Giant Outer Transiting Exoplanet Mass (GOTa EM) survey: VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations

N. Heidari; A. Alnajjarine; H. P. Osborn; D. Dragomir; P. Dalba; W. Benz; G. Hébrard; J. Laskar; N. Billot; M. N. Günther; T. G. Wilson; Y. Alibert; A. Bonfanti; A. Bieryla; C. Broeg; A. C.M. Correia; J. A. Egger; Z. Essack; E. Furlan; D. Gandolfi; N. Grieves; S. Howell; D. Lacourse; C. Pezzotti; T. Pritchard; S. G. Sousa; S. Ulmer-Moll; S. Villanueva; R. Alonso; J. Asquier; T. Bárczy; D. Barrado; S. C.C. Barros; W. Baumjohann; L. Borsato; A. Brandeker; M. Buder; A. Collier Cameron; S. Csizmadia; P. E. Cubillos; M. B. Davies; M. Deleuil; X. Delfosse; A. Deline; O. D.S. Demangeon; B. Demory; A. Derekas; B. Edwards; D. Ehrenreich; A. Erikson; A. Fortier; L. Fossati; M. Fridlund; K. Gazeas; M. Gillon; M. Güdel; J. Hasiba; A. Heitzmann; C. Helling; J. M. Jenkins; T. Keller; S. R. Kane; K. G. Stassun; L. L. Kiss; J. Korth; K. W.F. Lam; D. W. Latham; A. Lecavelier Des Etangs; A. Leleu; M. Lendl; P. F.L. Maxted; S. Mcdermott; B. Merín; C. Mordasini; V. Nascimbeni; G. Nowak; G. Olofsson; I. Pagano; E. Pallé; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; H. Rauer; I. Ribas; G. Ricker; N. C. Santos; G. Scandariato; S. Seager; D. Ségransan; A. E. Simon; A. M.S. Smith; M. Stalport; S. Striegel; S. Sulis; G. M. Szabó; S. Udry; V. Van Grootel; R. Vanderspek; J. Venturini; E. Villaver; V. Viotto; N. A. Walton; J. N. Winn; S. Wolf

doi:10.1051/0004-6361/202556700

Giant Outer Transiting Exoplanet Mass (GOTa EM) survey: VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations

N. Heidari
, A. Alnajjarine
, H. P. Osborn
, D. Dragomir
, P. Dalba
, W. Benz
, G. Hébrard
, J. Laskar
, N. Billot
, M. N. Günther
, T. G. Wilson
, Y. Alibert
, A. Bonfanti
, A. Bieryla
, C. Broeg
, A. C.M. Correia
, J. A. Egger
, Z. Essack
, E. Furlan
, D. Gandolfi

N. Grieves, S. Howell, D. Lacourse, C. Pezzotti, T. Pritchard, S. G. Sousa, S. Ulmer-Moll, S. Villanueva, R. Alonso, J. Asquier, T. Bárczy, D. Barrado, S. C.C. Barros, W. Baumjohann, L. Borsato, A. Brandeker, M. Buder, A. Collier Cameron, S. Csizmadia, P. E. Cubillos, M. B. Davies, M. Deleuil, X. Delfosse, A. Deline, O. D.S. Demangeon, B. Demory, A. Derekas, B. Edwards, D. Ehrenreich, A. Erikson, A. Fortier, L. Fossati, M. Fridlund, K. Gazeas, M. Gillon, M. Güdel, J. Hasiba, A. Heitzmann, C. Helling, J. M. Jenkins, T. Keller, S. R. Kane, K. G. Stassun, L. L. Kiss, J. Korth, K. W.F. Lam, D. W. Latham, A. Lecavelier Des Etangs, A. Leleu, M. Lendl, P. F.L. Maxted, S. Mcdermott, B. Merín, C. Mordasini, V. Nascimbeni, G. Nowak, G. Olofsson, I. Pagano, E. Pallé, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, H. Rauer, I. Ribas, G. Ricker, N. C. Santos, G. Scandariato, S. Seager, D. Ségransan, A. E. Simon, A. M.S. Smith, M. Stalport, S. Striegel, S. Sulis, G. M. Szabó, S. Udry, V. Van Grootel, R. Vanderspek, J. Venturini, E. Villaver, V. Viotto, N. A. Walton, J. N. Winn, S. Wolf

