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20 results on '"Mullally, S. E."'

1. The first JWST spectrum of a GRB afterglow: No bright supernova in observations of the brightest GRB of all time, GRB 221009A

Author

Levan, A. J., Lamb, G. P., Schneider, B., Hjorth, J., Zafar, T., Postigo, A. de Ugarte, Sargent, B., Mullally, S. E., Izzo, L., D'Avanzo, P., Burns, E., Fernández, J. F. Agüí, Barclay, T., Bernardini, M. G., Bhirombhakdi, K., Bremer, M., Brivio, R., Campana, S., Chrimes, A. A., D'Elia, V., Della Valle, M., De Pasquale, M., Ferro, M., Fong, W., Fruchter, A. S., Fynbo, J. P. U., Gaspari, N., Gompertz, B. P., Hartmann, D. H., Hedges, C. L., Heintz, K. E., Hotokezaka, K., Jakobsson, P., Kann, D. A., Kennea, J. A., Laskar, T., Floc'h, E. Le, Malesani, D. B., Melandri, A., Metzger, B. D., Oates, S. R., Pian, E., Piranomonte, S., Pugliese, G., Racusin, J. L., Rastinejad, J. C., Ravasio, M. E., Rossi, A., Saccardi, A., Salvaterra, R., Sbarufatti, B., Starling, R. L. C., Tanvir, N. R., Thöne, C. C., van der Horst, A. J., Vergani, S. D., Watson, D., Wiersema, K., Wijers, R. A. M. J., and Xu, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present JWST and Hubble Space Telescope (HST) observations of the afterglow of GRB 221009A, the brightest gamma-ray burst (GRB) ever observed. This includes the first mid-IR spectra of any GRB, obtained with JWST/NIRSPEC (0.6-5.5 micron) and MIRI (5-12 micron), 12 days after the burst. Assuming that the intrinsic spectral slope is a single power-law, with $F_{\nu} \propto \nu^{-\beta}$, we obtain $\beta \approx 0.35$, modified by substantial dust extinction with $A_V = 4.9$. This suggests extinction above the notional Galactic value, possibly due to patchy extinction within the Milky Way or dust in the GRB host galaxy. It further implies that the X-ray and optical/IR regimes are not on the same segment of the synchrotron spectrum of the afterglow. If the cooling break lies between the X-ray and optical/IR, then the temporal decay rates would only match a post jet-break model, with electron index $p<2$, and with the jet expanding into a uniform ISM medium. The shape of the JWST spectrum is near-identical in the optical/nIR to X-shooter spectroscopy obtained at 0.5 days and to later time observations with HST. The lack of spectral evolution suggests that any accompanying supernova (SN) is either substantially fainter or bluer than SN 1998bw, the proto-type GRB-SN. Our HST observations also reveal a disc-like host galaxy, viewed close to edge-on, that further complicates the isolation of any supernova component. The host galaxy appears rather typical amongst long-GRB hosts and suggests that the extreme properties of GRB 221009A are not directly tied to its galaxy-scale environment., Comment: Accepted for publication to the Astrophysical Journal Letters for the GRB 221009A Special Issue. The results of this paper are under press embargo until March 28, 18 UT. 19 pages, 8 figures, 2 tables

Published
2023
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2. TOI-220 $b$: a warm sub-Neptune discovered by TESS

Author

Hoyer, S., Gandolfi, D., Armstrong, D. J., Deleuil, M., Acuña, L., de Medeiros, J. R., Goffo, E., Lillo-Box, J., Mena, E. Delgado, Lopez, T. A., Santerne, A., Sousa, S., Fridlund, M., Adibekyan, V., Collins, K. A., Serrano, L. M., Cortés-Zuleta, P., Howell, S. B., Deeg, H., Aguichine, A., Barragán, O., Bryant, E. M., Martins, B. L. Canto, Collins, K. I., Cooke, B. F., Díaz, R. F., Esposito, M., Furlan, E., Hojjatpanah, S., Jackman, J., Jenkins, J. M., Jensen, E. L. N., Latham, D. W., Leão, I. C., Matson, R. A., Nielsen, L. D., Osborn, A., Otegi, J. F., Rodler, F., Sabotta, S., Scott, N. J., Seager, S., Stockdale, C., Strøm, P. A., Vanderspek, R., Van Eylen, V., Wheatley, P. J., Winn, J. N., Almenara, J. M., Barrado, D., Barros, S. C. C., Bayliss, D., Bouchy, F., Boyd, P. T., Cabrera, J., Cochran, W. D., Demangeon, O., Doty, J. P., Dumusque, X., Figueira, P., Fong, W., Grziwa, S., Hatzes, A. P., Kabáth, P., Knudstrup, E., Korth, J., Livingston, J. H., Luque, R., Mousis, O., Mullally, S. E., Osborn, H. P., Pallé, E., Persson, C. M., Redfield, S., Santos, N. C., Smith, J., Šubjak, J., Twicken, J. D., Udry, S., and Yahalomi, D. A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

In this paper we report the discovery of TOI-220 $b$, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 $\pm$ 1.0 M$_{Earth}$ and radius of 3.03 $\pm$ 0.15 R$_{Earth}$, implying a bulk density of 2.73 $\pm$ 0.47 $\textrm{g cm}^{-3}$. TOI-220 $b$ orbits a relative bright (V=10.4) and old (10.1$\pm$1.4 Gyr) K dwarf star with a period of $\sim$10.69 d. Thus, TOI-220 $b$ is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 $b$ internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core., Comment: Accepted for publication in MNRAS

Published
2021
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3. Masses and compositions of three small planets orbiting the nearby M dwarf L231-32 (TOI-270) and the M dwarf radius valley

