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1. Masses and compositions of three small planets orbiting the nearby M dwarf L231-32 (TOI-270) and the M dwarf radius valley

Author

Vincent, Van E, Astudillo-Defru, N., Bonfils, X., Hirano, T, Luque, R., Lam, Kin Wai, Justesen, A. B., Winn, J.N., Gandolfi, D., Nowak, Gabriel, Palle, Enric, Albrecht, S., Dai, F., Campos Estrada, Beatriz, Owen, James E., Foreman-Mackey, Daniel, Fridlund, M., Korth, Judith, Mathur, S., Vincent, Van E, Astudillo-Defru, N., Bonfils, X., Hirano, T, Luque, R., Lam, Kin Wai, Justesen, A. B., Winn, J.N., Gandolfi, D., Nowak, Gabriel, Palle, Enric, Albrecht, S., Dai, F., Campos Estrada, Beatriz, Owen, James E., Foreman-Mackey, Daniel, Fridlund, M., Korth, Judith, and Mathur, S.

Published
2021

2. A remnant planetary core in the hot-Neptune desert

Author

Armstrong, David J., Lopez, Théo A, Adibekyan, V., Booth, Richard A., Bryant, E., Collins, Karen A., Deleuil, Magali, Emsenhuber, A., Huang, C., King, George W., Lillo-Box, Jorge, Lissauer, Jack J., Matthews, Elisabeth, Mousis, Olivier, Nielsen, L. D., Osborn, Hugh, Otegi, Jon, Santos, N. C., Sousa, S. G., Stassun, Keivan G., Veras, Dimitri, Ziegler, Carl, Acton, Jack S., Almenara, Jose M., Anderson, David R., Barrado y Navascués, David, Barros, Susana C.C., Bayliss, Daniel, Belardi, Claudia, Bouchy, F., Briceño, César, Brogi, Matteo, Brown, David J. A., Burleigh, Matthew R., Casewell, Sarah L., Chaushev, Alexander, Ciardi, David R., Collins, Kevin I., Colón, Knicole D., Cooke, Benjamin F., Crossfield, Ian J. M., Díaz, Rodrigo F., Delgado-Mena, E., Demangeon, O.D.S., Dorn, Caroline, Dumusque, X., Eigmuller, Ph., Fausnaugh, Michael, Figueira, P., Gan, Tianjun, Gandhi, Siddharth, Gill, Samuel, Gonzales, Erica J., Goad, Michael R., Günther, Maximilian N., Helled, Ravit, Hojjatpanah, Saeed, Howell, Steve B., Jackman, James, Jenkins, James S., Jenkins, J., Jensen, Eric L. N., Kennedy, Grant M., Latham, D., Law, Nicholas, Lendl, M., Lozovsky, Michael, Mann, Andrew W., Moyano, Maximiliano, McCormac, James, Meru, Farzana, Mordasini, Christoph, Osborn, Ares, Pollacco, Don, Queloz, D., Raynard, Liam, Ricker, George R., Rowden, Pamela, Santerne, Alexandre, Schlieder, Joshua E., Seager, S., Sha, Lizhou, Tan, Thiam-Guan, Tilbrook, Rosanna H., Ting, Eric, Udry, Stephane, Vanderspek, Roland, Watson, Christopher, West, Richard G., Wilson, P. A., Winn, J.N., Wheatley, P. J., Villaseñor, Jesus Noel, Vines, Jose I., Zhan, Zhuchang, Armstrong, David J., Lopez, Théo A, Adibekyan, V., Booth, Richard A., Bryant, E., Collins, Karen A., Deleuil, Magali, Emsenhuber, A., Huang, C., King, George W., Lillo-Box, Jorge, Lissauer, Jack J., Matthews, Elisabeth, Mousis, Olivier, Nielsen, L. D., Osborn, Hugh, Otegi, Jon, Santos, N. C., Sousa, S. G., Stassun, Keivan G., Veras, Dimitri, Ziegler, Carl, Acton, Jack S., Almenara, Jose M., Anderson, David R., Barrado y Navascués, David, Barros, Susana C.C., Bayliss, Daniel, Belardi, Claudia, Bouchy, F., Briceño, César, Brogi, Matteo, Brown, David J. A., Burleigh, Matthew R., Casewell, Sarah L., Chaushev, Alexander, Ciardi, David R., Collins, Kevin I., Colón, Knicole D., Cooke, Benjamin F., Crossfield, Ian J. M., Díaz, Rodrigo F., Delgado-Mena, E., Demangeon, O.D.S., Dorn, Caroline, Dumusque, X., Eigmuller, Ph., Fausnaugh, Michael, Figueira, P., Gan, Tianjun, Gandhi, Siddharth, Gill, Samuel, Gonzales, Erica J., Goad, Michael R., Günther, Maximilian N., Helled, Ravit, Hojjatpanah, Saeed, Howell, Steve B., Jackman, James, Jenkins, James S., Jenkins, J., Jensen, Eric L. N., Kennedy, Grant M., Latham, D., Law, Nicholas, Lendl, M., Lozovsky, Michael, Mann, Andrew W., Moyano, Maximiliano, McCormac, James, Meru, Farzana, Mordasini, Christoph, Osborn, Ares, Pollacco, Don, Queloz, D., Raynard, Liam, Ricker, George R., Rowden, Pamela, Santerne, Alexandre, Schlieder, Joshua E., Seager, S., Sha, Lizhou, Tan, Thiam-Guan, Tilbrook, Rosanna H., Ting, Eric, Udry, Stephane, Vanderspek, Roland, Watson, Christopher, West, Richard G., Wilson, P. A., Winn, J.N., Wheatley, P. J., Villaseñor, Jesus Noel, Vines, Jose I., and Zhan, Zhuchang

