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1. K2-79b and K2-222b: Mass Measurements of Two Small Exoplanets with Periods beyond 10 days that Overlap with Periodic Magnetic Activity Signals

Author

Chantanelle Nava, Mercedes López-Morales, Annelies Mortier, Li Zeng, Helen A. C. Giles, Allyson Bieryla, Andrew Vanderburg, Lars A. Buchhave, Ennio Poretti, Steven H. Saar, Xavier Dumusque, David W. Latham, David Charbonneau, Mario Damasso, Aldo S. Bonomo, Christophe Lovis, Andrew Collier Cameron, Jason D. Eastman, Alessandro Sozzetti, Rosario Cosentino, Marco Pedani, Francesco Pepe, Emilio Molinari, Dimitar Sasselov, Michel Mayor, Manu Stalport, Luca Malavolta, Ken Rice, Christopher A. Watson, A. F. Martinez Fiorenzano, Luca Di Fabrizio, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Nava, Chantanelle [0000-0001-8838-3883], López-Morales, Mercedes [0000-0003-3204-8183], Mortier, Annelies [0000-0001-7254-4363], Zeng, Li [0000-0003-1957-6635], Giles, Helen AC [0000-0001-6777-4797], Bieryla, Allyson [0000-0001-6637-5401], Vanderburg, Andrew [0000-0001-7246-5438], Buchhave, Lars A [0000-0003-1605-5666], Poretti, Ennio [0000-0003-1200-0473], Saar, Steven H [0000-0001-7032-8480], Dumusque, Xavier [0000-0002-9332-2011], Latham, David W [0000-0001-9911-7388], Charbonneau, David [0000-0002-9003-484X], Damasso, Mario [0000-0001-9984-4278], Bonomo, Aldo S [0000-0002-6177-198X], Eastman, Jason D [0000-0003-3773-5142], Sozzetti, Alessandro [0000-0002-7504-365X], Pedani, Marco [0000-0002-5752-6260], Molinari, Emilio [0000-0002-1742-7735], Sasselov, Dimitar [0000-0001-7014-1771], Mayor, Michel [0000-0002-9352-5935], Malavolta, Luca [0000-0002-6492-2085], Martinez Fiorenzano, AF [0000-0002-4272-4272], Apollo - University of Cambridge Repository, Nava, C [0000-0001-8838-3883], López-Morales, M [0000-0003-3204-8183], Mortier, A [0000-0001-7254-4363], Zeng, L [0000-0003-1957-6635], Giles, HAC [0000-0001-6777-4797], Bieryla, A [0000-0001-6637-5401], Vanderburg, A [0000-0001-7246-5438], Buchhave, LA [0000-0003-1605-5666], Poretti, E [0000-0003-1200-0473], Saar, SH [0000-0001-7032-8480], Dumusque, X [0000-0002-9332-2011], Latham, DW [0000-0001-9911-7388], Charbonneau, D [0000-0002-9003-484X], Damasso, M [0000-0001-9984-4278], Bonomo, AS [0000-0002-6177-198X], Eastman, JD [0000-0003-3773-5142], Sozzetti, A [0000-0002-7504-365X], Pedani, M [0000-0002-5752-6260], Molinari, E [0000-0002-1742-7735], Sasselov, D [0000-0001-7014-1771], Mayor, M [0000-0002-9352-5935], and Malavolta, L [0000-0002-6492-2085]

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), The Solar System, Exoplanets, and Astrobiology, Exoplanet astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, Stellar activity, QC Physics, Space and Planetary Science, astro-ph.EP, QB Astronomy, QC, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We present mass and radius measurements of K2-79b and K2-222b, two transiting exoplanets orbiting active G-type stars. Their respective 10.99d and 15.39d orbital periods fall near periods of signals induced by stellar magnetic activity. The two signals might therefore interfere and lead to an inaccurate estimate of exoplanet mass. We present a method to mitigate these effects when radial velocity and activity indicator observations are available over multiple observing seasons and the orbital period of the exoplanet is known. We perform correlation and periodogram analyses on sub-sets composed of each target's two observing seasons, in addition to the full data sets. For both targets, these analyses reveal an optimal season with little to no interference at the orbital period of the known exoplanet. We make a confident mass detection of each exoplanet by confirming agreement between fits to the full radial velocity set and the optimal season. For K2-79b, we measure a mass of 11.8 $\pm$ 3.6 $M_{Earth}$ and a radius of 4.09 $\pm$ 0.17 $R_{Earth}$. For K2-222b, we measure a mass of 8.0 $\pm$ 1.8 $M_{Earth}$ and a radius of 2.35 $\pm$ 0.08 $R_{Earth}$. According to model predictions, K2-79b is a highly irradiated Uranus-analog and K2-222b hosts significant amounts of water ice. We also present an RV solution for a candidate second companion orbiting K2-222 at 147.5d., Comment: 33 pages, 17 figures, 13 tables

Published
2022
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2. TOI-4010: A System of Three Large Short-Period Planets With a Massive Long-Period Companion

Author

Kunimoto, Michelle, Vanderburg, Andrew, Huang, Chelsea X., Davis, M. Ryleigh, Affer, Laura, Cameron, Andrew Collier, Charbonneau, David, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martnez, Ghedina, Adriano, Haywood, R. D., Lienhard, Florian, López-Morales, Mercedes, Mayor, Michel, Pepe, Francesco, Pinamonti, Matteo, Poretti, Ennio, Maldonado, Jesús, Rice, Ken, Sozzetti, Alessandro, Wilson, Thomas G., Udry, Stéphane, Baptista, Jay, Barkaoui, Khalid, Becker, Juliette, Benni, Paul, Bieryla, Allyson, Bosch-Cabot, Pau, Ciardi, David R., Collins, Karen A., Collins, Kevin I., Evans, Elise, Dupuy, Trent J., Goliguzova, Maria V., Guerra, Pere, Kraus, Adam, Lissauer, Jack J., Huber, Daniel, Murgas, Felipe, Palle, Enric, Quinn, Samuel N., Safonov, Boris S., Schwarz, Richard P., Shporer, Avi, Stassun, Keivan G., Jenkins, Jon M., Latham, David W., Ricker, George R., Seager, Sara, Vanderspek, Roland, Winn, Joshua, Essack, Zahra, Lewis, Hannah M., Rose, Mark E., Kunimoto, M [0000-0001-9269-8060], Vanderburg, A [0000-0001-7246-5438], Huang, CX [0000-0003-0918-7484], Davis, MR [0000-0002-7451-4704], Affer, L [0000-0001-5600-3778], Cameron, AC [0000-0002-8863-7828], Charbonneau, D [0000-0002-9003-484X], Cosentino, R [0000-0003-1784-1431], Damasso, M [0000-0001-9984-4278], Dumusque, X [0000-0002-9332-2011], Fiorenzano, AFM [0000-0002-4272-4272], Ghedina, A [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Lienhard, F [0000-0003-4047-0771], López-Morales, M [0000-0003-3204-8183], Mayor, M [0000-0002-9352-5935], Pepe, F [0000-0002-9815-773X], Pinamonti, M [0000-0002-4445-1845], Poretti, E [0000-0003-1200-0473], Maldonado, J [0000-0002-2218-5689], Rice, K [0000-0002-6379-9185], Sozzetti, A [0000-0002-7504-365X], Wilson, TG [0000-0001-8749-1962], Udry, S [0000-0001-7576-6236], Baptista, J [0000-0002-9306-1704], Barkaoui, K [0000-0003-1464-9276], Becker, J [0000-0002-7733-4522], Benni, P [0000-0001-6981-8722], Bieryla, A [0000-0001-6637-5401], Bosch-Cabot, P [0000-0002-1514-5558], Ciardi, DR [0000-0002-5741-3047], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Dupuy, TJ [0000-0001-9823-1445], Goliguzova, MV [0000-0003-2228-7914], Guerra, P [0000-0002-4308-2339], Kraus, A [0000-0001-9811-568X], Lissauer, JJ [0000-0001-6513-1659], Huber, D [0000-0001-8832-4488], Murgas, F [0000-0001-9087-1245], Palle, E [0000-0003-0987-1593], Quinn, SN [0000-0002-8964-8377], Safonov, BS [0000-0003-1713-3208], Schwarz, RP [0000-0001-8227-1020], Shporer, A [0000-0002-1836-3120], Stassun, KG [0000-0002-3481-9052], Jenkins, JM [0000-0002-4715-9460], Latham, DW [0000-0001-9911-7388], Ricker, GR [0000-0003-2058-6662], Seager, S [0000-0002-6892-6948], Vanderspek, R [0000-0001-6763-6562], Winn, J [0000-0002-4265-047X], Essack, Z [0000-0002-2482-0180], Lewis, HM [0000-0002-7871-085X], Rose, ME [0000-0003-4724-745X], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Exoplanets, Exoplanet dynamics, FOS: Physical sciences, DAS, 5109 Space Sciences, Hot Neptunes, QB Astronomy, Transit photometry, Exoplanet systems, 51 Physical Sciences, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We report the confirmation of three exoplanets transiting TOI-4010 (TIC-352682207), a metal-rich K dwarf observed by TESS in Sectors 24, 25, 52, and 58. We confirm these planets with HARPS-N radial velocity observations and measure their masses with 8 - 12% precision. TOI-4010 b is a sub-Neptune ($P = 1.3$ days, $R_{p} = 3.02_{-0.08}^{+0.08}~R_{\oplus}$, $M_{p} = 11.00_{-1.27}^{+1.29}~M_{\oplus}$) in the hot Neptune desert, and is one of the few such planets with known companions. Meanwhile, TOI-4010 c ($P = 5.4$ days, $R_{p} = 5.93_{-0.12}^{+0.11}~R_{\oplus}$, $M_{p} = 20.31_{-2.11}^{+2.13}~M_{\oplus}$) and TOI-4010 d ($P = 14.7$ days, $R_{p} = 6.18_{-0.14}^{+0.15}~R_{\oplus}$, $M_{p} = 38.15_{-3.22}^{+3.27}~M_{\oplus}$) are similarly-sized sub-Saturns on short-period orbits. Radial velocity observations also reveal a super-Jupiter-mass companion called TOI-4010 e in a long-period, eccentric orbit ($P \sim 762$ days and $e \sim 0.26$ based on available observations). TOI-4010 is one of the few systems with multiple short-period sub-Saturns to be discovered so far., Comment: 26 pages, 16 figures, published in AJ; (v3) added missing citation

Published
2023
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3. Independent Validation of the Temperate Super-Earth HD 79211 b using HARPS-N

Author

Victoria DiTomasso, Chantanelle Nava, Mercedes López-Morales, Allyson Bieryla, Ryan Cloutier, Luca Malavolta, Annelies Mortier, Lars A. Buchhave, Keivan G. Stassun, Alessandro Sozzetti, Aldo Stefano Bonomo, David Charbonneau, Andrew Collier Cameron, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martínez Fiorenzano, Adriano Ghedina, Avet Harutyunyan, R. D. Haywood, David Latham, Emilio Molinari, Francesco A. Pepe, Matteo Pinamonti, Ennio Poretti, Ken Rice, Dimitar Sasselov, Manu Stalport, Stéphane Udry, Christopher Watson, Thomas G. Wilson, DiTomasso, Victoria [0000-0003-0741-7661], Nava, Chantanelle [0000-0001-8838-3883], López-Morales, Mercedes [0000-0003-3204-8183], Bieryla, Allyson [0000-0001-6637-5401], Cloutier, Ryan [0000-0001-5383-9393], Malavolta, Luca [0000-0002-6492-2085], Mortier, Annelies [0000-0001-7254-4363], Buchhave, Lars A [0000-0003-1605-5666], Stassun, Keivan G [0000-0002-3481-9052], Sozzetti, Alessandro [0000-0002-7504-365X], Bonomo, Aldo Stefano [0000-0002-6177-198X], Charbonneau, David [0000-0002-9003-484X], Collier Cameron, Andrew [0000-0002-8863-7828], Cosentino, Rosario [0000-0003-1784-1431], Damasso, Mario [0000-0001-9984-4278], Dumusque, Xavier [0000-0002-9332-2011], Martínez Fiorenzano, AF [0000-0002-4272-4272], Ghedina, Adriano [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Latham, David [0000-0001-9911-7388], Molinari, Emilio [0000-0002-1742-7735], Pinamonti, Matteo [0000-0002-4445-1845], Poretti, Ennio [0000-0003-1200-0473], Rice, Ken [0000-0002-6379-9185], Sasselov, Dimitar [0000-0001-7014-1771], Stalport, Manu [0000-0003-0996-6402], Udry, Stéphane [0000-0001-7576-6236], Watson, Christopher [0000-0002-9718-3266], Wilson, Thomas G [0000-0001-8749-1962], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
MCC, Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, The Solar System, Exoplanets, and Astrobiology, Exoplanets, FOS: Physical sciences, Astronomy and Astrophysics, 3rd-DAS, 5109 Space Sciences, Astrobiology, M dwarf stars, Binary stars, QC Physics, Rare Diseases, Space and Planetary Science, astro-ph.EP, QB Astronomy, Exoplanet detection methods, Solar System, 51 Physical Sciences, QC, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

We present high-precision radial velocities (RVs) from the HARPS-N spectrograph for HD79210 and HD79211, two M0V members of a gravitationally-bound binary system. We detect a planet candidate with a period of $24.421^{+0.016}_{-0.017}$ days around HD79211 in these HARPS-N RVs, validating the planet candidate originally identified in CARMENES RV data alone. Using HARPS-N, CARMENES and HIRES RVs spanning a total of 25 years, we further refine the planet candidate parameters to $P=24.422\pm0.014$ days, $K=3.19\pm0.27$ m/s, $M$ sin $i = 10.6 \pm 1.2 M_\oplus$, and $a = 0.142 \pm0.005$ au. We do not find any additional planet candidate signals in the data of HD79211 nor do we find any planet candidate signals in HD79210. This system adds to the number of exoplanets detected in binaries with M dwarf members, and serves as a case study for planet formation in stellar binaries., Comment: Accepted for publication in AJ, 29 pages, 17 figures

Published
2023
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4. TOI-1695 b: A Water World Orbiting an Early M Dwarf in the Planet Radius Valley

