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J/A+A/527/A145      Chamaeleon I 870um sources               (Belloche+, 2011)

The end of star formation in Chamaeleon I ? A LABOCA census of starless and protostellar cores. Belloche A., Schuller F., Parise B., Andre P., Hatchell J., Jorgensen J.K., Bontemps S., Weiss A., Menten , K.M., Muders D. <Astron. Astrophys. 527, A145 (2011)> =2011A&A...527A.145B
ADC_Keywords: Molecular clouds ; Millimetric/submm sources Keywords: stars: formation - ISM: individual objects: Chamaeleon I - ISM: structure - evolution - dust, extinction - stars: protostars Abstract: Chamaeleon I is the most active region in terms of star formation in the Chamaeleon molecular cloud complex. Although it is one of the nearest low-mass star forming regions, its population of prestellar and protostellar cores is not known and a controversy exists concerning its history of star formation. Our goal is to search for prestellar and protostellar cores and characterize the earliest stages of star formation in this cloud. Description: Table 2 lists the sources extracted with GAUSSCLUMPS from the filtered 870 micron continuum emission map of Chamaeleon I obtained with the bolometer camera LABOCA at the APEX telescope. These sources are listed in the order in which they were found by GAUSSCLUMPS, i.e. roughly in order of decreasing peak flux density. The 870 micron dust continuum emission map of the Chamaeleon I molecular cloud is available in FITS format. The data were obtained with the bolometer camera LABOCA at the APEX telescope. They were calibrated, reduced, co-added, gridded, smoothed to an effective angular resolution of 21.2" (FWHM), and written in FITS format with the BoA software. The flux density unit is Jy/21.2"-beam. The coordinates are equatorial (J2000) and the offsets are in RADIO projection. Objects: ----------------------------------------- RA (2000) DE Designation(s) ----------------------------------------- 11 06 48 -77 18.0 Cham I = NAME Cha 1 ----------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 96 118 Sources extracted with Gaussclumps in the 870um continuum sum map of Cha I at scale 5, and possible associations found in the SIMBAD database table5.dat 96 9 Additional compact sources with SIMBAD association with a formal peak flux density above 3.5σ in the 870um continuum map of Cha I filtered up to scale 5 table6.dat 86 60 Characteristics of starless (or Class 0) sources extracted with Gaussclumps in the 870um continuum map of Cha I filtered up to scale 5 table8.dat 83 16 Characteristics of YSOs extracted with Gaussclumps in the 870um continuum map of Cha I filtered up to scale 5 table9.dat 83 5 Characteristics of the additional compact sources listed in Table 5 cha1_870.fit 2880 10039 FITS file of the 870 micron continuum emission map of Chamaeleon I
Byte-by-byte Description of file: table[25].dat
Bytes Format Units Label Explanations
1- 2 I2 --- Seq [1/84] Source sequential number (1) 4- 5 I2 h RAh Right ascension (J2000) 7- 8 I2 min RAm Right ascension (J2000) 10- 14 F5.2 s RAs Right ascension (J2000) 16 A1 --- DE- Declination sign (J2000) 17- 18 I2 deg DEd Declination (J2000) 20- 21 I2 arcmin DEm Declination (J2000) 23- 26 F4.1 arcsec DEs Declination (J2000) 28- 32 F5.3 Jy Fp Peak flux density at 870um (in Jy/21.2"-beam) 34- 38 F5.3 Jy Ftot Total flux density at 870um 40- 44 F5.1 arcsec amaj Major axis (FWHM) 46- 49 F4.1 arcsec amin Minor axis (FWHM) 51- 55 F5.1 deg PA [-90/90] Position angle (east from north) 57- 60 F4.1 arcsec Size ? Mean source size (geometrical mean of amaj and amin) 62- 63 A2 --- Type Type of source based on the possible associations found in the SIMBAD database (2) 65- 87 A23 --- SIMBAD Source found in the SIMBAD database within the FWHM ellipse 89- 91 A3 --- Stype SIMBAD type of the SIMBAD source 93- 96 F4.1 arcsec Dist ? Distance of the possibly associated SIMBAD source to the fitted peak position of the LABOCA source
Note (1): Sequential number 1-84 in table2, and Additional sequential number 1-5 in table5. Note (2): Type of source based on the associations found in the SIMBAD database as follows: C = starless core or Class 0 protostar S = young stellar object (Class I or more evolved) Sc = candidate association with a YSO R = residual of a stronger nearby source A = artefact