Abstract

The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to large uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary processes provide a route to understanding planetary interiors. Planets found in and near the typically barren hot-Neptune ‘desert’ (a region in mass–radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b and NGTS-4b, on which photoevaporation has removed a substantial part of their outer atmospheres. Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune’s but an anomalously large mass of 39.1−2.6+2.7 Earth masses and a density of 5.2−0.8+0.7 grams per cubic centimetre, similar to Earth’s. Interior-structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9−0.9+0.8 per cent of the total planetary mass. The planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial gas accretion, perhaps through gap opening or late formation. Although photoevaporation rates cannot account for the mass loss required to reduce a Jupiter-like gas giant, they can remove a small (a few Earth masses) hydrogen and helium envelope on timescales of several billion years, implying that any remaining atmosphere on TOI-849b is likely to be enriched by water or other volatiles from the planetary interior. We conclude that TOI-849b is the remnant core of a giant planet.

Published
2020

3. Mass determinations of the three mini-Neptunes transiting TOI-125

Author

Nielsen, L. D., Gandolfi, D., Armstrong, David J., Jenkins, James S., Fridlund, M., Santos, N. C., Dai, F., Adibekyan, V., Luque, R., Steffen, J.H., Espósito, Massimiliano, Meru, Farzana, Sabotta, S., Bolmont, E., Kossakowski, D., Otegi, Jon, Murgas, F., Stalport, M., Rodler, F., Diaz, M., Kurtovic, N.T., Ricker, George R., Vanderspek, Roland, Latham, D., Seager, S., Winn, J.N., Jenkins, Jon M., Allart, R, Almenara, Jose M., Barrado y Navascués, David, Barros, Susana C.C., Bayliss, Daniel, Berdiñas, Z. M., Boisse, I., Bouchy, F., Boyd, P., Brown, David J. A., Bryant, E., Burke, C., Cochran, W.D., Cooke, Benjamin F., Demangeon, O.D.S., Díaz, Rodrigo F., Dittmann, J., Dorn, Caroline, Dumusque, X., García, R.A., González-Cuesta, L., Grziwa, S., Georgieva, I., Guerrero, N., Hatzes, Artie P., Helled, Ravit, Henze, C.E., Hojjatpanah, Saeed, Korth, J., Lam, K.W.F., Lillo-Box, Jorge, Lopez, Théo A, Livingston, J., Mathur, Savita, Mousis, Olivier, Narita, N., Osborn, Hugh, Pallé, Enric, Peña Rojas, Pablo A., Persson, C.M., Quinn, S. N., Rauer, Heike, Redfield, S., Santerne, Alexandre, dos Santos, L. A., Seidel, J.V., Sousa, S. G., Ting, Eric, Turbet, M, Udry, Stephane, Vanderburg, A., Van Eylen, V., Vines, Jose I., Wheatley, P. J., Wilson, P. A., Nielsen, L. D., Gandolfi, D., Armstrong, David J., Jenkins, James S., Fridlund, M., Santos, N. C., Dai, F., Adibekyan, V., Luque, R., Steffen, J.H., Espósito, Massimiliano, Meru, Farzana, Sabotta, S., Bolmont, E., Kossakowski, D., Otegi, Jon, Murgas, F., Stalport, M., Rodler, F., Diaz, M., Kurtovic, N.T., Ricker, George R., Vanderspek, Roland, Latham, D., Seager, S., Winn, J.N., Jenkins, Jon M., Allart, R, Almenara, Jose M., Barrado y Navascués, David, Barros, Susana C.C., Bayliss, Daniel, Berdiñas, Z. M., Boisse, I., Bouchy, F., Boyd, P., Brown, David J. A., Bryant, E., Burke, C., Cochran, W.D., Cooke, Benjamin F., Demangeon, O.D.S., Díaz, Rodrigo F., Dittmann, J., Dorn, Caroline, Dumusque, X., García, R.A., González-Cuesta, L., Grziwa, S., Georgieva, I., Guerrero, N., Hatzes, Artie P., Helled, Ravit, Henze, C.E., Hojjatpanah, Saeed, Korth, J., Lam, K.W.F., Lillo-Box, Jorge, Lopez, Théo A, Livingston, J., Mathur, Savita, Mousis, Olivier, Narita, N., Osborn, Hugh, Pallé, Enric, Peña Rojas, Pablo A., Persson, C.M., Quinn, S. N., Rauer, Heike, Redfield, S., Santerne, Alexandre, dos Santos, L. A., Seidel, J.V., Sousa, S. G., Ting, Eric, Turbet, M, Udry, Stephane, Vanderburg, A., Van Eylen, V., Vines, Jose I., Wheatley, P. J., and Wilson, P. A.