Author

Collin Cherubim, Ryan Cloutier, David Charbonneau, Chris Stockdale, Keivan G. Stassun, Richard P. Schwarz, Boris Safonov, Annelies Mortier, Pablo Lewin, David W. Latham, Keith Horne, Raphaëlle D. Haywood, Erica Gonzales, Maria V. Goliguzova, Karen A. Collins, David R. Ciardi, Allyson Bieryla, Alexandre A. Belinski, Bill Wohler, Christopher A. Watson, Roland Vanderspek, Stéphane Udry, Alessandro Sozzetti, Damien Ségransan, Dimitar Sasselov, George R. Ricker, Ken Rice, Ennio Poretti, Giampaolo Piotto, Francesco Pepe, Emilio Molinari, Giuseppina Micela, Michel Mayor, Christophe Lovis, Mercedes López-Morales, Jon M. Jenkins, Zahra Essack, Xavier Dumusque, John P. Doty, Knicole D. Colón, Andrew Collier Cameron, Lars A. Buchhave, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Cherubim, Collin [0000-0002-8466-5469], Cloutier, Ryan [0000-0001-5383-9393], Charbonneau, David [0000-0002-9003-484X], Stockdale, Chris [0000-0003-2163-1437], Stassun, Keivan G [0000-0002-3481-9052], Schwarz, Richard P [0000-0001-8227-1020], Safonov, Boris [0000-0003-1713-3208], Mortier, Annelies [0000-0001-7254-4363], Lewin, Pablo [0000-0003-0828-6368], Latham, David W [0000-0001-9911-7388], Horne, Keith [0000-0003-1728-0304], Haywood, Raphaëlle D [0000-0001-9140-3574], Collins, Karen A [0000-0001-6588-9574], Ciardi, David R [0000-0002-5741-3047], Bieryla, Allyson [0000-0001-6637-5401], Belinski, Alexandre A [0000-0003-3469-0989], Wohler, Bill [0000-0002-5402-9613], Watson, Christopher A [0000-0002-9718-3266], Vanderspek, Roland [0000-0001-6763-6562], Udry, Stéphane [0000-0001-7576-6236], Sozzetti, Alessandro [0000-0002-7504-365X], Ségransan, Damien [0000-0003-2355-8034], Sasselov, Dimitar [0000-0001-7014-1771], Ricker, George R [0000-0003-2058-6662], Rice, Ken [0000-0002-6379-9185], Poretti, Ennio [0000-0003-1200-0473], Piotto, Giampaolo [0000-0002-9937-6387], Molinari, Emilio [0000-0002-1742-7735], Micela, Giuseppina [0000-0002-9900-4751], Mayor, Michel [0000-0002-9352-5935], López-Morales, Mercedes [0000-0003-3204-8183], Jenkins, Jon M [0000-0002-4715-9460], Essack, Zahra [0000-0002-2482-0180], Dumusque, Xavier [0000-0002-9332-2011], Doty, John P [0000-0003-2996-8421], Colón, Knicole D [0000-0001-8020-7121], Cameron, Andrew Collier [0000-0002-8863-7828], Buchhave, Lars A [0000-0003-1605-5666], and Apollo - University of Cambridge Repository

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), MCC, Space and Planetary Science, The Solar System, Exoplanets, and Astrobiology, FOS: Physical sciences, QB Astronomy, Astronomy and Astrophysics, 5109 Space Sciences, 3rd-DAS, 51 Physical Sciences, QB, Astrophysics - Earth and Planetary Astrophysics
Abstract

Characterizing the bulk compositions of transiting exoplanets within the M dwarf radius valley offers a unique means to establish whether the radius valley emerges from an atmospheric mass loss process or is imprinted by planet formation itself. We present the confirmation of such a planet orbiting an early M dwarf ($T_{\rm mag} = 11.0294 \pm 0.0074, M_s = 0.513 \pm 0.012\ M_\odot, R_s = 0.515 \pm 0.015\ R_\odot, T_{\rm eff} =3690\pm 50 K$): TOI-1695 b ($P = 3.13$ days, $R_p = 1.90^{+0.16}_{-0.14}\ R_\oplus$). TOI-1695 b's radius and orbital period situate the planet between model predictions from thermally-driven mass loss versus gas depleted formation, offering an important test case for radius valley emergence models around early M dwarfs. We confirm the planetary nature of TOI-1695 b based on five sectors of TESS data and a suite of follow-up observations including 49 precise radial velocity measurements taken with the HARPS-N spectrograph. We measure a planetary mass of $6.36 \pm 1.00\ M_\oplus$, which reveals that TOI-1695 b is inconsistent with a purely terrestrial composition of iron and magnesium silicate, and instead is likely a water-rich planet. Our finding that TOI-1695 b is not terrestrial is inconsistent with the planetary system being sculpted by thermally driven mass loss. We present a statistical analysis of seven well-characterized planets within the M dwarf radius valley demonstrating that a thermally-driven mass loss scenario is unlikely to explain this population., 22 pages, 11 figures. Accepted in AJ

Published
2022
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5. K2-111: an old system with two planets in near-resonance†

Author

Lars A. Buchhave, Valentina D'Odorico, Laura Affer, Dimitar Sasselov, Annelies Mortier, C. Allende Prieto, Christopher A. Watson, Aldo F. M. Fiorenzano, Paolo Molaro, A. Collier Cameron, Nuno C. Santos, Marco Riva, C. Lovis, Nelson J. Nunes, David Charbonneau, Jesus Maldonado, S. G. Sousa, Enric Palle, Giampaolo Piotto, Aldo S. Bonomo, Adriano Ghedina, Cristina Martins, Richard G. West, Andrew Vanderburg, David W. Latham, Giuseppina Micela, Vardan Adibekyan, Francesco Pepe, G. Lo Curto, Ken Rice, Mahmoudreza Oshagh, Avet Harutyunyan, Alexandre Cabral, Andrea Mehner, P. Di Marcantonio, Antonio Manescau, Rafael Rebolo, Matteo Pinamonti, M. R. Zapatero Osorio, François Bouchy, Baptiste Lavie, Denis Mégevand, Luca Malavolta, Stéphane Udry, David F. Phillips, David Ehrenreich, Jorge Lillo-Box, A. Suárez Mascareño, T. G. Wilson, S. C. C. Barros, Rosario Cosentino, Olivier Demangeon, M. Mayor, Xavier Dumusque, Mercedes López-Morales, Walter Boschin, E. Delgado Mena, Emilio Molinari, Serena Benatti, Alessandro Sozzetti, P. Figueira, Raphaëlle D. Haywood, Ennio Poretti, Stefano Cristiani, J. Haldemann, Yann Alibert, J. I. González Hernández, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Science and Technology Facilities Council (STFC), Istituto Nazionale di Astrofisica (INAF), Swiss National Science Foundation (SNSF), Fundação para a Ciência e a Tecnologia (FCT), National Aeronautics and Space Administration (NASA), European Research Council (ERC), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Cabral, A. [0000-0002-9433-871X], Suárez Mascareño, A. [0000-0002-3814-5323], Molaro, P. [0000-0002-0571-4163], Mena, E. D. [0000-0003-4434-2195], Buchhave, L. A. [0000-0003-1605-5666], Vanderburg, A. [0000-0001-7246-5438], Barros, S. [0000-0003-2434-3625], Haldemann, J. [0000-0003-1231-2389], Cosentino, R. [0000-0003-1784-1431], Sozzetti, A. [0000-0002-7504-365X], Adibekyan, V. [0000-0002-0601-6199], Wilson, T. G. [0000-0001-8749-1962], Cameron, A. [0000-0002-8863-7828], Santos, N. [0000-0003-4422-2919], Ministerio de Ciencia e Innovación (MICINN), Science and Technology Facilities Council (STFC), ST/R000824/1 ST/P000312/1 PTDC/FIS-AST/32113/2017, Istituto Nazionale Astrofisica (INAF) Agenzia Spaziale Italiana (ASI), 2018-16-HH.0, Swiss National Science Foundation (SNSF), 140649 152721 166227 184618, Fundação para a Ciência e a Tecnologia (FCT) through Investigador FCT, IF/00650/2015/CP1273/CT0001 IF/00849/2015/CP1273/CT0003 IF/00028/2014/CP1215/CT0002 IF/01312/2014/CP1215/CT0004 DL 57/2016/CP1364/CT0004, FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao, National Aeronautics and Space Administration (NASA), NNX17AB59G NAS5-26555 NNX13AC07G, Research Projects of National Relevance (PRIN), 201278X4FL, MCTES, PTDC/FIS-AST/32113/2017, European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES), ITA, USA, GBR, DEU, ESP, CHL, DNK, PRT, CHE, Mortier, Annelies [0000-0001-7254-4363], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, 530 Physics, stars: individual (K2-111), FOS: Physical sciences, Astrophysics, Spectroscopic, 01 natural sciences, spectroscopic [Techniques], techniques: photometric, Planet, individual [Stars], techniques: radial velocities, 0103 physical sciences, QB Astronomy, 010303 astronomy & astrophysics, QC, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], 520 Astronomy, individual (K2-111) [Stars], photometric [Techniques], Astronomy and Astrophysics, 3rd-DAS, Radius, 500 Science, Planetary system, 620 Engineering, Orbital period, Radial velocity, detection [Planets and satellites], Photometry (astronomy), QC Physics, 13. Climate action, Space and Planetary Science, astro-ph.EP, Terrestrial planet, techniques: spectroscopic, K2-111, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

This paper reports on the detailed characterisation of the K2-111 planetary system with K2, WASP, and ASAS-SN photometry as well as high-resolution spectroscopic data from HARPS-N and ESPRESSO. The host, K2-111, is confirmed to be a mildly evolved ($\log g=4.17$), iron-poor ([Fe/H]$=-0.46$), but alpha-enhanced ([$\alpha$/Fe]$=0.27$), chromospherically quiet, very old thick disc G2 star. A global fit, performed by using PyORBIT shows that the transiting planet, K2-111b, orbits with a period $P_b=5.3518\pm0.0004$ d, and has a planet radius of $1.82^{+0.11}_{-0.09}$ R$_\oplus$ and a mass of $5.29^{+0.76}_{-0.77}$ M$_\oplus$, resulting in a bulk density slightly lower than that of the Earth. The stellar chemical composition and the planet properties are consistent with K2-111b being a terrestrial planet with an iron core mass fraction lower than the Earth. We announce the existence of a second signal in the radial velocity data that we attribute to a non-transiting planet, K2-111c, with an orbital period of $15.6785\pm 0.0064$ days, orbiting in near-3:1 mean-motion resonance with the transiting planet, and a minimum planet mass of $11.3\pm1.1$ M$_\oplus$. Both planet signals are independently detected in the HARPS-N and ESPRESSO data when fitted separately. There are potentially more planets in this resonant system, but more well-sampled data are required to confirm their presence and physical parameters., Comment: Accepted for publication in MNRAS on 28 Sept 2020. Paper is 18 pages with an additional 12 pages of supplementary material. Data is available at https://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/MNRAS/499/5004

Published
2020
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6. Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESS

Author

Lacedelli, G, Wilson, TG, Malavolta, L, Hooton, MJ, Collier Cameron, A, Alibert, Y, Mortier, A, Bonfanti, A, Haywood, RD, Hoyer, S, Piotto, G, Bekkelien, A, Vanderburg, AM, Benz, W, Dumusque, X, Deline, A, Lopez-Morales, M, Borsato, L, Rice, K, Fossati, L, Latham, DW, Brandeker, A, Poretti, E, Sousa, SG, Sozzetti, A, Salmon, S, Burke, CJ, Van Grootel, V, Fausnaugh, MM, Adibekyan, V, Huang, CX, Osborn, HP, Mustill, AJ, Palle, E, Bourrier, V, Nascimbeni, V, Alonso, R, Anglada, G, Barczy, T, Barrado Y Navascues, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Billot, N, Bonfils, X, Broeg, C, Buchhave, LA, Cabrera, J, Charnoz, S, Cosentino, R, Csizmadia, S, Davies, MB, Deleuil, M, Delrez, L, Demangeon, O, Demory, BO, Ehrenreich, D, Erikson, A, Esparza-Borges, E, Floren, HG, Fortier, A, Fridlund, M, Futyan, D, Gandolfi, D, Ghedina, A, Gillon, M, Güdel, M, Guterman, P, Harutyunyan, A, Heng, K, Isaak, KG, Jenkins, JM, Kiss, L, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, Lovis, C, Magrin, D, Marafatto, L, Martinez Fiorenzano, AF, Maxted, PFL, Mayor, M, Micela, G, Molinari, E, Murgas, F, Narita, N, Olofsson, G, Ottensamer, R, Pagano, I, Pasetti, A, Pedani, M, Pepe, FA, Peter, G, Phillips, DF, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Ratti, F, Lacedelli, G [0000-0002-4197-7374], Wilson, TG [0000-0001-8749-1962], Malavolta, L [0000-0002-6492-2085], Hooton, MJ [0000-0003-0030-332X], Collier Cameron, A [0000-0002-8863-7828], Mortier, A [0000-0001-7254-4363], Borsato, L [0000-0003-0066-9268], Rice, K [0000-0002-6379-9185], Sousa, SG [0000-0001-9047-2965], Sozzetti, A [0000-0002-7504-365X], Osborn, HP [0000-0002-4047-4724], Mustill, AJ [0000-0002-2086-3642], Nascimbeni, V [0000-0001-9770-1214], Buchhave, LA [0000-0003-1605-5666], Csizmadia, S [0000-0001-6803-9698], Delrez, L [0000-0001-6108-4808], Gandolfi, D [0000-0001-8627-9628], Lendl, M [0000-0001-9699-1459], Maxted, PFL [0000-0003-3794-1317], and Apollo - University of Cambridge Repository

Subjects
techniques: photometric, stars: individual: TOI-561 (TIC 377064495, Gaia EDR3 3850421005290172416), techniques: radial velocities, planets and satellites: fundamental parameters, planets and satellites: interiors
Abstract

We present a precise characterization of the TOI-561 planetary system obtained by combining previously published data with TESS and CHEOPS photometry, and a new set of $62$ HARPS-N radial velocities (RVs). Our joint analysis confirms the presence of four transiting planets, namely TOI-561 b ($P = 0.45$ d, $R = 1.42$ R$_\oplus$, $M = 2.0$ M$_\oplus$), c ($P = 10.78$ d, $R = 2.91$ R$_\oplus$, $M = 5.4$ M$_\oplus$), d ($P = 25.7$ d, $R = 2.82$ R$_\oplus$, $M = 13.2$ M$_\oplus$) and e ($P = 77$ d, $R = 2.55$ R$_\oplus$, $M = 12.6$ M$_\oplus$). Moreover, we identify an additional, long-period signal ($>450$ d) in the RVs, which could be due to either an external planetary companion or to stellar magnetic activity. The precise masses and radii obtained for the four planets allowed us to conduct interior structure and atmospheric escape modelling. TOI-561 b is confirmed to be the lowest density ($\rho_{\rm b} = 3.8 \pm 0.5$ g cm$^{-3}$) ultra-short period (USP) planet known to date, and the low metallicity of the host star makes it consistent with the general bulk density-stellar metallicity trend. According to our interior structure modelling, planet b has basically no gas envelope, and it could host a certain amount of water. In contrast, TOI-561 c, d, and e likely retained an H/He envelope, in addition to a possibly large water layer. The inferred planetary compositions suggest different atmospheric evolutionary paths, with planets b and c having experienced significant gas loss, and planets d and e showing an atmospheric content consistent with the original one. The uniqueness of the USP planet, the presence of the long-period planet TOI-561 e, and the complex architecture make this system an appealing target for follow-up studies.

