TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit

A Alqasim; N Grieves; N M Rosário; D Gandolfi; J H Livingston; S Sousa; K A Collins; J K Teske; M Fridlund; J A Egger; J Cabrera; C Hellier; A F Lanza; V Van Eylen; F Bouchy; R J Oelkers; G Srdoc; S Shectman; M Günther; E Goffo; T Wilson; L M Serrano; A Brandeker; S X Wang; A Heitzmann; A Bonfanti; L Fossati; Y Alibert; L Delrez; R Sefako; S Barros; K I Collins; O D S Demangeon; S H Albrecht; R Alonso; J Asquier; T Barczy; D Barrado; W Baumjohann; T Beck; W Benz; N Billot; L Borsato; C Broeg; E M Bryant; R P Butler; W D Cochran; A Collier Cameron; A C M Correia; J D Crane; Sz Csizmadia; P E Cubillos; M B Davies; T Daylan; M Deleuil; A Deline; B -O Demory; A Derekas; B Edwards; D Ehrenreich; A Erikson; Z Essack; A Fortier; K Gazeas; M Gillon; M Gudel; J Hasiba; A P Hatzes; Ch Helling; T Hirano; S B Howell; S Hoyer; K G Isaak; J M Jenkins; S Kanodia; L L Kiss; J Korth; K W F Lam; J Laskar; A  Lecavelier des Etangs; M Lendl; M B Lund; R Luque; A W Mann; D Magrin; P F L Maxted; C Mordasini; N Narita; V Nascimbeni; G Nowak; G Olofsson; H P Osborn; H L M Osborne; D Osip; R Ottensamer; I Pagano; E Palle; G Peter; G Piotto; D Pollacco; D Queloz; R Ragazzoni; N Rando; H Rauer; S Redfield; I Ribas; M Rice; G R Ricker; M Rieder; S Salmon; N C Santos; G Scandariato; S Seager; D Segransan; A Shporer; A E Simon; A M S Smith; M Stalport; Gy M Szabo; I Thompson; J D Twicken; S Udry; R Vanderspek; V Van Grootel; J Venturini; E Villaver; J Villaseñor; V Viotto; I Walter; N A Walton; J N Winn; S W Yee

doi:10.1093/mnras/stae1767

TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit

A Alqasim^*, N Grieves, N M Rosário, D Gandolfi^*, J H Livingston, S Sousa, K A Collins, J K Teske, M Fridlund, J A Egger, J Cabrera, C Hellier, A F Lanza, V Van Eylen, F Bouchy, R J Oelkers, G Srdoc, S Shectman, M Günther, E GoffoT Wilson, L M Serrano, A Brandeker, S X Wang, A Heitzmann, A Bonfanti, L Fossati, Y Alibert, L Delrez, R Sefako, S Barros, K I Collins, O D S Demangeon, S H Albrecht, R Alonso, J Asquier, T Barczy, D Barrado, W Baumjohann, T Beck, W Benz, N Billot, L Borsato, C Broeg, E M Bryant, R P Butler, W D Cochran, A Collier Cameron, A C M Correia, J D Crane, Sz Csizmadia, P E Cubillos, M B Davies, T Daylan, M Deleuil, A Deline, B -O Demory, A Derekas, B Edwards, D Ehrenreich, A Erikson, Z Essack, A Fortier, K Gazeas, M Gillon, M Gudel, J Hasiba, A P Hatzes, Ch Helling, T Hirano, S B Howell, S Hoyer, K G Isaak, J M Jenkins, S Kanodia, L L Kiss, J Korth, K W F Lam, J Laskar, A Lecavelier des Etangs, M Lendl, M B Lund, R Luque, A W Mann, D Magrin, P F L Maxted, C Mordasini, N Narita, V Nascimbeni, G Nowak, G Olofsson, H P Osborn, H L M Osborne, D Osip, R Ottensamer, I Pagano, E Palle, G Peter, G Piotto, D Pollacco, D Queloz, R Ragazzoni, N Rando, H Rauer, S Redfield, I Ribas, M Rice, G R Ricker, M Rieder, S Salmon, N C Santos, G Scandariato, S Seager, D Segransan, A Shporer, A E Simon, A M S Smith, M Stalport, Gy M Szabo, I Thompson, J D Twicken, S Udry, R Vanderspek, V Van Grootel, J Venturini, E Villaver, J Villaseñor, V Viotto, I Walter, N A Walton, J N Winn, S W Yee

^*Corresponding author for this work

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

Abstract

We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of R_p = 2.5 ± 0.1 R⊕ and a mass of M_p = 10.5^+2.2_-2.1 M⊕, implying a bulk density of ρ_p = 3.6 ± 0.8 g cm^-3. Our internal composition modelling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39^+0.08_-0.07, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b’s formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star$-$star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI-757.

