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J/ApJ/705/144       Molecular and atomic gas in the LMC. II.      (Fukui+, 2009)

Molecular and atomic gas in the Large Magellanic Cloud. II. Three-dimensional correlation between CO and H I. Fukui Y., Kawamura A., Wong T., Murai M., Iritani H., Mizuno N., Mizuno Y., Onishi T., Hughes A., Ott J., Muller E., Staveley-Smith L., Kim S. <Astrophys. J., 705, 144-155 (2009)> =2009ApJ...705..144F
ADC_Keywords: Molecular clouds ; Magellanic Clouds ; Radio lines ; Interstellar medium Keywords: galaxies: ISM - ISM: atoms - ISM: clouds - ISM: molecules - Magellanic Clouds - radio lines: ISM Abstract: We compare the CO (J=1-0) and HI emission in the Large Magellanic Cloud in three dimensions, i.e., including a velocity axis in addition to the two spatial axes, with the aim of elucidating the physical connection between giant molecular clouds (GMCs) and their surrounding HI gas. The CO(J=1-0) data set is from the second NANTEN CO survey (Fukui et al. 2008, Cat. J/ApJS/178/56) and the HI data set is from the merged Australia Telescope Compact Array (ATCA) and Parkes Telescope surveys (Kim et al. 2003ApJS..148..473K). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 82 123 List of selected 123 giant molecular clouds (GMCs)
See also: VII/64 : CO Observations of Galaxies (Verter 1985) J/ApJS/184/1 : Molecular clouds in the LMC by NANTEN. II. (Kawamura+, 2009) J/ApJ/699/1092 : Giant molecular clouds (SRBY) (Heyer+, 2009) J/ApJS/178/56 : CO observations of LMC Giant Molecular clouds (Fukui+, 2008) J/ApJ/686/948 : CO in extragalactic giant molecular clouds (Bolatto+, 2008) J/A+A/417/421 : WSRT wide-field HI survey. II. (Braun+, 2004) J/PASJ/53/971 : CO catalog of LMC molecular clouds (Mizuno+, 2001) J/A+AS/131/73 : Catalogue of HI maps of galaxies. I. (Martin 1998) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 3 I3 --- GMC [1/271] Giant Molecular Cloud number (1) 5- 9 A5 --- --- [LMC N] 11- 20 A10 --- Name GMC name (JHHMM+DDMM) (1) 22- 24 A3 --- Type I, II, or III type from Kawamura et al. (2009, Cat. J/ApJS/184/1) (2) 26 I1 h RAh CO peak hour of right ascension (B1950) (3) 28- 31 F4.1 min RAm Minute of right ascension (B1950) 33 A1 --- DE- CO peak sign of declination (B1950) (3) 34- 35 I2 deg DEd Degree of declination (B1950) 37- 38 I2 arcmin DEm Arcminute of declination (B1950) 40- 42 I3 pc R CO radius from Fukui et al. (2008, Cat. J/ApJS/178/56) 44 I1 h RAH.h HI peak hour of right ascension (B1950) (3) 46- 49 F4.1 min RAH.m Minute of right ascension (B1950) 51 A1 --- DEH.- HI peak sign of declination (B1950) (3) 52- 53 I2 deg DEH.d Degree of declination (B1950) 55- 56 I2 arcmin DEH.m Arcminute of declination (B1950) 58 A1 --- f_RHI [*] *: HI clouds whose extent is poorly defined 59- 61 I3 pc RHI ? Radius of the HI envelope (4) 63- 65 F3.1 10+21cm-2 NHI HI column density 67- 69 I3 pc Delt Deviation between CO and HI peak positions (CO(α,δ)-HI(α,δ)) 71- 82 A12 --- Comm Other GMCs in the same HI cloud (5)
Note (1): GMC name from Fukui et al. (2008, Cat. J/ApJS/178/56) (<[FKM2008] NNN> or <[FKM2008] LMC N JHHMM+DDMM> in Simbad). Note that in 68 cases, the name is truncated in JHHMM+DDM format. Note (2): These classes are interpreted as an evolutionary sequence from Type I to III; the lifetime of a GMC is estimated to be a few x10Myr in total. * Type I GMCs show no signs of active star formation in the sense that no O stars are being formed. * Type II GMCs are associated with small HII region(s), indicating the formation of isolated O stars, but do not host any stellar clusters identified by Bica et al. (1996ApJS..102...57B). * Type III GMCs are actively forming stars as shown by their association with large HII regions and young stellar clusters. Note (3): Position of peak integrated intensity. Data are from Fukui et al. (2008, Cat. J/ApJS/178/56). Note (4): HI cloud radius defined as R=(S/π)0.5. Here S is the cloud area, calculated by summing the areas of all pixels detected above 80% of the peak integrated intensity level. Note (5): HI clouds including two or more GMCs: the numbers show GMCs that are located in the same HI cloud.
History: From electronic version of the journal References: Wong et al. Paper I. 2009ApJ...696..370W
(End) Emmanuelle Perret [CDS] 01-Dec-2011
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