Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

H P Osborn; G Nowak; G Hébrard; T Masseron; J Lillo-Box; E Pallé; A Bekkelien; H-G Florén; P Guterman; A E Simon; V Adibekyan; A Bieryla; L Borsato; A Brandeker; D R Ciardi; A Collier Cameron; K A Collins; J A Egger; D Gandolfi; M J Hooton; D W Latham; M Lendl; E C Matthews; A Tuson; S Ulmer-Moll; A Vanderburg; T G Wilson; C Ziegler; Y Alibert; R Alonso; G Anglada; L Arnold; J Asquier; D Barrado y Navascues; W Baumjohann; T Beck; A A Belinski; W Benz; F Biondi; I Boisse; X Bonfils; C Broeg; L A Buchhave; T Bárczy; S C C Barros; J Cabrera; C Cardona Guillen; I Carleo; A Castro-González; S Charnoz; J Christiansen; P Cortes-Zuleta; S Csizmadia; S Dalal; M B Davies; M Deleuil; X Delfosse; L Delrez; B-O Demory; A B Dunlavey; D Ehrenreich; A Erikson; R B Fernandes; A Fortier; T Forveille; L Fossati; M Fridlund; M Gillon; R F Goeke; M V Goliguzova; E J Gonzales; M N Günther; M Güdel; N Heidari; C E Henze; S Howell; S Hoyer; J I Frey; K G Isaak; J M Jenkins; F Kiefer; L Kiss; J Korth; P F L Maxted; J Laskar; A Lecavelier des Etangs; C Lovis; M B Lund; R Luque; D Magrin; J M Almenara; E Martioli; M Mecina; J V Medina; D Moldovan; M Morales-Calderón; G Morello; C Moutou; F Murgas; E L N Jensen; V Nascimbeni; G Olofsson; R Ottensamer; I Pagano; G Peter; G Piotto; D Pollacco; D Queloz; R Ragazzoni; N Rando; H Rauer; I Ribas; G Ricker; O D S Demangeon; A M S Smith; N Santos; G Scandariato; S Seager; S G Sousa; M Steller; G M Szabó; D Ségransan; N Thomas; S Udry; B Ulmer; V Van Grootel; R Vanderspek; N Walton; J N Winn

doi:10.1093/mnras/stad1319

Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

H P Osborn^*, G Nowak, G Hébrard, T Masseron, J Lillo-Box, E Pallé, A Bekkelien, H-G Florén, P Guterman, A E Simon, V Adibekyan, A Bieryla, L Borsato, A Brandeker, D R Ciardi, A Collier Cameron, K A Collins, J A Egger, D Gandolfi, M J HootonD W Latham, M Lendl, E C Matthews, A Tuson, S Ulmer-Moll, A Vanderburg, T G Wilson, C Ziegler, Y Alibert, R Alonso, G Anglada, L Arnold, J Asquier, D Barrado y Navascues, W Baumjohann, T Beck, A A Belinski, W Benz, F Biondi, I Boisse, X Bonfils, C Broeg, L A Buchhave, T Bárczy, S C C Barros, J Cabrera, C Cardona Guillen, I Carleo, A Castro-González, S Charnoz, J Christiansen, P Cortes-Zuleta, S Csizmadia, S Dalal, M B Davies, M Deleuil, X Delfosse, L Delrez, B-O Demory, A B Dunlavey, D Ehrenreich, A Erikson, R B Fernandes, A Fortier, T Forveille, L Fossati, M Fridlund, M Gillon, R F Goeke, M V Goliguzova, E J Gonzales, M N Günther, M Güdel, N Heidari, C E Henze, S Howell, S Hoyer, J I Frey, K G Isaak, J M Jenkins, F Kiefer, L Kiss, J Korth, P F L Maxted, J Laskar, A Lecavelier des Etangs, C Lovis, M B Lund, R Luque, D Magrin, J M Almenara, E Martioli, M Mecina, J V Medina, D Moldovan, M Morales-Calderón, G Morello, C Moutou, F Murgas, E L N Jensen, V Nascimbeni, G Olofsson, R Ottensamer, I Pagano, G Peter, G Piotto, D Pollacco, D Queloz, R Ragazzoni, N Rando, H Rauer, I Ribas, G Ricker, O D S Demangeon, A M S Smith, N Santos, G Scandariato, S Seager, S G Sousa, M Steller, G M Szabó, D Ségransan, N Thomas, S Udry, B Ulmer, V Van Grootel, R Vanderspek, N Walton, J N Winn

