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13 results on '"Winters, J. G."'

1. High-energy spectra of LTT 1445A and GJ 486 reveal flares and activity

Author

Diamond-Lowe, H., King, G. W., Youngblood, A., Brown, A., Howard, W. S., Winters, J. G., Wilson, D. J., France, K., Mendonça, J. M., Buchhave, L. A., Corrales, L., Kreidberg, L., Medina, A. A., Bean, J. L., Berta-Thompson, Z. K., Evans-Soma, T. M., Froning, C., Duvvuri, G. M., Kempton, E. M. -R., Miguel, Y., Pineda, J. S., and Schneider, C.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The high-energy radiative output, from the X-ray to the ultraviolet, of exoplanet host stars drives photochemical reactions and mass loss in the upper regions of planetary atmospheres. In order to place constraints on the atmospheric properties of the three closest terrestrial exoplanets transiting M dwarfs, we observe the high-energy spectra of the host stars LTT1445A and GJ486 in the X-ray with XMM-Newton and Chandra and in the ultraviolet with HST/COS and STIS. We combine these observations with estimates of extreme ultraviolet flux, reconstructions of the Ly-a lines, and stellar models at optical and infrared wavelengths to produce panchromatic spectra from 1A--20um for each star. While LTT1445Ab, LTT1445Ac, and GJ486b do not possess primordial hydrogen-dominated atmospheres, we calculate that they are able to retain pure CO2 atmospheres if starting with 10, 15, and 50% of Earth's total CO2 budget, respectively, in the presence of their host stars' stellar wind. We use age-activity relationships to place lower limits of 2.2 and 6.6 Gyr on the ages of the host stars LTT1445A and GJ486. Despite both LTT1445A and GJ486 appearing inactive at optical wavelengths, we detect flares at ultraviolet and X-ray wavelengths for both stars. In particular, GJ486 exhibits two flares with absolute energies of 10^29.5 and 10^30.1 erg (equivalent durations of 4357+/-96 and 19724+/-169 s) occurring three hours apart, captured with HST/COS G130M. Based on the timing of the observations, we suggest that these high-energy flares are related and indicative of heightened flaring activity that lasts for a period of days, but our interpretations are limited by sparse time-sampling. Consistent high-energy monitoring is needed to determine the duration and extent of high-energy activity on individual M dwarfs, as well as the population as a whole., Comment: 21 pages, published in A&A

Published
2024
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2. The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc

Author

Luque, R., Fulton, B. J., Kunimoto, M., Amado, P. J., Gorrini, P., Dreizler, S., Hellier, C., Henry, G. W., Molaverdikhani, K., Morello, G., Peña-Moñino, L., Pérez-Torres, M., Pozuelos, F. J., Shan, Y., Anglada-Escudé, G., Béjar, V. J. S., Bergond, G., Boyle, A. W., Caballero, J. A., Charbonneau, D., Ciardi, D. R., Dufoer, S., Espinoza, N., Everett, M., Fischer, D., Hatzes, A. P., Henning, Th., Hesse, K., Howard, A., Howell, S. B., Isaacson, H., Jeffers, S. V., Jenkins, J. M., Kane, S. R., Kemmer, J., Khalafinejad, S., Kidwell Jr., R. C., Kossakowski, D., Latham, D. W., Lillo-Box, J., Lissauer, J. J., Montes, D., Orell-Miquel, J., Pallé, E., Pollacco, D., Quirrenbach, A., Reffert, S., Reiners, A., Ribas, I., Ricker, G. R., Rogers, L. A., Sanz-Forcada, J., Schlecker, M., Schweitzer, A., Seager, S., Shporer, A., Stassun, K. G., Stock, S., Tal-Or, L., Ting, E. B., Trifonov, T., Vanaverbeke, S., Vanderspek, R., Villaseñor, J., Winn, J. N., Winters, J. G., and Osorio, M. R. Zapatero

