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 FossatiD 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

^*Corresponding author for this work

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

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 theRVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planetsallowed us to conduct interior structure and atmospheric escape modelling. TOI-561b is confirmed to be the lowest density (ρ_b = 3.8 ± 0.5 gcm⁻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 band c having experienced significant gas loss, and planets d and e showing anatmospheric 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
Pages (from-to)	4551-4571
Number of pages	21
Journal	Monthly Notices of the Royal Astronomical Society
Volume	511
Issue number	3
Early online date	28 Jan 2022
DOIs	https://doi.org/10.1093/mnras/stac199
Publication status	Published - 1 Apr 2022

Keywords

Planets and satellites: interiors
Stars: individual: TOI-561 (TIC 377064495
Gaia EDR3 3850421005290172416)
Techniques: photometric
Techniques: radial velocities
Planets and satellites: fundamental parameters

Access to Document

10.1093/mnras/stac199

Lacedelli_2022_MNRAS_architecture-internal-structure-TOI-561_AAM
Copyright © 2022 The Author(s) Published by Oxford University Press on behalf of the 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 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/10.1093/mnras/stac199.
Accepted author manuscript, 8.42 MB

Astronomy at St Andrews 2018-2021: Astronomy at St Andrews 2018-2021
Jardine, M. M. (PI), Bonnell, I. A. (CoI), Cameron, A. C. (CoI), Cyganowski, C. J. (CoI), Dominik, M. (CoI), Helling, C. (CoI), Horne, K. D. (CoI), Scholz, A. (CoI), Tojeiro, R. (CoI), Weijmans, A.-M. (CoI), Wild, V. (CoI), Woitke, P. (CoI), Wood, K. (CoI) & Zhao, H. (CoI)
1/04/18 → 31/03/22
Project: Standard
Support for the PLATO Development: Support for the PLATO Development Phase 2017-2022: Planet candidate ranking and validation
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/08/17 → 31/12/22
Project: Standard

Cite this

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{17eb646bd6844b038e88633efe908c58,

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 theRVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planetsallowed us to conduct interior structure and atmospheric escape modelling. TOI-561b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 gcm−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 band c having experienced significant gas loss, and planets d and e showing anatmospheric 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.",

keywords = "Planets and satellites: interiors, Stars: individual: TOI-561 (TIC 377064495, Gaia EDR3 3850421005290172416), Techniques: photometric, Techniques: radial velocities, Planets and satellites: fundamental parameters",

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 {Lecavelier des Etangs}, A and M Lendl and C Lovis and D Magrin and L Marafatto and {Martinez Fiorenzano}, {A F} 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}",

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

year = "2022",

month = apr,

day = "1",

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, Lecavelier des Etangs, A, Lendl, M, Lovis, C, Magrin, D, Marafatto, L, Martinez Fiorenzano, AF, 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 - Lecavelier des Etangs, A

AU - Lendl, M

AU - Lovis, C

AU - Magrin, D

AU - Marafatto, L

AU - Martinez Fiorenzano, A F

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

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

PY - 2022/4/1

Y1 - 2022/4/1

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 theRVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planetsallowed us to conduct interior structure and atmospheric escape modelling. TOI-561b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 gcm−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 band c having experienced significant gas loss, and planets d and e showing anatmospheric 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 theRVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planetsallowed us to conduct interior structure and atmospheric escape modelling. TOI-561b is confirmed to be the lowest density (ρb = 3.8 ± 0.5 gcm−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 band c having experienced significant gas loss, and planets d and e showing anatmospheric 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.

KW - Planets and satellites: interiors

KW - Stars: individual: TOI-561 (TIC 377064495

KW - Gaia EDR3 3850421005290172416)

KW - Techniques: photometric

KW - Techniques: radial velocities

KW - Planets and satellites: fundamental parameters

U2 - 10.1093/mnras/stac199

DO - 10.1093/mnras/stac199

M3 - 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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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

Cite this