ACCESS - III. The nature of star formation in the Shapley supercluster

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

doi:10.1111/j.1365-2966.2010.17892.x

Cited by 29 publications

(38 citation statements)

References 155 publications

(243 reference statements)

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“…The values of are about 1.3 mag brighter than in z ∼ 0 clusters (e.g. Haines et al 2011a), but consistent with field values at z ∼ 0.5 (Arnouts et al 2005). The faint‐end slopes are, however, somewhat shallower in our case.…”

Section: The Cluster Environment and Galaxy Evolutionsupporting

confidence: 84%

The Cosmic Web and galaxy evolution around the most luminous X-ray cluster: RX J1347.5−1145

Verdugo¹,

Lerchster²,

Böhringer³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In this paper we study large‐scale structures and their galaxy content around the most X‐ray luminous cluster known, RX J1347.5−1145 at z= 0.45. We make use of u*g′r′i′z′ Canada–France–Hawaii Telescope (CFHT) MegaCam photometry together with VIsible MultiObject Spectrograph (VIMOS) Very Large Telescope (VLT) spectroscopy to identify structures around RX J1347 on a scale of ∼20 × 20 Mpc2. We construct maps of the galaxy distribution and the fraction of blue galaxies. We study the photometric galaxy properties as a function of the environment traced by the galaxy density. We identify group candidates based on galaxy overdensities and study their galaxy content. We also use available Galaxy Evolution Explorer (GALEX) near‐ultraviolet imaging to identify strong unobscured star‐forming galaxies. We find that the large‐scale structure around RX J1347 extends in the north‐east–south‐west direction for at least 20 Mpc, over a region in which most of the group candidates are located, some of which show X‐ray emission in archival XMM–Newton observations. As in other studies, we find that the fraction of blue galaxies (Fblue) is a function of galaxy number density, but the bulk of the trend is due to galaxies belonging to massive systems. The fraction of ultraviolet‐ (UV‐) bright galaxies is also a function of environment, but their relative number compared with the blue population seems to be constant regardless of the environment. These UV emitters also have similar properties at all galaxy densities, indicating that the transition between galaxy types occurs over short time‐scales. Candidate galaxy groups show a large variation in their galaxy content and Fblue in those groups displays little dependence on galaxy number density. This may indicate possible differences in their evolutionary status, or suggest that the processes acting in groups are different from those in clusters. The large‐scale structure around rich clusters provides a dynamic environment for galaxy evolution. In the case of RX J1347, the transformation may start within infalling groups and finish with the removal of the cold gas once galaxies are accreted into massive systems.

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Section: The Cluster Environment and Galaxy Evolutionsupporting

confidence: 84%

The Cosmic Web and galaxy evolution around the most luminous X-ray cluster: RX J1347.5−1145

Verdugo¹,

Lerchster²,

Böhringer³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…These fractions indicate that, overall, the dominant mode of star formation in IR-emitting galaxies across the whole supercluster is that of normal late-type galaxies. Haines et al (2011b) reached the same conclusion from their analysis of IR and UV data for the nearby Shapley supercluster.…”

