Eclipsing Binaries From the Cstar Project at Dome A, Antarctica

Yang, Ming; Zhang, Hui; Wang, Songhu; Zhou, Ji-Lin; Zhou, Xu; Wang, Lingzhi; Wang, Lifan; Wittenmyer, R. A.; Liu, Hui-Gen; Meng, Zeyang; Ashley, M. C. B.; Storey, J. W. V.; Bayliss, Daniel; Tinney, C. G.; Wang, Ying; Wu, Dong-Hong; Liang, En-Si; Zhang, Yu; Zhou, Fan; Li, Feng; Gong, Xuefei; Lawrence, Jon; Liu, Qiang; Luong-Van, D.; Ma, Jun; Wu, Zhenyu; Yan, Jun; Yang, Huigen; Yang, Ji; Yuan, Xiangyan; Zhang, Tianmeng; Zhu, Zhenxi; Zou, Hu

doi:10.1088/0067-0049/217/2/28

Cited by 16 publications

(13 citation statements)

References 51 publications

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“…Various efforts have been made to reduce the systematic errors and to push the photometric precision below a few mmag, including the modeling of the inhomogeneous effects of clouds (Wang et al 2012), the ghost images (Meng et al 2013), and the systematic diurnal residuals (Wang et al 2014b). Based on the detrended light curves obtained during the 2008 winter season, comprehensive studies on exoplanet candidates (Wang et al 2014a), stellar variability , eclipsing binaries (Yang et al 2015), and stellar flares (Liang et al 2016) were carried out. Other independent studies include those on variable sources (Wang et al 2011(Wang et al , 2013Oelkers et al 2015), and specific studies on the pulsation modes of RR Lyrae stars (Huang et al 2015) and δ Scuti variables based on the CSTAR observations in single or multiple years from 2008 through 2010.…”

Section: Introductionmentioning

confidence: 99%

Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera

Yang

Moore

Krisciunas

et al. 2017

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The summit of the Antarctic plateau, Dome A, is proving to be an excellent site for optical, near-infrared, and terahertz astronomical observations. Gattini is a wide-field camera installed on the PLATO instrument module as part of the Chinese-led traverse to Dome A in 2009 January. We present here the measurements of sky brightness with the Gattini ultra-large field of view ( ´ 90 90 ) in the photometric B-, V-, and R-bands; cloud cover statistics measured during the 2009 winter season; and an estimate of the sky transparency. A cumulative probability distribution indicates that the darkest 10% of the nights at Dome A have sky brightness of S B =22.98, S V =21.86, and S R =21.68 mag arcsec −2 . These values were obtained during the year 2009 with minimum aurora, and they are comparable to the faintest sky brightness at Maunakea and the best sites of northern Chile. Since every filter includes strong auroral lines that effectively contaminate the sky brightness measurements, for instruments working around the auroral lines, either with custom filters or with high spectral resolution instruments, these values could be easily obtained on a more routine basis. In addition, we present example light curves for bright targets to emphasize the unprecedented observational window function available from this ground-based site. These light curves will be published in a future paper.

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Section: Introductionmentioning

confidence: 99%

Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera

Yang

Moore

Krisciunas

et al. 2017

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“…The luminosities of the components are computed with L=4πσR 2 T 4 as L 1 =2.62L e and L 2 =0.064L e , respectively, and the spectral type of the secondary star is estimated as K4 according to its temperature. The parameters obtained from this work and those from Yang et al (2015) are listed in Table 4. According to the morphologies of automated classifier, CSTAR036162 was classified as a semi-detached binary system by Yang et al (2015).…”

Section: Cstar036162mentioning

confidence: 99%

“…CSTAR consists of four 14.5 cm optical Schmidt-Cassegrain telescopes, each of which has a field of view of 4°.5×4°.5 with different (g, r, i and open) Sloan filters (Frei et al 1996;. Fifty-three eclipsing binaries among more than 260 variable stars have been detected from the three-year observations (Yang et al 2015). Three stars, CSTAR036162, CSTAR055495, and CSTAR057775, are found to have relatively high precision and long duration coverage data in three filters, and they receive top priority to be analyzed among these eclipsing binary stars.…”

