Near-resonance in a System of Sub-Neptunes from TESS

Samuel N. Quinn; Juliette C. Becker; Joseph E. Rodriguez; Sam Hadden; Chelsea X. Huang; Timothy D. Morton; Fred C. Adams; David Armstrong; Jason D. Eastman; Jonathan Horner; Stephen R. Kane; Jack J. Lissauer; Joseph D. Twicken; Andrew Vanderburg; Rob Wittenmyer; George R. Ricker; Roland K. Vanderspek; David W. Latham; Sara Seager; Joshua N. Winn; Jon M. Jenkins; Eric Agol; Khalid Barkaoui; Charles A. Beichman; François Bouchy; L. G. Bouma; Artem Burdanov; Jennifer Campbell; Roberto Carlino; Scott M. Cartwright; David Charbonneau; Jessie L. Christiansen; David Ciardi; Karen A. Collins; Kevin I. Collins; Dennis M. Conti; Ian J. M. Crossfield; Tansu Daylan; Jason Dittmann; John Doty; Diana Dragomir; Elsa Ducrot; Michael Gillon; Ana Glidden; Robert F. Goeke; Erica J. Gonzales; Krzysztof G. Helminiak; Elliott P. Horch; Steve B. Howell; Emmanuel Jehin; Eric L. N. Jensen; John F. Kielkopf; Martti H. Kristiansen; Nicholas Law; Andrew W. Mann; Maxime Marmier; Rachel A. Matson; Elisabeth Matthews; Tsevi Mazeh; Mayuko Mori; Felipe Murgas; Catriona Murray; Norio Narita; Louise D. Nielsen; Gaël Ottoni; Enric Palle; Rafal Pawlaszek; Francesco Pepe; Jerome Pitogo de Leon; Francisco J. Pozuelos; Howard M. Relles; Joshua E. Schlieder; Daniel Sebastian; Damien Ségransan; Avi Shporer; Keivan G. Stassun; Motohide Tamura; Stéphane Udry; Ian Waite; Jennifer G. Winters; Carl Ziegler

doi:10.3847/1538-3881/ab3f2b

Near-resonance in a System of Sub-Neptunes from TESS

Samuel N. Quinn^*, Juliette C. Becker, Joseph E. Rodriguez, Sam Hadden, Chelsea X. Huang, Timothy D. Morton, Fred C. Adams, David Armstrong, Jason D. Eastman, Jonathan Horner, Stephen R. Kane, Jack J. Lissauer, Joseph D. Twicken, Andrew Vanderburg, Rob Wittenmyer, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. WinnJon M. Jenkins, Eric Agol, Khalid Barkaoui, Charles A. Beichman, François Bouchy, L. G. Bouma, Artem Burdanov, Jennifer Campbell, Roberto Carlino, Scott M. Cartwright, David Charbonneau, Jessie L. Christiansen, David Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, Jason Dittmann, John Doty, Diana Dragomir, Elsa Ducrot, Michael Gillon, Ana Glidden, Robert F. Goeke, Erica J. Gonzales, Krzysztof G. Helminiak, Elliott P. Horch, Steve B. Howell, Emmanuel Jehin, Eric L. N. Jensen, John F. Kielkopf, Martti H. Kristiansen, Nicholas Law, Andrew W. Mann, Maxime Marmier, Rachel A. Matson, Elisabeth Matthews, Tsevi Mazeh, Mayuko Mori, Felipe Murgas, Catriona Murray, Norio Narita, Louise D. Nielsen, Gaël Ottoni, Enric Palle, Rafal Pawlaszek, Francesco Pepe, Jerome Pitogo de Leon, Francisco J. Pozuelos, Howard M. Relles, Joshua E. Schlieder, Daniel Sebastian, Damien Ségransan, Avi Shporer, Keivan G. Stassun, Motohide Tamura, Stéphane Udry, Ian Waite, Jennifer G. Winters, Carl Ziegler