Author

Van Eylen, Vincent, Astudillo-Defru, N., Bonfils, X., Livingston, J., Hirano, T., Luque, R., Lam, K. W. F., Justesen, A. B., Winn, J. N., Gandolfi, D., Nowak, G., Palle, E., Albrecht, S., Dai, F., Estrada, B. Campos, Owen, J. E., Foreman-Mackey, D., Fridlund, M., Korth, J., Mathur, S., Forveille, T., Mikal-Evans, T., Osborne, H. L. M., Ho, C. S. K., Almenara, J. M., Artigau, E., Barragán, O., Barros, S. C. C., Bouchy, F., Cabrera, J., Caldwell, D. A., Charbonneau, D., Chaturvedi, P., Cochran, W. D., Csizmadia, S., Damasso, M., Delfosse, X., De Medeiros, J. R., Díaz, R. F., Doyon, R., Esposito, M., Fűrész, G., Figueira, P., Georgieva, I., Goffo, E., Grziwa, S., Guenther, E., Hatzes, A. P., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Lavie, B., Lovis, C., Mennickent, R. E., Mullally, S. E., Murgas, F., Narita, N., Pepe, F. A., Persson, C. M., Redfield, S., Ricker, G. R., Santos, N. C., Seager, S., Serrano, L. M., Smith, A. M. S., Mascareño, A. Suárez, Subjak, J., Twicken, J. D., Udry, S., Vanderspek, R., and Osorio, M. R. Zapatero

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

We report on precise Doppler measurements of L231-32 (TOI-270), a nearby M dwarf ($d=22$ pc, $M_\star = 0.39$ M$_\odot$, $R_\star = 0.38$ R$_\odot$), which hosts three transiting planets that were recently discovered using data from the Transiting Exoplanet Survey Satellite (TESS). The three planets are 1.2, 2.4, and 2.1 times the size of Earth and have orbital periods of 3.4, 5.7, and 11.4 days. We obtained 29 high-resolution optical spectra with the newly commissioned Echelle Spectrograph for Rocky Exoplanet and Stable Spectroscopic Observations (ESPRESSO) and 58 spectra using the High Accuracy Radial velocity Planet Searcher (HARPS). From these observations, we find the masses of the planets to be $1.58 \pm 0.26$, $6.15 \pm 0.37$, and $4.78 \pm 0.43$ M$_\oplus$, respectively. The combination of radius and mass measurements suggests that the innermost planet has a rocky composition similar to that of Earth, while the outer two planets have lower densities. Thus, the inner planet and the outer planets are on opposite sides of the `radius valley' -- a region in the radius-period diagram with relatively few members, which has been interpreted as a consequence of atmospheric photo-evaporation. We place these findings into the context of other small close-in planets orbiting M dwarf stars, and use support vector machines to determine the location and slope of the M dwarf ($T_\mathrm{eff} < 4000$ K) radius valley as a function of orbital period. We compare the location of the M dwarf radius valley to the radius valley observed for FGK stars, and find that its location is a good match to photo-evaporation and core-powered mass loss models. Finally, we show that planets below the M dwarf radius valley have compositions consistent with stripped rocky cores, whereas most planets above have a lower density consistent with the presence of a H-He atmosphere., Comment: Accepted for publication in MNRAS

Published
2021
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4. Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey

Author

Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštienė, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Horta, F. Grau, Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., and Henze, C. E.

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

We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of $19.7\pm 1.6$ $M_{\mathrm{Jup}}$ and a radius of $1.47\pm0.10$ $R_{\mathrm{Jup}}$, the first sub-stellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright ($V$ = 12.3 mag) fast-rotating F-type star with a projected rotational velocity $v\sin{ i_*}=40\pm10$ km/s. We use the isochrone placement algorithm to characterize the host star, which has effective temperature $7000\pm200$ K, mass $1.68\pm0.10$ $M_{\mathrm{Sun}}$, radius $1.56\pm0.10$ $R_{\mathrm{Sun}}$ and approximate age $0.27_{-0.15}^{+0.09}$ Gyr. GPX-1 b has an orbital period of $\sim$1.75 d, and a transit depth of $0.90\pm0.03$ %. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a sub-stellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data is affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of Doppler tomography., Comment: 13 pages, 13 figures, accepted to MNRAS in May 2021

Published
2020
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5. The TOI-763 system: sub-Neptunes orbiting a Sun-like star

Author

Fridlund, M., Livingston, J., Gandolfi, D., Persson, C. M., Lam, K. W. F., Stassun, K. G., Hellier, C., Korth, J., Hatzes, A. P., Malavolta, L., Luque, R., Redfield, S., Guenther, E. W., Albrecht, S., Barragan, O., Benatti, S., Bouma, L., Cabrera, J., Cochran, W. D., Csizmadia, Sz., Dai, F., Deeg, H. J., Esposito, M., Georgieva, I., Grziwa, S., Cuesta, L. González, Hirano, T., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Mathur, S., Mullally, S. E., Narita, N., Nowak, G., Olofsson, A. O. H., Palle, E., Pätzold, M., Pompei, E., Rauer, H., Ricker, G., Rodler, F., Seager, S., Serrano, L. M., Smith, A. M. S., Spina, L., Subjak, J., Tenenbaum, P., Ting, E. B., Vanderburg, A., Vanderspek, R., Van Eylen, V., Villanueva, S., and Winn, J. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We report the discovery of a planetary system orbiting TOI-763 (aka CD-39 7945), a $V=10.2$, high proper motion G-type dwarf star that was photometrically monitored by the TESS space mission in Sector 10. We obtain and model the stellar spectrum and find an object slightly smaller than the Sun, and somewhat older, but with a similar metallicity. Two planet candidates were found in the light curve to be transiting the star. Combining TESS transit photometry with HARPS high-precision radial velocity follow-up measurements confirm the planetary nature of these transit signals. We determine masses, radii, and bulk densities of these two planets. A third planet candidate was discovered serendipitously in the radial velocity data. The inner transiting planet,TOI-763 b, has an orbital period of $P_\mathrm{b}$ = 5.6~days, a mass of $M_\mathrm{b}$ = $9.8\pm0.8$ $M_\oplus$, and a radius of $R_\mathrm{b}$ = $2.37\pm0.10$ $R_\oplus$. The second transiting planet,TOI-763 c, has an orbital period of $P_\mathrm{c}$ = 12.3~days, a mass of $M_\mathrm{c}$ = $9.3\pm1.0$ $M_\oplus$, and a radius of $R_\mathrm{c}$ = $2.87\pm0.11$ $R_\oplus$. We find the outermost planet candidate to orbit the star with a period of $\sim$48~days. If confirmed as a planet it would have a minimum mass of $M_\mathrm{d}$ = $9.5\pm1.6$ $M_\oplus$. We investigated the TESS light curve in order to search for a mono transit by planet~d without success. We discuss the importance and implications of this planetary system in terms of the geometrical arrangements of planets orbiting G-type stars.

