2021A&A...656A..83Y


Query : 2021A&A...656A..83Y

2021A&A...656A..83Y - Astronomy and Astrophysics, volume 656A, 83-83 (2021/12-1)

Gas and stellar dynamics in Stephan's Quintet. Mapping the kinematics in a closely interacting compact galaxy group.

YTTERGREN M., MISQUITTA P., SANCHEZ-MONGE A., VALENCIA-S M., ECKART A., ZENSUS A. and PEITL-THIESEN T.

Abstract (from CDS):

In nearby compact galaxy groups we can study the complex processes of galaxy interactions at high resolution and obtain a window into a time in the history of the Universe when the galaxies were closely spaced and the intergalactic medium was awash with gas. Stephan's Quintet is a nearby compact galaxy group and a perfect laboratory for studying the process of galaxy evolution through galaxy harassment and interaction. By analysing the kinematics of Stephan's Quintet we aim to provide an increased understanding of the group, the history of the interactions, their cause and effect, and the details regarding the physical processes occurring as galaxies interact. Ionised gas and stellar kinematics have been studied using data from the Large Binocular Telescope, while the molecular gas kinematics have been obtained from CO observations using the IRAM 30m telescope. Large areas of the group have been mapped and analysed. We obtain a total ionised gas mass in the regions chosen for closer analysis of 20.1±0.2.1010M and a total H2 gas mass of 21±2.109M in the observed area (spectra integrated over the velocity range covering Stephan's Quintet), while the star-forming clouds show an impressive complexity, with gas congregations at multiple velocities at many locations throughout the group. We map the large-scale nuclear wind in NGC7319 and its decoupled gas and stellar disk. With our high resolution data we can, for the first time, reveal the Seyfert 1 nature of NGC7319 and fit the narrow-line region and broad-line region of the Hα line. While the 12CO (1 - 0) map shows significant emission in the area in or near NGC7319, the bridge, and the star-forming ridge, the 12CO (2 - 1) emission shows a prevalence to the star-forming ridge, an area south of the NGC7318 pair, and shows an extension towards NGC7317 - connecting NGC7317 to the centre of the group, indicating a previous interaction. NGC7317 may also be a prime candidate for studies of the process of galaxy harassment. Furthermore, we connect the kinematical structures in Stephan's Quintet to the history of the group and the ongoing interaction with NGC7318B. Through our extensive observations of Stephan's Quintet we trace and present the kinematics and evolution of the complex processes and structures occurring in this nearby interactive group.

Abstract Copyright: © M. Yttergren et al. 2021

Journal keyword(s): galaxies: evolution - galaxies: kinematics and dynamics - galaxies: groups: individual: Stephan's Quintet

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 BD+52 913 WD* 05 05 30.6180977592 +52 49 51.919301604 10.25 11.44 11.69 11.93 12.108 DA.8 1058 0
2 BD+33 2642 pA* 15 51 59.8854348048 +32 56 54.329485272 9.806 10.61 10.73 10.884 10.961 O7p 410 0
3 4C 31.63 BLL 22 03 14.9756830008 +31 45 38.269473228   15.85 15.58 14.33   ~ 479 1
4 NGC 7317 Sy2 22 35 51.8681746944 +33 56 41.758033380 15.10 14.57 13.60 12.72   ~ 167 1
5 NGC 7318A GiP 22 35 56.85 +33 57 54.3   14.4   13.13   ~ 129 0
6 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 404 1
7 NGC 7318 IG 22 35 57.912 +33 57 56.27           ~ 38 0
8 NGC 7318B GiP 22 35 58.3903354632 +33 57 57.827617524   14.06   12.47   ~ 132 0
9 NGC 7320 GiG 22 36 03.4059680280 +33 56 53.623460220 13.12 13.23 12.63 12.38   ~ 185 3
10 NGC 7319 Sy2 22 36 03.602 +33 58 33.18   14.57 13.53 12.65   ~ 275 0
11 NGC 7320C G 22 36 20.3659207800 +33 59 06.140904000   17       ~ 46 0
12 3C 454.3 Bla 22 53 57.7480438728 +16 08 53.561508864   16.57 16.10 15.22   ~ 2728 2

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2023.01.30-21:28:55

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