The K20 survey. V. The evolution of the near-IR Luminosity Function

By L. Pozzetti, A. Cimatti, G. Zamorani, E. Daddi, N. Menci, A. Fontana, A. Renzini, M. Mignoli, F. Poli, P. Saracco and 5 more. 2003

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We present the galaxy rest-frame near-IR Luminosity Function (LF) and its cosmic evolution to z 1:5 based on a spectroscopic survey of a magnitude limited sample of galaxies with Ks < 20 (the K20 survey, Cimatti et al. 2002b). The LFs have been derived in the rest-frame J and Ks bands. Their evolution is traced using three dierent redshift bins (zmean ' 0:5; 1; 1:5) and comparing them to the Local near-IR Luminosity Function. The luminosity functions at dierent redshifts are fairly well fitted by Schechter functions at z< 1:3. The faint-end of the LFs (L< L) is consistent with the local estimates, with no evidence for a change either in the slope or normalization up to z< 1:3. At higher redshift this part of the luminosity function is not well sampled by our data. Viceversa, the density of luminous galaxies ( MKs 5l ogh70< 25:5) is higher than locally at all redshifts and relatively constant or mildly increasing with redshift within our sample. The data are consistent with a mild luminosity evolutionboth in the J -a ndKs -band up toz' 1:5, with an amplitude of aboutMJ ' 0:69 0:12 and MK ' 0:54 0:12 at z 1. Pure density evolution is not consistent with the observed LF at z 1. Moreover, we find that red and early-type galaxies dominate the bright-end of the LF , and that their number density shows at most a small decrease (<30%) up to z' 1, thus suggesting that massive elliptical galaxies were already in place at z' 1a ndthey should have formed their stars and assembled their mass at higher redshift.There appears to be a correlation of the optical/near-IR colors with near-IR luminosities, the most luminous/massive galaxies being red/old, the low-luminous galaxies being instead dominated by blue young stellar populations. We also investigate the evolution of the near-IR comoving luminosity density to z' 1:5, finding a slow evolution with redshift ((z)=(z= 0)(1+z) () with(J)' 0:70 and(Ks)' 0:37). Finally, we compare the observed LFs with the predictions of a set of the most updated hierarchical merging models. Such a comparison shows that the current versions of hierarchical models overpredict significantly the density of low luminosity galaxies at z 1 and underpredict the density of luminous galaxies at z 1, whereas passive evolution models are more consistent with the data up to z 1:5. The GIF model (Kaufmann et al. 1999) shows a clear deficiency of red luminous galaxies at z 1 compared to our observations and predicts a decrease of luminous galaxies with redshift not observed in our sample.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/04558947da9119d858fd56ee95ed7972b442af81

