ICCUB Annual Report 2014
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Photospheric Activity, Rotation and Magnetic Interaction in LHS 6343 A
Astronomy & Astrophysics manuscript no. lhs6343_v9 c ESO 2018 May 4, 2018 Photospheric activity, rotation and magnetic interaction in LHS 6343 A E. Herrero1, A. F. Lanza2, I. Ribas1, C. Jordi3, and J. C. Morales1, 3 1 Institut de Ciències de l’Espai (CSIC-IEEC), Campus UAB, Facultat de Ciències, Torre C5 parell, 2a pl, 08193 Bellaterra, Spain, e-mail: [email protected], [email protected], [email protected] 2 INAF - Osservatorio Astrofisico di Catania, via S. Sofia, 78, 95123 Catania, Italy, e-mail: [email protected] 3 Dept. d’Astronomia i Meteorologia, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Martí Franquès 1, E08028 Barcelona, Spain, e-mail: [email protected] Received <date> / Accepted <date> ABSTRACT Context. The Kepler mission has recently discovered a brown dwarf companion transiting one member of the M4V+M5V visual binary system LHS 6343 AB with an orbital period of 12.71 days. Aims. The particular interest of this transiting system lies in the synchronicity between the transits of the brown dwarf C component and the main modulation observed in the light curve, which is assumed to be caused by rotating starspots on the A component. We model the activity of this star by deriving maps of the active regions that allow us to study stellar rotation and the possible interaction with the brown dwarf companion. Methods. An average transit profile was derived, and the photometric perturbations due to spots occulted during transits are removed to derive more precise transit parameters. We applied a maximum entropy spot model to fit the out-of-transit optical modulation as observed by Kepler during an uninterrupted interval of 500 days. -
Lhs 6343 C: a Transiting Field Brown Dwarf Discovered by the Kepler Mission∗
The Astrophysical Journal, 730:79 (11pp), 2011 April 1 doi:10.1088/0004-637X/730/2/79 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. LHS 6343 C: A TRANSITING FIELD BROWN DWARF DISCOVERED BY THE KEPLER MISSION∗ John Asher Johnson1,2, Kevin Apps3, J. Zachary Gazak4, Justin R. Crepp1, Ian J. Crossfield5, Andrew W. Howard6, Geoff W. Marcy6, Timothy D. Morton1, Carly Chubak6, and Howard Isaacson6 1 Department of Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125, USA; [email protected] 2 NASA Exoplanet Science Institute (NExScI), CIT Mail Code 100-22, 770 South Wilson Avenue, Pasadena, CA 91125, USA 3 Cheyne Walk Observatory, 75B Cheyne Walk, Horley, Surrey, RH6 7LR, UK 4 Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 5 Department of Physics and Astronomy, University of California Los Angeles, Los Angeles, CA 90095, USA 6 Department of Astronomy, University of California, Mail Code 3411, Berkeley, CA 94720, USA Received 2010 September 8; accepted 2011 January 18; published 2011 March 8 ABSTRACT We report the discovery of a brown dwarf that transits one member of the M+M binary system LHS 6343 AB every 12.71 days. The transits were discovered using photometric data from the Kepler public data release. The LHS 6343 stellar system was previously identified as a single high proper motion M dwarf. We use adaptive optics imaging to resolve the system into two low-mass stars with masses 0.370 ± 0.009 M and 0.30 ± 0.01 M, respectively, and a projected separation of 0.55. -
Abstracts Connecting to the Boston University Network
20th Cambridge Workshop: Cool Stars, Stellar Systems, and the Sun July 29 - Aug 3, 2018 Boston / Cambridge, USA Abstracts Connecting to the Boston University Network 1. Select network ”BU Guest (unencrypted)” 2. Once connected, open a web browser and try to navigate to a website. You should be redirected to https://safeconnect.bu.edu:9443 for registration. If the page does not automatically redirect, go to bu.edu to be brought to the login page. 3. Enter the login information: Guest Username: CoolStars20 Password: CoolStars20 Click to accept the conditions then log in. ii Foreword Our story starts on January 31, 1980 when a small group of about 50 astronomers came to- gether, organized by Andrea Dupree, to discuss the results from the new high-energy satel- lites IUE and Einstein. Called “Cool Stars, Stellar Systems, and the