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

Author

Cloutier, Ryan, Charbonneau, David, Stassun, Keivan G., Murgas, Felipe, Mortier, Annelies, Massey, Robert, Lissauer, Jack J., Latham, David W., Irwin, Jonathan, Haywood, Raphaëlle D., Guerra, Pere, Girardin, Eric, Giacalone, Steven A., Bosch-Cabot, Pau, Bieryla, Allyson, Winn, Joshua, Watson, Christopher A., Vanderspek, Roland, Udry, Stéphane, Tamura, Motohide, Sozzetti, Alessandro, Shporer, Avi, Ségransan, Damien, Seager, Sara, Savel, Arjun B., Sasselov, Dimitar, Rose, Mark, Ricker, George, Rice, Ken, Quintana, Elisa V., Quinn, Samuel N., Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Pedani, Marco, Parviainen, Hannu, Palle, Enric, Narita, Norio, Molinari, Emilio, Micela, Giuseppina, McDermott, Scott, Mayor, Michel, Matson, Rachel A., Fiorenzano, Aldo F. Martinez, Lovis, Christophe, López-Morales, Mercedes, Kusakabe, Nobuhiko, Jensen, Eric L. N., Jenkins, Jon M., Huang, Chelsea X., Howell, Steve B., Harutyunyan, Avet, Fűrész, Gábor, Fukui, Akihiko, Esquerdo, Gilbert A., Esparza-Borges, Emma, Dumusque, Xavier, Dressing, Courtney D., Fabrizio, Luca Di, Collins, Karen A., Cameron, Andrew Collier, Christiansen, Jessie L., Cecconi, Massimo, Buchhave, Lars A., Boschin, Walter, Andreuzzi, Gloria, Cloutier, Ryan, Charbonneau, David, Stassun, Keivan G., Murgas, Felipe, Mortier, Annelies, Massey, Robert, Lissauer, Jack J., Latham, David W., Irwin, Jonathan, Haywood, Raphaëlle D., Guerra, Pere, Girardin, Eric, Giacalone, Steven A., Bosch-Cabot, Pau, Bieryla, Allyson, Winn, Joshua, Watson, Christopher A., Vanderspek, Roland, Udry, Stéphane, Tamura, Motohide, Sozzetti, Alessandro, Shporer, Avi, Ségransan, Damien, Seager, Sara, Savel, Arjun B., Sasselov, Dimitar, Rose, Mark, Ricker, George, Rice, Ken, Quintana, Elisa V., Quinn, Samuel N., Piotto, Giampaolo, Phillips, David, Pepe, Francesco, Pedani, Marco, Parviainen, Hannu, Palle, Enric, Narita, Norio, Molinari, Emilio, Micela, Giuseppina, McDermott, Scott, Mayor, Michel, Matson, Rachel A., Fiorenzano, Aldo F. Martinez, Lovis, Christophe, López-Morales, Mercedes, Kusakabe, Nobuhiko, Jensen, Eric L. N., Jenkins, Jon M., Huang, Chelsea X., Howell, Steve B., Harutyunyan, Avet, Fűrész, Gábor, Fukui, Akihiko, Esquerdo, Gilbert A., Esparza-Borges, Emma, Dumusque, Xavier, Dressing, Courtney D., Fabrizio, Luca Di, Collins, Karen A., Cameron, Andrew Collier, Christiansen, Jessie L., Cecconi, Massimo, Buchhave, Lars A., Boschin, Walter, and Andreuzzi, Gloria

Abstract

Studies of close-in planets orbiting M dwarfs have suggested that the M-dwarf radius valley may be well explained by distinct formation timescales between enveloped terrestrials and rocky planets that form at late times in a gas-depleted environment. This scenario is at odds with the picture that close-in rocky planets form with a primordial gaseous envelope that is subsequently stripped away by some thermally driven mass-loss process. These two physical scenarios make unique predictions of the rocky/enveloped transition's dependence on orbital separation such that studying the compositions of planets within the M-dwarf radius valley may be able to establish the dominant physics. Here, we present the discovery of one such keystone planet: the ultra-short-period planet TOI-1634 b (P = 0.989 days, , R⊕) orbiting a nearby M2 dwarf (Ks = 8.7, Rs = 0.450 R⊙, Ms = 0.502 M⊙) and whose size and orbital period sit within the M-dwarf radius valley. We confirm the TESS-discovered planet candidate using extensive ground-based follow-up campaigns, including a set of 32 precise radial velocity measurements from HARPS-N. We measure a planetary mass of M⊕, which makes TOI-1634 b inconsistent with an Earth-like composition at and thus requires either an extended gaseous envelope, a large volatile-rich layer, or a rocky composition that is not dominated by iron and silicates to explain its mass and radius. The discovery that the bulk composition of TOI-1634 b is inconsistent with that of Earth supports the gas-depleted formation mechanism to explain the emergence of the radius valley around M dwarfs with M⊙.

