 ≤ zabs ≤ 3.104 from the ESO Ultra-Violet Echelle Spectrograph (UVES) Advanced Data Products Quasar Sample (EUADP). We combine these results with other measurements from the literature to produce a compilation of metallicity measurements for 92 sub-DLAs as well as a sample of 362 DLAs. We apply a multi-element analysis to quantify the amount of dust in these two classes of systems. We find that either the element depletion patterns in these systems differ from the Galactic depletion patterns or they have a different nucleosynthetic history than our own Galaxy. We propose a new method to derive the velocity width of absorption profiles, using the modelled Voigt profile features. The correlation between the velocity width ΔV90 of the absorption profile and the metallicity is found to be tighter for DLAs than for sub-DLAs. We report hints of a bimodal distribution in the [Fe/H] metallicity of low redshift (z < 1.25) sub-DLAs, which is unseen at higher redshifts. This feature can be interpreted as a signature from the metal-poor, accreting gas and the metal-rich, outflowing gas, both being traced by sub-DLAs at low redshifts.

  18. In situ measurement of water vapor in the stratosphere with a cryogenically cooled Lyman-Alpha hygrometer

    NASA Astrophysics Data System (ADS)

    Schwab, J. J.; Weinstock, E. M.; Nee, J. B.; Anderson, J. G.

    1990-08-01

    In situ measurements of water vapor in the stratosphere with a new instrument are reported. The instrument has been designed to observe daytime water vapor from a multi-instrument balloon gondola that simultaneously measures free radicals such as OH, HO2, and O3 in the stratosphere up to 40 km. Lyman-alpha photofragment fluorescence is used to measure water molecules in a flowing sample of ambient air. Outgassing from the interior walls of the instrument is avoided by cooling the walls with liquid nitrogen to a temperature near or below the dewpoint of the environment and by drawing air through the instrument with a fan. A brief description of the instrument is given, followed by the results of the first our balloon flights. Because frost formation in the scattering chamber resulted in a large and variable background, the data from July 15, 1987, have a relatively modest signal-to-noise ratio. The measured mixing ratio for this flight varies from 3.0-5.5 ppmv over the altitude range of 17-34 km. Adjustments in the cooling protocol for the flights of July 6, 1988, July 28, and August 25, 1989, result in a much higher signal-to-noise ratio. Profiles from these three flights are similar to, but somewhat higher, than the 1987 profile. The July 1988 and August 1989 profiles exhibit the highest mixing ratios, reaching peak values of about 6.5 ppmv near 35 km. Implications of these four measurements are discussed, as are the issues of short- and long-term variability of stratospheric water vapor.

  19. An extreme [O III] emitter at z = 3.2: a low metallicity Lyman continuum source

    NASA Astrophysics Data System (ADS)

    de Barros, S.; Vanzella, E.; Amorín, R.; Castellano, M.; Siana, B.; Grazian, A.; Suh, H.; Balestra, I.; Vignali, C.; Verhamme, A.; Zamorani, G.; Mignoli, M.; Hasinger, G.; Comastri, A.; Pentericci, L.; Pérez-Montero, E.; Fontana, A.; Giavalisco, M.; Gilli, R.

    2016-01-01

    Aims: Cosmic reionization is an important process occurring in the early epochs of the Universe. However, because of observational limitations due to the opacity of the intergalactic medium to Lyman continuum photons, the nature of ionizing sources is still not well constrained. While high-redshift star-forming galaxies are thought to be the main contributors to the ionizing background at z> 6, it is impossible to directly detect their ionizing emission. Therefore, looking at intermediate redshift analogues (z ~ 2-4) can provide useful hints about cosmic reionization. Methods: We investigate the physical properties of one of the best Lyman continuum emitter candidate at z = 3.212 found in the GOODS-S/CANDELS field with photometric coverage from the U to the MIPS 24 μm band and VIMOS/VLT and MOSFIRE/Keck spectroscopy. These observations allow us to derive physical properties such as stellar mass, star formation rate, age of the stellar population, dust attenuation, metallicity, and ionization parameter, and to determine how these parameters are related to the Lyman continuum emission. Results: Investigation of the UV spectrum confirms a direct spectroscopic detection of the Lyman continuum emission with S/N> 5. Non-zero Lyα flux at the systemic redshift and high Lyman-α escape fraction (fesc(Lyα) ≥ 0.78) suggest a low H i column density. The weak C and Si low-ionization absorption lines are also consistent with a low covering fraction along the line of sight. The subsolar abundances are consistent with a young and extreme starburst. The [O iii]λλ4959,5007+Hβ equivalent width (EW) is one of the largest reported for a galaxy at z> 3 (EW( [ O iii ] λλ4959,5007 + Hβ) ≃ 1600 Å, rest-frame; 6700 Å observed-frame) and the near-infrared spectrum shows that this is mainly due to an extremely strong [O iii] emission. The large observed [O iii]/[O ii] ratio (>10) and high ionization parameter are consistent with prediction from photoionization models in the

  20. Strong H I Lyman-α variations from an 11 Gyr-old host star: a planetary origin?

    NASA Astrophysics Data System (ADS)

    Bourrier, V.; Ehrenreich, D.; Allart, R.; Wyttenbach, A.; Semaan, T.; Astudillo-Defru, N.; Gracia-Berná, A.; Lovis, C.; Pepe, F.; Thomas, N.; Udry, S.

    2017-06-01

    Kepler-444 provides a unique opportunity to probe the atmospheric composition and evolution of a compact system of exoplanets smaller than the Earth. Five planets transit this bright K star at close orbital distances, but they are too small for their putative lower atmosphere to be probed at optical/infrared wavelengths. We used the Space Telescope Imaging Spectrograph instrument on board the Hubble Space Telescope to search for the signature of the planet's upper atmospheres at six independent epochs in the Lyman-α line. We detect significant flux variations during the transits of both Kepler-444 e and f ( 20%), and also at a time when none of the known planets was transiting ( 40%). Variability in the transition region and corona of the host star might be the source of these variations. Yet, their amplitude over short timescales ( 2-3 h) is surprisingly strong for this old (11.2 ± 1.0 Gyr) and apparently quiet main-sequence star. Alternatively, we show that the in-transit variations could be explained by absorption from neutral hydrogen exospheres trailing the two outer planets (Kepler-444 e and f). They would have to contain substantial amounts of water to replenish hydrogen exospheres such as these, which would reveal them to be the first confirmed ocean planets. The out-of-transit variations, however, would require the presence of an as-yet-undetected Kepler-444 g at larger orbital distance, casting doubt on the planetary origin scenario. Using HARPS-N observations in the sodium doublet, we derived the properties of two interstellar medium clouds along the line of sight toward Kepler-444. This allowed us to reconstruct the stellar Lyman-α line profile and to estimate the extreme-UV (XUV) irradiation from the star, which would still allow for a moderate mass loss from the outer planets after 11.2 Gyr. Follow-up of the system at XUV wavelengths will be required to assess this tantalizing possibility.

  1. Estimation of the solar Lyman alpha flux from ground based measurements of the Ca II K line

    NASA Technical Reports Server (NTRS)

    Rottman, G. J.; Livingston, W. C.; White, O. R.

    1990-01-01

    Measurements of the solar Lyman alpha and Ca II K from October 1981 to April 1989 show a strong correlation (r = 0.95) that allows estimation of the Lyman alpha flux at 1 AU from 1975 to December 1989. The estimated Lyman alpha strength of 3.9 x 10 to the 11th + or - 0.15 x 10 to the 11th photons/s sq cm on December 7, 1989 is at the same maximum levels seen in Cycle 21. Relative to other UV surrogates (sunspot number, 10.7 cm radio flux, and He I 10830 line strength), Lyman alpha estimates computed from the K line track the SME measurements well from solar maximum, through solar minimum, and into Cycle 22.

  2. Remote sensing of neutral temperatures in the Earth's thermosphere using the Lyman-Birge-Hopfield bands of N2: Comparisons with satellite drag data

    NASA Astrophysics Data System (ADS)

    Krywonos, Andrey; Murray, D. J.; Eastes, R. W.; Aksnes, A.; Budzien, S. A.; Daniell, R. E.

    2012-09-01

    This paper presents remotely sensed neutral temperatures obtained from ultraviolet observations and compares them with temperatures from the NRLMSISE-00 version of the Mass Spectrometer and Incoherent Scatter (MSIS) model (unconstrained and constrained to match the total densities from satellite drag). Latitudinal profiles of the temperatures in the Earth's thermosphere are obtained by inversion of high-resolution (˜1.3 Å) observations of the (1,1) and (5,4) Lyman-Birge-Hopfield (LBH) bands of N2. The spectra are from the High resolution Ionospheric and Thermospheric Spectrograph (HITS) instrument aboard the Advanced Research and Global Observation Satellite (ARGOS). The results indicate that on each day examined there was consistency between the remotely sensed thermospheric temperatures, the densities from coincident satellite drag measurements at adjacent altitudes, and the NRLMSISE-00 model.

  3. Dust properties of Lyman-break galaxies at z ~ 3

    NASA Astrophysics Data System (ADS)

    Álvarez-Márquez, J.; Burgarella, D.; Heinis, S.; Buat, V.; Lo Faro, B.; Béthermin, M.; López-Fortín, C. E.; Cooray, A.; Farrah, D.; Hurley, P.; Ibar, E.; Ilbert, O.; Koekemoer, A. M.; Lemaux, B. C.; Pérez-Fournon, I.; Rodighiero, G.; Salvato, M.; Scott, D.; Taniguchi, Y.; Vieira, J. D.; Wang, L.

    2016-03-01

    Context. Since the mid-1990s, the sample of Lyman-break galaxies (LBGs) has been growing thanks to the increasing sensitivities in the optical and in near-infrared telescopes for objects at z> 2.5. However, the dust properties of the LBGs are poorly known because the samples are small and/or biased against far-infrared (far-IR) or submillimeter (submm) observations. Aims: This work explores from a statistical point of view the far-IR and submm properties of a large sample of LBGs at z ~ 3 that cannot be individually detected from current far-IR observations. Methods: We select a sample of 22, 000 LBGs at 2.5

  4. Solar hydrogen Lyman-α variation during solar cycles 21 and 22

    NASA Astrophysics Data System (ADS)

    Kent Tobiska, W.; Pryor, Wayne R.; Ajello, Joseph M.

    1997-05-01

    A full-disk, line-integrated solar Lyman-α dataset is presented that spans two solar cycles. The dataset is created partially from AE-E and SME data that is scaled to the Pioneer Venus Orbiter Ultraviolet Spectrometer (PVOUVS) upwind Lyman-α sky background data which is converted to a solar surrogate. PVOUVS measurements overlap AE-E, SME, and UARS observing periods and are calibrated to UARS/SOLSTICE irradiance units at 1 AU. The scaled AE-E/SME, the SOLSTICE, and the PVOUVS surrogate data in the interim between the satellites collectively form a composite dataset with a quiet sun value of 3.0+/-0.1×1011 photons cm-2s-1 common for three solar minima and a solar maximum value of 6.75+/-0.25×1011 photons cm-2s-1 common to cycles 21 and 22.

  5. Solar hydrogen Lyman-α variation during solar cycles 21 and 22

    NASA Astrophysics Data System (ADS)

    Tobiska, W. Kent; Pryor, Wayne R.; Ajello, Joseph M.

    1997-05-01

    A full-disk, line-integrated solar Lyman-α dataset is presented that spans two solar cycles. The dataset is created partially from AE-E and SME data that is scaled to the Pioneer Venus Orbiter Ultraviolet Spectrometer (PVOUVS) upwind Lyman-α sky background data which is converted to a solar surrogate. PVOUVS measurements overlap AE-E, SME, and UARS observing periods and are calibrated to UARS/SOLSTICE irradiance units at 1 AU. The scaled AE-E/SME, the SOLSTICE, and the PVOUVS surrogate data in the interim between the satellites collectively form a composite dataset with a quiet sun value of 3.0±0.1 × 1011 photons cm-2s-1 common for three solar minima and a solar maximum value of 6.75±0.25 × 1011 photons cm-2s-1 common to cycles 21 and 22.

  6. Detection of Lyman continuum absorption in the BL Lacertae object PKS 0735+178

    NASA Technical Reports Server (NTRS)

    Bregman, J. N.; Glassgold, A. E.; Huggins, P. J.

    1981-01-01

    The detection of the Lyman edge in the BL Lac object PKS 0735+178 at the absorption red shift determined by optical measurements leads to a lower limit for the column density of atomic hydrogen, N(H I) not less than 4(17)/sq cm. The Lyman-alpha absorption line appears to have been detected, but only an approximate upper limit can be obtained from the data, of the order of 2(19)/sq cm. This amount of atomic hydrogen is less than that for a line of sight through the disk of a normal spiral galaxy. It is suggested that the absorbing material exists either in the halo of a galaxy or in the tenuous, extended, gaseous disk of a galaxy.

  7. Competition between pressure and gravity confinement in Lyman Alpha forest observations

    NASA Technical Reports Server (NTRS)

    Charlton, Jane C.; Salpeter, Edwin E.; Linder, Suzanne M.

    1994-01-01

    A break in the distribution function of Lyman Alpha clouds (at a typical redshift of 2.5) has been reported by Petit-jean et al. (1993). This feature is what would be expected from a transition between pressure confinement and gravity confinement (as predicted in Charlton, Salpeter & Hogan 1993). The column density at which the feature occurs has been used to determine the external confining pressure approximately 10 per cu cm K, which could be due to a hot, intergalactic medium. For models that provide a good fit to the data, the contribution of the gas in clouds to omega is small. The specific shape of the distribution function at the transition (predicted by models to have a nonmonotonic slope) can serve as a diagnostic of the distribution of dark matter around Lyman Alpha forest clouds, and the present data already eliminate certain models.

  8. Self-regulating galaxy formation. Part 1: HII disk and Lyman alpha pressure

    NASA Technical Reports Server (NTRS)

    Cox, D. P.

    1983-01-01

    Assuming a simple but physically based prototype for behavior of interstellar material during formation of a disk galaxy, coupled with the lowest order description of infall, a scenario is developed for self-regulated disk galaxy formation. Radiation pressure, particularly that of Lyman depha (from fluorescence conversion Lyman continuum), is an essential component, maintaining an inflated disk and stopping infall when only a small fraction of the overall perturbation has joined the disk. The resulting galaxies consist of a two dimensional family whose typical scales and surface density are expressable in terms of fundamental constants. The model leads naturally to galaxies with a rich circumgalactic environment and flat rotation curves (but is weak in its analysis of the subsequent evolution of halo material).

  9. The Early Years: Lyman Spitzer, Jr. and the Physics of Star Formation

    NASA Astrophysics Data System (ADS)

    Elmegreen, Bruce G.

    The discovery of the interstellar medium and the early work of Lyman Spitzer, Jr. are reviewed here in the context of the remarkable observation in the early 1950's that star formation continues in the present age. Prior to this observation, stars were thought to have formed only at the beginning of the universe. The main debate in the 1930's was whether stars had the young age of ~3 Gyr suggested by the expansion of the universe and the meteorites, or the old age of 10^{13} yr suggested by thermalized stellar motions. The adoption of Ambartsumian's claim of modern-day star formation was slow and mixed in the early 1950's. While some astronomers like Adriaan Blaauw immediately followed, adding more from their own data, others were slow to change. By the end of the 1950's, Lyman had deduced the basic theory for star formation that we would recognize today.

  10. Large Area Lyman Alpha Survey: Finding Young Galaxies at z=4.5

    NASA Astrophysics Data System (ADS)

    Malhotra, S.; Rhoads, J.; Dey, A.; Stern, D.; Spinrad, H.

    Strong Lyα emission is a signpost of young stars and the absence of dust and thus indicates young galaxies. To find such a population of young galaxies at z=4.5 we started the Large Area Lyman Alpha survey (LALA). This survey achieves an unprecedented combination of volume and sensitivity by using narrow-band filters on a large format (36' × 36') camera on the 4 meter telescope at KPNO. The volume density and star-formation contribution of the Lyα emitters at z=4.5 is comparable to that of Lyman break galaxies. With many candidates and a few spectroscopic confirmations in hand we discuss what the properties of Lyα emitters imply for galaxy and star formation in the early universe.

  11. Lyman-alpha clouds as a relic of primordial density fluctuations

    NASA Technical Reports Server (NTRS)

    Bond, J. R.; Szalay, A. S.; Silk, J.

    1988-01-01

    Primordial density fluctuations are studied using a CDM model and primordial clouds some of which are expanding, driven by pressure gradients created when the medium is photionized, and some of which are massive enough to continue collapsing in spite of the pressure. Normalization of CDM models to the clustering properties on large scales are used to predict the parameters of collapsing clouds of subgalactic mass at early epochs. It is shown that the abundance and dimensions of these clouds are comparable to those of the Lyman-alpha systems. The evolutionary history of the clouds is computed, utilizing a spherically symmetric hydrodynamics code with the dark matter treated as a collisionless fluid, and the H I column density distribution is evaluated as a function of N(H I) and redshift. The observed cloud parameters come out naturally in the CDM model and suggest that Lyman-alpha clouds are the missing link between primordial density fluctuations and the formation of galaxies.

  12. Effect of the Lyman-alpha forest on the ultraviolet continua of very high redshift quasars

    SciTech Connect

    Steidel, C.C.; Sargent, W.L.W.

    1987-02-01

    Moderate resolution spectra are reported for eight high-redshift quasars (z over 2.7) observed with the Hale 5.08 m telescope. Newly-determined redshifts and apparent continuum visual magnitudes are tabulated for the objects Q0014 + 8118, Q0308 + 1902, Q0731 + 6519, Q0805 + 0441, Q0903 + 1734, Q0941 + 2606, Q0956 + 1217 and Q1358 + 1134 over the observed wavelength range 3200-10,000 A. It is shown that low resolution spectra, such as obtained with the IUE, can yield continuum levels significantly below those detected at very high resolution due to line and continuum absorption by neutral hydrogen along the line of sight to the quasar being studied. Estimates are made of the fractional flux decrement below Lyman-alpha and above Lyman-beta emission due to the intervening material. 38 references.

  13. LRO-Lyman Alpha Mapping Project (LAMP) Observations of the GRAIL Impact Plumes

    NASA Astrophysics Data System (ADS)

    Retherford, Kurt D.; Greathouse, T. K.; Hurley, D. M.; Gladstone, G. R.; Hayne, P. O.; Paige, D. A.; Greenhagen, B. T.; Sefton-Nash, E.; Zuber, M. T.; Smith, D. E.; Colaprete, A.; Kaufmann, D. E.; Miles, P. F.; Grava, C.; Throop, H.; Feldman, P. D.; Hendrix, A. R.; Pryor, W. R.; Stubbs, T. J.; Glenar, D. A.; Parker, J. W.; Stern, S. A.

    2013-10-01

    The Lyman Alpha Mapping Project (LAMP) UV spectrograph on the Lunar Reconnaissance Orbiter (LRO) was positioned to directly view the expanding gas plumes from the two GRAIL spacecraft impacts on 17 December 2012. LAMP detected resonantly scattered emissions from Hg and H atoms in the sunlit regions of these plumes. The spectral, spatial, and light-curve analyses used in these gas detections are consistent with previous LAMP observations of the LCROSS impact into the permanently shadowed region of Cabeus crater. LAMP's detection of atomic H by Lyman-α emission at the Moon (a first) was facilitated by pointing at the nightside surface to eliminate sky background noise. Volatile transport of Hg and H species is known to concentrate them near the poles, and in the context of LRO-Diviner temperature measurements of these high-latitude (75.6° N) impact sites the LAMP detections address this process.

  14. Response of the H-geocorona to geomagnetic disturbances studied by TWINS Lyman-alpha data

    NASA Astrophysics Data System (ADS)

    Zoennchen, Jochen; Nass, Uwe; Fahr, Hans

    2016-04-01

    We have studied the variation of the exospheric H-density distribution during two geomagnetic storms of different strength in terms of their Dst-index values. This analysis is based on continuously monitored Lyman-alpha data observed by the TWINS1/2-LAD instruments. Since solar Lyman-alpha radiation is resonantly backscattered from geocoronal neutral hydrogen (H), the resulting resonance glow intensity in the optically thin regime is proportional to H-column density along the line of sight (LOS). We quantify the amplitude of the H-density's response to geomagnetic activity for different (observed) angular regions and radial Earth-distances. Interestingly the H-exosphere responded with a comparable density increase to both storms of different strength. Careful analysis of the geomagnetic H-density effect indicates that the temporal density response is well correlated with the Kp-index daily sum, but not with the Dst-index in case of the two analysed storms.

  15. Performance Characterization of UV Science Cameras Developed for the Chromospheric Lyman-Alpha Spectro-Polarimeter

    NASA Technical Reports Server (NTRS)

    Champey, P.; Kobayashi, K.; Winebarger, A.; Cirtain, J.; Hyde, D.; Robertson, B.; Beabout, D.; Beabout, B.; Stewart, M.

    2014-01-01

    The NASA Marshall Space Flight Center (MSFC) has developed a science camera suitable for sub-orbital missions for observations in the UV, EUV and soft X-ray. Six cameras will be built and tested for flight with the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), a joint National Astronomical Observatory of Japan (NAOJ) and MSFC sounding rocket mission. The goal of the CLASP mission is to observe the scattering polarization in Lyman-alpha and to detect the Hanle effect in the line core. Due to the nature of Lyman-alpha polarization in the chromosphere, strict measurement sensitivity requirements are imposed on the CLASP polarimeter and spectrograph systems; science requirements for polarization measurements of Q/I and U/I are 0.1 percent in the line core. CLASP is a dual-beam spectro-polarimeter, which uses a continuously rotating waveplate as a polarization modulator, while the waveplate motor driver outputs trigger pulses to synchronize the exposures. The CCDs are operated in frame-transfer mode; the trigger pulse initiates the frame transfer, effectively ending the ongoing exposure and starting the next. The strict requirement of 0.1 percent polarization accuracy is met by using frame-transfer cameras to maximize the duty cycle in order to minimize photon noise. Coating the e2v CCD57-10 512x512 detectors with Lumogen-E coating allows for a relatively high (30 percent) quantum efficiency at the Lyman-alpha line. The CLASP cameras were designed to operate with 10 e-/pixel/second dark current, 25 e- read noise, a gain of 2.0 +/- 0.5 and 1.0 percent residual non-linearity. We present the results of the performance characterization study performed on the CLASP prototype camera; dark current, read noise, camera gain and residual non-linearity.

  16. Performance Characterization of UV Science Cameras Developed for the Chromospheric Lyman-Alpha Spectro-Polarimeter

    NASA Technical Reports Server (NTRS)

    Champey, Patrick; Kobayashi, Ken; Winebarger, Amy; Cirtain, Jonathan; Hyde, David; Robertson, Bryan; Beabout, Brent; Beabout, Dyana; Stewart, Mike

    2014-01-01

    The NASA Marshall Space Flight Center (MSFC) has developed a science camera suitable for sub-orbital missions for observations in the UV, EUV and soft X-ray. Six cameras will be built and tested for flight with the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), a joint National Astronomical Observatory of Japan (NAOJ) and MSFC sounding rocket mission. The goal of the CLASP mission is to observe the scattering polarization in Lyman-alpha and to detect the Hanle effect in the line core. Due to the nature of Lyman-alpha polarization in the chromosphere, strict measurement sensitivity requirements are imposed on the CLASP polarimeter and spectrograph systems; science requirements for polarization measurements of Q/I and U/I are 0.1 percent in the line core. CLASP is a dual-beam spectro- polarimeter, which uses a continuously rotating waveplate as a polarization modulator, while the waveplate motor driver outputs trigger pulses to synchronize the exposures. The CCDs are operated in frame-transfer mode; the trigger pulse initiates the frame transfer, effectively ending the ongoing exposure and starting the next. The strict requirement of 0.1 percent polarization accuracy is met by using frame-transfer cameras to maximize the duty cycle in order to minimize photon noise. Coating the e2v CCD57-10 512x512 detectors with Lumogen-E coating allows for a relatively high (30 percent) quantum efficiency at the Lyman-alpha line. The CLASP cameras were designed to operate with a gain of 2.0 +/- 0.5, less than or equal to 25 e- readout noise, less than or equal to 10 e-/second/pixel dark current, and less than 0.1percent residual non-linearity. We present the results of the performance characterization study performed on the CLASP prototype camera; system gain, dark current, read noise, and residual non-linearity.

  17. Path integral formalism for the spectral line shape in plasmas: Lyman-{alpha} with fine structure

    SciTech Connect

    Bedida, N.; Meftah, M. T.; Boland, D.; Stamm, R.

    2008-10-22

    We examine in this work the expression of the dipolar autocorrelation function for an emitter in the plasma using the path integrals formalism. The results for Lyman alpha lines with fine structure are retrieved in a compact formula. The expression of the dipolar autocorrelation function takes into account the ions dynamics and the fine structure effects. The electron's effect is represented by the impact operator {phi}{sub e} in the final formula.

  18. Probing Cosmological Reionization with the High-redshift Lyman-alpha Forest

    NASA Astrophysics Data System (ADS)

    D'Aloisio, Anson; McQuinn, Matthew; Trac, Hy

    2017-06-01

    When the first galaxies emerged, ~100 - 500 million years after the Big Bang, their starlight likely reionized and heated the intergalactic hydrogen that had existed since cosmological recombination. Much is currently unknown about this process, including what spatial structure it had, when it started and completed, and even which sources drove it. In this talk, I will discuss what recent and upcoming observations of the high-redshift Lyman-alpha forest could tell us about the reionization process.

  19. Calculation of the quasi-energies and resonances behavior of the hydrogen Lyman-alpha problem

    NASA Astrophysics Data System (ADS)

    Ruyten, Wilhelmus M.

    1992-03-01

    Recently, Bakshi and Kalman presented numerical results for the quasi-energies of the n = 2 multiplet in the hydrogen Lyman-alpha transition for a plasma in which both strong static and oscillating electric fields are present. Recent work on related magnetic and optical resonance problems provides a simplified mathematical treatment, as well as greater insight into the complex resonance behavior of this interaction.

  20. Calculation of the quasi-energies and resonances behavior of the hydrogen Lyman-alpha problem

    NASA Technical Reports Server (NTRS)

    Ruyten, Wilhelmus M.

    1992-01-01

    Recently, Bakshi and Kalman presented numerical results for the quasi-energies of the n = 2 multiplet in the hydrogen Lyman-alpha transition for a plasma in which both strong static and oscillating electric fields are present. Recent work on related magnetic and optical resonance problems provides a simplified mathematical treatment, as well as greater insight into the complex resonance behavior of this interaction.

  1. Estimating Exospheric Hydrogen Density Using Lyman-a Solar Irradiance Measurements From SOLSTICE

    NASA Astrophysics Data System (ADS)

    Pierrat, Z.; Snow, M. A.; Machol, J. L.

    2016-12-01

    The final layer of the earth's atmosphere, the exosphere, extends from 500km-10,000km above the earth's surface and is characterized by atomic densities of hydrogen so low that atomic collisions seldom occur. The small amount of hydrogen, however, still has a significant impact on satellite drag and satellite sensor observations that must look through the exosphere. The Solar Radiation Comparison Experiment (SORCE), which orbits well within the exosphere, at 645km, exemplifies this effect. The Solar-Stellar Irradiance Comparison Experiment (SOLSTICE) on SORCE samples a wide range of solar spectral irradiances, including Lyman-a, and is impacted by the effects of exospheric hydrogen. As solar photons enter the exosphere, hydrogen scatters Lyman-a out of the line of sight to SOLSTICE. SOLSTICE measures over a range of path lengths through the exosphere as it orbits, dependent on the angle between the satellite and the sun. The longer the path length, the more scattering of light occurs before reaching the satellite. By correcting the data from SOLSTICE for Lyman-a scattering, we not only produce a better solar irradiance data set for climate and other studies, but we can also learn more about the density of hydrogen in the exosphere. SORCE has been in orbit since 2003, so we can track the changes in the density of exospheric hydrogen through the solar cycle. This research is aimed at determining the impact of Lyman-a scattering on the SOLSTICE data set, finding a function to model the density of hydrogen in the exosphere, and tracking the changes in exospheric hydrogen density through time. This information will improve our understanding of the interactions between the sun and the upper atmosphere, as well as helping improve satellite drag models.

