SIMBAD references

2018ApJ...853..195W - Astrophys. J., 853, 195-195 (2018/February-1)

Herschel and ALMA observations of massive SZE-selected clusters.

WU J.F., AGUIRRE P., BAKER A.J., DEVLIN M.J., HILTON M., HUGHES J.P., INFANTE L., LINDNER R.R. and SIFON C.

Abstract (from CDS):

We present new Herschel observations of four massive, Sunyaev-Zel'dovich effect-selected clusters at 0.3 z 1.1, two of which have also been observed with the Atacama Large Millimeter/submillimeter Array (ALMA). We detect 19 Herschel/Photoconductor Array Camera and Spectrometer (PACS) counterparts to spectroscopically confirmed cluster members, five of which have redshifts determined via CO (4-3) and [C I] (3P13P0) lines. The mean [C I]/CO line ratio is 0.19 ± 0.07 in brightness temperature units, consistent with previous results for field samples. We do not detect significant stacked ALMA dust continuum or spectral-line emission, implying upper limits on mean interstellar medium (H2 + H I) and molecular gas masses. An apparent anticorrelation of LIR with clustercentric radius is driven by the tight relation between star formation rate and stellar mass. We find an average specific star formation rate of log(sSFR/yr–1) = -10.36, which is below the SFR–M* correlation measured for field galaxies at similar redshifts. The fraction of infrared-bright galaxies (IRBGs; log(LIR/L) 10.6) per cluster and average sSFR rise significantly with redshift. For CO detections, we find fgas∼0.2, comparable to those of field galaxies, and gas depletion timescales of about 2 Gyr. We use radio observations to distinguish active galactic nuclei (AGNs) from star-forming galaxies. At least four of our 19 Herschel cluster members have qIR 1.8, implying an AGN fraction fAGN 0.2 for our PACS-selected sample.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): galaxies: clusters: general - galaxies: evolution - galaxies: ISM - galaxies: ISM

Status in Simbad:  being processed

Simbad objects: 14

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2019.09.21-09:45:20

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