Science.gov

Sample records for field south ecdfs

  1. The Taiwan ECDFS Near-Infrared Survey: Ultra-deep J and KS Imaging in the Extended Chandra Deep Field-South

    NASA Astrophysics Data System (ADS)

    Hsieh, Bau-Ching; Wang, Wei-Hao; Hsieh, Chih-Chiang; Lin, Lihwai; Yan, Haojing; Lim, Jeremy; Ho, Paul T. P.

    2012-12-01

    We present ultra-deep J and KS imaging observations covering a 30' × 30' area of the Extended Chandra Deep Field-South (ECDFS) carried out by our Taiwan ECDFS Near-Infrared Survey (TENIS). The median 5σ limiting magnitudes for all detected objects in the ECDFS reach 24.5 and 23.9 mag (AB) for J and KS , respectively. In the inner 400 arcmin2 region where the sensitivity is more uniform, objects as faint as 25.6 and 25.0 mag are detected at 5σ. Thus, this is by far the deepest J and KS data sets available for the ECDFS. To combine TENIS with the Spitzer IRAC data for obtaining better spectral energy distributions of high-redshift objects, we developed a novel deconvolution technique (IRACLEAN) to accurately estimate the IRAC fluxes. IRACLEAN can minimize the effect of blending in the IRAC images caused by the large point-spread functions and reduce the confusion noise. We applied IRACLEAN to the images from the Spitzer IRAC/MUSYC Public Legacy in the ECDFS survey (SIMPLE) and generated a J+KS -selected multi-wavelength catalog including the photometry of both the TENIS near-infrared and the SIMPLE IRAC data. We publicly release the data products derived from this work, including the J and KS images and the J+KS -selected multi-wavelength catalog.

  2. THE TAIWAN ECDFS NEAR-INFRARED SURVEY: ULTRA-DEEP J AND K{sub S} IMAGING IN THE EXTENDED CHANDRA DEEP FIELD-SOUTH

    SciTech Connect

    Hsieh, Bau-Ching; Wang, Wei-Hao; Hsieh, Chih-Chiang; Lin, Lihwai; Lim, Jeremy; Ho, Paul T. P.; Yan Haojing

    2012-12-15

    We present ultra-deep J and K{sub S} imaging observations covering a 30' Multiplication-Sign 30' area of the Extended Chandra Deep Field-South (ECDFS) carried out by our Taiwan ECDFS Near-Infrared Survey (TENIS). The median 5{sigma} limiting magnitudes for all detected objects in the ECDFS reach 24.5 and 23.9 mag (AB) for J and K{sub S} , respectively. In the inner 400 arcmin{sup 2} region where the sensitivity is more uniform, objects as faint as 25.6 and 25.0 mag are detected at 5{sigma}. Thus, this is by far the deepest J and K{sub S} data sets available for the ECDFS. To combine TENIS with the Spitzer IRAC data for obtaining better spectral energy distributions of high-redshift objects, we developed a novel deconvolution technique (IRACLEAN) to accurately estimate the IRAC fluxes. IRACLEAN can minimize the effect of blending in the IRAC images caused by the large point-spread functions and reduce the confusion noise. We applied IRACLEAN to the images from the Spitzer IRAC/MUSYC Public Legacy in the ECDFS survey (SIMPLE) and generated a J+K{sub S} -selected multi-wavelength catalog including the photometry of both the TENIS near-infrared and the SIMPLE IRAC data. We publicly release the data products derived from this work, including the J and K{sub S} images and the J+K{sub S} -selected multi-wavelength catalog.

  3. VizieR Online Data Catalog: Ultra-deep catalog of X-ray groups in ECDF-S (Finoguenov+, 2015)

    NASA Astrophysics Data System (ADS)

    Finoguenov, A.; Tanaka, M.; Cooper, M.; Allevato, V.; Cappelluti, N.; Choi, A.; Heymans, C.; Bauer, F. E.; Ziparo, F.; Ranalli, P.; Silverman, J.; Brandt, W. N.; Xue, Y. Q.; Mulchaey, J.; Howes, L.; Schmid, C.; Wilman, D.; Comastri, A.; Hasinger, G.; Mainieri, V.; Luo, B.; Tozzi, P.; Rosati, P.; Capak, P.; Popesso, P.

    2015-06-01

    The ECDF-S area has been a frequent target of X-ray observations with both Chandra and XMM. After the first 1Ms Chandra observation (Giacconi et al., 2002, Cat. J/ApJS/139/369), the area was named the Chandra Deep Field South. The extension of the CDF-S survey to 2Ms (Luo et al., 2008, Cat. J/ApJS/179/19) and later to 4Ms of exposure time (Xue et al., 2011, Cat. J/ApJS/195/10), via a large Director's Discretionary Time project, has now provided our most sensitive 0.5-8keV view of the distant AGNs and galaxies. This paper does not include the 3Ms Chandra observations of the field taken in 2014. For cataloguing the groups, we also include the ECDF-S data (Lehmer et al., 2005, Cat. J/ApJS/161/21), which consist of four Chandra ACIS-I pointings, 250ks each, defining the square shape of the exposure and sensitivity maps. (1 data file).

  4. Ultra-deep catalog of X-ray groups in the Extended Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Finoguenov, A.; Tanaka, M.; Cooper, M.; Allevato, V.; Cappelluti, N.; Choi, A.; Heymans, C.; Bauer, F. E.; Ziparo, F.; Ranalli, P.; Silverman, J.; Brandt, W. N.; Xue, Y. Q.; Mulchaey, J.; Howes, L.; Schmid, C.; Wilman, D.; Comastri, A.; Hasinger, G.; Mainieri, V.; Luo, B.; Tozzi, P.; Rosati, P.; Capak, P.; Popesso, P.

    2015-04-01

    Aims: We present the detection, identification and calibration of extended sources in the deepest X-ray dataset to date, the Extended Chandra Deep Field South (ECDF-S). Methods: Ultra-deep observations of ECDF-S with Chandra and XMM-Newton enable a search for extended X-ray emission down to an unprecedented flux of 2 × 10-16 ergs s-1 cm-2. By using simulations and comparing them with the Chandra and XMM data, we show that it is feasible to probe extended sources of this flux level, which is 10 000 times fainter than the first X-ray group catalogs of the ROSAT all sky survey. Extensive spectroscopic surveys at the VLT and Magellan have been completed, providing spectroscopic identification of galaxy groups to high redshifts. Furthermore, available HST imaging enables a weak-lensing calibration of the group masses. Results: We present the search for the extended emission on spatial scales of 32'' in both Chandra and XMM data, covering 0.3 square degrees and model the extended emission on scales of arcminutes. We present a catalog of 46 spectroscopically identified groups, reaching a redshift of 1.6. We show that the statistical properties of ECDF-S, such as log N - log S and X-ray luminosity function are broadly consistent with LCDM, with the exception that dn/dz/dΩ test reveals that a redshift range of 0.2 < z < 0.5 in ECDF-S is sparsely populated. The lack of nearby structure, however, makes studies of high-redshift groups particularly easier both in X-rays and lensing, due to a lower level of clustered foreground. We present one and two point statistics of the galaxy groups as well as weak-lensing analysis to show that the detected low-luminosity systems are indeed low-mass systems. We verify the applicability of the scaling relations between the X-ray luminosity and the total mass of the group, derived for the COSMOS survey to lower masses and higher redshifts probed by ECDF-S by means of stacked weak lensing and clustering analysis, constraining any possible

  5. VizieR Online Data Catalog: ECDFS sources optical/IR counterparts (Bonzini+, 2013)

    NASA Astrophysics Data System (ADS)

    Bonzini, M.; Padovani, P.; Mainieri, V.; Kellermann, K. I.; Miller, N.; Rosati, P.; Tozzi, P.; Vattakunnel, S.

    2015-10-01

    We consider a sample of 883 radio sources detected at 1.4GHz in a deep Very Large Array (VLA) survey of the Extended Chandra Deep Field-South (E-CDFS) that reaches a best rms sensitivity of 6uJy. We used deep Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS) data. The IRAC data were obtained as part of the Spitzer IRAC/MUSYC Public Legacy Survey in the Extended CDF-South (SIMPLE) survey (Damen et al., 2011ApJ...727....1D, Cat. J/ApJ/727/1). It covers an area of about 1600 arcmin2 centred on the E-CDFS. The typical 5σ flux density limits are 1.1, 1.3, 6.3 and 7.6uJy at 3.6, 4.5, 5.8 and 8.0um, respectively. We also use MIPS 24um data from the Far-Infrared Deep Extragalactic Legacy (FIDEL) survey (Dickinson & FIDEL Team, 2007AAS...211.5216D). The E-CDFS has been mapped in the X-ray band by Chandra. A total of 129 radio sources have a counterpart in the 4 Ms observations of the CDFS presented in Xue et al. (2011ApJS..195...10X, Cat. J/ApJS/195/10) and another 99 in the main E-CDFS catalogue by Lehmer et al. (2005ApJS..161...21L, Cat. J/ApJS/161/21) obtained with shallower (250ks) observations in each of four pointings. The list of the X-ray counterparts of the radio sources is given in Bonzini et al. (2012ApJS..203...15B, Cat. J/ApJS/203/15). (1 data file).

  6. CANDELS/GOODS-S, CDFS, and ECDFS: photometric redshifts for normal and X-ray-detected galaxies

    SciTech Connect

    Hsu, Li-Ting; Salvato, Mara; Nandra, Kirpal; Brusa, Marcella; Bender, Ralf; Buchner, Johannes; Brightman, Murray; Georgakakis, Antonis; Donley, Jennifer L.; Kocevski, Dale D.; Guo, Yicheng; Barro, Guillermo; Faber, Sandra M.; Rangel, Cyprian; Willner, S. P.; Ashby, Matthew L. N.; Budavári, Tamás; Szalay, Alexander S.; Dahlen, Tomas; and others

    2014-11-20

    We present photometric redshifts and associated probability distributions for all detected sources in the Extended Chandra Deep Field South (ECDFS). This work makes use of the most up-to-date data from the Cosmic Assembly Near-IR Deep Legacy Survey (CANDELS) and the Taiwan ECDFS Near-Infrared Survey (TENIS) in addition to other data. We also revisit multi-wavelength counterparts for published X-ray sources from the 4 Ms CDFS and 250 ks ECDFS surveys, finding reliable counterparts for 1207 out of 1259 sources (∼96%). Data used for photometric redshifts include intermediate-band photometry deblended using the TFIT method, which is used for the first time in this work. Photometric redshifts for X-ray source counterparts are based on a new library of active galactic nuclei/galaxy hybrid templates appropriate for the faint X-ray population in the CDFS. Photometric redshift accuracy for normal galaxies is 0.010 and for X-ray sources is 0.014 and outlier fractions are 4% and 5.2%, respectively. The results within the CANDELS coverage area are even better, as demonstrated both by spectroscopic comparison and by galaxy-pair statistics. Intermediate-band photometry, even if shallow, is valuable when combined with deep broadband photometry. For best accuracy, templates must include emission lines.

  7. CANDELS/GOODS-S, CDFS, and ECDFS: Photometric Redshifts for Normal and X-Ray-Detected Galaxies

    NASA Astrophysics Data System (ADS)

    Hsu, Li-Ting; Salvato, Mara; Nandra, Kirpal; Brusa, Marcella; Bender, Ralf; Buchner, Johannes; Donley, Jennifer L.; Kocevski, Dale D.; Guo, Yicheng; Hathi, Nimish P.; Rangel, Cyprian; Willner, S. P.; Brightman, Murray; Georgakakis, Antonis; Budavári, Tamás; Szalay, Alexander S.; Ashby, Matthew L. N.; Barro, Guillermo; Dahlen, Tomas; Faber, Sandra M.; Ferguson, Henry C.; Galametz, Audrey; Grazian, Andrea; Grogin, Norman A.; Huang, Kuang-Han; Koekemoer, Anton M.; Lucas, Ray A.; McGrath, Elizabeth; Mobasher, Bahram; Peth, Michael; Rosario, David J.; Trump, Jonathan R.

    2014-11-01

    We present photometric redshifts and associated probability distributions for all detected sources in the Extended Chandra Deep Field South (ECDFS). This work makes use of the most up-to-date data from the Cosmic Assembly Near-IR Deep Legacy Survey (CANDELS) and the Taiwan ECDFS Near-Infrared Survey (TENIS) in addition to other data. We also revisit multi-wavelength counterparts for published X-ray sources from the 4 Ms CDFS and 250 ks ECDFS surveys, finding reliable counterparts for 1207 out of 1259 sources (~96%). Data used for photometric redshifts include intermediate-band photometry deblended using the TFIT method, which is used for the first time in this work. Photometric redshifts for X-ray source counterparts are based on a new library of active galactic nuclei/galaxy hybrid templates appropriate for the faint X-ray population in the CDFS. Photometric redshift accuracy for normal galaxies is 0.010 and for X-ray sources is 0.014 and outlier fractions are 4% and 5.2%, respectively. The results within the CANDELS coverage area are even better, as demonstrated both by spectroscopic comparison and by galaxy-pair statistics. Intermediate-band photometry, even if shallow, is valuable when combined with deep broadband photometry. For best accuracy, templates must include emission lines.

  8. Limits on the LyC signal from z ~ 3 sources with secure redshift and HST coverage in the E-CDFS field

    NASA Astrophysics Data System (ADS)

    Guaita, L.; Pentericci, L.; Grazian, A.; Vanzella, E.; Nonino, M.; Giavalisco, M.; Zamorani, G.; Bongiorno, A.; Cassata, P.; Castellano, M.; Garilli, B.; Gawiser, E.; Le Brun, V.; Le Fèvre, O.; Lemaux, B. C.; Maccagni, D.; Merlin, E.; Santini, P.; Tasca, L. A. M.; Thomas, R.; Zucca, E.; De Barros, S.; Hathi, N. P.; Amorin, R.; Bardelli, S.; Fontana, A.

    2016-03-01

    Context. Determining the strength of the Lyman continuum (LyC) and the fraction of LyC escape have implications for the properties of the emitting sources at any redshift, but also for the re-ionization of the Universe at z > 6. Aims: We aim to measure the LyC signal from a sample of sources in the Chandra deep field south. We collect star-forming galaxies (SFGs) and active galactic nuclei (AGN) with accurate spectroscopic redshifts, for which Hubble Space Telescope (HST) coverage and multi-wavelength photometry are available. Methods: We selected a sample of about 200 sources at z ~ 3. Taking advantage of HST resolution, we applied a careful cleaning procedure and rejected sources showing nearby clumps with different colours, which could be lower-z interlopers. Our clean sample consisted of 86 SFGs (including 19 narrow-band selected Lyα emitters) and 8 AGN (including 6 detected in X-rays). We measured the LyC flux from aperture photometry in four narrow-band filters covering wavelengths below a 912 Å rest frame (3.11 < z < 3.53). We estimated the ratio between ionizing (LyC flux) and 1400 Å non-ionizing emissions for AGN and galaxies. Results: By running population synthesis models, we assume an average intrinsic Lν(1400 Å)/Lν(900 Å) ratio of 5 as the representative value for our sample. With this value and an average treatment of the lines of sight of the inter-galactic medium, we estimate the LyC escape fraction relative to the intrinsic value (fescrel(LyC)). We do not directly detect ionizing radiation from any individual SFG, but we are able to set a 1(2)σ upper limit of fescrel(LyC) < 12(24)%. This result is consistent with other non-detections published in the literature. No meaningful limits can be calculated for the sub-sample of Lyα emitters. We obtain one significant direct detection for an AGN at z = 3.46, with fescrel(LyC) = (72 ± 18)%. Conclusions: Our upper limit on fescrel(LyC) implies that the SFGs studied here do not present either the

  9. A Wide-Field Survey in the Chandra Deep Field-South Region: A Combined GTO + GO Approach

    NASA Astrophysics Data System (ADS)

    Garmire, Gordon

    2013-09-01

    We propose to perform a wide-field (2.2 square degree) survey around the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South (E-CDF-S). This survey will complement the large observational investments made in multi-square-degree surveys in the CDF-S region by Spitzer, Herschel, the Australia Telescope Compact Array, PRIMUS, Pan-STARRS, DES, LSST, and other facilities. It will allow us to identify the most-luminous active galaxies to z = 1.5-2 and to investigate large-scale structures in the CDF-S region. This is the GTO component of a GTO + GO project; the associated GO observations will be proposed as a Cycle 15 Large Project.

  10. The 2 Ms Chandra Deep Field-North Survey and the 250 ks Extended Chandra Deep Field-South Survey: Improved Point-source Catalogs

    NASA Astrophysics Data System (ADS)

    Xue, Y. Q.; Luo, B.; Brandt, W. N.; Alexander, D. M.; Bauer, F. E.; Lehmer, B. D.; Yang, G.

    2016-06-01

    We present improved point-source catalogs for the 2 Ms Chandra Deep Field-North (CDF-N) and the 250 ks Extended Chandra Deep Field-South (E-CDF-S) Surveys, implementing a number of recent improvements in Chandra source-cataloging methodology. For CDF-N/E-CDF-S, we provide a main catalog that contains 683/1003 X-ray sources detected with wavdetect at a false-positive probability threshold of 10‑5 that also satisfy a binomial-probability source-selection criterion of P\\lt 0.004/P < 0.002. Such an approach maximizes the number of reliable sources detected: a total of 196/275 main-catalog sources are new compared to the Alexander et al. CDF-N/Lehmer et al. E-CDF-S main catalogs. We also provide CDF-N/E-CDF-S supplementary catalogs that consist of 72/56 sources detected at the same wavdetect threshold and having P of 0.004–0.1/0.002–0.1 and {K}s≤slant 22.9/{K}s≤slant 22.3 mag counterparts. For all ≈ 1800 CDF-N and E-CDF-S sources, including the ≈ 500 newly detected ones (these being generally fainter and more obscured), we determine X-ray source positions utilizing centroid and matched-filter techniques; we also provide multiwavelength identifications, apparent magnitudes of counterparts, spectroscopic and/or photometric redshifts, basic source classifications, and estimates of observed active galactic nucleus and galaxy source densities around respective field centers. Simulations show that both the CDF-N and E-CDF-S main catalogs are highly reliable and reasonably complete. Background and sensitivity analyses indicate that the on-axis mean flux limits reached represent a factor of ≈ 1.5–2.0 improvement over the previous CDF-N and E-CDF-S limits. We make our data products publicly available.

  11. THE TAIWAN ECDFS NEAR-INFRARED SURVEY: VERY BRIGHT END OF THE LUMINOSITY FUNCTION AT z > 7

    SciTech Connect

    Hsieh, Bau-Ching; Wang, Wei-Hao; Lin, Lihwai; Lim, Jeremy; Ho, Paul T. P.; Yan, Haojing; Karoji, Hiroshi; Tsai, Chao-Wei

    2012-04-10

    The primary goal of the Taiwan ECDFS Near-Infrared Survey (TENIS) is to find well-screened galaxy candidates at z > 7 (z' dropout) in the Extended Chandra Deep Field-South (ECDFS). To this end, TENIS provides relatively deep J and K{sub s} data ({approx}25.3 ABmag, 5{sigma}) for an area of 0.5 Multiplication-Sign 0.5 deg. Leveraged with existing data at mid-infrared to optical wavelengths, this allows us to screen for the most luminous high-z objects, which are rare and thus require a survey over a large field to be found. We introduce new color selection criteria to select a z > 7 sample with minimal contaminations from low-z galaxies and Galactic cool stars; to reduce confusion in the relatively low angular resolution Infrared Array Camera (IRAC) images, we introduce a novel deconvolution method to measure the IRAC fluxes of individual sources. Illustrating perhaps the effectiveness at which we screen out interlopers, we find only one z > 7 candidate, TENIS-ZD1. The candidate has a weighted z{sub phot} of 7.8, and its colors and luminosity indicate a young (45M years old) starburst galaxy with a stellar mass of 3.2 Multiplication-Sign 10{sup 10} M{sub Sun }. The result matches with the observational luminosity function analysis and the semianalytic simulation result based on the Millennium Simulations, which may over predict the volume density for high-z massive galaxies. The existence of TENIS-ZD1, if confirmed spectroscopically to be at z > 7, therefore poses a challenge to current theoretical models for how so much mass can accumulate in a galaxy at such a high redshift.

  12. The Taiwan ECDFS Near-Infrared Survey: Very Bright End of the Luminosity Function at z > 7

    NASA Astrophysics Data System (ADS)

    Hsieh, Bau-Ching; Wang, Wei-Hao; Yan, Haojing; Lin, Lihwai; Karoji, Hiroshi; Lim, Jeremy; Ho, Paul T. P.; Tsai, Chao-Wei

    2012-04-01

    The primary goal of the Taiwan ECDFS Near-Infrared Survey (TENIS) is to find well-screened galaxy candidates at z > 7 (z' dropout) in the Extended Chandra Deep Field-South (ECDFS). To this end, TENIS provides relatively deep J and Ks data (~25.3 ABmag, 5σ) for an area of 0.5 × 0.5 deg. Leveraged with existing data at mid-infrared to optical wavelengths, this allows us to screen for the most luminous high-z objects, which are rare and thus require a survey over a large field to be found. We introduce new color selection criteria to select a z > 7 sample with minimal contaminations from low-z galaxies and Galactic cool stars; to reduce confusion in the relatively low angular resolution Infrared Array Camera (IRAC) images, we introduce a novel deconvolution method to measure the IRAC fluxes of individual sources. Illustrating perhaps the effectiveness at which we screen out interlopers, we find only one z > 7 candidate, TENIS-ZD1. The candidate has a weighted z phot of 7.8, and its colors and luminosity indicate a young (45M years old) starburst galaxy with a stellar mass of 3.2 × 1010 M ⊙. The result matches with the observational luminosity function analysis and the semianalytic simulation result based on the Millennium Simulations, which may over predict the volume density for high-z massive galaxies. The existence of TENIS-ZD1, if confirmed spectroscopically to be at z > 7, therefore poses a challenge to current theoretical models for how so much mass can accumulate in a galaxy at such a high redshift.

  13. CANDELS/GOODS-S, CDFS, ECDFS: Photometric Redshifts For X-Ray Detected AGNs

    NASA Astrophysics Data System (ADS)

    Hsu, L.; Salvato, M.; Nandra, K.; Brusa, M.

    2014-07-01

    We present photometric redshifts for X-ray sources, as well as new multi-wavelength identifications in the 4Ms-CDFS/ECDFS. To find counterparts of the X-ray sources efficiently, we use a new method based on Bayesian statistics with priors on magnitudes and position errors, making associations with optical and near/mid-infrared data simultaneously. Specifically taking advantage of high-resolution HST/WFC3 data in the Cosmic Assembly Near-IR Deep Legacy Survey (CANDELS) and homogeneous data from the Taiwan ECDFS Near-IR Survey (TENIS), 97% of X-ray sources have multi-wavelength counterparts. To compute photo-z, in addition to the CANDELS data, the de-blended intermediate-band photometry (by TFIT method) is used for the first time in this field. Furthermore, we adopt a new set of AGN-galaxy hybrid templates which are more representative of population. These hybrids are composed of semi-empirical galaxy templates that include emission lines, in addition to type1/2 AGNs. In the entire field, we achieve a photo-z accuracy of 0.014 with 5.3% outliers. The WFC3/NIR data allow us to reach more accurate redshifts up to 7. The results are particularly accurate when incorporating the intermediate bands and emission lines that pinpoint strong line features from AGNs. The photo-z accuracy is three times better when including them in the fitting.

  14. SENSITIVE SEARCH FOR RADIO VARIABLES AND TRANSIENTS IN THE EXTENDED CHANDRA DEEP FIELD SOUTH

    SciTech Connect

    Mooley, K. P.; Kulkarni, S. R.; Horesh, A.; Frail, D. A.; Ofek, E. O.; Miller, N. A.

    2013-05-10

    We report on an analysis of the Extended Chandra Deep Field South (E-CDFS) region using archival data from the Very Large Array, with the goal of studying radio variability and transients at the sub-milliJansky level. The 49 epochs of E-CDFS observations at 1.4 GHz sample timescales from 1 day to 3 months. We find that only a fraction (1%) of unresolved radio sources above 40 {mu}Jy are variable at the 4{sigma} level. There is no evidence that the fractional variability changes along with the known transition of radio-source populations below 1 mJy. Optical identifications of the sources show that the variable radio emission is associated with the central regions of an active galactic nucleus or a star-forming galaxy. After a detailed comparison of the efficacy of various source-finding algorithms, we use the best to carry out a transient search. No transients were found. This implies that the areal density of transients with peak flux density greater than 0.21 mJy is less than 0.37 deg{sup -2} (at a confidence level of 95%). This result is approximately an order of magnitude below the transient rate measured at 5 GHz by Bower et al. but it is consistent with more recent upper limits from Frail et al. Our findings suggest that the radio sky at 1.4 GHz is relatively quiet. For multi-wavelength transient searches, such as the electromagnetic counterparts to gravitational waves, this frequency may be optimal for reducing the high background of false positives.

  15. The 2 Ms Chandra Deep Field-North Survey and the 250 ks Extended Chandra Deep Field-South Survey: Improved Point-Source Catalogs

    NASA Astrophysics Data System (ADS)

    Xue, Y.; Luo, B.; Brandt, W.; Alexander, D.; Bauer, F.; Lehmer, B.; Yang, G.

    2016-06-01

    We present improved point-source catalogs for the 2Ms CDF-N and the 250ks E-CDF-S, implementing a number of recent improvements in Chandra source-cataloging methodology. For the CDF-N/E-CDF-S, we provide a main catalog that contains 683/1003 X-ray sources detected with wavdetect at a false-positive probability threshold of 1E-5 that also satisfy a binomial-probability source-selection criterion of P<0.004/P<0.002. Such an approach maximizes the number of reliable sources detected: a total of 196/275 main-catalog sources are new compared to the A03 CDF-N/L05 E-CDF-S main catalogs. We also provide CDF-N/E-CDF-S supplementary catalogs that consist of 72/56 sources detected at the same wavdetect threshold and having P of 0.004-0.1/0.002-0.1 and K_s<22.9/K_s<22.3 counterparts. For all ≈1800 CDF-N and E-CDF-S sources, including the ≈500 newly detected ones, we determine X-ray source positions utilizing centroid and matched-filter techniques; we also provide multiwavelength identifications, apparent magnitudes of counterparts, spectroscopic and/or photometric redshifts, basic source classifications, and estimates of observed AGN and galaxy source densities around respective field centers. Simulations show that both the CDF-N and E-CDF-S main catalogs are highly reliable and reasonably complete. Background and sensitivity analyses indicate that the on-axis mean flux limits reached represent a factor of ≈1.5-2.0 improvement over the previous CDF-N and E-CDF-S limits.

  16. X-RAY PROPERTIES OF THE z {approx} 4.5 Ly{alpha} EMITTERS IN THE CHANDRA DEEP FIELD SOUTH REGION

    SciTech Connect

    Zheng, Z. Y.; Wang, J. X.; Finkelstein, S. L.; Finkelstein, K. D.; Malhotra, S.; Rhoads, J. E. E-mail: jxw@ustc.edu.c

    2010-07-20

    We report the first X-ray detection of Ly{alpha} emitters (LAEs) at redshift z {approx} 4.5. One source (J033127.2-274247) is detected in the Extended Chandra Deep Field-South (ECDF-S) X-ray data and has been spectroscopically confirmed as a z = 4.48 quasar with L{sub X} = 4.2 x 10{sup 44} erg s{sup -1}. The single detection gives an Ly{alpha} quasar density of {approx} 2.7{sup +6.2} {sub -2.2} x 10{sup -6} Mpc{sup -3}, consistent with the X-ray luminosity function of quasars. Another 22 LAEs in the central Chandra Deep Field-South region are not detected individually, but their co-added counts yield an S/N = 2.4 (p = 99.83%) detection at soft band, with an effective exposure time of {approx}36 Ms. Further analysis of the equivalent width (EW) distribution shows that all the signals come from 12 LAE candidates with EW{sub rest}< 400 A and 2 of them contribute about half of the signal. From follow-up spectroscopic observations, we find that one of the two is a low-redshift emission-line galaxy, and the other is a Lyman break galaxy at z = 4.4 with little or no Ly{alpha} emission. Excluding these two and combined with ECDF-S data, we derive a 3{sigma} upper limit on the average X-ray flux of F {sub 0.5-2.0keV} < 1.6 x 10{sup -18} erg cm{sup -2} s{sup -1}, which corresponds to an average luminosity of (L {sub 0.5-2keV}) <2.4 x 10{sup 42} erg s{sup -1} for z {approx} 4.5 LAEs. If the average X-ray emission is due to star formation, it corresponds to a star formation rate (SFR) of <180-530 M {sub sun} yr{sup -1}. We use this SFR {sub X} as an upper limit of the unobscured SFR to constrain the escape fraction of Ly{alpha} photons and find a lower limit of f{sub esc,Ly{alpha}} > 3%-10%. However, our upper limit on the SFR {sub X} is {approx}7 times larger than the upper limit on SFR {sub X} on z {approx} 3.1 LAEs in the same field and at least 30 times higher than the SFR estimated from Ly{alpha} emission. From the average X-ray-to-Ly{alpha} line ratio, we estimate that

  17. An alma survey of sub-millimeter galaxies in the extended Chandra deep field south: Sub-millimeter properties of color-selected galaxies

    SciTech Connect

    Decarli, R.; Walter, F.; Hodge, J. A.; Rix, H.-W.; Schinnerer, E.; Smail, I.; Swinbank, A. M.; Karim, A.; Simpson, J. M.; Chapman, S.; Coppin, K. E. K.; Cox, P.; Dannerbauer, H.; Greve, T. R.; Ivison, R.; Knudsen, K. K.; Lindroos, L.; Van der Werf, P.; Weiß, A.

    2014-01-10

    We study the sub-millimeter properties of color-selected galaxies via a stacking analysis applied for the first time to interferometric data at sub-millimeter wavelengths. We base our study on 344 GHz ALMA continuum observations of ∼20''-wide fields centered on 86 sub-millimeter sources detected in the LABOCA Extended Chandra Deep Field South (ECDFS) Sub-millimeter Survey. We select various classes of galaxies (K-selected, star-forming sBzK galaxies, extremely red objects, and distant red galaxies) according to their optical/near-infrared fluxes. We find clear, >10σ detections in the stacked images of all these galaxy classes. We include in our stacking analysis Herschel/SPIRE data to constrain the dust spectral energy distribution of these galaxies. We find that their dust emission is well described by a modified blackbody with T {sub dust} ≈ 30 K and β = 1.6 and infrared luminosities of (5-11) × 10{sup 11} L {sub ☉} or implied star formation rates of 75-140 M {sub ☉} yr{sup –1}. We compare our results with those of previous studies based on single-dish observations at 870 μm and find that our flux densities are a factor 2-3 higher than previous estimates. The discrepancy is observed also after removing sources individually detected in ALESS maps. We report a similar discrepancy by repeating our analysis on 1.4 GHz observations of the whole ECDFS. Hence, we find tentative evidence that galaxies that are associated in projected and redshift space with sub-mm bright sources are brighter than the average population. Finally, we put our findings in the context of the cosmic star formation rate density as a function of redshift.

  18. The NuSTAR Extragalactic Surveys: Initial Results and Catalog from the Extended Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Mullaney, J. R.; Del-Moro, A.; Aird, J.; Alexander, D. M.; Civano, F. M.; Hickox, R. C.; Lansbury, G. B.; Ajello, M.; Assef, R.; Ballantyne, D. R.; Balok´, M.; Bauer, F. E.; Brandt, W. N.; Boggs, S. E.; Brightman, M.; Christensen, F. E.; Comastri, A.; Craig, W. W.; Elvis, M.; Forster, K.; Gandhi, P.; Grefenstette, B. W.; Hailey, C. J.; Harrison, F. A.; Koss, M.; LaMassa, S. M.; Luo, B.; Madsen, K. K.; Puccetti, S.; Saez, C.; Stern, D.; Treister, E.; Urry, C. M.; Wik, D. R.; Zappacosta, L.; Zhang, W.

    2015-08-01

    We present the initial results and the source catalog from the Nuclear Spectroscopic Telescope Array (NuSTAR) survey of the Extended Chandra Deep Field South (hereafter, ECDFS)—currently the deepest contiguous component of the NuSTAR extragalactic survey program. The survey covers the full ≈30‧ × 30‧ area of this field to a maximum depth of ≈360 ks (≈ 220 ks when corrected for vignetting at 3-24 keV), reaching sensitivity limits of ≈ 1.3× {10}-14 {erg} {{{s}}}-1 {{cm}}-2 (3-8 keV), ≈ 3.4× {10}-14 {erg} {{{s}}}-1 {{cm}}-2 (8-24 keV), and ≈ 3.0× {10}-14 {erg} {{{s}}}-1 {{cm}}-2 (3-24 keV). A total of 54 sources are detected over the full field, although five of these are found to lie below our significance threshold once contaminating flux from neighboring (i.e., blended) sources is taken into account. Of the remaining 49 that are significant, 19 are detected in the 8-24 keV band. The 8-24 to 3-8 keV band ratios of the 12 sources that are detected in both bands span the range 0.39-1.7, corresponding to a photon index range of {{Γ }}≈ 0.5-2.3, with a median photon index of \\bar{{{Γ }}}=1.70+/- 0.52. The redshifts of the 49 sources in our main sample span the range z=0.21-2.7, and their rest-frame 10-40 keV luminosities (derived from the observed 8-24 keV fluxes) span the range {L}10-40 {keV}≈ (0.7-300)× {10}43 {erg} {{{s}}}-1, sampling below the “knee” of the X-ray luminosity function out to z˜ 0.8-1. Finally, we identify one NuSTAR source that has neither a Chandra nor an XMM-Newton counterpart, but that shows evidence of nuclear activity at infrared wavelengths and thus may represent a genuine, new X-ray source detected by NuSTAR in the ECDFS.

  19. VizieR Online Data Catalog: A K-selected catalog of the ECDFS from MUSYC (Taylor+, 2009)

    NASA Astrophysics Data System (ADS)

    Taylor, E. N.; Franx, M.; van Dokkum, P. G.; Quadri, R. F.; Gawiser, E.; Bell, E. F.; Barrientos, L. F.; Blanc, G. A.; Castander, F. J.; Damen, M.; Gonzalez-Perez, V.; Hall, P. B.; Herrera, D.; Hildebrandt, H.; Kriek, M.; Labbe, I.; Lira, P.; Maza, J.; Rudnick, G.; Treister, E.; Urry, C. M.; Willis, J. P.; Wuyts, S.

    2010-01-01

    Hildebrandt et al. (2006A&A...452.1121H) have collected all (up until 2005 December) archival UU38BRVI imaging data taken using the Wide Field Imager (WFI) on the ESO MPG 2.2m telescope. We have supplemented the WFI optical data with original z'-band imaging taken using Mosaic-II camera on the CTIO 4m Blanco telescope. The ECDFS data were taken in 2005 January. The new MUSYC NIR imaging consists of two mosaics in the J and K bands obtained using the Infrared Sideport Imager (ISPI) on the CTIO Blanco 4m telescope. The data were taken over the course of 15 nights, in 4 separate observing runs between 2003 January and 2004 February. (3 data files).

  20. GRAVITATIONAL LENS CANDIDATES IN THE E-CDFS

    SciTech Connect

    More, A.; More, S.; Jahnke, K.; Gallazzi, A.; Bell, E. F.; Barden, M.; Haeussler, B.

    2011-06-10

    We report 10 lens candidates in the Extended Chandra Deep Field South from the GEMS survey. Nine of the systems are new detections and only one of the candidates is a known lens system. For the most promising five systems including the known lens system, we present results from preliminary lens mass modeling, which tests if the candidates are plausible lens systems. Photometric redshifts of the candidate lens galaxies are obtained from the COMBO-17 galaxy catalog. Stellar masses of the candidate lens galaxies within the Einstein radius are obtained by using the z-band luminosity and the V-z color-based stellar mass-to-light ratios. As expected, the lensing masses are found to be larger than the stellar masses of the candidate lens galaxies. These candidates have similar dark matter fractions as compared to lenses in SLACS and COSMOS. They also roughly follow the halo-mass-stellar-mass relation predicted by the subhalo abundance matching technique. One of the candidate lens galaxies qualifies as a luminous infrared galaxy and may not be a true lens because the arc-like feature in the system is likely to be an active region of star formation in the candidate lens galaxy. Among the five best candidates, one is a confirmed lens system, one is likely a lens system, two are less likely to be lenses, and the status of one of the candidates is ambiguous. Spectroscopic follow-up of these systems is still required to confirm lensing and/or for more accurate determination of the lens masses and mass density profiles.

  1. Field Problems in the South Bronx.

    ERIC Educational Resources Information Center

    Madrigal, Stasia, Ed.

    1983-01-01

    Articles in this issue of the bulletin of the Hispanic Research Center focus on the problems of collecting demographic and social data in the South Bronx. The introductory article summarizes the contents of this issue. The second (by Lloyd H. Rogler, Osvaldo Barreras, and Rosemary Santana Cooney) is based on the experiences of field workers…

  2. NO EVIDENCE FOR EVOLUTION IN THE FAR-INFRARED-RADIO CORRELATION OUT TO z {approx} 2 IN THE EXTENDED CHANDRA DEEP FIELD SOUTH

    SciTech Connect

    Mao, Minnie Y.; Huynh, Minh T.; Helou, George; Norris, Ray P.; Dickinson, Mark; Frayer, Dave; Monkiewicz, Jacqueline A.

    2011-04-20

    We investigate the 70 {mu}m far-infrared-radio correlation (FRC) of star-forming galaxies in the Extended Chandra Deep Field South (ECDFS) out to z > 2. We use 70 {mu}m data from the Far-Infrared Deep Extragalactic Legacy Survey (FIDEL), which comprises the most sensitive ({approx}0.8 mJy rms) and extensive far-infrared deep field observations using MIPS on the Spitzer Space Telescope, and 1.4 GHz radio data ({approx}8 {mu}Jy beam{sup -1} rms) from the Very Large Array. In order to quantify the evolution of the FRC, we use both survival analysis and stacking techniques, which we find give similar results. We also calculate the FRC using total infrared luminosity and rest-frame radio luminosity, q{sub TIR}, and find that q{sub TIR} is constant (within 0.22) over the redshift range 0-2. We see no evidence for evolution in the FRC at 70 {mu}m, which is surprising given the many factors that are expected to change this ratio at high redshifts.

  3. INTERIOR PERSPECTIVE, LOOKING SOUTH SOUTHWEST WITH FIELD SET UP IN ...

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

    INTERIOR PERSPECTIVE, LOOKING SOUTH SOUTHWEST WITH FIELD SET UP IN FOOTBALL CONFIGURATION. FIELD SEATING ROTATES TO ACCOMMODATE BASEBALL GAMES. - Houston Astrodome, 8400 Kirby Drive, Houston, Harris County, TX

  4. THE LABOCA SURVEY OF THE EXTENDED CHANDRA DEEP FIELD SOUTH: TWO MODES OF STAR FORMATION IN ACTIVE GALACTIC NUCLEUS HOSTS?

    SciTech Connect

    Lutz, D.; Shao, L.; Foerster Schreiber, N. M.; Genzel, R.; Mainieri, V.; Rafferty, D.; Brandt, W. N.; Hasinger, G.; Weiss, A.; Menten, K. M.; Walter, F.; Greve, T. R.; Smail, I.; Coppin, K.; Alexander, D. M.; Chapman, S.; Gawiser, E.; Kurczynski, P.; Ivison, R. J.; Koekemoer, A. M.

    2010-04-01

    We study the co-existence of star formation and active galactic nucleus (AGN) activity in Chandra X-ray-selected AGN by analyzing stacked 870 {mu}m submillimeter emission from a deep and wide map of the Extended Chandra Deep Field South (ECDFS), obtained with the LABOCA instrument at the APEX telescope. The total X-ray sample of 895 sources with median redshift z {approx} 1 drawn from the combined (E)CDFS X-ray catalogs is detected at >11sigma significance at a mean submillimeter flux of 0.49 +- 0.04 mJy, corresponding to a typical star formation rate (SFR) around 30 M{sub sun} yr{sup -1} for a T = 35 K, beta = 1.5 graybody far-infrared spectral energy distribution. The good signal-to-noise ratio permits stacking analyses for major subgroups, splitting the sample by redshift, intrinsic luminosity, and AGN obscuration properties. We observe a trend of SFR increasing with redshift. An increase of SFR with AGN luminosity is indicated at the highest L{sub 2-10{sub keV}} {approx}> 10{sup 44} erg s{sup -1} luminosities only. Increasing trends with X-ray obscuration as expected in some AGN evolutionary scenarios are not observed for the bulk of the X-ray AGN sample but may be present for the highest intrinsic luminosity objects with L{sub 2-10{sub keV}} {approx}> 10{sup 44} erg s{sup -1}. This behavior suggests a transition between two modes in the co-existence of AGN activity and star formation. For the bulk of the sample, the X-ray luminosity and obscuration of the AGN are not intimately linked to the global SFR of their hosts. The hosts are likely massive and forming stars secularly, at rates similar to the pervasive star formation seen in massive galaxies without an AGN at similar redshifts. In these systems, star formation is not linked to a specific state of the AGN and the period of moderately luminous AGN activity may not highlight a major evolutionary transition of the galaxy. The change indicated toward more intense star formation, and a more pronounced increase

  5. The Multiwavelength Survey by Yale-Chile (MUSYC): Deep Medium-band Optical Imaging and High-quality 32-band Photometric Redshifts in the ECDF-S

    NASA Astrophysics Data System (ADS)

    Cardamone, Carolin N.; van Dokkum, Pieter G.; Urry, C. Megan; Taniguchi, Yoshi; Gawiser, Eric; Brammer, Gabriel; Taylor, Edward; Damen, Maaike; Treister, Ezequiel; Cobb, Bethany E.; Bond, Nicholas; Schawinski, Kevin; Lira, Paulina; Murayama, Takashi; Saito, Tomoki; Sumikawa, Kentaro

    2010-08-01

    We present deep optical 18-medium-band photometry from the Subaru telescope over the ~30' × 30' Extended Chandra Deep Field-South, as part of the Multiwavelength Survey by Yale-Chile (MUSYC). This field has a wealth of ground- and space-based ancillary data, and contains the GOODS-South field and the Hubble Ultra Deep Field. We combine the Subaru imaging with existing UBVRIzJHK and Spitzer IRAC images to create a uniform catalog. Detecting sources in the MUSYC "BVR" image we find ~40,000 galaxies with R AB < 25.3, the median 5σ limit of the 18 medium bands. Photometric redshifts are determined using the EAzY code and compared to ~2000 spectroscopic redshifts in this field. The medium-band filters provide very accurate redshifts for the (bright) subset of galaxies with spectroscopic redshifts, particularly at 0.1 < z < 1.2 and at z >~ 3.5. For 0.1 < z < 1.2, we find a 1σ scatter in Δz/(1 + z) of 0.007, similar to results obtained with a similar filter set in the COSMOS field. As a demonstration of the data quality, we show that the red sequence and blue cloud can be cleanly identified in rest-frame color-magnitude diagrams at 0.1 < z < 1.2. We find that ~20% of the red sequence galaxies show evidence of dust emission at longer rest-frame wavelengths. The reduced images, photometric catalog, and photometric redshifts are provided through the public MUSYC Web site. Based (in part) on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

  6. THE MULTIWAVELENGTH SURVEY BY YALE-CHILE (MUSYC): DEEP MEDIUM-BAND OPTICAL IMAGING AND HIGH-QUALITY 32-BAND PHOTOMETRIC REDSHIFTS IN THE ECDF-S

    SciTech Connect

    Cardamone, Carolin N.; Van Dokkum, Pieter G.; Urry, C. Megan; Brammer, Gabriel; Taniguchi, Yoshi; Gawiser, Eric; Bond, Nicholas; Taylor, Edward; Damen, Maaike; Treister, Ezequiel; Cobb, Bethany E.; Schawinski, Kevin; Lira, Paulina; Murayama, Takashi; Saito, Tomoki; Sumikawa, Kentaro

    2010-08-15

    We present deep optical 18-medium-band photometry from the Subaru telescope over the {approx}30' x 30' Extended Chandra Deep Field-South, as part of the Multiwavelength Survey by Yale-Chile (MUSYC). This field has a wealth of ground- and space-based ancillary data, and contains the GOODS-South field and the Hubble Ultra Deep Field. We combine the Subaru imaging with existing UBVRIzJHK and Spitzer IRAC images to create a uniform catalog. Detecting sources in the MUSYC 'BVR' image we find {approx}40,000 galaxies with R {sub AB} < 25.3, the median 5{sigma} limit of the 18 medium bands. Photometric redshifts are determined using the EAzY code and compared to {approx}2000 spectroscopic redshifts in this field. The medium-band filters provide very accurate redshifts for the (bright) subset of galaxies with spectroscopic redshifts, particularly at 0.1 < z < 1.2 and at z {approx}> 3.5. For 0.1 < z < 1.2, we find a 1{sigma} scatter in {Delta}z/(1 + z) of 0.007, similar to results obtained with a similar filter set in the COSMOS field. As a demonstration of the data quality, we show that the red sequence and blue cloud can be cleanly identified in rest-frame color-magnitude diagrams at 0.1 < z < 1.2. We find that {approx}20% of the red sequence galaxies show evidence of dust emission at longer rest-frame wavelengths. The reduced images, photometric catalog, and photometric redshifts are provided through the public MUSYC Web site.

