Table 4.

Observed parameters and TIC-based seismic mass results for our targets.

TIC IDHDName|$T_{\mathrm{eff}}$||$\mathrm{\nu }_{\mathrm{max,obs,SYD}}$||$\mathrm{\Delta \nu }_{\mathrm{obs,SYD}}$|Source of parallax
(K)(⁠|$\mathrm{\mu }$|Hz)(⁠|$\mathrm{\mu }$|Hz)
(1)(2)(3)(4)a(5)(6)(7)
61290830 8564895167.59 |$\pm$| 1.9613.64 |$\pm$| 0.05Gaia eDR3
171345790 04324 Sex5027191.34 |$\pm$| 4.9413.88 |$\pm$| 0.11Gaia eDR3
5630694103 6165009416.04 |$\pm$| 6.6330.54 |$\pm$| 0.16Gaia eDR3
6013637115 65946 Hya513658.42 |$\pm$| 1.71dHipparcos
1155705979314796160.49 |$\pm$| 3.4613.17 |$\pm$| 0.09Gaia eDR3
2992167210 0115025212.34 |$\pm$| 5.2115.19 |$\pm$| 0.20Gaia eDR3
3255097084074922101.15 |$\pm$| 1.935.25 |$\pm$| 0.19Gaia eDR3
47336943215 0495108470.78 |$\pm$| 12.4829.30 |$\pm$| 0.09Gaia eDR3
4840137247 5624976133.48 |$\pm$| 4.4111.13 |$\pm$| 0.11Gaia eDR3
5387308856084877157.49 |$\pm$| 15.5612.77 |$\pm$| 0.48Gaia DR2
14132684218 8854725g46.62 |$\pm$| 0.874.40 |$\pm$| 0.20bGaia DR2
204350437218 59488 Aqr443910.31 |$\pm$| 0.691.11 |$\pm$| 0.41Hipparcos
37482836722 79612 Tau501458.36 |$\pm$| 2.345.43 |$\pm$| 0.12Gaia DR2
37486086440 40936 Dor4806161.84 |$\pm$| 1.0812.94 |$\pm$||$-$|0.05bHipparcos
38239307018 3223 Eri470640.14 |$\pm$| 1.15dHipparcos
422432907115 20257 Vir4889139.50 |$\pm$| 1.8111.96 |$\pm$||$-$|0.11bHipparcos
43624368237 16040 Ori482641.73 |$\pm$| 1.014.20 |$\pm$| 0.55cHipparcos
TIC IDHDName|$T_{\mathrm{eff}}$||$\mathrm{\nu }_{\mathrm{max,obs,SYD}}$||$\mathrm{\Delta \nu }_{\mathrm{obs,SYD}}$|Source of parallax
(K)(⁠|$\mathrm{\mu }$|Hz)(⁠|$\mathrm{\mu }$|Hz)
(1)(2)(3)(4)a(5)(6)(7)
61290830 8564895167.59 |$\pm$| 1.9613.64 |$\pm$| 0.05Gaia eDR3
171345790 04324 Sex5027191.34 |$\pm$| 4.9413.88 |$\pm$| 0.11Gaia eDR3
5630694103 6165009416.04 |$\pm$| 6.6330.54 |$\pm$| 0.16Gaia eDR3
6013637115 65946 Hya513658.42 |$\pm$| 1.71dHipparcos
1155705979314796160.49 |$\pm$| 3.4613.17 |$\pm$| 0.09Gaia eDR3
2992167210 0115025212.34 |$\pm$| 5.2115.19 |$\pm$| 0.20Gaia eDR3
3255097084074922101.15 |$\pm$| 1.935.25 |$\pm$| 0.19Gaia eDR3
47336943215 0495108470.78 |$\pm$| 12.4829.30 |$\pm$| 0.09Gaia eDR3
4840137247 5624976133.48 |$\pm$| 4.4111.13 |$\pm$| 0.11Gaia eDR3
5387308856084877157.49 |$\pm$| 15.5612.77 |$\pm$| 0.48Gaia DR2
14132684218 8854725g46.62 |$\pm$| 0.874.40 |$\pm$| 0.20bGaia DR2
204350437218 59488 Aqr443910.31 |$\pm$| 0.691.11 |$\pm$| 0.41Hipparcos
37482836722 79612 Tau501458.36 |$\pm$| 2.345.43 |$\pm$| 0.12Gaia DR2
37486086440 40936 Dor4806161.84 |$\pm$| 1.0812.94 |$\pm$||$-$|0.05bHipparcos
38239307018 3223 Eri470640.14 |$\pm$| 1.15dHipparcos
422432907115 20257 Vir4889139.50 |$\pm$| 1.8111.96 |$\pm$||$-$|0.11bHipparcos
43624368237 16040 Ori482641.73 |$\pm$| 1.014.20 |$\pm$| 0.55cHipparcos

Notes.A machine-readable version of the table for all the 249 oscillating stars is available as online downloadable material and from CDS.

a

Source: TESS Input Catalogue (Stassun et al. 2018). We adopted an uncertainty of 100 K in the effective temperature (Thygesen et al. 2012).

b

|$\mathrm{\Delta \nu }$| found using the echelle module.

c

Tentative detection.

d

No |$\mathrm{\Delta \nu }$| detection.

