DOCSLIB.ORG

Inferring Atmospheric Characteristics from Transiting Exoplanets

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Inferring Atmospheric Characteristics from Transiting Exoplanets Inferring Atmospheric Characteristics From Transiting Exoplanets Jean-Michel Désert Caltech - Sagan Fellow Sagan Summer School, July 26th 2012 jeudi 26 juillet 2012 Inferring Atmospheric Characteristics From Transiting Exoplanets Image credit: THIERRY LEGAULT Jean-Michel Désert Caltech - Sagan Fellow Sagan Summer School, July 26th 2012 jeudi 26 juillet 2012 Inferring Atmospheric Characteristics From Transiting Exoplanets Image credit: THIERRY LEGAULT Jean-Michel Désert Caltech - Sagan Fellow Sagan Summer School, July 26th 2012 jeudi 26 juillet 2012 I) From Transits (Eclipses) Depths to Atmospheric Signals II) Pushing Observational Limits III) New Frontiers for Atmospheric Studies 4 jeudi 26 juillet 2012 Atmospheric Structure jeudi 26 juillet 2012 Atmospheric Structure [Adapted from Fortney 2008] jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup Updated from Winn et al. (2008) 7 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup Updated from Winn et al. (2008) 7 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup ★ First atmosphere: 2 -4 (atm /R* ) ~ 10 NaI 0.0232 ± 0.0057 % [ Charbonneau et al. 2002] Updated from Winn et al. (2008) 7 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup ★ First atmosphere: 2 -4 (atm /R* ) ~ 10 NaI 0.0232 ± 0.0057 % [ Charbonneau et al. 2002] ★ Exosphere H ~ 15 ± 4% [ Vidal-Madjar et al. 2003] Updated from Winn et al. (2008) 7 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup ★ First atmosphere: 2 -4 (atm /R* ) ~ 10 NaI 0.0232 ± 0.0057 % [ Charbonneau et al. 2002] ★ Exosphere H ~ 15 ± 4% [ Vidal-Madjar et al. 2003] ★ First direct lights: 2 -3 Tp /T*(Rp /R* ) ~ 10 TB (24 µm)~ 1130 ± 150 K [ Deming et al. 2005] Updated from Winn et al. (2008) 7 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup Updated from Winn et al. (2008) 8 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup Updated from Winn et al. (2008) 8 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup ★ First atmosphere: 2 -4 (atm /R* ) ~ 10 NaI 0.0232 ± 0.0057 % [ Charbonneau et al. 2002] Updated from Winn et al. (2008) 8 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup ★ First atmosphere: 2 -4 (atm /R* ) ~ 10 NaI 0.0232 ± 0.0057 % [ Charbonneau et al. 2002] ★ Exosphere H ~ 15 ± 4% [ Vidal-Madjar et al. 2003] Updated from Winn et al. (2008) 8 jeudi 26 juillet 2012 HD209458b: 12 years of transits ★ First transit: 2 -2 (Rp /R* ) ~ 10 [ Charbonneau et al. 2000] ~ 1.6% [ Henry et al. 2000] 1.27±0.02 Rjup ★ First atmosphere: 2 -4 (atm /R* ) ~ 10 NaI 0.0232 ± 0.0057 % [ Charbonneau et al. 2002] ★ Exosphere H ~ 15 ± 4% [ Vidal-Madjar et al. 2003] ★ First direct lights: 2 -3 Tp /T*(Rp /R* ) ~ 10 TB (24 µm)~ 1130 ± 150 K [ Deming et al. 2005] Updated from Winn et al. (2008) 8 jeudi 26 juillet 2012 Probing Transiting Exoplanet Atmospheres Reflected: Emitted: Transmitted: jeudi 26 juillet 2012 Probing Transiting Exoplanet Atmospheres Reflected: Emitted: Hot-Jupiters Transmitted: - Albedo, Temperature - Thermal profile - Composition - Dynamics jeudi 26 juillet 2012 Transmission Spectroscopy ΔF/F= (Fout – Fin) / Fout Transit depth 2 ΔF/F= (Rp /R* ) b = a/R cosi * jeudi 26 juillet 2012 Transmission Spectroscopy ΔF/F= (Fout – Fin) / Fout Transit depth 2 ΔF/F= (Rp /R* ) Rp = Rc + zatm b = a/R cosi * jeudi 26 juillet 2012 Transmission Spectroscopy ΔF/F= (Fout – Fin) / Fout Transit depth 2 ΔF/F= (Rp /R* ) Rp = Rc + zatm RJup ~1 % ~0.01 % b = a/R cosi R ~0.01 % ~10-5 * ⊕ jeudi 26 juillet 2012 Transmission Spectroscopy ΔF/F= (Fout – Fin) / Fout Transit depth 2 ΔF/F= (Rp /R* ) Rp(λ) = Rc + zatm(λ) RJup ~1 % ~0.01 % b = a/R cosi R ~0.01 % ~10-5 * ⊕ jeudi 26 juillet 2012 Transmission Spectroscopy ΔF/F= (Fout – Fin) / Fout Transit depth 2 ΔF/F= (Rp /R* ) Rp(λ) = Rc + zatm(λ) R ~1 % ~0.01 % ΔF/F(λ)=> λ Jup Rp( ) -5 b = a/R cosi R ~0.01 % ~10 * ⊕ jeudi 26 juillet 2012 Transmission Spectroscopy ΔF/F= (Fout – Fin) / Fout Transit depth 2 ΔF/F= (Rp /R* ) Rp(λ) = Rc + zatm(λ) R ~1 % ~0.01 % ΔF/F(λ)=> λ Jup Rp( ) -5 b = a/R cosi R ~0.01 % ~10 * ⊕ Berta et al. (2011) jeudi 26 juillet 2012 Transmission Spectroscopy -τ I0 I=I0e 12 jeudi 26 juillet 2012 Transmission Spectroscopy Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Scale Height H(z) = kT(z)/μg Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Scale Height H(z) = kT(z)/μg Hydrostatic equilibrium: Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Scale Height H(z) = kT(z)/μg Hydrostatic equilibrium: What do we measure? Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Scale Height H(z) = kT(z)/μg Hydrostatic equilibrium: What do we measure? (λ) Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Scale Height H(z) = kT(z)/μg Hydrostatic equilibrium: What do we measure? (λ) => ∆Rp = H ∆ln(σ) Lecavelier et al. (2008) 13 jeudi 26 juillet 2012 Transmission Spectroscopy z(λ) Scale Height H(z) = kT(z)/μg Hydrostatic equilibrium: What do we measure? (λ) => ∆Rp = H ∆ln(σ) To remember: Lecavelier et al. (2008) Rpl(λ) => f(P , T, n) 13 ∆Rpl(λ) => T jeudi 26 juillet 2012 Transiting Exoplanets 10 ( ) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) 14 jeudi 26 juillet 2012 Emission Measurements (IR) 10 ( ) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) jeudi 26 juillet 2012 Transmission Measurements (XEUV -> IR) 10 ( ) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) 16 jeudi 26 juillet 2012 Hot-Jupiters Survey Transmission Spectroscopy Space-based Surveys: HST-WFC3 13 Hot-Jupiters (PI: D. Deming) 10 ( ) HST-STIS 13 Hot-Jupiters (PI: D. Sing) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) 17 jeudi 26 juillet 2012 Hot-Jupiters Survey Transmission Spectroscopy Space-based Surveys: HST-WFC3 13 Hot-Jupiters (PI: D. Deming) 10 ( ) HST-STIS 13 Hot-Jupiters (PI: D. Sing) Ground-based Surveys: 1 Planet Radius Radius Planet NIR: Magellan (PI: JM Désert / J. Bean) 0.01 0.1 1 Semi-majorOptical: axis Gemini (AU) (PI: JM Désert) 18 jeudi 26 juillet 2012 Transmission Measurements (XEUV -> IR) 10 ( ) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) 19 jeudi 26 juillet 2012 M-dwarfs Opportunity 10 ( ) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) 