LoCuSS: Shedding new light on the massive lensing cluster Abell 1689 – the view from<i>Herschel</i>

Haines, C. P.; Smith, Graham P.; Pereira, M. J.; Egami, Eiichi; Moran, Sean M.; Hardegree-Ullman, E.; Rawle, Tim; Rex, M.

doi:10.1051/0004-6361/201014692

Cited by 29 publications

(33 citation statements)

References 40 publications

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“…This represents the first measurement of the 70‐μm galaxy LF of a local cluster with Spitzer , and should prove a useful local benchmark to follow the evolution in the infrared properties of cluster galaxies with ongoing and future surveys (e.g. Haines et al 2009a,b, 2010a; Braglia et al 2010; Chung et al 2010; Rawle et al 2010; Smith et al 2010) with Spitzer and particularly Herschel whose PACS instrument covers rest‐frame 70 μm beyond z ∼ 1.…”

Section: Discussionmentioning

confidence: 79%

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

Haines

Busarello

Merluzzi

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present panoramic Spitzer/MIPS mid‐ and far‐infrared (MIR/FIR) and GALEX ultraviolet imaging of the most massive and dynamically active system in the local Universe, the Shapley supercluster at z= 0.048, covering the five clusters that make up the supercluster core. We combine these data with existing spectroscopic data from 814 confirmed supercluster members to produce the first study of a local rich cluster including both ultraviolet and infrared luminosity functions (LFs). This joint analysis allows us to produce a complete census of star formation (both obscured and unobscured), extending down to star formation rates (SFRs) ∼0.02–0.05 M⊙ yr−1, and quantify the level of obscuration of star formation among cluster galaxies, providing a local benchmark for comparison to ongoing and future studies of cluster galaxies at higher redshifts with Spitzer and Herschel. The GALEX near‐ultraviolet (NUV) and far‐ultraviolet (FUV) luminosity functions (LFs) obtained have steeper faint‐end slopes than the local field population, due largely to the contribution of massive, quiescent galaxies at MFUV≳−16. The 24‐ and 70‐μm galaxy LFs for the Shapley supercluster instead have shapes fully consistent with those obtained for the Coma cluster and for the local field galaxy population. This apparent lack of environmental dependence for the shape of the FIR luminosity function suggests that the bulk of the star‐forming galaxies that make up the observed cluster infrared LF have been recently accreted from the field and have yet to have their star formation activity significantly affected by the cluster environment. We estimate a global SFR of 327 M⊙ yr−1 over the whole supercluster core, of which just ∼20 per cent is visible directly in the ultraviolet continuum and ∼80 per cent is reprocessed by dust and emitted in the infrared. The level of obscuration (LIR/LFUV) in star‐forming galaxies is seen to increase linearly with LK over 2 orders of magnitude in stellar mass.

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Section: Discussionmentioning

confidence: 79%

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

Haines

Busarello

Merluzzi

et al. 2010

Monthly Notices of the Royal Astronomical Society

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“…2) within a clustercentric radius of R < 1.5 r 200 and lying inside the caustics in the velocity-radius plane (see Haines et al 2010 for an example). Just (24 ± 3)% (46/192) of these galaxies are LIRGs (L TIR > 10 11 L ) and none are ultra-luminous IR galaxies (ULIRGs; L TIR > 10 12 L ).…”

Section: Resultsmentioning

confidence: 99%

“…Calculation of the total IR luminosities (8 < λ < 1000 μm) discussed in Sect. 4 are described by Haines et al (2010).…”

