Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS

Nataliea Lowson; George Zhou; Chelsea X. Huang; Duncan J. Wright; Billy Edwards; Emma Nabbie; Alex Venner; Samuel N. Quinn; Karen A. Collins; Edward Gillen; Matthew Battley; Amaury Triaud; Coel Hellier; Sara Seager; Joshua N. Winn; Jon M. Jenkins; Bill Wohler; Avi Shporer; Richard P. Schwarz; Felipe Murgas; Enric Pallé; David R. Anderson; Richard G. West; Robert A. Wittenmyer; Brendan P. Bowler; Jonathan Horner; Stephen R. Kane; John Kielkopf; Peter Plavchan; Hui Zhang; Tyler Fairnington; Jack Okumura; Matthew W. Mengel; Brett C. Addison

doi:10.1093/mnras/stad2756

Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS

Nataliea Lowson^*, George Zhou, Chelsea X. Huang, Duncan J. Wright, Billy Edwards, Emma Nabbie, Alex Venner, Samuel N. Quinn, Karen A. Collins, Edward Gillen, Matthew Battley, Amaury Triaud, Coel Hellier, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Bill Wohler, Avi Shporer, Richard P. Schwarz, Felipe MurgasEnric Pallé, David R. Anderson, Richard G. West, Robert A. Wittenmyer, Brendan P. Bowler, Jonathan Horner, Stephen R. Kane, John Kielkopf, Peter Plavchan, Hui Zhang, Tyler Fairnington, Jack Okumura, Matthew W. Mengel, Brett C. Addison

^*Corresponding author for this work

Physics and Astronomy

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Abstract

We report the discovery of two mini-Neptunes in near 2:1 resonance orbits (P = 7.610303 d for HIP 113103 b and P = 14.245651 d for HIP 113103 c ) around the adolescent K-star HIP 113103 (TIC 121490076 ). The planet system was first identified from the TESS mission, and was confirmed via additional photometric and spectroscopic observations, including a ∼17.5 hour observation for the transits of both planets using ESA CHEOPS . We place ≤4.5 min and ≤2.5 min limits on the absence of transit timing variations over the three year photometric baseline, allowing further constraints on the orbital eccentricities of the system beyond that available from the photometric transit duration alone. With a planetary radius of Rp = 1.829+0.096−0.067
R⊕, HIP 113103 b resides within the radius gap, and this might provide invaluable information on the formation disparities between super-Earths and mini-Neptunes. Given the larger radius Rp = 2.40+0.10−0.08
R⊕ for HIP 113103 c , and close proximity of both planets to HIP 113103 , it is likely that HIP 113103 b might have lost (or is still losing) its primordial atmosphere. We therefore present simulated atmospheric transmission spectra of both planets using JWST , HST , and Twinkle . It demonstrates a potential metallicity difference (due to differences in their evolution) would be a challenge to detect if the atmospheres are in chemical equilibrium. As one of the brightest multi sub-Neptune planet systems suitable for atmosphere follow up, HIP 113103 b and HIP 113103 c could provide insight on planetary evolution for the sub-Neptune K-star population.

Original language	English
Article number	stad2756
Journal	Monthly Notices of the Royal Astronomical Society: Letters
Early online date	12 Sept 2023
DOIs	https://doi.org/10.1093/mnras/stad2756
Publication status	E-pub ahead of print - 12 Sept 2023

