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J/A+AS/116/95       Magellanic Clouds PNe line intensities (Leisy+, 1996)

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)
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 Hβ. 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:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table7 table8
Bytes Format Units Label Explanations
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
Note (1): scale F(Hbeta)=100
Byte-by-byte Description of file: table78a
Bytes Format Units Label Explanations
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
Courtesy: P. Leisy
(End) Patricia Bauer [CDS] 09-Jan-1996
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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