2010A&A...521A..65N


Query : 2010A&A...521A..65N

2010A&A...521A..65N - Astronomy and Astrophysics, volume 521, A65-65 (2010/10-1)

Energetics of the molecular gas in the H2 luminous radio galaxy 3C 326: evidence for negative AGN feedback.

NESVADBA N.P.H., BOULANGER F., SALOME P., GUILLARD P., LEHNERT M.D., OGLE P., APPLETON P., FALGARONE E. and PINEAU DES FORETS G.

Abstract (from CDS):

We present a detailed analysis of the gas conditions in the H2 luminous radio galaxy 3C 326 N at z∼0.1, which has a low star-formation rate (SFR∼0.07M/yr) in spite of a gas surface density similar to those in starburst galaxies. Its star-formation efficiency is likely a factor ∼10-50 lower than those of ordinary star-forming galaxies. Combining new IRAM CO emission-line interferometry with existing Spitzer mid-infrared spectroscopy, we find that the luminosity ratio of CO and pure rotational H2 line emission is factors 10-100 lower than what is usually found. This suggests that most of the molecular gas is warm. The Na D absorption-line profile of 3C 326 N in the optical suggests an outflow with a terminal velocity of ~-1800km/s and a mass outflow rate of 30-40M/yr, which cannot be explained by star formation. The mechanical power implied by the wind, of order 1043erg/s, is comparable to the bolometric luminosity of the emission lines of ionized and molecular gas. To explain these observations, we propose a scenario where a small fraction of the mechanical energy of the radio jet is deposited in the interstellar medium of 3C 326 N, which powers the outflow, and the line emission through a mass, momentum and energy exchange between the different gas phases of the ISM. Dissipation times are of order 107–8yrs, similar or greater than the typical jet lifetime. Small ratios of CO and PAH surface brightnesses in another 7 H2 luminous radio galaxies suggest that a similar form of AGN feedback could be lowering star-formation efficiencies in these galaxies in a similar way. The local demographics of radio-loud AGN suggests that secular gas cooling in massive early-type galaxies of ≥1011M could generally be regulated through a fundamentally similar form of ``maintenance-phase'' AGN feedback.

Abstract Copyright:

Journal keyword(s): galaxies: evolution - galaxies: ISM - galaxies: jets - radio continuum: galaxies - radio lines: galaxies

Simbad objects: 17

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Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NGC 315 LIN 00 57 48.8590525608 +30 21 08.842041360 12.80 12.20 11.16 11.26   ~ 750 2
2 NGC 383 rG 01 07 24.9647814840 +32 24 45.132586200   13.6 12.14     ~ 750 3
3 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5616 6
4 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6704 3
5 NAME Centaurus A Sy2 13 25 27.6039817176 -43 01 09.493008456   8.18 6.84 6.66   ~ 4262 3
6 3C 293.0 BLL 13 52 17.8719816576 +31 26 46.487381604   16.10 15.10     ~ 444 3
7 2MASX J15520913+2005477 G 15 52 09.1120432368 +20 05 48.211598760   17.87 17.08     ~ 137 1
8 2MASX J15520920+2005237 rG 15 52 09.1938375312 +20 05 23.180614152   17.87 17.08     ~ 126 2
9 3C 326 Rad 15 52 26.60 +20 06 00.0   17.87 17.08     ~ 214 3
10 3C 338.0 QSO 16 28 38.2446374616 +39 33 04.235250060   12.78 11.78     ~ 729 5
11 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13083 0
12 3C 386.0 rG 18 38 26.25747 +17 11 49.6210           ~ 191 1
13 NAME Cyg A Sy2 19 59 28.35645829 +40 44 02.0966496   16.22 15.10     ~ 2247 2
14 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 756 0
15 3C 424 BLL 20 48 12.030 +07 01 17.48   18 18.40     ~ 139 1
16 3C 443 Rad 22 13.9 +26 34           ~ 2 0
17 NAME Stephan's Quintet CGG 22 35 57.5 +33 57 36           ~ 397 1

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2022.08.09-02:42:43

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