Searching for Dust in the Intracluster Medium from Reddening of Background Galaxies

Müller, S.; Wu, Szu-Ying; Hsieh, Bau-Ching; Gonzalez, Ruben L.; Loinard, Laurent; Yee, H. K. C.; Gladders, M. D.

doi:10.1086/529583

Cited by 40 publications

(51 citation statements)

References 51 publications

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“…The comparison with the IR-SFR to X-ray luminosity ratios measured for the two clusters Coma and MS1054-0321 (Bai et al 2007a) confirms that the measured SFR may be insufficient to explain the high IR to X-ray luminosity ratio derived by our stacking analysis. Moreover, our upper limit to the dust in the ICM is of the same order as that measured by Muller et al (2008) from their search for statistical reddening of background galaxies behind a sample of 458 RCD clusters with z < 0.5. Their extinction value converted into an upper limit to the dust mass within the central Mpc is 8 × 10 9 M .…”

Section: Discussionsupporting

confidence: 64%

“…A statistical detection of intracluster dust extinction towards SDSS quasars located behind clusters of galaxies was obtained by Chelouche et al (2007). An upper limit was also derived by Muller et al (2008) by studying the statistical reddening of galaxies behind 458 RCS clusters. Finally, Bai et al (2007b) derived upper limits at 24 and 70 μm from observations by the Spitzer telescope of the cluster Abell 2029 (z = 0.08).…”

Section: Introductionmentioning

confidence: 99%

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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: 64%

Section: Introductionmentioning

confidence: 99%

The infrared luminosity of galaxy clusters

Giard

Montier

Pointecouteau

et al. 2008

A&A

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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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“…They found mean E(B À V ) values of a few ; 10 À3 mag for sight lines passing $1 Mpc from the clusters' centers. However, a recent study found no evidence of dust in 0:2 < z < 0:5 clusters from a photometric study of color excesses in several bands and, assuming a Galactic extinction law, derived an average visual extinction of hA V i ¼ 0:004 AE 0:010 mag (Muller et al 2008).…”

Section: Introductionmentioning

confidence: 97%

The Transparency of Galaxy Clusters

Bovy

Moustakas

2008

Astrophysical Journal

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If galaxy clusters contain intracluster dust, the spectra of galaxies lying behind clusters should show attenuation by dust absorption. We compare the optical (3500Y7200 8) spectra of 60,267 luminous, early-type galaxies selected from the Sloan Digital Sky Survey to search for the signatures of intracluster dust in z $ 0:05 clusters. We select massive, quiescent (i.e., non-star-forming) galaxies using an EW( H ) 2 8 cut and consider galaxies in three bins of velocity dispersion ranging from 150 to 300 km s À1 . The uniformity of early-type galaxy spectra in the optical allows us to construct inverse-variance-weighted composite spectra with high signal-to-noise ratios (ranging from 10 2 to 10 3 ). We compare the composite spectra of galaxies that lie behind and adjacent to galaxy clusters and find no convincing evidence of dust attenuation on scales of $0.15Y2 Mpc; we derive a generic limit of E(B À V ) < 3 ; 10 À3 mag on scales of $1Y2 Mpc at the 99% confidence level, using conservative jackknife error bars, corresponding to a dust mass P10 8 M . On scales smaller than 1 Mpc, this limit is slightly weaker, E(B À V ) < 8 ; 10 À3 mag.

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Searching for Dust in the Intracluster Medium from Reddening of Background Galaxies

Cited by 40 publications

References 51 publications

The infrared luminosity of galaxy clusters

The infrared luminosity of galaxy clusters

THECHANDRAVIEW OF THE LARGEST QUASAR LENS SDSS J1029+2623

The Transparency of Galaxy Clusters

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