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185 results on '"Smith, Alexis M. S."'

151. K2-155: A Bright Metal-poor M Dwarf with Three Transiting Super-Earths

Author

Hirano, Teruyuki, primary, Dai, Fei, additional, Livingston, John H., additional, Fujii, Yuka, additional, Cochran, William D., additional, Endl, Michael, additional, Gandolfi, Davide, additional, Redfield, Seth, additional, Winn, Joshua N., additional, Guenther, Eike W., additional, Prieto-Arranz, Jorge, additional, Albrecht, Simon, additional, Barragan, Oscar, additional, Cabrera, Juan, additional, Cauley, P. Wilson, additional, Csizmadia, Szilard, additional, Deeg, Hans, additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, Fridlund, Malcolm, additional, Fukui, Akihiko, additional, Grziwa, Sascha, additional, Hatzes, Artie P., additional, Korth, Judith, additional, Narita, Norio, additional, Nespral, David, additional, Niraula, Prajwal, additional, Nowak, Grzegorz, additional, Pätzold, Martin, additional, Palle, Enric, additional, Persson, Carina M., additional, Rauer, Heike, additional, Ribas, Ignasi, additional, Smith, Alexis M. S., additional, and Eylen, Vincent Van, additional

Published
2018
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152. Exoplanets around Low-mass Stars Unveiled byK2

Author

Hirano, Teruyuki, primary, Dai, Fei, additional, Gandolfi, Davide, additional, Fukui, Akihiko, additional, Livingston, John H., additional, Miyakawa, Kohei, additional, Endl, Michael, additional, Cochran, William D., additional, Alonso-Floriano, Francisco J., additional, Kuzuhara, Masayuki, additional, Montes, David, additional, Ryu, Tsuguru, additional, Albrecht, Simon, additional, Barragan, Oscar, additional, Cabrera, Juan, additional, Csizmadia, Szilard, additional, Deeg, Hans, additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, Fridlund, Malcolm, additional, Grziwa, Sascha, additional, Guenther, Eike W., additional, Hatzes, Artie P., additional, Korth, Judith, additional, Kudo, Tomoyuki, additional, Kusakabe, Nobuhiko, additional, Narita, Norio, additional, Nespral, David, additional, Nowak, Grzegorz, additional, Pätzold, Martin, additional, Palle, Enric, additional, Persson, Carina M., additional, Prieto-Arranz, Jorge, additional, Rauer, Heike, additional, Ribas, Ignasi, additional, Sato, Bun’ei, additional, Smith, Alexis M. S., additional, Tamura, Motohide, additional, Tanaka, Yusuke, additional, Van Eylen, Vincent, additional, and Winn, Joshua N., additional

Published
2018
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153. Three Small Planets Transiting a Hyades Star

Author

Livingston, John H., primary, Dai, Fei, additional, Hirano, Teruyuki, additional, Gandolfi, Davide, additional, Nowak, Grzegorz, additional, Endl, Michael, additional, Velasco, Sergio, additional, Fukui, Akihiko, additional, Narita, Norio, additional, Prieto-Arranz, Jorge, additional, Barragan, Oscar, additional, Cusano, Felice, additional, Albrecht, Simon, additional, Cabrera, Juan, additional, Cochran, William D., additional, Csizmadia, Szilard, additional, Deeg, Hans J., additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, Fridlund, Malcolm, additional, Grziwa, Sascha, additional, Guenther, Eike W., additional, Hatzes, Artie P., additional, Kawauchi, Kiyoe, additional, Korth, Judith, additional, Nespral, David, additional, Palle, Enric, additional, Pätzold, Martin, additional, Persson, Carina M., additional, Rauer, Heike, additional, Smith, Alexis M. S., additional, Tamura, Motohide, additional, Tanaka, Yusuke, additional, Van Eylen, Vincent, additional, Watanabe, Noriharu, additional, and Winn, Joshua N., additional

Published
2018
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154. EPIC 211391664b: A 32 Earth-mass Neptune-size Planet in a 10 Day Orbit Transiting an F8 Star

Author

Barragán, Oscar, Grziwa, Sascha, Gandolfi, Davide, Fridlund, Malcolm, Endl, Michael, Deeg, Hans J., Cagigal, Manuel P., LANZA, Antonino Francesco, Prada Moroni, Pier G., Smith, Alexis M. S., Korth, Judith, Bedell, Megan, Cabrera, Juan, Cochran, William D., CUSANO, FELICE, Csizmadia, Szilard, Eigmüller, Philipp, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Nespral, David, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, and ITA

Abstract

We report the discovery of K2-98b (EPIC 211391664b), a transiting Neptune-size planet monitored by the K2 mission during its Campaign 5. We combine the K2 time-series data with ground-based photometric and spectroscopic follow-up observations to confirm the planetary nature of the object and derive its mass, radius, and orbital parameters. K2-98b is a warm Neptune-like planet in a 10 day orbit around a V = 12.2 mag F-type star with M_star = 1.074 ± 0.042 M_sun, R_star = 1.311 (-0.048, +0.083) R_sun, and age of 5.2 (-1.0, +1.2) Gyr. We derive a planetary mass and radius of M_planet = 32.2 ± 8.1 M_earth and R_planet = 4.3 (-0.2, +0.3) R_earth. K2-98b joins the relatively small group of Neptune-size planets whose mass and radius have been derived with a precision better than 25%. We estimate that the planet will be engulfed by its host star in ∼3 Gyr, due to the evolution of the latter toward the red giant branch.

Published
2016

155. Three Super-Earths Transiting the Nearby Star GJ 9827

Author

Niraula, Prajwal, primary, Redfield, Seth, additional, Dai, Fei, additional, Barragán, Oscar, additional, Gandolfi, Davide, additional, Cauley, P. Wilson, additional, Hirano, Teruyuki, additional, Korth, Judith, additional, Smith, Alexis M. S., additional, Prieto-Arranz, Jorge, additional, Grziwa, Sascha, additional, Fridlund, Malcolm, additional, Persson, Carina M., additional, Justesen, Anders Bo, additional, Winn, Joshua N., additional, Albrecht, Simon, additional, Cochran, William D., additional, Csizmadia, Szilard, additional, Duvvuri, Girish M., additional, Endl, Michael, additional, Hatzes, Artie P., additional, Livingston, John H., additional, Narita, Norio, additional, Nespral, David, additional, Nowak, Grzegorz, additional, Pätzold, Martin, additional, Palle, Enric, additional, and Van Eylen, Vincent, additional

Published
2017
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156. The Discovery and Mass Measurement of a New Ultra-short-period Planet: K2-131b

Author

Dai, Fei, primary, Winn, Joshua N., additional, Gandolfi, Davide, additional, Wang, Sharon X., additional, Teske, Johanna K., additional, Burt, Jennifer, additional, Albrecht, Simon, additional, Barragán, Oscar, additional, Cochran, William D., additional, Endl, Michael, additional, Fridlund, Malcolm, additional, Hatzes, Artie P., additional, Hirano, Teruyuki, additional, Hirsch, Lea A., additional, Johnson, Marshall C., additional, Bo Justesen, Anders, additional, Livingston, John, additional, Persson, Carina M., additional, Prieto-Arranz, Jorge, additional, Vanderburg, Andrew, additional, Alonso, Roi, additional, Antoniciello, Giuliano, additional, Arriagada, Pamela, additional, Butler, R. P., additional, Cabrera, Juan, additional, Crane, Jeffrey D., additional, Cusano, Felice, additional, Csizmadia, Szilárd, additional, Deeg, Hans, additional, Dieterich, Sergio B., additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, Everett, Mark E., additional, Fukui, Akihiko, additional, Grziwa, Sascha, additional, Guenther, Eike W., additional, Henry, Gregory W., additional, Howell, Steve B., additional, Johnson, John Asher, additional, Korth, Judith, additional, Kuzuhara, Masayuki, additional, Narita, Norio, additional, Nespral, David, additional, Nowak, Grzegorz, additional, Palle, Enric, additional, Pätzold, Martin, additional, Rauer, Heike, additional, Rodríguez, Pilar Montañés, additional, Shectman, Stephen A., additional, Smith, Alexis M. S., additional, Thompson, Ian B., additional, Eylen, Vincent Van, additional, Williamson, Michael W., additional, and Wittenmyer, Robert A., additional