Abstract

The Transiting Exoplanet Survey Satellite, TESS, is currently carrying out an all-sky search for small planets transiting bright stars. In the first year of the TESS survey, a steady progress was made in achieving the mission's primary science goal of establishing bulk densities for 50 planets smaller than Neptune. During that year, the TESS's observations were focused on the southern ecliptic hemisphere, resulting in the discovery of three mini-Neptunes orbiting the star TOI-125, a V = 11.0 K0 dwarf. We present intensive HARPS radial velocity observations, yielding precise mass measurements for TOI-125b, TOI-125c, and TOI-125d. TOI-125b has an orbital period of 4.65 d, a radius of 2.726 ± 0.075 RE, a mass of 9.50 ± 0.88 ME, and is near the 2:1 mean motion resonance with TOI-125c at 9.15 d. TOI-125c has a similar radius of 2.759 ± 0.10 RE and a mass of 6.63 ± 0.99 ME, being the puffiest of the three planets. TOI-125d has an orbital period of 19.98 d and a radius of 2.93 ± 0.17 RE and mass 13.6 ± 1.2 ME. For TOI-125b and d, we find unusual high eccentricities of 0.19 ± 0.04 and 0.17^{+0.08}_{-0.06}, respectively. Our analysis also provides upper mass limits for the two low-SNR planet candidates in the system; for TOI-125.04 (RP = 1.36 RE, P = 0.53 d), we find a 2¿ upper mass limit of 1.6 ME, whereas TOI-125.05 (R_P=4.2^{+2.4}_{-1.4} RE, P = 13.28 d) is unlikely a viable planet candidate with an upper mass limit of 2.7 ME. We discuss the internal structure of the three confirmed planets, as well as dynamical stability and system architecture for this intriguing exoplanet system.

Published
2020

4. MuSCAT2 multicolour validation of TESS candidates: An ultra-short-period substellar object around an M dwarf

Author

Parviainen, H., Pallé, Enric, Zapatero Osorio, María Rosa, Montañés-Rodríguez, P., Murgas, F., Narita, N., Hidalgo, D., Béjar, Victor J. S., Korth, J., Monelli, M., Casasayas-Barris, N., Crouzet, N., de León, J., Fukui, A., Hernández, A., Klagyivik, P., Kusakabe, N., Luque, R., Mori, M., Nishiumi, T., Prieto-Arranz, J., Tamura, Motohide, Watanabe, N., Burke, C., Charbonneau, David, Collins, Karen A., Collins, Kevin I., Cont, D., Garcia Soto, A., Jenkins, James S., Jenkins, Jon M., Levine, A., Li, J., Rinehart, S., Seager, S., Tenenbaum, P., Ting, Eric, Vanderspek, Roland, Vezie, M., Winn, J.N., Parviainen, H., Pallé, Enric, Zapatero Osorio, María Rosa, Montañés-Rodríguez, P., Murgas, F., Narita, N., Hidalgo, D., Béjar, Victor J. S., Korth, J., Monelli, M., Casasayas-Barris, N., Crouzet, N., de León, J., Fukui, A., Hernández, A., Klagyivik, P., Kusakabe, N., Luque, R., Mori, M., Nishiumi, T., Prieto-Arranz, J., Tamura, Motohide, Watanabe, N., Burke, C., Charbonneau, David, Collins, Karen A., Collins, Kevin I., Cont, D., Garcia Soto, A., Jenkins, James S., Jenkins, Jon M., Levine, A., Li, J., Rinehart, S., Seager, S., Tenenbaum, P., Ting, Eric, Vanderspek, Roland, Vezie, M., and Winn, J.N.

Abstract

Context. We report the discovery of TOI 263.01 (TIC 120916706), a transiting substellar object (R = 0.87 RJup) orbiting a faint M3.5 V dwarf (V = 18.97) on a 0.56 d orbit. Aims. We setout to determine the nature of the Transiting Exoplanet Survey Satellite (TESS) planet candidate TOI 263.01 using ground-based multicolour transit photometry. The host star is faint, which makes radial-velocity confirmation challenging, but the large transit depth makes the candidate suitable for validation through multicolour photometry. Methods. Our analysis combines three transits observed simultaneously in r′, i′, and zs bands usingthe MuSCAT2 multicolour imager, three LCOGT-observed transit light curves in g′, r′, and i′ bands, a TESS light curve from Sector 3, and a low-resolution spectrum for stellar characterisation observed with the ALFOSC spectrograph. We modelled the light curves with PYTRANSIT using a transit model that includes a physics-based light contamination component, allowing us to estimate the contamination from unresolved sources from the multicolour photometry. Using this information we were able to derive the true planet-star radius ratio marginalised over the contamination allowed by the photometry.Combining this with the stellar radius, we were able to make a reliable estimate of the absolute radius of the object. Results. The ground-based photometry strongly excludes contamination from unresolved sources with a significant colour difference to TOI 263. Furthermore, contamination from sources of the same stellar type as the host is constrained to levels where the true radius ratio posterior has a median of 0.217 and a 99 percentile of0.286. The median and maximum radius ratios correspond to absolute planet radii of 0.87 and 1.41 RJup, respectively,which confirms the substellar nature of the planet candidate. The object is either a giant planetor a brown dwarf (BD) located deep inside the so-called "brown dwarf desert". Both possibilities offer a challenge to c

Published
2020

5. HD 2685 b: a hot Jupiter orbiting an early F-type star detected by TESS

Author

Ségransan, D., Pepe, F., Osip, D., Doty, J., Sedaghati, E., Relles, H., Ziegler, C., Tenenbaum, P., Jenkins, J.M., Nielsen, L.D., Cruz, B., Paredes, L.A., Sarkis, P., Matthews, E., Furész, G., Bayliss, D., Henning, T., Lovis, C., Haworth, K., Matson, R., Schlieder, J., Turner, O., Vanderburg, A., Law, N.M., Brahm, R., Jones, M.I., Bakos, G., Howell, S., Latham, D.W., Jordán, A., Dittmann, J., Christiansen, J.L., Mann, A.W., Gonzales, E., Henry, T., Hodari-Sadiki, J., Suc, V., Winn, J.N., Marmier, M., Tokovinin, A., Udry, S., Davies, M., Smith, J.C., Bouchy, F., Crossfield, I., Seager, S., Laughlin, G., Collins, K.A., Shporer, A., Wang, S., Espinoza, N., Beichman, C., and Ciardi, D.

