TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group

Andrew W. Mann; Marshall C. Johnson; Andrew Vanderburg; Adam L. Kraus; Aaron C. Rizzuto; MacKenna L. Wood; Jonathan L. Bush; Keighley Rockcliffe; Elisabeth R. Newton; David W. Latham; Eric E. Mamajek; George Zhou; Samuel N. Quinn; Pa Chia Thao; Serena Benatti; Rosario Cosentino; Silvano Desidera; Avet Harutyunyan; Christophe Lovis; Annelies Mortier; Francesco A. Pepe; Ennio Poretti; Thomas G. Wilson; Martti H. Kristiansen; Robert Gagliano; Thomas Jacobs; Daryll M. Lacourse; Mark Omohundro; Hans Martin Schwengeler; Ivan A. Terentev; Stephen R. Kane; Michelle L. Hill; Markus Rabus; Gilbert A. Esquerdo; Perry Berlind; Karen A. Collins; Gabriel Murawski; Nezar Hazam Sallam; Michael M. Aitken; Bob Massey; George R. Ricker; Roland Vanderspek; Sara Seager; Joshua N. Winn; Jon M. Jenkins; Thomas Barclay; Douglas A. Caldwell; Diana Dragomir; John P. Doty; Ana Glidden; Peter Tenenbaum; Guillermo Torres; Joseph D. Twicken; Steven Villanueva

doi:10.3847/1538-3881/abae64

TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group

Andrew W. Mann^*, Marshall C. Johnson, Andrew Vanderburg, Adam L. Kraus, Aaron C. Rizzuto, MacKenna L. Wood, Jonathan L. Bush, Keighley Rockcliffe, Elisabeth R. Newton, David W. Latham, Eric E. Mamajek, George Zhou, Samuel N. Quinn, Pa Chia Thao, Serena Benatti, Rosario Cosentino, Silvano Desidera, Avet Harutyunyan, Christophe Lovis, Annelies MortierFrancesco A. Pepe, Ennio Poretti, Thomas G. Wilson, Martti H. Kristiansen, Robert Gagliano, Thomas Jacobs, Daryll M. Lacourse, Mark Omohundro, Hans Martin Schwengeler, Ivan A. Terentev, Stephen R. Kane, Michelle L. Hill, Markus Rabus, Gilbert A. Esquerdo, Perry Berlind, Karen A. Collins, Gabriel Murawski, Nezar Hazam Sallam, Michael M. Aitken, Bob Massey, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Thomas Barclay, Douglas A. Caldwell, Diana Dragomir, John P. Doty, Ana Glidden, Peter Tenenbaum, Guillermo Torres, Joseph D. Twicken, Steven Villanueva

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

Abstract

Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets (<1 Gyr) offer an opportunity to probe the critical early stages of this evolution, where planets evolve the fastest. However, most of the known young planets orbit prohibitively faint stars. We present the discovery of two planets transiting HD 63433 (TOI 1726, TIC 130181866), a young Sun-like (M∗=0.99±0.03) star. Through kinematics, lithium abundance, and rotation, we confirm that HD 63433 is a member of the Ursa Major moving group (τ=414±23 Myr). Based on the TESS light curve and updated stellar parameters, we estimate the planet radii are 2.15±0.10R⊕ and 2.67±0.12R⊕, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using HARPS-N velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V=6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.

Original language	English
Article number	179
Number of pages	18
Journal	Astronomical Journal
Volume	160
Issue number	179
DOIs	https://doi.org/10.3847/1538-3881/abae64
Publication status	Published - 24 Sept 2020

Keywords

Young star clusters
Exoplanet evolution
Transits
Exoplanet astronomy
Stellar activity
Stellar rotation
Exoplanet dynamics

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Mann-2020-TESS-hunt-for-young-and-AJ-AAM
Copyright © 2020 The American Astronomical Society. All rights reserved. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-3881/abae64.
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Mann, A. W., Johnson, M. C., Vanderburg, A., Kraus, A. L., Rizzuto, A. C., Wood, M. L., Bush, J. L., Rockcliffe, K., Newton, E. R., Latham, D. W., Mamajek, E. E., Zhou, G., Quinn, S. N., Thao, P. C., Benatti, S., Cosentino, R., Desidera, S., Harutyunyan, A., Lovis, C., ... Villanueva, S. (2020). TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group. Astronomical Journal, 160(179), Article 179. https://doi.org/10.3847/1538-3881/abae64

