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 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:
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RA (2000) DE Designation(s)
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13 51 03.6 -51 12 21 NGC 5307 = HD 120489
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 59 195 Line Intensities
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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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 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)
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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.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 07-Nov-2003