Abstract

We report on the confirmation of a transiting giant planet around the relatively hot (Teff = 6801 ± 76 K) star HD 2685, whose transit signal was detected in Sector 1 data of NASA's TESS mission. We confirmed the planetary nature of the transit signal using Doppler velocimetric measurements with CHIRON, CORALIE, and FEROS, as well as using photometric data obtained with the Chilean-Hungarian Automated Telescope and the Las Cumbres Observatory. From the joint analysis of photometry and radial velocities, we derived the following parameters for HD 2685 b: P = 4.12688-0.00004+0.00005 days, e = 0.091-0.047+0.039, MP = 1.17 ± 0.12 MJ, and RP =1.44 ± 0.05 RJ. This system is a typical example of an inflated transiting hot Jupiter in a low- eccentricity orbit. Based on the apparent visual magnitude (V = 9.6 mag) of the host star, this is one of the brightest known stars hosting a transiting hot Jupiter, and it is a good example of the upcoming systems that will be detected by TESS during the two-year primary mission. This is also an excellent target for future ground- and space-based atmospheric characterization as well as a good candidate for measuring the projected spin-orbit misalignment angle through the Rossiter- McLaughlin effect. Tables of the photometry are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/625/A16

Published
2019

6. A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS

Author

Huber, D. Chaplin, W.J. Chontos, A. Kjeldsen, H. Christensen-Dalsgaard, J. Bedding, T.R. Ball, W. Brahm, R. Espinoza, N. Henning, T. Jordán, A. Sarkis, P. Knudstrup, E. Albrecht, S. Grundahl, F. Andersen, M.F. Pallé, P.L. Crossfield, I. Fulton, B. Howard, A.W. Isaacson, H.T. Weiss, L.M. Handberg, R. Lund, M.N. Serenelli, A.M. Rørsted Mosumgaard, J. Stokholm, A. Bieryla, A. Buchhave, L.A. Latham, D.W. Quinn, S.N. Gaidos, E. Hirano, T. Ricker, G.R. Vanderspek, R.K. Seager, S. Jenkins, J.M. Winn, J.N. Antia, H.M. Appourchaux, T. Basu, S. Bell, K.J. Benomar, O. Bonanno, A. Buzasi, D.L. Campante, T.L. Çelik Orhan, Z. Corsaro, E. Cunha, M.S. Davies, G.R. Deheuvels, S. Grunblatt, S.K. Hasanzadeh, A. Di Mauro, M.P. A. García, R. Gaulme, P. Girardi, L. Guzik, J.A. Hon, M. Jiang, C. Kallinger, T. Kawaler, S.D. Kuszlewicz, J.S. Lebreton, Y. Li, T. Lucas, M. Lundkvist, M.S. Mann, A.W. Mathis, S. Mathur, S. Mazumdar, A. Metcalfe, T.S. Miglio, A. F. G. Monteiro, M.J.P. Mosser, B. Noll, A. Nsamba, B. Joel Ong, J.M. Örtel, S. Pereira, F. Ranadive, P. Régulo, C. Rodrigues, T.S. Roxburgh, I.W. Aguirre, V.S. Smalley, B. Schofield, M. Sousa, S.G. Stassun, K.G. Stello, D. Tayar, J. White, T.R. Verma, K. Vrard, M. Yildiz, M. Baker, D. Bazot, M. Beichmann, C. Bergmann, C. Bugnet, L. Cale, B. Carlino, R. Cartwright, S.M. Christiansen, J.L. Ciardi, D.R. Creevey, O. Dittmann, J.A. Nascimento, J.-D.D. Eylen, V.V. Fürész, G. Gagné, J. Gao, P. Gazeas, K. Giddens, F. Hall, O.J. Hekker, S. Ireland, M.J. Latouf, N. Lebrun, D. Levine, A.M. Matzko, W. Natinsky, E. Page, E. Plavchan, P. Mansouri-Samani, M. McCauliff, S. Mullally, S.E. Orenstein, B. Soto, A.G. Paegert, M. Van Saders, J.L. Schnaible, C. Soderblom, D.R. Szabó, R. Tanner, A. Tinney, C.G. Teske, J. Thomas, A. Trampedach, R. Wright, D. Yuan, T.T. Zohrabi, F.

Abstract

We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V = 8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R∗ = 2.943 ± 0.064 Ro), mass (M∗ = 1.212 ± 0.074 Mo), and age (4.9 ± 1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a "hot Saturn" (Rp = 9.17 ± 0.33 R⊕) with an orbital period of ∼14.3 days, irradiance of F = 343 ± 24 F⊕, and moderate mass (Mp = 60.5 ± 5.7 M⊕) and density (ρp = 0.431 ± 0.062 g cm-3). The properties of HD 221416 b show that the host-star metallicity-planet mass correlation found in sub-Saturns (4-8 R⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology. © 2019. The American Astronomical Society. All rights reserved..

