30Th March – 1St April 2016 University of Exeter
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Evans.2013.HD189733.Albedo.Pdf
ORE Open Research Exeter TITLE The Deep Blue Color of HD 189733b: Albedo Measurements with Hubble Space Telescope/Space Telescope Imaging Spectrograph at Visible Wavelengths AUTHORS Evans, T.M.; Pont, F.; Sing, David K.; et al. JOURNAL Astrophysical Journal DEPOSITED IN ORE 15 December 2014 This version available at http://hdl.handle.net/10871/16042 COPYRIGHT AND REUSE Open Research Exeter makes this work available in accordance with publisher policies. A NOTE ON VERSIONS The version presented here may differ from the published version. If citing, you are advised to consult the published version for pagination, volume/issue and date of publication The Astrophysical Journal Letters, 772:L16 (5pp), 2013 August 1 doi:10.1088/2041-8205/772/2/L16 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE DEEP BLUE COLOR OF HD 189733b: ALBEDO MEASUREMENTS WITH HUBBLE SPACE TELESCOPE/SPACE TELESCOPE IMAGING SPECTROGRAPH AT VISIBLE WAVELENGTHS Thomas M. Evans1,Fred´ eric´ Pont2,DavidK.Sing2, Suzanne Aigrain1, Joanna K. Barstow1, Jean-Michel Desert´ 3,7, Neale Gibson4, Kevin Heng5, Heather A. Knutson3, and Alain Lecavelier des Etangs6 1 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK; [email protected] 2 School of Physics, University of Exeter, EX4 4QL Exeter, UK 3 Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA 4 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany 5 University of Bern, Center for Space and Habitability, Sidlerstrasse 5, CH-3012 Bern, Switzerland 6 Institut d’Astrophysique de Paris, UMR7095 CNRS, Universite Pierre et Marie Curie, 98 bis Boulevard Arago, F-75014 Paris, France Received 2013 May 31; accepted 2013 June 15; published 2013 July 11 ABSTRACT We present a secondary eclipse observation for the hot Jupiter HD 189733b across the wavelength range 290–570 nm made using the Space Telescope Imaging Spectrograph on the Hubble Space Telescope. -
Javier Peralta Calvillo Generated From: Editor CVN De FECYT Date of Document: 24/01/2021 V 1.4.3 4154B7e2be6a86b67f637261e4ad3d11
Javier Peralta Calvillo Generated from: Editor CVN de FECYT Date of document: 24/01/2021 v 1.4.3 4154b7e2be6a86b67f637261e4ad3d11 This electronic file (PDF) has embedded CVN technology (CVN-XML). The CVN technology of this file allows you to export and import curricular data from and to any compatible data base. List of adapted databases available at: http://cvn.fecyt.es/ 4154b7e2be6a86b67f637261e4ad3d11 General quality indicators of scientific research This section describes briefly the main quality indicators of scientific production (periods of research activity, experience in supervising doctoral theses, total citations, articles in journals of the first quartile, H index...). It also includes other important aspects or peculiarities. My name is Javier Peralta and I was born in Algeciras (1979, Spain). I graduated in Physics at the University of La Laguna (Spain) in 2003, specializing in the fields of Astrophysics and Applied Physics. In 2009, I got an European PhD degree in Physics at the University of the Basque Country (Spain) with the highest qualification ("Cum Laude") . My PhD research, supervised by Professors Agustín Sánchez-Lavega and Ricardo Hueso, focused on the atmospheric dynamics of the planet Venus using data from the space missions Galileo and Venus Express. As a result, 6 articles were published in international peer review journals (4 of them as first author) along with more than 80 citations which allowed to be awarded in 2012 with the “Extraordinary Prize of Doctorate” granted by the University of the Basque Country. After my PhD, I spent the last 10 years (2009-2019) working in different research institutions as postdoctoral researcher: 2 years at IAA/CSIC in Granada (Spain), 3 years at the Astronomical Observatory of Lisbon (CAAUL/OAL, Portugal) and 5 years at the Institute of Space and Astronautical Science of Japan (ISAS/JAXA), funded by JAXA's International Top Young Fellowship (ITYF). -
Suzanne Aigrain on Behalf of the Corot Exoplanet Science Team Why Space?
