2012A&A...546A..68A


Query : 2012A&A...546A..68A

2012A&A...546A..68A - Astronomy and Astrophysics, volume 546A, 68-68 (2012/10-1)

Winds of change - a molecular outflow in NGC 1377 ? The anatomy of an extreme FIR-excess galaxy.

AALTO S., MULLER S., SAKAMOTO K., GALLAGHER J.S., MARTIN S. and COSTAGLIOLA F.

Abstract (from CDS):

Our goal was to investigate the molecular gas distribution and kinematics in the extreme far-infrared (FIR) excess galaxy NGC 1377 and to address the nature and evolutionary status of the buried source. We used high- (0.65"x0.52", (65x52 pc)) and low- (4.88"x2.93") resolution SubMillimeter Array (SMA) observations to image the 12CO and 13CO 2-1 line emission. We find bright, complex 12CO 2-1 line emission in the inner 400 pc of NGC 1377. The 12CO 2-1 line has wings that are tracing a kinematical component that appears to be perpendicular to the component traced by the line core. Together with an intriguing X-shape of the integrated intensity and dispersion maps, this suggests that the molecular emission of NGC 1377 consists of a disk-outflow system. Lower limits to the molecular mass and outflow rate are Mout(H2)>1x107M and {dot}(M)>8M/yr. The age of the proposed outflow is estimated to be 1.4Myr, the extent to be 200pc and the outflow speed to be Vout=140km/s. The total molecular mass in the SMA map is estimated to Mtot(H2)=1.5x108M (on a scale of 400pc) while in the inner r=29pc the molecular mass is Mcore(H2)=1.7x107M with a corresponding H2 column density of N(H2)=3.4x1023cm–2 and an average 12CO 2-1 brightness temperature of 19K. 13CO 2-1 emission is found at a factor 10 fainter than 12CO in the low-resolution map while C18O 2-1 remains undetected. We find weak 1mm continuum emission of 2.4mJy with spatial extent less than 400pc. Observing the molecular properties of the FIR-excess galaxy NGC 1377 allows us to probe the early stages of nuclear activity and the onset of feedback in active galaxies. The age of the outflow supports the notion that the current nuclear activity is young - a few Myr. The outflow may be powered by radiation pressure from a compact, dust enshrouded nucleus, but other driving mechanisms are possible. The buried source may be an active galactic nucleus (AGN) or an extremely young (1Myr) compact starburst. Limitations on size and mass lead us to favor the AGN scenario, but additional studies are required to settle this question. In either case, the wind with its implied mass outflow rate will quench the nuclear power source within the very short time of 5-25Myr. It is possible, however, that the gas is unable to escape the galaxy and may eventually fall back onto NGC 1377 again.

Abstract Copyright:

Journal keyword(s): galaxies: evolution - galaxies: individual: NGC 1377 - galaxies: active - galaxies: starburst - radio lines: ISM - ISM: molecules

Simbad objects: 10

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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 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3049 2
2 NGC 1266 AGN 03 16 00.749 -02 25 38.53   14   12.46   ~ 265 1
3 QSO B0332-403 BLL 03 34 13.6547438706 -40 08 25.401996186 18.54 18.35 17.87 17.5   ~ 285 1
4 NGC 1377 GiG 03 36 39.077 -20 54 08.14   13.38   12.12   ~ 199 0
5 QSO B0338-214 BLL 03 40 35.60786053 -21 19 31.1720263   16.04 17.1 17.07   ~ 155 1
6 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1102 3
7 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5482 6
8 NGC 3256 IG 10 27 51.284 -43 54 13.55   11.83 11.33 10.62 11.9 ~ 781 2
9 QSO B1921-293 BLL 19 24 51.05595514 -29 14 30.1210524   18.71 18.21 15.07   ~ 738 0
10 3C 454.3 Bla 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2605 2

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2021.09.27-18:05:01

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