54 results on '"Tom Louden"'
Search Results
2. NGTS-7Ab: an ultrashort-period brown dwarf transiting a tidally locked and active M dwarf
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James A G Jackman, Peter J Wheatley, Dan Bayliss, Samuel Gill, Simon T Hodgkin, Matthew R Burleigh, Ian P Braker, Maximilian N Günther, Tom Louden, Oliver Turner, David R Anderson, Claudia Belardi, François Bouchy, Joshua T Briegal, Edward M Bryant, Juan Cabrera, Sarah L Casewell, Alexander Chaushev, Jean C Costes, Szilard Csizmadia, Philipp Eigmüller, Anders Erikson, Boris T Gänsicke, Edward Gillen, Michael R Goad, James S Jenkins, James McCormac, Maximiliano Moyano, Louise D Nielsen, Don Pollacco, Katja Poppenhaeger, Didier Queloz, Heike Rauer, Liam Raynard, Alexis M S Smith, Stéphane Udry, Jose I Vines, Christopher A Watson, and Richard G West
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- 2019
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3. NGTS-6b: an ultrashort period hot-Jupiter orbiting an old K dwarf
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Jose I Vines, James S Jenkins, Jack S Acton, Joshua Briegal, Daniel Bayliss, François Bouchy, Claudia Belardi, Edward M Bryant, Matthew R Burleigh, Juan Cabrera, Sarah L Casewell, Alexander Chaushev, Benjamin F Cooke, Szilárd Csizmadia, Philipp Eigmüller, Anders Erikson, Emma Foxell, Samuel Gill, Edward Gillen, Michael R Goad, James A G Jackman, George W King, Tom Louden, James McCormac, Maximiliano Moyano, Louise D Nielsen, Don Pollacco, Didier Queloz, Heike Rauer, Liam Raynard, Alexis M S Smith, Maritza G Soto, Rosanna H Tilbrook, Ruth Titz-Weider, Oliver Turner, Stéphane Udry, Simon R Walker, Christopher A Watson, Richard G West, and Peter J Wheatley
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- 2019
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4. Detection of a giant flare displaying quasi-periodic pulsations from a pre-main-sequence M star by the Next Generation Transit Survey
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James A G Jackman, Peter J Wheatley, Chloe E Pugh, Dmitrii Y Kolotkov, Anne-Marie Broomhall, Grant M Kennedy, Simon J Murphy, Roberto Raddi, Matthew R Burleigh, Sarah L Casewell, Philipp Eigmüller, Edward Gillen, Maximilian N Günther, James S Jenkins, Tom Louden, James McCormac, Liam Raynard, Katja Poppenhaeger, Stéphane Udry, Christopher A Watson, and Richard G West
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- 2018
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5. NGTS-2b: an inflated hot-Jupiter transiting a bright F-dwarf
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Liam Raynard, Michael R Goad, Edward Gillen, Louise D Nielsen, Christopher A Watson, Andrew P G Thompson, James McCormac, Daniel Bayliss, Maritza Soto, Szilard Csizmadia, Alexander Chaushev, Matthew R Burleigh, Richard Alexander, David J Armstrong, François Bouchy, Joshua T Briegal, Juan Cabrera, Sarah L Casewell, Bruno Chazelas, Benjamin F Cooke, Philipp Eigmüller, Anders Erikson, Boris T Gänsicke, Andrew Grange, Maximilian N Günther, Simon T Hodgkin, Matthew J Hooton, James S Jenkins, Gregory Lambert, Tom Louden, Lionel Metrailler, Maximiliano Moyano, Don Pollacco, Katja Poppenhaeger, Didier Queloz, Roberto Raddi, Heike Rauer, Andrew M Read, Barry Smalley, Alexis M S Smith, Oliver Turner, Stéphane Udry, Simon R Walker, Richard G West, and Peter J Wheatley
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- 2018
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6. Mapping exoplanet atmospheres in high energy environments
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Tom Louden
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High energy ,Environmental science ,Exoplanet ,Astrobiology - Abstract
Exoplanet atmospheres are often treated as a single monolithic whole in transmission spectroscopy, while in reality they are dynamic and complex objects rich with inhomogeneities. We will show that using the technique of transit limb scanning it is possible to recover additional information on the spatial, chemical and velocity distributions of planet atmospheres that would otherwise have been lost. We will present results of transit limb scanning applied to a variety of hot jupiters, in particular using high resolution data of the sodium absorption to recover the equatorial and polar wind speeds on several planets spanning the temperature regime, and a new model of the metastable helium outflow of WASP 107b, where we find strong evidence of an extended comet-like tail. In each case we fit a variety of models with different atmosphere architecture in increasing complexity to the time resolved high resolution transmission spectra, using a Bayesian evidence approach to model comparison in order to find the model that best explained the data. Mapping exoplanets will be the key to solving a number of theoretical issues, as atmospheric wind speed is governed by the level of drag in the atmosphere, which is not well constrained by theoretical models. Similarly, the shape of helium outflows on evaporating planets will be important to proper determinations of evaporation rate, which sculpts the shape of the entire planet population.
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- 2021
7. Detection of a giant flare displaying quasi-periodic pulsations from a pre-main-sequence M star by the Next Generation Transit Survey
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Maximilian N. Günther, Matthew R. Burleigh, Dmitrii Y. Kolotkov, James S. Jenkins, Peter J. Wheatley, Sarah L. Casewell, Stéphane Udry, Edward Gillen, Richard G. West, James A. G. Jackman, James McCormac, Philipp Eigmüller, Liam Raynard, Christopher A. Watson, Katja Poppenhaeger, Anne-Marie Broomhall, Simon J. Murphy, Grant M. Kennedy, Roberto Raddi, Tom Louden, and Chloe E. Pugh
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Extrasolare Planeten und Atmosphären ,Data products ,Astrophysics::High Energy Astrophysical Phenomena ,Library science ,stars: pre-main-sequence ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Virtual observatory ,7. Clean energy ,01 natural sciences ,Infrared Processing and Analysis Center ,stars: individual: NGTS J121939.5-355557 ,stars: low-mass ,Observatory ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Transit (satellite) ,Astrophysics::Galaxy Astrophysics ,National data ,Physics ,010308 nuclear & particles physics ,Astronomy and Astrophysics ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,stars: flare ,Astrophysics::Earth and Planetary Astrophysics ,Quasi periodic ,Administration (government) - Abstract
This research is based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is funded by a consortium of institutes consisting of the University of Warwick, the University of Leicester, Queen’s University Belfast, the University of Geneva, the Deutsches Zentrum fur Luft- und Raumfahrt e.V. (DLR; under the ‘Grosinvestition GI-NGTS’), the University of Cambridge, together with the UK Science and Technology Facilities Council (STFC; project reference ST/M001962/1). JAGJ is supported by STFC PhD studentship 1763096. PJW and RGW are supported by the STFC consolidated grant ST/P000495/1. AMB acknowledges the support of the Institute of Advanced Study, University of Warwick, and is also supported by the STFC consolidated grant ST/P000320/1. MNG is supported by the STFC award reference 1490409 as well as the Isaac Newton Studentship. CEP acknowledges support from the European Research Council under the SeismoSun Research Project No. 321141. JSJ acknowledges support by Fondecyt grant 1161218 and partial support by CATA-Basal (PB06, CONICYT). DYK acknowledges support by the STFC consolidated grant ST/P000320/1. GMK is supported by the Royal Society as a Royal Society University Research Fellow. We also acknowledge and thank the ISSI team led by AMB for useful discussions. This publication makes use of data products from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the WISE, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. The national facility capability for SkyMapper has been funded through ARC LIEF grant LE130100104 from the Australian Research Council, awarded to the University of Sydney, the Australian National University, Swinburne University of Technology, the University of Queensland, the University of Western Australia, the University of Melbourne, Curtin University of Technology, Monash University and the Australian Astronomical Observatory. SkyMapper is owned and operated by the Australian National University’s Research School of Astronomy and Astrophysics. The survey data were processed and provided by the SkyMapper Team at the ANU. The SkyMapper node of the All-Sky Virtual Observatory (ASVO) is hosted at the National Computational Infrastructure (NCI). Development and support the SkyMapper node of the ASVO has been funded in part by Astronomy Australia Limited (AAL) and the Australian Government through the Commonwealth’s Education Investment Fund (EIF) and National Collaborative Research Infrastructure Strategy (NCRIS), particularly the National eResearch Collaboration Tools and Resources (NeCTAR) and the Australian National Data Service Projects (ANDS). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
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- 2018
8. The near-UV transit of HD 189733b with the XMM-Newton optical monitor
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Vincent Bourrier, Maria Steinrueck, Alain Lecavelier des Etangs, David Ehrenreich, George King, Tom Louden, Lia Corrales, Panayotis Lavvas, Peter J. Wheatley, University of Michigan [Ann Arbor], University of Michigan System, University of Warwick [Coventry], Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), University of Arizona, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,planets and satellites: atmospheres ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,ultraviolet: planetary systems ,FOS: Physical sciences ,Astronomy and Astrophysics ,Radius ,Astrophysics ,01 natural sciences ,3. Good health ,planets and satellites: individual: HD 189733b ,Wavelength ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Hot Jupiter ,Roche lobe ,Absorption (logic) ,Transit (astronomy) ,Spectral resolution ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present analysis of XMM-Newton Optical Monitor observations in the near-ultraviolet of HD 189733, covering twenty primary transits of its hot Jupiter planet. The transit is clearly detected with both the UVW2 and UVM2 filters, and our fits to the data reveal transit depths in agreement with that observed optically. The measured depths correspond to radii of $1.059^{+0.046}_{-0.050}$ and $0.94^{+0.15}_{-0.17}$ times the optically-measured radius (1.187 R$_{\rm J}$ at 4950 \r{A}) in the UVW2 and UVM2 bandpasses, respectively. We also find no statistically significant variation in the transit depth across the 8 year baseline of the observations. We rule out extended broadband absorption towards or beyond the Roche lobe at the wavelengths investigated, although observations with higher spectral resolution are required to determine if absorption out to those distances from the planet is present in individual near-UV lines., Comment: 7 pages, 7 figures, 3 tables; accepted for publication in MNRAS
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- 2021
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9. An Ultra-Hot Neptune in the Neptune desert
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Todd C. Klaus, Jose I. Vines, Ruth Titz-Weider, Motohide Tamura, Jessie L. Christiansen, Samuel N. Quinn, M. G. Soto, J. Villasenor, Pablo Rojas, George R. Ricker, Simon R. Walker, Maximiliano Moyano, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Andrés Jordán, Juan Cabrera, Pascal Torres, Michael R. Goad, Jerome de Leon, Giovanni Isopi, David R. Ciardi, Daniel Bayliss, K. I. Collins, Peter J. Wheatley, Jack J. Lissauer, Norio Narita, David W. Latham, François Bouchy, Sarah L. Casewell, Oliver Turner, Mayuko Mori, Andrea Ercolino, Cristobal Petrovich, Richard G. West, E. Foxell, Claudia Belardi, Philipp Eigmüller, James McCormac, Tom Louden, Eric D. Lopez, Liam Raynard, Benjamin F. Cooke, Edward Gillen, George W. King, Allyson Bieryla, Karen A. Collins, Matias Diaz, Heike Rauer, David J. Armstrong, Jack S. Acton, James A. G. Jackman, Don Pollacco, Anders Erikson, Néstor Espinoza, Michael Vezie, Samuel Gill, Nicholas M. Law, Carl Ziegler, Jon M. Jenkins, Edward M. Bryant, Rafael Brahm, Alexis M. S. Smith, Charles Beichman, Boris T. Gänsicke, Roland Vanderspek, Andrew W. Mann, Taku Nishiumi, Pía Cortés-Zuleta, Didier Queloz, Rosanna H. Tilbrook, Matthew J. Hooton, Louise D. Nielsen, Joshua N. Winn, Christopher J. Burke, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, James S. Jenkins, Christopher E. Henze, Stéphane Udry, F. Mallia, Christopher A. Watson, Jenkins, JS [0000-0003-2733-8725], Espinoza, N [0000-0001-9513-1449], Brahm, R [0000-0002-9158-7315], Cortés-Zuleta, P [0000-0002-6174-4666], Wheatley, PJ [0000-0003-1452-2240], Winn, JN [0000-0002-4265-047X], Seager, S [0000-0002-6892-6948], Jenkins, JM [0000-0002-4715-9460], Bieryla, A [0000-0001-6637-5401], Christiansen, JL [0000-0002-8035-4778], Mori, M [0000-0003-1368-6593], Narita, N [0000-0001-8511-2981], Nishiumi, T [0000-0003-1510-8981], Tamura, M [0000-0002-6510-0681], Lissauer, JJ [0000-0001-6513-1659], Collins, KA [0000-0001-6588-9574], Collins, KI [0000-0003-2781-3207], Armstrong, DJ [0000-0002-5080-4117], Bayliss, D [0000-0001-6023-1335], Cabrera, J [0000-0001-6653-5487], Casewell, SL [0000-0003-2478-0120], Eigmüller, P [0000-0003-4096-0594], Günther, MN [0000-0002-3164-9086], Hooton, MJ [0000-0003-0030-332X], Queloz, D [0000-0002-3012-0316], Smith, AMS [0000-0002-2386-4341], Udry, S [0000-0001-7576-6236], Watson, CA [0000-0002-9718-3266], West, RG [0000-0001-6604-5533], and Apollo - University of Cambridge Repository
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Extrasolare Planeten und Atmosphären ,Earth and Planetary Astrophysics (astro-ph.EP) ,astro-ph.SR ,010504 meteorology & atmospheric sciences ,Leitungsbereich PF ,Library science ,FOS: Physical sciences ,Astronomy and Astrophysics ,Northern ireland ,01 natural sciences ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Political science ,0103 physical sciences ,astro-ph.EP ,Astrophysics::Solar and Stellar Astrophysics ,Christian ministry ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Research center ,Solar and Stellar Astrophysics (astro-ph.SR) ,0105 earth and related environmental sciences ,QB ,Astrophysics - Earth and Planetary Astrophysics - Abstract
About one out of 200 Sun-like stars has a planet with an orbital period shorter than one day: an ultra-short-period planet (Sanchis-ojeda et al. 2014; Winn et al. 2018). All of the previously known ultra-short-period planets are either hot Jupiters, with sizes above 10 Earth radii (Re), or apparently rocky planets smaller than 2 Re. Such lack of planets of intermediate size (the "hot Neptune desert") has been interpreted as the inability of low-mass planets to retain any hydrogen/helium (H/He) envelope in the face of strong stellar irradiation. Here, we report the discovery of an ultra-short-period planet with a radius of 4.6 Re and a mass of 29 Me, firmly in the hot Neptune desert. Data from the Transiting Exoplanet Survey Satellite (Ricker et al. 2015) revealed transits of the bright Sun-like star \starname\, every 0.79 days. The planet's mean density is similar to that of Neptune, and according to thermal evolution models, it has a H/He-rich envelope constituting 9.0^(+2.7)_(-2.9)% of the total mass. With an equilibrium temperature around 2000 K, it is unclear how this "ultra-hot Neptune" managed to retain such an envelope. Follow-up observations of the planet's atmosphere to better understand its origin and physical nature will be facilitated by the star's brightness (Vmag=9.8)., Comment: 26 pages, 10 figures, 3 tables. Published in Nature Astronomy (21/09/2020)