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Space Physics
Abstract

We report the discovery of a multi-planetary system transiting the M0 V dwarf HD 260655 (GJ 239, TOI-4599). The system consists of at least two transiting planets, namely HD 260655 b, with a period of 2.77 d, a radius of R$_b$ = 1.240$\pm$0.023 R$_\oplus$, a mass of M$_b$ = 2.14$\pm$0.34 M$_\oplus$, and a bulk density of $\rho_b$ = 6.2$\pm$1.0 g cm$^{-3}$, and HD 260655 c, with a period of 5.71 d, a radius of R$_c$ = 1.533$^{+0.051}_{-0.046}$ R$_\oplus$, a mass of M$_c$ = 3.09$\pm$0.48 M$_\oplus$, and a bulk density of $\rho_c$ = 4.7$^{+0.9}_{-0.8}$ g cm$^{-3}$. The planets were detected in transit by the TESS mission and confirmed independently with archival and new precise radial velocities obtained with the HIRES and CARMENES instruments since 1998 and 2016, respectively. At a distance of 10 pc, HD 260655 becomes the fourth closest known multi-transiting planet system after HD 219134, LTT 1445 A, and AU Mic. Due to the apparent brightness of the host star (J = 6.7 mag), both planets are among the most suitable rocky worlds known today for atmospheric studies with the JWST, both in transmission and emission., Comment: 24 pages, 17 figures. Accepted for publication in A&A

Published
2022
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3. A Second Planet Transiting LTT 1445A and a Determination of the Masses of Both Worlds

Author

Winters, J. G., Cloutier, R., Medina, A. A., Irwin, J. M., Charbonneau, D., Astudillo-Defru, N., Bonfils, X., Howard, A. W., Isaacson, H., Bean, J. L., Seifahrt, A., Teske, J. K., Eastman, J. D., Twicken, J. D., Collins, K. A., Jensen, E. L. N., Quinn, S. N., Payne, M. J., Kristiansen, M. H., Spencer, A., Vanderburg, A., Zechmeister, M., Weiss, L. M., Wang, S. X., Wang, G., Udry, S., Terentev, I. A., Sturmer, J., Stefansson, G., Shporer, A., Shectman, S., Sefako, R., Schwengeler, H. M., Schwarz, R. P., Scarsdale, N., Rubenzahl, R. A., Roy, A., Rosenthal, L. J., Robertson, P., Petigura, E. A., Pepe, F., Omohundro, M., Murphy, J. M. A., Murgas, F., Movcnik, T., Montet, B. T., Mennickent, R., Mayo, A. W., Massey, B., Lubin, J., Lovis, C., Lewin, P., Kasper, D., Kane, S. R., Jenkins, J. M., Huber, D., Horne, K., Hill, M. L., Gorrini, P., Giacalone, S., Fulton, B., Forveille, T., Figueira, P., Fetherolf, T., Dressing, C., Diaz, R. F., Delfosse, X., Dalba, P. A., Dai, F., Cortes, C. C., Crossfield, I. J. M., Crane, J. D., Conti, D. M., Collins, K. I., Chontos, A., Butler, R. P., Brown, P., Brady, M., Behmard, A., Beard, C., Batalha, N. M., and Almenara, J. -M.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 parsecs. The primary star LTT 1445A (0.257 M_Sun) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.4 days, making it the second closest known transiting exoplanet system, and the closest one for which the host is an M dwarf. Using TESS data, we present the discovery of a second planet in the LTT 1445 system, with an orbital period of 3.1 days. We combine radial velocity measurements obtained from the five spectrographs ESPRESSO, HARPS, HIRES, MAROON-X, and PFS to establish that the new world also orbits LTT 1445A. We determine the mass and radius of LTT 1445Ab to be 2.87+/-0.25 M_Earth and 1.304^{+0.067}_{-0.060} R_Earth, consistent with an Earth-like composition. For the newly discovered LTT 1445Ac, we measure a mass of 1.54^{+0.20}_{-0.19} M_Earth and a minimum radius of 1.15 R_Earth, but we cannot determine the radius directly as the signal-to-noise of our light curve permits both grazing and non-grazing configurations. Using MEarth photometry and ground-based spectroscopy, we establish that star C (0.161 M_Sun) is likely the source of the 1.4-day rotation period, and star B (0.215 M_Sun) has a likely rotation period of 6.7 days. We estimate a probable rotation period of 85 days for LTT 1445A. Thus, this triple M-dwarf system appears to be in a special evolutionary stage where the most massive M dwarf has spun down, the intermediate mass M dwarf is in the process of spinning down, while the least massive stellar component has not yet begun to spin down., Comment: Accepted to the Astronomical Journal. 4 tables, 10 figures; RV table available upon request

