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J/MNRAS/447/817    Spectrum of the planetary nebula NGC 6210    (Bohigas+, 2015)

Echelle spectroscopy and photoionization modelling of the entire planetary nebula NGC 6210. Bohigas J., Escalante V., Rodriguez M., Dufour R.J. <Mon. Not. R. Astron. Soc., 447, 817-835 (2015)> =2015MNRAS.447..817B (SIMBAD/NED BibCode)
ADC_Keywords: Nebulae, planetary ; Spectroscopy Keywords: ISM: abundances - ISM: individual objects: NGC 6210 Abstract: High-resolution spectroscopy of NGC 6210, show that recombination line abundances of O+2 and Ne+2 are two to three times larger than forbidden line abundances, Te(O+2) is smaller than Te(N+) and possibly Te(S+), the ionized mass is ∼0.07 M and the progenitor zero-age main-sequence mass is 1.2-2 M. If electrons are in equilibrium, recombination lines are likely produced in a cold low-density medium. A photoionization model (cloudy 13.03) with a positive density gradient and two exciting sources, reproduced most of the optical spectrum, the temperature distribution of the nebula, HeII 4686/HeI 5876, [OII]3726/[OIII]5007 and [OII]3726/3729, but not the other density sensitive line ratios. Including fluorescence and recombination, we found good agreement with observed CII and CIII line intensities, OII and OIII model intensities which are 2.6 and 7.8 times smaller than observed and large erratic differences with observations in CIII, NII and NIII lines. UV and IR data suggest that [OII] emission is from a region ∼6 times less dense than assumed by the model and that IR lines are produced in a medium where the density is ∼1000/cm3. There may be a lower density medium beyond a dense ring described by the photoionization model, as well as a cold low-density component. A multicomponent model is required to reproduce the entire spectrum of NGC 6210. Description: Spectroscopy was carried out on 2005 July, using the 2.1 m f/7.5 telescope at OAN, and the Echelle spectrograph with a 400 lines/mm cross-disperser, no blocking filters and a 1.7 mm wide and 2.0 mm long slit (∼22 arcsecx27 arcsec). The slit was fully open in order to minimize problems related to incomplete coverage (Bohigas 2008ApJ...674..954B) and capture all the emission produced by the inner nebula. The detector was a SITE 1024x1024 pixel CCD. Objects: --------------------------------------------------- RA (ICRS) DE Designation(s) --------------------------------------------------- 16 44 29.49 +23 47 59.7 NGC 6210 = HD 151121 --------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 110 351 NGC 6210 spectrum
See also: V/100 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae (Acker+ 1996) J/AZh/82/437 : Calculated chemical composition of galactic PN (Holovatyy+, 2005) J/A+A/561/A119 : Spectra of stars and planetary nebulae (Moni Bidin+, 2014) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 62 A62 --- Trans Transition identification 64- 70 F7.2 0.1nm lambda ? Laboratory wavelength λlab (Å) (1) 72- 79 F8.3 --- Fobs ? Mean flux relative to Hβ/100 (1) 81- 86 F6.3 --- e_Fobs ? Uncertainty in Fobs (in FHβ=100) (1) 88- 95 F8.3 --- Iobs ? Dereddened line flux (in FHβ=100) (1) 97-103 F7.2 --- Exp2 ? Line flux from the positive density gradient model (in FHβ=100) (2) 105-110 F6.2 --- Exp0 ? Line flux from the constant density model (in FHβ=100) (3)
Note (1): F(Hβ)=8.74±0.03x10-11 erg/cm2/s; C(Hβ)=0.12. Note (2): Exp2 stands for the model where NH∝R2. Note (3): Exp0 stands for the model where NH is uniform.
History: From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 09-Nov-2017
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