Published
2021

52. An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Author

Massachusetts Institute of Technology. Department of Physics, Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Crossfield, Ian Jm, Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris, Massachusetts Institute of Technology. Department of Physics, Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Crossfield, Ian Jm, Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris

Abstract

Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios., United States. National Aeronautics and Space Administration (Grant NNX15AC90G), United States. National Aeronautics and Space Administration (Grant NNX17AB59G)

Published
2021

53. Erratum: 'An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star' (2019, AJ, 158, 165)

Author

Mayo, Andrew W., Rajpaul, Vinesh M., Buchhave, Lars A., Dressing, Courtney D., Mortier, Annelies, Zeng, Li, Fortenbach, Charles D., Aigrain, Suzanne, Bonomo, Aldo S., Cameron, Andrew Collier, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martinez, Haywood, Raphaëlle D., Latham, David W., López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Rice, Ken, Sozzetti, Alessandro, Udry, Stephane, Mayo, Andrew W., Rajpaul, Vinesh M., Buchhave, Lars A., Dressing, Courtney D., Mortier, Annelies, Zeng, Li, Fortenbach, Charles D., Aigrain, Suzanne, Bonomo, Aldo S., Cameron, Andrew Collier, Charbonneau, David, Coffinet, Adrien, Cosentino, Rosario, Damasso, Mario, Dumusque, Xavier, Fiorenzano, A. F. Martinez, Haywood, Raphaëlle D., Latham, David W., López-Morales, Mercedes, Malavolta, Luca, Micela, Giusi, Molinari, Emilio, Pearce, Logan, Pepe, Francesco, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Rice, Ken, Sozzetti, Alessandro, and Udry, Stephane

Abstract

The semimajor axis and planet insolation flux of Kepler-538b were incorrectly calculated in the published article. This error did not impact any other parameters or any other results in the paper. Table 2 has been included in full here with the corrected semimajor axis and planet insolation flux values.

Published
2020

54. A Second Terrestrial Planet Orbiting the Nearby M Dwarf LHS 1140

Author

Ment, Kristo, Dittmann, Jason A., Astudillo-Defru, Nicola, Charbonneau, David, Irwin, Jonathan, Bonfils, Xavier, Murgas, Felipe, Almenara, Jose-Manuel, Forveille, Thierry, Agol, Eric, Ballard, Sarah, Berta-Thompson, Zachory K., Bouchy, François, Cloutier, Ryan, Delfosse, Xavier, Doyon, Rene, Dressing, Courtney D., Esquerdo, Gilbert A., Haywood, Raphaëlle D., Kipping, David M., Latham, David W., Lovis, Christophe, Newton, Elisabeth R., Pepe, Francesco, Rodriguez, Joseph E., Santos, Nuno C., Tan, Thiam-Guan, Udry, Stéphane, Winters, Jennifer G., Wünsche, Anaël, Dittmann, Jason, Berta-Thompson, Zachory, Dressing, Courtney, Esquerdo, Gilbert, Haywood, Raphaëlle, Kipping, David, Latham, David, Newton, Elisabeth, Rodriguez, Joseph, Santos, Nuno, Winters, Jennifer, Universidad de Concepción [Chile], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), University of Washington [Seattle], Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Departement de physique and Observatoire du Mont Megantic, Université de Montréal [Montréal], Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Department of Astrophysical and Planetary Sciences [Boulder], University of Colorado [Boulder], SUPA School of Physics and Astronomy [St Andrews], University of St Andrews [Scotland], European Organization for Nuclear Research (CERN), Smithsonian Institution-Harvard University [Cambridge], Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université de Montréal (UdeM), SUPA School of Physics and Astronomy [University of St Andrews], and University of St Andrews [Scotland]-Scottish Universities Physics Alliance (SUPA)

Subjects
planets and satellites: detection, 010504 meteorology & atmospheric sciences, Doppler spectroscopy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, planets and satellites: terrestrial planets, techniques: photometric, Planet, 0103 physical sciences, techniques: radial velocities, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Stellar atmosphere, Astronomy and Astrophysics, Radius, Radial velocity, Orbit, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

LHS 1140 is a nearby mid-M dwarf known to host a temperate rocky super-Earth (LHS 1140 b) on a 24.737-day orbit. Based on photometric observations by MEarth and Spitzer as well as Doppler spectroscopy from HARPS, we report the discovery of an additional transiting rocky companion (LHS 1140 c) with a mass of $1.81\pm0.39~{\rm M_{Earth}}$ and a radius of $1.282\pm0.024~{\rm R_{Earth}}$ on a tighter, 3.77795-day orbit. We also obtain more precise estimates of the mass and radius of LHS 1140 b to be $6.98\pm0.89~{\rm M_{Earth}}$ and $1.727\pm0.032~{\rm R_{Earth}}$. The mean densities of planets b and c are $7.5\pm1.0~\rm{g/cm^3}$ and $4.7\pm1.1~\rm{g/cm^3}$, respectively, both consistent with the Earth's ratio of iron to magnesium silicate. The orbital eccentricities of LHS 1140 b and c are consistent with circular orbits and constrained to be below 0.06 and 0.31, respectively, with 90% confidence. Because the orbits of the two planets are co-planar and because we know from previous analyses of Kepler data that compact systems of small planets orbiting M dwarfs are commonplace, a search for more transiting planets in the LHS 1140 system could be fruitful. LHS 1140 c is one of the few known nearby terrestrial planets whose atmosphere could be studied with the upcoming James Webb Space Telescope., Comment: 22 pages, 8 figures, accepted by AJ

Published
2019
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55. Using HARPS-N to characterise the long-period planets in the PH-2 and Kepler-103 systems