Bibliographical note

18 pages, 12 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society

Acknowledgements
We would like to acknowledge and pay respect to Australia’s Aboriginal and Torres Strait Islander peoples, who are the traditional custodians of the lands, the waterways and the skies all across Australia. We thank Australia’s Aboriginal and Torres Strait Islander peoples for sharing and caring for the land on which we are able to learn. In particular, we pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Yuggera nations, upon which the Minerva-Australis facility is situated, and analysis for this paper was undertaken. We would also like to acknowledge and pay our deepest respects to the Indigenous Elders, ancestors and descendants who are the traditional custodians of the land upon which the CTIO, SAAO, and ESO 3.6 m are situated. This includes (but may
not be exclusive to) the Diaguita and Khoisan nations. GZ thanks
the support of the ARC DECRA program DE210101893. CXH
thanks the support of the ARC DECRA program DE200101840.
GZ, SQ thank the support of the TESS Guest Investigator Program G03007. CH thanks the support of the ARC DECRA program
DE200101840. KAC acknowledges support from the TESS mission
via subaward s3449 from MIT. This research has used data from
the CTIO/SMARTS 1.5m telescope, which is operated as part of
the SMARTS Consortium by RECONS. This work makes use of
data from the European Space Agency (ESA) mission CHEOPS
via the CHEOPS Guest Observers Program AO-3-10. This work
has made use of data from the European Space Agency (ESA) mission Gaia, processed by the Gaia Data Processing and Analysis
Consortium (DPAC). Funding for the DPAC has been provided by
national institutions, in particular the institutions participating in
the Gaia Multilateral Agreement. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This work makes use of data from the Minerva-Australis facility. Minerva-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40182901 and 51NF40205606. Funding for the TESS mission is provided by NASA’s Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which
is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.

Keywords

astro-ph.EP

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10.1093/mnras/stad2756Licence: Creative Commons: Attribution (CC BY)

LowsonN2023Two_AAMonlineAccepted author manuscript, 1.23 MBLicence: Creative Commons: Attribution (CC BY)

Cite this

Lowson, N., Zhou, G., Huang, C. X., Wright, D. J., Edwards, B., Nabbie, E., Venner, A., Quinn, S. N., Collins, K. A., Gillen, E., Battley, M., Triaud, A., Hellier, C., Seager, S., Winn, J. N., Jenkins, J. M., Wohler, B., Shporer, A., Schwarz, R. P., ... Addison, B. C. (2023). Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS. Monthly Notices of the Royal Astronomical Society: Letters, Article stad2756. Advance online publication. https://doi.org/10.1093/mnras/stad2756

@article{05f8c596404740088840930d68d41c00,

title = "Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS",

abstract = "We report the discovery of two mini-Neptunes in near 2:1 resonance orbits (P = 7.610303 d for HIP 113103 b and P = 14.245651 d for HIP 113103 c ) around the adolescent K-star HIP 113103 (TIC 121490076 ). The planet system was first identified from the TESS mission, and was confirmed via additional photometric and spectroscopic observations, including a ∼17.5 hour observation for the transits of both planets using ESA CHEOPS . We place ≤4.5 min and ≤2.5 min limits on the absence of transit timing variations over the three year photometric baseline, allowing further constraints on the orbital eccentricities of the system beyond that available from the photometric transit duration alone. With a planetary radius of Rp = 1.829+0.096−0.067R⊕, HIP 113103 b resides within the radius gap, and this might provide invaluable information on the formation disparities between super-Earths and mini-Neptunes. Given the larger radius Rp = 2.40+0.10−0.08R⊕ for HIP 113103 c , and close proximity of both planets to HIP 113103 , it is likely that HIP 113103 b might have lost (or is still losing) its primordial atmosphere. We therefore present simulated atmospheric transmission spectra of both planets using JWST , HST , and Twinkle . It demonstrates a potential metallicity difference (due to differences in their evolution) would be a challenge to detect if the atmospheres are in chemical equilibrium. As one of the brightest multi sub-Neptune planet systems suitable for atmosphere follow up, HIP 113103 b and HIP 113103 c could provide insight on planetary evolution for the sub-Neptune K-star population.",

keywords = "astro-ph.EP",

author = "Nataliea Lowson and George Zhou and Huang, {Chelsea X.} and Wright, {Duncan J.} and Billy Edwards and Emma Nabbie and Alex Venner and Quinn, {Samuel N.} and Collins, {Karen A.} and Edward Gillen and Matthew Battley and Amaury Triaud and Coel Hellier and Sara Seager and Winn, {Joshua N.} and Jenkins, {Jon M.} and Bill Wohler and Avi Shporer and Schwarz, {Richard P.} and Felipe Murgas and Enric Pall{\'e} and Anderson, {David R.} and West, {Richard G.} and Wittenmyer, {Robert A.} and Bowler, {Brendan P.} and Jonathan Horner and Kane, {Stephen R.} and John Kielkopf and Peter Plavchan and Hui Zhang and Tyler Fairnington and Jack Okumura and Mengel, {Matthew W.} and Addison, {Brett C.}",