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- 2020
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10. NGTS J214358.5−380102 – NGTS discovery of the most eccentric known eclipsing M-dwarf binary system
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Philipp Eigmüller, Benjamin F. Cooke, Matthew R. Burleigh, James S. Jenkins, Stéphane Udry, Sarah L. Casewell, Michael R. Goad, David R. Anderson, Richard G. West, James McCormac, Samuel Gill, Maximiliano Moyano, Liam Raynard, Monika Lendl, Louise D. Nielsen, Daniel Bayliss, Richard Alexander, Claudia Belardi, Rossanna H. Tilbrook, Tom Louden, Peter J. Wheatley, Jack S. Acton, James A. G. Jackman, Edward M. Bryant, Christopher A. Watson, and Jose I. Vines
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Physics ,Extrasolare Planeten und Atmosphären ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,European research ,Library science ,binaries: eclipsing ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,eclipsing [binaries] ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Administration (government) ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery of NGTS J214358.5-380102, an eccentric M-dwarf binary discovered by the Next Generation Transit Survey. The system period of 7.618 days is greater than many known eclipsing M-dwarf binary systems. Its orbital eccentricity of $0.323^{+0.0014}_{-0.0037}$, is large relative to the period and semi-major axis of the binary. Global modelling of photometry and radial velocities indicate stellar masses of $M_A$=$0.426 ^{+0.0056}_{-0.0049}$, $M_B$=$0.455 ^{+0.0058}_{-0.0052}$ and stellar radii $R_A$=$0.461 ^{+0.038}_{-0.025}$ $R_B$=$0.411 ^{+0.027}_{-0.039}$, respectively. Comparisons with stellar models for low mass stars show that one star is consistent with model predictions whereas the other is substantially oversized. Spectral analysis of the system suggests a primary of spectral type M3V, consistent with both modelled masses and radii, and with SED fitting of NGTS photometry. As the most eccentric eclipsing M-dwarf binary known, NGTS J214358.5-380102 provides an interesting insight into the strength of tidal effects in the circularisation of stellar orbits., Comment: Accepted for Publication in MNRAS
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- 2020
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11. MOVES III. Simultaneous X-ray and ultraviolet observations unveiling the variable environment of the hot Jupiter HD 189733b
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Rim Fares, Vincent Bourrier, Peter J. Wheatley, David Ehrenreich, Joe Llama, A. Lecavelier des Etangs, Moira Jardine, Tom Louden, Christiane Helling, George W. King, Aline A. Vidotto, Science & Technology Facilities Council, University of St Andrews. St Andrews Centre for Exoplanet Science, University of St Andrews. School of Physics and Astronomy, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
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Planet-star interactions ,stars: chromospheres ,chromospheres, coronae [Stars] ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,individual: HD 189733 [Stars] ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,ISM: clouds ,spectroscopic [Techniques] ,0103 physical sciences ,Hot Jupiter ,planet-star interactions ,media_common.cataloged_instance ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,European union ,010303 astronomy & astrophysics ,QC ,Astrophysics::Galaxy Astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,media_common ,coronae ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Horizon (archaeology) ,010308 nuclear & particles physics ,individual: HD189733b [Planets and satellites] ,European research ,stars: individual: HD 189733 ,planets and satellites: individual: HD189733b ,Astronomy ,Astronomy and Astrophysics ,DAS ,Variable (computer science) ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - High Energy Astrophysical Phenomena ,clouds [ISM] ,techniques: spectroscopic ,Astrophysics - Earth and Planetary Astrophysics - Abstract
In this third paper of the MOVES (Multiwavelength Observations of an eVaporating Exoplanet and its Star) programme, we combine Hubble Space Telescope far-ultraviolet observations with XMM-Newton/Swift X-ray observations to measure the emission of HD 189733 in various FUV lines, and its soft X-ray spectrum. Based on these measurements we characterise the interstellar medium toward HD 189733 and derive semi-synthetic XUV spectra of the star, which are used to study the evolution of its high-energy emission at five different epochs. Two flares from HD 189733 are observed, but we propose that the long-term variations in its spectral energy distribution have the most important consequences for the environment of HD 189733b. Reduced coronal and wind activity could favour the formation of a dense population of Si$^{2+}$ atoms in a bow-shock ahead of the planet, responsible for pre- and in-transit absorption measured in the first two epochs. In-transit absorption signatures are detected in the Lyman-$\alpha$ line in the second, third and fifth epochs, which could arise from the extended planetary thermosphere and a tail of stellar wind protons neutralised via charge-exchange with the planetary exosphere. We propose that increases in the X-ray irradiation of the planet, and decreases in its EUV irradiation causing lower photoionisation rates of neutral hydrogen, favour the detection of these signatures by sustaining larger densities of H$^{0}$ atoms in the upper atmosphere and boosting charge-exchanges with the stellar wind. Deeper and broader absorption signatures in the last epoch suggest that the planet entered a different evaporation regime, providing clues as to the link between stellar activity and the structure of the planetary environment., Comment: 22 pages, 21 figures, accepted for publication in MNRAS on 23 January 2020
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- 2020
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12. LRG-BEASTS: Ground-based Detection of Sodium and a Steep Optical Slope in the Atmosphere of the Highly Inflated Hot-Saturn WASP-21b
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Matteo Brogi, Tom Louden, George W. King, C McGruder, I. Skillen, L. Alderson, Gregory W. Henry, James Kirk, Mercedes López-Morales, and Peter J. Wheatley
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Scattering ,Metallicity ,FOS: Physical sciences ,Astronomy and Astrophysics ,Scale height ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Exoplanet ,Atmosphere ,symbols.namesake ,Space and Planetary Science ,Saturn ,William Herschel Telescope ,symbols ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Rayleigh scattering ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the optical transmission spectrum of the highly inflated Saturn-mass exoplanet WASP-21b, using three transits obtained with the ACAM instrument on the William Herschel Telescope through the LRG-BEASTS survey (Low Resolution Ground-Based Exoplanet Atmosphere Survey using Transmission Spectroscopy). Our transmission spectrum covers a wavelength range of 4635-9000 Angstrom, achieving an average transit depth precision of 197ppm compared to one atmospheric scale height at 246ppm. We detect Na I absorption in a bin width of 30 Angstrom, at >4$\sigma$ confidence, which extends over 100 Angstrom. We see no evidence of absorption from K I. Atmospheric retrieval analysis of the scattering slope indicates it is too steep for Rayleigh scattering from H$_2$, but is very similar to that of HD 189733b. The features observed in our transmission spectrum cannot be caused by stellar activity alone, with photometric monitoring of WASP-21 showing it to be an inactive star. We therefore conclude that aerosols in the atmosphere of WASP-21b are giving rise to the steep slope that we observe, and that WASP-21b is an excellent target for infra-red observations to constrain its atmospheric metallicity., Comment: Accepted for publication in MNRAS. 21 pages, 10 tables, 16 figures
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- 2020
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13. A low-mass eclipsing binary within the fully convective zone from the Next Generation Transit Survey
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Alexis M. S. Smith, A. Thompson, Matthew R. Burleigh, Maximilian N. Günther, Maximiliano Moyano, Sarah L. Casewell, Edward Gillen, Peter J. Wheatley, Louise D. Nielsen, Richard G. West, James McCormac, James S. Jenkins, Claudia Belardi, Liam Raynard, Didier Queloz, Tom Louden, M. R. Goad, François Bouchy, Alexander Chaushev, Christopher A. Watson, E. J. W. de Mooij, Daniel Bayliss, Katja Poppenhaeger, Ph. Eigmüller, and James A. G. Jackman
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Physics ,Astrophysics - Solar and Stellar Astrophysics ,010308 nuclear & particles physics ,Space and Planetary Science ,Observatory ,0103 physical sciences ,Library science ,Astronomy and Astrophysics ,Partial support ,010303 astronomy & astrophysics ,01 natural sciences ,Transit (satellite) - Abstract
This publication is based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS instrument and operations are funded by the consortium institutes and by the UK Science and Technology Facilities Council (STFC; project reference ST/M001962/1). The WHT and its service program are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This paper also uses observations made at the South African Astronomical Observatory (SAAO). SLC acknowledges support from LISEO at the University of Leicester. EG acknowledges support from the Winton foundation. MRG and MRB are supported by an STFC consolidated grant (ST/N000757/1). PJW, RGW and TL are supported by an STFC consolidated grant (ST/P000495/1). JSJ acknowledges support by FONDECYT grant 1161218 and partial support by CATA-Basal (PB06, CONICYT). This work utilizes the ELLC exoplanet and binary star model developed by P. F. L. Maxted, and we thank him for his specific recommendations for using this model.
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- 2018
14. ACCESS and LRG-BEASTS: A Precise New Optical Transmission Spectrum of the Ultrahot Jupiter WASP-103b
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Daniel Apai, Ian C. Weaver, Ian Skillen, Mercedes Lopez-Morales, Andrés Jordán, Monika Lendl, Nikole K. Lewis, Tom Louden, Florian Rodler, Ryan J. MacDonald, Benjamin V. Rackham, Chima McGruder, Peter J. Wheatley, Néstor Espinoza, Alex Bixel, David J. Osip, Jamie Wilson, Neale P. Gibson, James Kirk, and Nikolay Nikolov
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Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Jupiter ,Transmission (telecommunications) ,Space and Planetary Science ,Hot Jupiter ,Spectrum (functional analysis) ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present a new ground-based optical transmission spectrum of the ultrahot Jupiter WASP-103b ($T_{eq} = 2484$K). Our transmission spectrum is the result of combining five new transits from the ACCESS survey and two new transits from the LRG-BEASTS survey with a reanalysis of three archival Gemini/GMOS transits and one VLT/FORS2 transit. Our combined 11-transit transmission spectrum covers a wavelength range of 3900--9450A with a median uncertainty in the transit depth of 148 parts-per-million, which is less than one atmospheric scale height of the planet. In our retrieval analysis of WASP-103b's combined optical and infrared transmission spectrum, we find strong evidence for unocculted bright regions ($4.3\sigma$) and weak evidence for H$_2$O ($1.9\sigma$), HCN ($1.7\sigma$), and TiO ($2.1\sigma$), which could be responsible for WASP-103b's observed temperature inversion. Our optical transmission spectrum shows significant structure that is in excellent agreement with the extensively studied ultrahot Jupiter WASP-121b, for which the presence of VO has been inferred. For WASP-103b, we find that VO can only provide a reasonable fit to the data if its abundance is implausibly high and we do not account for stellar activity. Our results highlight the precision that can be achieved by ground-based observations and the impacts that stellar activity from F-type stars can have on the interpretation of exoplanet transmission spectra., Comment: 33 pages, 17 figures, 7 tables. Accepted for publication in AJ
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- 2021
15. NGTS-10b: The shortest period hot Jupiter yet discovered
- Author
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Michael R. Goad, Oliver Turner, Richard G. West, James McCormac, Liam Raynard, Juan Cabrera, Matthew J. Hooton, Christopher A. Watson, Matthew R. Burleigh, François Bouchy, Jose I. Vines, Joshua T. Briegal, Maximiliano Moyano, James S. Jenkins, Boris T. Gänsicke, E. Foxell, Simon Hodgkin, Benjamin F. Cooke, Monika Lendl, David R. Anderson, Alexander Chaushev, Paul Chote, Philipp Eigmüller, Louise D. Nielsen, M. Soto, Tom Louden, Stéphane Udry, David J. Armstrong, Bruno Chazelas, Simon R. Walker, Alexis M. S. Smith, Peter J. Wheatley, James A. G. Jackman, Don Pollacco, Gregory Lambert, Daniel Bayliss, Anders Erikson, Edward Gillen, Sarah L. Casewell, Szilard Csizmadia, Emma Longstaff, Maximilian N. Günther, Heike Rauer, Barry Smalley, David Brown, Didier Queloz, J. Costes, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Hooton, Matthew John [0000-0003-0030-332X], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
- Subjects
Extrasolare Planeten und Atmosphären ,FOS: Physical sciences ,Library science ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,techniques: photometric ,QB460 ,stars: individual: NGTS-10 ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,planetary systems ,010303 astronomy & astrophysics ,QC ,Astrophysics::Galaxy Astrophysics ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,European research ,Leitungsbereich PF ,Astronomy and Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,QB799 ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of a new ultra-short period transiting hot Jupiter from the Next Generation Transit Survey (NGTS). NGTS-10b has a mass and radius of $2.162\,^{+0.092}_{-0.107}$ M$_{\rm J}$ and $1.205\,^{+0.117}_{-0.083}$ R$_{\rm J}$ and orbits its host star with a period of $0.7668944\pm0.0000003$ days, making it the shortest period hot Jupiter yet discovered. The host is a $10.4\pm2.5$ Gyr old K5V star ($T_\mathrm{eff}$=$4400\pm100$\,K) of Solar metallicity ([Fe/H] = $-0.02\pm0.12$\,dex) showing moderate signs of stellar activity. NGTS-10b joins a short list of ultra-short period Jupiters that are prime candidates for the study of star-planet tidal interactions. NGTS-10b orbits its host at just $1.46\pm0.18$ Roche radii, and we calculate a median remaining inspiral time of $38$\,Myr and a potentially measurable transit time shift of $7$\,seconds over the coming decade, assuming a stellar tidal quality factor $Q'_{\rm s}=2\times10^{7}$., 16 pages, 19 figures and 5 tables. Submitted 27 Sept 2019. Accepted 10 Jan 2020. Published 20 Feb 2020