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Name, Cha1-CNN 10- 11 I2 --- Seq [1/84] Numbering of Gaussclumps sources like in Table 2 13- 17 F5.1 arcsec FWHM1 Size of the fitted Gaussian (1) 18 A1 --- --- [x] 19- 22 F4.1 arcsec FWHM2 Size of the fitted Gaussian (1) 24- 27 F4.1 kAU FWHMa1 Size of the fitted Gaussian (1) 28 A1 --- --- [x] 29- 31 F3.1 kAU FWHMa2 Size of the fitted Gaussian (1) 33- 35 F3.1 --- Ra Aspect ratio (1) 37- 40 F4.1 10+21cm-2 Npeak Peak H2 column density (2) 42- 45 F4.1 mag AV Visual extinction derived from 2MASS 47- 51 F5.3 Msun Mpeak Mass in the central beam (HPBW = 21.2") (3) 53- 57 F5.3 Msun Mtot Total mass derived from the Gaussian fit (3) 58- 62 F5.3 Msun M50" Mass computed from the flux measured in an aperture of 50" in diameter (3) 64- 65 I2 % CM Mass concentration Mpeak/M50" 67- 68 I2 % e_CM Statistical rms uncertainty on CM 70- 73 F4.1 10+5cm-3 npeak Beam-averaged free-particle density within the central beam (4) 75- 78 F4.1 10+5cm-3 n50" Mean free-particle density computed for the mass M50" in the aperture of diameter 50" (4) 80- 82 F3.1 --- cn Density contrast npeak/n50" 84- 86 F3.1 --- e_cn Statistical rms uncertainty on cn
Note (1): Sizes smaller than 25.4" were set to 25.4" to compute the deconvolved sizes, in order to account for a fit inaccuracy corresponding to a 5σ detection in peak flux density. As a result, the minimum size that can be measured is about 2100AU. The aspect ratio is the ratio of the deconvolved sizes along the major and minor axes. Note (2): Peak H2 column density computed assuming a dust opacity of 0.01cm2/g. The statistical rms uncertainty is 1.1x1021cm-2. Note (3): The statistical rms uncertainties of Mpeak and M50" are 0.006 and 0.011M, respectively. Note (4): The statistical rms uncertainties of npeak and n50" are 5.6x104 and 7.2x103cm-3, respectively.
Byte-by-byte Description of file: table[89].dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Name, Cha1-SNN 10- 11 I2 --- Seq [1/87] Numbering of Gaussclumps sources like in table2 (table8) or table5 (table9) 13- 16 F4.1 arcsec FWHM1 Size of the fitted Gaussian (1) 17 A1 --- --- [x] 18- 21 F4.1 arcsec FWHM2 Size of the fitted Gaussian (1) 23- 26 F4.1 kAU FWHMa1 Deconvolved source size (1) 27 A1 --- --- [x] 28- 30 F3.1 kAU FWHMa2 Deconvolved source size (1) 32- 36 F5.1 --- SNR Peak signal-to-noise ratio of the fitted Gaussian 38- 42 F5.2 10+21cm-2 Npeak Peak H_2_ column density (2) 44- 47 F4.1 mag AV Visual extinction derived from 2MASS 49- 54 F6.4 Msun Mpeak Mass in the central beam (HPBW=21.2") (3) 56- 61 F6.4 Msun Mtot Total mass derived from the Gaussian fit (3) 63- 68 F6.4 Msun M50" Mass computed from the flux measured in an aperture of 50" in diameter (3) 70- 72 I3 % CM Mass concentration Mpeak/M50" 74- 76 I3 % e_CM Statistical rms uncertainty on CM 78- 81 A4 --- Class Infrared class of the nearest YSO listed in column SIMBAD of table 2 (table8) or table5 (table9) 83 I1 --- Ref Reference (4)
Note (1): The deconvolved size is computed from the fitted size multiplied by (1+1/SNR), with SNR the peak signal-to-noise ratio, and therefore is an upper limit in most cases. A zero value means that the uncertainty was still underestimated. Note (2): Peak H2 column density computed assuming a dust temperature of 20K and a dust opacity of 0.03cm2/g. The statistical rms uncertainty is 1.5x1020cm-2. Note (3): The statistical rms uncertainties of Mpeak and M50" are 0.0009 and 0.0015M, respectively. Note (4): References as follows: 2 = Luhman et al. (2008, Cat. J/ApJ/675/1375) 3 = Furlan et al. (2009, Cat. J/ApJ/703/1964) 4 = Henning et al. (1993A&A...276..129H) 5 = Luhman & Muench (2008, Cat. J/ApJ/684/654)
Acknowledgements: Arnaud Belloche, belloche(at)mpifr-bonn.mpg.de References: * 14-Feb-2011: table 2 and fits file (from author) * 06-Feb-2014: tables 5, 6, 8 and 9 added (from electronic version)
(End) Patricia Vannier [CDS] 06-Jan-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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