Suzanne Aigrain on behalf of the CoRoT exoplanet science team Why space? • Atmosphere limits precision photometry from the ground • Scintillation limit ~2 mmag • Representative transit depths for Sun-like star • Jupiter: 10 mmag • Neptune: 1.3 mmag • Earth: 0.1 mmag • Weather and daytime limit temporal coverage from the ground • Many sources of noise transit timescales removed • colour dependent differential extinction, seeing, etc... 27 December 2006 The satellite • PI: Annie Baglin, LESIA, Meudon • CNES PROTEUS bus • 27cm aperture telescope • Soyuz II-1b launcher from Baikonour • Polar orbit • 2.5 year minimum lifetime Payload 27cm telescope layout focal box Full images, windowing and target selection Focal planeSeismology detector (Vincent Lapeyrere) Exopplnat detector (Farid Karioty) • Sismo field • 5 windows / CCD • 5.7 < mV < 9.5 • 32s sampling (1s on request) • frame transfer mode • used for astrometry 2.8° • 10 bright stars • 10 background windows • 11600 faint stars • 400 background windows CoRoT_Booklet_talks_summer2007 2 seismo exo SCAO Pointing stability Barycenter X of the stellar image x-coord of stellar image barycenter Stability performances : x axis: rms 0.12 pixel y axis: rms 0.15 pixel ~ 0RMS.3 a stability:rc sec. 0.12 pixel in x 0.15 pixel in y ~0.3 arcsec Vibrations due to the entrance and exit form ecclipses vibrations due to Earth eclipse ingress and egress CoRoT_Booklet_talks_summer2007 3 Exo field 2.8° • Exo field • up to 6000 LCs / CCD • 11.5 < mV < 16 • 512s sampling (32s for 500 objects / CCD) • 3 colours for -
Cvetoje- Vic, Anthony Cheetham, Frantz Martinache, Barnaby Norris, Peter Tuthill
Dr Benjamin Pope Lecturer in Astrophysics and DECRA Fellow Advisor: Prof. David Hogg Affiliation: School of Mathematics & Physics University of Queensland, St Lucia, QLD 4072, Australia and Centre for Astrophysics University of Southern Queensland, West Street, Toowoomba, QLD 4350, Australia Homepage: benjaminpope.github.io email: [email protected] orcid: 0000-0003-2595-9114 Education and Previous Positions 2017-2020 NASA Sagan Fellow, New York University Advisor: Prof. David Hogg 2017 Postdoctoral Research Associate, University of Sydney Advisor: Prof. Peter Tuthill 2013-2017 Doctor of Philosophy in Astrophysics, University of Oxford Thesis: “Observing Bright Stars and their Planets from the Earth and from Space” Balliol College | Supervisors: Prof. Suzanne Aigrain, Prof. Patrick Roche 2013-14 Master of Science in Astrophysics, University of Sydney Thesis: “Vision and Revision: Wavefront Sensing from the Image Domain” Supervisor: Prof. Peter Tuthill 2012 Bachelor of Science (Advanced) with Honours in Physics, University of Sydney First Class Honours, with the University Medal Thesis: “Dancing in the Dark: Kernel Phase Interferometry of Ultracool Dwarfs” Supervisors: Prof. Peter Tuthill, Dr. Frantz Martinache 2010-2011 Study Abroad at the University of California, Berkeley Research project with Prof. Charles H. Townes, Infrared Spatial Interferometer. Grants ARC Discovery Early Career Research Award (DECRA) AUD $444,075.00 NASA TESS Cycle 3 Guest Investigator USD $50,000 TESS Cycle 2 Guest Investigator USD $50,000 Balliol Balliol Interdisciplinary Institute Research Grant College GBP £3,000 Teaching 2021 Extragalactic Astrophysics & Cosmology, University of Queensland 2019 Master of Data Science Guest Lecturer, NYU Center for Data Science 2017 Bayesian Reasoning Honours Lecturer, University of Sydney 2017 Honours Project Supervisor, University of Sydney Supervised Alison Wong and Matthew Edwards, both to First Class Honours and PhD acceptance. -