Published
2022

7. All-sky visible and near infrared space astrometry

Author

Łukasz Wyrzykowski, Erik Høg, Anthony G. A. Brown, Valeri V. Makarov, Barbara McArthur, Sergei A. Klioner, Nicholas A. Walton, Fran Jiménez-Esteban, Daniel Hestroffer, Jose A. Caballero, Johan P. U. Fynbo, Jan Rybizki, Oscar A. Gonzalez, Paolo Tanga, Yuan-Sen Ting, Nathan J. Secrest, Roger Mor, Antonella Vallenari, Alessandro Sozzetti, Mattia Vaccari, Carme Jordi, Naoteru Gouda, Cristina Chiappini, Lennart Lindegren, Jeff J. Andrews, David Hobbs, Anna M. Moore, Tomaž Zwitter, Paul J. McMillan, Daisuke Kawata, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Lund University, Hobbs, D [0000-0002-2696-1366], Apollo - University of Cambridge Repository, Hobbs, D. [0000-0002-2696-1366], Brown, A. [0000-0002-7419-9679], Sozzetti, A. [0000-0002-7504-365X], and Secrest, N. [0000-0002-4902-8077]

Subjects
Computer science, Milky Way, media_common.quotation_subject, Space Misiion, space mission, 01 natural sciences, Space mission, Galactic dynamics, Photometry, Observational astronomy, 0103 physical sciences, Space Astronometry, 010303 astronomy & astrophysics, media_common, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Space astrometry, Galactic dynamics, Near-infrared spectroscopy, Astronomy, Gaia, Astronomy and Astrophysics, Astrometry, Stars, Photometry (astronomy), Space and Planetary Science, Sky, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Space astrometry, Reference frame
Abstract

Hobbs, David, et al., The era of all-sky space astrometry began with the Hipparcos mission in 1989 and provided the first very accurate catalogue of apparent magnitudes, positions, parallaxes and proper motions of 120 000 bright stars at the milliarcsec (or milliarcsec per year) accuracy level. Hipparcos has now been superseded by the results of the Gaia mission. The second Gaia data release contained astrometric data for almost 1.7 billion sources with tens of microarcsec (or microarcsec per year) accuracy in a vast volume of the Milky Way and future data releases will further improve on this. Gaia has just completed its nominal 5-year mission (July 2019), but is expected to continue in operations for an extended period of an additional 5 years through to mid 2024. Its final catalogue to be released ∼ 2027, will provide astrometry for ∼ 2 billion sources, with astrometric precisions reaching 10 microarcsec. Why is accurate astrometry so important? The answer is that it provides fundamental data which underpin much of modern observational astronomy as will be detailed in this White Paper. All-sky visible and Near-InfraRed (NIR) astrometry with a wavelength cutoff in the K-band is not just focused on a single or small number of key science cases. Instead, it is extremely broad, answering key science questions in nearly every branch of astronomy while also providing a dense and accurate visible-NIR reference frame needed for future astronomy facilities., Open access funding provided by Lund University.

Published
2021
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8. HADES RV programme with HARPS-N at TNG: XIV. A candidate super-Earth orbiting the M-dwarf GJ 9689 with a period close to half the stellar rotation period

Author

J. Maldonado, A. Petralia, M. Damasso, M. Pinamonti, G. Scandariato, E. González-Álvarez, L. Affer, G. Micela, A. F. Lanza, G. Leto, E. Poretti, A. Sozzetti, M. Perger, P. Giacobbe, R. Zanmar Sánchez, A. Maggio, J. I. González Hernández, R. Rebolo, I. Ribas, A. Suárez-Mascareño, B. Toledo-Padrón, A. Bignamini, E. Molinari, E. Covino, R. Claudi, S. Desidera, E. Herrero, J. C. Morales, I. Pagano, G. Piotto, La Caixa, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Ministerio de Ciencia e Innovación (España), European Commission, Maldonado, J. [0000-0002-2218-5689], Petralia, A. [0000-0002-9882-1020], Damasso, M. [0000-0001-9984-4278], Pinamonti, M. [0000-0002-4445-1845], Affer, L. [0000-0001-5600-3778], Lanza, A. F. [0000-0001-5928-7251], Leto, G. [0000-0002-0040-5011], Poretti, E. [0000-0003-1200-0473], Sozzetti, A. [0000-0002-7504-365X], Perger, M. [0000-0001-7098-0372], Zanmar Sánchez, R. [0000-0002-6997-0887], Maggio, A. [0000-0001-5154-6108], González Hernández, J. I. [0000-0002-0264-7356], Ribas, I. [0000-0002-6689-0312], Toledo Padrón, B. [0000-0002-8194-215X], Bignamini, A. [0000-0002-5606-6354], Molinari, E. [0000-0002-1742-7735], Covino, E. [0000-0002-7579-2298], Claudi, R. [0000-0001-7707-5105], Desidera, S. [0000-0001-8613-2589], and Agencia Estatal de Investigación (AEI)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), GJ 9689, radial velocities [Techniques], 010308 nuclear & particles physics, Stars: individual, FOS: Physical sciences, Techniques: spectroscopic, Astronomy and Astrophysics, individual: GJ 9689 [Stars], Stars: late-type, 01 natural sciences, spectroscopic [Techniques], late type [Stars], Planetary systems, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [Stars], individual [Stars], Techniques: radial velocities, 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract

[Context] It is now well-established that small, rocky planets are common around low-mass stars. However, the detection of such planets is challenged by the short-term activity of host stars. [Aims] The HARPS-N red Dwarf Exoplanet Survey programme is a long-term project at the Telescopio Nazionale Galileo aimed at monitoring nearby, early-type, M dwarfs, using the HARPS-N spectrograph to search for small, rocky planets. [Methods] A total of 174 HARPS-N spectroscopic observations of the M0.5V-type star GJ 9689 taken over the past seven years have been analysed. We combined these data with photometric measurements to disentangle signals related to the stellar activity of the star from possible Keplerian signals in the radial velocity data. We ran an MCMC analysis, applying Gaussian process regression techniques to model the signals present in the data. [Results] We identify two periodic signals in the radial velocity time series, with periods of 18.27 and 39.31 d. The analysis of the activity indexes, photometric data, and wavelength dependency of the signals reveals that the 39.31 d signal corresponds to the stellar rotation period. On the other hand, the 18.27 d signal shows no relation to any activity proxy or the first harmonic of the rotation period. We, therefore, identify it as a genuine Keplerian signal. The best-fit model describing the newly found planet, GJ 9689 b, corresponds to an orbital period of Pb = 18.27 ± 0.01 d and a minimum mass of MP sini = 9.65 ± 1.41 M⊕., J.M. and G.M. acknowledge support from the accordo attua-tivo ASI-INAF n.2021-5-HH.0 “Partecipazione italiana alla fase B2/C della mis-sione Ariel”. A.P., A.M., M.P., and A.S. acknowledge partial contribution from the agreement ASI-INAF n.2018-16-HH.0. E.G.A. acknowledges support from the Spanish Ministery for Science, Innovation, and Universities through projects AYA-2016-79425-C3-1/2/3-P, AYA2015-69350-C3-2-P, ESP2017-87676-C5-2-R, ESP2017-87143-R. The Centro de Astrobiología (CAB, CSIC-INTA) is a Center of Excellence “Maria de Maeztu”. M.P and I.R acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-BC33, as well as the support of the Generalitat de Catalunya/CERCA programme. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramón y Cajal program RYC-2013-14875. B.T.P. acknowledges Fundación La Caixa for the financial support received in the form of a Ph.D. contract. A.S.M. acknowledges financial support from the Spanish MICINN under the 2019 Juan de la Cierva Programme. B.T.P., A.S.M., J.I.G.H., R.R. acknowledge financial support from the Spanish MICINN AYA2017-86389-P. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/ gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Published
2021

9. The atmosphere of HD 209458b seen with ESPRESSO. No detectable planetary absorptions at high resolution

Author

Vardan Adibekyan, M. R. Zapatero Osorio, Yann Alibert, P. Di Marcantonio, François Bouchy, Cristina Martins, N. Casasayas-Barris, Francesco Borsa, Andrea Mehner, Giuseppina Micela, Paolo Molaro, S. Cristiani, Francesco Pepe, Nuno C. Santos, J. Lillo-Box, C. Lovis, Enric Palle, Vincent Bourrier, G. Lo Curto, Gang Chen, Rafael Rebolo, Fei Yan, O. D. S. Demangeon, J. I. González Hernández, V. D Odorico, Stéphane Udry, M. Stangret, S. G. Sousa, Mahmoudreza Oshagh, C. Allende Prieto, B. Lavie, A. Suárez Mascareño, P. Figueira, Alessandro Sozzetti, David Ehrenreich, R. Génova Santos, Romain Allart, Nelson J. Nunes, Hugo M. Tabernero, E. Poretti, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Yan, F. [0000-0001-9585-9034], Sozzetti, A. [0000-0002-7504-365X], Nunes, N. [0000-0002-3837-6914], Santos, N. [0000-0003-4422-2919], National Natural Science Foundation of China (NSFC), Deutsche Forschungsgemeinschaft (DFG), European Research Council (ERC), Fundacao para a Ciencia e a Tecnologia (FCT), Istituto Nazionale di Astrofisica (INAF), Agencia Estatal de Investigación (AEI), Swiss National Science Foundation (SNSF), ITA, ESP, PRT, and CHE

Subjects
individual: HD 209458b [Planets and satellites], Absorption spectroscopy, Gas giant, FOS: Physical sciences, Astrophysics, 01 natural sciences, Astronomical spectroscopy, spectroscopic [Techniques], Atmosphere, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, observational [Methods], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Line (formation), Physics, Earth and Planetary Astrophysics (astro-ph.EP), Atmospheric models, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, atmospheres [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We observed two transits of the iconic gas giant HD 209458b between 380 and 780 nm, using the high-resolution ESPRESSO spectrograph. The derived planetary transmission spectrum exhibits features at all wavelengths where the parent star shows strong absorption lines, for example, NaI, MgI, FeI, FeII, CaI, VI, H$\alpha$, and KI. We interpreted these features as the signature of the deformation of the stellar line profiles due to the Rossiter-McLaughlin effect, combined with the centre-to-limb effects on the stellar surface, which is in agreement with similar reports recently presented in the literature. We also searched for species that might be present in the planetary atmosphere but not in the stellar spectra, such as TiO and VO, and obtained a negative result. Thus, we find no evidence of any planetary absorption, including previously reported NaI, in the atmosphere of HD 209458b. The high signal-to-noise ratio in the transmission spectrum allows us to compare the modelled deformation of the stellar lines in assuming different one-dimensional stellar atmospheric models. We conclude that the differences among various models and observations remain within the precision limits of the data. However, the transmission light curves are better explained when the centre-to-limb variation is not included in the computation and only the Rossiter-McLaughlin deformation is considered. This demonstrates that ESPRESSO is currently the best facility for spatially resolving the stellar surface spectrum in the optical range using transit observations and carrying out empirical validations of stellar models., Comment: 21 pages, 19 figures. Accepted

Published
2021

10. TOI-1634 b: An Ultra-short-period Keystone Planet Sitting inside the M-dwarf Radius Valley

Author

Gilbert A. Esquerdo, Walter Boschin, Lars A. Buchhave, Allyson Bieryla, Karen A. Collins, Eric L. N. Jensen, Nobuhiko Kusakabe, David F. Phillips, Chelsea X. Huang, Jack J. Lissauer, Steve B. Howell, Norio Narita, E. Girardin, Christopher A. Watson, Enric Palle, Damien Ségransan, R. D. Haywood, P. Guerra, David W. Latham, S. Giacalone, Jonathan Irwin, Avi Shporer, Keivan G. Stassun, Giampaolo Piotto, E. Esparza-Borges, Gloria Andreuzzi, Felipe Murgas, Marco Pedani, Francesco Pepe, Mercedes Lopez-Morales, Scott McDermott, Courtney D. Dressing, Robert Massey, Motohide Tamura, George R. Ricker, Annelies Mortier, Giuseppina Micela, Jessie L. Christiansen, Emilio Molinari, Pau Bosch-Cabot, Jon M. Jenkins, Roland Vanderspek, Aldo F. M. Fiorenzano, Samuel N. Quinn, Hannu Parviainen, Ken Rice, Avet Harutyunyan, Akihiko Fukui, Sara Seager, Elisa V. Quintana, Massimo Cecconi, Mark E. Rose, R. Cloutier, Luca Di Fabrizio, Joshua N. Winn, Alessandro Sozzetti, Arjun B. Savel, Andrew Collier Cameron, David Charbonneau, Rachel A. Matson, Michel Mayor, Dimitar Sasselov, Christophe Lovis, Stéphane Udry, Gábor Fűrész, Xavier Dumusque, Cloutier, R [0000-0001-5383-9393], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Murgas, F [0000-0001-9087-1245], Mortier, A [0000-0001-7254-4363], Massey, R [0000-0001-8879-7138], Lissauer, JJ [0000-0001-6513-1659], Latham, DW [0000-0001-9911-7388], Haywood, RD [0000-0001-9140-3574], Guerra, P [0000-0002-4308-2339], Giacalone, SA [0000-0002-8965-3969], Bieryla, A [0000-0001-6637-5401], Winn, J [0000-0002-4265-047X], Watson, CA [0000-0002-9718-3266], Vanderspek, R [0000-0001-6763-6562], Udry, S [0000-0001-7576-6236], Tamura, M [0000-0002-6510-0681], Sozzetti, A [0000-0002-7504-365X], Shporer, A [0000-0002-1836-3120], Ségransan, D [0000-0003-2355-8034], Seager, S [0000-0002-6892-6948], Savel, AB [0000-0002-2454-768X], Sasselov, D [0000-0001-7014-1771], Rose, M [0000-0003-4724-745X], Ricker, G [0000-0003-2058-6662], Rice, K [0000-0002-6379-9185], Quintana, EV [0000-0003-1309-2904], Quinn, SN [0000-0002-8964-8377], Piotto, G [0000-0002-9937-6387], Phillips, D [0000-0001-5132-1339], Pedani, M [0000-0002-5752-6260], Parviainen, H [0000-0001-5519-1391], Palle, E [0000-0003-0987-1593], Narita, N [0000-0001-8511-2981], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], Mayor, M [0000-0002-9352-5935], Matson, RA [0000-0001-7233-7508], López-Morales, M [0000-0003-3204-8183], Kusakabe, N [0000-0001-9194-1268], Jensen, ELN [0000-0002-4625-7333], Jenkins, JM [0000-0002-4715-9460], Huang, CX [0000-0003-0918-7484], Howell, SB [0000-0002-2532-2853], Fukui, A [0000-0002-4909-5763], Esquerdo, GA [0000-0002-9789-5474], Esparza-Borges, E [0000-0002-2341-3233], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Collins, KA [0000-0001-6588-9574], Cameron, AC [0000-0002-8863-7828], Christiansen, JL [0000-0002-8035-4778], Buchhave, LA [0000-0003-1605-5666], Boschin, W [0000-0001-9978-9109], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Radius, 3rd-DAS, Sitting, Exoplantet strcuture, QC Physics, Space and Planetary Science, Planet, astro-ph.EP, Period (geology), QB Astronomy, Planetary system formation, Low mass stars, Astrophysics::Earth and Planetary Astrophysics, Transit photometry, QC, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Studies of close-in planets orbiting M dwarfs have suggested that the M dwarf radius valley may be well-explained by distinct formation timescales between enveloped terrestrials, and rocky planets that form at late times in a gas-depleted environment. This scenario is at odds with the picture that close-in rocky planets form with a primordial gaseous envelope that is subsequently stripped away by some thermally-driven mass loss process. These two physical scenarios make unique predictions of the rocky/enveloped transition's dependence on orbital separation such that studying the compositions of planets within the M dwarf radius valley may be able to establish the dominant physics. Here, we present the discovery of one such keystone planet: the ultra-short period planet TOI-1634 b ($P=0.989$ days, $F=121 F_{\oplus}$, $r_p = 1.790^{+0.080}_{-0.081} R_{\oplus}$) orbiting a nearby M2 dwarf ($K_s=8.7$, $R_s=0.45 R_{\odot}$, $M_s=0.50 M_{\odot}$) and whose size and orbital period sit within the M dwarf radius valley. We confirm the TESS-discovered planet candidate using extensive ground-based follow-up campaigns, including a set of 32 precise radial velocity measurements from HARPS-N. We measure a planetary mass of $4.91^{+0.68}_{-0.70} M_{\oplus}$, which makes TOI-1634 b inconsistent with an Earth-like composition at $5.9\sigma$ and thus requires either an extended gaseous envelope, a large volatile-rich layer, or a rocky portion that is not dominated by iron and silicates to explain its mass and radius. The discovery that the bulk composition of TOI-1634 b is inconsistent with that of the Earth favors the gas-depleted formation mechanism to explain the emergence of the radius valley around M dwarfs with $M_s\lesssim 0.5 M_{\odot}$., Comment: 27 pages, 13 figures, accepted to AAS journals. Our time series are included as a csv file in the arXiv source files