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Citations in the corpus

Galaxies–intergalactic medium interaction calculation – I. Galaxy formation as a function of large-scale environment (2009, background): “Observations indicate that star formation in the most massive galaxies observed today essentially concluded at z ∼ 1 (e.g. Drory et al. 2003, 2005; Pozzetti et al. 2003; Fontana et al. 2004; Kodama et al. 2004), and that their SFRs were higher in the past than they are at present (e.g. Cowie et al.…”
Strong size evolution of the most massive galaxies since z~2 (2007, background): “This decline is moderate sincez∼1 and much stronger at even higher redshifts (Daddi, Cimatti & Renzini 2000; Pozzetti et al. 2003; Bell et al. 2004; Drory et al. 2004, 2005; Daddi et al. 2005; Saracco et al. 2005; Faber et al. 2005; Pozzetti et al. 2007).”
Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “…et al. (2004) and Balogh et al. (2004), (U − V) vs. MB (upper right; Cross et al. 2004; Giallongo et al. 2005; McIntosh et al. 2005a), (U − B) vs.MB (lower left; Willmer et al. 2005; Faber et al. 2005), and (R−K) vs. MK (lower right; Roche et al. 2002; Pozzetti et al. 2003; Fontana et al. 2004).”
Quasar Feedback: The Missing Link in Structure Formation (2004, methodology): “Here we restrict our attention to Ks-measurements as taken by Pozzetti et al. (2003), as such infrared measurements are most sensitive to the overall galaxy stellar masses rather than a combination of stellar masses and formation histories (e.g., Madau et al. 1998).”
A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts (2003, methodology): “Figure 11 compares the predicted rest-frame K-band luminosity function at z = 1.5 with the observational determination by Pozzetti et al. (2003), which, at the highest luminosities, is substantially above predictions of the models by Kauffmann et al. (1999), Cole et al. (2000), and Menci et al.…”
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).”
Can the faint submillimetre galaxies be explained in the Λ cold dark matter model (2005, methodology): “…recently, Granato et al. (2004) have developed a coupled model for the evolution of galactic spheroids and quasistellar objects (QSOs), which successfully reproduces the counts of SMGs and the evolution of the K-band luminosity function with redshift (e.g. Pozzetti et al. 2003; Drory et al. 2004).”
Breaking the hierarchy of galaxy formation (2005, methodology): “…in the CDM cosmology have consistently had difficulty in simultaneously accounting for the presentday galaxy luminosity function and for the number of apparently massive galaxies observed at redshifts z ∼ 1–2 (Drory et al. 2003, 2005; Pozzetti et al. 2003; Fontana et al. 2004; Kodama et al. 2004).”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, background): “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).”
The VIMOS VLT deep survey: the assembly history of the stellar mass in galaxies: from the young to the old universe (2007, unknown): “…is growing but still controversial evidence in near-IR (NIR) surveys that luminous and rather massive old galaxies were already quite common at z ∼ 1 (Pozzetti et al. 2003; Fontana et al. 2004; Saracco et al. 2004, 2005; Caputi et al. 2006a) and up to z ∼ 2 (Cimatti et al. 2004; Glazebrook et al.…”
The 2df SDSS LRG and QSO survey: evolution of the luminosity function of luminous red galaxies to z= 0.6 (2006, result): “This is consistent with earlier (but smaller in number) studies of high-redshift red (early-type) galaxies from the CFRS (Lilly et al. 1995; Schade et al. 1999), CNOC2 (Lin et al. 1999) and K20 (Pozzetti et al. 2003) surveys.”
The K20 survey. VII. The spectroscopic catalogue: spectral properties and evolution of the galaxy population ⋆, ⋆⋆ (2005, background): “…by different models of galaxy formation (Cimatti et al. 2002b, Paper IV), the evolution of the near-infrared luminosity density and luminosity (Pozzetti et al. 2003, Paper V), the X-ray and morphological properties of EROs (Brusa et al. 2002; Cimatti et al. 2003), the study of the large scale…”
Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation (2005, methodology): “The evolution of the luminosity function as a function of color since z ∼ 1 was also investigated by Pozzetti et al. (2003), who used the near-infrared-selected K20 survey of Cimatti et al. (2002b) and divided the sample using the color of Sa galaxies.”
The environmental dependence of the relations between stellar mass, structure, star formation and nuclear activity in galaxies (2004, background): “Studies of the evolution of the rest-frame near-IR luminosity function suggest that characteristic stellar masses of galaxies have evolved only weakly from z ∼ 1 to the present (e.g. Pozzetti et al 2003; Somerville et al 2003).”
A new measurement of the evolving near-infrared galaxy luminosity function out to z≃ 4: a continuing challenge to theoretical models of galaxy formation (2008, background): “…of the near-infrared LF with redshift, with the evolution being very slow from the local Universe up to z ∼ 0.5 and then progressively faster (Glazebrook et al. 1995; Bolzonella et al. 2002; Pozzetti et al. 2003; Dickinson et al. 2003; Drory et al. 2003; Caputi et al. 2006; Saracco et al. 2006).”
The VIMOS-VLT deep survey - Evolution of the galaxy luminosity function up to z = 2 in first epoch data (2004, unknown): “In the near-IR, Pozzetti et al. (2003) measure an evolution consistent with a mild luminosity evolution both in the J and K bands with ∆MJ ∼ −0.7 and ∆MK ∼ −0.5 at z ∼ 1.”
Intergalactic Photon Spectra from the Far-IR to the UV Lyman Limit for 0 < z < 6 and the Optical Depth of the Universe to High-Energy Gamma Rays (2005, background): “The assumptions made by SS98 for SEDs at various redshifts are now supported by various observational results on galaxy evolution in the near IR-UV (Cowie et al. 1996, Pozzetti et al. 2003, Malkan, Webb & Konopacky 2003, Havens et al. 2004, Yee et al. 2005).”
Near-Infrared Bright Galaxies at z ≃ 2. Entering the Spheroid Formation Epoch? (2003, result): “Recent results from the K20 project (Cimatti et al. 2002a,b,c; Daddi et al. 2002; Pozzetti et al. 2003) appear to be at variance with these expectations.”