Published
2019

7. Detection and characterization of an ultra-dense sub-Neptunian planet orbiting the Sun-like star K2-292

Author

Luque, R., Nowak, G., Pallé, E., Dai, F., Kaminski, Adrian, Nagel, E., Hidalgo, D., Bauer, FF, Lafarga, M., Livingston, J., Barragán, O., Hirano, T., Fridlund, M., Gandolfi, D., Justesen, A. B., Hjorth, M., Van Eylen, V., Winn, J. N., Esposito, M., Morales, J.C., Albrecht, S., Alonso, R., Winn, J.N., Amado, Pedro J., Beck, P., Caballero, J. A., Cabrera, J., Cochran, W.D., Csizmadia, S., Deeg, H., Eigmuller, Ph., Endl, M., Erikson, A., Fukui, A., Grziwa, S., Guenther, E.W., Hatzes, A. P., Knudstrup, E., Korth, J., Lam, K.W.F., Lund, M. N., Mathur, S., Montañés-Rodríguez, P., Narita, N., Nespral, D., Niraula, P., Pätzold, M., Persson, C.M., Prieto-Arranz, J., Quirrenbach, A., Ribas, Ignasi, La Caixa, Japan Society for the Promotion of Science, Danish National Research Foundation, German Research Foundation, Swedish National Space Board, European Commission, Max Planck Society, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, European Research Council (ERC), Ministerio de Economía y Competitividad (MINECO), Japan Society for the Promotion of Science (JSPS), Danish National Research Foundation (DNRF), Deutsche Forschungsgemeinschaft (DFG), Swedish National Space Agency (SNSA), Japan Society for the Promotion of Science (JSPS), KAKENHI grant, Japan Science and Technology Agency (JST), PRESTO Grant, Danmarks Grundforskningsfond (DNRF), Deutsche Forschungsgemeinschaft (DFG), priority program xploring the Diversity of Exoplanets in the Mass-Density Diagram, and European Commission (EC)

Subjects
Extrasolare Planeten und Atmosphären, Ultra dense, Star (game theory), Astrophysics, Characterization (mathematics), 01 natural sciences, stars: individual: K2-292, techniques: photometric, Planet, Neptune, 0103 physical sciences, techniques: radial velocities, individual: HD 119130 [Stars], 010303 astronomy & astrophysics, individual: K2-292 [Stars], planetary systems, Physics, radial velocities [Techniques], 010308 nuclear & particles physics, photometric [Techniques], Leitungsbereich PF, Order (ring theory), techniques: high angular resolution, Astronomy and Astrophysics, Radius, Orbit, Planetary systems, high angular resolution [Techniques], 13. Climate action, Space and Planetary Science, Stars: individual: HD 119130, Stars: individual: K2-292, Techniques: high angular resolution, Techniques: photometric, Techniques: radial velocities, stars: individual: HD 119130
Abstract

We present the discovery and characterization of a new transiting planet from Campaign 17 of the Kepler extended mission K2. The planet K2-292 b is a warm sub-Neptune on a 17 day orbit around a bright (V = 9.9 mag) solar-like G3 V star with a mass and radius of M∗ = 1.00 ± 0.03 MȮ and R∗ = 1.09 ± 0.03 RȮ, respectively. We modeled simultaneously the K2 photometry and CARMENES spectroscopic data and derived a radius of Rp=2.63-0.10+0.12 RȮ and mass of Mp=24.5-4.4+4.4 MȮ, yielding a mean density of ρp=7.4-1.5+1.6 g cm-3, which makes it one of the densest sub-Neptunian planets known to date. We also detected a linear trend in the radial velocities of K2-292 (γRV =-0.40-0.07+0.07 m s-1 d-1) that suggests a long-period companion with a minimum mass on the order of 33 MȮ. If confirmed, it would support a formation scenario of K2-292 b by migration caused by Kozai-Lidov oscillations. © 2019 ESO., Funding for the K2 mission is provided by the NASA Science Mission directorate. 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. CARMENES is an instrument for the Centro Astronomico Hispano-Aleman de Calar Alto (CAHA, Almeria, Spain) funded by the German Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de Investigaciones Cientificas (CSIC), the European Union through FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES Consortium. R.L. has received funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 713673 and financial support through the >la Caixa> INPhINIT Fellowship Grant for Doctoral studies at Spanish Research Centres of Excellence, >la Caixa> Banking Foundation, Barcelona, Spain. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through grants ESP2013-48391-C4-2-R and AYA2016-79425-C3, and supported by the Japan Society for Promotion of Science (JSPS) KAKENHI Grant Number JP16K17660, JP18H01265 and JP18H05439, and JST PRESTO Grant Number JPMJPR1775. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106). K.W.F.L acknowledges the support of the DFG priority program SPP 1992 >Exploring the Diversity of Exoplanets in the Mass-Density Diagram> (RA 714/14-1). M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency.

Published
2019
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8. Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization

Author

National Aeronautics and Space Administration (US), Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), German Research Foundation, Klaus Tschira Foundation, Heising Simons Foundation, Ministry of Education, Culture, Sports, Science and Technology (Japan), Japan Society for the Promotion of Science, European Southern Observatory, Luque, R., Pallé, Enric, Kossakowski, D., Dreizler, S., Kemmer, J., Espinoza, Néstor, Burt, J., Anglada-Escudé, Guillem, Béjar, Victor J. S., Caballero, J. A., Collins, Karen A., Collins, KI., Cortés-Contreras, M., Díez-Alonso, E., Feng, Fabo, Hatzes, Artie P., Hellier, C, Henning, Thomas, Jeffers, Sandra V., Kaltenegger, L., Kürster, M., Madden, J., Molaverdikhani, K., Montes, D., Narita, N., Nowak, G., Ofir, A., Oshagh, M., Parviainen, H., Quirrenbach, Andreas, Reffert, S., Reiners, Ansgar, Rodríguez-López, Cristina, Schlecker, M., Stock, S., Trifonov, T., Winn, J.N., Zapatero Osorio, María Rosa, Zechmeister, Mathias, Amado, Pedro J., Anderson, D.R., Batalha, N.E., Bauer, Florian Franz, Bluhm, P., Burke, C.J., Butler, R.P., Caldwell, D.A., Chen, G., Crane, J.D., Dragomir, D., Dressing, C.D., Dynes, S., Jenkins, Jon M., Kaminski, A., Klahr, H., Kotani, T., Lafarga, M., Latham, David W., Lewin, P., McDermott, S., Montañés-Rodríguez, P., Morales, Juan Carlos, Murgas, F., Nagel, Evangelos, Pedraz, S., Ribas, Ignasi, Ricker, G.R., Rowden, P., Seager, S., Shectman, S.A., Tamura, M., Teske, J., Twicken, Joseph D., Vanderspeck, R., Wang, Sharon X., Wohler, Bill, National Aeronautics and Space Administration (US), Max Planck Society, Consejo Superior de Investigaciones Científicas (España), European Commission, Ministerio de Economía y Competitividad (España), German Research Foundation, Klaus Tschira Foundation, Heising Simons Foundation, Ministry of Education, Culture, Sports, Science and Technology (Japan), Japan Society for the Promotion of Science, European Southern Observatory, Luque, R., Pallé, Enric, Kossakowski, D., Dreizler, S., Kemmer, J., Espinoza, Néstor, Burt, J., Anglada-Escudé, Guillem, Béjar, Victor J. S., Caballero, J. A., Collins, Karen A., Collins, KI., Cortés-Contreras, M., Díez-Alonso, E., Feng, Fabo, Hatzes, Artie P., Hellier, C, Henning, Thomas, Jeffers, Sandra V., Kaltenegger, L., Kürster, M., Madden, J., Molaverdikhani, K., Montes, D., Narita, N., Nowak, G., Ofir, A., Oshagh, M., Parviainen, H., Quirrenbach, Andreas, Reffert, S., Reiners, Ansgar, Rodríguez-López, Cristina, Schlecker, M., Stock, S., Trifonov, T., Winn, J.N., Zapatero Osorio, María Rosa, Zechmeister, Mathias, Amado, Pedro J., Anderson, D.R., Batalha, N.E., Bauer, Florian Franz, Bluhm, P., Burke, C.J., Butler, R.P., Caldwell, D.A., Chen, G., Crane, J.D., Dragomir, D., Dressing, C.D., Dynes, S., Jenkins, Jon M., Kaminski, A., Klahr, H., Kotani, T., Lafarga, M., Latham, David W., Lewin, P., McDermott, S., Montañés-Rodríguez, P., Morales, Juan Carlos, Murgas, F., Nagel, Evangelos, Pedraz, S., Ribas, Ignasi, Ricker, G.R., Rowden, P., Seager, S., Shectman, S.A., Tamura, M., Teske, J., Twicken, Joseph D., Vanderspeck, R., Wang, Sharon X., and Wohler, Bill

Abstract

We report the detection of a transiting Earth-size planet around GJ 357, a nearby M2.5 V star, using data from the Transiting Exoplanet Survey Satellite (TESS). GJ 357 b (TOI-562.01) is a transiting, hot, Earth-sized planet (T-eq = 525 +/- 11 K) with a radius of R-b = 1.217 +/- 0.084 R-circle plus and an orbital period of P-b = 3.93 d. Precise stellar radial velocities from CARMENES and PFS, as well as archival data from HIRES, UVES, and HARPS also display a 3.93-day periodicity, confirming the planetary nature and leading to a planetary mass of M-b = 1.84 +/- 0.31 M-circle plus. In addition to the radial velocity signal for GJ 357 b, more periodicities are present in the data indicating the presence of two further planets in the system: GJ 357 c, with a minimum mass of M-c = 3.40 +/- 0.46 M-circle plus in a 9.12 d orbit, and GJ 357 d, with a minimum mass of M-d = 6.1 +/- 1.0 M-circle plus in a 55.7 d orbit inside the habitable zone. The host is relatively inactive and exhibits a photometric rotation period of P-rot = 78 +/- 2 d. GJ 357 b is to date the second closest transiting planet to the Sun, making it a prime target for further investigations such as transmission spectroscopy. Therefore, GJ 357 b represents one of the best terrestrial planets suitable for atmospheric characterization with the upcoming JWST and ground-based ELTs.© ESO 2019

