Galaxy groups in the 2dF Galaxy Redshift Survey: effects of environment on star formation

Martínez, H.; Zandivarez, Ariel; Domínguez, M.; Merchán, Manuel; Lambas, D. García

doi:10.1046/j.1365-8711.2002.05626.x

Cited by 49 publications

(63 citation statements)

References 21 publications

(27 reference statements)

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“…Martínez et al 2002;Bai et al 2010;Wetzel et al 2012Wetzel et al , 2013McGee et al 2011;Rasmussen et al 2012). Wetzel et al (2013) studied the quenching timescale of satellite galaxies and find that the SFR in groups evolve unaffected for 2−4 Gyr after the infall, and then the star formation quenches rapidly.…”

Section: Introductionmentioning

confidence: 99%

Comparing galaxy populations in compact and loose groups of galaxies

Coenda

Muriel

Martínez

2014

A&A

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Aims. This paper is part of a series in which we systematically compare the properties of galaxies in compact groups, loose groups, and the field. In this paper we focus our study on the age and star formation in galaxies. Methods. For galaxies in selected samples of compact groups, loose groups, and field galaxies, we compare the distributions of D n (4000) as an age indicator and the specific star formation rate as an indicator of on-going star formation. We analyse the dependence of these parameters on galaxy type and stellar mass and, for group galaxies, their dependence on the dynamic state of the system. We study the relative fraction of galaxies dominated by old stellar populations as a function of galaxy stellar mass. We perform a similar analysis for galaxies that have high specific star formation rates. Results. Galaxies in compact groups have, on average, older stellar populations than their loose-group or field counterparts. Earlytype galaxies in compact groups formed their stars and depleted their gas content more rapidly than in the other environments. We have found evidence of two populations of late-type galaxies in dynamically old compact groups: one with normal specific star formation rates and another with markedly reduced star formation. Conclusions. Processes that transform galaxies from star forming to quiescent act upon galaxies faster and more effectively in compact groups. The unique characteristics of compact groups make them an extreme environment for galaxies, where the transition to quiescence occurs rapidly.

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Section: Introductionmentioning

confidence: 99%

Comparing galaxy populations in compact and loose groups of galaxies

Coenda

Muriel

Martínez

2014

A&A

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“…Elliptical galaxies also tend to be redder, more luminous, more metal-rich, more gas-poor, and older in stellar population than spirals and irregulars (e.g., Tammann, Yahill, & Sandage 1979;Kormendy & Djorgovski 1989;Roberts & Haynes 1994). Indeed, it has also been found that color, luminosity, surface brightness, gas content, stellar population age, and star formation rate are all correlated with the overdensity of the galaxy environment (e.g., Kennicutt 1983;Balogh et al 2001;Martínez et al 2002;Lewis et al 2002;Blanton et al 2003c;Gomez et al 2002). Along the same lines, studies of the clustering of galaxies have found different clustering amplitudes for galaxies of different types, colors, and luminosities (e.g., Davis & Geller 1976;Mo, McGaugh, & Bothun 1994;Park et al 1994;Norberg et al 2002;Zehavi et al 2002).…”

Section: Introductionmentioning

confidence: 99%

The Overdensities of Galaxy Environments as a Function of Luminosity and Color

Blanton

Eisenstein²,

Gunn

et al. 2003

The Astrophysical Journal

307

291

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We study the mean environments of galaxies in the Sloan Digital Sky Survey (SDSS) as a function of restframe luminosity and color. Overdensities in galaxy number are estimated in 8 and 1 h Ϫ1 Mpc spheres centered on 115,000 galaxies taken from the SDSS spectroscopic sample. We find that, at constant color, overdensity is independent of luminosity for galaxies with the blue colors of spirals. This suggests that at fixed star formation history, spiral-galaxy mass is a very weak function of environment. Overdensity does depend on luminosity for galaxies with the red colors of early types; both low-luminosity and high-luminosity red galaxies are found to be in highly overdense regions.

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“…These high-redshift, poor groups are particularly interesting since they should be the precursors of present-day clusters with moderate masses. Furthermore, there is some observational evidence that galaxy properties depend on cluster richness in the sense that cluster galaxies are more evolved than group galaxies (Zabludoff & Mulchaey 1998;Tran et al 2001;Balogh et al 2002;Martínez et al 2002;Tanaka et al 2005Tanaka et al , 2007bKoyama et al 2007;Gilbank et al 2008). Galaxies in Article published by EDP Sciences rich clusters and in poor groups may follow different evolutionary paths.…”

Section: Introductionmentioning

confidence: 99%

The environmental dependence of properties of galaxies around the RDCSJ0910+54 cluster atz = 1.1

Tanaka¹,

Finoguenov²,

Kodama³

et al. 2008

A&A

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We report on the environmental dependence of properties of galaxies around the RDCSJ0910+54 cluster at z = 1.1. We obtained multi-band wide-field images of the cluster with Suprime-Cam and MOIRCS on Subaru and WFCAM on UKIRT. Also, an intensive spectroscopic campaign was carried out using LRIS on Keck and FOCAS on Subaru. We collected 161 spectra with secure redshifts, with which we calibrated a larger sample of photometric redshifts. We discover a possible large-scale structure around the cluster in the form of three clumps of galaxies. Two out of the three newly discovered clumps of galaxies are detected as extended X-ray sources, suggesting that they are bound systems. There seem to be filaments of galaxies in between the clumps. This is potentially one of the largest structures found so far in the z > 1 Universe. We then examined stellar populations of galaxies in the structure. First, we quantified the color-radius relation. Red galaxies have already become the dominant population in the cores of rich clusters at z ∼ 1, and the fraction of red galaxies has not strongly changed since then. The red fraction depends on the richness of clusters in the sense that it is higher in rich clusters than in poor groups. We confirm that this trend is not due to possible biases in photometric redshifts. Next, we examined red sequence galaxies. The luminosity function of red galaxies in rich clusters is consistent with one in local clusters. On the other hand, the luminosity function of red galaxies in poor groups shows a deficit of faint red galaxies. This confirms our earlier findings that galaxies follow an environment-dependent down-sizing evolution. Interestingly, the truncation magnitude of the red sequence appears brighter than found in the RDCS J1252−29 field at z = 1.24. This suggests that there is a large variation in the evolutionary phases of galaxies in groups with similar masses. Further studies of high redshift clusters will be a promising way of addressing the role of nature and nurture effects in shaping the environmental dependence of galaxy properties observed in the local Universe.

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Galaxy groups in the 2dF Galaxy Redshift Survey: effects of environment on star formation

Cited by 49 publications

References 21 publications

Comparing galaxy populations in compact and loose groups of galaxies

Comparing galaxy populations in compact and loose groups of galaxies

The Overdensities of Galaxy Environments as a Function of Luminosity and Color

The environmental dependence of properties of galaxies around the RDCSJ0910+54 cluster atz = 1.1

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