Sun,” the meeting empha- sized the solar stellar connection and focused discussion on “several topics … in which the similarity is manifest: the structures of chromospheres and coronae, stellar activity, and the phenomena of mass loss,” according to the preface of the resulting, “Special Report of the Smithsonian Astrophysical Observatory.” We could easily have chosen the same topics for this meeting. Over the summer of 1980, the group met again in Bonas, France and then back in Cambridge in 1981. Nearly 40 years on, I am comfortable saying these workshops have evolved to be the premier conference series for cool star research. Cool Stars has been held largely biennially, alternating between North America and Europe. Over that time, the field of stellar astro- physics has been upended several times, first by results from Hubble, then ROSAT, then Keck and other large aperture ground-based adaptive optics telescopes. -
A Survey of M Stars in the Field of View of Kepler Space Telescope
The Astrophysics of Planetary Systems: Formation, Structure, and Dynamical Evolution Proceedings IAU Symposium No. 276, 2010 c International Astronomical Union 2011 A. Sozzetti, M. G. Lattanzi & A. P. Boss , eds. doi:10.1017/S1743921311020746 A survey of M stars in the field of view of Kepler space telescope Mahmoudreza Oshagh1, Nader Haghighipour2 and Nuno C. Santos1 1 Centro de Astrof´ısica, Faculdade de Ciˆencias, Universidade do Porto, Rua das Estrelas, 4150–762 Porto, Portugal email: [email protected] 2 Institute for Astronomy and NASA Astrobiology Institute, University of Hawaii-Manoa, 2680 Woodlawn Drive, Honolulu, HI 96822,USA Abstract. M dwarfs constitute more than 70% of the stars in the solar neighborhood. They are cooler and smaller than Sun-like stars and have less-massive disks which suggests that planets around these stars are more likely to be Neptune-size or smaller. The transit depths and transit times of planets around M stars are large and well-matched to the Kepler temporal resolution. As a result, M stars have been of particular interest for searching for planets in both radial velocity and transit photometry surveys. We have recently started a project on searching for possible planet-hosting M stars in the publicly available data from Kepler space telescope. We have used four criteria, namely, the magnitude, proper motion, H-Ks and J-H colors, and searched for M stars in Q0 and Q1 data sets. We have been able to find 108 M stars among which 54 had not been previously identified among Kepler’s targets. We discuss the details of our selection process and present the results. -
Arxiv:1408.0401V1 [Astro-Ph.EP] 2 Aug 2014 Page Intentionally Left Blank
arXiv:1408.0401v1 [astro-ph.EP] 2 Aug 2014 Page intentionally left blank. Development and Application of Tools to Characterize Transiting Astrophysical Systems A dissertation presented by Bence B´eky to The Department of Astronomy in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the subject of Astronomy and Astrophysics Harvard University Cambridge, Massachusetts 2014 April Copyright c 2014 Bence B´eky All rights reserved. Dissertation Advisor: Author: Dr. Matthew Holman Bence B´eky Development and Application of Tools to Characterize Transiting Astrophysical Systems Abstract Since the discovery of the first exoplanets (planets outside our Solar System) more than 20 years ago, there has been an increasing need for photometric and spectroscopic models to characterize these systems. While imaging has been used extensively for Solar System bodies and extended objects like galaxies, the small angular extent of typical planetary systems makes it difficult or impossible to resolve them. Spatially integrated observations like measuring the total brightness or spectrum, however, can be conducted at a resonable cost. This thesis focuses on photometric models in the context of transiting systems, which exhibit a number of phenomena that can be exploited for characterization. First, we showcase the popular methods of transiting exoplanet discovery and characterization by ground based observations on the hot Jupiter HAT-P-27b. We demonstrate how transits allow us to constrain planetary mass, radius, and orbital inclination, which would not be possible based only on, for example, radial velocity measurements. Next, we perform reflection spectroscopy on HAT-P-1b, another hot Jupiter, using the binary companion of the host star as a reference to remove systematic errors from iii the signal. -
