Emission lines in the optical spectrum of 3 Cen A
(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)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/134124
- author
- Wahlgren, Glenn LU and Hubrig, S.
- organization
- publishing date
- 2004
- 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
- 2016-04-01 15:57:00
- date last changed
- 2024-01-10 22:43:21
@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}},
keywords = {{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 = {{https://lup.lub.lu.se/search/files/4522799/624412.pdf}},
doi = {{10.1051/0004-6361:20034257}},
volume = {{418}},
year = {{2004}},
}