Planets in Binary Systems Searching for High Contrast Binaries with ShaneAO Lea Hirsch 3 rd Year Graduate Student UC Berkeley Department of Astronomy

Slides:

Advertisements

Similar presentations

General Astrophysics with TPF-C David Spergel Princeton.

Advertisements

High Contrast AO Imaging at the MMT with ARIES SDI Laird Close, Beth Biller, Eric Nielsen Don McCarthy & MMT AO Group (Steward Obs)

20 April 2001AAO Workshop1 Optical & IR Interferometry Bill Tango School of Physics University of Sydney.

N EW ULTRA COLD DWARF BINARIES New discoveries and follow up observations University of Hertfordshire Joana Gomes.

Overview on Extra Solar Planets Rahul I. Patel PHY 599 – Grad Seminar Oct. 18 th 2010.

CHARA Collaboration Year-Five Science Review A Survey of Stellar Families Multiplicity of Solar-type Stars Deepak Raghavan Ph.D. Dissertation Talk March.

Deriving the true mass of an unresolved BD companion by AO aided astrometry Eva Meyer MPIA, Heidelberg Supervisor: Martin Kürster New Technologies for.

Observing binaries with GAIA: large gains after much effort... Staffan Söderhjelm Lund Observatory.

Science with the Very Large Telescope Interferometer (VLT-I) Jean-Baptiste Le Bouquin (ESO, Chile) for VLTI Team, AMBER team, MIDI team, PRIMA team… The.

The new version of Binary stars database (BDB) P. Kaygorodov 1, B. Debray 2, N. Kolesnikov 3, D. Kovaleva 1, O. Malkov 1 1 INASAN, 2 Observatoire de Besançon,

Gaspard Duchêne (UC Berkeley, Obs. Grenoble) Andy Boden (Caltech), Guillermo Torres (CfA Harvard), Andrea Ghez (UCLA), Quinn Konopacky (LLNL) Keck Science.

Science Team Management Claire Max Sept 14, 2006 NGAO Team Meeting.

Other Science from Microlensing Surveys I or Microlenses as Stellar Probes By Jonathan Devor.

TIGER The TIGER Instrument Overview Phil Hinz - PI July 13, 2010.

Near & Long Term Planet Searches (not a review) S. R. Kulkarni California Institute of Technology.

The Stars: A Celestial Census

The Next 25(?) Years Future Missions to Search for Extra-solar Planets and Life.

Intensity and Distance Intensity depends on luminosity and distance Inverse-square law discovered by Newton Magnitude system used in astronomy.

M. Shao - 1 SIM Space Interferometry Mission A NASA Origins Mission SIM GRID.

Robo-AO First Science Workshop May 20, The Demo Period Robo-AO Science Workshop Agenda.

19 July 2005Yale Astrometry Workshop / Horch 21 Optical Interferometry Elliott Horch, University of Massachusetts Dartmouth, USA.

The true orbits of visual binaries can be determined from their observed orbits as projected in the plane of the sky. Once the true orbit has been computed,

22 March 2005 AST 2010: Chapter 171 The Stars: A Celestial Census.

Adam L. Kraus February 1, 2007 Multiple Star Formation at the Bottom of the IMF.

Chapter 14 Our Galaxy The Milky Way Revealed Our Goals for Learning What does our galaxy look like? How do stars orbit in our galaxy?

The Nature of the Stars Chapter 19. Parallax.

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

Astrometry of Binary Stars: What Are We Waiting For? Elliott Horch, Southern Connecticut State University 9/21/20081Stars in Motion BU 151AB 1 arcsec Andor.

ISNS Phenomena of Nature 1. Imaging –use a camera to take pictures (images) –Photometry  measure total amount of light from an object 2.Spectroscopy.

Constellations and Planets in the Night Sky Created for TCSS.

CHARA Collaboration Year-Five Science Review. The Separated Fringe Packet Survey Chris Farrington CHARA / Mt. Wilson March 2009 Collaborators: T.A ten.

The B-V colors and photometric variability of Nix and Hydra, Pluto’s two small satellites Max Mutchler (STScI) S. Alan Stern (SwRI) Hal Weaver (JHU/APL)

Olivier Absil Chargé de Recherches FNRS AEOS group 3 rd ARC meeting – March 4 th, 2011 Imaging faint companions with interferometric closure phases 3 rd.

Clio: 3-5  m planet-finding AO camera Ari Heinze (Steward Observatory) Collaborators: P. Hinz (Steward), S. Sivanandam (Steward), M. Freed (Optical Sciences),

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,

Searching for Brown Dwarf Companions to Nearby Stars Michael W. McElwain, James E. Larkin & Adam J. Burgasser (UC Los Angeles) Background on Brown Dwarfs.

AST 443/PHY 517 : Observational Techniques November 6, 2007 ASTROMETRY By: Jackie Faherty.

The Planets of Other Stars. The Astronomy Diagnostic Test (ADT): The Sequel On the first day of class, the University requested that everyone fill out.

Albireo: The Boy Scout star Chapter 5: Binary stars and stellar masses.

The Nature of the Stars Chapter 19. Parallax.

DARWIN The InfraRed Space Interferometer. Status of exo-planet search Stars (Solar type) observed: Planets detected: ~ 86 Radial velocity measurement.

