No Excess of Rr Lyrae Stars in the Canis Major Overdensity

Mateu, C.; Vivas, A. Katherina; Zinn, R.; Miller, L.; Abad, C.

doi:10.1088/0004-6256/137/5/4412

Cited by 47 publications

(48 citation statements)

References 62 publications

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“…Mateu et al 2009) have questioned this due to the lack of blue horizontal branch stars in the CMa CMD compared to this and other clusters also potentially associated with the CMa overdensity, such as NGC 1851, NGC 2298 and NGC 2808. Further study of these clusters is therefore crucial to improving our understanding of the structure of the Galactic disc, as Martin et al (2004) also suggested that CMa is made up of a mixture of thin and thick disc and spiral arm populations of the Milky Way.…”

Section: Introductionmentioning

confidence: 93%

Constraining the parameters of globular cluster NGC 1904 from its variable star population

Kains

Bramich

Jaimes

et al. 2012

A&A

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Aims. We present the analysis of 11 nights of V and I time-series observations of the globular cluster NGC 1904 (M 79). Using this we searched for variable stars in this cluster and attempted to refine the periods of known variables, making use of a time baseline spanning almost 8 years. We use our data to derive the metallicity and distance of NGC 1904. Methods. We used difference imaging to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible.Results. Out of 13 stars previously classified as variables, we confirm that 10 are bona fide variables. We cannot detect variability in one other within the precision of our data, while there are two which are saturated in our data frames, but we do not find sufficient evidence in the literature to confirm their variability. We also detect a new RR Lyrae variable, giving a total number of confirmed variable stars in NGC 1904 of 11. Using the Fourier parameters, we find a cluster metallicity [Fe/H] ZW = −1.63 ± 0.14, or [Fe/H] UVES = −1.57 ± 0.18, and a distance of 13.3 ± 0.4 kpc (using RR0 variables) or 12.9 kpc (using the one RR1 variable in our sample for which Fourier decomposition was possible).

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Section: Introductionmentioning

confidence: 93%

Constraining the parameters of globular cluster NGC 1904 from its variable star population

Kains

Bramich

Jaimes

et al. 2012

A&A

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“…Miss-classification of the type c stars is a non-negligible possibility because if there are relatively few epochs in the light curves, eclipsing binaries of the type W UMa may mimic the shape of type c RR Lyrae stars. The contamination due to this type of stars is higher at lower galactic latitude, for example, when the disk population is large (see Vivas et al 2004;Mateu et al 2009, for a complete discussion). High-amplitude δ Scuti stars, which are also more common in the disk population, may have periods as long as type c stars, which makes them an additional source of A15, page 6 of 11 contamination.…”

Section: Comparison With the Properties Of The Cluster Rr Lyrae Starsmentioning

confidence: 99%

Searching for tidal tails aroundωCentauri using RR Lyrae stars

Fernández-Trincado¹,

Vivas²,

Mateu³

et al. 2015

A&A

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We present a survey of RR Lyrae stars in an area of 50 deg 2 around the globular cluster ω Centauri, aimed at detecting debris material from the alleged progenitor galaxy of the cluster. We detected 48 RR Lyrae stars, only 11 of which have been previously reported. Ten of the eleven previously known stars were found inside the tidal radius of the cluster. The rest were located outside the tidal radius up to distances of ∼6 degrees from the center of the cluster. Several of these stars are located at distances similar to that of ω Centauri. We investigate the probability that they may have been stripped off the cluster. To do this, we studied their properties (mean periods) by calculating the expected halo and thick-disk population of RR Lyrae stars in this part of the sky, analyzing the radial velocity of a sub-sample of the RR Lyrae stars, and finally, studying the probable orbits of this sub-sample around the Galaxy. The results of these investigations do not support the scenario that there is significant tidal debris around ω Centauri, which confirms previous studies on the region. It is puzzling that tidal debris has been found elsewhere but not near the cluster itself.

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“…The former are easily detectable thanks to their brightness and characteristic light curves (see e.g. Mateu et al 2009;Prior et al 2009). The latter are about 3.5 mag fainter than RR Lyrae stars but at least 100 times more abundant.…”

Section: The Survey Strega@vstmentioning

confidence: 99%

STREGA: STRucture and Evolution of the GAlaxy – I. Survey overview and first results★

Marconi

Musella

Criscienzo

et al. 2014

Monthly Notices of the Royal Astronomical Society

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STREGA (STRucture and Evolution of the GAlaxy) is a Guaranteed Time survey being performed at the VST (the ESO VLT Survey Telescope) to map about 150 square degrees in the Galactic halo, in order to constrain the mechanisms of galactic formation and evolution. The survey is built as a five-year project, organized in two parts: a core program to explore the surrounding regions of selected stellar systems and a second complementary part to map the southern portion of the Fornax orbit and extend the observations of the core program. The adopted stellar tracers are mainly variable stars (RR Lyraes and Long Period Variables) and Main Sequence Turn-off stars for which observations in the g,r,i bands are obtained. We present an overview of the survey and some preliminary results for three observing runs that have been completed. For the region centered on ω Cen (37 deg 2 ), covering about three tidal radii, we also discuss the detected stellar density radial profile and angular distribution, leading to the identification of extratidal cluster stars. We also conclude that the cluster tidal radius is about 1.2 deg, in agreement with values in the literature based on the Wilson model.

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No Excess of Rr Lyrae Stars in the Canis Major Overdensity

Cited by 47 publications

References 62 publications

Constraining the parameters of globular cluster NGC 1904 from its variable star population

Constraining the parameters of globular cluster NGC 1904 from its variable star population

Searching for tidal tails aroundωCentauri using RR Lyrae stars

STREGA: STRucture and Evolution of the GAlaxy – I. Survey overview and first results★

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