The Catalina Surveys Southern periodic variable star catalogue

Drake, A. J.; Djorgovski, S. G.; Catelan, M.; Graham, M. J.; Mahabal, A.; Larson, S. M.; Christensen, E.; Torrealba, G.; Beshore, E. C.; McNaught, R. H.; Garradd, G. J.; Belokurov, V.; Koposov, S. E.

doi:10.1093/mnras/stx1085

Cited by 167 publications

(149 citation statements)

References 85 publications

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“…Its estimated photometric period is 0.768 d (VSX catalogue, Watson et al 2006). Nevertheless, its SB1 nature seems well established because the maximum RV difference is of the order of 100 km s −1 over only 1 d. Another SB1 candidate, GES 12394853-3653483, is reported in the VSX catalogue 6 -originally from the Catalina Sky Survey (Drake et al 2017) -as an eclipsing system of type EA (β Perseitype, i.e. Algol) with a photometric period of 1.438 d and an amplitude of 0.58 mag.…”

Section: False Positivesmentioning

confidence: 99%

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Merle

Swaelmen

Eck

et al. 2020

A&A

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Context. Multiple stellar systems play a fundamental role in the formation and evolution of stellar populations in galaxies. Recent and ongoing large ground-based multi-object spectroscopic surveys significantly increase the sample of spectroscopic binaries (SBs) allowing analyses of their statistical properties. Aims. We investigate the repeated spectral observations of the Gaia-ESO Survey internal data release 5 (GES iDR5) to identify and characterise SBs with one visible component (SB1s) in fields covering mainly the discs, the bulge, the CoRot fields, and some stellar clusters and associations. Methods. A statistical χ 2 -test is performed on spectra of the iDR5 subsample of approximately 43 500 stars characterised by at least two observations and a signal-to-noise ratio larger than three. In the GES iDR5, most stars have four observations generally split into two epochs. A careful estimation of the radial velocity (RV) uncertainties is performed. Our sample of RV variables is cleaned from contamination by pulsation-and/or convection-induced variables using Gaia DR2 parallaxes and photometry. Monte-Carlo simulations using the SB9 catalogue of spectroscopic orbits allow to estimate our detection efficiency and to correct the SB1 rate to evaluate the GES SB1 binary fraction and its relation to effective temperature and metallicity. Results. We find 641 (resp., 803) FGK SB1 candidates at the 5σ (resp., 3σ) level. The maximum RV differences range from 2.2 km s −1 at the 5σ confidence level (1.6 km s −1 at 3σ) to 133 km s −1 (in both cases). Among them a quarter of the primaries are giant stars and can be located as far as 10 kpc. The orbital-period distribution is estimated from the RV standard-deviation distribution and reveals that the detected SB1s probe binaries with log P[d] 4. We show that SB1s with dwarf primaries tend to have shorter orbital periods than SB1s with giant primaries. This is consistent with binary interactions removing shorter period systems as the primary ascends the red giant branch. For two systems, tentative orbital solutions with periods of 4 and 6 d are provided. After correcting for detection efficiency, selection biases, and the present-day mass function, we estimate the global GES SB1 fraction to be in the range 7-14% with a typical uncertainty of 4%. A small increase of the SB1 frequency is observed from K-towards F-type stars, in agreement with previous studies. The GES SB1 frequency decreases with metallicity at a rate of (−9 ± 3)% dex −1 in the metallicity range −2.7 ≤[Fe/H]≤ +0.6. This anticorrelation is obtained with a confidence level higher than 93% on a homogeneous sample covering spectral types FGK and a large range of metallicities. When the present-day mass function is accounted for, this rate turns to (−4 ± 2)% dex −1 with a confidence level higher than 88%. In addition we provide the variation of the SB1 fraction with metallicity separately for F, G, and K spectral types, as well as for dwarf and giant primaries.