20 jeudi 26 juillet 2012 GJ-1214b GJ-1214b Charbonneau et al. (2009) +/-0.13 2.7 REarth +/-0.93 6.5 MEarth 10 560 K ( ) 1 Planet Radius Radius Planet 0.01 0.1 1 Semi-major axis (AU) 21 jeudi 26 juillet 2012 Transmission Spectroscopy of GJ1214b Désert et al. (2011) CH4 I Models By E. Kempton : Bean et al. (2010) jeudi 26 juillet 2012 GJ1214b: Distinguishing H-rich/H-poor atmospheres Désert et al. (2011) CH4 I Models By E. Kempton : Large H Bean et al. (2010) Small H jeudi 26 juillet 2012 GJ1214b: Distinguishing H-rich/H-poor atmospheres Désert et al. (2011) CH4 I Models By E. Kempton : Large H Bean et al. (2010) Rogers & Seager (2010) Small H Large H Small H Large H jeudi 26 juillet 2012 Transmission Spectroscopy of GJ1214b Désert et al. (2011) CH4 I H2O H2O I I Bean et al. (2010) jeudi 26 juillet 2012 Transmission Spectroscopy of GJ1214b Désert et al. (2011) J H K H2O H2O I I Bean et al. (2010) jeudi 26 juillet 2012 Transmission Spectroscopy of GJ1214b Désert et al. (2011) J H K H2O H2O I I Bean et al. (2010) HST/WFC3 jeudi 26 juillet 2012 Transmission Spectroscopy of GJ1214b Désert et al. (2011) J H K H2O H2O I I Bean et al. (2010) HST/WFC3 Berta et al. (2011) jeudi 26 juillet 2012 Transmission Spectroscopy of GJ1214b Désert et al. (2011) J H K H2O H2O I I Bean et al. (2010) HST/WFC3 jeudi 26 juillet 2012 Hot-Jupiters Survey with HST/WFC3 Sukrit Ranjan (CfA) jeudi 26 juillet 2012 Hot-Jupiters Survey with HST/WFC3 Sukrit Ranjan (CfA) Ranjan et al.
Load more

Recommended publications
  • Arxiv:2003.04650V1 [Astro-Ph.EP] 10 Mar 2020 Sphere (Arcangeli Et Al
    Astronomy & Astrophysics manuscript no. main c ESO 2020 March 11, 2020 Detection of Fe i and Fe ii in the atmosphere of MASCARA-2b using a cross-correlation method M. Stangret1,2, N. Casasayas-Barris1,2, E. Pallé1,2, F. Yan3, A. Sánchez-López4, M. López-Puertas4 1 Instituto de Astrofísica de Canarias, Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, 38200 San Cristobal de La Laguna, Spain 3 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany 4 Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, 18008 Granada, Spain Received 21 January 2020; accepted 27 February 2020 ABSTRACT Ultra-hot Jupiters are gas giants planets whose dayside temperature, due to the strong irradiation received from the host star, is greater than 2200 K. These kind of objects are perfect laboratories to study chemistry of exoplanetary upper atmospheres via trans- mission spectroscopy. Exo-atmospheric absorption features are buried in the noise of the in-transit residual spectra. However we can retrieve the information of hundreds of atmospheric absorption lines by performing a cross-correlation with an atmospheric transmission model, which allows us to greatly increase the exo-atmospheric signal. At the high-spectral resolution of our data, the Rossiter-McLaughlin effect and centre-to-limb variation have a strong contribution. Here, we present the first detection of Fe i and the confirmation of absorption features of Fe ii in the atmosphere of the ultra-hot Jupiter MASCARA-2b/KELT-20b, by using three transit observations with HARPS-N.