TRINITY COLLEGE Cambridge Trinity College Cambridge College Trinity Annual Record Annual
2016 TRINITY COLLEGE cambridge trinity college cambridge annual record annual record 2016 Trinity College Cambridge Annual Record 2015–2016 Trinity College Cambridge CB2 1TQ Telephone: 01223 338400 e-mail: [email protected] website: www.trin.cam.ac.uk Contents 5 Editorial 11 Commemoration 12 Chapel Address 15 The Health of the College 18 The Master’s Response on Behalf of the College 25 Alumni Relations & Development 26 Alumni Relations and Associations 37 Dining Privileges 38 Annual Gatherings 39 Alumni Achievements CONTENTS 44 Donations to the College Library 47 College Activities 48 First & Third Trinity Boat Club 53 Field Clubs 71 Students’ Union and Societies 80 College Choir 83 Features 84 Hermes 86 Inside a Pirate’s Cookbook 93 “… Through a Glass Darkly…” 102 Robert Smith, John Harrison, and a College Clock 109 ‘We need to talk about Erskine’ 117 My time as advisor to the BBC’s War and Peace TRINITY ANNUAL RECORD 2016 | 3 123 Fellows, Staff, and Students 124 The Master and Fellows 139 Appointments and Distinctions 141 In Memoriam 155 A Ninetieth Birthday Speech 158 An Eightieth Birthday Speech 167 College Notes 181 The Register 182 In Memoriam 186 Addresses wanted CONTENTS TRINITY ANNUAL RECORD 2016 | 4 Editorial It is with some trepidation that I step into Boyd Hilton’s shoes and take on the editorship of this journal. He managed the transition to ‘glossy’ with flair and panache. As historian of the College and sometime holder of many of its working offices, he also brought a knowledge of its past and an understanding of its mysteries that I am unable to match. -
FINESSE and ARIEL + CASE: Dedicated Transit Spectroscopy Missions for the Post-TESS Era
FINESSE and ARIEL + CASE: Dedicated Transit Spectroscopy Missions for the Post-TESS Era Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Jacob Bean (University of Chicago) Presented on behalf of the FINESSE/CASE science team: Mark Swain (PI), Nicholas Cowan, Jonathan Fortney, Caitlin Griffith, Tiffany Kataria, Eliza Kempton, Laura Kreidberg, David Latham, Michael Line, Suvrath Mahadevan, Jorge Melendez, Julianne Moses, Vivien Parmentier, Gael Roudier, Evgenya Shkolnik, Adam Showman, Kevin Stevenson, Yuk Yung, & Robert Zellem Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars **Candidate NASA MIDEX mission for launch in 2023** Objectives FINESSE will test theories of planetary origins and climate, transform comparative planetology, and open up exoplanet discovery space by performing a comprehensive, statistical, and uniform survey of transiting exoplanet atmospheres. Strategy • Transmission spectroscopy of 500 planets: Mp = few – 1,000 MEarth • Phase-resolved emission spectroscopy of a subset of 100 planets: Teq > 700 K • Focus on synergistic science with JWST: homogeneous survey, broader context, population properties, and bright stars Hardware • 75 cm aluminum Cassegrain telescope at L2 • 0.5 – 5.0 μm high-throughput prism spectrometer with R > 80 • Single HgCdTe detector with JWST heritage for science and guiding Origins | Climate | Discovery Advantages of Fast Infrared -
![Arxiv:2010.15996V1 [Astro-Ph.IM] 29 Oct 2020 Keywords: ARIEL, Exoplanets, Transit Photometry, Light Curves, Stellar Spots, Machine Learning](https://docslib.b-cdn.net/cover/2975/arxiv-2010-15996v1-astro-ph-im-29-oct-2020-keywords-ariel-exoplanets-transit-photometry-light-curves-stellar-spots-machine-learning-842975.webp)
Arxiv:2010.15996V1 [Astro-Ph.IM] 29 Oct 2020 Keywords: ARIEL, Exoplanets, Transit Photometry, Light Curves, Stellar Spots, Machine Learning