^*Corresponding author for this work

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Abstract

We report the Transiting Exoplanet Survey Satellite detection of a multi-planet system orbiting the V = 10.9 K0 dwarf TOI-125. We find evidence for up to five planets, with varying confidence. Three transit signals with high signal-to-noise ratio correspond to sub-Neptune-sized planets (2.76, 2.79, and 2.94 R ⊕), and we statistically validate the planetary nature of the two inner planets (P b = 4.65 days, P c = 9.15 days). With only two transits observed, we report the outer object (P .03 = 19.98 days) as a planet candidate with high signal-to-noise ratio. We also detect a candidate transiting super-Earth (1.4 R ⊕) with an orbital period of only 12.7 hr and a candidate Neptune-sized planet (4.2 R ⊕) with a period of 13.28 days, both at low signal-to-noise ratio. This system is amenable to mass determination via radial velocities and transit-timing variations, and provides an opportunity to study planets of similar size while controlling for age and environment. The ratio of orbital periods between TOI-125 b and c (P c /P b = 1.97) is slightly lower than an exact 2:1 commensurability and is atypical of multiple planet systems from Kepler, which show a preference for period ratios just wide of first-order period ratios. A dynamical analysis refines the allowed parameter space through stability arguments and suggests that despite the nearly commensurate periods, the system is unlikely to be in resonance.

Original language	English
Article number	177
Journal	Astrophysical Journal
Volume	158
Issue number	5
Number of pages	16
ISSN	0004-637X
DOIs	https://doi.org/10.3847/1538-3881/ab3f2b
Publication status	Published - 2019

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Quinn, S. N., Becker, J. C., Rodriguez, J. E., Hadden, S., Huang, C. X., Morton, T. D., Adams, F. C., Armstrong, D., Eastman, J. D., Horner, J., Kane, S. R., Lissauer, J. J., Twicken, J. D., Vanderburg, A., Wittenmyer, R., Ricker, G. R., Vanderspek, R. K., Latham, D. W., Seager, S., ... Ziegler, C. (2019). Near-resonance in a System of Sub-Neptunes from TESS. Astrophysical Journal, 158(5), Article 177. https://doi.org/10.3847/1538-3881/ab3f2b

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title = "Near-resonance in a System of Sub-Neptunes from TESS",

abstract = "We report the Transiting Exoplanet Survey Satellite detection of a multi-planet system orbiting the V = 10.9 K0 dwarf TOI-125. We find evidence for up to five planets, with varying confidence. Three transit signals with high signal-to-noise ratio correspond to sub-Neptune-sized planets (2.76, 2.79, and 2.94 R ⊕), and we statistically validate the planetary nature of the two inner planets (P b = 4.65 days, P c = 9.15 days). With only two transits observed, we report the outer object (P .03 = 19.98 days) as a planet candidate with high signal-to-noise ratio. We also detect a candidate transiting super-Earth (1.4 R ⊕) with an orbital period of only 12.7 hr and a candidate Neptune-sized planet (4.2 R ⊕) with a period of 13.28 days, both at low signal-to-noise ratio. This system is amenable to mass determination via radial velocities and transit-timing variations, and provides an opportunity to study planets of similar size while controlling for age and environment. The ratio of orbital periods between TOI-125 b and c (P c /P b = 1.97) is slightly lower than an exact 2:1 commensurability and is atypical of multiple planet systems from Kepler, which show a preference for period ratios just wide of first-order period ratios. A dynamical analysis refines the allowed parameter space through stability arguments and suggests that despite the nearly commensurate periods, the system is unlikely to be in resonance.",

author = "Quinn, {Samuel N.} and Becker, {Juliette C.} and Rodriguez, {Joseph E.} and Sam Hadden and Huang, {Chelsea X.} and Morton, {Timothy D.} and Adams, {Fred C.} and David Armstrong and Eastman, {Jason D.} and Jonathan Horner and Kane, {Stephen R.} and Lissauer, {Jack J.} and Twicken, {Joseph D.} and Andrew Vanderburg and Rob Wittenmyer and Ricker, {George R.} and Vanderspek, {Roland K.} and Latham, {David W.} and Sara Seager and Winn, {Joshua N.} and Jenkins, {Jon M.} and Eric Agol and Khalid Barkaoui and Beichman, {Charles A.} and Fran{\c c}ois Bouchy and Bouma, {L. G.} and Artem Burdanov and Jennifer Campbell and Roberto Carlino and Cartwright, {Scott M.} and David Charbonneau and Christiansen, {Jessie L.} and David Ciardi and Collins, {Karen A.} and Collins, {Kevin I.} and Conti, {Dennis M.} and Crossfield, {Ian J. M.} and Tansu Daylan and Jason Dittmann and John Doty and Diana Dragomir and Elsa Ducrot and Michael Gillon and Ana Glidden and Goeke, {Robert F.} and Gonzales, {Erica J.} and Helminiak, {Krzysztof G.} and Horch, {Elliott P.} and Howell, {Steve B.} and Emmanuel Jehin and Jensen, {Eric L. N.} and Kielkopf, {John F.} and Kristiansen, {Martti H.} and Nicholas Law and Mann, {Andrew W.} and Maxime Marmier and Matson, {Rachel A.} and Elisabeth Matthews and Tsevi Mazeh and Mayuko Mori and Felipe Murgas and Catriona Murray and Norio Narita and Nielsen, {Louise D.} and Ga{\"e}l Ottoni and Enric Palle and Rafal Pawlaszek and Francesco Pepe and Leon, {Jerome Pitogo de} and Pozuelos, {Francisco J.} and Relles, {Howard M.} and Schlieder, {Joshua E.} and Daniel Sebastian and Damien S{\'e}gransan and Avi Shporer and Stassun, {Keivan G.} and Motohide Tamura and St{\'e}phane Udry and Ian Waite and Winters, {Jennifer G.} and Carl Ziegler",

