The All-Wavelength Extended Groth Strip International Survey (AEGIS) Data Sets

Davis, Marc; Guhathakurta, Puragra; Konidaris, Nicholas P.; Newman, Jeffrey A.; Ashby, M. L. N.; Biggs, A. D.; Barmby, P.; Bundy, Kevin; Chapman, Scott; Coil, Alison L.; Conselice, Christopher J.; Cooper, Michael C.; Croton, Darren J.; Eisenhardt, Peter; Ellis, Richard S.; Faber, S. M.; Fang, Taotao; Fazio, G. G.; Georgakakis, A.; Gerke, Brian F.; Goss, W. M.; Gwyn, Stephen; Harker, Justin; Hopkins, A. M.; Huang, Jia-Sheng; Ivison, R. J.; Kassin, Susan; Kirby, Evan N.; Koekemoer, Anton M.; Koo, David C.; Laird, E. S.; Floc’h, E. Le; Lin, Lihwai; Lotz, Jennifer M.; Marshall, Phil; Martin, D. Christopher; Metevier, A. J.; Moustakas, Leonidas A.; Nandra, K.; Noeske, K. G.; Papovich, Casey; Phillips, Andrew C.; Rich, R. Michael; Rieke, G. H.; Rigopoulou, D.; Salim, Samir; Schiminovich, David; Simard, Luc; Smail, Ian; Small, Todd; Weiner, Benjamin J.; Willmer, Christopher N. A.; Willner, S. P.; Wilson, Gillian; Wright, E. L.; Yan, Renbin

doi:10.1086/517931

Cited by 513 publications

(302 citation statements)

References 60 publications

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“…The galaxy EGSY8p7 was detected in the Extended Groth Strip (EGS; Davis et al 2007) from deep ( 27.0  ) multi-band images in the CANDELS survey and first reported as one of four unusually bright (H 25.5 160 < ) candidate z 7 > galaxies by RB15. One of these, EGS-zs8-1, with z 7.92 0.36 phot =  was spectroscopically confirmed at z = 7.73 by O15.…”

Section: Datamentioning

confidence: 99%

Ly α EMISSION FROM A LUMINOUS z = 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION

Zitrin

Labbé

Belli

et al. 2015

ApJ

278

333

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We report the discovery of Lyman-alpha emission (Lyα) in the bright galaxy EGSY-2008532660 (hereafter EGSY8p7) , in good agreement with the photometric estimate. The line was detected independently on two nights using different slit orientations and its detection significance is 7.5s. An overlapping skyline contributes significantly to the uncertainty on the total line flux, although the significance of the detected line is robust to a variety of skyline-masking procedures. By direct addition and a Gaussian fit, we estimate a 95% confidence range of 1.0-2.5 × 10 −17 erg s −1 cm −2 , corresponding to a rest-frame equivalent width of 17-42 Å. EGSY8p7 is the most distant spectroscopically confirmed galaxy to date, and the third luminous source in the EGS field beyond z 7.5 phot  with detectable Lyα emission, viewed at a time when the intergalactic medium is believed to be fairly neutral. Although the reionization process was probably patchy, we discuss whether luminous sources with prominent IRAC color excesses may harbor harder ionizing spectra than the dominant fainter population, thereby creating earlier ionized bubbles. Further spectroscopic follow-up of such bright sources promises important insights into the early formation of galaxies.

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Section: Datamentioning

confidence: 99%

Ly α EMISSION FROM A LUMINOUS z = 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION

Zitrin

Labbé

Belli

et al. 2015

ApJ

278

333

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“…X-ray AGNs are identified using deep Chandra data (Laird et al 2009) obtained as part of the AEGIS survey of the EGS (Davis et al 2007). This data set consists of eight Chandra ACIS-I pointings, each with a total integration time of about 200 ks split in at least three shorter exposures obtained at different epochs.…”