Draft version November 2, 2020 Typeset using LATEX default style in AASTeX63 Lessons Learned from the 1st ARIEL Machine Learning Challenge: Correcting Transiting Exoplanet Light Curves for Stellar Spots Nikolaos Nikolaou ,1 Ingo P. Waldmann ,1 Angelos Tsiaras ,1 Mario Morvan ,1 Billy Edwards ,1 Kai Hou Yip ,1 Giovanna Tinetti ,1 Subhajit Sarkar,2 James M. Dawson,2 Vadim Borisov,3 Gjergji Kasneci,3 Matej Petkovic,´ 4 Tomaˇz Stepiˇsnik,4 Tarek Al-Ubaidi,5, 6 Rachel Louise Bailey ,6 Michael Granitzer ,7 Sahib Julka ,7 Roman Kern,8 Patrick Ofner ,8 Stefan Wagner,9 Lukas Heppe ,10 Mirko Bunse ,10 and Katharina Morik 10 1Department of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UK 2School of Physics and Astronomy, Cardiff University, The Parade, Cardiff, CF24 3AA, UK 3Department of Computer Science, University of Tuebingen, Tuebingen, Germany 4Joˇzef Stefan Institute, Ljubljana, Slovenia 5DCCS, Austria 6Space Research Institute, Austrian Academy of Sciences, Austria 7Chair of Data Science, University of Passau, Germany 8Know-Center GmbH - Research Center for Data-Driven Business & Big Data Analytics, Austria 9Commission for Astronomy, Austrian Academy of Sciences, Graz, Austria 10Artificial Intelligence Group, TU Dortmund University, Germany Submitted to ApJ ABSTRACT The last decade has witnessed a rapid growth of the field of exoplanet discovery and characterisation. However, several big challenges remain, many of which could be addressed using machine learning methodology. For instance, the most prolific method for detecting exoplanets and inferring several of their characteristics, transit photometry, is very sensitive to the presence of stellar spots. The current practice in the literature is to identify the effects of spots visually and correct for them manually or discard the affected data. -
Nawal Husnoo, Frédéric Pont, David Sing, Kevin Heng, Suzanne Aigrain, Leigh Fletcher, Jaemin Lee, Tom Evans
Opacity and spectra in hot Jupiters Nawal Husnoo, Frédéric Pont, David Sing, Kevin Heng, Suzanne Aigrain, Leigh Fletcher, Jaemin Lee, Tom Evans. Contact: [email protected]. We are developing a set of tools for generating absorption coeffcients for hot Jupiter atmospheres. We focus on the visible spectrum, where we plan to use the routines for generating "frst guess" models for the upcoming transmission spectra of hot Jupiters (HST program in progress, PI: Sing). We also plan to study the atmospheric temperature-pressure profle of hot Jupiters (Heng et al. 2011)[1], with a focus on the effects of various types of clouds. The transmission spectrum of an exoplanet allows us to probe the atmosphere for elemental and molecular species. In the visible spectrum, sodium, potassium, titanium oxide and vanadium oxide are expected to be dominant [2], (depending on the composition and temperature). Absorption due to clouds/hazes can also be relevant [3]. In this project, we seek "frst guess" models to guide the ongoing observations of transmission spectra of transiting planets with HST. We seek to link the transmission spectrum with the "refection spectrum" in the visible, and compare the effects of scattering due to grains and absorption due to gasses. Transmission spectrum We perform fnite element integration for visible light rays that travel in a grazing geometry through the planet's atmosphere to generate the transmission spectrum. Absorption from the radiatively active species in the atmosphere causes wavelength-selective dimming in the light. Figure 1 shows an example of a transmission spectrum (HD 189733b), where we have plotted a model that includes the sodium D lines, Figure 1: Plot showing the latest reduction of the transmission spectroscopy for HD 189733b (our and Mie scattering for small particles (r<<λ), giving the Rayleigh regime. -
