The Transparency of Galaxy Clusters

Bovy, Jo; Moustakas, John

doi:10.1086/592187

Cited by 26 publications

(37 citation statements)

References 73 publications

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“…Note that our stacking integrates the luminosity within a disk area of 10 radius, which translates into 1 Mpc radius at z = 0.1 and respectively 4 Mpc radius at z = 0.6. The dust abundance derived from this extinction measurement is consistent with the upper limit derived by Bovy et al (2008) from measurement of reddening of SDSS galaxies behind galaxy clusters and with theoretical predictions given by Popescu et al (2000). From Eq.…”

Section: Discussionsupporting

confidence: 88%

“…However, given other constraints on the abundance of intracluster dust (Z d 10 −5 from the extinction towards the outer parts of the SDSS clusters measured by Chelouche et al 2007 andBovy et al 2008), and the fact that the IR luminosity mimics the evolution of the SFR with redshift, we believe that it is more likely that the main contribution to the cluster IR luminosity is from the ongoing star formation in the member galaxies. From theoretical predictions calibrated with the afore mentioned extinction measurement, we expect that only a minor contribution (a few percent) could originate in intracluster dust.…”

Section: Resultsmentioning

confidence: 72%

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The infrared luminosity of galaxy clusters

Giard

Montier

Pointecouteau

et al. 2008

A&A

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Context. The cosmological models for the formation of the first stars and the large scale structures now raise the question of how many dust particles were released to the general diffuse gas and how these impact the star formation process. In this framework, we focus on the scale of galaxy clusters. Aims. The aim of this study is to quantify the infrared luminosity of clusters as a function of redshift and compare this with the X-ray luminosity. This can potentially constrain the origin of the infrared emission to be intracluster dust and/or dust heated by star formation in the cluster galaxies. Methods. We perform a statistical analysis of a large sample of galaxy clusters selected from existing databases and catalogues.We coadd the infrared IRAS and X-ray RASS images in the direction of the selected clusters within successive redshift intervals up to z = 1. Results. We find that the total infrared luminosity is very high and on average 20 times higher than the X-ray luminosity. If all the infrared luminosity is to be attributed to emission from diffuse intracluster dust, then the IR to X-ray ratio implies a dust-to-gas mass abundance of 5 × 10 −4 . However, the infrared luminosity shows a strong enhancement for 0.1 < z < 1, which cannot be attributed to cluster selection effects. We show that this enhancement is compatible with a star formation rate (SFR) in the member galaxies that is typical of the central Mpc of the Coma cluster at z = 0 and evolves with the redshift as (1 + z) 5 . Conclusions. It is likely that most of the infrared luminosity that we measure is generated by the ongoing star formation in the member galaxies. From theoretical predictions calibrated on extinction measurements (dust mass abundance equal to 10 −5 ), we expect only a minor contribution, of a few percent, from intracluster dust.

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Section: Discussionsupporting

confidence: 88%

Section: Resultsmentioning

confidence: 72%

The infrared luminosity of galaxy clusters

Giard

Montier

Pointecouteau

et al. 2008

A&A

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“…Chelouche et al (2007) analysed the reddening of a sample of quasars in the direction of the clusters of the SDSS-maxBCG catalogue, obtaining an estimate of Z d ≈ 10 −5 . A similar result has also been obtained by Bovy et al (2008) by measuring the dust absorption on the spectra of galaxies located behind local (z ∼ 0.05) galaxy clusters.…”