Astrophysical Sciences

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

Abstract

We present the characterisation of the TOI-6041 system, a bright (V = 9.84 ± 0.03) G7-type star hosting at least two planets. The inner planet, TOI-6041 b, is a warm Neptune with a radius of 4.55_-0.17^+0.18 R_⊕, initially identified as a single-transit event in TESS photometry. Subsequent observations with TESS and CHEOPS revealed additional transits, enabling the determination of its 26.04945_-0.00034^+0.00033 orbital period and the detection of significant transit-timing variations (TTVs), exhibiting a peak-to-peak amplitude of about 1 hour. Radial-velocity (RV) measurements obtained with the APF spectrographs allowed us to place a 3ÏÂ upper mass limit of 28.9 M_⊕ on TOI-6041 b. In addition, the RV data reveal a second companion, TOI-6041 c, on an 88 d orbit, with a minimum mass of 0.25 M_Jup. A preliminary TTV analysis suggested that the observed variations could be caused by gravitational perturbations from planet c; however, reproducing the observed amplitudes requires a relatively high eccentricity of about 0.3 for that planet. Our dynamical stability analysis indicates that such a configuration is dynamically viable and places a 1ÏÂ upper limit on the mass of TOI-6041 c at 0.8 M_Jup. An alternative is the presence of a third, low-mass planet located between planets b and c, or on an inner orbit relative to planet b -particularly near a mean-motion resonance with planet b -which could account for the observed variations. These findings remain tentative, and further RV and photometric observations are essential in to better constrain the mass of planet b and to refine the TTV modeling, thereby improving our understanding of the systema s dynamical architecture.

Original language	English (US)
Article number	A134
Journal	Astronomy and Astrophysics
Volume	707
DOIs	https://doi.org/10.1051/0004-6361/202556700
State	Published - Mar 1 2026

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Planets and satellites: detection
Planets and satellites: dynamical evolution and stability

Access to Document

10.1051/0004-6361/202556700

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Heidari, N., Alnajjarine, A., Osborn, H. P., Dragomir, D., Dalba, P., Benz, W., Hébrard, G., Laskar, J., Billot, N., Günther, M. N., Wilson, T. G., Alibert, Y., Bonfanti, A., Bieryla, A., Broeg, C., Correia, A. C. M., Egger, J. A., Essack, Z., Furlan, E., ... Wolf, S. (2026). Giant Outer Transiting Exoplanet Mass (GOTa EM) survey: VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations. Astronomy and Astrophysics, 707, Article A134. https://doi.org/10.1051/0004-6361/202556700

@article{c8022261f25e43aaa7145601e760b0b1,

title = "Giant Outer Transiting Exoplanet Mass (GOTa EM) survey: VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations",

abstract = "We present the characterisation of the TOI-6041 system, a bright (V = 9.84 ± 0.03) G7-type star hosting at least two planets. The inner planet, TOI-6041 b, is a warm Neptune with a radius of 4.55-0.17+0.18 R⊕, initially identified as a single-transit event in TESS photometry. Subsequent observations with TESS and CHEOPS revealed additional transits, enabling the determination of its 26.04945-0.00034+0.00033 orbital period and the detection of significant transit-timing variations (TTVs), exhibiting a peak-to-peak amplitude of about 1 hour. Radial-velocity (RV) measurements obtained with the APF spectrographs allowed us to place a 3{\"I}{\^A} upper mass limit of 28.9 M⊕ on TOI-6041 b. In addition, the RV data reveal a second companion, TOI-6041 c, on an 88 d orbit, with a minimum mass of 0.25 MJup. A preliminary TTV analysis suggested that the observed variations could be caused by gravitational perturbations from planet c; however, reproducing the observed amplitudes requires a relatively high eccentricity of about 0.3 for that planet. Our dynamical stability analysis indicates that such a configuration is dynamically viable and places a 1{\"I}{\^A} upper limit on the mass of TOI-6041 c at 0.8 MJup. An alternative is the presence of a third, low-mass planet located between planets b and c, or on an inner orbit relative to planet b -particularly near a mean-motion resonance with planet b -which could account for the observed variations. These findings remain tentative, and further RV and photometric observations are essential in to better constrain the mass of planet b and to refine the TTV modeling, thereby improving our understanding of the systema s dynamical architecture.",