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Section: False Positivesmentioning

confidence: 99%

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

Merle

Swaelmen

Eck

et al. 2020

A&A

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“…Drake et al (2014) used the Catalina Real-Time Transient Surveys DR1 to select a sample of 47,000 periodic variables, of which 16,797 are RR Lyrae, and the bulk of them are at R gc <40 kpc. In total, the Catalina Surveys RR Lyrae Data Release 1 6 (Drake et al 2013a(Drake et al , 2013b(Drake et al , 2014Torrealba et al 2015;Drake et al 2017) contains 43,599 RR Lyrae, of which 32,980 are RRab stars.…”

Section: Introductionmentioning

confidence: 99%

The Profile of the Galactic Halo from Pan-STARRS1 3π RR Lyrae

Hernitschek

Cohen

Rix

et al. 2018

ApJ

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We characterize the spatial density of the Pan-STARRS1 (PS1) sample of Rrab stars to study the properties of the old Galactic stellar halo. This sample, containing 44,403 sources, spans galactocentric radii of 0.55 kpcR gc 141 kpc with a distance precision of 3% and thus is able to trace the halo out to larger distances than most previous studies. After excising stars that are attributed to dense regions such as stellar streams, the Galactic disk and bulge, and halo globular clusters, the sample contains ∼11,000 sources within 20 kpcR gc 131 kpc. We then apply forward modeling using Galactic halo profile models with a sample selection function. Specifically, we use ellipsoidal stellar density models ρ(l, b, R gc ) with a constant and a radiusdependent halo flattening q(R gc ). Assuming constant flattening q, the distribution of the sources is reasonably well fit by a single power law with = 0.27 , an effective radius r eff =1.07±0.10 kpc, and a halo flattening of q=0.923±0.007. If we allow for a radius-dependent flattening q(R gc ), we find evidence for a distinct flattening of q∼0.8 of the inner halo at ∼25 kpc. Additionally, we find that the south Galactic hemisphere is more flattened than the north Galactic hemisphere. The results of our work are largely consistent with many earlier results (e.g., Watkins et al.; Iorio et al.). We find that the stellar halo, as traced in RR Lyrae stars, exhibits a substantial number of further significant over-and underdensities, even after masking all known overdensities.

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“…The rotational class consists of variable stars including the ellipsoidal variables (ELL) and spotted RS Canum Venaticorum (RS CVn) systems. A more detailed overview of the data set is given in Drake et al (2017) and Catelan & Smith (2015) gives a more detailed overview of the properties of the various types of pulsating stars.…”

Section: Datamentioning

confidence: 99%

“…This paper describes a new automatic classification pipeline for the classification of variable stars via application to archival data. To our knowledge, this is the first time the southern CRTS (Drake et al 2017) data set has been used to build/evaluate an automatic classification system. Similar work has been completed in recent years (Kim & Bailer-Jones 2016;Mahabal et al 2017;Narayan et al 2018), though the features used for learning are rarely evaluated in a statistically rigorous way.…”

Section: Introductionmentioning

confidence: 99%

Comparing Multiclass, Binary, and Hierarchical Machine Learning Classification schemes for variable stars

Hosenie

Lyon

Stappers

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Upcoming synoptic surveys are set to generate an unprecedented amount of data. This requires an automatic framework that can quickly and efficiently provide classification labels for several new object classification challenges. Using data describing 11 types of variable stars from the Catalina Real-Time Transient Surveys (CRTS), we illustrate how to capture the most important information from computed features and describe detailed methods of how to robustly use Information Theory for feature selection and evaluation. We apply three Machine Learning (ML) algorithms and demonstrate how to optimize these classifiers via cross-validation techniques. For the CRTS dataset, we find that the Random Forest (RF) classifier performs best in terms of balancedaccuracy and geometric means. We demonstrate substantially improved classification results by converting the multi-class problem into a binary classification task, achieving a balanced-accuracy rate of ∼99 per cent for the classification of δ-Scuti and Anomalous Cepheids (ACEP). Additionally, we describe how classification performance can be improved via converting a 'flat-multi-class' problem into a hierarchical taxonomy. We develop a new hierarchical structure and propose a new set of classification features, enabling the accurate identification of subtypes of cepheids, RR Lyrae and eclipsing binary stars in CRTS data.

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The Catalina Surveys Southern periodic variable star catalogue

Cited by 167 publications

References 85 publications

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

TheGaia-ESO Survey: detection and characterisation of single-line spectroscopic binaries

The Profile of the Galactic Halo from Pan-STARRS1 3π RR Lyrae

Comparing Multiclass, Binary, and Hierarchical Machine Learning Classification schemes for variable stars

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