- Published
- 2019
16. LRG-BEASTS: transmission spectroscopy and retrieval analysis of the highly-inflated Saturn-mass planet WASP-39b
- Author
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Ian Skillen, Mercedes Lopez-Morales, Néstor Espinoza, James McCormac, Peter J. Wheatley, Ian C. Weaver, Tom Louden, and James Kirk
- Subjects
Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010504 meteorology & atmospheric sciences ,Metallicity ,FOS: Physical sciences ,Astronomy and Astrophysics ,Scale height ,Astrophysics ,01 natural sciences ,Exoplanet ,Space and Planetary Science ,Planet ,Saturn ,0103 physical sciences ,Orders of magnitude (length) ,William Herschel Telescope ,Transit (astronomy) ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present a ground-based transmission spectrum and comprehensive retrieval analysis of the highly inflated Saturn-mass planet WASP-39b. We obtained low-resolution spectra ($R \approx 400$) of a transit of WASP-39b using the ACAM instrument on the 4.2m William Herschel Telescope as part of the LRG-BEASTS survey. Our transmission spectrum is in good agreement with previous ground- and space-based observations of WASP-39b, and covers a wavelength range of 4000-9000A. Previous analyses of this exoplanet have retrieved water abundances that span more than four orders of magnitude, which in turn lead to conclusions of a subsolar or highly supersolar atmospheric metallicity. In order to determine the cause of the large discrepancies in the literature regarding WASP-39b's atmospheric metallicity, we performed retrieval analyses of all literature data sets. Our retrievals, which assume equilibrium chemistry, recovered highly supersolar metallicities for all data sets. When running our retrievals on a combined spectrum, spanning 0.3-5$\mu$m, we recovered an atmospheric metallicity of $282^{+65}_{-58} \times$ solar. We find that stellar activity has a negligible effect on the derived abundances and instead conclude that different assumptions made during retrieval analyses lead to the reported water abundances that differ by orders of magnitude. This in turn has significant consequences for the conclusions we draw. This is the fourth planet to be observed as part of the LRG-BEASTS survey, which is demonstrating that 4m class telescopes can obtain low-resolution transmission spectra with precisions of around one atmospheric scale height., Comment: Final journal proof version. 21 pages, 9 figures, 6 tables
- Published
- 2019
17. NGTS-7Ab: An ultra-short period brown dwarf transiting a tidally-locked and active M dwarf
- Author
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Philipp Eigmüller, David R. Anderson, Michael R. Goad, J. Costes, Christopher A. Watson, Maximiliano Moyano, Dan Bayliss, I. P. Braker, Maximilian N. Günther, Jose I. Vines, Peter J. Wheatley, Claudia Belardi, Alexis M. S. Smith, Oliver Turner, Anders Erikson, Richard G. West, Stéphane Udry, James McCormac, Liam Raynard, Samuel Gill, Heike Rauer, Simon Hodgkin, Boris T. Gänsicke, Didier Queloz, Alexander Chaushev, Matthew R. Burleigh, James S. Jenkins, Sarah L. Casewell, Juan Cabrera, Edward Gillen, François Bouchy, Katja Poppenhaeger, James A. G. Jackman, Don Pollacco, Tom Louden, Edward M. Bryant, Louise D. Nielsen, Joshua T. Briegal, and Szilard Csizmadia
- Subjects
Extrasolare Planeten und Atmosphären ,Proper motion ,Brown dwarf ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Star (graph theory) ,01 natural sciences ,stars: low-mass ,stars: rotation ,0103 physical sciences ,Phase relation ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,010303 astronomy & astrophysics ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,stars: individual: NGTS-7A ,010308 nuclear & particles physics ,brown dwarfs [stars] ,Leitungsbereich PF ,Astronomy and Astrophysics ,Light curve ,low mass [stars] ,Tidal locking ,Orbit ,individual: NGTS-7A [stars] ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,rotation [stars] ,flare [stars] ,stars: flare ,Astrophysics::Earth and Planetary Astrophysics ,brown dwarfs ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery of NGTS-7Ab, a high mass brown dwarf transiting an M dwarf with a period of 16.2 hours, discovered as part of the Next Generation Transit Survey (NGTS). This is the shortest period transiting brown dwarf around a main or pre-main sequence star to date. The M star host (NGTS-7A) has an age of roughly 55 Myr and is in a state of spin-orbit synchronisation, which we attribute to tidal interaction with the brown dwarf acting to spin up the star. The host star is magnetically active and shows multiple flares across the NGTS and follow up lightcurves, which we use to probe the flare-starspot phase relation. The host star also has an M star companion at a separation of 1.13 arcseconds with very similar proper motion and systemic velocity, suggesting the NGTS-7 system is a hierarchical triple. The combination of tidal synchronisation and magnetic braking is expected to drive ongoing decay of the brown dwarf orbit, with a remaining lifetime of only 5-10 Myr., 21 pages, 16 figures, accepted for publication in the Monthly Notices of the Royal Astronomical Society
- Published
- 2019
18. NGTS-6b: An Ultra Short Period Hot-Jupiter Orbiting an Old K Dwarf
- Author
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Heike Rauer, Samuel Gill, Szilard Csizmadia, Maximiliano Moyano, Philipp Eigmüller, Christopher A. Watson, Sarah L. Casewell, Jose I. Vines, Ruth Titz-Weider, Claudia Belardi, Benjamin F. Cooke, Juan Cabrera, George W. King, Anders Erikson, François Bouchy, Alexis M. S. Smith, Daniel Bayliss, Michael R. Goad, E. Foxell, Edward Gillen, James A. G. Jackman, Don Pollacco, Edward M. Bryant, M. G. Soto, Oliver Turner, Jack S. Acton, Richard G. West, James McCormac, Liam Raynard, Simon R. Walker, Peter J. Wheatley, Louise D. Nielsen, Didier Queloz, Rosanna H. Tilbrook, Stéphane Udry, Alexander Chaushev, Matthew R. Burleigh, James S. Jenkins, Tom Louden, and Joshua T. Briegal
- Subjects
Extrasolare Planeten und Atmosphären ,planets and satellites: detection ,010504 meteorology & atmospheric sciences ,Gas giant ,Population ,FOS: Physical sciences ,01 natural sciences ,Planet ,0103 physical sciences ,Hot Jupiter ,Transit (astronomy) ,education ,planetary systems ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,education.field_of_study ,Leitungsbereich PF ,Astronomy ,Astronomy and Astrophysics ,Planetary system ,Photoevaporation ,Orbit ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of a new ultra-short period hot Jupiter from the Next Generation Transit Survey. NGTS-6b orbits its star with a period of 21.17~h, and has a mass and radius of $1.330^{+0.024}_{-0.028}$\mjup\, and $1.271^{+0.197}_{-0.188}$\rjup\, respectively, returning a planetary bulk density of 0.711$^{+0.214}_{-0.136}$~g~cm$^{-3}$. Conforming to the currently known small population of ultra-short period hot Jupiters, the planet appears to orbit a metal-rich star ([Fe/H]$=+0.11\pm0.09$~dex). Photoevaporation models suggest the planet should have lost 5\% of its gaseous atmosphere over the course of the 9.6~Gyrs of evolution of the system. NGTS-6b adds to the small, but growing list of ultra-short period gas giant planets, and will help us to understand the dominant formation and evolutionary mechanisms that govern this population., 10 pages, 11 figures. Paper accepted for publication in MNRAS
- Published
- 2019
19. Transit Signatures of Inhomogeneous Clouds on Hot Jupiters: Insights From Microphysical Cloud Modeling
- Author
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Peter Gao, Xi Zhang, Vivien Parmentier, Tom Louden, Diana Powell, and Laura Kreidberg
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010504 meteorology & atmospheric sciences ,Cloud cover ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Light curve ,01 natural sciences ,Exoplanet ,symbols.namesake ,Wavelength ,13. Climate action ,Space and Planetary Science ,Planet ,0103 physical sciences ,Spectral slope ,Hot Jupiter ,symbols ,Astrophysics::Earth and Planetary Astrophysics ,Rayleigh scattering ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,0105 earth and related environmental sciences - Abstract
We determine the observability in transmission of inhomogeneous cloud cover on the limbs of hot Jupiters through post processing a general circulation model to include cloud distributions computed using a cloud microphysics model. We find that both the east and west limb often form clouds, but that the different properties of these clouds enhances the limb to limb differences compared to the clear case. Using JWST it should be possible to detect the presence of cloud inhomogeneities by comparing the shape of the transit lightcurve at multiple wavelengths because inhomogeneous clouds impart a characteristic, wavelength dependent signature. This method is statistically robust even with limited wavelength coverage, uncertainty on limb darkening coefficients, and imprecise transit times. We predict that the short wavelength slope varies strongly with temperature. The hot limb of the hottest planets form higher altitude clouds composed of smaller particles leading to a strong rayleigh slope. The near infrared spectral features of clouds are almost always detectable, even when no spectral slope is visible in the optical. In some of our models a spectral window between 5 and 9 microns can be used to probe through the clouds and detect chemical spectral features. Our cloud particle size distributions are not log-normal and differ from species to species. Using the area or mass weighted particle size significantly alters the relative strength of the cloud spectral features compared to using the predicted size distribution. Finally, the cloud content of a given planet is sensitive to a species' desorption energy and contact angle, two parameters that could be constrained experimentally in the future., Comment: 21 pages, 17 figures, submitted to ApJ, revised following comments from referee
- Published
- 2019
- Full Text
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20. K2-265 b: a transiting rocky super-Earth
- Author
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T. Lopez, E. Foxell, Nuno C. Santos, David Barrado, Xavier Dumusque, Jorge Lillo-Box, Louise D. Nielsen, Tom Louden, François Bouchy, S. G. Sousa, James A. G. Jackman, Arthur Vigan, Don Pollacco, H. P. Osborn, James Kirk, George W. King, David R. Ciardi, Olivier Demangeon, Peter J. Wheatley, C. Lovis, S. C. C. Barros, R. Ligi, K. W. F. Lam, David J. Armstrong, Magali Deleuil, O. Mousis, V. Adibekyan, B. Brugger, Duncan A. Brown, E. Delgado Mena, Francesca Faedi, Jose-Manuel Almenara, Daniel Bayliss, James McCormac, Stéphane Udry, Alexandre Santerne, Aldo S. Bonomo, University of Warwick [Coventry], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidade do Porto = University of Porto, Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Centro de Astrofísica da Universidade do Porto (CAUP), Instituto de Astrofisica de Canarias (IAC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), Université Paris-Sud - Paris 11 (UP11), INAF - Osservatorio Astrofisico di Catania (OACT), School of Physics and Astronomy [Cardiff], Cardiff University, European Southern Observatory (ESO), Universidade do Porto, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Université de Genève (UNIGE)
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Super-Earth ,010504 meteorology & atmospheric sciences ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Planetary core ,FOS: Physical sciences ,Astronomy and Astrophysics ,Radius ,Astrophysics ,Orbital period ,01 natural sciences ,Photoevaporation ,Radial velocity ,Photometry (astronomy) ,13. Climate action ,Space and Planetary Science ,Planet ,[SDU]Sciences of the Universe [physics] ,0103 physical sciences ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of the super-Earth K2-265 b detected with K2 photometry. The planet orbits a bright (V_mag = 11.1) star of spectral type G8V with a period of 2.37 days. We obtained high-precision follow-up radial velocity measurements from HARPS, and the joint Bayesian analysis showed that K2-265 b has a radius of 1.71 +/- 0.11 R_earth and a mass of 6.54 +/- 0.84 M_earth, corresponding to a bulk density of 7.1 +/- 1.8 g/cm^3 . Composition analysis of the planet reveals an Earth-like, rocky interior, with a rock mass fraction of 80%. The short orbital period and small radius of the planet puts it below the lower limit of the photoevaporation gap, where the envelope of the planet could have eroded due to strong stellar irradiation, leaving behind an exposed core. Knowledge of the planet core composition allows us to infer the possible formation and evolution mechanism responsible for its current physical parameters., 14 pages, 9 figures, Accepted for publication in A&A
- Published
- 2018
21. Strong XUV irradiation of the Earth-sized exoplanets orbiting the ultracool dwarf TRAPPIST-1
- Author
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Tom Louden, David Ehrenreich, Vincent Bourrier, Michaël Gillon, and Peter J. Wheatley
- Subjects
Dwarf star ,010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Luminosity ,Primary (astronomy) ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Irradiation ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,QB ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Astronomy ,Astronomy and Astrophysics ,Exoplanet ,Space and Planetary Science ,Extreme ultraviolet ,Astrophysics::Earth and Planetary Astrophysics ,Circumstellar habitable zone ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present an XMM-Newton X-ray observation of TRAPPIST-1, which is an ultracool dwarf star recently discovered to host three transiting and temperate Earth-sized planets. We find the star is a relatively strong and variable coronal X-ray source with an X-ray luminosity similar to that of the quiet Sun, despite its much lower bolometric luminosity. We find L_x/L_bol=2-4x10^-4, with the total XUV emission in the range L_xuv/L_bol=6-9x10^-4, and XUV irradiation of the planets that is many times stronger than experienced by the present-day Earth. Using a simple energy-limited model we show that the relatively close-in Earth-sized planets, which span the classical habitable zone of the star, are subject to sufficient X-ray and EUV irradiation to significantly alter their primary and any secondary atmospheres. Understanding whether this high-energy irradiation makes the planets more or less habitable is a complex question, but our measured fluxes will be an important input to the necessary models of atmospheric evolution., 5 pages, published as a letter in MNRAS (accepted 16 September 2016)
- Published
- 2016
22. Single transit candidates from K2: detection and period estimation
- Author
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Susan Walker, Jessica Spake, Francesca Faedi, Amanda P. Doyle, James McCormac, James Kirk, D. J. A. Brown, Don Pollacco, David J. Armstrong, K. W. F. Lam, Tom Louden, and Hugh P. Osborn
- Subjects
Physics ,010308 nuclear & particles physics ,media_common.quotation_subject ,Binary number ,Astronomy ,Astronomy and Astrophysics ,Astrophysics ,Planetary system ,01 natural sciences ,Kepler ,Exoplanet ,Stars ,Space and Planetary Science ,Planet ,0103 physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Transit (astronomy) ,Eccentricity (behavior) ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,QB ,media_common - Abstract
