A catalogue of eclipsing variables

Malkov, O. Yu.; Oblak, E.; Snegireva, E. A.; Torra, J.

doi:10.1051/0004-6361:20053137

Cited by 175 publications

(118 citation statements)

References 37 publications

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“…In addition to querying for any existing RV values, we also queried for multiplicity flags from catalogues using VizieR (Dommanget & Nys 2002;Malkov et al 2006;Pourbaix et al 2004;Worley & Douglass 1996), whether the system has previously been identified to have one or more companions. Out of our sub-sample of the overall SACY sample and probing only the SB systems, we found the previous multiplicity results:…”

Section: B2 Archival Multiplicity Flagsmentioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2014

A&A

129

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Context. Dynamically undisrupted, young populations of stars are crucial in studying the role of multiplicity in relation to star formation. Loose nearby associations provide us with a great sample of close (<150 pc) pre-main sequence (PMS) stars across the very important age range (≈5−70 Myr) to conduct such research. Aims. We characterize the short period multiplicity fraction of the search for associations containing young stars (SACY) sample, accounting for any identifiable bias in our techniques and present the role of multiplicity fractions of the SACY sample in the context of star formation. Methods. Using the cross-correlation technique we identified double-lined and triple-lined spectroscopic systems (SB2/SB3s), in addition to this we computed radial velocity (RV) values for our subsample of SACY targets using several epochs of Fiber-fed Extended Range Optical Spectrograph (FEROS) and Ultraviolet and Visual Echelle Spectrograph (UVES) data. These values were used to revise the membership of each association that was then combined with archival data to determine significant RV variations across different data epochs characteristic of multiplicity; single-lined multiple systems (SB1). Results. We identified seven new multiple systems (SB1s: 5, SB2s: 2). We find no significant difference between the short period multiplicity fraction (F m ) of the SACY sample and that of close star-forming regions (≈1−2 Myr) and the field (F m ≤ 10%). These are seen both as a function of age and as a function of primary mass, M 1 , in the ranges P [1:200 day] and M 2 [0.08 M -M 1 ], respectively. Conclusions. Our results are consistent with the picture of universal star formation, when compared to the field and close star-forming regions (SFRs). We comment on the implications of the relationship between increasing multiplicity fraction with the primary mass within the close companion range in relation to star formation.

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Section: B2 Archival Multiplicity Flagsmentioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2014

A&A

129

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“…There has been a very large amount of effort invested in the search and characterization of eclipsing binaries in different evolutionary stages (Popper 1980;Strassmeier et al 1993Barrado et al 1994Malkov et al 2006). Recently a significant number of both low-mass and PMS EB have been incorporated into this essential database (Shkolnik et al 2008;Stassun et al 2014;David et al 2016).…”

Section: Sizes: Eclipsing Binariesmentioning

confidence: 99%

Clusters: Age Scales for Stellar Physics

Barrado

2016

EAS Publications Series

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Abstract. Ages are key to truly understand a large plethora of astrophysical phenomena. On the other hand, stellar clusters are open windows to understand stellar evolution, specifically, the change with time and mass of different stellar properties. As such, they are our laboratories where different theories can be tested, but without accurate ages, our knowledge would impaired. We revisit here a large number of age-dating techniques and discuss their advantages and draw-backs. In addition, a step-by step process is suggested in order to built a coherent age scale ladder, minimizing the error budget and the sources of uncertainty.

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“…Among the four previously-known sources from Table 2, three (KSP-V871, V977, V1099) are classified as eclipsing binaries (Christiansen et al 2008;Malkov et al 2006) while the other one (KSP-V981) is an AGN (Jones et al 2009). This shows that our classification is overall in a good agreement with previous results.…”

Section: Classifications and Variable Typesmentioning

confidence: 99%

“…In other words, while Malkov et al (2006) This list includes 18 objects in total, with 14 from Table 1 and 4 from Table 2; their object id. in this paper is listed in column (1), their name as appearing on SIMBAD is shown in column (2), and their primary reference is listed in column (3).…”

Section: Classifications and Variable Typesmentioning

confidence: 99%

Kmtnet Supernova Program Variable Objects I. NGC 2784 Field

He¹,

Neilson²,

Lee³

et al. 2016

Journal of The Korean Astronomical Society

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We present analyses of ∼1250 variable sources identified in a 20 square degree field toward NGC 2784 by the KMTNet Supernova Program. We categorize the variable sources into three groups based on their B-band variability. The first group consists of 31 high variability sources with their Bband RMS variability greater than 0.3 magnitudes. The second group of medium variability contains 265 sources with RMS variability between 0.05 and 0.3 magnitudes. The remaining 951 sources belong to the third group of low variability with an RMS variability smaller than 0.05 magnitudes. Of the entire ∼1250 sources, 4 clearly show periods of variability greater than 100 days, while the rest have periods shorter than ∼51 days or no reliable periods. The majority of the sources show either rather irregular variability or short periods faster than 2 days. Most of the sources with reliable period determination between 2 and 51 days belong to the low-variability group, although a few belong to the medium-variability group. All the variable sources with periods longer than 35 days appear to be very red with B − V > 1.5 and V − I > 2.1 magnitudes. We classify candidates of 51 Cepheids, 17 semi-regular variables, 3 Mira types, 2 RV(B) Tauri stars, 26 eclipsing binary systems and 1 active galactic nucleus. The majority of long-term variables in our sample belong to either Mira or semi-regular types, indicating that long-term variability may be more prominent in post-main sequence phases of late-type stars. The depth of the eclipsing dips of the 26 candidates for eclipsing binaries is equivalent to ∼0.61 as the average relative size of the two stars in the binary system. Our results illustrate the power of the KMTNet Supernova Program for future studies of variable objects.

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A catalogue of eclipsing variables

Cited by 175 publications

References 37 publications

Search for associations containing young stars (SACY)

Search for associations containing young stars (SACY)

Clusters: Age Scales for Stellar Physics

Kmtnet Supernova Program Variable Objects I. NGC 2784 Field

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