The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System

Anmol Desai; Emma V. Turtelboom; Caleb K. Harada; Courtney D. Dressing; David R. Rice; Joseph M.Akana Murphy; Casey L. Brinkman; Ashley Chontos; Ian J.M. Crossfield; Fei Dai; Michelle L. Hill; Tara Fetherolf; Steven Giacalone; Andrew W. Howard; Daniel Huber; Howard Isaacson; Stephen R. Kane; Jack Lubin; Mason G. MacDougall; Andrew W. Mayo; Teo Močnik; Alex S. Polanski; Malena Rice; Paul Robertson; Ryan A. Rubenzahl; Judah Van Zandt; Lauren M. Weiss; Allyson Bieryla; Lars A. Buchhave; Jon M. Jenkins; Veselin B. Kostov; Alan M. Levine; Jorge Lillo-Box; M. Paegert; Markus Rabus; S. Seager; Keivan G. Stassun; Eric B. Ting; David Watanabe; Joshua N. Winn

doi:10.3847/1538-3881/ad29ee

The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System

Anmol Desai, Emma V. Turtelboom^*, Caleb K. Harada, Courtney D. Dressing, David R. Rice, Joseph M.Akana Murphy, Casey L. Brinkman, Ashley Chontos, Ian J.M. Crossfield, Fei Dai, Michelle L. Hill, Tara Fetherolf, Steven Giacalone, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Jack Lubin, Mason G. MacDougall, Andrew W. MayoTeo Močnik, Alex S. Polanski, Malena Rice, Paul Robertson, Ryan A. Rubenzahl, Judah Van Zandt, Lauren M. Weiss, Allyson Bieryla, Lars A. Buchhave, Jon M. Jenkins, Veselin B. Kostov, Alan M. Levine, Jorge Lillo-Box, M. Paegert, Markus Rabus, S. Seager, Keivan G. Stassun, Eric B. Ting, David Watanabe, Joshua N. Winn

^*Corresponding author for this work

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Abstract

We present and confirm TOI-1751 b, a transiting sub-Neptune orbiting a slightly evolved, solar-type, metal-poor star (T _eff = 5996 ± 110 K, log ( g ) = 4.2 ± 0.1 , V = 9.3 mag, [Fe/H] = −0.40 ± 0.06 dex) every 37.47 days. We use TESS photometry to measure a planet radius of 2.77 − 0.07 + 0.15 R ⊕ . We also use both Keck/HIRES and APF/Levy radial velocities (RV) to derive a planet mass of 14.5 − 3.14 + 3.15 M ⊕ , and thus a planet density of 3.6 ± 0.9 g cm⁻³. There is also a long-period (∼400 days) signal that is observed in only the Keck/HIRES data. We conclude that this long-period signal is not planetary in nature and is likely due to the window function of the Keck/HIRES observations. This highlights the role of complementary observations from multiple observatories to identify and exclude aliases in RV data. Finally, we investigate the potential compositions of this planet, including rocky and water-rich solutions, as well as theoretical irradiated ocean models. TOI-1751 b is a warm sub-Neptune with an equilibrium temperature of ∼820 K. As TOI-1751 is a metal-poor star, TOI-1751 b may have formed in a water-enriched formation environment. We thus favor a volatile-rich interior composition for this planet.

Original language	English
Article number	194
Journal	Astronomical Journal
Volume	167
Issue number	5
Number of pages	18
ISSN	0004-6256
DOIs	https://doi.org/10.3847/1538-3881/ad29ee
Publication status	Published - 2024

Keywords

Radial velocity
Exoplanet structure
Transit photometry
Mini Neptunes

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Desai, A., Turtelboom, E. V., Harada, C. K., Dressing, C. D., Rice, D. R., Murphy, J. M. A., Brinkman, C. L., Chontos, A., Crossfield, I. J. M., Dai, F., Hill, M. L., Fetherolf, T., Giacalone, S., Howard, A. W., Huber, D., Isaacson, H., Kane, S. R., Lubin, J., MacDougall, M. G., ... Winn, J. N. (2024). The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System. Astronomical Journal, 167(5), Article 194. https://doi.org/10.3847/1538-3881/ad29ee

