Binaries: eclipsing
Tracing the structure of the Milky Way with detached eclipsing binaries from the VVV survey I The method and initial results
... There are a number of systems found even further, on distances corresponding to the Sagittarius dwarf spheroidal galaxy (Sgr dSph) and its stream. If confirmed, they would be the first eclipsing binaries ...
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Orbital and physical parameters of eclipsing binaries from the All Sky Automated Survey catalogue
... our eclipsing bina- ries, we used time-consistent photometric data ...Of Eclipsing BinariEs (PHOEBE; Prša & Zwitter 2005) code, which is an implementation of the Wilson-Devinney (WD) code (Wilson ...
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An Updated Catalog of 4680 Northern Eclipsing Binaries with Algol type Light curve Morphology in the Catalina Sky Surveys
... 205 eclipsing W UMa-type systems from CSS ( ...Close binaries are known to be signi fi cantly more active than wide binaries and single stars ( ...
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HATS 36b and 24 Other Transiting/Eclipsing Systems from the HATSouth K2 Campaign 7 Program
... This program shows the bene fi t of using high-precision K2 space-based photometry to vet candidates identi fi ed from ground-based surveys. This concept will naturally extend to the TESS mission ( Ricker et al. 2014 ) . ...
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An eclipsing post common envelope binary in the field of the Kepler mission
... the physical parameters of the components: radii, masses and ef- fective temperatures. This is one of the very few cases in which the mass and radii of the white dwarfs can be measured independently if precise enough ...
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THE ARAUCARIA PROJECT: A STUDY OF THE CLASSICAL CEPHEID IN THE ECLIPSING BINARY SYSTEM OGLE LMC562 05 9009 IN THE LARGE MAGELLANIC CLOUD
... The p-factor value for the Cepheid is marginally consistent with the prediction of the p-factor relation of Storm et al. ( 2011 ) , as opposed to the p-factor we derived for OGLE-LMC- CEP-0227 in P13, which is in signi fi ...
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Post common envelope binaries from SDSS IX: Constraining the common envelope efficiency
... The theoretical research presented here has become possible due to considerable observational efforts in the last decade. First of all, the SDSS (Adelman-McCarthy et al. 2008; Abazajian et al. 2009) proved to e ffi ciently ...
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Deep census of variable stars in a VLT/VIMOS field in Carina
... are eclipsing or ellip- soidal binaries, while the other half are pulsating variables of different types, mostly δ Scuti ...are eclipsing/ellipsoidal binaries, while three are pulsating ...
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The ACS survey of Galactic globular clusters XII Photometric binaries along the main sequence
... As anticipated in Sect. 2, we removed from our list all clus- ters for which we had no proper motion (two epochs data) and for which Girardi et al. (2005) model was prediction a field star contamination larger than 1%, ...
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Toward precise ages for single stars in the field Gyrochronology constraints at several Gyr using wide binaries I Ages for initial sample
... Before proceeding to the selection of targets, we briefly discuss the impact on our program of undetected higher order multiplicity among wide binaries (Correia et al. 2006; Tokovinin et al. 2010). If the evolved ...
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Unveiling the nature of INTEGRAL objects through optical spectroscopy X A new multi year, multi observatory campaign
... Within the framework of our program (running since 2004) of identification of hard X-ray INTEGRAL sources through optical spectroscopy, we present the results concerning the nature of 33 high-energy objects. The data ...
21
Globular Clusters and X Ray Point Sources in Centaurus A (NGC 5128)
... A few outlying X-ray sources in the BVI diagram are quite faint, and could represent contaminant sources (foreground stars or background galaxies). Furthermore, a few objects, shown in the (B V ) versus V plot, show ...
13
Luminosity functions of LMXBs in centaurus a : globular clusters versus the field
... law. Separating globular cluster and field sources, we find a statistically significant difference between the two luminosity distributions with a relative underabundance of faint sources in the globular cluster ...
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The influence of multiple stars on the high mass stellar initial mass function and age dating of young massive star clusters
... cent binaries or higher order multiples), the difference between the power-law index of the mass function (MF) of all stars and the observed MF is small ...unresolved binaries amongst pre-main-sequence ...
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Accretion of clumpy cold gas onto massive black hole binaries: a possible fast route to binary coalescence
... In currently favoured hierarchical cosmologies, the formation of massive black hole binaries (MBHBs) following galaxy mergers is unavoidable. Still, due the complex physics governing the (hydro)dynamics of the ...
18
The Globular Cluster NGC 6402 (M14) II Variable Stars
... We present time-series BV I photometry for the Galactic globular cluster NGC 6402 (M14). The data con- sists of ∼137 images per filter, obtained using the 0.9m and 1.0m SMARTS telescopes at the Cerro Tololo ...
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Supervised detection of anomalous light curves in massive astronomical catalogs
... Our method is suitable for exploring massive datasets given that the training process is performed offline. We tested our algorithm on 20 million light-curves from the MACHO catalog and generated a list of anomalous ...
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Unveiling the nature of INTEGRAL objects through optical spectroscopy VIII Identification of 44 newly detected hard X ray sources
... X-ray binaries, probably because of their larger obscuration in optical bands due to their location in the Galactic plane; like- wise, X-ray timing studies of course are more effective in dis- covering Galactic ...
21
A search for dormant binaries with degenerate components in omega Centauri and NGC 6397
... degenerate binaries from short-period, low-amplitude optical variables cataloged in existing surveys and measured their radial ...degenerate binaries; in particular, it is observed in optical counterparts ...
9
Post common envelope binaries from SDSS: VIII Evidence for disrupted magnetic braking
... compact binaries assumes magnetic braking to be very e ffi cient as long as the secondary star has a radiative core, but to be negligible if the secondary star is fully ...envelope binaries (PCEBs) crucially ...
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