2018A&A...616A.171P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST06:21:22

2018A&A...616A.171P - Astronomy and Astrophysics, volume 616A, 171-171 (2018/8-1)

Spatially resolved cold molecular outflows in ULIRGs.

PEREIRA-SANTAELLA M., COLINA L., GARCIA-BURILLO S., COMBES F., EMONTS B., AALTO S., ALONSO-HERRERO A., ARRIBAS S., HENKEL C., LABIANO A., MULLER S., PIQUERAS LOPEZ J., RIGOPOULOU D. and VAN DER WERF P.

Abstract (from CDS):

We present new CO(2-1) observations of three low-z (d∼350Mpc) ultra-luminous infrared galaxy (ULIRG) systems (six nuclei) observed with the Atacama large millimeter/submillimeter array (ALMA) at high spatial resolution (∼500pc). We detect massive cold molecular gas outflows in five out of six nuclei (Mout~(0.3-5)x108M). These outflows are spatially resolved with deprojected effective radii between 250pc and 1kpc although high-velocity molecular gas is detected up to Rmax∼0.5-1.8kpc (1-6kpc deprojected). The mass outflow rates are 12-400M/yr and the inclination corrected average velocity of the outflowing gas is 350-550km/s (vmax=500-900km/s). The origin of these outflows can be explained by the strong nuclear starbursts although the contribution of an obscured active galactic nucleus cannot be completely ruled out. The position angle (PA) of the outflowing gas along the kinematic minor axis of the nuclear molecular disk suggests that the outflow axis is perpendicular to the disk for three of these outflows. Only in one case is the outflow PA clearly not along the kinematic minor axis, which might indicate a different outflow geometry. The outflow depletion times are 15-80Myr. These are comparable to, although slightly shorter than, the star-formation (SF) depletion times (30-80Myr). However, we estimate that only 15-30% of the outflowing molecular gas will escape the gravitational potential of the nucleus. The majority of the outflowing gas will return to the disk after 5-10Myr and become available to form new stars. Therefore, these outflows will not likely completely quench the nuclear starbursts. These star-forming powered molecular outflows would be consistent with being driven by radiation pressure from young stars (i.e., momentum-driven) only if the coupling between radiation and dust increases with increasing SF rates. This can be achieved if the dust optical depth is higher in objects with higher SF. This is the case in at least one of the studied objects. Alternatively, if the outflows are mainly driven by supernovae (SNe), the coupling efficiency between the interstellar medium and SNe must increase with increasing SF levels. The relatively small sizes (<1kpc) and dynamical times (<3Myr) of the cold molecular outflows suggests that molecular gas cannot survive longer in the outflow environment or that it cannot form efficiently beyond these distances or times. In addition, the ionized and hot molecular phases have been detected for several of these outflows, so this suggests that outflowing gas can experience phase changes and indicates that the outflowing gas is intrinsically multiphase, likely sharing similar kinematics, but different mass and, therefore, different energy and momentum contributions.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: active - galaxies: ISM - galaxies: kinematics and dynamics - galaxies: nuclei - galaxies: starburst

Simbad objects: 16

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Number of rows : 16

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 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2931 2
2 NGC 1614 AGN 04 34 00.027 -08 34 44.57   14.66 13.99     ~ 601 0
3 NGC 3256 IG 10 27 51.284 -43 54 13.55   11.83 11.33 10.62 11.9 ~ 755 2
4 ESO 320-30 H2G 11 53 11.722 -39 07 48.72   13.30   11.86   ~ 153 1
5 [CAB2000] Ns AGN 12 13 45.928 +02 48 39.00           ~ 25 0
6 LEDA 39024 LIN 12 13 46.107 +02 48 41.50           ~ 311 1
7 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5320 1
8 2MASX J14373831-1500239 Sy1 14 37 38.317 -15 00 23.97   16.58 16.40     ~ 244 1
9 [CGM90] IRAS 14348-1447 NE GiP 14 37 38.35 -15 00 21.3           ~ 18 0
10 QSO B1514-24 BLL 15 17 41.8135246339 -24 22 19.482167214   15.13 14.00 13.95   ~ 645 3
11 IC 4553 SyG 15 34 57.22396 +23 30 11.6084   14.76 13.88     ~ 2683 4
12 NGC 6240 Sy2 16 52 58.861 +02 24 03.55   14.31 13.37     ~ 1481 2
13 6dFGS gJ172322.0-001701 LIN 17 23 21.943 -00 17 00.96   15.1       ~ 373 0
14 [CGM90] IRAS 22491-1808 W GiP 22 51 49.20 -17 52 22.1           ~ 7 1
15 [CGM90] IRAS 22491-1808 E GiP 22 51 49.30 -17 52 22.5           ~ 7 1
16 NAME South America H2G 22 51 49.307 -17 52 23.96   16.97       ~ 286 3

    Equat.    Gal    SGal    Ecl

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2020.07.13-06:21:22

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