Published
2017
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157. The Next Generation Transit Survey (NGTS)

Author

Wheatley, Peter J, primary, West, Richard G, additional, Goad, Michael R, additional, Jenkins, James S, additional, Pollacco, Don L, additional, Queloz, Didier, additional, Rauer, Heike, additional, Udry, Stéphane, additional, Watson, Christopher A, additional, Chazelas, Bruno, additional, Eigmüller, Philipp, additional, Lambert, Gregory, additional, Genolet, Ludovic, additional, McCormac, James, additional, Walker, Simon, additional, Armstrong, David J, additional, Bayliss, Daniel, additional, Bento, Joao, additional, Bouchy, François, additional, Burleigh, Matthew R, additional, Cabrera, Juan, additional, Casewell, Sarah L, additional, Chaushev, Alexander, additional, Chote, Paul, additional, Csizmadia, Szilárd, additional, Erikson, Anders, additional, Faedi, Francesca, additional, Foxell, Emma, additional, Gänsicke, Boris T, additional, Gillen, Edward, additional, Grange, Andrew, additional, Günther, Maximilian N, additional, Hodgkin, Simon T, additional, Jackman, James, additional, Jordán, Andrés, additional, Louden, Tom, additional, Metrailler, Lionel, additional, Moyano, Maximiliano, additional, Nielsen, Louise D, additional, Osborn, Hugh P, additional, Poppenhaeger, Katja, additional, Raddi, Roberto, additional, Raynard, Liam, additional, Smith, Alexis M S, additional, Soto, Maritza, additional, and Titz-Weider, Ruth, additional

Published
2017
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158. NGTS-1b: a hot Jupiter transiting an M-dwarf

Author

Bayliss, Daniel, primary, Gillen, Edward, additional, Eigmüller, Philipp, additional, McCormac, James, additional, Alexander, Richard D, additional, Armstrong, David J, additional, Booth, Rachel S, additional, Bouchy, François, additional, Burleigh, Matthew R, additional, Cabrera, Juan, additional, Casewell, Sarah L, additional, Chaushev, Alexander, additional, Chazelas, Bruno, additional, Csizmadia, Szilard, additional, Erikson, Anders, additional, Faedi, Francesca, additional, Foxell, Emma, additional, Gänsicke, Boris T, additional, Goad, Michael R, additional, Grange, Andrew, additional, Günther, Maximilian N, additional, Hodgkin, Simon T, additional, Jackman, James, additional, Jenkins, James S, additional, Lambert, Gregory, additional, Louden, Tom, additional, Metrailler, Lionel, additional, Moyano, Maximiliano, additional, Pollacco, Don, additional, Poppenhaeger, Katja, additional, Queloz, Didier, additional, Raddi, Roberto, additional, Rauer, Heike, additional, Raynard, Liam, additional, Smith, Alexis M S, additional, Soto, Maritza, additional, Thompson, Andrew P G, additional, Titz-Weider, Ruth, additional, Udry, Stéphane, additional, Walker, Simon R, additional, Watson, Christopher A, additional, West, Richard G, additional, and Wheatley, Peter J, additional

Published
2017
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159. The Transiting Multi-planet System HD 3167: A 5.7M⊕Super-Earth and an 8.3M⊕Mini-Neptune

Author

Gandolfi, Davide, primary, Barragán, Oscar, additional, Hatzes, Artie P., additional, Fridlund, Malcolm, additional, Fossati, Luca, additional, Donati, Paolo, additional, Johnson, Marshall C., additional, Nowak, Grzegorz, additional, Prieto-Arranz, Jorge, additional, Albrecht, Simon, additional, Dai, Fei, additional, Deeg, Hans, additional, Endl, Michael, additional, Grziwa, Sascha, additional, Hjorth, Maria, additional, Korth, Judith, additional, Nespral, David, additional, Saario, Joonas, additional, Smith, Alexis M. S., additional, Antoniciello, Giuliano, additional, Alarcon, Javier, additional, Bedell, Megan, additional, Blay, Pere, additional, Brems, Stefan S., additional, Cabrera, Juan, additional, Csizmadia, Szilard, additional, Cusano, Felice, additional, Cochran, William D., additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, González Hernández, Jonay I., additional, Guenther, Eike W., additional, Hirano, Teruyuki, additional, Suárez Mascareño, Alejandro, additional, Narita, Norio, additional, Palle, Enric, additional, Parviainen, Hannu, additional, Pätzold, Martin, additional, Persson, Carina M., additional, Rauer, Heike, additional, Saviane, Ivo, additional, Schmidtobreick, Linda, additional, Van Eylen, Vincent, additional, Winn, Joshua N., additional, and Zakhozhay, Olga V., additional

Published
2017
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160. Centroid vetting of transiting planet candidates from the Next Generation Transit Survey

Author

Günther, Maximilian N., primary, Queloz, Didier, additional, Gillen, Edward, additional, McCormac, James, additional, Bayliss, Daniel, additional, Bouchy, Francois, additional, Walker, Simon. R., additional, West, Richard G., additional, Eigmüller, Philipp, additional, Smith, Alexis M. S., additional, Armstrong, David J., additional, Burleigh, Matthew, additional, Casewell, Sarah L., additional, Chaushev, Alexander P., additional, Goad, Michael R., additional, Grange, Andrew, additional, Jackman, James, additional, Jenkins, James S., additional, Louden, Tom, additional, Moyano, Maximiliano, additional, Pollacco, Don, additional, Poppenhaeger, Katja, additional, Rauer, Heike, additional, Raynard, Liam, additional, Thompson, Andrew P. G., additional, Udry, Stéphane, additional, Watson, Christopher A., additional, and Wheatley, Peter J., additional

Published
2017
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161. Shallow transit follow‐up from Next‐Generation Transit Survey: Simultaneous observations of HD 106315 with 11 identical telescopes.

Author

Smith, Alexis M. S., Eigmüller, Philipp, Gurumoorthy, Ramanathan, Csizmadia, Szilárd, Bayliss, Daniel, Burleigh, Matthew R., Cabrera, Juan, Casewell, Sarah L., Erikson, Anders, Goad, Michael R., Grange, Andrew, Jenkins, James S., Pollacco, Don, Rauer, Heike, Raynard, Liam, Udry, Stéphane, West, Richard G., and Wheatley, Peter J.

