The Optical Gravitational Lensing Experiment. Miras and Semiregular Variables in the Large Magellanic Cloud

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dc.creatorSoszynski, I.
dc.creatorUdalski, A.
dc.creatorKubiak, M.
dc.creatorSzymanski, M. K.
dc.creatorPietrzynski, G.
dc.creatorZebrun, K.
dc.creatorSzewczyk, O.
dc.creatorWyrzykowski, L.
dc.creatorUlaczyk, K.
dc.date2005-12-22
dc.date2005-12-31
dc.date.accessioned2026-07-07T06:49:13Z
dc.date.available2026-07-07T06:49:13Z
dc.descriptionWe use the OGLE-II and OGLE-III data in conjunction with the 2MASS near-infrared (NIR) photometry to identify and study Miras and Semiregular Variables (SRVs) in the Large Magellanic Cloud. We found in total 3221 variables of both types, populating two of the series of NIR period-luminosity (PL) sequences. The majority of these objects are double periodic pulsators, with periods belonging to both PL ridges. We indicate that in the period - Wesenheit index plane the oxygen-rich and carbon-rich AGB stars from the NIR PL sequences C, C' and D split into well separated ridges. Thus, we discover an effective method of distinguishing between O-rich and C-rich Miras, SRVs and stars with Long Secondary Periods using their V and I-band photometry. We present an empirical method of estimating the mean K_s magnitudes of the Long Period Variables using single-epoch K_s measurements and complete light curves in the I-band. We utilize these corrected magnitudes to show that the O-rich and C-rich Miras and SRVs follow somewhat different K_s-band PL relations.
dc.description18 pages, 6 figures, LaTeX. Photometric data presented in the paper are available from the OGLE Internet archive: http://ogle.astrouw.edu.pl/ or its US mirror: http://bulge.princeton.edu/~ogle/
dc.identifierhttps://arxiv.org/abs/astro-ph/0512578
dc.identifierhttp://arxiv.org/abs/astro-ph/0512578
dc.identifierActa Astron. 55 (2005) 331
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/104258
dc.subjectAstrophysics
dc.titleThe Optical Gravitational Lensing Experiment. Miras and Semiregular Variables in the Large Magellanic Cloud
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