Transiting Exoplanet Survey Satellite May contain MIT, LL, GSFC, OSC proprietary information and be subject to U.S. Government Export Laws; U.S. recipient

Transiting Exoplanet Survey Satellite

May contain MIT, LL, GSFC, OSC proprietary information and be subject to U.S. Government Export Laws; U.S. recipient is responsible for compliance with all applicable U.S. export regulations.

David W. LathamHarvard-Smithsonian Center for Astrophysics

K2SciCon, Santa Barbara, 4 Nov 2015

TESS Precursor & Follow-up

Building on the Legacy of Kepler & K2

Sky coverage Kepler surveyed 1/400th of the sky K2 will survey 10 to 20 times more (1/40th to 1/20th of sky) TESS will cover (nearly) the entire sky The nearest and best transiting planets for follow-up

Kepler designed to provide statistics Reach Earth twins in one-year orbits around Sun-like stars Provide occurrence rates to inform future missions Just happens to allow breakthroughs in astrophysics But most KOIs are too faint for effective follow-up

K2SciCon 4 November 2015

Towards TESS Science

TESS designed to find the nearest transiting planets Emphasis on characterizing small planets similar to Earth Best targets for spectroscopy of exoplanet atmospheres Dream of detecting biomarkers as evidence for life

K2 can be viewed as rehearsal for TESS Completely open to community inputs & follow-up Lean and mean mission team with Kepler experience

Can TESS adopt the best of both worlds? Strong and active Science Team Working groups with participation of community experts Strong Guest Investigator Program, community involvement Effective support from MAST and NExSci


TESS Precursors I

Prepare TESS Input Catalog Used to select optimum planet-search targets Document all luminous objects that matter to transits Support data reductions (apertures, contamination) Support simulations, full frame image analysis Support Guest Investigator Program target selection

Provide prioritized Candidate Target List Planet search priorities set by sensitivity to small planets Merge targets from Guest Investigator programs Payload Operations Center figures out actual targets


TESS Precursors II

Target Selection Working Group very active Led by Josh Pepper & Keivan Stassun Frequent electronic meetings via WebEx TESS Dwarf Catalog under development for entire sky Draft version based on available catalogs and data New data will be incorporated as available Gaia data releases critically important: selection & analysis Special effort to include more (and later) M dwarfs Special effort to include key open cluster targets Set a wide net (e.g. hot stars, evolved stars, white dwarfs) Best systems likely to be Hipparcos stars


TESS Precursors III

TESS Input Catalog drafts Preparation led by Jonathan Irwin Version 1 delivered August 2015 Based on 2MASS, half billion entries Included ~3 million candidate dwarf targets Gaia first data release expected summer 2016 G magnitudes, space resolution, proper motions Improved T magnitudes Improved stellar parameters (parallaxes please!)


T Magnitudes by Willie Torres


TESS Science Office Organization & Roles

Located in Cambridge, Massachusetts CfA arm led by Dave Latham, Director of Science MIT arm led by Josh Winn, Deputy Director of Science

Prepare and Maintain the TESS Input Catalog Deliver improved versions as needed

Identify TESS Objects of Interest (TOIs) Based on data products from SPOC at NASA Ames Pipeline development led by Jon Jenkins Strong Kepler legacy

Deliver TOI Lists to MAST on 4 month schedule Move from human vetting to robo-vetting ASAP


Dave’s version of the flowdown per sector

~15,000 light curves ~1,000 threshold crossing events ~500 after flux triage ~200 after false positive rejection

Ephemeris matching, recon observations ~100 after eclipsing binary removal

Secondary eclipse implies self luminous comp ~20 high priority planet candidates

Promoted to spectroscopic follow-up ~80 lower priority planet candidates


False Positive Rejection

Ephemeris matching Need an all-sky EB catalog with ephemerides No existing catalogs with good completeness Full-frame images provide an opportunity But can they be processed quickly enough?

Seeing-limited images TESS pixels are 21 arc-seconds Meter-class CCDs can detect nearby EBs But require careful scheduling during events LCOGT and Mearth are on board Opportunity for others, e.g. KELT network

High-resolution imaging as needed (AO, speckle)K2SciCon 4 November 2015

Joey Rodriguez and KELT Network Poster


Spectroscopic Follow-up

Spectroscopic reconnaissance Initial observation(s) at quadrature(s) High resolution, modest SNR Check stellar parameters, rotation Requires careful scheduling Several meter-class facilities on board NRES@LCOGT, Sophie@OHP, TRES@FLWO, … Opportunity for other similar facilities

Extreme PRV follow-up for orbits & masses HARPS (N&S), HIRES, others on board Several new instruments too, e.g. EPRV@WIYN


TESS Follow-up Observing Program (TFOP)

TFOP Working Group getting organized Talk to me if you want to learn more

Discussions with NExSci underway Extension of CFOP and ExoFOP-K2 to TESS

Can we coordinate community efforts? Optimize use of resources Minimize duplication of effort

There will be plenty of follow-up work to go around



Documents

Transiting Exoplanet Survey Satellite May contain MIT, LL, GSFC, OSC proprietary information and be subject to U.S. Government Export Laws; U.S. recipient