Author

Dubber, Sophie C, Mortier, Annelies, Rice, Ken, Nava, Chantanelle, Malavolta, Luca, Giles, Helen, Coffinet, Adrien, Charbonneau, David, Vanderburg, Andrew, Bonomo, Aldo S, Boschin, Walter, Buchhave, Lars A., Cameron, Andrew Collier, Cosentino, Rosario, Dumusque, Xavier, Ghedina, Adriano, Harutyunyan, Avet, Haywood, Raphaëlle D, Latham, David, López-Morales, Mercedes, Micela, Giusi, Molinari, Emilio, Pepe, Francesco A, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Sasselov, Dimitar, Sozzetti, Alessandro, Udry, Stéphane, Dubber, Sophie C, Mortier, Annelies, Rice, Ken, Nava, Chantanelle, Malavolta, Luca, Giles, Helen, Coffinet, Adrien, Charbonneau, David, Vanderburg, Andrew, Bonomo, Aldo S, Boschin, Walter, Buchhave, Lars A., Cameron, Andrew Collier, Cosentino, Rosario, Dumusque, Xavier, Ghedina, Adriano, Harutyunyan, Avet, Haywood, Raphaëlle D, Latham, David, López-Morales, Mercedes, Micela, Giusi, Molinari, Emilio, Pepe, Francesco A, Phillips, David, Piotto, Giampaolo, Poretti, Ennio, Sasselov, Dimitar, Sozzetti, Alessandro, and Udry, Stéphane

Abstract

We present confirmation of the planetary nature of PH-2b, as well as the first mass estimates for the two planets in the Kepler-103 system. PH-2b and Kepler-103c are both long-period and transiting, a sparsely-populated category of exoplanet. We use Kepler light-curve data to estimate a radius, and then use HARPS-N radial velocities to determine the semi-amplitude of the stellar reflex motion and, hence, the planet mass.

Published
2019

56. An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Author

Massachusetts Institute of Technology. Department of Physics, Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Crossfield, Ian Jm, Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris, Massachusetts Institute of Technology. Department of Physics, Malavolta, Luca, Mayo, Andrew W., Louden, Tom, Rajpaul, Vinesh M., Bonomo, Aldo S., Crossfield, Ian Jm, Buchhave, Lars A., Kreidberg, Laura, Kristiansen, Martti H., Lopez-Morales, Mercedes, Mortier, Annelies, Vanderburg, Andrew, Coffinet, Adrien, Ehrenreich, David, Lovis, Christophe, Bouchy, Francois, Charbonneau, David, Ciardi, David R., Cameron, Andrew Collier, Cosentino, Rosario, Damasso, Mario, Dressing, Courtney D., Dumusque, Xavier, Everett, Mark E., Figueira, Pedro, Fiorenzano, Aldo F. M., Gonzales, Erica J., Haywood, Raphaëlle D., Harutyunyan, Avet, Hirsch, Lea, Howell, Steve B., Johnson, John Asher, Latham, David W., Lopez, Eric, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Nascimbeni, Valerio, Pepe, Francesco, Phillips, David F., Piotto, Giampaolo, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris

Abstract

Ultra-short period (USP) planets are a class of low-mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, and it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of a USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b, we thus inferred a radius of 1.51 ±0.05 R and a mass of 5.08 ±0.41 M, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV data set, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ±0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000 K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios., United States. National Aeronautics and Space Administration (Grant NNX15AC90G), United States. National Aeronautics and Space Administration (Grant NNX17AB59G)

Published
2019

58. Using HARPS-N to characterize the long-period planets in the PH-2 and Kepler-103 systems

Author

Dubber, Sophie C, primary, Mortier, Annelies, additional, Rice, Ken, additional, Nava, Chantanelle, additional, Malavolta, Luca, additional, Giles, Helen, additional, Coffinet, Adrien, additional, Charbonneau, David, additional, Vanderburg, Andrew, additional, Bonomo, Aldo S, additional, Boschin, Walter, additional, Buchhave, Lars A, additional, Cameron, Andrew Collier, additional, Cosentino, Rosario, additional, Dumusque, Xavier, additional, Ghedina, Adriano, additional, Harutyunyan, Avet, additional, Haywood, Raphaëlle D, additional, Latham, David, additional, López-Morales, Mercedes, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Pepe, Francesco A, additional, Phillips, David, additional, Piotto, Giampaolo, additional, Poretti, Ennio, additional, Sasselov, Dimitar, additional, Sozzetti, Alessandro, additional, and Udry, Stéphane, additional

Published
2019
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60. An 11 Earth-mass, Long-period Sub-Neptune Orbiting a Sun-like Star

Author

Mayo, Andrew W., primary, Rajpaul, Vinesh M., additional, Buchhave, Lars A., additional, Dressing, Courtney D., additional, Mortier, Annelies, additional, Zeng, Li, additional, Fortenbach, Charles D., additional, Aigrain, Suzanne, additional, Bonomo, Aldo S., additional, Cameron, Andrew Collier, additional, Charbonneau, David, additional, Coffinet, Adrien, additional, Cosentino, Rosario, additional, Damasso, Mario, additional, Dumusque, Xavier, additional, Fiorenzano, A. F. Martinez, additional, Haywood, Raphaëlle D., additional, Latham, David W., additional, López-Morales, Mercedes, additional, Malavolta, Luca, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Pearce, Logan, additional, Pepe, Francesco, additional, Phillips, David, additional, Piotto, Giampaolo, additional, Poretti, Ennio, additional, Rice, Ken, additional, Sozzetti, Alessandro, additional, and Udry, Stephane, additional

Published
2019
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62. An Accurate Mass Determination for Kepler-1655b, a Moderately Irradiated World with a Significant Volatile Envelope