Detectability of Atmospheric Features of Earth-Like Planets in the Habitable
Astronomy & Astrophysics manuscript no. Wunderlich_etal_2019_arxiv c ESO 2019 May 8, 2019 Detectability of atmospheric features of Earth-like planets in the habitable zone around M dwarfs Fabian Wunderlich1, Mareike Godolt1, John Lee Grenfell2, Steffen Städt3, Alexis M. S. Smith2, Stefanie Gebauer2, Franz Schreier3, Pascal Hedelt3, and Heike Rauer1; 2; 4 1 Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, Hardenbergstraße 36, 10623 Berlin, Germany e-mail: [email protected] 2 Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt, Rutherfordstraße 2, 12489 Berlin, Germany 3 Institut für Methodik der Fernerkundung, Deutsches Zentrum für Luft- und Raumfahrt, 82234 Oberpfaffenhofen, Germany 4 Institut für Geologische Wissenschaften, Freie Universität Berlin, Malteserstr. 74-100, 12249 Berlin, Germany ABSTRACT Context. The characterisation of the atmosphere of exoplanets is one of the main goals of exoplanet science in the coming decades. Aims. We investigate the detectability of atmospheric spectral features of Earth-like planets in the habitable zone (HZ) around M dwarfs with the future James Webb Space Telescope (JWST). Methods. We used a coupled 1D climate-chemistry-model to simulate the influence of a range of observed and modelled M-dwarf spectra on Earth-like planets. The simulated atmospheres served as input for the calculation of the transmission spectra of the hy- pothetical planets, using a line-by-line spectral radiative transfer model. To investigate the spectroscopic detectability of absorption bands with JWST we further developed a signal-to-noise ratio (S/N) model and applied it to our transmission spectra. Results. High abundances of methane (CH4) and water (H2O) in the atmosphere of Earth-like planets around mid to late M dwarfs increase the detectability of the corresponding spectral features compared to early M-dwarf planets. -
Part I Financial Statements and Schedule of Expenditures of Federal Awards
Part I Financial Statements and Schedule of Expenditures of Federal Awards Report of Independent Auditors To the Board of Overseers of Harvard College: Report on the Consolidated Financial Statements We have audited the accompanying consolidated financial statements of Harvard University (the “University”), which comprise the consolidated balance sheet as of June 30, 2016, and the related consolidated statements of changes in net assets with general operating account detail, changes in net assets of the endowment and cash flows for the year then ended, and the related notes to the financial statements. Management’s Responsibility for the Consolidated Financial Statements Management is responsible for the preparation and fair presentation of the consolidated financial statements in accordance with accounting principles generally accepted in the United States of America; this includes the design, implementation, and maintenance of internal control relevant to the preparation and fair presentation of consolidated financial statements that are free from material misstatement, whether due to fraud or error. Auditors’ Responsibility Our responsibility is to express an opinion on the consolidated financial statements based on our audit. We conducted our audit in accordance with auditing standards generally accepted in the United States of America and the standards applicable to financial audits contained in Government Auditing Standards, issued by the Comptroller General of the United States. Those standards require that we plan and perform the audit to obtain reasonable assurance about whether the consolidated financial statements are free from material misstatement. An audit involves performing procedures to obtain audit evidence about the amounts and disclosures in the consolidated financial statements. The procedures selected depend on our judgment, including the assessment of the risks of material misstatement of the consolidated financial statements, whether due to fraud or error. -