Subjects
TELESCOPES, SIGNAL-to-noise ratio, PLANETARY systems, EXTRASOLAR planets, PLANETARY orbits
Abstract

The Next Generation Transit Survey (NGTS) is a photometric survey for transiting exoplanets, consisting of 12 identical 0.2‐m telescopes. We report a measurement of the transit of HD 106315 c using a novel observing mode in which multiple NGTS telescopes observed the same target, with the aim of increasing the signal‐to‐noise ratio. Combining the data allows the robust detection of the transit, which has a depth less than 0.1%, rivaling the performance of much larger telescopes. We demonstrate the capability of NGTS to contribute to the follow‐up of K2 and Transiting Exoplanet Survey Satellite discoveries using this observing mode. In particular, NGTS is well‐suited to the measurement of shallow transits of bright targets. This is particularly important to improve orbital ephemerides of relatively long‐period planets, where only a small number of transits are observed from space. [ABSTRACT FROM AUTHOR]

Published
2020
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162. EPIC 219388192b-An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Author

Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Dai, Fei, Lanza, Antonino F., Hirano, Teruyuki, Barragan, Oscar, Fukui, Akihiko, Bruntt, Hans, Endl, Michael, Cochran, William D., Moroni, Pier G. Prada, Prieto-Arranz, Jorge, Kiilerich, Amanda, Nespral, David, Hatzes, Artie P., Albrecht, Simon, Deeg, Hans, Winn, Joshua N., Yu, Liang, Kuzuhara, Masayuki, Grziwa, Sascha, Smith, Alexis M. S., Guenther, Eike W., Van Eylen, Vincent, Csizmadia, Szilard, Fridlund, Malcolm, Cabrera, Juan, Eigmueller, Philipp, Erikson, Anders, Korth, Judith, Narita, Norio, Paetzold, Martin, Rauer, Heike, Ribas, Ignasi, Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Dai, Fei, Lanza, Antonino F., Hirano, Teruyuki, Barragan, Oscar, Fukui, Akihiko, Bruntt, Hans, Endl, Michael, Cochran, William D., Moroni, Pier G. Prada, Prieto-Arranz, Jorge, Kiilerich, Amanda, Nespral, David, Hatzes, Artie P., Albrecht, Simon, Deeg, Hans, Winn, Joshua N., Yu, Liang, Kuzuhara, Masayuki, Grziwa, Sascha, Smith, Alexis M. S., Guenther, Eike W., Van Eylen, Vincent, Csizmadia, Szilard, Fridlund, Malcolm, Cabrera, Juan, Eigmueller, Philipp, Erikson, Anders, Korth, Judith, Narita, Norio, Paetzold, Martin, Rauer, Heike, and Ribas, Ignasi

Abstract

We report the discovery of EPIC 219388192b, a transiting brown dwarf in a 5.3 day orbit around a member star of Ruprecht 147, the oldest nearby open cluster association, which was photometrically monitored by K2 during its Campaign 7. We combine the K2 time-series data with ground-based adaptive optics imaging and high-resolution spectroscopy to rule out false positive scenarios and determine the main parameters of the system. EPIC 219388192b has a radius of R-b= 0.937 +/- 0.032 R-Jup and mass of M-b= 36.84 +/- 0.97 M-Jup, yielding a mean density of 59.6 +/- 7.6 g cm(- 3). The host star is nearly a solar twin with mass M-star = 1.01 +/- 0.04 Me, radius R-star = 1.01 +/- 0.03 R-circle dot, effective temperature T-eff = 5850 +/- 85 K, and iron abundance [Fe/ H]. = 0.03 +/- 0.08 dex. Its age, spectroscopic distance, and reddening are consistent with those of Ruprecht 147, corroborating its cluster membership. EPIC 219388192b is the first mature brown dwarf with precise determinations of mass, radius, and age, and serves as benchmark for evolutionary models in the substellar regime.

Published
2017

163. K2-60b and K2-107b. A Sub-Jovian and a Jovian Planet from the K2 Mission

Author

Eigmueller, Philipp, Gandolfi, Davide, Persson, Carina M., Donati, Paolo, Fridlund, Malcolm, Csizmadia, Szilard, Barragan, Oscar, Smith, Alexis M. S., Cabrera, Juan, Korth, Judith, Grziwa, Sascha, Prieto-Arranz, Jorge, Nespral, David, Saario, Joonas, Cochran, William D., Cusano, Felice, Deeg, Hans J., Endl, Michael, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Paetzold, Martin, Rauer, Heike, Eigmueller, Philipp, Gandolfi, Davide, Persson, Carina M., Donati, Paolo, Fridlund, Malcolm, Csizmadia, Szilard, Barragan, Oscar, Smith, Alexis M. S., Cabrera, Juan, Korth, Judith, Grziwa, Sascha, Prieto-Arranz, Jorge, Nespral, David, Saario, Joonas, Cochran, William D., Cusano, Felice, Deeg, Hans J., Endl, Michael, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Paetzold, Martin, and Rauer, Heike

Abstract

We report the characterization and independent detection of K2-60b, as well as the detection and characterization of K2-107b, two transiting hot gaseous planets from the K2 space mission. We confirm the planetary nature of the two systems and determine their fundamental parameters combining the K2 time-series data with FIES @ NOT and HARPS-N @ TNG spectroscopic observations. K2-60b has a radius of 0.683 +/- 0.037 R-Jup and a mass of 0.426 +/- 0.037 M-Jup and orbits a G4 V star with an orbital period of 3.00267 +/- 0.00006 days. K2-107b has a radius of 1.44 +/- 0.15 R-Jup and a mass of 0.84 +/- 0.08 M-Jup and orbits an F9 IV star every 3.31392 +/- 0.00002 days. K2-60b is among the few planets at the edge of the so-called desert of short-period sub-Jovian planets. K2107b is a highly inflated Jovian planet orbiting an evolved star about to leave the main sequence.

Published
2017

164. The Transiting Multi-planet System HD3167: A 5.7M(circle plus) Super-Earth and an 8.3M(circle plus) Mini-Neptune

Author

Gandolfi, Davide, Barragan, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Dai, Fei, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmller, Philipp, Erikson, Anders, Gonzalez Hernandez, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suarez Mascareno, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Paetzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., Zakhozhay, Olga V., Gandolfi, Davide, Barragan, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Dai, Fei, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmller, Philipp, Erikson, Anders, Gonzalez Hernandez, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suarez Mascareno, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Paetzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., and Zakhozhay, Olga V.

Abstract

HD3167 is a bright (V = 8.9 mag) K0V star observed by the NASA's K2 space mission during its Campaign 8. It has been recently found to host two small transiting planets, namely, HD 3167b, an ultra short period (0.96 days) super-Earth, and HD 3167c, a mini-Neptune on a relatively long-period orbit (29.85 d). Here we present an intensive radial velocity follow-up of HD 3167 performed with the FIES@NOT, HARPS@ESO-3.6m, and HARPS-N@TNG spectrographs. We revise the system parameters and determine radii, masses, and densities of the two transiting planets by combining the K2 photometry with our spectroscopic data. With a mass of 5.69 +/- -0.44 M-circle plus, radius of 1.574 +/- -0.054 R-circle plus, and mean density of 8.00(-0.98)(+1.0) g/cm(-3), HD 3167b joins the small group of ultra-short period planets known to have a rocky terrestrial composition. HD 3167c has a mass of 8.33(-1.85)(+1.79) M-circle plus and a radius of 2.740(-0.100)(+0.106) R-circle plus, yielding a mean density of 2.21(-0.53)(+0.56) g/cm(-3), indicative of a planet with a composition comprising a solid core surrounded by a thick atmospheric envelope. The rather large pressure scale height (similar to 350 km) and the brightness of the host star make HD 3167c an ideal target for atmospheric characterization via transmission spectroscopy across a broad range of wavelengths. We found evidence of additional signals in the radial velocity measurements but the currently available data set does not allow us to draw any firm conclusion on the origin of the observed variation.