Published
2021
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4. A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS

Author

Astudillo-Defru, N., Cloutier, R., Wang, S. X., Teske, J., Brahm, R., Hellier, C., Ricker, G., Vanderspek, R., Latham, D., Seager, S., Winn, J. N., Jenkins, J. M., Collins, K. A., Stassun, K. G., Ziegler, C., Almenara, J. M., Anderson, D. R., Artigau, E., Bonfils, X., Bouchy, F., Briceño, C., Butler, R. P., Charbonneau, D., Conti, D. M., Crane, J., Crossfield, I. J . M., Davies, M., Delfosse, X., Díaz, R. F., Doyon, R., Dragomir, D., Eastman, J. D., Espinoza, N., Essack, Z., Feng, F., Figueira, P., Forveille, T., Gan, T., Glidden, A., Guerrero, N., Hart, R., Henning, Th., Horch, E. P., Isopi, G., Jenkins, J. S., Jordán, A., Kielkopf, J. F., Law, N., Lovis, C., Mallia, F., Mann, A. W., de Medeiros, J. R., Melo, C., Mennickent, R. E., Mignon, L., Murgas, F., Nusdeo, D. A., Pepe, F., Relles, H. M., Rose, M., Santos, N. C., Ségransan, D., Shectman, S., Shporer, A., Smith, J. C., Torres, P., Udry, S., Villasenor, J., Winters, J . G., and Zhou, G.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We report the detection of a transiting super-Earth-sized planet (R=1.39+-0.09 Rearth) in a 1.4-day orbit around L 168-9 (TOI-134),a bright M1V dwarf (V=11, K=7.1) located at 25.15+-0.02 pc. The host star was observed in the first sector of the Transiting Exoplanet Survey Satellite (TESS) mission and, for confirmation and planet mass measurement, was followed up with ground-based photometry, seeing-limited and high-resolution imaging, and precise radial velocity (PRV) observations using the HARPS and PFS spectrographs. Combining the TESS data and PRV observations, we find the mass of L168-9 b to be 4.60+-0.56 Mearth, and thus the bulk density to be 1.74+0.44-0.33 times larger than that of the Earth. The orbital eccentricity is smaller than 0.21 (95% confidence). This planet is a Level One Candidate for the TESS Mission's scientific objective - to measure the masses of 50 small planets - and is one of the most observationally accessible terrestrial planets for future atmospheric characterization., Comment: 14 pages, 8 figures, 3 tables. Accepted for publication in astronomy and Astrophysics

Published
2020
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5. The HD 260655 system: Two rocky worlds transiting a bright M dwarf at 10 pc

Author

Luque, R., primary, Fulton, B. J., additional, Kunimoto, M., additional, Amado, P. J., additional, Gorrini, P., additional, Dreizler, S., additional, Hellier, C., additional, Henry, G. W., additional, Molaverdikhani, K., additional, Morello, G., additional, Peña-Moñino, L., additional, Pérez-Torres, M., additional, Pozuelos, F. J., additional, Shan, Y., additional, Anglada-Escudé, G., additional, Béjar, V. J. S., additional, Bergond, G., additional, Boyle, A. W., additional, Caballero, J. A., additional, Charbonneau, D., additional, Ciardi, D. R., additional, Dufoer, S., additional, Espinoza, N., additional, Everett, M., additional, Fischer, D., additional, Hatzes, A. P., additional, Henning, Th., additional, Hesse, K., additional, Howard, A. W., additional, Howell, S. B., additional, Isaacson, H., additional, Jeffers, S. V., additional, Jenkins, J. M., additional, Kane, S. R., additional, Kemmer, J., additional, Khalafinejad, S., additional, Kidwell, R. C., additional, Kossakowski, D., additional, Latham, D. W., additional, Lillo-Box, J., additional, Lissauer, J. J., additional, Montes, D., additional, Orell-Miquel, J., additional, Pallé, E., additional, Pollacco, D., additional, Quirrenbach, A., additional, Reffert, S., additional, Reiners, A., additional, Ribas, I., additional, Ricker, G. R., additional, Rogers, L. A., additional, Sanz-Forcada, J., additional, Schlecker, M., additional, Schweitzer, A., additional, Seager, S., additional, Shporer, A., additional, Stassun, K. G., additional, Stock, S., additional, Tal-Or, L., additional, Ting, E. B., additional, Trifonov, T., additional, Vanaverbeke, S., additional, Vanderspek, R., additional, Villaseñor, J., additional, Winn, J. N., additional, Winters, J. G., additional, and Zapatero Osorio, M. R., additional