Author

Haywood, Raphaëlle D., primary, Vanderburg, Andrew, additional, Mortier, Annelies, additional, Giles, Helen A. C., additional, López-Morales, Mercedes, additional, Lopez, Eric D., additional, Malavolta, Luca, additional, Charbonneau, David, additional, Cameron, Andrew Collier, additional, Coughlin, Jeffrey L., additional, Dressing, Courtney D., additional, Nava, Chantanelle, additional, Latham, David W., additional, Dumusque, Xavier, additional, Lovis, Christophe, additional, Molinari, Emilio, additional, Pepe, Francesco, additional, Sozzetti, Alessandro, additional, Udry, Stéphane, additional, Bouchy, François, additional, Johnson, John A., additional, Mayor, Michel, additional, Micela, Giusi, additional, Phillips, David, additional, Piotto, Giampaolo, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Watson, Chris, additional, Affer, Laura, additional, Bonomo, Aldo S., additional, Buchhave, Lars A., additional, Ciardi, David R., additional, Fiorenzano, Aldo F., additional, and Harutyunyan, and Avet, additional

Published
2018
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63. An Ultra-short Period Rocky Super-Earth with a Secondary Eclipse and a Neptune-like Companion around K2-141

Author

Malavolta, Luca, primary, Mayo, Andrew W., additional, Louden, Tom, additional, Rajpaul, Vinesh M., additional, Bonomo, Aldo S., additional, Buchhave, Lars A., additional, Kreidberg, Laura, additional, Kristiansen, Martti H., additional, Lopez-Morales, Mercedes, additional, Mortier, Annelies, additional, Vanderburg, Andrew, additional, Coffinet, Adrien, additional, Ehrenreich, David, additional, Lovis, Christophe, additional, Bouchy, Francois, additional, Charbonneau, David, additional, Ciardi, David R., additional, Cameron, Andrew Collier, additional, Cosentino, Rosario, additional, Crossfield, Ian J. M., additional, Damasso, Mario, additional, Dressing, Courtney D., additional, Dumusque, Xavier, additional, Everett, Mark E., additional, Figueira, Pedro, additional, Fiorenzano, Aldo F. M., additional, Gonzales, Erica J., additional, Haywood, Raphaëlle D., additional, Harutyunyan, Avet, additional, Hirsch, Lea, additional, Howell, Steve B., additional, Johnson, John Asher, additional, Latham, David W., additional, Lopez, Eric, additional, Mayor, Michel, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Nascimbeni, Valerio, additional, Pepe, Francesco, additional, Phillips, David F., additional, Piotto, Giampaolo, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Udry, Stéphane, additional, and Watson, Chris, additional

Published
2018
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64. The Kepler-19 system:a thick-envelope super-Earth with two Neptune-mass companions characterized using radial velocities and transit timing variations

Author

Malavolta, Luca, Borsato, Luca, Granata, Valentina, Piotto, Giampaolo, Lopez, Eric, Vanderburg, Andrew, Figueira, Pedro, Mortier, Annelies, Nascimbeni, Valerio, Affer, Laura, Bonomo, Aldo S., Bouchy, Francois, Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Cosentino, Rosario, Dressing, Courtney D., Dumusque, Xavier, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Haywood, Raphaëlle D., Johnson, John Asher, Latham, David W., Lopez-Morales, Mercedes, Lovis, Christophe, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Motalebi, Fatemeh, Pepe, Francesco, Phillips, David F., Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar D., Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, Watson, Chris, Malavolta, Luca, Borsato, Luca, Granata, Valentina, Piotto, Giampaolo, Lopez, Eric, Vanderburg, Andrew, Figueira, Pedro, Mortier, Annelies, Nascimbeni, Valerio, Affer, Laura, Bonomo, Aldo S., Bouchy, Francois, Buchhave, Lars A., Charbonneau, David, Cameron, Andrew Collier, Cosentino, Rosario, Dressing, Courtney D., Dumusque, Xavier, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Haywood, Raphaëlle D., Johnson, John Asher, Latham, David W., Lopez-Morales, Mercedes, Lovis, Christophe, Mayor, Michel, Micela, Giusi, Molinari, Emilio, Motalebi, Fatemeh, Pepe, Francesco, Phillips, David F., Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar D., Ségransan, Damien, Sozzetti, Alessandro, Udry, Stéphane, and Watson, Chris

Published
2017

65. Radial-Velocity Variability of the Sun as a star with HARPS and HARPS-N

Author

Haywood, Raphaëlle D., and the HARPS-N science team, Feiden, Gregory, Fabbian, Damian, Simoniello, Rosaria, Collet, Remo, Criscuoli, Serena, Korhonen, Heidi, Krivova, Natalie, Oláh, Katalin, Shapiro, Alexander, Vidotto, Aline, and Vitas, Nikola

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

Since we can resolve the surface of the Sun directly, we can explore the origin of radial-velocity variations induced by individual solar surface features such as faculae/plage, sunspots and granulation. I will present my recent investigation of the radial-velocity variations of the Sun as a star, based on high-resolution HARPS spectra of reflected sunlight and simultaneous images from the Solar Dynamics Observatory. We found that faculae are the dominant source of activity-induced radial-velocity variations, via suppression of convective blueshift. We investigated possible proxies for activity-induced radial-velocity variations and found that optical lightcurves can only provide a partial representation of these signals; the full-disc magnetic flux, however, is an excellent tracer. In addition to this dataset, the HARPS-N spectrograph has been operating with a new solar telescope feed since 2015 July. I will present results from the first year observations, which show radial-velocity variations of up to 7-8 m/s. Identifying proxies for solar radial-velocity variations is key to understanding the radial-velocity variability of other Sun-like stars, and is also essential for other investigations such as exoplanet detection surveys.

