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

Huxor, Avon; Grebel, Eva K.

doi:10.1093/mnras/stv1631

Cited by 36 publications

(47 citation statements)

References 166 publications

(271 reference statements)

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“…As suggested by Mackey et al (2016), it is likely that these stars are part of the stream emanating from the North of the LMC. We also highlight in this figure two variable carbon stars that are present in our sample with green triangles (Huxor & Grebel 2015, where the IDs are HG31 and HG35). One of these stars is part of the Eastern excess described above, and the other is likely a member of the Mackey et al (2016) stream.…”

Section: Stellar Features With No Gaseous Counterpartmentioning

confidence: 95%

“…The stream identified by Mackey et al (2016) is also seen in our sample, and we find that the stream likely extends further East. The purple symbol in this figure indicates the position of the Carina dwarf galaxy, and the green triangles indicate variable carbon stars identified by Huxor & Grebel (2015). respect to its proper motion) is also seen in RRL stars (see Figure 16 of , adding weight to its credibility.…”

Section: Stellar Features With No Gaseous Counterpartmentioning

confidence: 99%

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The Clouds are breaking: tracing the Magellanic system with Gaia DR1 Mira variables

Deason

Belokurov

Erkal

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We exploit the first data release from the Gaia mission to identify candidate Mira variables in the outskirts of the Magellanic Clouds. The repeated observations of sources during the initial phase of the Gaia mission is used to identify stars that show signs of variability. This variability information, combined with infrared photometry from 2MASS and WISE, allows us to select a clean sample of giants in the periphery of the LMC. We find evidence for Miras surrounding the LMC out to ∼ 20 deg in all directions, apart from the North-West quadrant. Our sample does not generally follow the gas distribution of the Magellanic system; Miras are notably absent in the gaseous bridge between the LMC and SMC, but they are likely related to the stellar RR Lyrae bridge reported by . The stellar stream discovered by Mackey et al. (2016) to the North of the LMC is almost perfectly delineated by our Mira variables, and likely extends further East toward the Galactic plane. The presence of an intermediate-age population in this stream advocates an LMC disc origin. We also find a significant excess of Miras to the East of the LMC; these more diffusely distributed stars are likely stripped SMC stars due to interactions with the LMC. Miras are also identified in regions of the sky away from the Clouds; we locate stars likely associated with known massive substructures, and also find potential associations with stripped SMC debris above the Galactic plane.

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Section: Stellar Features With No Gaseous Counterpartmentioning

confidence: 95%

Section: Stellar Features With No Gaseous Counterpartmentioning

confidence: 99%

The Clouds are breaking: tracing the Magellanic system with Gaia DR1 Mira variables

Deason

Belokurov

Erkal

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Like RR Lyrae stars, these can be used to trace halo streams and the presence of dwarf galaxies (Huxor & Grebel 2015). Since LPVs are intrinsically much brighter than RR Lyrae, and often have much larger amplitudes as well, they can be used to detect much more distant halo features.…”

Section: Long-period Variablesmentioning

confidence: 99%

The Catalina Surveys Southern periodic variable star catalogue

Drake

Djorgovski

Catelan

et al. 2017

Monthly Notices of the Royal Astronomical Society

166

133

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Here, we present the results from our analysis of 6 yr of optical photometry taken by the Siding Spring Survey (SSS). This completes a search for periodic variable stars within the 30 000 deg 2 of the sky covered by the Catalina Surveys. The current analysis covers 81 million sources with declinations between −20 • and −75 • with median magnitudes in the range 11 < V < 19.5. We find approximately 34 000 new periodic variable stars in addition to the ∼9000 RR Lyrae that we previously discovered in SSS data. This brings the total number of periodic variables identified in Catalina data to ∼110 000. The new SSS periodic variable stars mainly consist of eclipsing binaries, RR Lyrae, LPVs, RS CVn stars, δ Scutis, and Anomalous Cepheids. By cross-matching these variable stars with those from prior surveys, we find that ∼90 per cent of the sources are new discoveries and recover ∼95 per cent of the known periodic variables in the survey region. For the known sources, we find excellent agreement between our catalogue and prior values of luminosity, period, and amplitude. However, we find many variable stars that had previously been misclassified. Examining the distribution of RR Lyrae, we find a population associated with the Large Magellanic Cloud (LMC) that extends more than 20 • from its centre confirming recent evidence for the existence of a very extended stellar halo in the LMC. By combining SSS photometry with Dark Energy Survey data, we identify additional LMC halo RR Lyrae, thus confirming the significance of the population.

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“…Martínez-Delgado et al 2001;Newberg et al 2002;Majewski et al 2003;Belokurov et al 2006;Koposov et al 2012;Huxor & Grebel 2015). Given the spatial extent of that system, it seems likely that some of the Galactic GCs might have formed within Sgr and been later accreted by the Milky Way.…”

Section: Introductionmentioning

confidence: 99%

The southern leading and trailing wraps of the Sagittarius tidal stream around the globular cluster Whiting 1

Carballo‐Bello

Corral-Santana

Martínez–Delgado

et al. 2017

Monthly Notices of the Royal Astronomical Society: Letters

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We present a study of the kinematics of 101 stars observed with VIMOS around Whiting 1, a globular cluster embedded in the Sagittarius tidal stream. The obtained velocity distribution shows the presence of two wraps of that halo substructure at the same heliocentric distance as that of the cluster and with well differentiated mean radial velocities. The most prominent velocity component seems to be associated with the trailing arm of Sagittarius with < v r >∼ −130 km s −1 , which is consistent with the velocity of Whiting 1. This result supports that this globular cluster was formed in Sagittarius and recently accreted by the Milky Way. The second component with < v r >∼ 120 km s −1 might correspond to the leading arm of Sagittarius, which has been predicted by numerical simulations but with no conclusive observational evidence of its existence presented so far. This detection of the old leading wrap of Sagittarius in the southern hemisphere may be used to confirm and further constrain the models for its orbit and evolution.

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

Cited by 36 publications

References 166 publications

The Clouds are breaking: tracing the Magellanic system with Gaia DR1 Mira variables

The Clouds are breaking: tracing the Magellanic system with Gaia DR1 Mira variables

The Catalina Surveys Southern periodic variable star catalogue

The southern leading and trailing wraps of the Sagittarius tidal stream around the globular cluster Whiting 1

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