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

Fuente: arXiv

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Main Authors:	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., Goffo, E., Wilson, T., Serrano, L. M., Brandeker, A., Wang, S. X., Heitzmann, A., Bonfanti, A., Fossati, L., Alibert, Y., Delrez, L., Sefako, R., Barros, S., Collins, K. I., Demangeon, O. D. S., Albrecht, S. H., Alonso, R., Asquier, J., Barczy, T., Barrado, D., Baumjohann, W., Beck, T., Benz, W., Billot, N., Borsato, L., Broeg, C., Bryant, E. M., Butler, R. P., Cochran, W. D., Cameron, A. Collier, Correia, A. C. M., Crane, J. D., Csizmadia, Sz., Cubillos, P. E., Davies, M. B., 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, A. P., Helling, Ch., Hirano, T., Howell, S. B., Hoyer, S., Isaak, K. G., Jenkins, J. M., Kanodia, S., Kiss, L. L., Korth, J., Lam, K. W. F., Laskar, J., Etangs, A. Lecavelier des, Lendl, M., Lund, M. B., Luque, R., Mann, A. W., Magrin, D., Maxted, P. F. L., Mordasini, C., Narita, N., Nascimbeni, V., Nowak, G., Olofsson, G., Osborn, H. P., Osborne, H. L. M., 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, G. R., Rieder, M., Salmon, S., Santos, N. C., Scandariato, G., Seager, S., Segransan, D., Shporer, A., Simon, A. E., Smith, A. M. S., Stalport, M., Szabo, Gy. M., Thompson, I., Twicken, J. D., Udry, S., Vanderspek, R., Van Grootel, V., Venturini, J., Villaver, E., Villaseñor, J., Viotto, V., Walter, I., Walton, N. A., Winn, J. N., Yee, S. W.
Format:	Preprint
Published:	2024
Subjects:	Earth and Planetary Astrophysics
Online Access:	Acceder al recurso
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author	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. Goffo, E. Wilson, T. Serrano, L. M. Brandeker, A. Wang, S. X. Heitzmann, A. Bonfanti, A. Fossati, L. Alibert, Y. Delrez, L. Sefako, R. Barros, S. Collins, K. I. Demangeon, O. D. S. Albrecht, S. H. Alonso, R. Asquier, J. Barczy, T. Barrado, D. Baumjohann, W. Beck, T. Benz, W. Billot, N. Borsato, L. Broeg, C. Bryant, E. M. Butler, R. P. Cochran, W. D. Cameron, A. Collier Correia, A. C. M. Crane, J. D. Csizmadia, Sz. Cubillos, P. E. Davies, M. B. 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, A. P. Helling, Ch. Hirano, T. Howell, S. B. Hoyer, S. Isaak, K. G. Jenkins, J. M. Kanodia, S. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Lund, M. B. Luque, R. Mann, A. W. Magrin, D. Maxted, P. F. L. Mordasini, C. Narita, N. Nascimbeni, V. Nowak, G. Olofsson, G. Osborn, H. P. Osborne, H. L. M. 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, G. R. Rieder, M. Salmon, S. Santos, N. C. Scandariato, G. Seager, S. Segransan, D. Shporer, A. Simon, A. E. Smith, A. M. S. Stalport, M. Szabo, Gy. M. Thompson, I. Twicken, J. D. Udry, S. Vanderspek, R. Van Grootel, V. Venturini, J. Villaver, E. Villaseñor, J. Viotto, V. Walter, I. Walton, N. A. Winn, J. N. Yee, S. W.