  2. STIS Spectroscopy of the Lyman-Alpha Forest Toward 3C 273

    NASA Technical Reports Server (NTRS)

    Heap, Sara R.; Williger, Gerard

    2002-01-01

    We present results on the low-redshift Lyman-alpha forest as based on high-resolution (7 km/s) STIS spectra of 3C 273. A total of 121 intergalactic Lyman-alpha-absorbing systems were detected, of which 60 are above the 3.5sigma completeness limit, logNu(sub HI) approximately equals 12.3. The median line-width parameter, b = 27 km/s, is similar to that seen at high redshift. However the distribution of HI column densities has a steeper slope, beta = 2.02+/-0.21, than is seen at high redshift. Overall, the observed Nu(sub HI)-b distribution is consistent with that derived from a ACDM hydrodynamic simulation. We have used NED to compile a list of 300 galaxies (91 from SDSS, 98 from APM) within 1 Mpc of the line of sight to 3C 273 and are working to find line-of-sight velocity correlations between the galaxies and detected Lyman-alpha absorbers.

  3. STIS Spectroscopy of the Lyman-Alpha Forest Toward 3C 273

    NASA Technical Reports Server (NTRS)

    Heap, Sara R.; Williger, Gerard

    2002-01-01

    We present results on the low-redshift Lyman-alpha forest as based on high-resolution (7 km/s) STIS spectra of 3C 273. A total of 121 intergalactic Lyman-alpha-absorbing systems were detected, of which 60 are above the 3.5sigma completeness limit, logNu(sub HI) approximately equals 12.3. The median line-width parameter, b = 27 km/s, is similar to that seen at high redshift. However the distribution of HI column densities has a steeper slope, beta = 2.02+/-0.21, than is seen at high redshift. Overall, the observed Nu(sub HI)-b distribution is consistent with that derived from a ACDM hydrodynamic simulation. We have used NED to compile a list of 300 galaxies (91 from SDSS, 98 from APM) within 1 Mpc of the line of sight to 3C 273 and are working to find line-of-sight velocity correlations between the galaxies and detected Lyman-alpha absorbers.

  4. The Lyman-alpha Solar Telescope for the ASO-S

    NASA Astrophysics Data System (ADS)

    Li, Hui

    2015-08-01

    The Lyman-alpha Solar Telescope (LST) is one of the payloads for the proposed Space-Borne Advanced Solar Observatory (ASO-S). LST consists of a Solar Disk Imager (SDI) with a field-of-view (FOV) of 1.2 Rsun, a Solar Corona Imager (SCI) with an FOV of 1.1 - 2.5 Rsun, and a full-disk White-light Solar Telescope (WST) with an FOV of 1.2 Rsun, which also serves as the guiding telescope. The SCI is designed to work at the Lyman-alpha waveband and white-light, while the SDI will work at the Lyman-alpha waveband only. The WST works both in visible (for guide) and ultraviolet (for science) white-light. The LST will observe the Sun from disk-center up to 2.5 solar radii for both solar flares and coronal mass ejections. In this presentation, I will give an introduction to LST, including scientific objectives, science requirement, instrument design and current status.

  5. Identification of a galaxy responsible for a high-redshift Lyman-α absorption system

    NASA Astrophysics Data System (ADS)

    Djorgovski, S. G.; Pahre, M. A.; Bechtold, J.; Elston, R.

    1996-07-01

    DAMPEDLyman-α systems are high-column-density intergalactic clouds of hydrogen, the existence of which is inferred from absorption lines appearing in the emission spectra of distant quasars. The galaxies believed to be responsible for these absorption systems have been suggested as possible progenitors of the normal disk galaxies observed in the local Universe1. Indeed, Lyman-α systems appear to contain a substantial fraction of the baryons known to exist in galaxies today2,3. Here we report the optical detection of a galaxy (designated DLA2233 + 131) associated with a known4 damped Lyman-α absorption system at a redshift of z = 3.150. The properties of this galaxy correspond closely to those expected of a young disk galaxy in the early stages of formation, and show no evidence for an active nucleus. This finding gives strong support to the idea that damped Lyman-α systems represent a population of young galaxies at high red-shifts.

  6. Spatial correlation between submillimetre and Lyman-alpha galaxies in the SSA 22 protocluster.

    PubMed

    Tamura, Yoichi; Kohno, Kotaro; Nakanishi, Kouichiro; Hatsukade, Bunyo; Iono, Daisuke; Wilson, Grant W; Yun, Min S; Takata, Tadafumi; Matsuda, Yuichi; Tosaki, Tomoka; Ezawa, Hajime; Perera, Thushara A; Scott, Kimberly S; Austermann, Jason E; Hughes, David H; Aretxaga, Itziar; Chung, Aeree; Oshima, Tai; Yamaguchi, Nobuyuki; Tanaka, Kunihiko; Kawabe, Ryohei

    2009-05-07

    Lyman-alpha emitters are thought to be young, low-mass galaxies with ages of approximately 10(8) yr (refs 1, 2). An overdensity of them in one region of the sky (the SSA 22 field) traces out a filamentary structure in the early Universe at a redshift of z approximately 3.1 (equivalent to 15 per cent of the age of the Universe) and is believed to mark a forming protocluster. Galaxies that are bright at (sub)millimetre wavelengths are undergoing violent episodes of star formation, and there is evidence that they are preferentially associated with high-redshift radio galaxies, so the question of whether they are also associated with the most significant large-scale structure growing at high redshift (as outlined by Lyman-alpha emitters) naturally arises. Here we report an imaging survey of 1,100-microm emission in the SSA 22 region. We find an enhancement of submillimetre galaxies near the core of the protocluster, and a large-scale correlation between the submillimetre galaxies and the low-mass Lyman-alpha emitters, suggesting synchronous formation of the two very different types of star-forming galaxy within the same structure at high redshift. These results are in general agreement with our understanding of the formation of cosmic structure.

  7. Lyman Alpha Blobs in a Filament at z=2.38

    NASA Technical Reports Server (NTRS)

    Williger, G.; Francis, P.; Mushotzky, R.; Palunas, P.; Teplitz, H.; Weaver, K.; White, R.; Woodgate, B.

    2004-01-01

    Bright, extended Lyman-alpha nebulae (known as blobs) appear to be common in the densest environments at high redshift, and may be an important stage in galaxy evolution. Up to now, Chandra data have not distinguished between the possible excitation mechanisms, but suggest that we are seeing dense excitation mechanisms, but suggest that we are seeing dense intracluster gas either falling into forming galaxies (cooling flows) or being expelled into the intracluster medium, enriching it. Optical and X-ray evidence also suggests that some blobs harbor AGN. We took a 20 ksec exposure with Chandra of four Lyman-alpha blobs in a large filament at $z=2.38$, which completed the X-ray observations of all currently known blobs. We will present flux constraints for the blobs from the Chandra data and optical spectra of the field taken with the AAT+2dF (see accompanying poster by Woodgate et al.). Possible mechanisms for the extended emission of the Lyman-alpha blobs will be discussed.

  8. Exploring the nature of the Lyman-α emitter CR7

    NASA Astrophysics Data System (ADS)

    Hartwig, Tilman; Latif, Muhammad A.; Magg, Mattis; Bromm, Volker; Klessen, Ralf S.; Glover, Simon C. O.; Whalen, Daniel J.; Pellegrini, Eric W.; Volonteri, Marta

    2016-10-01

    CR7 is the brightest Lyman-α emitter observed at z > 6, which shows very strong Lyman-α and He II 1640 Å line luminosities, but no metal-line emission. Previous studies suggest that CR7 hosts either young primordial stars with a total stellar mass of ˜107 M⊙ or a black hole of ≳106 M⊙. Here, we explore different formation scenarios for CR7 with a semi-analytical model, based on the random sampling of dark matter merger trees. We are unable to reproduce the observational constraints with a primordial stellar source, given our model assumptions, due to the short stellar lifetimes and the early metal enrichment. Black holes that are the remnants of the first stars are either not massive enough, or reside in metal-polluted haloes, ruling out this possible explanation of CR7. Our models instead suggest that direct collapse black holes, which form in metal-free haloes exposed to large Lyman-Werner fluxes, are more likely the origin of CR7. However, this result is derived under optimistic assumptions and future observations are necessary to further constrain the nature of CR7.

  9. The Lyman Alpha Imaging-Monitor Experiment (LAIME) for TESIS/CORONAS-PHOTON

    NASA Astrophysics Data System (ADS)

    Damé, L.; Koutchmy, S.; Kuzin, S.; Lamy, P.; Malherbe, J.-M.; Noëns, J.-C.

    LAIME the Lyman Alpha Imaging-Monitor Experiment is a remarkably simple no mechanisms and compact 100x100x400 mm full Sun imager to be flown with TESIS on the CORONAS-PHOTON mission launch expected before mid-2008 As such it will be the only true chromospheric imager to be flown in the next years supporting TESIS EUV-XUV imaging SDO and the Belgian LYRA Lyman Alpha flux monitor on the ESA PROBA-2 microsatellite launch expected in September 2007 We will give a short description of this unique O60 mm aperture imaging telescope dedicated to the investigating of the magnetic sources of solar variability in the UV and chromospheric and coronal disruptive events rapid waves Moreton waves disparitions brusques of prominences filaments eruptions and CMEs onset The resolution pixel is 2 7 arcsec the field of view 1 4 solar radius and the acquisition cadence could be as high as 1 image minute The back thinned E2V CCD in the focal plane is using frame transfer to avoid shutter and mechanisms Further more the double Lyman Alpha filtering allows a 40 AA FWHM bandwidth and excellent rejection yet providing a vacuum seal design of the telescope MgF2 entrance window Structural stability of the telescope focal length 1 m is preserved by a 4-INVAR bars design with Aluminium compensation in a large pm 10 o around 20 o

  10. Search for a direction in the forest of Lyman

    SciTech Connect

    Hazra, Dhiraj Kumar; Shafieloo, Arman E-mail: shafieloo@kasi.re.kr

    2015-11-01

    We report the first test of isotropy of the Universe using the Lyman-α forest data from the high redshift quasars (z>2) (the signal from the matter dominated epoch) from SDSS-III BOSS-DR9 datasets. Using some specified data cuts, we obtain the probability distribution function (PDF) of the Lyman-α forest transmitted flux and use the statistical moments of the PDF to address the isotropy of the Universe. In an isotropic Universe one would expect the transmitted flux to have consistent statistical characteristics in different parts of the sky. We trisect the total survey area of 3275 deg{sup 2} along the galactic latitude and using quadrant convention. We also make three subdivisions in the data for three different signal-to-noise-ratios (SNR). Finally we obtain and compare the statistical moments in the mean redshifts of 2.3, 2.6 and 2.9. We find, that the moments from all patches overall agree at all redshifts and at all SNRs. Since Lyman-α transmitted flux directly maps the neutral hydrogen distribution in the inter galactic medium (IGM), our results indicate, within the limited survey area and sensitivity of the data, the distribution of the neutral hydrogen in the Universe is consistent with isotropic distribution. Increase in survey area and larger amount of data are needed to perform this isotropy test in a bigger domain and different directions in the sky.

  11. Determining interstellar hydrogen and deuterium column densities by means of the Lyman channel of the SPECTRUM UV Rowland spectrograph: a pre-launch feasibility study

    NASA Astrophysics Data System (ADS)

    Franchini, Mariagrazia; Morossi, Carlo; Vladilo, G.

    1996-10-01

    Our current knowledge of production and destruction of light elements in astrophysical processes suggests that deuterium is produced during Big Bang nucleosynthesis and destroyed when cycled through stars. Primordial deuterium abundance can be determined by measuring the D/H ratio in a variety of astrophysical environments with different degrees of chemical evolution: the D/H ratio of unprocessed material directly gives the primordial value, while the ratio in processed material is expected to be lower and consistent with the predictions of galactic chemical evolution models. Here we focus our attention on deuterium abundance determinations of chemically processed material such as the interstellar gas in our Galaxy. Up to now, most of the determinations of deuterium abundance have been performed in the solar system or in local interstellar clouds. However, the overall accuracy of the measurements in local clouds is still insufficient to probe evolutionary trends. New D/H measurements in clouds at different locations in our Galaxy would be necessary to establish this issue, while interstellar measurements in nearby galaxies would give further constraints on the deuterium evolution in different galactic environments. With this goal in mind we have evaluated the capability of the Lyman channel of the SPECTRUM UV Rowland spectrography in determining deuterium column density in distant interstellar clouds. Three packages have been used to obtain realistic predicted spectra and to derive `observed' column densities: (1) the MIDAS package `CLOUD', to generate theoretical interstellar absorption profiles; (2) the `Synth' package developed in the IRAF environment by two of the authors to simulate spectroscopic observations of point sources obtainable with an astronomical spectrograph, (3) the FITLYMAN package inside the Lyman context of MIDAS to derive `observed' column densities from predicted spectra. The minimum exposure times, t(subscript min), required to obtain a

  12. Nebular emission and the Lyman continuum photon escape fraction in CALIFA early-type galaxies

    NASA Astrophysics Data System (ADS)

    Papaderos, P.; Gomes, J. M.; Vílchez, J. M.; Kehrig, C.; Lehnert, M. D.; Ziegler, B.; Sánchez, S. F.; Husemann, B.; Monreal-Ibero, A.; García-Benito, R.; Bland-Hawthorn, J.; Cortijo-Ferrero, C.; de Lorenzo-Cáceres, A.; del Olmo, A.; Falcón-Barroso, J.; Galbany, L.; Iglesias-Páramo, J.; López-Sánchez, Á. R.; Marquez, I.; Mollá, M.; Mast, D.; van de Ven, G.; Wisotzki, L.

    2013-07-01

    We use deep integral field spectroscopy data from the CALIFA survey to study the warm interstellar medium (wim) over the entire extent and optical spectral range of 32 nearby early-type galaxies (ETGs). We find that faint nebular emission is extended in all cases, and its surface brightness decreases roughly as ∝ r-α. The large standard deviation in the derived α (1.09 ± 0.67) argues against a universal power-law index for the radial drop-off of nebular emission in ETGs. Judging from the properties of their extranuclear component, our sample ETGs span a broad, continuous sequence with respect to their α, Hα equivalent width (EW) and Lyman continuum (Lyc) photon leakage fraction (plf). We propose a tentative subdivision into two groups: Type i ETGs are characterized by rather steep Hα profiles (α ≃ 1.4), comparatively large (≳1 Å), nearly radially constant EWs, and plf ≃ 0. Photoionization by post-AGB stars appears to be the main driver of extended nebular emission in these systems, with nonthermal sources being potentially important only in their nuclei. Typical properties of type II ETGs are shallower Hα profiles (α ≃ 0.8), very low (≲0.5 Å) EWs with positive radial gradients, and a mean plf ≳ 0.7, rising to ≳0.9 in their centers. Such properties point to a low, and inwardly decreasing wim density and/or volume filling factor. We argue that, because of extensive Lyc photon leakage, emission-line luminosities and EWs are reduced in type II ETG nuclei by at least one order of magnitude. Consequently, the line weakness of these ETGs is by itself no compelling evidence for their containing merely "weak"(sub-Eddington accreting) active galactic nuclei (AGN). In fact, Lyc photon escape, which has heretofore not been considered, may constitute a key element in understanding why many ETGs with prominent signatures of AGN activity in radio continuum and/or X-ray wavelengths show only faint emission lines and weak signatures of AGN activity in

  13. Characterization and application of a narrow band Lyman-alpha light source

    NASA Astrophysics Data System (ADS)

    McCarthy, Timothy J.

    The Lyman-alpha emission line shape of dissociated hydrogen atoms in a high pressure Ne environment is studied. Vacuum ultra-violet absorption spectroscopy using the emitted Lyman-alpha radiation allows for the measurement of trace concentrations of ground state deuterium atoms in a hydrogen environment. Near resonant energy transfer from Ne excimer molecules to dissociative excitation of hydrogen molecules is utilized to generate excited state, n = 2, hydrogen atoms. Plasmas are generated in systems containing 250 to 600 [Torr] Ne with an admixture of 0.10 [Torr] H2 using a 12 [keV] electron beam. Experimental data on the upper states of the Lyman-alpha transition is collected via a new application of the dc opto-galvanic effect in low temperature, high pressure plasmas. A model line shape containing a non-thermal equilibrium atomic velocity distribution and pressure effects is developed. Excess energy from second continuum Ne excimers is imparted primarily to the dissociated hydrogen atoms giving the excited atoms a large excess velocity component. The dominant pressure effect is van der Waals interactions between the excited hydrogen atoms and ground state Ne atoms. Adjustable model parameters are optimized to fit the experimental data. Pressure broadening is observed to be non-linear, with the largest deviations from the predicted widths occurring at the lowest Ne pressures, while pressure shifting is linear in Ne pressure. The higher pressure data approaches the theoretical ratio between pressure width and shift for van der Waals interactions. Smooth extrapolation of the fit parameters, toward the theoretical limit, allows for the calculation of a Lyman-alpha emission line shape at a Ne pressure of 760 [Torr]. Hydrogen is replaced with deuterium in the system to provide a light source for absorption spectroscopy of ground state deuterium atoms. A discharge tube is filled to 3.5 [Torr] with H2 after introduction of a small admixture of D2. A discharge is

  14. Medium-resolution spectroscopy of FORJ0332-3557: probing the interstellar medium and stellar populations of a lensed Lyman-break galaxy at z = 3.77

    NASA Astrophysics Data System (ADS)

    Cabanac, Rémi A.; Valls-Gabaud, David; Lidman, Chris

    2008-06-01

    We recently reported the discovery of FORJ0332-3557, a lensed Lyman-break galaxy at z = 3.77 in a remarkable example of strong galaxy-galaxy gravitational lensing. We present here a medium-resolution rest-frame ultraviolet (UV) spectrum of the source, which appears to be similar to the well-known Lyman-break galaxy MS1512-cB58 at z = 2.73. The spectral energy distribution is consistent with a stellar population of less than 30Ma, with an extinction of Av = 0.5 mag and an extinction-corrected star formation rate SFRUV of 200-300h-170Msolara-1. The Lyα line exhibits a damped profile in absorption produced by a column density of about NHI = (2.5 +/- 1.0) × 1021cm-2, superimposed on an emission line shifted both spatially (0.5 arcsec with respect to the UV continuum source) and in velocity space (+830kms-1 with respect to the low-ionization absorption lines from its interstellar medium), a clear signature of outflows with an expansion velocity of about 270kms-1. A strong emission line from HeII λ164.04 nm indicates the presence of Wolf-Rayet stars and reinforces the interpretation of a very young starburst. The metallic lines indicate subsolar abundances of elements Si, Al and C in the ionized gas phase. Based on observations made at the ESO VLT under programmes 74.A-0536 and 78.A-0240. E-mail: remi.cabanac@ast.obs-mip.fr (RAC); david.valls-gabaud@obspm.fr (DV-G); clidman@eso.org (CL)

  15. Spectroscopic Confirmation of Three Redshift z~5.7 Lyα Emitters from the Large-Area Lyman Alpha Survey

    NASA Astrophysics Data System (ADS)

    Rhoads, James E.; Dey, Arjun; Malhotra, Sangeeta; Stern, Daniel; Spinrad, Hyron; Jannuzi, Buell T.; Dawson, Steve; Brown, Michael J. I.; Landes, Emily

    2003-03-01

    Narrowband searches for Lyα emission are an efficient way of identifying star-forming galaxies at high redshifts. We present Keck Telescope spectra confirming redshifts z~5.7 for three objects discovered in the Large-Area Lyman Alpha (LALA) survey at Kitt Peak National Observatory. All three spectra show strong, narrow emission lines with the asymmetric profile that is characteristically produced in high-redshift Lyα emitters by preferential H I absorption in the blue wing of the line. These objects are undetected in deep BW, V, R, and λ~6600 Å narrowband images from the NOAO Deep Wide-Field Survey and from LALA, as expected from Lyman break and Lyα forest absorption at redshift z~5.7. All three objects show large equivalent widths (>~150 Å in the rest frame), suggesting at least one of the following: a top-heavy initial mass function, very low stellar metallicity, or the presence of an active nucleus. We consider the case for an active nucleus to be weak in all three objects due to the limited width of the Lyα emission line (less than 500 km s-1) and the absence of any other indicator of quasar activity. The three confirmed high-redshift objects were among four spectroscopically observed targets drawn from the sample of 18 candidates presented by Rhoads & Malhotra. Thus, these spectra support the Lyα emitter population statistics from our earlier photometric study, which imply little evolution in number density from z=5.7 to 4.5 and provide strong evidence that the reionization redshift is zr>5.7.

  16. Giant Lyman-alpha Nebulae in the Illustris Simulation

    NASA Astrophysics Data System (ADS)

    Gronke, Max; Bird, Simeon

    2017-02-01

    Several “giant” Lyα nebulae with an extent ≳300 kpc and observed Lyα luminosity of ≳1044 erg s‑1 cm‑2 arcsec‑2 have recently been detected, and it has been speculated that their presence hints at a substantial cold gas reservoir in small cool clumps not resolved in modern hydrodynamical simulations. We use the Illustris simulation to predict the Lyα emission emerging from large halos (M > 1011.5 M⊙) at z ∼ 2 and thus test this model. We consider both active galactic nucleus (AGN) and star driven ionization, and compare the simulated surface brightness maps, profiles, and Lyα spectra to a model where most gas is clumped below the simulation resolution scale. We find that with Illustris, no additional clumping is necessary to explain the extents, luminosities, and surface brightness profiles of the “giant Lyα nebulae” observed. Furthermore, the maximal extents of the objects show a wide spread for a given luminosity and do not correlate significantly with any halo properties. We also show how the detected size depends strongly on the employed surface brightness cutoff, and predict that further examples of such objects will be found in the near future.

  17. The hydrogen Lyman-alpha emission of Capella

    NASA Technical Reports Server (NTRS)

    Ayres, Thomas R.; Brown, A.; Gayley, K. G.; Linsky, Jeffrey L.

    1993-01-01

    We describe the hydrogen Ly-alpha emission of the spectroscopic binary Capella (G8 III + GO III) recorded at 0.1 A resolution by the International Ultraviolet Explorer. The overt changes in the composite line shape with orbital phase are controlled by the active GO III star and permit a dissection of the stellar components despite the obliteration of the central portion of the profile by atomic hydrogen and deuterium absorption along the 12.5 pc sightline. The Ly-alpha line shape of the active GO III star is surprisingly asymmetric and possibly is variable. Both characteristics suggest a stellar wind of moderate excitation (20,000-100,000 K), a key component of the coronal evolution scenario of Simon and Drake (1989) for the Hertzsprung-gap giants.

  18. The Spacelab Lyman alpha and white light coronagraphs program

    NASA Technical Reports Server (NTRS)

    Kohl, J. L.; Withbroe, G. L.; Weiser, H.; Macqueen, R. M.; Munro, R. H.

    1981-01-01

    The Harvard-Smithsonian Center for Astrophysics and the High Altitude Observatory have defined a joint coronagraphs experiment for a future Spacelab mission. The instrumentation package would include an ultraviolet light coronagraph to measure the intensity and profiles of spectral lines formed between 1.2 and 8 solar radii from sun center and a white light coronagraph to measure the intensity and polarization of visible light. The overall goals of the joint program are to use new coronal plasma diagnostic techniques to understand the physical processes and mechanisms operating in the solar corona, to understand the acceleration of high-speed and low-speed solar wind streams and to extrapolate this knowledge to other stars in order to help understand the physics of stellar coronae and stellar mass loss.

  19. KECK SPECTROSCOPY OF FAINT 3>z>7 LYMAN BREAK GALAXIES: A HIGH FRACTION OF LINE EMITTERS AT REDSHIFT SIX

    SciTech Connect

    Stark, Daniel P.; Ellis, Richard S.; Ouchi, Masami

    2011-02-10

    As Ly{alpha} photons are scattered by neutral hydrogen, a change with redshift in the Ly{alpha} equivalent width (EW) distribution of distant galaxies offers a promising probe of the degree of ionization in the intergalactic medium and hence when cosmic reionization ended. This simple test is complicated by the fact that Ly{alpha} emission can also be affected by variations in the kinematics and dust content of the host galaxies. In the first paper in this series, we demonstrated both a luminosity- and redshift-dependent trend in the fraction of Ly{alpha} emitters seen within color-selected 'Lyman break' galaxies (LBGs) over the range 3 < z < 6; lower luminosity galaxies and those at higher redshift show an increased likelihood of strong emission. Here, we present the results from 12.5 hr exposures with the Keck DEIMOS spectrograph focused primarily on LBGs at z {approx_equal} 6 which enable us to confirm the redshift dependence of line emission more robustly and to higher redshift than was hitherto possible. We find that 54% {+-} 11% of faint z {approx_equal} 6 LBGs show strong (W{sub Ly{alpha},0}>25 A) emission, an increase of 55% from a sample of similarly luminous z {approx_equal} 4 galaxies. With a total sample of 74 z {approx_equal} 6 LBGs, we determine the luminosity-dependent Ly{alpha} EW distribution. Assuming continuity in these trends to the new population of z {approx_equal} 7 sources located with the Hubble WFC3/IR camera, we predict that unless the neutral fraction rises in the intervening 200 Myr, the success rate for spectroscopic confirmation using Ly{alpha} emission should be high.

  20. A study of the circumgalactic medium at z ˜ 0.6 using damped Lyman α galaxies

    NASA Astrophysics Data System (ADS)

    Rahmani, Hadi; Péroux, Céline; Turnshek, David A.; Rao, Sandhya M.; Quiret, Samuel; Hamilton, Timothy S.; Kulkarni, Varsha P.; Monier, Eric M.; Zafar, Tayyaba

    2016-11-01

    We present the study of a sample of nine quasi-stellar object fields, with damped Lyman α (DLA) or sub-DLA systems at z ˜ 0.6, observed with the X-Shooter spectrograph at the Very Large Telescope. By suitably positioning the X-Shooter slit based on high spatial resolution images of Hubble Space Telescope/Advanced Camera for Surveys we are able to detect absorbing galaxies in seven out of nine fields (˜78 per cent success rate) at impact parameters from 10 to 30 kpc. In five out of seven fields the absorbing galaxies are confirmed via detection of multiple emission lines at the redshift of DLAs where only one out of five also emits a faint continuum. In two out of these five fields we detect a second galaxy at the DLA redshift. Extinction corrected star formation rates (SFRs) of these DLA galaxies, estimated using their Hα fluxes, are in the range 0.3-6.7 M⊙ yr-1. The emission metallicities of these five DLA galaxies are estimated to be from 0.2 to 0.9 Z⊙. Based on the Voigt profile fits to absorption lines we find the metallicity of the absorbing neutral gas to be in a range of 0.05-0.6 Z⊙. The two remaining DLA galaxies are quiescent galaxies with SFR < 0.4 M⊙ yr-1 (3σ) presenting continuum emission but no emission lines. Using X-Shooter spectrum we estimate i-band absolute magnitude of -19.5 ± 0.2 for both these DLA galaxies that indicates they are sub-L⋆ galaxies. Comparing our results with that of other surveys in the literature we find a possible redshift evolution of the SFR of DLA galaxies.

  1. Polarization Calibration of the Chromospheric Lyman-Alpha SpectroPolarimeter for a 0.1 % Polarization Sensitivity in the VUV Range. Part I: Pre-flight Calibration

    NASA Astrophysics Data System (ADS)

    Giono, G.; Ishikawa, R.; Narukage, N.; Kano, R.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.; Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J.

