Neutral hydrogen gas, past and future star formation in galaxies in and around the ‘Sausage’ merging galaxy cluster

Stroe, Andra; Oosterloo, Tom; Rottgering, Huub J.  A.; Sobral, David; van Weeren, Reinout; Dawson, William

doi:10.1093/mnras/stv1462

Title: Neutral hydrogen gas, past and future star formation in galaxies in and around the ‘Sausage’ merging galaxy cluster

Journal Article · Sat Jul 25 00:00:00 EDT 2015 · Monthly Notices of the Royal Astronomical Society

DOI:https://doi.org/10.1093/mnras/stv1462· OSTI ID:1430973

Stroe, Andra ^[1]; Oosterloo, Tom ^[2]; Rottgering, Huub J. A. ^[1]; Sobral, David ^[3]; van Weeren, Reinout ^[4]; Dawson, William ^[5]

Leiden Univ. (Netherlands). Leiden Observatory
ASTRON, Dwingeloo (The Netherlands); Kapteyn Astronomical Inst., Groningen (The Netherlands)
Leiden Univ. (Netherlands). Leiden Observatory; Univ. de Lisboa, Lisbon (Portugal). Inst. de Astroisica e Ciencias do Espaco, Observatorio Astronomico de Lisboa, and Dept. de Fisica
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)
Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)

CIZA J2242.8+5301 (z = 0.188, nicknamed ‘Sausage’) is an extremely massive (M₂₀₀ ~2.0 × 10¹⁵ M_⊙), merging cluster with shock waves towards its outskirts, which was found to host numerous emission line galaxies. We performed extremely deep Westerbork Synthesis Radio Telescope H i observations of the ‘Sausage’ cluster to investigate the effect of the merger and the shocks on the gas reservoirs fuelling present and future star formation (SF) in cluster members. By using spectral stacking, we find that the emission line galaxies in the ‘Sausage’ cluster have, on average, as much H i gas as field galaxies (when accounting for the fact cluster galaxies are more massive than the field galaxies), contrary to previous studies. Since the cluster galaxies are more massive than the field spirals, they may have been able to retain their gas during the cluster merger. The large H i reservoirs are expected to be consumed within ~0.75–1.0 Gyr by the vigorous SF and active galactic nuclei activity and/or driven out by the outflows we observe. We find that the star formation rate (SFR) in a large fraction of H α emission line cluster galaxies correlates well with the radio broad-band emission, tracing supernova remnant emission. This suggests that the cluster galaxies, all located in post-shock regions, may have been undergoing sustained SFR for at least 100 Myr. In conclusion, this fully supports the interpretation proposed by Stroe et al. and Sobral et al. that gas-rich cluster galaxies have been triggered to form stars by the passage of the shock.

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Research Organization:: Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)

Sponsoring Organization:: USDOE; National Aeronautics and Space Administration (NASA)

Grant/Contract Number:: AC52-07NA27344; IF/01154/2012/CP0189/CT0010; PF2-130104; PEst-OE/FIS/UI2751/2014

OSTI ID:: 1430973

Report Number(s):: LLNL-JRNL-748245; TRN: US1803010

Journal Information:: Monthly Notices of the Royal Astronomical Society, Vol. 452, Issue 3; ISSN 0035-8711

Publisher:: Royal Astronomical SocietyCopyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 16 works

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