MUSE sneaks a peek at extreme ram-pressure events^⋆

III. Tomography of UGC 6697, a massive galaxy falling into Abell 1367

¹ Università degli Studi di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano, Italy
e-mail: guido.consolandi@mib.infn.it
² Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, 85748 Garching, Germany
³ Universitäts-Sternwarte München, Schenierstrasse 1, 81679 München, Germany
⁴ Institute for Computational Cosmology, and Centre for Extragalactic Astronomy, Durham University, South Road, Durham, DH1 3LE, UK
⁵ Aix-Marseille Univ., CNRS, LAM, Laboratoire d’Astrophysique de Marseille, 130313 Marseille, France
⁶ Optical and Infrared Astronomy Division, National Astronomical Observatory of Japan, Mitaka, 181-8588 Tokyo, Japan
⁷ Graduate School of Science and Engineering, Hosei University, 3-7-2, Kajinocho, Koganei, 184-8584 Tokyo, Japan
⁸ Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1, Kagamiyama, Higashi-Hiroshima, 739-8526 Hiroshima, Japan

Received: 22 May 2017
Accepted: 19 July 2017

Abstract

We present the MUSE observations of UGC 6697, a giant (M_∗ ≈ 10¹⁰M_⊙) spiral galaxy infalling in the nearby cluster Abell 1367. During its high-velocity transit through the intracluster medium (ICM), the hydrodynamical interactions with the ICM produce a ≈ 100 kpc tail of ionized gas that we map with a mosaic of five MUSE pointings up to 60 kpc from the galaxy. CGCG 97087N, a small companion that lies at few arcminutes in projection from UGC 6697, is also showing signs of the hydrodynamic action of the ICM of the cluster. Along the whole extent of the tail, we detect diffuse Hα emission, and to a lesser extent, Hβ, [OIII]λ5007, and [OI]λ6300. By comparing the kinematics and distribution of gas and stars (as traced by the CaII triplet) for both galaxies, we separate the ionized gas, as traced by the Hα line, into a component that is still bound to the galaxy and a component that is stripped. We find that the bound component shows a low-velocity dispersion and line ratios consistent with photoionization by hot stars. The stripped gas is more turbulent, with velocity dispersions up to ≳100 km s^-1, and is excited by shocks, as traced by high values of [OI]/Hα and [NII]/Hα ratio. In the tail of UGC 6697, we identify numerous bright compact knots with line ratios typical of HII regions. These are distributed along the only streams of stripped gas that retain low-velocity dispersions (≲35 km s^-1). Despite being in the stripped gas, their physical properties are not different from normal HII regions in galactic disks. We find evidence of a past fast encounter between the two galaxies in the form of a double tail emerging from CGCG 97087N that connects with UGC 6697. This encounter might have increased the efficiency of the stripping process, leaving the stellar distribution and kinematics unaltered.