The JWST Early Release Science Program for the Direct Imaging of Extrasolar Planetary Systems

Transcription

1 The JWST Early Release Science Program for the Direct Imaging of Extrasolar Planetary Systems Sasha Hinkley (Exeter), Aarynn Carter (Exeter), Andrew Skemer (UCSC), Beth Biller (Edinburgh), & ~120 Additional Collaborators IAU Focus Meeting 11, Vienna 22 August 2018

2 Why Image Exoplanets and Disks with JWST? 3-5µm exoplanet imaging from the ground: modest sensitivity. λ > 5µm is completely unexplored for exoplanets (Caveat: some Spitzer/AKARI observations of free-floating BDs).

3 Why Image Exoplanets and Disks with JWST? 3-5µm exoplanet imaging from the ground: modest sensitivity. λ > 5µm is completely unexplored for exoplanets (Caveat: some Spitzer/AKARI observations of free-floating BDs). SPHERE, GPI

4 Why Image Exoplanets and Disks with JWST? 3-5µm exoplanet imaging from the ground: modest sensitivity. λ > 5µm is completely unexplored for exoplanets (Caveat: some Spitzer/AKARI observations of free-floating BDs). SPHERE, GPI SPHERE, GPI Skemer et al. (2012)

5 Why Image Exoplanets and Disks with JWST? 3-5µm exoplanet imaging from the ground: modest sensitivity. λ > 5µm is completely unexplored for exoplanets (Caveat: some Spitzer/AKARI observations of free-floating BDs). JWST will transform our understanding of their physical characteristics (mass, gravity, temperature, atmospheric composition/structure). SPHERE, GPI SPHERE, GPI

6 Why Image Exoplanets and Disks with JWST? 3-5µm exoplanet imaging from the ground: modest sensitivity. λ > 5µm is completely unexplored for exoplanets (Caveat: some Spitzer/AKARI observations of free-floating BDs). JWST will transform our understanding of their physical characteristics (mass, gravity, temperature, atmospheric composition/structure). The Early Release Science Program is our first-ever chance to observe exoplanets over their full luminous range. SPHERE, GPI SPHERE, GPI

7 Why Image Exoplanets and Disks with JWST? New classes of directly imaged planets: Saturn & Neptune analogues? Image courtesy of Marshall Perrin, STScI Need: Deep understanding of optimal strategies for observations, calibrations, & data analysis.

8 Why Image Exoplanets and Disks with JWST? Characterising planetary systems must include characterising debris discs. Planets drive ring structures & geometry. H 2 O ice features have been elusive from the ground. Fomalhaut High atmospheric CO 2 opacity has prevented debris disc imaging at 15µm: a primary wavelength expected to be used for JWST debris disc imaging going forward. Kalas et al. (2008)

9 Rationale for an ERS Program HST coronagraphy still being refined (e.g. Schneider et al. 2017). Need: best understanding of instrumental response, PSF stability, and PSF subtraction methods. Basic PSF subtraction Advanced PSF subtraction Raw HST Image of HR 8799 (1998) Soummer et al. (2011)

10 Rationale for an ERS Program HST coronagraphy still being refined (e.g. Schneider et al. 2017). Need: best understanding of instrumental response, PSF stability, and PSF subtraction methods. JWST in-flight performance, data gathering strategy, & optimal post-processing not yet defined. Given JWST s relatively short 5-10 lifetime, the correct observing strategy and data processing methods must be identified as early as possible. Basic PSF subtraction Advanced PSF subtraction Raw HST Image of HR 8799 (1998) Soummer et al. (2011)

11 Aarynn Carter, UK Exoplanet Meeting 2018 The JWST Early Release Science (ERS) Program Allocation of 500 hours of Director s Discretionary time Ensure open access to representative datasets in support of the preparation of Cycle 2 proposals. Engage a broad cross-section of the astronomical community in familiarising themselves with JWST data and scientific capabilities. Mar 2021? Sep 2021??? ERS Period Launch Cycle 1 Begins Cycle 2 Proposals Due Cycle 2 Begins

12 The JWST Exoplanet Early Release Science Programs Aarynn Carter, UK Exoplanet Meeting 2018 Results of the Early Release Science Selection Out of 106 submitted proposals, 8 were in the field of exoplanets and disks. Submitted Proposals 7.5 % 13 proposals were accepted: Galaxies, IGM, Black holes (6) Stellar Physics & Populations (4) Solar System, Exoplanets (3) 132 out of 487 hours allocated to the two accepted exoplanet proposals. Allocated Time 27 %

