Eclipsing Binary Stars in the Large and Small Magellanic Clouds from the MACHO Project: The Sample

Faccioli, L.; Alcock, C.; Cook, K. H.; Prochter, Gabriel E.; Protopapas, Pavlos; Syphers, David

doi:10.1086/521579

Cited by 51 publications

(61 citation statements)

References 68 publications

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“…We found it to be an eclipsing binary, which suggests binarity as a natural explanation for stars exhibiting such composite features in their spectra. This star was reported by Faccioli et al (2007) as an eclipsing binary, however we are the first to make the connection to its spectral type.…”

Section: Resultsmentioning

confidence: 74%

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Variability of massive stars with known spectral types in the Small Magellanic Cloud using 8 years of OGLE-III data

Kourniotis

Bonanos

Soszyński

et al. 2014

A&A

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We present a variability study of 4646 massive stars in the Small Magellanic Cloud (SMC) with known spectral types from the catalog of Bonanos et al. (2010) using the light curves from the OGLE-III database. The goal is to exploit the time domain information available through OGLE-III to gain insight into the processes that govern the evolution of massive stars. This variability survey of massive stars with known spectral types is larger than any previous survey by a factor of 7. We find that 60% of our sample (2766 stars) show no significant variability and 40% (1880 stars) exhibit variability distributed as follows: 807 stars display low-amplitude stochastic variability with fluctuations in the I-band of up to 0.05 mag, 443 stars present irregular variability of higher amplitude (76% of these are reported as variables for the first time), 205 are eclipsing binaries (including 101 newly discovered systems), 50 are candidate rotating variables, 126 are classical Cepheids, 188 stars exhibit short-term sinusoidal periodicity (P < 3 days) making them candidate "slowly pulsating B stars" and non-radial Be pulsators, and 61 periodic stars exhibit longer periods. We demonstrate the wealth of information provided in the time domain, by doubling the number of known massive eclipsing binary systems and identifying 189 new candidate early-type Be and 20 Oe stars in the SMC. In addition, we find that ∼80% of Be stars are photometrically variable in the OGLE-III time domain and provide evidence that short-term pulsating stars with additional photometric variability are rotating close to their break-up velocity.

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Section: Resultsmentioning

confidence: 74%

“…The input catalog contains 45 EBs that have already been analyzed by Hilditch et al (2005) and Harries et al (2003). We have also identified 59 EBs, using the VizieR catalog, which have been reported in previous works, mainly by Wyrzykowski et al (2004) and Faccioli et al (2007). Six of these have been spectroscopically confirmed.…”

Section: Resultsmentioning

confidence: 88%

Variability of massive stars with known spectral types in the Small Magellanic Cloud using 8 years of OGLE-III data

Kourniotis

Bonanos

Soszyński

et al. 2014

A&A

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“…For all of the systems we harvested the Macho (Faccioli et al 2007) and Ogle (Graczyk et al 2011) photometry available online. These photometric data were used both for minima times analysis as well as for light curve analysis.…”

Section: Photometrymentioning

confidence: 99%

Apsidal motion and absolute parameters for five LMC eccentric eclipsing binaries

Zasche

Wolf

2013

A&A

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Aims. As part of our observational projects at the La Silla Danish 1.54-meter telescope, we aim to measure the precise times of minimum light for eccentric eclipsing binaries in the Large Magellanic Cloud, needed for accurate determination of apsidal motion. Many new times of minima were derived from the photometric databases OGLE and MACHO. Several new minima were also observed. Methods. The O-C diagrams of the systems were analysed using all reliable timings found in the literature, and new or improved elements of apsidal motion were obtained. Light and radial velocity curves of MACHO 81.8881.47 and MACHO 79.5377.76 were analysed using the program PHOEBE. Results. We derived for the first time or significantly improved the relatively short periods of apsidal motion of 211 (12), 127 (8), 48 (13), 103 (20), and 42 (19) years, respectively. The internal structure constants, log k 2 , were found to be -2.37, -2.47, -2.17, -2.02, and -1.86 respectively, under the assumption that the component stars rotate pseudosynchronously. The relativistic effects are weak, up to 6% of the total apsidal motion rate. The masses for MACHO 81.8881.47 resulted in 5.51 (0.21) and 5.40 (0.19) M , while for MACHO 79.5377.76 the masses are 11.26 (0.35) and 11.27 (0.35) M , respectively.

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“…These systems are #0720, #2534, #3677, #4955, #5422, and #5434 (to this group of stars, two systems #0888 and #3951 also belong, but these were given a special focus in the following subsections). These binaries were also discovered by Udalski et al (1998) and Faccioli et al (2007); for some of them, a short note about their apsidal motion was published. The spectral types for these systems given by Evans et al (2004) and Bonanos et al (2010) are in good agreement with our spectral types that are estimated from the dereddened photometric indices.…”

Section: Notes On Individual Systemsmentioning

confidence: 61%

“…The core of our analysis lies on the huge photometric data sets, as obtained during the Macho (Faccioli et al 2007), Ogle II (Wyrzykowski et al 2004), and Ogle III (Graczyk et al 2011) surveys. These photometric data were used both for minima time analysis and for light curve analysis.…”

Section: Photometry and Light Curve Modellingmentioning

confidence: 99%

Apsidal motion and a light curve solution for eighteen SMC eccentric eclipsing binaries

Zasche

Wolf

Vraštil

et al. 2014

A&A

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Aims. The Danish 1.54-meter telescope at the La Silla observatory was used for photometric monitoring of selected eccentric eclipsing binaries located in the Small Magellanic Cloud. The new times of minima were derived for these systems, which are needed for accurate determination of the apsidal motion. Moreover, many new times of minima were derived from the photometric databases OGLE and MACHO. Eighteen early-type eccentric-orbit eclipsing binaries were studied. Methods. Their O-C diagrams of minima timings were analysed and the parameters of the apsidal motion were obtained. The light curves of these eighteen binaries were analysed using the program PHOEBE, giving the light curve parameters. For several systems, the additional third light also was detected. Results. We derived for the first time and significantly improved the relatively short periods of apsidal motion from 19 to 142 years for these systems. The relativistic effects are weak, up to 10% of the total apsidal motion rate. For one system (OGLE-SMC-ECL-0888), the third-body hypothesis was also presented, which agrees with high value of the third light for this system detected during the light curve solution.

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Eclipsing Binary Stars in the Large and Small Magellanic Clouds from the MACHO Project: The Sample

Abstract: We present a new sample of 4634 eclipsing binary stars in the Large Magellanic Cloud (LMC), expanding on a previous sample of 611 objects and a new sample of 1509 eclipsing binary stars in the Small Magellanic Cloud (SMC), that were identified in the 1 LFaccioli@lbl.gov 2

Cited by 51 publications

References 68 publications

Variability of massive stars with known spectral types in the Small Magellanic Cloud using 8 years of OGLE-III data

Variability of massive stars with known spectral types in the Small Magellanic Cloud using 8 years of OGLE-III data

Apsidal motion and absolute parameters for five LMC eccentric eclipsing binaries

Apsidal motion and a light curve solution for eighteen SMC eccentric eclipsing binaries

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