Spectroscopic Identification of Massive Galaxies at
                    <i>z</i>
                    ~ 2.3 with Strongly Suppressed Star Formation

Kriek, Mariska; Dokkum, Pieter van; Franx, Marijn; Quadri, Ryan; Gawiser, Eric; Herrera, David; Illingworth, G. D.; Labbé, Ivo; Lira, P.; Marchesini, Danilo; Rix, Hans─Walter; Rudnick, Gregory; Taylor, Edward N.; Toft, Sune; Urry, C. Megan; Wuyts, Stijn

doi:10.1086/508371

Cited by 228 publications

(315 citation statements)

References 38 publications

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“…In our data, very red objects having J − K s > 1.34 are found in the K s range between 21 and 24.5 peaking at K s ∼ 22.7. However, we note that to date there are very few spectroscopic redshifts for distant red galaxies in this field (see, e.g., Kriek et al 2006).…”

Section: Color Distributionsmentioning

confidence: 99%

The Great Observatories Origins Deep Survey

Retzlaff¹,

Rosati²,

Dickinson³

et al. 2010

A&A

135

125

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Aims. We present the final public data release of the VLT/ISAAC near-infrared imaging survey in the GOODS-South field. The survey covers an area of 172.5, 159.6 and 173.1 arcmin 2 in the J, H, and K s bands, respectively. For point sources total limiting magnitudes of J = 25.0, H = 24.5, and K s = 24.4 (5σ, AB) are reached within 75% of the survey area. Thus these observations are significantly deeper than the previous EIS Deep Public Survey which covers the same region. The image quality is characterized by a point spread function ranging between 0.34 and 0.65 FWHM. The images are registered to a common astrometric grid defined by the GSC 2 with an accuracy of ∼0.06 RMS over the whole field. The overall photometric accuracy, including all systematic effects, adds up to 0.05 mag. The data are publicly available from the ESO science archive facility. Methods. We describe the data reduction, the calibration, and the quality control process. The final data set is characterized in terms of astrometric and photometric properties, including the PSF and the curve of growth. We establish an empirical model for the sky background noise in order to quantify the variation of limiting depth and statistical photometric errors over the survey area. We define a catalog of K s -selected sources which contains JHK s photometry for 7079 objects. Differential aperture corrections were applied to the color measurements in order to avoid possible biases as a result of the variation of the PSF. We briefly discuss the resulting color distributions in the context of available redshift data. Furthermore, we estimate the completeness fraction and relative contamination due to spurious detections for source catalogs extracted from the survey data. For this purpose, an empirical study based on a deep K s image of the Hubble Ultra Deep Field is combined with extensive image simulations. Results. With respect to previous deep near-infrared surveys, the surface density of faint galaxies has been established with unprecedented accuracy by virtue of the unique combination of depth and area of this survey. We derived galaxy number counts over eight magnitudes in flux up to J = 25.25, H = 25.0, K s = 25.25 (in the AB system). Very similar faint-end logarithmic slopes between 0.24 and 0.27 mag −1 were measured in the three bands. We found no evidence for a significant change in the slope of the logarithmic galaxy number counts at the faint end.

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Section: Color Distributionsmentioning

confidence: 99%

The Great Observatories Origins Deep Survey

Retzlaff¹,

Rosati²,

Dickinson³

et al. 2010

A&A

135

125

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“…Four sources (W-57, W-67, W-108, and W-114) have spectroscopic redshifts assigned to their optical, infrared, or radio counterparts: Szokoly et al (2004), Kriek et al (2006), Norris et al (2006), Chapin et al (2010) respectively. The photometric redshifts in the area of the CDFS come from Luo et al (2010), where photometric redshifts are calculated for X-ray sources using up to 42 UV, optical, and infrared bands.…”