Published
2017

165. The Discovery and Mass Measurement of a New Ultra-short-period Planet: EPIC 228732031b

Author

Dai, Fei, Winn, Joshua N., Gandolfi, Davide, Wang, Sharon X., Teske, Johanna K., Burt, Jennifer, Albrecht, Simon, Barragan, Oscar, Cochran, William D., Endl, Michael, Fridlund, Malcolm, Hatzes, Artie P., Hirano, Teruyuki, Hirsch, Lea A., Johnson, Marshall C., Justesen, Anders Bo, Livingston, John, Persson, Carina M., Prieto-Arranz, Jorge, Vanderburg, Andrew, Alonso, Roi, Antoniciello, Giuliano, Arriagada, Pamela, Butler, R. P., Cabrera, Juan, Crane, Jeffrey D., Cusano, Felice, Csizmadia, Szilard, Deeg, Hans, Dieterich, Sergio B., Eigmueller, Philipp, Erikson, Anders, Everett, Mark E., Fukui, Akihiko, Grziwa, Sascha, Guenther, Eike W., Henry, Gregory W., Howell, Steve B., Johnson, John Asher, Korth, Judith, Kuzuhara, Masayuki, Narita, Norio, Nespral, David, Nowak, Grzegorz, Palle, Enric, Paetzold, Martin, Rauer, Heike, Montanes Rodriguez, Pilar, Shectman, Stephen A., Smith, Alexis M. S., Thompson, Ian B., Van Eylen, Vincent, Williamson, Michael W., Wittenmyer, Robert A., Dai, Fei, Winn, Joshua N., Gandolfi, Davide, Wang, Sharon X., Teske, Johanna K., Burt, Jennifer, Albrecht, Simon, Barragan, Oscar, Cochran, William D., Endl, Michael, Fridlund, Malcolm, Hatzes, Artie P., Hirano, Teruyuki, Hirsch, Lea A., Johnson, Marshall C., Justesen, Anders Bo, Livingston, John, Persson, Carina M., Prieto-Arranz, Jorge, Vanderburg, Andrew, Alonso, Roi, Antoniciello, Giuliano, Arriagada, Pamela, Butler, R. P., Cabrera, Juan, Crane, Jeffrey D., Cusano, Felice, Csizmadia, Szilard, Deeg, Hans, Dieterich, Sergio B., Eigmueller, Philipp, Erikson, Anders, Everett, Mark E., Fukui, Akihiko, Grziwa, Sascha, Guenther, Eike W., Henry, Gregory W., Howell, Steve B., Johnson, John Asher, Korth, Judith, Kuzuhara, Masayuki, Narita, Norio, Nespral, David, Nowak, Grzegorz, Palle, Enric, Paetzold, Martin, Rauer, Heike, Montanes Rodriguez, Pilar, Shectman, Stephen A., Smith, Alexis M. S., Thompson, Ian B., Van Eylen, Vincent, Williamson, Michael W., and Wittenmyer, Robert A.

Abstract

We report the discovery of a new ultra-short-period planet and summarize the properties of all such planets for which the mass and radius have been measured. The new planet, EPIC. 228732031b, was discovered in K2 Campaign 10. It has a radius of 1.81(-0.12)(+0.16) R-circle plus and orbits a G dwarf with a period of 8.9 hr. Radial velocities obtained with Magellan/PFS and TNG/HARPS-N show evidence for stellar activity along with orbital motion. We determined the planetary mass using two different methods: (1) the floating chunk offset method, based only on changes in velocity observed on the same night; and (2) a Gaussian process regression based on both the radial velocity and photometric time series. The results are consistent and lead to a mass measurement of 6.5. +/- 1.6 M-circle plus and a mean density of 6.0(-2.7)(+3.0) g cm(-3).

Published
2017

166. Three Super-Earths Transiting the Nearby Star GJ 9827

Author

Niraula, Prajwal, Redfield, Seth, Dai, Fei, Barragan, Oscar, Gandolfi, Davide, Cauley, P. Wilson, Hirano, Teruyuki, Korth, Judith, Smith, Alexis M. S., Prieto-Arranz, Jorge, Grziwa, Sascha, Fridlund, Malcolm, Persson, Carina M., Justesen, Anders Bo, Winn, Joshua N., Albrecht, Simon, Cochran, William D., Csizmadia, Szilard, Duvvuri, Girish M., Endl, Michael, Hatzes, Artie P., Livingston, John H., Narita, Norio, Nespral, David, Nowak, Grzegorz, Paetzold, Martin, Palle, Enric, Van Eylen, Vincent, Niraula, Prajwal, Redfield, Seth, Dai, Fei, Barragan, Oscar, Gandolfi, Davide, Cauley, P. Wilson, Hirano, Teruyuki, Korth, Judith, Smith, Alexis M. S., Prieto-Arranz, Jorge, Grziwa, Sascha, Fridlund, Malcolm, Persson, Carina M., Justesen, Anders Bo, Winn, Joshua N., Albrecht, Simon, Cochran, William D., Csizmadia, Szilard, Duvvuri, Girish M., Endl, Michael, Hatzes, Artie P., Livingston, John H., Narita, Norio, Nespral, David, Nowak, Grzegorz, Paetzold, Martin, Palle, Enric, and Van Eylen, Vincent

Abstract

We report on the discovery of three transiting planets around GJ. 9827. The planets have radii of 1.75 +/- 0.18, 1.36 +/- 0.14, and 2.11 (+0.22)(-0.21) R-circle plus, and periods of 1.20896, 3.6480, and 6.2014 days, respectively. The detection was made in Campaign 12 observations as part of our K2 survey of nearby stars. GJ 9827 is a V = 10.39 mag K6V star at a distance of 30.3 +/- 1.6 parsecs and the nearest star to be found hosting planets by Kepler and K2. The radial velocity follow- up, high- resolution imaging, and detection of multiple transiting objects near commensurability drastically reduce the false positive probability. The orbital periods of GJ 9827 b, c, and d planets are very close to the 1:3:5 mean motion resonance. Our preliminary analysis shows that GJ 9827 planets are excellent candidates for atmospheric observations. Besides, the planetary radii span both sides of the rocky and gaseous divide, hence the system will be an asset in expanding our understanding of the threshold.

Published
2017

167. EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Dai, Fei, Yu, Liang, Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Lanza, Antonino F., Hirano, Teruyuki, Barragán, Oscar, Fukui, Akihiko, Bruntt, Hans, Endl, Michael, Cochran, William D., Moroni, Pier G. Prada, Prieto-Arranz, Jorge, Kiilerich, Amanda, Nespral, David, Hatzes, Artie P., Albrecht, Simon, Deeg, Hans, Winn, Joshua N., Kuzuhara, Masayuki, Grziwa, Sascha, Smith, Alexis M. S., Guenther, Eike W., Van Eylen, Vincent, Csizmadia, Szilard, Fridlund, Malcolm, Cabrera, Juan, Eigmüller, Philipp, Erikson, Anders, Korth, Judith, Narita, Norio, Pätzold, Martin, Rauer, Heike, Ribas, Ignasi, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Dai, Fei, Yu, Liang, Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Lanza, Antonino F., Hirano, Teruyuki, Barragán, Oscar, Fukui, Akihiko, Bruntt, Hans, Endl, Michael, Cochran, William D., Moroni, Pier G. Prada, Prieto-Arranz, Jorge, Kiilerich, Amanda, Nespral, David, Hatzes, Artie P., Albrecht, Simon, Deeg, Hans, Winn, Joshua N., Kuzuhara, Masayuki, Grziwa, Sascha, Smith, Alexis M. S., Guenther, Eike W., Van Eylen, Vincent, Csizmadia, Szilard, Fridlund, Malcolm, Cabrera, Juan, Eigmüller, Philipp, Erikson, Anders, Korth, Judith, Narita, Norio, Pätzold, Martin, Rauer, Heike, and Ribas, Ignasi