    2016-12-01

    The Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) is a sounding rocket experiment designed to measure for the first time the linear polarization of the hydrogen Lyman-{α} line (121.6 nm) and requires a 0.1 % polarization sensitivity, which is unprecedented for a spectropolarimeter in the vacuum UV (VUV) spectral range.

  2. Detection of auroral hydrogen Lyman-Alpha emission from Uranus

    SciTech Connect

    Clarke, J.T.

    1982-12-15

    A series of observations of Uranus obtained with the short-wavelength spectrographs of the International Ultraviolet Explorer Observatory in 1982 April and June have revealed unexpectedly strong H Ly..cap alpha.. emission which varied between 430 and 850 Rayleighs in observed disk-averaged brightness over the course of these observations. The variability of the emission alone indicates that much of the emission must be produced by charged particle excitation of H in Uranus's upper atmosphere. In addition, comparison of these data with a model for resonant scattering of solar H Ly..cap alpha.. emission indicates that, over a wide range of model conditions, an emission brightness of even 430 Rayleighs (which was the lowest observed value) corresponds to an H column density on the order of 10/sup 17/ cm/sup -2/ in Uranus's upper atmosphere. At 20 AU from the Sun, solar EUV photodissociation of H/sub 2/ is insufficient to produce such a high column abundance of H, further supporting the identification of charged particle precipitation in Uranus's upper atmosphere. These data thus offer the first strong evidence for the presence of aurorae and therefore a magnetic field on Uranus.

  3. The Lyman-Continuum Fluxes and Stellar Parameters of O and Early B-Type Stars

    NASA Technical Reports Server (NTRS)

    Vacca, William D.; Garmany, Catherine D.; Shull, J. Michael

    1996-01-01

    Using the results of the most recent stellar atmosphere models applied to a sample of hot stars, we construct calibrations of effective temperature (T(sub eff)), and gravity (log(sub g)) with a spectral type and luminosity class for Galactic 0-type and early B-type stars. From the model results we also derive an empirical relation between the bolometric correction and T(sub eff) and log g. Using a sample of stars with known distances located in OB associations in the Galaxy and the Large Magellanic Cloud, we derive a new calibration of M(sub v) with spectral class. With these new calibrations and the stellar atmosphere models of Kurucz, we calculate the physical parameters and ionizing photon luminosities in the H(0) and He(0) continua for O and early B-type stars. We find substantial differences between our values of the Lyman- continuum luminosity and those reported in the literature. We also discuss the systematic discrepancy between O-type stellar masses derived from spectroscopic models and those derived from evolutionary tracks. Most likely, the cause of this 'mass discrepancy' lies primarily in the atmospheric models, which are plane parallel and hydrostatic and therefore do not account for an extended atmosphere and the velocity fields in a stellar wind. Finally, we present a new computation of the Lyman-continuum luminosity from 429 known O stars located within 2.5 kpc of the Sun. We find the total ionizing luminosity from this population ((Q(sub 0)(sup T(sub ot))) = 7.0 x 10(exp 51) photons/s) to be 47% larger than that determined using the Lyman continuum values tabulated by Panagia.

  4. New Horizons Alice sky Lyman-α at Pluto encounter: Importance for photochemistry

    NASA Astrophysics Data System (ADS)

    Retherford, K. D.; Gladstone, R.; Stern, S. A.; Weaver, H. A., Jr.; Young, L. A.; Olkin, C.; Cheng, A. F.; Greathouse, T.; Kammer, J.; Linscott, I.; Parker, A. H.; Parker, J. W.; Schindhelm, E.; Singer, K. N.; Steffl, A.; Strobel, D. F.; Summers, M. E.; Tsang, C.; Tyler, G. L.; Versteeg, M.; Woods, W. W.; Ennico Smith, K.; Hinson, D. P.; Pryor, W. R.; Cunningham, N. J.; Curdt, W.

    2015-12-01

    The third zone of our solar system, including the Pluto system, has a unique illumination environment at UV wavelengths. While direct solar Lyman-α emissions dominate the signal at 121.6 nm at classical solar system distances, the contribution of illumination by Interplanetary Medium (IPM) Lyman-α sky-glow is roughly on par at Pluto (Gladstone et al. 2015). The Pluto-Alice UV imaging spectrograph on New Horizons conducted several dedicated sky scans to measure the IPM Lyman-α both en route to and while at Pluto. These scans provide 6° by 360° great-circle swaths while spinning the spacecraft. Three sets of scans conducted en route are reported in Gladstone et al. (2012). During the Pluto encounter, sets of scans with six such swaths evenly spaced ~30° apart for all-sky coverage were obtained just before closest approach and again just after. These measurements agree well with brightness variations expected for IPM brightnesses peaking in the sunward direction and interspersed with detections of UV bright stars and other sky features. Previous studies estimated contributions of ~2/3rds direct solar Lyα and 1/3rd IPM Lyα. Our early results suggest that these model predictions need revision. These findings have important implications for determining the rates of photochemical reactions within Pluto's atmosphere that are driven by UV photons at 121.6 nm. Similarly, new constraints are provided to the rates of photolysis on Charon's polar winter nightside. These constraints are useful for understanding the volatile transport and long-term stability of the dark red region near Charon's pole discovered by New Horizons.

  5. An Attempt to Detect Coronal Mass Ejections in Lyman-α Using SOHO Swan

    NASA Astrophysics Data System (ADS)

    Mays, M. L.; St. Cyr, O. C.; Quémerais, E.; Ferron, S.; Bertaux, J.-L.; Yashiro, S.; Howard, R.

    2007-03-01

    In this study, the possibility that coronal mass ejections (CMEs) may be observed in neutral Lyman-α emission was investigated. An observing campaign was initiated for SWAN (Solar Wind ANisotropies), a Lyman-α scanning photometer on board the Solar and Heliospheric Observatory (SOHO) dedicated to monitoring the latitude distribution of the solar wind from its imprints on the interstellar sky background. This was part of SOHO Joint Observing Program (JOP) 159 and was an exploratory investigation as it was not known how, or even if, CMEs interact with the solar wind and interstellar neutral hydrogen at this distance (≈60 and 120 R S). The study addresses the lack of methods for tracking CMEs beyond the field-of-view of current coronagraphs (30 R S). In our first method we used LASCO, white-light coronagraphs on SOHO, and EIT, an extreme ultraviolet imaging telescope also on SOHO, to identify CME candidates which, subject to certain criteria, should have been observable in SWAN. The criteria included SWAN observation time and location, CME position angle, and extrapolated speed. None of the CME candidates that we discuss were identified in the SWAN data. For our second method we analyzed all of the SWAN data for 184 runs of the observing campaign, and this has yielded one candidate CME detection. The candidate CME appears as a dimming of the background Lyman-α intensity representing ≈10% of the original intensity, moving radially away from the Sun. Multiple candidate CMEs observed by LASCO and EIT were found which may have caused this dimming. Here we discuss the campaign, data analysis technique and statistics, and the results.

  6. The HST/ACS+WFC3 Survey for Lyman Limit Systems. II. Science

    NASA Astrophysics Data System (ADS)

    O'Meara, John M.; Prochaska, J. Xavier; Worseck, Gabor; Chen, Hsiao-Wen; Madau, Piero

    2013-03-01

    We present the first science results from our Hubble Space Telescope survey for Lyman limit absorption systems (LLS) using the low dispersion spectroscopic modes of the Advanced Camera for Surveys and the Wide Field Camera 3. Through an analysis of 71 quasars, we determine the incidence frequency of LLS per unit redshift and per unit path length, l(z) and l(X), respectively, over the redshift range 1 < z < 2.6, and find a weighted mean of l(X) =0.29 ± 0.05 for 2.0 < z < 2.5 through a joint analysis of our sample and that of Ribaudo et al. Through stacked spectrum analysis, we determine a median (mean) value of the mean free path to ionizing radiation at z = 2.4 of λ912 mfp = 243(252) h -1 72 Mpc, with an error on the mean value of ±43 h -1 72 Mpc. We also re-evaluate the estimates of λ912 mfp from Prochaska et al. and place constraints on the evolution of λ912 mfp with redshift, including an estimate of the "breakthrough" redshift of z = 1.6. Consistent with results at higher z, we find that a significant fraction of the opacity for absorption of ionizing photons comes from systems with N H I <=1017.5 cm-2 with a value for the total Lyman opacity of τLyman eff = 0.40 ± 0.15. Finally, we determine that at minimum, a 5-parameter (4 power law) model is needed to describe the column density distribution function f(N H I , X) at z ~ 2.4, find that f(N H I , X) undergoes no significant change in shape between z ~ 2.4 and z ~ 3.7, and provide our best fit model for f(N H I , X).

  7. Probing the Physical Properties of High-Redshift Lyman-Alpha Emitters with Spitzer

    NASA Astrophysics Data System (ADS)

    Finkelstein, Keely; Finkelstein, Steven; Rhoads, James E.; Malhotra, Sangeeta

    2015-08-01

    Abstract: Studies of Lyman Alpha emitting galaxies (LAEs) offer insight into an understanding of early galaxies and the build-up of galaxies at early times. To better understand these objects and constrain their stellar properties, we have observed a sample of 162 z=4.5 and 14 z=5.7 LAEs with deep Spitzer IRAC 3.6 and 4.5 micron imaging from the Spitzer Lyman Alpha Survey. This is by far the largest sample of high-redshift LAEs imaged with Spitzer, which probes rest-frame optical wavelengths at these redshifts, dramatically improving constraints on the stellar masses and star-formation rates. By fitting the spectral energy distributions of individual LAEs using ground-based optical, HST near-IR, and Spitzer mid-IR imaging, we show that our sample of LAEs has a wide range of stellar properties. For individual LAEs detected with IRAC, stellar mass ranges from 5x10^8 - 10^11 solar masses. In addition, we find a correlation between stellar mass and star formation rate (SFR), similar to trends measured at lower redshift (e.g. Noeske et al. 2007; Daddi et al. 2007). However for this sample of higher redshift LAEs, the LAE sequence is elevated compared to continuum-selected galaxies at the same redshift, meaning that for a given stellar mass, the LAEs tend to have higher star formation rates. However, a subset of massive LAEs sits on the continuum-selected galaxy trend, tentatively implying that there may be two mechanisms for Lyman alpha escape.

  8. Searching for candidates of Lyman continuum sources - revisiting the SSA22 field

    NASA Astrophysics Data System (ADS)

    Micheva, Genoveva; Iwata, Ikuru; Inoue, Akio K.; Matsuda, Yuichi; Yamada, Toru; Hayashino, Tomoki

    2017-02-01

    We present the largest to date sample of hydrogen Lyman continuum (LyC) emitting galaxy candidates at any redshift, with 18 Lyman α emitters (LAEs) and seven Lyman break galaxies (LBGs), obtained from the SSA22 field with Subaru/Suprime-Cam. The sample is based on the 159 LAEs and 136 LBGs observed in the field, all with spectroscopically confirmed redshifts, and these LyC candidates are selected as galaxies with counterparts in a narrow-band filter image which traces LyC at z ≥ 3.06. Many LyC candidates show a spatial offset between the rest-frame non-ionizing ultraviolet (UV) detection and the LyC-emitting substructure or between the Lyα emission and LyC. The possibility of foreground contamination complicates the analysis of the nature of LyC emitters, although statistically it is highly unlikely that all candidates in our sample are contaminated by foreground sources. Many viable LyC LAE candidates have flux density ratios inconsistent with standard models, while also having too blue UV slopes to be foreground contaminants. Stacking reveals no significant LyC detection, suggesting that there is a dearth of objects with marginal LyC signal strength, perhaps due to a bimodality in the LyC emission. The foreground contamination corrected 3σ upper limits of the observed average flux density ratios are fLyC/fUV < 0.08 from stacking LAEs and fLyC/fUV < 0.02 from stacking LBGs. There is a sign of a positive correlation between LyC and Lyα, suggesting that both types of photons escape via a similar mechanism. The LyC detection rate among protocluster LBGs is seemingly lower compared to the field.

  9. How Lyman Alpha Emission Depends on Galaxy Stellar Mass

    NASA Astrophysics Data System (ADS)

    Oyarzún, Grecco A.; Blanc, Guillermo A.; González, Valentino; Mateo, Mario; Bailey, John I., III; Finkelstein, Steven L.; Lira, Paulina; Crane, Jeffrey D.; Olszewski, Edward W.

    2016-04-01

    In this work, we show how the stellar mass (M *) of galaxies affects the 3 < z < 4.6 Lyα equivalent width (EW) distribution. To this end, we design a sample of 629 galaxies in the M * range 7.6\\lt {log}{M}*/{M}⊙ \\lt 10.6 from the 3D-HST/CANDELS survey. We perform spectroscopic observations of this sample using the Michigan/Magellan Fiber System, allowing us to measure Lyα fluxes and use 3D-HST/CANDELS ancillary data. In order to study the Lyα EW distribution dependence on M *, we split the whole sample in three stellar mass bins. We find that, in all bins, the distribution is best represented by an exponential profile of the form {dN}({M}*)/d{EW}={W}0{({M}*)}-1A({M}*){e}-{EW/{W}0({M}*)}. Through a Bayesian analysis, we confirm that lower M * galaxies have higher Lyα EWs. We also find that the fraction A of galaxies featuring emission and the e-folding scale W 0 of the distribution anti-correlate with M *, recovering expressions of the forms A({M}*)=-0.26(.13){log}{M}*/{M}⊙ +3.01(1.2) and {W}0({M}*)=-15.6(3.5){log}{M}*/{M}⊙ +166(34). These results are crucial for proper interpretation of Lyα emission trends reported in the literature that may be affected by strong M * selection biases.

  10. The Direct Detection of Lyman Continuum Emission from Star-forming Galaxies at z~3

    NASA Astrophysics Data System (ADS)

    Shapley, Alice E.; Steidel, Charles C.; Pettini, Max; Adelberger, Kurt L.; Erb, Dawn K.

    2006-11-01

    We present the results of rest-frame UV spectroscopic observations of a sample of 14 z~3 star-forming galaxies in the SSA 22a field. These spectra are characterized by unprecedented depth in the Lyman continuum region. For the first time, we have detected escaping ionizing radiation from individual galaxies at high redshift, with 2 of the 14 objects showing significant emission below the Lyman limit. We also measured the ratio of emergent flux density at 1500 Å to that in the Lyman continuum region, for the individual detections (C49 and D3) and the sample average. If a correction for the average IGM opacity is applied to the spectra of the objects C49 and D3, we find f1500/f900,corr,C49=4.5 and f1500/f900,corr,D3=2.9. The average emergent flux density ratio in our sample is =22, implying an escape fraction ~4.5 times lower than inferred from the composite spectrum from Steidel and coworkers. If this new estimate is representative of LBGs, their contribution to the metagalactic ionizing radiation field is Jν(900)~2.6×10-22 ergs s-1 cm-2 Hz-1 sr-1, comparable to the contribution of optically selected quasars at the same redshift. The sum of the contributions from galaxies and quasars is consistent with recent estimates of the level of the ionizing background at z~3, inferred from the H I Lyα forest optical depth. There is significant variance among the emergent far-UV spectra in our sample, yet the factors controlling the detection or nondetection of Lyman continuum emission from galaxies are not well determined. Because we do not yet understand the source of this variance, significantly larger samples will be required to obtain robust constraints on the galaxy contribution to the ionizing background at z~3 and beyond. Based, in part, on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA and was made possible by the

  11. Evaluation of miniature vacuum ultraviolet lamps for stability and operating characteristics, Lyman-Alpha task

    NASA Technical Reports Server (NTRS)

    Hurd, W. A.

    1985-01-01

    Modifications required to change the near ultraviolet source in the Optical Contamination Monitor to a source with output at or near the Lyman-Alpha hydrogen line are discussed. The effort consisted of selecting, acquiring and testing candidate miniature ultraviolet lamps with significant output in or near 121.6 nm. The effort also included selection of a miniature dc high-voltage power supply capable of operating the lamp. The power supply was required to operate from available primary power supplied by the Optical Effect Module (DEM) and it should be flight qualified or have the ability to be qualified by the user.

  12. The interstellar deuterium-to-hydrogen ratio - A reevaluation of Lyman absorption-line measurements

    NASA Technical Reports Server (NTRS)

    Mccullough, Peter R.

    1992-01-01

    The D/H ratio in the local interstellar medium is evaluated based upon previously published measurements of Lyman absorption lines together with the hypothesis that the D/H ratio is constant. A unique value for the D/H ratio of 1.5 (+/- 0.2) x 10 exp -5 by number is shown to be consistent with all published determinations made with the Copernicus and the International Ultraviolet Explorer satellites. The possibility that the D/H ratio may vary substantially in the local interstellar medium is considered and found to be unnecessary.

  13. Factors Affecting VUV Emission Spectrum near Lyman-{alpha} from a Hydrogen Plasma Source

    SciTech Connect

    Ogino, K.; Kasuya, T.; Shimamoto, S.; Wada, M.; Kimura, Y.; Nishiura, M.

    2011-09-26

    Vacuum ultra violet (VUV) emission spectra from plasmas near walls of different metallic materials were measured to estimate the effect upon the local production rate of vibrational excited hydrogen molecules due to plasma wall interaction. Among Cu, Mo, Ni, Ta and Ti, the intensity of band spectrum around Lyman-{alpha} had become the largest when Cu wall was used while it was the smallest for Ti. The role of particle reflection from the plasma electrode surface upon the H{sup -} production by a pure electron volume process is discussed.

  14. Lyman-alpha observations of comets West 1976 VI and P d'Arrest 1976 XI with Copernicus

    NASA Astrophysics Data System (ADS)

    Festou, M. C.; Keller, H. U.; Bertaux, J. L.; Barker, E. S.

    1983-02-01

    Lyman-alpha observations by the Copernicus satellite have been used to determine the production rates of hydrogen atoms of comets West 1976 VI and P/d'Arrest 1976 XI at a time when they were dynamically active (splitting or outburst of the nucleus). The observed Lyman-alpha line widths are in agreement with those observed in comet Kobayashi-Berger-Milon 1975 IX and, consequently, do not contradict the assumption that the H atoms are produced by the photodissociation of water vapor, even in CO(plus) rich comets..

  15. The Lyman-Alpha Forest in the Lensed Quasar Q0957+561 and the Characteristic Dimension of the Absorbing Clouds

    NASA Technical Reports Server (NTRS)

    Dolan, Joseph; Fisher, Richard R. (Technical Monitor)

    2001-01-01

    Far-ultraviolet spectra of the gravitational lens components Q0957+561 A and 9 were obtained with the Hubble Space Telescope Faint Object Spectrograph (FOS) at five equally spaced epochs, one every two weeks. We confirm the flux variability of the quasar's Lyman-alpha and 0 VI emission lines reported by Dolan et al. (1995) in IUE spectra. The fluxes in these lines vary on a time scale of weeks in the observer's rest frame, independently of each other and of the surrounding continuum. The individual spectra of each image were co-added to investigate the properties of the Lyman-alpha forest along the two lines of sight to the quasar. Absorption lines having equivalent width W > 0.3 A in the observer's frame not previously identified by Michalitsianos et al. (1997) as interstellar lines, metal lines, or higher order Lyman lines were taken to be Ly-alpha forest lines. The existence of each line in this consistently selected set was then verified by its presence in two archival FOS spectra with -1.5 times higher signal to noise than our co-added spectra. Ly-alpha forest lines with W > 0.3 A appear at 41 distinct wavelengths in the spectra of the two images. one absorption line in the spectrum of image A has no counterpart in the spectrum of image B and one line in image B has no counterpart in image A. Based on the separation of the lines of sight over the redshift range searched for Ly-forest lines, the density of the absorbing clouds in the direction of Q0957+561 must change significantly over a distance R = 160 (+120, -70)/ h(sub 50) kpc in the simplified model where the absorbers are treated as spherical clouds and the characteristic dimension, R, is the radius. (We adopt H(sub 0) = 50 h(sub 50) km/s/ kpc, q(sub 0) = 1/2, and lambda = 0 throughout the paper.) The 95% confidence interval on R extends from (50 - 950)/h(sub 50) kpc We show in the Appendix that the fraction of Ly-alpha forest lines that appear in only one spectrum can be expressed as a rapidly

  16. The Lyman-Alpha Forest in the Lensed Quasar Q0957+561 and the Characteristic Dimension of the Absorbing Clouds

    NASA Technical Reports Server (NTRS)

    Dolan, Joseph; Fisher, Richard R. (Technical Monitor)

    2001-01-01

    Far-ultraviolet spectra of the gravitational lens components Q0957+561 A and 9 were obtained with the Hubble Space Telescope Faint Object Spectrograph (FOS) at five equally spaced epochs, one every two weeks. We confirm the flux variability of the quasar's Lyman-alpha and 0 VI emission lines reported by Dolan et al. (1995) in IUE spectra. The fluxes in these lines vary on a time scale of weeks in the observer's rest frame, independently of each other and of the surrounding continuum. The individual spectra of each image were co-added to investigate the properties of the Lyman-alpha forest along the two lines of sight to the quasar. Absorption lines having equivalent width W > 0.3 A in the observer's frame not previously identified by Michalitsianos et al. (1997) as interstellar lines, metal lines, or higher order Lyman lines were taken to be Ly-alpha forest lines. The existence of each line in this consistently selected set was then verified by its presence in two archival FOS spectra with -1.5 times higher signal to noise than our co-added spectra. Ly-alpha forest lines with W > 0.3 A appear at 41 distinct wavelengths in the spectra of the two images. one absorption line in the spectrum of image A has no counterpart in the spectrum of image B and one line in image B has no counterpart in image A. Based on the separation of the lines of sight over the redshift range searched for Ly-forest lines, the density of the absorbing clouds in the direction of Q0957+561 must change significantly over a distance R = 160 (+120, -70)/ h(sub 50) kpc in the simplified model where the absorbers are treated as spherical clouds and the characteristic dimension, R, is the radius. (We adopt H(sub 0) = 50 h(sub 50) km/s/ kpc, q(sub 0) = 1/2, and lambda = 0 throughout the paper.) The 95% confidence interval on R extends from (50 - 950)/h(sub 50) kpc We show in the Appendix that the fraction of Ly-alpha forest lines that appear in only one spectrum can be expressed as a rapidly

  17. Progress in Research of Damped Lyman Alpha Systems (DLAs) (II): Methods of Measuring the Metal Column Densities in Absorption Clouds1,2

    NASA Astrophysics Data System (ADS)

    Hou, Jin-Liang; Yin, Jun; Fu, Cheng-Qi

    2015-04-01

    For the studies of intergalactic medium and galactic chemical evolution, it is a foundation to measure the abundances of metallic elements in the interstellar or intergalactic medium by using the absorption lines of damped Lyman alpha systems (DLAs) on the celestial spectra. Three methods exist for measuring the metal column density of gas clouds: the curve of growth (COG) method, the line profile fitting method (LPTM), and the apparent optical depth method (AODM). The COG method was developed in about half a century ago, so far it has been mainly applied in observations with a low spectral resolution. But the COG method is unaffected by the instrumental profile, and it is widely used in the case of optically-thin gas clouds. In recent years, most observations are done with high-resolution spectrographs, and in the case of the rapid development of computer technology, the LPTM and AODM, especially the LPTM, are more frequently adopted by most of astronomers. However, the LPTM has more free parameters to determine, so, it will consume more computing time, and sometimes will result in several convergent solutions. It will also introduce more deviations when one spectral line is blended seriously with other lines. The AODM is intermediate between the COG method and the LPTM, it shows favoritism to some people owing to its simplicity and reliability; but because of the possible existence of unresolved saturation structure in spectral lines, its application is restricted to some extent.

  18. The Impact of Unresolved Turbulence on the Escape Fraction of Lyman Continuum Photons

    NASA Astrophysics Data System (ADS)

    Safarzadeh, M.; Scannapieco, E.

    2016-11-01

    We investigate the relation between the turbulent Mach number ({ M }) and the escape fraction of Lyman continuum photons ({f}{esc}) in high-redshift galaxies. Approximating the turbulence as isothermal and isotropic, we show that the increase in the variance in column densities from { M }=1 to { M }=10 causes {f}{esc} to increase by ≈ 25%, and the increase from { M }=1 to { M }=20 causes {f}{esc} to increases by ≈ 50% for a medium with opacity τ ≈ 1. At a fixed Mach number, the correction factor for escape fraction relative to a constant column density case scales exponentially with the opacity in the cell, which has a large impact for simulated star-forming regions. Furthermore, in simulations of isotropic turbulence with full atomic/ionic cooling and chemistry, the fraction of HI drops by a factor of ≈ 2.5 at { M }≈ 10 even when the mean temperature is ≈ 5× {10}3 {{K}}. If turbulence is unresolved, these effects together enhance {f}{esc} by a factor \\gt 3 at Mach numbers above 10. Such Mach numbers are common at high redshifts where vigorous turbulence is driven by supernovae, gravitational instabilities, and merger activity, as shown both by numerical simulations and observations. These results, if implemented in the current hydrodynamical cosmological simulations to account for unresolved turbulence, can boost the theoretical predictions of the Lyman Continuum photon escape fraction and further constrain the sources of reionization.

  19. CTIO REU/PIA Observations: Lyman-Alpha Blob Candidates and RR Lyrae Variables

    NASA Astrophysics Data System (ADS)

    Kaleida, Catherine C.; Students, REU/PIA; van der Bliek, Nicole S.; Kunder, Andrea; Layden, Andrew C.; Hegel, Paul R.; Anderson, Tyler S.

    2012-02-01

    We request 8 nights on the CTIO 1.0-m as part of the upcoming 2012 CTIO REU/PIA program. The main focus of this proposal will be to provide direct, hands-on observational experience to 8 undergraduate students in observational techniques, astronomical data reduction, and multi-wavelength photometry. In order to expose the students to a variety of astronomical observations, we will observe RR Lyrae variable stars and Lyman Alpha Blob (LAB) candidates. The RR Lyrae variable star observations are in collaboration with the Bowling Green State University Variable Star Project (BGSUVSP). The variable stars will be observed in several colors to refine their calibration as distance indicators, determine extinction and place constraints on stellar models. LAB candidates were chosen from space-based UV data from Swift/UVOT of 50 fields of quasi-stellar objects (QSOs) in the redshift range 0.556Lyman-alpha emission. Additionally, a small fraction of the time will be allocated to observe scientifically interesting targets of the students own choosing.

  20. Discovery of a faint, star-forming, multiply lensed, Lyman-α blob

    NASA Astrophysics Data System (ADS)

    Caminha, G. B.; Karman, W.; Rosati, P.; Caputi, K. I.; Arrigoni Battaia, F.; Balestra, I.; Grillo, C.; Mercurio, A.; Nonino, M.; Vanzella, E.

    2016-11-01

    We report the discovery of a multiply lensed Lyman-α blob (LAB) behind the galaxy cluster AS1063 using the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope (VLT). The background source is at z = 3.117 and is intrinsically faint compared to almost all previously reported LABs. We used our highly precise strong lensing model to reconstruct the source properties, and we find an intrinsic luminosity of LLyα = 1.9 × 1042 erg s-1, extending to 33 kpc. We find that the LAB is associated with a group of galaxies, and possibly a protocluster, in agreement with previous studies that find LABs in overdensities. In addition to Lyman-α (Lyα) emission, we find C iv, He ii, and O iii] ultraviolet (UV) emission lines arising from the centre of the nebula. We used the compactness of these lines in combination with the line ratios to conclude that the Lyα nebula is likely powered by embedded star formation. Resonant scattering of the Lyα photons then produces the extended shape of the emission. Thanks to the combined power of MUSE and strong gravitational lensing, we are now able to probe the circumgalatic medium of sub-L∗ galaxies at z ≈ 3.