13 High Contrast Imaging of Exoplanets and Exoplanetary Systems with JWST (52 hours) The JWST Exoplanet Early Release Science Programs Aarynn Carter, UK Exoplanet Meeting 2018 PI: Sasha Hinkley Co-PI s: Beth Biller and Andy Skemer 4 Consortium face-to-face meetings: 2016 SPIE, Edinburgh Exoplanets 1, Davos STScI, Baltimore AAS, Austin. 121 Total Team Members: 55% United States 41% Europe & Canada 25% Female Team Members 45% Female Team Leaders

14 High Contrast Imaging of Exoplanets & Exoplanetary Systems with JWST PI / Co-PI Co-Investigator Science Collaborator Sasha Hinkley Beth Biller Andy Skemer Isabelle Baraffe Mickael Bonnefoy Brendan Bowler Aarynn Carter Christine Chen Elodie Choquet Thayne Currie Camilla Danielski Jonathan Fortney Carol Grady Alex Greenbaum Dean Hines Markus Janson Paul Kalas Grant Kennedy Adam Kraus Anne-Marie Lagrange Mike Liu Mark Marley Christian Marois Brenda Matthews Dimitri Mawet Stan Metchev Michael Meyer Max Millar-Blanchaer Marshall Perrin Laurent Pueyo Sascha Quanz Julien Rameau T.J. Rodigas Stephanie Sallum Benjamin Sargent Josh Schlieder Glenn Schneider Karl Stapelfeldt Pascal Tremblin Arthur Vigan Marie Ygouf Olivier Absil Suzanne Aigrain Jo Barstow Jean-Loup Baudino Russ Belikov Gordy Bjoraker Anthony Boccaletti Mariangela Bonavita Mark Booth Jeroen Bouwman Wolfgang Brandner Zack Briesemeister Marta Bryan Faustine Cantalloutbe Ludmila Carone Benjamin Charnay Gael Chauvin Anthony Cheetham Valentin Christiaens Ian Crossfield John Debes Zach Draper Trent DuPuy Sam Factor Romain Falla Markus Feldt Mike Fitzgerald Ryan Garland Thomas Henning Michael Ireland Patrick Irwin Hannah Jang-Condell Theodora Karalidi Christoph Keller Matt Kenworthy Pierre Kervella Hubert Klahr John Krist Masayuki Kuzuhara Pierre-Olivier Lagage Ralf Launhardt Jean-Francois Lestrade James Lloyd Anne-Lisse Maire Frantz Martinache Raquel Martinez Elisabeth Matthews Nathan Mayne Johan Mazoyer Mike McElwain Tiffany Meshkat Brittany Miles Farisa Morales Katie Morzinkski David Mouillet Andre Muller Mamadou N Diaye Deborah Padgett Eric Pantin Andreas Quirrenbach Abhijith Rajan Maxime Rizzo Laetitia Rodet Johannes Sahlmann Matthias Samland David Sing Anand Sivaramakrishnan Frans Snik Jordan Stone Motohide Tamura Niranjan Thatte Peter Tuthill Roy van Boekel Olivia Venot Joanna Vos Jason Wang Ji Wang John Wisniewski Mark Wyatt Neil Zimmerman 41 Co-I s 80 Science Collaborators 121 Total Team Members

15 HIP 65426b SPHERE Discovery image, Chauvin et. al, 2017 NIRCam F410M MIRI F1550C Bona Fide exoplanet (6-9 M Jup ) at 92 AU: announced July Planned Observations: NIRCAM+MIRI photometry. When combined with ground JHK, first dataset to cover full luminous wavelength range of an exoplanet. 1.0

16 VHS 1256b Gauza et al. (2015) Wide separation (8.1 ) enables spectroscopy across full JWST wavelength range: 2-28 µm (!!). Atmospheric abundances, cloud physics, silicates clouds at 8-12 µm. Near-IR Imaging to cross check flux calibration of spectroscopy, probe H2O features. F140M F182M MIRI MRS (5-28 μm) G395H (R~3000 to ~5.2 µm) G235H (R~1000)

