2019A&A...631A..22O


C.D.S. - SIMBAD4 rel 1.7 - 2020.02.25CET08:30:34

2019A&A...631A..22O - Astronomy and Astrophysics, volume 631A, 22-22 (2019/11-1)

Ubiquitous cold and massive filaments in cool core clusters.

OLIVARES V., SALOME P., COMBES F., HAMER S., GUILLARD P., LEHNERT M.D., POLLES F.L., BECKMANN R.S., DUBOIS Y., DONAHUE M., EDGE A., FABIAN A.C., McNAMARA B., ROSE T., RUSSELL H.R., TREMBLAY G., VANTYGHEM A., CANNING R.E.A., FERLAND G., GODARD B., PEIRANI S. and PINEAU DES FORETS G.

Abstract (from CDS):

Multi-phase filamentary structures around brightest cluster galaxies (BCG) are likely a key step of AGN-feedback. We observed molecular gas in three cool cluster cores, namely Centaurus, Abell S1101, and RXJ1539.5, and gathered ALMA (Atacama Large Millimeter/submillimeter Array) and MUSE (Multi Unit Spectroscopic Explorer) data for 12 other clusters. Those observations show clumpy, massive, and long (3-25kpc) molecular filaments, preferentially located around the radio bubbles inflated by the AGN. Two objects show nuclear molecular disks. The optical nebula is certainly tracing the warm envelopes of cold molecular filaments. Surprisingly, the radial profile of the Hα/CO flux ratio is roughly constant for most of the objects, suggesting that (i) between 1.2 and 6 times more cold gas could be present and (ii) local processes must be responsible for the excitation. Projected velocities are between 100 and 400km/s, with disturbed kinematics and sometimes coherent gradients. This is likely due to the mixing in projection of several thin (and as yet) unresolved filaments. The velocity fields may be stirred by turbulence induced by bubbles, jets, or merger-induced sloshing. Velocity and dispersions are low, below the escape velocity. Cold clouds should eventually fall back and fuel the AGN. We compare the radial extent of the filaments, rfil, with the region where the X-ray gas can become thermally unstable. The filaments are always inside the low-entropy and short-cooling-time region, where tcool/tff<20 (9 of 13 sources). The range of tcool/tff of 8-23 at rfil, is likely due to (i) a more complex gravitational potential affecting the free-fall time tff (sloshing, mergers, etc.) and (ii) the presence of inhomogeneities or uplifted gas in the ICM, affecting the cooling time tcool. For some of the sources, rfil lies where the ratio of the cooling time to the eddy-turnover time, tcool/teddy, is approximately unity.

Abstract Copyright: © V. Olivares et al. 2019

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: intracluster medium - galaxies: jets - galaxies: kinematics and dynamics - submillimeter: galaxies

Simbad objects: 32

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Number of rows : 32

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Phoenix Dwarf Galaxy Sy1 01 51 06.3 -44 26 41   13.48 13.2 12.69   ~ 442 2
2 NGC 708 BiC 01 52 46.482 +36 09 06.53 14.85 14.27 13.29 12.67 12.09 ~ 210 3
3 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 647 1
4 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 340 1
5 2MASX J03384056+0958119 LIN 03 38 40.568 +09 58 11.94   16.5       ~ 35 1
6 2MASX J07473129-1917403 BiC 07 47 31.296 -19 17 40.34   19.60       ~ 393 1
7 2MASX J08210226+0751479 BiC 08 21 02.2585309723 +07 51 47.233978089           ~ 11 0
8 RX J0821.0+0752 ClG 08 21 02.4 +07 51 47           ~ 49 1
9 NAME HYA SUPERCL SCG 08 57.9 +03 10           ~ 151 0
10 NAME Hya A LIN 09 18 05.651 -12 05 43.99   14.38 14.8     ~ 892 1
11 QSO B1104-445 QSO 11 07 08.6939954176 -44 49 07.617187122   17.84 18.2 17.37   ~ 178 1
12 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6104 3
13 NGC 4696 BiC 12 48 49.277 -41 18 39.92   11.21   10.7   ~ 450 3
14 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 962 2
15 ACO 1664 ClG 13 03 42.4 -24 14 44           ~ 110 0
16 3FHL J1304.2-2413 BLL 13 03 42.521 -24 14 42.81   16.95   15.83   ~ 28 1
17 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 3937 3
18 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1145 0
19 ACO 1796 ClG 13 50 16 -11 54.9           ~ 12 0
20 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 618 1
21 NAME SMM J14010+0252 Sy1 14 01 02.0854024806 +02 52 42.389426039   19.3       ~ 40 2
22 IC 4374 QSO 14 07 29.76224452 -27 01 04.2931696   13.61   11.79   ~ 118 3
23 ACO 3581 ClG 14 07 29.8 -27 01 04           ~ 162 3
24 QSO B1424-41 QSO 14 27 56.29756536 -42 06 19.4375991   18.48 17.7 16.30   ~ 337 1
25 2MASX J15393387-8335215 BiC 15 39 33.875 -83 35 21.52           ~ 8 0
26 2MAXI J1546-834 ClG 15 39 33.9 -83 35 32           ~ 18 0
27 NAME Curved Filament Rad 17 44 29 -29 01.6           ~ 10 1
28 ACO S 1101 ClG 23 13 58.5 -42 43 39           ~ 229 1
29 ESO 291-9 BiC 23 13 58.630 -42 43 39.31   14.68 14.6 14.537   ~ 47 3
30 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 487 0
31 2E 4728 LIN 23 25 19.731 -12 07 27.51   15.45 15.46     ~ 169 2
32 NAME Phoenix Cluster ClG 23 44 40.9 -42 41 54           ~ 115 0

    Equat.    Gal    SGal    Ecl

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2020.02.25-08:30:34

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