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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 130 23 List of datacubes
fits/* . 23 Individual fits datacubes
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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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)
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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.
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Acknowledgements:
Mika Saajasto, mika.saajasto(at)helsinki.fi
(End) Mika Saajasto [University of Helsinki], Patricia Vannier [CDS] 17-Aug-2017