Detection of p-mode Oscillations in HD 35833 with NEID and TESS

Arvind F. Gupta; Jacob Luhn; Jason T. Wright; Suvrath Mahadevan; Eric B. Ford; Guđmundur Stefánsson; Chad F. Bender; Cullen H. Blake; Samuel Halverson; Fred Hearty; Shubham Kanodia; Sarah E. Logsdon; Michael W. McElwain; Joe P. Ninan; Paul Robertson; Arpita Roy; Christian Schwab; Ryan C. Terrien

doi:10.3847/1538-3881/ac96f3

Detection of p-mode Oscillations in HD 35833 with NEID and TESS

Arvind F. Gupta, Jacob Luhn, Jason T. Wright, Suvrath Mahadevan, Eric B. Ford, Guđmundur Stefánsson, Chad F. Bender, Cullen H. Blake, Samuel Halverson, Fred Hearty, Shubham Kanodia, Sarah E. Logsdon, Michael W. McElwain, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien

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Abstract

We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude A_RV = 1.11 ± 0.09 m s⁻¹, photometric amplitude A _phot = 6.42 ± 0.60 ppm, frequency of maximum power ν_max = 595.71 ± 17.28 μHz, and mode spacing Δν = 36.65 ± 0.96 μHz) as well as a nondetection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times t < ν_max⁻¹ , and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by >4σ, hinting at gaps in the underlying physical models.

Original language	English
Article number	254
Pages (from-to)	1-13
Number of pages	13
Journal	Astronomical Journal
Volume	164
Issue number	6
DOIs	https://doi.org/10.3847/1538-3881/ac96f3
Publication status	Published - 1 Dec 2022

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Copyright © 2022. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

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Gupta, A. F., Luhn, J., Wright, J. T., Mahadevan, S., Ford, E. B., Stefánsson, G., Bender, C. F., Blake, C. H., Halverson, S., Hearty, F., Kanodia, S., Logsdon, S. E., McElwain, M. W., Ninan, J. P., Robertson, P., Roy, A., Schwab, C., & Terrien, R. C. (2022). Detection of p-mode Oscillations in HD 35833 with NEID and TESS. Astronomical Journal, 164(6), 1-13. Article 254. https://doi.org/10.3847/1538-3881/ac96f3

@article{317dc99f1bf24f13bcbcb1e739eb1b59,

title = "Detection of p-mode Oscillations in HD 35833 with NEID and TESS",

abstract = "We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude ARV = 1.11 ± 0.09 m s−1, photometric amplitude A phot = 6.42 ± 0.60 ppm, frequency of maximum power νmax = 595.71 ± 17.28 μHz, and mode spacing Δν = 36.65 ± 0.96 μHz) as well as a nondetection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times t < νmax−1 , and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by >4σ, hinting at gaps in the underlying physical models.",

author = "Gupta, {Arvind F.} and Jacob Luhn and Wright, {Jason T.} and Suvrath Mahadevan and Ford, {Eric B.} and Gu{\d}mundur Stef{\'a}nsson and Bender, {Chad F.} and Blake, {Cullen H.} and Samuel Halverson and Fred Hearty and Shubham Kanodia and Logsdon, {Sarah E.} and McElwain, {Michael W.} and Ninan, {Joe P.} and Paul Robertson and Arpita Roy and Christian Schwab and Terrien, {Ryan C.}",

note = "Copyright {\textcopyright} 2022. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.",

year = "2022",

month = dec,

day = "1",

doi = "10.3847/1538-3881/ac96f3",

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Gupta, AF, Luhn, J, Wright, JT, Mahadevan, S, Ford, EB, Stefánsson, G, Bender, CF, Blake, CH, Halverson, S, Hearty, F, Kanodia, S, Logsdon, SE, McElwain, MW, Ninan, JP, Robertson, P, Roy, A, Schwab, C & Terrien, RC 2022, 'Detection of p-mode Oscillations in HD 35833 with NEID and TESS', Astronomical Journal, vol. 164, no. 6, 254, pp. 1-13. https://doi.org/10.3847/1538-3881/ac96f3

TY - JOUR

T1 - Detection of p-mode Oscillations in HD 35833 with NEID and TESS

AU - Gupta, Arvind F.

AU - Luhn, Jacob

AU - Wright, Jason T.

AU - Mahadevan, Suvrath

AU - Ford, Eric B.

AU - Stefánsson, Guđmundur

AU - Bender, Chad F.

AU - Blake, Cullen H.

AU - Halverson, Samuel

AU - Hearty, Fred

AU - Kanodia, Shubham

AU - Logsdon, Sarah E.

AU - McElwain, Michael W.

AU - Ninan, Joe P.

AU - Robertson, Paul

AU - Roy, Arpita

AU - Schwab, Christian

AU - Terrien, Ryan C.

N1 - Copyright © 2022. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

PY - 2022/12/1

Y1 - 2022/12/1

N2 - We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude ARV = 1.11 ± 0.09 m s−1, photometric amplitude A phot = 6.42 ± 0.60 ppm, frequency of maximum power νmax = 595.71 ± 17.28 μHz, and mode spacing Δν = 36.65 ± 0.96 μHz) as well as a nondetection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times t < νmax−1 , and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by >4σ, hinting at gaps in the underlying physical models.

AB - We report the results of observations of p-mode oscillations in the G0 subgiant star HD 35833 in both radial velocities and photometry with NEID and TESS, respectively. We achieve separate, robust detections of the oscillation signal with both instruments (radial velocity amplitude ARV = 1.11 ± 0.09 m s−1, photometric amplitude A phot = 6.42 ± 0.60 ppm, frequency of maximum power νmax = 595.71 ± 17.28 μHz, and mode spacing Δν = 36.65 ± 0.96 μHz) as well as a nondetection in a TESS sector concurrent with the NEID observations. These data shed light on our ability to mitigate the correlated noise impact of oscillations with radial velocities alone and on the robustness of commonly used asteroseismic scaling relations. The NEID data are used to validate models for the attenuation of oscillation signals for exposure times t < νmax−1 , and we compare our results to predictions from theoretical scaling relations and find that the observed amplitudes are weaker than expected by >4σ, hinting at gaps in the underlying physical models.

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U2 - 10.3847/1538-3881/ac96f3

DO - 10.3847/1538-3881/ac96f3

M3 - Article

AN - SCOPUS:85142442777

SN - 0004-6256

VL - 164

SP - 1

EP - 13

JO - Astronomical Journal

JF - Astronomical Journal

IS - 6

M1 - 254

ER -

Detection of p-mode Oscillations in HD 35833 with NEID and TESS

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