ACCESS - II. A complete census of star formation in the Shapley supercluster - UV and IR luminosity functions

Haines, C. P.; Busarello, G.; Merluzzi, P.; Smith, Russell J.; Raychaudhury, Somak; Mercurio, A.; Smith, Graham P.

doi:10.1111/j.1365-2966.2010.17893.x

Cited by 29 publications

(47 citation statements)

References 137 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This corresponds to an average A FUV ≈ 1.3, in broad agreement with results for both field (Wyder et al 2005) and cluster samples (Cortese et al 2008b;Haines et al 2011). This implies similar levels of mean UV obscuration for galaxies across all types of global environment.…”

Section: Uv Luminosity Density In Groupssupporting

confidence: 89%

“…For example, Balogh et al (2004) used inferred Hα equivalent widths of galaxies within a large sample of lowredshift groups in the Sloan Digital Sky Survey (SDSS) and 2dF Galaxy Redshift Survey (2dFGRS) catalogs to show that the fraction of SF galaxies depends systematically on local density, but the actual star formation rate (SFR) in such galaxies does not. This has recently been shown to apply also at intermediate redshifts, z ∼ 0.4, and at fixed stellar mass (McGee et al 2011), and the result has further been extended to galaxies in both nearby (Haines et al 2011) and distant (z ∼ 1; Muzzin et al 2012) clusters and superclusters.…”

Section: Introductionmentioning

confidence: 67%

See 1 more Smart Citation

The Suppression of Star Formation and the Effect of the Galaxy Environment in Low-Redshift Galaxy Groups

Rasmussen

Mulchaey

Bai

et al. 2012

ApJ

View full text Add to dashboard Cite

Understanding the interaction between galaxies and their surroundings is central to building a coherent picture of galaxy evolution. Here we use Galaxy Evolution Explorer imaging of a statistically representative sample of 23 galaxy groups at z ≈ 0.06 to explore how local and global group environments affect the UV properties and dust-corrected star formation rates (SFRs) of their member galaxies. The data provide SFRs out to beyond 2R 200 in all groups, down to a completeness limit and limiting galaxy stellar mass of 0.06 M yr −1 and 1 × 10 8 M , respectively. At fixed galaxy stellar mass, we find that the fraction of star-forming group members is suppressed relative to the field out to an average radius of R ≈ 1.5 Mpc ≈ 2R 200 , mirroring results for massive clusters. For the first time, we also report a similar suppression of the specific SFR within such galaxies, on average by 40% relative to the field, thus directly revealing the impact of the group environment in quenching star formation within infalling galaxies. At fixed galaxy density and stellar mass, this suppression is stronger in more massive groups, implying that both local and global group environments play a role in quenching. The results favor an average quenching timescale of 2 Gyr and strongly suggest that a combination of tidal interactions and starvation is responsible. Despite their past and ongoing quenching, galaxy groups with more than four members still account for at least ∼25% of the total UV output in the nearby universe.

show abstract

Section: Uv Luminosity Density In Groupssupporting

confidence: 89%

Section: Introductionmentioning

confidence: 67%

The Suppression of Star Formation and the Effect of the Galaxy Environment in Low-Redshift Galaxy Groups

Rasmussen

Mulchaey

Bai

et al. 2012

ApJ

View full text Add to dashboard Cite

show abstract

“…The NUV luminosity function of Virgo is well fitted by a Schechter function with M * = −17.56 and α = −1.19. These values are close to those determined in the central 12 deg 2 by Boselli et al (2011), but are significantly different from those determined in Coma (Cortese et al 2008;Hammer et al 2012), A1367 (Cortese et al 2005), in the Shapley supercluster (Haines et al 2011), or in the field (Wyder et al 2005). The slope of the faint end of the NUV luminosity function of Virgo (α = −1.19) is significantly flatter than that of Coma, A1367, or the Shapley supercluster (α − 1.5/ − 1.6) as first seen by Boselli et al (2011); however, the slope is comparable to the value determined in the field (α = −1.16; Wyder et al 2005).…”