BENCHMARK TRANSITING BROWN DWARF LHS 6343 C: SPITZER SECONDARY ECLIPSE OBSERVATIONS YIELD BRIGHTNESS TEMPERATURE and MID-T SPECTRAL CLASS Benjamin T
Draft version Wednesday 11th July, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 BENCHMARK TRANSITING BROWN DWARF LHS 6343 C: SPITZER SECONDARY ECLIPSE OBSERVATIONS YIELD BRIGHTNESS TEMPERATURE AND MID-T SPECTRAL CLASS Benjamin T. Montet1,2, John Asher Johnson2, Jonathan J. Fortney3, Jean-Michel Desert4 (Dated: Wednesday 11th July, 2018, 05:38) Draft version Wednesday 11th July, 2018 ABSTRACT There are no field brown dwarf analogs with measured masses, radii, and luminosities, precluding our ability to connect the population of transiting brown dwarfs with measurable masses and radii and field brown dwarfs with measurable luminosities and atmospheric properties. LHS 6343 C, a weakly- irradiated brown dwarf transiting one member of an M+M binary in the Kepler field, provides the first opportunity to probe the atmosphere of a non-inflated brown dwarf with a measured mass and radius. Here, we analyze four Spitzer observations of secondary eclipses of LHS 6343 C behind LHS 6343 A. Jointly fitting the eclipses with a Gaussian process noise model of the instrumental systematics, we measure eclipse depths of 1:06 ± 0:21 ppt at 3.6µm and 2:09 ± 0:08 ppt at 4.5µm, corresponding to brightness temperatures of 1026 ± 57 K and 1249 ± 36 K, respectively. We then apply brown dwarf evolutionary models to infer a bolometric luminosity log(L?=L ) = −5:16 ± 0:04. Given the known physical properties of the brown dwarf and the two M dwarfs in the LHS 6343 system, these depths are consistent with models of a 1100 K T dwarf at an age of 5 Gyr and empirical observations of field T5-6 dwarfs with temperatures of 1070 ± 130 K. -
Photospheric Activity, Rotation, and Magnetic Interaction in LHS 6343 A⋆
A&A 553, A66 (2013) Astronomy DOI: 10.1051/0004-6361/201220518 & c ESO 2013 Astrophysics Photospheric activity, rotation, and magnetic interaction in LHS 6343 A E. Herrero1,A.F.Lanza2,I.Ribas1,C.Jordi3, and J. C. Morales1,3 1 Institut de Ciències de l’Espai (CSIC–IEEC), Campus UAB, Facultat de Ciències, Torre C5 parell, 2a pl, 08193 Bellaterra, Spain e-mail: [eherrero;iribas;morales]@ice.cat 2 INAF – Osservatorio Astrofisico di Catania, via S. Sofia, 78, 95123 Catania, Italy e-mail: [email protected] 3 Dept. d’Astronomia i Meteorologia, Institut de Ciències del Cosmos (ICC), Universitat de Barcelona (IEEC–UB), Martí Franquès 1, 08028 Barcelona, Spain e-mail: [email protected] Received 8 October 2012 / Accepted 5 March 2013 ABSTRACT Context. The Kepler mission has recently discovered a brown dwarf companion transiting one member of the M4V+M5V visual binary system LHS 6343 AB with an orbital period of 12.71 days. Aims. The particular interest of this transiting system lies in the synchronicity between the transits of the brown dwarf C component and the main modulation observed in the light curve, which is assumed to be caused by rotating starspots on the A component. We model the activity of this star by deriving maps of the active regions that allow us to study stellar rotation and the possible interaction with the brown dwarf companion. Methods. An average transit profile was derived, and the photometric perturbations due to spots occulted during transits are removed to derive more precise transit parameters. We applied a maximum entropy spot model to fit the out-of-transit optical modulation as observed by Kepler during an uninterrupted interval of ∼500 days. -
Observations of Transiting Exoplanets with the JWST
Observations of Transiting Exoplanets with the James Webb Space Telescope (JWST) Charles Beichman NASA Exoplanet Science Institute, California Institute of Technology, Jet Propulsion Laboratory Bjoern Benneke, Heather Knutson, Roger Smith California Institute of Technology Pierre-Olivier Lagage CEA, Saclay Courtney Dressing, David Latham Center for Astrophysics, Harvard University Jonathan Lunine Cornell University Stephan Birkmann, Pierre Ferruit, Giovanna Giardino European Space Agency Eliza Kempton Grinnell College arXiv:1411.1754v1 [astro-ph.IM] 6 Nov 2014 Sean Carey, Jessica Krick Infrared Procesing and Analysis Center, California Institute of Technology Pieter D. Deroo, Avi Mandell, Michael E. Ressler, Avi Shporer, Mark