Published
2017

168. The Transiting Multi-Planet System HD 3167: A 5.7 M ⊕ Super-Earth and an 8.3 M ⊕ Mini-Neptune

Author

Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Dai, Fei, Gandolfi, Davide, Barragán, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmüller, Philipp, Erikson, Anders, González Hernández, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suárez Mascareño, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Pätzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., Zakhozhay, Olga V., Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Dai, Fei, Gandolfi, Davide, Barragán, Oscar, Hatzes, Artie P., Fridlund, Malcolm, Fossati, Luca, Donati, Paolo, Johnson, Marshall C., Nowak, Grzegorz, Prieto-Arranz, Jorge, Albrecht, Simon, Deeg, Hans, Endl, Michael, Grziwa, Sascha, Hjorth, Maria, Korth, Judith, Nespral, David, Saario, Joonas, Smith, Alexis M. S., Antoniciello, Giuliano, Alarcon, Javier, Bedell, Megan, Blay, Pere, Brems, Stefan S., Cabrera, Juan, Csizmadia, Szilard, Cusano, Felice, Cochran, William D., Eigmüller, Philipp, Erikson, Anders, González Hernández, Jonay I., Guenther, Eike W., Hirano, Teruyuki, Suárez Mascareño, Alejandro, Narita, Norio, Palle, Enric, Parviainen, Hannu, Pätzold, Martin, Persson, Carina M., Rauer, Heike, Saviane, Ivo, Schmidtobreick, Linda, Van Eylen, Vincent, Winn, Joshua N., and Zakhozhay, Olga V.

Published
2017

170. EPIC 219388192b—An Inhabitant of the Brown Dwarf Desert in the Ruprecht 147 Open Cluster

Author

Nowak, Grzegorz, primary, Palle, Enric, additional, Gandolfi, Davide, additional, Dai, Fei, additional, Lanza, Antonino F., additional, Hirano, Teruyuki, additional, Barragán, Oscar, additional, Fukui, Akihiko, additional, Bruntt, Hans, additional, Endl, Michael, additional, Cochran, William D., additional, Moroni, Pier G. Prada, additional, Prieto-Arranz, Jorge, additional, Kiilerich, Amanda, additional, Nespral, David, additional, Hatzes, Artie P., additional, Albrecht, Simon, additional, Deeg, Hans, additional, Winn, Joshua N., additional, Yu, Liang, additional, Kuzuhara, Masayuki, additional, Grziwa, Sascha, additional, Smith, Alexis M. S., additional, Guenther, Eike W., additional, Eylen, Vincent Van, additional, Csizmadia, Szilard, additional, Fridlund, Malcolm, additional, Cabrera, Juan, additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, Korth, Judith, additional, Narita, Norio, additional, Pätzold, Martin, additional, Rauer, Heike, additional, and Ribas, Ignasi, additional

Published
2017
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171. K2-60b and K2-107b. A Sub-Jovian and a Jovian Planet from the K2 Mission

Author

Eigmüller, Philipp, primary, Gandolfi, Davide, additional, Persson, Carina M., additional, Donati, Paolo, additional, Fridlund, Malcolm, additional, Csizmadia, Szilard, additional, Barragán, Oscar, additional, Smith, Alexis M. S., additional, Cabrera, Juan, additional, Korth, Judith, additional, Grziwa, Sascha, additional, Prieto-Arranz, Jorge, additional, Nespral, David, additional, Saario, Joonas, additional, Cochran, William D., additional, Cusano, Felice, additional, Deeg, Hans J., additional, Endl, Michael, additional, Erikson, Anders, additional, Guenther, Eike W., additional, Hatzes, Artie P., additional, Pätzold, Martin, additional, and Rauer, Heike, additional

Published
2017
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172. K2-60b and epic 216468514b. A sub-jovian and a jovian planet from the k2 mission

Author

Eigmüller, Philipp, Gandolfi, Davide, Persson, Carina M., Donati, Paolo, Fridlund, Malcolm, Csizmadia, Szilard, Barragán, Oscar, Smith, Alexis M. S., Cabrera, Juan, Korth, Judith, Grziwa, Sascha, Prieto-Arranz, Jorge, Nespral, David, Saario, Joonas, Cochran, William D., Cusano, Felice, Deeg, Hans J., Endl, Michael, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Pätzold, Martin, Rauer, Heike, Eigmüller, Philipp, Gandolfi, Davide, Persson, Carina M., Donati, Paolo, Fridlund, Malcolm, Csizmadia, Szilard, Barragán, Oscar, Smith, Alexis M. S., Cabrera, Juan, Korth, Judith, Grziwa, Sascha, Prieto-Arranz, Jorge, Nespral, David, Saario, Joonas, Cochran, William D., Cusano, Felice, Deeg, Hans J., Endl, Michael, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Pätzold, Martin, and Rauer, Heike

Abstract

We report the characterization and independant detection of K2-60b, as well as the detection and characterization of EPIC 216468514b, two transiting hot gaseous planets from the K2 space mission. We confirm the planetary nature of the two systems and determine their fundamental parameters combining the K2 time-series data with FIES@NOT and HARPS-N@TNG spectroscopic observations. K2-60b has a radius of 0.683 +/- 0.037 RJup and a mass of 0.426 +/- 0.037 MJup and orbits a G4V star with an orbital period of 3.00267 +/- 0.00006 days. EPIC 216468514b has a radius of 1.44 +/- 0.15RJup and a mass of 0.84 +/- 0.08 MJup and orbits an F9 IV star every 3.31392 +/- 0.00002 days. K2-60b is among the few planets at the edge of the so-called "desert" of short-period sub Jovian planets. EPIC 216468514b is a highly inflated Jovian planet orbiting an evolved star about to leave the main sequence., Comment: 10 pages, 10 figures

Published
2016
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173. EPIC 219388192 b - an inhabitant of the brown dwarf desert in the Ruprecht 147 open cluster

Author

Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Dai, Fei, Lanza, Antonino F., Hirano, Teruyuki, Barragán, Oscar, Fukui, Akihiko, Bruntt, Hans, Endl, Michael, Cochran, William D., Prieto-Arranz, Jorge, Kiilerich, Amanda, Nespral, David, Hatzes, Artie P., Albrecht, Simon, Deeg, Hans, Winn, Joshua N., Yu, Liang, Kuzuhara, Masayuki, Grziwa, Sascha, Smith, Alexis M. S., Moroni, Pier G. Prada, Guenther, Eike W., Van Eylen, Vincent, Csizmadia, Szilard, Fridlund, Malcolm, Cabrera, Juan, Eigmüller, Philipp, Erikson, Anders, Korth, Judith, Narita, Norio, Pätzold, Martin, Rauer, Heike, Ribas, Ignasi, Nowak, Grzegorz, Palle, Enric, Gandolfi, Davide, Dai, Fei, Lanza, Antonino F., Hirano, Teruyuki, Barragán, Oscar, Fukui, Akihiko, Bruntt, Hans, Endl, Michael, Cochran, William D., Prieto-Arranz, Jorge, Kiilerich, Amanda, Nespral, David, Hatzes, Artie P., Albrecht, Simon, Deeg, Hans, Winn, Joshua N., Yu, Liang, Kuzuhara, Masayuki, Grziwa, Sascha, Smith, Alexis M. S., Moroni, Pier G. Prada, Guenther, Eike W., Van Eylen, Vincent, Csizmadia, Szilard, Fridlund, Malcolm, Cabrera, Juan, Eigmüller, Philipp, Erikson, Anders, Korth, Judith, Narita, Norio, Pätzold, Martin, Rauer, Heike, and Ribas, Ignasi