Today Oxford
www.oxfordtoday.ox.ac.uk Michaelmas Term 2010 Volume 23 No 1 OX FOR D TODAY THE UNIVERSITY MAGAZINE 20 | WILFRED THESIGER AFRICA SEEN THROUGH HIS LENS 30 | SCIENCE WHEN TO SHARE GENE DATA? 45 | GEOFFREY HILL SEAMUS PERRY ON OUR GREATEST LIVING POET PRIME MINISTERS Why has Oxford produced so many? OXF01.cover 1 8/10/10 3:37:5 pm FROM HOME Since 1821 the Oxfordand Cambridge Club has provided alumni of both universities with an exclusive home from home in the heartofthe Capital. Todaymembers can relax, dine and meetfriends in supremely elegant surroundings thatalso featurewell stocked libraries,sports facilities and first-class bedroom accommodation. Reciprocal clubs welcome members of the Oxfordand Cambridge Club in 35 countriesaround the world. Formoreinformation, please contact: [email protected] or call +44 (0)20 7321 5110 Oxfordand Cambridge Club,71Pall Mall,LondonSW1Y 5HD www.oxfordandcambridgeclub.co.uk OX FOR D TODAY EDITOR: Dr Richard Lofthouse DEPUTY ART EDITOR: Steven Goldring DESIGNER: Victoria Ford HEAD OF PUBLICATIONS AND WEB OFFICE: Anne Brunner-Ellis PRODUCTION EDITOR: Kate Lloyd SUB EDITOR: Elizabeth Tatham PICTURE EDITOR: Joanna Kay DESIGN DIRECTOR: Dylan Channon Thanks to Simon Kirrane, Esther Woodman, Helen Cox, Emma Swift EDITORIAL ENQUIRIES: Janet Avison Public Affairs Directorate Tel: 01865 280545 Fax: 01865 270178 [email protected] www.oxfordtoday.ox.ac.uk ALUMNI ENQUIRIES, INCLUDING CHANGE OF ADDRESS: Claire Larkin Alumni Offi ce Tel: 01865 611610 Michaelmas [email protected] COVER IMAGE: HARRY BORDEN/CORBIS OUTLINE, ROB JUDGES www.alumni.ox.ac.uk Term 2010 University of Oxford, University Offi ces, Wellington Square, Oxford OX1 2JD ADVERTISING ENQUIRIES: Marie Longstaff Future Plus, Beaufort Court, 30 Monmouth Street, Bath BA1 2BW Tel: 01225 822849 [email protected] www.futureplc.com Oxford Today is published in February, June and October. -
Gaussian Processes
Gaussian processes: the next step in exoplanet data analysis Suzanne Aigrain (University of Oxford) Neale Gibson, Tom Evans, Amy McQuillan Steve Roberts, Steve Reece, Mike Osborne ... let the data speak Gaussian processes: the next step in exoplanet data analysis Suzanne Aigrain (University of Oxford) Neale Gibson, Tom Evans, Amy McQuillan Steve Roberts, Steve Reece, Mike Osborne Gaussian processes for modelling systematics 5 high precision time-series stochastic correlated disentangle noise Figure 1. The ‘raw’ HD 189733 NICMOS dataset used as an example for our Gaussian process model. Left: Raw light curves of HD 189733 for each of the 18 wavelength channels, from 2.50µmto1.48µmtoptobottom.Right:Theopticalstateparametersextracted from the spectra plotted as a time series. These are used as the input parameters for our GP model. The red lines represent a GP regression on the input parameters, used to remove the noise and test how this effects the GP model. the noisy input parameters. We also checked that the choice wavelength channels. In this example, only orbits 2, 3 and 5 of hyperprior length scale had little effect on the results, by are used to determine the parameters and hyperparameters setting them to large values, and repeating the procedure of the GP (or ‘train’ the GP), and are shown by the red with varying length scales ensuring the transmission spec- points4. Orbit 4 (green points) was not used... in the traininglet the data speak tra were not significantly altered. set. Predictive distributions were calculated for orbits 2–5, and are shown by the grey regions, which plot the 1 and 2σ confidence intervals. -
