The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging

Giavalisco, Mauro; Ferguson, Henry C.; Koekemoer, Anton M.; Dickinson, Mark; Alexander, D. M.; Bauer, F. E.; Bergeron, J.; Biagetti, C.; Brandt, W. N.; Casertano, Stefano; Césarsky, C. J.; Chatzichristou, E.; Conselice, Christopher J.; Cristiani, S.; Costa, L. N. da; Dahlén, T.; Mello, Duília de; Eisenhardt, P.; Erben, T.; Fall, S. Michael; Fassnacht, C. D.; Fosbury, R. A. E.; Fruchter, A. S.; Gardner, Jonathan P.; Grogin, Norman A.; Hook, R. N.; Hornschemeier, A. E.; Idzi, R.; Jogee, Shardha; Kretchmer, C.; Laidler, V. G.; Lee, K. S.; Livio, Mario; Lucas, Ray A.; Madau, Piero; Mobasher, Bahram; Moustakas, Leonidas A.; Nonino, M.; Padovani, P.; Papovich, C.; Park, Y.; Ravindranath, Swara; Renzini, A.; Richardson, Marin; Riess, Adam G.; Rosati, P.; Schirmer, M.; Schreier, E.; Somerville, Rachel S.; Spinrad, Hyron; Stern, Daniel; Stiavelli, M.; Strolger, L.; Urry, C. Megan; Vandame, B.; Williams, Robert E.; Wolf, Christian

doi:10.1086/379232

Cited by 1,412 publications

(806 citation statements)

References 30 publications

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“…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. For example, the overscan correction method used to normalize bias levels can be done in a number of different ways 5 and are specified by a single processing parameter. This processing parameter is saved in the processing parameters of the image object to which it is applied.…”

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%

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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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Section: Reusability Of the Pipelinementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The data zoo in Astro-WISE

2012

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“…The announcement in spring 2000 of the first Spitzer Legacy opportunity led to the Great Observatories Origins Deep Survey (GOODS), to date the deepest wide-area multiwavelength survey carried out with Spitzer, Hubble, and Chandra (Dickinson et al 2003;Giavalisco et al 2004). By targeting the Spitzer Legacy, and later the Hubble Treasury, observations on the pre-existing Chandra deep fields, we leveraged substantial investments of observing time, probed AGN demographics at the peak of quasar activity The GOODS data are deep enough to detect AGN to very high redshift (z > ∼ 6), and the volume sampled ensures sizable AGN samples out to z ∼ 3.…”

Section: Deep Multiwavelength Surveysmentioning

confidence: 99%

Supermassive black holes in deep multiwavelength surveys

Urry¹,

Treister²

2011

Black Holes

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In recent years deep X-ray and infrared surveys have provided an efficient way to find accreting supermassive black holes, otherwise known as active galactic nuclei (AGN), in the young universe. Such surveys can, unlike optical surveys, find AGN obscured by high column densities of gas and dust. In those cases, deep optical data show only the host galaxy, which can then be studied in greater detail than in unobscured AGN. Some years ago the hard spectrum of the Xray "background" suggested that most AGN were obscured. Now GOODS, MUSYC, COSMOS and other surveys have confirmed this picture and given important quantitative constraints on AGN demographics. Specifically, we show that most AGN are obscured at all redshifts and the amount of obscuration depends on both luminosity and redshift, at least out to redshift z ∼ 2, the epoch of substantial black holes and galaxy growth. Larger-area deep infrared and hard X-ray surveys will be needed to reach higher redshifts and to probe fully the co-evolution of galaxies and black holes. Cosmic Growth of Black Holes and GalaxiesAbundant evidence indicates that the growth of a supermassive black hole is closely tied to the formation and evolution of the surrounding galaxy. The energy released from accretion onto the black hole affects star formation in the galaxy, probably limiting growth at the high-and low-mass ends, and of course the distribution and angular momentum of matter in the galaxy governs the amount of matter accumulated by the black hole (Silk & Rees 1998;King 2005;Rovilos et al. 2007). Emergent energy from accretion is also a factor in understanding ionization and radiation backgrounds (Hasinger 2000;Lawrence 2001). Understanding the growth history of these black holes is therefore critical to understanding the global evolution of structure in the Universe.Yet the demographics of supermassive black holes remain elusive. The largest samples of quasars and Active Galactic Nuclei (AGN), by which we mean supermassive black holes in a high accretion-rate phase †, have been found through optical selection (e.g., the Sloan Digital Sky Survey quasar sample; Schneider et al. 2002Schneider et al. , 2007, but, at least locally, these are not representative of the larger AGN population. Instead we need surveys less biased against obscured AGN.There are three reasons to suspect that most AGN are obscured by large column densities of gas and dust. First, a large body of evidence suggests that local AGN have geometries that are not spherically symmetric, and that different aspect angles present markedly different observed characteristics; this is referred to as AGN unification (Antonucci 1993;Urry & Padovani 1995). Second, AGN are more common at high redshift (z ∼ 2 − 3), where the average star formation rate is higher and thus it is even more likely that gas and dust surround the galaxy nucleus than at z ∼ 0. Third, and most important, obscured AGN are required to explain the shape of the X-ray "background" radiation.The X-ray "background" is actually the superposition of ind...

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“…The Great Observatories Origins Deep Survey (GOODS) [1] was designed to unite the deepest observations from space-and ground-based facilities in two carefully selected fields, the Hubble Deep Field-North (HDF-N) and Chandra Deep Field-South (CDFS). With the deepest X-ray observations, using the Chandra X-Ray Observatory (CXO) and XMM-Newton, these areas have also been observed with the Spitzer Space Telescope at infrared wavelengths as part of several Legacy programmes.…”

Section: Introductionmentioning

confidence: 99%

“…Revealing the activity in a galaxy (either from star-formation or an AGN), radio emission is essentially unaffected by dust obscuration, which severely affects optical selection criteria [2], and is known to be an important source of bias at high redshift [3]. Radio emission is also a powerful probe of the highest redshift Universe: the most luminous radio galaxies, powered by an AGN, can in principle already be detected to the epoch of reionization with the current deep radio surveys 1 . Looking for such High Redshift Radio Galaxies (HzRGs) becomes even more attractive as they are associated with the most massive systems and are considered to identify the location of proto-cluster environments [5].…”

Section: Introductionmentioning

confidence: 99%

A Somewhat Lower Frequency View of the Chandra Deep Field South

Afonso¹

2010

Proceedings of Panoramic Radio Astronomy: Wide-Field 1-2 GHz Research on Galaxy Evolution — PoS(PRA2009)

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The Chandra Deep Field South (CDFS) is one of the most extensively observed regions of the sky, with some of the deepest multi-wavelength coverage ever: Chandra and XMM-Newton Xray observations, multi-band HST-ACS optical imaging and mid-to far-IR Spitzer observations, extensive deep ground-based imaging and spectroscopy with 8-m class telescopes such as the VLT and, finally, deep 1.4-GHz radio observations with the ATCA and the VLA. We are currently using the GMRT to image this field at 325 MHz to very deep levels, which will allow us a first detailed glimpse of the nature of Ultra Steep Spectrum sources at the faintest radio flux levels.

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The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging

Cited by 1,412 publications

References 30 publications

The data zoo in Astro-WISE

The data zoo in Astro-WISE

Supermassive black holes in deep multiwavelength surveys

A Somewhat Lower Frequency View of the Chandra Deep Field South

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