Abstract

We report the discovery of EPIC 219388192 b, a transiting brown dwarf in a 5.3-day orbit around a member star of Ruprecht-147, the oldest nearby open cluster association, which was photometrically monitored by K2 during its Campaign 7. We combine the K2 time-series data with ground-based adaptive optics imaging and high resolution spectroscopy to rule out false positive scenarios and determine the main parameters of the system. EPIC 219388192 b has a radius of $R_\mathrm{b}$=$0.937\pm0.042$~$\mathrm{R_{Jup}}$ and mass of $M_\mathrm{b}$=$36.50\pm0.09$~$\mathrm{M_{Jup}}$, yielding a mean density of $59.0\pm8.1$~$\mathrm{g\,cm^{-3}}$. The host star is nearly a Solar twin with mass $M_\star$=$0.99\pm0.05$~$\mathrm{M_{\odot}}$, radius $R_\star$=$1.01\pm0.04$~$\mathrm{R_{\odot}}$, effective temperature $\mathrm{T_{eff}}$=$5850\pm85$~K and iron abundance [Fe/H]=$0.03\pm0.08$~dex. Its age, spectroscopic distance, and reddening are consistent with those of Ruprecht-147, corroborating its cluster membership. EPIC 219388192 b is the first brown dwarf with precise determinations of mass, radius and age, and serves as benchmark for evolutionary models in the sub-stellar regime., Comment: 13 pages, 11 figures, 4 tables, submitted to AAS Journals

Published
2016
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174. K2-98b: A 32 M-circle plus NEPTUNE-SIZE PLANET IN A 10 DAY ORBIT TRANSITING AN F8 STAR

Author

Barragan, Oscar, Grziwa, Sascha, Gandolfi, Davide, Fridlund, Malcolm, Endl, Michael, Deeg, Hans J., Cagigal, Manuel P., Lanza, Antonino F., Moroni, Pier G. Prada, Smith, Alexis M. S., Korth, Judith, Bedell, Megan, Cabrera, Juan, Cochran, William D., Cusano, Felice, Csizmadia, Szilard, Eigmueller, Philipp, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Nespral, David, Paetzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Barragan, Oscar, Grziwa, Sascha, Gandolfi, Davide, Fridlund, Malcolm, Endl, Michael, Deeg, Hans J., Cagigal, Manuel P., Lanza, Antonino F., Moroni, Pier G. Prada, Smith, Alexis M. S., Korth, Judith, Bedell, Megan, Cabrera, Juan, Cochran, William D., Cusano, Felice, Csizmadia, Szilard, Eigmueller, Philipp, Erikson, Anders, Guenther, Eike W., Hatzes, Artie P., Nespral, David, Paetzold, Martin, Prieto-Arranz, Jorge, and Rauer, Heike

Abstract

We report the discovery of K2-98b (EPIC 211391664b), a transiting Neptune-size planet monitored by the K2 mission during its Campaign 5. We combine the K2 time-series data with ground-based photometric and spectroscopic follow-up observations to confirm the planetary nature of the object and derive its mass, radius, and orbital parameters. K2-98b is a warm Neptune-like planet in a 10 day orbit around a V = 12.2 mag F-type star with M-star = 1.074 +/- 0.042 M-circle dot, R-star = 1.311(-0.048)(+0.083) R-circle dot, and age of 5.2(-1.0)(+1.2) Gyr We derive a planetary mass and radius of M-p = 32.2 +/- 8.1 M-circle plus and R-p = 4.3(-0.2)(+0.3) R-circle plus.K2-98b joins the relatively small group of Neptune-size planets whose mass and radius have been derived with a precision better than 25%. We estimate that the planet will be engulfed by its host star in similar to 3 Gyr, due to the evolution of the latter toward the red giant branch.

Published
2016

175. K2-98b: A 32M⊕NEPTUNE-SIZE PLANET IN A 10 DAY ORBIT TRANSITING AN F8 STAR

Author

Barragán, Oscar, primary, Grziwa, Sascha, additional, Gandolfi, Davide, additional, Fridlund, Malcolm, additional, Endl, Michael, additional, Deeg, Hans J., additional, Cagigal, Manuel P., additional, Lanza, Antonino F., additional, Moroni, Pier G. Prada, additional, Smith, Alexis M. S., additional, Korth, Judith, additional, Bedell, Megan, additional, Cabrera, Juan, additional, Cochran, William D., additional, Cusano, Felice, additional, Csizmadia, Szilard, additional, Eigmüller, Philipp, additional, Erikson, Anders, additional, Guenther, Eike W., additional, Hatzes, Artie P., additional, Nespral, David, additional, Pätzold, Martin, additional, Prieto-Arranz, Jorge, additional, and Rauer, Heike, additional

Published
2016
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176. WASP-80b has a dayside within the T-dwarf range

Author

Triaud, Amaury H. M. J., Gillon, Michael, Ehrenreich, David, Herrero, Enrique, Lendl, Monika, Anderson, David R., Cameron, Andrew Collier, Delrez, Laetitia, Demory, Brice-Olivier, Hellier, Coel, Heng, Keving, Jehin, Emmanuel, Maxted, Pierre F. L., Pollacco, Don, Queloz, Didier, Ribas, Ignasi, Smalley, Barry, Smith, Alexis M. S., Udry, Stephane, Triaud, Amaury H. M. J., Gillon, Michael, Ehrenreich, David, Herrero, Enrique, Lendl, Monika, Anderson, David R., Cameron, Andrew Collier, Delrez, Laetitia, Demory, Brice-Olivier, Hellier, Coel, Heng, Keving, Jehin, Emmanuel, Maxted, Pierre F. L., Pollacco, Don, Queloz, Didier, Ribas, Ignasi, Smalley, Barry, Smith, Alexis M. S., and Udry, Stephane

Abstract

WASP-80b is a missing link in the study of exo-atmospheres. It falls between the warm Neptunes and the hot Jupiters and is amenable for characterisation, thanks to its host star's properties. We observed the planet through transit and during occultation with Warm Spitzer. Combining our mid-infrared transits with optical time series, we find that the planet presents a transmission spectrum indistinguishable from a horizontal line. In emission, WASP-80b is the intrinsically faintest planet whose dayside flux has been detected in both the 3.6 and 4.5 $\mu$m Spitzer channels. The depths of the occultations reveal that WASP-80b is as bright and as red as a T4 dwarf, but that its temperature is cooler. If planets go through the equivalent of an L-T transition, our results would imply this happens at cooler temperatures than for brown dwarfs. Placing WASP-80b's dayside into a colour-magnitude diagram, it falls exactly at the junction between a blackbody model and the T-dwarf sequence; we cannot discern which of those two interpretations is the more likely. Flux measurements on other planets with similar equilibrium temperatures are required to establish whether irradiated gas giants, like brown dwarfs, transition between two spectral classes. An eventual detection of methane absorption in transmission would also help lift that degeneracy. We obtained a second series of high-resolution spectra during transit, using HARPS. We reanalyse the Rossiter-McLaughlin effect. The data now favour an aligned orbital solution and a stellar rotation nearly three times slower than stellar line broadening implies. A contribution to stellar line broadening, maybe macroturbulence, is likely to have been underestimated for cool stars, whose rotations have therefore been systematically overestimated. [abridged], Comment: 15 pages, 5 figures, 2 tables (and appendices), accepted for publication in MNRAS

Published
2015
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177. SPITZEROBSERVATIONS OF THE THERMAL EMISSION FROM WASP-43b

Author

Blecic, Jasmina, primary, Harrington, Joseph, additional, Madhusudhan, Nikku, additional, Stevenson, Kevin B., additional, Hardy, Ryan A., additional, Cubillos, Patricio E., additional, Hardin, Matthew, additional, Bowman, Oliver, additional, Nymeyer, Sarah, additional, Anderson, David R., additional, Hellier, Coel, additional, Smith, Alexis M. S., additional, and Cameron, Andrew Collier, additional

Published
2014
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180. SPITZER OBSERVATIONS OF THE THERMAL EMISSION FROM WASP-43b.