Published
2020
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6. TESS first look at evolved compact pulsators: Known ZZ Ceti stars of the southern ecliptic hemisphere as seen by TESS

Author

Bognár, Zs., Kawaler, S. D., Bell, K. J., Schrandt, C., Baran, A. S., Bradley, P. A., Hermes, J. J., Charpinet, S., Handler, G., Mullally, S. E., Murphy, S. J., Raddi, R., Sódor, Á., Tremblay, P. -E., Uzundag, M., and Zong, W.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Context. We present our findings on 18 formerly known ZZ Ceti stars observed by the TESS space telescope in 120s cadence mode during the survey observation of the southern ecliptic hemisphere. Aims. We focus on the frequency analysis of the space-based observations, comparing the results with the findings of the previous ground-based measurements. The frequencies detected by the TESS observations can serve as inputs for future asteroseismic analyses. Methods. We performed standard pre-whitening of the data sets to derive the possible pulsation frequencies of the different targets. In some cases, we fitted Lorentzians to the frequency groups that emerged as the results of short-term amplitude/phase variations that occurred during the TESS observations. Results. We detected more than 40 pulsation frequencies in seven ZZ Ceti stars observed in the 120s cadence by TESS, with better than 0.1 microHz precision. We found that HE 0532-5605 may be a new outbursting ZZ Ceti. Ten targets do not show any significant pulsation frequencies in their Fourier transforms, due to a combination of their intrinsic faintness and/or crowding on the large TESS pixels. We also detected possible amplitude/phase variations during the TESS observations in some cases. Such behaviour in these targets was not previously identified from ground-based observations., Comment: 21 pages, 19 figures, accepted for publication in Astronomy & Astrophysics

Published
2020
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7. The First JWST Spectrum of a GRB Afterglow: No Bright Supernova in Observations of the Brightest GRB of all Time, GRB 221009A

Author

Levan, A. J., primary, Lamb, G. P., additional, Schneider, B., additional, Hjorth, J., additional, Zafar, T., additional, de Ugarte Postigo, A., additional, Sargent, B., additional, Mullally, S. E., additional, Izzo, L., additional, D’Avanzo, P., additional, Burns, E., additional, Fernández, J. F. Agüí, additional, Barclay, T., additional, Bernardini, M. G., additional, Bhirombhakdi, K., additional, Bremer, M., additional, Brivio, R., additional, Campana, S., additional, Chrimes, A. A., additional, D’Elia, V., additional, Valle, M. Della, additional, De Pasquale, M., additional, Ferro, M., additional, Fong, W., additional, Fruchter, A. S., additional, Fynbo, J. P. U., additional, Gaspari, N., additional, Gompertz, B. P., additional, Hartmann, D. H., additional, Hedges, C. L., additional, Heintz, K. E., additional, Hotokezaka, K., additional, Jakobsson, P., additional, Kann, D. A., additional, Kennea, J. A., additional, Laskar, T., additional, Le Floc’h, E., additional, Malesani, D. B., additional, Melandri, A., additional, Metzger, B. D., additional, Oates, S. R., additional, Pian, E., additional, Piranomonte, S., additional, Pugliese, G., additional, Racusin, J. L., additional, Rastinejad, J. C., additional, Ravasio, M. E., additional, Rossi, A., additional, Saccardi, A., additional, Salvaterra, R., additional, Sbarufatti, B., additional, Starling, R. L. C., additional, Tanvir, N. R., additional, Thöne, C. C., additional, van der Horst, A. J., additional, Vergani, S. D., additional, Watson, D., additional, Wiersema, K., additional, Wijers, R. A. M. J., additional, and Xu, Dong, additional

Published
2023
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8. The First JWST Spectrum of a GRB Afterglow:No Bright Supernova in Observations of the Brightest GRB of all Time, GRB 221009A

Author

Levan, A. J., Lamb, G. P., Schneider, B., Hjorth, J., Zafar, T., de Ugarte Postigo, A., Sargent, B., Mullally, S. E., Izzo, L., D'Avanzo, P., Burns, E., Fernandez, J. F. Aguei, Barclay, T., Bernardini, M. G., Bhirombhakdi, K., Bremer, M., Brivio, R., Campana, S., Chrimes, A. A., D'Elia, V., Valle, M. Della, De Pasquale, M., Ferro, M., Fong, W., Fruchter, A. S., Fynbo, J. P. U., Gaspari, N., Gompertz, B. P., Hartmann, D. H., Hedges, C. L., Heintz, K. E., Hotokezaka, K., Jakobsson, P., Kann, D. A., Kennea, J. A., Laskar, T., Le Floc'h, E., Malesani, D. B., Melandri, A., Metzger, B. D., Oates, S. R., Pian, E., Piranomonte, S., Pugliese, G., Racusin, J. L., Rastinejad, J. C., Ravasio, M. E., Rossi, A., Saccardi, A., Salvaterra, R., Sbarufatti, B., Starling, R. L. C., Tanvir, N. R., Thoene, C. C., van der Horst, A. J., Vergani, S. D., Watson, D., Wiersema, K., Wijers, R. A. M. J., Xu, Dong, Levan, A. J., Lamb, G. P., Schneider, B., Hjorth, J., Zafar, T., de Ugarte Postigo, A., Sargent, B., Mullally, S. E., Izzo, L., D'Avanzo, P., Burns, E., Fernandez, J. F. Aguei, Barclay, T., Bernardini, M. G., Bhirombhakdi, K., Bremer, M., Brivio, R., Campana, S., Chrimes, A. A., D'Elia, V., Valle, M. Della, De Pasquale, M., Ferro, M., Fong, W., Fruchter, A. S., Fynbo, J. P. U., Gaspari, N., Gompertz, B. P., Hartmann, D. H., Hedges, C. L., Heintz, K. E., Hotokezaka, K., Jakobsson, P., Kann, D. A., Kennea, J. A., Laskar, T., Le Floc'h, E., Malesani, D. B., Melandri, A., Metzger, B. D., Oates, S. R., Pian, E., Piranomonte, S., Pugliese, G., Racusin, J. L., Rastinejad, J. C., Ravasio, M. E., Rossi, A., Saccardi, A., Salvaterra, R., Sbarufatti, B., Starling, R. L. C., Tanvir, N. R., Thoene, C. C., van der Horst, A. J., Vergani, S. D., Watson, D., Wiersema, K., Wijers, R. A. M. J., and Xu, Dong

