J/ApJ/703/736 Clump properties in the LMC 30 Dor region (Pineda+, 2009)
The influence of far-ultraviolet radiation on the properties of molecular clouds
in the 30 Dor region of the Large Magellanic Cloud.
Pineda J.L., Ott J., Klein U., Wong T., Muller E., Hughes A.
<Astrophys. J., 703, 736-751 (2009)>
=2009ApJ...703..736P 2009ApJ...703..736P
ADC_Keywords: Carbon monoxide ; Magellanic Clouds ; Molecular clouds ;
Interstellar medium ; Ultraviolet
Keywords: galaxies: ISM - ISM: molecules - ISM: structure - Magellanic Clouds
Abstract:
We present a complete 12CO(J=1-0) map of the prominent molecular
ridge in the Large Magellanic Cloud (LMC) obtained with the 22m ATNF
Mopra Telescope. The region stretches southward by ∼2° (or 1.7kpc)
from 30 Doradus, the most vigorous star-forming region in the Local
Group. The location of this molecular ridge is unique insofar as it
allows us to study the properties of molecular gas as a function of
the ambient radiation field in a low-metallicity environment. The mass
spectrum and the scaling relations between the properties of the CO
clumps in the molecular ridge are similar, but not identical, to those
that have been established for Galactic molecular clouds.
Description:
The 12CO(J=1-0) (115GHz) observations were made using the 22m ATNF
Mopra Telescope between 2005 June and September. A total of 120
fields, 5'x5' in size, were mapped using the on-the-fly mapping mode,
encompassing the entire 30 Dor molecular ridge.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 84 67 Clump properties in the 30 Dor molecular ridge
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See also:
J/ApJS/178/56 : CO observations of LMC Giant Molecular clouds (Fukui+, 2008)
J/PASJ/53/971 : CO catalog of LMC molecular clouds (Mizuno+, 2001)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/67] Clump number
(<[POK2009] NN> in Simbad)
4- 5 I2 h RAh Hour of right ascension (J2000)
7- 8 I2 min RAm Minute of right ascension (J2000)
10- 15 F6.3 s RAs Second of right ascension (J2000)
17 A1 --- DE- Sign of declination (J2000)
18- 19 I2 deg DEd Degree of declination (J2000)
21- 22 I2 arcmin DEm Arcminute of declination (J2000)
24- 28 F5.2 arcsec DEs Arcsecond of declination (J2000)
30- 34 F5.1 km/s Vlsr LSR velocity
36- 39 F4.1 km/s DelV FWHM of the observed line profile
(Δν'); deconvolved by the
instrumental resolution
41- 43 F3.1 km/s e_DelV DelV uncertainty
45- 48 F4.1 pc Rad Clump radius; deconvolved by the
instrumental resolution
50- 52 F3.1 pc e_Rad Rad uncertainty
54- 56 F3.1 K Tmb Brightness temperature
58- 60 F3.1 K e_Tmb Tmb uncertainty
62- 64 F3.1 K.km/s log(LCO) CO luminosity (1)
66- 68 F3.1 Msun log(Mvir) Virial mass (1)
70- 73 F4.1 10+20cm-2/(K.km/s) XCO CO-to-H2 conversion factor (XCO) (2)
75- 78 F4.1 10+20cm-2/(K.km/s) e_XCO XCO uncertainty
80- 84 F5.1 [-] Chi Strength of the FUV radiation field (3)
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Note (1): The CO luminosities and virial masses have typically errors of 50%.
Note (2): We estimate the value of XCO for clumps in the 30 Dor molecular
ridge assuming that they are in virial equilibrium. In this case,
XCO is calculated dividing the clump's virial mass -which we assume
is an accurate measure of the total mass of H2 present- by its CO
luminosity (see section 3.1 for further details).
Note (3): Strength of the FUV radiation field in units of the Draine
(1978ApJS...36..595D 1978ApJS...36..595D) field (χ0). They have typical errors of
20%, as this is the accuracy of the HIRES/IRAS images used to derive
this quantity (see section 3.2).
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 25-Oct-2011