Table 4.

Observed parameters and TIC-based seismic mass results for our targets.

TIC IDHDName|$T_{\mathrm{eff}}$||$\mathrm{\nu }_{\mathrm{max,obs,SYD}}$||$\mathrm{\Delta \nu }_{\mathrm{obs,SYD}}$|Source of parallax
(K)(⁠|$\mathrm{\mu }$|Hz)(⁠|$\mathrm{\mu }$|Hz)
(1)(2)(3)(4)a(5)(6)(7)
61290830 8564895167.59 |$\pm$| 1.9613.64 |$\pm$| 0.05Gaia eDR3
171345790 04324 Sex5027191.34 |$\pm$| 4.9413.88 |$\pm$| 0.11Gaia eDR3
5630694103 6165009416.04 |$\pm$| 6.6330.54 |$\pm$| 0.16Gaia eDR3
6013637115 65946 Hya513658.42 |$\pm$| 1.71dHipparcos
1155705979314796160.49 |$\pm$| 3.4613.17 |$\pm$| 0.09Gaia eDR3
2992167210 0115025212.34 |$\pm$| 5.2115.19 |$\pm$| 0.20Gaia eDR3
3255097084074922101.15 |$\pm$| 1.935.25 |$\pm$| 0.19Gaia eDR3
47336943215 0495108470.78 |$\pm$| 12.4829.30 |$\pm$| 0.09Gaia eDR3
4840137247 5624976133.48 |$\pm$| 4.4111.13 |$\pm$| 0.11Gaia eDR3
5387308856084877157.49 |$\pm$| 15.5612.77 |$\pm$| 0.48Gaia DR2
14132684218 8854725g46.62 |$\pm$| 0.874.40 |$\pm$| 0.20bGaia DR2
204350437218 59488 Aqr443910.31 |$\pm$| 0.691.11 |$\pm$| 0.41Hipparcos
37482836722 79612 Tau501458.36 |$\pm$| 2.345.43 |$\pm$| 0.12Gaia DR2
37486086440 40936 Dor4806161.84 |$\pm$| 1.0812.94 |$\pm$||$-$|0.05bHipparcos
38239307018 3223 Eri470640.14 |$\pm$| 1.15dHipparcos
422432907115 20257 Vir4889139.50 |$\pm$| 1.8111.96 |$\pm$||$-$|0.11bHipparcos
43624368237 16040 Ori482641.73 |$\pm$| 1.014.20 |$\pm$| 0.55cHipparcos
TIC IDHDName|$T_{\mathrm{eff}}$||$\mathrm{\nu }_{\mathrm{max,obs,SYD}}$||$\mathrm{\Delta \nu }_{\mathrm{obs,SYD}}$|Source of parallax
(K)(⁠|$\mathrm{\mu }$|Hz)(⁠|$\mathrm{\mu }$|Hz)
(1)(2)(3)(4)a(5)(6)(7)
61290830 8564895167.59 |$\pm$| 1.9613.64 |$\pm$| 0.05Gaia eDR3
171345790 04324 Sex5027191.34 |$\pm$| 4.9413.88 |$\pm$| 0.11Gaia eDR3
5630694103 6165009416.04 |$\pm$| 6.6330.54 |$\pm$| 0.16Gaia eDR3
6013637115 65946 Hya513658.42 |$\pm$| 1.71dHipparcos
1155705979314796160.49 |$\pm$| 3.4613.17 |$\pm$| 0.09Gaia eDR3
2992167210 0115025212.34 |$\pm$| 5.2115.19 |$\pm$| 0.20Gaia eDR3
3255097084074922101.15 |$\pm$| 1.935.25 |$\pm$| 0.19Gaia eDR3
47336943215 0495108470.78 |$\pm$| 12.4829.30 |$\pm$| 0.09Gaia eDR3
4840137247 5624976133.48 |$\pm$| 4.4111.13 |$\pm$| 0.11Gaia eDR3
5387308856084877157.49 |$\pm$| 15.5612.77 |$\pm$| 0.48Gaia DR2
14132684218 8854725g46.62 |$\pm$| 0.874.40 |$\pm$| 0.20bGaia DR2
204350437218 59488 Aqr443910.31 |$\pm$| 0.691.11 |$\pm$| 0.41Hipparcos
37482836722 79612 Tau501458.36 |$\pm$| 2.345.43 |$\pm$| 0.12Gaia DR2
37486086440 40936 Dor4806161.84 |$\pm$| 1.0812.94 |$\pm$||$-$|0.05bHipparcos
38239307018 3223 Eri470640.14 |$\pm$| 1.15dHipparcos
422432907115 20257 Vir4889139.50 |$\pm$| 1.8111.96 |$\pm$||$-$|0.11bHipparcos
43624368237 16040 Ori482641.73 |$\pm$| 1.014.20 |$\pm$| 0.55cHipparcos

Notes.A machine-readable version of the table for all the 249 oscillating stars is available as online downloadable material and from CDS.

a

Source: TESS Input Catalogue (Stassun et al. 2018). We adopted an uncertainty of 100 K in the effective temperature (Thygesen et al. 2012).

b

|$\mathrm{\Delta \nu }$| found using the echelle module.

c

Tentative detection.

d

No |$\mathrm{\Delta \nu }$| detection.

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