Photometric surveys such as Kepler have the precision to identify exoplanet and eclipsing binary candidates from only a single transit. K2, with its 75d campaign duration, is ideally suited to detect significant numbers of single-eclipsing objects. Here we develop a Bayesian transit-fitting tool ("Namaste: An Mcmc Analysis of Single Transit Exoplanets") to extract orbital information from single transit events. We achieve favourable results testing this technique on known Kepler planets, and apply the technique to 7 candidates identified from a targeted search of K2 campaigns 1, 2 and 3. We find EPIC203311200 to host an excellent exoplanet candidate with a period, assuming zero eccentricity, of $540 ^{+410}_{-230}$ days and a radius of $0.51 \pm 0.05 R_{Jup}$. We also find six further transit candidates for which more follow-up is required to determine a planetary origin. Such a technique could be used in the future with TESS, PLATO and ground-based photometric surveys such as NGTS, potentially allowing the detection of planets in reach of confirmation by Gaia., Comment: Submitted to MNRAS on 25th November 2015. 15 Pages
- Published
- 2016
23. Author Correction: An ultrahot Neptune in the Neptune desert
- Author
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Benjamin F. Cooke, Matias Diaz, Alexander Chaushev, Matthew R. Burleigh, Enric Palle, Michael R. Goad, James A. G. Jackman, Don Pollacco, Edward M. Bryant, James S. Jenkins, Andrew W. Mann, Giovanni Isopi, Jack J. Lissauer, Jack S. Acton, Samuel Gill, Christopher A. Watson, Todd C. Klaus, Rosanna H. Tilbrook, Christopher E. Henze, Philipp Eigmüller, Daniel Bayliss, David R. Ciardi, Norio Narita, Maximiliano Moyano, Cristobal Petrovich, Matthew J. Hooton, Didier Queloz, Stéphane Udry, Jessie L. Christiansen, Jose I. Vines, Andrés Jordán, Eric D. Lopez, M. G. Soto, Charles Beichman, Alexis M. S. Smith, Roland Vanderspek, Ruth Titz-Weider, Simon R. Walker, Jerome de Leon, K. I. Collins, Peter J. Wheatley, David W. Latham, Motohide Tamura, Michael Vezie, George R. Ricker, David J. Armstrong, Samuel N. Quinn, Rafael Brahm, Louise D. Nielsen, Oliver Turner, Sarah L. Casewell, Mayuko Mori, Carl Ziegler, Richard G. West, James McCormac, Anders Erikson, Néstor Espinoza, E. Foxell, Claudia Belardi, Juan Cabrera, George W. King, Liam Raynard, J. Villasenor, Tom Louden, Joshua N. Winn, Pablo Rojas, Edward Gillen, François Bouchy, Andrea Ercolino, Boris T. Gänsicke, Christopher J. Burke, Allyson Bieryla, Karen A. Collins, Heike Rauer, F. Mallia, Nicolás T. Kurtovic, Sara Seager, Sean McCauliff, Maximilian N. Günther, Jon M. Jenkins, Pía Cortés-Zuleta, Taku Nishiumi, Nicholas M. Law, and Pascal Torres
- Subjects
Desert (philosophy) ,Neptune ,Astronomy and Astrophysics ,Geology ,Astrobiology - Published
- 2020
24. NGTS-4b: A sub-Neptune Transiting in the Desert
- Author
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Michaël Gillon, Anders Erikson, Benjamin F. Cooke, Alexis M. S. Smith, Sandrine Sohy, Y. Almleaky, Paul Chote, George W. King, Michael R. Goad, Christopher A. Watson, Szilard Csizmadia, Daniel Bayliss, Edward Gillen, Philipp Eigmüller, Juan Cabrera, Matthew R. Burleigh, Artem Burdanov, Simon R. Walker, François Bouchy, Oliver Turner, Richard G. West, James McCormac, Emma Longstaff, Laetitia Delrez, James S. Jenkins, Boris T. Gänsicke, Claudia Belardi, Simon Hodgkin, Peter J. Wheatley, M. Soto, Maximilian N. Günther, Liam Raynard, M. Moyano, Alexander Chaushev, Stéphane Udry, Didier Queloz, David J. Armstrong, E. Foxell, Heike Rauer, Samantha Thompson, Sarah L. Casewell, Bruno Chazelas, Joshua T. Briegal, Louise D. Nielsen, C. Murray, Elsa Ducrot, Emmanuel Jehin, Tom Louden, James A. G. Jackman, Don Pollacco, Gregory Lambert, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
- Subjects
Extrasolare Planeten und Atmosphären ,planets and satellites: detection ,detection [planets and satellites] ,FOS: Physical sciences ,01 natural sciences ,photometric [techniques] ,techniques: photometric ,photometric ,stars: individual: NGTS-4- planetary systems ,satellites ,planets ,Neptune ,Planet ,stars: individual: NGTS-4 planetary systems ,0103 physical sciences ,Transit (astronomy) ,010303 astronomy & astrophysics ,planetary systems ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,Leitungsbereich PF ,Desert (particle physics) ,Astronomy ,Astronomy and Astrophysics ,NGTS-4 ,Radius ,Planetary system ,Orbit ,individual: NGTS-4- planetary systems [stars] ,13. Climate action ,Space and Planetary Science ,Magnitude (astronomy) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of NGTS-4b, a sub-Neptune-sized planet transiting a 13th magnitude K-dwarf in a 1.34d orbit. NGTS-4b has a mass M=$20.6\pm3.0$M_E and radius R=$3.18\pm0.26$R_E, which places it well within the so-called "Neptunian Desert". The mean density of the planet ($3.45\pm0.95$g/cm^3) is consistent with a composition of 100% H$_2$O or a rocky core with a volatile envelope. NGTS-4b is likely to suffer significant mass loss due to relatively strong EUV/X-ray irradiation. Its survival in the Neptunian desert may be due to an unusually high core mass, or it may have avoided the most intense X-ray irradiation by migrating after the initial activity of its host star had subsided. With a transit depth of $0.13\pm0.02$%, NGTS-4b represents the shallowest transiting system ever discovered from the ground, and is the smallest planet discovered in a wide-field ground-based photometric survey., Submitted to MNRAS
- Published
- 2018
25. Unmasking the hidden NGTS-3Ab: a hot Jupiter in an unresolved binary system
- Author
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Maximilian N. Günther, Katja Poppenhaeger, Maximiliano Moyano, Philipp Eigmüller, Y. Almleaky, Laetitia Delrez, Matthew R. Burleigh, Michaël Gillon, Michael R. Goad, Anders Erikson, Didier Queloz, Samantha Thompson, James S. Jenkins, Sarah L. Casewell, David J. Armstrong, Richard G. West, James McCormac, Juan Cabrera, Don Pollacco, Boris T. Gänsicke, Liam Raynard, Neale P. Gibson, Christopher A. Watson, Heike Rauer, Daniel Bayliss, Artem Burdanov, Alexis M. S. Smith, Barry Smalley, Stéphane Udry, Emmanuel Jehin, Sandrine Sohy, Peter J. Wheatley, Tom Louden, François Bouchy, Szilard Csizmadia, Benjamin F. Cooke, Edward Gillen, C. Murray, Elsa Ducrot, Queloz, Didier [0000-0002-3012-0316], Gillen, Edward [0000-0003-2851-3070], and Apollo - University of Cambridge Repository
- Subjects
•surveys ,Eclipses ,Binary number ,FOS: Physical sciences ,Astrophysics ,Joint analysis ,Surveys ,01 natural sciences ,Photometry (optics) ,•eclipses ,•planets and satellites: detection ,0103 physical sciences ,Hot Jupiter ,QB460 ,Binary system ,010303 astronomy & astrophysics ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,•binaries: eclipsing ,•occultations ,010308 nuclear & particles physics ,eclipsing [Binaries] ,Centroid ,•Astrophysics - Earth and Planetary Astrophysics ,Astronomy and Astrophysics ,Radial velocity ,detection [Planets and satellites] ,Space and Planetary Science ,astro-ph.EP ,Occultations ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery of NGTS-3Ab, a hot Jupiter found transiting the primary star of an unresolved binary system. We develop a joint analysis of multi-colour photometry, centroids, radial velocity (RV) cross-correlation function (CCF) profiles and their bisector inverse slopes (BIS) to disentangle this three-body system. Data from the Next Generation Transit Survey (NGTS), SPECULOOS and HARPS are analysed and modelled with our new blendfitter software. We find that the binary consists of NGTS-3A (G6V-dwarf) and NGTS-3B (K1V-dwarf) at 5 arcsec) and are prone to contamination by blended objects. With TESS on the horizon, it is pivotal for the candidate vetting to incorporate all available follow-up information from multi-colour photometry and RV CCF profiles., Accepted for publication in MNRAS 2 May 2018. 20 pages, 11 figures, 9 tables. This is the authors' version of the manuscript
- Published
- 2018
26. NGTS-2b: An inflated hot-Jupiter transiting a bright F-dwarf
- Author
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Katja Poppenhaeger, Don Pollacco, Lionel Metrailler, Maximiliano Moyano, Matthew R. Burleigh, Richard Alexander, Bruno Chazelas, Benjamin F. Cooke, Alexander Chaushev, James S. Jenkins, Daniel Bayliss, Michael R. Goad, Didier Queloz, Philipp Eigmüller, Heike Rauer, Szilard Csizmadia, Simon Hodgkin, Anders Erikson, Grégory L'Ambert, Edward Gillen, Oliver Turner, Richard G. West, James McCormac, Liam Raynard, Barry Smalley, Joshua T. Briegal, Matthew J. Hooton, Simon R. Walker, Stéphane Udry, Andrew Grange, Maximilian N. Günther, Peter J. Wheatley, Alexis M. S. Smith, Boris T. Gänsicke, A. Thompson, Christopher A. Watson, Louise D. Nielsen, Roberto Raddi, Sarah L. Casewell, M. Soto, Tom Louden, A. M. Read, Juan Cabrera, François Bouchy, David J. Armstrong, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Hooton, Matthew John [0000-0003-0030-332X], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,planets and satellites: detection ,detection [planets and satellites] ,Giant planet ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,01 natural sciences ,Exoplanet ,Photometry (optics) ,Transmission spectroscopy ,fundamental parameters [planets and satellites] ,Space and Planetary Science ,Planet ,planets and satellites: detection – planets and satellites: fundamental parameters ,0103 physical sciences ,Hot Jupiter ,QB460 ,010306 general physics ,planets and satellites: fundamental parameters ,010303 astronomy & astrophysics ,Rapid rotation ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of NGTS-2b, an inflated hot-Jupiter transiting a bright F5V star (2MASS J14202949-3112074; $T_{\rm eff}$=$6478^{+94}_{-89}$ K), discovered as part of the Next Generation Transit Survey (NGTS). The planet is in a P=4.51 day orbit with mass $0.74^{+0.13}_{-0.12}$ M$_{J}$, radius $1.595^{+0.047}_{-0.045}$ R$_{J}$ and density $0.226^{+0.040}_{-0.038}$ g cm$^{-3}$; therefore one of the lowest density exoplanets currently known. With a relatively deep 1.0% transit around a bright V=10.96 host star, NGTS-2b is a prime target for probing giant planet composition via atmospheric transmission spectroscopy. The rapid rotation ($vsin$i=$15.2\pm0.8$ km s$^{-1}$) also makes this system an excellent candidate for Rossiter-McLaughlin follow-up observations, to measure the sky-projected stellar obliquity. NGTS-2b was confirmed without the need for follow-up photometry, due to the high precision of the NGTS photometry., 12 pages, 8 figures, accepted for publication in MNRAS
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- 2018
27. An Earth-sized exoplanet with a Mercury-like composition
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R. Ligi, H. Giles, M. J. Hobson, Olivier Demangeon, James Kirk, Artyom Aguichine, Francesco Pepe, Amanda P. Doyle, V. Adibekyan, E. Delgado Mena, Daniel Bayliss, Francesca Faedi, James McCormac, Nuno C. Santos, K. W. F. Lam, David Barrado, Guillaume Hébrard, Alexandre Santerne, George W. King, Aldo S. Bonomo, Hugh P. Osborn, E. Foxell, Jorge Lillo-Box, Arthur Vigan, H. Gosselin, Rodrigo F. Díaz, Stéphane Udry, François Bouchy, Xavier Dumusque, J. J. Neal, João P. Faria, Tom Louden, S. G. Sousa, S. Hojjatpanah, B. Brugger, Duncan A. Brown, C. Lovis, Magali Deleuil, Jose-Manuel Almenara, Isabelle Boisse, S. C. C. Barros, Pedro Figueira, David J. Armstrong, James A. G. Jackman, Don Pollacco, Olivier Mousis, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
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Earth and Planetary Astrophysics (astro-ph.EP) ,Solar System ,010504 meteorology & atmospheric sciences ,[PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,FOS: Physical sciences ,Astronomy and Astrophysics ,Planetary system ,Protoplanetary disk ,01 natural sciences ,Mantle (geology) ,Silicate ,Exoplanet ,Astrobiology ,Physics::Geophysics ,chemistry.chemical_compound ,chemistry ,13. Climate action ,Planet ,0103 physical sciences ,Physics::Space Physics ,Terrestrial planet ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The Earth, Venus, Mars, and some extrasolar terrestrial planets have a mass and radius that is consistent with a mass fraction of about 30% metallic core and 70% silicate mantle. At the inner frontier of the solar system, Mercury has a completely different composition, with a mass fraction of about 70% metallic core and 30% silicate mantle. Several formation or evolution scenarios are proposed to explain this metal-rich composition, such as a giant impact, mantle evaporation, or the depletion of silicate at the inner-edge of the proto-planetary disk. These scenarios are still strongly debated. Here we report the discovery of a multiple transiting planetary system (K2-229), in which the inner planet has a radius of 1.165+/-0.066 Rearth and a mass of 2.59+/-0.43 Mearth. This Earth-sized planet thus has a core-mass fraction that is compatible with that of Mercury, while it was expected to be similar to that of the Earth based on host-star chemistry. This larger Mercury analogue either formed with a very peculiar composition or it has evolved since, e.g. by losing part of its mantle. Further characterisation of Mercury-like exoplanets like K2-229 b will help putting the detailed in-situ observations of Mercury (with Messenger and BepiColombo) into the global context of the formation and evolution of solar and extrasolar terrestrial planets., Accepted preprint in Nature Astronomy. Publisher-edited version available at http://rdcu.be/JRE7 Supplement materials available at https://www.nature.com/articles/s41550-018-0420-5
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- 2018
28. Automatic vetting of planet candidates from ground based surveys: Machine learning with NGTS
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Maximilian N. Günther, Christopher A. Watson, Lionel Metrailler, Matthew R. Burleigh, Alexis M. S. Smith, James S. Jenkins, Don Pollacco, Sarah L. Casewell, Didier Queloz, Michael R. Goad, Stéphane Udry, Katja Poppenhaeger, Edward Gillen, Heike Rauer, Simon R. Walker, Tom Louden, Simon Hodgkin, Peter J. Wheatley, Daniel Bayliss, Philipp Eigmüller, Richard G. West, James McCormac, Liam Raynard, David J. Armstrong, and François Bouchy
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detection [planets and satellites] ,statistical [methods] ,FOS: Physical sciences ,Machine learning ,computer.software_genre ,01 natural sciences ,QA76 ,Vetting ,Robustness (computer science) ,Planet ,0103 physical sciences ,False positive paradox ,data analysis [methods] ,general [planets and satellites] ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,business.industry ,Astronomy and Astrophysics ,Planetary system ,Exoplanet ,Random forest ,exoplanets ,Space and Planetary Science ,Survey data collection ,Artificial intelligence ,business ,Astrophysics - Instrumentation and Methods for Astrophysics ,computer ,Astrophysics - Earth and Planetary Astrophysics - Abstract
