Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

G Lacedelli; T G Wilson; L Malavolta; M J Hooton; A Collier Cameron; Y Alibert; A Mortier; A Bonfanti; R D Haywood; S Hoyer; G Piotto; A Bekkelien; A M Vanderburg; W Benz; X Dumusque; A Deline; M López-Morales; L Borsato; K Rice; L Fossati; D W Latham; A Brandeker; E Poretti; S G Sousa; A Sozzetti; S Salmon; C J Burke; V Van Grootel; M M Fausnaugh; V Adibekyan; C X Huang; H P Osborn; A J Mustill; E Pallé; V Bourrier; V Nascimbeni; R Alonso; G Anglada; T Bárczy; D Barrado y Navascues; S C C Barros; W Baumjohann; M Beck; T Beck; N Billot; X Bonfils; C Broeg; L A Buchhave; J Cabrera; S Charnoz; R Cosentino; Sz Csizmadia; M B Davies; M Deleuil; L Delrez; O Demangeon; B-O Demory; D Ehrenreich; A Erikson; E Esparza-Borges; H-G Florén; A Fortier; M Fridlund; D Futyan; D Gandolfi; A Ghedina; M Gillon; M Güdel; P Gutermann; A Harutyunyan; K Heng; K G Isaak; J M Jenkins; L Kiss; J Laskar; A Lecavelier des Etangs; M Lendl; C Lovis; D Magrin; L Marafatto; A F Martinez Fiorenzano; P F L Maxted; M Mayor; G Micela; E Molinari; F Murgas; N Narita; G Olofsson; R Ottensamer; I Pagano; A Pasetti; M Pedani; F A Pepe; G Peter; D F Phillips; D Pollacco; D Queloz; R Ragazzoni; N Rando; F Ratti; H Rauer; I Ribas; N C Santos; D Sasselov; G Scandariato; S Seager; D Ségransan; L M Serrano; A E Simon; A M S Smith; M Steinberger; M Steller; Gy Szabó; N Thomas; J D Twicken; S Udry; N Walton; J N Winn

doi:10.1093/mnras/stac199

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

G Lacedelli
, T G Wilson
, L Malavolta
, M J Hooton
, A Collier Cameron
, Y Alibert
, A Mortier
, A Bonfanti
, R D Haywood
, S Hoyer
, G Piotto
, A Bekkelien
, A M Vanderburg
, W Benz
, X Dumusque
, A Deline
, M López-Morales
, L Borsato
, K Rice
, L Fossati

D W Latham, A Brandeker, E Poretti, S G Sousa, A Sozzetti, S Salmon, C J Burke, V Van Grootel, M M Fausnaugh, V Adibekyan, C X Huang, H P Osborn, A J Mustill, E Pallé, V Bourrier, V Nascimbeni, R Alonso, G Anglada, T Bárczy, D Barrado y Navascues, S C C Barros, W Baumjohann, M Beck, T Beck, N Billot, X Bonfils, C Broeg, L A Buchhave, J Cabrera, S Charnoz, R Cosentino, Sz Csizmadia, M B Davies, M Deleuil, L Delrez, O Demangeon, B-O Demory, D Ehrenreich, A Erikson, E Esparza-Borges, H-G Florén, A Fortier, M Fridlund, D Futyan, D Gandolfi, A Ghedina, M Gillon, M Güdel, P Gutermann, A Harutyunyan, K Heng, K G Isaak, J M Jenkins, L Kiss, J Laskar, A Lecavelier des Etangs, M Lendl, C Lovis, D Magrin, L Marafatto, A F Martinez Fiorenzano, P F L Maxted, M Mayor, G Micela, E Molinari, F Murgas, N Narita, G Olofsson, R Ottensamer, I Pagano, A Pasetti, M Pedani, F A Pepe, G Peter, D F Phillips, D Pollacco, D Queloz, R Ragazzoni, N Rando, F Ratti, H Rauer, I Ribas, N C Santos, D Sasselov, G Scandariato, S Seager, D Ségransan, L M Serrano, A E Simon, A M S Smith, M Steinberger, M Steller, Gy Szabó, N Thomas, J D Twicken, S Udry, N Walton, J N Winn

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Abstract

We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (P = 0.45 d, R = 1.42 R_⊕, M = 2.0 M_⊕), c (P = 10.78 d, R = 2.91 R_⊕, M = 5.4 M_⊕), d (P = 25.7 d, R = 2.82 R_⊕, M = 13.2 M_⊕) and e (P = 77 d, R = 2.55 R_⊕, M = 12.6 R_⊕). Moreover, we identify an additional, long-period signal (>450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (ρ_b = 3.8 ± 0.5 g cm⁻³) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies

Original language	English
Journal	Monthly Notices of the Royal Astronomical Society
Volume	511
Issue number	3
Pages (from-to)	4551–4571
Number of pages	21
ISSN	0035-8711
DOIs	https://doi.org/10.1093/mnras/stac199
Publication status	Published - 2022

