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J/A+A/332/721      Planetary nebulae abundances (Perinotto+ 1998)

The chemical structure of bipolar planetary nebulae. II. 13 objects Perinotto M., Corradi R. <Astron. Astrophys. 332, 721 (1998)> =1998A&A...332..721P (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; Abundances Keywords: ISM: abundances - planetary nebulae: general Abstract: Long slit spectrophotometry of 13 bipolar planetary nebulae has been used to study their physical and chemical properties. In each nebula, one to seven different spatial regions have been considered in order to search for possible abundance variations through the nebulae. We obtained the following main results: - within the errors, the He, O, and N abundances are constant through all the nebulae. - the Ne, Ar, and S abundances are also constant, within the errors, but their face values have systematic increases toward the outer regions of the nebulae. These trends may be attributed to inaccuracies in the ionization correction factors, as predicted by Alexander & Balick (1997AJ....114..713A) for long-slit observations of extended PNe. The corresponding increase of the N abundance predicted by those authors is, however, generally not observed (with one exception). - The present sample contains some of the Galactic PNe with the highest He and N/O abundances known to date (M 3-2, He 2-111, NGC 6537). The highest He overabundances cannot by reproduced by any current model of AGB evolution. - Oxygen depletion is suggested for the nebulae with the highest N/O abundances, indicating that efficient ON cycle process has occurred in their progenitors. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 14 33 18 -60 49.6 Hen 2-111 = PN G315.0-00.3 15 04 09 -60 53.3 Hen 2-114 = PN G318.3-02.0 09 43 25.5 -57 16 53 Hen 2-36 = PN G279.6-03.1 12 28 47 -63 44.6 Hen 2-84 = PN G300.4-00.9 07 21 14.4 -18 08 34 M 1-13 = PN G232.4-01.8 07 37 18.9 -09 38 48 M 1-16 = PN G226.7+05.6 07 14 49 -27 50.4 M 3-2 = PN G240.3-07.6 15 34 16.6 -59 08 59 Mz 1 = PN G322.4-02.6 07 41 55.4 -18 12 31 NGC 2440 = HD 62166 = PN G234.8+02.4 09 16 01.5 -36 37 37 NGC 2818 = PN G261.9+08.5 09 27 03.0 -56 06 22 NGC 2899 = PN G277.1-03.8 16 12 58.2 -36 13 48 NGC 6072 = PN G342.1+10.8 18 05 13.0 -19 50 34 NGC 6537 = HD 312582 = PN G010.1+00.7 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file fluxes.dat 81 677 Observed line fluxes abund.dat 129 533 Abundances den.dat 39 13 Electronic densities tnii.dat 54 13 [NII] temperatures toiii.dat 54 13 [OIII] temperatures table1.tex 116 1161 LaTeX version of fluxes.dat table2.tex 105 433 LaTeX version of abund.dat, tnii.dat, toii.dat and den.dat
Byte-by-byte Description of file: fluxes.dat
Bytes Format Units Label Explanations
1- 8 A8 --- PN Planetary nebula name 11- 30 A20 --- Line Line identification 32- 37 F6.1 --- n3 ? Third region on the western lobe relative abundance (1) 39- 44 F6.1 --- n2 ? Second region on the western lobe relative abundance (1) 46- 51 F6.1 --- n1 ? First region on the western lobe relative abundance (1) 53- 58 F6.1 --- cen ? Central region relative abundance (1) 61- 66 F6.1 --- p1 ? First region on the eastern lobe relative abundance (1) 68- 73 F6.1 --- p2 ? Second region on the eastern lobe relative abundance (1) 76- 81 F6.1 --- P3 ? Third region on the eastern lobe relative abundance (1)
Note (1): Abundance relative to Hβ=100.
Byte-by-byte Description of file: abund.dat
Bytes Format Units Label Explanations
1- 8 A8 --- PN PN name 10- 23 A14 --- Ion Ion/Element 25- 29 A5 --- Line Line identification 33- 41 F9.3 --- n3 ? Abundance in the third region on the western lobe 43- 44 I2 --- e_n3 ? rms uncertainty on n3 47- 55 F9.3 --- n2 ? Abundance in the second region on the western lobe 57- 58 I2 --- e_n2 ? rms uncertainty on n2 59 A1 --- u_n2 Uncertainty flag on n2 61- 69 F9.3 --- n1 ? Abundance in the first region on the western lobe 71- 72 I2 --- e_n1 ? rms uncertainty on n1 73 A1 --- u_n1 Uncertainty flag on n1 75- 83 F9.3 --- cen ? Abundance in the central region 85- 86 I2 --- e_cen ? rms uncertainty on cen 87 A1 --- u_cen Uncertainty flag on cen 88- 96 F9.3 --- p1 ? Abundance in the first region on the eastern lobe 98- 99 I2 --- e_p1 ? rms uncertainty on p1 100 A1 --- u_p1 Uncertainty flag on p1 101-109 F9.3 --- p2 ? Abundance in the second region on the eastern lobe 111-112 I2 --- e_p2 ? rms uncertainty on p2 113 A1 --- u_p2 Uncertainty flag on p2 115-123 F9.3 --- p3 ? Abundance in the third region on the eastern lobe 125-126 I2 --- e_p3 ? rms uncertainty on p3
Byte-by-byte Description of file: den.dat
Bytes Format Units Label Explanations
1- 8 A8 --- PN Planetary nebula name 10- 12 I3 cm-3 Nen3 ? Third western region lobe electronic density 14- 16 I3 cm-3 Nen2 ? Second western region lobe electronic density 18- 21 I4 cm-3 Nen1 ? First western region lobe electronic density 23- 26 I4 cm-3 Necen ? Central region electronic density 28- 31 I4 cm-3 Nep1 ? First eastern region lob 33- 35 I3 cm-3 Nep2 ? Second eastern region lobe electronic density 37- 39 I3 cm-3 Nep3 ? Third eastern region lobe electronic density
Byte-by-byte Description of file: tnii.dat toiii.dat
Bytes Format Units Label Explanations
1- 8 A8 --- PN Planetary nebula name 10- 14 I5 K Tn3 ? Temperature for the third western region lobe 15 A1 --- n_Tn3 [a] a when adopted temperature 17- 21 I5 K Tn2 ? Temperature for the second western region lobe 22 A1 --- n_Tn2 [a] a when adopted temperature 24- 28 I5 K Tn1 ? Temperature for the first western region lobe 29 A1 --- n_Tn1 [a] a when adopted temperature 31- 35 I5 K Tcen ? Temperature for the central region 37- 41 I5 K Tp1 ? Temperature for the first eastern region lobe 43- 47 I5 K Tp2 ? Temperature for the second eastern region lobe 48 A1 --- n_Tp2 [a] a when adopted temperature 50- 54 I5 K Tp3 ? Temperature for the third eastern region lobe
Acknowledgements: Romano Corradi References: Corradi et al., Paper I. (IC 4406) 1997A&A...322..975C
(End) Patricia Bauer [CDS] 22-Jan-1998
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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