^*Corresponding author for this work

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

Abstract

HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R⊕ (HIP 9618 b) and 3.343 ± 0.039 R⊕ (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M⊕ for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M⊕. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08^+0.12_-0.05 M⊙) orbiting at 26.0^+19.0_-11.0 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (T_eq < 750 K) sub-Neptunes.

Original language	English
Pages (from-to)	3069-3089
Number of pages	21
Journal	Monthly Notices of the Royal Astronomical Society
Volume	523
Issue number	2
Early online date	8 Jun 2023
DOIs	https://doi.org/10.1093/mnras/stad1319
Publication status	Published - 1 Aug 2023

Keywords

Survey
Eclipses
Occultations
Planets and satellites: detection
Binaries: spectroscopic

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10.1093/mnras/stad1319

Osborn_2023_MNRAS_Two-warm-Neptunes_VoR
Copyright © 2023 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. 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 final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stad1319.
Final published version, 8.57 MB

https://arxiv.org/abs/2306.04450

Cite this

Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H.-G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Collier Cameron, A., Collins, K. A., Egger, J. A., Gandolfi, D., ... Winn, J. N. (2023). Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops. Monthly Notices of the Royal Astronomical Society, 523(2), 3069-3089. https://doi.org/10.1093/mnras/stad1319

@article{6a94b756264345eebd002384fe1b0667,

title = "Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops",

abstract = "HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R⊕ (HIP 9618 b) and 3.343 ± 0.039 R⊕ (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M⊕ for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M⊕. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+0.12-0.05 M⊙) orbiting at 26.0+19.0-11.0 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.",

keywords = "Survey, Eclipses, Occultations, Planets and satellites: detection, Binaries: spectroscopic",

author = "Osborn, \{H P\} and G Nowak and G H{\'e}brard and T Masseron and J Lillo-Box and E Pall{\'e} and A Bekkelien and H-G Flor{\'e}n and P Guterman and Simon, \{A E\} and V Adibekyan and A Bieryla and L Borsato and A Brandeker and Ciardi, \{D R\} and A Collier Cameron and Collins, \{K A\} and Egger, \{J A\} and D Gandolfi and Hooton, \{M J\} and Latham, \{D W\} and M Lendl and Matthews, \{E C\} and A Tuson and S Ulmer-Moll and A Vanderburg and Wilson, \{T G\} and C Ziegler and Y Alibert and R Alonso and G Anglada and L Arnold and J Asquier and D Barrado y Navascues and W Baumjohann and T Beck and Belinski, \{A A\} and W Benz and F Biondi and I Boisse and X Bonfils and C Broeg and Buchhave, \{L A\} and T B{\'a}rczy and Barros, \{S C C\} and J Cabrera and C Cardona Guillen and I Carleo and A Castro-Gonz{\'a}lez and S Charnoz and J Christiansen and P Cortes-Zuleta and S Csizmadia and S Dalal and Davies, \{M B\} and M Deleuil and X Delfosse and L Delrez and B-O Demory and Dunlavey, \{A B\} and D Ehrenreich and A Erikson and Fernandes, \{R B\} and A Fortier and T Forveille and L Fossati and M Fridlund and M Gillon and Goeke, \{R F\} and Goliguzova, \{M V\} and Gonzales, \{E J\} and G{\"u}nther, \{M N\} and M G{\"u}del and N Heidari and Henze, \{C E\} and S Howell and S Hoyer and Frey, \{J I\} and Isaak, \{K G\} and Jenkins, \{J M\} and F Kiefer and L Kiss and J Korth and Maxted, \{P F L\} and J Laskar and A Lecavelier des Etangs and C Lovis and Lund, \{M B\} and R Luque and D Magrin and Almenara, \{J M\} and E Martioli and M Mecina and Medina, \{J V\} and D Moldovan and M Morales-Calder{\'o}n and G Morello and C Moutou and F Murgas and Jensen, \{E L N\} and V Nascimbeni and G Olofsson and R Ottensamer and I Pagano and G Peter and G Piotto and D Pollacco and D Queloz and R Ragazzoni and N Rando and H Rauer and I Ribas and G Ricker and Demangeon, \{O D S\} and Smith, \{A M S\} and N Santos and G Scandariato and S Seager and Sousa, \{S G\} and M Steller and Szab{\'o}, \{G M\} and D S{\'e}gransan and N Thomas and S Udry and B Ulmer and V Van Grootel and R Vanderspek and N Walton and Winn, \{J N\}",