Original language	English
Article number	stae1767
Pages (from-to)	1-26
Number of pages	26
Journal	Monthly Notices of the Royal Astronomical Society
Volume	533
Issue number	1
Early online date	31 Jul 2024
DOIs	https://doi.org/10.1093/mnras/stae1767
Publication status	Published - Sept 2024

Keywords

Techniques: photometric
Techniques: radial velocities
Planets and satellites: composition
Planets and satellites: interiors
Stars: individual: TOI-757 (TIC 130924120)

Access to Document

10.1093/mnras/stae1767Licence: CC BY

H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON
Helling, C. (PI)
European Commission
1/06/20 → 31/05/24
Project: Standard
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

TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit (dataset)
Cameron, A. C. (Creator), VizieR On-line Data Catalog, 2024
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/533/1
Dataset

Cite this

Alqasim, A., Grieves, N., Rosário, N. M., Gandolfi, D., Livingston, J. H., Sousa, S., Collins, K. A., Teske, J. K., Fridlund, M., Egger, J. A., Cabrera, J., Hellier, C., Lanza, A. F., Van Eylen, V., Bouchy, F., Oelkers, R. J., Srdoc, G., Shectman, S., Günther, M., ... Yee, S. W. (2024). TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit. Monthly Notices of the Royal Astronomical Society, 533(1), 1-26. Article stae1767. https://doi.org/10.1093/mnras/stae1767

@article{6712aebd0a1b4bcf83cbbe302d734fce,

title = "TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit",

abstract = "We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of Rp = 2.5 ± 0.1 R⊕ and a mass of Mp = 10.5+2.2-2.1 M⊕, implying a bulk density of ρp = 3.6 ± 0.8 g cm-3. Our internal composition modelling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39+0.08-0.07, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b{\textquoteright}s formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star$-$star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI-757.",

keywords = "Techniques: photometric, Techniques: radial velocities, Planets and satellites: composition, Planets and satellites: interiors, Stars: individual: TOI-757 (TIC 130924120)",

author = "A Alqasim and N Grieves and Ros{\'a}rio, {N M} and D Gandolfi and Livingston, {J H} and S Sousa and Collins, {K A} and Teske, {J K} and M Fridlund and Egger, {J A} and J Cabrera and C Hellier and Lanza, {A F} and V Van Eylen and F Bouchy and Oelkers, {R J} and G Srdoc and S Shectman and M G{\"u}nther and E Goffo and T Wilson and Serrano, {L M} and A Brandeker and Wang, {S X} and A Heitzmann and A Bonfanti and L Fossati and Y Alibert and L Delrez and R Sefako and S Barros and Collins, {K I} and Demangeon, {O D S} and Albrecht, {S H} and R Alonso and J Asquier and T Barczy and D Barrado and W Baumjohann and T Beck and W Benz and N Billot and L Borsato and C Broeg and Bryant, {E M} and Butler, {R P} and Cochran, {W D} and Cameron, {A Collier} and Correia, {A C M} and Crane, {J D} and Sz Csizmadia and Cubillos, {P E} and Davies, {M B} and T Daylan and M Deleuil and A Deline and Demory, {B -O} and A Derekas and B Edwards and D Ehrenreich and A Erikson and Z Essack and A Fortier and K Gazeas and M Gillon and M Gudel and J Hasiba and Hatzes, {A P} and Ch Helling and T Hirano and Howell, {S B} and S Hoyer and Isaak, {K G} and Jenkins, {J M} and S Kanodia and Kiss, {L L} and J Korth and Lam, {K W F} and J Laskar and {Lecavelier des Etangs}, A and M Lendl and Lund, {M B} and R Luque and Mann, {A W} and D Magrin and Maxted, {P F L} and C Mordasini and N Narita and V Nascimbeni and G Nowak and G Olofsson and Osborn, {H P} and Osborne, {H L M} and D Osip and R Ottensamer and I Pagano and E Palle and G Peter and G Piotto and D Pollacco and D Queloz and R Ragazzoni and N Rando and H Rauer and S Redfield and I Ribas and M Rice and Ricker, {G R} and M Rieder and S Salmon and Santos, {N C} and G Scandariato and S Seager and D Segransan and A Shporer and Simon, {A E} and Smith, {A M S} and M Stalport and Szabo, {Gy M} and I Thompson and Twicken, {J D} and S Udry and R Vanderspek and V Van Grootel and J Venturini and E Villaver and J Villase{\~n}or and V Viotto and I Walter and Walton, {N A} and Winn, {J N} and Yee, {S W}",

