Direct Imaging of with JWST C. Beichman NASA Science Institute Jet Propulsion Laboratory California Instittue of Technology

NIRCam: Marie Ygouf, Tom Greene, Jorge Llop‐Sayson, John Krist, Jarron Leisenring, Mike Meyer, Josh Schleider, Klaus Hodapp, Tom Roellig, Marcia Rieke (PI) MIRI: P‐O Lagage, Gene Serabyn, George Rieke (PI), Andras Gaspar, Camilla Danielski STScI: Laurent Pueyo, Remi Soummer, Michael Perrin Pasadena: Renyu Hu, Dimitri Mawet Copyright 2017 California Institute of Technology. Government sponsorship acknowledged. JWST Will Revolutionize Comparative Planetology • Planet formation and evolution – Where and how do gaseous and rocky planets form? – How do planets migrate to get to present location? – What is nature and origin of planets on distant orbits? • Planetary and atmospheric physics – What is composition of atmospheres? – How is insolation redistributed globally? – Can we measure atmospheric dynamics and T(P) profiles? – What are effects of UV, flares on atmospheric chemistry? – How do clouds and hazes form? – How can we detect signatures of habitability?

Oct 2019 Spirit of Lyot 2 The Ongoing Exoplanet Census Coronagraphic Imaging With JWST Instruments

Boccaletti et al 2015

4‐6/D ~0.5”‐1” for NIRCam coronagraphy 0.05” at 3‐5 m for NIRISS 1‐2/D ~0.5” for MIRI FQPM Non Redundant Masking 4 /D for MIRI Lyot

• The Bad: − Large (132 nm) Wavefront Error • The Good: − Highly stable (2‐5 nm) over many hours • The Great: − Low thermal background at >2 m and > IWA

Oct 2019 Spirit of Lyot Sensitivity Depends on Planet and Age • JWST targets will be young Krist et al; Beichman et al; Perrin et al planets with ages of a few Myr to a few 100 Myr in nearest young clusters (10s of pc) and star formation regions (100 pc) • Outside of 1‐2” JWST reaches

from 1 MJup to sub‐Saturn for closest, youngest systems • Two major goals for GTO/ERS: Danielski et al 2019 – Characterize known planets with multi‐filter photometry and/or spectroscopy – Search for lower mass exoplanets than present ground‐based limits

Oct 2019 Spirit of Lyot Coronagraphic Performance • Depends critically on Pointing and Wavefront Error Drifts. Latest testing suggests WFE drifts at ~2 nm • Use reference star(s), small dithers, post‐processing to minimize stellar residuals to achieve 10‐5 at >1”

Raw Contrast

Perrin et al 2018

March 26, 2018 JPL ESI Symposium 6 Current Knowledge of Young • Incidence of giant planets on distant orbits is low – Does incidence increase with lower mass?  Core accretion followed by migration/near Nielsen et al 2019 ejection – Does incidence decrease with lower mass?  Disk fragmentation at marginal Jeans mass • JWST will push searches of known systems to lower masses than possible from ground at separations >2”

October 2019 Spirit of Lyot 7 Eps Eri b GTO/ERS Targets 51 Eri b Nearby stars with known planets and/or prominent disks. Many old friends • HR 8799 • Eps Eri HD 95086 b HIP 65426 • Vega • HD 95086 b • Fomalhaut • 51 Eri b • Eps Eri b • GU Psc b

HR 8799 Vega Fomalhaut Gu Psc

October 2019 Spirit of Lyot 8 Multiple Coronagraphic Imaging Programs • NIRCam & MIRI imaging of known young Jupiters – Lumin & Teff  radii, mass – Are there lower mass planets? • Blind Searches – /Saturn around Spiegel and Burrows 2011

brightest young stars, e.g. Spiegel and Burrows 2012 Vega, Fomalhaut, eps Eri – Uranus around M stars (<15pc, <150 Myr) at ~10 pc snowline Cycle 1 ERS Hinkley et al HD 95086 2.1 m 4.4m M Star Survey • Kepler suggests abundant

• NIRCam coronagraphy can reach MUranus for <150 Myr, 15 pc • NIRCam probes 10‐20 AU, close to CO snow line favored for formation of ice giants – NIRCam survey of ~10 objects at F444W at 3.5 hr/object and F322W2 to veto stars and galaxies

Meyer, Schleider et al Is There an Earth Orbiting Alpha Cen A?

March 26, 2018 JPL ESI Symposium 11 Detectability of  Cen A Planets • Depends critically on on‐orbit Jorge Llop‐Sayson performance of JWST, observation strategy to MIRI 15.5 m minimize thermal drifts • 3.5 hour observation w MIRI FQPM at 15.5 um could detect

0.5 RJup planets at SNR~5 (assuming WFE drift ~2 nm) • Completeness

increases above 5 R, but only 5‐10% consistent with existing PRV limits • See poster by Llop‐Sayson and Marie Ygouf

Oct 2019 COSPAR 2018 12 Direct Spectroscopy HR8799b Konopacky et al 2013 of Young Jupiters • Determine elemental abundances (C/O) to test formation mechanisms, e.g. core accretion (enhanced C/O) vs. fragmentation (stellar C/O) HR8799 NIRSPEC IFU • At separations >1~2” use Spectral Differential Imaging with NIRSpec IFU and MIRI LRS to obtain R~1,000‐3,000 spectra at 3‐12 m T and Y Dwarfs: WISE J0855‐07 Exoplanet Analogs • Free‐floating Y dwarfs

– 250< Teff<500 K, 3‐10 MJup – 24 within 20 pc – WISE J0855‐07: 4th closest object to Sun at 2.2 pc; Coldest (250K) • T dwarf companions to bright stars (HD19467, Crepp et al; HR 2562 B, PZ Tel B) with ages, masses, Fe/H to anchor models • NIRSpec and MIRI spectroscopy for abundances, Teff, clouds, • Critical tests for giant planet models Oct 2019 Spirit of Lyot Kuiper Belts, Asteroid Belts & Planets

• Giant planets (5‐20 MJup, 10‐1000 AU) more common around stars with disks: 6.3% vs. 0.7% (Meshkat et al 2018). Planets in the gap? • Characterize dust structures and 50K 150K properties (sizes, composition, ices) • Search for planets which may stir dust, sculpt disks into rings & gaps

Su et al 2013

Fomalhaut Spitzer HST JWST Oct 2019 Spirit of Lyot Observing Disks with JWST • NIRCam will study grain composition by observing scattered light out to 4.6 um, determining color (grain size), and identifying ices of H2O and CO2 • NIRSpec and MIRI spectroscopy (R~100 – 3000) at 1 – 30

μm, including water H2O, CO2, silicate features

From Chen et al (Astro2020 WP): Composite image of the b Pic (VLT/NaCo, Lagrange et al. 2010); GPI, Macintosh et From Su et al, JWST/MIRI F2550C al. 2014, Millar‐Blanchaer et al. 2015). Lyot coronagraph can resolve roughly half of known debris disks Oct 2019 Spirit of Lyot 16 Wide Range of Exoplanet Science • Exoplanet programs use all JWST instruments • Exoplanet science: 30% of GTO time (1000/3280 hr) • Exoplanet science: 27% of ERS program(133/488 hr)

July 16, 2018 COSPAR 2018 17 Conclusions • JWST will revolutionize characterization of exoplanets • Status: Launch delayed until March 2021

SPACE SPACE

Oct 2019 18