Abstract

We present James Webb Space Telescope (JWST) and Hubble Space Telescope (HST) observations of the afterglow of GRB 221009A, the brightest gamma-ray burst (GRB) ever observed. This includes the first mid-IR spectra of any GRB, obtained with JWST/Near Infrared Spectrograph (0.6-5.5 micron) and Mid-Infrared Instrument (5-12 micron), 12 days after the burst. Assuming that the intrinsic spectral slope is a single power law, with F ( nu ) proportional to nu (-beta ), we obtain beta approximate to 0.35, modified by substantial dust extinction with A ( V ) = 4.9. This suggests extinction above the notional Galactic value, possibly due to patchy extinction within the Milky Way or dust in the GRB host galaxy. It further implies that the X-ray and optical/IR regimes are not on the same segment of the synchrotron spectrum of the afterglow. If the cooling break lies between the X-ray and optical/IR, then the temporal decay rates would only match a post-jet-break model, with electron index p < 2, and with the jet expanding into a uniform ISM medium. The shape of the JWST spectrum is near-identical in the optical/near-IR to X-SHOOTER spectroscopy obtained at 0.5 days and to later time observations with HST. The lack of spectral evolution suggests that any accompanying supernova (SN) is either substantially fainter or bluer than SN 1998bw, the proto-type GRB-SN. Our HST observations also reveal a disk-like host galaxy, viewed close to edge-on, that further complicates the isolation of any SN component. The host galaxy appears rather typical among long-GRB hosts and suggests that the extreme properties of GRB 221009A are not directly tied to its galaxy-scale environment.

Published
2023

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

Author

Van Eylen, V, primary, Astudillo-Defru, N, additional, Bonfils, X, additional, Livingston, J, additional, Hirano, T, additional, Luque, R, additional, Lam, K W F, additional, Justesen, A B, additional, Winn, J N, additional, Gandolfi, D, additional, Nowak, G, additional, Palle, E, additional, Albrecht, S, additional, Dai, F, additional, Estrada, B Campos, additional, Owen, J E, additional, Foreman-Mackey, D, additional, Fridlund, M, additional, Korth, J, additional, Mathur, S, additional, Forveille, T, additional, Mikal-Evans, T, additional, Osborne, H L M, additional, Ho, C S K, additional, Almenara, J M, additional, Artigau, E, additional, Barragán, O, additional, Barros, S C C, additional, Bouchy, F, additional, Cabrera, J, additional, Caldwell, D A, additional, Charbonneau, D, additional, Chaturvedi, P, additional, Cochran, W D, additional, Csizmadia, S, additional, Damasso, M, additional, Delfosse, X, additional, De Medeiros, J R, additional, Díaz, R F, additional, Doyon, R, additional, Esposito, M, additional, Fűrész, G, additional, Figueira, P, additional, Georgieva, I, additional, Goffo, E, additional, Grziwa, S, additional, Guenther, E, additional, Hatzes, A P, additional, Jenkins, J M, additional, Kabath, P, additional, Knudstrup, E, additional, Latham, D W, additional, Lavie, B, additional, Lovis, C, additional, Mennickent, R E, additional, Mullally, S E, additional, Murgas, F, additional, Narita, N, additional, Pepe, F A, additional, Persson, C M, additional, Redfield, S, additional, Ricker, G R, additional, Santos, N C, additional, Seager, S, additional, Serrano, L M, additional, Smith, A M S, additional, Mascareño, A Suárez, additional, Subjak, J, additional, Twicken, J D, additional, Udry, S, additional, Vanderspek, R, additional, and Osorio, M R Zapatero, additional

Published
2021
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10. TOI-220b: a warm sub-Neptune discovered by TESS