Published
2022
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6. A hot terrestrial planet orbiting the bright M dwarf L 168-9 unveiled by TESS

Author

Astudillo-Defru, N., primary, Cloutier, R., additional, Wang, S. X., additional, Teske, J., additional, Brahm, R., additional, Hellier, C., additional, Ricker, G., additional, Vanderspek, R., additional, Latham, D., additional, Seager, S., additional, Winn, J. N., additional, Jenkins, J. M., additional, Collins, K. A., additional, Stassun, K. G., additional, Ziegler, C., additional, Almenara, J. M., additional, Anderson, D. R., additional, Artigau, E., additional, Bonfils, X., additional, Bouchy, F., additional, Briceño, C., additional, Butler, R. P., additional, Charbonneau, D., additional, Conti, D. M., additional, Crane, J., additional, Crossfield, I. J. M., additional, Davies, M., additional, Delfosse, X., additional, Díaz, R. F., additional, Doyon, R., additional, Dragomir, D., additional, Eastman, J. D., additional, Espinoza, N., additional, Essack, Z., additional, Feng, F., additional, Figueira, P., additional, Forveille, T., additional, Gan, T., additional, Glidden, A., additional, Guerrero, N., additional, Hart, R., additional, Henning, Th., additional, Horch, E. P., additional, Isopi, G., additional, Jenkins, J. S., additional, Jordán, A., additional, Kielkopf, J. F., additional, Law, N., additional, Lovis, C., additional, Mallia, F., additional, Mann, A. W., additional, de Medeiros, J. R., additional, Melo, C., additional, Mennickent, R. E., additional, Mignon, L., additional, Murgas, F., additional, Nusdeo, D. A., additional, Pepe, F., additional, Relles, H. M., additional, Rose, M., additional, Santos, N. C., additional, Ségransan, D., additional, Shectman, S., additional, Shporer, A., additional, Smith, J. C., additional, Torres, P., additional, Udry, S., additional, Villasenor, J., additional, Winters, J .G., additional, and Zhou, G., additional

Published
2020
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7. A 3D SEARCH FOR COMPANIONS TO 12 NEARBY M DWARFS

Author

Davison, Cassy L., primary, White, R. J., additional, Henry, T. J., additional, Riedel, A. R., additional, Jao, W-C., additional, Bailey III, J. I., additional, Quinn, S. N., additional, Cantrell, J. R., additional, Subasavage, J. P., additional, and Winters, J. G., additional

Published
2015
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8. The Closest M-Dwarf Quadruple System to the Sun

Author

NAVAL OBSERVATORY FLAGSTAFF AZ, Davison, Cassy L, White, R J, Jao, W C, Henry, T J, Bailey, III, J I, Quinn, S N, Cantrell, J R, Riedel, A R, Subasavage, J P, Winters, J G, NAVAL OBSERVATORY FLAGSTAFF AZ, Davison, Cassy L, White, R J, Jao, W C, Henry, T J, Bailey, III, J I, Quinn, S N, Cantrell, J R, Riedel, A R, Subasavage, J P, and Winters, J G