  7. Parade field, looking from corner of south Hutton St. And ...

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

    Parade field, looking from corner of south Hutton St. And Charlie Kelly Blvd. To the northeast towards the 400 series quarters. - Fitzsimons General Hospital, Bounded by East Colfax to south, Peoria Street to west, Denver City/County & Adams County Line to north, & U.S. Route 255 to east, Aurora, Adams County, CO

  8. VIEW SOUTH TOWARD MOVEABLE FIELD LEVEL SEATS. NOTE RETRACTABLE PENTAGONAL ...

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

    VIEW SOUTH TOWARD MOVEABLE FIELD LEVEL SEATS. NOTE RETRACTABLE PENTAGONAL LIGHT RING GONDOLA SUSPENDED FROM ROOF CUPOLA. SKY LIGHTS PAINTED OVER TO REDUCE GLARE FOR BASEBALL OUTFIELDERS. - Houston Astrodome, 8400 Kirby Drive, Houston, Harris County, TX

  9. Evaluation Field Building in South Asia: Reflections, Anecdotes, and Questions

    ERIC Educational Resources Information Center

    Hay, Katherine

    2010-01-01

    This article examines evaluation field building in South Asia and the role of international collaboration in this field building. The article explores aspects of the supply and demand of development evaluation and the political, historical, and systemic factors that bridge or block evaluation use. The article calls for and suggests elements to…

  10. Lyα-emitting Galaxies at z = 2.1 in ECDF-S: Building Blocks of Typical Present-day Galaxies?

    NASA Astrophysics Data System (ADS)

    Guaita, Lucia; Gawiser, Eric; Padilla, Nelson; Francke, Harold; Bond, Nicholas A.; Gronwall, Caryl; Ciardullo, Robin; Feldmeier, John J.; Sinawa, Shawn; Blanc, Guillermo A.; Virani, Shanil

    2010-05-01

    We discovered a sample of 250 Lyα emitting (LAE) galaxies at z ~= 2.1 in an ultra-deep 3727 Å narrow-band MUSYC image of the Extended Chandra Deep Field-South. The LAEs were selected to have rest-frame equivalent widths (EWs) >20 Å and emission-line fluxes F Lyα>2.0 × 10-17 erg cm-2 s-1, after carefully subtracting the continuum contributions from narrow-band photometry. The median emission-line flux of our sample is F Lyα = 4.2 × 10-17 erg cm-2 s-1, corresponding to a median Lyα luminosity L Lyα = 1.3 × 1042 erg s-1 at z ~= 2.1. At this flux, our sample is >=90% complete. Approximately 4% of the original NB-selected candidates were detected in X-rays by Chandra, and 7% were detected in the rest-frame far-UV by the Galaxy Evolution Explorer; these objects were eliminated to minimize contamination by active galactic nuclei and low-redshift galaxies. At L Lyα >= 1.3 × 1042 erg s-1, the EW distribution is unbiased and is represented by an exponential with scale-length 83 ±10 Å. Above this same luminosity threshold, we find a number density of 1.5 ± 0.5 × 10-3 Mpc-3. Neither the number density of LAEs nor the scale-length of their EW distribution show significant evolution from z ~= 3 to z ~= 2. We used the rest-frame UV luminosity to estimate a median star formation rate of 4 M sun yr-1. The median rest-frame UV slope, parameterized by the color B - R, is typical of dust-free, 0.5-1 Gyr old or moderately dusty, 300-500 Myr old population. Approximately 30% of our sample is consistent with being very young (age <100 Myr) galaxies without dust. Approximately 40% of the sample occupies the z ~ 2 star-forming galaxy locus in the UVR two-color diagram, but the true percentage could be significantly higher taking into account photometric errors. Clustering analysis reveals that LAEs at z ~= 2.1 have r 0 = 4.8 ± 0.9 Mpc, corresponding to a bias factor b = 1.8 ± 0.3. This implies that z ~= 2.1 LAEs reside in dark matter halos with median masses log(M/M sun

  11. North south asymmetry in the coronal and photospheric magnetic fields

    NASA Astrophysics Data System (ADS)

    Virtanen, I.; Mursula, K.

    2013-12-01

    Several recent studies have shown that the Heliospheric current sheet (HCS) is southward shifted during about three years in the solar declining phase (the so-called bashful ballerina phenomenon). We study the hemispherical asymmetry in the photospheric and coronal magnetic fields using Wilcox Solar Observatory (WSO) measurements of the photospheric magnetic field since 1976 and the potential field source surface (PFSS) model. Multipole analysis of the photospheric magnetic field shows that during the late declining phase of solar cycles since 1970s, bashful ballerina phenomenon is a consequence of g02 quadrupole term, signed oppositely to the dipole moment. Surges of new flux transport magnetic field from low latitudes to the poles, thus leading to a systematically varying contribution to the g02-term from different latitudes. In the case of a north-south asymmetric flux production this is seen as a quadrupole contribution traveling towards higher latitudes. When the quadrupole term is largest the main contribution comes from the polar latitudes. At least during the four recent solar cycles the g02-term arises because the magnitude of the southern polar field is larger than in the north in the declining phase of the cycle. Magnetic flux is transported polewards by the meridional flow and it is most likely that besides the north-south asymmetric production of the magnetic flux, also the asymmetric transportation may significantly contribute to the observed asymmetry of polar field intensities. The overall activity during solar cycle is not significantly different in the northern and southern hemispheres, but hemispheres tend to develop in a different phase.

  12. View of South TwentySixth Street. Stairs to sports field on ...

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

    View of South Twenty-Sixth Street. Stairs to sports field on right which are seen in photo no. HABS CA-2783-3. Buildings No. 25, 26, 27, seen left to right at rear, looking south - Easter Hill Village, Bordered by South Twenty-sixth Street, South Twenty-eighth Street, Hinkley Avenue, Foothill Avenue & Corto Square, Richmond, Contra Costa County, CA

  13. South Belridge fields, Borderland basin, U. S. , San Joaquin Valley

    SciTech Connect

    Miller, D.D. ); McPherson, J.G. )

    1991-03-01

    South Belridge is a giant field in the west San Joaquin Valley, Kern County. Cumulative field production is approximately 700 MMBO and 220 BCFG, with remaining recoverable reserves of approximately 500 MMBO. The daily production is nearly 180 MBO from over 6100 active wells. The focus of current field development and production is the shallow Tulare reservoir. Additional probable diatomite reserves have been conservatively estimated at 550 MMBO and 550 BCFG. South Belridge field has two principal reservoir horizons; the Mio-Pliocene Belridge diatomite of the upper Monterey Formation, and the overlying Plio-Pleistocene Tulare Formation. The field lies on the crest of a large southeast-plunging anticline, sub-parallel to the nearby San Andreas fault system. The reservoir trap in both the Tulare and diatomite reservoir horizons is a combination of structure, stratigraphic factors, and tar seals; the presumed source for the oil is the deeper Monterey Formation. The diatomite reservoir produces light oil (20-32{degree} API gravity) form deep-marine diatomite and diatomaceous shales with extremely high porosity (average 60%) and low permeability (average 1 md). In contrast, the shallow ({lt}1000 ft (305 m) deep) overlying Tulare reservoir produces heavy oil (13-14{degree} API gravity) from unconsolidated, arkosic, fluviodeltaic sands of high porosity (average 35%) and permeability (average 3000 md). The depositional model is that of a generally prograding fluviodeltaic system sourced in the nearby basin-margin highlands. More than 6000 closely spaced, shallow wells are the key to steamflood production from hundreds of layered and laterally discontinuous reservoir sands which create laterally and vertically discontinuous reservoir flow units.

  14. Multicolor Observations of the Hubble Deep Field South

    NASA Astrophysics Data System (ADS)

    Vanzella, Eros; Cristiani, Stefano; Saracco, Paolo; Arnouts, Stephane; Bianchi, Simone; D'Odorico, Sandro; Fontana, Adriano; Giallongo, Emanuele; Grazian, Andrea

    2001-11-01

    We present a deep multicolor (U, B, V, I, Js, H, Ks) catalog of galaxies in the Hubble Deep Field South, based on observations obtained with the HST WFPC2 in 1998 and VLT-ISAAC in 1999. The photometric procedures were tuned to derive a catalog optimized for the estimation of photometric redshifts. In particular we adopted a ``conservative'' detection threshold, which resulted in a list of 1611 objects. The behavior of the observed source counts is in general agreement with the previous results of Casertano et al. in the Hubble Deep Field South and Williams et al. in the Hubble Deep Field North, while the corresponding counts in the Hubble Deep Field North provided by Fernández-Soto, Lanzetta, & Yahil are systematically lower by a factor 1.5 beyond IAB=26. After correcting for the incompleteness of the source counts, the object surface density at IAB<=27.5 is estimated to be 220 arcmin-2, in agreement with the corresponding measure of Volonteri et al. and providing an estimate of the extragalactic background light in the I band consistent with the work of Madau & Pozzetti. The comparison between the median V-I color in the Hubble Deep Field North and South shows a significant difference around IAB~26, possibly due to the presence of large-scale structure at z~1 in the HDF-N. High-redshift galaxy candidates (90 U dropouts and 17 B dropouts) were selected by means of color diagrams, down to a magnitude IAB=27, with a surface density of (21+/-1) and (3.9+/-0.9) arcmin-2, respectively. Eleven extremely red objects [with (I-K)AB>2.7] were selected down to KAB=24, plus three objects whose upper limit to the Ks flux is still compatible with the selection criterion. The corresponding surface density of EROs is (2.5+/-0.8) arcmin-2 [(3.2+/-0.9) arcmin-2 if we include the three Ks upper limits]. They show a remarkably nonuniform spatial distribution and are classified with roughly equal fractions in the categories of elliptical and starburst galaxies.

  15. A New South America Electric Field Monitor Network

    NASA Astrophysics Data System (ADS)

    Raulin, J.; Tacza, J.; Macotela, E. L.; Norabuena, E. O.

    2013-12-01

    In this paper we present the installation and operation of a new network of sensors located in South America in order to monitor the atmospheric electric field.The network is composed of five sensors installed at different locations spread over in Argentina and Perú.The main goals of such new instrumental facility is to provide continuous measurements of the diurnal variations of the atmospheric electric field during undisturbed (fair weather) conditions. Our aim is to study the variations of the daily Carnegie curve in different timescales: (i) monthly and seasonal changes; (ii) short and long-term related to transient explosive solar phenomena, geomagnetic disturbances, and the solar activity cycle, respectively; (iii) time and space variations and their relation with seismic activity occurrence in the region. Here we present the calibration of the different sensors as well as the resulting daily and monthly curves. We also discuss the ability of such data base to investigate the above scientific problems.

  16. The South Carolina Coastal Erosion Study: Nearshore Hydrodynamics Field Experiment

    NASA Astrophysics Data System (ADS)

    Haas, K. A.; Voulgaris, G.; Demir, H.; Work, P. A.; Hanes, D. M.

    2004-12-01

    As part of the South Carolina Coastal Erosion Study (SCCES) a nearshore field experiment was carried out for five days in December 2003 just north of Myrtle Beach, South Carolina, providing measurements of the waves, currents and morphological evolution. This experiment occurred concurrently with an extensive field campaign several kilometers offshore which included measurements of the waves and currents on and near a significant sand shoal. The purpose of the nearshore experiment was to aid in the identification of the effect of the offshore shoal on the nearshore processes. The resulting dataset will be used for verification of numerical models being used to investigate the hydrodynamics of the region. The experiment was carried out from December 10 to December 15 and consisted of measurements of the waves and currents, extensive surveys of the bathymetry every day, grab samples of the sediments, and video imagery. The hydrodynamics were measured using two Sontek Triton downward-looking Acoustic Doppler Velocimeters and two Nortek AquaDopp profilers arranged in a cross-shore line from inside the swash to several surf zone widths past the breakers. The bathymetric surveying was accomplished using both a differential GPS system and a total station. Surveying was performed each day in order to capture the morphological changes. On the last day, seven sediment samples were taken along a single cross-section to determine the sediment characteristics across the beach. Additionally, a video camera was located on a balcony of the top floor of a nearby hotel providing an excellent field of view of the entire experimental area. Digital video was captured directly onto a computer during all daylight hours and many control points were surveyed in each day to facilitate rectification of the imagery. A variety of conditions were encountered during the experiment, including two storm fronts which passed through, generating wind speeds up to 15 m/s. The first storm generated

  17. South Fence Road -- Phase 1 field operations summary

    SciTech Connect

    McCord, J.P.; Neel, D.

    1996-03-01

    The South Fence Road (SFR) project is part of the Sandia National Laboratories, New Mexico (SNL/NM) Site-Wide Hydrogeologic Characterization (SWHC) task. The SWHC task has as its objective the reduction of uncertainty about the rate and direction of groundwater flow in the SNL/NM/Kirtland Air Force Base (KAFB) area. The SFR project area is located along the southern boundary of SNL/KAFB. This project area was selected to provide site-specific information related to geology and groundwater hydrology within the Hubbell Spring/Tijeras/Sandia fault complex. Specific objectives included determining the depth to the Santa Fe Group/bedrock contact, the depth to the water table, and the hydrogeologic complexities related to faulting. This report is a basic data report from the first phase of field operations associated with the drilling, logging, completion, and development of South Fence Road Wells SFR-1D and SFR-1S, SFR-2, SFR-3D and SFR-3S, and SFR-4. These test/monitoring wells were installed as part of Sandia National Laboratories, New Mexico, Environmental Restoration Project.

  18. EIS Data on the Chandra Deep Field South Released

    NASA Astrophysics Data System (ADS)

    2001-03-01

    The purpose of this note is to announce that the ESO Imaging Survey programme has released a full set of optical/infrared data covering the socalled Chandra Deep Field South (CDF-S) rapidly becoming a favoured target for cosmological studies in the southern hemisphere. The field was originally selected for deep X-ray observations with Chandra and XMM. The former have already been completed producing the deepest high-resolution X-ray image ever taken with a total integration time of one million seconds. The data obtained by EIS include J and Ks infrared observations of an area of 0.1 square degree nearly matching the Chandra image down to JAB ~ 23.4 and KAB ~ 22.6 and UU'BVRI optical observations over 0.25 square degree, matching the XMM field of view, reaching 5 s limiting magnitudes of U'AB = 26.0, UAB = 25.7, BAB = 26.4, VAB = 25.4, RA B = 25.5 and IA B = 24.7 mag, as measured within a 2 ´ FWHM aperture.

  19. Bob West field: Extending upper Wilcox production in south Texas

    SciTech Connect

    Montgomery, S.L.

    1997-05-01

    Discovered in 1990 near the southern limit of the upper Wilcox gas-producing trend in south Texas, Bob West field is the largest pool to date in this trend, with probable reserves of up to 1 Tcf. The field produces from seven major sandstone {open_quotes}packages,{close_quotes} comprising 27 individual reservoirs and distributed over 3500 productive acres. The sandstones represent either fluvial/deltaic deposits or delta-margin barrier bar and strand-plain sediments. Porosities range up to 20%, but permeabilities are low, commonly less than 1.5 md. Artificial stimulation is therefore required to establish commercial rates of production. Bob West lies on a faulted anticline between two major growth-fault structures, with several stages of structural development evident. Such development has directly affected sandstone thickness. Rates of production are higher at Bob West than at other upper Wilcox fields due to commingling of zones, large-scale fracture treatments, and directional drilling. Discovery at Bob West has significant implications for renewed exploration in this part of the upper Wilcox gas trend.

  20. Incidense of spider mites in South Texas cotton fields

    Technology Transfer Automated Retrieval System (TEKTRAN)

    The incidence of spider mites was evaluated· in four locations of south Texas between Progreso (Hidalgo Co.) to Bishop (Nueces Co.). This is an area with a south to north transect of 125 miles from south Progreso to north Bishop (respectively).The other two intermediate sampled locations were Harlin...

  1. Spiculitic chert reservoir in Glick Field, South-Central Kansas

    SciTech Connect

    Rogers, J.P.; Longman, M.W.; Lloyd, R.M.

    1995-01-01

    Glick Field, located in Kiowa and Comanche counties of southern Kansas, was discovered in 1957 and has produced more than 362 BCF from Mississippian Osage chert, commonly referred to as the {open_quotes}Chat.{close_quotes} Other {open_quotes}CHAT{close_quotes} reservoirs in Kansas and Oklahoma produce mainly from mixed chert and dolomite beneath the pre-Pennsylvanian unconformity, but Glick Field`s reservoir is dominated by chert containing abundant sponge spicules. Glick Field is a stratigraphic trap with production ending where the spiculitic facies pinches out into tight limestones to the south and west which provide a lateral seal. Additionally, updip, to the northeast, the productive facies is truncated by the unconformity. Reworked chert conglomerates overlying the spiculitic reservoir at the unconformity also produce some gas. The spiculitic chert forming the reservoir was desposited below storm wavebase and grades laterally in all directions into echinoderm and brachiopod-rich skeletal wackestones and lime mudstones. Even where completely silicified, these associated limestone are tight. Thus, the reservoir is an in situ oval-shaped complex of internally brecciated sponge mats and bioherms capped in part by the chert conglomerate. The spiculitic chert contains up to 50% porosity in molds after sponge spicules, matrix micropores and vugs are connected in part by fracture and breccia porosity. Distribution of the sponge bioherms which form the reservoir facies was partly controlled by a subtle change on the shallow Mississippian carbonate shelf from clean skeletal limestones southward into shaly (and probably more anoxic) carbonates known locally as the {open_quotes}Cowley Facies.{close_quotes} The sponge bioherms formed most commonly just updip from this boundary, which can be mapped across southern Kansas. Thus, lithologic mapping provides a potential exploration tool with which to find other stratigraphically trapped spiculitic reservoirs in the area.

  2. Subsidence and well failure in the South Belridge Diatomite field

    SciTech Connect

    Rouffignac, E.P. de; Bondor, P.L.; Karanikas, J.M. Hara, S.K.

    1995-12-31

    Withdrawal of fluids from shallow, thick and low strength rock can cause substantial reservoir compaction leading to surface subsidence and well failure. This is the case for the Diatomite reservoir, where over 10 ft of subsidence have occurred in some areas. Well failure rates have averaged over 3% per year, resulting in several million dollars per year in well replacement and repair costs in the South Belridge Diatomite alone. A program has been underway to address this issue, including experimental, modeling and field monitoring work. An updated elastoplastic rock law based on laboratory data has been generated which includes not only standard shear failure mechanisms but also irreversible pore collapse occurring at low effective stresses (<150 psi). This law was incorporated into a commercial finite element geomechanics simulator. Since the late 1980s, a network of level survey monuments has been used to monitor subsidence at Belridge. Model predictions of subsidence in Section 33 compare very well with field measured data, which show that water injection reduces subsidence from 7--8 inches per year to 1--2 inches per year, but does not abate well failure.

  3. A Comment on "Evaluation Field Building in South Asia: Reflections, Anecdotes, and Questions"

    ERIC Educational Resources Information Center

    Kumar, A. K. Shiva

    2010-01-01

    This paper presents the author's comment on "Evaluation Field Building in South Asia: Reflections, Anecdotes, and Questions" by Katherine Hay. Hay raises a number of extremely relevant issues relating to evaluation field building in South Asia. In this paper, the author aims to underscore the importance of three priorities for initiating public…

  4. Fracturing results in diatomaceous earth formations, South Belridge Field, California

    SciTech Connect

    Strubhar, M.K.; Medin, W.L.

    1982-09-01

    Fracturing significantly increases light oil production rates at South Belridge making this an economically successful technique for exploitation of the Reef Ridge reservoir. No fracturing mechanics problems were encountered in any of the treatments. The loosely consolidated formations behaved mechanically much like brittle, elastic rocks. Net oil and gross production is typified by initial high rates and an early rapid decline. The major cause of this early rapid decline is the transient flow effect. This behavior is typical of low permeability oil and gas production. Fractures are vertical, as shown by gamma ray and temperature logs run following several treatments. The fractures grow slightly out of the perforated intervals (10 to 15 feet). Loss of fracture conductivity due to fines migration, scale deposition, and/or fracture healing (imbedment) is not a serious problem. Oil viscosity can vary as much as ten-fold. Some wells produce significant amounts of gas--100 to 200 MCFPD initially. The formation is primarily diatomaceous earth which is very fine particle size siliceous material composed of whole or fragmented diatom tests (skeletons). There is no evidence that clay swelling or dispersion is a problem. Field and laboratory data support this conclusion. Aqueous fracturing fluids were successfully used which confirmed laboratory tests on cores.

  5. Opium Field Detection in South Oxfordshire Using SAR Polarimetry

    NASA Astrophysics Data System (ADS)

    Walker, Nick; Marino, Armando

    2011-03-01

    To-date the use of satellite imagery to monitor the growth of illicit crops such as marijuana, opium and coca has mostly been conducted using optical frequencies. However, it is well known that while optical imagery can be hampered by localised aerosols such as thin clouds, cirrus, haze and smoke, these do not present a problem for Synthetic Aperture Radar (SAR). In recent years a new generation of satellite borne sensors have also been equipped with enhanced polarimetric capabilities, which can potentially help with detecting and classifying different terrain types. For these reasons we believe it is useful to consider whether high resolution polarimetric SAR data can be applied to illicit crop detection.In this paper we present the results of an experiment whereby opium poppy fields were successfully detected in the south Oxfordshire region in the UK using RadarSat-2 quad-polarisation imagery. It should be noted that these crops are not being grown illicitly but instead are being cultivated for medicinal reasons in parts of the UK. It is interesting to note that the poppies cultivated for opium in the UK have white flowers rather than the more familiar red as can be seen from the photograph in Figure 1, which was taken 11 days earlier in the season compared to Figure 4 and Figure 5.

  6. Galaxy Merger Identification in the CANDELS GOODS-South Field

    NASA Astrophysics Data System (ADS)

    O'Leary, Erin M.; Kartaltepe, J. S.

    2013-01-01

    We analyzed a catalog of 7,628 galaxies at 0South field in order to identify a sample of galaxy mergers and interactions. Mergers are believed to play a fundamental role in galaxy evolution. Developing methods to robustly and efficiently identify mergers becomes vital as we look to higher redshifts. We explored merger identification based on visual morphology classification and preliminary attempts with automated methods. Using multiple detailed visual morphology classifications for each galaxy conducted by the CANDELS structure and morphology team, we created selection criteria to identify mergers from this visual classification catalog. We chose galaxies with high interaction classification and evidence of merger signatures (i.e. tidal features, double nuclei) to generate a catalog of 1051 galaxies we are confident are mergers. This represents a conservative sample of possible mergers. For comparison, we also tested automated merger identification techniques previously used for lower redshift (z<1) galaxies. This is one of the first large investigations of galaxy mergers at z>1. O’Leary was supported by the NOAO/KPNO Research Experiences for Undergraduates (REU) Program which is funded by the National Science Foundation Research Experiences for Undergraduates Program and the Department of Defense ASSURE program through Scientific Program Order No. 13 (AST-0754223) of the Cooperative Agreement No. AST-0132798 between the Association of Universities for Research in Astronomy (AURA) and the NSF.

  7. Michael Young and the Curriculum Field in South Africa

    ERIC Educational Resources Information Center

    Hoadley, Ursula

    2015-01-01

    The paper addresses the question of what we should make of Michael Young's recent work with respect to curriculum theory by considering the particular case of South African curriculum reform. The paper thus traces two trajectories: the evolution of Michael Young's ideas over time and South African curriculum reform in the post-apartheid period.…

  8. Wide Field Imaging of the Hubble Deep Field-South Region III: Catalog

    NASA Technical Reports Server (NTRS)

    Palunas, Povilas; Collins, Nicholas R.; Gardner, Jonathan P.; Hill, Robert S.; Malumuth, Eliot M.; Rhodes, Jason; Teplitz, Harry I.; Woodgate, Bruce E.

    2002-01-01

    We present 1/2 square degree uBVRI imaging around the Hubble Deep Field - South. These data have been used in earlier papers to examine the QSO population and the evolution of the correlation function in the region around the HDF-S. The images were obtained with the Big Throughput Camera at CTIO in September 1998. The images reach 5 sigma limits of u approx. 24.4, B approx. 25.6, V approx. 25.3, R approx. 24.9 and I approx. 23.9. We present a catalog of approx. 22,000 galaxies. We also present number-magnitude counts and a comparison with other observations of the same field. The data presented here are available over the world wide web.

  9. Evaluation Field Building in South Asia: Insights from the Rear View Mirror

    ERIC Educational Resources Information Center

    Grob, George F.

    2010-01-01

    The author enjoyed reading Katharine Hay's ambitious and humbling visions for evaluation field building in South Asia. She has successfully positioned herself on a high mountain with a wonderful set of binoculars that enable her to see the entire evaluation landscape of South Asia. She magically sees and describes significant historical forces and…

  10. South Carolina Field Recordings in the Archive of Folk Culture.

    ERIC Educational Resources Information Center

    Hall, Stephanie A., Comp.

    This document describes recordings of the Library of Congress's unique collections of folklife and ethnomusicology from South Carolina. Information given includes length of recording, name of recorder, dates of recording, and content of recording. Recordings include songs, spirituals, hymns, sermons, prayers, dialect tales, and street songs.…

  11. THE SUB-mJy RADIO POPULATION OF THE E-CDFS: OPTICAL AND INFRARED COUNTERPART IDENTIFICATION

    SciTech Connect

    Bonzini, M.; Mainieri, V.; Padovani, P.; Rosati, P.; Kellermann, K. I.; Miller, N.; Tozzi, P.; Balestra, I.; Vattakunnel, S.; Brandt, W. N.; Luo, B.; Xue, Y. Q.

    2012-11-15

    We study a sample of 883 sources detected in a deep Very Large Array survey at 1.4 GHz in the Extended Chandra Deep Field South. This paper focuses on the identification of their optical and infrared (IR) counterparts. We use a likelihood-ratio technique that is particularly useful when dealing with deep optical images to minimize the number of spurious associations. We find a reliable counterpart for 95% of our radio sources. Most of the counterparts (74%) are detected at optical wavelengths, but there is a significant fraction (21%) that are only detectable in the IR. Combining newly acquired optical spectra with data from the literature, we are able to assign a redshift to 81% of the identified radio sources (37% spectroscopic). We also investigate the X-ray properties of the radio sources using the Chandra 4 Ms and 250 ks observations. In particular, we use a stacking technique to derive the average properties of radio objects undetected in the Chandra images. The results of our analysis are collected in a new catalog containing the position of the optical/IR counterpart, the redshift information, and the X-ray fluxes. It is the deepest multi-wavelength catalog of radio sources, which will be used for future study of this galaxy population.

  12. High Latitude Meridional Flow on the Sun May Explain North-South Polar Field Asymmetry

    NASA Technical Reports Server (NTRS)

    Kosak, Katie; Upton, Lisa; Hathaway, David

    2012-01-01

    We measured the flows of magnetic elements on the Sun at very high latitudes by analyzing magnetic images from the Helioseismic and Magnetic Imager (HMI) on the NASA Solar Dynamics Observatory (SDO) Mission. Magnetic maps constructed using a fixed, and north-south symmetric, meridional flow profile give weaker than observed polar fields in the North and stronger than observed polar fields in the South during the decline of Cycle 23 and rise of Cycle 24. Our measurements of the meridional flow at high latitudes indicate systematic north-south differences. In the fall of 2010 (when the North Pole was most visible), there was a strong flow in the North while in the spring of 2011 (when the South Pole was most visible) the flow there was weaker. With these results, we have a possible solution to this polar field asymmetry. The weaker flow in the South should keep the polar fields from becoming too strong while the stronger flow in the North should strengthen the field there. In order to gain a better understanding of the Solar Cycle and magnetic flux transport on the Sun, we need further observations and analyses of the Sun s polar regions in general and the polar meridional flow in particular.

  13. High Latitude Meridional Flow on the Sun May Explain North-South Polar Field Asymmetry

    NASA Technical Reports Server (NTRS)

    Kosak, Katie; Upton, Lisa; Hathaway, David

    2012-01-01

    We measured the flows of magnetic elements on the Sun at very high latitudes by analyzing magnetic images from the Helioseismic and Magnetic Imager (HMI) on the NASA Solar Dynamics Observatory (SDO) Mission. Magnetic maps constructed using a fixed, and north-south symmetric, meridional flow profile give weaker than observed polar fields in the North and stronger than observed polar fields in the South during the decline of Cycle 23 and rise of Cycle 24. Our measurements of the meridional flow at high latitudes indicate systematic north-south differences. There was a strong flow in the North while the flow in the South was weaker. With these results, we have a possible solution to the polar field asymmetry. The weaker flow in the South should keep the polar fields from becoming too strong while the stronger flow in the North should strengthen the field there. In order to gain a better understanding of the Solar Cycle and magnetic flux transport on the Sun, we need further observations and analyses of the Sun's polar regions in general and the polar meridonal flow in particular.

  14. High Latitude Meridional Flow on the Sun May Explain North-South Polar Field Asymmetry

    NASA Technical Reports Server (NTRS)

    Kosak, Katie; Upton, Lisa; Hathaway, David

    2012-01-01

    We measured the flows of magnetic elements on the Sun at very high latitudes by analyzing magnetic images from the Helioseismic and Magnetic Imager (HMI) on the NASA Solar Dynamics Observatory (SDO) Mission. Magnetic maps constructed using a fixed, and north ]south symmetric, meridional flow profile give weaker than observed polar fields in the North and stronger than observed polar fields in the South during the decline of Cycle 23 and rise of Cycle 24. Our measurements of the meridional flow at high latitudes indicate systematic north ]south differences. There was a strong flow in the North while the flow in the South was weaker. With these results, we have a possible solution to the polar field asymmetry. The weaker flow in the South should keep the polar fields from becoming too strong while the stronger flow in the North should strengthen the field there. In order to gain a better understanding of the Solar Cycle and magnetic flux transport on the Sun, we need further observations and analyses of the Sun fs polar regions in general and the polar meridional flow in particular

  15. Mixing of biogenic siliceous and terrigenous clastic sediments: South Belridge field and Beta field, California

    SciTech Connect

    Schwartz, D.E. )

    1990-05-01

    The intermixing and interbedding of biogenically derived siliceous sediment with terrigenous clastic sediment in reservoirs of upper Miocene age provides both reservoir rock and seal and influences productivity by affecting porosity and permeability. Miocene reservoirs commonly contain either biogenic-dominated cyclic diatomite, porcelanite, or chert (classic Monterey Formation) or clastic-dominated submarine fan sequences with interbedded or intermixed siliceous members of biogenic origin. Biogenic-clastic cycles, 30-180 ft thick, at South Belridge field were formed by episodic influx of clastic sediment from distant submarine fans mixing with slowly accumulating diatomaceous ooze. The cycles consist of basal silt and pelletized massive diatomaceous mudstone, overlain by burrowed, faintly bedded clayey diatomite and topped by laminated diatomite. Cycle tops have higher porosity and permeability, lower grain density, and higher oil saturation than clay and silt-rich portions of the cycles. Submarine fan sediments forming reservoirs at the Beta field are comprised of interbedded sands and silts deposited in a channelized middle fan to outer fan setting. Individual turbidites display fining-upward sequences, with oil-bearing sands capped by wet micaceous silts. Average sands are moderately to poorly sorted, fine- to medium-grained arkosic arenites. Sands contain pore-filling carbonate and porcelaneous cements. Porcelaneous cement consists of a mixture of opal-A, opal-CT, and chert with montmorillonite and minor zeolite. This cement is an authigenic material precipitated in intergranular pore space. The origin of the opal is biogenic, with recrystallization of diatom frustules (opal-A) into opal-CT lepispheres and quartz crystals. Porcelaneous cement comprises 4-21% of the bulk volume of the rock. Seventy percent of the bulk volume of the cement is micropore space.

  16. Glacier surface velocity fields in South Shetland Islands

    NASA Astrophysics Data System (ADS)

    Osmanoglu, B.; Giseke, H.; Navarro, F. J.; Rueckamp, M.; Falk, U.; Corcuera, M. I.; Braun, M.

    2011-12-01

    In this study surface velocity of glaciers in South Shetland Islands (Antarctic Peninsula) are calculated based on synthetic aperture radar data from ALOS PALSAR and TerraSAR-X as well as differential GPS measurements. The obtained glacier velocities will be used to calculate the total glacier mass budget and to better understand the contribution of the study areas to the sea level rise. Only recent studies have examined the region for mass balance and sea level rise estimates. However, larger scale mass budget computations are not yet available. Ice dynamics obtained from satellite data have only been derived in a few occasions, often due to lacking spatial resolution or temporal decorrelation. Hence, any spacebased information on ice dynamics can significantly improve estimates of calving fluxes and mass loss. In this study we analysed over 30 PALSAR and 30 TSX scenes acquired over the King George Island and Livingston Island, the two largest islands in the South Shetland Island group. In the study areas the glacier velocities are calculated using two independent data sets; namely satellite radar imagery and GPS. Feature-tracking methods are applied to the radar imagery to obtain glacier velocities using Gamma Interferometric SAR Processor and TU-Delft DORIS. Results from Gamma and Doris software packages are compared to each other as well as GPS measurements where available. For a subset of the study area tracking results from different acquisitions modes (stripmap and spotlight) and orbits are compared. Comparison of glacier velocities obtained by radar and GPS provide an estimate for the uncertainties in the measured rates. The results obtained from all data sets are then compiled to construct a map of glacier velocities for the entire island group.

  17. Bacterial diversity of rice fields in the South of Brazil

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Irrigated rice fields are aquatic agroecosystems directly influenced by agricultural practices, which include agrochemical application and the input of nutrients related to resource of irrigation. In addition, root exudation and the levels of soil mineral nutrients are important modifiers of the rhi...

  18. A brief overview of the history of veterinary field services in South Africa.

    PubMed

    Brückner, Gideon K

    2014-01-01

    The historical evolution of veterinary services in South Africa is closely linked to the colonial history of the past and the eventual political formation of the Union of South Africa in 1910, as well as the establishment of a fully democratic South Africa in 1994. The majority of the early pioneering veterinarians had close links to military activities and were originally mostly of British origin. The appointment of the first colonial chief veterinary officers occurred in the late 1800s. These appointments were dictated by the need to combat devastating animal diseases, such as rinderpest and African horse sickness, mainly because they affected draught oxen (used for travel) and horses (used in combat). Veterinary field services was established in 1962 as a separate functional entity within government services when M.C. Lambrechts became Director of Veterinary Services of South Africa. In the context of this article, veterinary field services refers to that sphere of veterinary service delivery conducted by government-appointed or seconded veterinarians applying disease control and prevention, as required by animal health legislation. Paging through the history of veterinary field services in South Africa confirms that the problems faced by the veterinary services of today were just as real during the times of our pioneers. The pioneers of veterinary services transformed unknown animal diseases into textbook descriptions still used today and also demonstrated the important link to, and use of, the observations made by farmers, as well as the need for continued basic and applied research on animal diseases. This article provided a brief overview of the evolution of veterinary field services and the important role played by pioneers over the last two centuries to make South Africa relatively free and safe from the most important trade-sensitive and economically important animal diseases. PMID:25685939

  19. G-2 and G-3 reservoirs, Delta South field, Nigeria - 2. Simulation of water injection

    SciTech Connect

    Thakur, G.C.; Stanat, P.L.; Aruna, M.; Ajayi, S.A.; Poston, S.

    1982-01-01

    A description is given of a two-dimensional, three-phase, black-oil simulation of the G-2 and G-3 reservoirs in the Delta South field offshore Nigeria. The purpose of these studies was to investigate, from an engineering standpoint, various operating schemes for optimizing the oil recovery from each of these highly gravity-segregated reservoirs. 4 refs.

  20. South Lake Arthur field and occurrence of buried structures along Oligocene trend of southwestern Louisiana

    SciTech Connect

    Prescott, M.P.

    1988-09-01

    Significant gas reserves have recently been discovered in the Miogypsinoides sands along the Oligocene trend at the South Lake Arthur field. Detailed subsurface maps and seismic data are presented to exhibit the extent and nature of this local structure and to demonstrate future opportunities along the Oligocene trend.

  1. Soccer field at West 101st102nd streets, Riverside Park, looking south ...

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

    Soccer field at West 101st-102nd streets, Riverside Park, looking south with railroad retaining wall in background. - Henry Hudson Parkway, Extending 11.2 miles from West 72nd Street to Bronx-Westchester border, New York County, NY

  2. Summary of South Fence Road phase II 1993 field operations at Site SFR-4

    SciTech Connect

    Foutz, W.L.; McCord, J.P.

    1996-05-01

    This report is a basic data report for field operations associated with the drilling, logging, completion, and development of South Fence Road Wells SFR-4P and SFR-4T. These test/monitoring wells were installed as part of Sandia National Laboratories, New Mexico, Environmental Restoration Project.

  3. Summary of South Fence Road phase II 1993 field operations at site SFR-3

    SciTech Connect

    Foutz, W.L.; McCord, J.P.

    1996-05-01

    This report is a basic data report fro field operations associated with the drilling, logging, completion, and development of South Fence Road Wells SFR-3P and SFR-3T. These test/monitoring wells were installed as part of Sandia National Laboratories, New Mexico, Environmental Restoration Project.

  4. High-Resolution Local Crustal Magnetic Field Modeling of the Martian South Pole

    NASA Astrophysics Data System (ADS)

    Plattner, A.; Simons, F. J.

    2014-12-01

    The Mars Global Surveyor (MGS) satellite mission has brought us a wealth of information about the Martian magnetic field. Besides determining that Mars currently does not possess an active core field, MGS revealed that Mars contains an unexpectedly wide crustal magnetic field intensity range. In its orbit insertion, MGS performed a series of low altitude passes down to around 100 km above surface. During this mission phase the magnetic field measurements were active. In particular the nighttime low-altitude data are of high interest because they contain minimal noise from solar wind. Since these data only cover a small portion of the planet's surface, to date all Martian crustal magnetic field models blend the highest-quality data with lower quality measurements collected either at higher satellite altitudes or during daytime. In this contribution we present a locally inverted crustal magnetic field model for the Martian South Polar region calculated from only the highest-quality MGS data using locally constructed altitude vector Slepian functions. The South Polar region of Mars contains the southern part of the strongly magnetized Terra Sirenum and the area south of the Tharsis volcanic highland. Besides parts of planetary scale features our area of data coverage also contains local features such as the presumably volcanic Australe Montes and the Prometheus impact crater. These ingredients compose a highly heterogeneous crustal magnetic field. We show that even for our dense low-altitude low-noise data set the inversion for the crustal magnetic field of a weakly magnetized region adjacent to a region containing a strong magnetic field leads to artifacts in the weak region. With our local method we can avoid these artifacts by selecting subregions of roughly homogeneous field intensity and individually invert for crustal magnetic fields from data within only these subregions. This regional and subregional modeling allows us to reveal previously obscured crustal

  5. Estimated north-south conponent of the electric field in the geomagnetotail plasma sheet

    SciTech Connect

    Lui, A.T.Y.; Akasofu, S.

    1980-11-01

    It is shown that the north-south component of electric fields in the plasma sheet can be estimated uniquely from simultaneous measurements of plasma flow components (v/sub x/, v/sub y/) and the magnetic field components (B/sub x/, B/sub y/) in the equatorial plane. The estimated field strength ranges from 0.3 to 7.8 mv/m during substorms at geocentric distances beyond approx.15 R/sub e/. During the magnetospheric substorm expansion phase, the north-south component of the electric fields is almost oppositely directed from what one would expect on the basis of projection of the general pattern of the ionospheric electric field to the plasma sheet along geomagnetic field lines (assumed to be equipotential). It is only during the recovery phase when both electric field patterns become similar. The result also suggests that strong fields occur preferentially near the plasma sheet boundary rather than near the neutral sheet region.

  6. Palaeomagnetic evidence for the persistence or recurrence of geomagnetic main field anomalies in the South Atlantic

    NASA Astrophysics Data System (ADS)

    Shah, Jay; Koppers, Anthony A. P.; Leitner, Marko; Leonhardt, Roman; Muxworthy, Adrian R.; Heunemann, Christoph; Bachtadse, Valerian; Ashley, Jack A. D.; Matzka, Jürgen

    2016-05-01

    We present a dataset of a full-vector palaeomagnetic study of Late Pleistocene lavas from the island Tristan da Cunha in the South Atlantic Ocean. The current day geomagnetic field intensity in this region is approximately 25 μT, compared to an expected value of ∼43 μT; this phenomenon is known as the South Atlantic geomagnetic Anomaly (SAA). Geomagnetic field models extending back to the last 10 ka find no evidence for this being a persistent feature of the geomagnetic field, albeit, all models are constructed from data which is particularly sparse in the southern hemisphere. New 40Ar/39Ar incremental heating dating indicates the studied lavas from Tristan da Cunha extruded between 90 and 46 ka. Palaeointensity estimations of eight lava flows made using the Thellier method yield an average palaeointensity of 18 ± 6 μT and virtual axial dipole moment (VADM) of 3.1 ± 1.2 ×1022 Am2. The lava flows demonstrate four time intervals comparable to the present day SAA, where the average VADM of the Tristan da Cunha lavas is weaker than the global VADM average. This suggests a persistent or recurring low intensity anomaly to the main geomagnetic field similar to the SAA existed in the South Atlantic between 46 and 90 ka.

  7. Measuring the economic impact of climate change on major South African field crops: a Ricardian approach

    NASA Astrophysics Data System (ADS)

    Gbetibouo, G. A.; Hassan, R. M.

    2005-07-01

    This study employed a Ricardian model to measure the impact of climate change on South Africa's field crops and analysed potential future impacts of further changes in the climate. A regression of farm net revenue on climate, soil and other socio-economic variables was conducted to capture farmer-adapted responses to climate variations. The analysis was based on agricultural data for seven field crops (maize, wheat, sorghum, sugarcane, groundnut, sunflower and soybean), climate and edaphic data across 300 districts in South Africa. Results indicate that production of field crops was sensitive to marginal changes in temperature as compared to changes in precipitation. Temperature rise positively affects net revenue whereas the effect of reduction in rainfall is negative. The study also highlights the importance of season and location in dealing with climate change showing that the spatial distribution of climate change impact and consequently needed adaptations will not be uniform across the different agro-ecological regions of South Africa. Results of simulations of climate change scenarios indicate many impacts that would induce (or require) very distinct shifts in farming practices and patterns in different regions. Those include major shifts in crop calendars and growing seasons, switching between crops to the possibility of complete disappearance of some field crops from some region.

  8. Generation of a North/South Magnetic Field Component from Variations in the Photospheric Magnetic Field

    NASA Astrophysics Data System (ADS)

    Ulrich, Roger K.; Tran, Tham

    2016-04-01

    We address the problem of calculating the transverse magnetic field in the solar wind outside of the hypothetical sphere that is called the source surface where the solar wind originates. This calculation must overcome a widely used fundamental assumption about the source surface - the field is normally required to be purely radial at the source surface. Our model rests on the fact that a change in the radial field strength at the source surface is a change in the field line density. Surrounding field lines must move laterally to accommodate this field line density change. As the outward wind velocity drags field lines past the source surface, this lateral component of motion produces a tilt, implying there is a transverse component to the field. An analytic method of calculating the lateral translation speed of the field lines is developed. We apply the technique to an interval of approximately two Carrington rotations at the beginning of 2011 using 2-h averages of data from the Helioseismic Magnetic Imager instrument onboard the Solar Dynamics Observatory spacecraft. We find that the value of the transverse magnetic field is dominated on a global scale by the effects of high-latitude concentrations of field lines that are buffeted by supergranular motions.

  9. Estimates of the North--South electric field component in the magnetotail low latitude boundary layer

    SciTech Connect

    Candidi, M.; Orsini, S.

    1981-06-01

    The measurements of 0/sup +/ ions drift velocity in the magnetotail boundary layer are used to infer the North--South E/sub z/ component of the local electric field. It is shown that E/sub z/ is generally a substantial component of the field and that it reverses its sign from the dawn to the dusk side of the northern magnetotail between X/sub SM/ = -15 R/sub E/ and X/sub SM/ = -23 R/sub E/.

  10. Study on the time difference of solar polar field reversal between the north and south hemisphere

    NASA Astrophysics Data System (ADS)

    Shukuya, D.; Kusano, K.

    2013-12-01

    Dynamo is a mechanism whereby the kinetic energy of plasma is converted to the magnetic energy. This mechanism works to generate and maintain the solar and stellar magnetic field. Since the sun is only a star whose magnetic field can be directly observed, the understanding of solar dynamo can provide clues to clarify dynamo mechanisms. On the other hand, because solar activities, which are caused by solar dynamo, can influence the Earth's climate, solar variability is an important issue also to understand long-term evolution of the Earth's climate. It is widely known that the polarity of the solar magnetic fields on the north and south poles periodically reverses at every sunspot maxima. It is also known that the reversal at one pole is followed by that on the other pole. The time difference of magnetic field reversal between the poles was first noted by Babcock (1959) from the very first observation of polar field. Recently, it was confirmed by detailed observations with the HINODE satellite (Shiota et al. 2012). Svalgaard and Kamide (2013) indicated that there is a relationship between the time difference of the polarity reversal and the hemispheric asymmetry of the sunspot activity. However, the mechanisms for the hemispheric asymmetry are still open to be revealed. In this paper, we study the asymmetric feature of the solar dynamo based on the flux transport dynamo model (Chatterjee et al. 2004) to explain the time difference of magnetic polarity reversal between the north and south poles. In order to calculate long-term variations of solar activities, we use the mean field kinematic dynamo model, which is derived from magnetohydrodynamics (MHD) equation through the mean field and other approximations. We carried out the mean field dynamo simulations using the updated SURYA code which was developed originally by Choudhuri and his collaborators (2004). We decomposed the symmetric and asymmetric components of magnetic field, which correspond respectively to the

  11. Rotation of the photospheric magnetic fields: A north-south asymmetry

    NASA Technical Reports Server (NTRS)

    Antonucci, E.; Hoeksema, J. T.; Scherrer, P. H.