State of the art exoplanet transit surveys are producing ever increasing quantities of data. To make the best use of this resource, in detecting interesting planetary systems or in determining accurate planetary population statistics, requires new automated methods. Here we describe a machine learning algorithm that forms an integral part of the pipeline for the NGTS transit survey, demonstrating the efficacy of machine learning in selecting planetary candidates from multi-night ground based survey data. Our method uses a combination of random forests and self-organising-maps to rank planetary candidates, achieving an AUC score of 97.6\% in ranking 12368 injected planets against 27496 false positives in the NGTS data. We build on past examples by using injected transit signals to form a training set, a necessary development for applying similar methods to upcoming surveys. We also make the \texttt{autovet} code used to implement the algorithm publicly accessible. \texttt{autovet} is designed to perform machine learned vetting of planetary candidates, and can utilise a variety of methods. The apparent robustness of machine learning techniques, whether on space-based or the qualitatively different ground-based data, highlights their importance to future surveys such as TESS and PLATO and the need to better understand their advantages and pitfalls in an exoplanetary context., Accepted for publication in MNRAS, 15 pages
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- 2018
29. The Next Generation Transit Survey (NGTS)
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Hugh P. Osborn, Louise D. Nielsen, Heike Rauer, Stéphane Udry, Christopher A. Watson, Francesca Faedi, Matthew R. Burleigh, Maximilian N. Günther, Richard G. West, James McCormac, Liam Raynard, Lionel Metrailler, Ruth Titz-Weider, Maximiliano Moyano, James S. Jenkins, Andrés Jordán, Sarah L. Casewell, Katja Poppenhaeger, David J. Armstrong, Roberto Raddi, Anders Erikson, Edward Gillen, M. Soto, James A. G. Jackman, Don Pollacco, Bruno Chazelas, Paul Chote, Simon Hodgkin, Gregory Lambert, Andrew Grange, Daniel Bayliss, Boris T. Gänsicke, Szilard Csizmadia, Joao Bento, Michael R. Goad, L. Genolet, E. Foxell, Alexis M. S. Smith, Tom Louden, Simon R. Walker, Peter J. Wheatley, Didier Queloz, Juan Cabrera, François Bouchy, Philipp Eigmüller, Alexander Chaushev, Queloz, Didier [0000-0002-3012-0316], Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], and Apollo - University of Cambridge Repository
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planets and satellites: detection ,FOS: Physical sciences ,Field of view ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,7. Clean energy ,techniques: photometric ,surveys ,Observatory ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,planetary systems ,Astrophysics::Galaxy Astrophysics ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,First light ,Planetary system ,Exoplanet ,Stars ,instrumentation: photometers ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,atmospheric effects ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We describe the Next Generation Transit Survey (NGTS), which is a ground-based project searching for transiting exoplanets orbiting bright stars. NGTS builds on the legacy of previous surveys, most notably WASP, and is designed to achieve higher photometric precision and hence find smaller planets than have previously been detected from the ground. It also operates in red light, maximising sensitivity to late K and early M dwarf stars. The survey specifications call for photometric precision of 0.1 per cent in red light over an instantaneous field of view of 100 square degrees, enabling the detection of Neptune-sized exoplanets around Sun-like stars and super-Earths around M dwarfs. The survey is carried out with a purpose-built facility at Cerro Paranal, Chile, which is the premier site of the European Southern Observatory (ESO). An array of twelve 20cm f/2.8 telescopes fitted with back-illuminated deep-depletion CCD cameras are used to survey fields intensively at intermediate Galactic latitudes. The instrument is also ideally suited to ground-based photometric follow-up of exoplanet candidates from space telescopes such as TESS, Gaia and PLATO. We present observations that combine precise autoguiding and the superb observing conditions at Paranal to provide routine photometric precision of 0.1 per cent in 1 hour for stars with I-band magnitudes brighter than 13. We describe the instrument and data analysis methods as well as the status of the survey, which achieved first light in 2015 and began full survey operations in 2016. NGTS data will be made publicly available through the ESO archive., 20 pages, 17 Figures, Accepted for publication in MNRAS
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- 2018
30. LRG-BEASTS III : ground-based transmission spectrum of the gas giant orbiting the cool dwarf WASP-80
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James Kirk, James McCormac, Peter J. Wheatley, George W. King, I. Skillen, Patrick G. J. Irwin, and Tom Louden
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Gas giant ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Spectral line ,Atmosphere ,Planet ,0103 physical sciences ,Hot Jupiter ,William Herschel Telescope ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Exoplanet ,Grism ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We have performed ground-based transmission spectroscopy of the hot Jupiter orbiting the cool dwarf WASP-80 using the ACAM instrument on the William Herschel Telescope (WHT) as part of the LRG-BEASTS programme. This is the third paper of a ground-based transmission spectroscopy survey of hot Jupiters using low-resolution grism spectrographs. We observed two transits of the planet and have constructed transmission spectra spanning a wavelength range of 4640-8840A. Our transmission spectrum is inconsistent with a previously claimed detection of potassium in WASP-80b's atmosphere, and is instead most consistent with a haze. We also do not see evidence for sodium absorption at a resolution of 100A., Comment: 11 pages, 9 figures. Accepted for publication in MNRAS
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- 2018
31. An ultra-short period rocky super-Earth with a secondary eclipse and a Neptune-like companion around K2-141
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Annelies Mortier, Mark E. Everett, John Asher Johnson, Giampaolo Piotto, Mercedes Lopez-Morales, Andrew Vanderburg, Pedro Figueira, Luca Malavolta, Andrew Collier Cameron, Laura Kreidberg, Michel Mayor, David F. Phillips, A. Coffinet, Courtney D. Dressing, Valerio Nascimbeni, Martti H. Kristiansen, Mario Damasso, Christopher A. Watson, Xavier Dumusque, Aldo F. M. Fiorenzano, David Ehrenreich, Vinesh M. Rajpaul, Tom Louden, Eric D. Lopez, David Charbonneau, F. Bouchy, David W. Latham, Raphaëlle D. Haywood, Lars A. Buchhave, Damien Ségransan, Erica J. Gonzales, Andrew W. Mayo, Steve B. Howell, Stéphane Udry, Lea A. Hirsch, Francesco Pepe, Alessandro Sozzetti, Ken Rice, Avet Harutyunyan, Rosario Cosentino, Aldo S. Bonomo, David R. Ciardi, Emilio Molinari, Dimitar Sasselov, Christophe Lovis, Giuseppina Micela, Ian J. M. Crossfield, Science & Technology Facilities Council, European Commission, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
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astro-ph.SR ,interiors [planets and satellites] ,010504 meteorology & atmospheric sciences ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,individual (K2-141b, K2-141c) [Planets and satellites] ,photometric [techniques] ,Atmosphere ,techniques: photometric ,individual (K2-141) [Stars] ,Geometric albedo ,Neptune ,Planet ,techniques: radial velocities ,0103 physical sciences ,QB Astronomy ,Transit (astronomy) ,composition [planets and satellites] ,individual: K2-141 [stars] ,planetary systems ,010303 astronomy & astrophysics ,QC ,Solar and Stellar Astrophysics (astro-ph.SR) ,QB ,0105 earth and related environmental sciences ,planets and satellites: composition ,planets and satellites: individual (K2-141b, K2-141c) ,planets and satellites: interiors ,stars: individual (K2-141) ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,K2-141c) ,Super-Earth ,radial velocities [techniques] ,Astronomy and Astrophysics ,3rd-DAS ,Planetary system ,Light curve ,individual: K2-141b [planets and satellites] ,QC Physics ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,astro-ph.EP ,K2-141c ,Astrophysics::Earth and Planetary Astrophysics ,planets and satellites: individual (K2-141b ,Astrophysics - Earth and Planetary Astrophysics - 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, 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 an 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 $1.51\pm0.05~R_\oplus$ and a mass of $5.08\pm0.41~M_\oplus$, 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 dataset, 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 $0.30 \pm 0.06$ in the Kepler bandpass, or by thermal emission from the surface of the planet at $\sim$3000K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios., Comment: 16 pages, 10 figures., accepted for publication in AJ
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- 2018
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32. Global Climate and Atmospheric Composition of the Ultra-hot Jupiter WASP-103b from HST and Spitzer Phase Curve Observations
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Keivan G. Stassun, Kevin B. Stevenson, Jacob Arcangeli, Mickael Bonnefoy, Gregory W. Henry, Michael R. Line, Tom Louden, Jacqueline K. Faherty, Michael H. Williamson, Jean-Michel Desert, Jacob L. Bean, Adam P. Showman, Vivien Parmentier, Jonathan J. Fortney, Laura Kreidberg, Thomas G. Beatty, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), 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]), and Low Energy Astrophysics (API, FNWI)
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Brightness ,010504 meteorology & atmospheric sciences ,Gas giant ,Brown dwarf ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,0103 physical sciences ,Hot Jupiter ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,planets and satellites: atmospheres ,planets and satellites: individual: WASP-103b ,Astronomy and Astrophysics ,Phase curve ,Surface gravity ,Exoplanet ,planets and satellites: gaseous planets ,13. Climate action ,Space and Planetary Science ,[SDU]Sciences of the Universe [physics] ,Brightness temperature ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present thermal phase curve measurements for the hot Jupiter WASP-103b observed with Hubble/WFC3 and Spitzer/IRAC. The phase curves have large amplitudes and negligible hotspot offsets, indicative of poor heat redistribution to the nightside. We fit the phase variation with a range of climate maps and find that a spherical harmonics model generally provides the best fit. The phase-resolved spectra are consistent with blackbodies in the WFC3 bandpass, with brightness temperatures ranging from $1880\pm40$ K on the nightside to $2930 \pm 40$ K on the dayside. The dayside spectrum has a significantly higher brightness temperature in the Spitzer bands, likely due to CO emission and a thermal inversion. The inversion is not present on the nightside. We retrieved the atmospheric composition and found the composition is moderately metal-enriched ($\mathrm{[M/H]} = 23^{+29}_{-13}\times$ solar) and the carbon-to-oxygen ratio is below 0.9 at $3\,\sigma$ confidence. In contrast to cooler hot Jupiters, we do not detect spectral features from water, which we attribute to partial H$_2$O dissociation. We compare the phase curves to 3D general circulation models and find magnetic drag effects are needed to match the data. We also compare the WASP-103b spectra to brown dwarfs and young directly imaged companions and find these objects have significantly larger water features, indicating that surface gravity and irradiation environment play an important role in shaping the spectra of hot Jupiters. These results highlight the 3D structure of exoplanet atmospheres and illustrate the importance of phase curve observations for understanding their complex chemistry and physics., Comment: 25 pages, 17 figures, 7 tables; accepted to AJ
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- 2018
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33. The Transiting Exoplanet Community Early Release Science Program for JWST
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Jacob L. Bean, Kevin B. Stevenson, Natalie M. Batalha, Zachory Berta-Thompson, Laura Kreidberg, Nicolas Crouzet, Björn Benneke, Michael R. Line, David K. Sing, Hannah R. Wakeford, Heather A. Knutson, Eliza M.-R. Kempton, Jean-Michel Désert, Ian Crossfield, Natasha E. Batalha, Julien de Wit, Vivien Parmentier, Joseph Harrington, Julianne I. Moses, Mercedes Lopez-Morales, Munazza K. Alam, Jasmina Blecic, Giovanni Bruno, Aarynn L. Carter, John W. Chapman, Leen Decin, Diana Dragomir, Thomas M. Evans, Jonathan J. Fortney, Jonathan D. Fraine, Peter Gao, Antonio García Muñoz, Neale P. Gibson, Jayesh M. Goyal, Kevin Heng, Renyu Hu, Sarah Kendrew, Brian M. Kilpatrick, Jessica Krick, Pierre-Olivier Lagage, Monika Lendl, Tom Louden, Nikku Madhusudhan, Avi M. Mandell, Megan Mansfield, Erin M. May, Giuseppe Morello, Caroline V. Morley, Nikolay Nikolov, Seth Redfield, Jessica E. Roberts, Everett Schlawin, Jessica J. Spake, Kamen O. Todorov, Angelos Tsiaras, Olivia Venot, William C. Waalkes, Peter J. Wheatley, Robert T. Zellem, Daniel Angerhausen, David Barrado, Ludmila Carone, Sarah L. Casewell, Patricio E. Cubillos, Mario Damiano, Miguel de Val-Borro, Benjamin Drummond, Billy Edwards, Michael Endl, Nestor Espinoza, Kevin France, John E. Gizis, Thomas P. Greene, Thomas K. Henning, Yucian Hong, James G. Ingalls, Nicolas Iro, Patrick G. J. Irwin, Tiffany Kataria, Fred Lahuis, Jérémy Leconte, Jorge Lillo-Box, Stefan Lines, Joshua D. Lothringer, Luigi Mancini, Franck Marchis, Nathan Mayne, Enric Palle, Emily Rauscher, Gaël Roudier, Evgenya L. Shkolnik, John Southworth, Mark R. Swain, Jake Taylor, Johanna Teske, Giovanna Tinetti, Pascal Tremblin, Gregory S. Tucker, Roy van Boekel, Ingo P. Waldmann, Ian C. Weaver, Tiziano Zingales, University of Chicago, Space Telescope Science Institute (STSci), NASA Ames Research Center (ARC), Department of Astrophysical and Planetary Sciences [Boulder], University of Colorado [Boulder], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Instituto de Astrofisica de Canarias (IAC), Universidad de La Laguna [Tenerife - SP] (ULL), Département de Physique [Montréal], Université de Montréal [Montréal], School of Earth and Space Exploration [Tempe] (SESE), Arizona State University [Tempe] (ASU), University of Exeter, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Grinnell College, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Central Florida [Orlando], Space Science Institute [Boulder] (SSI), New York University [Abu Dhabi], NYU System (NYU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institute of Astronomy [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), University of California [Santa Cruz] (UCSC), University of California, Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Zentrum für Astronomie und Astrophysik [Berlin] (ZAA), Technische Universität Berlin (TUB), Astrophysics Research Centre [Belfast] (ARC), Queen's University [Belfast] (QUB), Center for Space and Habitability (CSH), University of Bern, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Brown University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Austrian Academy of Sciences (OeAW), University of Warwick [Coventry], Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), GSFC Solar System Exploration Division, NASA Goddard Space Flight Center (GSFC), University of Michigan [Ann Arbor], University