  1. Optimization of microwave Hydrogen plasma discharges to mimic Lyman alpha (121.6 nm) solar irradiations

    NASA Astrophysics Data System (ADS)

    Benilan, Y.; Gazeau, M.-C.; Es-Sebbar, E.-T.; Jolly, A.; Arzoumanian, E.; Fray, N.; Cottin, H.

    2011-10-01

    We present the results obtained in low pressure microwave plasmas sustained in flowing mixtures of H2/He with the addition of Ar. We investigated experimentally their properties in terms of VUV emissions and photons fluxes using a VUV spectrometer. The spectra are dominated by Lyman alpha at 121.6 nm and H2 band emissions around 160 nm. The addition of Ar in the H2/He mixture largely affects the line emission. Lyman alpha emission increases by a factor of 2 in the presence of 20% Ar while the H2 bands decreases. This is a way to improve the monochromaticity of the lamp. Chemical actinometry method is used to determine the photons flux. We measured the temporal evolution of CO production issued from CO2 photolysis. A photon flux of 4.1015 s-1 is obtained for a power of 100 W. The photon flux varies linearly with the power at a rate of 6.1013 s1.W1. Those results are applied to studies on methane photolysis and help to explain mismatch between photochemical models and experiments.

  2. A Very Large Array search for emission from HI associated with nearby Lyman alpha absorbers

    NASA Technical Reports Server (NTRS)

    Van Gorkom, J. H.; Bahcall, J. N.; Jannuzi, B. T.; Schneider, D. P.

    1993-01-01

    We present a sensitive Very Large Array (VLA) search for H I emission from the vicinity of the Lyman alpha clouds in the Virgo Cluster, which were recently discovered with Hubble Space Telescope (HST) in absorption toward the nearest quasar 3C273. We searched an area of 40 by 40 arcmin centered on 3C273, covering a velocity range from 840 to 1840 km/s. The bandpass was self-calibrated on 3C273 leading to a spectral dynamic range of better than 10(exp 5) to 1. No H I was detected. The rms noise in the final images corresponds to a 3 sigma column density sensitivity of 2.8 x 10(exp 19) sq cm on scales of a few kpc. Small H I clouds could have been detected down to a few times 10(exp 6) solar mass. Our failure to detect H I emission at the higher column densities sets a lower limit to the radius of the Lyman alpha clouds of 3.9 kpc, assuming a spherical geometry.

  3. Lenses in the forest: cross--correlation of the Lyman-alpha flux with CMB lensing

    SciTech Connect

    Vallinotto, Alberto; Das, Sudeep; Spergel, David N.; Viel, Matteo; /Trieste Observ. /INFN, Trieste

    2009-03-01

    We present a theoretical estimate for a new observable: the cross-correlation between the Lyman-{alpha}-flux fluctuations in quasar (QSO) spectra and the convergence of the cosmic microwave background (CMB) as measured along the same line-of-sight. As a first step toward the assessment of its detectability, we estimate the signal-to-noise ratio using linear theory. Although the signal-to-noise is small for a single line-of-sight and peaks at somewhat smaller redshifts than those probed by the Lyman-{alpha} forest, we estimate a total signal-to-noise of 9 for cross-correlating QSO spectra of SDSSIII with Planck and 20 for cross-correlating with a future polarization based CMB experiment. The detection of this effect would be a direct measure of the neutral hydrogen-matter cross-correlation and could provide important information on the growth of structures at large scales in a redshift range which is still poorly probed by observations.

  4. The hydrogen coma of Comet P/Halley observed in Lyman-alpha using sounding rockets

    NASA Technical Reports Server (NTRS)

    Mccoy, R. P.; Meier, R. R.; Keller, H. U.; Opal, C. B.; Carruthers, G. R.

    1992-01-01

    Hydrogen Lyman-alpha (121.6 nm) images of Comet P/Halley were obtained using sounding rockets launched from White Sands Missile Range on 24.5 February and 13.5 March 1986. The second rocket was launched 13 hours before the fly-by of the Giotto spacecraft. An electrographic camera on both flights provided Lyman-alpha images covering a 20 field of view with 3 arcmin resolution. The data from both flights have been compared with a time-dependent model of hydrogen kinetics. To match the measured isophote contours, hydrogen sources with velocity components of 8 km/s and 20 km/s (from OH and H2O respectively) as well as a low velocity component (about 2 km/s) are required. This low velocity component is thought to result from thermalization of fast hydrogen atoms within the collision zone, providing an important diagnostic of temperature and density near the nucleus. Hydrogen production rates of 3.8 x 10 exp 30/s and 1.7 x 10 exp 30/s have been obtained for the two observations.

  5. Impacts of Geomagnetic Storms on the Terrestrial H-Exosphere Using Twins-Lyman Stereo Data

    NASA Astrophysics Data System (ADS)

    Nass, U.; Zoennchen, J.; Fahr, H. J.; Goldstein, J.

    2015-12-01

    Based on continuously monitored Lyman-alpha data registered by the TWINS1/2-LAD instruments we have studied the impact of a weaker and a stronger geomagnetic storm on the exospheric H-density distribution between heights of 3--8 Earth-radii. As is well known, solar Lyman-alpha radiation is resonantly backscattered from geocoronal neutral hydrogen (H). The resulting resonance glow intensity in the optically thin regime is proportional to H column density along the line of sight (LOS). Here we present the terrestrial exospheric response to geomagnetic storms. We quantify the reaction to geomagnetic activity in form of amplitude and temporal response of the H-density, sampled at different geocentric distances. We find that even in case of a weak storm, the exospheric H-density in regions above the exobase reacts with a suprisingly large increase in a remarkably short time period of less than half a day. Careful analysis of this geomagnetic density effect indicates that it is an expansion in the radial scale height of the exospheric H-density, developing from exobasic heights.

  6. Lyman Break Analogs: Constraints on the Formation of Extreme Starbursts at Low and High Redshift

    NASA Technical Reports Server (NTRS)

    Goncalves, Thiago S.; Overzier, Roderik; Basu-Zych, Antara; Martin, D. Christopher

    2011-01-01

    Lyman Break Analogs (LBAs), characterized by high far-UV luminosities and surface brightnesses as detected by GALEX, are intensely star-forming galaxies in the low-redshift universe (z approximately equal to 0.2), with star formation rates reaching up to 50 times that of the Milky Way. These objects present metallicities, morphologies and other physical properties similar to higher redshift Lyman Break Galaxies (LBGs), motivating the detailed study of LBAs as local laboratories of this high-redshift galaxy population. We present results from our recent integral-field spectroscopy survey of LBAs with Keck/OSIRIS, which shows that these galaxies have the same nebular gas kinematic properties as high-redshift LBGs. We argue that such kinematic studies alone are not an appropriate diagnostic to rule out merger events as the trigger for the observed starburst. Comparison between the kinematic analysis and morphological indices from HST imaging illustrates the difficulties of properly identifying (minor or major) merger events, with no clear correlation between the results using either of the two methods. Artificial redshifting of our data indicates that this problem becomes even worse at high redshift due to surface brightness dimming and resolution loss. Whether mergers could generate the observed kinematic properties is strongly dependent on gas fractions in these galaxies. We present preliminary results of a CARMA survey for LBAs and discuss the implications of the inferred molecular gas masses for formation models.

  7. Synthesis, biological profile, and quantitative structure-activity relationship of a series of novel 3-hydroxy-3-methylglutaryl coenzyme A reductase inhibitors.

    PubMed

    Sit, S Y; Parker, R A; Motoc, I; Han, W; Balasubramanian, N; Catt, J D; Brown, P J; Harte, W E; Thompson, M D; Wright, J J

    1990-11-01

    A series of 9,9-bis(4-fluorophenyl)-3,5-dihydroxy-8-(alkyltetrazol-5-yl)- 6,8-nonadienoic acid derivatives 1 were synthesized and found to inhibit competitively the enzyme 3-hydroxy-3-methylglutaryl coenzyme A (HMG-CoA) reductase. The analogues having 1N-methyltetrazol-5-yl attached to the C8-position (3a, 4a, R1 = R2 = F) are the most active in suppressing cholesterol biosynthesis in both in vitro and in vivo models: the IC50 for the chiral form of 3a is 19 nM, Ki = 4.3 x 10(-9)M when Km for HMG-CoA is 28 x 10(-6) M;1 the ED50 (oral) value corresponding to the lactone derivative (4a, BMY 22089) is approximately 0.1 mg/kg. Further, BMY 21950 is nearly 2 orders of magnitude more active in parenchymal heptaocytes, from which most of the serum cholesterol originates, than in other cell preparations (such as spleen, testes, ileum, adrenal, and ocular lens epithelial cells; Table III). This apparent tissue specificity may be highly beneficial since the blocking of cholesterol biosynthesis in other vital organs could eventually lead to undesirable side effects. In addition to the chemical synthesis and biological evaluation, a theoretical study aimed at relating the HMG-CoA reductase inhibitory potency to the three-dimensional structure of the inhibitors was undertaken. With a combination of molecular mapping and 3D-QSAR techniques, it was possible to determine a logical candidate for the conformation of the bound inhibitor and to quantitatively relate inhibitory potency to the shape and size of both the binding site and the C8-substituent.

  8. First continuous time series of tropical, mid-latitudinal and polar middle-atmospheric wind profile measurements with a ground-based microwave Doppler-spectro-radiometer

    NASA Astrophysics Data System (ADS)

    Rüfenacht, Rolf; Kämpfer, Niklaus; Murk, Axel; Eriksson, Patrick; Buehler, Stefan A.; Kivi, Rigel; Keckhut, Philippe; Hauchecorne, Alain; Duflot, Valentin

    2014-05-01

    Wind is one of the key parameters for the characterisation of the atmosphere and the understanding of its dynamics. Despite this, no continuously operating instrument for wind measurements in the upper stratosphere and lower mesosphere existed so far. Aiming to contribute to the closing of this data gap by exploiting the potential of microwave radiometry the Institute of Applied Physics of the University of Bern built a ground-based 142 GHz Doppler-spectro-radiometer with the acronym WIRA (WInd RAdiometer). WIRA is specifically designed for the measurement of middle-atmospheric horizontal wind and is sensitive to the altitude range between 35 and 70 km. The architecture of the radiometer is fairly compact what makes it transportable and suitable for campaign use. WIRA is conceived in a way that it can be operated remotely and does hardly require any maintenance. The operational use of WIRA started in September 2010. Since a technical upgrade in autumn 2012 which drastically increased the signal to noise ratio of the instrument, the meridional component is permanently measured along with the zonal wind to get a full picture of the horizontal wind field. During the last year the wind retrieval algorithm has been entirely rebuilt and tested. It is now based on the optimal estimation technique (OEM) and uses an upgraded version of the ARTS/QPACK radiative transfer and inversion model. Time series of middle-atmospheric wind from measurement campaigns of 7 to 11 months duration at mid and high latitude sites (Bern, 46°57' N, 7°26' E; Sodankylä, 67°22' N, 26°38' E; Observatoire de Haute-Provence, 43°56' N, 5°43' E) have been obtained. In September 2013 WIRA was moved to Observatoire du Maïdo (21°04' S, 55°23' E) to study the dynamics of the tropical middle atmosphere. The measurements have been compared to the data from the ECMWF model. Generally good agreement has been found in the stratosphere, however systematic discrepancies exist in the mesosphere. At the

  9. Twenty years of research on fungal-plant interactions on Lyman Glacier forefront—lessons learned and questions yet unanswered

    Treesearch

    Ari Jumpponen; Shawn P. Brown; James M. Trappe; Efrén Cázares; Rauni. Strömmer

    2012-01-01

    Retreating glaciers and the periglacial areas that they vacate produce a harsh environment of extreme radiation, nutrient limitations and temperature oscillations. They provide a model system for studying mechanisms that drive the establishment and early assembly of communities. Here, we synthesize more than 20 years of research at the Lyman Glacier forefront in the...

  10. The Lyman Continuum Escape Fraction of Emission Line-selected z ˜ 2.5 Galaxies Is Less Than 15%

    NASA Astrophysics Data System (ADS)

    Rutkowski, Michael J.; Scarlata, Claudia; Henry, Alaina; Hayes, Matthew; Mehta, Vihang; Hathi, Nimish; Cohen, Seth; Windhorst, Rogier; Koekemoer, Anton M.; Teplitz, Harry I.; Haardt, Francesco; Siana, Brian

    2017-06-01

    Recent work suggests that strong emission line, star-forming galaxies (SFGs) may be significant Lyman continuum leakers. We combine archival Hubble Space Telescope broadband ultraviolet and optical imaging (F275W and F606W, respectively) with emission line catalogs derived from WFC3 IR G141 grism spectroscopy to search for escaping Lyman continuum (LyC) emission from homogeneously selected z ˜ 2.5 SFGs. We detect no escaping Lyman continuum from SFGs selected on [O ii] nebular emission (N = 208) and, within a narrow redshift range, on [O iii]/[O ii]. We measure 1σ upper limits to the LyC escape fraction relative to the non-ionizing UV continuum from [O ii] emitters, f esc ≲ 5.6%, and strong [O iii]/[O ii] > 5 ELGs, f esc ≲ 14.0%. Our observations are not deep enough to detect f esc ˜ 10% typical of low-redshift Lyman continuum emitters. However, we find that this population represents a small fraction of the star-forming galaxy population at z ˜ 2. Thus, unless the number of extreme emission line galaxies grows substantially to z ≳ 6, such galaxies may be insufficient for reionization. Deeper survey data in the rest-frame ionizing UV will be necessary to determine whether strong line ratios could be useful for pre-selecting LyC leakers at high redshift.

  11. Indications for axial asymmetries in the interplanetary hydrogen distribution derived from Pioneer-10 Lyman-alpha data

    NASA Technical Reports Server (NTRS)

    Scherer, K.; Judge, D. L.

    1992-01-01

    It is presently noted that Pioneer 10's highly spatially resolved Lyman-alpha data exhibit a backscattered resonance glow with a persistent spatially-resolved asymmetry. The first harmonic amplitude ranges from about 5-10 percent of the mean value, and is observed continuously throughout the two years of this analysis period.

  12. Probing re-ionization with quasar spectra: the impact of the intrinsic Lyman α emission line shape uncertainty

    NASA Astrophysics Data System (ADS)

    Kramer, R. H.; Haiman, Z.

    2009-12-01

    Arguably the best hope of understanding the tail end of the re-ionization of the intergalactic medium (IGM) at redshift z > 6 is through the detection and characterization of the Gunn-Peterson damping wing absorption of the IGM in bright quasar spectra. However, the use of quasar spectra to measure the IGM damping wing requires a model of the quasar's intrinsic Lyman α emission line. Here we quantify the uncertainties in the intrinsic line shapes, and how those uncertainties affect the determination of the IGM neutral fraction. We have assembled a catalogue of high-resolution Hubble Space Telescope spectra of the emission lines of unobscured low-redshift quasars, and have characterized the variance in the shapes of their lines. We then add simulated absorption from the high-redshift IGM to these quasar spectra in order to determine the corresponding uncertainties in re-ionization constraints using current and future samples of z > 6 quasar spectra. We find that, if the redshift of the Lyman α emission line is presumed to coincide with the systemic redshift determined from metal lines, the inferred IGM neutral fraction is systematically biased to low values due to a systematic blueshift of the Lyman α line relative to the metal lines. If a similar blueshift persists in quasars at z > 6, this bias strengthens previous claims of a significant neutral hydrogen fraction at z ~ 6. The bias can be reduced by including a Lyman α blueshift in the modelling procedure, or by excising wavelengths near the Lyman α line centre from the modelling. Intrinsic Lyman α line shape variations still induce significant scatter in the inferred xIGM values. Nevertheless, this scatter still allows a robust distinction between a highly ionized (xIGM ~ 10-3) and a neutral (xIGM = 1) IGM with even a few bright quasars. We conclude that if the variations of the intrinsic Lyman α emission line shapes in high-z quasars are similar to those at low-z, this variation will not limit the

  13. INDIRECT EVIDENCE FOR ESCAPING IONIZING PHOTONS IN LOCAL LYMAN BREAK GALAXY ANALOGS

    SciTech Connect

    Alexandroff, Rachael M.; Heckman, Timothy M.; Borthakur, Sanchayeeta; Overzier, Roderik; Leitherer, Claus

    2015-09-10

    A population of early star-forming galaxies is the leading candidate for the re-ionization of the universe. It is still unclear, however, what conditions and physical processes would enable a significant fraction of the ionizing (Lyman continuum) photons to escape from these gas-rich galaxies. In this paper we present the results of the analysis of Hubble Space Telescope Cosmic Origins Spectrograph far-UV (FUV) spectroscopy plus ancillary multi-waveband data of a sample of 22 low-redshift galaxies that are good analogs to typical star-forming galaxies at high redshift. We measure three parameters that provide indirect evidence of the escape of ionizing radiation (leakiness): (1) the residual intensity in the cores of saturated interstellar low-ionization absorption lines, which indicates incomplete covering by that gas in the galaxy; (2) the relative amount of blueshifted Lyα line emission, which can indicate the existence of holes in the neutral hydrogen on the front-side of the galaxy outflow, and (3) the relative weakness of the [S ii] optical emission lines that trace matter-bounded H ii regions. We show that our residual intensity measures are only negligibly affected by infilling from resonance emission lines. We find all three diagnostics agree well with one another. We use these diagnostics to rank-order our sample in terms of likely leakiness, noting that a direct measure of escaping Lyman continuum has recently been made for one of the leakiest members of our sample. We then examine the correlations between our ranking and other proposed diagnostics of leakiness. We find a good correlation with the equivalent width of the Lyα emission line, but no significant correlations with either the flux ratio of the [O iii]/[O ii] emission lines or the ratio of star-formation rates derived from the (dust-corrected) FUV and Hα luminosities. Turning to galaxy properties, we find the strongest correlations with leakiness are with the compactness of the star

  14. THE HST/ACS+WFC3 SURVEY FOR LYMAN LIMIT SYSTEMS. II. SCIENCE

    SciTech Connect

    O'Meara, John M.; Prochaska, J. Xavier; Worseck, Gabor; Madau, Piero

    2013-03-10

    We present the first science results from our Hubble Space Telescope survey for Lyman limit absorption systems (LLS) using the low dispersion spectroscopic modes of the Advanced Camera for Surveys and the Wide Field Camera 3. Through an analysis of 71 quasars, we determine the incidence frequency of LLS per unit redshift and per unit path length, l(z) and l(X), respectively, over the redshift range 1 < z < 2.6, and find a weighted mean of l(X) =0.29 {+-} 0.05 for 2.0 < z < 2.5 through a joint analysis of our sample and that of Ribaudo et al. Through stacked spectrum analysis, we determine a median (mean) value of the mean free path to ionizing radiation at z = 2.4 of {lambda}{sup 912}{sub mfp} = 243(252) h {sup -1}{sub 72} Mpc, with an error on the mean value of {+-}43 h {sup -1}{sub 72} Mpc. We also re-evaluate the estimates of {lambda}{sup 912}{sub mfp} from Prochaska et al. and place constraints on the evolution of {lambda}{sup 912}{sub mfp} with redshift, including an estimate of the ''breakthrough'' redshift of z = 1.6. Consistent with results at higher z, we find that a significant fraction of the opacity for absorption of ionizing photons comes from systems with N{sub H{sub I}} {<=}10{sup 17.5} cm{sup -2} with a value for the total Lyman opacity of {tau}{sup Lyman}{sub eff} = 0.40 {+-} 0.15. Finally, we determine that at minimum, a 5-parameter (4 power law) model is needed to describe the column density distribution function f(N{sub H{sub I}}, X) at z {approx} 2.4, find that f(N{sub H{sub I}}, X) undergoes no significant change in shape between z {approx} 2.4 and z {approx} 3.7, and provide our best fit model for f(N{sub H{sub I}}, X).

  15. Narrowband Lyman-continuum imaging of galaxies at z ∼ 2.85

    SciTech Connect

    Mostardi, R. E.; Shapley, A. E.; Nestor, D. B.; Steidel, C. C.; Trainor, R. F.; Reddy, N. A.

    2013-12-10

    We present results from a survey for z ∼ 2.85 Lyman-continuum (LyC) emission in the HS1549+1933 field and place constraints on the amount of ionizing radiation escaping from star-forming galaxies. Using a custom narrowband filter (NB3420) tuned to wavelengths just below the Lyman limit at z ≥ 2.82, we probe the LyC spectral region of 49 Lyman break galaxies (LBGs) and 91 Lyα emitters (LAEs) spectroscopically confirmed at z ≥ 2.82. Four LBGs and seven LAEs are detected in NB3420. Using V-band data probing the rest-frame nonionizing UV, we observe that many NB3420-detected galaxies exhibit spatial offsets between their LyC and nonionizing UV emission and are characterized by extremely blue NB3420–V colors, corresponding to low ratios of nonionizing to ionizing radiation (F {sub UV}/F {sub LyC}) that are in tension with current stellar population synthesis models. We measure average values of (F {sub UV}/F {sub LyC}) for our LBG and LAE samples, correcting for foreground galaxy contamination and H I absorption in the intergalactic medium. We find (F{sub UV}/F{sub LyC}){sub corr}{sup LBG}=82±45 and (F{sub UV}/F{sub LyC}){sub corr}{sup LAE}=7.4±3.6. These flux density ratios correspond, respectively, to relative LyC escape fractions of f{sub esc,} {sub rel}{sup LBG}=5%--8% and f{sub esc,} {sub rel}{sup LAE}=18%--49%, absolute LyC escape fractions of f{sub esc}{sup LBG}=1%--2% and f{sub esc}{sup LAE}=5%--15%, and a comoving LyC emissivity from star-forming galaxies of 8.8-15.0 × 10{sup 24} erg s{sup –1} Hz{sup –1} Mpc{sup –3}. In order to study the differential properties of galaxies with and without LyC detections, we analyze narrowband Lyα imaging and rest-frame near-infrared imaging, finding that while LAEs with LyC detections have lower Lyα equivalent widths on average, there is no substantial difference in the rest-frame near-infrared colors of LBGs or LAEs with and without LyC detections. These preliminary results are consistent with an

  16. A Lyman Break Galaxy in the Epoch of Reionization from Hubble Space Telescope (HST) Grism Spectroscopy

    NASA Technical Reports Server (NTRS)

    Rhoads, James E.; Malhotra, Sangeeta; Stern, Daniel K.; Gardner, Jonathan P.; Dickinson, Mark; Pirzkal, Norbert; Spinrad, Hyron; Reddy, Naveen; Dey, Arjun; Hathi, Nimish; hide

    2013-01-01

    Slitless grism spectroscopy from space offers dramatic advantages for studying high redshift galaxies: high spatial resolution to match the compact sizes of the targets, a dark and uniform sky background, and simultaneous observation over fields ranging from five square arcminutes (HST) to over 1000 square arcminutes (Euclid). Here we present observations of a galaxy at z = 6.57 the end of the reioinization epoch identified using slitless HST grism spectra from the PEARS survey (Probing Evolution And Reionization Spectroscopically) and reconfirmed with Keck + DEIMOS. This high redshift identification is enabled by the depth of the PEARS survey. Substantially higher redshifts are precluded for PEARS data by the declining sensitivity of the ACS grism at greater than lambda 0.95 micrometers. Spectra of Lyman breaks at yet higher redshifts will be possible using comparably deep observations with IR-sensitive grisms.

  17. Lyman-{alpha} radiation of a metastable hydrogen beam to measure electric fields

    SciTech Connect

    Lejeune, A.; Cherigier-Kovacic, L.; Doveil, F.

    2011-10-31

    The interaction between a metastable H(2s) atomic hydrogen beam and an external electric field leads to the emission of the Lyman-{alpha} line. It originates in the Stark mixing of the near-degenerate 2s{sub 1/2} and 2p{sub 1/2} levels separated by the Lamb shift. The quenched radiation proportional to the square of the electric field amplitude is recovered in vacuum by using such an atomic probe beam. We observe the strong enhancement of the signal when the field is oscillating at the Lamb shift frequency. This technique is applied in a plasma, offering an alternative way to measure weak electric fields by direct and non-intrusive means.

  18. Mariner 9 ultraviolet spectrometer experiment - Mars airglow spectroscopy and variations in Lyman alpha.

    NASA Technical Reports Server (NTRS)

    Barth, C. A.; Stewart, A. I.; Hord, C. W.; Lane, A. L.

    1972-01-01

    Mariner 9 ultraviolet spectrometer observations show the Mars airglow consists principally of emissions that arise from the interaction of solar ultraviolet radiation with carbon dioxide, the principal constituent of the Mars atmosphere. Two minor constituents, atomic hydrogen and atomic oxygen, also produce airglow emissions. The airglow measurements show that ionized carbon dioxide is only a minor constituent of the ionosphere. Using the airglow measurements of atomic oxygen, it is possible to infer that the major ion is ionized molecular oxygen. The escape rate of atomic hydrogen measured by Mariner 9 is approximately the same as that measured two years earlier by Mariner 6 and 7. If the current escape rate has been operating for 4.5 billion years and if water vapor is the ultimate source, an amount of oxygen has been generated that is far in excess of that observed at present. Mariner 9 observations of Mars Lyman alpha emission over a period of 120 days show variations of 20%.

  19. X-Ray Emission from Ultraviolet Luminous Galaxies and Lyman Break Galaxies

    NASA Technical Reports Server (NTRS)

    Hornschemeier, Ann; Ptak, A. F.; Salim, S.; Heckman, T. P.; Overzier, R.; Mallery, R.; Rich, M.; Strickland, D.; Grimes, J.

    2009-01-01

    We present results from an XMM mini-survey of GALEX-selected Ultraviolet-Luminous Galaxies (UVLGs) that appear to include an interesting subset that are analogs to the distant (3Lyman Break Galaxies (LBGs). The 2-10 kev X-ray emission of LBGs appear to be broadly similar to that of galaxies in the local Universe, possibly indicating similarity in the production of accreting binaries over large evolutionary timescales in the Universe. We have detected luminous X-ray emission from one UVLG that permits basic X-ray spectroscopic analysis, and have direct X-ray constraints on a total of 6 UVLGs. We find evidence for likely large scatter in the assumed X-ray/star-formation rate relation for LBGs.

  20. Voyager measurements of hydrogen Lyman-α diffuse emission from the Milky Way.

    PubMed

    Lallement, Rosine; Quémerais, Eric; Bertaux, Jean-Loup; Sandel, Bill R; Izmodenov, Vlad

    2011-12-23

    Doppler-shifted hydrogen Lyman-alpha (Lyα) emission from galaxies is currently measured and used in cosmology as an indicator of star formation. Until now, the Milky Way emission has not been detected, owing to far brighter local sources, including the H (hydrogen) glow, i.e., solar Lyα radiation backscattered by interstellar atoms that flow within the solar system. Because observations from the Voyager spacecraft, now leaving the heliosphere, are decreasingly affected by the H glow, the ultraviolet spectrographs are detecting Lyα diffuse emission from our Galaxy. The surface brightness toward nearby star-forming regions is about 3 to 4 rayleighs. The escape fraction of the radiation from the brightest H II regions is on the order of 3% and is highly spatially variable. These results will help in constraining models of Lyα radiation transfer in distant galaxies.

  1. Low-redshift Lyman-alpha absorption lines and the dark matter halos of disk galaxies

    NASA Technical Reports Server (NTRS)

    Maloney, Philip

    1992-01-01

    Ultraviolet observations of the low-redshift quasar 3C 273 using the Hubble Space Telescope have revealed many more Lyman-alpha absorption lines than would be expected from extrapolation of the absorption systems seen toward QSOs at z about 2. It is shown here that these absorption lines can plausibly be produced by gas at large radii in the disks of spiral and irregular galaxies; the gas is confined by the dark matter halos and ionized and heated by the extragalactic radiation field. This scenario does not require the extragalactic ionizing radiation field to decline as rapidly with decreasing z as the QSO emissivity. Observations of Ly-alpha absorption through the halos of known galaxies at low redshift will constrain both the extragalactic background and the properties of galactic halos.