Discriminating Planetary Migration Mechanisms by Direct Imaging Norio Narita National Astronomical Observatory of Japan on behalf of SEEDS/HiCIAO/AO188.

A Dedicated Search for Transiting Extrasolar Planets using a Doppler Survey and Photometric Follow-up A Proposal for NASA's Research Opportunities in Space.

Direct imaging of substellar objects around young and nearby stars: The SACY sample N. Huélamo (Laeff-INTA, Spain) H. Bouy (UC Berkeley) C. Torres (LNA,

23 November 2015what do we know from the exo-planets? Florian Rodler What do we know about the exo-planets? & How to detect direct signals from exo-planets?

The Search for Extra-Solar Planets Dr Martin Hendry Dept of Physics and Astronomy.

April 2001 OPTICON workshop in Nice 1 PSF-fitting with SExtractor Emmanuel BERTIN (TERAPIX)

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

Early science on exoplanets with Gaia A. Mora 1, L.M. Sarro 2, S. Els 3, R. Kohley 1 1 ESA-ESAC Gaia SOC. Madrid. Spain 2 UNED. Artificial Intelligence.

15 Dec 2005GWDAW 10 LIGO-G Z1 Overview of LIGO Scientific Collaboration Inspiral Searches Alexander Dietz Louisiana State University for the LIGO.

Eva Meyer MPIA-Student-Workshop, Italy Various information from different detection methods.

Binary Stars (Chapter 21 of book). The Types of Binary Stars Visual Binaries Eclipsing Binaries Spectroscopic Binaries.

Universe Tenth Edition Chapter 17 The Nature of the Stars Roger Freedman Robert Geller William Kaufmann III.

1 VLBA Orbits of Young Binary Stars Rosa M. Torres – CRyA, UNAM Laurent Loinard – CRyA, UNAM Amy Mioduszewski – DSOC, NRAO Luis F. Rodríguez – CRyA, UNAM.

July 25th, 2000WFC3 Critical Science Review1 Performance Summary in Key Science Areas Verify that WFC3 as designed is capable of carrying out the WFC3.

CONSTELLATIONS. WHAT are they? When we look into the night sky, it appears that everything is attached to the “dome” of the sky.

Extra Solar Planet Science With a Non Redundant mask

S4E1 Students will compare and contrast the physical attributes of stars, star patterns, and planets. Recognize the physical attributes of stars in the.

Chapitre 1- Introduction

Gemini South telescope makes the case for multiple Earth-sized planets

Exoplanets EXOPLANETS Talk prepared by: Santanu Mohapatra(14PH20032)

GPI Astrometric Calibration

Subaru Measurements of the Rossiter-McLaughlin Effect

An Overview of the HST Treasury Program on the Orion Nebula

Observing Very Young Stars with GPI

Goals Explain how we measure stellar distances Explain the difference between apparent and absolute brightness Explain how we classify stars Describe the.

Presentation transcript:

Planets in Binary Systems Searching for High Contrast Binaries with ShaneAO Lea Hirsch 3 rd Year Graduate Student UC Berkeley Department of Astronomy ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley

Project Overview ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley 25 pc Volume-Limited Stellar Sample: 0.55 < B-V < 1.1 (F8 – K5) Within +/- 1 M V of Main Sequence Distance < 25 pc Declination > -10°

Science Goals ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley CHARA interferometry (Raghavan 2010) V band RoboAO (Riddle+ 2014) i’ band SB2 (Kolbl+ 2014) SB1 HIRES RV Trends (But no orbital solutions or companion masses) ShaneAO K s band (arcsec)

ShaneAO Methodology ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley Finger E - W orientation of finger K s filter 3 x 30-second integrations per position 5 x 30-second skies per star Srinath+ 2014

Speckle Structure ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley July 16, 2014 HIP 64979HD HD HD HD HD HD HD HD HD HIP HD HD HIP HIP 1473

Speckle Structure ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley Nov 4, 2014 HIP HIP HD HD HD 1160HD 1461 HD 3196 HD 4356HD 4915HD 6101HD 10008HD 13798HD 16160HD HD 18632HD 20619HD HD 22484HD HD 26913HD HD 35112HD 38858HD 42618HD 43587HD 50281HD HD 60491

LOCI Algorithm ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley PSF reconstruction from reference images all images from same night reconstruct small “optimization regions” as weighted sum of reference images HD Lafrenière+ 2007

LOCI Algorithm ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley PSF reconstruction from reference images all images from same night reconstruct small “optimization regions” as weighted sum of reference images HIP

LOCI Algorithm ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley PSF reconstruction from reference images all images from same night reconstruct small “optimization regions” as weighted sum of reference images HIP

Future Outlook Improve LOCI code Astrometry : using diffraction spikes to accurately determine stars’ locations Return to these systems next year to check common proper motion for any faint companions detected ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley

Final Questions ShaneAO Workshop  Dec 17, 2014 at UCSC Lea Hirsch  UC Berkeley Why is the appearance of the speckles different from one hour/night to the next? Can ShaneAO be optimized to minimize the speckles? Is there a better algorithm than LOCI to carry out PSF reconstruction and reveal faint companions?