2016A&A...593A..30M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.09CEST23:36:00

2016A&A...593A..30M - Astronomy and Astrophysics, volume 593A, 30-30 (2016/9-1)

Another piece of the puzzle: The fast H I outflow in Mrk 231.

MORGANTI R., VEILLEUX S., OOSTERLOO T., TENG S.H. and RUPKE D.

Abstract (from CDS):

We present the detection, performed with the Westerbork Synthesis Radio Telescope (WSRT) and the Karl Jansky Very Large Array (VLA), of a fast HI 21cm outflow in the ultra-luminous infrared galaxy Mrk 231. The outflow is observed as shallow HI absorption blueshifted ∼1300km/s with respect to the systemic velocity and located against the inner kpc of the radio source. The outflowing gas has an estimated column density between 5 and 15x1018Tspin/cm2. We derive the Tspin to lie in the range 400-2000K and the corresponding HI densities are nHI∼10-100cm–3. Our results complement previous findings and confirm the multiphase nature of the outflow in Mrk 231. Although effects of the interaction between the radio plasma and the surrounding medium cannot be ruled out, the energetics and the lack of a clear kpc-scale jet suggest that the most likely origin of the HI outflow is a wide-angle nuclear wind, as earlier proposed to explain the neutral outflow traced by NaI and molecular gas in this source. Our results suggest that an HI component is present in fast outflows regardless of the acceleration mechanism (wind vs. jet driven) and that it must be connected with common properties of the pre-interaction gas involved. Considering the observed similarity of their column densities, the HI outflow likely represents the inner part of the broad wind identified on larger scales in atomic NaI. The mass outflow rate of the HI outflow (between 8 and 18M/yr) does not appear to be as large as that observed in molecular gas, partly owing to the smaller sizes of the outflowing region sampled by the HI absorption. These characteristics are commonly seen in other cases of outflows driven by the active galactic nucleus (AGN) suggesting that the HI may represent a short intermediate phase in the rapid cooling of the gas. The results further confirm HI as a good tracer for AGN-driven outflows not only in powerful radio sources. We also obtained deeper continuum images than previously available. They confirm the complex structure of the radio continuum originating both from the AGN and star formation. At the resolution obtained with the VLA (∼1'') we do not see a kpc-scale jet. Instead, we detect a plateau of emission, likely due to star formation, surrounding the bright nuclear region. We also detect a poorly collimated bridge which may represent the channel feeding the southern lobe. The unprecedented depth of the low-resolution WSRT image reveals radio emission extending 50'' (43kpc) to the south and 20'' (17kpc) to the north.

Abstract Copyright: © ESO, 2016

Journal keyword(s): galaxies: active - galaxies: individual: Mrk 231 - ISM: jets and outflows - radio lines: galaxies

VizieR on-line data: <Available at CDS (J/A+A/593/A30): fig4.dat list.dat fits/*>

Simbad objects: 9

goto Full paper

goto View the reference in ADS

Number of rows : 9

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 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4093 2
2 NGC 3079 Sy2 10 01 57.80342 +55 40 47.2428 11.57 11.54 10.86     ~ 1248 3
3 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1779 3
4 ICRF J131337.8+545823 Sy2 13 13 37.85316548 +54 58 23.8993959     21.735 20.374   ~ 28 1
5 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3716 1
6 ICRF J134733.3+121724 Sy2 13 47 33.36161542 +12 17 24.2402572   19.28 18.44 15.718   ~ 524 3
7 UGC 8782 LIN 13 52 17.765 +31 26 46.10   16.10 15.10     ~ 420 3
8 IC 1065 Sy2 14 49 21.5921149894 +63 16 13.816373757   17.30 16.39     ~ 333 1
9 IC 5063 Sy2 20 52 02.329 -57 04 07.60   12.92 13.60 11.30   ~ 545 1

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2016A&A...593A..30M and select 'bookmark this link' or equivalent in the popup menu


2020.07.09-23:36:00

© Université de Strasbourg/CNRS

    • Contact