Author

Hoyer, S., Gandolfi, D., Armstrong, D. J., Deleuil, M., Acuna, L., de Medeiros, J. R., Goffo, E., Lillo-Box, J., Delgado Mena, E., Lopez, T. A., Santerne, A., Sousa, S., Fridlund, M., Adibekyan, V, Collins, K. A., Serrano, L. M., Cortes-Zuleta, P., Howell, S. B., Deeg, H., Aguichine, A., Barragan, O., Bryant, E. M., Canto Martins, B. L., Collins, K., I, Cooke, B. F., Diaz, R. F., Esposito, M., Furlan, E., Hojjatpanah, S., Jackman, J., Jenkins, J. M., Jensen, E. L. N., Latham, D. W., Leao, I. C., Matson, R. A., Nielsen, L. D., Osborn, A., Otegi, J. F., Rodler, F., Sabotta, S., Scott, N. J., Seager, S., Stockdale, C., Strom, P. A., Vanderspek, R., Van Eylen, V., Wheatley, P. J., Winn, J. N., Almenara, J. M., Barrado, D., Barros, S. C. C., Bayliss, D., Bouchy, F., Boyd, P. T., Cabrera, J., Cochran, W. D., Demangeon, O., Doty, J. P., Dumusque, X., Figueira, P., Fong, W., Grziwa, S., Hatzes, A. P., Kabath, P., Knudstrup, E., Korth, J., Livingston, J. H., Luque, R., Mousis, O., Mullally, S. E., Osborn, H. P., Palle, E., Persson, C. M., Redfield, S., Santos, N. C., Smith, J., Subjak, J., Twicken, J. D., Udry, S., Yahalomi, D. A., Hoyer, S., Gandolfi, D., Armstrong, D. J., Deleuil, M., Acuna, L., de Medeiros, J. R., Goffo, E., Lillo-Box, J., Delgado Mena, E., Lopez, T. A., Santerne, A., Sousa, S., Fridlund, M., Adibekyan, V, Collins, K. A., Serrano, L. M., Cortes-Zuleta, P., Howell, S. B., Deeg, H., Aguichine, A., Barragan, O., Bryant, E. M., Canto Martins, B. L., Collins, K., I, Cooke, B. F., Diaz, R. F., Esposito, M., Furlan, E., Hojjatpanah, S., Jackman, J., Jenkins, J. M., Jensen, E. L. N., Latham, D. W., Leao, I. C., Matson, R. A., Nielsen, L. D., Osborn, A., Otegi, J. F., Rodler, F., Sabotta, S., Scott, N. J., Seager, S., Stockdale, C., Strom, P. A., Vanderspek, R., Van Eylen, V., Wheatley, P. J., Winn, J. N., Almenara, J. M., Barrado, D., Barros, S. C. C., Bayliss, D., Bouchy, F., Boyd, P. T., Cabrera, J., Cochran, W. D., Demangeon, O., Doty, J. P., Dumusque, X., Figueira, P., Fong, W., Grziwa, S., Hatzes, A. P., Kabath, P., Knudstrup, E., Korth, J., Livingston, J. H., Luque, R., Mousis, O., Mullally, S. E., Osborn, H. P., Palle, E., Persson, C. M., Redfield, S., Santos, N. C., Smith, J., Subjak, J., Twicken, J. D., Udry, S., and Yahalomi, D. A.

Abstract

In this paper, we report the discovery of TOI-220b, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements, we estimate a planetary mass of 13.8 +/- 1.0M(circle plus) and radius of 3.03 +/- 0.15R(circle plus), implying a bulk density of 2.73 +/- 0.47. TOI-220b orbits a relative bright (V=10.4) and old (10.1 +/- 1.4Gyr) K dwarf star with a period of similar to 10.69d. Thus, TOI-220b is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220b internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core.

Published
2021

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

Author

Van Eylen, V., Astudillo-Defru, N., Bonfils, X., Livingston, J., Hirano, T., Luque, R., Lam, K. W. F., Justesen, A. B., Winn, J. N., Gandolfi, D., Nowak, G., Palle, E., Albrecht, S., Dai, F., Estrada, B. Campos, Owen, J. E., Foreman-Mackey, D., Fridlund, M., Korth, J., Mathur, S., Forveille, T., Mikal-Evans, T., Osborne, H. L. M., Ho, C. S. K., Almenara, J. M., Artigau, E., Barragan, O., Barros, S. C. C., Bouchy, F., Cabrera, J., Caldwell, D. A., Charbonneau, D., Chaturvedi, P., Cochran, W. D., Csizmadia, S., Damasso, M., Delfosse, X., De Medeiros, J. R., Diaz, R. F., Doyon, R., Esposito, M., Furesz, G., Figueira, P., Georgieva, I, Goffo, E., Grziwa, S., Guenther, E., Hatzes, A. P., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Lavie, B., Lovis, C., Mennickent, R. E., Mullally, S. E., Murgas, F., Narita, N., Pepe, F. A., Persson, C. M., Redfield, S., Ricker, G. R., Santos, N. C., Seager, S., Serrano, L. M., Smith, A. M. S., Suarez Mascareno, A., Subjak, J., Twicken, J. D., Udry, S., Vanderspek, R., Zapatero Osorio, M. R., Van Eylen, V., Astudillo-Defru, N., Bonfils, X., Livingston, J., Hirano, T., Luque, R., Lam, K. W. F., Justesen, A. B., Winn, J. N., Gandolfi, D., Nowak, G., Palle, E., Albrecht, S., Dai, F., Estrada, B. Campos, Owen, J. E., Foreman-Mackey, D., Fridlund, M., Korth, J., Mathur, S., Forveille, T., Mikal-Evans, T., Osborne, H. L. M., Ho, C. S. K., Almenara, J. M., Artigau, E., Barragan, O., Barros, S. C. C., Bouchy, F., Cabrera, J., Caldwell, D. A., Charbonneau, D., Chaturvedi, P., Cochran, W. D., Csizmadia, S., Damasso, M., Delfosse, X., De Medeiros, J. R., Diaz, R. F., Doyon, R., Esposito, M., Furesz, G., Figueira, P., Georgieva, I, Goffo, E., Grziwa, S., Guenther, E., Hatzes, A. P., Jenkins, J. M., Kabath, P., Knudstrup, E., Latham, D. W., Lavie, B., Lovis, C., Mennickent, R. E., Mullally, S. E., Murgas, F., Narita, N., Pepe, F. A., Persson, C. M., Redfield, S., Ricker, G. R., Santos, N. C., Seager, S., Serrano, L. M., Smith, A. M. S., Suarez Mascareno, A., Subjak, J., Twicken, J. D., Udry, S., Vanderspek, R., and Zapatero Osorio, M. R.

