HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune

B A Nicholson; S Aigrain; N L Eisner; M Cretignier; O Barragán; L Kaye; J Taylor; J Owen; A Mortier; L Affer; W Boschin; L A Buchhave; A Collier Cameron; M Damasso; L Di Fabrizio; V DiTomasso; X Dumusque; A Ghedina; D W Latham; M López-Morales; V Lorenzi; A F Martínez Fiorenzano; E Molinari; M Pedani; M Pinamonti; K Rice; A Sozzetti

doi:10.1093/mnras/stae1821

HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune

B A Nicholson^*, S Aigrain, N L Eisner, M Cretignier, O Barragán, L Kaye, J Taylor, J Owen, A Mortier, L Affer, W Boschin, L A Buchhave, A Collier Cameron, M Damasso, L Di Fabrizio, V DiTomasso, X Dumusque, A Ghedina, D W Latham, M López-MoralesV Lorenzi, A F Martínez Fiorenzano, E Molinari, M Pedani, M Pinamonti, K Rice, A Sozzetti

^*Corresponding author for this work

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

Abstract

We present the characterisation of the two transiting planets around HD 152843 (TOI 2319, TIC 349488688) using an intensive campaign of HARPS-N radial velocities, and two sectors of TESS data. These data reveal a unique and fascinating system: HD 152843 b and c have near equal masses of around 9 M⊕ but differing radii of 3.05 ± 0.11 R⊕ and 5.94 _-0.16 ^+0.18 R⊕, respectively, and orbital periods of 11.62071_-0.000106^+9.6e-05 days and 19.502104 -_8.5e-05 ^+7.4e-05 days. This indicates that HD 152843 c is in the lowest fifth-percentile in density of the known exoplanet population, and has the longest orbital period among these low density planets. Further, HD 152843 c’s radius places it in the 'Saturn valley', the observed lack of planets larger than Neptune, but smaller than Saturn. The orbital periods of these planets indicate they are near a 5 : 3 mean motion resonance, indicating the possibility of transit timing variations, and hints at the possibility of interaction with a third planet at some point in the evolution of this system. Further, the brightness of the host star and the low density of HD 152843 c make it a key target for atmospheric characterisation.

Original language	English
Pages (from-to)	4632–4644
Journal	Monthly Notices of the Royal Astronomical Society
Volume	532
Issue number	4
Early online date	26 Jul 2024
DOIs	https://doi.org/10.1093/mnras/stae1821
Publication status	Published - Aug 2024

Keywords

Exoplanets
Stars: individual: TIC 349488688, HD 152843

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10.1093/mnras/stae1821Licence: CC BY

Nicholson-2024-HD152843b&c-MNRAS-532-4-4632-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 (https://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, 2.15 MBLicence: CC BY

PLATO 22-25: Support for the PLATO Development Phase 2022-2025: Planet candidate ranking and validation
Cameron, A. C. (PI)
Science & Technology Facilities Council
1/04/22 → 31/03/25
Project: Standard

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Nicholson, B. A., Aigrain, S., Eisner, N. L., Cretignier, M., Barragán, O., Kaye, L., Taylor, J., Owen, J., Mortier, A., Affer, L., Boschin, W., Buchhave, L. A., Cameron, A. C., Damasso, M., Fabrizio, L. D., DiTomasso, V., Dumusque, X., Ghedina, A., Latham, D. W., ... Sozzetti, A. (2024). HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune. Monthly Notices of the Royal Astronomical Society, 532(4), 4632–4644. https://doi.org/10.1093/mnras/stae1821

@article{7f755297383a4212be5ef49bc5b28436,

title = "HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune",

abstract = "We present the characterisation of the two transiting planets around HD 152843 (TOI 2319, TIC 349488688) using an intensive campaign of HARPS-N radial velocities, and two sectors of TESS data. These data reveal a unique and fascinating system: HD 152843 b and c have near equal masses of around 9 M⊕ but differing radii of 3.05 ± 0.11 R⊕ and 5.94 -0.16 +0.18 R⊕, respectively, and orbital periods of 11.62071-0.000106+9.6e-05 days and 19.502104 -8.5e-05 +7.4e-05 days. This indicates that HD 152843 c is in the lowest fifth-percentile in density of the known exoplanet population, and has the longest orbital period among these low density planets. Further, HD 152843 c{\textquoteright}s radius places it in the 'Saturn valley', the observed lack of planets larger than Neptune, but smaller than Saturn. The orbital periods of these planets indicate they are near a 5 : 3 mean motion resonance, indicating the possibility of transit timing variations, and hints at the possibility of interaction with a third planet at some point in the evolution of this system. Further, the brightness of the host star and the low density of HD 152843 c make it a key target for atmospheric characterisation.",

keywords = "Exoplanets, Stars: individual: TIC 349488688, HD 152843",

author = "Nicholson, {B A} and S Aigrain and Eisner, {N L} and M Cretignier and O Barrag{\'a}n and L Kaye and J Taylor and J Owen and A Mortier and L Affer and W Boschin and Buchhave, {L A} and Cameron, {A Collier} and M Damasso and Fabrizio, {L Di} and V DiTomasso and X Dumusque and A Ghedina and Latham, {D W} and M L{\'o}pez-Morales and V Lorenzi and Fiorenzano, {A F Mart{\'i}nez} and E Molinari and M Pedani and M Pinamonti and K Rice and A Sozzetti",

