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Emission lines in the optical spectrum of 3 Cen A

Wahlgren, Glenn LU and Hubrig, S. (2004) In Astronomy and Astrophysics 418(3). p.1073-1081
Abstract
Previously, weak emission lines had been detected at red wavelengths inthe spectra of a limited sample of mid to late B type main sequencestars. A fuller description of the occurrence and origins of these lineshas yet to be forwarded, in part due to the lack of observationsdetailing the spectral transitions involved. To address this deficiency,we present a line list of weak emission features found in the opticaland near infrared spectral region of the chemically peculiar He-weakstar 3 Cen A (HD 120709). Nearly 350 features, mostly associated withallowed transitions from high-excitation states of first ions, arecatalogued along with identifications. Prominent among the emissionlines are the spectra P II, Mn II, Fe II, Ni II and Cu II.... (More)
Previously, weak emission lines had been detected at red wavelengths inthe spectra of a limited sample of mid to late B type main sequencestars. A fuller description of the occurrence and origins of these lineshas yet to be forwarded, in part due to the lack of observationsdetailing the spectral transitions involved. To address this deficiency,we present a line list of weak emission features found in the opticaland near infrared spectral region of the chemically peculiar He-weakstar 3 Cen A (HD 120709). Nearly 350 features, mostly associated withallowed transitions from high-excitation states of first ions, arecatalogued along with identifications. Prominent among the emissionlines are the spectra P II, Mn II, Fe II, Ni II and Cu II. Emissionlines from Ca II, Si II and Hg II are also evident. Abundances aredetermined for several elements from synthetic spectrum fitting, withanomalies detected for the ions O I/II, P II/III and Si II/III. The LTEsynthetic spectrum fitting also revealed that the low excitation 4s-4ptransitions of Fe II predict an abundance that is greater than thatdetermined from higher excitation 4d-4f transitions. Several of theselatter transitions have upper energy levels that are found to beassociated with emission lines. We also present empirical considerationsfor the excitation processes leading to the weak emission lines.Based on observations obtained at the European Southern Observatory, LaSilla, Chile, No. 65.L-0316 and Paranal, Chile No. 266.D-5655.Tables 2 and 3 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/1073 (Less)
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author
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
line: identification, stars: abundances, stars: chemically peculiar, stars: emission, stars: individual: 3 Cen A
in
Astronomy and Astrophysics
volume
418
issue
3
pages
1073 - 1081
publisher
EDP Sciences
external identifiers
  • wos:000221646300026
  • scopus:2342486083
ISSN
1432-0746
DOI
10.1051/0004-6361:20034257
language
English
LU publication?
yes
id
83eae259-1c97-4b37-ba2d-ec7e93bc5d35 (old id 134124)
date added to LUP
2007-07-20 14:30:25
date last changed
2017-07-09 04:18:24
@article{83eae259-1c97-4b37-ba2d-ec7e93bc5d35,
  abstract     = {Previously, weak emission lines had been detected at red wavelengths inthe spectra of a limited sample of mid to late B type main sequencestars. A fuller description of the occurrence and origins of these lineshas yet to be forwarded, in part due to the lack of observationsdetailing the spectral transitions involved. To address this deficiency,we present a line list of weak emission features found in the opticaland near infrared spectral region of the chemically peculiar He-weakstar 3 Cen A (HD 120709). Nearly 350 features, mostly associated withallowed transitions from high-excitation states of first ions, arecatalogued along with identifications. Prominent among the emissionlines are the spectra P II, Mn II, Fe II, Ni II and Cu II. Emissionlines from Ca II, Si II and Hg II are also evident. Abundances aredetermined for several elements from synthetic spectrum fitting, withanomalies detected for the ions O I/II, P II/III and Si II/III. The LTEsynthetic spectrum fitting also revealed that the low excitation 4s-4ptransitions of Fe II predict an abundance that is greater than thatdetermined from higher excitation 4d-4f transitions. Several of theselatter transitions have upper energy levels that are found to beassociated with emission lines. We also present empirical considerationsfor the excitation processes leading to the weak emission lines.Based on observations obtained at the European Southern Observatory, LaSilla, Chile, No. 65.L-0316 and Paranal, Chile No. 266.D-5655.Tables 2 and 3 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/418/1073},
  author       = {Wahlgren, Glenn and Hubrig, S.},
  issn         = {1432-0746},
  keyword      = {line: identification,stars: abundances,stars: chemically peculiar,stars: emission,stars: individual: 3 Cen A},
  language     = {eng},
  number       = {3},
  pages        = {1073--1081},
  publisher    = {EDP Sciences},
  series       = {Astronomy and Astrophysics},
  title        = {Emission lines in the optical spectrum of 3 Cen A},
  url          = {http://dx.doi.org/10.1051/0004-6361:20034257},
  volume       = {418},
  year         = {2004},
}