Published
2016
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66. Radial-velocity variability of the Sun as a star with HARPS and HARPS-N

Author

Haywood, Raphaëlle D, Collier Cameron, Andrew, Dumusque, Xavier, Glenday, Alex, Latham, David W, Lovis, Christophe, Maldonado, Jesus, Micela, Giusi, Molinari, Emiliano, Mortier, Annelies, Pepe, Francesco, Phillips, David F, and Udry, Stephane

Subjects
Sun, Astrophysics::Solar and Stellar Astrophysics, magnetic activity, high-resolution spectroscopy, Sunspots, faculae/plage, Astrophysics::Earth and Planetary Astrophysics, exoplanets detection and characterisation, radial-velocity observations
Abstract

Since we can resolve the surface of the Sun directly, we can explore the origin of radial-velocity variations induced by individual solar surface features such as faculae/plage, sunspots and granulation. I will present my recent investigation of the radial-velocity variations of the Sun as a star, based on high-resolution HARPS spectra of reflected sunlight and simultaneous images from the Solar Dynamics Observatory. We found that faculae are the dominant source of activity-induced radial-velocity variations, via suppression of convective blueshift. We investigated possible proxies for activity-induced radial-velocity variations and found that optical lightcurves can only provide a partial representation of these signals; the full-disc magnetic flux, however, is an excellent tracer. In addition to this dataset, the HARPS-N spectrograph has been operating with a new solar telescope feed since 2015 July. I will present results from the first year observations, which show radial-velocity variations of up to 7-8 m/s. Identifying proxies for solar radial-velocity variations is key to understanding the radial-velocity variability of other Sun-like stars, and is also essential for other investigations such as exoplanet detection surveys. &nbsp

Published
2016
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67. Precise Masses in the WASP-47 System

Author

Vanderburg, Andrew, primary, Becker, Juliette C., additional, Buchhave, Lars A., additional, Mortier, Annelies, additional, Lopez, Eric, additional, Malavolta, Luca, additional, Haywood, Raphaëlle D., additional, Latham, David W., additional, Charbonneau, David, additional, López-Morales, Mercedes, additional, Adams, Fred C., additional, Bonomo, Aldo Stefano, additional, Bouchy, François, additional, Cameron, Andrew Collier, additional, Cosentino, Rosario, additional, Fabrizio, Luca Di, additional, Dumusque, Xavier, additional, Fiorenzano, Aldo, additional, Harutyunyan, Avet, additional, Johnson, John Asher, additional, Lorenzi, Vania, additional, Lovis, Christophe, additional, Mayor, Michel, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Pedani, Marco, additional, Pepe, Francesco, additional, Piotto, Giampaolo, additional, Phillips, David, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Udry, Stéphane, additional, and Watson, Chris, additional

Published
2017
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69. The Kepler-19 System: A Thick-envelope Super-Earth with Two Neptune-mass Companions Characterized Using Radial Velocities and Transit Timing Variations

Author

Malavolta, Luca, primary, Borsato, Luca, additional, Granata, Valentina, additional, Piotto, Giampaolo, additional, Lopez, Eric, additional, Vanderburg, Andrew, additional, Figueira, Pedro, additional, Mortier, Annelies, additional, Nascimbeni, Valerio, additional, Affer, Laura, additional, Bonomo, Aldo S., additional, Bouchy, Francois, additional, Buchhave, Lars A., additional, Charbonneau, David, additional, Cameron, Andrew Collier, additional, Cosentino, Rosario, additional, Dressing, Courtney D., additional, Dumusque, Xavier, additional, Fiorenzano, Aldo F. M., additional, Harutyunyan, Avet, additional, Haywood, Raphaëlle D., additional, Johnson, John Asher, additional, Latham, David W., additional, Lopez-Morales, Mercedes, additional, Lovis, Christophe, additional, Mayor, Michel, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Motalebi, Fatemeh, additional, Pepe, Francesco, additional, Phillips, David F., additional, Pollacco, Don, additional, Queloz, Didier, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Udry, Stéphane, additional, and Watson, Chris, additional

Published
2017
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70. A temperate rocky super-Earth transiting a nearby cool star

Author

Dittmann, Jason A., primary, Irwin, Jonathan M., additional, Charbonneau, David, additional, Bonfils, Xavier, additional, Astudillo-Defru, Nicola, additional, Haywood, Raphaëlle D., additional, Berta-Thompson, Zachory K., additional, Newton, Elisabeth R., additional, Rodriguez, Joseph E., additional, Winters, Jennifer G., additional, Tan, Thiam-Guan, additional, Almenara, Jose-Manuel, additional, Bouchy, François, additional, Delfosse, Xavier, additional, Forveille, Thierry, additional, Lovis, Christophe, additional, Murgas, Felipe, additional, Pepe, Francesco, additional, Santos, Nuno C., additional, Udry, Stephane, additional, Wünsche, Anaël, additional, Esquerdo, Gilbert A., additional, Latham, David W., additional, and Dressing, Courtney D., additional

Published
2017
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71. Kepler-21b:a rocky planet around a V=8.25 mag star

Author

Lopez-Morales, Mercedes, Haywood, Raphaëlle D., Coughlin, Jeffrey L., Zeng, Li, Buchhave, Lars A., Giles, Helen A. C., Affer, Laura, Bonomo, Aldo S., Charbonneau, David, Cameron, Andrew Collier, Consentino, Rosario, Dressing, Courtney D., Dumusque, Xavier, Figueira, Pedro, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Johnson, John Asher, Lovis, Christophe, Mayor, Michel, Motalebi, Fatemeh, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar, Segransan, Damien, Sozzetti, Alessandro, Udry, Stephane, Vanderburg, Andrew, Watson, Chris, Lopez-Morales, Mercedes, Haywood, Raphaëlle D., Coughlin, Jeffrey L., Zeng, Li, Buchhave, Lars A., Giles, Helen A. C., Affer, Laura, Bonomo, Aldo S., Charbonneau, David, Cameron, Andrew Collier, Consentino, Rosario, Dressing, Courtney D., Dumusque, Xavier, Figueira, Pedro, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Johnson, John Asher, Lovis, Christophe, Mayor, Michel, Motalebi, Fatemeh, Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar, Segransan, Damien, Sozzetti, Alessandro, Udry, Stephane, Vanderburg, Andrew, and Watson, Chris

