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J/ApJ/614/745         Optical and IUE spectra of NGC 7026         (Hyung+, 2004)

Optical and IUE spectra of the planetary nebula NGC 7026. Hyung S., Feibelman W.A. <Astrophys. J., 614, 745-756 (2004)> =2004ApJ...614..745H
ADC_Keywords: Nebulae, planetary ; Spectroscopy ; Ultraviolet Keywords: ISM: abundances - planetary nebulae: individual (NGC 7026) - plasmas - ultraviolet: ISM Abstract: We investigated spectroscopic data of the extended planetary nebula NGC 7026 in the wavelengths 3700-10050Å, secured with the Hamilton Echelle Spectrograph at Lick Observatory. This optical wavelength spectrum has been analyzed along with the International Ultraviolet Explorer (IUE) UV spectral data. Description: Five IUE spectra are available for NGC 7026: (1) on 1978 June 7, SWP 01738 (20'), SWP 1739 (40'), and LWR 01633 (20'); and (2) on 1994 August 3, SWP 51698 (180') and LWP 28800 (180'). The optical wavelength region observations were all done with the Hamilton Echelle Spectrograph (HES) at the coude focus of the 3m Shane telescope at the Lick Observatory on 1994 August and 2001 August. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 21 06 18.2 +47 51 05 NGC 7026 = PK 089+00 1 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 51 18 IUE (International Ultraviolet Explorer) spectral line intensity table4.dat 66 155 Optical spectrum of NGC 7026
See also: VI/110 : Final Merged Log of IUE Observations (NASA-ESA, 2000) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm lambdaObs Observed wavelength in Angstroms 9- 15 A7 0.1nm lambdaLab Laboratory wavelength in Angstroms 17- 23 A7 --- Ion Ion identification (1) 25- 29 F5.3 --- klambda Seaton's extinction parameter (Seaton, 1979MNRAS.187p..73S) 33- 37 F5.2 --- Int1 Interstellar extinction-corrected intensity for C(Hβ)=0.80 (2) 40- 44 F5.2 --- Int2 Interstellar extinction-corrected intensity for C(Hβ)=0.95 (2) 47- 50 F4.2 10-15W/m2/nm Flux UV flux in units of 10-13ergs/s/cm2/Å 51 A1 --- u_Flux [:] Estimated error on Flux (3)
Note (1): A question mark denotes a doubtful line identification. Note (2): The intensities are given based on the scale of I(Hβ)=100. Note (3): The colon for the fluxes means that the estimated error is large, ±25%, for weak or blended lines, while others are ±10%
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 8 F8.2 0.1nm lambdaObs ? Observed wavelength in Angstroms (1) 10- 17 F8.2 0.1nm lambdaLab ? Laboratory wavelength in Angstroms 19- 28 A10 --- Ion Ion identification (2) 30- 39 A10 --- Mult Multiplet identification (3) 41- 46 F6.3 --- klambda ? Seaton's extinction parameter (Seaton, 1979MNRAS.187p..73S) 48- 54 F7.3 --- IntW ? Interstellar extinction-corrected West position HES intensity for C(Hβ=0.80) (4) 56- 63 F8.3 --- IntC ? Interstellar extinction-corrected Central position HES intensity for C(Hβ=0.80) (4) 65- 66 I2 % RMS ? The 1sigma percentage error (5)
Note (1): Corrected for radial velocity. Note (2): See Hyung and Aller (1996MNRAS.278..551H) for the identifications and references therein. Note (3): From Moore's tabulations (1974, A Multiplet Table of Astrophysical Interest, National Bureau of Standards, No. 40 ; 1993, in Tables of Spectra of H, C, N, and O Atoms and Ions, ed. J. W. Gallagher (London: CRC)): dg = These unidentified lines are seen in other PNs, e.g. IC 4997 and NGC 7662; ? = Unlikely identification; ** = Lines severely affected by atmosphere; star = WR type line? Note (4): The intensities are given on the scale of I(Hβ)=100. Note (5): As deduced from the internal disagreement of spectral measurements (mostly for the west-position spectra or sometimes for the center-position ones) made with different chip settings, whenever two or more measurements are available.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 18-May-2005
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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