    [Show full text]
  • Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects
    AA57CH15_Madhusudhan ARjats.cls August 7, 2019 14:11 Annual Review of Astronomy and Astrophysics Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects Nikku Madhusudhan Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, United Kingdom; email: [email protected] Annu. Rev. Astron. Astrophys. 2019. 57:617–63 Keywords The Annual Review of Astronomy and Astrophysics is extrasolar planets, spectroscopy, planet formation, habitability, atmospheric online at astro.annualreviews.org composition https://doi.org/10.1146/annurev-astro-081817- 051846 Abstract Copyright © 2019 by Annual Reviews. Exoplanetary science is on the verge of an unprecedented revolution. The All rights reserved thousands of exoplanets discovered over the past decade have most recently been supplemented by discoveries of potentially habitable planets around nearby low-mass stars. Currently, the field is rapidly progressing toward de- tailed spectroscopic observations to characterize the atmospheres of these planets. Various surveys from space and the ground are expected to detect numerous more exoplanets orbiting nearby stars that make the planets con- ducive for atmospheric characterization. The current state of this frontier of exoplanetary atmospheres may be summarized as follows. We have entered the era of comparative exoplanetology thanks to high-fidelity atmospheric observations now available for tens of exoplanets. Access provided by Florida International University on 01/17/21. For personal use only. Annu. Rev. Astron. Astrophys. 2019.57:617-663. Downloaded from www.annualreviews.org Recent studies reveal a rich diversity of chemical compositions and atmospheric processes hitherto unseen in the Solar System. Elemental abundances of exoplanetary atmospheres place impor- tant constraints on exoplanetary formation and migration histories.
    [Show full text]
  • Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland)
    Abstracts of Extreme Solar Systems 4 (Reykjavik, Iceland) American Astronomical Society August, 2019 100 — New Discoveries scope (JWST), as well as other large ground-based and space-based telescopes coming online in the next 100.01 — Review of TESS’s First Year Survey and two decades. Future Plans The status of the TESS mission as it completes its first year of survey operations in July 2019 will bere- George Ricker1 viewed. The opportunities enabled by TESS’s unique 1 Kavli Institute, MIT (Cambridge, Massachusetts, United States) lunar-resonant orbit for an extended mission lasting more than a decade will also be presented. Successfully launched in April 2018, NASA’s Tran- siting Exoplanet Survey Satellite (TESS) is well on its way to discovering thousands of exoplanets in orbit 100.02 — The Gemini Planet Imager Exoplanet Sur- around the brightest stars in the sky. During its ini- vey: Giant Planet and Brown Dwarf Demographics tial two-year survey mission, TESS will monitor more from 10-100 AU than 200,000 bright stars in the solar neighborhood at Eric Nielsen1; Robert De Rosa1; Bruce Macintosh1; a two minute cadence for drops in brightness caused Jason Wang2; Jean-Baptiste Ruffio1; Eugene Chiang3; by planetary transits. This first-ever spaceborne all- Mark Marley4; Didier Saumon5; Dmitry Savransky6; sky transit survey is identifying planets ranging in Daniel Fabrycky7; Quinn Konopacky8; Jennifer size from Earth-sized to gas giants, orbiting a wide Patience9; Vanessa Bailey10 variety of host stars, from cool M dwarfs to hot O/B 1 KIPAC, Stanford University (Stanford, California, United States) giants. 2 Jet Propulsion Laboratory, California Institute of Technology TESS stars are typically 30–100 times brighter than (Pasadena, California, United States) those surveyed by the Kepler satellite; thus, TESS 3 Astronomy, California Institute of Technology (Pasadena, Califor- planets are proving far easier to characterize with nia, United States) follow-up observations than those from prior mis- 4 Astronomy, U.C.
    [Show full text]
  • Ground-Based Search for the Brightest Transiting Planets with the Multi-Site All-Sky Camera - MASCARA
    Ground-based search for the brightest transiting planets with the Multi-site All-Sky CAmeRA - MASCARA Ignas A. G. Snellena, Remko Stuika, Ramon Navarrob, Felix Bettonvilb, Matthew Kenworthya, Ernst de Mooijc , Gilles Ottena , Rik ter Horstb & Rudolf le Poolea aLeiden Observatory, Leiden University, Postbus 9513, 2300 RA, Leiden, The Netherlands bNOVA Optical and Infrared Instrumentation Division at ASTRON, PO Box 2, 7990 AA, Dwingeloo, The Netherlands cDepartment of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada ABSTRACT The Multi-site All-sky CAmeRA MASCARA is an instrument concept consisting of several stations across the globe, with each station containing a battery of low-cost cameras to monitor the near-entire sky at each location. Once all stations have been installed, MASCARA will be able to provide a nearly 24-hr coverage of the complete dark sky, down to magnitude 8, at sub-minute cadence. Its purpose is to find the brightest transiting exoplanet systems, expected in the V=4-8 magnitude range - currently not probed by space- or ground-based surveys. The bright/nearby transiting planet systems, which MASCARA will discover, will be the key targets for detailed planet atmosphere obs ervations. We present studies on the initial design of a MASCARA station, including the camera housing, domes, and computer equipment, and on the photometric stability of low-cost cameras showing that a precision of 0.3-1% per hour can be readily achieved. We plan to roll out the first MASCARA station before the end of 2013. A 5-station MASCARA can within two years discover up to a dozen of the brightest transiting planet systems in the sky.