@article{5dbb583b20c04a629f4cf9d93b6881b1,

title = "The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System",

abstract = "We present and confirm TOI-1751 b, a transiting sub-Neptune orbiting a slightly evolved, solar-type, metal-poor star (T eff = 5996 ± 110 K, log ( g ) = 4.2 ± 0.1 , V = 9.3 mag, [Fe/H] = −0.40 ± 0.06 dex) every 37.47 days. We use TESS photometry to measure a planet radius of 2.77 − 0.07 + 0.15 R ⊕ . We also use both Keck/HIRES and APF/Levy radial velocities (RV) to derive a planet mass of 14.5 − 3.14 + 3.15 M ⊕ , and thus a planet density of 3.6 ± 0.9 g cm−3. There is also a long-period (∼400 days) signal that is observed in only the Keck/HIRES data. We conclude that this long-period signal is not planetary in nature and is likely due to the window function of the Keck/HIRES observations. This highlights the role of complementary observations from multiple observatories to identify and exclude aliases in RV data. Finally, we investigate the potential compositions of this planet, including rocky and water-rich solutions, as well as theoretical irradiated ocean models. TOI-1751 b is a warm sub-Neptune with an equilibrium temperature of ∼820 K. As TOI-1751 is a metal-poor star, TOI-1751 b may have formed in a water-enriched formation environment. We thus favor a volatile-rich interior composition for this planet.",

keywords = "Radial velocity, Exoplanet structure, Transit photometry, Mini Neptunes",

author = "Anmol Desai and Turtelboom, {Emma V.} and Harada, {Caleb K.} and Dressing, {Courtney D.} and Rice, {David R.} and Murphy, {Joseph M.Akana} and Brinkman, {Casey L.} and Ashley Chontos and Crossfield, {Ian J.M.} and Fei Dai and Hill, {Michelle L.} and Tara Fetherolf and Steven Giacalone and Howard, {Andrew W.} and Daniel Huber and Howard Isaacson and Kane, {Stephen R.} and Jack Lubin and MacDougall, {Mason G.} and Mayo, {Andrew W.} and Teo Mo{\v c}nik and Polanski, {Alex S.} and Malena Rice and Paul Robertson and Rubenzahl, {Ryan A.} and {Van Zandt}, Judah and Weiss, {Lauren M.} and Allyson Bieryla and Buchhave, {Lars A.} and Jenkins, {Jon M.} and Kostov, {Veselin B.} and Levine, {Alan M.} and Jorge Lillo-Box and M. Paegert and Markus Rabus and S. Seager and Stassun, {Keivan G.} and Ting, {Eric B.} and David Watanabe and Winn, {Joshua N.}",

note = "Publisher Copyright: {\textcopyright} 2024. The Author(s). Published by the American Astronomical Society.",

year = "2024",

doi = "10.3847/1538-3881/ad29ee",

language = "English",

volume = "167",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "5",

}

Desai, A, Turtelboom, EV, Harada, CK, Dressing, CD, Rice, DR, Murphy, JMA, Brinkman, CL, Chontos, A, Crossfield, IJM, Dai, F, Hill, ML, Fetherolf, T, Giacalone, S, Howard, AW, Huber, D, Isaacson, H, Kane, SR, Lubin, J, MacDougall, MG, Mayo, AW, Močnik, T, Polanski, AS, Rice, M, Robertson, P, Rubenzahl, RA, Van Zandt, J, Weiss, LM, Bieryla, A, Buchhave, LA, Jenkins, JM, Kostov, VB, Levine, AM, Lillo-Box, J, Paegert, M, Rabus, M, Seager, S, Stassun, KG, Ting, EB, Watanabe, D & Winn, JN 2024, 'The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System', Astronomical Journal, vol. 167, no. 5, 194. https://doi.org/10.3847/1538-3881/ad29ee

TY - JOUR

T1 - The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System

AU - Desai, Anmol

AU - Turtelboom, Emma V.

AU - Harada, Caleb K.

AU - Dressing, Courtney D.

AU - Rice, David R.

AU - Murphy, Joseph M.Akana

AU - Brinkman, Casey L.

AU - Chontos, Ashley

AU - Crossfield, Ian J.M.