Published
2021
Full Text
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11. Detection Limits of Low-mass, Long-period Exoplanets Using Gaussian Processes Applied to HARPS-N Solar Radial Velocities

Author

Christopher A. Watson, M. Lopez-Morales, Massimo Cecconi, L. Malavolta, R. D. Haywood, Timothy Milbourne, M. Gonzalez, Dimitar Sasselov, David F. Phillips, Xavier Dumusque, J. Maldonado, Ken Rice, H. M. Cegla, S. H. Saar, Stéphane Udry, Rosario Cosentino, D. W. Latham, N. Buchschacher, Elisa Molinari, Ronald L. Walsworth, Adriano Ghedina, Giuseppina Micela, Francesco Pepe, Alessandro Sozzetti, C. H. Li, Susan E. Thompson, D. Charbonneau, E. Poretti, Annelies Mortier, Nicholas Langellier, A. Collier Cameron, Marcello Lodi, Langellier, N [0000-0003-2107-3308], Milbourne, TW [0000-0001-5446-7712], Phillips, DF [0000-0001-5132-1339], Haywood, RD [0000-0001-9140-3574], Saar, SH [0000-0001-7032-8480], Mortier, A [0000-0001-7254-4363], Malavolta, L [0000-0002-6492-2085], Thompson, S [0000-0002-8039-194X], Cameron, AC [0000-0002-8863-7828], Dumusque, X [0000-0002-9332-2011], Cegla, HM [0000-0001-8934-7315], Latham, DW [0000-0001-9911-7388], Maldonado, J [0000-0002-2218-5689], Buchschacher, N [0000-0002-3697-1541], Cecconi, M [0000-0001-5701-2529], Charbonneau, D [0000-0002-9003-484X], Cosentino, R [0000-0003-1784-1431], Ghedina, A [0000-0003-4702-5152], Lodi, M [0000-0002-5432-9659], López-Morales, M [0000-0003-3204-8183], Micela, G [0000-0002-9900-4751], Molinari, E [0000-0002-1742-7735], Poretti, E [0000-0003-1200-0473], Rice, K [0000-0002-6379-9185], Sasselov, D [0000-0001-7014-1771], Sozzetti, A [0000-0002-7504-365X], Udry, S [0000-0001-7576-6236], Walsworth, RL [0000-0003-0311-4751], Apollo - University of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
Radial velocity, astro-ph.SR, Solar activity, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 010309 optics, symbols.namesake, Long period, 0103 physical sciences, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, Gaussian regression, 010303 astronomy & astrophysics, Gaussian process, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Detection limit, Exoplanets, DAS, Astronomy and Astrophysics, Exoplanet, QC Physics, 13. Climate action, Space and Planetary Science, astro-ph.EP, symbols, Astrophysics::Earth and Planetary Astrophysics, Low Mass, astro-ph.IM
Abstract

Funding: A.C.C. acknowledges support from the Science and Technology Facilities Council (STFC) consolidated grant No. ST/R000824/1. Radial velocity (RV) searches for Earth-mass exoplanets in the habitable zone around Sun-like stars are limited by the effects of stellar variability on the host star. In particular, suppression of convective blueshift and brightness inhomogeneities due to photospheric faculae/plage and starspots are the dominant contribution to the variability of such stellar RVs. Gaussian process (GP) regression is a powerful tool for statistically modeling these quasi-periodic variations. We investigate the limits of this technique using 800 days of RVs from the solar telescope on the High Accuracy Radial velocity Planet Searcher for the Northern hemisphere (HARPS-N) spectrograph. These data provide a well-sampled time series of stellar RV variations. Into this data set, we inject Keplerian signals with periods between 100 and 500 days and amplitudes between 0.6 and 2.4 m s−1. We use GP regression to fit the resulting RVs and determine the statistical significance of recovered periods and amplitudes. We then generate synthetic RVs with the same covariance properties as the solar data to determine a lower bound on the observational baseline necessary to detect low-mass planets in Venus-like orbits around a Sun-like star. Our simulations show that discovering planets with a larger mass (~0.5 m s−1) using current-generation spectrographs and GP regression will require more than 12 yr of densely sampled RV observations. Furthermore, even with a perfect model of stellar variability, discovering a true exo-Venus (~0.1 m s−1) with current instruments would take over 15 yr. Therefore, next-generation spectrographs and better models of stellar variability are required for detection of such planets. Postprint

Published
2021
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12. The Galactic Anticentre

Author

Vincenzo Ripepi, A. de Torres, Annie C. Robin, Mariateresa Crosta, C. Diener, L. Noval, Daniel Michalik, P. J. Richards, L. Karbevska, K. Kruszyńska, E. Fraile, André Moitinho, Michał Pawlak, P. Panuzzo, M. Riello, Benoit Carry, A. Yoldas, Harry Enke, N. Tonello, P. Gavras, M. Vaillant, Rosanna Sordo, E. del Pozo, Lorenzo Rimoldini, M. Bernet, G. Orrù, W. van Reeven, J. M. Martín-Fleitas, S. Diakite, P. Burgess, P. Osborne, Derek W. Morris, M. I. Carnerero, Amina Helmi, Mike Smith, Iain A. Steele, Alessandro Sozzetti, M. Kontizas, A. Sagristà Sellés, Roberto Molinaro, B. Holl, D. Baines, D. Molina, J. Fernández-Hernández, S. Marinoni, Michele Bellazzini, Maria Süveges, Teresa Antoja, D. Barbato, Uwe Lammers, Isabella Pagano, Davide Massari, G. Plum, P. Ramos, G. Jevardat de Fombelle, M. Biermann, C. Crowley, Mathias Schultheis, D. W. Evans, P. A. Palicio, Paolo Montegriffo, Ramachrisna Teixeira, R. Blomme, Elmé Breedt, T. A. Lister, F. A. Jansen, Ruth Carballo, Marcella Marconi, A. Abreu Aramburu, J. M. Carrasco, F. Royer, S. Accart, A. Burlacu, S. Regibo, Andrej Prsa, M. Sarasso, Nicolas Rambaux, A. F. Mulone, Ana Ulla, Eric Gosset, Alessandra Mastrobuono-Battisti, George M. Seabroke, H. E. Delgado, Federico Marocco, C. Nicolas, T. Lebzelter, Nami Mowlavi, C. Barache, Nicoletta Sanna, G. Gracia-Abril, R. Santoveña, R. Haigron, N. Unger, Silvio Leccia, A. Jean-Antoine Piccolo, A. F. Lanza, Alberto Vecchiato, Thomas Wevers, F. Figueras, G. Busso, C. Fabre, P. Di Matteo, F. Riclet, F. Solitro, Eric Slezak, N. Samaras, João Alves, Emese Plachy, Timo Prusti, F. van Leeuwen, J. Osinde, O. Marchal, M. Ajaj, C. Ducourant, Tatiana Muraveva, Shay Zucker, H. Steidelmüller, Alberto Riva, D. Semeux, N. Cheek, Laurent Galluccio, Martin A. Barstow, Alex Bombrun, S. Liao, M. van Leeuwen, R. E. de Souza, P. de Laverny, T. Roegiers, Paul J. McMillan, G. Holland, Alexey Mints, G. Giuffrida, L. M. Sarro, Juan Zorec, G. Sadowski, P. Yvard, Carme Jordi, J. L. Halbwachs, Laurent Chemin, Ludovic Delchambre, M. Garcia-Reinaldos, Ugo Becciani, Diego Bossini, Ángel Gómez, Sergi Blanco-Cuaresma, Rossella Cancelliere, C. Fabricius, J. De Ridder, L. Eyer, L. Pulone, Simon Hodgkin, Ennio Poretti, F. De Angeli, M. Haywood, E. Anglada Varela, Antonella Vallenari, F. X. Pineau, D. Garabato, A. Guerrier, H. E. P. Lindstrøm, Thomas Hilger, I. Bellas-Velidis, Frédéric Arenou, Paolo Giacobbe, Ilaria Musella, Tristan Cantat-Gaudin, L. Palaversa, Pedro García-Lario, David Hobbs, C. Turon, E. Balbinot, P. de Teodoro, Sébastien Lambert, D. Katz, Angela Bragaglia, Anthony G. A. Brown, Paolo Tanga, P. Castro Sampol, J. C. Segovia, Alejandra Recio-Blanco, Yves Fremat, Jon Marchant, Jose M Hernandez, S. Ragaini, Sofia Randich, P. Re Fiorentin, J. F. Le Campion, Gisella Clementini, M. Segol, P. David, R. Drimmel, F. Crifo, J. Guiraud, M. David, R. L. Smart, M. Fabrizio, I. Gonzalez-Santamaria, D. Eappachen, M. G. Lattanzi, Miguel García-Torres, Andreas Korn, S. Voutsinas, László Molnár, Simchon Faigler, A. Mora, Nicholas Rowell, Antti Penttilä, R. Geyer, Sanjeev Khanna, Aldo Dell'Oro, H. E. Huckle, C. Dolding, N. Leclerc, Monica Rainer, R. Mor, J. Bakker, Maroussia Roelens, Douglas J. Marshall, A. G. Butkevich, Nigel Hambly, A. Masip, Laia Casamiquela, R. Messineo, Martin Altmann, A. M. Piersimoni, Alessandro Spagna, Gerry Gilmore, Stefano Bertone, Patrick Charlot, O. Vanel, Daniel Hestroffer, Marco Castellani, Sebastian L. Hidalgo, W. Roux, Łukasz Wyrzykowski, Krzysztof A. Rybicki, M. M. S. Marcos Santos, Raphael Guerra, Alberto Cellino, E. Poggio, Gérard Jasniewicz, J. J. González-Vidal, S. Cowell, Peter G. Jonker, C. M. Raiteri, S. Bartolomé, J. Álvarez Cid-Fuentes, Elisabetta Caffau, J. J. Aguado, N. R. Millar, Ulrike Heiter, Federica Spoto, Felix Franke, A. Baudesson-Stella, M. Barros, Tsevi Mazeh, A. Panahi, E. Brugaletta, R. Buzzi, Elena Pancino, G. Altavilla, E. Racero, Enrique Solano, Mikael Granvik, Minia Manteiga, C. Robin, Tomaz Zwitter, Deborah Busonero, Alberto Krone-Martins, Marc Audard, Kevin Benson, Christos Siopis, L. Balaguer-Núñez, C. A. L. Bailer-Jones, E. Poujoulet, O. L. Creevey, E. Szegedi-Elek, C. Fouron, Michael Davidson, E. Licata, Despina Hatzidimitriou, Mark Cropper, Z. Kostrzewa-Rutkowska, S. Managau, A. Dapergolas, Sergio Messina, Laszlo Szabados, H. I. Siddiqui, W. Löffler, Mario Gai, J.-B. Delisle, Leanne P. Guy, S. G. Baker, W. J. Cooper, Alfred Castro-Ginard, Conny Aerts, A. Lorca, Xavier Luri, Damien Ségransan, Grigori Fedorets, A. Garofalo, J. Juaristi Campillo, F. De Luise, F. Pailler, F. Taris, L. Bramante, Thierry Morel, T. Cornez, L. Martin Polo, M. Ramos-Lerate, Jordi Portell, E. Salguero, Sergei A. Klioner, K. Janßen, Ulrich Bastian, Stefan Jordan, P. Esquej, A. C. Lanzafame, Beatrice Bucciarelli, C. Panem, Y. Lebreton, Carlos Dafonte, S. Girona, D. Munoz, Dimitri Pourbaix, William Thuillot, J. H. J. de Bruijne, N. Brouillet, L. Chaoul, F. Torra, Alex Lobel, J.-L. Bassilana, Francesca Fragkoudi, M. Romero-Gómez, C. A. Stephenson, T. Pauwels, Eva Sciacca, Alessandro Bressan, Morgan Fouesneau, E. Livanou, E. Gerlach, X. Peñalosa Esteller, Roberto Morbidelli, L. Rohrbasser, Johannes Sahlmann, Elisa Distefano, P. Sartoretti, Karri Muinonen, Zoltan Balog, Y. Viala, J. Torra, H. Zhao, L. Siltala, G. Tauran, D. Souami, P. Madrero Pardo, David Teyssier, Jesus Salgado, J. Souchay, C. P. Murphy, Maria-Rosa L. Cioni, N. A. Walton, S. Bouquillon, Andrea Chiavassa, Agnes Fienga, Giovanni Comoretto, F. Julbe, A. Hutton, Yassine Damerdji, Richard I. Anderson, Pierre Fernique, Céline Reylé, M. Hauser, E. Utrilla, Pierre Kervella, C. Zurbach, Robert G. Mann, Ummi Abbas, Hector Canovas, D. L. Harrison, Y. Lasne, Mark Taylor, Y. Le Fustec, E. F. del Peloso, N. Bauchet, E. van Dillen, Jan Rybizki, N. Hładczuk, T. Boch, J. González-Núñez, Carine Babusiaux, C. Pagani, Krzysztof Nienartowicz, Eduard Masana, G. Kordopatis, N. Robichon, Luciana Bianchi, R. Gutiérrez-Sánchez, Arnaud Siebert, A. Kochoska, T. Carlucci, Jérôme Berthier, J. Castañeda, D. Vicente, R. De March, A. Garcia-Gutierrez, M. Weiler, F. Thévenin, Lennart Lindegren, Isabelle Lecoeur-Taïbi, Guy Rixon, Francois Mignard, P. M. Marrese, M. A. Álvarez, Caroline Soubiran, Rene Andrae, C. Ordénovic, A. Delgado, V. Sanchez Gimenez, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Universidad de Barcelona, Xunta de Galicia, European Commission, Centros de Excelencia Severo Ochoa, BARCELONA SUPERCOMPUTING CENTER (BSC), SEV2015-0493, Krone Martins, A. [0000-0002-2308-6623], McMillan, P. [0000-0002-8861-2620], Carrasco Martínez, J. P. [0000-0002-3029-5853], Sozzetti, A. [0000-0002-7504-365X], Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MINECO/ICTI2013-2016/MDM-2014-0369, Centrode Excelencia Científica Instituto de Ciencias del Cosmos Universidad de Barcelona, MINECO/ICTI2013-2016/SEV2015-0493, Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES), National Natural Science Foundation of China (NSFC), Estonian Ministry of Education and Research, Centre National D'Etudes Spatiales (CNES), Agence Nationale de la Recherche (ANR), Centre National de la Recherche Scientifique (CNRS), European Commission (EC), European Research Council (ERC), Institut des Sciences de l'Univers (INSU), Institut National Polytechnique (INP), Institut National de Physique nucleaire et de Physique des Particules (IN2P3), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Hungarian Academy of Sciences, Hungarian National Research, Development, and Innovation Office (NKFIH), Science Foundation Ireland (SFI), Israel Science Foundation (ISF), Agenzia Spaziale Italiana (ASI), Italian Istituto Nazionale di Astrofisica (INAF), Netherlands Organisation for Scientific Research (NWO), Polish National Science Centre, Ministry of Science and Higher Education (MNiSW), Fundacao para a Ciencia e a Tecnologia (FCT), Slovenian Research Agency, Agencia Estatal de Investigación (AEI), Generalitat de Catalunya, United Kingdom Science and Technology Facilities Council (STFC), United Kingdom Space Agency (UKSA), Gaia Collaboration, Universidad de Cantabria, Astronomy, Kapteyn Astronomical Institute, Institut de Ciencies del Cosmos (ICCUB), Universitat de Barcelona (UB), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), M2A 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Planetary-system research, Department of Physics, Particle Physics and Astrophysics, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), and Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
trigonometric parallaxes, SOLAR NEIGHBORHOOD, Astronomy, SAGITTARIUS DWARF GALAXY, Astrophysics, 01 natural sciences, sagittarius dwarf galaxy, 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], solar neighborhood, Astrophysics::Instrumentation and Methods for Astrophysics, Astrometry, Gelexy: kinematics and dynamics, Kinematics and Dynamics, Open clusters and asssociations: individual: Berkeley 29, sky survey, Disk, Physical Sciences, kinematics and dynamics [Gelexy], old open clusters, MILKY-WAY, Astrophysics::Earth and Planetary Astrophysics, open clusters and associations: individual: Berkeley 29, Galaxy: kinematics and dynamics, disk [Galaxy], individual: Berkeley 29 [open clusters and associations], Astrometria, Berkeley 29, EXPLORING HALO SUBSTRUCTURE, LOCAL KINEMATICS, Milky Way, FOS: Physical sciences, Open Clusters and Associations, Individual, exploring halo substructure, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Computer Science::Digital Libraries, stellar structure, Galaxy: disk, Open clusters and associations: individual: Saurer 1, Galactic halo, Halo, Settore FIS/05 - Astronomia e Astrofisica, individual: Berkeley 29 [Open clusters and asssociations], 0103 physical sciences, distances [stars], halo [Galaxy], Disc, Stars: distances, milky-way, Saurer 1, Astrophysics::Galaxy Astrophysics, canis-major, Science & Technology, 010308 nuclear & particles physics, TRIGONOMETRIC PARALLAXES, Galaxy: halo, stars: distances, open clusters and associations: individual: Saurer 1, Astrophysics - Astrophysics of Galaxies, Astronomy and Astrophysics, Galactic plane, kinematics and dynamics [Galaxy], 115 Astronomy, Space science, CANIS-MAJOR, Stars, Galaxy, Physics::History of Physics, Estels, individual: Saurer 1 [open clusters and associations], Distances, local kinematics, OLD OPEN CLUSTERS, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SKY SURVEY, Open cluster, STELLAR STRUCTURE
Abstract