note = "Funding: ACC acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1. The contributions at the Mullard Space Science Laboratory by EMB have been supported by STFC through the consolidated grant ST/W001136/1. This project has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No 724427)",

year = "2024",

month = sep,

doi = "10.1093/mnras/stae1767",

language = "English",

volume = "533",

pages = "1--26",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

Alqasim, A, Grieves, N, Rosário, NM, Gandolfi, D, Livingston, JH, Sousa, S, Collins, KA, Teske, JK, Fridlund, M, Egger, JA, Cabrera, J, Hellier, C, Lanza, AF, Van Eylen, V, Bouchy, F, Oelkers, RJ, Srdoc, G, Shectman, S, Günther, M, Goffo, E, Wilson, T, Serrano, LM, Brandeker, A, Wang, SX, Heitzmann, A, Bonfanti, A, Fossati, L, Alibert, Y, Delrez, L, Sefako, R, Barros, S, Collins, KI, Demangeon, ODS, Albrecht, SH, Alonso, R, Asquier, J, Barczy, T, Barrado, D, Baumjohann, W, Beck, T, Benz, W, Billot, N, Borsato, L, Broeg, C, Bryant, EM, Butler, RP, Cochran, WD, Cameron, AC, Correia, ACM, Crane, JD, Csizmadia, S, Cubillos, PE, Davies, MB, Daylan, T, Deleuil, M, Deline, A, Demory, B-O, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Essack, Z, Fortier, A, Gazeas, K, Gillon, M, Gudel, M, Hasiba, J, Hatzes, AP, Helling, C, Hirano, T, Howell, SB, Hoyer, S, Isaak, KG, Jenkins, JM, Kanodia, S, Kiss, LL, Korth, J, Lam, KWF, Laskar, J, Lecavelier des Etangs, A, Lendl, M, Lund, MB, Luque, R, Mann, AW, Magrin, D, Maxted, PFL, Mordasini, C, Narita, N, Nascimbeni, V, Nowak, G, Olofsson, G, Osborn, HP, Osborne, HLM, Osip, D, Ottensamer, R, Pagano, I, Palle, E, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Redfield, S, Ribas, I, Rice, M, Ricker, GR, Rieder, M, Salmon, S, Santos, NC, Scandariato, G, Seager, S, Segransan, D, Shporer, A, Simon, AE, Smith, AMS, Stalport, M, Szabo, GM, Thompson, I, Twicken, JD, Udry, S, Vanderspek, R, Van Grootel, V, Venturini, J, Villaver, E, Villaseñor, J, Viotto, V, Walter, I, Walton, NA, Winn, JN & Yee, SW 2024, 'TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit', Monthly Notices of the Royal Astronomical Society, vol. 533, no. 1, stae1767, pp. 1-26. https://doi.org/10.1093/mnras/stae1767