Published
2016

72. KEPLER-21b: A ROCKY PLANET AROUND AV= 8.25 mag STAR

Author

López-Morales, Mercedes, primary, Haywood, Raphaëlle D., additional, Coughlin, Jeffrey L., additional, Zeng, Li, additional, Buchhave, Lars A., additional, Giles, Helen A. C., additional, Affer, Laura, additional, Bonomo, Aldo S., additional, Charbonneau, David, additional, Cameron, Andrew Collier, additional, Consentino, Rosario, additional, Dressing, Courtney D., additional, Dumusque, Xavier, additional, Figueira, Pedro, additional, Fiorenzano, Aldo F. M., additional, Harutyunyan, Avet, additional, Johnson, John Asher, additional, Latham, David W., additional, Lopez, Eric D., additional, Lovis, Christophe, additional, Malavolta, Luca, additional, Mayor, Michel, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Mortier, Annelies, additional, Motalebi, Fatemeh, additional, Nascimbeni, Valerio, additional, Pepe, Francesco, additional, Phillips, David F., additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Segransan, Damien, additional, Sozzetti, Alessandro, additional, Udry, Stephane, additional, Vanderburg, Andrew, additional, and Watson, Chris, additional

Published
2016
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73. A 1.9 EARTH RADIUS ROCKY PLANET AND THE DISCOVERY OF A NON-TRANSITING PLANET IN THE KEPLER-20 SYSTEM

Author

Buchhave, Lars A., primary, Dressing, Courtney D., additional, Dumusque, Xavier, additional, Rice, Ken, additional, Vanderburg, Andrew, additional, Mortier, Annelies, additional, Lopez-Morales, Mercedes, additional, Lopez, Eric, additional, Lundkvist, Mia S., additional, Kjeldsen, Hans, additional, Affer, Laura, additional, Bonomo, Aldo S., additional, Charbonneau, David, additional, Cameron, Andrew Collier, additional, Cosentino, Rosario, additional, Figueira, Pedro, additional, Fiorenzano, Aldo F. M., additional, Harutyunyan, Avet, additional, Haywood, Raphaëlle D., additional, Johnson, John Asher, additional, Latham, David W., additional, Lovis, Christophe, additional, Malavolta, Luca, additional, Mayor, Michel, additional, Micela, Giusi, additional, Molinari, Emilio, additional, Motalebi, Fatemeh, additional, Nascimbeni, Valerio, additional, Pepe, Francesco, additional, Phillips, David F., additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Udry, Stéphane, additional, and Watson, Chris, additional

Published
2016
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74. The mass of Kepler-93b and the composition of terrestrial planets

Author

Dressing, Courtney D., Charbonneau, David, Dumusque, Xavier, Gettel, Sara, Pepe, Francesco, Cameron, Andrew Collier, Latham, David W., Molinari, Emilio, Udry, Stéphane, Affer, Laura, Bonomo, Aldo S., Buchhave, Lars A., Cosentino, Rosario, Figueira, Pedro, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Haywood, Raphaëlle D., Johnson, John Asher, Lopez-Morales, Mercedes, Lovis, Christophe, Malavolta, Luca, Mayor, Michel, Micela, Giusi, Motalebi, Fatemeh, Nascimbeni, Valerio, Phillips, David F., Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Szentgyorgyi, Andrew, Watson, Chris, Dressing, Courtney D., Charbonneau, David, Dumusque, Xavier, Gettel, Sara, Pepe, Francesco, Cameron, Andrew Collier, Latham, David W., Molinari, Emilio, Udry, Stéphane, Affer, Laura, Bonomo, Aldo S., Buchhave, Lars A., Cosentino, Rosario, Figueira, Pedro, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Haywood, Raphaëlle D., Johnson, John Asher, Lopez-Morales, Mercedes, Lovis, Christophe, Malavolta, Luca, Mayor, Michel, Micela, Giusi, Motalebi, Fatemeh, Nascimbeni, Valerio, Phillips, David F., Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar, Ségransan, Damien, Sozzetti, Alessandro, Szentgyorgyi, Andrew, and Watson, Chris

Published
2015

77. THE MASS OF Kepler-93b AND THE COMPOSITION OF TERRESTRIAL PLANETS

Author

Dressing, Courtney D., primary, Charbonneau, David, additional, Dumusque, Xavier, additional, Gettel, Sara, additional, Pepe, Francesco, additional, Collier Cameron, Andrew, additional, Latham, David W., additional, Molinari, Emilio, additional, Udry, Stéphane, additional, Affer, Laura, additional, Bonomo, Aldo S., additional, Buchhave, Lars A., additional, Cosentino, Rosario, additional, Figueira, Pedro, additional, Fiorenzano, Aldo F. M., additional, Harutyunyan, Avet, additional, Haywood, Raphaëlle D., additional, Johnson, John Asher, additional, Lopez-Morales, Mercedes, additional, Lovis, Christophe, additional, Malavolta, Luca, additional, Mayor, Michel, additional, Micela, Giusi, additional, Motalebi, Fatemeh, additional, Nascimbeni, Valerio, additional, Phillips, David F., additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Szentgyorgyi, Andrew, additional, and Watson, Chris, additional

Published
2015
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78. FrontMatter.