note = "Funding: BN would like to acknowledge support from STFC Consolidated Grant ST/S000488/1 (PI Balbus), and the University of Southern Queensland SAGE program. BN would also like to thank Dr Su Wang for her insights on planetary system dynamics. ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), the University of St Andrews, Queen{\textquoteright}s University Belfast, and the University of Edinburgh.",

year = "2024",

month = aug,

doi = "10.1093/mnras/stae1821",

language = "English",

volume = "532",

pages = "4632–4644",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

Nicholson, BA, Aigrain, S, Eisner, NL, Cretignier, M, Barragán, O, Kaye, L, Taylor, J, Owen, J, Mortier, A, Affer, L, Boschin, W, Buchhave, LA, Cameron, AC, Damasso, M, Fabrizio, LD, DiTomasso, V, Dumusque, X, Ghedina, A, Latham, DW, López-Morales, M, Lorenzi, V, Fiorenzano, AFM, Molinari, E, Pedani, M, Pinamonti, M, Rice, K & Sozzetti, A 2024, 'HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune', Monthly Notices of the Royal Astronomical Society, vol. 532, no. 4, pp. 4632–4644. https://doi.org/10.1093/mnras/stae1821

TY - JOUR

T1 - HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune

AU - Nicholson, B A

AU - Aigrain, S

AU - Eisner, N L

AU - Cretignier, M

AU - Barragán, O

AU - Kaye, L

AU - Taylor, J

AU - Owen, J

AU - Mortier, A

AU - Affer, L

AU - Boschin, W

AU - Buchhave, L A

AU - Cameron, A Collier

AU - Damasso, M

AU - Fabrizio, L Di

AU - DiTomasso, V

AU - Dumusque, X

AU - Ghedina, A

AU - Latham, D W

AU - López-Morales, M

AU - Lorenzi, V

AU - Fiorenzano, A F Martínez

AU - Molinari, E

AU - Pedani, M

AU - Pinamonti, M

AU - Rice, K

AU - Sozzetti, A

N1 - Funding: BN would like to acknowledge support from STFC Consolidated Grant ST/S000488/1 (PI Balbus), and the University of Southern Queensland SAGE program. BN would also like to thank Dr Su Wang for her insights on planetary system dynamics. ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), and the Italian National Astrophysical Institute (INAF), the University of St Andrews, Queen’s University Belfast, and the University of Edinburgh.

PY - 2024/8

Y1 - 2024/8

N2 - We present the characterisation of the two transiting planets around HD 152843 (TOI 2319, TIC 349488688) using an intensive campaign of HARPS-N radial velocities, and two sectors of TESS data. These data reveal a unique and fascinating system: HD 152843 b and c have near equal masses of around 9 M⊕ but differing radii of 3.05 ± 0.11 R⊕ and 5.94 -0.16 +0.18 R⊕, respectively, and orbital periods of 11.62071-0.000106+9.6e-05 days and 19.502104 -8.5e-05 +7.4e-05 days. This indicates that HD 152843 c is in the lowest fifth-percentile in density of the known exoplanet population, and has the longest orbital period among these low density planets. Further, HD 152843 c’s radius places it in the 'Saturn valley', the observed lack of planets larger than Neptune, but smaller than Saturn. The orbital periods of these planets indicate they are near a 5 : 3 mean motion resonance, indicating the possibility of transit timing variations, and hints at the possibility of interaction with a third planet at some point in the evolution of this system. Further, the brightness of the host star and the low density of HD 152843 c make it a key target for atmospheric characterisation.

AB - We present the characterisation of the two transiting planets around HD 152843 (TOI 2319, TIC 349488688) using an intensive campaign of HARPS-N radial velocities, and two sectors of TESS data. These data reveal a unique and fascinating system: HD 152843 b and c have near equal masses of around 9 M⊕ but differing radii of 3.05 ± 0.11 R⊕ and 5.94 -0.16 +0.18 R⊕, respectively, and orbital periods of 11.62071-0.000106+9.6e-05 days and 19.502104 -8.5e-05 +7.4e-05 days. This indicates that HD 152843 c is in the lowest fifth-percentile in density of the known exoplanet population, and has the longest orbital period among these low density planets. Further, HD 152843 c’s radius places it in the 'Saturn valley', the observed lack of planets larger than Neptune, but smaller than Saturn. The orbital periods of these planets indicate they are near a 5 : 3 mean motion resonance, indicating the possibility of transit timing variations, and hints at the possibility of interaction with a third planet at some point in the evolution of this system. Further, the brightness of the host star and the low density of HD 152843 c make it a key target for atmospheric characterisation.

KW - Exoplanets

KW - Stars: individual: TIC 349488688, HD 152843

U2 - 10.1093/mnras/stae1821

DO - 10.1093/mnras/stae1821

M3 - Article

SN - 0035-8711

VL - 532

SP - 4632

EP - 4644

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

HD152843 b & c: the masses and orbital periods of a sub-Neptune and a super-puff Neptune

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Keywords

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Projects

PLATO 22-25: Support for the PLATO Development Phase 2022-2025: Planet candidate ranking and validation

Cite this