Mapping H i 21-cm in the Klemola 31 group at z = 0.029: emission and absorption towards PKS 2020−370

Author:

Maina E K1ORCID,Mohapatra Abhisek2ORCID,Józsa G I G13,Gupta N2,Combes F4,Deka P2,Wagenveld J D3,Srianand R2ORCID,Balashev S A56ORCID,Chen Hsiao-Wen7ORCID,Krogager J-K8,Momjian E9,Noterdaeme P1011,Petitjean P10

Affiliation:

1. Department of Physics and Electronics, Rhodes University , PO Box 94, Makhanda, 6140, South Africa

2. Inter-University Centre for Astronomy and Astrophysics , Post Bag 4, Ganeshkhind, Pune 411 007, India

3. Max-Planck-Institut für Radioastronomie , Auf dem Hügel 69, D-53121 Bonn, Germany

4. Observatoire de Paris, LERMA, College de France, CNRS, PSL University, Sorbonne University , F-75014 Paris, France

5. Ioffe Institute , Politekhnicheskaya 26, 194021 Saint Petersburg, Russia

6. HSE University , 109028 Saint Petersburg, Russia

7. Department of Astronomy & Astrophysics, The University of Chicago , 5640 South Ellis Avenue, Chicago, IL 60637, USA

8. Université Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574 , F-69230 Saint-Genis-Laval, France

9. National Radio Astronomy Observatory , PO Box O, Socorro, NM 87801, USA

10. Institut d’Astrophysique de Paris, Sorbonne Université and CNRS , 98 bis boulevard Arago, F-75014 Paris, France

11. Franco-Chilean Laboratory for Astronomy , IRL 3386, CNRS and U. de Chile, Casilla 36-D Santiago, Chile

Abstract

ABSTRACT We present MeerKAT Absorption Line Survey (MALS) observations of the H i gas in the Klemola 31 galaxy group (z = 0.029), located along the line of sight to the radio-loud quasar PKS 2020−370 (z = 1.048). Four galaxies of the group are detected in H i emission, and H i absorption is also detected in front of PKS 2020−370 in Klemola 31A. The emission and absorption are somewhat compensating on the line of sight of the quasar, and the derived column density of the absorption appears underestimated, with respect to the neighbouring emission. A symmetric tilted-ring model of Klemola 31A, assuming the absorbing gas in regular rotation in the plane, yields a rather high spin temperature of 530 K. An alternative interpretation is that the absorbing gas is extra-planar, which will also account for its non-circular motion. The Na i/Ca ii ratio also suggests that the absorbing gas is unrelated to cold H i disc. Two of the galaxies in the Klemola group are interacting with a small companion, and reveal typical tidal tails, and velocity perturbations. Only one of the galaxies, ESO 400−13, reveals a strong H i deficiency, and a characteristic ram-pressure stripping, with a total asymmetry in the distribution of its gas. Since a small galaxy group as Klemola 31 is not expected to host a dense intra-group gas, this galaxy must be crossing the group at a very high velocity, mostly in the sky plane.

Funder

National Research Foundation

Tata Institute of Fundamental Research

NASA Exoplanet Science Institute

National Aeronautics and Space Administration

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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