Author

Haywood, Raphaëlle D.

Published
2016

79. THE KEPLER-10 PLANETARY SYSTEM REVISITED BY HARPS-N: A HOT ROCKY WORLD AND A SOLID NEPTUNE-MASS PLANET

Author

Dumusque, Xavier, primary, Bonomo, Aldo S., additional, Haywood, Raphaëlle D., additional, Malavolta, Luca, additional, Ségransan, Damien, additional, Buchhave, Lars A., additional, Cameron, Andrew Collier, additional, Latham, David W., additional, Molinari, Emilio, additional, Pepe, Francesco, additional, Udry, Stéphane, additional, Charbonneau, David, additional, Cosentino, Rosario, additional, Dressing, Courtney D., additional, Figueira, Pedro, additional, Fiorenzano, Aldo F. M., additional, Gettel, Sara, additional, Harutyunyan, Avet, additional, Horne, Keith, additional, Lopez-Morales, Mercedes, additional, Lovis, Christophe, additional, Mayor, Michel, additional, Micela, Giusi, additional, Motalebi, Fatemeh, additional, Nascimbeni, Valerio, additional, Phillips, David F., additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Sozzetti, Alessandro, additional, Szentgyorgyi, Andrew, additional, and Watson, Chris, additional

Published
2014
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80. An Earth-sized planet with an Earth-like density

Author

Pepe, Francesco, primary, Cameron, Andrew Collier, additional, Latham, David W., additional, Molinari, Emilio, additional, Udry, Stéphane, additional, Bonomo, Aldo S., additional, Buchhave, Lars A., additional, Charbonneau, David, additional, Cosentino, Rosario, additional, Dressing, Courtney D., additional, Dumusque, Xavier, additional, Figueira, Pedro, additional, Fiorenzano, Aldo F. M., additional, Gettel, Sara, additional, Harutyunyan, Avet, additional, Haywood, Raphaëlle D., additional, Horne, Keith, additional, Lopez-Morales, Mercedes, additional, Lovis, Christophe, additional, Malavolta, Luca, additional, Mayor, Michel, additional, Micela, Giusi, additional, Motalebi, Fatemeh, additional, Nascimbeni, Valerio, additional, Phillips, David, additional, Piotto, Giampaolo, additional, Pollacco, Don, additional, Queloz, Didier, additional, Rice, Ken, additional, Sasselov, Dimitar, additional, Ségransan, Damien, additional, Sozzetti, Alessandro, additional, Szentgyorgyi, Andrew, additional, and Watson, Christopher A., additional

Published
2013
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81. An astro-comb calibrated solar telescope to search for the radial velocity signature of Venus

Author

Phillips, David F., Glenday, Alex, Dumusque, Xavier, Buchschacher, Nicolas, Cameron, Andrew Collier, Cecconi, Massimo, Charbonneau, David, Cosentino, Rosario, Ghedina, Adriano, Haywood, Raphaelle D., Latham, David Winslow, Li, Chih-Hao, Lodi, Marcello, Lovis, Christophe, Molinari, Emilio, Pepe, Francesco, Sasselov, Dimitar D., Szentgyorgyi, Andrew H., Udry, Stephane, and Walsworth, Ronald Lee

Abstract

We recently demonstrated sub-m/s sensitivity in measuring the radial velocity (RV) between the Earth and Sun using a simple solar telescope feeding the HARPS-N spectrograph at the Italian National Telescope, which is calibrated with a green astro-comb. We are using the solar telescope to characterize the effects of stellar (solar) RV jitter due to activity on the solar surface with the goal of detecting the solar RV signal from Venus, thereby demonstrating the sensitivity of these instruments to detect true Earth-twin exoplanets., Physics

Published
2016
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82. The Mass of Kepler-93b and the Composition of Terrestrial Planets

Author

Dressing, Courtney Danielle, Charbonneau, David, Dumusque, Xavier, Gettel, Sara, Pepe, Francesco, Collier Cameron, Andrew, Latham, David Winslow, Molinari, Emilio, Udry, Stéphane, Affer, Laura, Bonomo, Aldo S., Buchhave, Lars A., Cosentino, Rosario, Figueira, Pedro, Fiorenzano, Aldo F. M., Harutyunyan, Avet, Haywood, Raphaelle D., Johnson, John Asher, Lopez-Morales, Mercedes, Lovis, Christophe, Malavolta, Luca, Mayor, Michel, Micela, Giusi, Motalebi, Fatemeh, Nascimbeni, Valerio, Phillips, David F., Piotto, Giampaolo, Pollacco, Don, Queloz, Didier, Rice, Ken, Sasselov, Dimitar D., Ségransan, Damien, Sozzetti, Alessandro, Szentgyorgyi, Andrew H., and Watson, Chris

Subjects
planetary systems, planets and satellites: composition, stars: individual (Kepler-93 = KOI 69 = KIC 3544595), techniques: radial velocities
Abstract

