Cool carbon stars in the halo

Mauron, N.; Kendall, T. R.; Gigoyan, K. S.

doi:10.1051/0004-6361:20052820

Cited by 24 publications

(43 citation statements)

References 25 publications

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“…Our primary source, providing just over half of all our variable carbon stars, comes from the lists published by the Mauron group (Mauron et al 2004;Mauron, Kendall, & Gigoyan 2005;Mauron, Gigoyan, & Kendall 2007b;Mauron 2008;Mauron et al 2014). These were selected from candidates based on 2MASS (Skrutskie et al 2006) photometry and then spectroscopically confirmed.…”

Section: Mauron Et Al Samplementioning

confidence: 99%

Tracing the tidal streams of the Sagittarius dSph, and halo Milky Way features, with carbon-rich long-period variables

Huxor

Grebel

2015

Mon. Not. R. Astron. Soc.

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We assemble 121 spectroscopically-confirmed halo carbon stars, drawn from the literature, exhibiting measurable variability in the Catalina Surveys. We present their periods and amplitudes, which are used to estimate distances from period-luminosity relationships. The location of the carbon stars -and their velocities when availableallow us to trace the streams of the Sagittarius (Sgr) dwarf spheroidal galaxy. These are compared to a canonical numerical simulation of the accretion of Sgr. We find that the data match this model well for heliocentric distances of 15-50 kpc, except for a virtual lack of carbon stars in the trailing arm just north of the Galactic Plane, and there is only tentative evidence of the leading arm south of the Plane. The majority of the sample can be attributed to the Sgr accretion. We also find groups of carbon stars which are not part of Sgr; most of which are associated with known halo substructures. A few have no obvious attribution and may indicate new substructure. We find evidence that there may be a structure behind the Sgr leading stream apocentre, at ∼100 kpc, and a more distant extension to the Pisces Overdensity also at ∼100 kpc. We study a further 75 carbon stars for which no good period data could be obtained, and for which NIR magnitudes and colours are used to estimate distances. These data add support for the features found at distances beyond 100 kpc.

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Section: Mauron Et Al Samplementioning

confidence: 99%

Tracing the tidal streams of the Sagittarius dSph, and halo Milky Way features, with carbon-rich long-period variables

Huxor

Grebel

2015

Mon. Not. R. Astron. Soc.

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“…A&A 513, A62 (2010) All such discoveries increased the importance of Sgr dSph not only as a "test case" of tidal merging, but as the source of a significant portion of the stellar population in the Halo. Majewski et al (2003) estimated that roughly 75% of highlatitude Halo M-giants originated from Sgr dSph debris, which also provided almost all Halo AGB C-stars (see Mauron et al 2005). Zijlstra et al (2006) estimated that up to 10% of the Halo material could come from Sgr dSph debris.…”

Section: Introductionmentioning

confidence: 99%

A wide angle view of the Sagittarius dwarf spheroidal galaxy

Giuffrida

Sbordone

Zaggia

et al. 2010

A&A

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Context. The Sagittarius dwarf Spheroidal Galaxy (Sgr dSph) provides us with a unique possibility of studying a dwarf galaxy merging event while still in progress. Moving along a short-period, quasi-polar orbit in the Milky Way Halo, Sgr dSph is being tidally dispersed along a huge stellar stream. Due to its low distance (25 kpc), the main body of Sgr dSph covers a vast area in the sky (roughly 15 × 7 degrees). Available photometric and spectroscopic studies have concentrated either on the central part of the galaxy or on the stellar stream, but the overwhelming majority of the galaxy body has never been probed. Aims. The aim of the present study is twofold. On the one hand, to produce color magnitude diagrams across the extension of Sgr dSph to study its stellar populations, searching for age and/or composition gradients (or lack thereof). On the other hand, to derive spectroscopic low-resolution radial velocities for a subsample of stars to determine membership to Sgr dSph for the purpose of high resolution spectroscopic follow-up. Methods. We used VIMOS@VLT to produce V and I photometry on 7 fields across the Sgr dSph minor and major axis, plus 3 more centered on the associated globular clusters Terzan 7, Terzan 8 and Arp 2. A last field has been centered on M 54, lying in the center of Sgr dSph. VIMOS high resolution spectroscopic mode has then been used to derive radial velocities for a subsample of the observed stars, concentrating on objects having colors and magnitudes compatible with the Sgr dSph red giant branch. Results. We present photometry for 320 000 stars across the main body of Sgr dSph, one of the richest, and safely the most wide-angle sampling ever produced for this fundamental object. We also provide robust memberships for more than one hundred stars, whose high resolution spectroscopic analysis will be the object of forthcoming papers. Sgr dSph appears remarkably uniform among the observed fields. We confirm the presence of a main Sgr dSph population characterized roughly by the same metallicity of 47 Tuc, but we also found the presence of multiple populations on the peripheral fields of the galaxy, with a metallicity spanning from [Fe/H] = -2.3 to a nearly solar value.