of Michigan System, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, The Foundation for Scientific and Industrial Research (SINTEF), College of Engineering, Mathematics and Physical Sciences [Exeter] (EMPS), Wesleyan University, Amsterdam University of Applied Sciences, Department of Physics and Astronomy [UCL London], University College of London [London] (UCL), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Blue Marble Space Institute of Science (BMSIS), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Department of Physics and Astronomy [Leicester], University of Leicester, Space Research Institute of Austrian Academy of Sciences (IWF), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Astrochemistry Laboratory [Greenbelt], Catholic University of America, McDonald Observatory, University of Texas at Austin [Austin], Center for Astrophysics and Space Astronomy [Boulder] (CASA), Department of Physics and Astronomy [Newark], University of Delaware [Newark], Cornell University, Infrared Processing and Analysis Center (IPAC), University of Vienna [Vienna], Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], SRON Netherlands Institute for Space Research (SRON), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Carl Sagan Center, SETI Institute, Department of Physics, University of Rome Tor Vergata, Maison de la Simulation (MDLS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Paris-Sud - Paris 11 (UP11)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Ames Laboratory [Ames, USA], Iowa State University (ISU)-U.S. Department of Energy (DOE), Low Energy Astrophysics (API, FNWI), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides ( CASSIOPEE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Plasmachemistry, CNR-IMIP, Katholieke Universiteit Leuven ( KU Leuven ), University of California [Santa Cruz] ( UCSC ), Eidgenössische Technische Hochschule, Swiss Federal Institute of Technology in Zürich ( ETH Zürich ), Max-Planck-Institut für Astronomie ( MPIA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), The Foundation for Scientific and Industrial Research ( SINTEF ), Laboratoire inter-universitaire des systèmes atmosphèriques ( LISA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Astrophysical Sciences [Princeton], Princeton University, Center for Astrophysics and Space Astronomy [Boulder] ( CASA ), University of Colorado Boulder [Boulder], Dept of Physics, University of Florida [Gainesville], Stony Brook University [The State University of New York] ( SBU ), ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), University College of London [London] ( UCL ), Maison de la Simulation ( MDLS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Recherche en Informatique et en Automatique ( Inria ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Iowa State University ( ISU ) -U.S. Department of Energy ( DOE ), Université de Montréal (UdeM), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), University of Central Florida [Orlando] (UCF), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Technische Universität Berlin (TU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Stiftelsen for INdustriell og TEknisk Forskning Digital [Trondheim] (SINTEF Digital), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Cornell University [New York], Università degli Studi di Roma Tor Vergata [Roma], Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Iowa State University (ISU)-U.S. Department of Energy [Washington] (DOE), Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Smithsonian Institution-Harvard University [Cambridge], Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), Harvard University-Smithsonian Institution, Technical University of Berlin / Technische Universität Berlin (TU), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Agence Spatiale Européenne = European Space Agency (ESA), and University of Oxford
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MODEL ATMOSPHERES ,Exclusive access ,010504 meteorology & atmospheric sciences ,Computer science ,Science program ,observational [methods] ,[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,FOS: Physical sciences ,MIDINFRARED INSTRUMENT ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astronomy & Astrophysics ,Planets and satellites: Individual ,01 natural sciences ,EXTRASOLAR GIANT PLANETS ,Planets and satellites: Atmospheres ,individual (WASP-79b, WASP-43b, WASP-18b) [planets and satellites] ,Settore FIS/05 - Astronomia e Astrofisica ,Methods: Observational ,Planet ,0103 physical sciences ,Early release ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,LIGHT CURVES ,Earth and Planetary Astrophysics (astro-ph.EP) ,Science & Technology ,Community engagement ,TIME-SERIES PHOTOMETRY ,THERMAL EMISSION ,James Webb Space Telescope ,Astrophysics::Instrumentation and Methods for Astrophysics ,WEBB-SPACE-TELESCOPE ,Astronomy and Astrophysics ,HOT-JUPITER ,atmospheres [planets and satellites] ,[ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP] ,Data science ,Methods observational ,Exoplanet ,13. Climate action ,Space and Planetary Science ,Physical Sciences ,HD 189733B ,Astrophysics::Earth and Planetary Astrophysics ,ATMOSPHERIC CIRCULATION ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The James Webb Space Telescope (JWST) presents the opportunity to transform our understanding of planets and the origins of life by revealing the atmospheric compositions, structures, and dynamics of transiting exoplanets in unprecedented detail. However, the high-precision, time-series observations required for such investigations have unique technical challenges, and prior experience with other facilities indicates that there will be a steep learning curve when JWST becomes operational. In this paper we describe the science objectives and detailed plans of the Transiting Exoplanet Community Early Release Science (ERS) Program, which is a recently approved program for JWST observations early in Cycle 1. The goal of this project, for which the obtained data will have no exclusive access period, is to accelerate the acquisition and diffusion of technical expertise for transiting exoplanet observations with JWST, while also providing a compelling set of representative datasets that will enable immediate scientific breakthroughs. The Transiting Exoplanet Community ERS Program will exercise the time-series modes of all four JWST instruments that have been identified as the consensus highest priorities, observe the full suite of transiting planet characterization geometries (transits, eclipses, and phase curves), and target planets with host stars that span an illustrative range of brightnesses. The observations in this program were defined through an inclusive and transparent process that had participation from JWST instrument experts and international leaders in transiting exoplanet studies. Community engagement in the project will be centered on a two-phase Data Challenge that culminates with the delivery of planetary spectra, time-series instrument performance reports, and open-source data analysis toolkits in time to inform the agenda for Cycle 2 of the JWST mission., Comment: PASP in press
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- 2018
34. Centroid vetting of transiting planet candidates from the Next Generation Transit Survey
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Andrew Grange, Sarah L. Casewell, Matthew R. Burleigh, Richard G. West, James McCormac, James S. Jenkins, Maximiliano Moyano, Christopher A. Watson, Liam Raynard, Alexis M. S. Smith, Stéphane Udry, Simon R. Walker, A. Thompson, Peter J. Wheatley, François Bouchy, Maximilian N. Günther, David J. Armstrong, Michael R. Goad, Alexander Chaushev, Edward Gillen, Philipp Eigmüller, Heike Rauer, Didier Queloz, Tom Louden, James A. G. Jackman, Don Pollacco, Katja Poppenhaeger, and Daniel Bayliss
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,planets and satellites: detection ,Data products ,010308 nuclear & particles physics ,Library science ,Astronomy ,FOS: Physical sciences ,Astronomy and Astrophysics ,eclipses ,01 natural sciences ,Infrared Processing and Analysis Center ,surveys ,Space and Planetary Science ,Observatory ,Vetting ,occultations ,0103 physical sciences ,astro-ph.EP ,(stars:) binaries: eclipsing ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The Next Generation Transit Survey (NGTS), operating in Paranal since 2016, is a wide-field survey to detect Neptunes and super-Earths transiting bright stars, which are suitable for precise radial velocity follow-up and characterisation. Thereby, its sub-mmag photometric precision and ability to identify false positives are crucial. Particularly, variable background objects blended in the photometric aperture frequently mimic Neptune-sized transits and are costly in follow-up time. These objects can best be identified with the centroiding technique: if the photometric flux is lost off-centre during an eclipse, the flux centroid shifts towards the centre of the target star. Although this method has successfully been employed by the Kepler mission, it has previously not been implemented from the ground. We present a fully-automated centroid vetting algorithm developed for NGTS, enabled by our high-precision auto-guiding. Our method allows detecting centroid shifts with an average precision of 0.75 milli-pixel, and down to 0.25 milli-pixel for specific targets, for a pixel size of 4.97 arcsec. The algorithm is now part of the NGTS candidate vetting pipeline and automatically employed for all detected signals. Further, we develop a joint Bayesian fitting model for all photometric and centroid data, allowing to disentangle which object (target or background) is causing the signal, and what its astrophysical parameters are. We demonstrate our method on two NGTS objects of interest. These achievements make NGTS the first ground-based wide-field transit survey ever to successfully apply the centroiding technique for automated candidate vetting, enabling the production of a robust candidate list before follow-up., Accepted for publication in MNRAS 25 Jul 2017. 15 pages, 15 figures, 3 tables. This is the authors' version of the manuscript
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- 2017
35. A precise optical transmission spectrum of the inflated exoplanet WASP-52b
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Patrick G. J. Irwin, Ian Skillen, Tom Louden, James Kirk, and Peter J. Wheatley
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,010504 meteorology & atmospheric sciences ,Opacity ,business.industry ,FOS: Physical sciences ,Astronomy and Astrophysics ,Scale height ,Astrophysics ,Light curve ,01 natural sciences ,Exoplanet ,Wavelength ,Optics ,Space and Planetary Science ,0103 physical sciences ,Hot Jupiter ,William Herschel Telescope ,Astrophysics::Earth and Planetary Astrophysics ,business ,010303 astronomy & astrophysics ,Noise (radio) ,0105 earth and related environmental sciences ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We have measured a precise optical transmission spectrum for WASP-52b, a highly inflated hot Jupiter with an equilibrium temperature of 1300 K. Two transits of the planet were observed spectroscopically at low resolution with the auxiliary-port camera (ACAM) on the William Herschel Telescope (WHT), covering a wide range of 4000-8750 ��. We use a Gaussian process approach to model the correlated noise in the multi-wavelength light curves, resulting in a high precision relative transmission spectrum with errors on the order of a pressure scale height. We attempted to fit a variety of different representative model atmospheres to the transmission spectrum, but did not find a satisfactory match to the entire spectral range. For the majority of the covered wavelength range (4000-7750 ��) the spectrum is flat, and can be explained by an optically thick and grey cloud layer at 0.1 mbar, but this is inconsistent with a slightly deeper transit at wavelengths $> 7750$ ��. We were not able to find an obvious systematic source for this feature, so this opacity may be the result of an additional unknown absorber., Submitted to MNRAS 17 Jan 2017, revised version after comments from reviewer, 12 pages, 10 figures
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- 2017
36. SPIDERMAN: an open-source code to model phase curves and secondary eclipses
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Laura Kreidberg and Tom Louden
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Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Brightness ,010504 meteorology & atmospheric sciences ,FOS: Physical sciences ,Astronomy and Astrophysics ,Markov chain Monte Carlo ,Phase curve ,01 natural sciences ,Exoplanet ,Celestial mechanics ,Computational physics ,Theoretical physics ,symbols.namesake ,Space and Planetary Science ,Geometric albedo ,Planet ,0103 physical sciences ,symbols ,Surface brightness ,Astrophysics::Earth and Planetary Astrophysics ,010303 astronomy & astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,0105 earth and related environmental sciences - Abstract
We present SPIDERMAN, a fast code for calculating exoplanet phase curves and secondary eclipses with arbitrary surface brightness distributions in two dimensions. Using a geometrical algorithm, the code solves exactly the area of sections of the disc of the planet that are occulted by the star. The code is written in C with a user-friendly Python interface, and is optimised to run quickly, with no loss in numerical precision. Approximately 1000 models can be generated per second in typical use, making Markov Chain Monte Carlo analyses practicable. The modular nature of the code allows easy comparison of the effect of multiple different brightness distributions for the dataset. As a test case we apply the code to archival data on the phase curve of WASP-43b using a physically motivated analytical model for the two dimensional brightness map. The model provides a good fit to the data; however, it overpredicts the temperature of the nightside. We speculate that this could be due to the presence of clouds on the nightside of the planet, or additional reflected light from the dayside. When testing a simple cloud model we find that the best fitting model has a geometric albedo of $0.32 \pm0.02$ and does not require a hot nightside. We also test for variation of the map parameters as a function of wavelength and find no statistically significant correlations., Comment: Submitted to MNRAS
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- 2017
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37. From dense hot Jupiter to low‐density Neptune: The discovery of WASP‐127b, WASP‐136b, and WASP‐138b
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Susan Walker, J. Rey, Coel Hellier, Laetitia Delrez, Don Pollacco, Michaël Gillon, Amanda P. Doyle, David R. Anderson, Luigi Mancini, Francesca Faedi, Amaury H. M. J. Triaud, P. Boumis, A. Collier Cameron, Oliver Turner, Richard G. West, Hugh P. Osborn, James McCormac, Francesco Pepe, J. Prieto-Arranz, K. L. Hay, Pierre F. L. Maxted, S. C. C. Barros, Monika Lendl, Enric Palle, Tom Louden, Didier Queloz, John Southworth, Duncan A. Brown, Guillaume Hébrard, Barry Smalley, Emmanuel Jehin, François Bouchy, Peter J. Wheatley, George W. King, David J. Armstrong, James Kirk, K. W. F. Lam, Damien Ségransan, Stéphane Udry, Aldo S. Bonomo, Thomas Henning, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, PPARC - Now STFC, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