    [Show full text]
  • KELT-25 B and KELT-26 B: a Hot Jupiter and a Substellar Companion Transiting Young a Stars Observed by TESS
    Swarthmore College Works Physics & Astronomy Faculty Works Physics & Astronomy 9-1-2020 KELT-25 B And KELT-26 B: A Hot Jupiter And A Substellar Companion Transiting Young A Stars Observed By TESS R. R. Martínez R. R. Martínez Follow this and additional works at: https://works.swarthmore.edu/fac-physics B. S. Gaudi Part of the Astrophysics and Astronomy Commons J.Let E. us Rodriguez know how access to these works benefits ouy G. Zhou Recommended Citation See next page for additional authors R. R. Martínez, R. R. Martínez, B. S. Gaudi, J. E. Rodriguez, G. Zhou, J. Labadie-Bartz, S. N. Quinn, K. Penev, T.-G. Tan, D. W. Latham, L. A. Paredes, J. F. Kielkopf, B. Addison, D. J. Wright, J. Teske, S. B. Howell, D. Ciardi, C. Ziegler, K. G. Stassun, M. C. Johnson, J. D. Eastman, R. J. Siverd, T. G. Beatty, L. Bouma, T. Bedding, J. Pepper, J. Winn, M. B. Lund, S. Villanueva Jr., D. J. Stevens, Eric L.N. Jensen, C. Kilby, J. D. Crane, A. Tokovinin, M. E. Everett, C. G. Tinney, M. Fausnaugh, David H. Cohen, D. Bayliss, A. Bieryla, P. A. Cargile, K. A. Collins, D. M. Conti, K. D. Colón, I. A. Curtis, D. L. Depoy, P. Evans, D. L. Feliz, J. Gregorio, J. Rothenberg, D. J. James, M. D. Joner, R. B. Kuhn, M. Manner, S. Khakpash, J. L. Marshall, K. K. McLeod, M. T. Penny, P. A. Reed, H. M. Relles, D. C. Stephens, C. Stockdale, M. Trueblood, P. Trueblood, X. Yao, R. Zambelli, R. Vanderspek, S.