Abstract

We report on precise Doppler measurements of L231-32 (TOI-270), a nearby M dwarf (d = 22pc, M-star = 0.39 M-circle dot, R-star = 0.38 R-circle dot), which hosts three transiting planets that were recently discovered using data from the Transiting Exoplanet Survey Satellite (TESS). The three planets are 1.2, 2.4, and 2.1 times the size of Earth and have orbital periods of 3.4, 5.7, and 11.4 d. We obtained 29 high-resolution optical spectra with the newly commissioned Echelle Spectrograph for Rocky Exoplanet and Stable Spectroscopic Observations (ESPRESSO) and 58 spectra using the High Accuracy Radial velocity Planet Searcher (HARPS). From these observations, we find the masses of the planets to be 1.58 +/- 0.26, 6.15 +/- 0.37, and 4.78 +/- 0.43 M-circle plus, respectively. The combination of radius and mass measurements suggests that the innermost planet has a rocky composition similar to that of Earth, while the outer two planets have lower densities. Thus, the inner planet and the outer planets are on opposite sides of the 'radius valley' - a region in the radius-period diagram with relatively few members - which has been interpreted as a consequence of atmospheric photoevaporation. We place these findings into the context of other small close-in planets orbiting M dwarf stars, and use support vector machines to determine the location and slope of the M dwarf (T-eff < 4000 K) radius valley as a function of orbital period. We compare the location of the M dwarf radius valley to the radius valley observed for FGK stars, and find that its location is a good match to photoevaporation and core-powered mass-loss models. Finally, we show that planets below the M dwarf radius valley have compositions consistent with stripped rocky cores, whereas most planets above have a lower density consistent with the presence of a H-He atmosphere.

Published
2021

12. TOI-220 b: a warm sub-Neptune discovered by TESS

Author

Hoyer, S., Gandolfi, D., Armstrong, D. J., Deleuil, M., Acuna, L., de Medeiros, J. R., Goffo, E., Lillo-Box, J., Delgado Mena, E., Lopez, T. A., Santerne, A., Sousa, S., Fridlund, M., Adibekyan, V, Collins, K. A., Serrano, L. M., Cortes-Zuleta, P., Howell, S. B., Deeg, H., Aguichine, A., Barragan, O., Bryant, E. M., Canto Martins, B. L., Collins, K., I, Cooke, B. F., Diaz, R. F., Esposito, M., Furlan, E., Hojjatpanah, S., Jackman, J., Jenkins, J. M., Jensen, E. L. N., Latham, D. W., Leao, I. C., Matson, R. A., Nielsen, L. D., Osborn, A., Otegi, J. F., Rodler, F., Sabotta, S., Scott, N. J., Seager, S., Stockdale, C., Strom, P. A., Vanderspek, R., Van Eylen, V., Wheatley, P. J., Winn, J. N., Almenara, J. M., Barrado, D., Barros, S. C. C., Bayliss, D., Bouchy, F., Boyd, P. T., Cabrera, J., Cochran, W. D., Demangeon, O., Doty, J. P., Dumusque, X., Figueira, P., Fong, W., Grziwa, S., Hatzes, A. P., Kabath, P., Knudstrup, E., Korth, J., Livingston, J. H., Luque, R., Mousis, O., Mullally, S. E., Osborn, H. P., Palle, E., Persson, C. M., Redfield, S., Santos, N. C., Smith, J., Subjak, J., Twicken, J. D., Udry, S., Yahalomi, D. A., Hoyer, S., Gandolfi, D., Armstrong, D. J., Deleuil, M., Acuna, L., de Medeiros, J. R., Goffo, E., Lillo-Box, J., Delgado Mena, E., Lopez, T. A., Santerne, A., Sousa, S., Fridlund, M., Adibekyan, V, Collins, K. A., Serrano, L. M., Cortes-Zuleta, P., Howell, S. B., Deeg, H., Aguichine, A., Barragan, O., Bryant, E. M., Canto Martins, B. L., Collins, K., I, Cooke, B. F., Diaz, R. F., Esposito, M., Furlan, E., Hojjatpanah, S., Jackman, J., Jenkins, J. M., Jensen, E. L. N., Latham, D. W., Leao, I. C., Matson, R. A., Nielsen, L. D., Osborn, A., Otegi, J. F., Rodler, F., Sabotta, S., Scott, N. J., Seager, S., Stockdale, C., Strom, P. A., Vanderspek, R., Van Eylen, V., Wheatley, P. J., Winn, J. N., Almenara, J. M., Barrado, D., Barros, S. C. C., Bayliss, D., Bouchy, F., Boyd, P. T., Cabrera, J., Cochran, W. D., Demangeon, O., Doty, J. P., Dumusque, X., Figueira, P., Fong, W., Grziwa, S., Hatzes, A. P., Kabath, P., Knudstrup, E., Korth, J., Livingston, J. H., Luque, R., Mousis, O., Mullally, S. E., Osborn, H. P., Palle, E., Persson, C. M., Redfield, S., Santos, N. C., Smith, J., Subjak, J., Twicken, J. D., Udry, S., and Yahalomi, D. A.

Abstract

In this paper, we report the discovery of TOI-220 b, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements, we estimate a planetary mass of 13.8 +/- 1.0M circle plus and radius of 3.03 +/- 0.15 R circle plus, implying a bulk density of 2.73 +/- 0.47 g cm(-3). TOI-220 b orbits a relative bright (V = 10.4) and old (10.1 +/- 1.4Gyr) K dwarf star with a period of similar to 10.69 d. Thus, TOI-220 b is a new warm sub-Neptune with very precise mass and radius determinations. A Bayesian analysis of the TOI-220 b internal structure indicates that due to the strong irradiation it receives, the low density of this planet could be explained with a steam atmosphere in radiative-convective equilibrium and a supercritical water layer on top of a differentiated interior made of a silicate mantle and a small iron core.

