J/AJ/160/18 M giant stars asteroseismology with Kepler and APOGEE (Auge+, 2020)
Beyond Gaia: asteroseismic distances of M giants using ground-based transient
surveys.
Auge C., Huber D., Heinze A., Shappee B.J., Tonry J., Chakrabarti S.,
Sanderson R.E., Denneau L., Flewelling H., Holoien T.W.-S., Kochanek C.S.,
Pignata G., Sickafoose A., Stalder B., Stanek K.Z., Stello D., Thompson T.A.
<Astron. J., 160, 18 (2020)>
=2020AJ....160...18A 2020AJ....160...18A
ADC_Keywords: Asteroseismology; Stars, giant; Effective temperatures;
Photometry; Optical
Keywords: Asteroseismology ; Stellar distance ; Ground-based astronomy ;
M giant stars
Abstract:
Evolved stars near the tip of the red giant branch show solar-like
oscillations with periods spanning hours to months and amplitudes
ranging from ∼1mmag to ∼100mmag. The systematic detection of the
resulting photometric variations with ground-based telescopes would
enable the application of asteroseismology to a much larger and more
distant sample of stars than is currently accessible with space-based
telescopes such as Kepler or the ongoing Transiting Exoplanet Survey
Satellite mission. We present an asteroseismic analysis of 493 M
giants using data from two ground-based surveys: the Asteroid
Terrestrial-impact Last Alert System (ATLAS) and the All-Sky Automated
Survey for Supernovae (ASAS-SN). By comparing the extracted
frequencies with constraints from Kepler, the Sloan Digital Sky Survey
Apache Point Observatory Galaxy Evolution Experiment, and Gaia we
demonstrate that ground-based transient surveys allow accurate
distance measurements to oscillating M giants with a precision of
∼15%. Using stellar population synthesis models we predict that ATLAS
and ASAS-SN can provide asteroseismic distances to ∼2x106 galactic M
giants out to typical distances of 20-50kpc, vastly improving the
reach of Gaia and providing critical constraints for Galactic
archeology and galactic dynamics.
Description:
We utilize photometry from the Asteroid Terrestrial-impact Last Alert
System (ATLAS) and All-Sky Automated Survey for Supernovae (ASAS-SN)
for our analysis. ATLAS is primarily designed to detect small
asteroids on their final approach to Earth. To achieve this ATLAS
scans all of the accessible sky every few nights using fully robotic
0.5m f/2 Wright Schmidt telescopes with a 5.4x5.4° field of view.
ATLAS began operations with one telescope on Haleakala on the
Hawaiian island of Maui in mid-2015, and began operations with their
second telescope early 2017 at the Maunaloa Observatory on the big
island of Hawai`i. Each ATLAS telescope takes four 30s exposures per
night of 200-250 target fields covering half of the accessible night
sky. ATLAS uses two customized, wide filters designed to optimize
detections of faint objects: the cyan filter (c) covering 420-650nm
and the orange filter (o) covering 560-820nm.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 38 71 Asteroseismic results for the Kepler sample
table2.dat 42 276 Asteroseismic results for the APOGEE sample
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
II/366 : ASAS-SN catalog of variable stars (Jayasinghe+, 2018-2020)
J/A+A/425/595 : OGLE+2MASS+DENIS LPV in Magellanic Clouds (Groenewegen,2004)
J/MNRAS/400/1945 : Light curves of 261 nearby pulsating M giants (Tabur+, 2009)
J/ApJ/763/32 : Galactic halo RRab stars from CSS (Drake+, 2013)
J/ApJ/765/L41 : Asteroseismic classification of KIC objects (Stello+, 2013)
J/ApJS/210/1 : Asteroseismic study of solar-type stars (Chaplin+, 2014)
J/ApJ/788/48 : X-ray through NIR photometry of NGC 2617 (Shappee+, 2014)
J/ApJ/827/50 : Kepler faint red giants (Mathur+, 2016)
J/ApJ/844/102 : KIC star plxs from asteroseismology vs Gaia (Huber+, 2017)
J/AJ/154/94 : APOGEE-2 data from DR16 (Majewski+, 2017)
J/ApJ/844/L4 : PS1 RRab stars tracing outer Virgo overdensity (Sesar+,2017)
J/ApJ/866/99 : Radii of KIC stars & planets using Gaia DR2 (Berger+, 2018)
J/AJ/156/241 : Catalog of variable stars measured by ATLAS (Heinze+, 2018)
J/ApJS/236/42 : Asteroseismology of ∼16000 Kepler red giants (Yu+, 2018)
J/AJ/158/227 : Asteroseismic parameters of RGB stars (Grunblatt+, 2019)
J/other/Sci/365.478 : Milky Way classical Cepheids sample (Skowron+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 I7 --- ID Kepler ID
9- 13 F5.2 --- mag [8.1/13.38] Kepler magnitude
15- 19 F5.3 uHz numax1 [0.16/0.88] Ground-based frequency of maximum power,
νmax (1)
21- 26 F6.3 d Per1 [13.1/70.8] Ground-based period
28- 32 F5.3 uHz numax2 [0.2/0.91] Kepler based frequency of maximum power,
νmax (2)
34- 38 F5.2 d Per2 [11.7/53.3] Kepler based period, days (3)
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Note (1): The ground-based νmax measurements have a typical fractional
error of 12%.
Note (2): Reference for numax2 is Stello+, 2014ApJ...788L..10S 2014ApJ...788L..10S.
Note (3): Reference for Per2 is Yu+, 2020MNRAS.493.1388Y 2020MNRAS.493.1388Y.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- ID APOGEE identifier
20- 24 F5.3 uHz numax [0.1/0.98] frequency of maximum power, νmax (1)
26- 30 F5.3 [cm/s2] logg1 [0.02/1.02] log, surface gravity, seismic
32- 35 I4 K Teff [3519/4146] Stellar effective temperature APOGEE (1)
37- 42 F6.3 [cm/s2] logg2 [-0.39/1.26] log, surface gravity, APOGEE
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Note (1): Typical uncertainties are 18% for νmax (see Figure 5) and
∼70K for Teff (see Ahumada+, 2019arXiv191202905A 2019arXiv191202905A).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 03-Dec-2020