    [Show full text]
  • An Ultrahot Neptune in the Neptune Desert
    LETTERS https://doi.org/10.1038/s41550-020-1142-z An ultrahot Neptune in the Neptune desert James S. Jenkins 1,2 ✉ , Matías R. Díaz1,2, Nicolás T. Kurtovic1, Néstor Espinoza 3, Jose I. Vines1, Pablo A. Peña Rojas1, Rafael Brahm 4,5,40, Pascal Torres4, Pía Cortés-Zuleta 1, Maritza G. Soto6, Eric D. Lopez7, George W. King8,9, Peter J. Wheatley 8,9, Joshua N. Winn 10, David R. Ciardi11, George Ricker12, Roland Vanderspek13, David W. Latham14, Sara Seager 12,15, Jon M. Jenkins 16, Charles A. Beichman11, Allyson Bieryla 14, Christopher J. Burke12, Jessie L. Christiansen 11, Christopher E. Henze16, Todd C. Klaus16, Sean McCauliff16, Mayuko Mori 17, Norio Narita 18,19,20,21,22, Taku Nishiumi 23, Motohide Tamura 17,20,21, Jerome Pitogo de Leon17, Samuel N. Quinn14, Jesus Noel Villaseñor12, Michael Vezie12, Jack J. Lissauer 16, Karen A. Collins 14, Kevin I. Collins 24, Giovanni Isopi25, Franco Mallia25, Andrea Ercolino25, Cristobal Petrovich26,27, Andrés Jordán5,28, Jack S. Acton29, David J. Armstrong 8,9, Daniel Bayliss 8, François Bouchy30, Claudia Belardi29, Edward M. Bryant8,9, Matthew R. Burleigh29, Juan Cabrera 31, Sarah L. Casewell 29, Alexander Chaushev32, Benjamin F. Cooke8,9, Philipp Eigmüller 31, Anders Erikson31, Emma Foxell8,9, Boris T. Gänsicke8, Samuel Gill8,9, Edward Gillen33, Maximilian N. Günther 12, Michael R. Goad29, Matthew J. Hooton 34, James A. G. Jackman8,9, Tom Louden8,9, James McCormac8,9, Maximiliano Moyano35, Louise D. Nielsen30, Don Pollacco8,9, Didier Queloz 33, Heike Rauer31,32,36, Liam Raynard29, Alexis M. S. Smith 31, Rosanna H. Tilbrook29, Ruth Titz-Weider31, Oliver Turner30, Stéphane Udry 30, Simon.
    [Show full text]
  • Atmospheres of Hot Alien Worlds
    Atmospheres of hot alien Worlds Atmospheres of hot alien Worlds Proefschrift ter verkrijging van de graad van Doctor aan de Universiteit Leiden, op gezag van Rector Magnificus prof.mr. C.J.J.M. Stolker, volgens besluit van het College voor Promoties te verdedigen op donderdag 5 juni 2014 klokke 10.00 uur door Matteo Brogi geboren te Grosseto, Italië in 1983 Promotiecommissie Promotors: Prof. dr. I. A. G. Snellen Prof. dr. C. U. Keller Overige leden: Prof. dr. C. Dominik University of Amsterdam Prof. dr. K. Heng University of Bern Prof. dr. E. F. van Dishoeck Dr. M. A. Kenworthy Prof. dr. H. J. A. Röttgering Ai miei genitori, per aver creduto in me, permettendomi di realizzare un sogno Contents 1 Introduction 1 1.1 Planet properties from transits and radial velocities . 2 1.2 Atmospheric characterization of exoplanets . 4 1.2.1 Atmospheres of transiting planets . 4 1.2.2 Challenges of space- and ground-based observations . 7 1.2.3 Ground-based, high resolution spectroscopy . 8 1.2.4 A novel data analysis . 10 1.3 Close-in planets and their environment . 10 1.3.1 From atmospheric escape to catastrophic evaporation . 12 1.4 This thesis . 12 2 The orbital trail of the giant planet t Boötis b 17 2.1 The CRIRES observations . 18 2.2 Data reduction and analysis . 19 2.2.1 Initial data reduction . 19 2.2.2 Removal of telluric line contamination . 19 2.2.3 Cross correlation and signal extraction . 21 2.3 The CO detection and the planet velocity trail .
    [Show full text]
  • The Multi-Site All-Sky Camera (MASCARA)
    A&A 601, A11 (2017) Astronomy DOI: 10.1051/0004-6361/201630319 & c ESO 2017 Astrophysics The Multi-site All-Sky CAmeRA (MASCARA) Finding transiting exoplanets around bright (mV < 8) stars G. J. J. Talens1, J. F. P. Spronck1, A.-L. Lesage1, G. P. P. L. Otten1, R. Stuik1, D. Pollacco2, and I. A. G. Snellen1 1 Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] 2 Department of Physics, University of Warwick, Coventry CV4 7AL, UK Received 22 December 2016 / Accepted 9 February 2017 ABSTRACT This paper describes the design, operations, and performance of the Multi-site All-Sky CAmeRA (MASCARA). Its primary goal is to find new exoplanets transiting bright stars, 4 < mV < 8, by monitoring the full sky. MASCARA consists of one northern station on La Palma, Canary Islands (fully operational since February 2015), one southern station at La Silla Observatory, Chile (operational from early 2017), and a data centre at Leiden Observatory in the Netherlands. Both MASCARA stations are equipped with five interline CCD cameras using wide field lenses (24 mm focal length) with fixed pointings, which together provide coverage down to airmass 3 of the local sky. The interline CCD cameras allow for back-to-back exposures, taken at fixed sidereal times with exposure times of 6.4 sidereal seconds. The exposures are short enough that the motion of stars across the CCD does not exceed one pixel during an integration. Astrometry and photometry are performed on-site, after which the resulting light curves are transferred to Leiden for further analysis.