Section: Discussionsupporting

confidence: 57%

Spitzerobservations of Abell 1763

Biviano

Fadda

Durret

et al. 2011

A&A

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Context. The study of galaxy luminosity functions (LFs) in different environments provides powerful constraints on the physics of galaxy evolution. The infrared (IR) LF is a particularly useful tool since it is directly related to the distribution of galaxy star-formation rates (SFRs). Aims. We aim to determine the galaxy IR LF as a function of the environment in a supercluster at redshift 0.23 to shed light on the processes driving galaxy evolution in and around clusters. Methods. We base our analysis on multi-wavelength data, which include optical, near-IR, and mid-to far-IR photometry, as well as redshifts from optical spectroscopy. We identify 467 supercluster members in a sample of 24-μm-selected galaxies, on the basis of their spectroscopic (153) and photometric (314) redshifts. IR luminosities and stellar masses are determined for supercluster members via spectral energy distribution fitting. Galaxies with active galactic nuclei are identified by a variety of methods and excluded from the sample. SFRs are obtained for the 432 remaining galaxies from their IR luminosities via the Kennicutt relation. Results. We determine the IR LF of the whole supercluster as well as the IR LFs of three different regions in the supercluster: the cluster core, a large-scale filament, and the cluster outskirts (excluding the filament). A comparison of the IR LFs of the three regions, normalized by the average number densities of r-band selected normal galaxies, shows that the filament (respectively, the core) contains the highest (respectively, the lowest) fraction of IR-emitting galaxies at all levels of IR luminosities, and the highest (respectively, the lowest) total SFR normalized by optical galaxy richness. Luminous IR galaxies (LIRGs) are almost absent in the core region. The relation between galaxy specific SFRs and stellar masses does not depend on the environment, and it indicates that most supercluster LIRGs are rather massive galaxies with relatively low specific SFRs. A comparison with previous IR LF determinations from the literature confirms that the mass-normalized total SFR in clusters increases with redshift, but more rapidly than previously suggested for redshifts < ∼ 0.4. Conclusions. The IR LF shows an environmental dependence that is not simply related to the local galaxy density. The filament, an intermediate-density region in the A1763 supercluster, contains the highest fraction of IR-emitting galaxies. We interpret our findings within a possible scenario for the evolution of galaxies in and around clusters.

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“…We also found evidence that the bulk of the star-forming galaxies have been recently accreted from the field and have yet to have their star-formation activity significantly affected by the cluster environment (Haines et al 2011a) and that the vast majority of SF seen in the SSCC comes from normal infalling spirals (Haines et al 2011b). Nevertheless, this analysis was limited to galaxies belonging to the SSCC and thus in an extremely dense environment.…”

Section: Access Project: Main Results and Open Issuesmentioning

confidence: 68%

“…Although these data do not cover the whole ShaSS region they are fundamental for our survey. The W3 data will enable us to measure the SFR down to 0.2 M⊙yr −1 at 5σ, while the W1-W3 colour allows us to reproduce and map the bimodal galaxy distributions seen in the f24/fK galaxy colours in the supercluster core (Haines et al 2011a), but over the entire supercluster region, splitting the supercluster galaxies into star-forming, transitional and passive populations. This is possible because we verified that a strong linear correlation exists between W1-W3 colour and f24/fK .…”

Section: Complementary Datamentioning

confidence: 99%

Shapley Supercluster Survey: Galaxy evolution from filaments to cluster cores

Merluzzi

Busarello

Haines

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an overview of a multi-wavelength survey of the Shapley supercluster (SSC; z∼0.05) covering a contiguous area of 260 h (SC 1327-312, SC 1329 showing evidence of cluster-cluster interactions. Optical (ugri) and near-infrared (K) imaging acquired with VST and VISTA allow us to study the galaxy population down to m ⋆ +6 at the supercluster redshift. A dedicated spectroscopic survey with AAOmega on the Anglo-Australian Telescope provides a magnitude-limited sample of supercluster members with 80% completeness at ∼m ⋆ +3. We derive the galaxy density across the whole area, demonstrating that all structures within this area are embedded in a single network of clusters, groups and filaments. The stellar mass density in the core of the SSC is always higher than 9×10 9 M ⊙ Mpc −3 , which is ∼40× the cosmic stellar mass density for galaxies in the local Universe. We find a new filamentary structure (∼7 Mpc long in projection) connecting the SSC core to the cluster A 3559, as well as previously unidentified density peaks. We perform a weak-lensing analysis of the central 1 deg 2 field of the survey obtaining for the central cluster A 3558 a mass of M 500 = 7.63 +3.88 −3.40 × 10 14 M ⊙ , in agreement with X-ray based estimates.

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ACCESS - III. The nature of star formation in the Shapley supercluster

Cited by 29 publications

References 155 publications

The Cosmic Web and galaxy evolution around the most luminous X-ray cluster: RX J1347.5−1145

The Cosmic Web and galaxy evolution around the most luminous X-ray cluster: RX J1347.5−1145

Spitzerobservations of Abell 1763

Shapley Supercluster Survey: Galaxy evolution from filaments to cluster cores

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