J/A+A/586/A37 M33 center and BCLMP302 [CII] spectroscopy (Mookerjea+, 2016)
Velocity resolved [C II] spectroscopy of the center and the BCLMP302 region of
M33 (HerM33es).
Mookerjea B., Israel F., Kramer C., Nikola T., Braine J., Ossenkopf V.,
Roellig M., Henkel C., van der Tak F.F.S., Wiedner M.
<Astron. Astrophys. 586, A37 (2016)>
=2016A&A...586A..37M 2016A&A...586A..37M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; H II regions ; Spectroscopy
Keywords: ISM: clouds - HII regions - photon-dominated regions (PDR) -
galaxies: individual: M33 - galaxies: star formation - galaxies: ISM
Abstract:
The forbidden fine structure transition of [CII] at 158 micron is one
of the major cooling lines of the interstellar medium (ISM). We aim to
understand the contribution of the ionized, atomic and molecular
phases of the ISM to the [CII] emission from clouds near the
dynamical center and the BCLMP302 HII region in the north of the
nearby galaxy M33 at a spatial resolution of 50pc.
We combine high resolution [CII] spectra taken with the Herschel/HIFI
spectrometer onboard the Herschel satellite with [CII] Herschel-PACS
maps and ground-based observations of CO(2-1) with IRAM 30m and HI
with VLA, all at the same spatial resolution. We decomposed the [CII]
spectra in terms of contribution from molecular and atomic gas
detected in CO(2-1) and HI, respectively.
Typically, the [CII] lines have widths intermediate between the
narrower CO(2-1) and broader HI line profiles. Comparison of spectra
show that the relative contribution of molecular and atomic gas traced
by CO(2-1) and HI varies substantially between positions and depends
mostly on the local physical conditions and geometry.
In both regions a larger fraction of the molecular gas is traced by [C
II] than by the canonical tracer CO. These results emphasize the need
for velocity-resolved observations to discern the contribution of
different components of the ISM to [C II] emission.
Description:
1-d spectra of [CII], HI and CO(2-1) in ascii format at selected
positions of the nucleus and in BCLMP302 region as presented in
Figures 8 and 9. Twelve positions in the center and 8 positions in
BCLMP302 were analyzed. All spectra are at a common spectral
resolution of 2.6km/s.
Filename convention: nucleus or bclmp302 for the respective regions.
Offsets are relative to 01:33:48.20 30:39:21.4 (J2000) for the center
and relative to 01:34:06.30 30:47:25.3 (J2000) for the BCLMP302
region.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 52 60 List of spectra
sp/* . 60 Individual spectra
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See also:
J/AJ/142/111 : Total infrared brightness and SFR in M33 (Boquien+, 2011)
J/A+A/549/A17 : M33 Giant Molecular Clouds IRAM spectra (Buchbender+, 2013)
J/A+A/552/A14 : SEDs of M33 HII regions (Relano+, 2013)
Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Region Region (BCLMP302 or nucleus)
10- 16 A7 --- Line Line observed
19- 21 I3 arcsec oRA Offset in right ascension (1)
23- 25 I3 arcsec oDE Offset in declination (1)
27- 52 A26 --- FileName Name of the spectrum file in subdirectory sp
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Note (1): Offsets are relative to
RA=01:33:48.20, DE=+30:39:21.4 (J2000) for the center and
RA=01:34:06.30, DE=+30:47:25.3 (J2000) for the BCLMP302 region.
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Byte-by-byte Description of file: sp/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 F17.12 km/s Vel Velocity
18- 39 E22.18 K Tmb ?=-1 Main bean temperature
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Acknowledgements:
Bhaswati Mookerjea, bhaswati(at)tifr.res.in
(End) Patricia Vannier [CDS] 18-Nov-2015