Abstract

Although the processes involved in single star formation have a wide variety of observational and theoretical constraints (e.g., McKee & Ostriker 2007), the complex physics involved in the formation of binary and especially multiple star systems is much less understood (e.g., Halbwachs et al. 2003; Tokovinin 2008; Duchene & Kraus 2013). Prompt fragmentation of a collapsing prestellar core is favored as setting the initial conditions for multiple star systems (e.g., Tohline 2002), though how this depends upon the initial conditions of the cloud core (e.g., metallicity, mass, etc.) is not well understood. Once initial fragments form, subsequent fragmentation (possibly within a disk), accretion from the remnant cloud core, N-body dynamics, and possibly orbital migration have been proposed to play competing roles in setting the final properties of multiple star systems (e.g., Bate 2000; Bonnell 2001; Delgado-Donate et al., Pub. in The Astronomical Journal, v147 n26 1-9p, Feb 2014. The original document contains color images.

Published
2013

9. Multiplicity of cool dwarfs

Author

Dupuy, T. J., Allen, P. R., Kraus, A. L., Biller, B., Blake, C. H., Davison, C., Deacon, N. R., Duchene, G., Geller, A. M., King, R. R., Law, N. M., Nguyen, Duy Cuong, Reipurth, B., Winters, J. G., Zhang, Z. H., Dupuy, T. J., Allen, P. R., Kraus, A. L., Biller, B., Blake, C. H., Davison, C., Deacon, N. R., Duchene, G., Geller, A. M., King, R. R., Law, N. M., Nguyen, Duy Cuong, Reipurth, B., Winters, J. G., and Zhang, Z. H.

Abstract

Multiple systems have long been used to probe the origin and evolution of stars of all masses. Only in the past 10-15 years have such studies been extended to brown dwarfs and the lowest mass stars through binary surveys of both young star forming regions and the older field population. In addition, a groundswell of interest in M dwarfs in recent years has resulted in large, modern datasets for these most common stars in the Galaxy, thereby enabling renewed perspectives on their multiplicity properties. These latest observational results have in turn fueled the many theories competing to explain the formation of low-mass stars and brown dwarfs. This Cool Stars 17 splinter session examined the current state of this field by reviewing results from the numerous observational techniques - radial velocities, astrometry, direct imaging, and synoptic surveys - that have been used to study multiplicity from the earliest embedded protostars to objects in young star forming regions, old and intermediate-age clusters, as well as the more heterogeneous field population., AuthorCount:15

Published
2013
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10. THE CLOSEST M-DWARF QUADRUPLE SYSTEM TO THE SUN

Author

Davison, Cassy L., primary, White, R. J., additional, Jao, W.-C., additional, Henry, T. J., additional, Bailey, J. I., additional, Quinn, S. N., additional, Cantrell, J. R., additional, Riedel, A. R., additional, Subasavage, J. P., additional, Winters, J. G., additional, and Crockett, C. J., additional

Published
2013
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12. The First Habitable-zone Earth-sized Planet from TESS. I. Validation of the TOI-700 System

