Architecture of TOI-561 planetary system

G Piotto; T Zingales; L Borsato; J A Egger; A C M Correia; A E Simon; H -G Florén; S G Sousa; P F L Maxted; D Nardiello; L Malavolta; T G Wilson; Y Alibert; V Adibekyan; A Bonfanti; R Luque; N C Santos; M J Hooton; L Fossati; A M S Smith; S Salmon; G Lacedelli; R Alonso; T Bárczy; D Barrado Navascues; S C C Barros; W Baumjohann; T Beck; W Benz; N Billot; A Brandeker; C Broeg; M Buder; A Collier Cameron; Sz Csizmadia; P E Cubillos; M B Davies; M Deleuil; A Deline; O D S Demangeon; B -O Demory; A Derekas; B Edwards; D Ehrenreich; A Erikson; A Fortier; M Fridlund; D Gandolfi; K Gazeas; M Gillon; M Güdel; M N Günther; A Heitzmann; Ch Helling; K G Isaak; L L Kiss; J Korth; K W F Lam; J Laskar; A Lecavelier des Etangs; M Lendl; P Leonardi; D Magrin; G Mantovan; C Mordasini; V Nascimbeni; G Olofsson; R Ottensamer; I Pagano; E Pallé; G Peter; R Ottensamer; D Pollacco; D Queloz; R Ragazzoni; N Rando; F Ratti; H Rauer; I Ribas; G Scandariato; D Ségransan; D Sicilia; M Stalport; S Sulis; Gy M Szabó; S Udry; S Ulmer-Moll; V Van Grootel; J Venturini; E Villaver; N A Walton; J N Winn; S Wolf

doi:10.1093/mnras/stae2440

Architecture of TOI-561 planetary system

G Piotto^*, T Zingales, L Borsato, J A Egger, A C M Correia, A E Simon, H -G Florén, S G Sousa, P F L Maxted, D Nardiello, L Malavolta, T G Wilson, Y Alibert, V Adibekyan, A Bonfanti, R Luque, N C Santos, M J Hooton, L Fossati, A M S SmithS Salmon, G Lacedelli, R Alonso, T Bárczy, D Barrado Navascues, S C C Barros, W Baumjohann, T Beck, W Benz, N Billot, A Brandeker, C Broeg, M Buder, A Collier Cameron, Sz Csizmadia, P E Cubillos, M B Davies, M Deleuil, A Deline, O D S Demangeon, B -O Demory, A Derekas, B Edwards, D Ehrenreich, A Erikson, A Fortier, M Fridlund, D Gandolfi, K Gazeas, M Gillon, M Güdel, M N Günther, A Heitzmann, Ch Helling, K G Isaak, L L Kiss, J Korth, K W F Lam, J Laskar, A Lecavelier des Etangs, M Lendl, P Leonardi, D Magrin, G Mantovan, C Mordasini, V Nascimbeni, G Olofsson, R Ottensamer, I Pagano, E Pallé, G Peter, R Ottensamer, D Pollacco, D Queloz, R Ragazzoni, N Rando, F Ratti, H Rauer, I Ribas, G Scandariato, D Ségransan, D Sicilia, M Stalport, S Sulis, Gy M Szabó, S Udry, S Ulmer-Moll, V Van Grootel, J Venturini, E Villaver, N A Walton, J N Winn, S Wolf

^*Corresponding author for this work

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

Abstract

We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561’s orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (R_p = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass (M_p = 12.4 ± 1.4 M⊕) estimates, implying a density of ρ_p = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet’s period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.

Original language	English
Pages (from-to)	2763-2774
Number of pages	12
Journal	Monthly Notices of the Royal Astronomical Society
Volume	535
Issue number	3
Early online date	21 Nov 2024
DOIs	https://doi.org/10.1093/mnras/stae2440
Publication status	Published - Dec 2024

Keywords

Techniques: photometric
Techniques: radial velocities
Ephemerides
Planets and satellites: dynamical evolution and stability
Planets and satellites: fundamental parameters
Planets and satellites: interiors

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10.1093/mnras/stae2440Licence: CC BY

Piotto-2024-Architecture-of-TOI-561-MNRAS-535-3-2763-CCBY
Copyright © 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
Final published version, 3.08 MBLicence: CC BY

https://arxiv.org/abs/2410.18169Licence: CC BY

Cite this

Piotto, G., Zingales, T., Borsato, L., Egger, J. A., Correia, A. C. M., Simon, A. E., Florén, H. .-G., Sousa, S. G., Maxted, P. F. L., Nardiello, D., Malavolta, L., Wilson, T. G., Alibert, Y., Adibekyan, V., Bonfanti, A., Luque, R., Santos, N. C., Hooton, M. J., Fossati, L., ... Wolf, S. (2024). Architecture of TOI-561 planetary system. Monthly Notices of the Royal Astronomical Society, 535(3), 2763-2774. https://doi.org/10.1093/mnras/stae2440