    1989-01-01

    During most of solar cycle 21 the large-scale photospheric field rotated more rapidly in the Northern Hemisphere than in the southern. The large-scale northern field rotated with a 26.9 day period (synodic), was centered at 15 degress N, and covered a latitude zone about 24 degrees wide. The large-scale southern field rotated with a periodicity of 28.1 days, was centered at 26 degrees S, and covered a latitude zone about 32 degrees wide. Our analysis showed rotational power at only a few discrete latitudes and frequencies in each hemisphere. The center of each peak lies near the sunspot differential rotation curve. The largest scale field contributes to the configuration of the coronal and interplanetary magnetic field (IMF). The strength of the first harmonic of the northern field suggests that this structure may be related to the 4-sector pattern observed in the IMF polarity. The southern field had much lower power at the first harmonic of the solar rotation rate and so would contribute only to a 2-sector structure in the IMF. These results were discovered in Fourier analysis of photospheric synoptic charts obtained at the Wilcox Solar Observatory from 1976 to 1986 and confirmed in higher resolution maps from the National Solar Observatory. Mt. Wilson magnetic field measurements from solar cycle 20 show a similar north-south asymmetry.

  12. Genetic type of natural gas in Ya13-1 gas field, South China Sea

    SciTech Connect

    Zhang Gang

    1995-08-01

    Ya13-1 is one of the largest gas field ever found in China in recent years. Studying on the genetic type of natural gas in the field is one of the key factors to determine the regional hydrocarbon potential--Qiongdongnan Basin and Yinggerhaii Basin, northwest part of South China Sea. Series of geochemical methods have been undertook including the analysis of the chemical composition of the natural gas and their isotopic ratio discussed in this paper. Other related studied including geological settings, gas-source correlations, geochemistry of the condensates and extractable compounds of source rocks, and thermal simulation and evaluation of the marine shales provides further informations. It is noticeable that the higher content of mercury (44000 ng/cubic meter) and aromatics such as benzene and toluene may be related to the joint of condensates, which derived from coal-bearing Oligocene shales in the adjacent Qingdingnan Basin. Studies show that the natural gas in Ya13-1 gas field belong to high to post mature non-associated gas derived in marine source rocks, and mainly come from Oligocene to Pliocene marine shales in Yinggerhai Basin. This is quite different with the former studies, which believe the gas derived from Oligocene coal-bearing strata of Yacheng formation, Qiongdongnan Basin. The new results of the studies make sure further a pretty good potential of gas resources in the northwest part ofSouth China Sea.

  13. Infrared Faint Radio Sources in the Extended Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Huynh, Minh T.

    2009-01-01

    Infrared-Faint Radio Sources (IFRSs) are a class of radio objects found in the Australia Telescope Large Area Survey (ATLAS) which have no observable counterpart in the Spitzer Wide-area Infrared Extragalactic Survey (SWIRE). The extended Chandra Deep Field South now has even deeper Spitzer imaging (3.6 to 70 micron) from a number of Legacy surveys. We report the detections of two IFRS sources in IRAC images. The non-detection of two other IFRSs allows us to constrain the source type. Detailed modeling of the SED of these objects shows that they are consistent with high redshift AGN (z > 2).

  14. Long period pulsation events in electron precipitation and magnetic fields at the South Pole

    SciTech Connect

    Paquette, J.A.

    1992-01-01

    Geomagnetic pulsation events with long (100-1000 second) periods that are accompanied by electron precipitation pulsations at the same frequency were reported at various latitudes. A search of the data from South Pole station for the period from 1982 to 1989 revealed over 200 such events. A comparison of these events with the predictions of Coroniti and Kennel was undertaken, including examination of VLF data, interplanetary magnetic field data, DMSP satellite data, and data from South Pole's conjugate station at Iqaluit, as well as the riometer and magnetometer data from South Pole used in the original search. Data from the IRIS Imaging Radiometer were also used when available. A consideration of the respective wave and particle transit times from the magnetic equator to the ground leads to an expectation that the onset of pulsations in the magnetometer data will lag the onset of pulsations in the riometer data by several minutes. This disparity in onset times, together with VLF modulation in the proper frequency range, serve as important indicators of whether or not an event can be explained by the above-cited theory. While about a third of the events fit the prediction of Coroniti and Kennel, another third cannot be explained by this theory, and possible alternative mechanisms are explored. The remaining third of the events appear at first to be inexplicable in terms of any transit time argument, but analysis of the IRIS data shows that this third class of events arises from differences in the spatial coverage of the instruments.

  15. Balloon observations of ultra-low-frequency waves in the electric field above the South Pole

    SciTech Connect

    Liao, B.; Benbrrook, J.R.; Bering E.A. III; Byrne, G.J.; Theall, J.R. )

    1988-01-01

    The physics of ultra-low-frequency waves in the magnetosphere, near the cusp and in the polar cap, is important because this region is one where ultra-low-frequency wave energy from the magnetopause can most easily enter the magnetosphere. During the 1985-1986 South Pole balloon campaign, eight stratospheric balloon payloads were launched from Amundsen-Scott Station, South Geographic Pole, Antarctica, to record data on ultra-low-frequency waves. The payloads were instrumented with three-axis double-probe electric field detectors and X-ray scintillation counters. This paper concentrates on the third flight of this series, which was launched at 2205 universal time on 21 December 1985. Good data were received from the payload until the transmitter failed at 0342 universal time on 22 December. During most of the four hours that the balloon was afloat, an intense ultra-low-frequency wave event was in progress. The electric-field data from this period have been examined in detail and compared with magnetic field data, obtained with ground-based fluxgate and induction magnetometers to determine the characteristics of the waves. After float was reached, the electric-field data in figure 1 show large-amplitude, quasi-periodic fluctuations suggesting the presence of intense ultra-low-frequency wave activity. In conclusion, the electric-field signature observed from flight 3 appears to have been essentially an electrostatic event or possibly a short-wavelength hydromagnetic wave with a varying and interesting polarization character. The authors are continuing the analysis of the data to determine the source of the observed ultra-low-frequency waves.

  16. NEAR-INFRARED-IMAGING POLARIMETRY TOWARD SERPENS SOUTH: REVEALING THE IMPORTANCE OF THE MAGNETIC FIELD

    SciTech Connect

    Sugitani, K.; Nakamura, F.; Tamura, M.; Kandori, R.; Watanabe, M.; Nishiyama, S.; Nagata, T.; Nagayama, T.; Sato, S.; Gutermuth, R. A.; Wilson, G. W.; Kawabe, R.

    2011-06-10

    The Serpens South embedded cluster, which is located in the constricted part of a long, filamentary, infrared dark cloud, is believed to be in a very early stage of cluster formation. We present results of near-infrared (JHKs) polarization observations of the filamentary cloud. Our polarization measurements of near-infrared point sources indicate a well-ordered global magnetic field that is perpendicular to the main filament, implying that the magnetic field is likely to have controlled the formation of the main filament. On the other hand, the sub-filaments, which converge on the central part of the cluster, tend to run along the magnetic field. The global magnetic field appears to be curved in the southern part of the main filament. Such morphology is consistent with the idea that the global magnetic field is distorted by gravitational contraction along the main filament toward the northern part, which contains larger mass. Applying the Chandrasekhar-Fermi method, the magnetic field strength is roughly estimated to be a few x100 {mu}G, suggesting that the filamentary cloud is close to magnetically critical.

  17. North-South Asymmetries in Earth's Magnetic Field - Effects on High-Latitude Geospace

    NASA Astrophysics Data System (ADS)

    Laundal, K. M.; Cnossen, I.; Milan, S. E.; Haaland, S. E.; Coxon, J.; Pedatella, N. M.; Förster, M.; Reistad, J. P.

    2016-07-01

    The solar-wind magnetosphere interaction primarily occurs at altitudes where the dipole component of Earth's magnetic field is dominating. The disturbances that are created in this interaction propagate along magnetic field lines and interact with the ionosphere-thermosphere system. At ionospheric altitudes, the Earth's field deviates significantly from a dipole. North-South asymmetries in the magnetic field imply that the magnetosphere-ionosphere-thermosphere (M-I-T) coupling is different in the two hemispheres. In this paper we review the primary differences in the magnetic field at polar latitudes, and the consequences that these have for the M-I-T coupling. We focus on two interhemispheric differences which are thought to have the strongest effects: 1) A difference in the offset between magnetic and geographic poles in the Northern and Southern Hemispheres, and 2) differences in the magnetic field strength at magnetically conjugate regions. These asymmetries lead to differences in plasma convection, neutral winds, total electron content, ion outflow, ionospheric currents and auroral precipitation.

  18. Traditional Geology Field Camp: A capstone course at South Dakota School of Mines and Technology (BHNSFS)

    NASA Astrophysics Data System (ADS)

    Uzunlar, N.; Lisenbee, A. L.

    2012-12-01

    The Black Hills Natural Sciences Field Station (BHNSFS) has provided field training in geology and geological engineering for more than 40 years, and since the 1980's as a consortium serving five schools with South Dakota School of Mines and Technology as the coordinator. The traditional summer geology field camp is a five week long, intense program aimed to prepare students for subsequent professional geologic experiences. It is delivered from two separate facilities, one in the Black Hills (South Dakota) from a beautiful log lodge along Sand Creek, in eastern Wyoming, and a second from the town of Taskesti along the North Anatolian fault approximately 200 km east of Istanbul, Turkey. At both locations, the courses maintain a strong emphasis on basic field applications, including the use of GPS as a mapping tool in most exercises. The preparation of well-written reports, based on field descriptions supplemented by research on the web or through published documents, is strongly emphasized. Projects at the Black Hills field camp includes mapping of Precambrian basement, Paleozoic stratigraphy, and Laramide Tertiary plutons and structural features as welll as post-Laramide,, faulted continental strata. The popular Taskesti field camp utilizes the diverse geology of the Tethyan realm, as well as the culture and history, of central Turkey (Anatolia). The course is based at a Turkish Government Earthquake Research Center facility along the North Anatolian fault. Students examine and map selected locations across the Izmir-Ankara suture including: 1) Deformed Cretaceous and Tertiary carbonate and clastic strata of the Sakarya micro-continent in a fore-arc basin; 2) Marble and skarn surrounding Eocene, subduction-related granite intruded into a passive margin sequence in the Sivrihisar region of central Anatolia; 3) Faulted and folded Neogene strata in the northern flank of the post-Tethyan, Haymana Basin and the contrasting terrains across the North Anatolian fault (J

  19. Numerical simulation of wave field in the South China Sea using WAVEWATCH III

    NASA Astrophysics Data System (ADS)

    Zhou, Liangming; Li, Zhanbin; Mou, Lin; Wang, Aifang

    2014-05-01

    Wave fields of the South China Sea (SCS) from 1976 to 2005 were simulated using WAVEWATCH III by inputting high-resolution reanalysis wind field datasets assimilated from several meteorological data sources. Comparisons of wave heights between WAVEWATCH III and TOPEX/Poseidon altimeter and buoy data show a good agreement. Our results show seasonal variation of wave direction as follows: 1. During the summer monsoon (April-September), waves from south occur from April through September in the southern SCS region, which prevail taking about 40% of the time; 2. During the winter monsoon (December-March), waves from northeast prevail throughout the SCS for 56% of the period; 3. The dominant wave direction in SCS is NE. The seasonal variation of wave height H s in SCS shows that in spring, H s ≥1 m in the central SCS region and is less than 1 m in other areas. In summer, H s is higher than in spring. During September-November, influenced by tropical cyclones, H s is mostly higher than 1 m. East of Hainan Island, H s>2 m. In winter, H s reaches its maximum value influenced by the north-east monsoon, and heights over 2 m are found over a large part of SCS. Finally, we calculated the extreme wave parameters in SCS and found that the extreme wind speed and wave height for the 100-year return period for SCS peaked at 45 m/s and 19 m, respectively, SE of Hainan Island and decreased from north to south.

  20. The MUSE 3D view of the Hubble Deep Field South

    NASA Astrophysics Data System (ADS)

    Bacon, R.; Brinchmann, J.; Richard, J.; Contini, T.; Drake, A.; Franx, M.; Tacchella, S.; Vernet, J.; Wisotzki, L.; Blaizot, J.; Bouché, N.; Bouwens, R.; Cantalupo, S.; Carollo, C. M.; Carton, D.; Caruana, J.; Clément, B.; Dreizler, S.; Epinat, B.; Guiderdoni, B.; Herenz, C.; Husser, T.-O.; Kamann, S.; Kerutt, J.; Kollatschny, W.; Krajnovic, D.; Lilly, S.; Martinsson, T.; Michel-Dansac, L.; Patricio, V.; Schaye, J.; Shirazi, M.; Soto, K.; Soucail, G.; Steinmetz, M.; Urrutia, T.; Weilbacher, P.; de Zeeuw, T.

    2015-03-01

    We observed Hubble Deep Field South with the new panoramic integral-field spectrograph MUSE that we built and have just commissioned at the VLT. The data cube resulting from 27 h of integration covers one arcmin2 field of view at an unprecedented depth with a 1σ emission-line surface brightness limit of 1 × 10-19 erg s-1 cm-2 arcsec-2, and contains ~90 000 spectra. We present the combined and calibrated data cube, and we performed a first-pass analysis of the sources detected in the Hubble Deep Field South imaging. We measured the redshifts of 189 sources up to a magnitude I814 = 29.5, increasing the number of known spectroscopic redshifts in this field by more than an order of magnitude. We also discovered 26 Lyα emitting galaxies that are not detected in the HST WFPC2 deep broad-band images. The intermediate spectral resolution of 2.3 Å allows us to separate resolved asymmetric Lyα emitters, [O ii]3727 emitters, and C iii]1908 emitters, and the broad instantaneous wavelength range of 4500 Å helps to identify single emission lines, such as [O iii]5007, Hβ, and Hα, over a very wide redshift range. We also show how the three-dimensional information of MUSE helps to resolve sources that are confused at ground-based image quality. Overall, secure identifications are provided for 83% of the 227 emission line sources detected in the MUSE data cube and for 32% of the 586 sources identified in the HST catalogue. The overall redshift distribution is fairly flat to z = 6.3, with a reduction between z = 1.5 to 2.9, in the well-known redshift desert. The field of view of MUSE also allowed us to detect 17 groups within the field. We checked that the number counts of [O ii]3727 and Lyα emitters are roughly consistent with predictions from the literature. Using two examples, we demonstrate that MUSE is able to provide exquisite spatially resolved spectroscopic information on the intermediate-redshift galaxies present in the field. Thisunique data set can be used for a

  1. VizieR Online Data Catalog: Spitzer-CANDELS catalog within 5 deep fields (Ashby+, 2015)

    NASA Astrophysics Data System (ADS)

    Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.; Dunlop, J. S.; Egami, E.; Faber, S. M.; Ferguson, H. C.; Grogin, N. A.; Hora, J. L.; Huang, J.-S.; Koekemoer, A. M.; Labbe, I.; Wang, Z.

    2015-08-01

    We chose to locate S-CANDELS inside the wider and shallower fields already covered by Spitzer Extended Deep Survey (SEDS), in regions that enjoy deep optical and NIR imaging from HST/CANDELS. These S-CANDELS fields are thus the Extended GOODS-south (aka the GEMS field, hereafter ECDFS; Rix et al. 2004ApJS..152..163R; Castellano et al. 2010A&A...511A..20C), the Extended GOODS-north (HDFN; Giavalisco et al. 2004, II/261; Wang et al. 2010, J/ApJS/187/251; Hathi et al. 2012ApJ...757...43H; Lin et al. 2012ApJ...756...71L), the UKIDSS UDS (aka the Subaru/XMM Deep Field, Ouchi et al. 2001ApJ...558L..83O; Lawrence et al. 2007, II/319), a narrow field within the EGS (Davis et al. 2007ApJ...660L...1D; Bielby et al. 2012A&A...545A..23B), and a strip within the UltraVista deep survey of the larger COSMOS field (Scoville et al. 2007ApJS..172...38S; McCracken et al. 2012, J/A+A/544/A156). The S-CANDELS observing strategy was designed to maximize the area covered to full depth within the CANDELS area. Each field was visited twice with six months separating the two visits. Table 1 lists the epochs for each field. All of the IRAC full-depth coverage is within the SEDS area (Ashby et al. 2013, J/ApJ/769/80), and almost all is within the area covered by HST for CANDELS. (6 data files).

  2. Secondary natural gas recovery in mature fluvial sandstone reservoirs, Frio Formation, Agua Dulce Field, South Texas

    SciTech Connect

    Ambrose, W.A.; Levey, R.A. ); Vidal, J.M. ); Sippel, M.A. ); Ballard, J.R. ); Coover, D.M. Jr. ); Bloxsom, W.E. )

    1993-09-01

    An approach that integrates detailed geologic, engineering, and petrophysical analyses combined with improved well-log analytical techniques can be used by independent oil and gas companies of successful infield exploration in mature Gulf Coast fields that larger companies may consider uneconomic. In a secondary gas recovery project conducted by the Bureau of Economic Geology and funded by the Gas Research Institute and the U.S. Department of Energy, a potential incremental natural gas resource of 7.7 bcf, of which 4.0 bcf may be technically recoverable, was identified in a 490-ac lease in Agua Dulce field. Five wells in this lease had previously produced 13.7 bcf from Frio reservoirs at depths of 4600-6200 ft. The pay zones occur in heterogeneous fluvial sandstones offset by faults associated with the Vicksburg fault zone. The compartments may each contain up to 1.0 bcf of gas resources with estimates based on previous completions and the recent infield drilling experience of Pintas Creek Oil Company. Uncontacted gas resources occur in thin (typically less than 10 ft) bypassed zones that can be identified through a computed log evaluation that integrates open-hole logs, wireline pressure tests, fluid samples, and cores. At Agua Dulce field, such analysis identified at 4-ft bypassed zone uphole from previously produced reservoirs. This reservoir contained original reservoir pressure and flowed at rates exceeding 1 mmcf/d. The expected ultimate recovery is 0.4 bcf. Methodologies developed in the evaluation of Agua Dulce field can be successfully applied to other mature gas fields in the south Texas Gulf Coast. For example, Stratton and McFaddin are two fields in which the secondary gas recovery project has demonstrated the existence of thin, potentially bypassed zones that can yield significant incremental gas resources, extending the economic life of these fields.

  3. North south asymmetry in the photospheric and coronal magnetic fields observed by different instruments

    NASA Astrophysics Data System (ADS)

    Virtanen, Ilpo; Mursula, Kalevi

    2015-04-01

    Several recent studies have shown that the solar and heliospheric magnetic fields are north-south asymmetric. The southward shift of the Heliospheric current sheet (HCS) (the so-called bashful ballerina phenomenon) is a persistent pattern, which occurs typically for about three years during the late declining phase of solar cycle. We study here the hemispherical asymmetry in the photospheric and coronal magnetic fields using Wilcox Solar Observatory (WSO), Mount Wilson, Kitt Peak, Solis, SOHO/MDI and SDO/HMI measurements of the photospheric magnetic field since the 1970s and the potential field source surface (PFSS) model.Multipole analysis of the photospheric magnetic field has shown that the bashful ballerina phenomenon is a consequence of g20 quadrupole term, which is oppositely signed to the dipole moment. We find that, at least during the four recent solar cycles, the g20 reflects the larger magnitude of the southern polar field during a few years in the declining phase of the cycle. Although the overall magnetic activity during the full solar cycle is not very different in the two hemispheres, the temporal distribution of activity is different, contributing to the asymmetry. The used data sets are in general in a good agreement with each other, but there are some significant deviations, especially in WSO data. Also, the data from Kitt Peak 512 channel magnetograph is known to suffer from zero level errors.We also note that the lowest harmonic coefficients do not scale with the overall magnitude in photospheric synoptic magnetic maps. Scaling factors based on histogram techniques can be as large as 10 (from Wilcox to HMI), but the corresponding difference in dipole strength is typically less than two. This is because the polar field has a dominant contribution to the dipole and quadrupole components. This should be noted, e.g., when using synoptic maps as input for coronal models.

  4. Magnetic fields on the sun and the north-south component of transient variations of the interplanetary magnetic field at 1 AU

    NASA Technical Reports Server (NTRS)

    Tang, F.; Akasofu, S.-I.; Smith, E.; Tsurutani, B.

    1985-01-01

    In order to study the relationship between solar magnetic fields and the transient variations of the north-south component B(Z) of the interplanetary magnetic field (IMF) at 1 AU, flares from unusual north-south oriented active regions, large IMF B(Z) events, and large flares with comprehensive flare index higher than 12 were collected. The associated IMF B(Z) changes or the magnetic field of the initiating flares are investigated. For those cases where an association between a transient B(Z) variation and an initiating flare is plausible, it is found that, for a given flare field, the orientation of the corresponding transient variation of B(Z) may be in agreement with the flare field, opposite to it, or more often, fluctuating in both magnitude and direction. Conversely, an IMF B(Z) event may originate in a flare field in the same magnetic orientation, opposite to it, or in the east-west orientation.

  5. Well kill (quenching) study of thermal producers in the South Belridge field, California

    SciTech Connect

    Fram, J.W.

    1994-08-01

    This paper presents a field study confirming that damage occurs during kill (quenching) operations of thermal producers in the South Belridge field, Kern County, CA. Implementation of the recommendations from this study are expected to decrease damage that occurs during quenching by an average of 0.5 BOPD/kill. Results indicate that producers completed with openhole, gravel-packed, slotted liners in high-permeability sandstones can sustain substantial, irreversible damage when subjected to unfiltered produced-water kills. The damage results when previously produced sand and fines, which have settled in the flowline, are reinjected into the wellbore. Most of the damage is in the slots and gravel pack. Previous studies, field tests, and laboratory work quantifying the amount and site of the damage are detailed. Methods of determining water-quality specifications needed to minimize damage that occurs during well kills are outlined. The approach presented can be used to identify and quantify damage in any field where producers require kills before workover operations. The current recommended kill procedure is also included.

  6. Overview of ASIAEX field experiments in the South and East China Seas

    NASA Astrophysics Data System (ADS)

    Lynch, James F.; Dahl, Peter H.

    2002-11-01

    In the spring of 2001 the Asian Seas International Acoustics Experiment (ASIAEX) was performed in the South and East China Seas. The ASIAEX program originated from the Office of Naval Research's initiative to develop a Sino-American cooperation in the field of ocean acoustics, and expanded to involve Taiwan, Korea, Singapore, and Japan. In the South China Sea, the emphasis was on lower frequency (50-600 Hz) acoustic propagation through complex oceanography along and across the shelfbreak. The oceanographic variability was driven at the mesoscale by the monsoonal wind stress, buoyancy fluxes from the Chinese coast, and by occasional Kuroshio intrusions through the Luzon Strait. Large, nonlinear internal waves also significantly affected the acoustics. In the East China Sea the emphasis was on low- to- midfrequency acoustic interaction with, and reverberation from, the sea floor and sea surface. The experimental site was chosen for flatness, to minimize the influence of bathymetric trends, and emphasize bottom roughness and subbottom structures, in the measurements. This talk will describe the scope of the ASIAEX experimental program, including the ocean acoustic and environmental characterization of the seafloor, sea surface, and water column. Results from various measurement programs will be described in separate papers.

  7. The Spitzer South Pole Telescope Deep Field: Survey Design and Infrared Array Camera Catalogs

    NASA Astrophysics Data System (ADS)

    Ashby, M. L. N.; Stanford, S. A.; Brodwin, M.; Gonzalez, A. H.; Martinez-Manso, J.; Bartlett, J. G.; Benson, B. A.; Bleem, L. E.; Crawford, T. M.; Dey, A.; Dressler, A.; Eisenhardt, P. R. M.; Galametz, A.; Jannuzi, B. T.; Marrone, D. P.; Mei, S.; Muzzin, A.; Pacaud, F.; Pierre, M.; Stern, D.; Vieira, J. D.

    2013-12-01

    The Spitzer South Pole Telescope Deep Field (SSDF) is a wide-area survey using Spitzer's Infrared Array Camera (IRAC) to cover 94 deg2 of extragalactic sky, making it the largest IRAC survey completed to date outside the Milky Way midplane. The SSDF is centered at (α, δ) = (23:30, -55:00), in a region that combines observations spanning a broad wavelength range from numerous facilities. These include millimeter imaging from the South Pole Telescope, far-infrared observations from Herschel/SPIRE, X-ray observations from the XMM XXL survey, near-infrared observations from the VISTA Hemisphere Survey, and radio-wavelength imaging from the Australia Telescope Compact Array, in a panchromatic project designed to address major outstanding questions surrounding galaxy clusters and the baryon budget. Here we describe the Spitzer/IRAC observations of the SSDF, including the survey design, observations, processing, source extraction, and publicly available data products. In particular, we present two band-merged catalogs, one for each of the two warm IRAC selection bands. They contain roughly 5.5 and 3.7 million distinct sources, the vast majority of which are galaxies, down to the SSDF 5σ sensitivity limits of 19.0 and 18.2 Vega mag (7.0 and 9.4 μJy) at 3.6 and 4.5 μm, respectively.

  8. Star Formation in Distant Red Galaxies: Spitzer Observations in the Hubble Deep Field-South

    NASA Astrophysics Data System (ADS)

    Webb, Tracy M. A.; van Dokkum, Pieter; Egami, Eiichi; Fazio, Giovanni; Franx, Marijn; Gawiser, Eric; Herrera, David; Huang, Jiasheng; Labbé, Ivo; Lira, Paulina; Marchesini, Danilo; Maza, José; Quadri, Ryan; Rudnick, Gregory; van der Werf, Paul

    2006-01-01

    We present Spitzer 24 μm imaging of 1.5Field-South of the Multiwavelength Survey by Yale-Chile. We detect 65% of the DRGs with KAB<23.2 mag at S24μm>~40 μJy and conclude that the bulk of the DRG population is dusty active galaxies. A mid-infrared (MIR) color analysis with IRAC data suggests that the MIR fluxes are not dominated by buried AGNs, and we interpret the high detection rate as evidence for a high average star formation rate of =130+/-30 Msolar yr-1. From this, we infer that DRGs are important contributors to the cosmic star formation rate density at z~2, at a level of ~0.02 Msolar yr-1 Mpc-3 to our completeness limit of KAB=22.9 mag.

  9. EVALUATION OF THE FLOOD POTENTIAL OF THE SOUTH HOUSE (BLINEBRY) FIELD, LEA COUNTY, NEW MEXICO

    SciTech Connect

    L. Stephen Melzer

    2000-12-01

    /11 respectively. Production of oil and gas has been established with several months of production now available to make a reserve analysis. Production histories and reserves estimation are provided. An assessment of the flood potential for the South House project area has been completed with work concentrated on South House rock property and pay thickness characterization and analog studies. For the analogs, the North Robertson area, located twenty miles to the northeast, and the Teague Field, located 20 miles to the south, have been utilized due to their readily available database and previous waterflood studies. The South House area does appear to merit further examination as the rock quality compares favorably with both analog Fields; however, current well spacings of 40-acres will provide only marginal economics based upon $23.00/barrel oil prices. Permeability and porosity relationships are provided as a conditional demonstration that rock quality may be sufficient for successful waterflooding of the project area. Further rock property work and pay continuity studies are recommended.

  10. The Spitzer-IRAC/MIPS Extragalactic Survey (SIMES) in the South Ecliptic Pole Field

    NASA Astrophysics Data System (ADS)

    Baronchelli, I.; Scarlata, C.; Rodighiero, G.; Franceschini, A.; Capak, P. L.; Mei, S.; Vaccari, M.; Marchetti, L.; Hibon, P.; Sedgwick, C.; Pearson, C.; Serjeant, S.; Menéndez-Delmestre, K.; Salvato, M.; Malkan, M.; Teplitz, H. I.; Hayes, M.; Colbert, J.; Papovich, C.; Devlin, M.; Kovacs, A.; Scott, K. S.; Surace, J.; Kirkpatrick, J. D.; Atek, H.; Urrutia, T.; Scoville, N. Z.; Takeuchi, T. T.

    2016-03-01

    We present the Spitzer-IRAC/MIPS Extragalactic survey (SIMES) in the South Ecliptic Pole field. The large area covered (7.7 deg2), together with one of the lowest Galactic cirrus emissions in the entire sky and a very extensive coverage by Spitzer, Herschel, Akari, and GALEX, make the SIMES field ideal for extragalactic studies. The elongated geometry of the SIMES area (≈4:1), allowing for significant cosmic variance reduction, further improves the quality of statistical studies in this field. Here we present the reduction and photometric measurements of the Spitzer/IRAC data. The survey reaches depths of 1.93 and 1.75 μJy (1σ) at 3.6 and 4.5 μm, respectively. We discuss the multiwavelength IRAC-based catalog, completed with optical, mid-, and far-IR observations. We detect 341,000 sources with {F}3.6μ {{m}}≥slant 3σ . Of these, 10% have an associated 24 μm counterpart, while 2.7% have an associated SPIRE source. We release the catalog through the NASA/IPAC Infrared Science Archive. Two scientific applications of these IRAC data are presented in this paper. First, we compute integral number counts at 3.6 μm. Second, we use the [3.6]-[4.5] color index to identify galaxy clusters at z > 1.3. We select 27 clusters in the full area, a result consistent with previous studies at similar depth.

  11. Turtle Bayou 1936-1983: case history of a major gas field in south Louisiana

    SciTech Connect

    Cronquist, C.

    1984-11-01

    Turtle Bayou field, located in the middle Miocene trend in south Louisiana, is nearing the end of a productive life spanning more than 30 years. Discovered by Shell Oil Co. in 1949 after unsuccessful attempts by two other companies, the field is a typical, low-relief, moderately faulted U.S. Gulf Coast structure, probably associated with deep salt movement. The productive interval includes 22 separate gas-bearing sands in a regressive sequence of sands and shales from approximately 6,500 to 12,000 ft (1980 to 3660 m). Now estimated to have contained about 1.2 trillion scf (34 X 10/sup 9/ std m/sup 3/) of gas in place, cumulative production through 1982 was 702 billion scf (20 X 10/sup 9/ std m/sup 3/). Cumulative condensate/gas ration (CGR) has been 20 bbl/MMcf (110 X 10/sup -6/ m/sup 3//m/sup 3/. Recovery mechanisms in individual reservoirs include strong bottomwater drive, partial edgewater drive, and pressure depletion. Recovery efficiencies in major reservoirs range form 40 to 83% of original gas in place (OGIP). On decline since 1973, it is anticipated the field will be essentially depleted in the next 5 years.

  12. Turtle Bayou--1936 to 1983--case history of a major gas field in South Louisiana

    SciTech Connect

    Cronquist, C.

    1983-10-01

    Turtle Bayou Field, located in the middle Miocene trend in South Louisiana, is nearing the end of a productive life which spans over 30 years. Discovered by Shell Oil Company in 1949 after unsuccessful attempts by two other majors, the field is a typical, low relief, moderately faulted Gulf Coast structure, probably associated with deep salt movement. The productive interval includes 22 separate gas-bearing sands in a regressive sequence of sands and shales from approximately 6500 to 12,000 feet. Now estimated to have contained about 1.2 trillion standard cubic feet of gas in place, cumulative production through 1982 was 702 billion standard cubic feet. Cumulative condensate-gas ratio has been 20 barrels per million. Recovery mechanisms in individual reservoirs include strong bottom water drive, partial edgewater drive, and pressure depletion. Recovery efficiencies in major reservoirs range from 40 to 75 percent of original gas in place. On decline since 1973, it is anticipated the field will be essentially depleted in the next five years.

  13. STAR FORMATION IN THE CHANDRA DEEP FIELD SOUTH: OBSERVATIONS CONFRONT SIMULATIONS

    SciTech Connect

    Damen, Maaike; Franx, Marijn; Foerster Schreiber, Natascha M.; Labbe, Ivo; Toft, Sune; Van Dokkum, Pieter G.; Wuyts, Stijn

    2009-11-01

    We investigate the star formation history of the universe using FIREWORKS, a multiwavelength survey of the Chandra Deep Field South. We study the evolution of the specific star formation rate (sSFR) with redshift in different mass bins from z = 0 to z approx 3. We find that the sSFR increases with redshift for all masses. The logarithmic increase of the sSFR with redshift is nearly independent of mass, but this cannot yet be verified at the lowest-mass bins at z>0.8, due to incompleteness. We convert the sSFRs to a dimensionless growth rate to facilitate a comparison with a semianalytic galaxy formation model that was implemented on the Millennium Simulation. The model predicts that the growth rates and sSFRs increase similarly with redshift for all masses, consistent with the observations. However, we find that for all masses, the inferred observed growth rates increase more rapidly with redshift than the model predictions. We discuss several possible causes for this discrepancy, ranging from field-to-field variance, conversions to SFR, and shape of the initial mass function. We find that none of these can solve the discrepancy completely. We conclude that the models need to be adapted to produce the steep increase in growth rate between redshift z = 0 and z = 1.

  14. Candidate high-redshift and primeval galaxies in Hubble Deep Field South

    NASA Astrophysics Data System (ADS)

    Clements, D. L.; Eales, S. A.; Baker, A. C.

    1999-09-01

    We present the results of colour selection of candidate high-redshift galaxies in Hubble Deep Field South (HDF-S) using the Lyman dropout scheme. The HDF-S data we discuss were taken in a number of different filters extending from the near-UV (F300W) to the infrared (F222M) in two different fields. This allows us to select candidates with redshifts from z~3 to z~12. We find 15 candidate z~3 objects (F300W dropouts), one candidate z~4 object (F450W dropout) and 16 candidate z~5 objects (F606W dropouts) in the ~4.7-arcmin^2 WFPC-2 field, and four candidate z~6 objects (optical dropouts) and one candidate z~8 object (F110W dropout) in the 0.84-arcmin^2 NICMOS-3 field. No F160W dropouts are found (z~12). We compare our selection technique with existing data for Hubble Deep Field North (HDF-N) and discuss alternative interpretations of the objects. We conclude that there are a number of lower redshift interlopers in the selections, including one previously identified object, and reject those objects most likely to be foreground contaminants. Even after this we conclude that the F606W dropout list is likely to still contain substantial foreground contamination. The lack of candidate very-high-redshift UV-luminous galaxies supports earlier conclusions by Lanzetta et al. We discuss the morphologies and luminosity functions of the high-redshift objects, and their cosmological implications.

  15. A Determination of the North-South Heliospheric Magnetic Field Component from Inner Corona Closed-loop Propagation

    NASA Astrophysics Data System (ADS)

    Jackson, B. V.; Hick, P. P.; Buffington, A.; Yu, H.-S.; Bisi, M. M.; Tokumaru, M.; Zhao, X.

    2015-04-01

    A component of the magnetic field measured in situ near the Earth in the solar wind is present from north-south fields from the low solar corona. Using the Current-sheet Source Surface model, these fields can be extrapolated upward from near the solar surface to 1 AU. Global velocities inferred from a combination of interplanetary scintillation observations matched to in situ velocities and densities provide the extrapolation to 1 AU assuming mass and mass flux conservation. The north-south field component is compared with the same ACE in situ magnetic field component—the Normal (Radial Tangential Normal) Bn coordinate—for three years throughout the solar minimum of the current solar cycle. We find a significant positive correlation throughout this period between this method of determining the Bn field compared with in situ measurements. Given this result from a study during the latest solar minimum, this indicates that a small fraction of the low-coronal Bn component flux regularly escapes from closed field regions. The prospects for Space Weather, where the knowledge of a Bz field at Earth is important for its geomagnetic field effects, is also now enhanced. This is because the Bn field provides the major portion of the Geocentric Solar Magnetospheric Bz field coordinate that couples most closely to the Earth’s geomagnetic field.

  16. The systematic search for z ≳ 5 active galactic nuclei in the Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Weigel, Anna K.; Schawinski, Kevin; Treister, Ezequiel; Urry, C. Megan; Koss, Michael; Trakhtenbrot, Benny

    2015-04-01

    We investigate early black hole (BH) growth through the methodical search for z ≳ 5 active galactic nuclei (AGN) in the Chandra Deep Field South. We base our search on the Chandra 4-Ms data with flux limits of 9.1 × 10-18 (soft, 0.5-2 keV) and 5.5 × 10-17 erg s-1 cm-2 (hard, 2-8 keV). At z ˜ 5, this corresponds to luminosities as low as ˜1042 (˜1043) erg s-1 in the soft (hard) band and should allow us to detect Compton-thin AGN with MBH > 107 M⊙ and Eddington ratios >0.1. Our field (0.03 deg2) contains over 600z ˜ 5 Lyman Break Galaxies. Based on lower redshift relations, we would expect ˜20 of them to host AGN. After combining the Chandra data with Great Observatories Origins Deep Survey (GOODS)/Advanced Camera for Surveys (ACS), CANDELS/Wide Field Camera 3 and Spitzer/Infrared Array Camera data, the sample consists of 58 high-redshift candidates. We run a photometric redshift code, stack the GOODS/ACS data, apply colour criteria and the Lyman Break Technique and use the X-ray Hardness Ratio. We combine our tests and using additional data find that all sources are most likely at low redshift. We also find five X-ray sources without a counterpart in the optical or infrared which might be spurious detections. We conclude that our field does not contain any convincing z ≳ 5 AGN. Explanations for this result include a low BH occupation fraction, a low AGN fraction, short, super-Eddington growth modes, BH growth through BH-BH mergers or in optically faint galaxies. By searching for z ≳ 5 AGN, we are setting the foundation for constraining early BH growth and seed formation scenarios.

  17. Spatial and Alignment Analyses for a field of Small Volcanic Vents South of Pavonis Mons Mars

    NASA Technical Reports Server (NTRS)

    Bleacher, J. E.; Glaze, L. S.; Greeley, R.; Hauber, E.; Baloga, S. M.; Sakimoto, S. E. H.; Williams, D. A.; Glotch, T. D.

    2008-01-01

    The Tharsis province of Mars displays a variety of small volcanic vent (10s krn in diameter) morphologies. These features were identified in Mariner and Viking images [1-4], and Mars Orbiter Laser Altimeter (MOLA) data show them to be more abundant than originally observed [5,6]. Recent studies are classifying their diverse morphologies [7-9]. Building on this work, we are mapping the location of small volcanic vents (small-vents) in the Tharsis province using MOLA, Thermal Emission Imaging System, and High Resolution Stereo Camera data [10]. Here we report on a preliminary study of the spatial and alignment relationships between small-vents south of Pavonis Mons, as determined by nearest neighbor and two-point azimuth statistical analyses. Terrestrial monogenetic volcanic fields display four fundamental characteristics: 1) recurrence rates of eruptions,2 ) vent abundance, 3) vent distribution, and 4) tectonic relationships [11]. While understanding recurrence rates typically requires field measurements, insight into vent abundance, distribution, and tectonic relationships can be established by mapping of remotely sensed data, and subsequent application of spatial statistical studies [11,12], the goal of which is to link the distribution of vents to causal processes.

  18. Hydrogeology and simulation of ground-water flow at the South Well Field, Columbus, Ohio

    USGS Publications Warehouse

    Cunningham, W.L.; Bair, E.S.; Yost, W.P.

    1996-01-01

    The City of Columbus, Ohio, operates four radial collector wells in southern Franklin County. The 'South Well Field' is completed in permeable outwash and ice-contact deposits, upon which flow the Scioto River and Big Walnut Creek. The wells are designed to yield approximately 42 million gallons per day; part of that yield results from induced infiltration of surface water from the Scioto River and Big Walnut Creek. The well field supplied up to 30 percent of the water supply of southern Columbus and its suburbs in 1991. This report describes the hydrogeology of southern Franklin County and a tran sient three-dimensional, numerical ground-water- flow model of the South Well Field. The primary source of ground water in the study area is the glacial drift aquifer. The glacial drift is composed of sand, gravel, and clay depos ited during the Illinoian and Wisconsinan glaciations. In general, thick deposits of till containing lenses of sand and gravel dominate the drift in the area west of the Scioto River. The thickest and most productive parts of the glacial drift aquifer are in the buried valleys in the central and eastern parts of the study area underlying the Scioto River and Big Walnut Creek. Horizontal hydraulic conductivity of the glacial drift aquifer differs spa tially and ranges from 30 to 375 feet per day. The specific yield ranges from 0.12 to 0.30. The secondary source of ground water within the study area is the underlying carbonate bedrock aquifer, which consists of Silurian and Devonian limestones, dolomites, and shales. The horizontal hydraulic conductivity of the carbonate bedrock aquifer ranges from 10 to 15 feet per day. The storage coefficient is about 0.0002. The ground-water-flow system in the South Well Field area is recharged by precipitation, regional ground-water flow, and induced stream infiltration. Yearly recharge rates varied spatially and ranged from 4.0 to 12.0 inches. The three-dimensional, ground-water-flow model was constructed by

  19. Diagenesis and reservoir quality of Paleocoene sandstones in the Kupe South field, Taranaki Basin, New Zealand

    SciTech Connect

    Martin, K.R. ); Baker, J.C. ); Hamilton, P.J. ); Thrasher, G.P. )

    1994-04-01

    The Kupe South field, Taranaki basin, New Zealand is a gas condensate and oil field offshore in the southern Taranaki basin. Its Paleocene reservoir sandstones contain a diagenetic mineral assemblage that records major shifts in pore-water composition during the burial history of the basin. Early calcite formed a shallow burial largely from meteoric depositional pore waters, whereas later chlorite/smectic records the downward passage of marine pore waters into the sandstones from overlying, marine mudrocks prior to significant sandstone compaction during the late Miocene. Late calcite and ferroan carbonates may record the presence of connate meteoric water expelled upward from nonmarine sedimentary rocks of the underyling Cretaceous sequence, whereas later kaolinite and secondary porosity formation are related to localized meteoric influx resulting from late Miocene to early Pliocene uplift and erosion of the reservoir section. Hydrocarbon entrapment occurred during further Pliocene to Holocene sediment accumulation. Labile-grain alteration has been less severe in the lower part of the hydrocarbon-bearing section than in the upper sands with the result that the lower sands contain mainly chlorite/smectite and the upper sands contain mainly ferroan carbonates and kaolinite formed by extensive alteration of labile grains and earlier formed chlorite/smectite. Reservoir quality in the lower sands is controlled mostly by grain size and the presence of chlorite/smectite, but in the upper sands, the presence of kaolinite is the single most important cause of poor reservoir quality. 36 refs., 13 figs., 3 tabs.

  20. Estimation of constitutive parameters for the Belridge Diatomite, South Belridge Diatomite Field

    SciTech Connect

    Fossum, A.F.; Fredrich, J.T.

    1998-06-01

    A cooperative national laboratory/industry research program was initiated in 1994 that improved understanding of the geomechanical processes causing well casing damage during oil production from weak, compactible formations. The program focused on the shallow diatomaceous oil reservoirs located in California`s San Joaquin Valley, and combined analyses of historical field data, experimental determination of rock mechanical behavior, and geomechanical simulation of the reservoir and overburden response to production and injection. Sandia National Laboratories` quasi-static, large-deformation structural mechanics finite element code JAS3D was used to perform the three-dimensional geomechanical simulations. One of the material models implemented in JAS3D to simulate the time-independent inelastic (non-linear) deformation of geomaterials is a generalized version of the Sandler and Rubin cap plasticity model (Sandler and Rubin, 1979). This report documents the experimental rock mechanics data and material cap plasticity models that were derived to describe the Belridge Diatomite reservoir rock at the South Belridge Diatomite Field, Section 33.

  1. BLAST OBSERVATIONS OF THE SOUTH ECLIPTIC POLE FIELD: NUMBER COUNTS AND SOURCE CATALOGS

    SciTech Connect

    Valiante, Elisabetta; Braglia, Filiberto G.; Chapin, Edward L.; Halpern, Mark; Marsden, Gaelen; Scott, Douglas; Ade, Peter A. R.; Griffin, Matthew; Hargrave, Peter C.; Mauskopf, Philip; Pascale, Enzo; Bock, James J.; Devlin, Mark J.; Klein, Jeff; Gundersen, Joshua O.; Hughes, David H.; Netterfield, Calvin B.; Olmi, Luca; Patanchon, Guillaume; Rex, Marie

    2010-12-15

    We present results from a survey carried out by the Balloon-borne Large Aperture Submillimeter Telescope (BLAST) on a 9 deg{sup 2} field near the South Ecliptic Pole at 250, 350, and 500 {mu}m. The median 1{sigma} depths of the maps are 36.0, 26.4, and 18.4 mJy, respectively. We apply a statistical method to estimate submillimeter galaxy number counts and find that they are in agreement with other measurements made with the same instrument and with the more recent results from Herschel/SPIRE. Thanks to the large field observed, the new measurements give additional constraints on the bright end of the counts. We identify 132, 89, and 61 sources with S/N {>=}4 at 250, 350, 500 {mu}m, respectively and provide a multi-wavelength combined catalog of 232 sources with a significance {>=}4{sigma} in at least one BLAST band. The new BLAST maps and catalogs are available publicly at http://blastexperiment.info.

  2. Definition of reservoir configuration in ancient glacial environment: case history from Rima field, south Oman

    SciTech Connect

    Penneycard, A.J.

