First Detection of Polarized Scattered Light from an Exoplanetary Atmosphere Berdyugina et al. (12/2007) Florian Herzele SE Aktuelle Forschung zu Extrasolaren.

Slides:

Advertisements

Similar presentations

II Escuela de Optica Biomedica, Puebla, 2011 Polarimeters Jessica C. Ramella-Roman, PhD.

Advertisements

GN/MAE155B1 Orbital Mechanics Overview 2 MAE 155B G. Nacouzi.

II Escuela de Optica Biomedica, Puebla, 2011 Modeling of polarized light transfer in scattering media Monte Carlo.

Asteroid’s Thermal Models AS3141 Benda Kecil dalam Tata Surya Prodi Astronomi 2007/2008 Budi Dermawan.

7. Radar Meteorology References Battan (1973) Atlas (1989)

Polarization of Light Waves

Binary Systems and Stellar Parameters The Classification of Binary Stars Mass Determination using visual Binaries Eclipsing,Spectroscopic Binaries The.

1 Determining the internal structure of extrasolar planets, and the phenomenon of retrograde planetary orbits Rosemary Mardling School of Mathematical.

HIGH-PRECISION PHOTOMETRY OF ECLIPSING BINARY STARS John Southworth + Hans Bruntt + Pierre Maxted + many others.

Phase Light Curves for Extrasolar Jupiters and Saturns U. Dyudina(5/1), P.Sackett(1), D. Bayliss(1), L Dones(2), H. Throop (2), C. Porco(3), S. Seager(4)

Theoretical Spectra and Atmospheres of Extrasolar Giant Planets (Sudarsky, Burrows, Hubeny 2003) Nick Cowan March 2006 Nick Cowan March 2006.

Phase Light Curves for Extrasolar Jupiters and Saturns ASA meeting, July 6, 2004 U. Dyudina(1), P.Sackett(1), D. Bayliss(1), L Dones(2), H. Throop (2),

New Moons Around Pluto Jau-Shian Liang Department of Physics, NTHU 2005/11/24.

Are there Planets outside the Solar System ? First answer : 1992 Discovery of the first Extra-Solar Planet around the pulsar PSR (Wolszczan &Frail)

Extrasolar Planets.I. 1.What do we know and how do we know it. 2.Basic planetary atmospheres 3.Successful observations and future plans.

Reflected Light From Extra Solar Planets Modeling light curves of planets with highly elliptical orbits Daniel Bayliss, Summer Student, RSAA, ANU Ulyana.

Lunar Observations of Changes in the Earth’s Albedo (LOCEA) Alexander Ruzmaikin Jet Propulsion Laboratory, California Institute of Technology in collaboration.

Satellite Orbits 인공위성 궤도

Polarimetry in Astronomy Or Do you know where your photons are coming from? Elizabeth Corbett AAO.

Dynamical modeling of the DI dust ejecta cloud Tanyu Bonev (Institute of Astronomy and National Astronomical Observatory, Bulgaria) and the ESO DI observing.

Multi-Frequency Circular Polarization Measurements of the Quasar 3C279 At Centimeter Wavelengths H.D. Aller and M.F. Aller (U. of Michigan) Introduction.

„We are not talking about cosmology...“ (A. Sozzetti)

Layers of the Solar Atmosphere Corona Chromosphere Photosphere Details of solar activity can be seen more easily in the hotter outer layers, which are.

What stellar properties can be learnt from planetary transits Adriana Válio Roque da Silva CRAAM/Mackenzie.

Nadiia Kostogryz & Svetlana Berdyugina

The mass ratio of the stellar components of a spectroscopic binary can be directly computed from their ratio in radial velocities. To derive the total.

SCIENCE PROGECT. The Earth Earth, which is our base from which we look into space, is constantly moving. Understanding this movement is one of the most.

Adriana V. R. Silva CRAAM/Mackenzie COROT /11/2005.

9.3 – Perform Reflections.

THE DIURNAL TEMPERATURE REGIME OF THE SURFICIAL REGOLITH OF PHOBOS IN THE LANDING SITE REGION OF THE FOBOS-GRUNT LANDER FOR DIFFERENT SEASONS: THE MODEL.

200 MG 500 MG TheoryObservation Authors Institutes RE J is a hydrogen rich strongly magnetic white dwarf discovered as an EUV source by the ROSAT.

Extrasolar planets. Detection methods 1.Pulsar timing 2.Astrometric wobble 3.Radial velocities 4.Gravitational lensing 5.Transits 6.Dust disks 7.Direct.

PHYSICAL CHARACTERIZATION OF ASTEROIDS NEON Group 5: Koraljka Mužić Nikola Vitas Grzegorz Nowak Mario Mars Simone Marchi (tutor) 5 th NEON SCHOOL, OHP,

Search for planetary candidates within the OGLE stars Adriana V. R. Silva & Patrícia C. Cruz CRAAM/Mackenzie COROT /11/2005.

Subaru HDS Transmission Spectroscopy of the Transiting Extrasolar Planet HD b The University of Tokyo Norio Narita collaborators Yasushi Suto, Joshua.

1B11 Foundations of Astronomy Extrasolar Planets Liz Puchnarewicz

The Search for Extrasolar Planets Since it appears the conditions for planet formation are common, we’d like to know how many solar systems there are,

Diversity of Data in the Search for Exoplanets Rachel Akeson NASA Exoplanet Science Institute California Institute of Technology.