AU - Dai, Fei

AU - Hill, Michelle L.

AU - Fetherolf, Tara

AU - Giacalone, Steven

AU - Howard, Andrew W.

AU - Huber, Daniel

AU - Isaacson, Howard

AU - Kane, Stephen R.

AU - Lubin, Jack

AU - MacDougall, Mason G.

AU - Mayo, Andrew W.

AU - Močnik, Teo

AU - Polanski, Alex S.

AU - Rice, Malena

AU - Robertson, Paul

AU - Rubenzahl, Ryan A.

AU - Van Zandt, Judah

AU - Weiss, Lauren M.

AU - Bieryla, Allyson

AU - Buchhave, Lars A.

AU - Jenkins, Jon M.

AU - Kostov, Veselin B.

AU - Levine, Alan M.

AU - Lillo-Box, Jorge

AU - Paegert, M.

AU - Rabus, Markus

AU - Seager, S.

AU - Stassun, Keivan G.

AU - Ting, Eric B.

AU - Watanabe, David

AU - Winn, Joshua N.

PY - 2024

Y1 - 2024

N2 - We present and confirm TOI-1751 b, a transiting sub-Neptune orbiting a slightly evolved, solar-type, metal-poor star (T eff = 5996 ± 110 K, log ( g ) = 4.2 ± 0.1 , V = 9.3 mag, [Fe/H] = −0.40 ± 0.06 dex) every 37.47 days. We use TESS photometry to measure a planet radius of 2.77 − 0.07 + 0.15 R ⊕ . We also use both Keck/HIRES and APF/Levy radial velocities (RV) to derive a planet mass of 14.5 − 3.14 + 3.15 M ⊕ , and thus a planet density of 3.6 ± 0.9 g cm−3. There is also a long-period (∼400 days) signal that is observed in only the Keck/HIRES data. We conclude that this long-period signal is not planetary in nature and is likely due to the window function of the Keck/HIRES observations. This highlights the role of complementary observations from multiple observatories to identify and exclude aliases in RV data. Finally, we investigate the potential compositions of this planet, including rocky and water-rich solutions, as well as theoretical irradiated ocean models. TOI-1751 b is a warm sub-Neptune with an equilibrium temperature of ∼820 K. As TOI-1751 is a metal-poor star, TOI-1751 b may have formed in a water-enriched formation environment. We thus favor a volatile-rich interior composition for this planet.

AB - We present and confirm TOI-1751 b, a transiting sub-Neptune orbiting a slightly evolved, solar-type, metal-poor star (T eff = 5996 ± 110 K, log ( g ) = 4.2 ± 0.1 , V = 9.3 mag, [Fe/H] = −0.40 ± 0.06 dex) every 37.47 days. We use TESS photometry to measure a planet radius of 2.77 − 0.07 + 0.15 R ⊕ . We also use both Keck/HIRES and APF/Levy radial velocities (RV) to derive a planet mass of 14.5 − 3.14 + 3.15 M ⊕ , and thus a planet density of 3.6 ± 0.9 g cm−3. There is also a long-period (∼400 days) signal that is observed in only the Keck/HIRES data. We conclude that this long-period signal is not planetary in nature and is likely due to the window function of the Keck/HIRES observations. This highlights the role of complementary observations from multiple observatories to identify and exclude aliases in RV data. Finally, we investigate the potential compositions of this planet, including rocky and water-rich solutions, as well as theoretical irradiated ocean models. TOI-1751 b is a warm sub-Neptune with an equilibrium temperature of ∼820 K. As TOI-1751 is a metal-poor star, TOI-1751 b may have formed in a water-enriched formation environment. We thus favor a volatile-rich interior composition for this planet.

KW - Radial velocity

KW - Exoplanet structure

KW - Transit photometry

KW - Mini Neptunes

U2 - 10.3847/1538-3881/ad29ee

DO - 10.3847/1538-3881/ad29ee

M3 - Journal article

AN - SCOPUS:85189921129

SN - 0004-6256

VL - 167

JO - Astronomical Journal

JF - Astronomical Journal

IS - 5

M1 - 194

ER -

The TESS-Keck Survey. XVIII. A Sub-Neptune and Spurious Long-period Signal in the TOI-1751 System

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