Aims. We aim to demonstrate the scientific potential of the Gaia Early Data Release 3 (EDR3) for the study of different aspects of the Milky Way structure and evolution and we provide, at the same time, a description of several practical aspects of the data and examples of their usage., Methods. We used astrometric positions, proper motions, parallaxes, and photometry from EDR3 to select different populations and components and to calculate the distances and velocities in the direction of the anticentre. In this direction, the Gaia astrometric data alone enable the calculation of the vertical and azimuthal velocities; also, the extinction is relatively low compared to other directions in the Galactic plane. We then explore the disturbances of the current disc, the spatial and kinematical distributions of early accreted versus in situ stars, the structures in the outer parts of the disc, and the orbits of open clusters Berkeley 29 and Saurer 1., Results. With the improved astrometry and photometry of EDR3, we find that: (i) the dynamics of the Galactic disc are very complex with oscillations in the median rotation and vertical velocities as a function of radius, vertical asymmetries, and new correlations, including a bimodality with disc stars with large angular momentum moving vertically upwards from below the plane, and disc stars with slightly lower angular momentum moving preferentially downwards; (ii) we resolve the kinematic substructure (diagonal ridges) in the outer parts of the disc for the first time; (iii) the red sequence that has been associated with the proto-Galactic disc that was present at the time of the merger with Gaia-Enceladus-Sausage is currently radially concentrated up to around 14 kpc, while the blue sequence that has been associated with debris of the satellite extends beyond that; (iv) there are density structures in the outer disc, both above and below the plane, most probably related to Monoceros, the Anticentre Stream, and TriAnd, for which the Gaia data allow an exhaustive selection of candidate member stars and dynamical study; and (v) the open clusters Berkeley 29 and Saurer 1, despite being located at large distances from the Galactic centre, are on nearly circular disc-like orbits., Conclusions. Even with our simple preliminary exploration of the Gaia EDR3, we demonstrate how, once again, these data from the European Space Agency are crucial for our understanding of the different pieces of our Galaxy and their connection to its global structure and history.

Published
2021
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13. A sub-Neptune and a non-transiting Neptune-mass companion unveiled by ESPRESSO around the bright late-F dwarf HD 5278 (TOI-130)

Author

J. I. González Hernández, Thomas Barclay, Yann Alibert, George R. Ricker, Keivan G. Stassun, Paolo Molaro, Stefano Cristiani, J. Haldemann, Jorge Lillo-Box, M. Fasnaugh, Giuseppina Micela, Stéphane Udry, François Bouchy, Baptiste Lavie, Enric Palle, G. Lo Curto, S. G. Sousa, J. F. Otegi, Francesco Pepe, Mahmoudreza Oshagh, Rafael Rebolo, Valentina D'Odorico, Jon M. Jenkins, Pedro Figueira, Nuno C. Santos, Carlos Martins, Nelson J. Nunes, Daniel Conde Rodriguez, Aldo S. Bonomo, David Ehrenreich, Joshua N. Winn, Mario Damasso, Ennio Poretti, Romain Allart, A. Suárez Mascareño, C. Lovis, Alexandre Cabral, J. D. Twicken, V. Adibekyan, Sara Seager, David R. Ciardi, M. R. Zapatero Osorio, P. Di Marcantonio, S. C. C. Barros, D. Mégevand, Alessandro Sozzetti, David W. Latham, Andrea Mehner, Sozzetti, A. [0000-0002-7504-365X], Nunes, N. [0000-0002-3837-6914], Haldemann, J. [0000-0003-1231-2389], Istituto Nazionale di Astrofisica (INAF), Agenzia Spaziale Italiana (ASI), iss National Science Foundation (SNSF), Fundacao para a Ciencia e a Tecnologia (FCT), European Commission (EC), European Research Council (ERC), Ministerio de Economía y Competitividad (MINECO), and Agencia Estatal de Investigación (AEI) http://dx.doi.org/10.13039/501100011033

Subjects
530 Physics, FOS: Physical sciences, Astrophysics, 01 natural sciences, individual: HD 5278 (TOI-130) [Stars], Espresso, Neptune, 0103 physical sciences, miscellaneous [Methods], 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], 010308 nuclear & particles physics, 520 Astronomy, photometric [Techniques], Astronomy and Astrophysics, Planetary system, 500 Science, 620 Engineering, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, composition [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. Transiting sub-Neptune-type planets, with radii approximately between 2 and 4 R⊕, are of particular interest as their study allows us to gain insight into the formation and evolution of a class of planets that are not found in our Solar System. Aims. We exploit the extreme radial velocity (RV) precision of the ultra-stable echelle spectrograph ESPRESSO on the VLT to unveil the physical properties of the transiting sub-Neptune TOI-130 b, uncovered by the TESS mission orbiting the nearby, bright, late F-type star HD 5278 (TOI-130) with a period of Pb = 14.3 days. Methods. We used 43 ESPRESSO high-resolution spectra and broad-band photometry information to derive accurate stellar atmospheric and physical parameters of HD 5278. We exploited the TESS light curve and spectroscopic diagnostics to gauge the impact of stellar activity on the ESPRESSO RVs. We performed separate as well as joint analyses of the TESS photometry and the ESPRESSO RVs using fully Bayesian frameworks to determine the system parameters. Results. Based on the ESPRESSO spectra, the updated stellar parameters of HD 5278 are Teff = 6203 ± 64 K, log g = 4.50 ± 0.11 dex, [Fe/H] = −0.12 ± 0.04 dex, M⋆ = 1.126−0.035+0.036 M⊙, and R⋆ = 1.194−0.016+0.017 R⊙. We determine HD 5278 b’s mass and radius to be Mb = 7.8−1.4+1.5 M⊕ and Rb = 2.45 ± 0.05R⊕. The derived mean density, ϱb = 2.9−0.5+0.6 g cm−3, is consistent with the bulk composition of a sub-Neptune with a substantial (~ 30%) water mass fraction and with a gas envelope comprising ~17% of the measured radius. Given the host brightness and irradiation levels, HD 5278 b is one of the best targetsorbiting G-F primaries for follow-up atmospheric characterization measurements with HST and JWST. We discover a second, non-transiting companion in the system, with a period of Pc = 40.87−0.17+0.18 days and a minimum mass of Mc sin ic = 18.4−1.9+1.8 M⊕. We study emerging trends in parameters space (e.g., mass, radius, stellar insolation, and mean density) of the growing population of transiting sub-Neptunes, and provide statistical evidence for a low occurrence of close-in, 10 − 15M⊕ companions around G-F primaries with Teff ≳ 5500 K. The authors acknowledge the ESPRESSO project team for its effort and dedication in building the ESPRESSO instrument. This work has received financial support from the ASI-INAF agreement no. 2018-16-HH.0. M.D. acknowledges financial support from the FP7-SPACE Project ETAEARTH (GA No. 313014). A.S. We gratefully acknowledges support from the Italian Space Agency (ASI) under contract 2018-24-HH.0. The INAF authors acknowledge financial support of the Italian Ministry of Education, University, and Research with PRIN 201278X4FL and the Progetti Premiali funding scheme.to acknowledge the Swiss National Science Foundation (SNSF) for supporting research with ESPRESSO through the SNSF grants no. 140649, 152721, and 166227. The ESPRESSO Instrument Project was partially funded through SNSF's FLARE Programme for large infrastructures. This work has been carried out in part within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. This work was supported by FCT -Funda cao para a Ciencia e Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionaliza cao by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987; PTDC/FIS-OUT/29048/2017 & IF/00852/2015. S.C.C.B. acknowledges support from FCT through contract nr. IF/01312/2014/CP1215/CT0004. S.G.S acknowledges the support from FCT through Investigator FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). 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). V.A. acknowledges the support from FCT through Investigator FCT contract nr. IF/00650/2015/CP1273/CT0001. Y.A. and J.H. acknowledge the Swiss National Science Foundation (SNSF) for supporting research through the SNSF grant 200 020_192038. J.I.G.H. acknowledges financial support from Spanish Ministry of Science and Innovation (MICINN) under the 2013 Ramon y Cajal programme RYC-2013-14 875. J.I.G.H., A.S.M., R.R., and C.A.P. acknowledge financial support from the Spanish MICINN AYA2017-86 389-P. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under the 2019 Juan de la Cierva Programme. R.A. is a Trottier Postdoctoral Fellow and acknowledges support from the Trottier Family Foundation. This work was supported in part through a grant from FRQNT. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualization, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch.This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST).; We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Peerreview

Published
2021
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14. Wolf 503 b: Characterization of a Sub-Neptune Orbiting a Metal-Poor K Dwarf

Author

Lauren M. Weiss, Ian J. M. Crossfield, Sean M. Mills, Mercedes Lopez-Morales, Björn Benneke, Johanna Teske, Varoujan Gorjian, Howard Isaacson, Sharon X. Wang, Emilio Molinari, Samuel K. Grunblatt, R. Paul Butler, Jennifer Burt, Ashley Chontos, Grzegorz Nowak, Aida Behmard, Stephen A. Shectman, Erik A. Petigura, Avet Harutyunyan, Annelies Mortier, Ennio Poretti, Xavier Dumusque, Michel Mayor, Andrew W. Howard, Molly R. Kosiarek, Evangelos Nagel, Rafael Luque, Jeffrey D. Crane, Enric Palle, David W. Latham, Adriano Ghedina, Aldo S. Bonomo, Benjamin J. Fulton, Rosario Cosentino, Sarah Blunt, Aldo F. M. Fiorenzano, Alessandro Sozzetti, Alex S. Polanski, Polanski, AS [0000-0001-7047-8681], Burt, JA [0000-0002-0040-6815], Nowak, G [0000-0002-7031-7754], López-Morales, M [0000-0003-3204-8183], Mortier, A [0000-0001-7254-4363], Poretti, E [0000-0003-1200-0473], Behmard, A [0000-0003-0012-9093], Benneke, B [0000-0001-5578-1498], Blunt, S [0000-0002-3199-2888], Bonomo, AS [0000-0002-6177-198X], Butler, RP [0000-0003-1305-3761], Chontos, A [0000-0003-1125-2564], Crane, JD [0000-0002-5226-787X], Dumusque, X [0000-0002-9332-2011], Fulton, BJ [0000-0003-3504-5316], Ghedina, A [0000-0003-4702-5152], Grunblatt, SK [0000-0003-4976-9980], Howard, AW [0000-0001-8638-0320], Isaacson, H [0000-0002-0531-1073], Kosiarek, MR [0000-0002-6115-4359], Latham, DW [0000-0001-9911-7388], Luque, R [0000-0002-4671-2957], Mayor, M [0000-0002-9352-5935], Mills, SM [0000-0002-4535-6241], Molinari, E [0000-0002-1742-7735], Nagel, E [0000-0002-4019-3631], Pallé, E [0000-0003-0987-1593], Petigura, EA [0000-0003-0967-2893], Shectman, SA [0000-0002-8681-6136], Sozzetti, A [0000-0002-7504-365X], Wang, SX [0000-0002-6937-9034], Weiss, LM [0000-0002-3725-3058], and Apollo - University of Cambridge Repository

