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  • Revealing the Field Sub-subgiant Population Using a . . . - IOPscience
    Sub-subgiant stars (SSGs) fall below the subgiant branch and or red of the giant branch in open and globular clusters, an area of the color–magnitude diagram (CMD) not populated by standard stellar evolution tracks One hypothesis is that SSGs result from rapid rotation in subgiants or giants due to tidal synchronization in a close binary
  • The Astrophysical Journal Supplement Series - IOPscience - Publishing . . .
    ApJS publishes catalogs and large compilations of data that can be used as reference by the astronomical community The journal also supports Special Issues, collections of thematically related papers published simultaneously in a single volume ApJS contains many of the most frequently cited papers in the astronomy and astrophysics literature
  • They Might Be Giants: An Efficient Color-based Selection of Red Giant Stars
    We present a color-based method for identifying red giants based on the Pan-STARRS grz and WISE W1 and W2 photometry We utilize a subsample of bright stars with precise parallaxes from Gaia’s second data release (DR2) to verify that the color-based selection reliably separates dwarfs from giants The selection is conservative in the
  • Testing the Limits of Precise Subgiant Characterization . . . - IOPscience
    selection, and to cover the entirety of the subgiant branch This effect is particularly pronounced for the northern sample, as it extends to fainter apparent magnitudes (see Section 2 2) 2 1 1 TESS Objects of Interest in Our Sample For completeness, we search for potential exoplanet candi-dates in our sample and find four stars in the TESS
  • On the Origin of Sub-subgiant Stars. I. Demographics - IOPscience
    binaries At least 65% (28 43) of the sub-subgiants in our sample are variables, 21 of which are known to be radial-velocity binaries Typical variability periods are 15 days At least 33% (14 43) of the sub-subgiants are Hα emitters These observational demographics provide strong evidence that binarity is important for sub-subgiant
  • A Maximum Likelihood Calibration of the Tip of the Red Giant Branch . . .
    High Latitude Field Giants Using Gaia Early Data Release 3 Parallaxes Siyang Li1, Stefano Casertano2, and Adam G Riess1,2 1 Department of Physics and Astronomy, for a sample of Milky Way stars Gaia is a European Space Agency project that launched in 2013 and has obtained astrometry and photometry of over 1 billion stars in the Milky
  • Origin of a Massive Hyper-runaway Subgiant Star LAMOST-HVS1 . . .
    Origin of a Massive Hyper-runaway Subgiant Star LAMOST-HVS1: Implication from Gaia and Follow-up Spectroscopy Kohei Hattori1, Monica Valluri1, Norberto Castro1,2, Ian U Roederer1,3, Guillaume Mahler1, and Gourav Khullar4,5 1 Department of Astronomy, University of Michigan, 1085 S University Avenue, Ann Arbor, MI 48109, USA; khattori@umich edu 2 Leibniz-Institut für Astrophysik Potsdam (AIP
  • Asteroseismic Diagram for Subgiants and Red Giants - IOPscience
    diagrams for the main-sequence, subgiant, and red giant phases However, the Δν and δν 02 diagram does not work well to infer the mass and age of a star in the subgiant phase, due to the degeneracy of the evolutionary tracks during this stage Along the RGB, the C-D diagrams, which are constructed using observational asteroseismic data and
  • ROTATING STARS FROM KEPLER OBSERVED WITH GAIA DR1 - IOPscience
    periods only for dwarf stars, the sample of Kepler–Gaia matched stars contains both main-sequence dwarfs and evolved stars (giants and subgiants) Previous studies have shown that significant contamination by giants or subgiants can affect the implied variability properties of dwarf stars (Ciardi et al 2011; Mann et al 2012)
  • A Catalog of Newly Identified Star Clusters in Gaia DR2 - IOPscience
    2015 5 (Gaia DR2) to epoch 2000, with their corresponding proper motions The Galactic longitude (l) and latitude (b) are calculated in the reference of epoch 2000 for a convenient crossmatch with earlier catalogs (see Section 4) In this study, we use eight stellar parameters of stars from Gaia DR2 in the primary sample: l, b, ϖ, ma cosd
  • AspGap: Augmented Stellar Parameters and Abundances for 37 . . . - IOPscience
    AspGap: Augmented Stellar Parameters and Abundances for 37 Million Red Giant Branch Stars from Gaia XP Low-resolution Spectra Jiadong Li (李佳东)1,2,3,4, Kaze W K Wong5, David W Hogg2,4,5, Hans-Walter Rix4, and Vedant Chandra6 1 Key Lab of Space Astronomy and Technology, National Astronomical Observatories, Beijing, 100101, Peopleʼs Republic of China
  • METALLICITIES OF PLANET-HOSTING STARS: A SAMPLE OF GIANTS . . . - IOPscience
    planet-hosting and control sample dwarf stars A comparison between the distributions of [Fe H] in planet-hosting main-sequence (MS) stars, subgiants, and giants within these samples finds that the MS stars and subgiants have the same mean metallicity of [Fe H] +0 11 dex, while the giant sample is typically more metal poor, having an





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