    1986-05-01

    The Al Khlata Formation (Permian-Carboniferous) is an important reservoir unit of the Eastern Flank province of South Oman. The formation consists of an unusual series of glacial sand, silt, shale, and diamictite exhibiting such gross heterogeneity that conventional correlation techniques are ineffective. A threefold palynologic subdivision has been developed, which has allowed the recognition of a number of genetically distinct units. Major periods of erosion separate the units, erosive processes dominating the 20-40 million year period during which the Al Khlata accumulated. Deposition occurred in a sequence of deep valleys cut into the early Al Khlata and underlying Haima (Cambrian-Ordovician) reservoirs. The extent of these deposits is controlled by the morphology of these incisive valleys. A case history of the large Rima field illustrates the use of palynology in unraveling the temporal and spatial relationships of the individual Al Khlata and Haima units. The resultant reservoir-geologic model of this internally complex fields has enabled more confident assessment of variations in well performance with reservoir type, and has guided plans for future offtake levels and overall development planning.

  3. Trace contraband detection field-test by the south Texas specialized crimes and narcotics task force.

    SciTech Connect

    Hannum, David W.; Shannon, Gary W.

    2006-04-01

    This report describes the collaboration between the South Texas Specialized Crimes and Narcotics Task Force (STSCNTF) and Sandia National Laboratories (SNL) in a field test that provided prototype hand-held trace detection technology for use in counter-drug operations. The National Institute of Justice (NIJ)/National Law Enforcement and Corrections Technology Center (NLECTC)/Border Research and Technology Center (BRTC) was contacted by STSCNTF for assistance in obtaining cutting-edge technology. The BRTC created a pilot project for Sandia National Laboratories (SNL) and the STSCNTF for the use of SNLs Hound, a hand-held sample collection and preconcentration system that, when combined with a commercial chemical detector, can be used for the trace detection of illicit drugs and explosives. The STSCNTF operates in an area of high narcotics trafficking where methods of concealment make the detection of narcotics challenging. Sandia National Laboratories (SNL) Contraband Detection Department personnel provided the Hound system hardware and operational training. The Hound system combines the GE VaporTracer2, a hand-held commercial chemical detector, with an SNL-developed sample collection and preconcentration system. The South Texas Task force reported a variety of successes, including identification of a major shipment of methamphetamines, the discovery of hidden compartments in vehicles that contained illegal drugs and currency used in drug deals, and the identification of a suspect in a nightclub shooting. The main advantage of the hand-held trace detection unit is its ability to quickly identify the type of chemical (drugs or explosives) without a long lag time for laboratory analysis, which is the most common analysis method for current law enforcement procedures.

  4. The South American Meridional B-field Array (SAMBA) and Pc4-5 Wave Studies

    NASA Astrophysics Data System (ADS)

    Sterner, Lt. Nathan; Zesta, Eftyhia; Boudouridis, Athanasios; Moldwin, Mark; Yizengaw, Endawoke; Chi, Peter

    The Antarctic continent, the only landmass in the southern polar region, offers the unique opportunity for observations that geomagnetically range from polar latitudes to well into the inner magnetosphere, thus enabling conjugate observations in a wide range of geomagnetic lat-itudes. The SAMBA (South American Meridional B-field Array) chain is a meridional chain of 12 magnetometers, 11 of them at L=1.1 to L=2.5 along the coast of Chile and in the Antarc-tica peninsula, and one auroral station along the same meridian. SAMBA is conjugate to the northern hemisphere MEASURE and McMAC chains, offering unique opportunities for inter-hemispheric studies. In particular, we study asymmetries in the power of ULF waves and the role of the ionosphere in such observed asymmetries. Utilizing conjugate magnetometer stations at L=1.7 and L=2.3, we previously demonstrated that the northern hemisphere consistently shows higher ULF wave power. One possible reason for the asymmetry is solar zenith angles differences with the northern hemisphere station being closer to the ecliptic plain and having a higher power ratio. These hemispheric differences were also observed with TEC measurements indicating that the north and south conjugate ionospheres are similarly asymmetric. The initial study was done with Pc3 waves, which include the resonance frequencies for the flux tubes of our conjugate stations. We now extend the study to Pc4 and Pc5 waves that reach the lower latitudes via different mechanisms and compare these waves to the resonant Pc3 waves.

  5. A COMPREHENSIVE NONPOINT SOURCE FIELD STUDY FOR SEDIMENT, NUTRIENTS AND PATHOGENS IN THE SOUTH FORK BROAD RIVER WATERSHED, GEORGIA

    EPA Science Inventory

    There is an urgent need for EPA to develop protocols for establishing Total Maximum Daily Loads (TMDLs) in streams, lakes and estuaries. A cooperative TMDL field data collection project between ORD and Region 4 is ongoing in the South Fork Broad River Watershed (SFBR), a 245.18 ...

  6. Hydraulic Fracturing of 403 Shallow Diatomite Wells in South Belridge Oil Field, Kern County, California, in 2014

    NASA Astrophysics Data System (ADS)

    Wynne, D. B.; Agusiegbe, V.

    2015-12-01

    We examine all 403 Hydraulic Fracture (HF) jobs performed by Aera Energy, LLC, in the South Belridge oil field, Kern County, CA in 2014. HFs in the South Belridge oil field are atypical amongst North American plays because the reservoir is shallow and produced via vertical wells. Our data set constitutes 88% of all HF jobs performed in CA oil fields in calendar-2014. The South Belridge field produces 11% of California's oil and the shallow HFs performed here differ from most HFs performed elsewhere. We discuss fracture modeling and methods and summary statistics, and modelled dimensions of fractures and their relationships to depth and reservoir properties. The 403 HFs were made in the diatomite-dominated Reef Ridge member of the Monterey Formation. The HFs began at an average depth of 1047 feet below ground (ft TVD) and extended an average of 626 ft vertically downward. The deepest initiation of HF was at 2380 ft and the shallowest cessation was at 639 ft TVD. The average HF was performed using 1488 BBL (62,496 gallons) of water. The HFs were performed in no more than 6 stages and nearly all were completed within one day. We (1) compare metrics of the South Belridge sample group with recent, larger "all-CA" and nationwide samples; and (2) conclude that if relationships of reservoir properties, well completion and HF are well understood, shallow diatomite HF may be optimized to enhance production while minimizing environmental impact.

  7. 76 FR 12132 - Notice of Availability of the Record of Decision for the Wright Area South Hilight Field Coal...

    Federal Register 2010, 2011, 2012, 2013, 2014

    2011-03-04

    ... Final EIS was publicly available on July 30, 2010 (75 FR 44951). This decision is subject to appeal to... Bureau of Land Management Notice of Availability of the Record of Decision for the Wright Area South Hilight Field Coal Lease-by-Application and Environmental Impact Statement, Wyoming AGENCY: Bureau of...

  8. VizieR Online Data Catalog: Chandra Deep Field South: multi-colour data (Wolf+, 2008)

    NASA Astrophysics Data System (ADS)

    Wolf, C.; Meisenheimer, K.; Kleinheinrich, M.; Borch, A.; Dye, S.; Gray, M.; Wisotzki, L.; Bell, E. F.; Rix, H.-W.; Cimatti, A.; Hasinger, G.; Szokoly, G.

    2004-04-01

    Table 3 contains the object catalogue of the COMBO-17 CDFS field. The observations were carried out with the Wide Field Imager (WFI) at the MPG/ESO 2.2-m telescope on La Silla, Chile, between October 1999 and January 2001 in four independent observing runs. The field measures 31.5'x30', is centered on RA=03:32:25, DE=-27:48:50 and contains the Chandra Deep Field South. The table contains 63501 objects found on the deep R-band image cdfs_r.fit by SExtractor with S/N>3. The 5-{sigma} magnitude limit for point sources is Rmag=26.0. Morphological information from the SExtractor measurement is included. Multiple observations in different observing runs of six different filters allow the identification of variable objects. The table contains positions, flags and flux measurements in UBVRI and 12 optical medium-band filters. In addition, we include multi-colour classification, photometric redshifts, luminosity distances and a number of absolute restframe magnitudes in different filters (Johnson, Sloan, Bessell). cdfsu.fit, cdfsb.fit, cdfsv.fit, cdfsr.fit and cdfs_i.fit are coadded sumframes in UBVRI of the CDFS field. These sumframes are stacked from flat-fielded and cosmic-corrected individual images by applying only full pixel shifts. Therefore, the coordinate frames differ slightly between the images. The coordinates in Table 3 refer to image cdfs_r.fit. The images in BVRI are obtained from observations carried out in observing run D (Oct 1999, see also Note (11) in the byte-by-byte description of table3.dat) while the U-band image is obtained from observing run G (Jan 2001). The exposure times are 14400s (U), 5000s (B), 8400s (V), 15000s (R) and 7550s (I). The intensity levels are given in units of photons hitting the detector (already corrected for the gain of the CCD). The data included here supersede the table2.dat of the COMBO-17 published in 2001 (J/A+A/377/442) (6 data files).

  9. Major Paleostress Field Differences on Complementary Margins of the South Atlantic

    NASA Astrophysics Data System (ADS)

    Salomon, E.; Koehn, D.; Passchier, C. W.; Hackspacher, P. C.; Glasmacher, P. A.

    2013-12-01

    We present a detailed study of paleostress fields of the Namibian and Brazilian passive continental margins of the South Atlantic to address a general debate on whether or not these complementary margins experienced similar tectonic histories (e.g. Cobbold et al., 2001; Al-Hajri et al., 2009; Japsen et al., 2012). In our study, we compare the NW of Namibia and the SE of Brazil with each other. These areas are largely covered by the flood basalts of the Paraná-Etendeka-Large Igneous Province overlying Neo-Proterozoic basement of the Pan-African orogeny. With an age of ~133 Ma the basalts were emplaced just before or during the onset of the South Atlantic opening and thus serve as a good time marker for rift- and post-rift-related tectonics. We studied mainly fault planes and associated striations within the flood basalts and compared the resulting stress patterns of both margins. Results reveal remarkable differences in the stress patterns for SE Brazil and NW Namibia. In NW Namibia, a WSW-ENE directed extensional stress field dominates and fits well with extension of the original continental rift and the passive margin. A second extensional stress field (σ3 SSW oriented) and a strike-slip system (σ1 NW oriented) appear only subdued. In contrast, the SE of Brazil is mainly characterized by two strike-slip systems (σ1 oriented SW and E, respectively) whereas an extensional stress field is almost non-existent. The strike-slip faulting of the Brazilian study area occur widespread across SE Brazil as they are also evident in other paleostress studies of the region and might thus be the result of far-field stresses. Margin-parallel faults are scarce, so it appears that rift-related extension was restricted to a narrower strip along the continent-ocean boundary, now lying offshore. In NW Namibia, the faults of the extensional stress regime run parallel to the sub-margin-parallel basement structure (i.e. shear zones and foliation) and hence indicate a reactivation of

  10. 3D airflow dynamics over transverse ridges Mpekweni, South Africa: implications for dune field migration behaviour

    NASA Astrophysics Data System (ADS)

    Jackson, Derek; Cooper, Andrew; Green, Andrew; Beyers, Meiring; Wiles, Errol; Benallack, Keegan

    2016-04-01

    Un-vegetated dune fields provide excellent opportunities to examine airflow dynamics over various types and scales of dune landforms. The three dimensional surface over which lower boundary layers travel, help adjust surface airflow and consequently the aeolian response of the dunes themselves. The use of computational fluid dynamic (CFD) modelling in recent studies now enables investigation of the 3D behaviour of airflow over complex terrain, providing new insights into heterogeneous surface flow and aeolian response of dune surfaces on a large (dunefield) scale. Using a largely un-vegetated coastal dune field site at Mpekweni, Eastern Cape, South Africa, a detailed (0.1m gridded) terrestrial laser scanning survey was conducted to create a high resolution topographical surface. Using local wind flow measurements and local met station records as input, CFD modelling was performed for a number of scenarios involving variable direction and magnitude to examine surface flow patterns across multiple dune forms. Near surface acceleration, expansion and separation of airflow inducing convergence and divergence (steering) of flow velocity streamlines are investigated. Flow acceleration over dune crests/brink lines is a key parameter in driving dune migration and slip face dynamics. Dune aspect ratio (height to length) is also important in determining the degree of crestal flow acceleration, with an increase in flow associated with increasing aspect ratios. Variations in dune height appear to be the most important parameter in driving general flow acceleration. The results from the study provide new insights into dune migration behaviour at this site as well as surface flow behaviour across multiple dune configurations and length scales within un-vegetated dune fields.

  11. Determination of the North-South Heliospheric Magnetic-Field Component from Inner-Corona Closed-Loop Propagation

    NASA Astrophysics Data System (ADS)

    Jackson, B. V.; Yu, H. S.; Hick, P. P.; Buffington, A.; Bisi, M. M.; Tokumaru, M.; Kim, J.; Hong, S.; Lee, B.; Yi, J.; Yun, J.

    2015-12-01

    We find that a portion of the north-south interplanetary magnetic field measured in situ near Earth is present from a direct outward mapping of closed fields from the low solar corona. Using the Current-Sheet Source Surface (CSSS) model (Zhao & Hoeksema, 1995 JGR 100, 19), these lower coronal fields are extrapolated upward from near the solar surface. Global velocities inferred from a combination of observations of interplanetary scintillation (IPS) matched to in-situ velocities and densities measured by spacecraft instrumentation provide an accurate outward timing to 1 AU from a model assuming conservation of mass and mass flux. The north-south field component at 1 AU is compared with the appropriate ACE magnetometer in-situ Normal (RTN) or Bn field coordinate (Jackson et al., 2015, ApJL, 803:L1). From a significant positive correlation between this method of determining the Bn field compared with in-situ measurements over a three-year period during the last solar minimum, we find that a small fraction of the low-coronal Bn component flux (~1%) regularly escapes from closed-field regions. Since the Bn field provides the major portion of the Geocentric Solar Magnetospheric (GSM) Bz field component that couples most closely to the Earth's geomagnetic field, the prospects for its determination using this technique for space weather use are being actively developed by our many colleague groups.

  12. Reservoir compaction of the Belridge Diatomite and surface subsidence, south Belridge field, Kern County, California

    SciTech Connect

    Bowersox, J.R.; Shore, R.A. )

    1990-05-01

    Surface subsidence due to reservoir compaction during production has been observed in many large oil fields. Subsidence is most obvious in coastal and offshore fields where inundation by the sea occurs. Well-known examples are Wilmington field in California and Ekofisk field in the North Sea. In South Belridge field, the Belridge Diatomite member of the late Miocene Reef Ridge Shale has proven prone to compaction during production. The reservoir, a high-porosity, low-permeability, highly compressive rock composed largely of diatomite and mudstone, is about 1,000 ft thick and lies at an average depth of 1,600 ft. Within the Belridge Diatomite, reservoir compaction due to withdrawal of oil and water in Sec. 12, T28S, R20E, MDB and M, was noticed after casing failures in producing wells began occurring and tension cracks, enlarged by hydrocompaction after a heavy rainstorm were observed. Surface subsidence in Sec. 12 has been monitored since April 1987, through the surveying of benchmark monuments. The average annualized subsidence rate during 1987 was {minus}1.86 ft/yr, {minus}0.92 ft/yr during 1988, and {minus}0.65 ft/yr during 1989; the estimated peak subsidence rate reached {minus}7.50 ft/yr in July 1985, after 1.5 yrs of production from the Belridge Diatomite reservoir. Since production from the Belridge Diatomite reservoir commenced in February 1984, the surface of the 160-ac producing area has subsided about 12.5 ft. This equates to an estimated reservoir compaction of 30 ft in the Belridge Diatomite and an average loss of reservoir porosity of 2.4% from 55.2 to 52.8%. Injection of water for reservoir pressure maintenance in the Belridge diatomite began in June 1987, and has been effective in mitigating subsidence to current rates and repressurizing the reservoir to near-initial pressure. An added benefit of water injection has been improved recovery of oil from the Belridge Diatomite by waterflood.

  13. Ground-based instrumentation for measurements of atmospheric conduction current and electric field at the South Pole

    NASA Technical Reports Server (NTRS)

    Byrne, G. J.; Benbrook, J. R.; Bering, E. A.; Few, A. A.; Morris, G. A.; Trabucco, W. J.; Paschal, E. W.

    1993-01-01

    Attention is given to instruments constructed to measure the atmospheric conduction current and the atmospheric electric field - two fundamental parameters of the global-electric circuit. The instruments were deployed at the Amundsen-Scott South Pole Station in January 1991 and are designed to operate continuously for up to one year without operator intervention. The atmospheric current flows into one hemisphere, through the electronics where it is measured, and out the other hemisphere. The electric field is measured by a field mill of the rotating dipole type. Sample data from the first days of operation at the South Pole indicate variations in the global circuit over time scales from minutes to hours to days.

  14. X-ray observations of dust obscured galaxies in the Chandra deep field south

    NASA Astrophysics Data System (ADS)

    Corral, A.; Georgantopoulos, I.; Comastri, A.; Ranalli, P.; Akylas, A.; Salvato, M.; Lanzuisi, G.; Vignali, C.; Koutoulidis, L.

    2016-08-01

    We present the properties of X-ray detected dust obscured galaxies (DOGs) in the Chandra deep field south. In recent years, it has been proposed that a significant percentage of the elusive Compton-thick (CT) active galactic nuclei (AGN) could be hidden among DOGs. This type of galaxy is characterized by a very high infrared (IR) to optical flux ratio (f24 μm/fR > 1000), which in the case of CT AGN could be due to the suppression of AGN emission by absorption and its subsequent re-emission in the IR. The most reliable way of confirming the CT nature of an AGN is by X-ray spectroscopy. In a previous work, we presented the properties of X-ray detected DOGs by making use of the deepest X-ray observations available at that time, the 2Ms observations of the Chandra deep fields, the Chandra deep field north (CDF-N), and the Chandra deep field south (CDF-S). In that work, we only found a moderate percentage (<50%) of CT AGN among the DOGs sample. However, we pointed out that the limited photon statistics for most of the sources in the sample did not allow us to strongly constrain this number. In this paper, we further explore the properties of the sample of DOGs in the CDF-S presented in that work by using not only a deeper 6Ms Chandra survey of the CDF-S, but also by combining these data with the 3Ms XMM-Newton survey of the CDF-S. We also take advantage of the great coverage of the CDF-S region from the UV to the far-IR to fit the spectral energy distributions (SEDs) of our sources. Out of the 14 AGN composing our sample, 9 are highly absorbed (NH > 1023 cm-2), whereas 2 look unabsorbed, and the other 3 are only moderately absorbed. Among the highly absorbed AGN, we find that only three could be considered CT AGN. In only one of these three cases, we detect a strong Fe Kα emission line; the source is already classified as a CT AGN with Chandra data in a previous work. Here we confirm its CT nature by combining Chandra and XMM-Newton data. For the other two CT

  15. A SEARCH FOR FIELD HORIZONTAL-BRANCH STARS NEAR THE SOUTH GALACTIC POLE

    SciTech Connect

    Ortiz, R.; Wilhelm, R.; Costa, R. D. D.; Rossi, S.

    2010-03-15

    Searches for field horizontal-branch (FHB) stars in the halo of the Galaxy in the past have been carried out by several techniques, such as objective-prism surveys and visual or infrared photometric surveys. By choosing adequate color criteria, it is possible to improve the efficiency of identifying bona fide FHB stars among the other objects that exhibit similar characteristics, such as main-sequence A-stars, blue stragglers, subdwarfs, etc. In this work, we report the results of a spectroscopic survey carried out near the south Galactic pole intended to validate FHB stars originally selected from the HK objective-prism survey of Beers and colleagues, based on near-infrared color indices. A comparison between the stellar spectra obtained in this survey with theoretical stellar atmosphere models allows us to determine T {sub eff}, log g, and [Fe/H] for 13 stars in the sample. Stellar temperatures were calculated from measured (B - V) {sub o}, when this measurement was available (16 stars). The color index criteria adopted in this work are shown to correctly classify 30% of the sample as FHB, 25% as non-FHB (main-sequence stars and subdwarfes), whereas 40% could not be distinguished between FHB and main-sequence stars. We compare the efficacy of different color criteria in the literature intended to select FHB stars, and discuss the use of the Mg II 4481 line to estimate the metallicity.

  16. Clay minerals as indicators for depositional environment in the south Hallettsville Field, Lavaca County, Texas

    SciTech Connect

    Freed, R.L.

    1980-01-01

    The South Hallettsville Field, Lavaca County, Texas, produces gas and condensate from Lower Wilcox sandstones and shales which have been interpreted as either channel turbidite deposits in outer-shelf to slope locations or as delta to pro-delta sands and muds. Thirteen core samples were analyzed by X-ray diffraction methods to determine whether a semiquantitative estimate of clay mineral content would aid in determining the depositional environment. Discrete illite, kaolinite, and chlorite are of particular interest because the presence of these minerals is interpreted as being due to original deposition. If a turbidity-type event occurred, the weight percents of nondiagenetic clays in this sequence should: (1) decrease significantly as the boundary is crossed between the shale and the overlying sandstone; and (2) gradually increase in progressively shallower samples within the sandstone. However, the weight percents for kaolinite and chlorite do not vary significantly; the illite content gradually decreases with shallower depths. This sequence is more compatible with a deltaic environment of deposition. 10 references.

  17. South Harmony Church field, Southwest Louisiana - Further insights on uppermost Wilcox shelf-margin trend

    SciTech Connect

    Belvedere, P.G.

    1988-01-01

    The uppermost Wilcox Group (Eocene) in the South Harmony Church field is a 2,000-ft thick sequence of single and multistory sandstones and shales. Cores of three separate intervals from four different wells display sedimentologic and lithologic features characteristic of inner shelf and shoreface deposition, representing an offshore bar complex. Typical lithofacies assemblages within an interval include, from top to bottom, (1) bioturbated, muddy sandstone--inner shelf, (2) less bioturbated, arenaceous sandstone--mostly inner shelf, (3) structureless to faintly horizontally laminated sandstone--mostly lower shoreface, and (4) horizontal to cross-laminated, and commonly deformed sandstone with shale and siltstone interbeds--lower surface. Sandstones are fine to very fine-grained, poorly to moderately well-sorted sublitharenites. Optimum reservoir quality is observed in the bioturbated, clean sandstones of the self-shoreface transition zone, where porosity ranges from 5 to 23% and permeability from less than 0.01 to 31 md. Porosity is mostly secondary and attributed to the leaching of labile constituents.

  18. Overview of the South American biomass burning analysis (SAMBBA) field experiment

    NASA Astrophysics Data System (ADS)

    Morgan, W. T.; Allan, J. D.; Flynn, M.; Darbyshire, E.; Hodgson, A.; Johnson, B. T.; Haywood, J. M.; Freitas, S.; Longo, K.; Artaxo, P.; Coe, H.

    2013-05-01

    Biomass burning represents one of the largest sources of particulate matter to the atmosphere, which results in a significant perturbation to the Earth's radiative balance coupled with serious negative impacts on public health. Globally, biomass burning aerosols are thought to exert a small warming effect of 0.03 Wm-2, however the uncertainty is 4 times greater than the central estimate. On regional scales, the impact is substantially greater, particularly in areas such as the Amazon Basin where large, intense and frequent burning occurs on an annual basis for several months (usually from August-October). Furthermore, a growing number of people live within the Amazon region, which means that they are subject to the deleterious effects on their health from exposure to substantial volumes of polluted air. Initial results from the South American Biomass Burning Analysis (SAMBBA) field experiment, which took place during September and October 2012 over Brazil, are presented here. A suite of instrumentation was flown on-board the UK Facility for Airborne Atmospheric Measurement (FAAM) BAe-146 research aircraft and was supported by ground based measurements, with extensive measurements made in Porto Velho, Rondonia. The aircraft sampled a range of conditions with sampling of fresh biomass burning plumes, regional haze and elevated biomass burning layers within the free troposphere. The physical, chemical and optical properties of the aerosols across the region will be characterized in order to establish the impact of biomass burning on regional air quality, weather and climate.

  19. X-ray Evolution of Normal Galaxies in the 6 Ms Chandra Deep Field-South

    NASA Astrophysics Data System (ADS)

    Lehmer, Bret; Basu-Zych, Antara; Mineo, Stefano; Brandt, W. Niel; Eufrasio, Rafael T.; Fragos, Tassos; Hornschemeier, Ann E.; Luo, Bin; Xue, Yongquan; Bauer, Franz E.; Gilfanov, Marat; Kalogera, Vassiliki; Ranalli, Piero; Schneider, Donald P.; Shemmer, Ohad; Tozzi, Paolo; Trump, Jonathan R.; Vignali, Cristian; Wang, JunXian; Yukita, Mihoko; Zezas, Andreas

    2016-04-01

    I will discuss recent efforts to quantify the evolution of X-ray binary (XRB) populations through cosmic time using the 6 Ms Chandra Deep Field-South (CDF-S) survey. The formation of XRBs is sensitive to galaxy properties like stellar age and metallicity---properties that have evolved significantly in the broader galaxy population throughout cosmic history. I will show that scaling relations between X-ray emission from low-mass XRBs (LMXBs) with stellar mass (LX/M) and high-mass XRBs (HMXBs) with star-formation rate (LX/SFR) change significantly with redshift, such that LX(LMXB)/M ~ (1+z)^2-3 and LX(HMXB)/SFR ~ (1+z). These findings are consistent with population synthesis models, which attribute the increase in LMXB and HMXB scaling relations with redshift as being due to declining host galaxy stellar ages and metallicities, respectively. These findings have important implications for the X-ray emission from young, low-metallicity galaxies at high redshift, which are likely to be more X-ray luminous per SFR and play a significant role in the heating of the intergalactic medium.

  20. Impacts of Humic Injection Experiments on the South Oyster Field Research Site

    SciTech Connect

    John F. McCarthy

    2004-04-27

    A closure plan for the South Oyster Focus Area (SOFA) is being implemented to assess the impacts of a series of experimental injections of microorganisms, tracers and chemical amendments on the chemical and physical properties of the aquifer. The proposed research addresses environmental monitoring of humic substances injected into the aquifer, as described in the Site Closure Plan for the South Oyster Field Research Site. The goal of the research is to demonstrate that the dissolved organic matter (DOM) in the groundwater at and downgradient from the injection site has returned to a pre-injection �baseline� conditions with respect to either the concentration or chemical composition of the DOM. For clarity, the humic solution injected during the experiment will be referred to as �humic injectate.� The term �DOM� will refer to the organic material recovered in the groundwater, which includes the autochthonous groundwater DOM as well as any of the humic injectate remaining in the groundwater. Specific objectives include: � Estimate the amount of humic material remaining in the aquifer at the completion of the push-pull experiment and the potential for environmental impacts due to release of humics retained on the sediments. � Monitor the DOM concentrations in groundwater over time at the injection well and at sampling locations within the potential downgradient plume of the injected tracers. � Evaluate the chemical composition of the DOM to determine whether the injection experiment had an impact of the chemical properties of the aquifer. The product of this research will be a contribution to the Site Closure Report documenting the impact of the humic experiments on the aquifer. Return of the aquifer to a �baseline� conditions will be achieved if the DOM concentrations in the groundwater are determined over the course of the research to have decreased to the pre-injection level, or if the chemical properties of

  1. The 17 July 2006 Tsunami Along the South Coast of Java, Indonesia: Field Survey and Near Field Tsunami Simulation

    NASA Astrophysics Data System (ADS)

    Lavigne, F.; Gomez, C.; Hebert, H.; Sladen, A.; Schindele, F.; Mardiatno, D.; Priyono, J.; Giffo, M.; Wassmer, P.

    2006-12-01

    The 17th July 2006, a tsunami struck the southern coast of Java, Indonesia. The triggering earthquake at 15:19 WIB was located about 200 km south from Pangandaran (9°24S-117°36E), with a magnitude reaching M_w = 7.7. In order to calibrate numerical models, field surveys were conducted by a team divided into threee groups - from the French CNRS and the Indonesian Research Center for Disasters - from Pangandaran district in West Java to Gunungkidul district in Central Java. The surveys began the day after the tsunami and lasted more than one month. Data collection involved measurements of the wave height and runup, inundation depth, flow direction, and chronology of the tsunami event. Two main waves were reported by eyewitnesses' accounts. The second wave reached locally 8 to 11 m high before its breaking at several sites. Depending on the nearshore topography, this wave broke either nearshore, on the beaches or up to 100 meters inland. Local runups up to 15 m asl were measured on cliffs at Nusa Kambangan Island. Inundation depth usually ranged 2 to 3 m from ground. The tsunami arrival time has been recorded precisely at several locations owing to good recorders: a clock which stopped working when struck by the tsunami, pictures taken by testimonies, or a video movie at the Cilacap power plant construction. The first wave reached the whole coast between Pangandaran and pantai Ayah between 16:15 and 16:20 WIB, one hour after the earthquake. Further East, Baron Beach in Central Java was struck around 16:30 WIB, and the tide gauge at Benoa (Bali) recorded the tsunami at 17:00 WIB. We discuss the source of the tsunami in trying several seismological models used to trigger the waves and compute their impact onland. We particularly stress on the tsunami effect in the Cilacap area where detailed bathymetric and topographic data have been used to refine the modeling. When compared to the high amplitudes measured, the results provide indications on the most realistic source

  2. Clusters, groups, and filaments in the Chandra deep field-south up to redshift 1

    SciTech Connect

    Dehghan, S.; Johnston-Hollitt, M.

    2014-03-01

    We present a comprehensive structure detection analysis of the 0.3 deg{sup 2} area of the MUSYC-ACES field, which covers the Chandra Deep Field-South (CDFS). Using a density-based clustering algorithm on the MUSYC and ACES photometric and spectroscopic catalogs, we find 62 overdense regions up to redshifts of 1, including clusters, groups, and filaments. We also present the detection of a relatively small void of ∼10 Mpc{sup 2} at z ∼ 0.53. All structures are confirmed using the DBSCAN method, including the detection of nine structures previously reported in the literature. We present a catalog of all structures present, including their central position, mean redshift, velocity dispersions, and classification based on their morphological and spectroscopic distributions. In particular, we find 13 galaxy clusters and 6 large groups/small clusters. Comparison of these massive structures with published XMM-Newton imaging (where available) shows that 80% of these structures are associated with diffuse, soft-band (0.4-1 keV) X-ray emission, including 90% of all objects classified as clusters. The presence of soft-band X-ray emission in these massive structures (M {sub 200} ≥ 4.9 × 10{sup 13} M {sub ☉}) provides a strong independent confirmation of our methodology and classification scheme. In the closest two clusters identified (z < 0.13) high-quality optical imaging from the Deep2c field of the Garching-Bonn Deep Survey reveals the cD galaxies and demonstrates that they sit at the center of the detected X-ray emission. Nearly 60% of the clusters, groups, and filaments are detected in the known enhanced density regions of the CDFS at z ≅ 0.13, 0.52, 0.68, and 0.73. Additionally, all of the clusters, bar the most distant, are found in these overdense redshift regions. Many of the clusters and groups exhibit signs of ongoing formation seen in their velocity distributions, position within the detected cosmic web, and in one case through the presence of tidally

  3. A Search for Field Horizontal-Branch Stars Near the South Galactic Pole

    NASA Astrophysics Data System (ADS)

    Ortiz, R.; Wilhelm, R.; Costa, R. D. D.; Rossi, S.; Beers, T. C.

    2010-03-01

    Searches for field horizontal-branch (FHB) stars in the halo of the Galaxy in the past have been carried out by several techniques, such as objective-prism surveys and visual or infrared photometric surveys. By choosing adequate color criteria, it is possible to improve the efficiency of identifying bona fide FHB stars among the other objects that exhibit similar characteristics, such as main-sequence A-stars, blue stragglers, subdwarfs, etc. In this work, we report the results of a spectroscopic survey carried out near the south Galactic pole intended to validate FHB stars originally selected from the HK objective-prism survey of Beers and colleagues, based on near-infrared color indices. A comparison between the stellar spectra obtained in this survey with theoretical stellar atmosphere models allows us to determine T eff, log g, and [Fe/H] for 13 stars in the sample. Stellar temperatures were calculated from measured (B - V) o , when this measurement was available (16 stars). The color index criteria adopted in this work are shown to correctly classify 30% of the sample as FHB, 25% as non-FHB (main-sequence stars and subdwarfes), whereas 40% could not be distinguished between FHB and main-sequence stars. We compare the efficacy of different color criteria in the literature intended to select FHB stars, and discuss the use of the Mg II 4481 line to estimate the metallicity. Based on observations obtained at the Pico dos Dias Observatory, operated by the National Laboratory for Astrophysics, Brazil.

  4. Schmallenberg virus infection in South American camelids: Field and experimental investigations.

    PubMed

    Schulz, Claudia; Beer, Martin; Hoffmann, Bernd

    2015-11-18

    During the first epizootic wave of the novel, teratogenic Schmallenberg virus (SBV, Orthobunyavirus) in ruminants in Northern Europe, serological evidence of a previous SBV-infection demonstrated that South American camelids (SAC) are also susceptible to SBV. However, their potential role in SBV spread remains unknown. To investigate the prevalence and course of SBV-infection in SAC, a German field study and an animal trial with three llamas and three alpacas were conducted. From September 2012 to December 2013, 313 of 502 SAC (62.35%) were found SBV seropositive, but negative for SBV-RNA. The estimated between-district (94.23% of 52) and median within-district (71.43%) and herd (73.13%) SBV seroprevalence in German SAC was similar to the seroprevalence reported in cattle herds and sheep flocks at the time. An age of >1 year was found a statistically significant risk factor for SBV-infection, which could be explained by the spatio-temporal spread of SBV in Germany during the study period. No clinical signs or an increase of abortion and congenital malformation associated with SBV-infection in SAC were reported by the study participants. Similar to SBV-infected ruminants, SBV-RNAemia in experimentally SBV-infected SAC was detected for a short time between days 3 and 7 after infection (dpi), and seroconversion occurred between 9 and 21 dpi. Despite the similar virological and serological results, the lack of clinical signs and congenital malformation associated with SBV-infection suggests that SBV causes subclinical infection in SAC. However, their role as reservoirs in the spread of SBV has to be further investigated. PMID:26361966

  5. Near-Field Deformation Associated with the M6.0 South Napa Earthquake Surface Rupture

    NASA Astrophysics Data System (ADS)

    Brooks, B. A.; Hudnut, K. W.; Glennie, C. L.; Ericksen, T.

    2014-12-01

    We characterize near-field deformation associated with the surface rupture of the M6.0 South Napa earthquake from repeat mobile laser scanning (MLS) surveys. Starting the day after the main shock, we operated, sometime simultaneously, short (~75 m range) and medium (~400m range) range laser scanners on a truck or backpack. We scanned most of the length of the principal and secondary surface ruptures at speeds less than 10 km/hr. Scanning occurred primarily in either suburban subdivisions or cultivated vineyards of varying varietals with differing leaf patterns and stages of maturity. Spot-spacing is dense enough (100s of points/m^2) to permit creation of 10-25cm digital elevation models of much of the surface rupture. Scanned features of the right-lateral rupture include classic mole tracks through a variety of soil types, en echelon cracks, offset vine rows, and myriad types of pavement-related deformation. We estimate coseismic surface displacements ranging from 5 to 45 cm by examining offset cultural features and vine rows and by comparing the MLS data with preexisting airborne laser scans from 2003 using point-cloud and solid-modeling methodologies. Additionally, we conducted repeat MLS scans to measure the magnitude and spatial variation of fault afterslip, exceeding 20 cm in some places, particularly in the southern portion of the rupture zone. We anticipate these data sets, in conjunction with independently collected ground-based alinement arrays and space-based geodetic data will contribute significant insight into topics of current debate including assessing the most appropriate material models for shallow fault zones and how shallow and deeper fault slip relate to one another.

  6. Electric field control of E region coherent echoes: Evidence from radar observations at the South Pole

    NASA Astrophysics Data System (ADS)

    Makarevich, Roman A.; Forsythe, V. V.; Kellerman, A. C.

    2015-03-01

    Characteristics and formation mechanisms of E region plasma irregularities at high latitudes are investigated using observations with the newly deployed Super Dual Auroral Radar Network (SuperDARN) radar at the South Pole Antarctic station (SPS) near a magnetic latitude (MLAT) of 75°S. It is shown that E region echo occurrence at SPS exhibits a diurnal variation that is significantly different from those at auroral and polar cap latitudes. Moreover, analysis of major spectral populations also showed a distinct and previously unreported diurnal pattern. The plasma drift velocity estimates are derived at E region ranges of SPS, leveraging the SPS radar's position well within the MLAT region where SuperDARN convection estimates are well constrained by the data. It is shown that E region irregularity occurrence increases when the convection direction is within the SPS field of view and/or when the plasma drift component is comparable with the nominal ion-acoustic speed Cs of 350 m/s. This is the expected behavior for irregularities generated directly by the modified two-stream plasma instability (MTSI). On the other hand, irregularity velocity dependence on convection velocity showed an unexpected saturation at velocity values smaller than nominal Cs. It is demonstrated that the convection velocity at which irregularity velocity starts to differ from the convection component and to approach a maximum value is dependent on the magnetic aspect angle. Moreover, the maximum velocity value itself also depends on the aspect angle. The observed behavior is discussed in context of recent models that involve evolving aspect angles as a key characteristic of MTSI saturation.

  7. A WFC3 Grism Emission Line Redshift Catalog in the GOODS-South Field

    NASA Astrophysics Data System (ADS)

    Morris, Aaron M.; Kocevski, Dale D.; Trump, Jonathan R.; Weiner, Benjamin J.; Hathi, Nimish P.; Barro, Guillermo; Dahlen, Tomas; Faber, Sandra M.; Finkelstein, Steven L.; Fontana, Adriano; Ferguson, Henry C.; Grogin, Norman A.; Grützbauch, Ruth; Guo, Yicheng; Hsu, Li-Ting; Koekemoer, Anton M.; Koo, David C.; Mobasher, Bahram; Pforr, Janine; Salvato, Mara; Wiklind, Tommy; Wuyts, Stijn

    2015-06-01

    We combine Hubble Space Telescope (HST)/Wide Field Camera3 (WFC3) imaging and G141 grism observations from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) and 3D-HST surveys to produce a catalog of grism spectroscopic redshifts for galaxies in the CANDELS/GOODS-South field. The WFC3/G141 grism spectra cover a wavelength range of 1.1≤slant λ ≤slant 1.7 μm with a resolving power of R∼ 130 for point sources, thus providing rest-frame optical spectra for galaxies out to z∼ 3.5. The catalog is selected in the H-band (F160W) and includes both galaxies with and without previously published spectroscopic redshifts. Grism spectra are extracted for all H-band detected galaxies with H ≤slant 24 and a CANDELS photometric redshift {{z}phot}≥slant 0.6. The resulting spectra are visually inspected to identify emission lines, and redshifts are determined using cross-correlation with empirical spectral templates. To establish the accuracy of our redshifts, we compare our results against high-quality spectroscopic redshifts from the literature. Using a sample of 411 control galaxies, this analysis yields a precision of {{σ }NMAD}=0.0028 for the grism-derived redshifts, which is consistent with the accuracy reported by the 3D-HST team. Our final catalog covers an area of 153 arcmin2 and contains 1019 redshifts for galaxies in GOODS-S. Roughly 60% (608/1019) of these redshifts are for galaxies with no previously published spectroscopic redshift. These new redshifts span a range of 0.677≤slant z≤slant 3.456 and have a median redshift of z = 1.282. The catalog contains a total of 234 new redshifts for galaxies at z\\gt 1.5. In addition, we present 20 galaxy pair candidates identified for the first time using the grism redshifts in our catalog, including four new galaxy pairs at z∼ 2, nearly doubling the number of such pairs previously identified.

  8. Ground based aerosol characterization during the South American Biomass Burning Analysis (SAMBBA) field experiment

    NASA Astrophysics Data System (ADS)

    Brito, J.; Rizzo, L. V.; Morgan, W. T.; Coe, H.; Johnson, B.; Haywood, J.; Longo, K.; Freitas, S.; Andreae, M. O.; Artaxo, P.

    2014-05-01

    This paper investigates the physical and chemical characteristics of aerosols at ground level at a site heavily impacted by biomass burning. The site is located near Porto Velho, Rondônia, in the Southwestern part of the Brazilian Amazon forest, and was selected for the deployment of a large suite of instruments, among them an Aerosol Chemical Speciation Monitor. Our measurements were made during the South American Biomass Burning Analysis (SAMBBA) field experiment, which consisted of a combination of aircraft and ground based measurements over Brazil, aiming to investigate the impacts of biomass burning emissions on climate, air quality, and numerical weather prediction over South America. The campaign took place during the dry season and the transition to the wet season in September/October 2012. During most of the campaign, the site was impacted by regional biomass burning pollution (average CO mixing ratio of 0.6 ppm), occasionally superimposed by intense (up to 2 ppm of CO), freshly emitted biomass burning plumes. Aerosol number concentrations ranged from ∼1000 cm-3 to peaks of up to 35 000 cm-3 during biomass burning (BB) events, corresponding to an average submicron mass mean concentrations of 13.7 μg m-3 and peak concentrations close to 100 μg m-3. Organic aerosol strongly dominated the submicron non-refractory composition, with an average concentration of 11.4 μg m-3. The inorganic species, NH4, SO4, NO3, and Cl, were observed on average at concentrations of 0.44, 0.34, 0.19, and 0.01 μg m-3, respectively. Equivalent Black Carbon (BCe) ranged from 0.2 to 5.5 μg m-3, with an average concentration of 1.3 μg m-3. During BB peaks, organics accounted for over 90% of total mass (submicron non-refractory plus BCe), among the highest values described in the literature. We examined the ageing of Biomass Burning Organic Aerosol (BBOA) using the changes in the H : C and O : C ratios, and found that throughout most of the aerosol processing (O : C ≅ 0

  9. Ground-based aerosol characterization during the South American Biomass Burning Analysis (SAMBBA) field experiment

    NASA Astrophysics Data System (ADS)

    Brito, J.; Rizzo, L. V.; Morgan, W. T.; Coe, H.; Johnson, B.; Haywood, J.; Longo, K.; Freitas, S.; Andreae, M. O.; Artaxo, P.

    2014-11-01

    This paper investigates the physical and chemical characteristics of aerosols at ground level at a site heavily impacted by biomass burning. The site is located near Porto Velho, Rondônia, in the southwestern part of the Brazilian Amazon rainforest, and was selected for the deployment of a large suite of instruments, among them an Aerosol Chemical Speciation Monitor. Our measurements were made during the South American Biomass Burning Analysis (SAMBBA) field experiment, which consisted of a combination of aircraft and ground-based measurements over Brazil, aimed to investigate the impacts of biomass burning emissions on climate, air quality, and numerical weather prediction over South America. The campaign took place during the dry season and the transition to the wet season in September/October 2012. During most of the campaign, the site was impacted by regional biomass burning pollution (average CO mixing ratio of 0.6 ppm), occasionally superimposed by intense (up to 2 ppm of CO), freshly emitted biomass burning plumes. Aerosol number concentrations ranged from ~1000 cm-3 to peaks of up to 35 000 cm-3 (during biomass burning (BB) events, corresponding to an average submicron mass mean concentrations of 13.7 μg m-3 and peak concentrations close to 100 μg m-3. Organic aerosol strongly dominated the submicron non-refractory composition, with an average concentration of 11.4 μg m-3. The inorganic species, NH4, SO4, NO3, and Cl, were observed, on average, at concentrations of 0.44, 0.34, 0.19, and 0.01 μg m-3, respectively. Equivalent black carbon (BCe) ranged from 0.2 to 5.5 μg m-3, with an average concentration of 1.3 μg m-3. During BB peaks, organics accounted for over 90% of total mass (submicron non-refractory plus BCe), among the highest values described in the literature. We examined the ageing of biomass burning organic aerosol (BBOA) using the changes in the H : C and O : C ratios, and found that throughout most of the aerosol processing (O : C &cong

  10. Discovery of a z ˜ 6 Galaxy in the Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Bunker, A. J.; Stanway, E. R.; Ellis, R. S.; McMahon, R. G.; McCarthy, P. J.

    2003-05-01

    We report the discovery of a luminous z=5.78 star-forming galaxy in the Chandra Deep Field South. This galaxy was selected as an ``i-drop'' from the GOODS public survey imaging with HST/ACS (object 3 in Stanway, Bunker & McMahon 2003, astro-ph/0302212). The large colour of (i'-z')AB=1.6 indicated a spectral break consistent with the Lyman-α forest absorption short-ward of Lyman-α at z≈ 6. The galaxy is very compact (marginally resolved with ACS with a half-light radius of 0.08 arcsec, so rhl<0.5 h-170 kpc). We have obtained a deep (5.5-hour) spectrum of this z'AB=24.7 galaxy with the DEIMOS optical spectrograph on Keck, and here we report the discovery of a single emission line centered on (8245+/- 1) Å detected at 20 σ with a flux of f≈ 2x 10-17 ergs cm-2 s-1. The line is clearly resolved with detectable structure at our resolution of better than 55 km s-1, and the only plausible interpretation consistent with the ACS photometry is that we are seeing Lyman-α emission from a z=5.78 galaxy. This is the highest redshift galaxy to be discovered and studied using HST data. The velocity width (Δ vFWHM=260 km s-1) and rest-frame equivalent width (Wrest Lyα =20 Å ) indicate that this line is most probably powered by star formation, as an AGN would typically have larger values. The starburst interpretation is supported by our non-detection of the high-ionization Nriptsize V λ 1240 Å emission line, and the absence of this source from the deep Chandra X-ray images. The star formation rate inferred from the rest-frame UV continuum is 33.8 h70-2 Msun yr-1 (Ω M=0.3, Ω Λ =0.7). This is the most luminous starburst known at z>5. Our spectroscopic redshift for this object confirms the validity of the i'-drop selection technique of Stanway, Bunker & McMahon (2003) to select star-forming galaxies at z≈ 6.