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Lacedelli, G., Wilson, T. G., Malavolta, L., Hooton, M. J., Cameron, A. C., Alibert, Y., Mortier, A., Bonfanti, A., Haywood, R. D., Hoyer, S., Piotto, G., Bekkelien, A., Vanderburg, A. M., Benz, W., Dumusque, X., Deline, A., López-Morales, M., Borsato, L., Rice, K., ... Winn, J. N. (2022). Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS. Monthly Notices of the Royal Astronomical Society, 511(3), 4551–4571. https://doi.org/10.1093/mnras/stac199

@article{a8eb27096af7419fa52a4a6608584af3,

title = "Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS",

abstract = "We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (P = 0.45 d, R = 1.42 R⊕, M = 2.0 M⊕), c (P = 10.78 d, R = 2.91 R⊕, M = 5.4 M⊕), d (P = 25.7 d, R = 2.82 R⊕, M = 13.2 M⊕) and e (P = 77 d, R = 2.55 R⊕, M = 12.6 R⊕). Moreover, we identify an additional, long-period signal (>450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 g cm−3) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies",

author = "G Lacedelli and Wilson, \{T G\} and L Malavolta and Hooton, \{M J\} and Cameron, \{A Collier\} and Y Alibert and A Mortier and A Bonfanti and Haywood, \{R D\} and S Hoyer and G Piotto and A Bekkelien and Vanderburg, \{A M\} and W Benz and X Dumusque and A Deline and M L{\'o}pez-Morales and L Borsato and K Rice and L Fossati and Latham, \{D W\} and A Brandeker and E Poretti and Sousa, \{S G\} and A Sozzetti and S Salmon and Burke, \{C J\} and \{Van Grootel\}, V and Fausnaugh, \{M M\} and V Adibekyan and Huang, \{C X\} and Osborn, \{H P\} and Mustill, \{A J\} and E Pall{\'e} and V Bourrier and V Nascimbeni and R Alonso and G Anglada and T B{\'a}rczy and Navascues, \{D Barrado y\} and Barros, \{S C C\} and W Baumjohann and M Beck and T Beck and N Billot and X Bonfils and C Broeg and Buchhave, \{L A\} and J Cabrera and S Charnoz and R Cosentino and Sz Csizmadia and Davies, \{M B\} and M Deleuil and L Delrez and O Demangeon and B-O Demory and D Ehrenreich and A Erikson and E Esparza-Borges and H-G Flor{\'e}n and A Fortier and M Fridlund and D Futyan and D Gandolfi and A Ghedina and M Gillon and M G{\"u}del and P Gutermann and A Harutyunyan and K Heng and Isaak, \{K G\} and Jenkins, \{J M\} and L Kiss and J Laskar and Etangs, \{A Lecavelier des\} and M Lendl and C Lovis and D Magrin and L Marafatto and Fiorenzano, \{A F Martinez\} and Maxted, \{P F L\} and M Mayor and G Micela and E Molinari and F Murgas and N Narita and G Olofsson and R Ottensamer and I Pagano and A Pasetti and M Pedani and Pepe, \{F A\} and G Peter and Phillips, \{D F\} and D Pollacco and D Queloz and R Ragazzoni and N Rando and F Ratti and H Rauer and I Ribas and Santos, \{N C\} and D Sasselov and G Scandariato and S Seager and D S{\'e}gransan and Serrano, \{L M\} and Simon, \{A E\} and Smith, \{A M S\} and M Steinberger and M Steller and Gy Szab{\'o} and N Thomas and Twicken, \{J D\} and S Udry and N Walton and Winn, \{J N\}",

year = "2022",

doi = "10.1093/mnras/stac199",

language = "English",

volume = "511",

pages = "4551–4571",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Lacedelli, G, Wilson, TG, Malavolta, L, Hooton, MJ, Cameron, AC, Alibert, Y, Mortier, A, Bonfanti, A, Haywood, RD, Hoyer, S, Piotto, G, Bekkelien, A, Vanderburg, AM, Benz, W, Dumusque, X, Deline, A, López-Morales, M, Borsato, L, Rice, K, Fossati, L, Latham, DW, Brandeker, A, Poretti, E, Sousa, SG, Sozzetti, A, Salmon, S, Burke, CJ, Van Grootel, V, Fausnaugh, MM, Adibekyan, V, Huang, CX, Osborn, HP, Mustill, AJ, Pallé, E, Bourrier, V, Nascimbeni, V, Alonso, R, Anglada, G, Bárczy, T, Navascues, DBY, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Billot, N, Bonfils, X, Broeg, C, Buchhave, LA, Cabrera, J, Charnoz, S, Cosentino, R, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demangeon, O, Demory, B-O, Ehrenreich, D, Erikson, A, Esparza-Borges, E, Florén, H-G, Fortier, A, Fridlund, M, Futyan, D, Gandolfi, D, Ghedina, A, Gillon, M, Güdel, M, Gutermann, P, Harutyunyan, A, Heng, K, Isaak, KG, Jenkins, JM, Kiss, L, Laskar, J, Etangs, ALD, Lendl, M, Lovis, C, Magrin, D, Marafatto, L, Fiorenzano, AFM, Maxted, PFL, Mayor, M, Micela, G, Molinari, E, Murgas, F, Narita, N, Olofsson, G, Ottensamer, R, Pagano, I, Pasetti, A, Pedani, M, Pepe, FA, Peter, G, Phillips, DF, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Santos, NC, Sasselov, D, Scandariato, G, Seager, S, Ségransan, D, Serrano, LM, Simon, AE, Smith, AMS, Steinberger, M, Steller, M, Szabó, G, Thomas, N, Twicken, JD, Udry, S, Walton, N & Winn, JN 2022, 'Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS', Monthly Notices of the Royal Astronomical Society, vol. 511, no. 3, pp. 4551–4571. https://doi.org/10.1093/mnras/stac199