  2. Direct method gas-phase oxygen abundances of four Lyman break analogs

    SciTech Connect

    Brown, Jonathan S.; Croxall, Kevin V.; Pogge, Richard W.

    2014-09-10

    We measure the gas-phase oxygen abundances in four Lyman break analogs using auroral emission lines to derive direct abundances. The direct method oxygen abundances of these objects are generally consistent with the empirically derived strong-line method values, confirming that these objects are low oxygen abundance outliers from the mass-metallicity (MZ) relation defined by star forming Sloan Digital Sky Survey galaxies. We find slightly anomalous excitation conditions (Wolf-Rayet features) that could potentially bias the empirical estimates toward high values if caution is not exercised in the selection of the strong-line calibration. The high rate of star formation and low oxygen abundance of these objects is consistent with the predictions of the fundamental metallicity relation, in which the infall of relatively unenriched gas simultaneously triggers an episode of star formation and dilutes the interstellar medium of the host galaxy.

  3. Studying Lyman-alpha escape and reionization in Green Pea galaxies

    NASA Astrophysics Data System (ADS)

    Yang, Huan; Malhotra, Sangeeta; Rhoads, James E.; Gronke, Max; Leitherer, Claus; Wofford, Aida; Dijkstra, Mark

    2017-01-01

    Green Pea galaxies are low-redshift galaxies with extreme [OIII]5007 emission line. We built the first statistical sample of Green Peas observed by HST/COS and used them as analogs of high-z Lyman-alpha emitters to study Ly-alpha escape and Ly-alpha sizes. Using the HST/COS 2D spectra, we found that Ly-alpha sizes of Green Peas are larger than the UV continuum sizes. We found many correlations between Ly-alpha escape fraction and galactic properties -- dust extinction, Ly-alpha kinematic features, [OIII]/[OII] ratio, and gas outflow velocities. We fit an empirical relation to predict Ly-alpha escape fraction from dust extinction and Ly-alpha red-peak velocity. In the JWST era, we can use this relation to derive the IGM HI column density along the line of sight of each high-z Ly-alpha emitter and probe the reionization process.

  4. Pollen Dispersal by Catapult: Experiments of Lyman J. Briggs on the Flower of Mountain Laurel

    NASA Astrophysics Data System (ADS)

    Nimmo, John R.; Hermann, Paula M.; Kirkham, M. B.; Landa, Edward R.

    2014-09-01

    The flower of Kalmia latifolia L. employs a catapult mechanism that flings its pollen to considerable distances. Physicist Lyman J. Briggs investigated this phenomenon in the 1950s after retiring as longtime director of the National Bureau of Standards, attempting to explain how hydromechanical effects inside the flower's stamen could make it possible. Briggs's unfinished manuscript implies that liquid under negative pressure generates stress, which, superimposed on the stress generated from the flower's growth habit, results in force adequate to propel the pollen as observed. With new data and biophysical understanding to supplement Briggs's experimental results and research notes, we show that his postulated negative-pressure mechanism did not play the exclusive and crucial role that he credited to it, though his revisited investigation sheds light on various related processes. Important issues concerning the development and reproductive function of Kalmia flowers remain unresolved, highlighting the need for further biophysical advances.

  5. AXUV bolometer and Lyman-α camera systems on the TCV tokamak

    NASA Astrophysics Data System (ADS)

    Degeling, A. W.; Weisen, H.; Zabolotsky, A.; Duval, B. P.; Pitts, R. A.; Wischmeier, M.; Lavanchy, P.; Marmillod, Ph.; Pochon, G.

    2004-10-01

    A set of seven twin slit cameras, each containing two 20-element linear absolute extreme ultraviolet photodiode arrays, has been installed on the Tokamak à Configuration Variable. One array in each camera will operate as a bolometer and the second as a Lyman-alpha (Lα) emission monitor for estimating the recycled neutral flux. The camera configuration was optimized by simulations of tomographic reconstructions of the expected Lα emission. The diagnostic will provide spatial and temporal resolution (10 μs) of the radiated power and the Lα emission that is considerably higher than previously achieved. This optimism is justified by extensive experience with prototype systems, which include first measurements of Lα light from the divertor.

  6. Resonance-enhanced two-photon ionization of ions by Lyman alpha radiation in gaseous nebulae.

    PubMed

    Johansson, S; Letokhov, V

    2001-01-26

    One of the mysteries of nebulae in the vicinity of bright stars is the appearance of bright emission spectral lines of ions, which imply fairly high excitation temperatures. We suggest that an ion formation mechanism, based on resonance-enhanced two-photon ionization (RETPI) by intense H Lyman alpha radiation (wavelength of 1215 angstroms) trapped inside optically thick nebulae, can produce these spectral lines. The rate of such an ionization process is high enough for rarefied gaseous media where the recombination rate of the ions formed can be 10(-6) to 10(-8) per second for an electron density of 10(3) to 10(5) per cubic centimeter in the nebula. Under such conditions, the photo-ions formed may subsequently undergo further RETPI, catalyzed by intense He i and He ii radiation, which also gets enhanced in optically thick nebulae that contain enough helium.

  7. Evidence for a Cool Neutral Medium in Damped Lyman-alpha Systems

    NASA Astrophysics Data System (ADS)

    Howk, J. C.

    2003-12-01

    I discuss the use of the relative populations of the fine-structure excited states of Si II and C II as temperature diagnostics in high-redshift damped Lyman-alpha systems (DLAs). The upper 2P3/2 states of these ions are populated through collisions with electrons and hydrogen as well as through direct pumping by CMB photons. The ratio of Si II* to C II* is dependent on the temperature of the gas, given the difference in the excitation energies for each ion; it depends only weakly on the density (so long as the densities in the absorber are not near the critical density of either ion). I demonstrate the application of this diagnostic, showing that the ISM in high-redshift DLAs must contain a cold neutral phase, implying they may be capable of forming stars. This work is presented in Howk, Wolfe, and Prochaska (2004).

  8. Low-redshift Lyman-alpha absorption lines and the dark matter halos of disk galaxies

    NASA Technical Reports Server (NTRS)

    Maloney, Philip

    1992-01-01

    Ultraviolet observations of the low-redshift quasar 3C 273 using the Hubble Space Telescope have revealed many more Lyman-alpha absorption lines than would be expected from extrapolation of the absorption systems seen toward QSOs at z about 2. It is shown here that these absorption lines can plausibly be produced by gas at large radii in the disks of spiral and irregular galaxies; the gas is confined by the dark matter halos and ionized and heated by the extragalactic radiation field. This scenario does not require the extragalactic ionizing radiation field to decline as rapidly with decreasing z as the QSO emissivity. Observations of Ly-alpha absorption through the halos of known galaxies at low redshift will constrain both the extragalactic background and the properties of galactic halos.

  9. Lyman-α Emission from an Infant Black Hole in the Early Universe

    SciTech Connect

    Wiggins, Brandon Kerry; Smidt, Joseph Michael; Johnson, Jarrett L.

    2016-01-01

    The COSMOS survey recently discovered an exotic young galaxy, COSMOS Redshift 7 (CR7), in the early universe (1 billion years after the Big Bang), which is devoid of evidence of elements heavier than hydrogen and helium. Whereas some believe this might be the first galaxy discovered with stars made only from these elements, others think CR7 may be powered by a newborn supermassive black hole. In this paper, we summarize for a general academic audience our efforts to model the creation of this galaxy through cosmological simulations. These state-of-the-art calculations include primordial chemistry and cooling and the interaction of x-rays from the black hole with surrounding gas. We simulate the process of light escaping this object with Monte Carlo Lyman-α transfer and compare our calculations with observations of CR7. Our work demonstrates the viability of the black hole interpretation for this intriguing object in the early universe.

  10. Spatially Resolved Emission of a z~3 Damped Lyman Alpha Galaxy with Keck/OSIRIS IFU

    NASA Astrophysics Data System (ADS)

    Christenson, Holly; Jorgenson, Regina

    2017-01-01

    The damped Lyman alpha (DLA) class of galaxies contains most of the neutral hydrogen gas over cosmic time. Few DLAs have been detected directly, which limits our knowledge of fundamental properties like size and mass. We present Keck/OSIRIS infrared integral field spectroscopy (IFU) observations of a DLA that was first detected in absorption toward a background quasar. Our observations use the Keck Laser Guide Star Adaptive Optics system to reduce the point-spread function of the quasar, making it possible to spatially resolve the DLA emission. We map this emission in O[III] 5007 Å. At redshift z~3, this DLA represents one of the highest redshift DLAs mapped with IFU spectroscopy. We present measurements of the star formation rate, metallicity, and gas mass of the galaxy.This project was supported in part by the NSF REU grant AST-1358980 and by the Nantucket Maria Mitchell Association.

  11. An Ultraviolet Ultra-luminous Lyman Break Galaxy at Z = 2.78 in NDWFS Boötes Field

    NASA Astrophysics Data System (ADS)

    Bian, Fuyan; Fan, Xiaohui; Jiang, Linhua; Dey, Arjun; Green, Richard F.; Maiolino, Roberto; Walter, Fabian; McGreer, Ian; Wang, Ran; Lin, Yen-Ting

    2012-10-01

    We present one of the most ultraviolet (UV) luminous Lyman break galaxies (LBGs; J1432+3358) at z = 2.78, discovered in the NOAO Deep Wide-Field Survey Boötes field. The R-band magnitude of J1432+3358 is 22.29 AB, more than two magnitudes brighter than typical L* LBGs at this redshift. The deep z-band image reveals two components of J1432+3358 separated by 1farcs0 with a flux ratio of 3:1. The high signal-to-noise ratio rest-frame UV spectrum shows Lyα emission line and interstellar medium absorption lines. The absence of N V and C IV emission lines, and the non-detection in X-ray and radio wavelengths and mid-infrared (MIR) colors indicates weak or no active galactic nuclei (<10%) in this galaxy. The galaxy shows a broader line profile, with a FWHM of about 1000 km s-1 and a larger outflow velocity (≈500 km s-1) than those of typical z ~ 3 LBGs. The physical properties are derived by fitting the spectral energy distribution (SED) with stellar synthesis models. The dust extinction, E(B - V) = 0.12, is similar to that in normal LBGs. The star formation rates (SFRs) derived from the SED fitting and the dust-corrected UV flux are consistent with each other, ~300 M ⊙ yr-1, and the stellar mass is (1.3 ± 0.3) × 1011 M ⊙. The SFR and stellar mass in J1432+3358 are about an order of magnitude higher than those in normal LBGs. The SED-fitting results support that J1432+3358 has a continuous star formation history, with a star formation episode of 6.3 × 108 yr. The morphology of J1432+3358 and its physical properties suggest that J1432+3358 is in an early phase of a 3:1 merger process. The unique properties and the low space number density (~10-7 Mpc-3) are consistent with the interpretation that such galaxies are either found in a short unobscured phase of the star formation or that a small fraction of intensive star-forming galaxies are unobscured. Based on (in part) data collected at Subaru Telescope, which is operated by the National Astronomical Observatory

  12. Photometric selection of z ~ 5 Lyman break galaxies in the ESO Remote Galaxy Survey

    NASA Astrophysics Data System (ADS)

    Douglas, L. S.; Bremer, M. N.; Stanway, E. R.; Lehnert, M. D.; Clowe, D.

    2009-12-01

    We describe the selection of a sample of photometrically defined Lyman break galaxies (LBGs) at z ~ 5 using the multiwavelength imaging data of the ESO (European Southern Observatory) Remote Galaxy Survey. The data are drawn from 10 widely separated fields covering a total sky area of 275arcmin2. Starting with a simple colour (R - I > 1.3) and magnitude (I < 26.3) cut to isolate the Lyman break and then refining the sample by applying further optical and near-infrared photometric criteria we identify a sample of 253 LBG candidates. We carefully model the completeness of this sample and the factors that affect its reliability. There is considerable overlap between this sample and a spectroscopically confirmed sample drawn from the same survey and this allows us to determine the reliability of the optical photometric selection (~60 per cent) and to show that the reliability can be significantly improved (to ~80 per cent) by applying near-infrared waveband criteria to exclude very red contaminants. Even this high level of reliability may compromise some statistical studies of LBG properties. We show that over 30 per cent of the highest reliability candidates have multiple ultraviolet (UV) luminous components and/or disturbed morphology in Hubble Space Telescope imaging, though it is unclear whether this represents multiple interacting/merging sources or individual large sources with multiple UV bright regions. Using this sample we confirm that the normalization of the bright end of the z = 5 UV luminosity function (down to M*) is lower than the same at z = 4 by a factor of 3. Using a Schechter fit we determine M*UV = -20.9 +/- 0.2. We discuss whether it is reasonable to expect the UV luminosity function to follow a Schechter function, given the UV emission is short lived and stochastic, and does not necessarily trace the underlying mass of the galaxy.

  13. Incorporating Single-nucleotide Polymorphisms Into the Lyman Model to Improve Prediction of Radiation Pneumonitis

    SciTech Connect

    Tucker, Susan L.; Li Minghuan; Xu Ting; Gomez, Daniel; Yuan Xianglin; Yu Jinming; Liu Zhensheng; Yin Ming; Guan Xiaoxiang; Wang Lie; Wei Qingyi; Mohan, Radhe; Vinogradskiy, Yevgeniy; Martel, Mary; Liao Zhongxing

    2013-01-01

    Purpose: To determine whether single-nucleotide polymorphisms (SNPs) in genes associated with DNA repair, cell cycle, transforming growth factor-{beta}, tumor necrosis factor and receptor, folic acid metabolism, and angiogenesis can significantly improve the fit of the Lyman-Kutcher-Burman (LKB) normal-tissue complication probability (NTCP) model of radiation pneumonitis (RP) risk among patients with non-small cell lung cancer (NSCLC). Methods and Materials: Sixteen SNPs from 10 different genes (XRCC1, XRCC3, APEX1, MDM2, TGF{beta}, TNF{alpha}, TNFR, MTHFR, MTRR, and VEGF) were genotyped in 141 NSCLC patients treated with definitive radiation therapy, with or without chemotherapy. The LKB model was used to estimate the risk of severe (grade {>=}3) RP as a function of mean lung dose (MLD), with SNPs and patient smoking status incorporated into the model as dose-modifying factors. Multivariate analyses were performed by adding significant factors to the MLD model in a forward stepwise procedure, with significance assessed using the likelihood-ratio test. Bootstrap analyses were used to assess the reproducibility of results under variations in the data. Results: Five SNPs were selected for inclusion in the multivariate NTCP model based on MLD alone. SNPs associated with an increased risk of severe RP were in genes for TGF{beta}, VEGF, TNF{alpha}, XRCC1 and APEX1. With smoking status included in the multivariate model, the SNPs significantly associated with increased risk of RP were in genes for TGF{beta}, VEGF, and XRCC3. Bootstrap analyses selected a median of 4 SNPs per model fit, with the 6 genes listed above selected most often. Conclusions: This study provides evidence that SNPs can significantly improve the predictive ability of the Lyman MLD model. With a small number of SNPs, it was possible to distinguish cohorts with >50% risk vs <10% risk of RP when they were exposed to high MLDs.

  14. First Constraints on Fuzzy Dark Matter from Lyman-α Forest Data and Hydrodynamical Simulations.

    PubMed

    Iršič, Vid; Viel, Matteo; Haehnelt, Martin G; Bolton, James S; Becker, George D

    2017-07-21

    We present constraints on the masses of extremely light bosons dubbed fuzzy dark matter (FDM) from Lyman-α forest data. Extremely light bosons with a de Broglie wavelength of ∼1  kpc have been suggested as dark matter candidates that may resolve some of the current small scale problems of the cold dark matter model. For the first time, we use hydrodynamical simulations to model the Lyman-α flux power spectrum in these models and compare it to the observed flux power spectrum from two different data sets: the XQ-100 and HIRES/MIKE quasar spectra samples. After marginalization over nuisance and physical parameters and with conservative assumptions for the thermal history of the intergalactic medium (IGM) that allow for jumps in the temperature of up to 5000 K, XQ-100 provides a lower limit of 7.1×10^{-22}  eV, HIRES/MIKE returns a stronger limit of 14.3×10^{-22}  eV, while the combination of both data sets results in a limit of 20×10^{-22}  eV (2σ C.L.). The limits for the analysis of the combined data sets increases to 37.5×10^{-22}  eV (2σ C.L.) when a smoother thermal history is assumed where the temperature of the IGM evolves as a power law in redshift. Light boson masses in the range 1-10×10^{-22}  eV are ruled out at high significance by our analysis, casting strong doubts that FDM helps solve the "small scale crisis" of the cold dark matter models.

  15. Wandering in the Lyman-alpha forest: a study of dark matter-dark radiation interactions

    NASA Astrophysics Data System (ADS)

    Krall, Rebecca; Cyr-Racine, Francis-Yan; Dvorkin, Cora

    2017-09-01

    The amplitude of large-scale matter fluctuations inferred from the observed Sunyaev-Zeldovich (SZ) cluster mass function and from weak gravitational lensing studies, when taken at face value, is in tension with measurements of the cosmic microwave background (CMB) and baryon acoustic oscillation (BAO). In this work, we revisit whether this possible discrepancy can be attributed to new interactions in the dark matter sector. Focusing on a cosmological model where dark matter interacts with a dark radiation species until the epoch of matter-radiation equality, we find that measurements of the Lyman-alpha flux power spectrum from the Sloan Digital Sky Survey provide no support to the hypothesis that new dark matter interactions can resolve the possible tension between CMB and large-scale structure (LSS). Indeed, while the addition of dark matter-dark radiation interactions leads to an improvement of 2Δ&ln;Script L=12 with respect to the standard Λ cold dark matter (ΛCDM) model when only CMB, BAO, and LSS data are considered, the inclusion of Lyman-alpha data reduces the improvement of the fit to 2Δ&ln;Script L=6 relative to ΛCDM . We thus conclude that the statistical evidence for new dark matter interactions (largely driven by the Planck SZ dataset) is marginal at best, and likely caused by systematics in the data. We also perform a Fisher forecast analysis for the reach of a future dataset composed of a CMB-S4 experiment combined with the Large Synoptic Survey Telescope galaxy survey. We find that the constraint on the effective number of fluid-like dark radiation species, Δ Nfluid, will be improved by an order of magnitude compared to current bounds.

  16. First Constraints on Fuzzy Dark Matter from Lyman-α Forest Data and Hydrodynamical Simulations

    NASA Astrophysics Data System (ADS)

    Iršič, Vid; Viel, Matteo; Haehnelt, Martin G.; Bolton, James S.; Becker, George D.

    2017-07-01

    We present constraints on the masses of extremely light bosons dubbed fuzzy dark matter (FDM) from Lyman-α forest data. Extremely light bosons with a de Broglie wavelength of ˜1 kpc have been suggested as dark matter candidates that may resolve some of the current small scale problems of the cold dark matter model. For the first time, we use hydrodynamical simulations to model the Lyman-α flux power spectrum in these models and compare it to the observed flux power spectrum from two different data sets: the XQ-100 and HIRES/MIKE quasar spectra samples. After marginalization over nuisance and physical parameters and with conservative assumptions for the thermal history of the intergalactic medium (IGM) that allow for jumps in the temperature of up to 5000 K, XQ-100 provides a lower limit of 7.1 ×10-22 eV , HIRES/MIKE returns a stronger limit of 14.3 ×10-22 eV , while the combination of both data sets results in a limit of 20 ×10-22 eV (2 σ C.L.). The limits for the analysis of the combined data sets increases to 37.5 ×10-22 eV (2 σ C.L.) when a smoother thermal history is assumed where the temperature of the IGM evolves as a power law in redshift. Light boson masses in the range 1 - 10 ×10-22 eV are ruled out at high significance by our analysis, casting strong doubts that FDM helps solve the "small scale crisis" of the cold dark matter models.

  17. The Lyman Continuum Escape Fraction of the Cosmic Horseshoe: A Test of Indirect Estimates

    NASA Astrophysics Data System (ADS)

    Vasei, Kaveh; Siana, Brian; Shapley, Alice E.; Quider, Anna M.; Alavi, Anahita; Rafelski, Marc; Steidel, Charles C.; Pettini, Max; Lewis, Geraint F.

    2016-11-01

    High-redshift star-forming galaxies are likely responsible for the reionization of the universe, yet direct detection of their escaping ionizing (Lyman continuum [LyC]) photons has proven to be extremely challenging. In this study, we search for escaping LyC of the Cosmic Horseshoe, a gravitationally lensed, star-forming galaxy at z = 2.38 with a large magnification of ∼24. Transmission at wavelengths of low-ionization interstellar absorption lines in the rest-frame ultraviolet suggests a patchy, partially transparent interstellar medium. This makes it an ideal candidate for direct detection of the LyC. We obtained a 10-orbit Hubble near-UV image using the Wide Field Camera 3 (WFC3)/UVIS F275W filter that probes wavelengths just below the Lyman limit at the redshift of the Horseshoe in an attempt to detect escaping LyC radiation. After fully accounting for the uncertainties in the opacity of the intergalactic medium (IGM) and accounting for the charge transfer inefficiency in the WFC3 CCDs, we find a 3σ upper limit for the relative escape fraction of {f}{esc,{rel}}\\lt 0.08. This value is a factor of five lower than the value (0.4) predicted by the 40% transmission in the low-ion absorption lines. Though possible, it is unlikely that the nondetection is due to a high-opacity line of sight through the IGM (\\lt 20% chance). We discuss several possible causes for the discrepancy between the escape fraction and the covering fraction and consider the implications for future attempts at both direct LyC detection and indirect estimates of the escape fraction.

  18. A Novel Suite of Hydrodynamical Simulations of the Lyman-Alpha Forest with Massive Neutrinos

    NASA Astrophysics Data System (ADS)

    Rossi, Graziano; Palanque-Delabrouille, N.; Yeche, C.; Viel, M.; Rich, J.; LeGoff, J.; Borde, A.

    2014-01-01

    We present a suite of state-of-the-art hydrodynamical simulations with cold dark matter, baryons and massive neutrinos, specifically targeted for modeling the low-density regions of the intergalactic medium (IGM) as probed by the Lyman-Alpha forest at high-redshift. The simulations span volumes ranging from (25 Mpc/h)^3 to (100 Mpc/h)^3, and are made using either 3×192^3 ~ 21 millions or 3×768^3 ~ 1.4 billion particles - with cosmological parameters compatible with the latest Planck (2013) results. While our realizations have been specifically designed to meet the requirements of the Baryon Acoustic Spectroscopic Survey (BOSS), they can also be utilized for upcoming or future experiments - such as eBOSS and MS-DESI - since the overall resolution can be further enhanced so that one could reach the equivalent of 3×3072^3 ~ 87 billion particles in a (100 Mpc/h)^3 box size. We improve on pre-exisiting modeling in several ways, in particular with new prescriptions for IGM radiative cooling and heating processes, a more updated re-ionization history, and initial conditions based on 2LPT rather than the Zeldovich approximation. Combining data from BOSS and the Planck satellite, and with a grid of corresponding LCDM simulations, our mocks will allow us to constrain cosmological parameters and neutrino masses directly from the Lyman-Alpha forest with unprecedented sensitivity. The simulations can also be useful for a broader variety of cosmological studies, and willl be made available to the scientific community upon request.

  19. The 27-day versus 13.5-day variations in the solar Lyman-alpha radiation and the radio wave absorption in the lower ionosphere over Europe

    NASA Technical Reports Server (NTRS)

    Delamorena, B. A.; Lastovicka, Jan; Rapoport, Z. TS.; Alberca, L.

    1989-01-01

    In order to clarify the question of solar periods in absorption, the pattern was studied of the solar Lyman-alpha radiation (the principal ionizing agent of the lower ionosphere) and of the radio wave absorption at five widely spaced places in Europe. When the solar Lyman-alpha flux variability is very well developed, then it dominates in the lower ionospheric variability. The most pronounced Lyman-alpha variation on time scale day-month is the solar rotation variation (about 27 days). When the Lyman-alpha variability is developed rather poorly, as it is typical for periods dominated by the 13.5 day variability, then the lower ionospheric variability appears to be dominated by variations of meteorological origin. The conclusions hold for all five widely spaced placed in Europe.

  20. Lyman-alpha, Far Infrared and , X-ray and Gamma-ray Observations Around the Maximum of Cycle 24 by the French-Chinese SMall Explorer for Solar Eruptions

    NASA Astrophysics Data System (ADS)

    Trottet, Gerard

    The SMall Explorer for Solar Eruptions (SMESE) is a French-Chinese project developed in the frame of the microsatellite program of Centre National d'Etudes Spatiales (CNES) which should be launched around the maximum of solar cylcle 24 (2012-2013). We describe the SMESE payload which includes a coronagraph and disk imager in Lyman-alpha (LYOT), a far infrared telescope (DESIR) and a hard X-ray and gamma-ray spectrometer (HEBS). We emphasize that these three instruments will provide unprecedented observations bringing unique information on: (a) the origin of coronal mass ejections (CME's); (b) the relationship between flares and CME's; (c) the characteristics of the most energetic particles accelerated at the Sun and (d) the energy transport in the solar atmosphere. SMESE will also provide the first measurements of the magnetic field in the solar corona. We finally describe the mission profile and context.

  1. A ground-based imaging study of galaxies causing damped Lyman α (DLA), sub-DLA and Lyman limit system absorption in quasar spectra

    NASA Astrophysics Data System (ADS)

    Rao, Sandhya M.; Belfort-Mihalyi, Michèle; Turnshek, David A.; Monier, Eric M.; Nestor, Daniel B.; Quider, Anna

    2011-09-01

    We present results from a search for galaxies that give rise to damped Lyman α (DLA), sub-DLA and Lyman limit system (LLS) absorption at redshifts 0.1 ≲z≲ 1 in the spectra of background quasars. The sample was formed from a larger sample of strong Mg II absorbers (Wλ27960≥ 0.3 Å) whose H I column densities were determined by measuring the Lyα line in Hubble Space Telescope ultraviolet spectra. Photometric redshifts, galaxy colours and proximity to the quasar sightline, in decreasing order of importance, were used to identify galaxies responsible for the absorption. Our sample includes 80 absorption systems for which the absorbing galaxies have been identified, of which 54 are presented here for the first time. In some cases a reasonable identification for the absorbing galaxy could not be made. The main results of this study are (i) the surface density of galaxies falls off exponentially with increasing impact parameter, b, from the quasar sightline relative to a constant background of galaxies, with an e-folding length of ≈46 kpc. Galaxies with b≳ 100 kpc calculated at the absorption redshift are statistically consistent with being unrelated to the absorption system, and are either background or foreground galaxies. (ii) ? is inversely correlated with b at the 3.0σ level of significance. DLA galaxies are found systematically closer to the quasar sightline, by a factor of 2, than are galaxies which give rise to sub-DLAs or LLSs. The median impact parameter is 17.4 kpc for the DLA galaxy sample, 33.3 kpc for the sub-DLA sample and 36.4 kpc for the LLS sample. We also find that the decline in ? with b can be roughly described by an exponential with an e-folding length of 12 kpc that occurs at ?. (iii) Absorber galaxy luminosity relative to L*, L/L*, is not significantly correlated with Wλ27960, ? or b. (iv) DLA, sub-DLA and LLS galaxies comprise a mix of spectral types, but are inferred to be predominantly late-type galaxies based on their spectral

  2. Use of Fabry-Perot annular summing spectroscopy to acquire geocoronal hydrogen Balmer-α line profile data

    NASA Astrophysics Data System (ADS)

    Nossal, Susan M.; Roesler, Fred L.; Coakley, Monica M.; Reynolds, Ronald J.