@article{67346f9e6ac64bd3b41c1946966f48be,

title = "TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group",

abstract = "Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets (<1 Gyr) offer an opportunity to probe the critical early stages of this evolution, where planets evolve the fastest. However, most of the known young planets orbit prohibitively faint stars. We present the discovery of two planets transiting HD 63433 (TOI 1726, TIC 130181866), a young Sun-like (M∗=0.99±0.03) star. Through kinematics, lithium abundance, and rotation, we confirm that HD 63433 is a member of the Ursa Major moving group (τ=414±23 Myr). Based on the TESS light curve and updated stellar parameters, we estimate the planet radii are 2.15±0.10R⊕ and 2.67±0.12R⊕, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using HARPS-N velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V=6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.",

keywords = "Young star clusters, Exoplanet evolution, Transits, Exoplanet astronomy, Stellar activity, Stellar rotation, Exoplanet dynamics",

author = "Mann, {Andrew W.} and Johnson, {Marshall C.} and Andrew Vanderburg and Kraus, {Adam L.} and Rizzuto, {Aaron C.} and Wood, {MacKenna L.} and Bush, {Jonathan L.} and Keighley Rockcliffe and Newton, {Elisabeth R.} and Latham, {David W.} and Mamajek, {Eric E.} and George Zhou and Quinn, {Samuel N.} and Thao, {Pa Chia} and Serena Benatti and Rosario Cosentino and Silvano Desidera and Avet Harutyunyan and Christophe Lovis and Annelies Mortier and Pepe, {Francesco A.} and Ennio Poretti and Wilson, {Thomas G.} and Kristiansen, {Martti H.} and Robert Gagliano and Thomas Jacobs and Lacourse, {Daryll M.} and Mark Omohundro and Schwengeler, {Hans Martin} and Terentev, {Ivan A.} and Kane, {Stephen R.} and Hill, {Michelle L.} and Markus Rabus and Esquerdo, {Gilbert A.} and Perry Berlind and Collins, {Karen A.} and Gabriel Murawski and Sallam, {Nezar Hazam} and Aitken, {Michael M.} and Bob Massey and Ricker, {George R.} and Roland Vanderspek and Sara Seager and Winn, {Joshua N.} and Jenkins, {Jon M.} and Thomas Barclay and Caldwell, {Douglas A.} and Diana Dragomir and Doty, {John P.} and Ana Glidden and Peter Tenenbaum and Guillermo Torres and Twicken, {Joseph D.} and Steven Villanueva",

note = "A.W.M. was supported through NASA's Astrophysics Data Analysis Program (80NSSC19K0583). M.L.W. was supported by a grant through NASA's K2 GO program (80NSSC19K0097). This material is based on work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1650116 to P.C.T. A.V.'s work was performed under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. D.D. acknowledges support from NASA through Caltech/JPL grant RSA-1006130 and through the TESS Guest Investigator Program grant 80NSSC19K1727.",

year = "2020",

month = sep,

day = "24",

doi = "10.3847/1538-3881/abae64",

language = "English",

volume = "160",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "179",

}

Mann, AW, Johnson, MC, Vanderburg, A, Kraus, AL, Rizzuto, AC, Wood, ML, Bush, JL, Rockcliffe, K, Newton, ER, Latham, DW, Mamajek, EE, Zhou, G, Quinn, SN, Thao, PC, Benatti, S, Cosentino, R, Desidera, S, Harutyunyan, A, Lovis, C, Mortier, A, Pepe, FA, Poretti, E, Wilson, TG, Kristiansen, MH, Gagliano, R, Jacobs, T, Lacourse, DM, Omohundro, M, Schwengeler, HM, Terentev, IA, Kane, SR, Hill, ML, Rabus, M, Esquerdo, GA, Berlind, P, Collins, KA, Murawski, G, Sallam, NH, Aitken, MM, Massey, B, Ricker, GR, Vanderspek, R, Seager, S, Winn, JN, Jenkins, JM, Barclay, T, Caldwell, DA, Dragomir, D, Doty, JP, Glidden, A, Tenenbaum, P, Torres, G, Twicken, JD & Villanueva, S 2020, 'TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group', Astronomical Journal, vol. 160, no. 179, 179. https://doi.org/10.3847/1538-3881/abae64

TY - JOUR

T1 - TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group

AU - Mann, Andrew W.

AU - Johnson, Marshall C.

AU - Vanderburg, Andrew

AU - Kraus, Adam L.

AU - Rizzuto, Aaron C.

AU - Wood, MacKenna L.

AU - Bush, Jonathan L.

