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J/A+A/608/A102      APEX CO and HI observations of Lupus I  (Gaczkowski+, 2017)

Squeezed between shells? On the origin of the Lupus I molecular cloud. II. APEX CO and GASS HI observations. Gaczkowski B., Roccatagliata V., Flaischlen S., Kroell D., Krause M.G.H. Burkert A., Diehl R., Fierlinger K., Ngoumou J., Preibisch T. <Astron. Astrophys. 608, A102 (2017)> =2017A&A...608A.102G (SIMBAD/NED BibCode)
ADC_Keywords: Carbon monoxide ; H II regions ; Infrared sources ; Interstellar medium Keywords: ISM: bubbles - ISM: clouds - ISM: kinematics and dynamics - ISM: structure - ISM: molecules - radio lines: ISM Abstract: Lupus I cloud is found between the Upper Scorpius (USco) and Upper Centaurus-Lupus (UCL) subgroups of the Scorpius-Centaurus OB association, where the expanding USco HI shell appears to interact with a bubble currently driven by the winds of the remaining B stars of UCL. Aims. We investigate whether the Lupus I molecular could have formed in a colliding flow, and in particular, how the kinematics of the cloud might have been influenced by the larger scale gas dynamics. We performed APEX 13CO(2-1)and C18O(2-1) line observations of three distinct parts of Lupus I that provide kinematic information on the cloud at high angular and spectral resolution. We compare those results to the atomic hydrogen data from the GASS HI survey and our dust emission results presented in the previous paper. Based on the velocity information, we present a geometric model for the interaction zone between the USco shell and the UCL wind bubble. We present evidence that the molecular gas of Lupus Iis tightly linked to the atomic material of the USco shell. The CO emission in Lupus Iis found mainly at velocities between vLSR=3-6km/s, which is in the same range as the HI velocities. Thus, the molecular cloud is co-moving with the expanding USco atomic HI shell. The gas in the cloud shows a complex kinematic structure with several line-of-sight components that overlay each other. The nonthermal velocity dispersion is in the transonic regime in all parts of the cloud and could be injected by external compression. Our observations and the derived geometric model agree with a scenario in which Lupus Iis located in the interaction zone between the USco shell and the UCL wind bubble. The kinematics observations are consistent with a scenario in which the Lupus Icloud formed via shell instabilities. The particular location of Lupus I between USco and UCL suggests that counterpressure from the UCL wind bubble and pre-existing density enhancements, perhaps left over from the gas stream that formed the stellar subgroups, may have played a role in its formation. Description: The FITS files contain the data cubes corresponding to the 13CO(3-2) and C18O(3-2) lines. They were taken using the Atacama Pathfinder EXperiment (APEX) telescope, with an angular resolution of 30" and a velocity resolution of 0.1km/s. Objects: ----------------------------------------- RA (2000) DE Designation(s) ----------------------------------------- 15 40 05.35 -33 36 44.4 Cut A (center) 15 42 49.80 -34 08 37.8 Cut B (center) 15 44 57.60 -34 17 13.3 Cut C (center) ----------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 114 6 List of FITS datacubes fits/* 0 6 Individual fits data cubes
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 21 I2 arcsec/pix Scale Scale of the image 23- 25 I3 --- Nx Number of pixels along X-axis 27- 29 I3 --- Ny Number of pixels along Y-axis 31- 34 I4 --- Nz Number of slides 36- 40 F5.1 km/s bVLSR Lower value of velocity interval 42- 46 F5.1 km/s BVLSR Upper value of velocity interval 48- 50 F3.1 km/s dVLSR Velocity resolution 52- 56 I5 Kibyte size Size of FITS file 58- 61 A4 --- Mol Molecule name 63- 92 A30 --- FileName Name of FITS file, in subdirectory fits 94-114 A21 --- Title Title of the file
Acknowledgements: Veronica Roccatagliata, roccatagliata(at)arcetri.astro.it References: Gaczkowski et al., Paper I 2015A&A...584A..36G
(End) Patricia Vannier [CDS] 14-Dec-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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