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J/A+AS/116/95       Magellanic Clouds PNe line intensities (Leisy+, 1996)
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Planetary nebulae in the Magellanic Clouds : I. Carbon abundances and TypeI PNe
      Leisy P., Dennefeld M.
     <Astron. Astrophys. Suppl. Ser. 116, 95 (1996)>
     =1996A&AS..116...95L      (SIMBAD/NED BibCode)
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ADC_Keywords: Planetary nebulae ; Spectroscopy ; Magellanic Clouds
Keywords: ISM: planetary nebulae : general - galaxies: Magellanic Clouds -
          galaxies: abundances - galaxies: evolution

Description:
    We present optical and ultraviolet spectroscopic observations of
    planetary nebulae (PNe) in the Large (LMC) and the Small Magellanic
    Clouds (SMC). For the visible spectra with highest S/N, line
    intensities have been measured to a few tenths of a percent of
    H_{beta}_. UV spectra are used for the determination of carbon
    abundances. This paper discusses the CNO cycle and its implications.
    We show that the CN or ON cycles are more effective with lower initial
    metallicities and are always complete for typeI nebulae. The latter
    cannot easily be distinguished from non-type I PNe on the basis of N
    or He abundance alone, as continuity exists in all of the standard
    diagrams. From the study of the C abundances, we deduce that the 3rd
    dredge-up is occurring in all PNe: its efficiency too is higher with
    lower initial metallicities, offering an easy explanation for the
    higher number of carbon stars found in metal-deficient galaxies. It
    is shown that this dredged-up carbon is sometimes transformed into
    nitrogen by Hot-Bottom Burning, but in a few objects only and not even
    in all the typeI PNe, which therefore do not form a homogeneous class.

File Summary:
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  FileName  Lrecl  Records   Explanations
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ReadMe         80        .   This file
table7         61      960   SMC PNe observed and corrected line intensities
table8         65     1019   LMC PNe observed and corrected line intensities
table78a       77       31   Flux, electronic density and temperature
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Byte-by-byte Description of file: table7 table8
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   Bytes Format Units   Label     Explanations
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   1-  8  A8    ---     Name      Planetary nebulae name
  10- 14  I5    ---     Lambda    Wavelength
  19- 33  A15   ---     Ident     Line identification
  37- 42  F6.3  ---     Flambda   Extinction curve value for Lambda
      44  A1    ---   l_Fobs      Limit flag on Fobs
  45- 50  F6.1  ---     Fobs      []? Observed line intensity (1)
      51  A1    ---   u_Fobs      Uncertainty flag on Fobs
      53  A1    ---   l_Fcor      Limit flag on Fcor
  54- 60  F7.1  ---     Fcor      []? Corrected line intensity (1)
      61  A1    ---   u_Fcor      Uncertainty flag on Fcor
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Note (1): scale F(Hbeta)=100
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Byte-by-byte Description of file: table78a
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   Bytes Format   Units     Label   Explanations
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   1-  7  A7      ---       Name    Planetary nebula name
      10  A1      ---     l_Fb      Limit flag on Fb
  11- 14  I4   10-16mW/m2   Fb      Flux Hbeta (10-16 erg/cm2/s-1)
  17- 20  F4.1    %       e_Fb      Hbeta uncertainty
  24- 28  I5      ---       Exp1    IUE exposure number (first number)
  32- 36  I5      ---       Exp2    []? IUE exposure number (second number)
  39- 43  I5      ---       Exp3    []? IUE exposure number (third number)
  46- 50  I5      cm-3      Ne      Electronic density
  53- 57  I5      K         T(OIII) ? [OIII] electronic temperature
  60- 64  I5      K         T(NII)  ? [NII] electronic temperature
  67- 70  F4.2    ---       Copt    Logarithmic extinction constant
  72- 75  F4.2    ---     e_Copt    rms uncertainty on Copt
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Courtesy: P. Leisy <Leisy@iap.fr>
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(End)                                         Patricia Bauer [CDS]   09-Jan-1996