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Gas giant ,Population ,NDAS ,FOS: Physical sciences ,Astrophysics ,individual: WASP-127 [Stars] ,01 natural sciences ,Settore FIS/05 - Astronomia e Astrofisica ,Neptune ,Planet ,0103 physical sciences ,Hot Jupiter ,QB Astronomy ,education ,010303 astronomy & astrophysics ,QC ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,education.field_of_study ,radial velocities [Techniques] ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,Subgiant ,individual: WASP-136 [Stars] ,photometric [Techniques] ,Giant planet ,Astronomy and Astrophysics ,Exoplanet ,Planetary systems ,QC Physics ,13. Climate action ,Space and Planetary Science ,individual: WASP-138 [Stars] ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report three newly discovered exoplanets from the SuperWASP survey. WASP-127b is a heavily inflated super-Neptune of mass 0.18 +/- 0.02 M_J and radius 1.37 +/- 0.04 R_J. This is one of the least massive planets discovered by the WASP project. It orbits a bright host star (Vmag = 10.16) of spectral type G5 with a period of 4.17 days. WASP-127b is a low-density planet that has an extended atmosphere with a scale height of 2500 +/- 400 km, making it an ideal candidate for transmission spectroscopy. WASP-136b and WASP-138b are both hot Jupiters with mass and radii of 1.51 +/- 0.08 M_J and 1.38 +/- 0.16 R_J, and 1.22 +/- 0.08 M_J and 1.09 +/- 0.05 R_J, respectively. WASP-136b is in a 5.22-day orbit around an F9 subgiant star with a mass of 1.41 +/- 0.07 M_sun and a radius of 2.21 +/- 0.22 R_sun. The discovery of WASP-136b could help constrain the characteristics of the giant planet population around evolved stars. WASP-138b orbits an F7 star with a period of 3.63 days. Its radius agrees with theoretical values from standard models, suggesting the presence of a heavy element core with a mass of ~10 M_earth. The discovery of these new planets helps in exploring the diverse compositional range of short-period planets, and will aid our understanding of the physical characteristics of both gas giants and low-density planets., Comment: 10 pages, 12 figures, 6 tables, accepted for publication in A&A
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- 2017
38. Transmission spectroscopy of the inflated exoplanet WASP-52b, and evidence for a bright region on the stellar surface
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V. S. Dhillon, Peter J. Wheatley, Tom Marsh, James Kirk, Chris M. Copperwheat, S. P. Littlefair, Tom Louden, and David J. Armstrong
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media_common.quotation_subject ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Planet ,0103 physical sciences ,Hot Jupiter ,William Herschel Telescope ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,QB ,media_common ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,Starspot ,Astronomy ,Astronomy and Astrophysics ,Scale height ,Planetary system ,Exoplanet ,13. Climate action ,Space and Planetary Science ,Sky ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We have measured the transmission spectrum of the extremely inflated hot Jupiter WASP-52b using simultaneous photometric observations in SDSS u', g' and a filter centred on the sodium doublet (NaI) with the ULTRACAM instrument mounted on the 4.2m William Herschel Telescope. We find that Rayleigh scattering is not the dominant source of opacity within the planetary atmosphere and find a transmission spectrum more consistent with wavelength-independent opacity such as from clouds. We detect an in-transit anomaly that we attribute to the presence of stellar activity and find that this feature can be more simply modelled as a bright region on the stellar surface akin to Solar faculae rather than spots. A spot model requires a significantly larger planet/star radius ratio than that found in previous studies. Our results highlight the precision that can be achieved by ground-based photometry with errors in the scaled planetary radii of less than one atmospheric scale height, comparable to HST observations., Comment: Accepted for publication in MNRAS. 11 pages, 6 figures, 2 tables
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- 2016
39. WASP-135b: A Highly Irradiated, Inflated Hot Jupiter Orbiting a G5V Star
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François Bouchy, Francesca Faedi, Richard G. West, James McCormac, Don Pollacco, Alexios Liakos, James Kirk, Enric Palle, Guillaume Hébrard, Jessica Spake, B. Courcol, Guy R. Davies, A. Collier Cameron, G. Bruno, Peter J. Wheatley, D. J. A. Brown, Stéphane Udry, Susan Walker, Tom Louden, J. Prieto Arranz, David R. Anderson, Coel Hellier, Amanda P. Doyle, K. W. F. Lam, P. Boumis, Pierre F. L. Maxted, David J. Armstrong, S. C. C. Barros, Y. Gómez Maqueo Chew, Hugh P. Osborn, 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), Virologia, Laboratorio Nacional de Investigacao Veterinaria (LNIV), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews [Scotland], University of Birmingham [Birmingham], Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Department of Astrophysics, Astronomy and Mechanics [Kapodistrian Univ], National and Kapodistrian University of Athens (NKUA), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), School of Physics and Astronomy, Department of Astronomy, Astrophysics and Mechanics [Athens], National and Kapodistrian University of Athens = University of Athens (NKUA | UoA), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), 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 ), Observatoire de Haute-Provence ( OHP ), Institut Pythéas ( OSU PYTHEAS ), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture ( IRSTEA ) -Institut de Recherche pour le Développement ( IRD ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), School of Physis & Astronomy, Department of Astronomy, Astrophysics and Mechanics, National and Kapodistrian University of Athens, Observatoire Astronomique de l'Université de Genève ( ObsGE ), Université de Genève ( UNIGE ), Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
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Angular momentum ,radial velocity, photometry [Techniques] ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Star (graph theory) ,01 natural sciences ,Planet ,0103 physical sciences ,Hot Jupiter ,QB Astronomy ,Astrophysics::Solar and Stellar Astrophysics ,Irradiation ,010306 general physics ,010303 astronomy & astrophysics ,QC ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,individual: WASP-135 [Stars] ,Astronomy and Astrophysics ,3rd-DAS ,Radius ,Orbital period ,Exoplanet ,Extrasolar planets ,QC Physics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of a new transiting planet from the WASP survey. WASP-135b is a hot Jupiter with a radius of 1.30 pm 0.09 Rjup, a mass of 1.90 pm 0.08 Mjup and an orbital period of 1.401 days. Its host is a Sun-like star, with a G5 spectral type and a mass and radius of 0.98 pm 0.06 Msun and 0.96 pm 0.05 Rsun respectively. The proximity of the planet to its host means that WASP-135b receives high levels of insolation, which may be the cause of its inflated radius. Additionally, we find weak evidence of a transfer of angular momentum from the planet to its star., 9 pages, 3 figures, accepted by Publications of the Astronomical Society of the Pacific
- Published
- 2016
40. Reconstructing the high energy irradiation of the evaporating hot Jupiter HD 209458b
- Author
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Kevin Briggs, Peter J. Wheatley, and Tom Louden
- Subjects
010504 meteorology & atmospheric sciences ,Cosmic Origins Spectrograph ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Luminosity ,Atmosphere ,Planet ,0103 physical sciences ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Space Telescope Imaging Spectrograph ,Astrophysics::Galaxy Astrophysics ,QB ,0105 earth and related environmental sciences ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Astronomy ,Astronomy and Astrophysics ,Exoplanet ,Space and Planetary Science ,Extreme ultraviolet ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The atmosphere of the exoplanet HD 209458b is undergoing sustained mass loss, believed to be caused by X-ray and extreme-ultraviolet (XUV) irradiation from its star. The majority of this flux is not directly observable due to interstellar absorption, but is required in order to correctly model the photo-evaporation of the planet and photo-ionisation of the outflow. We present a recovered high energy spectrum for HD\,209458 using a Differential Emission Measure (DEM) retrieval technique. We construct a model of the stellar corona and transition region for temperatures between 10$^{4.1}$ and 10$^{8}$ K which is constrained jointly by ultraviolet line strengths measured with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) and X-ray flux measurements from XMM-Newton. The total hydrogen ionising luminosity ($\lambda < 912$ \AA) is found to be 10$^{28.26}$ erg s$^{-1}$, which is similar to the value for the mean activity level of the Sun. This luminosity is incompatible with energy limited mass loss rates estimated from the same COS dataset, even the lower bound requires an uncomfortably high energetic efficiency of >40%. However, our luminosity is compatible with early estimates of the mass loss rate of HD 209458b based on results from the HST Space Telescope Imaging Spectrograph (STIS). Precisely reconstructed XUV irradiation is a key input to determining mass loss rates and efficiencies for exoplanet atmospheres., Comment: Submitted to MNRAS. 8 pages, 3 figures
- Published
- 2016
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41. High-energy environment of super-Earth 55 Cancri e
- Author
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Alfred Vidal-Madjar, Vincent Bourrier, Baptiste Lavie, Francesco Pepe, Peter J. Wheatley, Stéphane Udry, Aurélien Wyttenbach, A. Lecavelier des Etangs, Tom Louden, and David Ehrenreich
- Subjects
010504 meteorology & atmospheric sciences ,Population ,FOS: Physical sciences ,Flux ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,01 natural sciences ,Planet ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Coronal rain ,Emission spectrum ,education ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,education.field_of_study ,Super-Earth ,Astronomy and Astrophysics ,Corona ,Redshift ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The irradiation of close-in planets by their star influences their evolution and might be responsible for a population of ultra-short period planets eroded to their bare core. In orbit around a bright, nearby G-type star, the super-Earth 55 Cnc e offers the possibility to address these issues through UV transit observations. We used the Hubble Space Telescope to observe the transit in the FUV over 3 epochs in Apr. 2016, Jan. 2017, and Feb. 2017. These observations reveal significant short- and long-term variability in 55 Cnc chromospheric emission lines. In the last 2 epochs, we detected a larger flux in the C III, Si III, and Si IV lines after the planet passed the approaching quadrature, followed by a flux decrease in the Si IV doublet. In the second epoch these variations are contemporaneous with flux decreases in the Si II and C II doublet. All epochs show flux decreases in the N V doublet as well, albeit at different orbital phases. These flux decreases are consistent with absorption from optically thin clouds of gas, are mostly localized at low and redshifted radial velocities in the star rest frame, and occur preferentially before and during the transit. These 3 points make it unlikely that the variations are purely stellar, yet we show that the occulting material is also unlikely to originate from the planet. We tentatively propose that the motion of 55 Cnc e at the fringes of the stellar corona leads to the formation of a cool coronal rain. The inhomogeneity and temporal evolution of the stellar corona would be responsible for the differences between the visits. Additional variations are detected in the C II doublet in the first epoch and in the O I triplet in all epochs with a different behavior that points toward intrinsic stellar variability. Further observations at FUV wavelengths are required to disentangle between star-planet interactions and the activity of the star, Comment: 22 pages, 20 figures, accepted for publication in A&A
- Published
- 2018
42. Spatially resolved eastward winds and rotation of HD 189733b
- Author
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Peter J. Wheatley and Tom Louden
- Subjects
Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Rotation ,Redshift ,Blueshift ,Tidal locking ,Atmosphere ,Radial velocity ,Space and Planetary Science ,Planet ,Hot Jupiter ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Physics::Atmospheric and Oceanic Physics ,Astrophysics - Earth and Planetary Astrophysics ,QB - Abstract
We measure wind velocities on opposite sides of the hot Jupiter HD$\,$189733b by modeling sodium absorption in high-resolution HARPS transmission spectra. Our model implicitly accounts for the Rossiter-McLaughlin effect, which we show can explain the high wind velocities suggested by previous studies. Our results reveal a strong eastward motion of the atmosphere of HD$\,$189733b, with a redshift of $2.3^{+1.3}_{-1.5}$$\,$km$\,$s$^{-1}$ on the leading limb of the planet and a blueshift of $5.3^{+1.0}_{-1.4}$$\,$km$\,$s$^{-1}$ on the trailing limb. These velocities can be understood as a combination of tidally locked planetary rotation and an eastward equatorial jet; closely matching the predictions of atmospheric circulation models. Our results show that the sodium absorption of HD$\,$189733b is intrinsically velocity broadened and so previous studies of the average transmission spectrum are likely to have overestimated the role of pressure and thermal broadening., Comment: 5 pages, 4 figures, Accepted for publication in ApJL
- Published
- 2015
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43. K2-110 b: a massive mini-Neptune exoplanet
- Author
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Susan Walker, Daniel Bayliss, Olivier Demangeon, D. J. A. Brown, S. C. C. Barros, Don Pollacco, Isabelle Boisse, J. Lillo-Box, Nuno C. Santos, David Barrado, Vardan Adibekyan, Guillaume Hébrard, Emilio Molinari, Xavier Dumusque, David W. Latham, George W. King, Francesco Pepe, Magali Deleuil, David J. Armstrong, S. Hojjatpanah, Maxime Marmier, Jose-Manuel Almenara, Luca Malavolta, Alexandre Santerne, Rodrigo F. Díaz, D. Charbonneau, James McCormac, Stéphane Udry, François Bouchy, James Kirk, E. Delgado Mena, S. G. Sousa, Christophe Lovis, K. W. F. Lam, Hugh P. Osborn, Tom Louden, Andrew Collier Cameron, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, and University of St Andrews. St Andrews Centre for Exoplanet Science
- Subjects