AU - Rockcliffe, Keighley

AU - Newton, Elisabeth R.

AU - Latham, David W.

AU - Mamajek, Eric E.

AU - Zhou, George

AU - Quinn, Samuel N.

AU - Thao, Pa Chia

AU - Benatti, Serena

AU - Cosentino, Rosario

AU - Desidera, Silvano

AU - Harutyunyan, Avet

AU - Lovis, Christophe

AU - Mortier, Annelies

AU - Pepe, Francesco A.

AU - Poretti, Ennio

AU - Wilson, Thomas G.

AU - Kristiansen, Martti H.

AU - Gagliano, Robert

AU - Jacobs, Thomas

AU - Lacourse, Daryll M.

AU - Omohundro, Mark

AU - Schwengeler, Hans Martin

AU - Terentev, Ivan A.

AU - Kane, Stephen R.

AU - Hill, Michelle L.

AU - Rabus, Markus

AU - Esquerdo, Gilbert A.

AU - Berlind, Perry

AU - Collins, Karen A.

AU - Murawski, Gabriel

AU - Sallam, Nezar Hazam

AU - Aitken, Michael M.

AU - Massey, Bob

AU - Ricker, George R.

AU - Vanderspek, Roland

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Jenkins, Jon M.

AU - Barclay, Thomas

AU - Caldwell, Douglas A.

AU - Dragomir, Diana

AU - Doty, John P.

AU - Glidden, Ana

AU - Tenenbaum, Peter

AU - Torres, Guillermo

AU - Twicken, Joseph D.

AU - Villanueva, Steven

N1 - A.W.M. was supported through NASA's Astrophysics Data Analysis Program (80NSSC19K0583). M.L.W. was supported by a grant through NASA's K2 GO program (80NSSC19K0097). This material is based on work supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1650116 to P.C.T. A.V.'s work was performed under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. D.D. acknowledges support from NASA through Caltech/JPL grant RSA-1006130 and through the TESS Guest Investigator Program grant 80NSSC19K1727.

PY - 2020/9/24

Y1 - 2020/9/24

N2 - Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets (<1 Gyr) offer an opportunity to probe the critical early stages of this evolution, where planets evolve the fastest. However, most of the known young planets orbit prohibitively faint stars. We present the discovery of two planets transiting HD 63433 (TOI 1726, TIC 130181866), a young Sun-like (M∗=0.99±0.03) star. Through kinematics, lithium abundance, and rotation, we confirm that HD 63433 is a member of the Ursa Major moving group (τ=414±23 Myr). Based on the TESS light curve and updated stellar parameters, we estimate the planet radii are 2.15±0.10R⊕ and 2.67±0.12R⊕, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using HARPS-N velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V=6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.

AB - Exoplanets can evolve significantly between birth and maturity, as their atmospheres, orbits, and structures are shaped by their environment. Young planets (<1 Gyr) offer an opportunity to probe the critical early stages of this evolution, where planets evolve the fastest. However, most of the known young planets orbit prohibitively faint stars. We present the discovery of two planets transiting HD 63433 (TOI 1726, TIC 130181866), a young Sun-like (M∗=0.99±0.03) star. Through kinematics, lithium abundance, and rotation, we confirm that HD 63433 is a member of the Ursa Major moving group (τ=414±23 Myr). Based on the TESS light curve and updated stellar parameters, we estimate the planet radii are 2.15±0.10R⊕ and 2.67±0.12R⊕, the orbital periods are 7.11 and 20.55 days, and the orbital eccentricities are lower than about 0.2. Using HARPS-N velocities, we measure the Rossiter-McLaughlin signal of the inner planet, demonstrating that the orbit is prograde. Since the host star is bright (V=6.9), both planets are amenable to transmission spectroscopy, radial velocity measurements of their masses, and more precise determination of the stellar obliquity. This system is therefore poised to play an important role in our understanding of planetary system evolution in the first billion years after formation.

KW - Young star clusters

KW - Exoplanet evolution

KW - Transits

KW - Exoplanet astronomy

KW - Stellar activity

KW - Stellar rotation

KW - Exoplanet dynamics

U2 - 10.3847/1538-3881/abae64

DO - 10.3847/1538-3881/abae64

M3 - Article

AN - SCOPUS:85092609273

SN - 0004-6256

VL - 160

JO - Astronomical Journal

JF - Astronomical Journal

IS - 179

M1 - 179

ER -

TESS hunt for young and maturing exoplanets (THYME). III. A two-planet system in the 400 Myr Ursa major group

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Keywords

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