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J/ApJ/466/254                    NIR Imaging of R136 in 30 Dor (Brandl+ 1996)
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Adaptive optics near-infrared imaging of R136 in 30 Doradus: the stellar
population of a nearby starburst.
    Brandl B., Sams B.J., Bertoldi F., Eckart A., Genzel R., Drapatz S.,
    Hofmann R., Loewe M., Quirrenbach A.
   <Astrophys. J. 466, 254 (1996)>
   =1996ApJ...466..254B
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ADC_Keywords: Stars, dwarfs ; Photometry, UBVRIJKLMNH
Keywords: H II regions - infrared: stars - ISM: individual (30 Doradus) -
          Magellanic Clouds - stars: early type - techniques: image processing

Abstract:
    We report 0.15" resolution near-infrared (NIR) imaging of R136, the
    central region of 30 Doradus in the Large Magellanic Cloud. Our
    12.8"x12.8" images were recorded with the MPE camera SHARP II at the
    3.6m ESO telescope, using the adaptive optics system COME ON+. The
    high spatial resolution and sensitivity (20th magnitude in K) of our
    observations allow our H- and K-band images to be compared and
    combined with recent Hubble Space Telescope (HST) WFPC2 data of R136.
    We fit theoretical models with variable foreground extinction to the
    observed magnitudes of ~1000 stars (roughly half of which were
    detected in HST and NIR bands) and derive the stellar population in
    this starburst region. We find no red giants or supergiants; however,
    we detect ~110 extremely red sources which are probably young,
    pre-main-sequence low- or intermediate-mass stars. We obtained
    narrow-band images to identify known and new Wolf-Rayet stars by their
    He II (2.189um) and BrGamma (2.166um) emission lines. The presence
    of W-R stars and absence of red supergiants narrow the cluster age to
    3-5Myr, while the derived ratio of W-R to O stars of 0.05 in the
    central region favors an age of ~3.5Myr, with a relatively short
    starburst duration. For the O stars, the core radius is found to be
    0.1pc and appears to decrease with increasing stellar mass. The slope
    of the mass function is Gamma=-1.6 on average, but it steepens with
    increasing distance from the cluster center from Gamma=-1.3 in the
    inner 0.4pc to Gamma=-2.2 outside 0.8pc for stars more massive
    than 12 Msun. The radial variation of the mass function reveals strong
    mass segregation that is probably due to the cluster's dynamical
    evolution.

File Summary:
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 FileName    Lrecl    Records   Explanations
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ReadMe          80          .   This file
table3.dat      51        971   The 971 main sequence stars in our field of view
                                (YSO candidates and WR stars were excluded)
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Byte-per-byte Description of file: table3.dat
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   Bytes Format  Units   Label     Explanations
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   1-  4  I4     ---     Star      Star number from Hunter et al.
                                      (1995ApJ...488..179H)
   8- 10  I3     pix     Xpos      X position on detector (512x512 grid)
  13- 15  I3     pix     Ypos      Y position on detector (512x512 grid)
  18- 23  F6.2   mag     Umag      *?=-99.99 U magnitude
  25- 30  F6.2   mag     Vmag      *?=-99.99 V magnitude
  32- 37  F6.2   mag     Imag      *?=-99.99 I magnitude
  39- 44  F6.2   mag     Hmag      *?=-99.99 H magnitude
  46- 51  F6.2   mag     Kmag      *?=-99.99 K magnitude
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Note on Umag, Vmag, Imag:
  The U, V & I band magnitudes were converted from WFPC2 magnitudes
  according the the relations in Hunter et al. (1995ApJ...488..179H).
  Extinction was not taken into account.
Note on Hmag, Kmag:
  The H & K magnitudes were derived from the authors' observations
  with adaptive optics. Extinction is not taken into account.
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Origin: AAS CD-ROM series, Volume 7, 1996           Lee Brotzman [ADS] 22-Oct-96
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(End)                                                         [CDS]  03-Feb-1997