Dwarf star ,Ciencias Físicas ,NDAS ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,purl.org/becyt/ford/1 [https] ,Atmosphere ,Planet ,0103 physical sciences ,QB Astronomy ,DETECTION [PLANETS AND SATELLITES] ,Planets and satellites: Detection ,010303 astronomy & astrophysics ,QC ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Astronomy and Astrophysics ,Space and Planetary Science ,Physics ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,purl.org/becyt/ford/1.3 [https] ,Radius ,Exoplanet ,Astronomía ,Detection ,Photometry (astronomy) ,QC Physics ,13. Climate action ,Magnitude (astronomy) ,Mini-Neptune ,Planets and satellites ,CIENCIAS NATURALES Y EXACTAS ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of the exoplanet K2-110 b (previously EPIC212521166b) from K2 photometry orbiting in a 13.8637d period around an old, metal-poor K3 dwarf star. With a V-band magnitude of 11.9, K2-110 is particularly amenable to RV follow-up. A joint analysis of K2 photometry and high-precision RVs from 28 HARPS and HARPS-N spectra reveal it to have a radius of 2.6$\pm 0.1 R_{\oplus}$ and a mass of 16.7$\pm 3.2$~M$_{\oplus}$, hence a density of $5.2\pm1.2$ g.cm$^{-3}$, making it one of the most massive planets yet to be found with a sub-Neptune radius. When accounting for compression, the resulting Earth-like density is best fitted by a 0.2 M$_{\oplus}$ hydrogen atmosphere over an 16.5 M$_{\oplus}$ Earth-like interior, although the planet could also have significant water content. At 0.1~AU, even taking into account the old stellar age of $8 \pm 3$ Gyr, the planet is unlikely to have been significantly affected by EUV evaporation. However the planet likely disc-migrated to its current position making the lack of a thick H$_2$ atmosphere puzzling. This analysis has made K2-110 b one of the best-characterised mini-Neptunes with density constrained to less than 30%., Submitted to A&A, May 2016; Accepted April 2017
- Published
- 2017
44. WASP-104b and WASP-106b : two transiting hot Jupiters in 1.75-day and 9.3-day orbits
- Author
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Barry Smalley, François Bouchy, Guillaume Montagnier, J. W. Rostron, Monika Lendl, Francesca Faedi, Y. Gómez Maqueo Chew, Oliver Turner, Didier Queloz, H. P. Osborn, Emmanuel Jehin, Richard G. West, Duncan A. Brown, Michaël Gillon, Don Pollacco, Aldo S. Bonomo, David R. Anderson, Pierre F. L. Maxted, S. C. C. Barros, M. Neveu-VanMalle, Amaury H. M. J. Triaud, Susan Walker, Alexis M. S. Smith, Stéphane Udry, A. Collier Cameron, Francesco Pepe, Damien Ségransan, Tom Louden, Laetitia Delrez, David J. Armstrong, Guillaume Hébrard, Peter J. Wheatley, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, Department of Medicine - Halifax (DRA), Dalhousie University [Halifax], Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 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), University of St Andrews [Scotland], Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, European Southern Observatory (ESO), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
- Subjects
Star (game theory) ,fundamental parameters [Planets and satellites] ,FOS: Physical sciences ,Orbital eccentricity ,Astrophysics ,individual: WASP-104b [Stars] ,Jupiter ,Planet ,Hot Jupiter ,QB Astronomy ,10. No inequality ,QC ,individual: WASP-106b [Stars] ,QB ,Physics ,Earth and Planetary Astrophysics (astro-ph.EP) ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,Astronomy and Astrophysics ,Orbital period ,detection [Planets and satellites] ,Planetary systems ,QC Physics ,Space and Planetary Science ,Magnitude (astronomy) ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery from the WASP survey of two exoplanetary systems, each consisting of a Jupiter-sized planet transiting an 11th magnitude (V) main-sequence star. WASP-104b orbits its star in 1.75 d, whereas WASP-106b has the fourth-longest orbital period of any planet discovered by means of transits observed from the ground, orbiting every 9.29 d. Each planet is more massive than Jupiter (WASP-104b has a mass of $1.27 \pm 0.05 \mathrm{M_{Jup}}$, while WASP-106b has a mass of $1.93 \pm 0.08 \mathrm{M_{Jup}}$). Both planets are just slightly larger than Jupiter, with radii of $1.14 \pm 0.04$ and $1.09 \pm 0.04 \mathrm{R_{Jup}}$ for WASP-104 and WASP-106 respectively. No significant orbital eccentricity is detected in either system, and while this is not surprising in the case of the short-period WASP-104b, it is interesting in the case of WASP-106b, because many otherwise similar planets are known to have eccentric orbits., Comment: 8 pages, 6 figures, 5 tables. Accepted for publication in A&A
- Published
- 2014
45. The Next Generation Transit Survey (NGTS)
- Author
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Andrew Grange, Bruno Chazelas, Philipp Eigmüller, L. Genolet, Michael R. Goad, Joao Paulo da Silva Bento, Anders Erikson, Heike Rauer, Christopher A. Watson, Richard G. West, James McCormac, Simon R. Walker, Marion Neveu, Andrés Jordán, Nigel Bannister, Peter J. Wheatley, Juan Cabrera, Didier Queloz, Matthew R. Burleigh, K. A. Lawrie, Tom Louden, and Don Pollacco
- Subjects
media_common.quotation_subject ,QC1-999 ,Neptune-sized planets ,NGTS ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,Kepler ,Observatory ,Planet ,0103 physical sciences ,transit planet detection ,Astrophysics::Solar and Stellar Astrophysics ,Transit (astronomy) ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,Earth and Planetary Astrophysics (astro-ph.EP) ,010308 nuclear & particles physics ,Physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Radial velocity ,Stars ,Sky ,Astrophysics::Earth and Planetary Astrophysics ,Geology ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The Next Generation Transit Survey (NGTS) is a new ground-based sky survey designed to find transiting Neptunes and super-Earths. By covering at least sixteen times the sky area of Kepler we will find small planets around stars that are sufficiently bright for radial velocity confirmation, mass determination and atmospheric characterisation. The NGTS instrument will consist of an array of twelve independently pointed 20cm telescopes fitted with red-sensitive CCD cameras. It will be constructed at the ESO Paranal Observatory, thereby benefiting from the very best photometric conditions as well as follow up synergy with the VLT and E-ELT. Our design has been verified through the operation of two prototype instruments, demonstrating white noise characteristics to sub-mmag photometric precision. Detailed simulations show that about thirty bright super-Earths and up to two hundred Neptunes could be discovered. Our science operations are due to begin in 2014., Comment: Submitted to the conference proceedings of the RoPACS meeting "Hot Planets and Cool Stars" (Nov. 2012, Garching), 4 pages, 2 colour figures
- Published
- 2013
46. Next Generation Transit Survey (NGTS)
- Author
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Heike Rauer, Christopher A. Watson, Juan Cabrera, Bruno Chazelas, Tom Louden, Michael R. Goad, Andrés Jordán, Philipp Eigmüller, Richard G. West, K. A. Lawrie, James McCormac, Andrew Grange, Don Pollacco, L. Genolet, Joao Paulo da Silva Bento, Nigel Bannister, Anders Erikson, Marion Neveu, Matthew R. Burleigh, Didier Queloz, Simon R. Walker, and Peter J. Wheatley
- Subjects
Physics ,010308 nuclear & particles physics ,Gas giant ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Planetary system ,01 natural sciences ,Exoplanet ,Astrobiology ,Radial velocity ,planetary systems instrumentation: photometers techniques: photometric telescopes surveys ,Space and Planetary Science ,Planet ,Primary (astronomy) ,0103 physical sciences ,ddc:520 ,Terrestrial planet ,Astrophysics::Earth and Planetary Astrophysics ,Transit (astronomy) ,010306 general physics ,ddc:526 ,Astrophysics::Galaxy Astrophysics - Abstract
Dieser Beitrag ist mit Zustimmung des Rechteinhabers aufgrund einer (DFG geförderten) Allianz- bzw. Nationallizenz frei zugänglich. This publication is with permission of the rights owner freely accessible due to an Alliance licence and a national licence (funded by the DFG, German Research Foundation) respectively. The Next Generation Transit Survey (NGTS) is a new ground-based survey for transiting exoplanets. Our primary goal is to find the first statistically-significant sample of Neptunes and super-Earths that are bright enough for radial velocity confirmation. By measuring precise masses and radii we will constrain the bulk composition and internal structure of planets that span the transition between the gas giants and terrestrial planets. Our brightest exoplanets will also be suitable for atmospheric characterisation with large facilities such as the VLT, JWST and the E-ELT. NGTS construction began in June 2013, and the survey is due to commence in 2014.
- Published
- 2013
47. NGTS-1b: a hot Jupiter transiting an M-dwarf
- Author
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Anders Erikson, Maximilian N. Günther, Maximiliano Moyano, Daniel Bayliss, Francesca Faedi, M. Soto, Philipp Eigmüller, Richard G. West, Heike Rauer, Stéphane Udry, James McCormac, Didier Queloz, Richard Alexander, Liam Raynard, Matthew R. Burleigh, Michael R. Goad, Edward Gillen, Szilard Csizmadia, James S. Jenkins, David J. Armstrong, Sarah L. Casewell, Andrew Grange, James A. G. Jackman, Don Pollacco, Boris T. Gänsicke, Lionel Metrailler, Simon R. Walker, Christopher A. Watson, Juan Cabrera, Peter J. Wheatley, Alexander Chaushev, E. Foxell, Gregory Lambert, Ruth Titz-Weider, François Bouchy, Roberto Raddi, Katja Poppenhaeger, Bruno Chazelas, Tom Louden, Alexis M. S. Smith, A. Thompson, R. S. Booth, Simon Hodgkin, Gillen, Edward [0000-0003-2851-3070], Hodgkin, Simon [0000-0002-5470-3962], Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
- Subjects
stars: individual: NGTS ,FOS: Physical sciences ,Library science ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,techniques: photometric ,techniques: radial velocities ,0103 physical sciences ,media_common.cataloged_instance ,Astrophysics::Solar and Stellar Astrophysics ,European union ,planetary systems ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,media_common ,QB ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,010308 nuclear & particles physics ,European research ,1-planetary systems ,Astronomy ,Astronomy and Astrophysics ,13. Climate action ,Space and Planetary Science ,Astrophysics::Earth and Planetary Astrophysics ,stars: individual: NGTS-1 ,Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery of NGTS-1b, a hot-Jupiter transiting an early M-dwarf host ($T_{eff}=3916^{+71}_{-63}~K$) in a P=2.674d orbit discovered as part of the Next Generation Transit Survey (NGTS). The planet has a mass of $0.812^{+0.066}_{-0.075}~M_{J}$, making it the most massive planet ever discovered transiting an M-dwarf. The radius of the planet is $1.33^{+0.61}_{-0.33}~R_{J}$. Since the transit is grazing, we determine this radius by modelling the data and placing a prior on the density from the population of known gas giant planets. NGTS-1b is the third transiting giant planet found around an M-dwarf, reinforcing the notion that close-in gas giants can form and migrate similar to the known population of hot Jupiters around solar type stars. The host star shows no signs of activity, and the kinematics hint at the star being from the thick disk population. With a deep (2.5%) transit around a $K=11.9$ host, NGTS-1b will be a strong candidate to probe giant planet composition around M-dwarfs via JWST transmission spectroscopy., Comment: 10 pages, 7 figures, accepted for publication in MNRAS
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48. Transit Signatures of Inhomogeneous Clouds on Hot Jupiters: Insights from Microphysical Cloud Modeling.
- Author
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Diana Powell, Tom Louden, Laura Kreidberg, Xi Zhang, Peter Gao, and Vivien Parmentier
- Subjects
- *
HOT Jupiters , *PARTICLE size distribution , *MICROPHYSICS , *CLOUDINESS , *SPACE telescopes - Abstract
We determine the observability in transmission of inhomogeneous cloud cover on the limbs of hot Jupiters through post-processing a general circulation model to include cloud distributions computed using a cloud microphysics model. We find that both the east and west limbs often form clouds, but that the different properties of these clouds enhance the limb-to-limb differences compared to the clear case. Using the James Webb Space Telescope, it should be possible to detect the presence of cloud inhomogeneities by comparing the shape of the transit light curve at multiple wavelengths because inhomogeneous clouds impart a characteristic, wavelength-dependent signature. This method is statistically robust even with limited wavelength coverage, uncertainty on limb-darkening coefficients, and imprecise transit times. We predict that the short-wavelength slope varies strongly with temperature. The hot limbs of the hottest planets form higher-altitude clouds composed of smaller particles, leading to a strong Rayleigh slope. The near-infrared spectral features of clouds are almost always detectable, even when no spectral slope is visible in the optical. In some of our models a spectral window between 5 and 9 μm can be used to probe through the clouds and detect chemical spectral features. Our cloud particle size distributions are not lognormal and differ from species to species. Using the area- or mass-weighted particle size significantly alters the relative strength of the cloud spectral features compared to using the predicted size distribution. Finally, the cloud content of a given planet is sensitive to a species' desorption energy and contact angle, two parameters that could be constrained experimentally in the future. [ABSTRACT FROM AUTHOR]
- Published
- 2019
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49. LRG-BEASTS: Transmission Spectroscopy and Retrieval Analysis of the Highly Inflated Saturn-mass Planet WASP-39b.
- Author
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James Kirk, Mercedes López-Morales, Peter J. Wheatley, Ian C. Weaver, Ian Skillen, Tom Louden, James McCormac, and Néstor Espinoza
- Published
- 2019
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50. Astro2020 Science White Paper The Need for Laboratory Measurements and Ab Initio Studies to Aid Understanding of Exoplanetary Atmospheres
- Author
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Jonathan Fortney, Robinson, Tyler D., Shawn Domagal-Goldman, Del Genio, Anthony D., Gordon, Iouli E., Ehsan Gharib-Nezhad, Nikole Lewis, Clara Sousa-Silva, Vladimir Airapetian, Brian Drouin, Hargreaves, Robert J., Xinchuan Huang, Tijs Karman, Ramirez, Ramses M., Rieker, Gregory B., Jonathan Tennyson, Robin Wordsworth, Yurchenko, Sergei N., Johnson, Alexandria V., Lee, Timothy J., Chuanfei Dong, Stephen Kane, Mercedes Lopez-Morales, Thomas Fauchez, Timothy Lee, Marley, Mark S., Keeyoon Sung, Nader Haghighipour, Tyler Robinson, Sarah Horst, Peter Gao, Der-You Kao, Courtney Dressing, Roxana Lupu, Daniel Wolf Savin, Benjamin Fleury, Olivia Venot, Daniela Ascenzi, Stefanie Milam, Harold Linnartz, Murthy Gudipati, Guillaume Gronoff, Farid Salama, Lisseth Gavilan, Jordy Bouwman, Martin Turbet, Yves Benilan, Bryana Henderson, Natalie Batalha, Rebecca Jensen-Clem, Timothy Lyons, Richard Freedman, Edward Schwieterman, Jayesh Goyal, Luigi Mancini, Patrick Irwin, Jean-Michel Desert, Karan Molaverdikhani, John Gizis, Jake Taylor, Joshua Lothringer, Raymond Pierrehumbert, Robert Zellem, Natasha Batalha, Sarah Rugheimer, Jacob Lustig-Yaeger, Renyu Hu, Eliza Kempton, Giada Arney, Mike Line, Munazza Alam, Julianne Moses, Nicolas Iro, Laura Kreidberg, Jasmina Blecic, Tom Louden, Paul Molliere, Kevin Stevenson, Mark Swain, Kimberly Bott, Nikku Madhusudhan, Joshua Krissansen-Totton, Drake Deming, Irina Kitiashvili, Evgenya Shkolnik, Zafar Rustamkulov, Leslie Rogers, Laird Close, and Venot, Olivia
- Subjects
[SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]
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