The stellar masses of 25 000 galaxies at 0.2 ≤ z ≤ 1.0 
estimated by the COMBO-17 survey

Borch, Andrea; Meisenheimer, K.; Bell, Eric F.; Rix, Hans─Walter; Wolf, Christian; Dye, S.; Kleinheinrich, M.; Kovács, Zoltán; Wisotzki, L.

doi:10.1051/0004-6361:20054376

Cited by 307 publications

(526 citation statements)

References 79 publications

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“…Bundy et al 2005Bundy et al , 2006Borch et al 2006;Pannella et al 2006). Ilbert et al (2010) performed similar analyses out to redshifts of z ∼ 2 and found that, for quiescent galaxies, z ∼ 1 represents an epoch of transition in their stellar mass assembly, showing that the stellar mass density for the quiescent population increases by over an order of magnitude from z ∼ 2 to z ∼ 0.8, but only increases by a factor of 2 between z ∼ 0.8 and the present day.…”

Section: Introductionmentioning

confidence: 86%

The WIRCam Deep Survey

Bielby

Hudelot

McCracken

et al. 2012

A&A

171

208

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We present a new near-infrared imaging survey in the four CFHTLS deep fields: the WIRCam Deep Survey or "WIRDS". WIRDS comprises extremely deep, high quality (FWHM ∼ 0.6 ) J, H, and K s imaging covering a total effective area of 2.1 deg 2 and reaching AB 50% completeness limits of ≈24.5. We combine our images with the CFHTLS to create a unique eight-band ugrizJHK S photometric catalogues in the four CFHTLS deep fields; these four separate fields allow us to make a robust estimate of the effect of cosmic variance for all our measurements. We use these catalogues in combination with ≈9800 spectroscopic redshifts to estimate precise photometric redshifts (σ Δz/(1+z) 0.03 at i < 25), galaxy types, star-formation rates and stellar masses for a unique sample of ≈1.8 million galaxies. Our JHK s number counts are consistent with previous studies. We apply the "BzK" selection to our gzK filter set and find that the star forming BzK selection successfully selects 76% of star-forming galaxies in the redshift range 1.4 < z < 2.5 in our photometric catalogue, based on our photometric redshift measurement. Similarly the passive BzK selection returns 52% of the passive 1.4 < z < 2.5 population identified in the photometric catalogue. We present the mass functions of the total galaxy population as a function of redshift up to z = 2 and present fits using double Schechter functions. A mass-dependent evolution of the mass function is seen with the numbers of galaxies with masses of M 10 10.75 still evolving at z 1, but galaxies of higher mass reaching their present day numbers by z ∼ 0.8−1. This is consistent with the present picture of downsizing in galaxy evolution. We compare our results with the predictions of the GALFORM semi-analytical galaxy formation model and find that the simulations provide a relatively successful fit to the observed mass functions at intermediate masses (i.e. 10 log (M/M ) 11). However, as is common with semi-analytical predictions of the mass function, the GALFORM results under-predict the mass function at low masses (i.e. log (M/M ) 10), whilst the fit as a whole degrades beyond redshifts of z ∼ 1.2. All photometric catalogues and images are made publicly available from TERAPIX and CADC.

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Section: Introductionmentioning

confidence: 86%

The WIRCam Deep Survey

Bielby

Hudelot

McCracken

et al. 2012

A&A

171

208

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“…The stellar masses that we use were estimated by Borch et al (2006) using the COMBO-17 photometry in conjunction with a template library derived using the PEGASE stellar population models (Fioc & Rocca-Volmerange 1997) with solar metallicity and a Kroupa (2001) IMF. The different IMFs used by Whitaker et al and Borch et al would only change the stellar masses by ∼ 10%.…”

Section: Star Formation Ratesmentioning

confidence: 99%

OMEGA – OSIRIS Mapping of Emission-line Galaxies in A901/2 – I. Survey description, data analysis, and star formation and AGN activity in the highest density regions

