Israel, G. L.; Negueruela, I.; Campana, S.; Covino, S.; Di Paola, A.; Maxwell, D. H.; Norton, A. J.; Speziali, R.; Verrecchia, F. and Stella, L.
PDF (Version of Record)
- Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
|DOI (Digital Object Identifier) Link:||https://doi.org/10.1051/0004-6361:20010417|
|Google Scholar:||Look up in Google Scholar|
We report on the identification of the optical/IR counterpart of the 29.5-s transient X-ray pulsar GS 1843+009. We re-analysed an archival ROSAT HRI observation of GS 1843+009, obtaining a new refined position. The optical and IR follow-up observations carried out for the new error circle allowed us to find a relatively faint (V=20.9) and variable early type reddened star (V-R=2.1). The optical spectra show the Balmer and Paschen series in emission, while the IR observations confirm the presence of a flux excess (H=13.2, J-H=0.54), suggesting that the star is surrounded by a circumstellar envelope. Spectroscopic and photometric data together indicate a B0-B2 IV-Ve spectral-type star located at a distance of ≥ 10 kpc confirming the Be-star/X-ray binary nature of GS 1843+009.
|Item Type:||Journal Article|
|Copyright Holders:||2001 ESO|
|Keywords:||binary stars; pulsars; emission-line; Be stars; X-ray binaries|
|Academic Unit/School:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Users 6827 not found.|
|Date Deposited:||05 Jul 2006|
|Last Modified:||15 Jan 2017 17:12|
|Share this page:|
Download history for this item
These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.