Statistics and Exoplanets
FM 8: Statistics and Exoplanets Downloaded from https://www.cambridge.org/core. IP address: 170.106.202.8, on 29 Sep 2021 at 23:15:31, subject to the Cambridge Core terms of use, available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S1743921316002726 Astronomy in Focus, Volume 1, Focus Meeting 8 XXIXth IAU General Assembly, August 2015 c International Astronomical Union 2016 Piero Benvenuti, ed. doi:10.1017/S1743921316002726 Introduction Suzanne Aigrain1 and Eric Feigelson2 1 Department of Physics, University of Oxford, Keble Road, Oxford, OX3 9UU, UK email: [email protected] 2 TBD email: Department of Astronomy & Astrophysics and Center for Astrostatistics, Penn State University, 525 Davey Laboratory, University Park PA 16802 USA Abstract. The IAU’s Statistics and Exoplanets Focus Meeting brings together observers, mod- elers and methodologists to discuss the intricate challenges of extracting and interpreting faint planetary signals from dominant starlight. Initiated by the IAU’s new groups concentrating on astroinformatics and astrostatistics, the meeting stimulated the wider exoplanetary community as well as experts in data and science analysis. This proceedings presented selected papers from the Focus Meeting. Keywords. methods: data analysis, methods: statistical, (stars:) planetary systems 1. Motivation The discovery and characterization of exoplanets requires both superbly accurate in- strumentation and sophisticated statistical methods, to extract weak planetary signals from dominant starlight, very large samples and noisy datasets. While numerous exo- planet conferences take place each year, these mostly focus on observational results, their physical implications, and current or future instrument developments; the statistical as- pects of the papers presented, while important, are not usually central to the program. -
Postdoctoral Research Fellow At
Quentin CHANGEAT – French – phone: 0033 6 58 72 94 80 – emAil: [email protected] AcAdemic website: https://quentchangeat.github.io/ , ORCID: 0000-0001-6516-4493. Curriculum Vitae RESEARCH SUMMARY: My reseArch focuses on the AnAlysis of current And future observAtions of exoplAnets, plAnets outside our solAr- system, to understand the physics And the chemistry of their Atmospheres. Using dAta-oriented techniques, I have charActerised many plAnets observed with the Hubble And Spitzer Space Telescopes, ranging from the temperAte super-Earth LHS-1140b to the extremely-hot Jupiter KELT-9b. I have pioneered in the development of tools (TauREx3 and Alfnoor) AdApted to the analysis of large populations of Atmospheres and the extrAction of their 3D nAture from challenging phase-curve observations. I Also used those tools to evAluAte the performAnces of next generAtion telescopes such As ESA Ariel And NASA/ESA JWST in Answering some of the major questions of the field. My work is showing the importance of cross-disciplinary Approaches in understAnding exoplAnetary atmospheres. CURRENT POSITION(S): 2021 Dec – 2022 MAr: Postdoctoral Fellow for Research in Japan (JSPS fellowship) Division of Science, National Astronomical Observatory of Japan (Japan) 2021 – Current: Postdoctoral Research Fellow DepArtment of Physics And Astronomy, University College London (UK) Leadership roles: CoordinAtor of the SpectrAl RetrievAl working group for the ESA Ariel Mission. Developer of the TauREx and Alfnoor exoplAnet suites (more thAn 5000 downloAds). Co-PI HST Proposal 16457 (8 orbits) and external reviewer of HST Cycle 29. Founder of the UCT collAborAtion between UCL And the Tokyo Univ. exoplAnet groups.