Chies-Santos

Pino

Aragón-Salamanca

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present an overview of and first results from the OMEGA survey: the OSIRIS Mapping of Emission-line Galaxies in the multi-cluster system A901/2. The ultimate goal of this project is to study star formation and AGN activity across a broad range of environments at a single redshift. Using the tuneable-filter mode of the OSIRIS instrument on GTC, we target Hα and [Nii] emission lines over a ∼ 0.5 × 0.5 deg 2 region containing the z ∼ 0.167 multi-cluster system A901/2. In this paper we describe the design of the survey, the observations and the data analysis techniques developed. We then present early results from two OSIRIS pointings centred on the cores of the A901a and A902 clusters. AGN and star-forming (SF) objects are identified using the [Nii] / Hα vs. W Hα (WHAN) diagnostic diagram. The AGN hosts are brighter, more massive, and possess earlier-type morphologies than SF galaxies. Both populations tend to be located towards the outskirts of the high density regions we study. The typical Hα luminosity of these sources is significantly lower than that of field galaxies at similar redshifts, but greater than that found for A1689, a rich cluster at z ∼ 0.2. The Hα luminosities of our objects translate into star-formation rates (SFRs) between ∼ 0.02 and 6 M yr −1 . Comparing the relationship between stellar mass and Hα-derived SFR with that found in the field indicates a suppression of star formation in the cores of the clusters. These findings agree with previous investigations of this multi-cluster structure, based on other star formation indicators, and demonstrate the power of tuneable filters for this kind of study.

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“…Additionally 17-band COMBO-17 (Classifying Objects by Medium-Band Observations), Spitzer 24 μm, XMM-Newton X-ray data (Gilmour et al 2007) and gravitational lensing maps (Heymans et al 2008) are available. Photometric redshifts with errors δ z /(1 + z) ∼ 0.02 up to R = 24, spectral energy distributions (Wolf et al 2003) and stellar masses (Borch et al 2006) have been derived from the COMBO-17 survey as well as star-formation rates from the COMBO-17 UV and Spitzer 24 μm data (Bell et al 2007). Data from the Galaxy Evolution Explorer (GALEX), 2 degree Field (2dF) spectrograph, and Giant Meterwave Radio Telescope (GMRT) are also available.…”

Section: The Stages Data Setmentioning

confidence: 99%

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

Bösch

Böhm

Wolf

et al. 2013

A&A

Self Cite

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Aims. We present spectroscopic observations of 182 disk galaxies (96 in the cluster and 86 in the field environment) in the region of the Abell 901/902 multiple cluster system, which is located at a redshift of z ∼ 0.165. We estimate dynamical parameters of the four subclusters and analyse the kinematics of spiral galaxies, searching for indications of ram-pressure stripping. Furthermore, we focus on dusty red galaxies as a possible intermediate stage in the transformation of field galaxies to lenticulars when falling into the cluster. Methods. We obtained multi-object slit spectroscopy using the VLT instrument VIMOS. We carried out a redshift analysis, determined velocity dispersions using biweight statistics, and detected possible substructures with the Dressler-Shectman test. We exploited rotation curves from emission lines to analyse distortions in the gaseous disk of a galaxy, as well as HST/ACS images to quantify the morphological distortions of the stellar disk. Results. The presence of substructures and non-Gaussian redshift distributions indicate that the cluster system is dynamically young and not in a virialised state. We find evidence of two important galaxy populations. Morphologically distorted galaxies are probably subject to increased tidal interactions. They show pronounced rotation-curve asymmetries at intermediate cluster-centric radii and low rest-frame peculiar velocities. Morphologically undistorted galaxies show the strongest rotation-curve asymmetries at high rest-frame velocities and low cluster-centric radii. Supposedly, this group is strongly affected by ram-pressure stripping due to interaction with the intra-cluster medium. Among the morphologically undistorted galaxies, dusty red galaxies have particularly strong rotation-curve asymmetries, suggesting that ram pressure is an important factor in these galaxies. Furthermore, dusty red galaxies have on average a bulge-to-total ratio that is higher by a factor of two than cluster blue-cloud and field galaxies. The fraction of kinematically distorted galaxies is 75% higher in the cluster than in the field environment. This difference mainly stems from morphologically undistorted galaxies, indicating a cluster-specific interaction process that only affects the gas kinematics but not the stellar morphology. Also the ratio between gas and stellar scale length is reduced for cluster galaxies compared to the field sample. Both findings could be explained best by ram-pressure effects. Conclusions. Ram-pressure stripping seems to be an important interaction process in the multiple cluster system A901/902. Dusty red galaxies might be a crucial element in understanding the transformation of field disk galaxies into cluster lenticular galaxies.

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The stellar masses of 25 000 galaxies at 0.2 ≤ z ≤ 1.0 estimated by the COMBO-17 survey

Cited by 307 publications

References 79 publications

The WIRCam Deep Survey

The WIRCam Deep Survey

OMEGA – OSIRIS Mapping of Emission-line Galaxies in A901/2 – I. Survey description, data analysis, and star formation and AGN activity in the highest density regions

Ram pressure and dusty red galaxies – key factors in the evolution of the multiple cluster system Abell 901/902

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