Integrated specific star formation rates of galaxies, groups, and clusters : a continuous upper limit with stellar mass?

  title={Integrated specific star formation rates of galaxies, groups, and clusters : a continuous upper limit with stellar mass?},
  author={Georg Feulner and Ulrich Hopp and C. Mendes de Oliveira Universitaets-Sternwarte Muenchen and H Germany and Max-Planck-Institut fur extraterrestrische Physik and Garching and University of Auckland and New Zealand. and University of Canterbury},
  journal={Astronomy and Astrophysics},
Aims. We investigate the build-up of stellar mass through star formation in field galaxies, galaxy groups, and clusters in order to better understand the physical processes regulating star formation in different haloes. Methods. In order to do so we relate ongoing star formation activity to the stellar mass by studying the integrated specific star formation rate (SSFR), defined as the star-formation rate per unit stellar mass, as a function of integrated stellar mass for samples of field… 

Figures from this paper

The relation between star formation, morphology, and local density in high-redshift clusters and groups
We investigate how the [O II] properties and the morphologies of galaxies in clusters and groups at z = 0.4–0.8 depend on projected local galaxy density, and compare with the field at similar
UV Star Formation Rates in the Local Universe
We measure star formation rates (SFRs) of ≈50,000 optically selected galaxies in the local universe (z ≈ 0.1)—from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the
Downsizing of star-forming galaxies by gravitational processes
There is observed a trend that a lower mass galaxy forms stars at a later epoch. This downsizing of star-forming galaxies has been attributed to hydrodynamical or radiative feedback processes that
The Radio Luminosity Function and Galaxy Evolution in the Coma Cluster
We investigate the radio luminosity function and radio source population for two fields within the Coma cluster of galaxies, with the fields centered on the cluster core and southwest infall region
The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence
We use the UV-optical color magnitude diagram in combination with spectroscopic and photometric measurements derived from the SDSS spectroscopic sample to measure the distribution of galaxies in the
The contribution of star formation and merging to stellar mass buildup in galaxies
We present a formalism to reveal merging by subtracting the change in the galaxy stellar mass function (MF) due to mass-dependent star formation (SF) from the observed time derivative of the MF. We
A View of the M81 Galaxy Group via the Hα Window
We present images for 36 galaxies of the M81 Group obtained in the Hα line. Estimates of the Hα flux and star formation rate (SFR) are now available for all the known members of the group with
Environment and self-regulation in galaxy formation
The environment is known to affect the formation and evolution of galaxies considerably best visible through the well-known morphology-density relationship. It is less clear, though, whether the
The Munich Near-Infrared Cluster Survey – IX. Galaxy evolution to z ~ 2 from optically selected catalogues
We present B-, R- and I-band-selected galaxy catalogues based on the Munich Near-Infrared Cluster Survey (MUNICS) which, together with the previously used K-selected sample, serve as an important
The X-Ray Evolution of Early-Type Galaxies in the Extended Chandra Deep Field-South
We investigate the evolution over the last 6.3 Gyr of cosmic time (i.e., since z ≈ 0.7) of the average X-ray properties of early-type galaxies within the Extended Chandra Deep Field-South (E-CDF-S).


The connection between star formation and stellar mass: specific star formation rates to redshift one
We investigate the contribution of star formation to the growth of stellar mass in galaxies over the redshift range 0.5 < z < 1.1 by studying the redshift evolution of the specific star formation
Specific star formation rates to redshift 1.5
We present a study to determine how star formation contributes to galaxy growth since z = 1.5 over five decades in galaxy stellar mass. We investigate the specific star formation rate (SSFR; star
Specific star formation rates to redshift 5 from the fors deep field and the GOODS-S field
We explore the buildup of stellar mass in galaxies over the wide redshift range 0.4 < z < 5.0 by studying the evolution of the specific star formation rate (SSFR), defined as the star formation rate
The Mass Assembly and Star Formation Characteristics of Field Galaxies of Known Morphology.
The star formation rate per unit stellar mass indicates that massive systems completed the bulk of their star formation before redshift 1, whereas dwarf galaxies continue to undergo major episodes of activity until the present epoch.
Stellar populations in local star-forming galaxies – II. Recent star formation properties and stellar masses
We present the integrated properties of the stellar populations in the Universidad Complutense de Madrid (UCM) Survey galaxies. Applying the techniques described in the first paper of this series, we
The Star formation history of field galaxies
We develop a method for interpreting faint galaxy data which focuses on the integrated light radiated from the galaxy population as a whole. The emission history of the universe at ultraviolet,
Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate
We present a first analysis of deep 24 μm observations with the Spitzer Space Telescope of a sample of nearly 1500 galaxies in a thin redshift slice, 0.65 ≤ z < 0.75. We combine the infrared data
We examine the cosmic star formation rate (SFR) and its dependence on galaxy stellar mass over the redshift range 0.8 1010.8 M☉) was 6 times higher at z = 2 than it is today. It drops steeply from z
Hα-derived Star Formation Rates for Three z≃0.75 EDisCS Galaxy Clusters* **
We present H®-derived star-formation rates (SFRs) for three z ' 0.75 galaxy clusters. Our 1¾ flux limit corresponds to a star-formation rate of 0.10-0.24 h i2 100 Myr i1 , and our minimum reliable H®
Properties of galaxy groups in the Sloan Digital Sky Survey – I. The dependence of colour, star formation and morphology on halo mass
Using a large galaxy group catalogue constructed from the Sloan Digital Sky Survey Data Release 2, we investigate the correlation between various galaxy properties and halo mass. We split the