The Large UV Optical IR survey telescope. Debra Fischer

Transcription

1 The Large UV Optical IR survey telescope Debra Fischer Yale University

2 How do we identify worlds that are most promising for life? Host star insolation determines the probability of retaining water. Habitable zone: Luminosity is a good filter for identifying potentially habitable worlds. (Kaltenegger 2017, Zeng et al 2016)

3 Transiting Planets in the HZ (dots scale to 0-1, 1-1.5, R E ) (Kaltenegger 2017)

4 Period [days] ,000 Distances RV detected exoplanets Transiting exoplanets...distance matters! Distance from Earth [parsecs] Image credit: Hanno Rein Open Exoplanet Catalog

5 Transiting Planets the TESS difference Non-Kepler Kepler TESS (simulated) Barclay, Pepper, Quintana 2018 (image credit to Z. Berta-Thompson)

6 Image credit: Aki Roberge Inner working angle: For IWA = 100 mas 10pc): 4-m telescope, 6-m starshade, z=6200 km

7 Technology development: Full scale petal with edge profile for contrast < Photo credit: Aki Roberge

8 Advances in Coronagraphy Vector Vortex coronograph - Mostly insensitive to low-order - wavefront aberrations - Smaller inner working angle (~ 2!/D) - - High throughput, broad - instantaneous bandpass - - Machine learning post-processing - techniques

9 RV-detected Planets in the HZ (dots scale to 0-5, 5-10 M E ) All are orbiting lowmass stars We know the exoplanets are there How will we find them for next generation imaging missions? (Kaltenegger 2017)

10 Next-generation groundbased spectrographs; EXPRES just commissioned at the Lowell Obs 4.3-m DCT R=150, nm Vacuum chamber stability Vibration isolation Laser frequency comb Well-characterized CCD Short-term instrumental precision <10 cm/s.

11 The next generation of PRV instruments (e.g., ESPRESSO, EXPRES, NEID) are going to deliver rocky planets in the HZs around nearby stars.

12 Ecosystem of exoplanet missions: Gaia, TESS, CHEOPS, JWST, WFIRST NASA HQ four decadal mission concept studies to develop concept missions for next generation flagships. HabEx: image exoplanets, measure atmospheric spectra, general astrophysics Lynx: X-ray observatory with excellent angular resolution, high thoughput, large FOV, high spectral resolution OST: far IR observatory w/ 3 order magnitude gain in sensitivity relative to Herschel, high angular resolution, transmission spectroscopy

13 LUVOIR Large UV / Optical / Infrared Surveyor (LUVOIR) A space telescope concept in tradition of Hubble Broad science capabilities Far-UV to near-ir bandpass Two architectures: ~8-m and 15-m telescopes Suite of imagers and spectrographs 5-year prime mission, serviceable and upgradable Guest observer driven

14 Imagine astronomy with LUVOIR 2.4 m Low-mass galaxy at z = 2 with HST 15.1 m: LUVOIR-A Low-mass galaxy at z = 2 with LUVOIR-A Credit: G. Snyder (STScI)

15 Solar System remote sensing Pluto with HST Pluto with LUVOIR-A Credit: NASA / New Horizons / R. Parramon

16 Monitoring Solar System ocean moons Europa jets observed with HST UV hydrogen emission Europa jets observed with LUVOIR-A Roth et al. (2014) Credit: G. Ballester (LPL)

17 Imaging Earth 2.0 Solar System at13 parsec with coronagraph and 12-m telescope H 2 O H 2 O CH 4 Inner working angle ~ 3.5 λ / D O microns 2.4 microns Credit: L. Pueyo / M. N Diaye / A. Roberge

18 The exoplanet zoo Apriil 24, 2018 Credit: LUVOIR Tools

19 The LUVOIR instruments Observational challenge Faint planets next to bright stars Extreme Coronagraph for LIving Planetary Systems (ECLIPS) Contrast < Low resolution imaging spectroscopy Bandpass: 0.2 μm to 2.0 μm Tech development via WFIRST coronagraph WFIRST HLC WFIRST SPC Apriil 24,

20 The LUVOIR instruments Observational challenge Very cold to very hot gases LUVOIR UV Multi-Object Spectrograph (LUMOS) R = ,000 Bandpass: 100 nm to 400 nm FOV: 3 x 1.6 (FUV), 1.3 x 1.6 (NUV) FUV imaging channel Heritage from STIS, COS, & NIRSPEC Europa geysers HST STIS UV instrument

21 The LUVOIR instruments Observational challenge Imaging the ultra faint and very small at high resolution High-Definition Imager (HDI) 2 x 3 arcmin field-of-view Bandpass: 0.2 μm to 2.5 μm Nyquist sampled Micro-arcsec astrometry capability (measure planet masses, etc.) Heritage from HST WFC3 & WFIRST HST Wide Field Camera 3

22 POLLUX: a European contribution to the LUVOIR mission study UV spectro-polarimeter with high resolution point-source capability (R ~ 120,000). Circular + linear polarizations and unpolarized light Defined & designed by consortium of 10 European institutions, with leadership/support from CNES Builds off Arago mission concept. Instrument study could serve as basis for a future ESA contribution to LUVOIR

23 Segmented, deployable telescope

24 Difference between LUVOIR and HabEx? Both LUVOIR and HabEx have two primary science goals Habitable exoplanets & biosignatures Broad range of general astrophysics The two architectures will be driven by difference in focus For LUVOIR, both goals are on equal footing. LUVOIR will be a general purpose great observatory, a successor to HST and JWST in the 8 16 m class HabEx will be optimized for exoplanet imaging, but also enable a range of general astrophysics. It is a more focused mission in the m class Similar exoplanet goals, differing in quantitative levels of ambition

25 The discovery of exoplanets resonates with the public. From music bands

26 to Citizen Science. K2-138 system with 5 planets discovered with the help of Exoplanet Explorers (Zooniverse)

27 The discovery of exoplanets resonate with the public. From music bands to Citizen Science. Zooniverse Planet Hunters have (uniquely) discovered: 10% of Kepler planet candidates with P > 100d 50% of planet candidates with P > 600d. (Schmidt et al. 2016)

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