Published
2021

13. Discovery of a Young Low-Mass Brown Dwarf Transiting a Fast-Rotating F-Type Star by the Galactic Plane eXoplanet (GPX) Survey

Author

Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštiene, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Grau Horta, F., Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., Henze, C. E., Benni, P., Burdanov, A. Y., Krushinsky, V. V., Bonfanti, A., Hébrard, G., Almenara, J. M., Dalal, S., Demangeon, O. D. S., Tsantaki, M., Pepper, J., Stassun, K. G., Vanderburg, A., Belinski, A., Kashaev, F., Barkaoui, K., Kim, T., Kang, W., Antonyuk, K., Dyachenko, V. V., Rastegaev, D. A., Beskakotov, A., Mitrofanova, A. A., Pozuelos, F. J., Kuznetsov, E. D., Popov, A., Kiefer, F., Wilson, P. A., Ricker, G., Vanderspek, R., Latham, D. W., Seager, S., Jenkins, J. M., Sokov, E., Sokova, I., Marchini, A., Papini, R., Salvaggio, F., Banfi, M., Baştürk, Ö., Torun, Ş., Yalçınkaya, S., Ivanov, K., Valyavin, G., Jehin, E., Gillon, M., Pakštiene, E., Hentunen, V. -P., Shadick, S., Bretton, M., Wünsche, A., Garlitz, J., Jongen, Y., Molina, D., Girardin, E., Grau Horta, F., Naves, R., Benkhaldoun, Z., Joner, M. D., Spencer, M., Bieryla, A., Stevens, D. J., Jensen, E. L. N., Collins, K. A., Charbonneau, D., Quintana, E. V., Mullally, S. E., and Henze, C. E.

Abstract

We announce the discovery of GPX-1 b, a transiting brown dwarf with a mass of 19.7 ± 1.6 MJup and a radius of 1.47 ± 0.10 RJup, the first substellar object discovered by the Galactic Plane eXoplanet (GPX) survey. The brown dwarf transits a moderately bright (V = 12.3 mag) fast-rotating F-type star with a projected rotational velocity v sin i∗ = 40 ± 10 km s−1. We use the isochrone placement algorithm to characterize the host star, which has effective temperature 7000 ± 200 K, mass 1.68 ± 0.10 M☉, radius 1.56 ± 0.10 R☉, and approximate age 0.27-0.15+0.09 Gyr. GPX-1 b has an orbital period of -1.75 d and a transit depth of 0.90 ± 0.03 per cent. We describe the GPX transit detection observations, subsequent photometric and speckle-interferometric follow-up observations, and SOPHIE spectroscopic measurements, which allowed us to establish the presence of a substellar object around the host star. GPX-1 was observed at 30-min integrations by TESS in Sector 18, but the data are affected by blending with a 3.4 mag brighter star 42 arcsec away. GPX-1 b is one of about two dozen transiting brown dwarfs known to date, with a mass close to the theoretical brown dwarf/gas giant planet mass transition boundary. Since GPX-1 is a moderately bright and fast-rotating star, it can be followed-up by the means of the Doppler tomography. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

Published
2021

14. TOI-1259Ab - A Gas Giant Planet with 2.7 Per Cent Deep Transits and a Bound white Dwarf Companion

Author

Martin, D. V., El-Badry, K., Hodžić, V. K., Triaud, A. H. M. J., Angus, R., Birky, J., Foreman-Mackey, D., Hedges, C., Montet, B. T., Murphy, S. J., Santerne, A., Stassun, K. G., Stephan, A. P., Wang, J., Benni, P., Krushinsky, V., Chazov, N., Mishevskiy, N., Ziegler, C., Soubkiou, A., Benkhaldoun, Z., Boisse, I., Battley, M., Miller, N. J., Caldwell, D. A., Collins, K., Henze, C. E., Guerrero, N. M., Jenkins, J. M., Latham, D. W., Levine, A., McDermott, S., Mullally, S. E., Ricker, G., Seager, S., Shporer, A., Vanderburg, A., Vanderspek, R., Winn, J. N., Martin, D. V., El-Badry, K., Hodžić, V. K., Triaud, A. H. M. J., Angus, R., Birky, J., Foreman-Mackey, D., Hedges, C., Montet, B. T., Murphy, S. J., Santerne, A., Stassun, K. G., Stephan, A. P., Wang, J., Benni, P., Krushinsky, V., Chazov, N., Mishevskiy, N., Ziegler, C., Soubkiou, A., Benkhaldoun, Z., Boisse, I., Battley, M., Miller, N. J., Caldwell, D. A., Collins, K., Henze, C. E., Guerrero, N. M., Jenkins, J. M., Latham, D. W., Levine, A., McDermott, S., Mullally, S. E., Ricker, G., Seager, S., Shporer, A., Vanderburg, A., Vanderspek, R., and Winn, J. N.

Abstract

We present TOI-1259Ab, a 1.0RJup gas giant planet transiting a 0.71R⊙ K-dwarf on a 3.48 d orbit. The system also contains a bound white dwarf companion TOI-1259B with a projected distance of ∼1600 au from the planet host. Transits are observed in nine TESS sectors and are 2.7 per cent deep - among the deepest known - making TOI-1259Ab a promising target for atmospheric characterization. Our follow-up radial velocity measurements indicate a variability of semiamplitude $K=71\, \rm m\, s^{-1}$, implying a planet mass of 0.44MJup. By fitting the spectral energy distribution of the white dwarf, we derive a total age of $4.08^{+1.21}_{-0.53}$ Gyr for the system. The K dwarf's light curve reveals rotational variability with a period of 28 d, which implies a gyrochronology age broadly consistent with the white dwarf's total age. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

Published
2021

15. Discovery of a young low-mass brown dwarf transiting a fast-rotating F-type star by the Galactic Plane eXoplanet (GPX) survey