year = "2019",

doi = "10.3847/1538-3881/ab3f2b",

language = "English",

volume = "158",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "5",

}

Quinn, SN, Becker, JC, Rodriguez, JE, Hadden, S, Huang, CX, Morton, TD, Adams, FC, Armstrong, D, Eastman, JD, Horner, J, Kane, SR, Lissauer, JJ, Twicken, JD, Vanderburg, A, Wittenmyer, R, Ricker, GR, Vanderspek, RK, Latham, DW, Seager, S, Winn, JN, Jenkins, JM, Agol, E, Barkaoui, K, Beichman, CA, Bouchy, F, Bouma, LG, Burdanov, A, Campbell, J, Carlino, R, Cartwright, SM, Charbonneau, D, Christiansen, JL, Ciardi, D, Collins, KA, Collins, KI, Conti, DM, Crossfield, IJM, Daylan, T, Dittmann, J, Doty, J, Dragomir, D, Ducrot, E, Gillon, M, Glidden, A, Goeke, RF, Gonzales, EJ, Helminiak, KG, Horch, EP, Howell, SB, Jehin, E, Jensen, ELN, Kielkopf, JF, Kristiansen, MH, Law, N, Mann, AW, Marmier, M, Matson, RA, Matthews, E, Mazeh, T, Mori, M, Murgas, F, Murray, C, Narita, N, Nielsen, LD, Ottoni, G, Palle, E, Pawlaszek, R, Pepe, F, Leon, JPD, Pozuelos, FJ, Relles, HM, Schlieder, JE, Sebastian, D, Ségransan, D, Shporer, A, Stassun, KG, Tamura, M, Udry, S, Waite, I, Winters, JG & Ziegler, C 2019, 'Near-resonance in a System of Sub-Neptunes from TESS', Astrophysical Journal, vol. 158, no. 5, 177. https://doi.org/10.3847/1538-3881/ab3f2b

TY - JOUR

T1 - Near-resonance in a System of Sub-Neptunes from TESS

AU - Quinn, Samuel N.

AU - Becker, Juliette C.

AU - Rodriguez, Joseph E.

AU - Hadden, Sam

AU - Huang, Chelsea X.

AU - Morton, Timothy D.

AU - Adams, Fred C.

AU - Armstrong, David

AU - Eastman, Jason D.

AU - Horner, Jonathan

AU - Kane, Stephen R.

AU - Lissauer, Jack J.

AU - Twicken, Joseph D.

AU - Vanderburg, Andrew

AU - Wittenmyer, Rob

AU - Ricker, George R.

AU - Vanderspek, Roland K.

AU - Latham, David W.

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Jenkins, Jon M.

AU - Agol, Eric

AU - Barkaoui, Khalid

AU - Beichman, Charles A.

AU - Bouchy, François

AU - Bouma, L. G.

AU - Burdanov, Artem

AU - Campbell, Jennifer

AU - Carlino, Roberto

AU - Cartwright, Scott M.

AU - Charbonneau, David

AU - Christiansen, Jessie L.

AU - Ciardi, David

AU - Collins, Karen A.

AU - Collins, Kevin I.

AU - Conti, Dennis M.

AU - Crossfield, Ian J. M.