    1996-10-01

    A Fabry-Perot annular summing spectroscopy technique has been sued at the University of Wisconsin's Pine Bluff Observatory to acquire geocoronal Balmer-(alpha) line profile data with significantly improved precision and height resolution. The double-etalon Fabry-Perot interference pattern is imaged onto a photometrics PM512 CCD chip, thus enabling light to be gathered in multiple spectral bins simultaneously. In comparison with scanning systems we used earlier, the high quantum efficiency of the CCD and the multi-channel detection associated with the Fabry-Perot annular summing technique have enabled us to save a factor of about 10 in the integration time required for studies of the line profile. As a result, we are now able to both more precisely observe the line shape of the very faint Balmer- (alpha) emission and obtain data using shorter integration times. Our data illustrate the scientific potential for using this technique for the study of very faint extended emission line sources. The increase in the signal-to-noise of our data has enabled us to examine Balmer-(alpha) profile asymmetries which we have found to be compatible with predictions that on the order of 10 percent of the geocoronal Balmer-(alpha) excitation arises from cascades due to higher-member solar Lyman series excitation. This fine structure was overlooked in previous Balmer-(alpha) studies aimed at determining non-Maxwellian dynamical properties of exospheric hydrogen; we find that cascade excitation largely masks the expected very small dynamical perturbations to the line profile at low shadow heights, and must be more thoroughly studied before drawing conclusions about exospheric dynamics. Accounting for cascade laos leads to more realistic determinations of exospheric hydrogen temperatures near the exobase.

  3. The large-scale cross-correlation of Damped Lyman alpha systems with the Lyman alpha forest: first measurements from BOSS

    SciTech Connect

    Font-Ribera, Andreu; Miralda-Escudé, Jordi; Arnau, Eduard; Carithers, Bill; Ross, Nicholas P.; White, Martin; Lee, Khee-Gan; Noterdaeme, Pasquier; Pâris, Isabelle; Petitjean, Patrick; Rollinde, Emmanuel; Rich, James; Schneider, Donald P.; York, Donald G. E-mail: miralda@icc.ub.edu

    2012-11-01

    We present the first measurement of the large-scale cross-correlation of Lyα forest absorption and Damped Lyman α systems (DLA), using the 9th Data Release of the Baryon Oscillation Spectroscopic Survey (BOSS). The cross-correlation is clearly detected on scales up to 40h{sup −1}Mpc and is well fitted by the linear theory prediction of the standard Cold Dark Matter model of structure formation with the expected redshift distortions, confirming its origin in the gravitational evolution of structure. The amplitude of the DLA-Lyα cross-correlation depends on only one free parameter, the bias factor of the DLA systems, once the Lyα forest bias factors are known from independent Lyα forest correlation measurements. We measure the DLA bias factor to be b{sub D} = (2.17±0.20)β{sub F}{sup 0.22}, where the Lyα forest redshift distortion parameter β{sub F} is expected to be above unity. This bias factor implies a typical host halo mass for DLAs that is much larger than expected in present DLA models, and is reproduced if the DLA cross section scales with halo mass as M{sub h}{sup α}, with α = 1.1±0.1 for β{sub F} = 1. Matching the observed DLA bias factor and rate of incidence requires that atomic gas remains extended in massive halos over larger areas than predicted in present simulations of galaxy formation, with typical DLA proper sizes larger than 20 kpc in host halos of masses ∼ 10{sup 12}M{sub ☉}. We infer that typical galaxies at z ≅ 2 to 3 are surrounded by systems of atomic clouds that are much more extended than the luminous parts of galaxies and contain ∼ 10% of the baryons in the host halo.

  4. On the Frequency and Voltage-Dependent Profiles of the Surface States and Series Resistance of Au/ZnO/n-Si Structures in a Wide Range of Frequency and Voltage

    NASA Astrophysics Data System (ADS)

    Nikravan, Afsoun; Badali, Yosef; Altındal, Şemsettin; Uslu, İbrahim; Orak, İkram

    2017-06-01

    In order to interpret the electrical characteristics of fabricated Au/ZnO/n-Si structures as a function of frequency and voltage well, their capacitance-voltage (C-V) and conductance-voltage (G/ω-V) measurements were carried out in a wide range of frequencies (0.7 kHz-2 MHz) and voltages (± 6 V) by 50 mV steps at room temperature. Both the C-V and G/ω-V plots have reverse, depletion, and accumulation regions such as a metal-insulator/oxide semiconductor (MIS or MOS) structures. The values of doped-donor atoms (N D), Fermi energy level (E F), barrier height (ΦB), and series resistance (R s) of the structure were obtained as a function of frequency and voltage. While the value of N D decreases with increasing frequency almost as exponentially, the value of depletion width (W D) increases. The values of C and G/ω increase with decreasing frequency because the surface states (N ss) are able to follow the alternating current (AC) signal, resulting in excess capacitance (C ex) and conductance (G ex/ω), which depends on their relaxation time and the frequency of the AC signal. The voltage-dependent profiles of N ss were obtained from both the high-low frequency capacitance and Hill-Colleman methods. The other important parameter R s of the structure was also obtained from the Nicollian and Brews methods as a function of voltage.

  5. On the Frequency and Voltage-Dependent Profiles of the Surface States and Series Resistance of Au/ZnO/n-Si Structures in a Wide Range of Frequency and Voltage

    NASA Astrophysics Data System (ADS)

    Nikravan, Afsoun; Badali, Yosef; Altındal, Şemsettin; Uslu, İbrahim; Orak, İkram

    2017-10-01

    In order to interpret the electrical characteristics of fabricated Au/ZnO/n-Si structures as a function of frequency and voltage well, their capacitance-voltage ( C- V) and conductance-voltage ( G/ ω- V) measurements were carried out in a wide range of frequencies (0.7 kHz-2 MHz) and voltages (± 6 V) by 50 mV steps at room temperature. Both the C- V and G/ ω- V plots have reverse, depletion, and accumulation regions such as a metal-insulator/oxide semiconductor (MIS or MOS) structures. The values of doped-donor atoms ( N D), Fermi energy level ( E F), barrier height (ΦB), and series resistance ( R s) of the structure were obtained as a function of frequency and voltage. While the value of N D decreases with increasing frequency almost as exponentially, the value of depletion width ( W D) increases. The values of C and G/ ω increase with decreasing frequency because the surface states ( N ss) are able to follow the alternating current (AC) signal, resulting in excess capacitance ( C ex) and conductance ( G ex/ ω), which depends on their relaxation time and the frequency of the AC signal. The voltage-dependent profiles of N ss were obtained from both the high-low frequency capacitance and Hill-Colleman methods. The other important parameter R s of the structure was also obtained from the Nicollian and Brews methods as a function of voltage.

  6. Assiniboine Series.

    ERIC Educational Resources Information Center

    Allen, Minerva

    This series of illustrated booklets presents 13 Indian stories in a bilingual format of English and Assiniboine, an Indian tribal language. Written on the first grade level, the stories have the following titles: (1) "Orange Tree in Lodgepole"; (2) "Pretty Flower"; (3) Inktomi and the Rock"; (4) "Inktomi and the…

  7. Assiniboine Series.

    ERIC Educational Resources Information Center

    Allen, Minerva

    This series of illustrated booklets presents 13 Indian stories in a bilingual format of English and Assiniboine, an Indian tribal language. Written on the first grade level, the stories have the following titles: (1) "Orange Tree in Lodgepole"; (2) "Pretty Flower"; (3) Inktomi and the Rock"; (4) "Inktomi and the…

  8. Rest-Frame Mid-Infrared Detection of an Extremely Luminous Lyman Break Galaxy with the Spitzer Infrared Spectrograph (IRS)

    NASA Technical Reports Server (NTRS)

    Teplitz, H. I.; Charmandaris, V.; Armus, L.; Appleton, P. N.; Houck, J. R.; Soifer, B. T.; Weedman, D.; Brandl, B. R.; vanCleve, J.; Grillmair, C.; Uchid, K. I.

    2004-01-01

    We present the first rest-frame of approximately 4 microns detection of a Lyman break galaxy. The data were obtained using the 16 microns imaging capability of the Spitzer Infrared Spectrograph. The target object, J134026.44+634433.2, is an extremely luminous Lyman break galaxy at z=2.79, first identified in Sloan Digital Sky Survey (SDSS) spectra (as reported by Bentz et al.). The source is strongly detected with a flux of 0.94 +/- 0.02 mJy. Combining Spitzer and SDSS photometry with supporting ground-based J- and K-band data, we show that the spectral energy distribution is consistent with an actively star-forming galaxy. We also detect other objects in the Spitzer field of view, including a very red mid-infrared source. We find no evidence of a strong lens among the mid-infrared sources.

  9. Detection of a hydrogen corona in HST Lyman-alpha images of Europa in transit of Jupiter

    NASA Astrophysics Data System (ADS)

    Roth, L.; Ivchenko, N.; Retherford, K. D.; Schlatter, N. M.; Strobel, D. F.; Becker, T. M.; Saur, J.; Feldman, P.; McGrath, M. A.; Spencer, J. R.; Grava, C.; Nimmo, F.; Blöcker, A.

    2016-12-01

    We report far-ultraviolet observations of Europa in transit of Jupiter obtained with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Space Telescope (HST) on six occasions between December 2014 and March 2015. Absorption of Jupiter's bright hydrogen Lyman-alpha dayglow is present in a region several moon radii above the limb in all observations. The observed extended absorption provides the first detection of an atomic hydrogen corona at Europa. Molecular constituents in Europa's global sputtered atmosphere are shown to be optically thin to Lyman-alpha. The observations suggest a fast escaping H corona with a surface density of 2 x 103 cm-3, which matches the expected abundances from atmosphere simulations. Additionally, we search for anomalies around the limb of Europa due to absorption by localized high H2O abundances from active plumes. No significant local absorption features are detected.

  10. Rest-Frame Mid-Infrared Detection of an Extremely Luminous Lyman Break Galaxy with the Spitzer Infrared Spectrograph (IRS)

    NASA Technical Reports Server (NTRS)

    Teplitz, H. I.; Charmandaris, V.; Armus, L.; Appleton, P. N.; Houck, J. R.; Soifer, B. T.; Weedman, D.; Brandl, B. R.; vanCleve, J.; Grillmair, C.; hide

    2004-01-01

    We present the first rest-frame of approximately 4 microns detection of a Lyman break galaxy. The data were obtained using the 16 microns imaging capability of the Spitzer Infrared Spectrograph. The target object, J134026.44+634433.2, is an extremely luminous Lyman break galaxy at z=2.79, first identified in Sloan Digital Sky Survey (SDSS) spectra (as reported by Bentz et al.). The source is strongly detected with a flux of 0.94 +/- 0.02 mJy. Combining Spitzer and SDSS photometry with supporting ground-based J- and K-band data, we show that the spectral energy distribution is consistent with an actively star-forming galaxy. We also detect other objects in the Spitzer field of view, including a very red mid-infrared source. We find no evidence of a strong lens among the mid-infrared sources.

  11. Performance Characterization of UV Science Cameras Developed for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP)

    NASA Technical Reports Server (NTRS)

    Champey, Patrick; Kobayashi, Ken; Winebarger, Amy; Cirtin, Jonathan; Hyde, David; Robertson, Bryan; Beabout, Brent; Beabout, Dyana; Stewart, Mike

    2014-01-01

    The NASA Marshall Space Flight Center (MSFC) has developed a science camera suitable for sub-orbital missions for observations in the UV, EUV and soft X-ray. Six cameras will be built and tested for flight with the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), a joint National Astronomical Observatory of Japan (NAOJ) and MSFC sounding rocket mission. The goal of the CLASP mission is to observe the scattering polarization in Lyman-alpha and to detect the Hanle effect in the line core. Due to the nature of Lyman-alpha polarization in the chromosphere, strict measurement sensitivity requirements are imposed on the CLASP polarimeter and spectrograph systems; science requirements for polarization measurements of Q/I and U/I are 0.1% in the line core. CLASP is a dual-beam spectro-polarimeter, which uses a continuously rotating waveplate as a polarization modulator, while the waveplate motor driver outputs trigger pulses to synchronize the exposures. The CCDs are operated in frame-transfer mode; the trigger pulse initiates the frame transfer, effectively ending the ongoing exposure and starting the next. The strict requirement of 0.1% polarization accuracy is met by using frame-transfer cameras to maximize the duty cycle in order to minimize photon noise. Coating the e2v CCD57-10 512x512 detectors with Lumogen-E coating allows for a relatively high (30%) quantum efficiency at the Lyman-$\\alpha$ line. The CLASP cameras were designed to operate with =10 e- /pixel/second dark current, = 25 e- read noise, a gain of 2.0 and =0.1% residual non-linearity. We present the results of the performance characterization study performed on the CLASP prototype camera; dark current, read noise, camera gain and residual non-linearity.

  12. Diagnosing the reionization of the universe - The absorption spectrum of the intergalactic medium and Lyman alpha clouds

    NASA Technical Reports Server (NTRS)

    Giroux, Mark L.; Shapiro, Paul R.

    1991-01-01

    The thermal and ionization evolution of a uniform intergalactic medium composed of H and He and undergoing reionization is studied. The diagnosis of the metagalactic ionizing radiation background at z of about three using metal line ratios for Lyman limit quasar absorption line systems is addressed. The use of the He II Gunn-Peterson effect to diagnose the reionization source and/or nature of the Hy-alpha forest clouds is considered.

  13. Formación del contínuo de Lyman en atmósferas de estrellas B

    NASA Astrophysics Data System (ADS)

    Rohrmann, R. D.

    Se presentan resultados de modelos de atmósferas para estrellas tempranas que poseen una estructura cromosférica y una atmósfera extendida en expansión. Se analiza con rigurosidad el acople del campo de radiación en el continuo de Lyman y su relación con las poblaciones en equilibrio estadístico del H y He.

  14. Sowing Black Hole Seeds: Forming Direct Collapse Black Holes With Realistic Lyman-Werner Radiation Fields in Cosmological Simulations

    NASA Astrophysics Data System (ADS)

    Holley-Bockelmann, Kelly; Dunn, Glenna; Bellovary, Jillian M.; Christensen, Charlotte

    2016-01-01

    Luminous quasars detected at redshifts z > 6 require that the first black holes form early and grow to ~109 solar masses within one Gyr. Our work uses cosmological simulations to study the formation and early growth of direct collapse black holes. In the pre-reionization epoch, molecular hydrogen (H2) causes gas to fragment and form Population III stars, but Lyman-Werner radiation can suppress H2 formation and allow gas to collapse directly into a massive black hole. The critical flux required to inhibit H2 formation, Jcrit, is hotly debated, largely due to the uncertainties in the source radiation spectrum, H2 self-shielding, and collisional dissociation rates. Here, we test the power of the direct collapse model in a non-uniform Lyman-Werner radiation field, using an updated version of the SPH+N-body tree code Gasoline with H2 non-equilibrium abundance tracking, H2 cooling, and a modern SPH implementation. We vary Jcrit from 30 to 104 J21 to study the effect on seed black holes, focusing on black hole formation as a function of environment, halo mass, metallicity, and proximity of the Lyman-Werner source. We discuss the constraints on massive black hole occupation fraction in the quasar epoch, and implications for reionization, high-redshift X-ray background radiation, and gravitational waves.

  15. COMPARISON OF PIONEER 10, VOYAGER 1, AND VOYAGER 2 ULTRAVIOLET OBSERVATIONS WITH ANTI-SOLAR LYMAN-ALPHA BACKSCATTER SIMULATIONS

    SciTech Connect

    Fayock, B.; Zank, G. P.; Heerikhuisen, J. E-mail: garyp.zank@gmail.com

    2013-09-20

    Observations made by ultraviolet (UV) detectors on board Pioneer 10, Voyager 1, and Voyager 2 can be used to analyze the distribution of neutral hydrogen throughout the heliosphere, including the interaction regions of the solar wind and local interstellar medium. Previous studies of the long-term trend of decreasing intensity with increasing heliocentric distance established the need for more sophisticated heliospheric models. Here we use state-of-the-art three-dimensional (3D) magnetohydrodynamic (MHD) neutral models to simulate Lyman-alpha backscatter as would be seen by the three spacecrafts, exploiting a new 3D Monte Carlo radiative transfer code under solar minimum conditions. Both observations and simulations of the UV backscatter intensity are normalized for each spacecraft flight path at {approx}15 AU, and we focus on the slope of decreasing intensity over an increasing heliocentric distance. Comparisons of simulations with Voyager 1 Lyman-alpha data results in a very close match, while the Pioneer 10 comparison is similar due to normalization, but not considered to be in agreement. The deviations may be influenced by a low resolution of photoionization in the 3D MHD-neutral model, a lack of solar cycle activity in our simulations, and possibly issues with instrumental sensitivity. Comparing the slope of Voyager 2 and the simulated intensities yields an almost identical match. Our results predict a large increase in the Lyman-alpha intensity as the hydrogen wall is approached, which would signal an imminent crossing of the heliopause.

  16. PEP/HerMES/COSMOS: What are the dust properties of z ˜ 3 lyman break galaxies?

    NASA Astrophysics Data System (ADS)

    Álvarez-Márquez, A.; Burgarella, D.; Buat, V.; Heinis, S.; Pep/Hermes/Cosmos Teams

    2015-05-01

    Context. Since the mid-90's, the sample of Lyman break galaxies has been growing up thanks to the deeper and deeper sensitivities of the telescope in optical and in near-infrared for objects at z > 2.5. However, the dust properties of these Lyman break galaxies are still elusive of badly known because the samples are small and/or biased.} Aims. We explore the dust properties in a statistical way of a sample of Lyman break galaxies (LBGs) that can not be individually detected in Herschel maps. Methods. We apply a stacking method in the Herschel and AzTEC maps to LBGs selected at 2.5 < z < 3.5 by dropout technique. Thanks to the size of the sample (˜22 000 LBGs), we can split it in several bins as a function of their ultraviolet luminosity (L_{FUV}), their ultraviolet slope (β_{UV}) and their stellar mass (M_{*}) to better catch their variety. The stacking is corrected for the incompleteness in the priors and for the clustering of the stacked galaxies in ultraviolet. Results. We obtain the full infrared spectral energy distributions of our LBGs as a function of their L_{FUV}, their β_{UV} and their M_* and we can characterize them in terms of their dust attenuation A_{FUV}, their star formation rate (SFR).

  17. New approach for precise computation of Lyman-α forest power spectrum with hydrodynamical simulations

    SciTech Connect

    Borde, Arnaud; Palanque-Delabrouille, Nathalie; Rossi, Graziano; Yèche, Christophe; LeGoff, Jean-Marc; Rich, Jim; Bolton, James S. E-mail: nathalie.palanque-delabrouille@cea.fr E-mail: matteoviel@gmail.com E-mail: christophe.yeche@cea.fr E-mail: james.rich@cea.fr

    2014-07-01

    Current experiments are providing measurements of the flux power spectrum from the Lyman-α forests observed in quasar spectra with unprecedented accuracy. Their interpretation in terms of cosmological constraints requires specific simulations of at least equivalent precision. In this paper, we present a suite of cosmological N-body simulations with cold dark matter and baryons, specifically aiming at modeling the low-density regions of the inter-galactic medium as probed by the Lyman-α forests at high redshift. The simulations were run using the GADGET-3 code and were designed to match the requirements imposed by the quality of the current SDSS-III/BOSS or forthcoming SDSS-IV/eBOSS data. They are made using either 2 × 768{sup 3} ≅ 1 billion or 2 × 192{sup 3} ≅ 14 million particles, spanning volumes ranging from (25 Mpc h{sup −1}){sup 3} for high-resolution simulations to (100 Mpc h{sup −1}){sup 3} for large-volume ones. Using a splicing technique, the resolution is further enhanced to reach the equivalent of simulations with 2 × 3072{sup 3} ≅ 58 billion particles in a (100 Mpc h{sup −1}){sup 3} box size, i.e. a mean mass per gas particle of 1.2 × 10{sup 5}M{sub ⊙} h{sup −1}. We show that the resulting power spectrum is accurate at the 2% level over the full range from a few Mpc to several tens of Mpc. We explore the effect on the one-dimensional transmitted-flux power spectrum of four cosmological parameters (n{sub s}, σ{sub 8}, Ω{sub m} and H{sub 0}) and two astrophysical parameters (T{sub 0} and γ) that are related to the heating rate of the intergalactic medium. By varying the input parameters around a central model chosen to be in agreement with the latest Planck results, we built a grid of simulations that allows the study of the impact on the flux power spectrum of these six relevant parameters. We improve upon previous studies by not only measuring the effect of each parameter individually, but also probing the impact of the

  18. X-Ray Properties of Lyman Break Galaxies in the Hubble Deep Field North Region

    NASA Technical Reports Server (NTRS)

    Nandra, K.; Mushotzky, R. F.; Arnaud, K.; Steidel, C. C.; Adelberger, K. L.; Gardner, J. P.; Teplitz, H. I.; Windhorst, R. A.; White, Nicholas E. (Technical Monitor)

    2002-01-01

    We describe the X-ray properties of a large sample of z approximately 3 Lyman Break Galaxies (LBGs) in the region of the Hubble Deep Field North, derived from the 1 Ms public Chandra observation. Of our sample of 148 LBGs, four are detected individually. This immediately gives a measure of the bright AGN (active galactic nuclei) fraction in these galaxies of approximately 3 per cent, which is in agreement with that derived from the UV (ultraviolet) spectra. The X-ray color of the detected sources indicates that they are probably moderately obscured. Stacking of the remainder shows a significant detection (6 sigma) with an average luminosity of 3.5 x 10(exp 41) erg/s per galaxy in the rest frame 2-10 keV band. We have also studied a comparison sample of 95 z approximately 1 "Balmer Break" galaxies. Eight of these are detected directly, with at least two clear AGN based on their high X-ray luminosity and very hard X-ray spectra respectively. The remainder are of relatively low luminosity (< 10(exp 42) erg/s, and the X-rays could arise from either AGN or rapid star-formation. The X-ray colors and evidence from other wavebands favor the latter interpretation. Excluding the clear AGN, we deduce a mean X-ray luminosity of 6.6 x 10(exp 40) erg/s, a factor approximately 5 lower than the LBGs. The average ratio of the UV and X-ray luminosities of these star forming galaxies L(sub UV)/L (sub X), however, is approximately the same at z = 1 as it is at z = 3. This scaling implies that the X-ray emission follows the current star formation rate, as measured by the UV luminosity. We use our results to constrain the star formation rate at z approximately 3 from an X-ray perspective. Assuming the locally established correlation between X-ray and far-IR (infrared) luminosity, the average inferred star formation rate in each Lyman break galaxy is found to be approximately 60 solar mass/yr, in excellent agreement with the extinction-corrected UV estimates. This provides an external

  19. Studying low-redshift universe through observation of Damped Lyman-alpha quasar absorbers

    NASA Astrophysics Data System (ADS)

    Gharanfoli, Soheila

    2009-06-01

    In recent years, an extremely successful method to study galaxy formation and evolution, has been provided by observation of quasar absorbers. Quasar absorbers are systems intercepting our line-of-sight to a given quasar and thus produce a feature in the quasar spectrum, the so-called absorption lines. The Damped Lyman-a (DLA) and sub-Damped Lyman-a (sub-DLA) absorption features in quasar spectra are believed to be produced by intervening galaxies. However, the connection of quasar absorbers to galaxies is not well-understood, since attempts to image the absorbing galaxies have often failed. DLAs and sub-DLAs were originally thought to be the precursors of present day disk galaxies, but there is evidence that they may be dominated by gas-rich, proto-dwarf galaxies representing the basic building blocks of hierarchical growth of structure. While most DLAs appear to be metal-poor, a population of metal-rich absorbers, mostly sub-DLAs, has been discovered in recent spectroscopic studies. It is of great interest to image these metal-rich absorbers, especially with high spatial resolution, to understand the connection between the stellar and interstellar content of the underlying galaxies. This dissertation consists of several projects designed to further our understanding of galaxies and galactic structures associated with intervening quasar absorption lines. Two projects were completed that involved the imaging of 13 DLA/sub-DLA galaxies at z < 1. High angular resolution near-infrared images were obtained, using the Hokupa'a Adaptive Optics system with the QUIRC near-infrared camera on the 8-m Gemini-North telescope, and the Laser Guide Star Adaptive Optics system on the 10-m Keck telescope. Detailed properties of the identified absorber galaxies are described. They are shown to be drawn from a variety of morphological types with a range of luminosities, sizes, and impact parameters. In the other set of projects, follow-up spectroscopy was performed to confirm the

  20. The escape of Lyman photons from a young starburst: the case of Haro11†

    NASA Astrophysics Data System (ADS)

    Hayes, Matthew; Östlin, Göran; Atek, Hakim; Kunth, Daniel; Mas-Hesse, J. Miguel; Leitherer, Claus; Jiménez-Bailón, Elena; Adamo, Angela

    2007-12-01

    Lyman α (Lyα) is one of the dominant tools used to probe the star-forming galaxy population at high redshift (z). However, astrophysical interpretations of data drawn from Lyα alone hinge on the Lyα escape fraction which, due to the complex radiative transport, may vary greatly. Here, we map the Lyα emission from the local luminous blue compact galaxy Haro11, a known emitter of Lyα and the only known candidate for low-z Lyman continuum emission. To aid in the interpretation, we perform a detailed ultraviolet and optical multiwavelength analysis and model the stellar population, dust distribution, ionizing photon budget, and star-cluster population. We use archival X-ray observations to further constrain properties of the starburst and estimate the neutral hydrogen column density. The Lyα morphology is found to be largely symmetric around a single young star-forming knot and is strongly decoupled from other wavelengths. From general surface photometry, only very slight correlation is found between Lyα and Hα, E(B - V), and the age of the stellar population. Only around the central Lyα bright cluster do we find the Lyα/Hα ratio at values predicted by the recombination theory. The total Lyα escape fraction is found to be just 3 per cent. We compute that ~90 per cent of the Lyα photons that escape do so after undergoing multiple resonance scattering events, masking their point of origin. This leads to a largely symmetric distribution and, by increasing the distance that photons must travel to escape, decreases the escape probability significantly. While dust must ultimately be responsible for the destruction of Lyα, it plays a little role in governing the observed morphology, which is regulated more by interstellar medium kinematics and geometry. We find tentative evidence for local Lyα equivalent width in the immediate vicinity of star clusters being a function of cluster age, consistent with hydrodynamic studies. We estimate the intrinsic production

  1. Evidence for Black Hole Growth in Local Analogs to Lyman Break Galaxies

    NASA Technical Reports Server (NTRS)

    Jia, Jianjun; Ptak, Andrew; Heckman, Timothy M.; Overzier, Roderik A.; Hornschemeier, Ann; LaMassa, Stephanie M.

    2011-01-01

    We have used XMM-Newton to observe six Lyman break analogs (LBAs): members of the rare population of local galaxies that have properties that are very similar to distant Lyman break galaxies. Our six targets were specifically selected because they have optical emission-line properties that are intermediate between starbursts and Type 2 (obscured) active galactic nuclei (AGNs). Our new X-ray data provide an important diagnostic of the presence of an AGN. We find X-ray luminosities of order 10(sup 42) erg per second and ratios of X-ray to far-IR lummositles that are higher than values in pure starburst galaxies by factors ranging from approximately 3 to 30. This strongly suggests the presence of an AGN in at least some of the galaxies. The ratios of the luminosities of the hard (2-10 keV) X-ray to [O III] emission line are low by about an order of magnitude compared with Type 1 AGN, but are consistent with the broad range seen in Type 2 AGN. Either the AGN hard X-rays are significantly obscured or the [O III] emission is dominated by the starburst. We searched for an iron emission line at approximately 6.4 ke V, which is a key feature of obscured AGNs, but only detected emission at the approximately 2sigma level. Finally, we find that the ratios of the mid-infrared (24 micrometer) continuum to [O III]lambda 5007 luminosities in these LBAs are higher than the values for Type 2 AGN by an average of 0.8 dex. Combining all these clues, we conclude that an AGN is likely to be present, but that the bolometric luminosity is produced primarily by an intense starburst. If these black holes are radiating at the Eddington limit, their masses would lie in the range of 10(sup 5) - 10(sup 6) solar mass. These objects may offer ideal local laboratories to investigate the processes by which black holes grew in the early universe.