Author

Roland Vanderspek, Michele L. Silverstein, Danielle Dineen, Ethan Kruse, Stephen A. Rinehart, Matthew S. Clement, Emily A. Gilbert, Jessie L. Christiansen, Courtney D. Dressing, Joseph E. Rodriguez, Tansu Daylan, Christopher Lam, Keivan G. Stassun, Tianjun Gan, Sebastian Zieba, Nikole K. Lewis, Mario Di Sora, Veselin B. Kostov, Jonathan Brande, Jennifer G. Winters, George R. Ricker, Eric T. Wolf, Teresa Monsue, Eric D. Lopez, Karen A. Collins, Laura Kreidberg, Wei-Chun Jao, Stephen R. Kane, Naylynn Tañón Reyes, Andrew Couperus, Carl Ziegler, F. Mallia, Benjamin J. Shappee, Gabrielle Suissa, Kelsey Hoffman, Giovanni Covone, Laura D. Vega, Jeffrey C. Smith, Allison Youngblood, Bárbara Rojas-Ayala, Knicole D. Colón, Patricia T. Boyd, Fred C. Adams, Sean N. Raymond, Joel D. Hartman, Todd J. Henry, Geronimo L. Villanueva, Ravi Kumar Kopparapu, Avi Mandell, Christopher J. Burke, Giada Arney, Brianna Galgano, Mark E. Everett, Peter Tenenbaum, Gáspár Á. Bakos, Cesar Briceno, Samuel N. Quinn, Elisa V. Quintana, Mackenna L. Wood, Eve J. Lee, Alex R. Howe, Sarah E. Logsdon, Thomas Fauchez, Zahra Essack, Dennis M. Conti, Andrew W. Mann, Nora L. Eisner, Rishi R. Paudel, Jack J. Lissauer, Quadry Chance, Peter Plavchan, Lucianne M. Walkowicz, Fergal Mullally, Vladimir Airapetian, Eliot Halley Vrijmoet, Eric L. N. Jensen, David W. Latham, Thomas Barclay, Benjamin J. Hord, Joshua E. Schlieder, Nicholas M. Law, Jon M. Jenkins, Joshua N. Winn, Steve B. Howell, Susan E. Mullally, Andrew Vanderburg, David R. Ciardi, Lisa Kaltenegger, Jason F. Rowe, Luca Cacciapuoti, Giovanni Isopi, Sara Seager, Rachel A. Matson, Ryan Cloutier, Daria Pidhorodetska, 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), Gilbert, E. A., Barclay, T., Schlieder, J. E., Quintana, E. V., Hord, B. J., Kostov, V. B., Lopez, E. D., Rowe, J. F., Hoffman, K., Walkowicz, L. M., Silverstein, M. L., Rodriguez, J. E., Vanderburg, A., Suissa, G., Airapetian, V. S., Clement, M. S., Raymond, S. N., Mann, A. W., Kruse, E., Lissauer, J. J., Colon, K. D., Kopparapu, R. K., Kreidberg, L., Zieba, S., Collins, K. A., Quinn, S. N., Howell, S. B., Ziegler, C., Vrijmoet, E. H., Adams, F. C., Arney, G. N., Boyd, P. T., Brande, J., Burke, C. J., Cacciapuoti, L., Chance, Q., Christiansen, J. L., Covone, G., Daylan, T., Dineen, D., Dressing, C. D., Essack, Z., Fauchez, T. J., Galgano, B., Howe, A. R., Kaltenegger, L., Kane, S. R., Lam, C., Lee, E. J., Lewis, N. K., Logsdon, S. E., Mandell, A. M., Monsue, T., Mullally, F., Mullally, S. E., Paudel, R. R., Pidhorodetska, D., Plavchan, P., Reyes, N. T., Rinehart, S. A., Rojas-Ayala, B., Smith, J. C., Stassun, K. G., Tenenbaum, P., Vega, L. D., Villanueva, G. L., Wolf, E. T., Youngblood, A., Ricker, G. R., Vanderspek, R. K., Latham, D. W., Seager, S., Winn, J. N., Jenkins, J. M., Bakos, G. A., Briceño, C., Ciardi, D. R., Cloutier, R., Conti, D. M., Couperus, A., Di Sora, M., Eisner, N. L., Everett, M. E., Gan, T., Hartman, J. D., Henry, T., Isopi, G., Jao, W. -C., Jensen, E. L. N., Law, N., Mallia, F., Matson, R. A., Shappee, B. J., Le Wood, M., and Winters, J. G.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Dwarf star, 010504 meteorology & atmospheric sciences, Atmospheric escape, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], James Webb Space Telescope, Ecliptic, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Transit (astronomy), 010303 astronomy & astrophysics, Circumstellar habitable zone, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract

We present the discovery and validation of a three-planet system orbiting the nearby (31.1 pc) M2 dwarf star TOI-700 (TIC 150428135). TOI-700 lies in the TESS continuous viewing zone in the Southern Ecliptic Hemisphere; observations spanning 11 sectors reveal three planets with radii ranging from 1 R$_\oplus$ to 2.6 R$_\oplus$ and orbital periods ranging from 9.98 to 37.43 days. Ground-based follow-up combined with diagnostic vetting and validation tests enable us to rule out common astrophysical false-positive scenarios and validate the system of planets. The outermost planet, TOI-700 d, has a radius of $1.19\pm0.11$ R$_\oplus$ and resides in the conservative habitable zone of its host star, where it receives a flux from its star that is approximately 86% of the Earth's insolation. In contrast to some other low-mass stars that host Earth-sized planets in their habitable zones, TOI-700 exhibits low levels of stellar activity, presenting a valuable opportunity to study potentially-rocky planets over a wide range of conditions affecting atmospheric escape. While atmospheric characterization of TOI-700 d with the James Webb Space Telescope (JWST) will be challenging, the larger sub-Neptune, TOI-700 c (R = 2.63 R$_\oplus$), will be an excellent target for JWST and beyond. TESS is scheduled to return to the Southern Hemisphere and observe TOI-700 for an additional 11 sectors in its extended mission, which should provide further constraints on the known planet parameters and searches for additional planets and transit timing variations in the system., Accepted for publication in AJ (30 pages, 13 figures, 4 tables, 2 appendices)

Published
2020
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13. The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

