2020A&A...640A.104A


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.29CET21:50:52

2020A&A...640A.104A - Astronomy and Astrophysics, volume 640A, 104-104 (2020/8-1)

ALMA resolves the remarkable molecular jet and rotating wind in the extremely radio-quiet galaxy NGC 1377.

AALTO S., FALSTAD N., MULLER S., WADA K., GALLAGHER J.S., KONIG S., SAKAMOTO K., VLEMMINGS W., CECCOBELLO C., DASYRA K., COMBES F., GARCIA-BURILLO S., OYA Y., MARTIN S., VAN DER WERF P., EVANS A.S. and KOTILAINEN J.

Abstract (from CDS):

Submillimetre and millimetre line and continuum observations are important in probing the morphology, column density, and dynamics of the molecular gas and dust around obscured active galactic nuclei (AGNs) and their mechanical feedback. With very high-resolution (0.02"x0.03" (2x3pc)) ALMA 345GHz observations of CO 3-2, HCO+ 4-3, vibrationally excited HCN 4-3 ν2=1f, and continuum we have studied the remarkable, extremely radio-quiet, molecular jet and wind of the lenticular galaxy NGC 1377. The outflow structure is resolved, revealing a 150pc long, clumpy, high-velocity (∼600km/s), collimated molecular jet where the molecular emission is emerging from the spine of the jet with an average diameter of 3-7pc. The jet widens to 10-15pc about 25pc from the centre, which is possibly due to jet-wind interactions. A narrow-angle (50°-70°), misaligned and rotating molecular wind surrounds the jet, and both are enveloped by a larger-scale CO-emitting structure at near-systemic velocity. The jet and narrow wind have steep radial gas excitation gradients and appear turbulent with high gas dispersion (σ>40km/s). The jet shows velocity reversals that we propose are caused by precession, or more episodic directional changes. We discuss the mechanisms powering the outflow, and we find that an important process for the molecular jet and narrow wind is likely magneto-centrifugal driving. In contrast, the large-scale CO-envelope may be a slow wind, or cocoon that stems from jet-wind interactions. An asymmetric, nuclear r∼2pc dust structure with a high inferred molecular column density N(H2)≃1.8x1024cm–2 is detected in continuum and also shows compact emission from vibrationally excited HCN. The nuclear dust emission is hot (Td>180K) and its luminosity is likely powered by a buried AGN. The lopsided structure appears to be a warped disk, which is responsible for a significant part of the nuclear obscuration and possibly formed as a result of uneven gas inflows. The dynamical mass inside r=1.4pc is estimated to 9–3+2x106M, implying that the supermassive black hole (SMBH) has a high mass with respect to the stellar velocity dispersion of NGC 1377. We suggest that the SMBH of NGC 1377 is currently in a state of moderate growth, at the end of a more intense phase of accretion and also evolving from a state of more extreme nuclear obscuration. The nuclear growth may be fuelled by low-angular momentum gas inflowing from the gas ejected in the molecular jet and wind. Such a feedback-loop of cyclic outflows and central accretion could explain why there is still a significant reservoir of molecular gas in this ageing, lenticular galaxy. A feedback-loop would be an effective process in growing the nuclear SMBH and thus would constitute an important phase in the evolution of NGC 1377. This also invites new questions as to SMBH growth processes in obscured, dusty galaxies.

Abstract Copyright: © ESO 2020

Journal keyword(s): galaxies: evolution - galaxies: individual: NGC 1377 - galaxies: active - galaxies: nuclei - ISM: molecules - ISM: jets and outflows

VizieR on-line data: <Available at CDS (J/A+A/640/A104): list.dat fits/*>

Simbad objects: 10

goto Full paper

goto View the reference in ADS

Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 613 AGN 01 34 18.235 -29 25 06.56   10.77 12.71 9.50 10.6 ~ 352 3
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4141 2
3 QSO B0332-403 BLL 03 34 13.6547438706 -40 08 25.401996186 18.54 18.35 17.87 17.5   ~ 272 1
4 NGC 1377 GiG 03 36 39.077 -20 54 08.14   13.38   12.12   ~ 195 0
5 QSO B0338-214 BLL 03 40 35.60786053 -21 19 31.1720263   16.04 17.1 17.07   ~ 145 1
6 ESO 420-13 Sy2 04 13 49.699 -32 00 25.20   13.31 13.3 12.14   ~ 76 0
7 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1071 3
8 QSO B0521-365 BLL 05 22 57.9839686440 -36 27 30.847737786   15.26 14.62 14.48   ~ 726 2
9 NGC 4355 Sy2 12 26 54.628 -00 52 39.51   14.21 13.37     ~ 414 2
10 IC 5063 Sy2 20 52 02.329 -57 04 07.60   12.92 13.60 11.30   ~ 553 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2020A&A...640A.104A and select 'bookmark this link' or equivalent in the popup menu


2020.11.29-21:50:52

© Université de Strasbourg/CNRS

    • Contact