The FLAMINGOS Extragalactic Survey

Elston, R.; Gonzalez, Anthony H.; McKenzie, Eric; Brodwin, M.; Brown, M. J. I.; Cardona, G.; Dey, Arjun; Dickinson, Mark; Eisenhardt, Peter; Jannuzi, Buell T.; Lin, Yen-Ting; Mohr, J. J.; Raines, S. N.; Stanford, S. A.; Stern, Daniel

doi:10.1086/499423

Cited by 125 publications

(170 citation statements)

References 66 publications

(67 reference statements)

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“…For the Bootes field, we compiled multiwavelength catalogues from the NOAO Deep-Wide Field Survey (Jannuzi & Dey 1999) DR3, SDSS DR9 (Ahn et al 2012), GALEX GR7 3 , FLAMINGOS Extragalactic Survey (Elston et al 2006), and the Spitzer Deep-Wide Field Survey (Ashby et al 2009). We use the LR method to match our X-ray catalogues to the appropriate selection band for each of these surveys, assigning secure matches from the surveys in the order of priority indicated in the Hard (2-10 keV) Figure 1.…”

Section: Bootesmentioning

confidence: 99%

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Aird

Coil

Georgakakis

et al. 2015

Monthly Notices of the Royal Astronomical Society

358

559

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We present new measurements of the evolution of the X-ray luminosity functions (XLFs) of unabsorbed and absorbed Active Galactic Nuclei (AGNs) out to z ∼ 5. We construct samples containing 2957 sources detected at hard (2-7 keV) X-ray energies and 4351 sources detected at soft (0.5-2 keV) energies from a compilation of Chandra surveys supplemented by wide-area surveys from ASCA and ROSAT. We consider the hard and soft X-ray samples separately and find that the XLF based on either (initially neglecting absorption effects) is best described by a new flexible model parametrization where the break luminosity, normalization and faint-end slope all evolve with redshift. We then incorporate absorption effects, separately modelling the evolution of the XLFs of unabsorbed (20 < log N H < 22) and absorbed (22 < log N H < 24) AGNs, seeking a model that can reconcile both the hard-and soft-band samples. We find that the absorbed AGN XLF has a lower break luminosity, a higher normalization, and a steeper faint-end slope than the unabsorbed AGN XLF out to z ∼ 2. Hence, absorbed AGNs dominate at low luminosities, with the absorbed fraction falling rapidly as luminosity increases. Both XLFs undergo strong luminosity evolution which shifts the transition in the absorbed fraction to higher luminosities at higher redshifts. The evolution in the shape of the total XLF is primarily driven by the changing mix of unabsorbed and absorbed populations.

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Section: Bootesmentioning

confidence: 99%

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Aird

Coil

Georgakakis

et al. 2015

Monthly Notices of the Royal Astronomical Society

358

559

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“…Using K-band has an advantage over (also available) shorter wavelength bands as this band suffers the least from extinction. We have identified possible optical counterparts of the radio sources using the FLAMEX K S -band catalogue (Elston et al 2006). This survey covers 7.1 square degrees within the Boötes field.…”

Section: Identification Fraction Of Radio Sources Versus Spectral Indexmentioning

confidence: 99%

Deep low-frequency radio observations of the NOAO Boötes field

Intema

Weeren

Röttgering

et al. 2011

A&A

103

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In this article we present deep, high-resolution radio interferometric observations at 153 MHz to complement the extensively studied NOAO Boötes field. We provide a description of the observations, data reduction and source catalog construction. From our single pointing GMRT observation of ∼12 h we obtain a high-resolution (26 × 22 ) image of ∼11.3 square degrees, fully covering the Boötes field region and beyond. The image has a central noise level of ∼1.0 mJy beam −1 , which rises to 2.0-2.5 mJy beam −1 at the field edge, placing it amongst the deepest ∼150 MHz surveys to date. The catalog of 598 extracted sources is estimated to be ∼92 percent complete for >10 mJy sources, while the estimated contamination with false detections is <1 percent. The low rms position uncertainty of 1.24 facilitates accurate matching against catalogs at optical, infrared and other wavelengths. Differential source counts are determined down to 10 mJy. There is no evidence for flattening of the counts towards lower flux densities as observed in deep radio surveys at higher frequencies, suggesting that our catalog is dominated by the classical radio-loud AGN population that explains the counts at higher flux densities. Combination with available deep 1.4 GHz observations yields an accurate determination of spectral indices for 417 sources down to the lowest 153 MHz flux densities, of which 16 have ultra-steep spectra with spectral indices below −1.3. We confirm that flattening of the median spectral index towards low flux densities also occurs at this frequency. The detection fraction of the radio sources in NIR K S -band is found to drop with radio spectral index, which is in agreement with the known correlation between spectral index and redshift for brighter radio sources.