  11. The great observatories origins deep survey. VLT/VIMOS spectroscopy in the GOODS-south field

    NASA Astrophysics Data System (ADS)

    Popesso, P.; Dickinson, M.; Nonino, M.; Vanzella, E.; Daddi, E.; Fosbury, R. A. E.; Kuntschner, H.; Mainieri, V.; Cristiani, S.; Cesarsky, C.; Giavalisco, M.; Renzini, A.; GOODS Team

    2009-02-01

    Aims: We present the first results from the VIsible Multiobject Spectrograph (VIMOS) ESO/GOODS program of spectroscopy for faint galaxies in the Chandra Deep Field South (CDF-S). This program complements the FORS2 ESO/GOODS campaign. Methods: All 3312 spectra were obtained in service mode with VIMOS at the ESO/VLT UT3. The VIMOS LR-Blue and MR grisms were used to cover different redshift ranges. Galaxies at 1.8 < z < 3.5 were observed in the GOODS VIMOS-LR-Blue campaign. Galaxies at z < 1 and Lyman Break Galaxies at z > 3.5 were observed in the VIMOS MR survey. Results: Here we report results for the first 12 masks (out of 20 total). We extracted 2344 from 6 LR-Blue masks and 968 from 6 MR masks. A large percentage, 33% of the LR-Blue and 18% of the MR spectra, are serendipitous observations. We obtained 1481 and 656 redshifts in the LR-Blue and MR campaign, respectively, for a total success rate of 70% and 75%, respectively, which decrease to 63% and 68% when also the serendipitous targets are considered. The typical redshift accuracy is σz = 0.001. The reliability of the redshift estimate varies with the quality flag. The LR-Blue quality flag A redshifts are reliable at ~95% confidence level, flag B redshifs at ~70% and quality C et ~40%. The MR redshift reliability is somewhat higher: 100% for quality flag A, ~90% for quality flag B and ~70% for flag C. By complementing our VIMOS spectroscopic catalog with all existing spectroscopic redshifts publicly available in the CDF-S, we created a redshift master catalog. By comparing this redshift compilation with different photometric redshift catalogs we estimate the completeness level of the CDF-S spectroscopic coverage in several redshift bins. Conclusions: The completeness level is very high, >60%, at z < 3.5, and it is very uncertain at higher redshift. The master catalog was used also to estimate completeness and contamination levels of different galaxy photometric selection techniques. The BzK selection method

  12. A COMPREHENSIVE NONPOINT SOURCE FIELD STUDY FOR SEDIMENT, NUTRIENTS, AND PATHOGENS IN THE SOUTH FORK BROAD RIVER WATERSHED IN NORTHEAST GEORGIA

    EPA Science Inventory

    This technical report provides a description of the field project design, quality control, the sampling protocols and analysis methodology used, and standard operating procedures for the South Fork Broad River Watershed (SFBR) Total Maximum Daily Load (TMDL) project. This watersh...

  13. Reconnaissance of Field Sites for the Study of Chemical Weathering on the Guayana Shield, South America

    SciTech Connect

    Steefell, C I

    2003-02-01

    Despite the fact that chemical weathering of silicate rocks plays an important role in the draw-down of CO{sub 2} over geologic time scales (Berner and Berner, 1996), the overall controls on the rate of chemical weathering are still not completely understood. Lacking a mechanistic understanding of these controls, it remains difficult to evaluate a hypothesis such as that presented by Raymo and Ruddiman (1992), who suggested that enhanced weathering and CO{sub 2} draw-down resulting from the uplift of the Himalayas contributed to global cooling during the Cenozoic. At an even more fundamental level, the three to four order of magnitude discrepancy between laboratory and field weathering rates is still unresolved (White et al., 1996). There is as yet no comprehensive, mechanistic model for silicate chemical weathering that considers the coupled effects of precipitation, vadose zone flow, and chemical reactions. The absence of robust process models for silicate weathering and the failure to resolve some of these important questions may in fact be related-the controls on the overall rates of weathering cannot be understood without considering the weathering environment as one in which multiple, time-dependent chemical and physical processes are coupled (Malmstrom, 2000). Once chemical weathering is understood at a mechanistic process level, the important controls on chemical weathering (physical erosion, temperature, precipitation) can be folded into larger scale models tracking the global carbon cycle. Our goal in this study was to carry out the preliminary work needed to establish a field research site for chemical weathering om the Cuayana Shield in South America. The Guayana Shield is a Precambrian province greater than 1.5 billion years old covering portions of Venezuela, Guyana (the country), Surinam, French Guiana, and Brazil (Figure 1). More important than the age of the rocks themselves, however, is the age of the erosion surface developed on the Shield, with

  14. Tracking Holland Interest Codes: The Case of South African Field Guides

    ERIC Educational Resources Information Center

    Watson, Mark B.; Foxcroft, Cheryl D.; Allen, Lynda J.

    2007-01-01

    Holland believes that specific personality types seek out matching occupational environments and his theory codes personality and environment according to a six letter interest typology. Since 1985 there have been numerous American studies that have queried the validity of Holland's coding system. Research in South Africa is scarcer, despite…

  15. Organic Matter and Water Stability of Field Aggregates Affected by Tillage in South Dakota

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Increased tillage intensity has been associated with declines in soil organic matter (SOM). A case study was conducted (2001-2004) on adjacent farms (both in a two-year crop rotation) in eastern South Dakota to quantify tillage effects on components of SOM and soil aggregate stability. One farm used...

  16. Installation restoration program. Site investigation report for IRP site No. 12 and 13, South Dakota Air National Guard, 114th Fighter Wing, Joe Foss Field, Sioux Falls, South Dakota - Volume 1. Final report

    SciTech Connect

    1996-02-01

    Site Investigation Report for IRP Site No 12 and 13, South Dakota Air National Guard, 114th Fighter Wing, Joe Foss Field, Sioux Falls, South Dakota, Volume I. This is the first volume of a two volume site investigation report. Two sites (Site 12 - Ramp area and Site 13 - Motor Vehicle Maintenance Facility) was investigated under the Installation Restoration Program. Soil and groundwater samples were collected and analyzed. No further action was recommended on site 13 and quarterly sampling was recommended for site 12. South Dakota Regulators have agreed to both recommendations. Decision documents will be prepared for each site.

  17. Time lapse seismic observations and effects of reservoir compressibility at Teal South oil field

    NASA Astrophysics Data System (ADS)

    Islam, Nayyer

    One of the original ocean-bottom time-lapse seismic studies was performed at the Teal South oil field in the Gulf of Mexico during the late 1990's. This work reexamines some aspects of previous work using modern analysis techniques to provide improved quantitative interpretations. Using three-dimensional volume visualization of legacy data and the two phases of post-production time-lapse data, I provide additional insight into the fluid migration pathways and the pressure communication between different reservoirs, separated by faults. This work supports a conclusion from previous studies that production from one reservoir caused regional pressure decline that in turn resulted in liberation of gas from multiple surrounding unproduced reservoirs. I also provide an explanation for unusual time-lapse changes in amplitude-versus-offset (AVO) data related to the compaction of the producing reservoir which, in turn, changed an isotropic medium to an anisotropic medium. In the first part of this work, I examine regional changes in seismic response due to the production of oil and gas from one reservoir. The previous studies primarily used two post-production ocean-bottom surveys (Phase I and Phase II), and not the legacy streamer data, due to the unavailability of legacy prestack data and very different acquisition parameters. In order to incorporate the legacy data in the present study, all three post-stack data sets were cross-equalized and examined using instantaneous amplitude and energy volumes. This approach appears quite effective and helps to suppress changes unrelated to production while emphasizing those large-amplitude changes that are related to production in this noisy (by current standards) suite of data. I examine the multiple data sets first by using the instantaneous amplitude and energy attributes, and then also examine specific apparent time-lapse changes through direct comparisons of seismic traces. In so doing, I identify time-delays that, when

  18. Archaean atmospheric evolution: evidence from the Witwatersrand gold fields, South Africa

    NASA Astrophysics Data System (ADS)

    Frimmel, Hartwig E.

    2005-04-01

    The Witwatersrand gold fields in South Africa, the world's largest gold-producing province, play a pivotal role in the reconstruction of the Archaean atmosphere and hydrosphere. Past uncertainties on the genetic model for the gold caused confusion in the debate on Archaean palaeoenvironmental conditions. The majority of Witwatersrand gold occurs together with pyrite, uraninite and locally bitumen, on degradational surfaces of fluvial conglomerates that were laid down between 2.90 and 2.84 Ga in the Central Rand Basin. Although most of the gold appears as a precipitate within, or associated with, post-depositional hydrothermal phases and along microfractures, available microtextural, mineralogical, geochemical and isotopic data all indicate that this hydrothermal gold, analogous to some pyrite and uraninite, was derived from the local mobilisation of detrital particles. Some of the key pieces of evidence are a significant correlation of the gold, pyrite and uraninite with other heavy minerals as well as sedimentary lithofacies, local preservation of in-situ gold micronuggets and abundant rounded forms of pyrite and uraninite, compositional heterogeneity on a microscale of the gold as well as the rounded pyrite and uraninte, and radiometric age data that indicate an age of the gold, pyrite and uraninite that is older than the maximum age of deposition for the host sediment. None of these observations/data is compatible with any of the suggested hydrothermal models, in which auriferous fluids were introduced from an external source into the host rock succession after sediment deposition. In contrast, those arguments, used in favour of hydrothermal models, emphasise the microtextural position of most of the gold, which highlights the undisputed hydrothermal nature of that gold in its present position, but does not explain its ultimate source. Furthermore, the macro-scale setting of the stratiform ore deposits is in stark contrast to any known type of epigenetic

  19. The Chandra Deep Field-South Survey: 4 Ms Source Catalogs

    NASA Astrophysics Data System (ADS)

    Xue, Y. Q.; Luo, B.; Brandt, W. N.; Bauer, F. E.; Lehmer, B. D.; Broos, P. S.; Schneider, D. P.; Alexander, D. M.; Brusa, M.; Comastri, A.; Fabian, A. C.; Gilli, R.; Hasinger, G.; Hornschemeier, A. E.; Koekemoer, A.; Liu, T.; Mainieri, V.; Paolillo, M.; Rafferty, D. A.; Rosati, P.; Shemmer, O.; Silverman, J. D.; Smail, I.; Tozzi, P.; Vignali, C.

    2011-07-01

    We present source catalogs for the 4 Ms Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin2. We provide a main Chandra source catalog, which contains 740 X-ray sources that are detected with WAVDETECT at a false-positive probability threshold of 10-5 in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P < 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog sources. We determine X-ray source positions using centroid and matched-filter techniques and obtain a median positional uncertainty of ≈0farcs42. We also provide a supplementary catalog, which consists of 36 sources that are detected with WAVDETECT at a false-positive probability threshold of 10-5, satisfy the condition of 0.004 < P < 0.1, and have an optical counterpart with R < 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (≈97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (≈94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that >75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very

  20. THE CHANDRA DEEP FIELD-SOUTH SURVEY: 4 Ms SOURCE CATALOGS

    SciTech Connect

    Xue, Y. Q.; Luo, B.; Brandt, W. N.; Broos, P. S.; Schneider, D. P.; Bauer, F. E.; Lehmer, B. D.; Alexander, D. M.; Brusa, M.; Comastri, A.; Gilli, R.; Fabian, A. C.; Hasinger, G.; Hornschemeier, A. E.; Koekemoer, A.; Liu, T.; Mainieri, V.; Rosati, P.; Paolillo, M.; Rafferty, D. A.

    2011-07-01

    We present source catalogs for the 4 Ms Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin{sup 2}. We provide a main Chandra source catalog, which contains 740 X-ray sources that are detected with WAVDETECT at a false-positive probability threshold of 10{sup -5} in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P < 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog sources. We determine X-ray source positions using centroid and matched-filter techniques and obtain a median positional uncertainty of {approx}0.''42. We also provide a supplementary catalog, which consists of 36 sources that are detected with WAVDETECT at a false-positive probability threshold of 10{sup -5}, satisfy the condition of 0.004 < P < 0.1, and have an optical counterpart with R < 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen ({approx}97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 ({approx}94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that >75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and

  1. Glacier modeling in support of field observations of mass balance at South Cascade Glacier, Washington, USA

    USGS Publications Warehouse

    Josberger, Edward G.; Bidlake, William R.

    2010-01-01

    The long-term USGS measurement and reporting of mass balance at South Cascade Glacier was assisted in balance years 2006 and 2007 by a new mass balance model. The model incorporates a temperature-index melt computation and accumulation is modeled from glacier air temperature and gaged precipitation at a remote site. Mass balance modeling was used with glaciological measurements to estimate dates and magnitudes of critical mass balance phenomena. In support of the modeling, a detailed analysis was made of the "glacier cooling effect" that reduces summer air temperature near the ice surface as compared to that predicted on the basis of a spatially uniform temperature lapse rate. The analysis was based on several years of data from measurements of near-surface air temperature on the glacier. The 2006 and 2007 winter balances of South Cascade Glacier, computed with this new, model-augmented methodology, were 2.61 and 3.41 mWE, respectively. The 2006 and 2007 summer balances were -4.20 and -3.63 mWE, respectively, and the 2006 and 2007 net balances were -1.59 and -0.22 mWE. PDF version of a presentation on the mass balance of South Cascade Glacier in Washington state. Presented at the American Geophysical Union Fall Meeting 2010.

  2. An Intercomparison of RADARSAT-2, SMOS and Field Measured Soil Moisture in the Berambadi Watershed, South India

    NASA Astrophysics Data System (ADS)

    Tomer, S. K.; Al Bitar, A.; Sekhar, M.; Merlin, O.; Bandyopadhyay, S.; Kerr, Y. H.

    2012-12-01

    This study presents an intercomparison of the RADARSAT-2 derived soil moisture, SMOS derived soil moisture and field measured soil moisture in the Berambadi watershed, South India. Seventeen images of RADARSAT-2, SMOS products, and field data collected in the 50 field plots during 2010-2011 were used. The data were collected from field campaigns in the framework of AMBHAS project. A non parametric algorithm was developed based on the CDF transformation to retrieve the soil moisture from RADARSAT-2 backscatter coefficient at a spatial resolution of 100 m based on the measured soil moisture. The developed algorithm to retrieve surface soil moisture from RADARSAT-2 provided a good estimate of the field plot soil moisture with a RMSE of 0.05 cm3 cm-3. The average soil moisture from RADARSAT-2 and field measured soil moisture were compared to SMOS derived soil moisture at the watershed scale. Several averaging strategies were considered to take into account the surface heterogeneity and SMOS antenna patterns. Results were analysed by taking into consideration the soil texture heterogeneity, radio frequency interference effect and climatic effect. SMOS underestimated the soil moisture in compare to both RADARSAT-2 and field averaged soil moisture. A bias correction for the SMOS data is suggested using Clayton copula. SMOS showed a better correlation with the RADARSAT-2 watershed averaged soil moisture than directly averaged field soil moisture, as field campaign covered a smaller region of the watershed than RADARSAT-2 data. This shows the potential synergy between the use of active/passive microwave soil moisture for upscalling/downscalling soil moisture.

  3. Comparison of LANDSAT-2 and field spectrometer reflectance signatures of south Texas rangeland plant communities

    NASA Technical Reports Server (NTRS)

    Richardson, A. J.; Escobar, D. E.; Gausman, H. W.; Everitt, J. H. (Principal Investigator)

    1982-01-01

    The accuracy was assessed for an atmospheric correction method that depends on clear water bodies to infer solar and atmospheric parameters for radiative transfer equations by measuring the reflectance signature of four prominent south Texas rangeland plants with the LANDSAT satellite multispectral scanner (MSS) and a ground based spectroradiometer. The rangeland plant reflectances produced by the two sensors were correlated with no significant deviation of the slope from unity or of the intercept from zero. These results indicated that the atmospheric correction produced LANDSAT MSS estimates of rangeland plant reflectances that are as accurate as the ground based spectroradiometer.

  4. Floating production platforms and their applications in the development of oil and gas fields in the South China Sea

    NASA Astrophysics Data System (ADS)

    Zhang, Dagang; Chen, Yongjun; Zhang, Tianyu

    2014-03-01

    This paper studies the current available options for floating production platforms in developing deepwater oil fields and the potential development models of future oil and gas exploration in the South China Sea. A detailed review of current deepwater platforms worldwide was performed through the examples of industry projects, and the pros and cons of each platform are discussed. Four types of platforms are currently used for the deepwater development: tension leg platform, Spar, semi-submersible platform, and the floating production system offloading. Among these, the TLP and Spar can be used for dry tree applications, and have gained popularity in recent years. The dry tree application enables the extension of the drilling application for fixed platforms into floating systems, and greatly reduces the cost and complexity of the subsea operation. Newly built wet tree semi-submersible production platforms for ultra deepwater are also getting their application, mainly due to the much needed payload for deepwater making the conversion of the old drilling semi-submersible platforms impossible. These platforms have been used in different fields around the world for different environments; each has its own advantages and disadvantages. There are many challenges with the successful use of these floating platforms. A lot of lessons have been learned and extensive experience accumulated through the many project applications. Key technologies are being reviewed for the successful use of floating platforms for field development, and potential future development needs are being discussed. Some of the technologies and experience of platform applications can be well used for the development of the South China Sea oil and gas field.

  5. z {approx} 7 GALAXY CANDIDATES FROM NICMOS OBSERVATIONS OVER THE HDF-SOUTH AND THE CDF-SOUTH AND HDF-NORTH GOODS FIELDS

    SciTech Connect

    Bouwens, Rychard J.; Illingworth, Garth D.; Gonzalez, Valentino; Holden, Brad; Magee, Dan; Labbe, Ivo; Franx, Marijn; Conselice, Christopher J.; Blakeslee, John; Van Dokkum, Pieter; Marchesini, Danilo; Zheng Wei

    2010-12-20

    We use {approx}88 arcmin{sup 2} of deep ({approx}>26.5 mag at 5{sigma}) NICMOS data over the two GOODS fields and the HDF-South to conduct a search for bright z {approx}> 7 galaxy candidates. This search takes advantage of an efficient preselection over 58 arcmin{sup 2} of NICMOS H{sub 160}-band data where only plausible z {approx}> 7 candidates are followed up with NICMOS J{sub 110}-band observations. {approx}248 arcmin{sup 2} of deep ground-based near-infrared data ({approx}>25.5 mag, 5{sigma}) are also considered in the search. In total, we report 15 z{sub 850}-dropout candidates over this area-7 of which are new to these search fields. Two possible z {approx} 9 J{sub 110}-dropout candidates are also found, but seem unlikely to correspond to z {approx} 9 galaxies (given the estimated contamination levels). The present z {approx} 9 search is used to set upper limits on the prevalence of such sources. Rigorous testing is undertaken to establish the level of contamination of our selections by photometric scatter, low-mass stars, supernovae, and spurious sources. The estimated contamination rate of our z {approx} 7 selection is {approx}24%. Through careful simulations, the effective volume available to our z {approx}> 7 selections is estimated and used to establish constraints on the volume density of luminous (L*{sub z{sub ={sub 3}}}, or {approx}-21 mag) galaxies from these searches. We find that the volume density of luminous star-forming galaxies at z {approx} 7 is 13{sup +8}{sub -5} times lower than at z {approx} 4 and >25 times lower (1{sigma}) at z {approx} 9 than at z {approx} 4. This is the most stringent constraint yet available on the volume density of {approx}>L*{sub z{sub ={sub 3}}} galaxies at z {approx} 9. The present wide-area, multi-field search limits cosmic variance to {approx}<20%. The evolution we find at the bright end of the UV LF is similar to that found from recent Subaru Suprime-Cam, HAWK-I or ERS WFC3/IR searches. The present paper also

  6. Effects of CRP field age and cover type on ring-necked pheasants in eastern South Dakota

    USGS Publications Warehouse

    Eggebo, S.L.; Higgins, K.F.; Naugle, D.E.; Quamen, F.R.

    2003-01-01

    Loss of native grasslands to tillage has increased the importance of Conservation Reserve Program (CRP) grasslands to maintain ring-necked pheasant (Phasianus colchicus) populations. Despite the importance of CRP to pheasants, little is known about the effects of CRP field age and cover type on pheasant abundance and productivity in the northern Great Plains. Therefore, we assessed effects of these characteristics on pheasant use of CRP fields. We stratified CRP grasslands (n=42) by CRP stand age (old [10-13 yrs] vs. new [1-3 yrs] grasslands) and cover type (CP1 [cool-season grasslands] vs. CP2 [warm-season grasslands]) in eastern South Dakota and used crowing counts and roadside brood counts to index ring-necked pheasant abundance and productivity. Field-age and cover-type effects on pheasant abundance and productivity were largely the result of differences in vegetation structure among fields. More crowing pheasants were recorded in old cool-season CRP fields than any other age or cover type, and more broods were recorded in cool- than warm-season CRP fields. Extending existing CRP contracts another 5-10 years would provide the time necessary for new fields to acquire the vegetative structure used most by pheasants without a gap in habitat availability. Cool-season grass-legume mixtures (CP1) that support higher pheasant productivity should be given equal or higher ratings than warm-season (CP2) grass stands. We also recommend that United States Department of Agriculture administrators and field staff provide broader and more flexible guidelines on what seed mixtures can be used in CRP grassland plantings in the northern Great Plains. This would allow landowners and natural resource professionals who manage pheasant habitat to plant a mosaic of cool- and warm-season CRP grassland habitats.

  7. Source regions of long-period pulsation events in electron precipitation and magnetic fields at South Pole Station

    SciTech Connect

    Paquette, J.A.; Matthews, D.L.; Rosenberg, T.J.; Lanzerotti, L.J.; Inan, U.S.

    1994-03-01

    Pulsation events with long (100-1000 s) periods with a consistent frequency in both particle precipitation and surface geomagnetic field variations have been reported in the past from measurements made at various geomagnetic latitudes. An examination of broad beam riometer and magnetometer data from South Pole Station for the interval from 1982 to 1989 revealed nearly 200 such events. The onset times of these events were determined. This mechanism ascribes the occurrence of correlated magnetic and precipitation pulsations to ULF modulation of equatorial VLF wave-particle interactions. For this reason, VLF data from South Pole Station were also examined. Taking into consideration the ULF wave and particle transit times from an interaction region near the magnetic equator to the ground leads to an expectation that the onset of pulsations in the magnetometer data will lag the onset of pulsations in the riometer data by several minutes. This disparity in onset times, together with modulation of VLF emissions in the 0.5-1 kHz band, serves as an important indicator of whether or not an event can be explained by the above-cited theory. While about a third of the events fit the prediction of Coroniti and Kennel, another third do not. In these events, the onset of magnetic and precipitation pulsations is nearly simultaneous, and possible alternative generation mechanisms are explored. In the remaining third of the events, magnetic pulsations begin substantially earlier than precipitation pulsations. Events of this type appear at first to be inexplicable in terms of any transit time argument. However, data from the imaging riometer at South Pole Station indicate that this third class of events is probably not physically distinct from the first two but is the result of the differing areas to which the riometer and magnetometer are sensitive and can be accounted for by considering the effects of transverse motion of a persistent precipitation region. 24 refs., 13 rigs.

  8. Applications of exploration technologies to reservoir prediction and management -- Field examples of South-East Asia

    SciTech Connect

    Duval, B.C.; Allen, G.; Madaoui, K.; Gouadain, J.; Kremer, Y.

    1995-10-01

    The paper describes how modern geoscience techniques, developed for a large part in intensive exploration programs, can be used at the field level to improve reservoir prediction and production planning and also to optimize recovery. Detailed sedimentological studies has allowed the authors to determine the environment of the reservoir formations and help define the likely shape and size of individual sands and refine the reservoir model. An illustration is given by fields located in the Mahakam delta area of Kalimantan (Handil, Tunu) and in the Gulf of Thailand (Bongkot). Sequence stratigraphy assists in identifying efficient regional seals which, at field scale, lead to the recomposition of a great number of individual sands (several hundreds in some cases) into fewer flow units, making the system manageable from a reservoir standpoint. This technology was used extensively to delineate the giant Peciko gas field of Indonesia. The geophysical approach of reservoir parameters and the use of seismic attributes are rapidly expanding. The Yadana gas field in the Gulf of Martaban (Myanmar) is a case in point to show how porosities can be determined from impedances obtained by seismic inversion techniques. An example from the Bongkot field shows how 3D seismic and direct hydrocarbon indication technology (DHI) are used to deal with complex faulting to optimize deviated well profiles and improve recoveries.

  9. The generation and expulsion of gases in Ya131 gas field, South China Sea: implication of laboratory pyrolysis results

    NASA Astrophysics Data System (ADS)

    Geng, Ansong; Zhou, Yi; Fu, Jiamo; Sheng, Guoying; Zhang, Qiming

    1998-08-01

    Laboratory pyrolysis methods were used to determine the source and thermal maturity of the gas accumulation in the Ya131 gas field, South China Sea. The mudstone source rock samples used in the pyrolysis experiments were selected from the Yacheng and Meishan Formations in the Ying-Qiong Basin. The total amount of gases generated and expelled from the Yacheng Formation mudstone is larger than that from the Meishan Formation mudstone, suggesting that the gas generation potential of the Yacheng Formation is higher than that of the Meishan Formation. The similarity between the gases from the Ya131 field and the gases produced at the higher pyrolysis temperatures used in the maturation study, in terms of wetness, the amounts of C 1, C 2, C 3, and the percentages of C 1, C 2-C 4 and C 5-C 7, implies that the gases of the Ya131 field are high maturity gases. However, there are distinct differences between the normalised molecular compositions of the C 6 and C 7 species of the gases from the Ya131 field and those of the pyrolysis gases produced in the laboratory. Comparison of the stable carbon isotope composition of the n-alkanes, pristane (Pr) and phytane (Ph) in the saturated hydrocarbon fraction of the condensate from the Ya131 field with that of rock extracts from the Yacheng, Meishan, Ying-Huang Formations indicates no definite correlation between the condensate and the extracts. These observations suggest that there may be additional source rocks for the Ya131 field, existing within the deeper part of the basin.

  10. CANDIDATE CLUSTERS OF GALAXIES AT z > 1.3 IDENTIFIED IN THE SPITZER SOUTH POLE TELESCOPE DEEP FIELD SURVEY

    SciTech Connect

    Rettura, A.; Stern, D.; Martinez-Manso, J.; Gettings, D.; Gonzalez, A. H.; Mei, S.; Ashby, M. L. N.; Brodwin, M.; Stanford, S. A.; Bartlett, J. G.

    2014-12-20

    We present 279 galaxy cluster candidates at z > 1.3 selected from the 94 deg{sup 2} Spitzer South Pole Telescope Deep Field (SSDF) survey. We use a simple algorithm to select candidate high-redshift clusters of galaxies based on Spitzer/IRAC mid-infrared data combined with shallow all-sky optical data. We identify distant cluster candidates adopting an overdensity threshold that results in a high purity (80%) cluster sample based on tests in the Spitzer Deep, Wide-Field Survey of the Boötes field. Our simple algorithm detects all three 1.4 < z ≤ 1.75 X-ray detected clusters in the Boötes field. The uniqueness of the SSDF survey resides not just in its area, one of the largest contiguous extragalactic fields observed with Spitzer, but also in its deep, multi-wavelength coverage by the South Pole Telescope (SPT), Herschel/SPIRE, and XMM-Newton. This rich data set will allow direct or stacked measurements of Sunyaev-Zel'dovich effect decrements or X-ray masses for many of the SSDF clusters presented here, and enable a systematic study of the most distant clusters on an unprecedented scale. We measure the angular correlation function of our sample and find that these candidates show strong clustering. Employing the COSMOS/UltraVista photometric catalog in order to infer the redshift distribution of our cluster selection, we find that these clusters have a comoving number density n{sub c}=(0.7{sub −0.6}{sup +6.3})×10{sup −7} h{sup 3} Mpc{sup −3} and a spatial clustering correlation scale length r {sub 0} = (32 ± 7) h {sup –1} Mpc. Assuming our sample is comprised of dark matter halos above a characteristic minimum mass, M {sub min}, we derive that at z = 1.5 these clusters reside in halos larger than M{sub min}=1.5{sub −0.7}{sup +0.9}×10{sup 14} h{sup −1} M{sub ⊙}. We find that the mean mass of our cluster sample is equal to M{sub mean}=1.9{sub −0.8}{sup +1.0}×10{sup 14} h{sup −1} M{sub ⊙}; thus, our sample contains the progenitors of

  11. Candidate Clusters of Galaxies at z > 1.3 Identified in the Spitzer South Pole Telescope Deep Field Survey

    NASA Astrophysics Data System (ADS)

    Rettura, A.; Martinez-Manso, J.; Stern, D.; Mei, S.; Ashby, M. L. N.; Brodwin, M.; Gettings, D.; Gonzalez, A. H.; Stanford, S. A.; Bartlett, J. G.

    2014-12-01

    We present 279 galaxy cluster candidates at z > 1.3 selected from the 94 deg2 Spitzer South Pole Telescope Deep Field (SSDF) survey. We use a simple algorithm to select candidate high-redshift clusters of galaxies based on Spitzer/IRAC mid-infrared data combined with shallow all-sky optical data. We identify distant cluster candidates adopting an overdensity threshold that results in a high purity (80%) cluster sample based on tests in the Spitzer Deep, Wide-Field Survey of the Boötes field. Our simple algorithm detects all three 1.4 < z <= 1.75 X-ray detected clusters in the Boötes field. The uniqueness of the SSDF survey resides not just in its area, one of the largest contiguous extragalactic fields observed with Spitzer, but also in its deep, multi-wavelength coverage by the South Pole Telescope (SPT), Herschel/SPIRE, and XMM-Newton. This rich data set will allow direct or stacked measurements of Sunyaev-Zel'dovich effect decrements or X-ray masses for many of the SSDF clusters presented here, and enable a systematic study of the most distant clusters on an unprecedented scale. We measure the angular correlation function of our sample and find that these candidates show strong clustering. Employing the COSMOS/UltraVista photometric catalog in order to infer the redshift distribution of our cluster selection, we find that these clusters have a comoving number density nc = (0.7+6.3-0.6) × 10-7 h3 {Mpc}-3 and a spatial clustering correlation scale length r 0 = (32 ± 7) h -1 Mpc. Assuming our sample is comprised of dark matter halos above a characteristic minimum mass, M min, we derive that at z = 1.5 these clusters reside in halos larger than Mmin = 1.5+0.9-0.7 × 1014 h-1 M⊙ . We find that the mean mass of our cluster sample is equal to Mmean = 1.9+1.0-0.8 × 1014 h-1 M⊙ ; thus, our sample contains the progenitors of present-day massive galaxy clusters.

  12. Overview of the South American Biomass Burning Analysis (SAMBBA) field experiment in Brazil during Sept - Oct 2012

    NASA Astrophysics Data System (ADS)

    Johnson, Ben; Haywood, Jim; Longo, Karla; Coe, Hugh; Artaxo, Paulo; Morgan, William; Freitas, Saulo

    2013-04-01

    The South American Biomass Burning Analysis (SAMBBA) is an international research project investigating the impacts of biomass burning emissions on climate, air quality and numerical weather prediction over South America. The project involves a combination of measurements and modelling activities to assess the role of biomass burning and biogenic emissions in the earth system. This international collaboration has been led by a partnership between the Met Office, the Brazilian National Institute for Space research (INPE), the University of Sao Paulo, and a consortium of UK Universities. The measurement program was headed by the deployment of UK's Facility for Airborne Atmospheric Measurements (FAAM) BAe-146 research aircraft over Brazil during the dry season of September - October 2012. This was co-ordinated with ground-based measurements operated by the University of Sao Paulo and INPE. This successful field experiment now provides an excellent source of observations to build our understanding of biomass burning processes and improve model simulations of biomass burning aerosols and their interactions with biogenic emissions, atmospheric chemistry, clouds, radiation, and the terrestrial biosphere. This talk will summarise the field experiment, including the aircraft measurements and ground-based observations made during the dry season of 2012. Preliminary results will highlight the range of biomass burning and biogenic emissions observed from tropical forest, deforested zones and scrub-land. Case studies will also show infra-red camera images of fire radiative output, the evolution of large smoke plumes and the variable composition of background aerosol and extensive haze layers across the region. The lidar data and aircraft profiles also highlight the prevalence of elevated aerosol layers observed at altitudes of 3 - 7km, presumed to be detrainment from large smoke plumes, pyrocumulus and mid-level convection. The ground-based observations also highlight the

  13. Models of Active Glacial Isostasy Roofing Warm Subduction: Case of the South Patagonian Ice Field

    NASA Technical Reports Server (NTRS)

    Klemann, Volker; Ivins, Erik R.; Martinec, Zdenek; Wolf, Detlef

    2007-01-01

    Modern geodetic techniques such as precise Global Positioning System (GPS) and high-resolution space gravity mapping (Gravity Recovery and Climate Experiment, GRACE) make it possible to measure the present-day rate of viscoelastic gravitational Earth response to present and past glacier mass changes. The Andes of Patagonia contain glacial environments of dramatic mass change. These mass load changes occur near a tectonically active boundary between the Antarctic and South American plates. The mechanical strength of the continental side of this boundary is influenced by Neogene ridge subduction and by the subduction of a youthful oceanic slab. A ridge of young volcanos parallels the Pacific coastline. Release of volatiles (such as water) at depth along this ridge creates a unique rheological environment. To assess the influence of this rheological ridge structure on the observational land uplift rate, we apply a two dimensional viscoelastic Earth model. A numerical study is presented which examines the sensitivity of the glacial loading-unloading response to the complex structure at depth related to the subducting slab, the viscous wedge between slab and continental lithosphere, and the increase of elastic thickness from oceanic to continental lithosphere. A key feature revealed by our numerical experiments is a continuum flow wherein the slab subdues the material transport toward oceanic mantle and crust. The restricted flow is sensitive to the details of slab mechanical strength and penetration into the upper mantle. The reduced viscosity within the mantle wedge, however, enhances the load-induced material transport everywhere within the asthenosphere.

  14. Geology, compositional heterogeneities, and geochemical origin of the Yacheng gas field, Qiongdongnan Basin, South China Sea

    SciTech Connect

    Hao, F.; Li, S.; Sun, Y.; Zhang, Q.

    1998-07-01

    The Yacheng gas field is located in the footwall of the No. 1 fault, the boundary fault between the Yinggehai and Qiongdongnan basins. All strata are normally pressured in the gas field except for the Meishan Formation. The Meishan Formation is overpressured near the No. 1 fault in the gas field and in the adjacent Yinggehai Basin. An obvious thermal anomaly occurs below 3600 m in the gas field. This anomaly, characterized by an abrupt increase in drill-stem test and fluid-inclusion homogenization temperatures, vitrinite reflectance (R{sub o}), and Rock-Eval T{sub max}, and by an abnormally low temperature/R{sub o}/T{sub max} gradient, diminishes away from the Yinggehai Basin. The gases and condensates have abnormally high aromatic hydrocarbon contents and show obvious heterogeneities. Away from the No. 1 fault, the C{sub 2+} hydrocarbon content and C{sub 2+}/{Sigma}C{sub n} increase; carbon dioxide content decreases; {delta}{sup 13}C values for methane, ethane, and carbon dioxide become lighter; the heptane and isoheptane values decrease; and the relative contents of aromatic hydrocarbons, both in C{sub 6}/C{sub 7} light hydrocarbons and in the condensates, decrease. The gas field was charged from both the Qiongdongnan and the Yinggehai basins. Hydrocarbons sourced from the Qiongdongnan Basin have relatively low maturities, whereas hydrocarbons from the Yinggehai Basin have relatively higher maturities and seem to have been in association with hydrothermal fluids. The hydrothermal fluids from the Yinggehai Basin, in which methane, ethane, carbon dioxide, and especially aromatic hydrocarbons dissolved under the high-temperature and high-pressure subsurface conditions, migrated along the No. 1 fault and caused the abnormally high concentration of aromatic hydrocarbons, as well as the thermal anomalies in the gas field, especially near the No. 1 fault.

  15. A new South American network to study the atmospheric electric field and its variations related to geophysical phenomena

    NASA Astrophysics Data System (ADS)

    Tacza, J.; Raulin, J.-P.; Macotela, E.; Norabuena, E.; Fernandez, G.; Correia, E.; Rycroft, M. J.; Harrison, R. G.

    2014-12-01

    In this paper we present the capability of a new network of field mill sensors to monitor the atmospheric electric field at various locations in South America; we also show some early results. The main objective of the new network is to obtain the characteristic Universal Time diurnal curve of the atmospheric electric field in fair weather, known as the Carnegie curve. The Carnegie curve is closely related to the current sources flowing in the Global Atmospheric Electric Circuit so that another goal is the study of this relationship on various time scales (transient/monthly/seasonal/annual). Also, by operating this new network, we may also study departures of the Carnegie curve from its long term average value related to various solar, geophysical and atmospheric phenomena such as the solar cycle, solar flares and energetic charged particles, galactic cosmic rays, seismic activity and specific meteorological events. We then expect to have a better understanding of the influence of these phenomena on the Global Atmospheric Electric Circuit and its time-varying behavior.

  16. Local Lunar Gravity Field Analysis over the South Pole-aitken Basin from SELENE Farside Tracking Data

    NASA Technical Reports Server (NTRS)

    Goossens, Sander Johannes; Ishihara, Yoshiaki; Matsumoto, Koji; Sasaki, Sho

    2012-01-01

    We present a method with which we determined the local lunar gravity field model over the South Pole-Aitken (SPA) basin on the farside of the Moon by estimating adjustments to a global lunar gravity field model using SELENE tracking data. Our adjustments are expressed in localized functions concentrated over the SPA region in a spherical cap with a radius of 45deg centered at (191.1 deg E, 53.2 deg S), and the resolution is equivalent to a 150th degree and order spherical harmonics expansion. The new solution over SPA was used in several applications of geophysical analysis. It shows an increased correlation with high-resolution lunar topography in the frequency band l = 40-70, and admittance values are slightly different and more leveled when compared to other, global gravity field models using the same data. The adjustments expressed in free-air anomalies and differences in Bouguer anomalies between the local solution and the a priori global solution correlate with topographic surface features. The Moho structure beneath the SPA basin is slightly modified in our solution, most notably at the southern rim of the Apollo basin and around the Zeeman crater

  17. Monitoring of flood irrigation for the characterization of irrigation practices of grassland fields in the Crau region (South of France)

    NASA Astrophysics Data System (ADS)

    Alkassem Alosman, Mohamed; Ruy, Stéphane; Olioso, Albert; Flamain, Fabrice

    2015-04-01

    Surface irrigation (flooding and furrow) is the main irrigation technic in the world. This irrigation system is known as having poor water efficiency and that results in very large water losses through drainage and runoff out the field. Although these unused water amounts can generate positive externalities (wetlands and groundwater recharge), a decreased of water volume used in surface irrigation is sought in a context of limited water resource. In the Crau area (South of France), more than 12,500 ha of grassland are irrigated by flooding. There, at the regional scale, it is estimated that the water volumes brought into the field are very high; and ranges from 15,000; up to 20,000 m3.h-1.year-1; more than 78% of these amounts recharges the Crau aquifer (Saos, 2006). However, the actual volumes which are injected to the plot surface (the " irrigation dose ") are insufficiently known, because of the diversity of encountered agricultural practices and fields topography. For better characterizing these practices, a campaign of irrigation monitoring has been carried out during an irrigation season (March to September 2014) on a set of representative plots of soil variability, practices, and different stages of hay grow. Each grassland field has been also characterized from a topographical and pedological view point. A mobile device for measurements (soil moisture and water level probes, photographic monitoring, soil sampling, .. ) was deployed for each irrigation. A total of 35 irrigation events were followed. The data obtained allow describing accurately and quantitatively the variability in encountered irrigation practices. Combined with a flood irrigation model (Model CALHY, Bader et al., 2010, Hydrol. Sci. J., 55, 177-191), these data will be used to calculate the water balance at the field scale: amounts of injected, infiltrated and lost water by runoff or drainage. They will also offer different ways for optimizing the irrigation efficiency.

  18. Validation of in situ networks via field sampling: case study in the South Fork Experimental Watershed

    Technology Transfer Automated Retrieval System (TEKTRAN)

    The calibration and validation of soil moisture remote sensing products is complicated by the logistics of installing a soil moisture network for a long term period in an active landscape. Therefore, these stations are located along field boundaries or in non-representative sites with regards to so...

  19. FIELD EVALUATION OF A SWIRL DEGRITTER AT TAMWORTH, NEW SOUTH WALES, AUSTRALIA

    EPA Science Inventory

    This field evaluation program was initiated with the overall objective of providing information on the behaviour of a full scale swirl degritter designed and constructed in accordance with the shapes and proportions developed during model studies. The swirl degritter was designed...

  20. Petrology and depositional environment of Sunniland producing fields of south Florida

    SciTech Connect

    Mitchell-Tapping, H.J.

    1984-09-01

    Oil exploration began in Florida in 1901, but no oil was found until 1943. In November of that year, Humble Oil and Refining Co. made a discovery near Sunniland in southern Florida. This field and the producing zone were called Sunniland. No further discoveries were made in southern Florida until 1954 when the Forty-Mile field was discovered by Gulf Oil Co. Ten years later, in 1964, the Sunoco Felda field was discovered by Sun Oil Co., followed by West Sunoco Felda field in 1968. The examination of numerous cores and thin sections of this formation, both from producing fields and wildcat wells, reveals a sequence of deposition in the Sunniland formation. It has been reported that tintinnids or calpionellids have been observed in the lower mud section, but investigation of many thin sections from this section revealed only ostracod particles. Above the mudstone, the section becomes increasingly plentiful in fragmented microbored rudist particles and forams such as Orbitolina texana, Dictyoconus floridanus, and Coskinolina sunnilandensis. Above this section the sequence is considered regressive and consists of pellets and forams with a few mollusk fragments. This section is interpreted as the basal unit of a grainstone bar shoal. The grainstone bar shoal is made up of reworked particles of oysters (Texigryphea), coated caprinid fragments, forams, and echinoid fragments. For some years, the rocks of the Sunniland formation have been considered reefal, but based on the results of this study, these rocks are interpreted to be a barrier tidal-shoal bar deposited well behind the main reef crest, which lies farther offshore at the edge of the Florida escarpment.

  1. Statistical scaling, Shannon entropy, and Generalized space-time q-entropy of rainfall fields in tropical South America.

    PubMed

    Poveda, Germán; Salas, Hernán D

    2015-07-01

    We study diverse scaling and information theory characteristics of Mesoscale Convective Systems (MCSs) as seen by the Tropical Rainfall Measuring Mission (TRMM) over continental and oceanic regions of tropical South America, and 2-D radar rainfall fields from Amazonia. The bi-dimensional Fourier spectra of MCSs exhibit inverse power laws with respect to the spatial scale, whose scaling exponents, β, capture the type of spatial correlation of rainfall among the study regions, including those over the Andes of Colombia as well as over oceanic and Amazonian regions. The moment-scaling analysis evidences that the structure function deviates from simple scaling at order q > 1.0, thus signaling the multi-scaling nature of rainfall fields within MCSs in tropical South America, with departures from simple scaling associated with the physical characteristics of MCSs over the different study regions. Entropy is estimated for a large set of radar rainfall fields during the distinctive atmospheric regimes (Easterly and Westerly events) in this part of Amazonia. Results evidence that there are significant differences in the dynamics of rainfall among regimes. No clear-cut relationship is found between entropy and the first two statistical moments, but power fits in space and time, S(γ) ∼ γ(-η) for skewness and, S(κ) ∼ κ(-ϵ) for kurtosis. The exponents η and ϵ are statistically different between Easterly and Westerly events, although the significance of fits is less when L-moments are used to estimate skewness and kurtosis. Interesting differences are identified between the time and space generalized q-entropy functions of Amazonian rainfall fields. In both cases, the functions are a continuous set of power laws (analogous to the structure function in turbulence), S(T, q) ∼ T(β), and, S(λ, q) ∼ λ(β), covering a broad range of temporal and spatial scales. Both time and space generalized q-entropy functions exhibit linear growth in the

  2. Statistical scaling, Shannon entropy, and Generalized space-time q-entropy of rainfall fields in tropical South America

    NASA Astrophysics Data System (ADS)

    Poveda, Germán; Salas, Hernán D.