note = "18 pages, 12 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society Acknowledgements We would like to acknowledge and pay respect to Australia{\textquoteright}s Aboriginal and Torres Strait Islander peoples, who are the traditional custodians of the lands, the waterways and the skies all across Australia. We thank Australia{\textquoteright}s Aboriginal and Torres Strait Islander peoples for sharing and caring for the land on which we are able to learn. In particular, we pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Yuggera nations, upon which the Minerva-Australis facility is situated, and analysis for this paper was undertaken. We would also like to acknowledge and pay our deepest respects to the Indigenous Elders, ancestors and descendants who are the traditional custodians of the land upon which the CTIO, SAAO, and ESO 3.6 m are situated. This includes (but may not be exclusive to) the Diaguita and Khoisan nations. GZ thanks the support of the ARC DECRA program DE210101893. CXH thanks the support of the ARC DECRA program DE200101840. GZ, SQ thank the support of the TESS Guest Investigator Program G03007. CH thanks the support of the ARC DECRA program DE200101840. KAC acknowledges support from the TESS mission via subaward s3449 from MIT. This research has used data from the CTIO/SMARTS 1.5m telescope, which is operated as part of the SMARTS Consortium by RECONS. This work makes use of data from the European Space Agency (ESA) mission CHEOPS via the CHEOPS Guest Observers Program AO-3-10. This work has made use of data from the European Space Agency (ESA) mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This work makes use of data from the Minerva-Australis facility. Minerva-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40182901 and 51NF40205606. Funding for the TESS mission is provided by NASA{\textquoteright}s Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.",

year = "2023",

month = sep,

day = "12",

doi = "10.1093/mnras/stad2756",

language = "English",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "1745-3933",

publisher = "Oxford University Press",

}

Lowson, N, Zhou, G, Huang, CX, Wright, DJ, Edwards, B, Nabbie, E, Venner, A, Quinn, SN, Collins, KA, Gillen, E, Battley, M, Triaud, A, Hellier, C, Seager, S, Winn, JN, Jenkins, JM, Wohler, B, Shporer, A, Schwarz, RP, Murgas, F, Pallé, E, Anderson, DR, West, RG, Wittenmyer, RA, Bowler, BP, Horner, J, Kane, SR, Kielkopf, J, Plavchan, P, Zhang, H, Fairnington, T, Okumura, J, Mengel, MW & Addison, BC 2023, 'Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS', Monthly Notices of the Royal Astronomical Society: Letters. https://doi.org/10.1093/mnras/stad2756

TY - JOUR

T1 - Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS

AU - Lowson, Nataliea

AU - Zhou, George

AU - Huang, Chelsea X.

AU - Wright, Duncan J.

AU - Edwards, Billy

AU - Nabbie, Emma

AU - Venner, Alex

AU - Quinn, Samuel N.

AU - Collins, Karen A.

AU - Gillen, Edward

AU - Battley, Matthew

AU - Triaud, Amaury

AU - Hellier, Coel

AU - Seager, Sara

AU - Winn, Joshua N.

AU - Jenkins, Jon M.

AU - Wohler, Bill

AU - Shporer, Avi

AU - Schwarz, Richard P.

AU - Murgas, Felipe

AU - Pallé, Enric

AU - Anderson, David R.

AU - West, Richard G.

AU - Wittenmyer, Robert A.

AU - Bowler, Brendan P.

AU - Horner, Jonathan

AU - Kane, Stephen R.

AU - Kielkopf, John

AU - Plavchan, Peter

AU - Zhang, Hui

AU - Fairnington, Tyler

AU - Okumura, Jack

AU - Mengel, Matthew W.

AU - Addison, Brett C.

