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J/ApJ/425/122                       IMF from UV stellar photometry (Hill+, 1994)
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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)
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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_{sun}_) within the Lucke and Hodge (LH) associations is
  {gamma}=-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
  {gamma}=-1.74+/-0.3 (assuming continuous star formation), compared with
  {gamma}=-1.35, and {gamma}=-1.7+/-0.5, obtained for the Galaxy by
  Salpeter (1955) and Scalo (1986), respectively, and {gamma}=-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
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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
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Byte-per-byte Description of file: table2.dat
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   Bytes  Format  Units   Label    Explanations
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   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
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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

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Origin: AAS CD-ROM series, Volume 2, 1994
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(End)           Lee Brotzman [ADS] 09-May-1994, Patricia Bauer [CDS] 25-Oct-1994