Section: Photometry and Redshiftsmentioning

confidence: 99%

X-ray observations of sub-mm LABOCA galaxies in the eCDFS

Georgantopoulos

Rovilos

Comastri

2010

A&A

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We explore the X-ray properties of the 126 sub-mm galaxies (SMGs) of the LABOCA survey in the CDFS and the eCDFS regions. SMGs are believed to experience massive episodes of star formation. Our goal is to examine whether star formation coexists with AGN activity, determine the fraction of highly obscured AGN, and finally to obtain an idea of the dominant power mechanism in these sources. Using Spitzer and radio arcsecond positions for the SMGs, we find 14 sources with significant X-ray detections. For most of these there are only photometric redshifts available, with their median redshift at ∼2.3. Taking only the CDFS area into account that has the deepest X-ray observations, we estimate an X-ray AGN fraction of <26 ± 9% among SMGs. The X-ray spectral properties of the majority of the X-ray AGN that are associated with SMGs are consistent with high obscuration, >10 23 cm −2 , but there is no unambiguous evidence of Compton-thick sources. Detailed spectral energy distribution fittings show that the bulk of total IR luminosity originates in star forming processes, although a torus component is usually present. Finally, stacking analysis of the X-ray undetected SMGs reveals a signal in the soft (0.5-2 keV) and marginally in the hard (2-5 keV) X-ray bands. The hardness ratio of the stacked signal is relatively soft (−0.40 ± 0.10) corresponding to Γ ∼ 1.6. This argues against a high fraction of Compton-thick sources among the X-ray undetected SMGs.

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“…Nevertheless a significant population of massive galaxies has been found beyond z ∼ 1. Up to z 2.5, the most massive objects spectroscopically confirmed are similar to local early-type galaxies (ETGs): old (age of ∼1 Gyr), passively evolving, and of mass M > 10 11 M (Cimatti et al 2004;McCarthy et al 2004;Daddi et al 2005;Saracco et al 2005;Kriek et al 2006). At higher redshift the availability of multiwavelength data from deep surveys enabled searches for massive galaxy candidates to z 5−6.5.…”

Section: Introductionmentioning

confidence: 99%

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

Mancini

Matute

Cimatti

et al. 2009

A&A

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Aims. We constrain the space density and properties of massive galaxy candidates at redshifts of z ≥ 3.5 in the Great Observatories Origin Deep Survey North (GOODS-N) field. By selecting sources in the Spitzer + IRAC bands, a sample highly complete in stellarmass is assembled, including massive galaxies that are very faint in the optical/near-IR bands and would be missed by samples selected at shorter wavelengths. Methods. The z ≥ 3.5 sample was selected to m AB = 23 mag at 4.5 μm using photometric redshifts obtained by fitting the galaxies spectral energy distribution at optical, near-IR bands, and IRAC bands. We also require that the brightest band (in AB scale) in which candidates are detected is the IRAC 8.0 μm band to ensure that the near-IR 1.6 μm (rest-frame) peak is falling in or beyond this band. Results. We found 53 z ≥ 3.5 candidates, of masses in the range M ∼ 10 10 −10 11 M . At least ∼81% of these galaxies are missed by traditional Lyman Break selection methods based on ultraviolet light. Spitzer + MIPS emission is detected for 60% of the sample of z ≥ 3.5 galaxy candidates. Although in some cases this might suggest a residual contamination from lower redshift starforming galaxies or Active Galactic Nuclei, 37% of these objects are also detected in the sub-mm/mm bands in SCUBA, AzTEC, and MAMBO surveys, and have properties fully consistent with vigorous starburst galaxies at z ≥ 3.5. The comoving number density of galaxies with stellar masses of above 5 × 10 10 M (a reasonable stellar-mass completeness limit for our sample) is 2.6 × 10 −5 Mpc −3 (using the volume within 3.5 < z < 5), and the corresponding stellar mass density is ∼(2.9 ± 1.5) × 10 6 M Mpc −3 , or about 3% of the local density above the same stellar mass limit. For the subsample of MIPS-undetected galaxies, we measure a number density of ∼0.97 × 10 −5 Mpc −3 and a stellar mass density of ∼(1.15 ± 0.7) × 10 6 M Mpc −3 . Even in the unlikely case that these are all truly quiescent galaxies, this would imply an increase in the space density of passive galaxies by a factor of ∼15 between z ∼ 4 and z = 2, and by ∼100 to z = 0.

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Spectroscopic Identification of Massive Galaxies at z ~ 2.3 with Strongly Suppressed Star Formation

Cited by 228 publications

References 38 publications

The Great Observatories Origins Deep Survey

The Great Observatories Origins Deep Survey

X-ray observations of sub-mm LABOCA galaxies in the eCDFS

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

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