Subjects
Physics, Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Characterization (mathematics), 01 natural sciences, 010309 optics, Transmission spectroscopy, Radial velocity, Photometry (optics), Space and Planetary Science, Neptune, 0103 physical sciences, astro-ph.EP, Eccentricity (mathematics), 010303 astronomy & astrophysics, Mass fraction, Astrophysics - Earth and Planetary Astrophysics
Abstract

Using radial velocity measurements from four instruments, we report the mass and density of a $2.043\pm0.069 ~\rm{R}_{\oplus}$ sub-Neptune orbiting the quiet K-dwarf Wolf 503 (HIP 67285). In addition, we present improved orbital and transit parameters by analyzing previously unused short-cadence $K2$ campaign 17 photometry and conduct a joint radial velocity-transit fit to constrain the eccentricity at $0.41\pm0.05$. The addition of a transit observation by $Spitzer$ also allows us to refine the orbital ephemeris in anticipation of further follow-up. Our mass determination, $6.26^{+0.69}_{-0.70}~\rm{M}_{\odot}$, in combination with the updated radius measurements, gives Wolf 503 b a bulk density of $\rho = 2.92\pm ^{+0.50}_{-0.44}$ $\rm{g}~\rm{cm}^{-3}$. Using interior composition models, we find this density is consistent with an Earth-like core with either a substantial $\rm{H}_2\rm{O}$ mass fraction ($45^{+19.12}_{-16.15}\%$) or a modest H/He envelope ($0.5\pm0.28\%$). The low H/He mass fraction, along with the old age of Wolf 503 ($11\pm2$ Gyrs), makes this sub-Neptune an opportune subject for testing theories of XUV-driven mass loss while the brightness of its host ($J=8.3$ mag) makes it an attractive target for transmission spectroscopy., Comment: Accepted to ApJ 2021 July 15

Published
2021
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15. A pair of TESS planets spanning the radius valley around the nearby mid-M dwarf LTT 3780

Author

Andrew W. Mann, Dimitar Sasselov, Jon M. Jenkins, Charles A. Beichman, Steve B. Howell, F. Lienhard, David Charbonneau, Joseph E. Rodriguez, Giampaolo Piotto, Ken Rice, Avet Harutyunyan, Matteo Pinamonti, Eric D. Lopez, Laura Kreidberg, David W. Latham, Xavier Dumusque, Mercedes Lopez-Morales, Michel Mayor, George R. Ricker, Nicola Astudillo-Defru, Jack J. Lissauer, Douglas A. Caldwell, Kevin I. Collins, A. Magazzu, Joseph D. Twicken, Joshua E. Schlieder, Andrew Collier Cameron, David F. Phillips, Xavier Delfosse, Joshua N. Winn, Dennis M. Conti, M. Stalport, Rosario Cosentino, Sara Seager, Rodrigo F. Díaz, Annelies Mortier, Sébastien Lépine, Patricia T. Boyd, Rachel A. Matson, John F. Kielkopf, David R. Ciardi, Stéphane Udry, Cesar Briceno, Thierry Forveille, Nicholas M. Law, Samuel N. Quinn, Adriano Ghedina, Lars A. Buchhave, Ennio Poretti, Nuno C. Santos, Karen A. Collins, René Doyon, Xavier Bonfils, Emilio Molinari, Aldo F. M. Fiorenzano, Jason D. Eastman, Eric L. N. Jensen, Étienne Artigau, Alessandro Sozzetti, Jonathan Irwin, Michael Vezie, Benjamin V. Rackham, Pedro Figueira, Mario Damasso, L. Mignon, Damien Ségransan, Francesco Pepe, Claudio Melo, Carl Ziegler, Jennifer G. Winters, Elisabeth Matthews, José Renan de Medeiros, Luca Di Fabrizio, Giuseppina Micela, Christophe Lovis, Ian J. M. Crossfield, François Bouchy, Christopher J. Burke, J. M. Almenara, Roland Vanderspek, John Asher Johnson, Ryan Cloutier, Peter Tenenbaum, Christopher A. Watson, Courtney D. Dressing, Robert Massey, Erica J. Gonzales, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Universidad Católica de la Santísima Concepción (UCSC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Cloutier, R [0000-0001-5383-9393], Eastman, JD [0000-0003-3773-5142], Rodriguez, JE [0000-0001-8812-0565], Mortier, A [0000-0001-7254-4363], Pinamonti, M [0000-0002-4445-1845], Lienhard, F [0000-0003-4047-0771], Latham, DW [0000-0001-9911-7388], Collins, KA [0000-0001-6588-9574], Massey, R [0000-0001-8879-7138], Winters, JG [0000-0001-6031-9513], Charbonneau, D [0000-0002-9003-484X], Ziegler, C [0000-0002-0619-7639], Matthews, E [0000-0003-0593-1560], Kreidberg, L [0000-0003-0514-1147], Quinn, SN [0000-0002-8964-8377], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Winn, J [0000-0002-4265-047X], Jenkins, JM [0000-0002-4715-9460], Udry, S [0000-0001-7576-6236], Twicken, JD [0000-0002-6778-7552], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Santos, NC [0000-0003-4422-2919], Rackham, BV [0000-0002-3627-1676], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Molinari, E [0000-0002-1742-7735], Micela, G [0000-0002-9900-4751], De Medeiros, JR [0000-0001-8218-1586], Matson, RA [0000-0001-7233-7508], Mann, AW [0000-0003-3654-1602], Magazzú, A [0000-0003-1259-4371], López-Morales, M [0000-0003-3204-8183], Lissauer, JJ [0000-0001-6513-1659], Law, N [0000-0001-9380-6457], Kielkopf, JF [0000-0003-0497-2651], Jensen, ELN [0000-0002-4625-7333], Howell, SB [0000-0002-2532-2853], Ghedina, A [0000-0003-4702-5152], Forveille, T [0000-0003-0536-4607], Figueira, P [0000-0001-8504-283X], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Díaz, RF [0000-0001-9289-5160], Conti, DM [0000-0003-2239-0567], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Boyd, P [0000-0003-0442-4284], and Apollo - University of Cambridge Repository

Subjects
Radial velocity, 010504 meteorology & atmospheric sciences, Stellar mass, NDAS, FOS: Physical sciences, Astrophysics, M dwarf stars, 01 natural sciences, Planet, 0103 physical sciences, QB Astronomy, Spectroscopy, 010303 astronomy & astrophysics, Exoplanet systems, QC, 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Radius, Planetary system, Photoevaporation, Stars, QC Physics, Space and Planetary Science, astro-ph.EP, Transit photometry, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We present the confirmation of two new planets transiting the nearby mid-M dwarf LTT 3780 (TIC 36724087, TOI-732, $V=13.07$, $K_s=8.204$, $R_s$=0.374 R$_{\odot}$, $M_s$=0.401 M$_{\odot}$, d=22 pc). The two planet candidates are identified in a single TESS sector and are validated with reconnaissance spectroscopy, ground-based photometric follow-up, and high-resolution imaging. With measured orbital periods of $P_b=0.77$ days, $P_c=12.25$ days and sizes $r_{p,b}=1.33\pm 0.07$ R$_{\oplus}$, $r_{p,c}=2.30\pm 0.16$ R$_{\oplus}$, the two planets span the radius valley in period-radius space around low mass stars thus making the system a laboratory to test competing theories of the emergence of the radius valley in that stellar mass regime. By combining 63 precise radial-velocity measurements from HARPS and HARPS-N, we measure planet masses of $m_{p,b}=2.62^{+0.48}_{-0.46}$ M$_{\oplus}$ and $m_{p,c}=8.6^{+1.6}_{-1.3}$ M$_{\oplus}$, which indicates that LTT 3780b has a bulk composition consistent with being Earth-like, while LTT 3780c likely hosts an extended H/He envelope. We show that the recovered planetary masses are consistent with predictions from both photoevaporation and from core-powered mass loss models. The brightness and small size of LTT 3780, along with the measured planetary parameters, render LTT 3780b and c as accessible targets for atmospheric characterization of planets within the same planetary system and spanning the radius valley., Comment: Accepted to AJ. 8 figures, 6 tables. CSV file of the RV measurements (i.e. Table 2) are included in the source code

Published
2020
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16. ESPRESSO highlights the binary nature of the ultra-metal-poor giant HE 0107-5240

Author

Vardan Adibekyan, Piercarlo Bonifacio, Giuseppina Micela, J. I. González Hernández, Alessandro Sozzetti, M. R. Zapatero-Osorio, Paolo Molaro, Nelson J. Nunes, Ivo Saviane, P. Figueira, Yann Alibert, A. Suarez-Mascareno, Andrea Mehner, Sérgio F. Sousa, Elisabetta Caffau, V. D'Odorico, R. Genova, Lorenzo Monaco, Stéphane Udry, Ennio Poretti, David Ehrenreich, Nuno C. Santos, C. Lovis, C. Allende Prieto, Francesco Pepe, Cristina Martins, David Aguado, S. Cristiani, G. Cupani, P. Di Marcantonio, G. Lo Curto, Rafael Rebolo, Martins, C.J.A.P., Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Molaro, P. [0000-0002-0571-4163], Monaco, L. [0000-0002-3148-9836], Nunes, N. J. [0000-0002-3837-6914], Suarez Mascareño, A. [0000-0002-3814-5323], Aguado, D. [0000-0001-5200-3973], González Hernández, J. I. [0000-0002-0264-7356], Adibekyan, V. [0000-0002-0601-6199], Zapatero Osorio, M. R. [0000-0001-5664-2852], Figueira, P. [0000-0001-8504-283X], Sozzetti, A. [0000-0002-7504-365X], Santos, N. [0000-0003-4422-2919], Cupani, G. [0000-0002-6830-9093], Martins, C. J. A. P. [0000-0002-4886-9261], Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), Fundacao para a Ciencia e a Tecnologia (FCT), European Research Council (ERC), ITA, GBR, FRA, ESP, CHL, PRT, CHE, Portuguese Foundation for Science and Technology, POCI-01-0145-FEDER-028987, FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionaliza.cao, Portuguese Foundation for Science and Technology, IF/00650/2015/CP1273/CT0001, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), European Southern Observatory (ESO), Department of Applied Mathematics and Theoretical Physics (DAMTP), University of Cambridge [UK] (CAM), INAF - Osservatorio Astronomico di Palermo (OAPa), Universidad Andrés Bello [Santiago] (UNAB), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)

Subjects
[PHYS]Physics [physics], Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Binary number, abundances [Galaxy], Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galactic halo, Espresso, spectroscopic [Binaries], Space and Planetary Science, abundances [Stars], 0103 physical sciences, halo [Galaxy], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. The vast majority of the known stars of ultra low metallicity ([Fe=H] >-4:5) are known to be enhanced in carbon, and belong to the 'low-carbon band' (A(C) = log(C=H) + 12 7:6). It is generally, although not universally, accepted that this peculiar chemical composition reflects the chemical composition of the gas cloud out of which these stars were formed. The first ultra-metalpoor star discovered, HE 0107-5240, is also enhanced in carbon and belongs to the 'low-carbon band'. It has recently been claimed to be a long-period binary, based on radial velocity measurements. It has also been claimed that this binarity may explain its peculiar composition as being due to mass transfer from a former AGB companion. Theoretically, low-mass ratios in binary systems are much more favoured amongst Pop III stars than they are amongst solar-metallicity stars. Any constraint on the mass ratio of a system of such low metallicity would shed light on the star formation mechanisms in this metallicity regime. Aims.We acquired one high precision spectrum withESPRESSO in order to check the reality of the radial velocity variations. In addition we analysed all the spectra of this star in the ESO archive obtained with UVES to have a set of homogenously measured radial velocities. Methods. The radial velocities were measured using cross correlation against a synthetic spectrum template. Due to the weakness of metallic lines in this star, the signal comes only from the CH molecular lines of the G-band. Results. The measurement obtained in 2018 from an ESPRESSO spectrum demonstrates unambiguously that the radial velocity of HE 0107-5240 has increased from 2001 to 2018. Closer inspection of the measurements based on UVES spectra in the interval 2001-2006 show that there is a 96% probability that the radial velocity correlates with time, hence the radial velocity variations can already be suspected from the UVES spectra alone. Conclusions.We confirm the earlier claims of radial velocity variations in HE0107-5240. The simplest explanation of such variations is that the star is indeed in a binary system with a long period. The nature of the companion is unconstrained and we consider it is equally probable that it is an unevolved companion or a white dwarf. Continued monitoring of the radial velocities of this star is strongly encouraged., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Published
2020
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17. The GAPS Programme at TNG: XXI. A GIARPS case study of known young planetary candidates: confirmation of HD 285507 b and refutation of AD Leonis b