TY - JOUR

T1 - TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit

AU - Alqasim, A

AU - Grieves, N

AU - Rosário, N M

AU - Gandolfi, D

AU - Livingston, J H

AU - Sousa, S

AU - Collins, K A

AU - Teske, J K

AU - Fridlund, M

AU - Egger, J A

AU - Cabrera, J

AU - Hellier, C

AU - Lanza, A F

AU - Van Eylen, V

AU - Bouchy, F

AU - Oelkers, R J

AU - Srdoc, G

AU - Shectman, S

AU - Günther, M

AU - Goffo, E

AU - Wilson, T

AU - Serrano, L M

AU - Brandeker, A

AU - Wang, S X

AU - Heitzmann, A

AU - Bonfanti, A

AU - Fossati, L

AU - Alibert, Y

AU - Delrez, L

AU - Sefako, R

AU - Barros, S

AU - Collins, K I

AU - Demangeon, O D S

AU - Albrecht, S H

AU - Alonso, R

AU - Asquier, J

AU - Barczy, T

AU - Barrado, D

AU - Baumjohann, W

AU - Beck, T

AU - Benz, W

AU - Billot, N

AU - Borsato, L

AU - Broeg, C

AU - Bryant, E M

AU - Butler, R P

AU - Cochran, W D

AU - Cameron, A Collier

AU - Correia, A C M

AU - Crane, J D

AU - Csizmadia, Sz

AU - Cubillos, P E

AU - Davies, M B

AU - Daylan, T

AU - Deleuil, M

AU - Deline, A

AU - Demory, B -O

AU - Derekas, A

AU - Edwards, B

AU - Ehrenreich, D

AU - Erikson, A

AU - Essack, Z

AU - Fortier, A

AU - Gazeas, K

AU - Gillon, M

AU - Gudel, M

AU - Hasiba, J

AU - Hatzes, A P

AU - Helling, Ch

AU - Hirano, T

AU - Howell, S B

AU - Hoyer, S

AU - Isaak, K G

AU - Jenkins, J M

AU - Kanodia, S

AU - Kiss, L L

AU - Korth, J

AU - Lam, K W F

AU - Laskar, J

AU - Lecavelier des Etangs, A

AU - Lendl, M

AU - Lund, M B

AU - Luque, R

AU - Mann, A W

AU - Magrin, D

AU - Maxted, P F L

AU - Mordasini, C

AU - Narita, N

AU - Nascimbeni, V

AU - Nowak, G

AU - Olofsson, G

AU - Osborn, H P

AU - Osborne, H L M

AU - Osip, D

AU - Ottensamer, R

AU - Pagano, I

AU - Palle, E

AU - Peter, G

AU - Piotto, G

AU - Pollacco, D

AU - Queloz, D

AU - Ragazzoni, R

AU - Rando, N

AU - Rauer, H

AU - Redfield, S

AU - Ribas, I

AU - Rice, M

AU - Ricker, G R

AU - Rieder, M

AU - Salmon, S

AU - Santos, N C

AU - Scandariato, G

AU - Seager, S

AU - Segransan, D

AU - Shporer, A

AU - Simon, A E

AU - Smith, A M S

AU - Stalport, M

AU - Szabo, Gy M

AU - Thompson, I

AU - Twicken, J D

AU - Udry, S

AU - Vanderspek, R

AU - Van Grootel, V

AU - Venturini, J

AU - Villaver, E

AU - Villaseñor, J

AU - Viotto, V

AU - Walter, I

AU - Walton, N A

AU - Winn, J N

AU - Yee, S W

N1 - Funding: ACC acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). NAW acknowledges UKSA grant ST/R004838/1. The contributions at the Mullard Space Science Laboratory by EMB have been supported by STFC through the consolidated grant ST/W001136/1. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No 724427)

PY - 2024/9

Y1 - 2024/9

N2 - We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of Rp = 2.5 ± 0.1 R⊕ and a mass of Mp = 10.5+2.2-2.1 M⊕, implying a bulk density of ρp = 3.6 ± 0.8 g cm-3. Our internal composition modelling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39+0.08-0.07, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b’s formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star$-$star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI-757.

AB - We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-d orbit transiting a bright star (V = 9.7 mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of Rp = 2.5 ± 0.1 R⊕ and a mass of Mp = 10.5+2.2-2.1 M⊕, implying a bulk density of ρp = 3.6 ± 0.8 g cm-3. Our internal composition modelling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with e = 0.39+0.08-0.07, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b’s formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star$-$star interactions during the earlier epoch of the Galactic disc formation, given the low metallicity and older age of TOI-757.

KW - Techniques: photometric

KW - Techniques: radial velocities

KW - Planets and satellites: composition

KW - Planets and satellites: interiors

KW - Stars: individual: TOI-757 (TIC 130924120)

U2 - 10.1093/mnras/stae1767

DO - 10.1093/mnras/stae1767

M3 - Article

SN - 0035-8711

VL - 533

SP - 1

EP - 26

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

M1 - stae1767

ER -

TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit

Abstract

Keywords

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Projects

H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON

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

TOI–757 b: an eccentric transiting mini–Neptune on a 17.5–d orbit (dataset)

Cite this