Section: Chandra Imagingmentioning

confidence: 99%

AEGIS: THE CLUSTERING OF X-RAY ACTIVE GALACTIC NUCLEUS RELATIVE TO GALAXIES ATz∼ 1

Coil

Georgakakis

Newman

et al. 2009

ApJ

152

252

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We measure the clustering of nonquasar X-ray active galactic nucleus (AGN) at z = 0.7-1.4 in the AEGIS field. Using the cross-correlation of 113 Chandra-selected AGN, with a median log L X = 42.8 erg s −1 , with ∼5000 DEEP2 galaxies, we find that the X-ray AGNs are fitted by a power law with a clustering scale length of r 0 = 5.95 ± 0.90 h −1 Mpc and slope γ = 1.66 ± 0.22. X-ray AGNs have a similar clustering amplitude as red, quiescent and "green" transition galaxies at z ∼ 1 and are significantly more clustered than blue, starforming galaxies. The X-ray AGN clustering strength is primarily determined by the host galaxy color; AGNs in red host galaxies are significantly more clustered than AGNs in blue host galaxies, with a relative bias that is similar to that of red to blue DEEP2 galaxies. We detect no dependence of clustering on optical brightness, X-ray luminosity, or hardness ratio within the ranges probed here. We find evidence for galaxies hosting X-ray AGN to be more clustered than a sample of galaxies with matching joint optical color and magnitude distributions. This implies that galaxies hosting X-ray AGN are more likely to reside in groups and more massive dark matter halos than galaxies of the same color and luminosity without an X-ray AGN. In comparison to optically selected quasars in the DEEP2 fields, we find that X-ray AGNs at z ∼ 1 are more clustered than optically selected quasars (with a 2.6σ significance) and therefore may reside in more massive dark matter halos. Our results are consistent with galaxies undergoing a quasar phase while in the blue cloud before settling on the red sequence with a lower-luminosity X-ray AGN, if they are similar objects at different evolutionary stages.

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“…The modular approach to pipelining combined with the common data model makes the general optical image processing pipeline implemented in the Astro-WISE information system reusable for a vast number of instruments 4 . The ability to use the same module to process the data from different instruments is due to the fact that all instrument-dependent parameters are grouped in special classes and instrument-dependent processing is done on the calibration level.…”

Section: Reusability Of the Pipelinementioning

confidence: 99%

“…Box 800, 9700 AV Groningen, The Netherlands distribution of dark matter via galaxy weak lensing, correlations in galaxy and QSO distributions and growth of large-scale structures. Complex relationships such as evolution of galaxies and their environment and nuclear activity require combined analysis from radio to X-rays (GAMA [10], AEGIS [4], COS-MOS [11], Coma Legacy Survey [3], ATLAS3D [2], GOODS [5], HUDF [12]). The challenge for any information system hosting these datasets is no longer archiving of data products, but providing abilities to perform data mining and data reprocessing on a massive scale.…”

Section: Introductionmentioning

confidence: 99%

The data zoo in Astro-WISE

2012

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In this paper we describe the way the Astro-WISE information system (or simply Astro-WISE) supports the data from a wide range of instruments and combines multiple surveys and their catalogues. Astro-WISE allows ingesting of data from any optical instrument, survey or catalogue, processing of this data to create new catalogues and bringing in data from different surveys into a single catalogue, keeping all dependencies back to the original data. Full data lineage is kept on each step of compiling a new catalogue with an ability to add a new data source recursively. With these features, Astro-WISE allows not only combining and retrieving data from multiple surveys, but performing scientific data reduction and data mining down to the rawest data in the data processing chain within a single environment.

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The All-Wavelength Extended Groth Strip International Survey (AEGIS) Data Sets

Cited by 513 publications

References 60 publications

Ly α EMISSION FROM A LUMINOUS z = 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION

Ly α EMISSION FROM A LUMINOUS z = 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION

AEGIS: THE CLUSTERING OF X-RAY ACTIVE GALACTIC NUCLEUS RELATIVE TO GALAXIES ATz∼ 1

The data zoo in Astro-WISE

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