The K20 survey - III. Photometric and spectroscopic properties of the sample

By A. Cimatti, M. Mignoli, E. Daddi, L. Pozzetti, A. Fontana, P. Saracco, F. Poli, A. Renzini, G. Zamorani, T. Broadhurst and 5 more. 2002

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The K20 survey is an ESO VLT optical and near-infrared spectroscopic survey aimed at obtaining spectral infor- mation and redshifts of a complete sample of about 550 objects to Ks 20:0 over two independent fields with a total area of 52 arcmin 2 . In this paper we discuss the scientific motivation of such a survey, we describe the photometric and spectroscopic properties of the sample, and we release the Ks-band photometric catalog. Extensive simulations showed that the sample is photometrically highly complete to Ks= 20. The observed galaxy counts and the R Ks color distribution are consistent with literature results. We observed spectroscopically 94% of the sample, reaching a spectroscopic redshift identification complete- ness of 92% to Ks 20:0 for the observed targets, and of 87% for the whole sample (i.e. counting also the unobserved targets). Deep spectroscopy was complemented with multi-band deep imaging in order to derive tested and reliable photometric red- shifts for the galaxies lacking spectroscopic redshifts. The results show a very good agreement between the spectroscopic and the photometric redshifts with = 0:01 and with a dispersion ofz= 0:09. Using both the spectroscopic and the photometric redshifts, we reached an overall redshift completeness of about 98%. The size of the sample, the redshift complete- ness, the availability of high quality photometric redshifts and multicolor spectral energy distributions make the K20 survey database one of the most complete samples available to date for constraining the currently competing scenarios of galaxy formation and for a variety of other galaxy evolution studies.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

