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J/ApJ/595/247    Line intensities in the planetary nebula NGC 5307 (Ruiz+, 2003)

Very Large Telescope echelle spectrophotometry of the planetary nebula NGC 5307 and temperature variations. Ruiz M.T., Peimbert A., Peimbert M., Esteban C. <Astrophys. J. 595, 247 (2003)> =2003ApJ...595..247R
ADC_Keywords: Planetary nebulae ; Energy distributions ; Reddening Keywords: ISM: abundances - planetary nebulae: general - planetary nebulae: individual (NGC 5307) Abstract: Echelle spectrophotometry of the planetary nebula NGC 5307 is presented. The data consist of Very Large Telescope Ultraviolet Visual Echelle Spectrograph observations in the 3100-10360Å range. Electron temperatures and densities have been determined using different line intensity ratios. We determine the H, He, C, and O abundances based on recombination lines; these abundances are almost independent of the temperature structure of the nebula. We also determine the N, O, Ne, S, Cl, and Ar abundances based on collisionally excited lines; the ratios of these abundances relative to that of H depend strongly on the temperature structure of the nebula. Description: The observations were obtained with the Ultraviolet Visual Echelle Spectrograph at the Very Large Telescope Kueyen Telescope in Chile. We observed simultaneously with the red and blue arms, each in two settings, covering the region from 3100 to 10360Å. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 13 51 03.6 -51 12 21 NGC 5307 = HD 120489 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 59 195 Line Intensities
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 9 F9.3 0.1nm OWave ? Observed heliocentric wavelength in Angstroems 11- 18 F8.2 0.1nm LWave Adopted laboratory wavelength in Angstroems 20 A1 --- f_LWave [cd] c = Blue component; d = Red component 22- 27 A6 --- Ion Ion identification 29- 33 A5 --- Trans Transition identification (2) 35 A1 --- f_Trans [e] See Pequignot & Baluteau (1988A&A...206..298P) 37- 44 F8.3 --- Flux ? Observed flux relative to Hβ (3) 46- 53 F8.3 --- CFlux ? Reddening corrected flux relative to Hβ (4) 55- 58 F4.1 % e_Flux ? The 1σ percent error in CFlux (5)
Note (2): Multiplet number, or the Balmer (B), or Paschen (P), transitions for each line. Note (3): Where Flux is the observed flux in units of 11.84aW/m2 (100.00=1.184*10-12erg/cm2/s) Note (4): Where CFlux is the reddening corrected flux observed flux, with C(Hβ)=0.59dex, in units of 46.06aW/m2 (100.00=4.606*10-12erg/cm2/s) Note (5): Estimated from a signal-to-noise versus signal curve obtained from a fit to the dispersion in the observed to predicted line intensities for all the measured hydrogen lines.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 07-Nov-2003
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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