2009A&A...504..127F


Query : 2009A&A...504..127F

2009A&A...504..127F - Astronomy and Astrophysics, volume 504, 127-137 (2009/9-2)

Rotational structure and outflow in the infrared dark cloud 18223-3.

FALLSCHEER C., BEUTHER H., ZHANG Q., KETO E. and SRIDHARAN T.K.

Abstract (from CDS):

We examine an Infrared Dark Cloud (IRDC) at high spatial resolution as a means to study rotation, outflow, and infall at the onset of massive star formation. The IRDC 18223-3 was observed at 1.1mm and 1.3mm with the Submillimeter Array (SMA) and follow-up short spacing information was obtained with the IRAM 30m telescope. Additional data were taken at 3mm with the IRAM Plateau de Bure interferometer (PdBI). Submillimeter Array observations combined with IRAM 30m data in 12CO(2-1) reveal the outflow orientation in the IRDC 18223-3 region, and PdBI 3mm observations confirm this orientation in other molecular species. The implication of the outflow's presence is that an accretion disk is feeding it, so using line data for high density tracers such as C18O, N2H+, and CH3OH, we looked for indications of a velocity gradient perpendicular to the outflow direction. Surprisingly, this gradient turns out to be most apparent in CH3OH. The large size (28000 AU) of the flattened rotating object detected indicates that this velocity gradient cannot be due solely to a disk, but rather from inward spiraling gas within which a Keplerian disk likely exists. The rotational signatures can be modeled via rotationally infalling gas. From the outflow parameters, we derive properties of the source such as an outflow dynamical age of ∼37000years, outflow mass of ∼13M, and outflow energy of ∼1.7x1046erg. While the outflow mass and energy are clearly consistent with a high-mass star forming region, the outflow dynamical age indicates a slightly more evolved evolutionary stage than previous spectral energy distribution (SED) modeling indicates. The orientation of the molecular outflow associated with IRDC 18223-3 is in the northwest-southeast direction and velocity gradients orthogonal to the outflow reveal a large rotating structure likely harboring an accretion disk within. We also present a model of the observed methanol velocity gradient. The calculated outflow properties reveal that this is truly a massive star in the making. These data present evidence for one of the youngest known outflow/infall/disk systems in massive star formation. A tentative evolutionary picture for massive disks is discussed.

Abstract Copyright:

Journal keyword(s): stars: formation - stars: individual: IRDC 18223-3 - stars: early-type

VizieR on-line data: <Available at CDS (J/A+A/504/127): maps.dat fits/*>

Simbad objects: 13

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Number of rows : 13
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 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3794 3
2 GAL 192.16-03.82 HII 05 58 13.4 +16 32 00           ~ 137 1
3 3C 273 BLL 12 29 06.6998257176 +02 03 08.597629980   13.05 14.830 14.11   ~ 5584 1
4 3C 279 Bla 12 56 11.1663795384 -05 47 21.528432492   18.01 17.75 15.87   ~ 2889 2
5 QSO B1730-130 QSO 17 33 02.7055087032 -13 04 49.545516612   18 18.5 18.78 17.39 ~ 1067 1
6 QSO B1741-038 QSO 17 43 58.8561752304 -03 50 04.618401684     18.5 17.98   ~ 509 1
7 GRS G012.89 +00.49 HII 18 11 51.3 -17 31 29           ~ 162 0
8 NAME IRDC 18223-3 Y*O 18 25 08 -12 45.5           ~ 68 0
9 IRAS 18223-1243 Y*O 18 25 10.9307288448 -12 42 15.754722912           ~ 58 1
10 QSO B1908-202 QSO 19 11 09.6526857480 -20 06 55.109271780   18.21   18.14   ~ 253 0
11 IRAS 20126+4104 Y*O 20 14 25.8816769656 +41 13 36.879427236           B2.5-B0.5 416 0
12 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 756 0
13 3C 454.3 Bla 22 53 57.7480438728 +16 08 53.561508864   16.57 16.10 15.22   ~ 2691 2

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2022.08.18-04:13:42

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