Section: Nuv Luminosity Functionsupporting

confidence: 67%

“…The luminosity function is a statistical tool widely used to study the mean properties of large samples of galaxies. Often used in other wavelength domains, it has been derived at rest frame in the GALEX UV bands only for the general field (Wyder et al 2005) and for a few other nearby clusters (Coma, Cortese et al 2008;Hammer et al 2012;A1367, Cortese et al 2005; Shapley, Haines et al 2011). Compared to these previous works, the UV luminosity function derived from the GUViCS survey has the great advantage of including a significantly large number of objects with direct redshift measurements, of sampling a much wider range in galaxy density, from the core of the cluster out to the periphery (∼2 R vir ), and of including the dwarf galaxy population (NUV < ∼ −11.5 mag).…”

Section: Introductionmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

View full text Add to dashboard Cite

We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg 2 , an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV − i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = −1.19), here sampled down to ∼NUV = −11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M * = −17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments.

show abstract

“…Due to its exceptional role, the SC core has been studied at all energy bands, from the X-ray (e.g., Ettori et al [29], Gastaldello et al [30], Rossetti et al [31], Ursino et al [32]) to the radio (e.g., Venturi et al [33][34][35][36], Giacintucci et al [37,38]), and has a wealth of data from Galex Spitzer and deep AAT spectroscopy from the ACCESS survey (e.g., Haines et al [39], Merluzzi et al [40,41]), which further highlight intense merging activity.…”

Section: The Shapley Concentration In Contextmentioning

confidence: 99%

Extended Radio Emission in the Perhipheral Regions of the Shapley Concentration Core

et al. 2017

View full text Add to dashboard Cite

Abstract:The Shapley Concentration (SC) is a galaxy supercluster (few tens of degrees) in the Local Universe (∼0.048) which is currently undergoing cluster mergers and group accretion. It is a diversified environment, with cluster complexes in advanced evolutionary stage, groups of clusters in the very early stages of merger, fairly massive clusters with ongoing accretion activity, and smaller groups located in filaments. These features make the SC an ideal place to observe the signatures of the formation of large-scale structures in the Universe. As a matter of fact, the SC has been observed over a broad range of frequencies with the most important observatories, allowing for a unique multiband study. In this paper, we will present new results from an ongoing study of the Shapley Concentration Core, which is being carried out with the Giant Metrewave Radio Telescope (GMRT). Our work confirms the role played by radio observations in disentangling the details of the accretion and merging processes, and delivers a wealth of information in regions well outside the cluster cores. In particular, we will report on the discovery of a relic in the region between the two clusters A 3558 and A 3562, and of the radio properties of the brightest galaxy in the peripheral cluster A 3556.Keywords: Galaxy clusters; Shapley Concentration; radio sources Cluster Mergers and Diffuse Radio EmissionAccording to the hierarchical scenario, cluster mergers-the most energetic events in the Universe, with a total energy output of the order of 10 63 -10 64 erg-are the natural way to account for mass assembly: galaxy clusters form as a consequence of merger trees, to reach and exceed masses on the order of 10 15 M Sun . Cluster mergers deeply affect the dynamics of the galaxies, as well as the properties of the thermal intracluster medium and those of relativistic particles and magnetic field.The close connection between the properties of the radio emission in galaxy clusters and their dynamical state is now an established result. Giant radio halos and relics-Mpc-scale steep spectrum synchrotron radio sources (see Feretti et al. [1] for a recent observational overview)-are thought to be the result of particle re-acceleration due to turbulence and shocks, respectively, induced in the cluster volume during mergers and accretion processes (see Brunetti and Jones [2] for a recent theoretical review). While the details of the microphysics of these processes are still a matter of

show abstract

ACCESS - II. A complete census of star formation in the Shapley supercluster - UV and IR luminosity functions

Cited by 29 publications

References 137 publications

The Suppression of Star Formation and the Effect of the Galaxy Environment in Low-Redshift Galaxy Groups

The Suppression of Star Formation and the Effect of the Galaxy Environment in Low-Redshift Galaxy Groups

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Extended Radio Emission in the Perhipheral Regions of the Shapley Concentration Core

Contact Info

Product

Resources

About