Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/732/101           C18O cores in the S140 cloud           (Ikeda+, 2011)

Similarity between the C18O (J = 1-0) core mass function and the initial mass function (IMF) in the S140 region. Ikeda N., Kitamura Y. <Astrophys. J., 732, 101 (2011)> =2011ApJ...732..101I
ADC_Keywords: Interstellar medium ; Molecular clouds Keywords: ISM: clouds - ISM: individual objects (S140, L1204) - ISM: molecules - stars: formation Abstract: We present the results of C18O(J=1-0) mapping observations of a 20'x18' area in the Lynds 1204 molecular cloud associated with the Sharpless 2-140 (S140) HII region. The C18O cube (α-δ-νLSR) data show that there are three clumps of sizes ∼1pc in the region. Two of these have peculiar redshifted velocity components at their edges, which can be interpreted as the results of the interaction between the cloud and the Cepheus Bubble. From the C18O cube data, clumpfind identified 123 C18O cores, which have mean radius, velocity width in FWHM, and LTE mass of 0.36±0.07pc, 0.37±0.09km/s, and 41±29M, respectively. Considering the uncertainty in the C18O abundance, all the cores in S140 are most likely to be gravitationally bound. We derived a C18O core mass function (CMF), which shows a power-law-like behavior above a turnover at 30M. Description: The C18O (J=1-0) mapping observations were carried out during the period from 2010 January to February by using the Nobeyama 45m radio telescope. Our map covered a 20'x18' area, whose center was selected to be 22:20:18+63:22:12 (J2000). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 69 123 Physical properties of the C18O cores in the S140 cloud
See also: J/A+A/473/177 : A search for pre-biotic molecules (Wirstrom+, 2007) J/ApJS/141/157 : CO (J=1-0) data of cold IRAS sources (Yang+, 2002) J/A+A/358/257 : Molecular clouds SO and CS obs. II. (Nilsson+, 2000) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Running sequence number 5- 6 I2 h RAh Hour of right ascension (J2000) 8- 9 I2 min RAm Minute of right ascension (J2000) 11- 12 I2 s RAs Second of right ascension (J2000) 14 A1 --- DE- Sign of declination (J2000) 15- 16 I2 deg DEd Degree of declination (J2000) 18- 19 I2 arcmin DEm Arcminute of declination (J2000) 21- 22 I2 arcsec DEs Arcsecond of declination (J2000) 23- 24 A2 --- --- [.0] 26- 29 F4.1 km/s Vlsr LSR velocity 31- 34 F4.2 K TA Antenna peak temperature 36- 40 F5.1 arcsec Rad Beam-deconvolved radius Rcore in arcsec 42- 45 F4.2 pc Rc Beam-deconvolved radius Rcore in parsec (1) 47- 50 F4.2 km/s dv.c Velocity width in FWHM corrected for the spectrometer resolution (dvcore) (2) 52- 56 F5.1 Msun Mc LTE mass Mcore (3) 58- 61 F4.1 Msun Mv Virial mass Mvir (3) 63- 65 F3.1 --- Mv/Mc Ratio virial mass/LTE mass (3) 67- 69 F3.1 10+3cm-3 n Mean density of the C18O core (3)
Note (1): The typical uncertainty for Rcore is 0.04pc, derived from the uncertainty in the estimation of the core projected area. Note (2): The typical uncertainty for dvcore is 0.13km/s, corresponding to the velocity resolution. Note (3): The typical uncertainty for Mcore is a factor of three (see text). For Mvir, a factor of three, derived from the uncertainties in Rcore and dvcore. For Mvir/Mcore, a factor of four, derived from the uncertainties in Mcore and Mvir. For n, a factor of four, derived from the uncertainties in Rcore and Mcore.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-Oct-2012
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

catalogue service