The ASAS-SN catalogue of variable stars I: The Serendipitous Survey

Jayasinghe, T.; Kochanek, C. S.; Stanek, K. Z.; Shappee, B. J.; Holoien, T. W. S.; Thompson, T. A.; Prieto, J. L.; Dong, Subo; Pawlak, M.; Shields, J.; Pojmański, G.; Otero, S.; Britt, Chris; Will, D.

doi:10.1093/mnras/sty838

Cited by 357 publications

(317 citation statements)

References 72 publications

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“…• The photometric light curves in the V-band were collected from the All-Sky Automated Survey for Supernovae (ASAS-SN, Shappee et al 2014;Kochanek et al 2017;Jayasinghe et al 2018).…”

Section: Datamentioning

confidence: 99%

Evidence for Galactic disc RR Lyrae stars in the solar neighbourhood

Prudil

Dékány

Grebel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present a kinematical study of 314 RR Lyrae stars in the solar neighbourhood using the publicly available photometric, spectroscopic, and Gaia DR2 astrometric data to explore their distribution in the Milky Way. We report an overdensity of 22 RR Lyrae stars in the solar neighbourhood at a pericenter distance of between 5-9 kpc from the Galactic center. Their orbital parameters and their chemistry indicate that these 22 variables share the kinematics and the [Fe/H] values of the Galactic disc, with an average metallicity and tangential velocity of [Fe/H]=−0.60 dex and v θ = 241 km s −1 , respectively. From the distribution of the Galactocentric spherical velocity components, we find that these 22 disc-like RR Lyrae variables are not consistent with the Gaia Sausage (Gaia-Enceladus), unlike almost half of the local RR Lyrae stars. Chemical information from the literature shows that the majority of the selected pericenter peak RR Lyrae variables are α-poor, a property shared by typically much younger stars in the thin disc. Using the available photometry we rule out a possible misclassification with the known classical and anomalous Cepheids. The similar kinematic, chemical, and pulsation properties of these disc RR Lyrae stars suggest they share a common origin. In contrast, we find the RR Lyrae stars associated with the Gaia-Enceladus based on their kinematics and chemical composition show a considerable metallicity spread in the old population (∼ 1 dex).

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“…• The photometric light curves in the V-band were collected from the All-Sky Automated Survey for Supernovae (ASAS-SN, Shappee et al 2014;Kochanek et al 2017;Jayasinghe et al 2018).…”

Section: Datamentioning

confidence: 99%

Evidence for Galactic disc RR Lyrae stars in the solar neighbourhood

Prudil

Dékány

Grebel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The sample of known CBs was recently significantly increased thanks to new data from several sky surveys that provide high-cadence, long-term, high-precision photometric observations in a range of passbands, including, e.g., the Catalina Sky Survey (CSS; Marsh et al 2017), the Wide-field Infrared Survey Explorer catalogue (WISE ; Chen et al 2018b), the All-Sky Automated Survey for Supernovae (ASAS-SN; Jayasinghe et al 2018), the Northern Sky Variability Survey (NSVS; Gettel et al 2006), and the Asteroid Terrestrial-impact Last Alert System (ATLAS; Heinze et al 2018). As sample sizes increased, researchers have taken advantage of the data from various surveys and constructed genuine CB samples for further statistical study (Rucinski 1995;Norton et al 2011;Marsh et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Physical Parameters of Late-type Contact Binaries in the Northern Catalina Sky Survey

Sun

Chen

Deng

et al. 2020

ApJS

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We present the physical parameters of 2335 late-type contact binary (CB) systems extracted from the Catalina Sky Survey (CSS). Our sample was selected from the CSS Data Release 1 by strictly limiting the prevailing temperature uncertainties and light-curve fitting residuals, allowing us to almost eliminate any possible contaminants. We developed an automatic Wilson-Devinney-type code to derive the relative properties of CBs based on their light-curve morphology. By adopting the distances derived from CB (orbital) period-luminosity relations (PLRs), combined with the well-defined massluminosity relation for the systems' primary stars and assuming solar metallicity, we calculated the objects' masses, radii, and luminosities. Our sample of fully eclipsing CBs contains 1530 W-, 710 A-, and 95 B-type CBs. A comparison with literature data and with the results from different surveys confirms the accuracy and coherence of our measurements. The period distributions of the various CB subtypes are different, hinting at a possible evolutionary sequence. W-type CBs are clearly located in a strip in the total mass versus mass ratio plane, while A-type CBs may exhibit a slightly different dependence. There are no significant differences among the PLRs of A-and W-type CBs, but the PLR zero points are affected by their mass ratios and fill-out factors. Determination of zero-point differences for different types of CBs may help us improve the accuracy of the resulting PLRs. We demonstrate that automated approaches to deriving CB properties could be a powerful tool for application to the much larger CB samples expected to result from future surveys.

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“…In a series of papers, Jayasinghe et al (2018Jayasinghe et al ( , 2019b, we have been systematically identifying and classifying variables using data from The All-Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al 2014;Kochanek et al 2017). We have thus far discovered ∼220, 000 new variables and homogeneously classified both the new and previously known variables in the sample (Jayasinghe et al 2019a).…”

Section: Introductionmentioning

confidence: 99%

The ASAS-SN catalogue of variable stars – VII. Contact binaries are different above and below the Kraft break

Jayasinghe

Stanek

Kochanek

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We characterize ∼71, 200 W UMa type (EW) contact binaries, including ∼12, 600 new discoveries, using ASAS-SN V-band all-sky light curves along with archival data from Gaia, 2MASS, AllWISE, LAMOST, GALAH, RAVE, and APOGEE. There is a clean break in the EW period-luminosity relation at log(P/d) − 0.30, separating the longer period early-type (A sub-type) EW binaries from the shorter period, late-type (W sub-type) systems. The two populations are even more cleanly separated in the space of period and effective temperature, by T eff = 6710 K − 1760 K log(P/0.5 d). Early-type and late-type EW binaries follow opposite trends in T eff with orbital period. For longer periods, early-type EW binaries are cooler, while late-type systems are hotter. We derive period-luminosity relationships (PLRs) in the W J K , V, Gaia DR2 G, J, H, K s and W 1 bands for the late-type and early-type EW binaries separated both by period and effective temperature, and by period alone. The dichotomy of contact binaries is almost certainly related to the Kraft break and the related changes in envelope structure, winds and angular momentum loss.

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The ASAS-SN catalogue of variable stars I: The Serendipitous Survey

Cited by 357 publications

References 72 publications

Evidence for Galactic disc RR Lyrae stars in the solar neighbourhood

Evidence for Galactic disc RR Lyrae stars in the solar neighbourhood

Physical Parameters of Late-type Contact Binaries in the Northern Catalina Sky Survey

The ASAS-SN catalogue of variable stars – VII. Contact binaries are different above and below the Kraft break

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