# Presentation: 861086

## George Ricker 
MIT Kavli Institute

- George Ricker
- MIT Kavli Institute

***Transiting Exoplanet Survey Satellite***

- David Latham
- SAO

- 30 May 2008

## TESS Goals

- Bright Stars!
- FGK dwarfs: V= 4.5-13.5
- M dwarfs: I < +13
- All Sky Survey
- 40,000 deg2
- 2,500,000 target stars
- Identify ~1000 transiting planets
- Nearest and brightest for JWST
- Proposed Jan 2012 launch

## Census of TESS detections vs. planetary radius

| Total Exoplanets | 1622 |
| --- | --- |
| Gas Giants | 1093 (67%) |
| Neptunes | 414 (26%) |
| Super-Earths | 92 (5.7%) |
| Earth-Sized | 23 (1.4%) |

## TESS Detections by Stellar Type

- J. Winn in 2007;
- “pre-Lovis et al.”

## TESS Mission Design

| TESS Characteristic | Value or Range |
| --- | --- |
| CCD Detectors | Quad MIT/LL CCID-47s 
(4096x4096 imaging array @ 15μm/pixel)  |
| CCD Mode | Shutterless: 
1 s integrate, 2 ms frame transfer |
| CCD Space Flight History | 6 years operation on HETE-2 (as CCID-20)
Very low hot pixel rate in equatorial orbit |
| Lens Design | Petzval 6 element |
| Lens Aperture | 12.7 cm |
| Pixel Scale | 16.3" pixel-1 |
| Camera Field-of-View | 18° x 18° |
| Number of Cameras | 6 |
| Ensemble Field-of-View | 54° x 36° = 1944 deg2 |
| Pass Band | 600-1000 nm |
| Sensitivity (I band) | I = 11.7 (600s integration, S/N = 1000) |
| Photometric Precision (1σ) | 190 μmag at I=+8 in 600s |
| Data Downlink Rate | 10 Gbytes day-1 |
| Launch Date | 2012 |
| Survey Duration | 2 years for All Sky |

- Six Camera Ass’y

- TESS
- “all-dressed up”

## MIT/LL CCDs Selected for TESS

- MIT/LL CCID20 variant: 4K x 4K imager; 15 μm x 15 μm pixels
- Live Time: >99%
- 1s integration
- Frame store with 2ms transfer
- Flight qualified on HETE-2
- Very low hot pixel rate in equatorial orbit

## TESS “Stare & Step” Survey

- Sky Coverage:
- ~6000 sq. deg. per 96 min orbit

## TESS 2 yr Sky Coverage in Celestial Coordinates

**total time of exposure (in seconds) in a Two Year Mission**

## M Dwarf Spectra & TESS Passband

**GL 752B**
**M8**
**V-I = 4.3**
- mI= 12.8

**GL 411**
**M2**
**V-I = 2.1**
- mI= 5.3

**GL 213**
**M4**
**V-I = 2.8**
- mI= 8.7

**GL 406**
**M6**
**V-I = 4.0**
- mI= 9.5

- d= 2.39 pc

- d= 5.87 pc

- d= 2.54 pc

- d= 5.85 pc

- Spectra: Brett ‘95  Magnitudes: Bessell ‘91

## TESS Follow Up Plans & Contributors

**Observing Facilities**

- LCOGT (1m x 18; 0.4m x 40)
- FLWO (1.5m + TRES)
- Euler (1m + Coralie)
- Magellan (6.5m x 2)
- HARPS-S
- HARPS-NEF

## We hope you agree that TESS should have a high priority

## TESS Science Team

| Name | Institution | TESS Responsibility |
| --- | --- | --- |
| G. R. Ricker | MIT | Principal Investigator |
| D. W. Latham | CfA | Chief Mission Scientist; Follow-up science |
| K. A. Ennico | NASA Ames | NASA Project Scientist |
| R. Vanderspek | MIT | Payload Project Scientist; SOC Manager |
| G. Bakos | CfA | Transit detection algorithms |
| M. Brown | Los Cumbres | LCOGT spectroscopic & photometric follow-up |
| J. Burgasser | MIT | Target selection; MIT IR follow-up |
| D. Deming | NASA GSFC | JWST spectroscopic follow-up |
| J. P. Doty | Espace/ MIT | Payload systems engineer; SOC staff |
| W. Dunham | Lowell Observatory | Optical Design; Camera ground testing; SOFIA followup |
| J. L. Elliot | MIT | MIT follow-up photometry |
| J. Holman | CfA | CfA photometric follow-up (Mt. Hopkins) |
| S. Ida | Tokyo Tech | Theory of exoplanets |
| M. Jenkins | SETI | Adaptation of Kepler transit detection methods |
| G. Jernigan | Espace | Transit algorithms; SEO Serendipitous Science |
| N. Kawai | Tokyo Tech | Ground followup |
| J. Lissauer | NASA Ames | Theory of exoplanets |
| F. Martel | Espace/ MIT | Ground station network manager |
| D. Sasselov | CfA | Modeling of super-Earths; HARPS-N facility |
| R. H. Schingler | NASA Ames | Partnership and Public Participation Manager |
| S. Seager | MIT | Exoplanet modeling; SC Lead; JWST follow-up |
| G. Torres | CfA | CfA spectroscopic follow-up  |
| S. Udry | Geneva Observatory | Radial velocity follow-up with Coralie and HARPS-S |
| S. Villasenor | MIT | CCD Scientist; SOC staff |
| J. N. Winn | MIT | Light curve analysis; MIT follow-up photometry |