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.
© ESO, 2018
stars: formation - stars: early-type - ISM: individual objects: G47.06+0.26 - ISM: individual objects: N98 - HII regions
In ref list, Anderson et al. 2011 is 2011ApJS..194...32A, not 2011A&A...529L...6A.
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