keywords = "Planets and satellites: detection, Planets and satellites: dynamical evolution and stability",

author = "N. Heidari and A. Alnajjarine and Osborn, \{H. P.\} and D. Dragomir and P. Dalba and W. Benz and G. H{\'e}brard and J. Laskar and N. Billot and G{\"u}nther, \{M. N.\} and Wilson, \{T. G.\} and Y. Alibert and A. Bonfanti and A. Bieryla and C. Broeg and Correia, \{A. C.M.\} and Egger, \{J. A.\} and Z. Essack and E. Furlan and D. Gandolfi and N. Grieves and S. Howell and D. Lacourse and C. Pezzotti and T. Pritchard and Sousa, \{S. G.\} and S. Ulmer-Moll and S. Villanueva and R. Alonso and J. Asquier and T. B{\'a}rczy and D. Barrado and Barros, \{S. C.C.\} and W. Baumjohann and L. Borsato and A. Brandeker and M. Buder and \{Collier Cameron\}, A. and S. Csizmadia and Cubillos, \{P. E.\} and Davies, \{M. B.\} and M. Deleuil and X. Delfosse and A. Deline and Demangeon, \{O. D.S.\} and B. Demory and A. Derekas and B. Edwards and D. Ehrenreich and A. Erikson and A. Fortier and L. Fossati and M. Fridlund and K. Gazeas and M. Gillon and M. G{\"u}del and J. Hasiba and A. Heitzmann and C. Helling and Jenkins, \{J. M.\} and T. Keller and Kane, \{S. R.\} and Stassun, \{K. G.\} and Kiss, \{L. L.\} and J. Korth and Lam, \{K. W.F.\} and Latham, \{D. W.\} and \{Des Etangs\}, \{A. Lecavelier\} and A. Leleu and M. Lendl and Maxted, \{P. F.L.\} and S. Mcdermott and B. Mer{\'i}n and C. Mordasini and V. Nascimbeni and G. Nowak and G. Olofsson and I. Pagano and E. Pall{\'e} and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and H. Rauer and I. Ribas and G. Ricker and Santos, \{N. C.\} and G. Scandariato and S. Seager and D. S{\'e}gransan and Simon, \{A. E.\} and Smith, \{A. M.S.\} and M. Stalport and S. Striegel and S. Sulis and Szab{\'o}, \{G. M.\} and S. Udry and \{Van Grootel\}, V. and R. Vanderspek and J. Venturini and E. Villaver and V. Viotto and Walton, \{N. A.\} and Winn, \{J. N.\} and S. Wolf",

