The Galaxy mass function up to<i>z</i>$\mathsf{=4}$ in the GOODS-MUSIC sample: into the epoch of formation of massive galaxies

Fontana, A.; Salimbeni, S.; Grazian, A.; Giallongo, E.; Pentericci, L.; Nonino, M.; Fontanot, Fabio; Menci, Nicola; Monaco, Pierluigi; Cristiani, S.; Vanzella, E.; Santis, C. De; Gallozzi, S.

doi:10.1051/0004-6361:20065475

Cited by 383 publications

(605 citation statements)

References 36 publications

(86 reference statements)

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“…More specifically, stellar masses are derived from the comparison of SED and libraries of synthetic spectra, assuming a Salpeter (1955) Initial Mass Function (IMF) and simple stellar population (SPP) models (Bruzual & Charlot 2003), as described at length in Fontana et al (2006). SFRs have been estimated from SED fitting, using Bruzual & Charlot (2003) synthetic models and fitting the 3 We recall that our sample contains 16 sources detected only in the A03 sample and not present at all in the Tozzi et al (2006) spectral analysis.…”

Section: Host Galaxy Propertiesmentioning

confidence: 99%

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Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Brusa¹,

Fiore

Santini

et al. 2009

A&A

Self Cite

102

113

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Aims. The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. Methods. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties. Results. We found that X-ray selected (L X > ∼ 10 42 erg s −1 ) AGN show Spitzer colors consistent with both AGN and starburst dominated infrared continuum; the latter would not have been selected as AGN from infrared diagnostics. The host galaxies of X-ray selected obscured AGN are all massive (M * > 10 10 M ) and, in 50% of the cases, are also actively forming stars (1/SSFR < t Hubble ) in dusty environments. The median L/L Edd value of the active nucleus is between 2% and 10% depending on the assumed M BH /M * ratio. Finally, we found that the X-ray selected AGN fraction increases with the stellar mass up to a value of ∼30% at z > 1 and M * > 3 × 10 11 M , a fraction significantly higher than in the local Universe for AGN of similar luminosities.

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Section: Host Galaxy Propertiesmentioning

confidence: 99%

“…Statistical errors for both masses and SFR have been calculated from the 1σ convidence level in each parameter estimate by scanning the χ 2 levels, allowing the redshift to change within the errors in case of objects with photometric redshifts 4 (see Fontana et al 2006;Santini et al 2009). …”

Section: Host Galaxy Propertiesmentioning

confidence: 99%

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Brusa¹,

Fiore

Santini

et al. 2009

A&A

Self Cite

102

113

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“…The method we applied to estimate the rest-frame magnitudes and the other physical parameters (M, SFR, age) is described in previous papers (e.g., Fontana et al 2006). Briefly, we used a χ 2 minimisation analysis, comparing the observed SED of each galaxy to synthetic templates, and the redshift is fixed during the fitting process to the spectroscopic or photometric redshift derived in Grazian et al (2006a).…”

Section: The Goods-music Cataloguementioning

confidence: 99%

“…From the best-fitting template, we obtained, for each galaxy, the physical parameters that we used in the analysis. Clearly, the physical properties are subject to uncertainties and biases related to the synthetic libraries used to fit the galaxy SEDs; however, as shown in Fontana et al (2006), the extension of the SEDs to mid-IR wavelengths with IRAC tends to reduce the uncertainties on the derived stellar masses. For a detailed analysis of the uncertainties on the physical properties we refer to our previous papers Grazian et al 2007).…”

Section: The Goods-music Cataloguementioning

confidence: 99%

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni

Castellano

Pentericci

et al. 2009

A&A

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Aims. The aim of the present paper is to identify and study the properties and galactic content of groups and clusters in the GOODSSouth field up to z ∼ 2.5, and to analyse the physical properties of galaxies as a continuous function of environmental density up to high redshift. Methods. We used the deep (z 850 ∼ 26), multi-wavelength GOODS-MUSIC catalogue, which has a 15% of spectroscopic redshifts and accurate photometric redshifts for the remaining fraction. On these data, we applied a (2+1)D algorithm, previously developed by our group, that provides an adaptive estimate of the 3D density field. We supported our analysis with simulations to evaluate the purity and the completeness of the cluster catalogue produced by our algorithm. Results. We find several high-density peaks embedded in larger structures in the redshift range 0.4-2.5. From the analysis of their physical properties (mass profile, M 200 , σ v , L X , U − B vs. B diagram), we find that most of them are groups of galaxies, while two are poor clusters with masses a few times 10 14 M . For these two clusters we find from the Chandra 2Ms data an X-ray emission significantly lower than expected from their optical properties, suggesting that the two clusters are either not virialised or are gas poor. We find that the slope of the colour magnitude relation, for these groups and clusters, is constant at least up to z ∼ 1. We also analyse the dependence on environment of galaxy colours, luminosities, stellar masses, ages, and star formations. We find that galaxies in high-density regions are, on average, more luminous and massive than field galaxies up to z ∼ 2. The fraction of red galaxies increases with luminosity and with density up to z ∼ 1.2. At higher z this dependence on density disappears. The variation of galaxy properties as a function of redshift and density suggests that a significant change occurs at z ∼ 1.5-2.

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“…These difficulties have become more prominent in recent years as observational surveys at high redshift have improved. Massive galaxies (log M * / M⊙ 11.0) seem to have assembled most of their mass by z = 1, while the abundance of low-mass galaxies grows substantially at later times (Fontana et al 2006;Faber et al 2007;Pozzetti et al 2010;Marchesini et al 2009;Ilbert et al 2010;Marchesini et al 2010;Ilbert et al 2013;Muzzin et al 2013). Furthermore, vigorous star formation is almost ubiquitous in nearby low-mass galaxies, while most massive galaxies are currently red and appear to have formed few stars since z ∼ 1 (e.g.…”

Section: Introductionmentioning

confidence: 99%

Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses

Henriques

White

Thomas

et al. 2015

Monthly Notices of the Royal Astronomical Society

576

744

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We have updated the Munich galaxy formation model to the Planck first-year cosmology, while modifying the treatment of baryonic processes to reproduce recent data on the abundance and passive fractions of galaxies from z = 3 down to z = 0. Matching these more extensive and more precise observational results requires us to delay the reincorporation of wind ejecta, to lower the surface density threshold for turning cold gas into stars, to eliminate ram-pressure stripping in haloes less massive than ∼ 10 14 M ⊙ , and to modify our model for radio mode feedback. These changes cure the most obvious failings of our previous models, namely the overly early formation of low-mass galaxies and the overly large fraction of them that are passive at late times. The new model is calibrated to reproduce the observed evolution both of the stellar mass function and of the distribution of star formation rate at each stellar mass. Massive galaxies (log M * / M ⊙ 11.0) assemble most of their mass before z = 1 and are predominantly old and passive at z = 0, while lower mass galaxies assemble later and, for log M * / M ⊙ 9.5, are still predominantly blue and star forming at z = 0. This phenomenological but physically based model allows the observations to be interpreted in terms of the efficiency of the various processes that control the formation and evolution of galaxies as a function of their stellar mass, gas content, environment and time.

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The Galaxy mass function up toz$\mathsf{=4}$ in the GOODS-MUSIC sample: into the epoch of formation of massive galaxies

Cited by 383 publications

References 36 publications

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

Black hole growth and starburst activity atz= 0.6–4 in the Chandra Deep Field South

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses

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