@article{0607665386974eb48ef80576e268b63e,

title = "Architecture of TOI-561 planetary system",

abstract = "We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561{\textquoteright}s orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass (Mp = 12.4 ± 1.4 M⊕) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet{\textquoteright}s period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.",

keywords = "Techniques: photometric, Techniques: radial velocities, Ephemerides, Planets and satellites: dynamical evolution and stability, Planets and satellites: fundamental parameters, Planets and satellites: interiors",

author = "G Piotto and T Zingales and L Borsato and Egger, \{J A\} and Correia, \{A C M\} and Simon, \{A E\} and Flor{\'e}n, \{H -G\} and Sousa, \{S G\} and Maxted, \{P F L\} and D Nardiello and L Malavolta and Wilson, \{T G\} and Y Alibert and V Adibekyan and A Bonfanti and R Luque and Santos, \{N C\} and Hooton, \{M J\} and L Fossati and Smith, \{A M S\} and S Salmon and G Lacedelli and R Alonso and T B{\'a}rczy and D Barrado Navascues and Barros, \{S C C\} and W Baumjohann and T Beck and W Benz and N Billot and A Brandeker and C Broeg and M Buder and Cameron, \{A Collier\} and Sz Csizmadia and Cubillos, \{P E\} and Davies, \{M B\} and M Deleuil and A Deline and Demangeon, \{O D S\} and Demory, \{B -O\} and A Derekas and B Edwards and D Ehrenreich and A Erikson and A Fortier and M Fridlund and D Gandolfi and K Gazeas and M Gillon and M G{\"u}del and G{\"u}nther, \{M N\} and A Heitzmann and Ch Helling and Isaak, \{K G\} and Kiss, \{L L\} and J Korth and Lam, \{K W F\} and J Laskar and A Lecavelier des Etangs and M Lendl and P Leonardi and D Magrin and G Mantovan and C Mordasini and V Nascimbeni and G Olofsson and R Ottensamer and I Pagano and E Pall{\'e} and G Peter and R Ottensamer and D Pollacco and D Queloz and R Ragazzoni and N Rando and F Ratti and H Rauer and I Ribas and G Scandariato and D S{\'e}gransan and D Sicilia and M Stalport and S Sulis and Szab{\'o}, \{Gy M\} and S Udry and S Ulmer-Moll and V Van Grootel and J Venturini and E Villaver and Walton, \{N A\} and Winn, \{J N\} and S Wolf",

note = "Funding: ACC acknowledges support from STFC consolidated grant no. ST/V000861/1, and UKSA grant no. ST/X002217/1. PM acknowledges support from STFC research grant no. ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1.",

year = "2024",

month = dec,

doi = "10.1093/mnras/stae2440",

language = "English",

volume = "535",

pages = "2763--2774",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

Piotto, G, Zingales, T, Borsato, L, Egger, JA, Correia, ACM, Simon, AE, Florén, H-G, Sousa, SG, Maxted, PFL, Nardiello, D, Malavolta, L, Wilson, TG, Alibert, Y, Adibekyan, V, Bonfanti, A, Luque, R, Santos, NC, Hooton, MJ, Fossati, L, Smith, AMS, Salmon, S, Lacedelli, G, Alonso, R, Bárczy, T, Barrado Navascues, D, Barros, SCC, Baumjohann, W, Beck, T, Benz, W, Billot, N, Brandeker, A, Broeg, C, Buder, M, Cameron, AC, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Deline, A, Demangeon, ODS, Demory, B-O, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Fortier, A, Fridlund, M, Gandolfi, D, Gazeas, K, Gillon, M, Güdel, M, Günther, MN, Heitzmann, A, Helling, C, Isaak, KG, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lecavelier des Etangs, A, Lendl, M, Leonardi, P, Magrin, D, Mantovan, G, Mordasini, C, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Peter, G, Ottensamer, R, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Rauer, H, Ribas, I, Scandariato, G, Ségransan, D, Sicilia, D, Stalport, M, Sulis, S, Szabó, GM, Udry, S, Ulmer-Moll, S, Van Grootel, V, Venturini, J, Villaver, E, Walton, NA, Winn, JN & Wolf, S 2024, 'Architecture of TOI-561 planetary system', Monthly Notices of the Royal Astronomical Society, vol. 535, no. 3, pp. 2763-2774. https://doi.org/10.1093/mnras/stae2440