    [Show full text]
  • The Science of Echo Exoplanet Characterisation Observatory
    The science of EChO Exoplanet Characterisation Observatory Giovanna Tinetti & EChO consortium UK, France, Italy, Spain, MPS Germany, Poland, Denmark, Ireland,Un. Liege, Portugal, Hungary, US ~850 Exoplanets! Radial velocity, Transit Surveys Microlensing, Direct detec. ESA-GAIA -> 104 new planets! 1 The science of EChO – ROPACS ~250 Exoplanets (+x000 candidates) Radius, Mass & Orbit 2 The science of EChO – ROPACS 16/11/12 Exoplanets for which we have spectra: < 20 H2O, CO, CH 4, CO2, Na etc. identified, but data are sparse, degeneracy of interpretation Swain et al., 2009 3 The science of EChO – ROPACS 16/11/12 EPSC-DPS 2011 TESS PLATO E-ELT HUBBLE CoRoT VLT Finesse Early years The present The golden future 2000 2005 2010 2020 EChO Spitzer GAIA JWST Kepler Cheops SPICA 4 Big picture? 5 The science of EChO – ROPACS EChO Exoplanet Characterisation Observatory ESA M3 mission candidate – March 2011 ESA Science Team ESA EChO Study Team ØG. Tinetti ØK. Isaak ØP. Drossart ØL.Puig ØO. Krause ØM. Linder ØC. Lovis ØG. Micela ØM. Ollivier ØI. Ribas ØI. Snellen ØB. Swinyard Gaseous planets formed elsewhere and migrated Planet formation Energy budget C/O ratio Albedo/thermal emission Planet-star interaction Photochemistry+ Weather Day/night variation Temporal variability/ T-P profile Planet evolution + Escape/H3 8 The science of EChO – ROPACS 16/11/12 Terrestrial planets formed in situ? Or remnant of gaseous planets’ core? Primary or secondary atmosphere? Does the planet have H2 retained or not an atmosphere? Energy budget Spectral observations Albedo/thermal
    [Show full text]
  • Considerations for Planning TESS Extended Missions
    Considerations for planning TESS Extended Missions This document is intended to be a useful reference for those who are planning and proposing for TESS Extended Missions. It is a repository of ideas, questions, and links to relevant work regarding possible Extended Missions. The intention is to capture and organize ideas from the TESS Science Team in order to expedite and facilitate decision-making and proposal writing. An extended mission offers the chance to re-examine our top-level science priorities, sky scanning pattern, selection of short-cadence target stars, allocation of data volume between "target stars" and full-frame images, and many other mission parameters. Given the broad range of possibilities, we hope to gather input from a broad community of Co-investigators, Collaborators, Working Group members, Guest Investigators, Engineers, and other interested parties. The Simulations Working Group has prepared a memorandum (Bouma et al.) about 6 specific scenarios for a one-year Extended Mission. The scenarios are: 1. HEMI, which re-observes one of the ecliptic hemispheres in essentially the same manner as in the Primary Mission (i.e., neglecting the zone within 6° of the ecliptic); 2. HEMI+ECL, which re-observes one of the ecliptic hemispheres, but this time covering the entire hemisphere at the expense of the continuous-viewing zone near the pole; 3. POLE, which focuses on one of the two ecliptic poles; 4. ECL-LONG, which has a series of pointings with the long axis of the field-of-view along the ecliptic (in combination with some fields near the ecliptic pole, when the Earth or Moon would prevent effective observations of the ecliptic); 5.
