2013A&A...550A..81C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:29:13

2013A&A...550A..81C - Astronomy and Astrophysics, volume 550A, 81-81 (2013/2-1)

SiO collimated outflows driven by high-mass YSOs in G24.78+0.08.

CODELLA C., BELTRAN M.T., CESARONI R., MOSCADELLI L., NERI R., VASTA M. and ZHANG Q.

Abstract (from CDS):

The region G24.78+0.08, which is associated with a cluster of high-mass young stellar objects in different evolutionary stages, is one of the best laboratories to investigate massive star formation. We aim to image the molecular outflows towards G24.78+0.08 at high-angular resolution using SiO emission, which is considered the classical tracer of protostellar jets. In this way we study the mass loss process in which we previously detected a hypercompact ionised region, as well as rotation and infall signatures. We performed SiO observations with the VLA interferometer in the J=1-0 v=0 transition and with the SMA array in the 5-4 transition. A complementary IRAM 30-m single-dish survey in the (2-1), (3-2), (5-4), and (6-5) SiO lines was also carried out. Two collimated SiO high-velocity (up to 25km/s w.r.t. the systemic velocity) outflows driven by the A2 and C millimeter continuum massive cores have been imaged. On the other hand, we detected no SiO outflow driven by the young stellar objects in more evolved evolutionary phases that are associated with ultracompact (B) or hypercompact (A1) HII regions. The A2 outflow has also been traced using H2S. The LVG analysis of the SiO emission reveals high-density gas (103-104cm–3), with well constrained SiO column densities (0.5-1x1015cm–2). The driving source of the A2 outflow is associated with typical hot core tracers such as CH3OCHO (methyl formate), C2H3CN (vinyl cyanide), HCC13CN (cyanoacetilene), and (CH3)2CO (acetone). The driving source of the main SiO outflow in G24 has an estimated luminosity of a few 104L (typical of a late O-type star) and is embedded in the 1.3mm continuum core A2, which in turn is located at the centre of a hot core that rotates on a plane perpendicular to the outflow main axis. The present SiO images support a scenario similar to the low-mass case for massive star formation, where jets that are clearly traced by SiO emission, create outflows of swept-up ambient gas usually traced by CO.

Abstract Copyright:

Journal keyword(s): ISM: individual objects: G24.78+0.08 - ISM: molecules - stars: formation

Simbad objects: 24

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Number of rows : 24

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 LDN 1448 DNe 03 22.5 +30 35           ~ 466 0
2 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2001 1
3 3C 279 QSO 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2702 2
4 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3715 1
5 QSO B1741-038 QSO 17 43 58.85613396 -03 50 04.6166450     18.5 17.98   ~ 479 1
6 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1909 1
7 IRAS 18264-1152 cor 18 29 14.6846 -11 50 23.966           ~ 70 1
8 PMN J1832-1028 Rad 18 32 11.4 -10 28 13           ~ 12 0
9 GAL 024.78+00.08 HII 18 36.2 -07 13           ~ 73 0
10 NAME GAL 024.78+00.08 d Y*O 18 36 12.1 -07 11 59           ~ 5 0
11 [FCC2002] A2b Y*O 18 36 12.404 -07 12 08.50           ~ 4 0
12 [FCC2002] A2 Y*O 18 36 12.5 -07 12 10           ~ 18 0
13 [FCC2002] A1b Y*O 18 36 12.592 -07 12 11.00           ~ 5 0
14 [FCC2002] A1 Y*O 18 36 12.6 -07 12 11           ~ 29 0
15 [FCC2002] B Y*O 18 36 12.6 -07 12 09           ~ 8 0
16 [FCC2002] A1c Y*O 18 36 12.606 -07 12 12.00           ~ 5 0
17 NAME GAL 024.78+00.08 c Y*O 18 36 13.2 -07 11 59           ~ 10 0
18 IRAS 18566+0408 cor 18 59 10.3479 +04 12 18.220           ~ 119 1
19 QSO B1908-202 QSO 19 11 09.65289198 -20 06 55.1089891   18.21   18.14   ~ 235 0
20 IRAS 20126+4104 Y*O 20 14 25.8816186803 +41 13 36.869078243           B2.5-B0.5 396 0
21 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 484 0
22 LDN 1148 DNe 20 40 31.6 +67 21 45           ~ 59 0
23 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2505 2
24 IRAS 23151+5912 HII 23 17 21.0 +59 28 49           ~ 93 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:29:13

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