J/MNRAS/534/1775 Spectroscopic masses of 249 evolved stars (Malla+, 2024)
Benchmarking the spectroscopic masses of 249 evolved stars using
asteroseismology with TESS.
Malla S.P., Stello D., Montet B.T., Huber D., Hon M., Bedding T.R.,
Reyes C., Hey D.R.
<Mon. Not. R. Astron. Soc. 534, 1775-1786 (2024)>
=2024MNRAS.534.1775M 2024MNRAS.534.1775M (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology ; Stars, masses
Keywords: asteroseismology - stars: evolution - stars: fundamental parameters -
stars: oscillations (including pulsations) - stars: interiors
Abstract:
One way to understand planet formation is through studying the
correlations between planet occurrence rates and stellar mass.
However, measuring stellar mass in the red giant regime is very
difficult. In particular, the spectroscopic masses of certain evolved
stars, often referred to as 'retired A-stars', have been questioned in
the literature. Efforts to resolve this mass controversy using
spectroscopy, interferometry and asteroseismology have so far been
inconclusive. A recent ensemble study found a mass-dependent mass
offset, but the result was based on only 16 stars. With NASA's
Transiting Exoplanet Survey Satellite (TESS), we expand the
investigation of the mass discrepancy to a total of 92 low-luminosity
stars, synonymous with the retired A-stars. We measure their
characteristic oscillation frequency, numax, and the large frequency
separation, deltanu, from their TESS photometric time series. Using
these measurements and asteroseismic scaling relations, we derive
asteroseismic masses and compare them with spectroscopic masses from
five surveys, to comprehensively study the alleged mass-dependent mass
offset. We find a mass offset between spectroscopy and seismology that
increases with stellar mass. However, we note that adopting the
seismic mass scale does not have a significant effect on the planet
occurrence-mass-metallicity correlation for the so-called retired
A-stars. We also report seismic measurements and masses for 157 higher
luminosity giants (mostly helium-core- burning) from the spectroscopic
surveys.
Description:
We constructed a sample of 451 evolved stars from five different
spectroscopic sources:
Mortier et al. (2013A&A...557A..70M 2013A&A...557A..70M, Cat. J/A+A/557/A70, M13),
Jofre et al. (2015A&A...574A..50J 2015A&A...574A..50J, Cat. J/A+A/574/A50, J15),
Wittenmyer et al. (2016AJ....152...19W 2016AJ....152...19W, Cat. J/AJ/152/19, W16),
Ghezzi et al. (2018ApJ...860..109G 2018ApJ...860..109G, Cat. J/ApJ/860/109, G18),
and Stock et al. (2018A&A...616A..33S 2018A&A...616A..33S, Cat. J/A+A/616/A33, S18).
Of the 451 stars, we found 249 solar-like oscillators from 2-min
cadence TESS data and measured their numax and DELTAn.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 41 6 Star counts for TESS-spectroscopic overlap sample
table2.dat 69 5 Spectroscopic mass range covered for
TESS-spectroscopic overlap sample
table3.dat 108 451 TESS coverage and spectroscopic masses of
the targets
table4.dat 98 249 Observed parameters and TIC-based seismic mass
results for our targets
table5.dat 76 306 Seismic masses for our targets derived using
spectroscopic parameters
tablea1.dat 74 3 *Parallax sources used for our targets
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Note on tablea1.dat: Exceptions include stars who do not have Gaia parallaxes,
and stars whose fractional error in Gaia parallaxes is larger than in
Hipparcos.
