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

Physics and Astronomy

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

4 Downloads (Pure)

Abstract

We present the characterization 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^+0.18_-0.16R_⊕, respectively, and orbital periods of 11.62071^+9.6e−05_−0.000106 and 19.502104^+7.4e−05_−8.5e−05 d. 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 characterization.

Original language	English
Pages (from-to)	4632-4644
Number of pages	13
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

Bibliographical note

Publisher Copyright:
© 2024 The Author(s)

Keywords

exoplanets
stars: individual: TIC 349488688, HD 152843

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1093/mnras/stae1821Licence: Creative Commons: Attribution (CC BY)

NicholsonB2024HD152843Final published version, 2.15 MBLicence: Creative Commons: Attribution (CC BY)

Cite this

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 superpuff Neptune. Monthly Notices of the Royal Astronomical Society, 532(4), 4632-4644. https://doi.org/10.1093/mnras/stae1821

@article{9acf7d129cd8439abeb34620c03654ad,

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

abstract = "We present the characterization 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+0.18-0.16 R⊕, respectively, and orbital periods of 11.62071+9.6e−05−0.000106 and 19.502104+7.4e−05−8.5e−05 d. 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 {\textquoteleft}Saturn valley{\textquoteright}, 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 characterization.",

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 = "Publisher Copyright: {\textcopyright} 2024 The Author(s)",

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 = "SIPRI/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 superpuff 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

T2 - the masses and orbital periods of a sub-Neptune and a superpuff 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

PY - 2024/8

Y1 - 2024/8

N2 - We present the characterization 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+0.18-0.16 R⊕, respectively, and orbital periods of 11.62071+9.6e−05−0.000106 and 19.502104+7.4e−05−8.5e−05 d. 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 characterization.

AB - We present the characterization 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+0.18-0.16 R⊕, respectively, and orbital periods of 11.62071+9.6e−05−0.000106 and 19.502104+7.4e−05−8.5e−05 d. 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 characterization.

KW - exoplanets

KW - stars: individual: TIC 349488688, HD 152843

UR - http://www.scopus.com/inward/record.url?scp=85200776988&partnerID=8YFLogxK

U2 - 10.1093/mnras/stae1821

DO - 10.1093/mnras/stae1821

M3 - Article

AN - SCOPUS:85200776988

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 -