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J/A+A/608/A21         Radio cubes of G82.65-2.00               (Saajasto+, 2017)

Correlation of gas dynamics and dust in the evolved filament G82.65-02.00. Saajasto M., Juvela M., Dobashi K., Shimoikura T., Ristorcelli I., Montillaud J., Marshall D.J., Malinen J., Pelkonen V.-M., Feher O., Rivera-Ingraham A., Toth L.V., Montier L., Bernard J-P., Onishi T. <Astron. Astrophys. 608, A21 (2017)> =2017A&A...608A..21S (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Radio sources ; Molecular clouds Keywords: ISM: clouds - dust, extinction - ISM: structure - ISM: kinematics and dynamics - ISM: lines and bands Abstract: The combination of line and continuum observations can provide vital insight into the formation and fragmentation of filaments and the initial conditions for star formation. We have carried out line observations to map the kinematics of an evolved, actively star forming filament G82.65-2.00. The filament was first identified from the Planck data as a region of particularly cold dust emission and was mapped at 100-500m as a part of the Herschel key program Galactic Cold Cores. The Herschel observations cover the central part of the filament, corresponding to a filament length of ∼12pc at the assumed distance of 620pc. CO observations show that the filament has an intriguing velocity field with several velocity components around the filament. In this paper, we study the velocity structure in detail, to quantify possible mass accretion rate onto the filament, and study the masses of the cold cores located in the filament. We have carried out line observations of several molecules, including CO isotopologues, HCO+, HCN, and CS with the Osaka 1.85m telescope and the Nobeyama 45m telescope. The spectral line data are used to derive velocity and column density information. Description: This catalogue contains the radio data cubes of cold filament G82.65-2.00. The catalogue contains all of the observed molecular lines, however, please note that not all of the observed molecules were detected. The included data has been obtained from two telescopes, The 1.8 meter telescope located in Osaka Japan, and the 45 meter telescope located in Nobeyama, Japan. The data cubes are calibrated and a varying main beam efficiency correction, depending on the observed frequencies, was applied to scale the data to units of main beam temperature Tmb. For the Nobeyama observations, the frequency channels were re-sampled onto a 0.025km/s velocity grid, and smoothed to 0.2km/s resolution to reduce the noise. Overall, the noise levels are in the range of 0.1-0.5K for a velocity resolution of 0.2km/s. The velocity resolution of the Osaka observations is 0.07km/s at 230GHz and the Corresponding noise level is ∼0.6K. The Osaka observations cover almost the same area observed by Herschel space observatory, however, The Nobeyama observations only cover the central region of the field. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 130 23 List of datacubes fits/* 0 23 Individual fits datacubes
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) 21- 23 I3 --- Nx Number of pixels along X-axis 25- 27 I3 --- Ny Number of pixels along Y-axis 29- 32 I4 --- Nz Number of slices 34- 43 A10 "date" Obs.Date Observation date 45- 53 F9.4 km/s bVel Lower value of velocity interval 55- 62 F8.4 km/s BVel Upper value of velocity interval 64- 72 F9.7 km/s dVel Velocity resolution 74- 79 I6 Kibyte size Size of FITS file 81- 92 A12 --- FileName Name of FITS file, in subdirectory fits 94-130 A37 --- Title Title of the FITS file (1)
Note (1): The Y and N after the name of the molecule indicate if the molecule was detected (Y) or not detected (N). For a more detailed explanation Of the different molecules, please refer to paper.
Acknowledgements: Mika Saajasto, mika.saajasto(at)helsinki.fi
(End) Mika Saajasto [University of Helsinki], Patricia Vannier [CDS] 17-Aug-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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