Isolated Wolf-Rayet Stars and O Supergiants in the Galactic Center Region Identified via Paschen-alpha Excess
| Autor: | Mauerhan, Jon, Cotera, Angela, Dong, Hui, Morris, Mark, Wang, Daniel, Stolovy, Susan, Lang, Cornelia |
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| Rok vydání: | 2010 |
| Předmět: | |
| Zdroj: | ApJ (2010), 725, 188 |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1088/0004-637X/725/1/188 |
| Popis: | We report the discovery of 19 hot, evolved, massive stars near the Galactic center region (GCR). These objects were selected for spectroscopy owing to their detection as strong sources of Paschen-alpha emission-line excess, following a narrowband imaging survey of the central 0.65 x 0.25 degress (l, b) around Sgr A* with the Hubble Space Telescope. Discoveries include 5 carbon-type (WC) and 6 nitrogen-type (WN) Wolf-Rayet stars, 6 O supergiants, and 2 B supergiants. Two of the O supergiants have X-ray counterparts, the properties of which are broadly consistent with colliding-wind binaries and solitary O stars. The infrared photometry of 17 stars is consistent with the Galactic center distance, but 2 of them are located in the foreground. Several WC stars exhibit a relatively large infrared excesses, which is possibly the signature of thermal emission from hot dust. Most of the stars appear scattered throughout the GCR, with no relation to the three known massive young clusters; several others lie near the Arches and Quintuplet clusters and may have originated within one of these systems. The results of this work bring the total sample of Wolf-Rayet stars in the GCR to 92. All sources of strong P-alpha excess have been identified in the area surveyed with HST, which implies that the sample of WN stars in this region is near completion, and is dominated by late (WNL) types. The current WC sample, although probably not complete, is almost exclusively dominated by late (WCL) types. The observed Wolf-Rayet subtype distribution in the GCR is a reflection of the intrinsic rarity of early subtypes (WNE and WCE) in the inner Galaxy, an effect that is driven by metallicity. Comment: Correction to Fig 4,5,6,10, and Tables 3, 5. The spectrum of the previously known WC9 star WR101q had been mistakenly labeled as Star #19 in Fig. 5 of the original manuscript. Star #19 is actually a newly discovered WN5b star, whose spectrum was accidentally not included in the original paper. The correct WN5b spectrum is now included in Fig. 4. An erratum was submitted to ApJ on Aug 15, 2015 |
| Databáze: | arXiv |
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