    2015-07-01

    We study diverse scaling and information theory characteristics of Mesoscale Convective Systems (MCSs) as seen by the Tropical Rainfall Measuring Mission (TRMM) over continental and oceanic regions of tropical South America, and 2-D radar rainfall fields from Amazonia. The bi-dimensional Fourier spectra of MCSs exhibit inverse power laws with respect to the spatial scale, whose scaling exponents, β, capture the type of spatial correlation of rainfall among the study regions, including those over the Andes of Colombia as well as over oceanic and Amazonian regions. The moment-scaling analysis evidences that the structure function deviates from simple scaling at order q > 1.0, thus signaling the multi-scaling nature of rainfall fields within MCSs in tropical South America, with departures from simple scaling associated with the physical characteristics of MCSs over the different study regions. Entropy is estimated for a large set of radar rainfall fields during the distinctive atmospheric regimes (Easterly and Westerly events) in this part of Amazonia. Results evidence that there are significant differences in the dynamics of rainfall among regimes. No clear-cut relationship is found between entropy and the first two statistical moments, but power fits in space and time, S(γ) ˜ γ-η for skewness and, S(κ) ˜ κ-ɛ for kurtosis. The exponents η and ɛ are statistically different between Easterly and Westerly events, although the significance of fits is less when L-moments are used to estimate skewness and kurtosis. Interesting differences are identified between the time and space generalized q-entropy functions of Amazonian rainfall fields. In both cases, the functions are a continuous set of power laws (analogous to the structure function in turbulence), S(T, q) ˜ Tβ, and, S(λ, q) ˜ λβ, covering a broad range of temporal and spatial scales. Both time and space generalized q-entropy functions exhibit linear growth in the range -1.0 < q < -0.5, and

  3. Near-field monitoring of seismic source behavior at South African deep gold mines

    NASA Astrophysics Data System (ADS)

    Ogasawara, H.; Nakatani, M.; Iio, Y.; Ishii, H.; Yamada, T.; Naoi, M.; Yasutake, G.; Kawakata, H.; Yamamoto, A.; Yamauchi, T.; Nakao, S.; Yabe, Y.; Otsuki, K.; Satoh, T.; Kato, A.; Shinya, Y.; Nagata, K.; Kuwano, O.; Igarashi, T.; Miyake, H.; Ide, S.; van Aswegen, G.; Mendecki, A.; Ward, T.; SeeSA Research Group

    2007-12-01

    We introduce our SeeSA projects, as important as dense array monitoring According to a mining plan and a geological map detailing locations of faults or weakness, we can anticipate potential M > 2 seismic sources at depths of 2.0 - 3.6 km at South African gold mines. At such potential sources, we have installed instruments prior to an onset of irreversible process to monitor earthquake generation process. From the previous projects for periods of from a year to a few years, the possible widest dynamic range and resolution have revealed the finest detail of the process since 1995 in cooperation with ISS International Ltd and South African gold mines (Mponeng, Bambanani, Tau Tona, Buffelsfontein GM, and ERPM), Wits Univ., Geohydroseis CC., Seismogen CC., OHMS CC., GFZ, GMuG, CSIR. The talk summarizes examples of our successful monitoring and introduces some on-going projects. Highlighted are the following. Yamada et al. [05, 07] demonstrated that mine tremors have rupture process as complex as natural larger earthquakes and the scale dependency of rupture parameters is similar to that for natural larger earthquakes. We successfully recorded strain accumulations larger than 100 micro strain, followed by several hundreds of seismic events (-1 < M < 3; distance < ~ 250 m). The seismicity within about 100m from strainmeters caused frequent, seismic strain-steps; the largest recorded was greater than 100 micro strain by an M2.5 earthquake at a distance within ~100 m. One of the most important results were that no detectable accelerating precursors preceded strain-steps associated with several hundreds of the earthquakes (- 1 < M < 3) catalogued by mine's seismic networks (hereinafter Catalogued E/Q; Takeuchi 05), while significant post-seismic drifts followed some strain-steps by Catalogued E/Qs. Frequently observed were episodic strain changes with durations of much slower than strain-steps associated with the Catalogued E/Qs [Naoi et al. 06]. Striking were some examples

  4. Seismic-stratigraphic analysis of Hollingsworth field, Fall River County, South Dakota

    SciTech Connect

    Morel, J.A.; Bursk, P.H.; Finch, J.W.

    1986-08-01

    Hollingsworth field produces from a preserved dune in the second bench of the Leo member, Minnelusa Formation. It was discovered in 1984 by Citation Oil and Gas using high-resolution seismic data. The field was fully developed on the basis of seismic data and consists of five wells, all of which encountered the dune. Four wells produce oil, and one is used to reinject produced water. Both the Converse and Leo members consist of interbedded sandstones, shales, carbonates, and anhydrites with occasional preserved dunes. Hydrocarbon traps are formed by structural closure over the top of preserved dunes or by the occurrence of isolated sandstones encased in impermeable facies. The sandstone isopach anomalies occur in several benches of the Converse and Leo members. These are evidenced in outcrops and well logs. High-resolution seismic data can be used to locate these anomalies efficiently and economically.

  5. Validation of in Situ Networks Via Field Sampling: Case Study in the South Fork Experimental Watershed

    NASA Astrophysics Data System (ADS)

    Cosh, M. H.; McKee, L.; Bindlish, R.; Coopersmith, E. J.; Jackson, T. J.; Prueger, J. H.

    2014-12-01

    The calibration and validation of soil moisture remote sensing products is complicated by the logistics of installing a soil moisture network for a long term period in an active landscape. Therefore, these stations are located along field boundaries or in non-representative sites with regards to soil type or soil moisture. The representative character of this network can only be established by large scale field sampling to provide a calibration dataset. A team of samplers were deployed twice a week for the summer of 2014 to collect surface soil moisture data across a variety of land covers at 44 sites. These samples were compared and scaled to the domain to get a better understanding of the large scale soil moisture distributions and dynamics. In addition, comparisons are made to the Soil Moisture Ocean Salinity (SMOS) soil moisture product for the length of the network installation.

  6. Turtle Bayou - 1936 to 1983: case history of a major gas field in south Louisiana

    SciTech Connect

    Cronquist, C.

    1983-01-01

    Turtle Bayou field, located in the middle Miocene trend in S. Louisiana, is nearing the end of a productive life which spans over 30 yr. Discovered by Shell Oil Co. in 1949 after unsuccessful attempts by 2 other majors, the field is a typical, low relief, moderately faulted Gulf Coast structure, probably associated with deep salt movement. The productive interval includes 22 separate gas-bearing sands in a regressive sequence of sands and shales from approx. 6500 to 12,000 ft. Now estimated to have contained ca 1.2 trillion scf of gas in place, cumulative production through 1982 was 702 billion scf. Cumulative condensate-gas ratio has been 20 bbl/million. Recovery mechanisms in individual reservoirs include strong bottom water drive, partial edgewater drive, and pressure depletion. Recovery efficiencies in major reservoirs range from 40 to 75% of original gas in place.

  7. Miller field, a subtle upper Jurassic submarine fan trap in the South Viking Graben, United Kingdom sector, North Sea

    SciTech Connect

    McClure, N.M.; Brown, A.A. )

    1990-09-01

    The Miller field is situated at a depth of 4 km in the South Viking Graben, some 270 km northeast of Aberdeen, Scotland. The field was discovered in 1983 in previously relinquished UK Licence Blocks 16/7b and 16/8b. The discovery can be attributed to a detailed understanding of the regional sedimentological and seismic velocity models that predicted the presence of submarine fan sediments within a structural nose some 10 km away from the graben margin sediment source. The field reservoir comprises up to 100 m of oil-bearing Upper Jurassic, Brae Formation turbidites. Cores, electric logs, and well test analyses show the turbidites have excellent reservoir qualities. Porosity ranges from 12 to 23%, and net:gross ratios are typically greater than 0.75. The reservoir is highly productive with permeability typically in the range of 50 to 1200 md. The reservoir fluid is an undersaturated, CO{sub 2}-rich, sour, 37.5{degree} API oil sourced from the Kimmeridge Clay Formation, which overlies and interfingers the reservoir. The oil is trapped by a subtle combination of structural and stratigraphic mechanisms., The field will be developed using 30 wells drilled from a single platform. A total of ten wells (five producers and five injectors) will be pre-drilled through a template prior to platform installation. The first of these was spudded in March 1989 in preparation for first oil production planned for early 1992. Ultimate recovery is estimated to be around 300 MM STB and 0.57 tcf of associated gas.

  8. The First Public Release of South Pole Telescope Data: Maps of a 95 deg2 Field from 2008 Observations

    NASA Astrophysics Data System (ADS)

    Schaffer, K. K.; Crawford, T. M.; Aird, K. A.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Cho, H. M.; Crites, A. T.; de Haan, T.; Dobbs, M. A.; George, E. M.; Halverson, N. W.; Holder, G. P.; Holzapfel, W. L.; Hoover, S.; Hrubes, J. D.; Joy, M.; Keisler, R.; Knox, L.; Lee, A. T.; Leitch, E. M.; Lueker, M.; Luong-Van, D.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mohr, J. J.; Montroy, T. E.; Padin, S.; Plagge, T.; Pryke, C.; Reichardt, C. L.; Ruhl, J. E.; Shirokoff, E.; Spieler, H. G.; Stalder, B.; Staniszewski, Z.; Stark, A. A.; Story, K.; Vanderlinde, K.; Vieira, J. D.; Williamson, R.

    2011-12-01

    The South Pole Telescope (SPT) has nearly completed a 2500 deg2 survey of the southern sky in three frequency bands. Here, we present the first public release of SPT maps and associated data products. We present arcminute-resolution maps at 150 GHz and 220 GHz of an approximately 95 deg2 field centered at R.A. 82fdg7, decl. -55°. The field was observed to a depth of approximately 17 μK arcmin at 150 GHz and 41 μK arcmin at 220 GHz during the 2008 austral winter season. Two variations on map filtering and map projection are presented, one tailored for producing catalogs of galaxy clusters detected through their Sunyaev-Zel'dovich effect signature and one tailored for producing catalogs of emissive sources. We describe the data processing pipeline, and we present instrument response functions, filter transfer functions, and map noise properties. All data products described in this paper are available for download at http://pole.uchicago.edu/public/data/maps/ra5h30dec-55 and from the NASA Legacy Archive for Microwave Background Data Analysis server. This is the first step in the eventual release of data from the full 2500 deg2 SPT survey.

  9. Tolerance of nonindigenous cichlid fishes (Cichlasoma urophthalmus, Hemichromis letourneuxi) to low temperature: laboratory and field experiments in south Florida

    USGS Publications Warehouse

    Schofield, Pamela J.; Loftus, William F.; Kobza, Robert M.; Cook, Mark I.; Slone, Daniel H.

    2010-01-01

    The cold tolerance of two non-native cichlids (Hemichromis letourneuxi and Cichlasoma urophthalmus) that are established in south Florida was tested in the field and laboratory. In the laboratory, fishes were acclimated to two temperatures (24 and 28°C), and three salinities (0, 10, and 35 ppt). Two endpoints were identified: loss of equilibrium (11.5–13.7°C for C. urophthalmus; 10.8–12.5°C for H. letourneuxi), and death (9.5–11.1°C for C. urophthalmus; 9.1–13.3°C for H. letourneuxi). In the field, fishes were caged in several aquatic habitats during two winter cold snaps. Temperatures were lowest (4.0°C) in the shallow marsh, where no fish survived, and warmest in canals and solution-holes. Canals and ditches as shallow as 50 cm provided thermal refuges for these tropical fishes. Because of the effect on survival of different habitat types, simple predictions of ultimate geographic expansion by non-native fishes using latitude and thermal isoclines are insufficient for freshwater fishes.

  10. Surficial geology of the Safsaf region, south-central Egypt, derived from remote-sensing and field data

    USGS Publications Warehouse

    Davis, P.A.; Breed, C.S.; McCauley, J.F.; Schaber, G.G.

    1993-01-01

    We used a decorrelation-stretched image of Landsat Thematic Mapper (TM) Bands 1, 4, and 7 and field data to map and describe the main surficial units in the hyperarid Safsaf region in south-central Egypt. We show that the near-infrared bands on Landsat TM, which are sensitive to very subtle changes in mineralogy common to arid regions, significantly improve the geologist's capability to discriminate geologic units in desert regions. These data also provide the spatial and spectral information necessary to determine the migration patterns and provenance of eolian materials. The Safsaf area was the focus of our post flight field studies using Shuttle Imaging Radar (SIR) data following the discovery of buried paleochannels in North Africa. Most of the channels discernible on SIR images are not expressed in TM data, but traces of a few channels are present in both the SIR and the TM data within the Wadi Safsaf area. Here we present a detailed digital examination of the SIR and the TM-band reflectance and reflectance-ratio data at three locations of the more obvious surface expressions of the buried channels. Our results indicate that the TM expressions of the channels are not purely topographic but are more compositional in nature. Two possibilities may account for the TM expressions of the buried channels: 1) concentrations of windblown, iron-rich materials that accumulated along subtle curvilinear topograpohic traps, or 2) curvilinear exposures of an iron-rich underlying unit of the flat sand sheet. ?? 1993.

  11. Variations of a gradient of potential electrical field in the south of East Siberia

    NASA Astrophysics Data System (ADS)

    Krechetov, A. A.; Shamansky, U. V.

    2006-02-01

    In work the daily variations of a gradient of potential of an atmosphere electrical field close pulp and paper mill (Baikalsk region) and in the Lake Baikal are analyzed. For the analysis the results of measurements of a gradient of potential in seven items located on various distance from a source of pollution, on the same technique are used. Three are revealed such as a daily course of a gradient of potential, which are substantially caused by transformation of emissions by local winds in area of the lake Baikal. Spectral and components the analysis of results of measurements has allowed to reveal 2-nd and 7 hour periods of fluctuations.

  12. VizieR Online Data Catalog: z>~5 AGN in Chandra Deep Field-South (Weigel+, 2015)

    NASA Astrophysics Data System (ADS)

    Weigel, A. K.; Schawinski, K.; Treister, E.; Urry, C. M.; Koss, M.; Trakhtenbrot, B.

    2015-09-01

    The Chandra 4-Ms source catalogue by Xue et al. (2011, Cat. J/ApJS/195/10) is the starting point of this work. It contains 740 sources and provides counts and observed frame fluxes in the soft (0.5-2keV), hard (2-8keV) and full (0.5-8keV) band. All object IDs used in this work refer to the source numbers listed in the Xue et al. (2011, Cat. J/ApJS/195/10) Chandra 4-Ms catalogue. We make use of Hubble Space Telescope (HST)/Advanced Camera for Surveys (ACS) data from the Great Observatories Origins Deep Survey South (GOODS-south) in the optical wavelength range. We use catalogues and images for filters F435W (B), F606W (V), F775W (i) and 850LP (z) from the second GOODS/ACS data release (v2.0; Giavalisco et al., 2004, Cat. II/261). We use Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) Wide Field Camera 3 (WFC3)/infrared data from the first data release (DR1, v1.0) for passbands F105W (Y), F125W (J) and F160W (H) (Grogin et al., 2011ApJS..197...35G; Koekemoer et al., 2011ApJS..197...36K). To determine which objects are red, dusty, low-redshift interlopers, we also include the 3.6 and 4.5 micron Spitzer Infrared Array Camera (IRAC) channels. We use SIMPLE image data from the DR1 (van Dokkum et al., 2005, Spitzer Proposal, 2005.20708) and the first version of the extended SIMPLE catalogue by Damen et al. (2011, Cat. J/ApJ/727/1). (6 data files).

  13. A joint geophysical analysis of the Coso geothermal field, south-eastern California

    NASA Astrophysics Data System (ADS)

    Wamalwa, Antony M.; Mickus, Kevin L.; Serpa, Laura F.; Doser, Diane I.

    2013-01-01

    Three-dimensional density models derived from gravity data and two-dimensional resistivity models derived from magnetotelluric data collected in the vicinity of the Coso geothermal field are analyzed in order to determine the source region of the geothermal field. The derived models show zones of both low resistivity and low density at and below 6 km depth in the Devils Kitchen and the Coso Hot Springs areas. These zones agree with seismic reflection and tomography results which found a high amplitude reflector at 5 km and low velocities zones below 5 km. We interpret the density and resistivity zones to indicate the presence of cooling magmatic material that provides the heat for the shallower geothermal system in these regions. A zone marked by high resistivity and low density was found to lie directly above the interpreted partially melted region extending to within 1 km depth below the surface in the reservoir region where it is capped by a low resistivity clay zone. In addition, the density models indicate that the high density bodies occurring under volcanic outcrops may be mafic intrusions.

  14. A COMPREHENISVE NONPOINT SOURCE FIELD STUDY FOR SEDIMENT, NUTRIENTS AND PATHOGENS IN THE SOUTH FORK BROAD RIVER WATERSHED IN NORTHEAST GEORGIA

    EPA Science Inventory

    There is an urgent need for EPA to develop protocols for establishing Total Maximum Daily Loads (TMDLs) in streams, lakes and estuaries. A cooperative TMDL field data collection project between ORD and Region 4 is ongoing in the South Fork Broad River Watershed (SFBR), a 245.18 ...

  15. Reaction of common bean cultivars to the Asian soybean rust pathogen, Phakopsora pachyrhizi, under field conditions in South Africa and Brazil.

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Phakopsora pachyrhizi, the Asian soybean rust (ASR) pathogen, infects soybeans (Glycine max) and some 95 other leguminous species, including dry and snap beans (Phaseolus vulgaris). This pathogen has been reported infecting dry beans under field conditions in South Africa and the United States in 20...

  16. Exploitation of oil in a volcanic cone by horizontal drilling in the Elaine field, south Texas

    SciTech Connect

    Martinez, P.A.; Kushner, P.L.; Harbaugh, J.W.

    1991-03-01

    The Uvalde volcanic field west and southwest of San Antonio contains many buried volcanic cones that offer attractive places to exploit with horizontal drilling. These buried cones were formed by eruption of basaltic flows and cinders during the Cretaceous when the Austin Chalk and immediately overlying strate were deposited. The cones vary in size, some being as much as 2 mi in diameter and 1000 ft in vertical dimension. During eruptions, flows and ejecta reacted with sea water, producing intermixtures of basaltic material and limestone. These cones provide attractive targets for oil exploration. The Elaine field about 90 mi southwest of San Antonio is associated with a buried volcanic cone that is now being exploited with horizontal drilling. Horizontal Drilling and Production, Inc., ('HDP') drilled the Autumn 1 as the initial horizontal well at Elaine. A vertical hole was drilled through the cone and underlying Austin Chalk, reconfirming the presence of the oil zone at the contact between volcanics and chalk. Moving back up the hole, a cement plug was set within the volcanics, and a horizontal hole was directed on a N 70W azimuth. The inclined hole's vertical angle had progressively decreased with distance to about 30{degree} from the horizontal when the oil zone was reentered. The hole's inclination continued to decrease within the oil zone, becoming horizontal after about 600 ft. With further distance, the hole passed beneath the oil zone, where its inclination was then reversed so that it climbed gradually and reentered the oil zone before reaching its terminal distance of 1500 horizontal feet. The well was completed on August 17, 1990, with an indicated initial production of 1609 BOPD.

  17. Variations of the Geomagnetic Field During the Holocene-Pleistocene: Relative Paleointensity Records From South-Western Argentina

    NASA Astrophysics Data System (ADS)

    Gogorza, C. S.

    2008-05-01

    I present a review of the research carried out by the Group of Geomagnetism at Universidad Nacional del Centro (Argentina) on paleointensity records from bottom sediments from three lakes: Escondido (Gogorza et al., 2004), Moreno (Gogorza et al., 2006) and El Trébol (Gogorza et al., 2007; Irurzun et al., 2008) (South-Western Argentina, 41° S, 71° 30'W). Based on these studies, we construct a first relative (RPI) stack for South-Western Argentina covering the last 21,000 14C years BP. The degree of down-core homogeneity of magnetic mineral content as well as magnetic mineral concentration and grain sizes vary between all lakes and are quantified by high-resolution rock magnetic measurements. Rock magnetic studies suggest that the main carriers of magnetization are ferrimagnetic minerals, predominantly pseudo-single domain magnetite The remanent magnetization at 20 mT (NRM20mT) was normalized using the anhysteric remanent magnetization at 20mT (ARM20mT), the saturation of the isothermal remanent at 20 mT (SIRM20mT) and the low field magnetic susceptibility {k}. Coherence function analysis indicates that the normalised records are free of environmental influences. Our paleointensity (NRM20mT/ ARM20mT) versus age curve shows a good agreement with published records from other parts of the world suggesting that, in suitable sediments, paleointensity of the geomagnetic field can give a globally coherent, dominantly dipolar signal. References Gogorza, C.S.G., Irurzun, M.A., Chaparro, M.A.E., Lirio, J.M., Nuñez, H., Bercoff, P.G., Sinito, A.M. Relative Paleointensity of the Geomagnetic Field over the last 21,000 years bp from Sediment Cores, Lake El Trébol, (Patagonia, Argentina). Earth, Planets and Space. V58(10), 1323-1332. 2006. Gogorza, C.S.G., Sinito, A.M., Lirio, J.M., Nuñez, H., Chaparro, M.A.E., Bertorello, H.R. Paleointensity Studies on Holocene-Pleistocene Sediments from Lake Escondido, Argentina. Physical of the Earth and Planetary Interiors, Elsevier, ISSN

  18. Fluvial architecture and reservoir heterogeneity of middle Frio sandstones, Seeligson field, Jim Wells and Kleberg Counties, south Texas

    SciTech Connect

    Jirik, L.A.; Kerr, D.R.; Zinke, S.G.; Finley, R.J. )

    1990-05-01

    Evaluation of fluvial Frio reservoirs in south Texas reveals a complex architectural style potentially suited to the addition of incremental gas reserves through recognition of untapped compartments or bypassed gas zones. Seeligson field is being studied as part of a GRI/DOE/Texas-sponsored program, in cooperation with Oryx Energy Company and Mobil Exploration and Production U.S., Inc., and is designed to develop technologies and methodologies for increasing gas reserves from conventional reservoirs in mature fields. Seeligson field, discovered in 1937, has produced 2.2 tcf of gas from more than 50 middle Frio reservoirs. Cross sections as well as net sand and log facies maps illustrate depositional style, sandstone geometry, and reservoir heterogeneities. Far-offset vertical seismic profiles show laterally discontinuous reflections corresponding to the reservoirs. Lenticular lateral-bar sandstones dominate channel-fill deposits that together are commonly less than 50 ft thick, forming belts of sandstone approximately 2,500 ft wide. Crevasse-splay deposits commonly extend a few thousand feet beyond the channel system. Sand-rich channel-fill deposits are flanked by levee and overbank mudstones, isolating the reservoirs in narrow, dip-elongate trends. Deposition on an aggrading coastal plain resulted in a pattern of laterally stacked sandstone bodies that are widespread across the study area. Alternating periods of more rapid aggradation resulted in deposition of vertically stacked sandstones with limited areal distribution. Facies architecture of both depositional styles has implications for reservoir compartmentalization. Reservoir compartments within a laterally stacked system may be leaky, resulting from sandstone contact from producing wells along depositional axes. This effect is a major factor controlling incremental recovery. Reservoirs in vertically stacked systems should be better isolated.

  19. Mantle xenocrysts of Chompolo field of the alkaline volcanics, Aldan shield, South Yakutia.

    NASA Astrophysics Data System (ADS)

    Nikolenko, Evgeny; Tychkov, Nikolay; Afanasiev, Valentin

    2015-04-01

    New mineralogical and chemical constraints for 10 dikes, veins (360-800m) and pipes (60-110 m) of Chompolo field discovered in 1957-1958 are discussed. Feld is located within Central Aldan Archean and Paleoproterozoic granulite-orthogneiss superterrane of Aldan-Stanovoy Shield, with peak of metamorphism - 2.1-1.9 Ga (Smelov, Timofeev, 2007). Originally (Shilina and Zeitlin 1959) and later (Kostrovitsky and Garanin 1992, Ashchepkov, Vladykin et al. 2001) these rocks were classified as kimberlites by mineralogy including pyrope, Cr spinel, and Cr diopside. Panina and Vladykin (1994), Davies et al, (2006) identified them as lamprophyres and lamproites. The age of Chompolo rocks is pre-Jurassic (Vladimirov et. al., 1989) dated by 40Ar/39Ar as 164.7±1 Ma (233.7±2.2 next plato)(unpublished Ashchepkov). The Rb-Sr isochron for lamprophyre "intrusions 104" indicate later age of 131±4 Ma (Zaitsev, Smelov, 2010). Magmatic bodies (Aldanskaya, Sputnik, Gornaya, Ogonek, Perevalnaya, Kilier-E) were studied during 2012-2013 fieldworks. Most of igneous rocks occur as inequigranular volcanic breccias with micro- or crypto-crystalline groundmass of K feldspar (up to 16.3 wt.% K2O, up to 3.2 wt.% FeO), chlorite, opaque minerals, melanocratic xenocrysts and phenocrysts (garnet, pyroxene, amphibole, Cr spinel, apatite, zircon, mica), and abundant xenogenic fragments of wallrock and crystalline basement. Garnet chemistry records the presence of mantle and crustal material. Mantle garnets lack the common megacryst, wehrlite, and high-temperature lherzolite varieties. Mantle mineralization prevails in the Aldan dike and the Sputnik, Gornaya, and Ogonek pipes, while crustal and elcogitic material is in the Perevalnaya and Kilier-E pipes. The Cr spinel consists of (in wt%) 3.5 to 50.9 Al2O3, 18.6-63.5 wt% Cr2O3, 6.1 to 19.1 MgO, and 0 to 1.61 TiO2. Al and Cr in spinels are in inverse proportion. The Chompolo alkaline volcanic rocks are most similar to the Central Aldan lamproites in trace

  20. Holocene records of geomagnetic field behavior from a north-south transect along the western Antarctic Peninsula

    NASA Astrophysics Data System (ADS)

    Brachfeld, S. A.; Shah, D. P.; St-Onge, M.; St-Onge, G.

    2013-12-01

    Geochronology is inherently difficult when working with Antarctic margin sediments. Radiocarbon dating and oxygen isotope stratigraphy are challenging or impossible in sites with poor preservation of biogenic calcite. Radiocarbon dating of the acid insoluble organic matter (AIOM) is further complicated by organically lean sediment and the presence of reworked organic carbon or detrital carbon from sedimentary rocks. These complications limit the ability to interpret a paleoclimate record. Geomagnetic paleointensity dating is a proven 'tuning' technique that has been successfully applied in several studies around the Antarctic margin. However, the reference curves to which these sites were tuned were constructed primarily from Northern Hemisphere data. Here we present paleomagnetic secular variation (PSV) and relative paleointensity (RPI) data from three Antarctic Peninsula sites that possess independent chronologies and which have moderate to ultra-high sedimentation rates (40 - 700 cm/ka). Maxwell Bay, located in the volcanic South Shetland Islands, is an ultra-high-resolution site with strongly magnetic sediments from which the Shallow Drilling (SHALDRIL) program recovered a 108-m record spanning the last 14 ka. Outer Barilari Bay and Hugo Island Trough, which lie to the South along the western Antarctic Peninsula, are moderate resolution sites with a high proportion of biogenic silica. Maxwell Bay and Bariliari Bay are unique in that they possess homogenous sediment and uniform magnetic mineral assemblages, while also preserving biogenic calcite, a rare combination on the Antarctic margin. All three sites preserve strong, stable remanent magnetizations with an easily isolated characteristic component and MAD values generally < 2°, with the exception of turbidites, intervals with abundant dropstones, and biosiliceous ooze intervals. Inclination values fluctuate between the present-day value at the cores sites (-58°) and the geomagnetic axial dipole inclination

  1. An Integrated Study of the Grayburg/San Andres Reservoir Foster and South Cowden fields,

    SciTech Connect

    1997-12-31

    GEOPHYSICAL OBJECTIVES: The goals of work done this quarter were to (1) refine the maps of seismic-derived porosity for the upper Grayburg for reapplication to the production model, (2) determine rock fabric and porosity patterns for the lower Grayburg and the upper San Andres, (3) relate any seismic-derived porosity characteristics, particularly seismic waveform attributes, to the historical production of oil allocated to lower Grayburg and San Andres zones, and (4) to test other geologic attributes for possible inter-relationships. GEOLOGIC OBJECTIVES: Continue the integrated geological/geophysical effort to develop a usable seismic velocity/log porosity transform for each Grayburg producing interval. The lower Grayburg and San Andres core were revisited to glean lithology and porosity information for the seismic inversion model. Update recent production and injection for each well in the study area. Add new production and injection wells to spreadsheet. Continue evaluation of effectiveness of recent completions, plug backs and injector conversions by monitoring oil production and produced water composition. ENGINEERING OBJECTIVES: To build the most accurate reservoir picture by continued integration of all data types available and utilize that model to optimize oil production. Monitoring and testing of new and worked-over wells continues to test the early production models. Methods to improve water quality are being evaluated using normal field management procedures.

  2. GIS-based technology for marine geohazards in LW3-1 Gas Field of the South China Sea

    NASA Astrophysics Data System (ADS)

    Su, Tianyun; Liu, Lejun; Li, Xishuang; Hu, Guanghai; Liu, Haixing; Zhou, Lin

    2013-04-01

    The exploration and exploitation of deep-water oil-gas are apt to be suffered from high-risk geo-hazards such as submarine landslide, soft clay creep, shallow gas, excess pore-water pressure, mud volcano or mud diaper, salt dome and so on. Therefore, it is necessary to survey the seafloor topography, identify the unfavourable geological risks and investigate their environment and mechanism before exploiting the deep-water oil-gas. Because of complex environment, the submarine phenomenon and features, like marine geohazards, can not be recognized directly. Multi-disciplinary data are acquired and analysed comprehensively in order to get more clear understanding about the submarine processes. The data include multi-beam bathymetry data, sidescan sonar images, seismic data, shallow-bottom profiling images, boring data, etc.. Such data sets nowadays increase rapidly to large amounts, but may be heterogeneous and have different resolutions. It is difficult to make good management and utilization of such submarine data with traditional means. GIS technology can provide efficient and powerful tools or services in such aspects as spatial data management, processing, analysis and visualization. They further promote the submarine scientific research and engineering development. The Liwan 3-1 Gas Field, the first deep-water gas field in China, is located in the Zhu II Depression in the Zhujiang Basin along the continental slope of the northern South China Sea. The exploitation of this field is designed to establish subsea wellhead and to use submarine pipeline for the transportation of oil. The deep-water section of the pipeline route in the gas field is to be selected to pass through the northern continental slope of the South China Sea. To avoid huge economic loss and ecological environmental damage, it is necessary to evaluate the geo-hazards for the establishment and safe operation of the pipeline. Based on previous scientific research results, several survey cruises have

  3. Properties of submillimeter galaxies in the CANDELS-S goods-south field

    SciTech Connect

    Wiklind, Tommy; Dahlen, Tomas; Ferguson, Henry C.; Grogin, Norman A.; Koekemoer, Anton M.; Dickinson, Mark E.; Guo, Yicheng; Barro, Guillermo; Fontana, Adriano; Castellano, Marco; Davé, Romeel; Yan, Haojing; Acquaviva, Viviana; Ashby, Matthew L. N.; Caputi, Karina I.; Dekel, Avishai; Donley, Jennifer L.; and others

    2014-04-20

    We derive physical properties of 10 submillimeter galaxies located in the CANDELS coverage of the GOODS-S field. The galaxies were first identified as submillimeter sources with the LABOCA bolometer and subsequently targeted for 870 μm continuum observation with ALMA. The high angular resolution of the ALMA imaging allows secure counterparts to be identified in the CANDELS multiband data set. The CANDELS data provide deep photometric data from UV through near-infrared wavelengths. Using synthetic spectral energy distributions, we derive photometric redshifts, stellar masses, extinction, ages, and the star formation history. The redshift range is z = 1.65-4.76, with two of the galaxies located at z > 4. Two submillimeter galaxy (SMG) counterparts have stellar masses 2-3 orders of magnitude lower than the rest. The remaining SMG counterparts have stellar masses around 1 × 10{sup 11} M {sub ☉}. The stellar population in the SMGs is typically older than the expected duration of the submillimeter phase, suggesting that the star formation history of SMGs is more complex than a single burst. Non-parametric morphology indices suggest that the SMG counterparts are among the most asymmetric systems compared with galaxies of the same stellar mass and redshift. The Hubble Space Telescope images show that three of the SMGs are associated with ongoing mergers. The remaining counterparts are isolated. Estimating the dust and molecular gas mass from the submillimeter fluxes, and comparing with our stellar masses shows that the gas mass fraction of SMGs is ∼28% and that the final stellar mass is likely to be ∼(1-2) × 10{sup 11} M {sub ☉}.

  4. Stellar Masses from the CANDELS Survey: The GOODS-South and UDS Fields

    NASA Astrophysics Data System (ADS)

    Santini, P.; Ferguson, H. C.; Fontana, A.; Mobasher, B.; Barro, G.; Castellano, M.; Finkelstein, S. L.; Grazian, A.; Hsu, L. T.; Lee, B.; Lee, S.-K.; Pforr, J.; Salvato, M.; Wiklind, T.; Wuyts, S.; Almaini, O.; Cooper, M. C.; Galametz, A.; Weiner, B.; Amorin, R.; Boutsia, K.; Conselice, C. J.; Dahlen, T.; Dickinson, M. E.; Giavalisco, M.; Grogin, N. A.; Guo, Y.; Hathi, N. P.; Kocevski, D.; Koekemoer, A. M.; Kurczynski, P.; Merlin, E.; Mortlock, A.; Newman, J. A.; Paris, D.; Pentericci, L.; Simons, R.; Willner, S. P.

    2015-03-01

    We present the public release of the stellar mass catalogs for the GOODS-S and UDS fields obtained using some of the deepest near-IR images available, achieved as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey project. We combine the effort from 10 different teams, who computed the stellar masses using the same photometry and the same redshifts. Each team adopted their preferred fitting code, assumptions, priors, and parameter grid. The combination of results using the same underlying stellar isochrones reduces the systematics associated with the fitting code and other choices. Thanks to the availability of different estimates, we can test the effect of some specific parameters and assumptions on the stellar mass estimate. The choice of the stellar isochrone library turns out to have the largest effect on the galaxy stellar mass estimates, resulting in the largest distributions around the median value (with a semi interquartile range larger than 0.1 dex). On the other hand, for most galaxies, the stellar mass estimates are relatively insensitive to the different parameterizations of the star formation history. The inclusion of nebular emission in the model spectra does not have a significant impact for the majority of galaxies (less than a factor of 2 for ~80% of the sample). Nevertheless, the stellar mass for the subsample of young galaxies (age <100 Myr), especially in particular redshift ranges (e.g., 2.2 < z < 2.4, 3.2 < z < 3.6, and 5.5 < z < 6.5), can be seriously overestimated (by up to a factor of 10 for <20 Myr sources) if nebular contribution is ignored.

  5. Wide-Field Imaging of the Hubble Deep Field-South Region. II. The Evolution of Galaxy Clustering at z < 1

    NASA Astrophysics Data System (ADS)

    Teplitz, Harry I.; Hill, Robert S.; Malumuth, Eliot M.; Collins, Nicholas R.; Gardner, Jonathan P.; Palunas, Povilas; Woodgate, Bruce E.

    2001-02-01

    We present the galaxy-galaxy angular correlations as a function of photometric redshift in a deep, wide galaxy survey centered on the Hubble Deep Field-South (HDF-S). Images were obtained with the Big Throughput Camera on the Blanco 4 m telescope at CTIO, of 1/2 square degree in broadband uBVRI, reaching ~24 mag. Approximately 40,000 galaxies are detected in the survey. We determine photometric redshifts using galaxy template fitting to the photometry. Monte Carlo simulations show that redshifts from these data should be reliable out to z~1, where the 4000 Å break shifts into the I band. The inferred redshift distribution, n(z), shows good agreement with the distribution of galaxies measured in the Hubble Deep Field-North (HDF-N) and the Canada-France Redshift Survey. After assigning galaxies to redshift bins with width Δz=0.33, we determine the two-point angular correlation function in each bin. We find that the amplitude of the correlation, Aw, drops across the three bins to redshift z~1. Simple ɛ models of clustering evolution fit this result, with the best agreement for ɛ=0. Hierarchical cold dark matter models best fit in a low-density, Λ-dominated universe. Based on observations obtained at Cerro Tololo Inter-American Observatory, a division of the National Optical Astronomy Observatories, which is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation.

  6. CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD

    SciTech Connect

    Guo Yicheng; Barro, Guillermo; Faber, Sandra M.; Koo, David C.; Giavalisco, Mauro; Willner, S. P.; Ashby, Matthew L. N.; Donley, Jennifer L.; Fontana, Adriano; Galametz, Audrey; Grazian, Andrea; Kocevski, Dale D.; McGrath, Elizabeth J.; Peth, Michael; Salvato, Mara; Wuyts, Stijn; and others

    2013-08-15

    We present a UV to mid-infrared multi-wavelength catalog in the CANDELS/GOODS-S field, combining the newly obtained CANDELS HST/WFC3 F105W, F125W, and F160W data with existing public data. The catalog is based on source detection in the WFC3 F160W band. The F160W mosaic includes the data from CANDELS deep and wide observations as well as previous ERS and HUDF09 programs. The mosaic reaches a 5{sigma} limiting depth (within an aperture of radius 0.''17) of 27.4, 28.2, and 29.7 AB for CANDELS wide, deep, and HUDF regions, respectively. The catalog contains 34,930 sources with the representative 50% completeness reaching 25.9, 26.6, and 28.1 AB in the F160W band for the three regions. In addition to WFC3 bands, the catalog also includes data from UV (U band from both CTIO/MOSAIC and VLT/VIMOS), optical (HST/ACS F435W, F606W, F775W, F814W, and F850LP), and infrared (HST/WFC3 F098M, VLT/ISAAC Ks, VLT/HAWK-I Ks, and Spitzer/IRAC 3.6, 4.5, 5.8, 8.0 {mu}m) observations. The catalog is validated via stellar colors, comparison with other published catalogs, zero-point offsets determined from the best-fit templates of the spectral energy distribution of spectroscopically observed objects, and the accuracy of photometric redshifts. The catalog is able to detect unreddened star-forming (passive) galaxies with stellar mass of 10{sup 10} M{sub Sun} at a 50% completeness level to z {approx} 3.4 (2.8), 4.6 (3.2), and 7.0 (4.2) in the three regions. As an example of application, the catalog is used to select both star-forming and passive galaxies at z {approx} 2-4 via the Balmer break. It is also used to study the color-magnitude diagram of galaxies at 0 < z < 4.

  7. Reservoir geology of Crystal Viking field, Lower Cretaceous estuarine tidal channel-bay complex, south-central Alberta

    SciTech Connect

    Reinson, G.E.; Clark, J.E.; Foscolos, A.E.

    1988-10-01

    The Lower Cretaceous Viking Formation in the Crystal field of south-central Alberta contains a linear sandstone body, as much as 30 m thick, that forms a complicated dual-pool hydrocarbon reservoir. This contrasts sharply with most other Viking reservoirs, which are much thinner, are commonly oriented northwest, and are composed of a single hydrocarbon pool. Thickness, orientation, and pool duality are attributed to the complicated depositional history of the Viking in the Crystal region. The sandstone body is interpreted as a multistage tidal channel-fill deposit within a larger estuarine channel-bay complex, which rests unconformably on inner shelf-lower shoreface facies. A major lowstand of sea level that occurred approximately 97 m.y. ago is believed to be responsible for incisement of the estuarine valley, which was filled during rising sea level. A depositional model of progressive estuarine valley fill under transgressive conditions readily accounts for the occurrence of two hydrodynamically separated oil pools, and also for differences in reservoir continuity and performance trends within the main oil-bearing A pool. Highly productive wells in the main pool correspond to specific channel-fill deposits, or are situated in areas where deposits of successive channel stages are highly superimposed. Conversely, marginally productive wells and poor reservoir communication between producing wells occur in areas where the different channel-stage deposits diverge. 22 figures, 2 tables.

  8. An Integrated Study of the Grayburg/San Andres Reservoir, Foster and South Cowden Fields, Ector County Texas

    SciTech Connect

    Weinbrandt, Richard; Trentham, Robert C; Robinson, William

    1997-10-23

    For a part of the Foster and South Cowden (Grayburg-San Andres) oil fields, improvement in oil production has been accomplished, in part, by using "pipeline fracturing" technology in the most recent completion to improve fluid flow rates, and filtration of waterflood injection water to preserve reservoir permeability. The 3D seismic survey acquired in conjunction with this DOE project has been used to calculate a 3D seismic inversion model, which has been analyzed to provide detailed maps of porosity within the productive upper 250 feet of the Grayburg Formation. Geologic data, particularly from logs and cores, have been combined with the geophysical interpretation and production history information to develop a model of the reservoir that defines estimations of remaining producible oil. The integrated result is greater than the sum of its parts, since no single data form adequately describes the reservoir. Each discipline relies upon computer software that runs on PC-type computers, allowing virtually any size company to affordably access the technology required to achieve similar results.

  9. Screening and comparison of remedial alternatives for the South Field and flyash piles at the Fernald site

    SciTech Connect

    Bumb, A.C.; Jones, G.N.; Warner, R.D.

    1996-05-01

    The South Field, the Inactive Flyash Pile, and the Active Flyash Pile are in close proximity to each other and are part of Operable Unit 2 (OU2) at the Fernald Environmental Management Project (FEMP). The baseline risk assessment indicated that the exposure pathways which pose the most significant risk are external radiation from radionuclides in surface soils and use of uranium contaminated groundwater. This paper presents screening and comparison of various remedial alternatives considered to mitigate risks from the groundwater pathway. Eight remedial alternatives were developed which consisted of consolidation and capping, excavation and off-site disposal with or without treatment, excavation and on-site disposal with or without treatment and combinations of these. Risk-based source (soil) preliminary remediation levels (PRLs) and waste acceptance criteria (WACs) were developed for consolidation and capping, excavation, and on-site disposal cell. The PRLs and WACs were developed using an integrated modeling tool consisting of an infiltration model, a surface water model, a vadose zone model, and a three-dimensional contaminant migration model in saturated media. The PRLs and WACs were then used to determine need for soil treatment, determine excavation volumes, and screen remedial alternatives. The selected remedial alternative consisted of excavation and on-site disposal with off-site disposal of the fraction exceeding the WAC.

  10. THE VERY LARGE ARRAY 1.4 GHz SURVEY OF THE EXTENDED CHANDRA DEEP FIELD SOUTH: SECOND DATA RELEASE

    SciTech Connect

    Miller, Neal A.; Bonzini, Margherita; Mainieri, Vincenzo; Padovani, Paolo; Rosati, Piero; Fomalont, Edward B.; Kellermann, Kenneth I.; Tozzi, Paolo; Vattakunnel, Shaji

    2013-04-01

    Deep radio observations at 1.4 GHz for the Extended Chandra Deep Field South were performed in 2007 June through September and presented in a first data release. The survey was made using six separate pointings of the Very Large Array with over 40 hr of observation per pointing. In the current paper, we improve on the data reduction to produce a second data release (DR2) mosaic image. This DR2 image covers an area of about a third of a square degree, reaches a best rms sensitivity of 6 {mu}Jy, and has a typical sensitivity of 7.4 {mu}Jy per 2.''8 by 1.''6 beam. We also present a more comprehensive catalog, including sources down to peak flux densities of five or more times the local rms noise along with information on source sizes and relevant pointing data. We discuss in some detail the consideration of whether sources are resolved under the complication of a radio image created as a mosaic of separate pointings each suffering some degree of bandwidth smearing, and the accurate evaluation of the flux densities of such sources. Finally, the radio morphologies and optical/near-IR counterpart identifications are used to identify 17 likely multiple-component sources and arrive at a catalog of 883 radio sources, which is roughly double the number of sources contained in the first data release.

  11. Eddy covariance flux measurements over a man made lake during the ALEX 2014 field campaign in South Portugal

    NASA Astrophysics Data System (ADS)

    Salgado, R.; Potes, M.; Albino, A.; Rodrigues, C. M.

    2014-12-01

    Energy, vapor, CO2 and momentum exchanges between water and air were measured using the new IRGASON eddy covariance system, an integrated open-path CO2 /H2O Gas Analyser and 3D Sonic Anemometer, installed on a instrumented floating platform (Figure 1) in the Alqueva reservoir, a large man made lake (area of 250 km2) in South Portugal. Radiation sensors were also mounted on the raft in order to measure near surface up and down radiative fluxes, while the water temperature profile below the platform were continuously archived. An accelerometer was mounted on the support bar near the sonic anemometer in order to correct the vertical component of the wind due to the the raft swing. The measurements were performed during the ALqueva hydro-meteorological EXperiment, ALEX 2014, between June and September 2014. ALEX 2014 ( http://www.alex2014.cge.uevora.pt) was an integrated field campaign with measurements of chemical, physical and biological parameters at different experimental sites in the reservoir and in its surrounding area. Worldwide, there are few reported flux measurements over lakes. This set of observations contribute to improve the characterization of the exchanges between a lake and the atmosphere in a semi-arid climate. The eddy covariance estimates of lake evaporation are compared against other methods.

  12. Oil gravity distribution in the diatomite at South Belridge Field, Kern County, CA: Implications for oil sourcing and migration

    SciTech Connect

    Hill, D.W.; Sande, J.J.; Doe, P.H.

    1995-04-01

    Understanding oil gravity distribution in the Belridge Diatomite has led to economic infill development and specific enhanced recovery methods for targeted oil properties. To date more than 100 wells have provided samples used to determining vertical and areal distribution of oil gravity in the field. Detailed geochemical analyses were also conducted on many of the oil samples to establish different oil types, relative maturities, and to identify transformed oils. The geochemical analysis also helped identify source rock expulsion temperatures and depositional environments. The data suggests that the Belridge diatomite has been charged by a single hydrocarbon source rock type and was generated over a relatively wide range of temperatures. Map and statistical data support two distinct oil segregation processes occurring post expulsion. Normal gravity segregation within depositional cycles of diatomite have caused lightest oils to migrate to the crests of individual cycle structures. Some data suggests a loss of the light end oils in the uppermost cycles to the Tulare Formation above, or through early biodegradation. Structural rotation post early oil expulsion has also left older, heavier oils concentrated on the east flank of the structure. With the addition of other samples from the south central San Joaquin area, we have been able to tie the Belridge diatomite hydrocarbon charge into a regional framework. We have also enhanced our ability to predict oil gravity and well primary recovery by unraveling some key components of the diatomite oil source and migration history.

  13. VHF coherent scatter radar observations of mid-latitude F-region field-aligned irregularities over South Korea

    NASA Astrophysics Data System (ADS)

    Kwak, Y.; Yang, T.; Lee, J.; Hwang, J.; Kil, H.; Park, Y.

