2021A&A...656A..55M


Query : 2021A&A...656A..55M

2021A&A...656A..55M - Astronomy and Astrophysics, volume 656A, 55-55 (2021/12-1)

Taking snapshots of the jet-ISM interplay: The case of PKS 0023-26.

MORGANTI R., OOSTERLOO T., TADHUNTER C., BERNHARD E.P. and OONK J.B.R.

Abstract (from CDS):

We present high angular resolution (0.13-0.4 arcsec) ALMA CO(2-1) and 1.7 mm continuum observations of the far-infrared-bright galaxy PKS 0023-26 (z = 0.32), which hosts a young radio source as well as a luminous optical active galactic nucleus (AGN). Although young, the powerful radio source has already grown to a size of a few kiloparsec, making it potentially capable of affecting the interstellar medium (ISM) of the host galaxy. We detect a very extended distribution of molecular gas with a mass between 0.3 and 3 x 1010 M, depending on the XCO conversion factor. The gas has a maximum radial extent of ∼5 arcsec (24 kpc) from the nucleus and is distributed in an asymmetric structure offset from the radio galaxy and with a fairly smooth velocity gradient. At large radii, tails of gas are observed in the direction of companion galaxies, suggesting that tidal interactions may be responsible for the origin of the gas. Overall, the observed properties are reminiscent of the molecular structures observed in some galaxy clusters. However, in the inner few kiloparsec, across the entire extent of the radio continuum, the kinematics of the gas appears to be affected by the radio source. In the central, sub-kiloparsec region, we observe the brightest emission from the molecular gas and the broadest velocity profiles with a full width at zero intensity (FWZI) of ∼500 km s–1, which indicate that in this region a direct interaction of the jet with dense clouds and outflowing molecular gas is happening. On larger, kiloparsec-scales, the molecular gas appears to avoid the radio lobes, while gas with a somewhat smaller velocity dispersion (FWZI of ∼350 km s–1) is observed around the radio lobes. Thus, in these regions, the gas appears to be affected by the expanding cocoon surrounding the radio source, likely dispersing and heating preexisting molecular clouds. The observations suggest that the mode of coupling between radio jets and the ISM changes from an outflowing phase limited to the sub-kiloparsec region to a maintenance phase, excavating cavities devoid of dense gas, at larger radii. This reveals that, already on galaxy scales, the impact of the AGN is not limited to outflows. This is in accordance with predictions from numerical simulations. With a star-formation rate of 25 M yr–1, PKS 0023-26 is located on the SFR-M* relation for star forming galaxies. Thus, the AGN does not appear to have, at present, a major impact on the host galaxy in terms of the overall level of star-formation activity. However, as the jet and lobes expand throughout the galaxy in the coming few x107 yr, they will carry enough energy to be able to prevent further gas cooling and/or to inject turbulence and thus affect future star formation.

Abstract Copyright: © ESO 2021

Journal keyword(s): galaxies: active - galaxies: individual: PKS 0023-26 - ISM: jets and outflows - radio lines: galaxies

Status at CDS : Examining the need for a new acronym.

Simbad objects: 20

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Number of rows : 20
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 QSO B0023-263 BLL 00 25 49.15629900 -26 02 12.6141092   20.30 19.5 18.084   ~ 154 1
2 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 682 1
3 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1533 0
4 IC 450 Sy1 06 52 12.3346265592 +74 25 37.121227716   15.16 14.19     ~ 541 1
5 3C 171.0 Sy2 06 55 14.7 +54 08 59   19.94 19.08     ~ 251 0
6 NAME Hya A LIN 09 18 05.66848602 -12 05 43.8060823   14.38 14.8     ~ 980 1
7 NGC 3801 LIN 11 40 16.9446846648 +17 43 40.575768960   13.3       ~ 196 1
8 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5637 1
9 3C 277.3 BLL 12 54 12.0071453880 +27 37 33.952663740   15.94       ~ 358 1
10 NAME Centaurus A Sy2 13 25 27.61521044 -43 01 08.8050291   8.18 6.84 6.66   ~ 4320 3
11 MCG+05-33-005 LIN 13 48 52.4892734448 +26 35 34.353002688   14.0       ~ 228 2
12 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1220 0
13 NAME Teacup AGN Sy2 14 30 29.8820644560 +13 39 12.007458684   16.89 16.64     ~ 49 0
14 IC 1065 Sy2 14 49 21.5927137128 +63 16 13.799495280   17.30 16.39     ~ 353 1
15 QSO B1549-790 QSO 15 56 58.86979525 -79 14 04.2817241   18.80 18.800 17.84   ~ 194 1
16 IC 5063 Sy2 20 52 02.329 -57 04 07.60   12.92 13.60 11.30   ~ 611 1
17 LEDA 2831507 Sy2 22 53 03.1 -40 57 46     20.0     ~ 102 1
18 ICRF J225805.9-275821 Sy1 22 58 05.96287687 -27 58 21.2567572   17.34 16.77 17.20   ~ 335 1
19 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 526 0
20 2E 4728 LIN 23 25 19.731 -12 07 27.51   15.45 15.46     ~ 172 2

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2023.01.31-01:48:44

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