2020ApJ...889L..34S

Query : 2020ApJ...889L..34S

2020ApJ...889L..34S - Astrophys. J., 889, L34-L34 (2020/February-1)

Detection and characterization of oscillating red giants: first results from the TESS Satellite.

SILVA AGUIRRE V., STELLO D., STOKHOLM A., MOSUMGAARD J.R., BALL W.H., BASU S., BOSSINI D., BUGNET L., BUZASI D., CAMPANTE T.L., CARBONEAU L., CHAPLIN W.J., CORSARO E., DAVIES G.R., ELSWORTH Y., GARCIA R.A., GAULME P., HALL O.J., HANDBERG R., HON M., KALLINGER T., KANG L., LUND M.N., MATHUR S., MINTS A., MOSSER B., CELIK ORHAN Z., RODRIGUES T.S., VRARD M., YILDIZ M., ZINN J.C., ORTEL S., BECK P.G., BELL K.J., GUO Z., JIANG C., KUSZLEWICZ J.S., KUEHN C.A., LI T., LUNDKVIST M.S., PINSONNEAULT M., TAYAR J., CUNHA M.S., HEKKER S., HUBER D., MIGLIO A., MONTEIRO M.J.P.F.G., SLUMSTRUP D., WINTHER M.L., ANGELOU G., BENOMAR O., BODI A., DE MOURA B.L., DEHEUVELS S., DEREKAS A., DI MAURO M.P., DUPRET M.-A., JIMENEZ A., LEBRETON Y., MATTHEWS J., NARDETTO N., DO NASCIMENTO J.D., PEREIRA F., RODRIGUEZ DIAZ L.F., SERENELLI A.M., SPITONI E., STONKUTE E., SUAREZ J.C., SZABO R., VAN EYLEN V., VENTURA R., VERMA K., WEISS A., WU T., BARCLAY T., CHRISTENSEN-DALSGAARD J., JENKINS J.M., KJELDSEN H., RICKER G.R., SEAGER S. and VANDERSPEK R.

Abstract (from CDS):

Since the onset of the "space revolution" of high-precision high-cadence photometry, asteroseismology has been demonstrated as a powerful tool for informing Galactic archeology investigations. The launch of the NASA Transiting Exoplanet Survey Satellite (TESS) mission has enabled seismic-based inferences to go full sky-providing a clear advantage for large ensemble studies of the different Milky Way components. Here we demonstrate its potential for investigating the Galaxy by carrying out the first asteroseismic ensemble study of red giant stars observed by TESS. We use a sample of 25 stars for which we measure their global asteroseimic observables and estimate their fundamental stellar properties, such as radius, mass, and age. Significant improvements are seen in the uncertainties of our estimates when combining seismic observables from TESS with astrometric measurements from the Gaia mission compared to when the seismology and astrometry are applied separately. Specifically, when combined we show that stellar radii can be determined to a precision of a few percent, masses to 5%-10%, and ages to the 20% level. This is comparable to the precision typically obtained using end-of-mission Kepler data.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Asteroseismology - Fundamental parameters of stars - Red giant stars

VizieR on-line data: <Available at CDS (J/ApJ/889/L34): table1.dat>

Simbad objects: 24

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Number of rows : 24
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 HD 225197 HB* 00 04 19.7908158264 -16 31 44.531826852   6.872 5.769     K0III 47 0
2 HD 344 HB* 00 08 03.4868999832 -33 31 45.568976952   6.787 5.662     K1III 44 0
3 HD 1817 PM* 00 22 21.2823975888 -50 59 32.948588328   7.79 6.69     K2III 19 0
4 HD 3303 PM* 00 35 33.3389732928 -54 49 18.738166440   7.055 6.052     K0IV 34 0
5 * lam Tuc RG* 00 55 00.3110878776 -69 31 37.504702308   6.537 5.454     K2III 62 0
6 * gam Hor * 02 45 27.4775218536 -63 42 16.392445812   6.672 5.743     G8III/IV 29 0
7 * bet Ret SB* 03 44 11.9814420749 -64 48 24.890875477   4.968 3.833     K2-IIIb 120 0
8 HD 27304 PM* 04 14 48.5452781856 -62 11 30.520603428   6.57 5.46     K0III 37 0
9 HD 29399 PM* 04 33 33.9493392408 -62 49 25.236915132   6.822 5.780     K1III 59 0
10 * gam Men PM* 05 31 52.8525856360 -76 20 27.246061076 7.52 6.33 5.20 4.34 3.78 K2III 114 0
11 HD 37501 * 05 34 57.4327590840 -61 10 33.775355712   7.158 6.311     G6III 34 0
12 HD 196737 RG* 20 40 19.8279224592 -33 25 54.646146624   6.599 5.466     K1III 44 0
13 HD 198732 ** 20 53 01.15586 -23 46 59.5561       7.26   K0III 23 0
14 HD 200073 RG* 21 02 27.1654626504 -38 31 51.490444404   7.05 5.94     K2III 37 0
15 HD 203949 HB* 21 26 22.8744937632 -37 49 45.949824840   6.826 5.620     K2III 60 0
16 HD 205123 PM* 21 34 53.0739807936 -51 49 37.838616924   7.62 6.72     G6III/IV 19 0
17 HD 210056 PM* 22 11 54.9841578168 -76 06 57.678806160   7.141 6.127     K0III 24 0
18 HD 215852 PM* 22 48 28.1797765872 -27 33 51.690611736   7.76 6.83     G8III/IV 14 0
19 * 77 Aqr PM* 22 54 45.4698913584 -16 16 19.046212932   6.70 5.56     K2.5III 72 0
20 HD 217703 PM* 23 02 44.2505067936 -20 52 14.562297516   6.946 5.976     K0III 28 0
21 HD 219263 RG* 23 14 58.6198746888 -41 06 19.420415532   6.942 5.768     K2III 38 0
22 HD 219409 PM* 23 15 44.7278841264 -29 50 51.183281544   7.599 6.527     K0III 26 0
23 HD 222803 PM* 23 44 01.3214010225 -45 04 59.233482053   7.07 6.09     K1III/IV 39 0
24 HD 223677 PM* 23 51 43.0461787728 -40 49 39.636062112   7.76 6.66     K2III 12 0

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