note = "Publisher Copyright: {\textcopyright} The Authors 2026.",

year = "2026",

month = mar,

day = "1",

doi = "10.1051/0004-6361/202556700",

language = "English (US)",

volume = "707",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Heidari, N, Alnajjarine, A, Osborn, HP, Dragomir, D, Dalba, P, Benz, W, Hébrard, G, Laskar, J, Billot, N, Günther, MN, Wilson, TG, Alibert, Y, Bonfanti, A, Bieryla, A, Broeg, C, Correia, ACM, Egger, JA, Essack, Z, Furlan, E, Gandolfi, D, Grieves, N, Howell, S, Lacourse, D, Pezzotti, C, Pritchard, T, Sousa, SG, Ulmer-Moll, S, Villanueva, S, Alonso, R, Asquier, J, Bárczy, T, Barrado, D, Barros, SCC, Baumjohann, W, Borsato, L, Brandeker, A, Buder, M, Collier Cameron, A, Csizmadia, S, Cubillos, PE, Davies, MB, Deleuil, M, Delfosse, X, Deline, A, Demangeon, ODS, Demory, B, Derekas, A, Edwards, B, Ehrenreich, D, Erikson, A, Fortier, A, Fossati, L, Fridlund, M, Gazeas, K, Gillon, M, Güdel, M, Hasiba, J, Heitzmann, A, Helling, C, Jenkins, JM, Keller, T, Kane, SR, Stassun, KG, Kiss, LL, Korth, J, Lam, KWF, Latham, DW, Des Etangs, AL, Leleu, A, Lendl, M, Maxted, PFL, Mcdermott, S, Merín, B, Mordasini, C, Nascimbeni, V, Nowak, G, Olofsson, G, Pagano, I, Pallé, E, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rauer, H, Ribas, I, Ricker, G, Santos, NC, Scandariato, G, Seager, S, Ségransan, D, Simon, AE, Smith, AMS, Stalport, M, Striegel, S, Sulis, S, Szabó, GM, Udry, S, Van Grootel, V, Vanderspek, R, Venturini, J, Villaver, E, Viotto, V, Walton, NA, Winn, JN & Wolf, S 2026, 'Giant Outer Transiting Exoplanet Mass (GOTa EM) survey: VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations', Astronomy and Astrophysics, vol. 707, A134. https://doi.org/10.1051/0004-6361/202556700

TY - JOUR

T1 - Giant Outer Transiting Exoplanet Mass (GOTa EM) survey

T2 - VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations

AU - Heidari, N.

AU - Alnajjarine, A.

AU - Osborn, H. P.

AU - Dragomir, D.

AU - Dalba, P.

AU - Benz, W.

AU - Hébrard, G.

AU - Laskar, J.

AU - Billot, N.

AU - Günther, M. N.

AU - Wilson, T. G.

AU - Alibert, Y.

AU - Bonfanti, A.

AU - Bieryla, A.

AU - Broeg, C.

AU - Correia, A. C.M.

AU - Egger, J. A.

AU - Essack, Z.

AU - Furlan, E.

AU - Gandolfi, D.

AU - Grieves, N.

AU - Howell, S.

AU - Lacourse, D.

AU - Pezzotti, C.

AU - Pritchard, T.

AU - Sousa, S. G.

AU - Ulmer-Moll, S.

AU - Villanueva, S.

AU - Alonso, R.

AU - Asquier, J.

AU - Bárczy, T.

AU - Barrado, D.

AU - Barros, S. C.C.

AU - Baumjohann, W.

AU - Borsato, L.

AU - Brandeker, A.

AU - Buder, M.

AU - Collier Cameron, A.

AU - Csizmadia, S.

AU - Cubillos, P. E.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delfosse, X.

AU - Deline, A.

AU - Demangeon, O. D.S.

AU - Demory, B.

AU - Derekas, A.

AU - Edwards, B.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fortier, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gazeas, K.

AU - Gillon, M.

AU - Güdel, M.

AU - Hasiba, J.

AU - Heitzmann, A.

AU - Helling, C.

AU - Jenkins, J. M.

AU - Keller, T.

AU - Kane, S. R.

AU - Stassun, K. G.

AU - Kiss, L. L.

AU - Korth, J.

AU - Lam, K. W.F.

AU - Latham, D. W.

AU - Des Etangs, A. Lecavelier

AU - Leleu, A.

AU - Lendl, M.

AU - Maxted, P. F.L.

AU - Mcdermott, S.

AU - Merín, B.

AU - Mordasini, C.

AU - Nascimbeni, V.

AU - Nowak, G.

AU - Olofsson, G.

AU - Pagano, I.

AU - Pallé, E.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rauer, H.

AU - Ribas, I.

AU - Ricker, G.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Seager, S.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M.S.

AU - Stalport, M.

AU - Striegel, S.

AU - Sulis, S.

AU - Szabó, G. M.

AU - Udry, S.