Section: Constraints On Intracluster Dustsupporting

confidence: 83%

Infrared properties of the SDSS-maxBCG galaxy clusters

Roncarelli¹,

Pointecouteau²,

Giard³

et al. 2010

A&A

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Context. The physics of galaxy clusters has proven to be influenced by several processes connected with their galactic component which pollutes the intracluster medium (ICM) with metals, stars and dust. However, it is not clear whether the presence of diffuse dust can play a role in clusters physics since a characterisation of the infrared (IR) properties of galaxy clusters is very challenging and yet to be completely achieved. Aims. In our study we focus on the recent work of Giard et al. (2008, A&A, 490, 547) who performed a stacking analysis of the IRAS data in the direction of several thousands of galaxy clusters, providing a statistical characterisation of their IR luminosity and redshift evolution. We model the IR properties of the galactic population of the SDSS-maxBCG clusters (0.1 < z < 0.3) in order to check if it accounts for the entire observed signal and to constrain the possible presence of other components, like dust in the ICM. Methods. Starting from the optical properties of the galaxies of the SDSS-maxBCG clusters, we estimate their emission in the 60 and 100 μm IRAS bands making use of modeled spectral energy distributions of different spectral types (E/S0, Sa, Sb, Sc and starburst). We also consider the evolution of the galactic population/luminosity with redshift. Results. The total galactic emission, which is dominated by the contribution of star-forming late-type galaxies, is consistent with the observed signal. In fact, our galactic emission model slightly overestimates the observed fluxes, with the excess being concentrated in low-redshift clusters (z < ∼ 0.17). Conclusions. Our results indicate that, if present, the IR emission from intracluster dust must be very small compared to the one associated to the galaxy members. This translates into an upper limit on the dust-to-gas mass ratio in the ICM of Z d < ∼ 5 × 10 −5 . The excess in luminosity obtained at low redshift constitutes an indication that the cluster environment is driving a process of starformation quenching on its galaxy members.

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“…Thus, we cannot draw any firm conclusion about the origin of the absorption from this analysis. Both the mini-BAL features in the quasar spectrum (see Oguri et al 2008), which assures the presence of outflows in the sightline of this quasar, and the deficiency of dust in the ICM particularly near the center (Chelouche et al 2007;Muller et al 2008;Bovy et al 2008;Kitayama et al 2009) suggest that intrinsic absorption at the quasar redshift is the more likely scenario, although the anomalous flux ratios imply a faint galaxy near image C which might host the dust at the lens redshift. Indeed, a probable galaxy has recently been identified in the vicinity of image C in the HST image (Oguri et al 2012b), which might cause the extra absorption detected in image C. If the former interpretation is correct, the different absorptions between images B and C probe spatial variations of the absorption content, possibly related to the structure of disk wind outflows (Green 2006).…”

Section: Comparison With Optical and Radio Flux Ratiosmentioning

confidence: 95%

THECHANDRAVIEW OF THE LARGEST QUASAR LENS SDSS J1029+2623

Ota

Oguri

Dai

et al. 2012

ApJ

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We present results from Chandra observations of the cluster lens SDSS J1029+2623 at z l = 0.58, which is a gravitationally lensed quasar with the largest known image separation. We clearly detect X-ray emission both from the lensing cluster and the three lensed quasar images. The cluster has an X-ray temperature of kT = 8.1 +2.0 −1.2 keV and bolometric luminosity of L X = 9.6 × 10 44 erg s −1 . Its surface brightness is centered near one of the brightest cluster galaxies, and it is elongated east-west. We identify a subpeak northwest of the main peak, which is suggestive of an ongoing merger. Even so, the X-ray mass inferred from the hydrostatic equilibrium assumption appears to be consistent with the lensing mass from the Einstein radius of the system. We find significant absorption in the soft X-ray spectrum of the faintest quasar image, which can be caused by an intervening material at either the lens or source redshift. The X-ray flux ratios between the quasar images (after correcting for absorption) are in reasonable agreement with those at optical and radio wavelengths, and all the flux ratios are inconsistent with those predicted by simple mass models. This implies that microlensing effect is not significant for this system and dark matter substructure is mainly responsible for the anomalous flux ratios.

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The Transparency of Galaxy Clusters

Cited by 26 publications

References 73 publications

The infrared luminosity of galaxy clusters

The infrared luminosity of galaxy clusters

Infrared properties of the SDSS-maxBCG galaxy clusters

THECHANDRAVIEW OF THE LARGEST QUASAR LENS SDSS J1029+2623

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