TY - JOUR

T1 - Architecture of TOI-561 planetary system

AU - Piotto, G

AU - Zingales, T

AU - Borsato, L

AU - Egger, J A

AU - Correia, A C M

AU - Simon, A E

AU - Florén, H -G

AU - Sousa, S G

AU - Maxted, P F L

AU - Nardiello, D

AU - Malavolta, L

AU - Wilson, T G

AU - Alibert, Y

AU - Adibekyan, V

AU - Bonfanti, A

AU - Luque, R

AU - Santos, N C

AU - Hooton, M J

AU - Fossati, L

AU - Smith, A M S

AU - Salmon, S

AU - Lacedelli, G

AU - Alonso, R

AU - Bárczy, T

AU - Barrado Navascues, D

AU - Barros, S C C

AU - Baumjohann, W

AU - Beck, T

AU - Benz, W

AU - Billot, N

AU - Brandeker, A

AU - Broeg, C

AU - Buder, M

AU - Cameron, A Collier

AU - Csizmadia, Sz

AU - Cubillos, P E

AU - Davies, M B

AU - Deleuil, M

AU - Deline, A

AU - Demangeon, O D S

AU - Demory, B -O

AU - Derekas, A

AU - Edwards, B

AU - Ehrenreich, D

AU - Erikson, A

AU - Fortier, A

AU - Fridlund, M

AU - Gandolfi, D

AU - Gazeas, K

AU - Gillon, M

AU - Güdel, M

AU - Günther, M N

AU - Heitzmann, A

AU - Helling, Ch

AU - Isaak, K G

AU - Kiss, L L

AU - Korth, J

AU - Lam, K W F

AU - Laskar, J

AU - Lecavelier des Etangs, A

AU - Lendl, M

AU - Leonardi, P

AU - Magrin, D

AU - Mantovan, G

AU - Mordasini, C

AU - Nascimbeni, V

AU - Olofsson, G

AU - Ottensamer, R

AU - Pagano, I

AU - Pallé, E

AU - Peter, G

AU - Ottensamer, R

AU - Pollacco, D

AU - Queloz, D

AU - Ragazzoni, R

AU - Rando, N

AU - Ratti, F

AU - Rauer, H

AU - Ribas, I

AU - Scandariato, G

AU - Ségransan, D

AU - Sicilia, D

AU - Stalport, M

AU - Sulis, S

AU - Szabó, Gy M

AU - Udry, S

AU - Ulmer-Moll, S

AU - Van Grootel, V

AU - Venturini, J

AU - Villaver, E

AU - Walton, N A

AU - Winn, J N

AU - Wolf, S

N1 - Funding: ACC acknowledges support from STFC consolidated grant no. ST/V000861/1, and UKSA grant no. ST/X002217/1. PM acknowledges support from STFC research grant no. ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1.

PY - 2024/12

Y1 - 2024/12

N2 - We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561’s orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass (Mp = 12.4 ± 1.4 M⊕) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet’s period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.

AB - We present new observations from CHEOPS (CHaracterising ExOPlanet Satellite) and TESS (Transiting Exoplanet Survey Satellite) to clarify the architecture of the planetary system hosted by the old Galactic thick disc star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 d (TOI-561 b), 10.8 d (TOI-561 c), 25.7 d (TOI-561 d), and 77.1 d (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 d. The precise characterization of TOI-561’s orbital architecture is interesting since old and metal-poor thick disc stars are less likely to host ultrashort-period super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be 77.14399 ± 0.00025 d, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius (Rp = 2.517 ± 0.045 R⊕ from 5 per cent to 2 per cent precision) and mass (Mp = 12.4 ± 1.4 M⊕) estimates, implying a density of ρp = 0.778 ± 0.097 ρ⊕. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet’s period is finally constrained, allowing us to predict transit times through 2030 with 20-min accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f.

KW - Techniques: photometric

KW - Techniques: radial velocities

KW - Ephemerides

KW - Planets and satellites: dynamical evolution and stability

KW - Planets and satellites: fundamental parameters

KW - Planets and satellites: interiors

UR - https://www.scopus.com/pages/publications/85210285301

U2 - 10.1093/mnras/stae2440

DO - 10.1093/mnras/stae2440

M3 - Article

SN - 0035-8711

VL - 535

SP - 2763

EP - 2774

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Architecture of TOI-561 planetary system

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Keywords

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