TY - JOUR

T1 - Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

AU - Lacedelli, G

AU - Wilson, T G

AU - Malavolta, L

AU - Hooton, M J

AU - Cameron, A Collier

AU - Alibert, Y

AU - Mortier, A

AU - Bonfanti, A

AU - Haywood, R D

AU - Hoyer, S

AU - Piotto, G

AU - Bekkelien, A

AU - Vanderburg, A M

AU - Benz, W

AU - Dumusque, X

AU - Deline, A

AU - López-Morales, M

AU - Borsato, L

AU - Rice, K

AU - Fossati, L

AU - Latham, D W

AU - Brandeker, A

AU - Poretti, E

AU - Sousa, S G

AU - Sozzetti, A

AU - Salmon, S

AU - Burke, C J

AU - Van Grootel, V

AU - Fausnaugh, M M

AU - Adibekyan, V

AU - Huang, C X

AU - Osborn, H P

AU - Mustill, A J

AU - Pallé, E

AU - Bourrier, V

AU - Nascimbeni, V

AU - Alonso, R

AU - Anglada, G

AU - Bárczy, T

AU - Navascues, D Barrado y

AU - Barros, S C C

AU - Baumjohann, W

AU - Beck, M

AU - Beck, T

AU - Billot, N

AU - Bonfils, X

AU - Broeg, C

AU - Buchhave, L A

AU - Cabrera, J

AU - Charnoz, S

AU - Cosentino, R

AU - Csizmadia, Sz

AU - Davies, M B

AU - Deleuil, M

AU - Delrez, L

AU - Demangeon, O

AU - Demory, B-O

AU - Ehrenreich, D

AU - Erikson, A

AU - Esparza-Borges, E

AU - Florén, H-G

AU - Fortier, A

AU - Fridlund, M

AU - Futyan, D

AU - Gandolfi, D

AU - Ghedina, A

AU - Gillon, M

AU - Güdel, M

AU - Gutermann, P

AU - Harutyunyan, A

AU - Heng, K

AU - Isaak, K G

AU - Jenkins, J M

AU - Kiss, L

AU - Laskar, J

AU - Etangs, A Lecavelier des

AU - Lendl, M

AU - Lovis, C

AU - Magrin, D

AU - Marafatto, L

AU - Fiorenzano, A F Martinez

AU - Maxted, P F L

AU - Mayor, M

AU - Micela, G

AU - Molinari, E

AU - Murgas, F

AU - Narita, N

AU - Olofsson, G

AU - Ottensamer, R

AU - Pagano, I

AU - Pasetti, A

AU - Pedani, M

AU - Pepe, F A

AU - Peter, G

AU - Phillips, D F

AU - Pollacco, D

AU - Queloz, D

AU - Ragazzoni, R

AU - Rando, N

AU - Ratti, F

AU - Rauer, H

AU - Ribas, I

AU - Santos, N C

AU - Sasselov, D

AU - Scandariato, G

AU - Seager, S

AU - Ségransan, D

AU - Serrano, L M

AU - Simon, A E

AU - Smith, A M S

AU - Steinberger, M

AU - Steller, M

AU - Szabó, Gy

AU - Thomas, N

AU - Twicken, J D

AU - Udry, S

AU - Walton, N

AU - Winn, J N

PY - 2022

Y1 - 2022

N2 - We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (P = 0.45 d, R = 1.42 R⊕, M = 2.0 M⊕), c (P = 10.78 d, R = 2.91 R⊕, M = 5.4 M⊕), d (P = 25.7 d, R = 2.82 R⊕, M = 13.2 M⊕) and e (P = 77 d, R = 2.55 R⊕, M = 12.6 R⊕). Moreover, we identify an additional, long-period signal (>450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 g cm−3) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies

AB - We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of 62 HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b (P = 0.45 d, R = 1.42 R⊕, M = 2.0 M⊕), c (P = 10.78 d, R = 2.91 R⊕, M = 5.4 M⊕), d (P = 25.7 d, R = 2.82 R⊕, M = 13.2 M⊕) and e (P = 77 d, R = 2.55 R⊕, M = 12.6 R⊕). Moreover, we identify an additional, long-period signal (>450 d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 g cm−3) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies

U2 - 10.1093/mnras/stac199

DO - 10.1093/mnras/stac199

M3 - Journal article

SN - 0035-8711

VL - 511

SP - 4551

EP - 4571

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N and TESS

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