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J/ApJ/425/122        IMF from UV stellar photometry                (Hill+, 1994)

Initial mass functions from ultraviolet stellar photometry: a comparison of Lucke and Hodge OB Associations near 30 Doradus with the nearby field HILL J.K., ISENSEE J.E., CORNETT R.H., BOHLIN R.C., O'CONNELL R.W., ROBERTS M.S., SMITH A.M., STECHER T.P. <Astrophys. J. 425, 122 (1994)> =1994ApJ...425..122H (SIMBAD/NED Reference)
ADC_Keywords: Magellanic Clouds; Associations, stellar; Ultraviolet; Positional data; Magnitudes Keywords: Magellanic Clouds - stars: luminosity function, mass function - open clusters and associations: individual (30 Doradus) - ultraviolet: stars Abstract: UV stellar photometry is presented for 1563 stars within a 40' circular field in the LMC, excluding the 10'x10' field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope in bands centered at 1615A and 2558A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (>15M) within the Lucke and Hodge (LH) associations is γ=-1.08±0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is γ=-1.74±0.3 (assuming continuous star formation), compared with γ=-1.35, and γ=-1.7±0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and γ=-1.6 obtained for massive stars in the Galaxy by Garmany, Conti, & Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 58 1563 Observed and fitted stellar data table2.tex 78 1716 LaTeX table version of table2.dat aastab.sty 72 115 Style file for table2.tex environ.tex 77 125 LaTeX environment for table2.tex
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 4 I4 --- Star Running number of star 7- 13 F7.1 arcsec X X offset from J2000 fiducial position RA=5h 38m 44s, Decl.=-69deg 6' 32" 15- 21 F7.1 arcsec Y Y offset from J2000 fiducial position RA=5h 38m 44s, Decl.=-69deg 6' 32" 24- 28 F5.2 mag m162 B5 band magnitude (1615 A) 31- 35 F5.2 mag m256 A5 band magnitude (2558 A) 38- 40 I3 --- LH Lucke and Hodge association number, or zero 43- 46 F4.1 solMass Mass Fitted mass 49- 52 F4.2 mag E(B-V) Fitted E(B-V) within 30 Dor 55- 58 F4.2 mag rms rms magnitude difference between the observations and the best-fit model
References: Fitzpatrick E.L. 1985, ApJ 299, 219 Garmany C.D., Conti P.S. & Chiosi C. 1982 ApJ 263, 777 Hill J.K. et al. 1993, ApJ 413, 604 Salpeter E.E. 1955, ApJ 121, 161 Scalo J.M. 1986, Fund. Cosmic Phys. 11, 1 Schaerer D. et al. 1993, A&AS 98, 523 Origin: AAS CD-ROM series, Volume 2, 1994
(End) Lee Brotzman [ADS] 09-May-1994, Patricia Bauer [CDS] 25-Oct-1994
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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