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J/A+A/443/851       Effective temperature of 30 Dor population (Selman+, 2005)

The IMF of the field population of 30 Doradus. Selman F.J., Melnick J. <Astron. Astrophys., 443, 851-861 (2005)> =2005A&A...443..851S
ADC_Keywords: Magellanic Clouds ; Associations, stellar ; Photometry, UBV ; Effective temperatures Keywords: star formation - galaxies: stellar content - galaxies: Magellanic Clouds - galaxies: star clusters - techniques: photometric - methods: statistical Abstract: The star-formation history and IMF of the field population of the 30 Doradus super-association is determined using Wide Field Imager photometry. The cluster NGC 2070 and the OB association LH104 are also studied and used for comparison. The star-formation history of the 30∼Doradus super-association appears to be characterized by a large increase in star-formation activity 10Myr to 20Myr ago. This seems to be the case across the whole eastern half of the LMC as demonstrated by the ages of stellar populations as far away as 30 Doradus and Shapley's Constellation III. Star-formation appears to be occurring at a constant rate in the field and in loose associations, and in bursts in the clusters. The field IMF is found to have almost the exact Salpeter slope in the range 7M≤M≤40M, at odds with previous claims. We find that, for objects with more complex star-formation histories, Be stars and selective incompleteness strongly affect the determination of the IMF for M>40M, naturally explaining the observed deviation of the high mass IMF slope from the Salpeter value.The present work supports the idea of a universal IMF. Description: Catalog of observed and physical parameters for the stars in the 30 Doradus super-association. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 153 12993 Observed and physical parameters of stars in 30 Doradus table3.dat 77 98 Spectroscopic and photometric Teff for stars in selected fields
See also: II/187 : 30 Doradus OB Associations (Parker 1992) J/A+A/341/98 : The ionizing cluster of 30 Doradus. I. (Selman+ 1999) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 I8 --- Seq Star unique ID in this work 12- 17 F6.1 pix Xpos X position (0.238 arcsec/pixels) 21- 26 F6.1 pix Ypos Y position (0.238 arcsec/pixels) 32- 37 F6.3 mag Vmag WFI V band magnitude 40- 44 F5.3 mag e_Vmag The 1σ uncertainty in V 48- 53 F6.3 mag (B-V) WFI (B-V) colour index 56- 60 F5.3 mag e_(B-V) The 1σ uncertainty in (B-V) 64- 69 F6.3 mag (U-B) WFI (U-B) colour index 72- 76 F5.3 mag e_(U-B) The 1σ uncertainty in (U-B) 81- 85 F5.3 [K] LogTeff Log of the effective temperature 87- 93 F7.3 mag Mbol Bolometric magnitude 96 I1 --- LC Luminosity class 100-107 F8.3 Myr Age Age 110-114 F5.1 solMass Mini Initial mass 119-123 F5.3 mag E(B-V) Colour excess 127-132 F6.3 --- Uchi DAOPHOT allstar Chi avg. for WFI U band 134-139 F6.3 --- Bchi DAOPHOT allstar Chi avg. for WFI B band 141-146 F6.3 --- Vchi DAOPHOT allstar Chi avg. for WFI V band 148-153 F6.3 --- sharp DAOPHOT allstar sharp WFI UBV average
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 I8 --- Seq Sequential number 10- 15 A6 --- Name Name (1) 17- 32 A16 --- SpType MK spectral type (2) 34- 37 F4.2 K Teff Spectroscopic effective temperature 38 A1 --- --- [-] 39- 42 F4.2 K Teff2 ? Lower limit of Teff when interval 45- 50 F6.3 mag Vmag V magnitude 52- 56 F5.3 mag e_Vmag rms uncertainty on Vmag 58- 61 F4.2 [K] log(Teff)ph Photometric effective temperature 63- 65 F3.1 --- chi Goodness of the psf profile fit 67- 77 A11 --- SName Simbad name
Note (1): The reference identification are from: p = Parker, 1993, Cat. II/187, [P93] NNNN in Simbad wb = Walborn & Blades, 1997ApJS..112..457W, [WB97] NN st = Schild & Testor, 1992A&AS...92..729S, [ST92] N-NN Note (2): The spectral types are taken from the compilation in Paper II, (Selman et al., 1999A&A...347..532S) for the neighborhood of the Tarantula; from Walborn & Blades (1997ApJS..112..457W) for Hodge 301; and from Schild & Testor (1992A&AS...92..729S) for LH104.
Acknowledgements: Fernando J. Selman, fselman(at)eso.org References: Selman et al., Paper I 1999A&A...341...98S, Cat. J/A+A/341/98 Selman et al., Paper II 1999A&A...347..532S
(End) Fernando Selman [ESO, Chile], Patricia Vannier [CDS] 18-Nov-2005
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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