WFIRST, the Wide Field InfraRed Survey Telescope, is a NASA observatory designed to settle essential questions in the areas of dark energy, exoplanets, and infrared astrophysics. The telescope has a primary mirror that is 2.4 meters in diameter (7.9 feet), and is the same size as the Hubble Space Telescope's primary mirror. WFIRST will have two instruments, the Wide Field Instrument, and the Coronagraph Instrument.
The Wide Field Instrument will have a field of view that is 100 times greater than the Hubble infrared instrument, capturing more of the sky with less observing time. As the primary instrument, the Wide Field Instrument will measure light from a billion galaxies over the course of the mission lifetime. It will perform a microlensing survey of the inner Milky Way to find ~2,600 exoplanets. The Coronagraph Instrument will perform high contrast imaging and spectroscopy of dozens of individual nearby exoplanets.
WFIRST (NASA-led and managed by NASA's Goddard Space Flight Center) is designed for a 5-year mission, and will launch on a EELV out of Cape Canaveral.
JPL is building WFIRST's Coronographic Instrument (CGI) and is involved with detector validation and developing CGI's science capabilities. GSFC is responsible for the WFIRST Project. The WFIRST Science Center functions are the joint responsibility of the Infrared Processing and Analysis Center (IPAC), the Space Telescope Science Institute (STScI), and GSFC.
Overview of the Coronagraph Instrument (CGI)
The light from an exoplanet, as it would be seen in reflected starlight, is fainter than the host star by factors of 100,000,000 or more, and well beyond the reach of today's observatories on the ground or in space. The CGI is one of two instruments on board WFIRST. The spacecraft is now in design Phase B and is scheduled for launch to L2 in 2025. WFIRST CGI will demonstrate the first high-performance coronagraph system in space capable of direct imaging of mature exoplanet systems (such as our own) in reflected starlight, paving the way to a future possible NASA mission aimed at imaging and characterizing faint Earth-like planets.
Objectives of the Coronagraph Instrument (CGI)
Current ground-based and space-based instruments are limited to the detection of bright (self-luminous) young exoplanets, a million times fainter than their host star and located > 0.3 arc seconds away. A successful CGI technology demonstration, i.e., just meeting its baseline technical requirements (BTRs), will be capable of detecting planetary companions 20 million times fainter than their host star and located > 0.15 arc seconds away. Performance models based on current lab results predict the CGI would be capable of detecting planetary companions a billion times fainter than their host star and located > 0.15" away. CGI provides a crucial stepping stone in the preparation of future missions aiming to image and characterize Earth-like planets 10 billion times fainter than their host star and located 0.1 arc seconds away.
Critical CGI Technology Demonstrations
The Coronagraph Instrument on WFIRST is an advanced technology demonstrator for future missions aiming to directly image Earth-like exoplanets. CGI will demonstrate for the first time in space the technologies for future missions needed to image and characterize rocky planets in the habitable zones of nearby stars. By demonstrating these tools in an integrated end-to-end system and enabling scientific observing operations, NASA will validate performance models and provide the pathway for potential future flagship missions.
CGI Science Capabilities
Direct Imaging of Exoplanets: 2019
The WFIRST Coronagraph Instrument relies on the stability of a Space Observatory
WFIRST-CGI pioneers space coronagraph technologies
WFIRST-CGI provides guaranteed science return for circumstellar disks
Exoplanet ImagingFollowing the recommendations of the Astro2010 decadal survey, the WFIRST Coronagraph Instrument (CGI) advances and demonstrates key technologies as enablers for the next generation of Earth-observing exoplanet observatories in space. The CGI is one of two instruments on the Wide Field Infrared Survey Telescope, a NASA project now in the design (Phase B) stage and scheduled for launch in 2025.
The CGI will demonstrate in space, for the first time, key enabling technologies for future Earth imaging missions, including precision optical wavefront control with deformable mirrors, sensitive photon-counting imaging detectors, selectable coronagraph observing modes, low-resolution integral field spectroscopy, advanced algorithms for wavefront sensing and control, high-fidelity integrated spacecraft and coronagraph modeling, and post-processing methods to extract images and spectra. CGI is designed to demonstrate space coronagraphy at sensitivity levels of Jovian-mass planets and faint debris disks in reflected starlight.
Following initial commissioning and formal technology demonstrations in the first eighteen months of operations, NASA envisions a Participating Science Program to engage the exoplanet community. In these panels, we describe how CGI science will advance community goals in exoplanet astronomy and how it will validate key technologies for future exoplanet missions, now envisioned as HabEx and LUVOIR.
- Two selectable coronagraph modes (HLC and SPC)
- Pair of deformable mirrors for precision wavefront control
- Photon-counting EMCCD imaging sensors
- Integral field spectrograph (R=50)
- Autonomous operations on orbit
- Data post-processing algorithms
- Starshade compatibility
- References to the recent CGI literature
Emulating WFIRST data in the lab
JPL's Precision Projector Laboratory (PPL) uses a testbed designed to emulate astronomical data using real detectors in order to validate the Wide Field Instrument's strict requirements on photometry, astrometry, and especially galaxy shape measurement. The PPL testbed rapidly generates a range of customizable "scenes" (e.g. stars, galaxies, spectra) on large format detectors to uncover subtle systematic effects that can evade conventional detector testing and degrade science measurements. Once understood, detector issues may be mitigated via changes to hardware, calibration, mission operations, or data analysis. More info: https://arxiv.org/abs/1801.06599
- 2.4 m telescope used by both
- The Wide Field instrument
- The Coronagraph Instrument