DEEP U BAND AND R IMAGING OF GOODS-SOUTH: OBSERVATIONS, DATA REDUCTION AND FIRST RESULTS, (2009, methodology): “Blue squares show foreground galaxies at z 1.8 from the FORS2 GOODS (Vanzella et al. 2008), K20 (Cimatti et al. 2002) spectroscopic campaigns, and from the VIMOS Medium Resolution GOODS spectroscopic campaign (Popesso et al. 2009).”
The VIMOS VLT Deep Survey. Evolution of the luminosity functions by galaxy type up to z = 1.5 from first epoch data (2005, unknown): “Other results suggest a strong number density evolution of early type galaxies (Bell et al. 2004; Faber et al. 2006); conversely, in the K20 survey (Cimatti et al. 2002), Pozzetti et al. (2003) found that red and early type galaxies dominate the bright end of the LF and that their number density…”
Galaxies in the Hubble Ultra Deep Field. I. Detection, Multiband Photometry, Photometric Redshifts, and Morphology (2006, unknown): “Previous studies have identified a group of galaxies at z = 0.67 and a (denser) cluster of galaxies at z = 0.73 in the wider CDF-S field (Cimatti et al. 2002, Gilli et al. 2003, Croom et al. 2001, VVDS, FORS2).”
Near-Infrared Bright Galaxies at z ≃ 2. Entering the Spheroid Formation Epoch? (2003, background): “The agreement between the observed redshift distribution atz> 1.7 and the PLE model described in Cimatti et al. (2002c) is therefore likely to be just chance.”
Passively Evolving Early-Type Galaxies at 1.4 ≲ z ≲ 2.5 in the Hubble Ultra Deep Field (2005, unknown): “This object is also part of the K20 survey (Cimatti et al. 2002b) with a measured redshift of z ¼ 1:553.”
The SWIRE-VVDS-CFHTLS surveys: stellar mass assembly over the last 10 Gyr. Evidence for a major build up of the red sequence between z = 2 and z = 1 (2007, background): “An important population of EROs at z ≥ 1 has been discovered (K20 survey: Cimatti et al. 2002), with roughly half of them being old stellar systems (Cimatti et al. 2004).”
Star Formation and Extinction in Redshift z~2 Galaxies: Inferences from Spitzer MIPS Observations (2006, result): “GalaxieswithKs < 20 (e.g., K20 samples; Cimatti et al. 2002a, 2002b) have hLIRi (1 2) ; 1012 L , similar to the value found byDaddi et al. (2005) forKs < 20 BzKselected galaxies in the GOODS-N field.”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, methodology): “…by non-spheroidal galaxies is larger at higher redshifts, amounting to 30% at z ∼ 0.75 (Bell et al. 2004a, Weiner et al. 2005), and may increase beyond that (Cimatti et al. 2002a, 2003; Yan & Thompson 2003; Gilbank et al. 2003; Moustakas et al. 2004).”
The Great Observatories Origins Deep Survey: Initial Results from Optical and Near-Infrared Imaging (2003, methodology): “They were tested against spectroscopic redshifts from the K20 survey (Cimatti et al. 2002), kindly provided by A. Cimatti, and also against redshifts measured with VLT FORS2 for the GOODS program.”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “Such observations indicate that the number of bright red galaxies at zk 1 may be larger than earlier predictions based on SAM (e.g., Cimatti et al. 2002a; Calura et al. 2004; Pozzetti et al. 2003; Somerville et al. 2004; Glazebrook et al. 2004).”
A New Photometric Technique for the Joint Selection of Star-forming and Passive Galaxies at 1.4 ≲ z ≲ 2.5 (2004, methodology): “…et al. 2002; Champan et al. 2003), observing the emission at X-ray or radio wavelengths that are not extincted by dust (e.g., Norman et al. 2004; Haarsma et al. 2000), and selecting very red objects in near-infrared samples that are less affected by dust extinction (Cimatti et al. 2002a, 2003).”
A Census of Optical and Near-Infrared Selected Star-forming and Passively Evolving Galaxies at Redshift z ~ 2 (2005, background): “The K20 and FIRES selection criteria were developed to take advantage of the sensitivity of rest-frame optical light and color to stellar mass and the strength of the Balmer break, respectively, for z ∼ 2 galaxies (e.g., Cimatti et al. 2002a; Franx et al. 2003).”
THE NEWFIRM MEDIUM-BAND SURVEY: PHOTOMETRIC CATALOGS, REDSHIFTS, AND THE BIMODAL COLOR DISTRIBUTION OF GALAXIES OUT TO z ∼ 3 (2011, background): “…must be made for studies of complete samples of high redshift galaxies, where one can either work with small, bright spectroscopic samples (Cimatti et al. 2002; Kriek et al. 2008b), or use large samples that rely on less accurate broadband photometric redshifts (e.g. Dickinson et al.…”
Mass downsizing and ``top-down'' assembly of early-type galaxies (2006, methodology): “…K-band selected surveys uncovered a substantial populationof old (1-4 Gyr), massive (M > 1011M⊙), passively evolving E/S0 galaxies at 1< z < 2 (e.g. Cimatti et al. 2002a, 2004; McCarthy et al. 2004; Glazebrook et al. 2004: Daddi et al. 2005a; Saracco et al. 2005), and showed that the…”
The VIMOS-VLT deep survey - Evolution of the galaxy luminosity function up to z = 2 in first epoch data (2004, unknown): “Data from two additional fields (the CDFS and the field around the QSO 0055-269), on which the K20 spectroscopic survey is based (Cimatti et al. 2002), have been added to constrain the bright-end of the LF.”
GMASS ultradeep spectroscopy of galaxies at $z$ ~ 2 - II. Superdense passive galaxies: how did they form and evolve? (2008, methodology): “We also explored how the picture changes at lower redshifts using the small, but highly complete spectroscopic sample of K20 Survey (Cimatti et al. 2002b) ETGs at 0.8 < z < 1.3 for which also the absorption line velocity dispersion (σV) is available.”
The Mass Assembly Histories of Galaxies of Various Morphologies in the GOODS Fields (2005, background): “The K20 sample (Cimatti et al. 2002) has good spectroscopic coverage (92”
AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: THE REDSHIFT DISTRIBUTION AND EVOLUTION OF SUBMILLIMETER GALAXIES (2013, background): “The spectroscopic sample is collated from a wide range of sources (Cristiani et al. 2000; Croom et al. 2001; Cimatti et al. 2002; Teplitz et al. 2003; Bunker et al. 2003; Le Fèvre et al. 2004; Zheng et al. 2004; Szokoly et al. 2004; Strolger et al. 2004; Stanway et al. 2004; van der Wel et al.…”
The Build-up of the Colour-Magnitude Relation (2005, background): “Recent near-IR studies such as the K20 Survey (Cimatti et al. 2002a,b,c; Daddi et al. 2002; Fontana 2004), FIRES (Franx et al. 2003; van Dokkum et al. 2003; Rudnick et al. 2003; Schreiber et al. 2004) and part of GOODS (Giavalisco et al. 2004; Daddi et al. 2004; Moustakas et al. 2004; Somerville et ”
The K20 survey. VI. The distribution of the stellar masses in galaxies up to z 2 (2004, methodology): “In the K20 dataset, the evolution of bright, massive galaxies has been investigated up to z ≃ 2 through the study of the K–limited redshift distribution (Cimatti et al. 2002b) and the near–IR luminosity functions (Pozzetti et al. 2003).”