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See also:
J/A+A/557/A70 : Evolved planet hosts - stellar parameters (Mortier+, 2013)
J/A+A/574/A50 : Chemical abundances of giants and subgiants (Jofre+, 2015)
J/AJ/152/19 : Pan-Pacific Planet Search (PPPS). V. 164 stars
(Wittenmyer+, 2016)
J/ApJ/860/109 : Keck HIRES obs. of 245 subgiants (retired A stars)
(Ghezzi+, 2018)
J/A+A/616/A33 : Stellar parameters of 372 giant stars (Stock+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 18 A18 --- Source Spectroscopic source,
or "Total unique stars" (G1)
20- 22 I3 --- Nobs Number of stars observed by TESS
24- 26 I3 --- Nosc Number of oscillating stars
28- 30 I3 --- Nobslow Number of low-luminosity stars observed by TESS
32- 33 I2 --- Nosclow Number of oscillating low-luminosity stars
35- 37 I3 --- Nobshigh Number of high-luminosity stars observed by TESS
39- 41 I3 --- Noschigh Number of oscillating high-luminosity stars
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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- 3 A3 --- Source Spectroscopic source (G1)
5- 14 A10 Msun Mspec Spectroscopic mass range for all 451 stars
16- 25 A10 Msun Mspecosc Spectroscopic mass for all 249
oscillating stars
27- 36 A10 Msun Mspeclow Spectroscopic mass range for all 168
low luminosity stars
38- 47 A10 Msun Mspecosclow Spectroscopic mass range for all 92
oscillating low luminosity stars
49- 58 A10 Msun Mspechigh Spectroscopic mass range for all 283
high luminosity stars
60- 69 A10 Msun Mspecoschigh Spectroscopic mass range for all 157
oscillating high luminosity stars
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC Star Identifier in the TESS Input Catalogue
11- 16 I6 --- HD ? HD Identifier
18- 32 A15 --- Name Commonly known name(s)
34- 37 F4.2 mag Tmag Tess Magnitude
39- 40 I2 --- Sector Number of sectors of data used in the analysis
42- 45 F4.2 Msun MassM13 ? Spectroscopic mass from M13 (G1)
47- 50 F4.2 Msun e_MassM13 ? Error in spectroscopic mass from M13
52- 55 F4.2 Msun MassJ15 ? Spectroscopic mass from J15 (G1)
57- 60 F4.2 Msun e_MassJ15 ? Error in spectroscopic mass from M13
62- 65 F4.2 Msun MassW16 ? Spectroscopic mass from W16 (G1)
67- 70 F4.2 Msun e_MassW16 ? Error in spectroscopic mass from M13
72- 76 F5.3 Msun MassG18 ? Spectroscopic mass from G18 (G1)
78- 82 F5.3 Msun e_MassG18 ? Error in spectroscopic mass from M13
84- 87 F4.2 Msun MassS18 ? Spectroscopic mass from S18 (G1)
89-106 F18.16 Msun e_MassS18 ? Error in spectroscopic mass from M13
108 A1 --- Category [LH] Whether the star is a
low- or high-luminosity star
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC Star Identifier in the TESS Input Catalogue
11- 16 I6 --- HD HD Identifier
18- 23 A6 --- Name Commonly known name
25- 28 I4 K Teff Effective temperature
30- 35 F6.2 muHz numax Observed nu_max obtained using SYD pipeline
37- 41 F5.2 muHz e_numax Error in observed nu_max obtained
using SYD pipeline
43- 47 F5.2 muHz dnu ?=- Observed dnu obtained
using SYD pipeline
50- 53 F4.2 muHz e_dnu ?=- Error in observed dnu obtained
using SYD pipeline
55- 63 A9 --- plxSource Source of Parallax
65- 98 A34 --- Remarks Remarks
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC Star Identifier in the TESS Input Catalogue
11- 16 I6 --- HD HD Identifier
18- 23 A6 --- Name Commonly known names
25- 30 F6.2 Lsun L Isoclassify-based Luminosity
32- 36 F5.2 Lsun e_L Error in isoclassify-based Luminosity
38- 41 F4.2 Msun M1 numax-only based seismic mass
derived using Eq. 1
43- 46 F4.2 Msun e_M1 Error in numax-only based seismic mass
derived using Eq. 1
48- 51 F4.2 Msun M2 ? dnu-only based seismic mass
derived using Eq. 2
53- 56 F4.2 Msun e_M2 ? dnu-only based seismic mass
derived using Eq. 2
58- 62 F5.2 Msun M3 ? numax and dnu-based seismic mass
derived using Eq. 3
64- 68 F5.2 Msun e_M3 ? numax and dnu-based seismic mass
derived using Eq. 3
70- 76 A7 --- Source Spectroscopic source used
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Source Source of Parallax
11- 28 A18 --- Criteria Criteria for the correction applied
30- 67 A38 --- Correction The correction we applied to the parallax
69- 71 I3 --- Ntot Number of stars in our entire sample for
which we adopt this parallax source
73- 74 I2 --- Ntotosc Number of oscillating stars in our sample for
which we adopt this parallax source
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Global notes:
Note (G1): Spectroscopic sources referred to in this paper as follows:
M13 = Mortier et al. (2013A&A...557A..70M 2013A&A...557A..70M, Cat. J/A+A/557/A70)
J15 = Jofre et al. (2015A&A...574A..50J 2015A&A...574A..50J, Cat. J/A+A/574/A50)
W16 = Wittenmyer et al. (2016AJ....152...19W 2016AJ....152...19W, Cat. J/AJ/152/19)
G18 = Ghezzi et al. (2018ApJ...860..109G 2018ApJ...860..109G, Cat. J/ApJ/860/109)
S18 = Stock et al. (2018A&A...616A..33S 2018A&A...616A..33S, Cat. J/A+A/616/A33)
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Acknowledgements:
Sai Prathyusha Malla, saipmalla(at)gmail.com
(End) Patricia Vannier [CDS] 09-Oct-2024