Author

Benni, P, primary, Burdanov, A Y, additional, Krushinsky, V V, additional, Bonfanti, A, additional, Hébrard, G, additional, Almenara, J M, additional, Dalal, S, additional, Demangeon, O D S, additional, Tsantaki, M, additional, Pepper, J, additional, Stassun, K G, additional, Vanderburg, A, additional, Belinski, A, additional, Kashaev, F, additional, Barkaoui, K, additional, Kim, T, additional, Kang, W, additional, Antonyuk, K, additional, Dyachenko, V V, additional, Rastegaev, D A, additional, Beskakotov, A, additional, Mitrofanova, A A, additional, Pozuelos, F J, additional, Kuznetsov, E D, additional, Popov, A, additional, Kiefer, F, additional, Wilson, P A, additional, Ricker, G, additional, Vanderspek, R, additional, Latham, D W, additional, Seager, S, additional, Jenkins, J M, additional, Sokov, E, additional, Sokova, I, additional, Marchini, A, additional, Papini, R, additional, Salvaggio, F, additional, Banfi, M, additional, Baştürk, Ö, additional, Torun, Ş, additional, Yalçınkaya, S, additional, Ivanov, K, additional, Valyavin, G, additional, Jehin, E, additional, Gillon, M, additional, Pakštienė, E, additional, Hentunen, V-P, additional, Shadick, S, additional, Bretton, M, additional, Wünsche, A, additional, Garlitz, J, additional, Jongen, Y, additional, Molina, D, additional, Girardin, E, additional, Grau Horta, F, additional, Naves, R, additional, Benkhaldoun, Z, additional, Joner, M D, additional, Spencer, M, additional, Bieryla, A, additional, Stevens, D J, additional, Jensen, E L N, additional, Collins, K A, additional, Charbonneau, D, additional, Quintana, E V, additional, Mullally, S E, additional, and Henze, C E, additional

Published
2021
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16. TOI-220 b: a warm sub-Neptune discovered by TESS

Author

Hoyer, S, primary, Gandolfi, D, additional, Armstrong, D J, additional, Deleuil, M, additional, Acuña, L, additional, de Medeiros, J R, additional, Goffo, E, additional, Lillo-Box, J, additional, Delgado Mena, E, additional, Lopez, T A, additional, Santerne, A, additional, Sousa, S, additional, Fridlund, M, additional, Adibekyan, V, additional, Collins, K A, additional, Serrano, L M, additional, Cortés-Zuleta, P, additional, Howell, S B, additional, Deeg, H, additional, Aguichine, A, additional, Barragán, O, additional, Bryant, E M, additional, Canto Martins, B L, additional, Collins, K I, additional, Cooke, B F, additional, Díaz, R F, additional, Esposito, M, additional, Furlan, E, additional, Hojjatpanah, S, additional, Jackman, J, additional, Jenkins, J M, additional, Jensen, E L N, additional, Latham, D W, additional, Leão, I C, additional, Matson, R A, additional, Nielsen, L D, additional, Osborn, A, additional, Otegi, J F, additional, Rodler, F, additional, Sabotta, S, additional, Scott, N J, additional, Seager, S, additional, Stockdale, C, additional, Strøm, P A, additional, Vanderspek, R, additional, Van Eylen, V, additional, Wheatley, P J, additional, Winn, J N, additional, Almenara, J M, additional, Barrado, D, additional, Barros, S C C, additional, Bayliss, D, additional, Bouchy, F, additional, Boyd, P T, additional, Cabrera, J, additional, Cochran, W D, additional, Demangeon, O, additional, Doty, J P, additional, Dumusque, X, additional, Figueira, P, additional, Fong, W, additional, Grziwa, S, additional, Hatzes, A P, additional, Kabáth, P, additional, Knudstrup, E, additional, Korth, J, additional, Livingston, J H, additional, Luque, R, additional, Mousis, O, additional, Mullally, S E, additional, Osborn, H P, additional, Pallé, E, additional, Persson, C M, additional, Redfield, S, additional, Santos, N C, additional, Smith, J, additional, Šubjak, J, additional, Twicken, J D, additional, Udry, S, additional, and Yahalomi, D A, additional

Published
2021
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17. The TOI-763 system: sub-Neptunes orbiting a Sun-like star

Author

Fridlund, M, primary, Livingston, J, additional, Gandolfi, D, additional, Persson, C M, additional, Lam, K W F, additional, Stassun, K G, additional, Hellier, C, additional, Korth, J, additional, Hatzes, A P, additional, Malavolta, L, additional, Luque, R, additional, Redfield, S, additional, Guenther, E W, additional, Albrecht, S, additional, Barragan, O, additional, Benatti, S, additional, Bouma, L, additional, Cabrera, J, additional, Cochran, W D, additional, Csizmadia, S, additional, Dai, F, additional, Deeg, H J, additional, Esposito, M, additional, Georgieva, I, additional, Grziwa, S, additional, González Cuesta, L, additional, Hirano, T, additional, Jenkins, J M, additional, Kabath, P, additional, Knudstrup, E, additional, Latham, D W, additional, Mathur, S, additional, Mullally, S E, additional, Narita, N, additional, Nowak, G, additional, Olofsson, A O H, additional, Palle, E, additional, Pätzold, M, additional, Pompei, E, additional, Rauer, H, additional, Ricker, G, additional, Rodler, F, additional, Seager, S, additional, Serrano, L M, additional, Smith, A M S, additional, Spina, L, additional, Subjak, J, additional, Tenenbaum, P, additional, Ting, E B, additional, Vanderburg, A, additional, Vanderspek, R, additional, Van Eylen, V, additional, Villanueva, S, additional, and Winn, J N, additional

Published
2020
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18. TESS first look at evolved compact pulsators

Author

Bognár, Zs., primary, Kawaler, S. D., additional, Bell, K. J., additional, Schrandt, C., additional, Baran, A. S., additional, Bradley, P. A., additional, Hermes, J. J., additional, Charpinet, S., additional, Handler, G., additional, Mullally, S. E., additional, Murphy, S. J., additional, Raddi, R., additional, Sódor, Á., additional, Tremblay, P.-E., additional, Uzundag, M., additional, and Zong, W., additional

Published
2020
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20. 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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