Author

Marcello Lodi, A. F. Lanza, Andrea Bignamini, M. Sozzi, Gaetano Scandariato, C. Riverol, Jesus Maldonado, Luca Malavolta, Giuseppe Leto, R. G. Gratton, Massimo Cecconi, Katia Biazzo, Carlo Baffa, Riccardo Claudi, G. Falcini, N. Buchschacher, Marco Pedani, Elisabetta Giani, Silvano Desidera, Concepción Iglesias González, H. Perez Ventura, Luigi Mancini, Daniela Fantinel, Antonio Maggio, Salvo Scuderi, Ennio Poretti, Ulf Seemann, Andrea Tozzi, Matthias Mallonn, José Guerra, A. Galli, Giuseppina Micela, E. Alei, Valerio Nascimbeni, Avet Harutyunyan, Matteo Pinamonti, G. Frustagli, Aldo S. Bonomo, Monica Rainer, Alfio Puglisi, Aldo F. M. Fiorenzano, Livia Origlia, Serena Benatti, Alessandro Sozzetti, Isabella Pagano, Andrea Baruffolo, Adriano Ghedina, Paolo Giacobbe, M. Gonzalez, Ernesto Oliva, Ilaria Carleo, Francesca Ghinassi, Rosario Cosentino, Elvira Covino, M. Esposito, N. Hernandez, Giampaolo Piotto, M. Hernandez Diaz, Luca Fini, J. San Juan, Seth Redfield, M. Iuzzolino, Nicoletta Sanna, L. Riverol, Laura Affer, Francesco Borsa, Emilio Molinari, Mario Damasso, E. González-Álvarez, V. Billotti, Carleo, I, Malavolta, L, Lanza, A, Damasso, M, Desidera, S, Borsa, F, Mallonn, M, Pinamonti, M, Gratton, R, Alei, E, Benatti, S, Mancini, L, Maldonado, J, Biazzo, K, Esposito, M, Frustagli, G, Gonzalez-Alvarez, E, Micela, G, Scandariato, G, Sozzetti, A, Affer, L, Bignamini, A, Bonomo, A, Claudi, R, Cosentino, R, Covino, E, Fiorenzano, A, Giacobbe, P, Harutyunyan, A, Leto, G, Maggio, A, Molinari, E, Nascimbeni, V, Pagano, I, Pedani, M, Piotto, G, Poretti, E, Rainer, M, Redfield, S, Baffa, C, Baruffolo, A, Buchschacher, N, Billotti, V, Cecconi, M, Falcini, G, Fantinel, D, Fini, L, Galli, A, Ghedina, A, Ghinassi, F, Giani, E, Gonzalez, C, Gonzalez, M, Guerra, J, Hernandez DIaz, M, Hernandez, N, Iuzzolino, M, Lodi, M, Oliva, E, Origlia, L, Perez Ventura, H, Puglisi, A, Riverol, C, Riverol, L, San Juan, J, Sanna, N, Scuderi, S, Seemann, U, Sozzi, M, Tozzi, A, Claudi, R. [0000-0001-7707-5105], Leto, G. [0000-0002-0040-5011], Piotto, G. [0000-0002-9937-6387], Bonomo, A. S. [0000-0002-6177-198X], Sozzetti, A. [0000-0002-7504-365X], Biazzo, K. [0000-0002-1892-2180], Ghedina, A. [0000-0003-4702-5152], Damasso, M. [0000-0001-9984-4278], Cosentino, R. [0000-0003-1784-1431], Agenzia Spaziale Italiana (ASI), 2014-025-R.1.2015, European Commission (EC), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, and Agenzia Spaziale Italiana (ASI)

Subjects
Planetary system, astro-ph.SR, 010504 meteorology & atmospheric sciences, instrumentation: spectrographs, planetary systems, techniques: spectroscopic, stars: activity, techniques: radial velocities, FOS: Physical sciences, Orbital eccentricity, Astrophysics, 01 natural sciences, spectroscopic [Techniques], Planet, spectrographs, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, spectrographs [Instrumentation], 10. No inequality, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Planetary migration, Physics, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], Techniques: radial velocitie, Settore FIS/05, Astronomy and Astrophysics, Instrumentation: spectrograph, Radial velocity, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, astro-ph.EP, Astrophysics::Earth and Planetary Astrophysics, activity [Stars], Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. The existence of hot Jupiters is still not well understood. Two main channels are thought to be responsible for their current location: a smooth planet migration through the protoplanetary disk or the circularization of an initial highly eccentric orbit by tidal dissipation leading to a strong decrease in the semimajor axis. Different formation scenarios result in different observable effects, such as orbital parameters (obliquity and eccentricity) or frequency of planets at different stellar ages. Aims. In the context of the GAPS Young Objects project, we are carrying out a radial velocity survey with the aim of searching and characterizing young hot-Jupiter planets. Our purpose is to put constraints on evolutionary models and establish statistical properties, such as the frequency of these planets from a homogeneous sample. Methods. Since young stars are in general magnetically very active, we performed multi-band (visible and near-infrared) spectroscopy with simultaneous GIANO-B + HARPS-N (GIARPS) observing mode at TNG. This helps in dealing with stellar activity and distinguishing the nature of radial velocity variations: stellar activity will introduce a wavelength-dependent radial velocity amplitude, whereas a Keplerian signal is achromatic. As a pilot study, we present here the cases of two known hot Jupiters orbiting young stars: HD 285507 b and AD Leo b. Results. Our analysis of simultaneous high-precision GIARPS spectroscopic data confirms the Keplerian nature of the variation in the HD 285507 radial velocities and refines the orbital parameters of the hot Jupiter, obtaining an eccentricity consistent with a circular orbit. Instead, our analysis does not confirm the signal previously attributed to a planet orbiting AD Leo. This demonstrates the power of the multi-band spectroscopic technique when observing active stars., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Published
2020

18. Identifying Exoplanets with Deep Learning. IV. Removing Stellar Activity Signals from Radial Velocity Measurements Using Neural Networks

Author

Zoe. L. de Beurs, Andrew Vanderburg, Christopher J. Shallue, Xavier Dumusque, Andrew Collier Cameron, Christopher Leet, Lars A. Buchhave, Rosario Cosentino, Adriano Ghedina, Raphaëlle D. Haywood, Nicholas Langellier, David W. Latham, Mercedes López-Morales, Michel Mayor, Giusi Micela, Timothy W. Milbourne, Annelies Mortier, Emilio Molinari, Francesco Pepe, David F. Phillips, Matteo Pinamonti, Giampaolo Piotto, Ken Rice, Dimitar Sasselov, Alessandro Sozzetti, Stéphane Udry, Christopher A. Watson, De Beurs, ZL [0000-0002-7564-6047], Vanderburg, A [0000-0001-7246-5438], Shallue, CJ [0000-0002-7585-9974], Dumusque, X [0000-0002-9332-2011], Cameron, AC [0000-0002-8863-7828], Leet, C [0000-0003-2369-0481], Buchhave, LA [0000-0003-1605-5666], Cosentino, R [0000-0003-1784-1431], Ghedina, A [0000-0003-4702-5152], Haywood, RD [0000-0001-9140-3574], Langellier, N [0000-0003-2107-3308], Latham, DW [0000-0001-9911-7388], López-Morales, M [0000-0003-3204-8183], Mayor, M [0000-0002-9352-5935], Micela, G [0000-0002-9900-4751], Milbourne, TW [0000-0001-5446-7712], Mortier, A [0000-0001-7254-4363], Molinari, E [0000-0002-1742-7735], Phillips, DF [0000-0001-5132-1339], Pinamonti, M [0000-0002-4445-1845], Piotto, G [0000-0002-9937-6387], Rice, K [0000-0002-6379-9185], Sasselov, D [0000-0001-7014-1771], Sozzetti, A [0000-0002-7504-365X], Udry, S [0000-0001-7576-6236], Apollo - University of Cambridge Repository, Apollo-University Of Cambridge Repository, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science

Subjects
QA75, FOS: Computer and information sciences, Radial velocity, Computer Science - Machine Learning, astro-ph.SR, Exoplanet astronomy, QA75 Electronic computers. Computer science, cs.LG, FOS: Physical sciences, Machine Learning (cs.LG), QB Astronomy, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, Solar and Stellar Astrophysics (astro-ph.SR), QB, Earth and Planetary Astrophysics (astro-ph.EP), The Solar System, Exoplanets, and Astrobiology, Astronomy and Astrophysics, DAS, QC Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, astro-ph.EP, Convolutional neural networks, Astrophysics - Instrumentation and Methods for Astrophysics, astro-ph.IM, Astrophysics - Earth and Planetary Astrophysics
Abstract

Exoplanet detection with precise radial velocity (RV) observations is currently limited by spurious RV signals introduced by stellar activity. We show that machine learning techniques such as linear regression and neural networks can effectively remove the activity signals (due to starspots/faculae) from RV observations. Previous efforts focused on carefully filtering out activity signals in time using modeling techniques like Gaussian Process regression (e.g. Haywood et al. 2014). Instead, we systematically remove activity signals using only changes to the average shape of spectral lines, and no information about when the observations were collected. We trained our machine learning models on both simulated data (generated with the SOAP 2.0 software; Dumusque et al. 2014) and observations of the Sun from the HARPS-N Solar Telescope (Dumusque et al. 2015; Phillips et al. 2016; Collier Cameron et al. 2019). We find that these techniques can predict and remove stellar activity from both simulated data (improving RV scatter from 82 cm/s to 3 cm/s) and from more than 600 real observations taken nearly daily over three years with the HARPS-N Solar Telescope (improving the RV scatter from 1.753 m/s to 1.039 m/s, a factor of ~ 1.7 improvement). In the future, these or similar techniques could remove activity signals from observations of stars outside our solar system and eventually help detect habitable-zone Earth-mass exoplanets around Sun-like stars., Comment: 28 pages, 14 figures, Accepted for publication in the Astronomical Journal

Published
2020
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19. Toi-1235 b: A keystone super-earth for testing radius valley emergence models around early m dwarfs

Author

Cloutier, R, Rodriguez, JE, Irwin, J, Charbonneau, D, Stassun, KG, Mortier, A, Latham, DW, Isaacson, H, Howard, AW, Udry, S, Wilson, TG, Watson, CA, Pinamonti, M, Lienhard, F, Giacobbe, P, Guerra, P, Collins, KA, Beiryla, A, Esquerdo, GA, Matthews, E, Matson, RA, Howell, SB, Furlan, E, Crossfield, IJM, Winters, JG, Nava, C, Ment, K, Lopez, ED, Ricker, G, Vanderspek, R, Seager, S, Jenkins, JM, Ting, EB, Tenenbaum, P, Sozzetti, A, Sha, L, Ségransan, D, Schlieder, JE, Sasselov, D, Roy, A, Robertson, P, Rice, K, Poretti, E, Piotto, G, Phillips, D, Pepper, J, Pepe, F, Molinari, E, Mocnik, T, Micela, G, Mayor, M, Martinez Fiorenzano, AF, Mallia, F, Lubin, J, Lovis, C, López-Morales, M, Kosiarek, MR, Kielkopf, JF, Kane, Jensen, ELN, Isopi, G, Huber, D, Hill, ML, Harutyunyan, A, Gonzales, E, Giacalone, S, Ghedina, A, Ercolino, A, Dumusque, X, Dressing, CD, Damasso, M, Dalba, PA, Cosentino, R, Conti, DM, Colón, KD, Collins, KI, Cameron, AC, Ciardi, D, Christiansen, J, Chontos, A, Cecconi, M, Caldwell, DA, Burke, C, Buchhave, L, Beichman, C, Behmard, A, Beard, C, Akana Murphy, JM, Cloutier, R [0000-0001-5383-9393], Rodriguez, JE [0000-0001-8812-0565], Charbonneau, D [0000-0002-9003-484X], Stassun, KG [0000-0002-3481-9052], Mortier, A [0000-0001-7254-4363], Latham, DW [0000-0001-9911-7388], Isaacson, H [0000-0002-0531-1073], Howard, AW [0000-0001-8638-0320], Udry, S [0000-0001-7576-6236], Collins, KA [0000-0001-6588-9574], Beiryla, A [0000-0001-6637-5401], Esquerdo, GA [0000-0002-9789-5474], Matthews, E [0000-0003-0593-1560], Matson, RA [0000-0001-7233-7508], Howell, SB [0000-0002-2532-2853], Winters, JG [0000-0001-6031-9513], Nava, C [0000-0001-8838-3883], Ment, K [0000-0001-5847-9147], Ricker, G [0000-0003-2058-6662], Vanderspek, R [0000-0001-6763-6562], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Ting, EB [0000-0002-8219-9505], Tenenbaum, P [0000-0002-1949-4720], Sozzetti, A [0000-0002-7504-365X], Sha, L [0000-0001-5401-8079], Ségransan, D [0000-0003-2355-8034], Schlieder, JE [0000-0001-5347-7062], Sasselov, D [0000-0001-7014-1771], Roy, A [0000-0001-8127-5775], Robertson, P [0000-0003-0149-9678], Poretti, E [0000-0003-1200-0473], Piotto, G [0000-0002-9937-6387], Pepper, J [0000-0002-3827-8417], Molinari, E [0000-0002-1742-7735], Mocnik, T [0000-0003-4603-556X], Micela, G [0000-0002-9900-4751], Lubin, J [0000-0001-8342-7736], López-Morales, M [0000-0003-3204-8183], Kielkopf, JF [0000-0003-0497-2651], Kane, SR [0000-0002-7084-0529], Jensen, ELN [0000-0002-4625-7333], Huber, D [0000-0001-8832-4488], Hill, ML [0000-0002-0139-4756], Giacalone, S [0000-0002-8965-3969], Ghedina, A [0000-0003-4702-5152], Dumusque, X [0000-0002-9332-2011], Dressing, CD [0000-0001-8189-0233], Dalba, PA [0000-0002-4297-5506], Cosentino, R [0000-0003-1784-1431], Conti, DM [0000-0003-2239-0567], Colón, KD [0000-0001-8020-7121], Collins, KI [0000-0003-2781-3207], Ciardi, D [0000-0002-5741-3047], Christiansen, J [0000-0002-8035-4778], Chontos, A [0000-0003-1125-2564], Caldwell, DA [0000-0003-1963-9616], Burke, C [0000-0002-7754-9486], Buchhave, L [0000-0003-1605-5666], Behmard, A [0000-0003-0012-9093], Beard, C [0000-0001-7708-2364], Akana Murphy, JM [0000-0001-8898-8284], and Apollo - University of Cambridge Repository

Subjects
Radial velocity, Exoplanet formation, Transit photometry, M dwarf stars, Exoplanet structure
Abstract

Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally-driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/non-rocky transition in period-radius space. Here we present the confirmation of TOI-1235 b ($P=3.44$ days, $r_p=1.738^{+0.087}_{-0.076}$ R$_{\oplus}$), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/non-rocky transition around early M dwarfs ($R_s=0.630\pm 0.015$ R$_{\odot}$, $M_s=0.640\pm 0.016$ M$_{\odot}$). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial-velocities from HARPS-N and HIRES. We measure a planet mass of $6.91^{+0.75}_{-0.85}$ M$_{\oplus}$ which implies an iron core mass fraction of $20^{+15}_{-12}$% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like and we constrain a H/He envelope mass fraction to be $