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“…There are no such objects with K > 11 because AGB stars as faint as this in K (and consequently very distant in the halo) are very rare, and are only found with specific methods (see, e.g. Mauron et al 2004Mauron et al , 2005. We suggest that HES objects with J − K < 1 are red giant branch objects, or for a small fraction, dwarfs (see below).…”

Section: Discussionmentioning

confidence: 87%

“…This is obviously due to its blue−visible spectral range. For example, HES missed 11 C stars listed in Mauron et al (2004Mauron et al ( , 2005, although these objects satisfy R < 16, b < −30 • and δ < +2 • . The reason is that their B − R colour is too large and the signal at blue wavelengths is too faint.…”

Section: Mass Photometrymentioning

confidence: 99%

“…Appendices and Table 1 are only available in electronic form at http://www.aanda.org Mauron et al (2004Mauron et al ( , 2005 where candidate C stars were selected by their photometric colours in the 2MASS point-source catalogue (Skrutskie et al 2006) and with |b| > 20 • . Together, these works identified ∼130 cool AGB C stars located in the halo and with distances up to 130 kpc.…”

Section: Introductionmentioning

confidence: 99%

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The properties of carbon stars found in the Byurakan and the Hamburg/ESO surveys

Mauron¹,

Gigoyan

Kendall

2006

A&A

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Aims. We analyse two samples of high latitude carbon stars found in two objective-prism surveys: the First Byurakan survey (FBS) and the Hamburg/ESO survey (HES). We determine the composition of these samples in cool AGB stars, warmer giants and dwarf carbon stars. Methods. We list 44 new carbon stars found in the FBS and use near-infrared photometric catalogues (DENIS, 2MASS) to investigate the observational and statistical properties of the surveys. The SuperCOSMOS and USNO-B1.0 catalogues are used to study proper motions and to identify dwarfs. Results. The colour-magnitude and colour-colour diagrams, either with visual magnitudes or with infrared data, show that the HES selects faint and relatively warm carbon stars, whereas FBS is less deep, but gives cooler objects. By comparing DENIS and 2MASS photometry, we find that HES objects with J − K ≤ 1 are mostly non-variable giants while clear variability is often seen for J − K ≥ 1, indicating AGB stars. By using SuperCOSMOS proper motions, 9 HES objects are found to have a proper motion µ greater than 30 mas yr −1 (3σ detection). Five of these objects are detected at the ≥5σ level. These 9 HES objects are dwarf carbon stars, including two that could belong to the halo population. The 9 carbon dwarfs are remarkably bright and deserve further study.

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Cool carbon stars in the halo

Cited by 24 publications

References 25 publications

Tracing the tidal streams of the Sagittarius dSph, and halo Milky Way features, with carbon-rich long-period variables

Tracing the tidal streams of the Sagittarius dSph, and halo Milky Way features, with carbon-rich long-period variables

A wide angle view of the Sagittarius dwarf spheroidal galaxy

The properties of carbon stars found in the Byurakan and the Hamburg/ESO surveys

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