  2. EVIDENCE FOR ELEVATED X-RAY EMISSION IN LOCAL LYMAN BREAK GALAXY ANALOGS

    SciTech Connect

    Basu-Zych, Antara R.; Lehmer, Bret D.; Hornschemeier, Ann E.; Ptak, Andrew F.; Goncalves, Thiago S.; Fragos, Tassos; Heckman, Timothy M.; Overzier, Roderik A.; Schiminovich, David

    2013-09-10

    Our knowledge of how X-ray emission scales with star formation at the earliest times in the universe relies on studies of very distant Lyman break galaxies (LBGs). In this paper, we study the relationship between the 2-10 keV X-ray luminosity (L{sub X}), assumed to originate from X-ray binaries (XRBs), and star formation rate (SFR) in ultraviolet (UV) selected z < 0.1 Lyman break analogs (LBAs). We present Chandra observations for four new Galaxy Evolution Explorer selected LBAs. Including previously studied LBAs, Haro 11 and VV 114, we find that LBAs demonstrate L{sub X}/SFR ratios that are elevated by {approx}1.5{sigma} compared to local galaxies, similar to the ratios found for stacked LBGs in the early universe (z > 2). Unlike some of the composite LBAs studied previously, we show that these LBAs are unlikely to harbor active galactic nuclei, based on their optical and X-ray spectra and the spatial distribution of the X-rays in three spatially extended cases. Instead, we expect that high-mass X-ray binaries (HMXBs) dominate the X-ray emission in these galaxies, based on their high specific SFRs (sSFRs {identical_to} SFR/M{sub *} {>=} 10{sup -9} yr{sup -1}), which suggest the prevalence of young stellar populations. Since both UV-selected populations (LBGs and LBAs) have lower dust attenuations and metallicities compared to similar samples of more typical local galaxies, we investigate the effects of dust extinction and metallicity on the L{sub X}/SFR for the broader population of galaxies with high sSFRs (>10{sup -10} yr{sup -1}). The estimated dust extinctions (corresponding to column densities of N{sub H} < 10{sup 22} cm{sup -2}) are expected to have insignificant effects on observed L{sub X}/SFR ratio for the majority of galaxy samples. We find that the observed relationship between L{sub X}/SFR and metallicity appears consistent with theoretical expectations from XRB population synthesis models. Therefore, we conclude that lower metallicities, related to

  3. Contamination on Lyman continuum emission at z >~ 3: implication on the ionizing radiation evolution

    NASA Astrophysics Data System (ADS)

    Vanzella, E.; Siana, B.; Cristiani, S.; Nonino, M.

    2010-06-01

    We investigate the possibility of contamination by lower redshift interlopers in the measure of the ionizing radiation escaping from high-redshift galaxies. Taking advantage of the new ultradeep Very Large Telescope/Visible Multiobject Spectrograph U-band number counts in the Great Observatories Origins Deep Survey (GOODS)-South field, we calculate the expected probability of contamination by low-redshift interlopers as a function of the U magnitude and the image spatial resolution (point spread function). Assuming that ground-based imaging or spectroscopy cannot resolve objects lying within a 0.5-arcsec radius of each other, then each z >~ 3 galaxy has a 2.1 and 3.2 per cent chance of foreground contamination, adopting surface density U-band number counts down to 27.5 and 28.5, respectively. Those probabilities increase to 8.5 and 12.6 per cent, assuming 1.0-arcsec radius. If applied to the estimates reported in the literature at redshift ~3 for which a Lyman continuum has been observed directly, the probability that at least one-third of them are affected by foreground contamination is larger than 50 per cent. From a Monte Carlo simulation, we estimate the median integrated contribution of foreground sources to the Lyman continuum flux (f900). Current estimations from stacked data are >2σ of the median integrated pollution by foreground sources. If the correction to the observed f900 flux is applied, the relative escape fraction decreases by a factor of ~1.3 and 2, depending on the cases reported in literature. The spatial cross-correlation between the U-band ultradeep catalogue and a sample of galaxies at z >~ 3.4 in the GOODS-South field produces a number of U-band detected systems fully consistent with the expected superposition statistics. Indeed, each of them shows the presence of at least one offset contaminant in the Advanced Camera for Surveys images. An exemplary case of a foreground contamination in the Hubble Ultra Deep Field at redshift 3.797 by a

  4. Evidence for Black Hole Growth in Local Analogs to Lyman Break Galaxies

    NASA Technical Reports Server (NTRS)

    Jia, Jianjun; Ptak, Andrew; Heckman, Timothy M.; Overzier, Roderik A.; Hornschemeier, Ann; LaMassa, Stephanie M.

    2011-01-01

    We have used XMM-Newton to observe six Lyman break analogs (LBAs): members of the rare population of local galaxies that have properties that are very similar to distant Lyman break galaxies. Our six targets were specifically selected because they have optical emission-line properties that are intermediate between starbursts and Type 2 (obscured) active galactic nuclei (AGNs). Our new X-ray data provide an important diagnostic of the presence of an AGN. We find X-ray luminosities of order 10(sup 42) erg per second and ratios of X-ray to far-IR lummositles that are higher than values in pure starburst galaxies by factors ranging from approximately 3 to 30. This strongly suggests the presence of an AGN in at least some of the galaxies. The ratios of the luminosities of the hard (2-10 keV) X-ray to [O III] emission line are low by about an order of magnitude compared with Type 1 AGN, but are consistent with the broad range seen in Type 2 AGN. Either the AGN hard X-rays are significantly obscured or the [O III] emission is dominated by the starburst. We searched for an iron emission line at approximately 6.4 ke V, which is a key feature of obscured AGNs, but only detected emission at the approximately 2sigma level. Finally, we find that the ratios of the mid-infrared (24 micrometer) continuum to [O III]lambda 5007 luminosities in these LBAs are higher than the values for Type 2 AGN by an average of 0.8 dex. Combining all these clues, we conclude that an AGN is likely to be present, but that the bolometric luminosity is produced primarily by an intense starburst. If these black holes are radiating at the Eddington limit, their masses would lie in the range of 10(sup 5) - 10(sup 6) solar mass. These objects may offer ideal local laboratories to investigate the processes by which black holes grew in the early universe.

  5. Exploring the Overabundance of ULXs in Metal- and Dust-Poor Local Lyman Break Analogs

    NASA Technical Reports Server (NTRS)

    Basu-Zych, Antara R.; Lehmer, Bret; Fragos, Tassos; Hornschemeier, Ann; Yukita, Mihoko; Zezas, Andreas; Ptak, Andy

    2016-01-01

    We have studied high-mass X-ray binary (HMXB) populations within two low-metallicity, starburst galaxies, Haro 11 and VV 114. These galaxies serve as analogs to high-redshift (z greater than 2) Lyman break galaxies and, within the larger sample of Lyman break analogs (LBAs), they are sufficiently nearby (less than 87 Mpc) to be spatially resolved by Chandra. Previous studies of the X-ray emission in LBAs have found that the 2-10 keV luminosity per star formation rate (SFR) in these galaxies is elevated, potentially because of their low metallicities (12 + log[O/H] = 8.3-8.4). Theoretically, the progenitors of XRBs forming in lower metallicity environments lose less mass from stellar winds over their lifetimes, producing more massive compact objects (i.e., neutron stars and black holes), and thus resulting in more numerous and luminous HMXBs per SFR. In this paper, we have performed an in-depth study of the only two LBAs that have spatially resolved 2-10 keV emission with Chandra to present the bright end of the X-ray luminosity distribution of HMXBs (L(sub X) approximately greater than 10(exp 39) erg s(exp -1); ultraluminous X-ray sources, ULXs) in these low-metallicity galaxies, based on eight detected ULXs. Compared with the star-forming galaxy X-ray luminosity function (XLF) presented by Mineo et al., Haro 11 and VV 114 host approximately equal to 4 times more L(sub X) greater than 10(exp 40) erg s(exp -1) sources than expected given their SFRs. We simulate the effects of source blending from crowded lower-luminosity HMXBs using the star-forming galaxy XLF and then vary the XLF normalizations and bright-end slopes until we reproduce the observed point source luminosity distributions. We find that these LBAs have a shallower bright-end slope (gamma(sub 2) = 1.90) than the standard XLF (gamma(sub 2) 2.73). If we conservatively assume that the brightest X-ray source from each galaxy is powered by an accreting supermassive black hole rather than an HMXB and

  6. Exploring the Overabundance of ULXs in Metal- and Dust-poor Local Lyman Break Analogs

    NASA Astrophysics Data System (ADS)

    Basu-Zych, Antara R.; Lehmer, Bret; Fragos, Tassos; Hornschemeier, Ann; Yukita, Mihoko; Zezas, Andreas; Ptak, Andy

    2016-02-01

    We have studied high-mass X-ray binary (HMXB) populations within two low-metallicity, starburst galaxies, Haro 11 and VV 114. These galaxies serve as analogs to high-redshift (z\\gt 2) Lyman break galaxies and, within the larger sample of Lyman break analogs (LBAs), they are sufficiently nearby (<87 Mpc) to be spatially resolved by Chandra. Previous studies of the X-ray emission in LBAs have found that the 2-10 keV luminosity per star formation rate (SFR) in these galaxies is elevated, potentially because of their low metallicities (12+{log}[{{O}}/{{H}}]=8.3{--}8.4). Theoretically, the progenitors of XRBs forming in lower metallicity environments lose less mass from stellar winds over their lifetimes, producing more massive compact objects (i.e., neutron stars and black holes), and thus resulting in more numerous and luminous HMXBs per SFR. In this paper, we have performed an in-depth study of the only two LBAs that have spatially resolved 2-10 keV emission with Chandra to present the bright end of the X-ray luminosity distribution of HMXBs ({L}{{X}} ≳ 1039 erg s-1 ultraluminous X-ray sources, ULXs) in these low-metallicity galaxies, based on eight detected ULXs. Compared with the star-forming galaxy X-ray luminosity function (XLF) presented by Mineo et al., Haro 11 and VV 114 host ≈ 4 times more {L}{{X}} \\gt {10}40 erg s-1 sources than expected given their SFRs. We simulate the effects of source blending from crowded lower-luminosity HMXBs using the star-forming galaxy XLF and then vary the XLF normalizations and bright-end slopes until we reproduce the observed point source luminosity distributions. We find that these LBAs have a shallower bright-end slope ({γ }2=1.90) than the standard XLF ({γ }2=2.73). If we conservatively assume that the brightest X-ray source from each galaxy is powered by an accreting supermassive black hole rather than an HMXB and eliminate these sources from consideration, the luminosity distribution becomes poorly constrained but

  7. The Lyman α forest power spectrum from the XQ-100 Legacy Survey

    NASA Astrophysics Data System (ADS)

    Iršič, Vid; Viel, Matteo; Berg, Trystyn A. M.; D'Odorico, Valentina; Haehnelt, Martin G.; Cristiani, Stefano; Cupani, Guido; Kim, Tae-Sun; López, Sebastian; Ellison, Sara; Becker, George D.; Christensen, Lise; Denney, Kelly D.; Worseck, Gábor; Bolton, James S.

    2017-04-01

    We present the Lyman α flux power spectrum measurements of the XQ-100 sample of quasar spectra obtained in the context of the European Southern Observatory Large Programme 'Quasars and their absorption lines: a legacy survey of the high redshift universe with VLT/XSHOOTER'. Using 100 quasar spectra with medium resolution and signal-to-noise ratio, we measure the power spectrum over a range of redshifts z = 3-4.2 and over a range of scales k = 0.003-0.06 km-1 s. The results agree well with the measurements of the one-dimensional power spectrum found in the literature. The data analysis used in this paper is based on the Fourier transform and has been tested on synthetic data. Systematic and statistical uncertainties of our measurements are estimated, with a total error (statistical and systematic) comparable to the one of the BOSS data in the overlapping range of scales, and smaller by more than 50 per cent for higher redshift bins (z > 3.6) and small scales (k > 0.01 km-1 s). The XQ-100 data set has the unique feature of having signal-to-noise ratios and resolution intermediate between the two data sets that are typically used to perform cosmological studies, i.e. BOSS and high-resolution spectra (e.g. UVES/VLT or HIRES). More importantly, the measured flux power spectra span the high-redshift regime that is usually more constraining for structure formation models.

  8. Statistical properties of damped Lyman-alpha systems from Sloan Digital Sky Survey DR12

    NASA Astrophysics Data System (ADS)

    Bird, Simeon; Garnett, Roman; Ho, Shirley

    2017-04-01

    We present new estimates for the statistical properties of damped Lyman-α absorbers (DLAs). We compute the column density distribution function at z > 2, the line density, dN/dX, and the neutral hydrogen density, ΩDLA. Our estimates are derived from the DLA catalogue of Garnett et al. (2016), which uses the Sloan Digital Sky Survey III Data Release 12 (SDSS-III DR12) quasar spectroscopic survey. This catalogue provides a probability that a given spectrum contains a DLA. It allows us to use even the noisiest data without biasing our results and thus substantially increases our sample size. We measure a non-zero column density distribution function at 95 per cent confidence for all column densities N_H I< 5× 10^{22} cm-2. We make the first measurements from SDSS of dN/dX and ΩDLA at z > 4. We show that our results are insensitive to the signal-to-noise ratio of the spectra, but that there is a residual dependence on quasar redshift for z < 2.5, which may be due to remaining systematics in our analysis.

  9. Characterizing the Lyman-alpha forest flux probability distribution function using Legendre polynomials

    NASA Astrophysics Data System (ADS)

    Cieplak, Agnieszka; Slosar, Anze

    2017-01-01

    The Lyman-alpha forest has become a powerful cosmological probe of the underlying matter distribution at high redshift. It is a highly non-linear field with much information present beyond the two-point statistics of the power spectrum. The flux probability distribution function (PDF) in particular has been used as a successful probe of small-scale physics. In addition to the cosmological evolution however, it is also sensitive to pixel noise, spectrum resolution, and continuum fitting, all of which lead to possible biased estimators. Here we argue that measuring coefficients of the Legendre polynomial expansion of the PDF offers several advantages over the binned PDF as is commonly done. Since the n-th coefficient can be expressed as a linear combination of the first n moments of the field, this allows for the coefficients to be measured in the presence of noise and allows for a clear route towards marginalization over the mean flux. In addition, we use hydrodynamic cosmological simulations to demonstrate that in the presence of noise, a finite number of these coefficients are well measured with a very sharp transition into noise dominance. This compresses the information into a finite small number of well-measured quantities.

  10. Eight per cent leakage of Lyman continuum photons from a compact, star-forming dwarf galaxy.

    PubMed

    Izotov, Y I; Orlitová, I; Schaerer, D; Thuan, T X; Verhamme, A; Guseva, N G; Worseck, G

    2016-01-14

    One of the key questions in observational cosmology is the identification of the sources responsible for ionization of the Universe after the cosmic 'Dark Ages', when the baryonic matter was neutral. The currently identified distant galaxies are insufficient to fully reionize the Universe by redshift z ≈ 6 (refs 1-3), but low-mass, star-forming galaxies are thought to be responsible for the bulk of the ionizing radiation. As direct observations at high redshift are difficult for a variety of reasons, one solution is to identify local proxies of this galaxy population. Starburst galaxies at low redshifts, however, generally are opaque to Lyman continuum photons. Small escape fractions of about 1 to 3 per cent, insufficient to ionize much surrounding gas, have been detected only in three low-redshift galaxies. Here we report far-ultraviolet observations of the nearby low-mass star-forming galaxy J0925+1403. The galaxy is leaking ionizing radiation with an escape fraction of about 8 per cent. The total number of photons emitted during the starburst phase is sufficient to ionize intergalactic medium material that is about 40 times as massive as the stellar mass of the galaxy.

  11. THE NATURE OF DAMPED LYMAN-α AND Mg II ABSORBERS EXPLORED THROUGH THEIR DUST CONTENTS

    SciTech Connect

    Fukugita, Masataka; Ménard, Brice

    2015-02-01

    We estimate the abundance of dust in damped Lyman-α absorbers (DLAs) by statistically measuring the excess reddening they induce on their background quasars. We detect systematic reddening behind DLAs consistent with the SMC-type reddening curve and inconsistent with the Milky Way type. We find that the derived dust-to-gas ratio is, on average, inversely proportional to the column density of neutral hydrogen, implying that the amount of dust is constant, regardless of the column density of hydrogen. It means that the average metallicity is inversely proportional to the column density of hydrogen, unless the average dust-to-metal ratio varies with the hydrogen column density. This indicates that the prime origin of metals seen in DLAs is not by in situ star formation, with which Z∼N{sub H} {sub I}{sup +0.4} is expected from the empirical star formation law, contrary to our observation. We interpret the metals observed in absorbers to be deposited dominantly from nearby galaxies by galactic winds ubiquitous in intergalactic space. When extrapolating the relation between dust-to-gas ratio and H I column density to lower column density, we find a value that is consistent with what is observed for Mg II absorbers.

  12. The Temporal Behaviour of Lyman-alpha During Solar Flares Using SDO/EVE

    NASA Astrophysics Data System (ADS)

    Milligan, Ryan

    2015-04-01

    The Lyα line of hydrogen at 1216Å is the strongest emission line in the solar spectrum. It is formed in the mid-to-upper chromosphere and is a primary driver of changes in terrestrial ionospheric density. It has also recently been shown to dominate the radiative losses during an X-class solar flare (Milligan et al. 2014). Despite the diagnostic potential of Lyα there are relatively few papers in the literature that discuss changes in Lyα emission during solar flares. The MEGS-P broadband (100Å) diode on SDO/EVE measures full-disk Lyα emission at 10s cadence making it ideal for studying such variations. Although formed in the chromosphere, the temporal variations in Lyα appear more gradual in nature, with rise times of tens of minutes, compared to just a few minutes in other chromospheric features, such as Hα, He II, Lyman continuum, C III, etc. In fact, in many large events, emission detected by MEGS-P appears to obey the Neupert Effect; i.e. the time derivate of Lyα closely matches that of impulsive chromospheric emission. Here I will discuss a number of conditions, both solar and instrumental, that may explain why this relationship seems to exist. I shall also compare MEGS-P observations with spectrally and temporally resolved Lyα measurements from SORCE/SOLSTICE.

  13. Non-LTE effects on the strength of the Lyman edge in quasar accretion disks

    NASA Technical Reports Server (NTRS)

    Stoerzer, H.; Hauschildt, P. H.; Allard, F.

    1994-01-01

    We have calculated UV/EUV (300 A which is less than or equal to lambda which is less than or equal to 1500 A) continuous energy distributions of accretion disks in the centers of active galactic nuclei (AGNs) for disk luminosities in the range 0.1 L(sub Edd) less than or equal to L(sub acc) less than 1.0 L(sub Edd) and central masses ranging from 10(exp 8) solar mass to 10(exp 9) solar mass. The vertical gas pressure structure of the disk and the disk height are obtained analytically; the temperature stratification and the resulting continuum radiation fields are calculated numerically. We have included non-Local Thermodynamic Equilibrium (LTE) effects of both the ionization equilibrium and the level populations of hydrogen and helium. We show that these non-LTE effects reduce the strength of the Lyman edge when comapred to the LTE case. In non-LTE we find that the edge can be weakly in emission or absorption for disks seen face-on, depending on the disk parameters.

  14. The Lyman-α Solar Telescope (LST) for the ASO-S mission

    NASA Astrophysics Data System (ADS)

    Li, Hui

    The Lyman-α (Lyα) Solar Telescope (LST) is one of the payloads for the proposed Space-Borne Advanced Solar Observatory (ASO-S). LST consists of a Solar Disk Imager (SDI) with a field-of-view (FOV) of 1.2 R⊙ (R⊙ = solar radius), a Solar Corona Imager (SCI) with an FOV of 1.1 - 2.5 R⊙, and a full-disk White-light Solar Telescope (WST) with the same FOV as the SDI, which also serves as the guiding telescope. The SCI is designed to work in the Lyα (121.6 nm) waveband and white-light (for polarization brightness observation), while the SDI will work in the Lyα waveband only. The WST works in both visible (for guide) and ultraviolet (for science) broadband. The LST will observe the Sun from disk-center up to 2.5 R⊙ for both solar flares and coronal mass ejections with high tempo-spatial resolution

  15. Study of performance loss of Lyman alpha filters due to chemical contamination

    NASA Astrophysics Data System (ADS)

    Faye, Delphine; Zhang, Xueyan; Etcheto, Pierre; Auchère, Frédéric

    2017-05-01

    Observations in the UV and EUV allow many diagnostics of the outer layers of the stars and the Sun so that more and more space telescopes are developed to operate in this fundamental spectral range. However, absorption by residual contaminants coming from polymers outgassing causes critical effects such as loss of signal, spectral shifts, stray light… Thus, a cleanliness and contamination control plan has to be defined to mitigate the risk of damage of sensitive surfaces. In order to specify acceptable cleanliness levels, it is paramount to improve our knowledge and understanding of contamination effects, especially in the UV/EUV range. Therefore, an experimental study has been carried out in collaboration between CNES and IAS, in the frame of the development of the Extreme UV Imager suite for the ESA Solar Orbiter mission; this instrument consists of two High Resolution Imagers and one Full Sun Imager designed for narrow pass-band EUV imaging of the solar corona, and thus very sensitive to contamination. Here, we describe recent results of performance loss measured on representative optical samples. Six narrow pass-band filters, with a multilayer coating designed to select the solar Lyman Alpha emission ray, were contaminated with different amounts of typical chemical species. The transmittance spectra were measured between 100 and 200 nm under high vacuum on the SOLEIL synchrotron beam line. They were compared before and after contamination, and also after a long exposure of the contaminated area to EUV-visible radiations.

  16. Optimizing BAO measurements with non-linear transformations of the Lyman-α forest

    SciTech Connect

    Wang, Xinkang; Font-Ribera, Andreu; Seljak, Uroš E-mail: afont@lbl.gov

    2015-04-01

    We explore the effect of applying a non-linear transformation to the Lyman-α forest transmitted flux F=e{sup −τ} and the ability of analytic models to predict the resulting clustering amplitude. Both the large-scale bias of the transformed field (signal) and the amplitude of small scale fluctuations (noise) can be arbitrarily modified, but we were unable to find a transformation that increases significantly the signal-to-noise ratio on large scales using Taylor expansion up to the third order. In particular, however, we achieve a 33% improvement in signal to noise for Gaussianized field in transverse direction. On the other hand, we explore an analytic model for the large-scale biasing of the Lyα forest, and present an extension of this model to describe the biasing of the transformed fields. Using hydrodynamic simulations we show that the model works best to describe the biasing with respect to velocity gradients, but is less successful in predicting the biasing with respect to large-scale density fluctuations, especially for very nonlinear transformations.

  17. LYMAN BREAK GALAXIES AT z approx 5: REST-FRAME UV SPECTRA. III

    SciTech Connect

    Kajino, Hiroki; Ohta, Kouji; Yabe, Kiyoto; Yuma, Suraphong; Iwata, Ikuru; Akiyama, Masayuki; Tamura, Naoyuki; Aoki, Kentaro; Sawicki, Marcin

    2009-10-10

    We present results of optical spectroscopic observations of candidates of Lyman break galaxies (LBGs) at z approx 5 in the region, including the GOODS-N and the J0053+1234 regions by using Gemini Multi-Object Spectrograph North and South, respectively. Among 25 candidates, five objects are identified to be at z approx 5 (two of them were already identified by an earlier study) and one object very close to the color-selection window turned out to be a foreground galaxy. With this spectroscopically identified sample and those from previous studies, we derived the lower limits on the number density of bright (M{sub UV} < -22.0 mag) LBGs at z approx 5. These lower limits are comparable to or slightly smaller than the number densities of UV luminosity functions (UVLFs) that show the smaller number density among z approx 5 UVLFs in literature. However, by considering that there remain many LBG candidates without spectroscopic observations, the number density of bright LBGs is expected to increase by a factor of two or more. The evidence for the deficiency of UV luminous LBGs with large Lyalpha equivalent widths was reinforced. We discuss possible causes for the deficiency and prefer the interpretation of dust absorption.

  18. SPECTROSCOPIC CONFIRMATION OF FAINT LYMAN BREAK GALAXIES NEAR REDSHIFT FIVE IN THE HUBBLE ULTRA DEEP FIELD

    SciTech Connect

    Rhoads, James E.; Malhotra, Sangeeta; Cohen, Seth; Grogin, Norman; Hathi, Nimish; Ryan, Russell; Straughn, Amber; Windhorst, Rogier A. Pirzkal, Norbert; Xu Chun; Koekemoer, Anton; Panagia, Nino; Dickinson, Mark; Ferreras, Ignacio; Gronwall, Caryl; Kuemmel, Martin; Walsh, Jeremy; Meurer, Gerhardt; Pasquali, Anna; Yan, H.-J.

    2009-05-20

    We present the faintest spectroscopically confirmed sample of z {approx} 5 Lyman break galaxies (LBGs) to date. The sample is based on slitless grism spectra of the Hubble Ultra Deep Field region from the Grism ACS Program for Extragalactic Science (GRAPES) and Probing Evolution and Reionization Spectroscopically (PEARS) projects, using the G800L grism on the Hubble Space Telescope Advanced Camera for Surveys. We report here confirmations of 39 galaxies, preselected as candidate LBGs using photometric selection criteria. We compare a 'traditional' V-dropout selection, based on the work of Giavalisco et al., to a more liberal one (with V - i > 0.9), and find that the traditional criteria are about 64% complete and 81% reliable. We also study the Ly{alpha} emission properties of our sample. We find that Ly{alpha} emission is detected in {approx}1/4 of the sample, and that the liberal V-dropout color selection includes {approx}55% of previously published line-selected Ly{alpha} sources. Finally, we examine our stacked two-dimensional spectra. We demonstrate that strong, spatially extended ({approx}1'') Ly{alpha} emission is not a generic property of these LBGs, but that a modest extension of the Ly{alpha} photosphere (compared to the starlight) may be present in those galaxies with prominent Ly{alpha} emission.

  19. Direct Method Gas-phase Oxygen Abundances of Four Lyman Break Analogs

    NASA Astrophysics Data System (ADS)

    Brown, Jonathan S.; Croxall, Kevin V.; Pogge, Richard W.

    2014-09-01

    We measure the gas-phase oxygen abundances in four Lyman break analogs using auroral emission lines to derive direct abundances. The direct method oxygen abundances of these objects are generally consistent with the empirically derived strong-line method values, confirming that these objects are low oxygen abundance outliers from the mass-metallicity (MZ) relation defined by star forming Sloan Digital Sky Survey galaxies. We find slightly anomalous excitation conditions (Wolf-Rayet features) that could potentially bias the empirical estimates toward high values if caution is not exercised in the selection of the strong-line calibration. The high rate of star formation and low oxygen abundance of these objects is consistent with the predictions of the fundamental metallicity relation, in which the infall of relatively unenriched gas simultaneously triggers an episode of star formation and dilutes the interstellar medium of the host galaxy. Based on data acquired using the Large Binocular Telescope (LBT). The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are the University of Arizona on behalf of the Arizona university system; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellschaft, Germany, representing the Max-Planck Society, the Astrophysical Institute Potsdam, and Heidelberg University; the Ohio State University, and the Research Corporation, on behalf of the University of Notre Dame, University of Minnesota, and University of Virginia.