Photometric detection of the starlight reflection by a “Pegasi” planet Martin Vannier (1), Tristan Guillot (2), Suzanne Aigrain (1) (1) ESO, Chile (2)

Transit Searches: Technique. The “Transit” Method Viewing angle ~ orbital plane! Delta L / L ~ ( R planet / R star ) 2 Jupiter: ~ 1-2 % Earth: ~

Explorations of the Outer Solar System B. Scott Gaudi Harvard-Smithsonian Center for Astrophysics.

Dirk Terrell Southwest Research Institute Dirk Terrell Southwest Research Institute Eclipsing Binary.

Asteroids Rotation Period Study the photometric curve Rotation period Shape Is it binary? Surface composition spectroscopy.

Extrasolar planets. Detection methods 1.Pulsar Timing Pulsars are rapidly rotating neutron stars, with extremely regular periods Anomalies in these periods.

Polarimetry in Astronomy Or Do you know where your photons are coming from? Elizabeth Corbett AAO.

Spectroscopic Transits

Spin-Orbit Alignment Angles and Planetary Migration of Jovian Exoplanets Norio Narita National Astronomical Observatory of Japan.

8.2 Area of a Surface of Revolution

The University of Tokyo Norio Narita

 s r p/s Return Visit Optimization for Planet Finding Missions Dmitry Savransky and N. Jeremy Kasdin, Princeton University Abstract We present and expand.

Polarized Light from Exoplanets: The Key to Clouds and Hazes?

9.3 – Perform Reflections. Reflection: Transformation that uses a line like a mirror to reflect an image Line of Reflection: Mirror line in a reflection.

Introduction to On-Orbit Thermal Environments

Timing Transits to Find Extrasolar Earths Eric Agol, Jason Steffen (UW) Re’em Sari (Caltech) Will Clarkson (Southampton) (MNRAS, in press)

R EMOTE DETECTION OF BIOLOGICAL PIGMENTS BY SPECTRO - POLARIMETRY Svetlana BERDYUGINA 1,2, Tina ŠANTL-TEMKIV 3, Kai FINSTER 3,4, Jefferey R. KUHN 2, Dave.

Biosignatures Svetlana Berdyugina

Measuring the Spin-Orbit Alignments of Transiting Exoplanetary Systems: The Case for TrES-1 Norio Narita, Keigo Enya, Bun'ei Sato, Yasuhiro Ohta, Joshua.

IAU253 Transiting Planets: May

1 / 12 Simultaneous Spectroscopic & Photometric Observations of a Transit of TrES-1b Norio Narita (UT, JSPS Fellow) Collaborators K. Enya (JAXA), B. Sato.

Pre-Cursor Data Needed for JWST Transit and Eclipse Observations

SPARTAN-V Selective Pointing Apparatus for Research of Turbulence and Atmospheric Noise Variation Brian Ibeling and Christopher Nie.

UVIS Calibration Update

Photometric Analysis of Asteroids

UVIS Calibration Update

Universal Gravitation

Norio Narita National Astronomical Observatory of Japan

Direct imaging discovery of a Jovian exoplanet within a triple-star system by Kevin Wagner, Dániel Apai, Markus Kasper, Kaitlin Kratter, Melissa McClure,

The University of Tokyo Norio Narita

Scattering in Planetary Atmospheres

Presentation transcript:

First Detection of Polarized Scattered Light from an Exoplanetary Atmosphere Berdyugina et al. (12/2007) Florian Herzele SE Aktuelle Forschung zu Extrasolaren Planeten WS 07/08

Planetary Atmospheres Light scattered in planetary atmospheres is linearly polarized perpendicular to scattering plane Characterized by Stokes parameters q and u, normalized to total flux During revolution scattering angle changes = Stokes parameters vary  Determination of orbital parameters

System HD NameHD b Discovered in2005 M.sin i1.15 (± 0.046) MJ Semi major axis (± ) AU Orbital period (± 2e-05) days Eccentricity0 Radius1.156 (± 0.032) RJ T transit (± ) Inclination85.76 (± 0.29) deg. Update18/04/07

What they did and how Observations in with double image CCD polarimeter remotely controlled 60cm KVA telescope on La Palma Rotating superachromatic plate as retarder and calcite plate as analyzer Cylces of 16 exposures (retarder rotated at 22.5°)

Stokes Parameter X-axis: north-south Y-axis: east-west

When they did it 2006: 10-15s 2x16 positions;  = % 2007: 20-30s 4x16 positions;  = % Overall: 93 nightly measurements for each Stokes parameter

Obtained Data

Assumptions Lambert sphere approximation Rayleigh scattering  2 minimization procedure Simulated sample of Monte Carlo measurements

Lambert Sphere light falling on it is scattered such that the apparent brightness of the surface to an observer is the same regardless of the observer's angle of view Perfectly reflecting surface with geometrical albedo p=2/3

Rayleigh Scattering

 2 Distribution

Orbital Parameters Fixed paramters:orbital period P, transit / periastron epoch T 0, semi-major axis a, radius of the star R * Free parameters: eccentricity e, inclination i, longitude of the ascending node , radius of Lambert sphere R L, constant shift in Stokes parameters  u and  q

Inclination Inclination can be tested by photometric data but polarimetry can destinguish between i>90° (clockwise roation) and i<90° (counterclockwise) At i=0° q and u have the same amplitude For i≠0°: relative amplitude is influenced by , variations appear only at certain longitudes

Best-fit Solution (1)Errors of measurements have Gaussian distribution (2)Signal is not spurious (3)Solution is robust to errors

Results 180° -≈ < ≈30% if evaporating halo exists

Interpretation Excellent agreement between known values in e and i indicate plausibility of Rayleigh scattering Planet has extended atmosphere effectively scattering in blue Small particles like H, H 2, H 2 O or even small dust grains (≤ 5  m, e.g. silicate) might be present

Planetary Motion