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Title: From the inner to outer Milky Way: a photometric sample of 2.6 million red clump stars

Abstract

ABSTRACT Large pristine samples of red clump stars are highly sought after given that they are standard candles and give precise distances even at large distances. However, it is difficult to cleanly select red clumps stars because they can have the same Teff and log g as red giant branch stars. Recently, it was shown that the asteroseismic parameters, $$\rm {\Delta }$$P and $$\rm {\Delta \nu }$$, which are used to accurately select red clump stars, can be derived from spectra using the change in the surface carbon to nitrogen ratio ([C/N]) caused by mixing during the red giant branch. This change in [C/N] can also impact the spectral energy distribution. In this study, we predict the $$\rm {\Delta }$$P, $$\rm {\Delta \nu }$$, Teff, and log g using 2MASS, AllWISE, Gaia, and Pan-STARRS data in order to select a clean sample of red clump stars. We achieve a contamination rate of ∼20 per cent, equivalent to what is achieved when selecting from Teff and log g derived from low-resolution spectra. Finally, we present two red clump samples. One sample has a contamination rate of ∼20 per cent and ∼405 000 red clump stars. The other has a contamination of ∼33 per cent and ∼2.6 million red clump stars that includes ∼75 000 stars at distances >10 kpc. For |b| > 30 deg, we find ∼15 000 stars with contamination rate of ∼9 per cent. The scientific potential of this catalogue for studying the structure and formation history of the Galaxy is vast, given that it includes millions of precise distances to stars in the inner bulge and distant halo where astrometric distances are imprecise.

Authors:
ORCiD logo [1];  [2];  [3]; ORCiD logo [1]
  1. Department of Astronomy, the University of Texas at Austin, 2515 Speedway Boulevard, Austin, TX 78712, USA
  2. Institute for Advanced Study, Princeton, NJ 08540, USA, Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA, Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA, Research School of Astronomy & Astrophysics, Australian National University, Cotter Road, Weston, ACT 2611, Australia
  3. High Energy Physics Division, Argonne National Laboratory, Lemont, IL 60439, USA, Kavli Institute for Cosmological Physics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA
Publication Date:
Sponsoring Org.:
USDOE
OSTI Identifier:
1631777
Grant/Contract Number:  
AC02-06CH11357
Resource Type:
Published Article
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 495 Journal Issue: 3; Journal ID: ISSN 0035-8711
Publisher:
Oxford University Press
Country of Publication:
United Kingdom
Language:
English

Citation Formats

Lucey, Madeline, Ting, Yuan-Sen, Ramachandra, Nesar S., and Hawkins, Keith. From the inner to outer Milky Way: a photometric sample of 2.6 million red clump stars. United Kingdom: N. p., 2020. Web. doi:10.1093/mnras/staa1226.
Lucey, Madeline, Ting, Yuan-Sen, Ramachandra, Nesar S., & Hawkins, Keith. From the inner to outer Milky Way: a photometric sample of 2.6 million red clump stars. United Kingdom. doi:https://doi.org/10.1093/mnras/staa1226
Lucey, Madeline, Ting, Yuan-Sen, Ramachandra, Nesar S., and Hawkins, Keith. Sat . "From the inner to outer Milky Way: a photometric sample of 2.6 million red clump stars". United Kingdom. doi:https://doi.org/10.1093/mnras/staa1226.
@article{osti_1631777,
title = {From the inner to outer Milky Way: a photometric sample of 2.6 million red clump stars},
author = {Lucey, Madeline and Ting, Yuan-Sen and Ramachandra, Nesar S. and Hawkins, Keith},
abstractNote = {ABSTRACT Large pristine samples of red clump stars are highly sought after given that they are standard candles and give precise distances even at large distances. However, it is difficult to cleanly select red clumps stars because they can have the same Teff and log g as red giant branch stars. Recently, it was shown that the asteroseismic parameters, $\rm {\Delta }$P and $\rm {\Delta \nu }$, which are used to accurately select red clump stars, can be derived from spectra using the change in the surface carbon to nitrogen ratio ([C/N]) caused by mixing during the red giant branch. This change in [C/N] can also impact the spectral energy distribution. In this study, we predict the $\rm {\Delta }$P, $\rm {\Delta \nu }$, Teff, and log g using 2MASS, AllWISE, Gaia, and Pan-STARRS data in order to select a clean sample of red clump stars. We achieve a contamination rate of ∼20 per cent, equivalent to what is achieved when selecting from Teff and log g derived from low-resolution spectra. Finally, we present two red clump samples. One sample has a contamination rate of ∼20 per cent and ∼405 000 red clump stars. The other has a contamination of ∼33 per cent and ∼2.6 million red clump stars that includes ∼75 000 stars at distances >10 kpc. For |b| > 30 deg, we find ∼15 000 stars with contamination rate of ∼9 per cent. The scientific potential of this catalogue for studying the structure and formation history of the Galaxy is vast, given that it includes millions of precise distances to stars in the inner bulge and distant halo where astrometric distances are imprecise.},
doi = {10.1093/mnras/staa1226},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 3,
volume = 495,
place = {United Kingdom},
year = {2020},
month = {5}
}

Journal Article:
Free Publicly Available Full Text
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DOI: https://doi.org/10.1093/mnras/staa1226

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