Selecting M Giants With Infrared Photometry: Distances, Metallicities, and the Sagittarius Stream

Li, Jing; Smith, M. C.; Zhong, Jing; Hou, Jinliang; Carlin, Jeffrey L.; Newberg, Heidi Jo; Liu, Chao; Chen, Li; Li, Linlin; Shao, Zhengyi; Small, E.; Tian, Hao

doi:10.3847/0004-637x/823/1/59

Cited by 40 publications

(57 citation statements)

References 64 publications

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“…From the top panel of the Figure 11 and 12, the K-giants show that faint and bright stream are also different in V Y and metallicity, bright stream is obviously higher in V Y and metallicity than faint stream, and in bottom panels of Figure 11 and 12, BHBs also show a similar result. The M-giants members almost only cover on bright stream, which is consistent with the result found in Li et al (2016). To examine the difference of V Y and metallicity between faint and bright stream appeared in K-giants and BHBs sample, in Figure 13 and 14, we divide the bifurcation into leading bright, faint stream and trailing bright, faint stream according to the dash-dotted line in Figure 10.…”

Section: Bifurcations In Sagittarius Streamsupporting

confidence: 79%

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Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars

Yang

Xue²,

et al. 2019

ApJ

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We characterize the kinematic and chemical properties of ∼3,000 Sagittarius (Sgr) stream stars, including K-giants, M-giants, and BHBs, select from SEGUE-2, LAMOST, and SDSS separately in Integrals-of-Motion space. The orbit of Sgr stream is quite clear from the velocity vector in X-Z plane. Stars traced by K-giants and M-giants present the apogalacticon of trailing steam is ∼ 100 kpc. The metallicity distributions of Sgr K-, M-giants, and BHBs present that the M-giants are on average the most metal-rich population, followed by K-giants and BHBs. All of the K-, M-giants, and BHBs indicate that the trailing arm is on average more metal-rich than leading arm, and the K-giants show that the Sgr debris is the most metal-poor part. The α-abundance of Sgr stars exhibits a similar trend with the Galactic halo stars at lower metallicity ([Fe/H] <∼ −1.0 dex), and then evolve down to lower [α/Fe] than disk stars at higher metallicity, which is close to the evolution pattern of α-element of Milky Way dwarf galaxies. We find V Y and metallicity of K-giants have gradients along the direction of line-of-sight from the Galactic center in X-Z plane, and the K-giants show that V Y increases with metallicity at [Fe/H] >∼ −1.5 dex. After dividing the Sgr stream into bright and faint stream according to their locations in equatorial coordinate, the K-giants and BHBs show that the bright and faint stream present different V Y and metallicities, the bright stream is on average higher in V Y and metallicity than the faint stream.

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Section: Bifurcations In Sagittarius Streamsupporting

confidence: 79%

“…There is no distance error of individual LAM-OST M-giant either. Li et al (2016) declared a typical distance precision of 20%. LAMOST M-giants have a typical radial velocity error of about 5 km s −1 (Zhong et al 2015), a median error of 0.17 dex in metallicity, and a median [α/M] error of 0.06 dex.…”

Section: Datamentioning

confidence: 99%

Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars

Yang

Xue²,

et al. 2019

ApJ

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“…A similar analysis separating cool giants and dwarfs was done by Li et al (2016). A comparison between the active (black contours) and inactive sample (gray contours) shows a relative lack of cool inactive dwarfs because the majority of stars is active in this region of the color-color diagram.…”

Section: Colors Of Active Starsmentioning

confidence: 96%

Chromospherically Active Stars in the Rave Survey. Ii. Young Dwarfs in the Solar Neighborhood

Žerjal

Zwitter

Matijevič

et al. 2017

ApJ

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A large sample of over 38,000 chromospherically active candidate solar-like stars and cooler dwarfs from the RAVE survey is addressed in this paper. An improved activity identification with respect to the previous study was introduced to build a catalog of field stars in the solar neighborhood with an excess emission flux in the calcium infrared triplet wavelength region. The central result of this work is the calibration of the age-activity relation for main-sequence dwarfs in a range from a few 10 Myr up to a few Gyr. It enabled an order of magnitude age estimation of the entire active sample. Almost 15,000 stars are shown to be younger than 1 Gyr and ∼2000 younger than 100 Myr. . They overlap with the reference pre-main-sequence RAVE stars often displaying X-ray emission. The activity level increasing with the color reveals their different nature from the solar-like stars and probably represents an underlying dynamo-generating magnetic fields in cool stars. Of the RAVE objects from DR5, 50% are found in the TGAS catalog and supplemented with accurate parallaxes and proper motions by Gaia. This makes the database of a large number of young stars in a combination with RAVE's radial velocities directly useful as a tracer of the very recent large-scale star formation history in the solar neighborhood. The data are available online in the Vizier database.

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“…More than 99% of the M giants from LAMOST DR4 had search radius less than 3" in the ALLWISE Source Catalog, and we obtained 5 photometric bands for these stars (J,H,K,W1 andW2). The details for our selection criteria are the same as those in Section 3.1 of Li et al (2016).…”

Section: Giant Samplementioning

confidence: 99%

Detecting the Sagittarius Stream with LAMOST DR4 M Giants and Gaia DR2

Liu

Xue

et al. 2019

ApJ

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We use LAMOST DR4 M giants combined with Gaia DR2 proper motions and ALL-WISE photometry to obtain an extremely pure sample of Sagittarius (Sgr) stream stars.Using TiO5 and CaH spectral indices as an indicator, we selected out a large sample of M giant stars from M dwarf stars in LAMOST DR4 spectra. Considering the position, distance, proper motion and the angular momentum distribution, we obtained 164 pure Sgr stream stars. We find that the trailing arm has higher energy than the leading arm in same angular momentum. The trailing arm we detected extends to a heliocentric distance of ∼ 130 kpc atΛ ⊙ ∼ 170 • , which is consistent with the feature found in RR Lyrae in Sesar et al. (2017b). Both of these detections of Sgr, in M giants and in RR Lyrae, imply that the Sgr stream may contain multiple stellar populations with a broad metallicity range.

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Selecting M Giants With Infrared Photometry: Distances, Metallicities, and the Sagittarius Stream

Cited by 40 publications

References 64 publications

Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars

Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars

Chromospherically Active Stars in the Rave Survey. Ii. Young Dwarfs in the Solar Neighborhood

Detecting the Sagittarius Stream with LAMOST DR4 M Giants and Gaia DR2

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