2018A&A...609A..43X


Query : 2018A&A...609A..43X

2018A&A...609A..43X - Astronomy and Astrophysics, volume 609A, 43-43 (2018/1-1)

Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26.

XU J.-L., XU Y., ZHANG C.-P., LIU X.-L., YU N., NING C.-C. and JU B.-G.

Abstract (from CDS):

Aims. We performed a multi-wavelength study toward the filamentary cloud G47.06+0.26 to investigate the gas kinematics and star formation.
Methods. We present the 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) observations of G47.06+0.26 obtained with the Purple Mountain Observation (PMO) 13.7m radio telescope to investigate the detailed kinematics of the filament. Radio continuum and infrared archival data were obtained from the NRAO VLA Sky Survey (NVSS), the APEX Telescope Large Area Survey of the Galaxy (ATLASGAL), the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) survey, and the Multi-band Imaging Photometer Survey of the Galaxy (MIPSGAL). To trace massive clumps and extract young stellar objects in G47.06+0.26, we used the BGPS catalog v2.0 and the GLIMPSE I catalog, respectively.
Results. The 12CO (J=1-0) and 13CO (J=1-0) emission of G47.06+0.26 appear to show a filamentary structure. The filament extends about 45' (58.1pc) along the east-west direction. The mean width is about 6.8pc, as traced by the 13CO (J=1-0) emission. G47.06+0.26 has a linear mass density of ∼361.5M/pc. The external pressure (due to neighboring bubbles and H II regions) may help preventing the filament from dispersing under the effects of turbulence. From the velocity-field map, we discern a velocity gradient perpendicular to G47.06+0.26. From the Bolocam Galactic Plane Survey (BGPS) catalog, we found nine BGPS sources in G47.06+0.26, that appear to these sources have sufficient mass to form massive stars. We obtained that the clump formation efficiency (CFE) is ∼18% in the filament. Four infrared bubbles were found to be located in, and adjacent to, G47.06+0.26. Particularly, infrared bubble N98 shows a cometary structure. CO molecular gas adjacent to N98 also shows a very intense emission. HII regions associated with infrared bubbles can inject the energy to surrounding gas. We calculated the kinetic energy, ionization energy, and thermal energy of two HII regions in G47.06+0.26. From the GLIMPSE I catalog, we selected some Class I sources with an age of ∼105yr, which are clustered along the filament. The feedback from the HII regions may cause the formation of a new generation of stars in filament G47.06+0.26.

Abstract Copyright: © ESO, 2018

Journal keyword(s): stars: formation - stars: early-type - ISM: individual objects: G47.06+0.26 - ISM: individual objects: N98 - HII regions

CDS comments: In ref list, Anderson et al. 2011 is 2011ApJS..194...32A, not 2011A&A...529L...6A.

Simbad objects: 17

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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 W 3 MoC 02 27 04.10 +61 52 27.1           ~ 1013 3
2 LDN 1641 MoC 05 39.0 -07 00           ~ 466 0
3 [ABB2014] WISE G046.965+00.315 bub 19 16 18.3 +12 36 39           ~ 5 0
4 BGPS G047.121+00.295 smm 19 16 40.3976 +12 44 19.783           ~ 5 0
5 [ERG2015] 6798 smm 19 16 40.9521 +12 38 09.231           ~ 7 0
6 [ERG2015] 6804 smm 19 16 41.3710 +12 47 52.041           ~ 6 0
7 [WWS2012] G047.05+00.25 cor 19 16 41.9410 +12 39 22.994           ~ 10 0
8 [WTG2015] G47 ISM 19 16.7 +12 40           ~ 9 1
9 [ABB2014] WISE G047.181+00.320 bub 19 16 42.0 +12 48 06           ~ 3 0
10 HRDS G047.028+00.232 HII 19 16 43.6 +12 37 35           ~ 5 1
11 BGPS G047.231+00.337 mm 19 16 43.8811 +12 51 20.592           ~ 4 0
12 BGPS G047.250+00.347 mm 19 16 44.0001 +12 52 41.072           ~ 4 0
13 BGPS G047.099+00.265 smm 19 16 44.4021 +12 42 19.353           ~ 5 0
14 BGPS G047.222+00.325 mm 19 16 45.5754 +12 50 34.967           ~ 4 0
15 [SPK2012] MWP1G047270+003500S bub 19 16 45.6 +12 53 45           ~ 2 0
16 [ABB2014] WISE G047.028+00.216 bub 19 16 46.2 +12 37 20           ~ 14 1
17 [ERG2015] 6808 smm 19 16 46.9861 +12 54 03.864           ~ 7 0

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2023.02.09-10:24:59

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