    2011-12-01

    We examine the mid-latitude F-region field-aligned irregularity (FAI) activity during 2010-2011 by using the VHF coherent scatter radar data in Daejeon (36.2°N, 127.1°E; dip latitude 26.7°N), South Korea. The VHF radar has been operated since December 2009 and provides a unique opportunity to investigate the variability of the FAI activity with local time, season, solar flux, and magnetic activity. Our preliminary results during the solar minimum show that FAIs preferentially occur at post-sunset and pre-sunrise and during the June solstice. The seasonal variation of the FAI occurrence frequency is similar to that of the electron density irregularities observed by the C/NOFS satellite. For one event, we observed the association of the FAIs with a medium-scale traveling ionospheric disturbance (MSTID). Our study extends to the investigation of the correlations between the irregularities in the equatorial region and middle latitudes and between the conjugate F regions, and the causal linkage of the FAIs with the E-region perturbations. For this purpose, we analyze the VHF radar and C/NOFS data during 2010-2011.

  14. Field and experimental evidence for coseismic ruptures along shallow creeping faults in forearc sediments of the Crotone Basin, South Italy

    NASA Astrophysics Data System (ADS)

    Balsamo, Fabrizio; Aldega, Luca; De Paola, Nicola; Faoro, Igor; Storti, Fabrizio

    2014-05-01

    Large seismic slip occurring along shallow creeping faults in tectonically active areas represents an unsolved paradox, which is largely due to our poor understanding of the mechanics governing creeping faults, and to the lack of documented geological evidence showing how coseismic rupturing overprints creep in near-surface conditions. In this contribution we integrate field, petrophysical, mineralogical and friction data to characterize the signature of coseismic ruptures propagating along shallow creeping faults affecting unconsolidated forearc sediments of the seismically active Crotone Basin, in South Italy. Field observations of fault zones show widespread foliated cataclasites in fault cores, locally overprinted by sharp slip surfaces decorated by thin (0.5-1.5 cm) black gouge layers. Compared to foliated cataclasites, black gouges have much lower grain size, porosity and permeability, which may have facilitated slip weakening by thermal fluid pressurization. Moreover, black gouges are characterized by distinct mineralogical assemblages compatible with high temperatures (180-200°C) due to frictional heating during seismic slip. Foliated cataclasites and black gouges were also produced by laboratory friction experiments performed on host sediments at sub-seismic (≤ 0.1 m/s) and seismic (1 m/s) slip rates, respectively. Black gouges display low friction coefficients (0.3) and velocity-weakening behaviours, as opposed to high friction coefficients (0.65) and velocity-strengthening behaviours shown by the foliated cataclasites. Our results show that narrow black gouges developed within foliated cataclasites represent a potential diagnostic marker for episodic seismic activity in shallow creeping faults. These findings can help understanding the time-space partitioning between aseismic and seismic slip of faults at shallow crustal levels, impacting on seismic hazard evaluation of subduction zones and forearc regions affected by destructive earthquakes and

  15. A FLUX-LIMITED SAMPLE OF z {approx} 1 Ly{alpha} EMITTING GALAXIES IN THE CHANDRA DEEP FIELD SOUTH ,

    SciTech Connect

    Barger, A. J.; Wold, I. G. B.; Cowie, L. L.

    2012-04-20

    We describe a method for obtaining a flux-limited sample of Ly{alpha} emitters from Galaxy Evolution Explorer (GALEX) grism data. We show that the multiple GALEX grism images can be converted into a three-dimensional (two spatial axes and one wavelength axis) data cube. The wavelength slices may then be treated as narrowband images and searched for emission-line galaxies. For the GALEX NUV grism data, the method provides a Ly{alpha} flux-limited sample over the redshift range z = 0.67-1.16. We test the method on the Chandra Deep Field South field, where we find 28 Ly{alpha} emitters with faint continuum magnitudes (NUV > 22) that are not present in the GALEX pipeline sample. We measure the completeness by adding artificial emitters and measuring the fraction recovered. We find that we have an 80% completeness above a Ly{alpha} flux of 10{sup -15} erg cm{sup -2} s{sup -1}. We use the UV spectra and the available X-ray data and optical spectra to estimate the fraction of active galactic nuclei in the selection. We report the first detection of a giant Ly{alpha} blob at z < 1, though we find that these objects are much less common at z = 1 than at z = 3. Finally, we compute limits on the z {approx} 1 Ly{alpha} luminosity function and confirm that there is a dramatic evolution in the luminosity function over the redshift range z = 0-1.

  16. ESO imaging survey. Deep public survey: Multi-color optical data for the Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Arnouts, S.; Vandame, B.; Benoist, C.; Groenewegen, M. A. T.; da Costa, L.; Schirmer, M.; Mignani, R. P.; Slijkhuis, R.; Hatziminaoglou, E.; Hook, R.; Madejsky, R.; Rité, C.; Wicenec, A.

    2001-11-01

    This paper presents multi-passband optical data obtained from observations of the Chandra Deep Field South (CDF-S), located at alpha ~ 3h 32m, delta ~ -27o 48'. The observations were conducted at the ESO/MPG 2.2 m telescope at La Silla using the 8kx8k Wide-Field Imager (WFI). This data set, taken over a period of one year, represents the first field to be completed by the ongoing Deep Public Survey (DPS) being carried out as a part of the ESO Imaging Survey (EIS) project. This paper describes the optical observations, the techniques employed for un-supervised pipeline processing and the general characteristics of the final data set. Image processing has been performed using multi-resolution image decomposition techniques adapted to the EIS pipeline. The automatic processing steps include standard de-bias and flat-field, automatic removal of satellite tracks, de-fringing/sky-subtraction, image stacking/mosaicking and astrometry. Stacking of dithered images is carried out using pixel-based astrometry which enables the efficient removal of cosmic rays and image defects, yielding remarkably clean final images. The final astrometric calibration is based on a pre-release of the GSC-II catalog and has an estimated intrinsic accuracy of la 0.10 arcsec, with all passbands sharing the same solution. The paper includes data taken in six different filters (U'UBVRI). The data cover an area of about 0.25 square degrees reaching 5sigma limiting magnitudes of U'AB=26.0, UAB=25.7, BAB=26.4, VAB=25.4, RAB=25.5 and IAB= 24.7 mag, as measured within a 2 x FWHM aperture. The optical data covers an area of ~ 0.1 square degrees for which moderately deep observations in two near-infrared bands are also available, reaching 5sigma limiting magnitudes of JAB ~ 23.4 and KAB ~ 22.6. The current optical/infrared data also fully encompass the region of the deep X-ray observations recently completed by the Chandra telescope. The optical data presented here, as well as the infrared data released

  17. Co-transmission of the non-transmissible South African Babesia bovis S24 vaccine strain during mixed infection with a field isolate.

    PubMed

    Combrink, M P; Troskie, P C; de Klerk, D G; Pienaar, R; Latif, A A; Mans, B J

    2015-03-01

    The South African Babesia bovis live blood vaccine, originating from a field isolate attenuated by 23 serial syringe passages in splenectomized calves, has lost the ability to infect the natural vector Rhipicephalus (Boophilus) microplus. In this study, infection with mixed parasites from the vaccine strain and a field isolate, resulted in transmission of both genotype populations. Comparing the field isolate and transmitted combination indicated no significant difference in their virulence, while challenge of vaccinated cattle with these isolates showed the ability of the vaccine to protect against both. Limiting dilution of the transmitted combination, followed by infection of splenectomized cattle (n=34) yielded no single infections for the vaccine strain genotype, seven clonal lines of the field isolate and one mixture of vaccine strain and field isolate. Only one of two field isolate clonal lines selected for vector transmission study was transmitted. Showing that B. bovis isolates can contain both tick transmissible and non-transmissible subpopulations. The findings of this study also indicate the probability of vaccine co-infection transmission occurring in the field, which may result in new genotype populations of B. bovis. However, the impact of this recombination with field isolates is considered negligible since a genotypically diverse population of B. bovis is already present in South Africa. PMID:25544307

  18. SURVEYS AND FIELD OBSERVATIONS OF HARMONIA AXYRIDIS AND OTHER COCCINELLIDAE (COLEOPTERA) IN EASTERN AND CENTRAL SOUTH DAKOTA

    Technology Transfer Automated Retrieval System (TEKTRAN)

    Harmonia axyridis, a coccinellid native to Asia, was discovered in South Dakota in 1996, but its distribution and habitat use in the state had remained undetermined. We sampled coccinellids from various habitats, including agricultural and natural areas, in eastern and central South Dakota in 2000 a...

  19. The Great Observatories Origins Deep Survey. VLT/VIMOS spectroscopy in the GOODS-south field: Part II

    NASA Astrophysics Data System (ADS)

    Balestra, I.; Mainieri, V.; Popesso, P.; Dickinson, M.; Nonino, M.; Rosati, P.; Teimoorinia, H.; Vanzella, E.; Cristiani, S.; Cesarsky, C.; Fosbury, R. A. E.; Kuntschner, H.; Rettura, A.

    2010-03-01

    Context. We present the full data set of the VIsible Multi-Object Spectrograph (VIMOS) spectroscopic campaign of the ESO/GOODS program in the Chandra Deep Field South (CDFS), which complements the FORS2 ESO/GOODS spectroscopic campaign. Aims: The ESO/GOODS spectroscopic programs are aimed at reaching signal-to-noise ratios adequate to measure redshifts for galaxies with AB magnitudes in the range ~24-25 in the B and R band using VIMOS, and in the z band using FORS2. Methods: The GOODS/VIMOS spectroscopic campaign is structured in two separate surveys using two different VIMOS grisms. The VIMOS Low Resolution Blue (LR-Blue) and Medium Resolution (MR) orange grisms have been used to cover different redshift ranges. The LR-Blue campaign is aimed at observing galaxies mainly at 1.8 < z < 3.5, while the MR campaign mainly aims at galaxies at z < 1 and Lyman Break Galaxies (LBGs) at z > 3.5. Results: The full GOODS/VIMOS spectroscopic campaign consists of 20 VIMOS masks. This release adds 8 new masks to the previous release (12 masks, Popesso et al. 2009, A&A, 494, 443). In total we obtained 5052 spectra, 3634 from the 10 LR-Blue masks and 1418 from the 10 MR masks. A significant fraction of the extracted spectra comes from serendipitously observed sources: ~21% in the LR-Blue and ~16% in the MR masks. We obtained 2242 redshifts in the LR-Blue campaign and 976 in the MR campaign for a total success rate of 62% and 69% respectively, which increases to 66% and 73% if only primary targets are considered. The typical redshift uncertainty is estimated to be σz ≃ 0.00084 (~255 km s-1) for the LR-Blue grism and σz ≃ 0.00040 (~120 km s-1) for the MR grism. By complementing our VIMOS spectroscopic catalog with all existing spectroscopic redshifts publicly available in the CDFS, we compiled a redshift master catalog with 7332 entries, which we used to investigate large scale structures out to z ≃ 3.7. We produced stacked spectra of LBGs in a few bins of equivalent width

  20. A SEARCH FOR LYMAN BREAK GALAXIES IN THE CHANDRA DEEP FIELD SOUTH USING SWIFT ULTRAVIOLET/OPTICAL TELESCOPE

    SciTech Connect

    Basu-Zych, Antara R.; Hornschemeier, Ann E.; Hoversten, Erik A.; Gronwall, Caryl; Lehmer, Bret E-mail: Ann.Hornschemeier@nasa.gov E-mail: caryl@astro.psu.edu

    2011-10-01

    While the Swift satellite is primarily designed to study gamma-ray bursts, its ultraviolet and optical imaging and spectroscopy capabilities are also being used for a variety of scientific programs. In this study, we use the UV/Optical Telescope (UVOT) instrument on board Swift to discover 0.5 < z < 2 Lyman break galaxies (LBGs). UVOT has covered {approx}266 arcmin{sup 2} at >60 ks exposure time, achieving a limiting magnitude of u < 24.5, in the Chandra Deep Field South (CDF-S). Applying UVOT near-ultraviolet color selection, we select 50 UV-dropouts from this UVOT CDF-S data. We match the selected sources with available multiwavelength data from Great Observatories Origins Deep Survey (GOODS) South, Multiwavelength Survey by Yale-Chile, and COMBO-17 to characterize the spectral energy distributions for these galaxies and determine stellar masses, star formation rates (SFRs), and dust attenuations. We compare these properties for LBGs selected in this paper versus z {approx} 3 LBGs and other CDF-S galaxies in the same redshift range (0.5 < z < 2), identified using photometric redshift techniques. The z {approx} 1 LBGs have stellar masses of (logM{sub *}/M{sub sun}) = 9.4 {+-} 0.6, which is slightly lower than z {approx} 3 LBGs ((logM{sub *}/Ms{sub un}) = 10.2 {+-} 0.4) and slightly higher compared with the z {approx} 1 CDF-S galaxies ((logM{sub *}/M{sub sun}) = 8.7 {+-} 0.7). Similarly, our sample of z {approx} 1 LBGs has SFRs (derived using both ultraviolet and infrared data, where available) of (logSFR/(M{sub sun} yr{sup -1})) = 0.7 {+-} 0.6, nearly an order of magnitude lower than z {approx} 3 LBGs ((logSFR/M{sub sun} yr{sup -1}) = 1.5 {+-} 0.4), but slightly higher than the comparison z {approx} 1 sample of CDF-S galaxies ((logSFR/M{sub sun} yr{sup -1}) = 0.2 {+-} 0.7). We find that our z {approx} 1 UV-dropouts have (A{sub FUV}) = 2.0 {+-} 1.0, which is higher than z {approx} 3 LBGs ((A{sub FUV}) = 1.0 {+-} 0.5), but similar to the distribution of dust

  1. Quantification and regionalization of groundwater recharge in South-Central Kansas: Integrating field characterization, statistical analysis, and GIS

    USGS Publications Warehouse

    Sophocleous, M.

    2000-01-01

    A practical methodology for recharge characterization was developed based on several years of field-oriented research at 10 sites in the Great Bend Prairie of south-central Kansas. This methodology combines the soil-water budget on a storm-by-storm year-round basis with the resulting watertable rises. The estimated 1985-1992 average annual recharge was less than 50mm/year with a range from 15 mm/year (during the 1998 drought) to 178 mm/year (during the 1993 flood year). Most of this recharge occurs during the spring months. To regionalize these site-specific estimates, an additional methodology based on multiple (forward) regression analysis combined with classification and GIS overlay analyses was developed and implemented. The multiple regression analysis showed that the most influential variables were, in order of decreasing importance, total annual precipitation, average maximum springtime soil-profile water storage, average shallowest springtime depth to watertable, and average springtime precipitation rate. Therefore, four GIS (ARC/INFO) data "layers" or coverages were constructed for the study region based on these four variables, and each such coverage was classified into the same number of data classes to avoid biasing the results. The normalized regression coefficients were employed to weigh the class rankings of each recharge-affecting variable. This approach resulted in recharge zonations that agreed well with the site recharge estimates. During the "Great Flood of 1993," when rainfall totals exceeded normal levels by -200% in the northern portion of the study region, the developed regionalization methodology was tested against such extreme conditions, and proved to be both practical, based on readily available or easily measurable data, and robust. It was concluded that the combination of multiple regression and GIS overlay analyses is a powerful and practical approach to regionalizing small samples of recharge estimates.

  2. Bent-tailed radio sources in the australia telescope large area survey of the Chandra deep field south

    SciTech Connect

    Dehghan, S.; Johnston-Hollitt, M.; Franzen, T. M. O.; Norris, R. P.; Miller, N. A.

    2014-11-01

    Using the 1.4 GHz Australia Telescope Large Area Survey, supplemented by the 1.4 GHz Very Large Array images, we undertook a search for bent-tailed (BT) radio galaxies in the Chandra Deep Field South. Here we present a catalog of 56 detections, which include 45 BT sources, 4 diffuse low-surface-brightness objects (1 relic, 2 halos, and 1 unclassified object), and a further 7 complex, multi-component sources. We report BT sources with rest-frame powers in the range 10{sup 22} ≤ P {sub 1.4} {sub GHz} ≤ 10{sup 26} W Hz{sup –1}, with redshifts up to 2 and linear extents from tens of kiloparsecs up to about 1 Mpc. This is the first systematic study of such sources down to such low powers and high redshifts and demonstrates the complementary nature of searches in deep, limited area surveys as compared to shallower, large surveys. Of the sources presented here, one is the most distant BT source yet detected at a redshift of 2.1688. Two of the sources are found to be associated with known clusters: a wide-angle tail source in A3141 and a putative radio relic which appears at the infall region between the galaxy group MZ 00108 and the galaxy cluster AMPCC 40. Further observations are required to confirm the relic detection, which, if successful, would demonstrate this to be the least powerful relic yet seen with P {sub 1.4} {sub GHz} = 9 × 10{sup 22} W Hz{sup –1}. Using these data, we predict future 1.4 GHz all-sky surveys with a resolution of ∼10 arcsec and a sensitivity of 10 μJy will detect of the order of 560,000 extended low-surface-brightness radio sources of which 440,000 will have a BT morphology.

  3. THE BLACK HOLE-BULGE MASS RELATION OF ACTIVE GALACTIC NUCLEI IN THE EXTENDED CHANDRA DEEP FIELD-SOUTH SURVEY

    SciTech Connect

    Schramm, Malte; Silverman, John D.

    2013-04-10

    We present results from a study to determine whether relations-established in the local universe-between the mass of supermassive black holes (SMBHs) and their host galaxies are in place at higher redshifts. We identify a well-constructed sample of 18 X-ray-selected, broad-line active galactic nuclei (AGNs) in the Extended Chandra Deep Field-South Survey with 0.5 < z < 1.2. This redshift range is chosen to ensure that Hubble Space Telescope (HST) imaging is available with at least two filters that bracket the 4000 A break, thus providing reliable stellar mass estimates of the host galaxy by accounting for both young and old stellar populations. We compute single-epoch, virial black hole (BH) masses from optical spectra using the broad Mg II emission line. For essentially all galaxies in our sample, their total stellar mass content agrees remarkably well, given their BH masses, with local relations of inactive galaxies and active SMBHs. We further decompose the total stellar mass into bulge and disk components separately with full knowledge of the HST point-spread function. We find that {approx}80% of the sample is consistent with the local M{sub BH}-M{sub *,{sub Bulge}} relation even with 72% of the host galaxies showing the presence of a disk. In particular, bulge-dominated hosts are more aligned with the local relation than those with prominent disks. We further discuss the possible physical mechanisms that are capable of building up the stellar mass of the bulge from an extended disk of stars over the subsequent 8 Gyr.

  4. Variability Selected Low-Luminosity Active Galactic Nuclei in the 4 Ms Chandra Deep Field-South

    NASA Technical Reports Server (NTRS)

    Young, M.; Brandt, W. N.; Xue, Y. Q.; Paolillo, D. M.; Alexander, F. E.; Bauer, F. E.; Lehmer, B. D.; Luo, B.; Shemmer, O.; Schneider, D. P.; Vignail, C.

    2012-01-01

    The 4 Ms Chandra Deep Field-South (CDF-S) and other deep X-ray surveys have been highly effective at selecting active galactic nuclei (AGN). However, cosmologically distant low-luminosity AGN (LLAGN) have remained a challenge to identify due to significant contribution from the host galaxy. We identify long-term X ray variability (approx. month years, observed frame) in 20 of 92 CDF-S galaxies spanning redshifts approx equals 00.8 - 1.02 that do not meet other AGN selection criteria. We show that the observed variability cannot be explained by X-ray binary populations or ultraluminous X-ray sources, so the variability is most likely caused by accretion onto a supermassive black hole. The variable galaxies are not heavily obscured in general, with a stacked effective power-law photon index of Gamma(sub Stack) approx equals 1.93 +/- 0.13, and arc therefore likely LLAGN. The LLAGN tend to lie it factor of approx equal 6-89 below the extrapolated linear variability-luminosity relation measured for luminous AGN. This may he explained by their lower accretion rates. Variability-independent black-hole mass and accretion-rate estimates for variable galaxies show that they sample a significantly different black hole mass-accretion-rate space, with masses a factor of 2.4 lower and accretion rates a factor of 22.5 lower than variable luminous AGNs at the same redshift. We find that an empirical model based on a universal broken power-law power spectral density function, where the break frequency depends on SMBH mass and accretion rate, roughly reproduces the shape, but not the normalization, of the variability-luminosity trends measured for variable galaxies and more luminous AGNs.

  5. Bent-tailed Radio Sources in the Australia Telescope Large Area Survey of the Chandra Deep Field South

    NASA Astrophysics Data System (ADS)

    Dehghan, S.; Johnston-Hollitt, M.; Franzen, T. M. O.; Norris, R. P.; Miller, N. A.

    2014-11-01

    Using the 1.4 GHz Australia Telescope Large Area Survey, supplemented by the 1.4 GHz Very Large Array images, we undertook a search for bent-tailed (BT) radio galaxies in the Chandra Deep Field South. Here we present a catalog of 56 detections, which include 45 BT sources, 4 diffuse low-surface-brightness objects (1 relic, 2 halos, and 1 unclassified object), and a further 7 complex, multi-component sources. We report BT sources with rest-frame powers in the range 1022 <= P 1.4 GHz <= 1026 W Hz-1, with redshifts up to 2 and linear extents from tens of kiloparsecs up to about 1 Mpc. This is the first systematic study of such sources down to such low powers and high redshifts and demonstrates the complementary nature of searches in deep, limited area surveys as compared to shallower, large surveys. Of the sources presented here, one is the most distant BT source yet detected at a redshift of 2.1688. Two of the sources are found to be associated with known clusters: a wide-angle tail source in A3141 and a putative radio relic which appears at the infall region between the galaxy group MZ 00108 and the galaxy cluster AMPCC 40. Further observations are required to confirm the relic detection, which, if successful, would demonstrate this to be the least powerful relic yet seen with P 1.4 GHz = 9 × 1022 W Hz-1. Using these data, we predict future 1.4 GHz all-sky surveys with a resolution of ~10 arcsec and a sensitivity of 10 μJy will detect of the order of 560,000 extended low-surface-brightness radio sources of which 440,000 will have a BT morphology.

  6. Counts and Sizes of Galaxies in the Hubble Deep Field South: Implications for the Next Generation Space Telescope

    NASA Astrophysics Data System (ADS)

    Gardner, Jonathan P.; Satyapal, Shobita

    2000-06-01

    Science objectives for the Next Generation Space Telescope (NGST) include a large component of galaxy surveys, both imaging and spectroscopy. The Hubble Deep Field data sets include the deepest observations ever made in the ultraviolet, optical, and near-infrared, reaching depths comparable to that expected for NGST spectroscopy. We present the source counts, galaxy sizes, and isophotal filling factors of the Hubble Deep Field South (HDF-S) images. The observed integrated galaxy counts reach over 500 galaxies per square arcminute at magnitudes AB < 30. We extend these counts to fainter levels and further into the infrared using galaxy-count models. It was determined from the HDF (North) and other deep Wide Field Planetary Camera 2 imaging that fainter galaxies are smaller. This trend continues to AB=29 in the high-resolution HDF-S Space Telescope Imaging Spectrograph (STIS) image, where galaxies have a typical half-light radius of 0.1". We have run extensive Monte Carlo simulations of the galaxy detection in the HDF-S, and we show that the small measured sizes are not due to selection effects until AB > 29. We compare observed sizes in the optical and near-infrared using the HDF-S Near Infrared Camera and Multi-Object Spectrometer image, showing that after taking into account the different point-spread functions and pixel sizes of the images, galaxies are smaller in the near-infrared than they are in the optical. We analyze the isophotal filling factor of the HDF-S STIS image and show that this image is mostly empty sky even at the limits of galaxy detection, a conclusion we expect to hold true for NGST spectroscopy. At the surface brightness limits expected for NGST imaging, however, about a quarter of the sky is occupied by the outer isophotes of AB < 30 galaxies, requiring deblending to detect the faintest objects. We discuss the implications of these data on several design concepts for the NGST near-infrared spectrography. We compare the effects of resolution

  7. AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: NEAR-INFRARED MORPHOLOGIES AND STELLAR SIZES

    SciTech Connect

    Chen, Chian-Chou; Smail, Ian; Swinbank, A. M.; Simpson, J. M.; Ma, Cheng-Jiun; Alexander, D. M.; Danielson, A. L. R.; Edge, A. C.; Biggs, A. D.; Ivison, R. J.; Brandt, W. N.; Chapman, S. C.; Coppin, K. E. K.; Dannerbauer, H.; Greve, T. R.; Karim, A.; Menten, Karl M.; Schinnerer, E.; Walter, F.; Wardlow, J. L.; and others

    2015-02-01

    We analyze Hubble Space Telescope WFC3/H {sub 160}-band observations of a sample of 48 Atacama Large Millimeter/submillimeter Array detected submillimeter galaxies (SMGs) in the Extended Chandra Deep Field South field, to study their stellar morphologies and sizes. We detect 79% ± 17% of the SMGs in the H {sub 160}-band imaging with a median sensitivity of 27.8 mag, and most (80%) of the nondetections are SMGs with 870 μm fluxes of S {sub 870} < 3 mJy. With a surface brightness limit of μ {sub H} ∼ 26 mag arcsec{sup –2}, we find that 82% ± 9% of the H {sub 160}-band-detected SMGs at z = 1-3 appear to have disturbed morphologies, meaning they are visually classified as either irregulars or interacting systems, or both. By determining a Sérsic fit to the H {sub 160} surface brightness profiles, we derive a median Sérsic index of n = 1.2 ± 0.3 and a median half-light radius of r{sub e} = 4.4{sub −0.5}{sup +1.1} kpc for our SMGs at z = 1-3. We also find significant displacements between the positions of the H {sub 160} component and 870 μm emission in these systems, suggesting that the dusty starburst regions and less-obscured stellar distribution are not colocated. We find significant differences in the sizes and the Sérsic index between our z = 2-3 SMGs and z ∼ 2 quiescent galaxies, suggesting that a major transformation of the stellar light profile is needed in the quenching processes if SMGs are progenitors of the red-and-dead z ∼ 2 galaxies. Given the short-lived nature of SMGs, we postulate that the majority of the z = 2-3 SMGs with S {sub 870} ≳ 2 mJy are early/mid-stage major mergers.

  8. Climate-sensitive subsea permafrost and related gas expulsions on the South Kara Sea shelf. Field studies and modeling results.

    NASA Astrophysics Data System (ADS)

    Portnov, Alexey; Mienert, Jurgen; Serov, Pavel

    2015-04-01

    Thawing subsea permafrost controls methane release bearing a considerable impact on the climate-sensitive Arctic environment. Significant expulsion of methane into shallow Russian shelf areas may continue to rise into the atmosphere on the Arctic shelves in response to intense degradation of relict subsea permafrost. The release of formerly trapped gas, essentially methane, is linked to the permafrost evolution. Modeling of the permafrost at the West Yamal shelf allowed describing its evolution from the Late Pleistocene to Holocene. During the previous work we detected extensive emissions of free gas into the water column at the boundary between today's shallow water permafrost and deeper water non-permafrost areas. These gas expulsions formed seismic and hydro-acoustic anomalies on the high-resolution seismic records. We supposed that in the water depths <20m continuous ice-bearing permafrost plays a role of a seal through which gas can not migrate. We integrate 1D modeling results of relict permafrost distributions with these field data from the South Kara Sea. Modeling results suggest a highly-dynamic permafrost system that directly responds to even minor variations of lower and upper boundary conditions, e.g. heat flux from below and/or bottom water temperature changes from above. We present several scenarios of permafrost evolution and show that potentially minimal modern extent of the permafrost at the West Yamal shelf is limited by ~17 m isobaths, whereas maximal probable extent coincides with ~100 m isobaths. The model also predicts seaward tapering of relict permafrost with its maximal thickness 275-390 m near the shore line. We also present sensitivity analysis which define the wider range of modeling results depending on the changing input parameters (e.g. geothermal heat flux, bottom water temperature, porosity of the sediments). The model adapts well to corresponding field data, providing crucial information about the modern permafrost conditions

  9. UV-DROPOUT GALAXIES IN THE GOODS-SOUTH FIELD FROM WFC3 EARLY RELEASE SCIENCE OBSERVATIONS

    SciTech Connect

    Hathi, N. P.; Ryan, R. E.; Cohen, S. H.; Windhorst, R. A.; Rutkowski, M. J.; Yan, H.; McCarthy, P. J.; O'Connell, R. W.; Koekemoer, A. M.; Bond, H. E.; Balick, B.; Calzetti, D.; Disney, M. J.; Dopita, M. A.; Frogel, Jay A.; Hall, D. N. B.; Holtzman, J. A.; Kimble, R. A.; Paresce, F.; Saha, A.

    2010-09-10

    We combine new high sensitivity ultraviolet (UV) imaging from the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) with existing deep HST/Advanced Camera for Surveys optical images from the Great Observatories Origins Deep Survey (GOODS) program to identify UV-dropouts, which are Lyman break galaxy (LBG) candidates at z {approx_equal} 1-3. These new HST/WFC3 observations were taken over 50 arcmin{sup 2} in the GOODS-South field as a part of the Early Release Science program. The uniqueness of these new UV data is that they are observed in three UV/optical (WFC3 UVIS) channel filters (F225W, F275W, and F336W), which allows us to identify three different sets of UV-dropout samples. We apply Lyman break dropout selection criteria to identify F225W-, F275W-, and F336W-dropouts, which are z {approx_equal} 1.7, 2.1, and 2.7 LBG candidates, respectively. We use multi-wavelength imaging combined with available spectroscopic and photometric redshifts to carefully access the validity of our UV-dropout candidates. Our results are as follows: (1) these WFC3 UVIS filters are very reliable in selecting LBGs with z {approx_equal} 2.0, which helps to reduce the gap between the well-studied z {approx}> 3 and z {approx} 0 regimes; (2) the combined number counts with average redshift z {approx_equal} 2.2 agree very well with the observed change in the surface densities as a function of redshift when compared with the higher redshift LBG samples; and (3) the best-fit Schechter function parameters from the rest-frame UV luminosity functions at three different redshifts fit very well with the evolutionary trend of the characteristic absolute magnitude, M*, and the faint-end slope, {alpha}, as a function of redshift. This is the first study to illustrate the usefulness of the WFC3 UVIS channel observations to select z {approx}< 3 LBGs. The addition of the new WFC3 on the HST has made it possible to uniformly select LBGs from z {approx_equal} 1 to z {approx_equal} 9 and

  10. UV-dropout Galaxies in the Goods-South Field from WFC3 Early Release Science Observations

    NASA Astrophysics Data System (ADS)

    Hathi, N. P.; Ryan, R. E., Jr.; Cohen, S. H.; Yan, H.; Windhorst, R. A.; McCarthy, P. J.; O'Connell, R. W.; Koekemoer, A. M.; Rutkowski, M. J.; Balick, B.; Bond, H. E.; Calzetti, D.; Disney, M. J.; Dopita, M. A.; Frogel, Jay A.; Hall, D. N. B.; Holtzman, J. A.; Kimble, R. A.; Paresce, F.; Saha, A.; Silk, J. I.; Trauger, J. T.; Walker, A. R.; Whitmore, B. C.; Young, E. T.

    2010-09-01

    We combine new high sensitivity ultraviolet (UV) imaging from the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST) with existing deep HST/Advanced Camera for Surveys optical images from the Great Observatories Origins Deep Survey (GOODS) program to identify UV-dropouts, which are Lyman break galaxy (LBG) candidates at z ~= 1-3. These new HST/WFC3 observations were taken over 50 arcmin2 in the GOODS-South field as a part of the Early Release Science program. The uniqueness of these new UV data is that they are observed in three UV/optical (WFC3 UVIS) channel filters (F225W, F275W, and F336W), which allows us to identify three different sets of UV-dropout samples. We apply Lyman break dropout selection criteria to identify F225W-, F275W-, and F336W-dropouts, which are z ~= 1.7, 2.1, and 2.7 LBG candidates, respectively. We use multi-wavelength imaging combined with available spectroscopic and photometric redshifts to carefully access the validity of our UV-dropout candidates. Our results are as follows: (1) these WFC3 UVIS filters are very reliable in selecting LBGs with z ~= 2.0, which helps to reduce the gap between the well-studied z >~ 3 and z ~ 0 regimes; (2) the combined number counts with average redshift z ~= 2.2 agree very well with the observed change in the surface densities as a function of redshift when compared with the higher redshift LBG samples; and (3) the best-fit Schechter function parameters from the rest-frame UV luminosity functions at three different redshifts fit very well with the evolutionary trend of the characteristic absolute magnitude, M*, and the faint-end slope, α, as a function of redshift. This is the first study to illustrate the usefulness of the WFC3 UVIS channel observations to select z <~ 3 LBGs. The addition of the new WFC3 on the HST has made it possible to uniformly select LBGs from z ~= 1 to z ~= 9 and significantly enhance our understanding of these galaxies using HST sensitivity and resolution.

  11. Deep 20-GHz survey of the Chandra Deep Field South and SDSS Stripe 82: source catalogue and spectral properties

    NASA Astrophysics Data System (ADS)

    Franzen, Thomas M. O.; Sadler, Elaine M.; Chhetri, Rajan; Ekers, Ronald D.; Mahony, Elizabeth K.; Murphy, Tara; Norris, Ray P.; Waldram, Elizabeth M.; Whittam, Imogen H.

    2014-04-01

    We present a source catalogue and first results from a deep, blind radio survey carried out at 20 GHz with the Australia Telescope Compact Array, with follow-up observations at 5.5, 9 and 18 GHz. The Australia Telescope 20 GHz (AT20G) deep pilot survey covers a total area of 5 deg2 in the Chandra Deep Field South and in Stripe 82 of the Sloan Digital Sky Survey. We estimate the survey to be 90 per cent complete above 2.5 mJy. Of the 85 sources detected, 55 per cent have steep spectra (α _{1.4}^{20} < -0.5) and 45 per cent have flat or inverted spectra (α _{1.4}^{20} ≥ -0.5). The steep-spectrum sources tend to have single power-law spectra between 1.4 and 18 GHz, while the spectral indices of the flat- or inverted-spectrum sources tend to steepen with frequency. Among the 18 inverted-spectrum (α _{1.4}^{20} ≥ 0.0) sources, 10 have clearly defined peaks in their spectra with α _{1.4}^{5.5} > 0.15 and α 9^{18} < -0.15. On a 3-yr time-scale, at least 10 sources varied by more than 15 per cent at 20 GHz, showing that variability is still common at the low flux densities probed by the AT20G-deep pilot survey. We find a strong and puzzling shift in the typical spectral index of the 15-20-GHz source population when combining data from the AT20G, Ninth Cambridge and Tenth Cambridge surveys: there is a shift towards a steeper-spectrum population when going from ˜1 Jy to ˜5 mJy, which is followed by a shift back towards a flatter-spectrum population below ˜5 mJy. The 5-GHz source-count model by Jackson & Wall, which only includes contributions from FRI and FRII sources, and star-forming galaxies, does not reproduce the observed flattening of the flat-spectrum counts below ˜5 mJy. It is therefore possible that another population of sources is contributing to this effect.

  12. Microanalysis of the aerosol collected over south-central New Mexico during the alive field experiment, May-December 1989

    NASA Astrophysics Data System (ADS)

    Sheridan, Patrick J.; Schnell, Russel C.; Kahl, Jonathan D.; Boatman, Joe F.; Garvey, Dennis M.

    Thirty-eight size-segregated aerosol samples were collected in the lower troposphere over the high desert of south-central New Mexico, using cascade impactors mounted onboard two research aircraft. Four of these samples were collected in early May, sixteen in mid-July, and the remaining ones in December 1989, during three segments of the ALIVE field initiative. Analytical electron microscope analyses of aerosol deposits and individual particles from these samples were performed to physically and chemically characterize the major particulate species present in the aerosol. Air-mass trajectories arriving at the sampling area in the May program were quite different from those calculated for the July period. In general, the May trajectories showed strong westerly winds, while the July winds were weaker and southerly, consistently passing over or very near the border cities of El Paso, Texas, and Ciudad Juarez, Mexico. Aerosol samples collected during the May period were predominantly fine (0.1-0.5 μm dia.), liquid H 2SO 4 droplets. Samples from the July experiment were comprised mostly of fine, solid (NH 4) 2SO 4 or mostly neutralized sulfate particles. In both sampling periods, numerous other particle classes were observed, including many types with probable terrestrial or anthropogenic sources. The numbers of these particles, however, were small when compared with the sulfates. Composite particle types, including sulfate/crustal and sulfate/carbonaceous, were also found to be present. The major differences in aerosol composition between the May and July samples (i.e. the extensive neutralization of sulfates in the July samples) can be explained by considering the different aerosol transport pathways and the proximity of the July aerosol to the El Paso/Juarez urban plume. Winds during the December experiment were quite variable, and may have contributed to the widely varying aerosol compositions observed in these samples. When the aircraft sampled the El Paso

  13. Horizontal and vertical deformation field in New Caledonia, South West Pacific, derived from more than 20 years of GNSS measurements

    NASA Astrophysics Data System (ADS)

    Ballu, V.; Calmant, S.; Valty, P.; Gravelle, M.; Sakic, P.; Aucan, J.; Pelletier, B.

    2015-12-01

    New Caledonia is located in the South West Pacific Ocean, on the Australian Plate just before its subduction under the North Fiji Basin. Because it is on the subducting side of the plate interface, New Caledonia is considered to be stable to first order and not to undergo rapid deformation. However, moderate seismicity is recorded close to the plate interface, in the southern part of the main land and along the Loyalty ridge. In addition, the main island and Loyalty ridge are subjected to long-term vertical deformation due to the flexure of the plate entering subduction. A geodetic network was installed since the early days of GPS (~1990) and has been further developed and occasionally measured since. Due to the low number of global GNSS recording stations in the early 1990s, the positioning accuracy that can be achieved with these data is poor compared to present-day standards, and expected movements are slow (possibly less than 1 mm/yr). However, the >20 year length of the time series may allow us to determine the current deformation field in New Caledonia and Loyalty Ridge. We pay special care in using older GNSS data for characterizing ground motions, reprocessing all available data using a range of different processing strategies and products. We calculated daily positions from double-differenced ionosphere-free carrier phase data in a global network using the GAMIT software and combined and aligned the results on the ITRF2008 using the CATREF software, according to the processing strategy developed as part of the current ULR6 (www.sonel.org) reprocessing campaign for IGS. We compare the double difference results with those obtained in PPP mode using JPL GIPSY software as well as CNES GINS software and different products (MIT, JPL and GRG orbits and clocks provided in the framework of the IGS2 reprocessing campaign). We present both the results for New Caledonia and an analysis of the applicability of these different processing strategies to older GNSS

  14. The ATLAS 5.5 GHz survey of the extended Chandra Deep Field South: the second data release

    NASA Astrophysics Data System (ADS)

    Huynh, M. T.; Bell, M. E.; Hopkins, A. M.; Norris, R. P.; Seymour, N.

    2015-11-01

    We present a new image of the 5.5 GHz radio emission from the extended Chandra Deep Field South. Deep radio observations at 5.5 GHz were obtained in 2010 and presented in the first data release. A further 76 h of integration has since been obtained, nearly doubling the integration time. This paper presents a new analysis of all the data. The new image reaches 8.6 μJy rms, an improvement of about 40 per cent in sensitivity. We present a new catalogue of 5.5 GHz sources, identifying 212 source components, roughly 50 per cent more than were detected in the first data release. Source counts derived from this sample are consistent with those reported in the literature for S5.5 GHz > 0.1 mJy but significantly lower than published values in the lowest flux density bins (S5.5 GHz < 0.1 mJy), where we have more detected sources and improved statistical reliability. The 5.5 GHz radio sources were matched to 1.4 GHz sources in the literature and we find a mean spectral index of -0.35 ± 0.10 for S5.5 GHz > 0.5 mJy, consistent with the flattening of the spectral index observed in 5 GHz sub-mJy samples. The median spectral index of the whole sample is αmed = -0.58, indicating that these observations may be starting to probe the star-forming population. However, even at the faintest levels (0.05 < S5.5 GHz < 0.1 mJy), 39 per cent of the 5.5 GHz sources have flat or inverted radio spectra. Four flux density measurements from our data, across the full 4.5-6.5 GHz bandwidth, are combined with those from literature and we find 10 per cent of sources (S5.5 GHz ≳ 0.1 mJy) show significant curvature in their radio spectral energy distribution spanning 1.4-9 GHz.

  15. EMISSION-LINE GALAXIES FROM THE HUBBLE SPACE TELESCOPE PROBING EVOLUTION AND REIONIZATION SPECTROSCOPICALLY (PEARS) GRISM SURVEY. I. THE SOUTH FIELDS

    SciTech Connect

    Straughn, Amber N.; Gardner, Jonathan P.; Pirzkal, Norbert; Grogin, Norman; Panagia, Nino; Meurer, Gerhardt R.; Cohen, Seth H.; Windhorst, Rogier A.; Malhotra, Sangeeta; Rhoads, James; Jansen, Rolf A.; Hathi, Nimish P.; Di Serego Alighieri, Sperello; Gronwall, Caryl; Walsh, Jeremy; Pasquali, Anna; Xu, Chun

    2009-10-15

    We present results of a search for emission-line galaxies (ELGs) in the southern fields of the Hubble Space Telescope Probing Evolution And Reionization Spectroscopically (PEARS) grism survey. The PEARS South Fields consist of five Advanced Camera for Surveys pointings (including the Hubble Ultra Deep Field) with the G800L grism for a total of 120 orbits, revealing thousands of faint object spectra in the GOODS-South region of the sky. ELGs are one subset of objects that are prevalent among the grism spectra. Using a two-dimensional detection and extraction procedure, we find 320 emission lines originating from 226 galaxy 'knots' within 192 individual galaxies. Line identification results in 118 new grism-spectroscopic redshifts for galaxies in the GOODS-South Field. We measure emission-line fluxes using standard Gaussian fitting techniques. At the resolution of the grism data, the H{beta} and [O III] doublet are blended. However, by fitting two Gaussian components to the H{beta} and [O III] features, we find that many of the PEARS ELGs have high [O III]/H{beta} ratios compared to other galaxy samples of comparable luminosities. The star formation rates of the ELGs are presented, as well as a sample of distinct giant star-forming regions at z {approx} 0.1-0.5 across individual galaxies. We find that the radial distances of these H II regions in general reside near the galaxies' optical continuum half-light radii, similar to those of giant H II regions in local galaxies.

  16. A compilation of field surveys on gaseous elemental mercury (GEM) from contrasting environmental settings in Europe, South America, South Africa and China: separating fads from facts.

    PubMed

    Higueras, Pablo; Oyarzun, Roberto; Kotnik, Joze; Esbrí, José María; Martínez-Coronado, Alba; Horvat, Milena; López-Berdonces, Miguel Angel; Llanos, Willians; Vaselli, Orlando; Nisi, Barbara; Mashyanov, Nikolay; Ryzov, Vladimir; Spiric, Zdravko; Panichev, Nikolay; McCrindle, Rob; Feng, Xinbin; Fu, Xuewu; Lillo, Javier; Loredo, Jorge; García, María Eugenia; Alfonso, Pura; Villegas, Karla; Palacios, Silvia; Oyarzún, Jorge; Maturana, Hugo; Contreras, Felicia; Adams, Melitón; Ribeiro-Guevara, Sergio; Niecenski, Luise Felipe; Giammanco, Salvatore; Huremović, Jasna

    2014-08-01

    Mercury is transported globally in the atmosphere mostly in gaseous elemental form (GEM, [Formula: see text]), but still few worldwide studies taking into account different and contrasted environmental settings are available in a single publication. This work presents and discusses data from Argentina, Bolivia, Bosnia and Herzegovina, Brazil, Chile, China, Croatia, Finland, Italy, Russia, South Africa, Spain, Slovenia and Venezuela. We classified the information in four groups: (1) mining districts where this contaminant poses or has posed a risk for human populations and/or ecosystems; (2) cities, where the concentration of atmospheric mercury could be higher than normal due to the burning of fossil fuels and industrial activities; (3) areas with natural emissions from volcanoes; and (4) pristine areas where no anthropogenic influence was apparent. All the surveys were performed using portable LUMEX RA-915 series atomic absorption spectrometers. The results for cities fall within a low GEM concentration range that rarely exceeds 30 ng m(-3), that is, 6.6 times lower than the restrictive ATSDR threshold (200 ng m(-3)) for chronic exposure to this pollutant. We also observed this behavior in the former mercury mining districts, where few data were above 200 ng m(-3). We noted that high concentrations of GEM are localized phenomena that fade away in short distances. However, this does not imply that they do not pose a risk for those working in close proximity to the source. This is the case of the artisanal gold miners that heat the Au-Hg amalgam to vaporize mercury. In this respect, while GEM can be truly regarded as a hazard, because of possible physical-chemical transformations into other species, it is only under these localized conditions, implying exposure to high GEM concentrations, which it becomes a direct risk for humans. PMID:24379158

  17. Hydrology and water quality near the South Well Field, southern Franklin County, Ohio, with emphasis on the simulation of ground-water flow and transport of Scioto River. Water resources investigation

    SciTech Connect

    Childress, C.J.O.; Sheets, R.A.; Bair, E.S.