Published
2019

9. A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270

Author

Kavli Institute for Theoretical Physics, John Templeton Foundation, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Science and Technology Facilities Council (UK), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Economía y Competitividad (España), European Commission, Heising Simons Foundation, National Aeronautics and Space Administration (US), Swiss National Science Foundation, Fédération Wallonie-Bruxelles, Günther, M.N., Pozuelos, Francisco José, Dittmann, J.A., Dragomir, D., Kane, S.R., Daylan, Tansu, Feinstein, A.D., Huang, C.X., Morton, T.D., Bonfanti, A., Bouma, L.G., Burt, J., Collins, Karen A., Lissauer, J.J., Matthews, E., Montet, B.T., Vanderburg, A., Wang, Shanshan, Winters, J.G., Ricker, G.R., Vanderspek, R.K., Latham, David W., Seager, S., Winn, J.N., Jenkins, Jon M., Armstrong, J.D., Barkaoui, K., Batalha, N., Bean, J.L., Caldwell, D.A., Ciardi, D.R., Collins, K.I., Crossfield, I., Fausnaugh, Michael, Furesz, G., Gan, T., Gillon, M., Guerrero, N., Horne, K., Howell, S.B., Ireland, M., Isopi, G., Jehin, E., Kielkopf, J.F., Lepine, S., Mallia, F., Matson, R.A., Myers, G., Pallé, Enric, Suárez Yanes, Juan Carlos, Kavli Institute for Theoretical Physics, John Templeton Foundation, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Science and Technology Facilities Council (UK), Comisión Nacional de Investigación Científica y Tecnológica (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Economía y Competitividad (España), European Commission, Heising Simons Foundation, National Aeronautics and Space Administration (US), Swiss National Science Foundation, Fédération Wallonie-Bruxelles, Günther, M.N., Pozuelos, Francisco José, Dittmann, J.A., Dragomir, D., Kane, S.R., Daylan, Tansu, Feinstein, A.D., Huang, C.X., Morton, T.D., Bonfanti, A., Bouma, L.G., Burt, J., Collins, Karen A., Lissauer, J.J., Matthews, E., Montet, B.T., Vanderburg, A., Wang, Shanshan, Winters, J.G., Ricker, G.R., Vanderspek, R.K., Latham, David W., Seager, S., Winn, J.N., Jenkins, Jon M., Armstrong, J.D., Barkaoui, K., Batalha, N., Bean, J.L., Caldwell, D.A., Ciardi, D.R., Collins, K.I., Crossfield, I., Fausnaugh, Michael, Furesz, G., Gan, T., Gillon, M., Guerrero, N., Horne, K., Howell, S.B., Ireland, M., Isopi, G., Jehin, E., Kielkopf, J.F., Lepine, S., Mallia, F., Matson, R.A., Myers, G., Pallé, Enric, and Suárez Yanes, Juan Carlos

Abstract

One of the primary goals of exoplanetary science is to detect small, temperate planets passing (transiting) in front of bright and quiet host stars. This enables the characterization of planetary sizes, orbits, bulk compositions, atmospheres and formation histories. These studies are facilitated by small and cool M dwarf host stars. Here we report the Transiting Exoplanet Survey Satellite (TESS) discovery of three small planets transiting one of the nearest and brightest M dwarf hosts observed to date, TOI-270 (TIC 259377017, with K-magnitude 8.3, and 22.5 parsecs away from Earth). The M3V-type star is transited by the super-Earth-sized planet TOI-270 b (1.247−0.083+0.089R) and the sub-Neptune-sized planets TOI-270 c (2.42 ± 0.13 R) and TOI-270 d (2.13 ± 0.12 R). The planets orbit close to a mean-motion resonant chain, with periods (3.36 days, 5.66 days and 11.38 days, respectively) near ratios of small integers (5:3 and 2:1). TOI-270 is a prime target for future studies because (1) its near-resonance allows the detection of transit timing variations, enabling precise mass measurements and dynamical studies; (2) its brightness enables independent radial-velocity mass measurements; (3) the outer planets are ideal for atmospheric characterization via transmission spectroscopy; and (4) the quietness of the star enables future searches for habitable zone planets. Altogether, very few systems with small, temperate exoplanets are as suitable for such complementary and detailed characterization as TOI-270.© 2019, The Author(s), under exclusive licence to Springer Nature Limited.

Published
2019

10. The Rossiter-McLaughlin effect for exoplanets

Author

Winn J.N.

Subjects
Physics, QC1-999
Abstract

There are now more than 30 stars with transiting planets for which the stellar obliquity—or more precisely its sky projection—has been measured, via the eponymous effect of Rossiter and McLaughlin. The history of these measurements is intriguing. For 8 years a case was gradually building that the orbits of hot Jupiters are always well-aligned with the rotation of their parent stars. Then in a sudden reversal, many misaligned systems were found, and it now seems that even retrograde systems are not uncommon. I review the measurement technique underlying these discoveries, the patterns that have emerged from the data, and the implications for theories of planet formation and migration.

Published
2011
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14. Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi

