The study of unclassified B[e] stars and candidates in the Galaxy and Magellanic Clouds. (arXiv:1906.04268v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Condori_C/0/1/0/all/0/1">C. A. H. Condori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fernandes_M/0/1/0/all/0/1">M. Borges Fernandes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraus_M/0/1/0/all/0/1">M. Kraus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Panoglou_D/0/1/0/all/0/1">D. Panoglou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guerrero_C/0/1/0/all/0/1">C. A. Guerrero</a>
We investigated 12 unclassified B[e] stars or candidates, 8 from the Galaxy,
2 from the Large Magellanic Cloud (LMC) and 2 from the Small Magellanic Cloud
(SMC). Based on the analysis of high-resolution spectroscopic (FEROS) and
photometric data, we confirmed the presence of the B[e] phenomenon for all
objects of our sample, except for one (IRAS 07455-3143). We derived their
effective temperature, spectral type, luminosity class, interstellar extinction
and, using the distances from Gaia DR2, we obtained their bolometric magnitude,
luminosity and radius. Modeling of the forbidden lines present in the FEROS
spectra revealed information about the kinematics and geometry of the
circumstellar medium of these objects. In addition, we analyzed the light
curves of four stars, finding their most probable periods. The evolutionary
stage of 11 stars of our sample is suggested from their position on the HR
diagram, taking into account evolutionary tracks of stars with solar, LMC and
SMC metallicities. As results, we identified B and B[e] supergiants, B[e] stars
probably at the main sequence or close to its end, post-AGB and HAeB[e]
candidates, and A[e] stars in the main sequence or in the pre-main sequence.
However, our most remarkable results are the identification of the third A[e]
supergiant (ARDB,54, the first one in the LMC), and of an “LBV impostor” in
the SMC (LHA 115-N82).
We investigated 12 unclassified B[e] stars or candidates, 8 from the Galaxy,
2 from the Large Magellanic Cloud (LMC) and 2 from the Small Magellanic Cloud
(SMC). Based on the analysis of high-resolution spectroscopic (FEROS) and
photometric data, we confirmed the presence of the B[e] phenomenon for all
objects of our sample, except for one (IRAS 07455-3143). We derived their
effective temperature, spectral type, luminosity class, interstellar extinction
and, using the distances from Gaia DR2, we obtained their bolometric magnitude,
luminosity and radius. Modeling of the forbidden lines present in the FEROS
spectra revealed information about the kinematics and geometry of the
circumstellar medium of these objects. In addition, we analyzed the light
curves of four stars, finding their most probable periods. The evolutionary
stage of 11 stars of our sample is suggested from their position on the HR
diagram, taking into account evolutionary tracks of stars with solar, LMC and
SMC metallicities. As results, we identified B and B[e] supergiants, B[e] stars
probably at the main sequence or close to its end, post-AGB and HAeB[e]
candidates, and A[e] stars in the main sequence or in the pre-main sequence.
However, our most remarkable results are the identification of the third A[e]
supergiant (ARDB,54, the first one in the LMC), and of an “LBV impostor” in
the SMC (LHA 115-N82).
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