note = "Funding: ACC acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.",

year = "2023",

month = aug,

day = "1",

doi = "10.1093/mnras/stad1319",

language = "English",

volume = "523",

pages = "3069--3089",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

}

Osborn, HP, Nowak, G, Hébrard, G, Masseron, T, Lillo-Box, J, Pallé, E, Bekkelien, A, Florén, H-G, Guterman, P, Simon, AE, Adibekyan, V, Bieryla, A, Borsato, L, Brandeker, A, Ciardi, DR, Collier Cameron, A, Collins, KA, Egger, JA, Gandolfi, D, Hooton, MJ, Latham, DW, Lendl, M, Matthews, EC, Tuson, A, Ulmer-Moll, S, Vanderburg, A, Wilson, TG, Ziegler, C, Alibert, Y, Alonso, R, Anglada, G, Arnold, L, Asquier, J, Barrado y Navascues, D, Baumjohann, W, Beck, T, Belinski, AA, Benz, W, Biondi, F, Boisse, I, Bonfils, X, Broeg, C, Buchhave, LA, Bárczy, T, Barros, SCC, Cabrera, J, Cardona Guillen, C, Carleo, I, Castro-González, A, Charnoz, S, Christiansen, J, Cortes-Zuleta, P, Csizmadia, S, Dalal, S, Davies, MB, Deleuil, M, Delfosse, X, Delrez, L, Demory, B-O, Dunlavey, AB, Ehrenreich, D, Erikson, A, Fernandes, RB, Fortier, A, Forveille, T, Fossati, L, Fridlund, M, Gillon, M, Goeke, RF, Goliguzova, MV, Gonzales, EJ, Günther, MN, Güdel, M, Heidari, N, Henze, CE, Howell, S, Hoyer, S, Frey, JI, Isaak, KG, Jenkins, JM, Kiefer, F, Kiss, L, Korth, J, Maxted, PFL, Laskar, J, Lecavelier des Etangs, A, Lovis, C, Lund, MB, Luque, R, Magrin, D, Almenara, JM, Martioli, E, Mecina, M, Medina, JV, Moldovan, D, Morales-Calderón, M, Morello, G, Moutou, C, Murgas, F, Jensen, ELN, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Ricker, G, Demangeon, ODS, Smith, AMS, Santos, N, Scandariato, G, Seager, S, Sousa, SG, Steller, M, Szabó, GM, Ségransan, D, Thomas, N, Udry, S, Ulmer, B, Van Grootel, V, Vanderspek, R, Walton, N & Winn, JN 2023, 'Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops', Monthly Notices of the Royal Astronomical Society, vol. 523, no. 2, pp. 3069-3089. https://doi.org/10.1093/mnras/stad1319