Section: Observations and Data Analysismentioning

confidence: 99%

LoCuSS: Probing galaxy transformation physics withHerschel

Smith¹,

Haines²,

Pereira

et al. 2010

A&A

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We present an early broad-brush analysis of Herschel/PACS observations of star-forming galaxies in 8 galaxy clusters drawn from our survey of 30 clusters at z 0.2. We define a complete sample of 192 spectroscopically confirmed cluster members down to L TIR > 3 × 10 10 L and L K > 0.25 L K . The average K-band and bolometric infrared luminosities of these galaxies both fade by a factor of ∼2 from clustercentric radii of ∼2 r 200 to ∼0.5 r 200 , indicating that as galaxies enter the clusters ongoing star-formation stops first in the most massive galaxies, and that the specific star-formation rate (SSFR) is conserved. On smaller scales the average SSFR jumps by ∼25%, suggesting that in cluster cores processes including ram pressure stripping may trigger a final episode of star-formation that presumably exhausts the remaining gas. This picture is consistent with our comparison of the Herschel-detected cluster members with the cluster mass distributions, as measured in our previous weak-lensing study of these clusters. For example, the spatial distribution of the Herschel sources is positively correlated with the structures in the weak-lensing mass maps at ∼5σ significance, with the strongest signal seen at intermediate group-like densities. The strong dependence of the total cluster IR luminosity on cluster mass -L TIR ∝ M 2 virial -is also consistent with accretion of galaxies and groups of galaxies (i.e. the substructure mass function) driving the cluster IR luminosity. The most surprising result is that roughly half of the Herschel-detected cluster members have redder S 100 /S 24 flux ratios than expected, based on the Rieke et al. models. On average cluster members are redder than non-members, and the fraction of red galaxies increases towards the cluster centers, both of which indicate that these colors are not attributable to systematic photometric errors. Our future goals include to intepret physically these red galaxies, and to exploit this unique large sample of clusters with unprecedented multi-wavelength observations to measure the cluster-cluster scatter in S0 progenitor populations, and to intepret that scatter in the context of the hierarchical assembly of clusters.

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“…However, more recent studies have shown that a significant fraction (∼30 per cent) of galaxies along the red sequence are actively forming stars, and appear red due to the presence of dust (Wolf, Gray & Meisenheimer 2005; Haines, Gargiulo & Merluzzi 2008). These dusty red‐sequence galaxies appear particularly prevalent in intermediate‐density environments on the outskirts of clusters (Gallazzi et al 2009; Haines et al 2010a).…”

Section: Bimodality In the Infrared Coloursmentioning

confidence: 99%

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

Haines¹,

Busarello²,

Merluzzi³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present a joint analysis of panoramic Spitzer/MIPS mid‐ and far‐infrared (MIR/FIR) and GALEX ultraviolet imaging of the most massive and dynamically active structure in the local Universe, the Shapley supercluster at z= 0.048, covering the five clusters that make up the supercluster core. Combining this with existing spectroscopic data from 814 confirmed supercluster members and 1.4‐GHz radio continuum maps, this represents the largest complete census of star formation (both obscured and unobscured) in local cluster galaxies to date, extending down to star formation rates (SFRs) ∼ 0.02–0.05 M⊙ yr−1. We take advantage of this comprehensive panchromatic data set to perform a detailed analysis of the nature of star formation in cluster galaxies of the kind previously limited to local field galaxy surveys such as SINGS, using several quite independent diagnostics of the quantity and intensity of star formation to develop a coherent view of the types of star formation within cluster galaxies. We observe a robust bimodality in the infrared (f24 μm/fK) galaxy colours, which we are able to identify as another manifestation of the broad split into star‐forming spiral and passive elliptical galaxy populations seen in UV–optical surveys. This diagnostic also allows the identification of galaxies in the process of having their star formation quenched as the infrared analogue to the ultraviolet ‘green valley’ population. The bulk of supercluster galaxies on the star‐forming sequence have specific‐SFRs consistent with local field specific‐SFR– relations of Elbaz et al. (2007), and form a tight FIR–radio correlation (0.24 dex) confirming that their FIR emission is due to star formation. We show that 85 per cent of the global SFR is quiescent star formation within spiral discs, as manifest by the observed sequence in the (LIR/FFUV)–(FUV−NUV) plane – the IRX (infrared‐to‐ultraviolet ratio)–β relation – being significantly offset from the starburst relation of Kong et al. (2004), while their FIR–radio colours indicate dust heated by low‐intensity star formation. Just 15 per cent of the global SFR is due to nuclear starbursts. The vast majority of star formation seen in cluster galaxies comes from normal infalling spirals that have yet to be affected by the cluster environment.

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LoCuSS: Shedding new light on the massive lensing cluster Abell 1689 – the view fromHerschel

Cited by 29 publications

References 40 publications

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

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

LoCuSS: Probing galaxy transformation physics withHerschel

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

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