J/A+A/614/A135 Spectra of 78 PN central stars (Weidmann+, 2018)
Towards an improvement in the spectral description of central stars of
planetary nebulae.
Weidmann W., Gamen R., Mast D., Farina C., Gimeno G., Schmidt E.O.,
Ashley R.P., Peralta de Arriba L., Sowicka P., Ordonez-Etxeberria I.
<Astron. Astrophys. 614, A135 (2018)>
=2018A&A...614A.135W 2018A&A...614A.135W (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Planetary nebulae ; Stars, population II
Keywords: planetary nebulae: general - stars: Population II -
stars: early-type - surveys
Abstract:
There are more than 3000 known Galactic planetary nebulae (PNe), but
only 492 central stars of Galactic planetary nebulae (CSPN) have known
spectral types. It is vital to increase this number in order to have
reliable statistics, which will lead to an increase of our
understanding of these amazing objects.
We aim to contribute to the knowledge of central stars of planetary
nebulae and stellar evolution.
This observational study is based on Gemini Multi-Object Spectrographs
(GMOS) and with the Intermediate Dispersion Spectrograph (IDS) at the
Isaac Newton Telescope (INT) spectra of 78 CSPN. The objects were
selected because they did not have any previous classification, or the
present classification is ambiguous. These new high quality spectra
allowed us to identify the key stellar lines for determining spectral
classification in the Morgan-Keenan (MK) system.
We have acquired optical spectra of a large sample of CSPN. From the
observed targets, 50 are classified here for the first time while for
28 the existing classifications have been improved. In seven objects
we have identified a P-Cygni profile at the HeI lines. Six of these
CSPN are late O-type. The vast majority of the stars in the sample
exhibit an absorption-type spectrum, and in one case we have found
wide emission lines typical of [WR] stars. We give a complementary,
and preliminary, classification criterion to obtain the sub-type of
the O(H)-type CSPN. Finally, we give a more realistic value of the
proportion of CSPN that are rich or poor in hydrogen.
Description:
Spectral classification of 78 central stars of Galactic planetary
nebulae. The spectra were obtained with Gemini Multi-Object
Spectrographs (GMOS) and with the Intermediate Dispersion Spectrograph
(IDS) at the Isaac Newton Telescope (INT).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea3.dat 112 78 Spectral types from our observations
fits/* . 81 Individual fits spectrum files
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See also:
V/84 : Strasbourg-ESO Catalogue of Galactic Planetary Nebulae
(Acker+, 1992)
J/A+A/526/A6 : Central stars of planetary nebulae (Weidmann+, 2011)
J/A+A/531/A172 : Central stars of planetary nebulae. II. (Weidmann+, 2011)
Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq Sequential number
4- 17 A14 --- Name Main designation
19- 28 A10 --- PNG PNG name (based on galactic position)
30- 46 A17 --- SpType Spectral type of central star (1)
48 A1 --- Tel [GI] Telescope (G: GEMINI/GMOS, I: INT/IDS)
50- 51 A2 --- HeII4542 [AE-? ] HeII at 4542Å detection flag (2)
53- 56 A4 --- HeII4686 [AE-?+ N/D] HeII at 4686Å detection flag (2)
58- 60 A3 --- HeII5412 [AE-? N/D] HeII at 5412Å detection flag (2)
62- 63 A2 --- HeI4471 [AE-? ] HeI at 4471Å detection flag (2)
65- 66 A2 --- Hb4861 [AE-? ] Hβ detection flag (2)
68- 69 A2 --- NV4603 [AE-? ] NV at 4603-4619Å detection flag (2)
71- 74 A4 --- CIV5806 [AE-?+ N/D] CIV at 5801-5812Å detection
flag (2)
76 A1 --- NS [y/n] Indicates whether or not it was possible
to subtract the nebular component.
78- 93 A16 --- FileName Name of the spectrum file in subdirectory fits
94 A1 --- --- [,]
96-112 A17 --- FileName2 Name of second spectrum file in subdirectory
fits
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Note (1): Spectral types as follows:
O(H) = Balmer and HeII absorption lines detected
H-rich = Balmer lines detected but neither HeI or HeII
O = Only HeII absorptions lines detected
cont. = A high S/N spectrum in which no stellar features and HeII
emission lines were detected
Emission line = Spectrum where no absorption lines are present but the
observed emission lines have a stellar origin
Note (2): Detection flags as follows:
A = absorption
E = emission
- = undetected ion
N/D = data available
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Acknowledgements:
Walter Alfredo Weidmann, walter(at)oac.unc.edu.ar
(End) Walter A. Weidmann [OAC, Argentina], Patricia Vannier [CDS] 05-Feb-2018