    [Show full text]
  • Abstracts Book
    LIST OF PARTICIPANTS - INVITED AND CONTRIBUTED PAPERS - POSTERS TABLE OF CONTENTS List of participants p.2 to 4 Abstracts of oral communications Invited and contributed papers p. 5 to 83 Abstract of posters p. 85 to 122 Index p. 122 to 123 1 LIST OF PARTICIPANTS ADAMCZYK Michalina Toru´nCentre for Astronomy AKHENAK La¨etitia Institut d’Astrophysique de Paris ALIBERT Yann Physikalisches Institut, University of Bern ALLARD Nicole GEPI, Observatoire de Paris ALVES DE OLIVEIRA Catarina European Space Agency AUCLAIR-DESROTOUR Pierre IMCCE, Observatoire de Paris BARAFFE Isabelle Group of Astrophsics, University of Exeter BATALHA Natalie NASA Ames Research Center BAYLISS Daniel Observatoire de Gen`eve BEAULIEU Jean-Philippe Institut d’Astrophysique de Paris BENNEKE Bjrn California Institute of Technology BENNETT David University of Notre Dame BERTA-THOMPSON Zachory Massachusetts Institute of Technology BOFFIN Henri European Southern Observatory BOISSE Isabelle Laboratoire d’Astrophysique de Marseille BONOMO Aldo Stefano Observatorio Astrofisico di Torino BORGNIET Simon Institut de Plan´etologie et d’Astrophysique de Grenoble BOUE´ Gwena¨el IMCCE, Observatoire de Paris BOURRIER Vincent Observatoire de Gen`eve BROGI Matteo University of Colorado at Boulder BRUNO Giovanni Laboratoire d’Astrophysique de Marseille BRYAN Marta California Institute of Technology CARLEO Ilaria Astronomical Observatory of Padua CASSAN Arnaud Institut dAstrophysique de Paris CHABRIER Gilles Centre de Recherche en Astrophysique de Lyon CHARBONNEAU David Harvard Center for
    [Show full text]
  • Discovery of WASP-174B: Doppler Tomography of a Near-Grazing Transit
    MNRAS 000,1{8 (2018) Preprint 10 August 2018 Compiled using MNRAS LATEX style file v3.0 Discovery of WASP-174b: Doppler tomography of a near-grazing transit L.Y. Temple,1? C. Hellier1, Y. Almleaky2;3, D.R. Anderson1, F. Bouchy4, D.J.A. Brown5;6, A. Burdanov8, A. Collier Cameron7, L. Delrez9, M. Gillon8, R. Hall9, E. Jehin8, M. Lendl10;4, P.F.L. Maxted1, L. D. Nielsen4, F. Pepe4, D. Pollacco5;6, D. Queloz9, D. S´egransan4, B. Smalley1, S. Sohy8, S. Thompson9, A.H.M.J. Triaud11, O.D. Turner4;1, S. Udry4, R.G. West5 1Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK 2Space and Astronomy Department, Faculty of Science, King Abdulaziz University, 21589 Jeddah, Saudi Arabia 3King Abdullah Centre for Crescent Observations and Astronomy (KACCOA), Makkah Clock, Saudia Arabia 4Observatoire astronomique de l'Universit´ede Gen`eve 51 ch. des Maillettes, 1290 Sauverny, Switzerland 5Department of Physics, University of Warwick, Gibbet Hill Road, Coventry, CV4 7AL, UK 6Centre for Exoplanets and Habitability, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 7SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK 8Space sciences, Technologies and Astrophysics Research (STAR) Institute, Universit´ede Li`ege, All´ee du 6 Ao^ut17, 4000 Li`ege, Belgium 9Cavendish Laboratory, J J Thomson Avenue, Cambridge, CB3 0HE, UK 10Space Research Institute, Austrian Academy of Sciences, Schmiedlstr. 6, 80 42, Graz, Austria 11School of Physics & Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We report the discovery and tomographic detection of WASP-174b, a planet with a near-grazing transit on a 4.23-d orbit around a V = 11.9, F6V star with [Fe/H] = 0.09 ± 0.09.
    [Show full text]