TY - JOUR

T1 - Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

AU - Osborn, H P

AU - Nowak, G

AU - Hébrard, G

AU - Masseron, T

AU - Lillo-Box, J

AU - Pallé, E

AU - Bekkelien, A

AU - Florén, H-G

AU - Guterman, P

AU - Simon, A E

AU - Adibekyan, V

AU - Bieryla, A

AU - Borsato, L

AU - Brandeker, A

AU - Ciardi, D R

AU - Collier Cameron, A

AU - Collins, K A

AU - Egger, J A

AU - Gandolfi, D

AU - Hooton, M J

AU - Latham, D W

AU - Lendl, M

AU - Matthews, E C

AU - Tuson, A

AU - Ulmer-Moll, S

AU - Vanderburg, A

AU - Wilson, T G

AU - Ziegler, C

AU - Alibert, Y

AU - Alonso, R

AU - Anglada, G

AU - Arnold, L

AU - Asquier, J

AU - Barrado y Navascues, D

AU - Baumjohann, W

AU - Beck, T

AU - Belinski, A A

AU - Benz, W

AU - Biondi, F

AU - Boisse, I

AU - Bonfils, X

AU - Broeg, C

AU - Buchhave, L A

AU - Bárczy, T

AU - Barros, S C C

AU - Cabrera, J

AU - Cardona Guillen, C

AU - Carleo, I

AU - Castro-González, A

AU - Charnoz, S

AU - Christiansen, J

AU - Cortes-Zuleta, P

AU - Csizmadia, S

AU - Dalal, S

AU - Davies, M B

AU - Deleuil, M

AU - Delfosse, X

AU - Delrez, L

AU - Demory, B-O

AU - Dunlavey, A B

AU - Ehrenreich, D

AU - Erikson, A

AU - Fernandes, R B

AU - Fortier, A

AU - Forveille, T

AU - Fossati, L

AU - Fridlund, M

AU - Gillon, M

AU - Goeke, R F

AU - Goliguzova, M V

AU - Gonzales, E J

AU - Günther, M N

AU - Güdel, M

AU - Heidari, N

AU - Henze, C E

AU - Howell, S

AU - Hoyer, S

AU - Frey, J I

AU - Isaak, K G

AU - Jenkins, J M

AU - Kiefer, F

AU - Kiss, L

AU - Korth, J

AU - Maxted, P F L

AU - Laskar, J

AU - Lecavelier des Etangs, A

AU - Lovis, C

AU - Lund, M B

AU - Luque, R

AU - Magrin, D

AU - Almenara, J M

AU - Martioli, E

AU - Mecina, M

AU - Medina, J V

AU - Moldovan, D

AU - Morales-Calderón, M

AU - Morello, G

AU - Moutou, C

AU - Murgas, F

AU - Jensen, E L N

AU - Nascimbeni, V

AU - Olofsson, G

AU - Ottensamer, R

AU - Pagano, I

AU - Peter, G

AU - Piotto, G

AU - Pollacco, D

AU - Queloz, D

AU - Ragazzoni, R

AU - Rando, N

AU - Rauer, H

AU - Ribas, I

AU - Ricker, G

AU - Demangeon, O D S

AU - Smith, A M S

AU - Santos, N

AU - Scandariato, G

AU - Seager, S

AU - Sousa, S G

AU - Steller, M

AU - Szabó, G M

AU - Ségransan, D

AU - Thomas, N

AU - Udry, S

AU - Ulmer, B

AU - Van Grootel, V

AU - Vanderspek, R

AU - Walton, N

AU - Winn, J N

N1 - Funding: ACC acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.

PY - 2023/8/1

Y1 - 2023/8/1

N2 - HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R⊕ (HIP 9618 b) and 3.343 ± 0.039 R⊕ (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M⊕ for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M⊕. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+0.12-0.05 M⊙) orbiting at 26.0+19.0-11.0 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.

AB - HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R⊕ (HIP 9618 b) and 3.343 ± 0.039 R⊕ (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M⊕ for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M⊕. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+0.12-0.05 M⊙) orbiting at 26.0+19.0-11.0 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.

KW - Survey

KW - Eclipses

KW - Occultations

KW - Planets and satellites: detection

KW - Binaries: spectroscopic

UR - https://www.scopus.com/pages/publications/85162768259

U2 - 10.1093/mnras/stad1319

DO - 10.1093/mnras/stad1319

M3 - Article

SN - 0035-8711

VL - 523

SP - 3069

EP - 3089

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

Abstract

Keywords

Access to Document

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AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation

HIP 9618 light and radial velocity curves : J/MNRAS/523/3069

Cite this

Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

Abstract

Keywords

Access to Document

Other files and links

Fingerprint

Projects

AO2 - Professor Andrew Cameron: Project AO2 - Andrew Cameron

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021

Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation

Datasets

HIP 9618 light and radial velocity curves : J/MNRAS/523/3069

Cite this