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“…Subsequent spectroscopic observations of cluster members confirmed 12 of these candidates with further observations to follow. They determine initial cluster redshift estimates using photometric redshifts based on deep optical data from the NOAO Deep Wide-Field Survey (NDWFS; Jannuzi et al 2004), NIR data from FLAMEX (Elston et al 2006) and IRAC Shallow Survey [3.6] and [4.5] imaging. With this combination they successfully identify clusters up to redshifts of z ∼ 1.5, with the success of the identification of a z = 1.41 cluster (Stanford et al 2005), at the time the highest redshift spectroscopically confirmed galaxy cluster.…”

Section: Introductionmentioning

confidence: 99%

The WIRCAM Deep Infrared Cluster Survey

Bielby

Finoguenov

Tanaka

et al. 2010

A&A

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Aims. We use a combination of CFHTLS deep optical data, WIRcam Deep Survey (WIRDS) near-infrared data and XMM-Newton survey data to identify z > ∼ 1.1 clusters in the CFHTLS D1 and D4 fields. Counterparts to such clusters can not be identified without deep near-infrared data and as such the total of ≈1 deg 2 of J, H and K s band imaging provided by WIRDS is an indispensable tool in such work. Methods. Using public XMM X-ray data, we identify extended X-ray sources in the two fields. The resulting catalogue of extended X-ray sources was then analyzed for optical/near-infrared counterparts, using a red-sequence algorithm applied to the deep optical and near-infrared data. Redshifts of candidate groups and clusters were estimated using the median photometric redshifts of detected counterparts and where available these were combined with spectroscopic data (from VVDS deep and ultra-deep and using AAT AAOmega data). Additionally, we surveyed X-ray point sources for potential group systems at the limit of our detection range in the X-ray data. A catalogue of z > 1.1 cluster candidates in the two fields has been compiled and cluster masses, radii and temperatures have been estimated using the scaling relations. Results. The catalogue of group and cluster candidates consists of 15 z > ∼ 1.1 objects. We find several massive clusters (M > ∼ 10 14 M ) and a number of lower mass clusters/groups. Three of the detections are previously published extended X-ray sources. Of note is JKSC 041 (previously detected via Chandra X-ray data and reported as a z = 1.9 cluster based on UKIDSS infrared imaging) for which we identify a number of structures at redshifts of z = 0.8, z = 0.96, z = 1.13 and z = 1.49 (but see no evidence of a structure at z = 1.9). We also make an independent detection of the massive cluster, XMMXCS J2215.9-1738, for which we estimate a redshift of z = 1.37 (compared to the spectroscopically confirmed redshift of z = 1.45). We use the z > ∼ 1.1 catalogue to compare the cluster number counts in these fields with models based on WMAP 7-year cosmology and find that the models slightly over-predict the observations, whilst at z > 1.5 we do not detect any clusters. We note that cluster number counts at z > ∼ 1.1 are highly sensitive to the cosmological model, however a significant reduction in present statistical (due to available survey area) and systematic (due to cluster scaling relations) uncertainties is required in order to confidently constrain cosmological parameters using cluster number counts at high redshift.

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The FLAMINGOS Extragalactic Survey

Cited by 125 publications

References 66 publications

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z∼ 5

Deep low-frequency radio observations of the NOAO Boötes field

The WIRCAM Deep Infrared Cluster Survey

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