Author

Blecic, Jasmina, Harrington, Joseph, Madhusudhan, Nikku, Stevenson, Kevin B., Hardy, Ryan A., Cubillos, Patricio E., Hardin, Matthew, Bowman, Oliver, Nymeyer, Sarah, Anderson, David R., Hellier, Coel, Smith, Alexis M. S., and Cameron, Andrew Collier

Subjects
HEAT radiation & absorption, TEMPERATURE of stars, HOT Jupiters, ASTRONOMICAL photometry, BRIGHTNESS temperature measurement
Abstract

WASP-43b is one of the closest-orbiting hot Jupiters, with a semimajor axis of a = 0.01526 ± 0.00018 AU and a period of only 0.81 days. However, it orbits one of the coolest stars with a hot Jupiter (T* = 4520 ± 120 K), giving the planet a modest equilibrium temperature of Teq = 1440 ± 40 K, assuming zero Bond albedo and uniform planetary energy redistribution. The eclipse depths and brightness temperatures from our jointly fit model are 0.347% ± 0.013% and 1670 ± 23 K at 3.6 μm and 0.382% ± 0.015% and 1514 ± 25 K at 4.5 μm. The eclipse timings improved the estimate of the orbital period, P, by a factor of three (P = 0.81347436 ± 1.4 × 10–7 days) and put an upper limit on the eccentricity (). We use our Spitzer eclipse depths along with four previously reported ground-based photometric observations in the near-infrared to constrain the atmospheric properties of WASP-43b. The data rule out a strong thermal inversion in the dayside atmosphere of WASP-43b. Model atmospheres with no thermal inversions and fiducial oxygen-rich compositions are able to explain all the available data. However, a wide range of metallicities and C/O ratios can explain the data. The data suggest low day-night energy redistribution in the planet, consistent with previous studies, with a nominal upper limit of about 35% for the fraction of energy incident on the dayside that is redistributed to the nightside. [ABSTRACT FROM AUTHOR]

Published
2014
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181. NGTS-33b: a young super-Jupiter hosted by a fast-rotating massive hot star.

Author

Alves, Douglas R, Jenkins, James S, Vines, Jose I, Battley, Matthew P, Lendl, Monika, Bouchy, François, Nielsen, Louise D, Gill, Samuel, Moyano, Maximiliano, Anderson, D R, Burleigh, Matthew R, Casewell, Sarah L, Goad, Michael R, Hawthorn, Faith, Kendall, Alicia, McCormac, James, Osborn, Ares, Smith, Alexis M S, Udry, Stéphane, and Wheatley, Peter J

Subjects
*NATURAL satellites, *SUPERGIANT stars, *HOT Jupiters, *EMISSION spectroscopy, *PLANETARY systems
Abstract

In the last few decades, planet search surveys have been focusing on solar-type stars, and only recently the high-mass regimes. This is mostly due to challenges arising from the lack of instrumental precision, and more importantly, the inherent active nature of fast-rotating massive stars. Here, we report NGTS-33b (TOI-6442b), a super-Jupiter planet with mass, radius, and orbital period of 3.6 |$\pm$| 0.3 M |$_{\rm J}$|⁠ , 1.64 |$\pm$| 0.07 R |$_{\rm J}$|⁠ , and |$2.827\,972 \pm 0.000\,001$|  d, respectively. The host is a fast-rotating (⁠|$0.6654 \pm 0.0006$|  d) and hot (T |$_{\rm eff}$| = 7437 |$\pm$| 72 K) A9V type star, with a mass and radius of 1.60 |$\pm$| 0.11 M |$_{\odot }$| and 1.47 |$\pm$| 0.06 R |$_{\odot }$|⁠ , respectively. Planet structure and gyrochronology models show that NGTS-33 is also very young with age limits of 10–50 Myr. In addition, membership analysis points towards the star being part of the Vela OB2 association, which has an age of |$\sim$| 20–35 Myr, thus providing further evidence about the young nature of NGTS-33. Its low bulk density of 0.19 |$\pm$| 0.03 g cm |$^{-3}$| is 13 per cent smaller than expected when compared to transiting hot Jupiters (HJs) with similar masses. Such cannot be solely explained by its age, where an up to 15 per cent inflated atmosphere is expected from planet structure models. Finally, we found that its emission spectroscopy metric is similar to JWST community targets, making the planet an interesting target for atmospheric follow-up. Therefore, NGTS-33b's discovery will not only add to the scarce population of young, massive and HJs, but will also help place further strong constraints on current formation and evolution models for such planetary systems. [ABSTRACT FROM AUTHOR]

Published
2025
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182. WASP-80b has a dayside within the T-dwarf range

Author

Triaud, Amaury H. M. J., Gillon, Michaël, Ehrenreich, David, Herrero, Enrique, Lendl, Monika, Anderson, David R., Collier Cameron, Andrew, Delrez, Laetitia, Demory, Brice-Olivier, Hellier, Coel, Heng, Kevin, Jehin, Emmanuel, Maxted, Pierre F. L., Pollacco, Don, Queloz, Didier, Ribas, Ignasi, Smalley, Barry, Smith, Alexis M. S., Udry, Stéphane, Triaud, Amaury H. M. J., Gillon, Michaël, Ehrenreich, David, Herrero, Enrique, Lendl, Monika, Anderson, David R., Collier Cameron, Andrew, Delrez, Laetitia, Demory, Brice-Olivier, Hellier, Coel, Heng, Kevin, Jehin, Emmanuel, Maxted, Pierre F. L., Pollacco, Don, Queloz, Didier, Ribas, Ignasi, Smalley, Barry, Smith, Alexis M. S., and Udry, Stéphane

183. The Transiting Multi-planet System HD15337: Two Nearly Equal-mass Planets Straddling the Radius Gap

Author

Gandolfi, Davide, Fossati, Luca, Livingston, John H, Stassun, Keivan G, Grziwa, Sascha, Barragan, Oscar, Fridlund, Malcolm, Kubyshkina, Daria, Persson, Carina M, Dai, Fei, Lam, Kristine W F, Albrecht, Simon, Batalha, Natalie, Beck, Paul G, Bo Justesen, Anders, Cabrera, Juan, Cartwright, Scott, Cochran, William D, Csizmadia, Szilard, Davies, Misty D, Deeg, Hans J, Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Esposito, Massimiliano, Garcia, Rafael A, Goeke, Robert, González-Cuesta, Lucía, Guenther, Elke W, Hatzes, Artie P, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Kabath, Petr, Knudstrup, Emil, Korth, Judith, Li, Jie, Luque, Rafael, Mathur, Savita, Montañes Rodríguez, Pilar, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Palle, Enric, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M S, Rowden, Pamela, Torres, Guillermo, Van Eylen, Vincent, Vezie, Michael L, Gandolfi, Davide, Fossati, Luca, Livingston, John H, Stassun, Keivan G, Grziwa, Sascha, Barragan, Oscar, Fridlund, Malcolm, Kubyshkina, Daria, Persson, Carina M, Dai, Fei, Lam, Kristine W F, Albrecht, Simon, Batalha, Natalie, Beck, Paul G, Bo Justesen, Anders, Cabrera, Juan, Cartwright, Scott, Cochran, William D, Csizmadia, Szilard, Davies, Misty D, Deeg, Hans J, Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Esposito, Massimiliano, Garcia, Rafael A, Goeke, Robert, González-Cuesta, Lucía, Guenther, Elke W, Hatzes, Artie P, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Kabath, Petr, Knudstrup, Emil, Korth, Judith, Li, Jie, Luque, Rafael, Mathur, Savita, Montañes Rodríguez, Pilar, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Palle, Enric, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M S, Rowden, Pamela, Torres, Guillermo, Van Eylen, Vincent, and Vezie, Michael L