Swain, Gautam Vasisht Jet Propulsion Laboratory, California Institute of Technology { 2 { George Ricker Massachusetts Institute of Technology Jeroen Bouwman, Ian Crossfield Max Planck Institute of Astrophysics Tom Greene, Steve Howell NASA Ames Research Center Jessie Christiansen, David Ciardi NASA Exoplanet Science Institute, California Institute of Technology Mark Clampin, Matt Greenhouse NASA Goddard Spaceflight Center Alessandro Sozzetti Osservatorio Astronomico Di Torino Paul Goudfrooij, Dean Hines, Tony Keyes, Janice Lee, Peter McCullough, Massimo Robberto, John Stansberry, Jeff Valenti Space Telescope Science Institute Marcia Rieke, George Rieke University of Arizona Jonathan Fortney University of California, Santa Cruz Jacob Bean, Laura Kreidberg University of Chicago Drake Deming { 3 { University of Maryland Lo¨ıcAlbert, Ren´eDoyon Universit´ede Montr´eal David Sing University of Exeter Received ; accepted { 4 { Contents 1 Introduction 8 2 Key Science Opportunities 12 2.1 Transit and Secondary Eclipse Spectroscopy . 13 2.1.1 Giant Planet Spectroscopy . 13 2.1.2 Spectroscopy of super-Earths and mini-Neptunes . 16 2.1.3 Terrestrial Planet Spectroscopy . -
Benjamin T. Montet
BENJAMIN T. MONTET Department of Astronomy and Astrophysics [email protected] 5640 S. Ellis Ave. http://www.astro.uchicago.edu/~bmontet Chicago, IL 60637 SCIENTIFIC RESEARCH INTERESTS Planetary dynamics, transit timing studies of exoplanetary systems, M dwarfs and their companions, exoplanet populations, stellar activity EDUCATION 2011-2016: California Institute of Technology, Pasadena, CA Doctor of Philosophy in Astrophysics, defended July 2016 Thesis: \Low-mass Stars and their Companions" Advisor: Professor John Johnson Master of Science, Astrophysics, received June 2013 2007-2011: University of Illinois at Urbana-Champaign, Urbana, IL Bachelor of Science in Physics Bachelor of Science in Astronomy Minor in Mathematics Graduated summa cum laude, Bronze Tablet (top 3% of graduating class) APPOINTMENTS 2016-Present: Carl Sagan Fellow, University of Chicago, Chicago, IL 2011-2016: Graduate Research Assistant, California Institute of Technology, Pasadena, CA TEACHING AND ADVISING Undergraduate Advisor, California Institute of Technology Juliette Becker (Michigan), Transit Timing Variations with Kepler Presented at the Second Kepler Science Conference (2013), 223rd Meeting of the American Astronomical Society (2014) Paper in preparation Undergraduate Mentor, Banneker Institute, Harvard University Justin Otor (Princeton), The Mass and Orbit of Kepler-56d 2015 Summer research project, work presented at Harvard University, 227th Meeting of the American Astronomical Society (2016) Paper submitted to The Astronomical Journal Guadalupe Tovar -
Doppler-Beaming in the Kepler Light Curve of LHS 6343 A
Astronomy & Astrophysics manuscript no. lhs6343˙db˙v6 c ESO 2021 September 17, 2021 Doppler-beaming in the Kepler light curve of LHS 6343 A (Research Note) E. Herrero1, A. F. Lanza2, I. Ribas1, C. Jordi3, A. Collier Cameron4, and J. C. Morales5 1 Institut de Ci`encies de l’Espai (CSIC-IEEC), Campus UAB, Facultat de Ci`encies, Torre C5 parell, 2a pl, 08193 Bellaterra, Spain, e-mail: [email protected], [email protected], [email protected] 2 INAF - Osservatorio Astrofisico di Catania, via S. Sofia, 78, 95123 Catania, Italy, e-mail: [email protected] 3 Dept. d’Astronomia i Meteorologia, Institut de Ci`encies del Cosmos (ICC), Universitat de Barcelona (IEEC-UB), Mart´ı Franqu`es 1, E08028 Barcelona, Spain, e-mail: [email protected] 4 SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife KY16 9SS, e-mail: [email protected] 5 LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 06, Univ. Paris-Diderot, 5 Pl. Jules Janssen, 92195 Meudon CEDEX, France, e-mail: [email protected] Received date / Accepted date ABSTRACT Context. Kepler observations revealed a brown dwarf eclipsing the M-type star LHS 6343 A with a period of 12.71 days. In addition, an out-of-eclipse light modulation with the same period and a relative semi-amplitude of ∼ 2 × 10−4 was observed showing an almost constant phase lag to the eclipses produced by the brown dwarf. In a previous work, we concluded that this was due to the light modulation induced by photospheric active regions in LHS 6343 A.