author_facet	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. Goffo, E. Wilson, T. Serrano, L. M. Brandeker, A. Wang, S. X. Heitzmann, A. Bonfanti, A. Fossati, L. Alibert, Y. Delrez, L. Sefako, R. Barros, S. Collins, K. I. Demangeon, O. D. S. Albrecht, S. H. Alonso, R. Asquier, J. Barczy, T. Barrado, D. Baumjohann, W. Beck, T. Benz, W. Billot, N. Borsato, L. Broeg, C. Bryant, E. M. Butler, R. P. Cochran, W. D. Cameron, A. Collier Correia, A. C. M. Crane, J. D. Csizmadia, Sz. Cubillos, P. E. Davies, M. B. 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, A. P. Helling, Ch. Hirano, T. Howell, S. B. Hoyer, S. Isaak, K. G. Jenkins, J. M. Kanodia, S. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Lund, M. B. Luque, R. Mann, A. W. Magrin, D. Maxted, P. F. L. Mordasini, C. Narita, N. Nascimbeni, V. Nowak, G. Olofsson, G. Osborn, H. P. Osborne, H. L. M. 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, G. R. Rieder, M. Salmon, S. Santos, N. C. Scandariato, G. Seager, S. Segransan, D. Shporer, A. Simon, A. E. Smith, A. M. S. Stalport, M. Szabo, Gy. M. Thompson, I. Twicken, J. D. Udry, S. Vanderspek, R. Van Grootel, V. Venturini, J. Villaver, E. Villaseñor, J. Viotto, V. Walter, I. Walton, N. A. Winn, J. N. Yee, S. W.
contents	We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day 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 $R_{\mathrm{p}} = 2.5 \pm 0.1 R_{\oplus}$ and a mass of $M_{\mathrm{p}} = 10.5^{+2.2}_{-2.1} M_{\oplus}$, implying a bulk density of $ρ_{\text{p}} = 3.6 \pm 0.8$ g cm$^{-3}$. Our internal composition modeling 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 disk formation, given the low metallicity and older age of TOI-757.
format	Preprint
id	arxiv_https___arxiv_org_abs_2407_20525
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit 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. Goffo, E. Wilson, T. Serrano, L. M. Brandeker, A. Wang, S. X. Heitzmann, A. Bonfanti, A. Fossati, L. Alibert, Y. Delrez, L. Sefako, R. Barros, S. Collins, K. I. Demangeon, O. D. S. Albrecht, S. H. Alonso, R. Asquier, J. Barczy, T. Barrado, D. Baumjohann, W. Beck, T. Benz, W. Billot, N. Borsato, L. Broeg, C. Bryant, E. M. Butler, R. P. Cochran, W. D. Cameron, A. Collier Correia, A. C. M. Crane, J. D. Csizmadia, Sz. Cubillos, P. E. Davies, M. B. 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, A. P. Helling, Ch. Hirano, T. Howell, S. B. Hoyer, S. Isaak, K. G. Jenkins, J. M. Kanodia, S. Kiss, L. L. Korth, J. Lam, K. W. F. Laskar, J. Etangs, A. Lecavelier des Lendl, M. Lund, M. B. Luque, R. Mann, A. W. Magrin, D. Maxted, P. F. L. Mordasini, C. Narita, N. Nascimbeni, V. Nowak, G. Olofsson, G. Osborn, H. P. Osborne, H. L. M. 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, G. R. Rieder, M. Salmon, S. Santos, N. C. Scandariato, G. Seager, S. Segransan, D. Shporer, A. Simon, A. E. Smith, A. M. S. Stalport, M. Szabo, Gy. M. Thompson, I. Twicken, J. D. Udry, S. Vanderspek, R. Van Grootel, V. Venturini, J. Villaver, E. Villaseñor, J. Viotto, V. Walter, I. Walton, N. A. Winn, J. N. Yee, S. W. Earth and Planetary Astrophysics We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day 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 $R_{\mathrm{p}} = 2.5 \pm 0.1 R_{\oplus}$ and a mass of $M_{\mathrm{p}} = 10.5^{+2.2}_{-2.1} M_{\oplus}$, implying a bulk density of $ρ_{\text{p}} = 3.6 \pm 0.8$ g cm$^{-3}$. Our internal composition modeling 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 disk formation, given the low metallicity and older age of TOI-757.
title	TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit
topic	Earth and Planetary Astrophysics
url	https://arxiv.org/abs/2407.20525