AU - Van Grootel, V.

AU - Vanderspek, R.

AU - Venturini, J.

AU - Villaver, E.

AU - Viotto, V.

AU - Walton, N. A.

AU - Winn, J. N.

AU - Wolf, S.

PY - 2026/3/1

Y1 - 2026/3/1

N2 - We present the characterisation of the TOI-6041 system, a bright (V = 9.84 ± 0.03) G7-type star hosting at least two planets. The inner planet, TOI-6041 b, is a warm Neptune with a radius of 4.55-0.17+0.18 R⊕, initially identified as a single-transit event in TESS photometry. Subsequent observations with TESS and CHEOPS revealed additional transits, enabling the determination of its 26.04945-0.00034+0.00033 orbital period and the detection of significant transit-timing variations (TTVs), exhibiting a peak-to-peak amplitude of about 1 hour. Radial-velocity (RV) measurements obtained with the APF spectrographs allowed us to place a 3ÏÂ upper mass limit of 28.9 M⊕ on TOI-6041 b. In addition, the RV data reveal a second companion, TOI-6041 c, on an 88 d orbit, with a minimum mass of 0.25 MJup. A preliminary TTV analysis suggested that the observed variations could be caused by gravitational perturbations from planet c; however, reproducing the observed amplitudes requires a relatively high eccentricity of about 0.3 for that planet. Our dynamical stability analysis indicates that such a configuration is dynamically viable and places a 1ÏÂ upper limit on the mass of TOI-6041 c at 0.8 MJup. An alternative is the presence of a third, low-mass planet located between planets b and c, or on an inner orbit relative to planet b -particularly near a mean-motion resonance with planet b -which could account for the observed variations. These findings remain tentative, and further RV and photometric observations are essential in to better constrain the mass of planet b and to refine the TTV modeling, thereby improving our understanding of the systema s dynamical architecture.

AB - We present the characterisation of the TOI-6041 system, a bright (V = 9.84 ± 0.03) G7-type star hosting at least two planets. The inner planet, TOI-6041 b, is a warm Neptune with a radius of 4.55-0.17+0.18 R⊕, initially identified as a single-transit event in TESS photometry. Subsequent observations with TESS and CHEOPS revealed additional transits, enabling the determination of its 26.04945-0.00034+0.00033 orbital period and the detection of significant transit-timing variations (TTVs), exhibiting a peak-to-peak amplitude of about 1 hour. Radial-velocity (RV) measurements obtained with the APF spectrographs allowed us to place a 3ÏÂ upper mass limit of 28.9 M⊕ on TOI-6041 b. In addition, the RV data reveal a second companion, TOI-6041 c, on an 88 d orbit, with a minimum mass of 0.25 MJup. A preliminary TTV analysis suggested that the observed variations could be caused by gravitational perturbations from planet c; however, reproducing the observed amplitudes requires a relatively high eccentricity of about 0.3 for that planet. Our dynamical stability analysis indicates that such a configuration is dynamically viable and places a 1ÏÂ upper limit on the mass of TOI-6041 c at 0.8 MJup. An alternative is the presence of a third, low-mass planet located between planets b and c, or on an inner orbit relative to planet b -particularly near a mean-motion resonance with planet b -which could account for the observed variations. These findings remain tentative, and further RV and photometric observations are essential in to better constrain the mass of planet b and to refine the TTV modeling, thereby improving our understanding of the systema s dynamical architecture.

KW - Planets and satellites: detection

KW - Planets and satellites: dynamical evolution and stability

UR - https://www.scopus.com/pages/publications/105033014134

UR - https://www.scopus.com/pages/publications/105033014134#tab=citedBy

U2 - 10.1051/0004-6361/202556700

DO - 10.1051/0004-6361/202556700

M3 - Article

AN - SCOPUS:105033014134

SN - 0004-6361

VL - 707

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A134

ER -

Giant Outer Transiting Exoplanet Mass (GOTa EM) survey: VII. TOI-6041: A multi-planet system including a warm Neptune exhibiting strong transit-timing variations

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