Section: Introductionmentioning

confidence: 99%

“…Photometric light curves of the three binaries in the i band were collected by CSTAR in 2008 and extracted by Wang et al (2011). With the light curves, Yang et al (2015) provided the orbital parameters, including the temperature ratio (T 2 /T 1 ), eccentricity (e), and sine of inclination (sin i) of the systems by using the Eclipsing Binaries via Articial Intelligence method (EBAI; automated modeling, Devinney et al 2005Devinney et al , 2006. The results indicate that CSTAR036162 and CSTAR055495 are semi-detached systems while CSTAR057775 is a contact system.…”

Section: Introductionmentioning

confidence: 99%

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Photometric Solutions of Three Eclipsing Binary Stars Observed from Dome A, Antarctica

Liu

Zong

et al. 2018

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Based on spectroscopic observations for the eclipsing binaries CSTAR036162 and CSTAR055495 with the WiFeS/2.3 m telescope at SSO and CSTAR057775 with the Mage/MagellanI at LCO in 2017, stellar parameters are derived. More than 100 nights of almost-continuous light curves reduced from the time-series photometric observations by CSTAR at Dome A of Antarctic in i in 2008 and in g and r in 2009, respectively, are applied to find photometric solutions for the three binaries with the Wilson-Devinney code. The results show that CSTAR036162 is a detached configuration with the mass ratio q=0.354±0.0009, while CSTAR055495 is a semi-detached binary system with the unusual q=0.946±0.0006, which indicates that CSTAR055495 may be a rare binary system with mass ratio close to one and the secondary component filling its Roche Lobe. This implies that a mass-ratio reversal has just occurred and CSTAR055495 is in a rapid mass-transfer stage. Finally, CSTAR057775 is believed to be an A-type WUMa binary with q=0.301±0.0008 and a fill-out factor of f=0.742(8).

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“…A total of 1879 EBs from the Kepler mission (Prša et al 2011a) were also analyzed using the EBAI ANN, and their physical parameters were extracted from their LCs. More recently, Yang et al (2015) employed the EBAI pipeline to calculate the physical parameters of 50 EBs observed with the Chinese Small Telescope ARray (CSTAR). In spite of these successful applications, it must be kept in mind that only some of the physical parameters can be extracted from the LCs, namely those that have a significant effect on the LC and differ between EB subtypes.…”

Section: Introductionmentioning

confidence: 99%

Physical Parameters of Northern Eclipsing Binaries in the Catalina Sky Survey

Παπαγεωργίου

Catelan

Christopoulou

et al. 2019

ApJS

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We present the physical properties for 2281 northern eclipsing binary (EB) stars with eclipsing Algol (EA)-type light-curve (LC) morphology, based on data extracted from the Catalina Sky Survey (CSS). Our study is based on the analysis of the Eclipsing Binary via Artificial Intelligence (EBAI) artificial neural network (ANN) tool. An intensive search for the optimal ANN topology was performed. In order to feed the ANN with LCs that are representative of the CSS observations, two independent methods, based on template fitting and on the Two-Gaussian Model, were applied. As a result, five principal physical parameters were determined using only the CSS LCs, namely the temperature ratio,

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Eclipsing Binaries From the Cstar Project at Dome A, Antarctica

Cited by 16 publications

References 51 publications

Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera

Optical Sky Brightness and Transparency during the Winter Season at Dome A Antarctica from the Gattini-All-Sky Camera

Photometric Solutions of Three Eclipsing Binary Stars Observed from Dome A, Antarctica

Physical Parameters of Northern Eclipsing Binaries in the Catalina Sky Survey

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