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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 84 67 Clump properties in the 30 Dor molecular ridge
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
Bytes Format Units Label Explanations
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 (X_CO_) (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)
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) 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).
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 25-Oct-2011
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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