    1991-01-01

    At present (1990), about 15 percent of the total water supply for the City of Columbus, Ohio, is provided by ground water withdrawn from the South Well Field in southern Franklin County. Much of the flow of Scioto River at the South Well Field originates from the Jackson Pike Wastewater Treatment Facility (WTF), one of two municipal wastewater-treatment plants operated by the City of Columbus. The Jackson Pike WTF discharges effluent into Scioto River about 6 mi upstream from the South Well Field. The U.S. Geological Survey (USGS), undertook a study to evaluate the hydrologic consequences of changes in effluent discharge to Scioto River and to clarify the interaction of Scioto River and carbonate bedrock and glacial drift aquifers at the South Well Field. The report describes the hydrology and water quality of the South Well Field area by presenting the results of (1) surface-water-transport simulations of a conservative constituent during low flow of Scioto River from Frank Road to the South Well Field and (2) ground-water-flow simulations of the glacial drift and carbonate bedrock aquifers at the South Well Field. The simulations are examined along with surface-water and ground-water quality to describe the relation between the quantity and quality of flow in the Scioto River; the nature of the ground-water-flow system; and the quantity, quality, and sources of water pumped from the South Well Field. Data collection in the study area in August and September 1987 and 1988 included sampling for surface-water and ground-water quality and measurement of surface-water discharge, Scioto River travel-times, ground-water levels, and vertical riverbed hydraulic conductivity.

  18. Levelling or Playing the Field? The Politics of Access to University Education in Post-Apartheid South Africa.

    ERIC Educational Resources Information Center

    Naidoo, Rajani

    1998-01-01

    Provides an account of access policies in relation to university education in South Africa by analyzing the practices surrounding the report "A Framework for Transformation." Argues that the repositioning of equity, economic development, and academic standards within the arena of the National Commission on Higher Education has shaped access…

  19. Higher Education Research as a Field of Study in South Korea: Inward but Starting to Look Outward

    ERIC Educational Resources Information Center

    Jung, Jisun

    2015-01-01

    This study aims to explore the development of higher education research in South Korea based on historical and scientometric perspectives. After the evolution of the country's higher education research community is presented, articles focusing on higher education from 1995 to 2012 are analysed. In total, 145 articles in international journals and…

  20. Comparing the performance of coupled soil-vegetation-atmosphere models at two contrasting field sites in South-West Germany

    NASA Astrophysics Data System (ADS)

    Gayler, S.; Wöhling, T.; Priesack, E.; Wizemann, H.-D.; Wulfmeyer, V.; Ingwersen, J.; Streck, T.

    2012-04-01

    of their structural complexity on two winter wheat research fields under different climate in South-West Germany. We investigate the ability of the models to simultaneously fit measured soil water contents, leaf area development and actual evapotranspiration rates from eddy-covariance measurements. The calibration of the models is performed in a multi-criteria context using three objective functions, which describe the discrepancy between measurements and simulations of the three data types. We use the AMALGAM evolutionary search algorithm to simultaneously estimate the most important plant and soil hydraulic parameters. The results show that the trade-off in fitting soil moisture, leaf area development and evapotranspiration can be quite large for those models that represent plant processes by simple concepts. However, these trade-offs are smaller for the more mechanistic plant growth models, so that it can be expected that these optimized mechanistic models will provide the basis for improved simulations of land-surface-atmosphere feedback processes.

  1. Predicting plant water content in Eucalyptus grandis forest stands in KwaZulu-Natal, South Africa using field spectra resampled to the Sumbandila Satellite Sensor

    NASA Astrophysics Data System (ADS)

    Oumar, Z.; Mutanga, O.

    2010-06-01

    The measurement of plant water content is essential to assess stress and disturbance in forest plantations. Traditional techniques to assess plant water content are costly, time consuming and spatially restrictive. Remote sensing techniques offer the alternative of a non-destructive and instantaneous method of assessing plant water content over large spatial scales where ground measurements would be impossible on a regular basis. In the context of South Africa, due to the cost and availability of imagery, studies focusing on the estimation of plant water content using remote sensing data have been limited. With the scheduled launch of the South African satellite SumbandilaSat evident in 2009, it is imperative to test the utility of this satellite in estimating plant water content. This study resamples field spectral data measured from a field spectrometer to the band settings of the SumbandilaSat in order to test its potential in estimating plant water content in a Eucalyptus plantation. The resampled SumbandilaSat wavebands were input into a neural network due to its ability to model non-linearity in a dataset and its inherent ability to perform better than conventional linear models. The integrated approach involving neural networks and the resampled field spectral data successfully predicted plant water content with a correlation coefficient of 0.74 and a root mean square error (RMSE) of 1.41% on an independent test dataset outperforming the traditional multiple regression method of estimation. The best-trained neural network algorithm that was chosen for assessing the relationship between plant water content and the SumbandilaSat bands was based on a few points only and more research is required to test the robustness and effectiveness of this sensor in estimating plant water content across different species and seasons. This is critical for monitoring plantation health in South Africa using a cheaply available local sensor containing key vegetation wavelengths.

  2. A validation study of a rapid field-based rating system for discriminating among flow permanence classes of headwater streams in South Carolina.

    PubMed

    Fritz, Ken M; Wenerick, William R; Kostich, Mitch S

    2013-11-01

    Rapid field-based protocols for classifying flow permanence of headwater streams are needed to inform timely regulatory decisions. Such an existing method was developed for and has been used in North Carolina since 1998. The method uses ordinal scoring of 26 geomorphology, hydrology, and biology attributes of streams. The attribute scores are summed and compared to threshold scores to assign a flow permanence class. Our study objective was to evaluate the method's ability to classify the flow permanence of forested stream reaches from Piedmont and Southeastern Plains ecoregions in South Carolina. Ephemeral reaches scored significantly lower than intermittent and perennial reaches, but scores from intermittent and perennial reaches did not differ. Scores collected in the dry and wet seasons were strongly correlated, indicating that the method was seasonally stable. Scores had positive nonlinear relationships with the maximum recorded wet duration and the proportion of the record that reaches were wet, but were not related to drying frequency. Scores of the presence of baseflow in the dry season were more important in flow permanence classification than those from the wet season. Other important attributes and parameters in discriminating flow classes were macrobenthos, rooted upland plants, bankfull width, drainage area, and ecoregion. Although the North Carolina method did not consistently differentiate intermittent from perennial reaches, the indicator-based approach is a strong foundation from which to build a protocol for South Carolina. Adding measures like bankfull width and drainage area, weighting by ecoregion, or shifting thresholds may be warranted modifications for South Carolina. PMID:24000112

  3. South Pole NO Observations: An Assessment of the Factors Controlling the Large Variability Seen in the ISCAT 2000 Field Study

    NASA Astrophysics Data System (ADS)

    Davis, D. D.; Buhr, M.; Lefer, B.; Shetter, R.; Oncley, S.; Semmer, S.; Lenschow, D.

    2001-12-01

    In December of 1998, the first observations of NO at South Pole were recorded. The surprisingly high levels observed (e.g. median value 225 pptv) were examined in the context of three possible sources: local pollution, long-range transport, and snow surface emissions. Of these possibilities, only the snow source was found to be credible. Of particular significance in our arriving at this conclusion was the fact that other investigators had previous to the ISCAT study reported evidence for a significant snow source of NO. These observations were reported at Summit, Greenland, Alert, Canada, and even at a coastal Antarctic site. What made the South Pole ISCAT 1998 results so unusual was the finding that the median NO level was over one order of magnitude greater than at any other global site. Speculation at the conclusion of the ISCAT 1998 study was that an enhanced NO source strength from the snow at South Pole in conjunction with a very shallow mixing depth were major contributing factors promoting this difference. The ISCAT 2000 study has provided an opportunity to examine the above hypothesis in considerable detail. Centrally important in this new study were measurements of: 1) NO levels at several different heights above the snow surface; 2) NO snow to atmosphere fluxes; 3) NO levels within the snowpack as a function of depth; and 4) more intensive MET observations. The findings from these new observations have provided considerable insight into the large variability seen in South Pole NO (i.e. 10 to 500 pptv) and will be discussed.

  4. Field study on the choice of friends in two multi-racial pre-schools (South Africa/London).

    PubMed

    Exenberger, Silvia

    2003-06-01

    The present research examined the influence of the two independent variables sex and race on the choice of friends in pre-school children. Data for this investigation were collected in two pre-schools, one situated in Stellenbosch, South Africa, the other in London, U.K. Both schools have in common that they accommodate children of different racial backgrounds (black, white, and coloured children), but the children's experience with desegregated classrooms differ. Friendship was operational defined with thirteen categories, summarized to the basic category pro-social behaviour. Fifty hours of free-play time were taped with one video camera in South Africa, and hundred hours were taped with two video cameras in London. The results showed that sex and race interact in their effect on the choice of friends. In South Africa race is supposed to be a strong indicator for friendship choices, especially for black children, whereas the black children in London choose friends more or less on the basis of sex. PMID:12872548

  5. Consolidation of geologic studies of geopressured-geothermal resources in Texas: Barrier-bar tidal-channel reservoir facies architecture, Jackson Group, Prado field, South Texas; Final report

    SciTech Connect

    Seni, S.J.; Choh, S.J.

    1994-01-01

    Sandstone reservoirs in the Jackson barrier/strandplain play are characterized by low recovery efficiencies and thus contain a large hydrocarbon resource target potentially amenable to advanced recovery techniques. Prado field, Jim Hogg County, South Texas, has produced over 23 million bbl of oil and over 32 million mcf gas from combination structural-stratigraphic traps in the Eocene lower Jackson Group. Hydrocarbon entrapment at Prado field is a result of anticlinal nosing by differential compaction and updip pinch-out of barrier bar sandstone. Relative base-level lowering resulted in forced regression that established lower Jackson shoreline sandstones in a relatively distal location in central Jim Hogg County. Reservoir sand bodies at Prado field comprise complex assemblages of barrier-bar, tidal-inlet fill, back-barrier bar, and shoreface environments. Subsequent progradation built the barrier-bar system seaward 1 to 2 mi. Within the barrier-bar system, favorable targets for hydrocarbon reexploration are concentrated in tidal-inlet facies because they possess the greatest degree of depositional heterogeneity. The purpose of this report is (1) to describe and analyze the sand-body architecture, depositional facies variations, and structure of Prado field, (2) to determine controls on distribution of hydrocarbons pertinent to reexploration for bypassed hydrocarbons, (3) to describe reservoir models at Prado field, and (4) to develop new data affecting the suitability of Jackson oil fields as possible candidates for thermally enhanced recovery of medium to heavy oil.

  6. Chemical flood progress evaluation test, South Pass Block 27 field, Plaquemines Parish, Louisiana. Final report, September 28, 1979-May 16, 1980

    SciTech Connect

    Johnston, J. R.; Guillory, A. J.

    1981-02-01

    A field test of a surfactant flooding process has been designed for a reservoir located in the South Pass Block 27 field, Plaquemines Parish, Louisiana. The objectives of the test are to continue chemical flooding research by applying the process in a reservoir which is a candidate for this enhanced oil recovery technique if the process is proved economically viable. The plan is to acquire field data which will lead to a better understanding of how the process works under reservoir conditions at a well-to-well distance intermediate to laboratory floods and economic well spacing. The initial step in starting the field test began late in 1979 when the first pilot injection-residual oil saturation determination well was drilled and pressured cored in the selected test reservoir, the N/sub 4/ sand Reservoir B, at about 8000 feet. A log-inject-log measurement in this well has also been completed to provide an added evaluation. This report documents the results of the N/sub 4/, sand residual oil saturation measurements in Well SL 1011 No. 88. The Shell-DOE contract is restricted to this phase of the field test. Results indicate a waterswept residual oil saturation less than 20% at the objective location based on coring and PNC log-inject-log measurements. The value is lower than anticipated. Consequently, an alternate test site must be selected if the field test plans are continued.

  7. Comparative Analysis of Visual Field Plotting by Octopus Interzeag 1-2-3, Humphrey Field Analyser II and Frequency Doubling Perimetry in Glaucoma Patients in South Indian Population

    PubMed Central

    Suma, Elangovan; Prabhu, D Ranjit

    2015-01-01

    Purpose Standard achromatic perimetry tests the differential light sensitivity whereas the frequency doubling technology tests the contrast sensitivity. The aim of this study was to compare and correlate the visual field indices with three different types of perimeters namely frequency doubling perimetry (FDP), Humphrey field analyser (HFA) and Octopus Interzeag 1-2-3 (OI) for detecting glaucomatous field defects. Design Prospective cross-sectional observational study. Materials and Methods Hundred eyes of 50 glaucoma patients were studied. All the patients underwent visual field examinations by Octopus Interzeag 1-2-3, Humphrey field Analyser II and Frequency Doubling perimetry (FDP). The correlations of the global indices were compared. The time taken to perform the test with the three perimeters was analysed. Results The visual field plotting by the perimeters were comparable and significant positive correlation was observed. The time taken to perform visual field test by Octopus Interzeag 1-2-3 was shorter than the other two methods. Conclusion The visual field plotting by Octopus Interzeag 1-2-3, Humphrey field analyser and frequency doubling technology perimetry were comparable and Octopus field plotting takes lesser time than the rest two methods. PMID:26393152

  8. Field and laboratory data describing physical and chemical characteristics of metal-contaminated flood-plain deposits downstream from Lead, west-central South Dakota

    USGS Publications Warehouse

    Marron, D.C.

    1988-01-01

    Samples from metal-contaminated flood-plain sediments at 9 sites downstream from Lead, in west-central South Dakota, were collected during the summers of 1985-87 to characterize aspects of the sedimentology, chemistry, and geometry of a deposit that resulted from the discharge of a large volume of mining wastes into a river system. Field and laboratory data include stratigraphic descriptions, chemical contents and grain-size distributions of samples, and surveyed flood-plain positions of samples. This report describes sampling-site locations, and methods of sample collection and preservation, and subsequent laboratory analysis. Field and laboratory data are presented in 4 figures and 11 tables in the ' Supplemental Data ' section at the back of the report. (USGS)

  9. Field-trip guide to volcanic and volcaniclastic deposits of the lower Jurassic Talkeetna formation, Sheep Mountain, south-central Alaska

    USGS Publications Warehouse

    Draut, Amy E.; Clift, Peter D.; Blodgett, Robert B.

    2006-01-01

    This guide provides information for a one-day field trip in the vicinity of Sheep Mountain, just north of the Glenn Highway in south-central Alaska. The Lower Jurassic Talkeetna Formation, consisting of extrusive volcanic and volcaniclastic sedimentary rocks of the Talkeetna arc complex, is exposed on and near Sheep Mountain. Field-trip stops within short walking distance of the Glenn Highway (approximately two hours’ drive from Anchorage) are described, which will be visited during the Geological Society of America Penrose meeting entitled Crustal Genesis and Evolution: Focus on Arc Lower Crust and Shallow Mantle, held in Valdez, Alaska, in July 2006. Several additional exposures of the Talkeetna Formation on other parts of Sheep Mountain that would need to be accessed with longer and more strenuous walking or by helicopter are also mentioned.

  10. Evaluation of a total dissolved solids model in comparison to actual field data measurements in the Cheyenne River, South Dakota, U.S.A.

    PubMed

    Berdanier, Bruce W; Ziadat, Anf H

    2006-06-01

    During the summers of 2002 and 2004, in-stream integrated flow and concentration measurements for the total dissolved solids in the Cheyenne River, South Dakota, USA was conducted in order to compare the obtained actual field measurements with the predictions values made by the Bureau of Reclamation in the Environmental Impact Statement. In comparison to the actual field measurements conducted in this study, The Bureau of Reclamation extension of a small database used in the analysis for the impact of operations at the Angostura Unit over the past 50 years and into the future to predict the annual total dissolved solid loadings doesn't represent the actual loading values and various conditions in the study area. Additional integrated flow and concentration sampling is required to characterize the impact of the current Angostura Dam operations and Angostura Irrigation District return flows on the Cheyenne River in different seasons of the year. PMID:16917716

  11. Mid-Infrared Properties and Color Selection for X-Ray-Detected Active Galactic Nuclei in the MUSYC Extended Chandra Deep Field-South

    NASA Astrophysics Data System (ADS)

    Cardamone, Carolin N.; Urry, C. Megan; Damen, Maaike; van Dokkum, Pieter; Treister, Ezequiel; Labbé, Ivo; Virani, Shanil N.; Lira, Paulina; Gawiser, Eric

    2008-06-01

    We present the mid-infrared colors of X-ray-detected AGNs and explore mid-infrared selection criteria. Using a statistical matching technique, the likelihood ratio, over 900 IRAC counterparts were identified with a new MUSYC X-ray source catalog that includes ~1000 published X-ray sources in the Chandra Deep Field-South and Extended Chandra Deep Field-South. Most X-ray-selected AGNs have IRAC spectral shapes consistent with power-law slopes, fν propto να, and display a wide range of colors, -2 <= α <= 2. Although X-ray sources typically fit to redder (more negative α) power laws than non-X-ray-detected galaxies, more than 50% do have flat or blue (galaxy-like) spectral shapes in the observed 3-8 μm band. Only a quarter of the X-ray-selected AGNs detected at 24 μm are well fit by featureless red power laws in the observed 3.6-24 μm, likely the subset of our sample whose infrared spectra are dominated by emission from the central AGN region. Most IRAC color selection criteria fail to identify the majority of X-ray-selected AGNs, finding only the more luminous AGNs, the majority of which have broad emission lines. In deep surveys, these color selection criteria select 10%-20% of the entire galaxy population and miss many moderate-luminosity AGNs.

  12. South Africa

    NASA Technical Reports Server (NTRS)

    2002-01-01

    This true-color image of South Africa was acquired on May 14, 2000, by NASA's Moderate-resolution Imaging Spectroradiometer, or MODIS. The image was produced using a combination of the sensor's 250-m and 500-m resolution visible wavelength bands. As part of the opening ceremony to begin the joint U.S.-South Africa SAFARI Field Experiment, NASA presented print copies of this image as GIFts to Dr. Ben Ngubane, Minister of Arts, Science and Technology, and Honorable Advocate Ngoaka Ramathlodi, Premier of the Northern Province, South Africa. The area shown in this image encompasses seven capital cities and a number of the region's distinctive geological features can be seen clearly. Toward the northern (top) central part of the image, the browns and tans comprise the Kalahari Desert of southern Botswana. The Tropic of Capricorn runs right through the heart of the Kalahari and the Botswanan capital city of Gaborone sits on the Limpopo River, southeast of the Kalahari. Along the western coastline of the continent is the country of Namibia, where the Namib Desert is framed against the sea by the Kaokoveld Mountains. The Namibian capital of Windhoek is obscured by clouds. Looking closely in the center of the image, the Orange River can be seen running from east to west, demarcating the boundary between Namibia and South Africa. On the southwestern corner of the continent is the hook-like Cape of Good Hope peninsula and Cape Town, the parliamentary capital of South Africa. Running west to east away from Cape Town are the Great Karroo Mountains. The shadow in this image conveys a sense of the very steep grade of the cliffs along the southern coast of South Africa. Port Elizabeth sits on the southeasternmost point of South Africa, and a large phytoplankton bloom can be seen in the water about 100 miles east of there. Moving northward along the east coast, the Drakensberg Mountains are visible. The two small nations of Lesotho and Swaziland are in this region, completely

  13. Tracing the Mass-Dependent Star Formation History of Late-Type Galaxies using X-ray Emission: Results from the CHANDRA Deep Fields

    NASA Technical Reports Server (NTRS)

    Lehmer, B.D; Brandt, W.N.; Schneider, D.P.; Steffen, A.T.; Alexander, D.M.; Bell, E.F.; Hornschemeier, A.E.; McIntosh, D.H.; Bauer, F.E.; Gilli, R.; Mainieri, V.; Silverman, J.D.; Tozzi, P.; Wolf, C.

    2008-01-01

    We report on the X-ray evolution over the last approx.9 Gyr of cosmic history (i.e., since z = 1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S. respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies. which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of approx. 5-10) in the X-ray-to-optical mean luminosity ratio (L(sub x)/L(sub B)) and the X-ray-to-stellar-mass mean ratio (L(sub x)/M(sub *)) for galaxy populations selected by L(sub B) and M(sub *), respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L(sub x)/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR = 1-100 Solar Mass/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star-formation activity out to z approx. 1.4. We find that the star-formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z = 0.2-1, which is consistent with previous studies of how star-formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z approx. 3 and estimate that L(sub x)/L(sub B) at z approx. 3 is similar to its value at z = 1.4.

  14. Fracture development in Paleozoic shale of Chongqing area (South China). Part two: Numerical simulation of tectonic stress field and prediction of fractures distribution

    NASA Astrophysics Data System (ADS)

    Zeng, Weite; Ding, Wenlong; Zhang, Jinchuan; Zhang, Yeqian; Guo, Ling; Jiu, Kai; Li, Yifan

    2013-10-01

    A tectonics sedimentation evolution has been researched in Southeast Chongqing, and the reasonable Longmaxi shale highstand system tract (HST) and transgressive system tract (TST) geological model were built respectively based on the rock mechanical test and acoustic emission experiment which the samples are from field outcrop and the Yuye-1 well. The Longmaxi shale two-dimension tectonic stress field during the Cenozoic was simulated by the finite element method, and the distribution of fractures was predicted. The research results show that the tectonic stress field and the distribution of fractures were controlled by lithology and structure. As a result of Cretaceous movement, there are trough-like folds (wide spaced synclines), battlement-like folds (similar spaces between synclines and anticlines) and ejective folds (wide spaced anticlines), which are regularly distributed from southeast to northwest in the study area. Since the strain rate and other physical factors such as the viscosity are not taken into account, and the stress intensity is the main factor that determines the tectonic strength. Therefore, the stronger tectonic strength leads the higher stress intensity in the eastern and southeastern study area than in the northwest. The fracture zones are mainly concentrated in the fold axis, transition locations of faults and folds, the regions where are adjacent to faults. The fragile mineral contents (such as siliceous rock, carbonate rock and feldspar) in the shelf facies shale from south of the study area are higher than in the bathyal facies and abyssal facies shale from center of the study area. The shales characterized by low Poisson's ratio and high elastic modulus from south of the study area are easily broken during Cenozoic orogenic movement.

  15. Arsenic accumulation and phosphorus status in two rice (Oryza sativa L.) cultivars surveyed from fields in South China.

    PubMed

    Lu, Ying; Dong, Fei; Deacon, Claire; Chen, Huo-Jun; Raab, Andrea; Meharg, Andrew A

    2010-05-01

    The consumption of paddy rice (Oryza sativa L.) is a major inorganic arsenic exposure pathway in S.E. Asia. A multi-location survey was undertaken in Guangdong Province, South China to assess arsenic accumulation and speciation in 2 rice cultivars, one an Indica and the other a hybrid Indica. The results showed that arsenic concentrations in rice tissue increased in the order grain < husk < straw < root. Rice grain arsenic content of 2 rice cultivars was significant different and correlated with phosphorus concentration and molar ratio of P/As in shoot, being higher for the Indica cultivar than for the hybrid Indica, which suggests altering shoot phosphorus status as a promising route for breeding rice cultivars with reduced grain arsenic. Speciation of grain arsenic, performed using HPLC-ICP-MS, identified inorganic arsenic as the dominant arsenic species present in the rice grain. PMID:20045585

  16. Petrophysical properties and geology of selected intervals in the Frio Formation, Stratton field, South Texas for modeling interwell seismic logging response

    SciTech Connect

    Collier, H.A.; Parra, J.O.

    1996-09-01

    Seismic or continuity logging consists of locating a seismic source in one borehole near or in a low-velocity layer and deploying a detector array in a second borehole. Detection of guided waves transmitted between the two wells indicates bed connectivity. The guided wave signatures are either leaky modes or normal modes (or both). The technique has numerous applications in various types of heterogeneous geological environments, including many Gulf Coast gas reservoirs. It can be used to determine the continuity of beds between wells, estimate and locate variations in the thickness of beds, and estimate the average rock physical properties of the beds. Stratton field was selected as the Gulf-Coast-gas-play type field for a project to model interwell seismic logging responses. Stratton is a mature gas field located in the south Texas Gulf Coast, about 30 miles southwest of Corpus Christi. It encompasses over 120,000 acres in portions of Kleberg, Nueces, and Jim Wells counties. Stratton is one of 29 fields in the Frio Formation fluvial-deltaic lay associated with the Vicksburg fault zone along the Texas Gulf Coast Basin. This poster presentation explains the technique of interwell seismic logging, documents the petrophysical properties and geology of intervals in the upper and middle Frio, and presents the results of the forward modeling tests.

  17. An Integrated Study of the Grayburg/San Andres Reservoir, Foster and South Cowden Fields, Ector County, Texas, Class II

    SciTech Connect

    Trentham, Robert C.; Weinbrandt, Richard; Robinson, William C.; Widner, Kevin

    2001-05-03

    The objectives of the project were to: (1) Thoroughly understand the 60-year history of the field. (2) Develop a reservoir description using geology and 3D seismic. (3) Isolate the upper Grayburg in wells producing from multiple intervals to stop cross flow. (4) Re-align and optimize the upper Grayburg waterflood. (5) Determine well condition, identify re-frac candidates, evaluate the effectiveness of well work and obtain bottom hole pressure data for simulation utilizing pressure transient testing field wide. (6) Quantitatively integrate all the data to guide the field operations, including identification of new well locations utilizing reservoir simulation.

  18. Spatial heterogeneity of temperature across alpine boulder fields in New South Wales, Australia: multilevel modelling of drivers of microhabitat climate.

    PubMed

    Shi, Haijing; Paull, David; Rayburg, Scott

    2016-07-01

    Understanding the spatial heterogeneity of temperatures across a region is significant for identification and protection of potential microhabitats for species conservation. However, this task is proving difficult because multiple factors drive the temperatures of microhabitats and their effect differs at different scales. In the Australian alpine region, boulder field habitats have been identified as important refugia for a range of small mammals. Vegetation cover and elevation have been found to drive thermal buffering at the level of single sampling sites within boulder fields, whereas the aspect and inclination of slopes have been found to affect thermal buffering at the level of clusters of boulder fields. But how the rock structure (number of rock layers, rock size and cavity of boulders) influences microclimate of boulder fields remains an open question. We used a multilevel modelling approach to detect the factors driving microhabitat temperatures in different seasons at different spatial scales in an Australian alpine region. We found that significant temperature differences existed within and between clusters of boulder fields in different seasons. Besides elevation and vegetation cover, the number of rock layers and rock cavity size also exerts important influences on extreme temperatures at the site (i.e. single boulder field) scale. Topographical variables such as slope gradient and elevation influenced minimum temperatures at the boulder field cluster scale. Variations in boulder field temperatures were significant at fine scales, with variations in minimum temperatures exceeding those of maximum temperatures. We suggest that variations in slope gradient and elevation, interacting with vegetation cover, the number of rock layers and rock cavity size can lead to fine-grained thermal variability, which potentially provides refugia for species at microsites, even when regional climatic conditions become less suitable for their survival. PMID:26511483

  19. Spatial heterogeneity of temperature across alpine boulder fields in New South Wales, Australia: multilevel modelling of drivers of microhabitat climate

    NASA Astrophysics Data System (ADS)

    Shi, Haijing; Paull, David; Rayburg, Scott

    2015-10-01

    Understanding the spatial heterogeneity of temperatures across a region is significant for identification and protection of potential microhabitats for species conservation. However, this task is proving difficult because multiple factors drive the temperatures of microhabitats and their effect differs at different scales. In the Australian alpine region, boulder field habitats have been identified as important refugia for a range of small mammals. Vegetation cover and elevation have been found to drive thermal buffering at the level of single sampling sites within boulder fields, whereas the aspect and inclination of slopes have been found to affect thermal buffering at the level of clusters of boulder fields. But how the rock structure (number of rock layers, rock size and cavity of boulders) influences microclimate of boulder fields remains an open question. We used a multilevel modelling approach to detect the factors driving microhabitat temperatures in different seasons at different spatial scales in an Australian alpine region. We found that significant temperature differences existed within and between clusters of boulder fields in different seasons. Besides elevation and vegetation cover, the number of rock layers and rock cavity size also exerts important influences on extreme temperatures at the site (i.e. single boulder field) scale. Topographical variables such as slope gradient and elevation influenced minimum temperatures at the boulder field cluster scale. Variations in boulder field temperatures were significant at fine scales, with variations in minimum temperatures exceeding those of maximum temperatures. We suggest that variations in slope gradient and elevation, interacting with vegetation cover, the number of rock layers and rock cavity size can lead to fine-grained thermal variability, which potentially provides refugia for species at microsites, even when regional climatic conditions become less suitable for their survival.

  20. Spatial heterogeneity of temperature across alpine boulder fields in New South Wales, Australia: multilevel modelling of drivers of microhabitat climate

    NASA Astrophysics Data System (ADS)

    Shi, Haijing; Paull, David; Rayburg, Scott

    2016-07-01

    Understanding the spatial heterogeneity of temperatures across a region is significant for identification and protection of potential microhabitats for species conservation. However, this task is proving difficult because multiple factors drive the temperatures of microhabitats and their effect differs at different scales. In the Australian alpine region, boulder field habitats have been identified as important refugia for a range of small mammals. Vegetation cover and elevation have been found to drive thermal buffering at the level of single sampling sites within boulder fields, whereas the aspect and inclination of slopes have been found to affect thermal buffering at the level of clusters of boulder fields. But how the rock structure (number of rock layers, rock size and cavity of boulders) influences microclimate of boulder fields remains an open question. We used a multilevel modelling approach to detect the factors driving microhabitat temperatures in different seasons at different spatial scales in an Australian alpine region. We found that significant temperature differences existed within and between clusters of boulder fields in different seasons. Besides elevation and vegetation cover, the number of rock layers and rock cavity size also exerts important influences on extreme temperatures at the site (i.e. single boulder field) scale. Topographical variables such as slope gradient and elevation influenced minimum temperatures at the boulder field cluster scale. Variations in boulder field temperatures were significant at fine scales, with variations in minimum temperatures exceeding those of maximum temperatures. We suggest that variations in slope gradient and elevation, interacting with vegetation cover, the number of rock layers and rock cavity size can lead to fine-grained thermal variability, which potentially provides refugia for species at microsites, even when regional climatic conditions become less suitable for their survival.

  1. Development of a spatially targeted field sampling technique for the southern cattle tick, Rhipicephalus microplus, by mapping white-tailed deer, Odocoileus virginianus, habitat in South Texas.

    PubMed

    Phillips, Pamela L; Welch, John B; Kramer, Matthew

    2014-01-01

    The objective of our study was to determine whether satellite remote sensed data could be used to identify white-tailed deer, Odocoileus virginianus (Zimmerman) (Artiodactyla: Cervidae), habitat and target locations for sampling free-living larvae of the southern cattle tick, Rhipicephalus (Boophilus) microplus (Canestrini) (Ixodida: Ixodidae) in South Texas. Two methods for mapping white-tailed deer habitat were used, an object-oriented method to identify closed canopies and waterways for deer movement and two vegetation indices: the Normalized Difference Vegetation Index and the Modified Soil Adjusted Vegetation Index to identify forage for deer. These two data sets of favorable white-tailed deer habitat were combined within a geographic information system to identify locations for sampling ticks. Larvae of R. (B.) microplus, were sampled in Zapata County, Texas, by walking transects with attached flannel panels to jeans. Although the data set and sampling period were limited, data analysis demonstrated that sampling of free-living larvae of R. (B.) microplus can be conducted in South Texas, and larvae were most abundant in areas that harbored O. virginianus. Spatial analysis of satellite imagery to classify white-tailed deer/southern cattle tick habitat proved efficacious and may be useful in directing sampling activities in the field. PMID:25368044

  2. Development of a Spatially Targeted Field Sampling Technique for the Southern Cattle Tick, Rhipicephalus microplus, by Mapping Whitetailed Deer, Odocoileus virginianus, Habitat in South Texas

    PubMed Central

    Phillips, Pamela L.; Welch, John B.; Kramer, Matthew

    2014-01-01

    The objective of our study was to determine whether satellite remote sensed data could be used to identify white-tailed deer, Odocoileus virginianus (Zimmerman) (Artiodactyla: Cervidae), habitat and target locations for sampling free-living larvae of the southern cattle tick, Rhipicephalus (Boophilus) microplus (Canestrini) (Ixodida: Ixodidae) in South Texas. Two methods for mapping white-tailed deer habitat were used, an object-oriented method to identify closed canopies and waterways for deer movement and two vegetation indices: the Normalized Difference Vegetation Index and the Modified Soil Adjusted Vegetation Index to identify forage for deer. These two data sets of favorable white-tailed deer habitat were combined within a geographic information system to identify locations for sampling ticks. Larvae of R. (B.) microplus, were sampled in Zapata County, Texas, by walking transects with attached flannel panels to jeans. Although the data set and sampling period were limited, data analysis demonstrated that sampling of free-living larvae of R. (B.) microplus can be conducted in South Texas, and larvae were most abundant in areas that harbored O. virginianus. Spatial analysis of satellite imagery to classify white-tailed deer/southern cattle tick habitat proved efficacious and may be useful in directing sampling activities in the field. PMID:25368044

  3. Ground based chemical characterization of submicron aerosol during the South American Biomass Burning Analysis (SAMBBA) field experiment

    NASA Astrophysics Data System (ADS)

    Brito, Joel; Artaxo, Paulo; Varanda Rizzo, Luciana; Johnson, Ben; Haywood, Jim; Longo, Karla; Freitas, Saulo; Coe, Hugh

    2013-04-01

    This work presents the results of an Aerosol Chemical Speciation Monitor (ACSM) which was successfully operated at a ground station in Porto Velho, Brazil, during the South American Biomass Burning Analysis (SAMBBA). SAMBBA is an international research project based on experimental and modeling activities designed to investigate the impacts of biomass burning emissions on climate, air quality and numerical weather prediction over South America. The measurement program was headed by the deployment of UK's Facility for Airborne Atmospheric Measurements (FAAM) BAe-146 research aircraft over Brazil during the dry season of 2012. The aircraft operation was coordinated with ground-based measurements at Porto Velho, operated by the University of Sao Paulo. Besides the aerosol chemical speciation, continuous measurements of aerosol size distribution and optical properties were carried out at the ground station, together with CO, CO2 and O3. Filters for trace elements measured by XRF and for OC/EC determined using a Sunset instrument were also collected at the ground based component of SAMBBA. The ACSM collected data for three weeks during September 2012. This period included a strong biomass burning event which showed a marked peak in f60, linked with Levoglucosan, a well-known biomass burning marker. During the biomass burning event, organics concentrations rose up to 80 μg/m3, black carbon close to 6 μg/m3 and CO mixing ratio above 2 ppmv. Fast biomass burning aerosol processing in the atmosphere could be observed through the relative contributions of C2H3O+ vs. CO2+ relative to total organic mass (f44 vs. f43). A clear diurnal variation throughout the sampling period has been observed for organic aerosols with a median peak of 9 μg/m3 at 04:00 LT and a minima of 5 μg/m3 at 18:00 LT. Preliminary results indicate that organics are responsible for 85% of PM1 non-refractory aerosols. The data set will allow the study of interactions between biomass burning and biogenic

  4. Exploring the Usefulness of MISR-HR Products to Estimate Maize Crop Extent and Using Field Evidence to Evaluate the Results in South Africa's Free State Province

    NASA Astrophysics Data System (ADS)

    Verstraete, M. M.; Knox, N. M.; Hunt, L. A.; Kleyn, L.

    2014-12-01

    The MISR instrument on NASA's Terra platform has been operating for almost 15 years. Standard products are generated at a spatial resolution of 1.1 km or coarser, but a recently developed method to re-analyze the Level-1B2 data allows the retrieval of biogeophysical products at the native spatial resolution of the instrument (275 m). This development opens new opportunities to better address issues such as the management of agricultural production and food security. South African maize production is of great economic and social importance, not only nationally, but on the global market too, being one of the top ten maize producing countries. Seasonal maize production statistics are currently based on a combination of field measurements and estimates derived from manually digitizing high resolution imagery from the SPOT satellite. The field measurements are collected using the Producer Independent Crop Estimate System (PICES) developed by Crop Estimates Committee of the Department of Agriculture, Forestry and Fisheries. There is a strong desire to improve the quality of these statistics, to generate those earlier, and to automate the process to encompass larger areas. This paper will explore the feasibility of using the MISR-HR spectral and directional products, combined with the finer spatial resolution and the relatively frequent coverage afforded by that instrument, to address these needs. The study area is based in the Free State, South Africa, one of the primary maize growing areas in the country, and took place during the 2012-2013 summer growing season. The significance of the outcomes will be evaluated in the context of the 14+ years of available MISR data.

  5. Distribution of Pleuroncodes monodon larvae over the continental shelf of south-central Chile: Field and modeling evidence for partial local retention and transport

    NASA Astrophysics Data System (ADS)

    Yannicelli, Beatriz; Castro, Leonardo; Parada, Carolina; Schneider, Wolfgang; Colas, Francois; Donoso, David

    2012-01-01

    In situ and modeled spatial distribution of squat lobster ( Pleuroncodes monodon) larvae over the continental shelf off south central Chile (35-37°S) was analyzed along with currents and hydrography. We aimed to identify the main larval transport/retention characteristics in the study area, which constitutes the southernmost P. monodon fishing grounds embedded in the Humboldt Current System. We hypothesized that the main contribution to population renewal originates in the two persistent adult aggregations close to the nursery ground that occurs over a continental shelf terrace limited by two submarine canyons. Two extensive bio-physical field campaigns were carried out during the main 2001-2002 upwelling season field data indicated that larvae were released from late austral winter to spring from spots to the north and south of the nursery. Zoea I were found mainly below 50 m depth in southward-flowing waters, whereas older zoea dominated in northward flowing layers above 50 m. Larvae were circumscribed between the coast and the shelf break front and pelagic retention areas were identified over the widest shelf area. Megalopa and juveniles during March, were only found over the nursery area. Individual based simulations coupled to the output of a hydrodynamic model (climatological configuration) for the studied area, showed that the release sites close to the nursery made the largest contribution to recruitment. Sites further north could also contribute to recruitment if hatching occurred later in the upwelling season. The contribution of vertical behavior to larval success was also important, as was the former’s interaction with the site and time of larval release. Our results support the relevance of coastal circulation (affected by topography) on the persistence of P. monodon populations off southern Chile, and the modulation of temporal variability. These results might apply to other abundant species in the area.

  6. A field test for competitive effects of Aedes albopictus on A. aegypti in South Florida: differences between sites of coexistence and exclusion?

    PubMed Central

    Juliano, Steven A.; Lounibos, L. Philip; O’Meara, George F.

    2007-01-01

    We tested whether interspecific competition from Aedes albopictus had measurable effects on A. aegypti at the typical numbers of larval mosquitoes found in cemetery vases in south Florida. We also tested whether the effect of interspecific competition from A. albopictus on A. aegypti differed between sites where A. aegypti either persists or went extinct following invasion by A. albopictus. Similar experiments manipulating numbers of A. albopictus in cemetery vases were conducted at three sites of A. aegypti persistence and three sites where A. aegypti was apparently extinct. The experiments were done using numbers of larvae that were determined by observed numbers of larvae for each site, and with resources (leaf detritus) that accumulated in experimental vases placed into each field site. In both the early rainy season (when number of mosquito larvae was low) and the late rainy season (when number of mosquito larvae was high), there was a significant effect of treatment on developmental progress of experimental A. aegypti. In the late rainy season, when numbers of larvae were high, there was also a significant effect of treatment on survivorship of A. aegypti. However, the competition treatment × site type (A. aegypti persists vs extinct) interaction was never significant, indicating that the competitive effect of A. albopictus on A. aegypti did not differ systematically between persistence versus extinction sites. Thus, although competition from A. albopictus is strong under field conditions at all sites, we find no evidence that variation in the impact of interspecific competition is associated with coexistence or exclusion. Interspecific competition among larvae is thus a viable explanation for exclusion or reduction of A. aegypti in south Florida, but variation in the persistence of A. aegypti following invasion does not seem to be primarily a product of variation in the conditions in the aquatic environments of cemetery vases. PMID:15024640

  7. Seasonal thermal fronts on the northern South China Sea shelf: Satellite measurements and three repeated field surveys

    NASA Astrophysics Data System (ADS)

    Jing, Zhiyou; Qi, Yiquan; Fox-Kemper, Baylor; Du, Yan; Lian, Shumin

    2016-03-01

    Seasonal thermal fronts associated with wind-driven coastal downwelling/upwelling in the northern South China Sea are investigated using satellite measurements and three repeated fine-resolution mapping surveys in winter, spring, and summer. The results show that vigorous thermal fronts develop over the broad shelf with variable widths and intensities in different seasons, which tend to be approximately aligned with the 20-100 m isobaths. Driven by the prevailing winter/summer monsoon, the band-shaped fronts were observed with a magnitude exceeding 0.1°C/km in the subsurface, and accompanied by energetic coastal downwelling/upwelling due to shoreward/offshore Ekman transport. The downward/upward tilting of seasonal thermoclines across the shelf exceeds 20 m, significantly contributing to the development of thermal fronts over the shelf. In addition, the diagnostic analysis of Potential Vorticity (PV) suggests that the summer frontal activities induced by the coastal upwelling are more stable to convection and symmetric instabilities in comparison to the winter fronts associated with downwelling-favorable monsoon forcing. This is primarily due to their essential differences in the upper ocean stratification and horizontal buoyancy gradients arising from wind forcing. At the same time, the coastal currents are substantially regulated by the seasonal winds. An expected lag correlation between the velocity from mooring measurements and alongshore wind stress is detected near the frontal region. These results indicate that seasonal wind forcing plays an important role in the frontal activities and coastal water transport over the shelf.

  8. Fluid transport by solitary waves along growing faults. A field example from the South Eugene Island Basin, Gulf of Mexico

    NASA Astrophysics Data System (ADS)

    Revil, A.; Cathles, L. M.

    2002-09-01

    The Red Fault system is one of the main growth faults found in the South Eugene Island Basin, a salt withdrawal minibasin located offshore Louisiana, in the Gulf of Mexico. This fault system corresponds to a lateral boundary between fluid overpressured compartments. In addition, there is a set of observations indicating that the Red Fault system exhibits rapid episodic migration of fluids. This fault represents an example of preferential pathway for the upward episodic migration of overpressured hydrocarbons from deep, heavily pressured, compartments on time scales of years. The migrations of fluids into active growing faults could take the form of propagating surges (solitary waves) that propagate upward along the fault planes in a wave-like manner at km/yr. Solitary waves represent a very efficient mechanism for the upward transport of fluids along growth faults in sedimentary basins generating its own permeability. In addition, this mechanism is compatible with the fact that the fault plane is observed to sustain a static pore fluid pressure difference between its two sides. The propagation of solitary waves in active growth faults appears as a fundamental mechanism to understand the nature of upward fast migration of fluids along active growth faults in compartimentalized sedimentary basins.

  9. Multiple episodes of dolomitization in the Arbuckle Group, Arbuckle Mountains, south-central Oklahoma: Field, petrographic, and geochemical evidence

    SciTech Connect

    Gao, G.; Land, L.S.; Elmore, R.D.

    1995-04-03

    The Cambro-Ordovician Arbuckle Group in the Arbuckle Mountains, south-central Oklahoma, had a complex history of dolomitization that resulted in two different geometries of dolomite bodies: stratal dolomite, of stratigraphically consistent, widespread distribution, and non-stratal dolomite, of stratigraphically inconsistent, local occurrence. Stratal dolomite includes the Royer and Butterly units in the lower Arbuckle Group. Most stratal dolomite samples are coarsely crystalline and have {sup 87}Sr/{sup 86}Sr ratios similar to Late Cambrian limestone and coeval seawater. All stratal dolomite and Arbuckle limestone samples have low {Delta}{sup 18}O values. Nonstratal dolomite is present in two areas: the Tishomingo Anticline and the Arbuckle Anticline. In the Tishomingo Anticline area, massive bodies (> 10 km{sup 2}) of nonstratal dolomite are present in a paleokarst system of pre-Middle Ordovician age. The petrographic and isotopic characteristics suggest that the nonstratal dolomite probably resulted from dolomitization of recrystallized limestone by post-Early Ordovician seawater. In the Arbuckle Anticline area, nonstratal dolomite is present as small irregular bodies that are related to Pennsylvanian faults and are associated with the margins of stratal Butterly dolomite. The nonstratal dolomite, medium to coarsely crystalline and brightly luminescent, is characterized by high {sup 87}Sr/{sup 86}Sr ratios values, and Fe and Mn concentrations, relative to all Arbuckle carbonates. Such compositions suggest that this type of dolomite probably originated from fluids that were derived from the adjacent basin(s) during late Paleozoic time.

  10. Tsunami vulnerability of buildings and people in South Java - field observations after the July 2006 Java tsunami

    NASA Astrophysics Data System (ADS)

    Reese, S.; Cousins, W. J.; Power, W. L.; Palmer, N. G.; Tejakusuma, I. G.; Nugrahadi, S.

    2007-10-01

    A team of scientists from New Zealand and Indonesia undertook a reconnaissance mission to the South Java area affected by the tsunami of 17 July 2006. The team used GPS-based surveying equipment to measure ground profiles and inundation depths along 17 transects across affected areas near the port city of Cilacap and the resort town of Pangandaran. The purpose of the work was to acquire data for calibration of models used to estimate tsunami inundations, casualty rates and damage levels. Additional information was gathered from interviews with eyewitnesses. The degree of damage observed was diverse, being primarily dependant on water depth and the building construction type. Water depths were typically 2 to 4 m where housing was seriously damaged. Damage levels ranged from total for older brick houses, to about 50% for newer buildings with rudimentary reinforced-concrete beams and columns, to 5-20% for engineered residential houses and multi-storey hotels with heavier RC columns. "Punchout" of weak brick walls was widespread. Despite various natural warning signs very few people were alerted to the impending tsunami. Hence, the death toll was significant, with average death and injury rates both being about 10% of the people exposed, for water depths of about 3 m.