N1 - 18 pages, 12 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society Acknowledgements We would like to acknowledge and pay respect to Australia’s Aboriginal and Torres Strait Islander peoples, who are the traditional custodians of the lands, the waterways and the skies all across Australia. We thank Australia’s Aboriginal and Torres Strait Islander peoples for sharing and caring for the land on which we are able to learn. In particular, we pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Yuggera nations, upon which the Minerva-Australis facility is situated, and analysis for this paper was undertaken. We would also like to acknowledge and pay our deepest respects to the Indigenous Elders, ancestors and descendants who are the traditional custodians of the land upon which the CTIO, SAAO, and ESO 3.6 m are situated. This includes (but may not be exclusive to) the Diaguita and Khoisan nations. GZ thanks the support of the ARC DECRA program DE210101893. CXH thanks the support of the ARC DECRA program DE200101840. GZ, SQ thank the support of the TESS Guest Investigator Program G03007. CH thanks the support of the ARC DECRA program DE200101840. KAC acknowledges support from the TESS mission via subaward s3449 from MIT. This research has used data from the CTIO/SMARTS 1.5m telescope, which is operated as part of the SMARTS Consortium by RECONS. This work makes use of data from the European Space Agency (ESA) mission CHEOPS via the CHEOPS Guest Observers Program AO-3-10. This work has made use of data from the European Space Agency (ESA) mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This work makes use of data from the Minerva-Australis facility. Minerva-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40182901 and 51NF40205606. Funding for the TESS mission is provided by NASA’s Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products.

PY - 2023/9/12

Y1 - 2023/9/12

N2 - We report the discovery of two mini-Neptunes in near 2:1 resonance orbits (P = 7.610303 d for HIP 113103 b and P = 14.245651 d for HIP 113103 c ) around the adolescent K-star HIP 113103 (TIC 121490076 ). The planet system was first identified from the TESS mission, and was confirmed via additional photometric and spectroscopic observations, including a ∼17.5 hour observation for the transits of both planets using ESA CHEOPS . We place ≤4.5 min and ≤2.5 min limits on the absence of transit timing variations over the three year photometric baseline, allowing further constraints on the orbital eccentricities of the system beyond that available from the photometric transit duration alone. With a planetary radius of Rp = 1.829+0.096−0.067R⊕, HIP 113103 b resides within the radius gap, and this might provide invaluable information on the formation disparities between super-Earths and mini-Neptunes. Given the larger radius Rp = 2.40+0.10−0.08R⊕ for HIP 113103 c , and close proximity of both planets to HIP 113103 , it is likely that HIP 113103 b might have lost (or is still losing) its primordial atmosphere. We therefore present simulated atmospheric transmission spectra of both planets using JWST , HST , and Twinkle . It demonstrates a potential metallicity difference (due to differences in their evolution) would be a challenge to detect if the atmospheres are in chemical equilibrium. As one of the brightest multi sub-Neptune planet systems suitable for atmosphere follow up, HIP 113103 b and HIP 113103 c could provide insight on planetary evolution for the sub-Neptune K-star population.

AB - We report the discovery of two mini-Neptunes in near 2:1 resonance orbits (P = 7.610303 d for HIP 113103 b and P = 14.245651 d for HIP 113103 c ) around the adolescent K-star HIP 113103 (TIC 121490076 ). The planet system was first identified from the TESS mission, and was confirmed via additional photometric and spectroscopic observations, including a ∼17.5 hour observation for the transits of both planets using ESA CHEOPS . We place ≤4.5 min and ≤2.5 min limits on the absence of transit timing variations over the three year photometric baseline, allowing further constraints on the orbital eccentricities of the system beyond that available from the photometric transit duration alone. With a planetary radius of Rp = 1.829+0.096−0.067R⊕, HIP 113103 b resides within the radius gap, and this might provide invaluable information on the formation disparities between super-Earths and mini-Neptunes. Given the larger radius Rp = 2.40+0.10−0.08R⊕ for HIP 113103 c , and close proximity of both planets to HIP 113103 , it is likely that HIP 113103 b might have lost (or is still losing) its primordial atmosphere. We therefore present simulated atmospheric transmission spectra of both planets using JWST , HST , and Twinkle . It demonstrates a potential metallicity difference (due to differences in their evolution) would be a challenge to detect if the atmospheres are in chemical equilibrium. As one of the brightest multi sub-Neptune planet systems suitable for atmosphere follow up, HIP 113103 b and HIP 113103 c could provide insight on planetary evolution for the sub-Neptune K-star population.

KW - astro-ph.EP

U2 - 10.1093/mnras/stad2756

DO - 10.1093/mnras/stad2756

M3 - Article

SN - 1745-3933

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

M1 - stad2756

ER -

Two mini-Neptunes Transiting the Adolescent K-star HIP 113103 Confirmed with TESS and CHEOPS

Abstract

Bibliographical note

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