2022A&A...666A..94O


Query : 2022A&A...666A..94O

2022A&A...666A..94O - Astronomy and Astrophysics, volume 666A, 94 (2022/10-1)

Gas condensation in brightest group galaxies unveiled with MUSE Morphology and kinematics of the ionized gas.

OLIVARES V., SALOME P., HAMER S.L., COMBES F., GASPARI M., KOLOKYTHAS K., O'SULLIVAN E., BECKMANN R.S., BABUL A., POLLES F.L., LEHNERT M., LOUBSER S.I., DONAHUE M., GENDRON-MARSOLAIS M.-L., LAGOS P., PINEAU DES FORETS G., GODARD B., ROSE T., TREMBLAY G., FERLAND G. and GUILLARD P.

Abstract (from CDS):

The origin of the cold gas in central galaxies in groups is still a matter of debate. We present Multi-Unit Spectroscopic Explorer (MUSE) observations of 18 optically selected local (z ≤ 0.017) brightest group galaxies (BGGs) to study the kinematics and distribution of the optical emission-line gas. MUSE observations reveal a distribution of gas morphologies including ten complex networks of filaments extending up to ∼10 kpc to two compact (< 3 kpc) and five extended (> 5 kpc) disk-dominated structures. Some rotating disks show rings and elongated structures arising from the central disk. The kinematics of the stellar component is mainly rotation-dominated, which is very different from the disturbed kinematics and distribution found in the filamentary sources. The ionized gas is kinematically decoupled from the stellar component for most systems, suggesting an external origin for the gas. We also find that the Hα luminosity correlates with the cold molecular gas mass. By exploring the thermodynamical properties of the X-ray atmospheres, we find that the filamentary structures and compact disks are found in systems with small central entropy values, K, and tcool/teddy ratios. This suggests that, similar to brightest cluster galaxies (BCGs) in cool core clusters, the ionized filaments and the cold gas associated to them are likely formed from hot halo gas condensations via thermal instabilities, which is consistent with the chaotic cold accretion simulations (as shown via the C ratio, Tat, and k plot). We note that the presence of gaseous rotating disks is more frequent than in BCGs. An explanation for the origin of the gas in those objects is a contribution to gas fueling by wet mergers or group satellites, as qualitatively hinted at by some sources of the present sample. Nonetheless, we discuss the possibility that some extended disks could also be a transition stage in an evolutionary sequence including filaments, extended disks, and compact disks, as described by hot gas condensation models of cooling flows.

Abstract Copyright: © V. Olivares et al. 2022

Journal keyword(s): galaxies: groups: general - galaxies: clusters: intracluster medium - galaxies: kinematics and dynamics - methods: observational - techniques: imaging spectroscopy

Simbad objects: 45

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Number of rows : 45
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 LGG 9 GrG 00 39 09 +02 53.0           ~ 7 0
2 NGC 193 rG 00 39 18.5878961880 +03 19 52.605787764   14.3       ~ 141 1
3 LGG 18 GrG 01 10 41.2 +32 11 23           ~ 11 0
4 NGC 410 GiG 01 10 58.9016492712 +33 09 07.053878052 13.08 12.52 11.48     ~ 155 2
5 NGC 584 Sy2 01 31 20.7231919800 -06 52 04.770287472 11.93 11.44 10.48     ~ 403 2
6 NAME NGC 584 Group GrG 01 33 21.4 -07 01 17           ~ 20 0
7 LGG 31 GrG 01 48 28.3 +11 59 06           ~ 4 0
8 NGC 677 GiG 01 49 14.0467760952 +13 03 19.235854008   14.3       ~ 81 0
9 NGC 777 Sy2 02 00 14.9065707744 +31 25 45.850721628 13.09 12.49 11.45     ~ 182 2
10 LGG 42 GrG 02 00 38 +32 10.8           ~ 8 0
11 NGC 924 GiG 02 26 46.8206455368 +20 29 51.036018756   13.8       ~ 64 0
12 LGG 58 GrG 02 28 27 +31 32.5           ~ 6 0
13 LGG 61 GrG 02 29 19 +20 21.2           ~ 6 0
14 NGC 940 GiG 02 29 27.5145865368 +31 38 27.587114304   13.4       ~ 42 0
15 NGC 978 GiG 02 34 46.9664367984 +32 50 46.296266352   13.3       ~ 38 0
16 MCG+05-07-017 GiP 02 34 48.1 +32 50 29   15       ~ 9 0
17 LGG 66 GrG 02 35 56.9 +32 55 49           ~ 6 0
18 LGG 72 GrG 02 42 41.4 +32 25 13           ~ 5 0
19 NGC 1060 GiG 02 43 15.045 +32 25 30.04 13.71 13.00 11.81     ~ 112 1
20 NGC 1167 LIN 03 01 42.3322774176 +35 12 20.300948892   13.84 12.77     ~ 357 2
21 ACO 426 ClG 03 19 47.2 +41 30 47           ~ 2269 1
22 LGG 103 GrG 03 43 07.8 -04 18 07           ~ 13 0
23 NGC 1453 EmG 03 46 27.2307890592 -03 58 07.831476768   13   11.30   ~ 181 0
24 NGC 1587 GiP 04 30 39.9359019384 +00 39 41.922470340   13.3       ~ 141 0
25 NGC 1588 GiP 04 30 43.77 +00 39 53.0   14.1       ~ 83 0
26 LGG 117 GrG 04 31 53.6 +00 32 58           ~ 7 0
27 NGC 2563 GiG 08 20 35.6870161656 +21 04 04.111020012   13.7 12.39     ~ 155 1
28 NAME Hya A LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 1014 1
29 NGC 4008 GiG 11 58 17.0179882800 +28 11 32.877043224   13.1       ~ 78 0
30 LGG 262 GrG 11 58 24.6 +27 50 01           ~ 5 0
31 NGC 4169 Sy2 12 12 18.7701840312 +29 10 45.851425968   12.9 12.34 11.67   ~ 142 1
32 LGG 276 GrG 12 12 43.2 +29 01 07           ~ 10 0
33 LGG 278 GrG 12 17 45.9 +06 09 17           ~ 9 0
34 NGC 4261 LIN 12 19 23.2160630 +05 49 29.700024   13.92 12.87     ~ 1227 0
35 NGC 4636 LIN 12 42 49.8333280080 +02 41 15.951929028   12.62 11.84     ~ 1119 1
36 ESO 507-25 LIN 12 51 31.846 -26 27 07.74   12.47   10.91 11.9 ~ 84 0
37 LGG 310 GrG 12 52 29 -26 36.9           ~ 7 0
38 ACO 1664 ClG 13 03 42.4 -24 14 44           ~ 127 0
39 NGC 5044 BiC 13 15 23.9607836592 -16 23 07.547751744   11.9   10.74   ~ 503 0
40 NAME NGC 5846 Group GrG 15 05 47.0 +01 34 25           ~ 153 0
41 NGC 5846 BiC 15 06 29.253 +01 36 20.29   11.9   9.74   ~ 853 1
42 LGG 421 GrG 18 32 43 +22 40.3           ~ 4 0
43 NGC 6658 GiG 18 33 55.6327067976 +22 53 17.737619712   15.0       ~ 44 0
44 NGC 7619 GiG 23 20 14.524 +08 12 22.63   12.7       ~ 450 0
45 NAME NGC 7619 Group GrG 23 20 32.1 +08 22 26           ~ 45 0

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