17 Coronagraphy of the The JWST Exoplanet Early Release Science Programs HR 4796A disc Near and Mid-IR Coronagraphy Probe on and off of the 3.0μm water ice feature. Aarynn Carter, UK Exoplanet Meeting 2018 F300M F360M Observe at 15.5μm to calibrate disk continuum, effective temperature and spatial variations across the disk. Filacchione, 2014 HST STIS Schneider et al. (2009)

18 NIRISS Aperture Masking Interferometry JWST Goal: understand residual phase errors that set contrast floor. Expected Sensitivity at 3.8µm for the HIP system: 8-9 magnitudes at ~λ/d: young planets at ~15 AU. JWST Aperture Mask Interferogram

19 Task Instrumental mode NIRCAM & MIRI (Exoplanet) Target Specifics Science Time (hr) HIP 65426b NIRCam coronagraphy (2-5 µm). Charged Time (hr) MIRI coronagraphy (11 & 15 µm) NIRCAM & MIRI (Debris Disks) HR 4796 NIRCam 3.0 and 3.6 µm. MIRI 4-Quadrant Phase Mask Coronagraph at 15 µm NIRSPEC IFU MIRI MRS VHS 1256b NIRSpec IFU ( µm). MIRI Medium Resolution Spectrograph (5 28 µm) NIRISS NIRISS 3.8 µm HIP Totals: 30 52

20 Working Subgroups Principal Investigators: Sasha Hinkey (PI), Beth Biller (co-pi), Andrew Skemer (co-pi) 1. Exoplanet Imaging with NIRCam & MIRI Leads: Sasha Hinkley, Laurent Pueyo 2. Debris Disk Imaging with NIRCam+MIRI Leads: Elodie Choquet, Max Millar-Blanchaer 3. Exoplanet Spectra with NIRSPEC + MIRI. Leads: Andy Skemer, Mickael Bonnefoy 4. Aperture Masking Interf metry w/ NIRISS. Leads: Alex Greenbaum, Stephanie Sallum 5. PlanetAtmosphere Modelling (Theory) Leads: Jonathan Fortney, Isabelle Baraffe Science Enabling products Contrast metrics µm datasets. Recommendations for PSF subtraction methods µm test datasets with resolved images. PSF subtraction recommendations µm exoplanet fluxes to inform future surveys. Multi-spectral test datasets for artificial, point source injection. 3.8 µm AMI dataset w/ two calibrators. Identification of AMI limiting systematics. Full standalone spectral retrieval tool. State-of-the-art models customized for JWST bandpasses. Working Group: Quality Assurance Verification Overall Lead: Beth Biller. Quality Assurance Lead: Glenn Schneider, Feedback

21 Find Out More About our Program

22 Find Out More About our Program

23 Additional Slides

24 Exoplanet Direct Imaging Direct Spectroscopy: Detailed Characterization. Dynamical interactions between planets and disks. Technically challenging. β Pictoris b HR 8799 bcde HR 4796 A 51 Eridani b 1 arcsecond Oppenheimer & Hinkley, Annual Reviews of Astronomy & Astrophysics, 2009

25 The JWST Exoplanet Early Release Science Programs Aarynn Carter, UK Exoplanet Meeting 2018 Representative Datasets in Common Modes We have synthesized the needs of our community to identify best practices. Science Enabling Products Contrast curves across all modes for a variety of reduction methods. High contrast imaging analysis pipeline, based on pyklip (Wang et al. 2015). Aperture masking analysis pipeline. PSF Library (in comb. with GTO programs). Theoretical exoplanet atmosphere and evolutionary models + atmospheric retrieval package. Analysis of best practices distributed via STSci Webcast Briefings.

26 0.5 Why Study Exoplanets and Disks with JWST? 0.5 SEDs of Brown Dwarfs & Free Floating Planets are very different from young planets (e.g. Cushing et al 2006). Potential Differences: surface gravity, insolation, silicate or iron clouds? Essential for preparing for Cycle 2 & beyond.

27 Wavelength (µm) Why Study Exoplanets and Disks with JWST? Measure abundances of dominant molecules in atmospheres: CH 4, CO, CO 2, H 2 O, NH 3. Measuring major Carbon & Oxygen species will allow us to measure the C/O ratio (formation constraints?). M Dwarf L Dwarf T Dwarf Jupiter

28 Exoplanet Direct Imaging Outer architectures of planetary systems Overall frequency at outer separations Bowler et al. (2016) Grey: radial velocity Orange: Direct Imaging