Author

Jason F. Rowe, Francisco J. Pozuelos, Lucianne M. Walkowicz, Christopher J. Burke, Stephen R. Kane, Eric L. N. Jensen, Brett M. Morris, Daniel Foreman-Mackey, Jonathan Brande, Jessie L. Christiansen, Jon M. Jenkins, Jennifer G. Winters, Thomas Fauchez, Zahra Essack, C. Murray, Elsa Ducrot, Caroline V. Morley, Roland Vanderspek, Charles Beichman, Keivan G. Stassun, Daria Pidhorodetska, Jeffrey Volosin, James D. Armstrong, Laura Vega, Courtney D. Dressing, Elisabeth Matthews, Stephen A. Rinehart, Khalid Barkaoui, Erica J. Gonzales, Susan E. Mullally, Natalie E. Batalha, David Quinn, Elisa V. Quintana, Luca Cacciapuoti, Michaël Gillon, Norio Narita, Vickie Eakin Moran, Samuel Hadden, Ian J. M. Crossfield, Giada Arney, Peter Tenenbaum, Laetitia Delrez, Giovanni Isopi, Sarah E. Moran, Tsevi Mazeh, Teresa Monsue, Matthew Ritsko, David Charbonneau, Knicole D. Colón, Adina D. Feinstein, Giovanni Covone, Dennis M. Conti, Rachel A. Matson, Michael J. Ireland, Kevin I. Collins, Joseph D. Twicken, Christopher Lam, Naylynn Tañón Reyes, Shane Hynes, Philip S. Muirhead, Aaron Hamann, Daniel Bayliss, George R. Ricker, Artem Burdanov, Avi Shporer, Tianjun Gan, Ravi Kumar Kopparapu, Mark E. Everett, Elliott P. Horch, Mark Clampin, Benjamin T. Montet, EnricP alle, David R. Ciardi, Emmanuel Jehin, Joshua E. Schlieder, Shawn Domagal-Goldman, Gerard T. van Belle, Koji Mukai, Eric B. Ting, John F. Kielkopf, Joshua N. Winn, Hannah Hocutt, Sara Seager, Kelsey Hoffman, Fergal Mullally, Joseph E. Rodriguez, Jonathan Irwin, Pamela Rowden, Ramotholo Sefako, Karen A. Collins, Laura Kreidberg, Daniel Sebastian, Thomas Barclay, Andrew W. Mann, Ethan Kruse, Dennis Afanasev, Andrew Carson, Lisa Kaltenegger, Avi Mandell, David W. Latham, Christina Hedges, Eric D. Lopez, Nikole K. Lewis, Howard M. Relles, Patricia T. Boyd, Jeffrey L. Coughlin, F. Mallia, Keith Horne, Sahar Shahaf, Emily A. Gilbert, Jack J. Lissauer, Steve B. Howell, Allison Youngblood, Geert Barentsen, Veselin B. Kostov, Kostov, V. B., Schlieder, J. E., Barclay, T., Quintana, E. V., Colon, K. D., Brande, J., Collins, K. A., Feinstein, A. D., Hadden, S., Kane, S. R., Kreidberg, L., Kruse, E., Lam, C., Matthews, E., Montet, B. T., Pozuelos, F. J., Stassun, K. G., Winters, J. G., Ricker, G., Vanderspek, R., Latham, D., Seager, S., Winn, J., Jenkins, J. M., Afanasev, D., Armstrong, J. J. D., Arney, G., Boyd, P., Barentsen, G., Barkaoui, K., Batalha, N. E., Beichman, C., Bayliss, D., Burke, C., Burdanov, A., Cacciapuoti, L., Carson, A., Charbonneau, D., Christiansen, J., Ciardi, D., Clampin, M., Collins, K. I., Conti, D. M., Coughlin, J., Covone, G., Crossfield, I., Delrez, L., Domagal-Goldman, S., Dressing, C., Ducrot, E., Essack, Z., Everett, M. E., Fauchez, T., Foreman-Mackey, D., Gan, T., Gilbert, E., Gillon, M., Gonzales, E., Hamann, A., Hedges, C., Hocutt, H., Hoffman, K., Horch, E. P., Horne, K., Howell, S., Hynes, S., Ireland, M., Irwin, J. M., Isopi, G., Jensen, E. L. N., Jehin, E., Kaltenegger, L., Kielkopf, J. F., Kopparapu, R., Feenberg, ANDREW LEWIS, Lopez, E., Lissauer, J. J., Mann, A. W., MALLIA MILANES, Giovanna, Mandell, A., Matson, R. A., Mazeh, T., Monsue, T., Moran, S. E., Moran, V., Morley, C. V., Aledort, Louis Morri, Muirhead, P., Mukai, K., Mullally, S., Mullally, F., Murray, ALAN TODD, Narita, N., Palle, E., Pidhorodetska, D., Quinn, D., Relles, H., Rinehart, S., Ritsko, M., Rodriguez, J. E., Rowden, P., Rowe, J. F., Sebastian, D., Sefako, R., Shahaf, S., Shporer, A., Reyes, N. T., Tenenbaum, P., Ting, E. B., Twicken, J. D., Van Belle, G. T., Vega, L., Volosin, J., Walkowicz, L. M., Youngblood, A., 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
planets and satellites: detection, 010504 meteorology & atmospheric sciences, Metallicity, FOS: Physical sciences, 01 natural sciences, techniques: photometric, Planet, 0103 physical sciences, QB Astronomy, Transit (astronomy), stars: individual (TIC 307210830, TOI-175), individual (TIC 307210830, TOI-175) [Stars], 010303 astronomy & astrophysics, QC, QB, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, photometric [Techniques], James Webb Space Telescope, Astronomy, Astronomy and Astrophysics, 3rd-DAS, Planetary system, Exoplanet, detection [Planets and satellites], Photometry (astronomy), QC Physics, Space and Planetary Science, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the Transiting Exoplanet Survey Satellite (TESS) discovery of three terrestrial-sized planets transiting L 98-59 (TOI-175, TIC 307210830) -- a bright M dwarf at a distance of 10.6 pc. Using the Gaia-measured distance and broad-band photometry we find that the host star is an M3 dwarf. Combined with the TESS transits from three sectors, the corresponding stellar parameters yield planet radii ranging from 0.8REarth to 1.6REarth. All three planets have short orbital periods, ranging from 2.25 to 7.45 days with the outer pair just wide of a 2:1 period resonance. Diagnostic tests produced by the TESS Data Validation Report and the vetting package DAVE rule out common false positive sources. These analyses, along with dedicated follow-up and the multiplicity of the system, lend confidence that the observed signals are caused by planets transiting L 98-59 and are not associated with other sources in the field. The L 98-59 system is interesting for a number of reasons: the host star is bright (V = 11.7 mag, K = 7.1 mag) and the planets are prime targets for further follow-up observations including precision radial-velocity mass measurements and future transit spectroscopy with the James Webb Space Telescope; the near resonant configuration makes the system a laboratory to study planetary system dynamical evolution; and three planets of relatively similar size in the same system present an opportunity to study terrestrial planets where other variables (age, metallicity, etc.) can be held constant. L 98-59 will be observed in 4 more TESS sectors, which will provide a wealth of information on the three currently known planets and have the potential to reveal additional planets in the system., 27 pages, 22 figures, AJ accepted

Published
2019

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