AU - Daylan, Tansu

AU - Dittmann, Jason

AU - Doty, John

AU - Dragomir, Diana

AU - Ducrot, Elsa

AU - Gillon, Michael

AU - Glidden, Ana

AU - Goeke, Robert F.

AU - Gonzales, Erica J.

AU - Helminiak, Krzysztof G.

AU - Horch, Elliott P.

AU - Howell, Steve B.

AU - Jehin, Emmanuel

AU - Jensen, Eric L. N.

AU - Kielkopf, John F.

AU - Kristiansen, Martti H.

AU - Law, Nicholas

AU - Mann, Andrew W.

AU - Marmier, Maxime

AU - Matson, Rachel A.

AU - Matthews, Elisabeth

AU - Mazeh, Tsevi

AU - Mori, Mayuko

AU - Murgas, Felipe

AU - Murray, Catriona

AU - Narita, Norio

AU - Nielsen, Louise D.

AU - Ottoni, Gaël

AU - Palle, Enric

AU - Pawlaszek, Rafal

AU - Pepe, Francesco

AU - Leon, Jerome Pitogo de

AU - Pozuelos, Francisco J.

AU - Relles, Howard M.

AU - Schlieder, Joshua E.

AU - Sebastian, Daniel

AU - Ségransan, Damien

AU - Shporer, Avi

AU - Stassun, Keivan G.

AU - Tamura, Motohide

AU - Udry, Stéphane

AU - Waite, Ian

AU - Winters, Jennifer G.

AU - Ziegler, Carl

PY - 2019

Y1 - 2019

N2 - We report the Transiting Exoplanet Survey Satellite detection of a multi-planet system orbiting the V = 10.9 K0 dwarf TOI-125. We find evidence for up to five planets, with varying confidence. Three transit signals with high signal-to-noise ratio correspond to sub-Neptune-sized planets (2.76, 2.79, and 2.94 R ⊕), and we statistically validate the planetary nature of the two inner planets (P b = 4.65 days, P c = 9.15 days). With only two transits observed, we report the outer object (P .03 = 19.98 days) as a planet candidate with high signal-to-noise ratio. We also detect a candidate transiting super-Earth (1.4 R ⊕) with an orbital period of only 12.7 hr and a candidate Neptune-sized planet (4.2 R ⊕) with a period of 13.28 days, both at low signal-to-noise ratio. This system is amenable to mass determination via radial velocities and transit-timing variations, and provides an opportunity to study planets of similar size while controlling for age and environment. The ratio of orbital periods between TOI-125 b and c (P c /P b = 1.97) is slightly lower than an exact 2:1 commensurability and is atypical of multiple planet systems from Kepler, which show a preference for period ratios just wide of first-order period ratios. A dynamical analysis refines the allowed parameter space through stability arguments and suggests that despite the nearly commensurate periods, the system is unlikely to be in resonance.

AB - We report the Transiting Exoplanet Survey Satellite detection of a multi-planet system orbiting the V = 10.9 K0 dwarf TOI-125. We find evidence for up to five planets, with varying confidence. Three transit signals with high signal-to-noise ratio correspond to sub-Neptune-sized planets (2.76, 2.79, and 2.94 R ⊕), and we statistically validate the planetary nature of the two inner planets (P b = 4.65 days, P c = 9.15 days). With only two transits observed, we report the outer object (P .03 = 19.98 days) as a planet candidate with high signal-to-noise ratio. We also detect a candidate transiting super-Earth (1.4 R ⊕) with an orbital period of only 12.7 hr and a candidate Neptune-sized planet (4.2 R ⊕) with a period of 13.28 days, both at low signal-to-noise ratio. This system is amenable to mass determination via radial velocities and transit-timing variations, and provides an opportunity to study planets of similar size while controlling for age and environment. The ratio of orbital periods between TOI-125 b and c (P c /P b = 1.97) is slightly lower than an exact 2:1 commensurability and is atypical of multiple planet systems from Kepler, which show a preference for period ratios just wide of first-order period ratios. A dynamical analysis refines the allowed parameter space through stability arguments and suggests that despite the nearly commensurate periods, the system is unlikely to be in resonance.

U2 - 10.3847/1538-3881/ab3f2b

DO - 10.3847/1538-3881/ab3f2b

M3 - Journal article

SN - 0004-637X

VL - 158

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 5

M1 - 177

ER -

Near-resonance in a System of Sub-Neptunes from TESS

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