# 2012A&A...545A...3M

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 Query : 2012A&A...545A...3M

2012A&A...545A...3M - Astronomy and Astrophysics, volume 545A, 3-3 (2012/9-1)

13CO and C18O J=2-1 mapping of the environment of the class 0 protostellar core SMM 3 in Orion B9.

MIETTINEN O.

Abstract (from CDS):

Observations of molecular spectral lines provide information on the gas kinematics and chemistry of star-forming regions. We attempt to achieve a better understanding of the gas distribution and velocity field around the deeply embedded Class 0 protostar SMM 3 in the Orion B9 star-forming region. Using the APEX 12-m telescope, we mapped the line emission from the J=2-1 rotational transition of two CO isotopologues, 13CO and C18O, over a 4'x4' region around Orion B9/SMM 3. Both the 13CO and C18O lines exhibit two well-separated velocity components at about 1.3 and 8.7km/s. The emission of both CO isotopologues is more widely distributed than the submillimetre dust continuum emission as probed by LABOCA. The LABOCA 870-µm peak position of SMM 3 is devoid of strong CO isotopologue emission, which is consistent with our earlier detection of strong CO depletion in the source. No signatures of a large-scale outflow were found towards SMM 3. The 13CO and C18O emission seen at ∼1.3km/s is concentrated into a single clump-like feature at the eastern part of the map. The peak H2 column density towards a C18O maximum of the low-velocity component is estimated to be ∼1022cm–2. A velocity gradient was found across both the 13CO and C18O maps. Interestingly, SMM 3 lies on the border of this velocity gradient. The 13CO and C18O emission at ∼1.3km/s is likely to originate from the low-velocity part'' of Orion B. Our analysis suggests that it contains high density gas (∼1022 H2 molecules per cm2), which conforms to our earlier detection of deuterated species at similarly low radial velocities. Higher-resolution observations would be needed to clarify the outflow activity of SMM 3. The sharp velocity gradient in the region might represent a shock front resulting from the feedback from the nearby expanding HII region NGC 2024. The formation of SMM 3, and possibly of the other members of Orion B9, might have been triggered by this feedback.

Journal keyword(s): stars: formation - stars: protostars - ISM: clouds - ISM: individual objects: Orion B9/SMM 3 - submillimeter: ISM - ISM: kinematics and dynamics

Full paper

 Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HH 211 Y*O 03 43 56.52 +32 00 52.8           ~ 342 0
2 IC 348 OpC 03 44 32 +32 09.5           ~ 1327 1
3 Ass Ori OB 1b As* 05 34.0 -01 30           ~ 256 0
4 M 42 HII 05 35 01.5 -05 26 24           ~ 3953 0
5 NAME Flame Nebula HII 05 41 42.7 -01 54 44           ~ 698 1
6 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1291 0
7 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1119 1
8 HH 92 HH 05 42 21.1 -01 18 29           ~ 16 0
9 IRAS 05399-0121 Y*O 05 42 27.68 -01 20 01.0           ~ 40 0
10 NAME Ori B9 Cloud Cld 05 42 30.5 -01 20 33           ~ 20 0
11 [MHH2009c] SMM 3 smm 05 42 44.4 -01 16 03           ~ 9 0
12 [MHH2009c] SMM 7 smm 05 43 22.1 -01 13 46           ~ 7 0
13 IRAS 05413-0104 IR 05 43 51.5 -01 02 52           ~ 81 0
14 RAFGL 865 C* 06 04 00.04728 +07 25 52.0104           C-rich 98 0
15 * rho Oph ** 16 25 35.11766 -23 26 49.8150 4.30 4.85 4.63 4.27 3.96 B2IV+B2V 632 0
16 LDN 1746 DNe 17 11.3 -27 22           ~ 127 0
17 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 375 1

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2022.12.06-08:30:39