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Date and Time of the Query: 2018-07-20 T07:12:40 PDT
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For refcode 2007AJ....134.2474M:
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Copyright by American Astronomical Society. Reproduced by permission
2007AJ....134.2474M A Survey of Local Group Galaxies Currently Forming Stars. III. A Search for Luminous Blue Variables and Other H{alpha} Emission-Line Stars Massey, Philip; McNeill, Reagin T.; Olsen, K. A. G.; Hodge, Paul W.; Blaha, Cynthia; Jacoby, George H.; Smith, R. C.; Strong, Shay B. Abstract. We describe a search for H{alpha} emission-line stars in M31, M33, and seven dwarfs in or near the Local Group (IC 10, NGC 6822, WLM, Sextans B, Sextans A, Pegasus, and the Phoenix dwarf) using interference filter imaging with the KPNO and CTIO 4 m telescopes and Mosaic cameras. The survey is aimed primarily at identifying new luminous blue variables (LBVs) from their spectroscopic similarity to known LBVs, avoiding the bias toward photometric variability, which may require centuries to manifest itself if LBVs go through long quiescent periods. Follow-up spectroscopy with WIYN confirms that our survey detected a wealth of stars whose spectra are similar to the known LBVs. We "classify" the spectra of known LBVs and compare these to the spectra of the new LBV candidates. We demonstrate spectacular spectral variability for several of the new LBV candidates, such as AM2, previously classified as a Wolf-Rayet star (WR), which now shows Fe I, Fe II, and Balmer emission lines but neither the N III {lambda}{lambda}4634, 4642 nor the He II {lambda}4686 emission it did in 1982. Profound spectral changes are also noted for other suspected and known LBVs. Several of the LBV candidates also show >0.5 mag changes in V over the past 10-20 years. The number of known or suspected LBVs is now 24 in M31, 37 in M33, 1 in NGC 6822, and 3 in IC 10. We estimate that the total number of LBVs in M31 and M33 may be several hundred, in contrast to the eight known historically through large-scale photometric variability. This has significant implications for the timescale of the LBV phase. We also identify a few new WRs and peculiar emission-line objects.
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