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 2015MNRAS.447..817B (SIMBAD/NED BibCode)
ADC_Keywords: Planetary nebulae ; 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 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