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SEEDisCS. I. Molecular gas in galaxy clusters and their large-scale structure: The case of CL1411.1−1148 at z ∼ 0.5

Spérone-Longin, D. and Jablonka, P. and Combes, F. and Castignani, G. and Krips, M. and Rudnick, G. and Zaritsky, D. and Finn, R. A. and De Lucia, G. and Desai, V. (2021) SEEDisCS. I. Molecular gas in galaxy clusters and their large-scale structure: The case of CL1411.1−1148 at z ∼ 0.5. Astronomy and Astrophysics, 647 . Art. No. A156. ISSN 0004-6361. doi:10.1051/0004-6361/202038904.

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We investigate how the galaxy reservoirs of molecular gas fuelling star formation are transformed while the host galaxies infall onto galaxy cluster cores. As part of the Spatially Extended ESO Distant Cluster Survey (SEEDisCS), we present CO(3-2) observations of 27 star-forming galaxies obtained with the Atacama Large Millimeter Array. These sources are located inside and around CL1411.1−1148 at z = 0.5195, within five times the cluster virial radius. These targets were selected to have stellar masses (M_(star)), colours, and magnitudes similar to those of a field comparison sample at similar redshift drawn from the Plateau de Bure high-z Blue Sequence Survey (PHIBSS2). We compare the cold gas fraction (μH₂ = MH₂/M_(star)), specific star formation rates (SFR/M_(star)) and depletion timescales (t_(depl) = MH₂/SFR) of our main-sequence galaxies to the PHIBSS2 subsample. While the most of our galaxies (63%) are consistent with PHIBSS2, the remainder fall below the relation between μH₂ and M_(star) of the PHIBSS2 galaxies at z ∼ 0.5. These low-μH₂ galaxies are not compatible with the tail of a Gaussian distribution, hence they correspond to a new population of galaxies with normal SFRs but low gas content and low depletion times (≲1 Gyr), absent from previous surveys. We suggest that the star formation activity of these galaxies has not yet been diminished by their low fraction of cold molecular gas.

Item Type:Article
Related URLs:
URLURL TypeDescription
Spérone-Longin, D.0000-0002-3752-2502
Combes, F.0000-0003-2658-7893
Rudnick, G.0000-0001-5851-1856
Zaritsky, D.0000-0002-5177-727X
Finn, R. A.0000-0001-8518-4862
Desai, V.0000-0002-1340-0543
Additional Information:© ESO 2021. Article published by EDP Sciences. Received 13 July 2020; Accepted 19 January 2021; Published online 26 March 2021. We thank the anonymous referee whose detailed comments helped to improve the presentation of the paper. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.1.01324.S and ADS/JAO.ALMA#2017.1.00257.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The authors are indebted to the International Space Science Institute (ISSI), Bern, Switzerland, for supporting and funding the international team “The Effect of Dense Environments on Gas in Galaxies over 10 Billion Years of Cosmic Time”. We are grateful to the Numpy (Oliphant 2006; Van Der Walt et al. 2011), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007), IPython (Pérez & Granger 2007) and Astropy (Astropy Collaboration 2013, 2018) teams for providing the scientific community with essential Python tools.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
International Space Science Institute (ISSI)UNSPECIFIED
Subject Keywords:galaxies: evolution – galaxies: clusters: general – submillimeter: galaxies
Record Number:CaltechAUTHORS:20210503-132407716
Persistent URL:
Official Citation:SEEDisCS - I. Molecular gas in galaxy clusters and their large-scale structure: The case of CL1411.1−1148 at z ∼ 0.5. D. Spérone-Longin, P. Jablonka, F. Combes, G. Castignani, M. Krips, G. Rudnick, D. Zaritsky, R. A. Finn, G. De Lucia and V. Desai. A&A, 647 (2021) A156; DOI:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108945
Deposited By: Tony Diaz
Deposited On:03 May 2021 22:28
Last Modified:03 May 2021 22:28

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