Kepler-93b is a 1.478 ± 0.019 R⊕ planet with a 4.7 day period around a bright (V = 10.2), astroseismically characterized host star with a mass of 0.911 ± 0.033 M and a radius of 0.919 ± 0.011 R. Based on 86 radial velocity observations obtained with the HARPS-N spectrograph on the Telescopio Nazionale Galileo and 32 archival Keck/HIRES observations, we present a precise mass estimate of 4.02±0.68 M⊕. The corresponding high density of 6.88±1.18 g cm−3 is consistent with a rocky composition of primarily iron and magnesium silicate. We compare Kepler-93b to other dense planets with well-constrained parameters and find that between 1 and 6 M⊕, all dense planets including the Earth and Venus are well-described by the same fixed ratio of iron to magnesium silicate. There are as of yet no examples of such planets with masses > 6 M⊕. All known planets in this mass regime have lower densities requiring significant fractions of volatiles or H/He gas. We also constrain the mass and period of the outer companion in the Kepler-93 system from the long-term radial velocity trend and archival adaptive optics images. As the sample of dense planets with well-constrained masses and radii continues to grow, we will be able to test whether the fixed compositional model found for the seven dense planets considered in this paper extends to the full population of 1–6 M⊕ planets., Astronomy

Published
2015
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83. The HARPS-N Rocky Planet Search

Author

Motalebi, F., Udry, S., Gillon, M., Lovis, C., Ségransan, D., Buchhave, L. A., Demory, B. O., Malavolta, L., Dressing, Courtney Danielle, Sasselov, Dimitar D., Rice, K., Charbonneau, David, Collier Cameron, A., Latham, David Winslow, Molinari, E., Pepe, F., Affer, L., Bonomo, A. S., Cosentino, R., Dumusque, X., Figueira, P., Fiorenzano, A. F. M., Gettel, S., Harutyunyan, A., Haywood, Raphaelle D., Johnson, John Asher, Lopez, E., Lopez-Morales, Maria Mercedes, Mayor, M., Micela, G., Mortier, A., Nascimbeni, V., Philips, D., Piotto, G., Pollacco, D., Queloz, D., Sozzetti, A., Vanderburg, A., and Watson, C. A.

Subjects
techniques: radial velocities, techniques: photometric, stars: individual: HD 219134, binaries: eclipsing, instrumentation: spectrographs
Abstract

We know now from radial velocity surveys and transit space missions that planets only a few times more massive than our Earth are frequent around solar-type stars. Fundamental questions about their formation history, physical properties, internal structure, and atmosphere composition are, however, still to be solved. We present here the detection of a system of four low-mass planets around the bright (V = 5.5) and close-by (6.5 pc) star HD 219134. This is the first result of the Rocky Planet Search programme with HARPS-N on the Telescopio Nazionale Galileo in La Palma. The inner planet orbits the star in 3.0935 ± 0.0003 days, on a quasicircular orbit with a semi-major axis of 0.0382 ± 0.0003 AU. Spitzer observations allowed us to detect the transit of the planet in front of the star making HD 219134 b the nearest known transiting planet to date. From the amplitude of the radial velocity variation (2.25 ± 0.22 ms−1 ) and observed depth of the transit (359 ± 38 ppm), the planet mass and radius are estimated to be 4.36 ± 0.44 M⊕ and 1.606 ± 0.086 R⊕, leading to a mean density of 5.76 ± 1.09 g cm−3 , suggesting a rocky composition. One additional planet with minimum-mass of 2.78 ± 0.65 M⊕ moves on a close-in, quasi-circular orbit with a period of 6.767 ± 0.004 days. The third planet in the system has a period of 46.66 ± 0.08 days and a minimum-mass of 8.94 ± 1.13 M⊕, at 0.233 ± 0.002 AU from the star. Its eccentricity is 0.46 ± 0.11. The period of this planet is close to the rotational period of the star estimated from variations of activity indicators (42.3 ± 0.1 days). The planetary origin of the signal is, however, the preferred solution as no indication of variation at the corresponding frequency is observed for activity-sensitive parameters. Finally, a fourth additional longer-period planet of mass of 71 M⊕ orbits the star in 1842 days, on an eccentric orbit (e = 0.34 ± 0.17) at a distance of 2.56 AU., Astronomy

Published
2015
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85. BackMatter.

Author

Haywood, Raphaëlle D.

Published
2016

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

Author

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

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

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

Published
2022
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87. Radial-Velocity Signatures Of Magnetic Features On The Sun Observed As A Star

Author

Palumbo, Michael L., Haywood, Raphaëlle D., Saar, Steven H., and Dupree, Andrea K.

Subjects
Active Regions, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Radial Velocity, Solar Activity, Solar Magnetic Fields
Abstract

In recent years, the search for Earth-mass planets using radial-velocity measurements has become increasingly limited by signals arising from stellar activity. Individual magnetic features induce localized changes in intensity and velocity, which combine to change the apparent radial velocity of the star. Therefore it is critical to identify an indicator of activity-driven radial-velocity variations on the timescale of stellar rotation periods. We use 617.3 nm photospheric filtergrams, magnetograms, and dopplergrams from SDO/HMI and 170.0 nm chromospheric filtergrams from AIA to identify magnetically-driven solar features and reconstruct the integrated solar radial velocity with six samples per day over the course of 2014. Breaking the solar image up into regions of umbrae, penumbrae, quiet Sun, network, and plages, we find a distinct variation in the center-to-limb intensity-weighted velocity for each region. In agreement with past studies, we find that the suppression of convective blueshift is dominated by plages and network, rather than dark photospheric features. In the future, this work will be highly useful for identifying indicators which correlate with rotationally modulated radial-velocity variations. This will allow us to break the activity barrier that currently precludes the precise characterization of exoplanet properties at the lowest masses., This work was supported by the NSF-REU solar physics program at SAO, grant number AGS-1560313. This work was performed in part under contract with the California Institute of Technology (Caltech)/Jet Propulsion Laboratory (JPL) funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute.

Published
2017
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