Author

William J. Chaplin, Aldo M. Serenelli, Andrea Miglio, Thierry Morel, J. Ted Mackereth, Fiorenzo Vincenzo, Hans Kjeldsen, Sarbani Basu, Warrick H. Ball, Amalie Stokholm, Kuldeep Verma, Jakob Rørsted Mosumgaard, Victor Silva Aguirre, Anwesh Mazumdar, Pritesh Ranadive, H. M. Antia, Yveline Lebreton, Joel Ong, Thierry Appourchaux, Timothy R. Bedding, Jørgen Christensen-Dalsgaard, Orlagh Creevey, Rafael A. García, Rasmus Handberg, Daniel Huber, Steven D. Kawaler, Mikkel N. Lund, Travis S. Metcalfe, Keivan G. Stassun, Michäel Bazot, Paul G. Beck, Keaton J. Bell, Maria Bergemann, Derek L. Buzasi, Othman Benomar, Diego Bossini, Lisa Bugnet, Tiago L. Campante, Zeynep Çelik Orhan, Enrico Corsaro, Lucía González-Cuesta, Guy R. Davies, Maria Pia Di Mauro, Ricky Egeland, Yvonne P. Elsworth, Patrick Gaulme, Hamed Ghasemi, Zhao Guo, Oliver J. Hall, Amir Hasanzadeh, Saskia Hekker, Rachel Howe, Jon M. Jenkins, Antonio Jiménez, René Kiefer, James S. Kuszlewicz, Thomas Kallinger, David W. Latham, Mia S. Lundkvist, Savita Mathur, Josefina Montalbán, Benoit Mosser, Andres Moya Bedón, Martin Bo Nielsen, Sibel Örtel, Ben M. Rendle, George R. Ricker, Thaíse S. Rodrigues, Ian W. Roxburgh, Hossein Safari, Mathew Schofield, Sara Seager, Barry Smalley, Dennis Stello, Róbert Szabó, Jamie Tayar, Nathalie Themeßl, Alexandra E. L. Thomas, Roland K. Vanderspek, Walter E. van Rossem, Mathieu Vrard, Achim Weiss, Timothy R. White, Joshua N. Winn, Mutlu Yıldız, European Commission, European Research Council, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Generalitat de Catalunya, Chaplin W.J., Serenelli A.M., Miglio A., Morel T., Mackereth J.T., Vincenzo F., Kjeldsen H., Basu S., Ball W.H., Stokholm A., Verma K., Mosumgaard J.R., Silva Aguirre V., Mazumdar A., Ranadive P., Antia H.M., Lebreton Y., Ong J., Appourchaux T., Bedding T.R., Christensen-Dalsgaard J., Creevey O., Garcia R.A., Handberg R., Huber D., Kawaler S.D., Lund M.N., Metcalfe T.S., Stassun K.G., Bazot M., Beck P.G., Bell K.J., Bergemann M., Buzasi D.L., Benomar O., Bossini D., Bugnet L., Campante T.L., Orhan Z.C., Corsaro E., Gonzalez-Cuesta L., Davies G.R., Di Mauro M.P., Egeland R., Elsworth Y.P., Gaulme P., Ghasemi H., Guo Z., Hall O.J., Hasanzadeh A., Hekker S., Howe R., Jenkins J.M., Jimenez A., Kiefer R., Kuszlewicz J.S., Kallinger T., Latham D.W., Lundkvist M.S., Mathur S., Montalban J., Mosser B., Bedon A.M., Nielsen M.B., Ortel S., Rendle B.M., Ricker G.R., Rodrigues T.S., Roxburgh I.W., Safari H., Schofield M., Seager S., Smalley B., Stello D., Szabo R., Tayar J., Themessl N., Thomas A.E.L., Vanderspek R.K., van Rossem W.E., Vrard M., Weiss A., White T.R., Winn J.N., Yildiz M., Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Department of Psychology, St John's University, Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), School of Physics and Astronomy, University of Birmingham [Birmingham], Centre Européen de Recherche et de Formation Avancée en Calcul Scientifique (CERFACS), Danish AsteroSeismology Centre (DASC), Aarhus University [Aarhus], Department of Astronomy, Yale University [New Haven], Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institut de Physique de Rennes (IPR), Université de Rennes (UR)-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), 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 Paris Cité (UPCité), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Sydney Institute for Astronomy (SIfA), The University of Sydney, Joseph Louis LAGRANGE (LAGRANGE), 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), Research institute of Computer Vision and Robotics [Girona] (VICOROB), Universitat de Girona (UdG), Department of Physics and Astronomy [Aarhus], Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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 Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), NASA Ames Research Center (ARC), Centre for Automation and Robotics (CAR), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad Politécnica de Madrid (UPM), Kiepenheuer-Institut für Sonnenphysik (KIS), Stellar Astrophysics Centre [Aarhus] (SAC), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), High Altitude Observatory (HAO), National Center for Atmospheric Research [Boulder] (NCAR), Département des Sciences et Gestion de l'Environnement/Océanologie [Liège], Université de Liège, Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), High Speed Networks Laboratory, Dept. of Telecommunications and Media Informatics, Budapest University of Technology and Economics [Budapest] (BME), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Observatoire de Paris, Université Paris sciences et lettres (PSL), Ege Üniversitesi, CERFACS [Toulouse], 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)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidad Politécnica de Madrid (UPM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), PSL Research University (PSL), 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), 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, and 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)

Subjects
010504 meteorology & atmospheric sciences, Milky Way, Population, GAIA, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, CHEMICAL-COMPOSITION, Q1, 01 natural sciences, Asteroseismology, 0103 physical sciences, QB460, Satellite galaxy, STELLAR HALOES, Astrophysics::Solar and Stellar Astrophysics, 10. No inequality, education, 010303 astronomy & astrophysics, QB600, QC, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Dwarf galaxy, QB, Physics, [PHYS]Physics [physics], education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], ACCRETION HISTORY, Astronomy and Astrophysics, DISC, Astrophysics - Astrophysics of Galaxies, Galaxy, MODEL, Stars, Astrophysics - Solar and Stellar Astrophysics, DARK-MATTER HALOES, ROTATION, Halo, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SOLAR-LIKE OSCILLATIONS, QB799
Abstract

This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). et al., Over the course of its history, the Milky Way has ingested multiple smaller satellite galaxies. Although these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to date precisely the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called Gaia–Enceladus, leading to substantial pollution of the chemical and dynamical properties of the Milky Way. Here we identify the very bright, naked-eye star ν Indi as an indicator of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be 11.0±0.7 (stat) ±0.8 (sys) billion years. The star bears hallmarks consistent with having been kinematically heated by the Gaia–Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 billion years ago, at 68% and 95% confidence, respectively. Computations based on hierarchical cosmological models slightly reduce the above limits., J.M. acknowledge support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, grant agreement number 772293). A.M.S. is partially supported by the Spanish Government (ESP2017-82674-R) and Generalitat de Catalunya (2017-SGR-1131). T.L.C. acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement number 792848 (PULSATION). K.J.B., S.H., J.S.K. and N.T. are supported by the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement number 338251 (StellarAges). E.C. is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement number 664931. L.G.-C. acknowledges support from the MINECO FPI-SO doctoral research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610. S.M. acknowledges support from the Spanish ministry through the Ramon y Cajal fellowship number RYC-2015-17697. This work was supported by FEDER through COMPETE2020 (POCI-01-0145-FEDER-030389. A.M.B. acknowledges funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No 749962 (project THOT).

Published
2020
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