  20. Non-parametric 3D map of the intergalactic medium using the Lyman-alpha forest

    NASA Astrophysics Data System (ADS)

    Cisewski, Jessi; Croft, Rupert A. C.; Freeman, Peter E.; Genovese, Christopher R.; Khandai, Nishikanta; Ozbek, Melih; Wasserman, Larry

    2014-05-01

    Visualizing the high-redshift Universe is difficult due to the dearth of available data; however, the Lyman-alpha forest provides a means to map the intergalactic medium at redshifts not accessible to large galaxy surveys. Large-scale structure surveys, such as the Baryon Oscillation Spectroscopic Survey (BOSS), have collected quasar (QSO) spectra that enable the reconstruction of H I density fluctuations. The data fall on a collection of lines defined by the lines of sight (LOS) of the QSO, and a major issue with producing a 3D reconstruction is determining how to model the regions between the LOS. We present a method that produces a 3D map of this relatively uncharted portion of the Universe by employing local polynomial smoothing, a non-parametric methodology. The performance of the method is analysed on simulated data that mimics the varying number of LOS expected in real data, and then is applied to a sample region selected from BOSS. Evaluation of the reconstruction is assessed by considering various features of the predicted 3D maps including visual comparison of slices, probability density functions (PDFs), counts of local minima and maxima, and standardized correlation functions. This 3D reconstruction allows for an initial investigation of the topology of this portion of the Universe using persistent homology.

  1. Water vapor content in the polar atmosphere measured by Lyman-alpha/OH fluorescence method

    NASA Technical Reports Server (NTRS)

    Iwasaka, Y.; Saitoh, S.; Ono, A.

    1985-01-01

    The water vapor of the polar stratosphere possibly plays an important role in various aeronomical processes; for example, OH radical formation through photodissociation of H2O, formation of water cluster ions, radiative energy transfer in the lower stratosphere, condensation onto particulate matter, and so on. In addition to these, it has been speculated, from the viewpoint of global transport and/or budget of water vapor, that the polar stratosphere functions as an active sink. STANFORD (1973) emphasized the existence of the stratospheric Cist cloud in the polar stratosphere which brought a large loss rate of stratospheric water vapor through a so-called freeze-out of cloud particles from the stratosphere into the troposphere. However, these geophysically interesting problems unfortunately remain to be solved, owing to the lack of measurements on water vapor distribution and its temporal variation in the polar stratosphere. The water vapor content measured at Syowa Station (69.00 deg S, 39.35 deg E), Antarctica using a balloon-borne hygrometer (Lyman - alpha/OH fluorescence type) is discussed.

  2. Central powering of the largest Lyman-α nebula is revealed by polarized radiation.

    PubMed

    Hayes, Matthew; Scarlata, Claudia; Siana, Brian

    2011-08-17

    High-redshift Lyman-α (Lyα) blobs are extended, luminous but rare structures that seem to be associated with the highest peaks in the matter density of the Universe. Their energy output and morphology are similar to those of powerful radio galaxies, but the source of the luminosity is unclear. Some blobs are associated with ultraviolet or infrared bright galaxies, suggesting an extreme starburst event or accretion onto a central black hole. Another possibility is gas that is shock-excited by supernovae. But not all blobs are associated with galaxies, and these ones may instead be heated by gas falling into a dark-matter halo. The polarization of the Lyα emission can in principle distinguish between these options, but a previous attempt to detect this signature returned a null detection. Here we report observations of polarized Lyα from the blob LAB1 (ref. 2). Although the central region shows no measurable polarization, the polarized fraction (P) increases to ∼20 per cent at a radius of 45 kiloparsecs, forming an almost complete polarized ring. The detection of polarized radiation is inconsistent with the in situ production of Lyα photons, and we conclude that they must have been produced in the galaxies hosted within the nebula, and re-scattered by neutral hydrogen.

  3. The Lyman-alpha forest power spectrum from the XQ-100 Legacy Survey

    NASA Astrophysics Data System (ADS)

    Iršič, Vid; Viel, Matteo; Berg, Trystyn A. M.; D'Odorico, Valentina; Haehnelt, Martin G.; Cristiani, Stefano; Cupani, Guido; Kim, Tae-Sun; López, Sebastian; Ellison, Sara; Becker, George D.; Christensen, Lise; Denney, Kelly D.; Worseck, Gábor; Bolton, James S.

    2016-12-01

    We present the Lyman-α flux power spectrum measurements of the XQ-100 sample of quasar spectra obtained in the context of the European Southern Observatory Large Programme "Quasars and their absorption lines: a legacy survey of the high redshift universe with VLT/XSHOOTER". Using 100 quasar spectra with medium resolution and signal-to-noise ratio we measure the power spectrum over a range of redshifts z = 3 - 4.2 and over a range of scales k = 0.003 - 0.06 km-1 s. The results agree well with the measurements of the one-dimensional power spectrum found in the literature. The data analysis used in this paper is based on the Fourier transform and has been tested on synthetic data. Systematic and statistical uncertainties of our measurements are estimated, with a total error (statistical and systematic) comparable to the one of the BOSS data in the overlapping range of scales, and smaller by more than 50% for higher redshift bins (z > 3.6) and small scales (k > 0.01 km-1 s). The XQ-100 data set has the unique feature of having signal-to-noise ratios and resolution intermediate between the two data sets that are typically used to perform cosmological studies, i.e. BOSS and high-resolution spectra (e.g. UVES/VLT or HIRES). More importantly, the measured flux power spectra span the high redshift regime which is usually more constraining for structure formation models.

  4. Pollen dispersal by catapult: Experiments of Lyman J. Briggs on the flower of mountain laurel

    USGS Publications Warehouse

    Nimmo, John R.; Hermann, Paula M.; Kirkham, M.B.; Landa, Edward R.

    2014-01-01

    The flower of Kalmia latifolia L. employs a catapult mechanism that flings its pollen to considerable distances. Physicist Lyman J. Briggs investigated this phenomenon in the 1950s after retiring as longtime director of the National Bureau of Standards, attempting to explain how hydromechanical effects inside the flower’s stamen could make it possible. Briggs’s unfinished manuscript implies that liquid under negative pressure generates stress, which, superimposed on the stress generated from the flower’s growth habit, results in force adequate to propel the pollen as observed. With new data and biophysical understanding to supplement Briggs’s experimental results and research notes, we show that his postulated negative-pressure mechanism did not play the exclusive and crucial role that he credited to it, though his revisited investigation sheds light on various related processes. Important issues concerning the development and reproductive function of Kalmia flowers remain unresolved, highlighting the need for further biophysical advances.

  5. Lyman A. Brewer III (1907-1988): surgeon-scientist, inspirational teacher, and humanist.

    PubMed

    Carter, R

    1998-12-01

    Dr. Lyman Augustus Brewer III, a distinguished, colorful thoracic surgeon and among the first to practice that specialty in the West, died on June 25, 1988, in Los Angeles, California, after a courageous battle with lymphoma. Dr. Brewer was a great humanist, innovative clinical surgeon, charismatic teacher, and surgical leader. In World War II, Lieutenant Colonel Brewer served in the Second Auxiliary Surgical Group in the Mediterranean and European theaters and helped define criteria that became the standard for the management of thoracic war injuries. Out of this experience he authored the classic paper, "The Wet Lung in War Casualties." Dr. Brewer's scientific contributions embraced the broad spectrum of thoracic surgical topics, including treatment of tuberculosis, classification of lung cancer, bronchial stump buttressing using the pericardial fat pad (Brewer fat pad), and management of esophageal perforation. Dr Brewer wrote seven books and more than 100 papers, and served as First Vice President of The American College of Surgeons and as President of the American Association for Thoracic Surgery, The Society of Thoracic Surgeons, and The Pacific Coast Surgical Association.

  6. Non-LTE effects on the strength of the Lyman edge in quasar accretion disks

    NASA Technical Reports Server (NTRS)

    Stoerzer, H.; Hauschildt, P. H.; Allard, F.

    1994-01-01

    We have calculated UV/EUV (300 A which is less than or equal to lambda which is less than or equal to 1500 A) continuous energy distributions of accretion disks in the centers of active galactic nuclei (AGNs) for disk luminosities in the range 0.1 L(sub Edd) less than or equal to L(sub acc) less than 1.0 L(sub Edd) and central masses ranging from 10(exp 8) solar mass to 10(exp 9) solar mass. The vertical gas pressure structure of the disk and the disk height are obtained analytically; the temperature stratification and the resulting continuum radiation fields are calculated numerically. We have included non-Local Thermodynamic Equilibrium (LTE) effects of both the ionization equilibrium and the level populations of hydrogen and helium. We show that these non-LTE effects reduce the strength of the Lyman edge when comapred to the LTE case. In non-LTE we find that the edge can be weakly in emission or absorption for disks seen face-on, depending on the disk parameters.

  7. Morphologies and faint neighbors of z=4.5 Lyman Alpha Emitting Galaxies

    NASA Astrophysics Data System (ADS)

    Malhotra, Sangeeta

    2002-07-01

    We propose to image one ACS field containing four spectroscopically confirmed Ly-alpha emitters at z=4.5 in restframe UV and a narrowband filter containing the Ly-alpha line. These observations will {A} Reveal the morphology of the four spectroscopically confirmed sources. The high equivalent widths of the Ly-alpha line in these four galaxies in particular and this population in general cannot be explained without invoking one or more of: extreme youth of the stellar population, zero metallicity, energetic winds or type II quasars. Comparison of morphologies in the line and continuum would help favor or rule out some of these possibilties. This would also tell us whether the star-formation is uniformly distributed or centrally concentrated or concentrated but in many clumps? Proximity of these galaxies {average projected physical separation of 200 kpc, with one pair 30 kpc apart} also makes interactions likely. {B} Extend the luminosity function of Ly-alpha sources by 2.5 magnitudes due to better spatial resolution of HST and sensitivity of ACS. We will be able to detect sources with line flux of eq 2 * 10^-18 ergcm2s over 11.5 sq-arcmins { 100 sources}. This complements the LALA {Large Area Lyman Alpha} survey which covers 1/3 square-degree to a line sensitivity of eq 2 * 10^- 17. Thus we get a picture of this patch of young universe in two ways: statistics of faint galaxies and morphologies of relatively bright ones.

  8. Physical properties of local star-forming analogues to z ˜ 5 Lyman-break galaxies

    NASA Astrophysics Data System (ADS)

    Greis, Stephanie M. L.; Stanway, Elizabeth R.; Davies, Luke J. M.; Levan, Andrew J.

    2016-07-01

    Intense, compact, star-forming galaxies are rare in the local Universe but ubiquitous at high redshift. We interpret the 0.1-22 μm spectral energy distributions of a sample of 180 galaxies at 0.05 < z < 0.25 selected for extremely high surface densities of inferred star formation in the ultraviolet. By comparison with well-established stellar population synthesis models, we find that our sample comprises young (˜60-400 Myr), moderate mass (˜6 × 109 M⊙) star-forming galaxies with little dust extinction (mean stellar continuum extinction Econt(B - V) ˜ 0.1) and find star formation rates of a few tens of solar masses per year. We use our inferred masses to determine a mean specific star formation rate for this sample of ˜10-9 yr-1, and compare this to the specific star formation rates in distant Lyman-break galaxies (LBGs), and in other low-redshift populations. We conclude that our sample's characteristics overlap significantly with those of the z ˜ 5 LBG population, making ours the first local analogue population well tuned to match those high-redshift galaxies. We consider implications for the origin and evolution of early galaxies.

  9. Lyman-α Emission from an Infant Black Hole in the Early Universe

    DOE PAGES

    Wiggins, Brandon Kerry; Smidt, Joseph Michael; Johnson, Jarrett L.

    2016-01-01

    The COSMOS survey recently discovered an exotic young galaxy, COSMOS Redshift 7 (CR7), in the early universe (1 billion years after the Big Bang), which is devoid of evidence of elements heavier than hydrogen and helium. Whereas some believe this might be the first galaxy discovered with stars made only from these elements, others think CR7 may be powered by a newborn supermassive black hole. In this paper, we summarize for a general academic audience our efforts to model the creation of this galaxy through cosmological simulations. These state-of-the-art calculations include primordial chemistry and cooling and the interaction of x-raysmore » from the black hole with surrounding gas. We simulate the process of light escaping this object with Monte Carlo Lyman-α transfer and compare our calculations with observations of CR7. Our work demonstrates the viability of the black hole interpretation for this intriguing object in the early universe.« less

  10. Spectroscopic Confirmation of Faint Lyman Break Galaxies Near Redshift Five in the Hubble Ultra Deep Field

    NASA Astrophysics Data System (ADS)

    Rhoads, James E.; Malhotra, Sangeeta; Pirzkal, Norbert; Dickinson, Mark; Cohen, Seth; Grogin, Norman; Hathi, Nimish; Xu, Chun; Ferreras, Ignacio; Gronwall, Caryl; Koekemoer, Anton; Kümmel, Martin; Meurer, Gerhardt; Panagia, Nino; Pasquali, Anna; Ryan, Russell; Straughn, Amber; Walsh, Jeremy; Windhorst, Rogier A.; Yan, Hao-Jing

    2009-05-01

    We present the faintest spectroscopically confirmed sample of z ~ 5 Lyman break galaxies (LBGs) to date. The sample is based on slitless grism spectra of the Hubble Ultra Deep Field region from the Grism ACS Program for Extragalactic Science (GRAPES) and Probing Evolution and Reionization Spectroscopically (PEARS) projects, using the G800L grism on the Hubble Space Telescope Advanced Camera for Surveys. We report here confirmations of 39 galaxies, preselected as candidate LBGs using photometric selection criteria. We compare a "traditional" V-dropout selection, based on the work of Giavalisco et al., to a more liberal one (with V - i > 0.9), and find that the traditional criteria are about 64% complete and 81% reliable. We also study the Lyα emission properties of our sample. We find that Lyα emission is detected in ~1/4 of the sample, and that the liberal V-dropout color selection includes ~55% of previously published line-selected Lyα sources. Finally, we examine our stacked two-dimensional spectra. We demonstrate that strong, spatially extended (~1'') Lyα emission is not a generic property of these LBGs, but that a modest extension of the Lyα photosphere (compared to the starlight) may be present in those galaxies with prominent Lyα emission.

  11. Squeezing the window on isocurvature modes with the Lyman-{alpha} forest

    SciTech Connect

    Beltran, Maria; Garcia-Bellido, Juan; Lesgourgues, Julien; Viel, Matteo

    2005-11-15

    Various recent studies proved that cosmological models with a significant contribution from cold dark matter isocurvature perturbations are still compatible with most recent data on cosmic microwave background anisotropies and on the shape of the galaxy power spectrum, provided that one allows for a very blue spectrum of primordial entropy fluctuations (n{sub iso}>2). However, such models predict an excess of matter fluctuations on small scales, typically below 40h{sup -1} Mpc. We show that the proper inclusion of high-resolution high signal-to-noise Lyman-{alpha} forest data excludes most of these models. The upper bound on the isocurvature fraction {alpha}=f{sub iso}{sup 2}/(1+f{sub iso}{sup 2}), defined at the pivot scale k{sub 0}=0.05 Mpc{sup -1}, is pushed down to {alpha}<0.4, while n{sub iso}=1.9{+-}1.0 (95% confidence limits). We also study the bounds on curvaton models characterized by maximal correlation between curvature and isocurvature modes, and a unique spectral tilt for both. We find that f{sub iso}<0.05 (95% C.L.) in that case. For double-inflation models with two massive inflatons coupled only gravitationally, the mass ratio should obey R<3 (95% C.L.)

  12. From Mirrors to Windows: Lyman-alpha Radiative Transfer in a Very Clumpy Medium

    NASA Astrophysics Data System (ADS)

    Gronke, Max; Dijkstra, Mark; McCourt, Michael; Oh, S. Peng

    2016-12-01

    Lyman-alpha (Lyα) is the strongest emission line in the universe and is frequently used to detect and study the most distant galaxies. Because Lyα is a resonant line, photons typically scatter prior to escaping; this scattering process complicates the interpretation of Lyα spectra, but also encodes a wealth of information about the structure and kinematics of neutral gas in the Galaxy. Modeling the Lyα line therefore allows us to study tiny-scale features of the gas. Curiously, observed Lyα spectra can be modeled successfully with very simple, homogeneous geometries (such as an expanding, spherical shell), whereas more realistic, multiphase geometries often fail to reproduce the observed spectra. This seems paradoxical since the gas in galaxies is known to be multiphase. In this Letter, we show that spectra emerging from clumpy geometries with a large number (≳ 10 for a clump column density of {N}{{H}{{I}},{cl}}∼ {10}17 {{cm}}-2) of clouds along the line of sight converge to the predictions from simplified, homogeneous models. We suggest that this resolves the apparent discrepancy and may provide a way to study the gas structure in galaxies on scales far smaller than can be probed in either cosmological simulations or direct (i.e., spatially resolved) observations.

  13. Performance characteristics of the imaging MAMA detector systems for SOHO, STIS, and FUSE/Lyman

    NASA Technical Reports Server (NTRS)

    Timothy, J. G.

    1991-01-01

    Imaging Extreme Ultraviolet (EUV) Multi-Anode Microchannel Array (MAMA) detector systems with formats of 360 x 1024 pixels and pixel dimensions of 25 x 25 sq microns are being fabricated and tested for flight in two instruments on the ESA/NASA Solar and Heliospheric Observatory (SOHO). In addition, very-large-format (1024 x 1024)- and (2048 x 2048)-pixel Far Ultraviolet (FUV) and EUV MAMA detectors with pixel dimensions of 25 x 25 sq microns are being fabricated and tested for use in the NASA Goddard Space Flight Center's Hubble Space Telescope Imaging Spectrograph (STIS), a second-generation instrument scheduled for in-orbit installation in 1997. Finally, FUV MAMA detectors with formats of 224 x 960 pixels and pixel dimensions of 14 x 14 sq microns are being evaluated as prototypes of the detector for the prime FUV spectrograph of the Far Ultraviolet Spectroscopic Explorer (FUSE/Lyman) mission. The configurations and performance characteristics of the different detector systems are described, and the plans for further development of the Advanced Technology MAMA detector system discussed.

  14. Hydrogen Balmer alpha intensity distributions and line profiles from multiple scattering theory using realistic geocoronal models

    NASA Technical Reports Server (NTRS)

    Anderson, D. E., Jr.; Meier, R. R.; Hodges, R. R., Jr.; Tinsley, B. A.

    1987-01-01

    The H Balmer alpha nightglow is investigated by using Monte Carlo models of asymmetric geocoronal atomic hydrogen distributions as input to a radiative transfer model of solar Lyman-beta radiation in the thermosphere and atmosphere. It is shown that it is essential to include multiple scattering of Lyman-beta radiation in the interpretation of Balmer alpha airglow data. Observations of diurnal variation in the Balmer alpha airglow showing slightly greater intensities in the morning relative to evening are consistent with theory. No evidence is found for anything other than a single sinusoidal diurnal variation of exobase density. Dramatic changes in effective temperature derived from the observed Balmer alpha line profiles are expected on the basis of changing illumination conditions in the thermosphere and exosphere as different regions of the sky are scanned.

  15. Hydrogen Balmer alpha intensity distributions and line profiles from multiple scattering theory using realistic geocoronal models

    NASA Technical Reports Server (NTRS)

    Anderson, D. E., Jr.; Meier, R. R.; Hodges, R. R., Jr.; Tinsley, B. A.

    1987-01-01

    The H Balmer alpha nightglow is investigated by using Monte Carlo models of asymmetric geocoronal atomic hydrogen distributions as input to a radiative transfer model of solar Lyman-beta radiation in the thermosphere and atmosphere. It is shown that it is essential to include multiple scattering of Lyman-beta radiation in the interpretation of Balmer alpha airglow data. Observations of diurnal variation in the Balmer alpha airglow showing slightly greater intensities in the morning relative to evening are consistent with theory. No evidence is found for anything other than a single sinusoidal diurnal variation of exobase density. Dramatic changes in effective temperature derived from the observed Balmer alpha line profiles are expected on the basis of changing illumination conditions in the thermosphere and exosphere as different regions of the sky are scanned.

  16. Lyman-Break Galaxies at z>~4 and the Evolution of the Ultraviolet Luminosity Density at High Redshift

    NASA Astrophysics Data System (ADS)

    Steidel, Charles C.; Adelberger, Kurt L.; Giavalisco, Mauro; Dickinson, Mark; Pettini, Max

    1999-07-01

    We present initial results of a survey for star-forming galaxies in the redshift range 3.8<~z<~4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg2 to an apparent magnitude of IAB=25.0. Spectroscopic redshifts in the range 3.61<=z<=4.81 have been obtained for 48 of these galaxies; their median redshift is =4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7<~z<~3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z~4 and z~3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [ρUV(z=3)/ρUV(z=4)=1.1+/-0.3]. We see no evidence at these bright magnitudes for the steep decline in the star formation density inferred from fainter photometric Lyman-break galaxies in the Hubble deep field (HDF). The HDF provides the only existing data on Lyman-break galaxy number densities at fainter magnitudes. We have reanalyzed the z~3 and z~4 Lyman-break galaxies in the HDF using our improved knowledge of the spectral energy distributions of these galaxies, and we find, like previous authors, that faint Lyman-break galaxies appear to be rarer at z~4 than z~3. This might signal a large change in the faint-end slope of the Lyman-break galaxy luminosity function between redshifts z~3 and z~4, or, more likely, be due to significant variance in the number counts within the small volumes probed by the HDF at high redshifts (~160 times smaller than the ground-based surveys discussed here). If the true luminosity density at z~4 is somewhat higher than implied by the HDF, as our ground-based sample suggests, then the emissivity of star formation as a function of redshift would appear essentially constant for all z>1

  17. Measurements of D_A and H at z=2.4 from the SDSS-III/DR11 BOSS Lyman-alpha sample

    NASA Astrophysics Data System (ADS)

    Schlegel, David J.; Delubac, T.; Busca, N. G.; Rich, J.; Bailey, S. J.; Bautista, J.; Front, A.; Kirkby, D.; Le Goff, J.; Pieri, M.; Slosar, A.; Aubourg, E.; Blomqvist, M.; Bolton, A. S.; Borde, A.; Carithers, W.; Croft, R. A.; Dawson, K. S.; Eisenstein, D.; Hamilton, J.; Ho, S.; Hogg, D. W.; Lee, K.; Lundgren, B.; Margala, D.; Miralda-Escudé, J.; Myers, A. D.; Noterdaeme, P.; Palanque-Delabrouille, N.; Paris, I.; Petitjean, P.; Ross, N.; Rossi, G.; Viel, M.; Weinberg, D. H.; White, M.; Yeche, C.; Sloan Digital Sky Survey (SDSS-III) Baryon Oscillation Spectroscopic Survey (BOSS)

    2014-01-01

    We present the most precise measures of the Baryon Acoustic Oscillation (BAO) scale at z=2.4 from the 3-dimensional clustering of the Lyman alpha forest. The Hubble parameter (BAO scale along the line of sight) is measured to 3% precision. The angular diameter distance (perpendicular to the line of sight) is measured to 5% precision. These results make use of the Sloan Digital Sky Survey III (SDSS-III) Data Release 11 (DR11), with 135 000 high-redshift quasar spectra covering 9000 square degrees. This study supersedes the previous measurements of Busca et al. (2013) and Slosar et al. (2013) with a gain of nearly a factor of three in the amount of Lyman alpha spectra data. We also perform a detailed study of the covariance matrix of the Lyman alpha correlation, which is validated with both simulations and subsampling (data-only) techniques.

  18. Lyman Alpha Camera for Io's SO2 atmosphere and Europa's water plumes

    NASA Astrophysics Data System (ADS)

    McEwen, Alfred S.; Sandel, Bill; Schneider, Nick

    2014-05-01

    The Student Lyman-Alpha Mapper (SLAM) was conceived for the Io Volcano Observer (IVO) mission proposal (McEwen et al., 2014) to determine the spatial and temporal variations in Io's SO2 atmosphere by recording the H Ly-α reflection over the disk (Feldman et al., 2000; Feaga et al., 2009). SO2 absorbs at H Ly-α, thereby modulating the brightness of sunlight reflected by the surface, and measures the density of the SO2 atmosphere and its variability with volcanic activity and time of day. Recently, enhancements at the Ly-α wavelength (121.57 nm) were seen near the limb of Europa and interpreted as active water plumes ~200 km high (Roth et al., 2014). We have a preliminary design for a very simple camera to image in a single bandpass at Ly-α, analogous to a simplified version of IMAGE EUV (Sandel et al. 2000). Our goal is at least 50 resolution elements across Io and/or Europa (~75 km/pixel), ~3x better than HST STIS, to be acquired at a range where the radiation noise is below 1E-4 hits/pixel/s. This goal is achieved with a Cassegrain-like telescope with a 10-cm aperture. The wavelength selection is achieved using a simple self-filtering mirror in combination with a solar-blind photocathode. A photon-counting detector based on a sealed image intensifier preserves the poisson statistics of the incoming photon flux. The intensifier window is coated with a solar-blind photocathode material (CsI). The location of each photon event is recorded by a position-sensitive anode based on crossed delay-line or wedge-and-strip technology. The sensitivity is 0.01 counts/pixel/sec/R, sufficient to estimate SO2 column abundances ranging from 1E15 to 1E17 per cm2 in a 5 min (300 sec) exposure. Sensitivity requirements to search for and image Europa plumes may be similar. Io's Ly-α brightness of ~3 kR exceeds the 0.8 kR brightness of Europa's plume reported by Roth et al. (2014), but the plume brightness is a direct measurement rather than inferring column abundance from

  19. Lyman alpha emitting galaxies at high redshift: Direct detection of young galaxies in a young universe

    NASA Astrophysics Data System (ADS)

    Dawson, Steven Arthur

    /DEIMOS follow-up observations to candidates selected in the Large Area Lyman Alpha (LALA) survey. We conclude that if there is evolution in the Lya luminosity function over these epochs, its significance is below the statistical uncertainty of these data. This result supports the conclusion from several smaller samples of high-redshift Lya---emitters that the intergalactic medium remains largely reionized from the local universe out to z [approximate] 6.5. However, it is somewhat at odds with the pronounced drop in the cosmic star formation rate density recently measured between z ~ 3 and z ~ 6 in Lyman-break galaxies, and therefore potentially sheds light on the relationship between the two populations. (Abstract shortened by UMI.)

  20. [O III] Emission and Gas Kinematics in a Lyman-alpha Blob at z ~ 3.1

    NASA Astrophysics Data System (ADS)

    McLinden, Emily M.; Malhotra, Sangeeta; Rhoads, James E.; Hibon, Pascale; Weijmans, Anne-Marie; Tilvi, Vithal

    2013-04-01

    We present spectroscopic measurements of the [O III] emission line from two subregions of strong Lyα emission in a radio-quiet Lyman-alpha blob (LAB). The blob under study is LAB1 at z ~ 3.1, and the [O III] detections are from the two Lyman break galaxies (LBGs) embedded in the blob halo. The [O III] measurements were made with LUCIFER on the 8.4 m Large Binocular Telescope and NIRSPEC on 10 m Keck Telescope. Comparing the redshift of the [O III] measurements to Lyα redshifts from SAURON allows us to take a step toward understanding the kinematics of the gas in the blob. Using both LUCIFER and NIRSPEC we find velocity offsets between the [O III] and Lyα redshifts that are modestly negative or consistent with 0 km s-1 in both subregions studied (ranging from -72 ± 42- + 6 ± 33 km s-1). A negative offset means Lyα is blueshifted with respect to [O III] a positive offset then implies Lyα is redshifted with respect to [O III]. These results may imply that outflows are not primarily responsible for Lyman alpha escape in this LAB, since outflows are generally expected to produce a positive velocity offset. In addition, we present an [O III] line flux upper limit on a third region of LAB1, a region that is unassociated with any underlying galaxy. We find that the [O III] upper limit from the galaxy-unassociated region of the blob is at least 1.4-2.5 times fainter than the [O III] flux from one of the LBG-associated regions and has an [O III] to Lyα ratio measured at least 1.9-3.4 times smaller than the same ratio measured from one of the LBGs.