2002A&A...387..931B


Query : 2002A&A...387..931B

2002A&A...387..931B - Astronomy and Astrophysics, volume 387, 931-943 (2002/6-1)

IRAS 05358+3543: Multiple outflows at the earliest stages of massive star formation.

BEUTHER H., SCHILKE P., GUETH F., McCAUGHREAN M., ANDERSEN M., SRIDHARAN T.K. and MENTEN K.M.

Abstract (from CDS):

We present a high-angular-resolution molecular line and millimeter continuum study of the massive star formation site IRAS 05358+3543. Observations with the Plateau de Bure Interferometer in CO 1-0, SiO 2-1 and H13CO+ 1-0 reveal at least three outflows which cannot be separated in single-dish data. Observations at millimeter and sub-millimeter wavelengths from the IRAM 30 m telescope and the CSO provide additional information on the region. The most remarkable feature is a highly collimated (collimation factor ∼10) and massive (>10 M) bipolar outflow of ∼1pc length, which is part of a quadrupolar outflow system. The three observed molecular outflows forming the IRAS 05358+3543 outflow system resemble, in structure and collimation, those typical of low-mass star-forming regions. They might therefore, just like low-mass outflows, be explained by shock entrainment models of jets. We estimate a mass accretion rate of ∼10–4M/yr, sufficient to overcome the radiative pressure of the central object and to build up a massive star, lending further support to the hypothesis that massive star formation occurs similarly to low-mass star formation, only with higher accretion rates and energetics. In the millimeter continuum, we find three sources near the center of the quadrupolar outflow, each with a mass of 75-100M. These cores are associated with a complex region of infrared reflection nebulosities and their embedded illuminating sources. The molecular line data show that SiO is found mostly in the outflows, whereas H13CO+ traces core-like structures, though likely with varying relative abundances. Thermal CH3OH comprises both features and can be disentangled into a core-tracing component at the line center, and wing emission following the outflows. A CO line-ratio study (using data of the J=1-0, 2-1 and 6-5 transitions) reveals local temperature gradients.

Abstract Copyright:

Journal keyword(s): molecular data - stars: early-type - stars: formation - stars: individual: IRAS 05358+3543 - ISM: jets and outflows

Nomenclature: Fig.7, Table 3: [BSG2002] mmN (Nos mm1-mm3).

Simbad objects: 22

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Number of rows : 22
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 HH 288 HH 00 37 13.6 +64 04 15           ~ 23 0
2 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 370 0
3 RAFGL 618 pA* 04 42 53.6242032600 +36 06 53.400902220   16.32   12.59   C-rich 1002 0
4 SH 2-233 HII 05 38 31.5 +35 51 19           ~ 66 1
5 IRAS 05358+3543 Y*O 05 39 09.92 +35 45 17.2           ~ 164 0
6 [BSG2002] mm3 mm 05 39 12.49 +35 45 55.2           ~ 20 0
7 [PCS2000] IR 93 IR 05 39 12.7 +35 45 53           ~ 5 0
8 [BSG2002] mm2 mm 05 39 12.78 +35 45 50.6           ~ 3 0
9 2MASS J05391280+3545430 * 05 39 12.80 +35 45 43.0           ~ 2 0
10 NAME IRAS 05358+3543 mm mm 05 39 13.0 +35 45 54           ~ 4 0
11 [BSG2002] mm1 mm 05 39 13.08 +35 45 50.5           ~ 15 0
12 SH 2-231 Y*O 05 39 13.2 +35 45 48           ~ 132 0
13 [PCS2000] IR 58 * 05 39 13.3 +35 45 54           ~ 4 0
14 SH 2-235 B HII 05 40 52.366 +35 41 29.43   17       ~ 179 1
15 SH 2-235 HII 05 41.1 +35 50           ~ 221 0
16 SH 2-232 HII 05 42 28 +36 11.4           ~ 54 0
17 6C 054850+375340 QSO 05 52 17.93691536 +37 54 25.2824392           ~ 28 1
18 GAL 192.16-03.82 HII 05 58 13.4 +16 32 00           ~ 143 1
19 IRAS 20126+4104 Y*O 20 14 25.8816769656 +41 13 36.879427236           B2.5-B0.5 441 0
20 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 802 0
21 4C 06.69 Bla 21 48 05.45866779 +06 57 38.6041877   16.85 16.47 15.06   ~ 676 1
22 Mol 160 Rad 23 40 54.5 +61 10 28           ~ 105 0

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