Abstract

We report the discovery of a super-Earth and a sub-Neptune transiting the star HD 15337 (TOI-402, TIC 120896927), a bright (V = 9) K1 dwarf observed by the Transiting Exoplanet Survey Satellite (TESS) in Sectors 3 and 4. We combine the TESS photometry with archival High Accuracy Radial velocity Planet Searcher spectra to confirm the planetary nature of the transit signals and derive the masses of the two transiting planets. With an orbital period of 4.8 days, a mass of ${7.51}_{-1.01}^{+1.09}\,{M}_{\oplus }$ and a radius of 1.64 ± 0.06 R ⊕, HD 15337 b joins the growing group of short-period super-Earths known to have a rocky terrestrial composition. The sub-Neptune HD 15337 c has an orbital period of 17.2 days, a mass of ${8.11}_{-1.69}^{+1.82}\,{{\rm{M}}}_{\oplus }$, and a radius of 2.39 ± 0.12 R ⊕, suggesting that the planet might be surrounded by a thick atmospheric envelope. The two planets have similar masses and lie on opposite sides of the radius gap, and are thus an excellent testbed for planet formation and evolution theories. Assuming that HD 15337 c hosts a hydrogen-dominated envelope, we employ a recently developed planet atmospheric evolution algorithm in a Bayesian framework to estimate the history of the high-energy (extreme ultraviolet and X-ray) emission of the host star. We find that at an age of 150 Myr, the star possessed on average between 3.7 and 127 times the high-energy luminosity of the current Sun.

184. The Transiting Multi-planet System HD15337: Two Nearly Equal-mass Planets Straddling the Radius Gap

Author

Gandolfi, Davide, Fossati, Luca, Livingston, John H, Stassun, Keivan G, Grziwa, Sascha, Barragan, Oscar, Fridlund, Malcolm, Kubyshkina, Daria, Persson, Carina M, Dai, Fei, Lam, Kristine W F, Albrecht, Simon, Batalha, Natalie, Beck, Paul G, Bo Justesen, Anders, Cabrera, Juan, Cartwright, Scott, Cochran, William D, Csizmadia, Szilard, Davies, Misty D, Deeg, Hans J, Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Esposito, Massimiliano, Garcia, Rafael A, Goeke, Robert, González-Cuesta, Lucía, Guenther, Elke W, Hatzes, Artie P, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Kabath, Petr, Knudstrup, Emil, Korth, Judith, Li, Jie, Luque, Rafael, Mathur, Savita, Montañes Rodríguez, Pilar, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Palle, Enric, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M S, Rowden, Pamela, Torres, Guillermo, Van Eylen, Vincent, Vezie, Michael L, Gandolfi, Davide, Fossati, Luca, Livingston, John H, Stassun, Keivan G, Grziwa, Sascha, Barragan, Oscar, Fridlund, Malcolm, Kubyshkina, Daria, Persson, Carina M, Dai, Fei, Lam, Kristine W F, Albrecht, Simon, Batalha, Natalie, Beck, Paul G, Bo Justesen, Anders, Cabrera, Juan, Cartwright, Scott, Cochran, William D, Csizmadia, Szilard, Davies, Misty D, Deeg, Hans J, Eigmüller, Philipp, Endl, Michael, Erikson, Anders, Esposito, Massimiliano, Garcia, Rafael A, Goeke, Robert, González-Cuesta, Lucía, Guenther, Elke W, Hatzes, Artie P, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Kabath, Petr, Knudstrup, Emil, Korth, Judith, Li, Jie, Luque, Rafael, Mathur, Savita, Montañes Rodríguez, Pilar, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Palle, Enric, Pätzold, Martin, Prieto-Arranz, Jorge, Rauer, Heike, Redfield, Seth, Ribas, Ignasi, Skarka, Marek, Smith, Alexis M S, Rowden, Pamela, Torres, Guillermo, Van Eylen, Vincent, and Vezie, Michael L

Abstract

We report the discovery of a super-Earth and a sub-Neptune transiting the star HD 15337 (TOI-402, TIC 120896927), a bright (V = 9) K1 dwarf observed by the Transiting Exoplanet Survey Satellite (TESS) in Sectors 3 and 4. We combine the TESS photometry with archival High Accuracy Radial velocity Planet Searcher spectra to confirm the planetary nature of the transit signals and derive the masses of the two transiting planets. With an orbital period of 4.8 days, a mass of ${7.51}_{-1.01}^{+1.09}\,{M}_{\oplus }$ and a radius of 1.64 ± 0.06 R ⊕, HD 15337 b joins the growing group of short-period super-Earths known to have a rocky terrestrial composition. The sub-Neptune HD 15337 c has an orbital period of 17.2 days, a mass of ${8.11}_{-1.69}^{+1.82}\,{{\rm{M}}}_{\oplus }$, and a radius of 2.39 ± 0.12 R ⊕, suggesting that the planet might be surrounded by a thick atmospheric envelope. The two planets have similar masses and lie on opposite sides of the radius gap, and are thus an excellent testbed for planet formation and evolution theories. Assuming that HD 15337 c hosts a hydrogen-dominated envelope, we employ a recently developed planet atmospheric evolution algorithm in a Bayesian framework to estimate the history of the high-energy (extreme ultraviolet and X-ray) emission of the host star. We find that at an age of 150 Myr, the star possessed on average between 3.7 and 127 times the high-energy luminosity of the current Sun.

185. Mass determination of two Jupiter-sized planets orbiting slightly evolved stars: TOI-2420 b and TOI-2485 b.

Author

Carleo, Ilaria, Barrágan, Oscar, Persson, Carina M., Fridlund, Malcolm, Lam, Kristine W. F., Messina, Sergio, Gandolfi, Davide, Smith, Alexis M. S., Johnson, Marshall C., Cochran, William, Osborne, Hannah L. M., Brahm, Rafael, Ciardi, David R., Collins, Karen A., Everett, Mark E., Giacalone, Steven, Guenther, Eike W., Hatzes, Artie, Hellier, Coel, and Horner, Jonathan

Subjects
*NATURAL satellites, *HOT Jupiters, *PLANETARY systems, *PLANETARY mass, *PLANETARY orbits
Abstract

Context. Hot and warm Jupiters might have undergone the same formation and evolution path, but the two populations exhibit different distributions of orbital parameters. This challenges our understanding of their actual origin. Aims. We report the results of our warm Jupiters survey, which was carried out with the CHIRON spectrograph within the KESPRINT collaboration. We addressed the question of the population origin by studying two planets that might help to bridge the gap between the two populations. Methods. We confirm two planets and determine their mass. One is a hot Jupiter (with an orbital period shorter than 10 days), TOI-2420 b, and the other is a warm Jupiter, TOI-2485 b. We analyzed them using a wide variety of spectral and photometric data in order to characterize these planetary systems. Results. We found that TOI-2420 b has an orbital period of Pb=5.8 days, a mass of Mb=0.9 MJ, and a radius of Rb=1.3 RJ, with a planetary density of 0.477 g cm−3. TOI-2485 b has an orbital period of Pb=11.2 days, a mass of Mb=2.4 MJ, and a radius of Rb=1.1 RJ with a density of 2.36 g cm−3. Conclusions. With the current parameters, the migration history for TOI-2420 b and TOI-2485 b is unclear: Scenarios of a high-eccentricity migration cannot be ruled out, and the characteristics of TOI-2485 b even support this scenario. [ABSTRACT FROM AUTHOR]

Published
2024
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