Published
2020

20. WASP-127b: a misaligned planet with a partly cloudy atmosphere and tenuous sodium signature seen by ESPRESSO

Author

P. Di Marcantonio, M. Cretignier, Alessandro Sozzetti, Stéphane Udry, Vincent Bourrier, P. Figueira, J. I. González Hernández, Stefano Cristiani, Vardan Adibekyan, François Bouchy, Baptiste Lavie, Olivier Demangeon, Núria Casasayas-Barris, A. Suárez Mascareño, Cristina Martins, Nuno C. Santos, Marco Riva, C. Lovis, Enric Palle, Antonio Manescau, Denis Mégevand, Hans Dekker, Nelson J. Nunes, Monika Lendl, Alexandre Cabral, Andrea Mehner, Ennio Poretti, Lorenzo Pino, M. R. Zapatero Osorio, Francesco Pepe, Willy Benz, Yann Alibert, G. Lo Curto, S. G. Sousa, Valentina D'Odorico, Paolo Molaro, Rafael Rebolo, Hugo M. Tabernero, Giuseppina Micela, M. Amate, Xavier Dumusque, Jorge Lillo-Box, Francesco Borsa, Romain Allart, C. Allende Prieto, Filippo Maria Zerbi, R. Génova Santos, Mahmoudreza Oshagh, David Ehrenreich, Swiss National Science Foundation (SNSF), European Research Council (ERC), Fundacao para a Ciencia e a Tecnologia (FCT), Istituto Nazionale di Astrofisica (INAF), Allart, R. [0000-0002-1199-9759], Pino, L. [0000-0002-1321-8856], Zapatero Osorio, M. R. [0000-0001-5664-2852], Pallé, E. [0000-0003-0987-1593], Pepe, F. [0000-0002-9815-773X], Cristiani, S. [0000-0002-2115-5234], Rebolo, R. [0000-0003-3767-7085], Bourrier, V. [0000-0002-9148-034X], Demangeon, O. D. S. [0000-0001-7918-0355], Lendl, M. [0000-0001-9699-1459], Lillo Box, J. [0000-0003-3742-1987], Sozzetti, A. [0000-0002-7504-365X], Tabernero, H. [0000-0002-8087-4298], Adibekyan, V. [0000-0002-0601-6199], Allende Prieto, C. [0000-0002-0084-572X], Cabral, A. [0000-0002-9433-871X], D´Odorico, V. [0000-0003-3693-3091], Di Marcantonio, P. [0000-0003-3168-2289], González Hernández, J. I. [0000-0002-0264-7356], Mehner, A. [0000-0002-9564-3302], Molaro, P. [0000-0002-0571-4163], Poretti, E. [0000-0003-1200-0473], Zerbi, F. M. [0000-0002-9996-973X], European Research Council (ERC) under the European Union, FEDER through COMPETE2020 Programa Operacional Competitividade e Internacionalizacao, Research Projects of National Relevance (PRIN), 201278X4FL, and Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737

Subjects
individual: WASP-127b [Planets and satellites], Atmospheres, 010504 meteorology & atmospheric sciences, Satellites, FOS: Physical sciences, Planets, Context (language use), Astrophysics, Spectroscopic, 01 natural sciences, spectroscopic [Techniques], Atmosphere, Planet, 0103 physical sciences, observational [Methods], Transit (astronomy), Observational, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy and Astrophysics, Exoplanet, Blueshift, Orbit, WASP-127b, 13. Climate action, Space and Planetary Science, atmospheres [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context The study of exoplanet atmospheres is essential for understanding the formation, evolution, and composition of exoplanets. The transmission spectroscopy technique is playing a significant role in this domain. In particular, the combination of state-of-The-Art spectrographs at low-And high-spectral resolution is key to our understanding of atmospheric structure and composition. Aims. We observed two transits of the close-in sub-Saturn-mass planet, WASP-127b, with ESPRESSO in the frame of the Guaranteed Time Observations Consortium. We aim to use these transit observations to study the system architecture and the exoplanet atmosphere simultaneously. Methods. We used the Reloaded Rossiter-McLaughlin technique to measure the projected obliquity λ and the projected rotational velocity veq sin(i∗). We extracted the high-resolution transmission spectrum of the planet to study atomic lines. We also proposed a new cross-correlation framework to search for molecular species and we applied it to water vapor. Results. The planet is orbiting its slowly rotating host star (veq sin(i∗) = 0.53-0.05+0.07 km s-1) on a retrograde misaligned orbit (λ =-128.41-5.46+5.60 °). We detected the sodium line core at the 9-σ confidence level with an excess absorption of 0.34 ± 0.04%, a blueshift of 2.74 ± 0.79 km s-1, and a full width at half maximum of 15.18 ± 1.75 km s-1. However, we did not detect the presence of other atomic species but set upper limits of only a few scale heights. Finally, we put a 3-σ upper limit on the average depth of the 1600 strongest water lines at equilibrium temperature in the visible band of 38 ppm. This constrains the cloud-deck pressure between 0.3 and 0.5 mbar by combining our data with low-resolution data in the near-infrared and models computed for this planet. Conclusions. WASP-127b, with an age of about 10 Gyr, is an unexpected exoplanet by its orbital architecture but also by the small extension of its sodium atmosphere (~7 scale heights). ESPRESSO allows us to take a step forward in the detection of weak signals, thus bringing strong constraints on the presence of clouds in exoplanet atmospheres. The framework proposed in this work can be applied to search for molecular species and study cloud-decks in other exoplanets., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Published
2020
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21. An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star

Author

Alessandro Sozzetti, Charles D. Fortenbach, Mario Damasso, David W. Latham, Rosario Cosentino, Emilio Molinari, David Charbonneau, Lars A. Buchhave, Ken Rice, Annelies Mortier, A. F. Martinez Fiorenzano, David F. Phillips, Suzanne Aigrain, Giuseppina Micela, Raphaëlle D. Haywood, Stéphane Udry, Ennio Poretti, Aldo S. Bonomo, Vinesh Rajpaul, Logan A. Pearce, Courtney D. Dressing, Giampaolo Piotto, Luca Malavolta, Li Zeng, Mercedes Lopez-Morales, Francesco Pepe, A. Coffinet, Andrew Collier Cameron, Xavier Dumusque, Andrew W. Mayo, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Mayo, AW [0000-0002-7216-2135], Buchhave, LA [0000-0003-1605-5666], Dressing, CD [0000-0001-8189-0233], Mortier, A [0000-0001-7254-4363], Zeng, L [0000-0003-1957-6635], Fortenbach, CD [0000-0001-5286-639X], Aigrain, S [0000-0003-1453-0574], Bonomo, AS [0000-0002-6177-198X], Cameron, AC [0000-0002-8863-7828], Charbonneau, D [0000-0002-9003-484X], Dumusque, X [0000-0002-9332-2011], Haywood, RD [0000-0001-9140-3574], Latham, DW [0000-0001-9911-7388], López-Morales, M [0000-0003-3204-8183], Malavolta, L [0000-0002-6492-2085], Molinari, E [0000-0002-1742-7735], Pearce, L [0000-0003-3904-7378], Piotto, G [0000-0002-9937-6387], Poretti, E [0000-0003-1200-0473], Sozzetti, A [0000-0002-7504-365X], and Apollo - University of Cambridge Repository

Subjects
planets and satellites: detection, Planetary equilibrium temperature, 010504 meteorology & atmospheric sciences, fundamental parameters [Planets and satellites], FOS: Physical sciences, Astrophysics, 01 natural sciences, techniques: photometric, Planet, Neptune, techniques: radial velocities, 0103 physical sciences, QB Astronomy, planets and satellites: composition, planets and satellites: fundamental parameters, planets and satellites: gaseous planets, methods: data analysis, data analysis [Methods], 010303 astronomy & astrophysics, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], photometric [Techniques], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 3rd-DAS, Earth mass, Exoplanet, Radial velocity, detection [Planets and satellites], gaseous planets [Planets and satellites], Photometry (astronomy), 13. Climate action, Space and Planetary Science, astro-ph.EP, composition [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract

Although several thousands of exoplanets have now been detected and characterized, observational biases have led to a paucity of long-period, low-mass exoplanets with measured masses and a corresponding lag in our understanding of such planets. In this paper we report the mass estimation and characterization of the long-period exoplanet Kepler-538b. This planet orbits a Sun-like star (V = 11.27) with M_* = 0.892 +/- (0.051, 0.035) M_sun and R_* = 0.8717 +/- (0.0064, 0.0061) R_sun. Kepler-538b is a 2.215 +/- (0.040, 0.034) R_earth sub-Neptune with a period of P = 81.73778 +/- 0.00013 d. It is the only known planet in the system. We collected radial velocity (RV) observations with HIRES on Keck I and HARPS-N on the TNG. We characterized stellar activity by a Gaussian process with a quasi-periodic kernel applied to our RV and cross correlation function full width at half maximum (FWHM) observations. By simultaneously modeling Kepler photometry, RV, and FWHM observations, we found a semi-amplitude of K = 1.68 +/- (0.39, 0.38) m s^-1 and a planet mass of M_p = 10.6 +/- (2.5, 2.4) M_earth. Kepler-538b is the smallest planet beyond P = 50 d with an RV mass measurement. The planet likely consists of a significant fraction of ices (dominated by water ice), in addition to rocks/metals, and a small amount of gas. Sophisticated modeling techniques such as those used in this paper, combined with future spectrographs with ultra high-precision and stability will be vital for yielding more mass measurements in this poorly understood exoplanet regime. This in turn will improve our understanding of the relationship between planet composition and insolation flux and how the rocky to gaseous transition depends on planetary equilibrium temperature., Comment: Published in AJ, 17 pages, 8 figures, 3 tables

Published
2019
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22. Nightside condensation of iron in an ultrahot giant exoplanet

Author

Claudio Cumani, João Coelho, Alessandro Sozzetti, David Alves, S. Deiries, Alessio Zanutta, Alexandre Cabral, Andrea Mehner, Luca Pasquini, Paolo Di Marcantonio, Luca Oggioni, Cristina Martins, Nelson J. Nunes, Andrea Modigliani, Antonio Manescau, Olivier Demangeon, Monika Lendl, Christophe Lovis, Matteo Aliverti, Emeline Bolmont, François Bouchy, Jonay I. González Hernández, Gaspare Lo Curto, Bernard Delabre, Heather M. Cegla, V. Baldini, Igor Coretti, Gerardo Avila, Willy Benz, Pedro Santos, Eric Müller, Hugo M. Tabernero, Olaf Iwert, Roberto Cirami, Francesco Pepe, F. Tenegi, Paolo Conconi, Mário J. P. F. G. Monteiro, Marco Landoni, Matteo Genoni, Paolo Spanò, Manuel Abreu, Stéphane Udry, M. Moschetti, Jean-Louis Lizon, Xavier Dumusque, J. Knudstrup, Valentina D'Odorico, Romain Allart, M. Affolter, Núria Casasayas-Barris, Baptiste Lavie, Sérgio F. Sousa, Christopher Broeg, Denis Mégevand, Nuno C. Santos, Marco Riva, Enric Palle, Giorgio Pariani, Edoardo Maria Alberto Redaelli, Vincent Bourrier, Filippo Maria Zerbi, Alex Segovia Milla, Florian Kerber, Damien Ségransan, Rafael Rebolo, I. Hughes, Francesco Borsa, Paolo Santin, Samuel Santana Tschudi, Antonio Gouveia Oliveira, Giuseppina Micela, Pedro Figueira, Charles Maire, Andrea Bianco, Maria Rosa Zapatero Osorio, Danuta Sosnowska, Nathan Hara, Ricardo Génova Santos, David Ehrenreich, Paolo Molaro, Vardan Adibekyan, T. Bandy, Yann Alibert, Jose Luis Rasilla, M. A. Monteiro, Carlos Allende Prieto, L. Genolet, Stefano Cristiani, A. Fragoso, Alejandro Suárez Mascareño, Julia V. Seidel, Ennio Poretti, M. Amate, Hans Dekker, Giorgio Calderone, G. Cupani, Suárez Mascareño, A. [0000-0002-3814-5323], Abreu, M. [0000-0002-0716-9568], Coelho, P. [0000-0002-4339-0550], Monteiro, M. J. [0000-0003-0513-8116], Tabernero, H. [0000-0002-8087-4298], Nunes, N. J. [0000-0002-3837-6914], Cabral, A. [0000-0002-9433-871X], Molaro, P. [0000-0002-0571-4163], Redaelli, E. M. A. [0000-0001-8185-2122], Zapatero Osorio, M. R. [0000-0001-5664-2852], Castro Alves, D. [0000-0001-7026-2514], Seidel, J. V. [0000-0002-7990-9596], Martins, C. J. A. P. [0000-0002-4886-9261], Adibekyan, V. [0000-0002-0601-6199], Zerbi, F. M. [0000-0002-9996-973X], Monteiro, M. [0000-0001-5644-0898], Mehner, A. [0000-0002-9564-3302], Santos, N. [0000-0003-4422-2919], Cegla, H. [0000-0001-8934-7315], Sozzetti, A. [0000-0002-7504-365X], Allart, R. [0000-0002-1199-9759], Landoni, M. [0000-0001-5570-5081], Coretti, I. [0000-0001-9374-3249], FEDER, Portuguese funds through FCT (Fundacao para a Ciencia e a Tecnologia), Spanish Ministry for Science, Innovation and Universities (MICIU), MICIU under the 2013 Ramon y Cajal programme MICIU, Council (ERC) under the European Union's Horizon 2020 research and innovation programme (project FOUR ACES), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, João M. P. Coelho. [0000-0002-4339-0550], European Research Council (ERC), Swiss National Science Foundation (SNSF), Fundacao para a Ciencia e a Tecnologia (FCT), Agencia Estatal de Investigación (AEI), Ministerio de Economía y Competitividad (MINECO), ITA, DEU, ESP, CHL, PRT, and CHE

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, 010504 meteorology & atmospheric sciences, Terminator (solar), Condensation, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Exoplanet, Article, Starlight, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Atmospheric chemistry, 0103 physical sciences, Physics::Space Physics, Transit (astronomy), Astrophysics::Earth and Planetary Astrophysics, Spectroscopy, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

Ehrenreich, D.et al., Ultrahot giant exoplanets receive thousands of times Earth’s insolation. Their high-temperature atmospheres (greater than 2,000 kelvin) are ideal laboratories for studying extreme planetary climates and chemistry. Daysides are predicted to be cloud-free, dominated by atomic species and much hotter than nightsides. Atoms are expected to recombine into molecules over the nightside, resulting in different day and night chemistries. Although metallic elements and a large temperature contrast have been observed, no chemical gradient has been measured across the surface of such an exoplanet. Different atmospheric chemistry between the day-to-night (‘evening’) and night-to-day (‘morning’) terminators could, however, be revealed as an asymmetric absorption signature during transit. Here we report the detection of an asymmetric atmospheric signature in the ultrahot exoplanet WASP-76b. We spectrally and temporally resolve this signature using a combination of high-dispersion spectroscopy with a large photon-collecting area. The absorption signal, attributed to neutral iron, is blueshifted by −11 ± 0.7 kilometres per second on the trailing limb, which can be explained by a combination of planetary rotation and wind blowing from the hot dayside. In contrast, no signal arises from the nightside close to the morning terminator, showing that atomic iron is not absorbing starlight there. We conclude that iron must therefore condense during its journey across the nightside., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

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