The TESS Project

Transcription

The TESS Project

Transiting Exoplanet Survey Satellite
The Transi*ng Exoplanet Survey Satellite (TESS): Opportuni*es for Commensal Survey Science
George Ricker
Bou-ques & Experiments: 2015
Caltech— Pasadena, CA
28-‐29 August 2015
TESS — Discovering New Earths and Super-‐Earths in the Solar Neighborhood
1
TESS Institutional Par tners
Ames
TESS Science Team
So Many Stars...So LiLle Time
Primary Goal: Discover Transiting Earths and Super-‐
Earths Orbiting Bright, Nearby Stars
Rocky Planets & Water Worlds
§ Habitable Planets
§
Discover the “Best” ~1000 Small Exoplanets
“Best” Means “Readily Characterizable”
• Bright Host Stars
• Measurable Mass & Atmospheric Properties
§ Present: Only 3 small transiting exoplanets orbiting bright hosts are known
§
Large Area Survey of Bright Stars
§ Sun-‐like stars: +2 to +12 magnitude
§ M dwarfs known within ~60 parsecs
§ “All sky” observaEons in 2 years:
> 200,000 target stars at <2 min cadence
• > 20,000,000 stars in full frames at 30 min cadence
•
Launch in August 2017
3
TESS Stars Will Be Brighter than Kepler Stars
u
How do we arrange for brighter stars?
§
u
Two ways... 2017
Increase solid angle coverage
§ ΩTESS ≃ 400 ΩKepler 2009
§ Number of accessible bright stars increased by same factor
u
Select stars that are much closer
§ TESS: ~10 2 light-‐yr
§ Kepler: ~10 3 light-‐yr
1/R2 dependence means TESS stars are ~100 <mes brighter on average
4
TRILEGAL SimulaEon of Expected TESS DetecEons
u
TRIdimensional modeL of thE GALaxy (Girardi et al. 2005)
§
Monte Carlo populaEon synthesis code that models the Milky Way with four components
Thin Disk
• Thick Disk
• Halo
• Bulge
•
u
u
Details are given in Sullivan et al. (arXiv:1506.08845)
AnimaYon follows showing transiYng planets expected at increasing distances from Sun
§
§
§
§
§
3 pc
10 pc
30 pc
100 pc
300 pc
5
S
Animation by Zach Berta-Thompson
potentially
habitable
Simulated ½ Hour Stacked Full Frame TESS Image = Targeted 2min, 10x10 “Postage Stamps” => 2% of FOV
DefiniYon:
2.8°
Full Frame Image = FFI = 100% of FOV
FFI Stack: 900 TESS images @ 2s/integra:on
PorYon of Image Stack Shown:
2.8°
= 8 deg2 out of 570 deg2/camera
= 0.34% of instantaneous TESS FOV
Stars with 30 Minute Cadence Photometry
TESS
Kepler
20,000,000
170,000
Discovering New Earths and Super-‐Earths in the Solar Neighborhood
7
one camera:
24 degrees
8 deg2
one camera:
24 degrees
constellations by H. A. Rey
30-minute cadence
for full frame images
one camera:
24 degrees
(>30 million objects in survey…)
Pointing of the
TESS Cameras
( 4 Total)
TESS Sky Mapping Strategy
http://www.youtube.com/watch?v=mpViVEO-ymc
12
TESS 2-‐year Sky Coverage Map
TESS 2-year sky coverage map
27 days
54 days
81 days
108 days
189 days
351 days
JWST
continuous
viewing zone
13
TESS Orbit InserEon
14
TESS’s Novel High Orbit
Uninterrupted viewing for >95% of Yme Orbital Periods:
TESS = 13.7 days
Moon = 27.4 days
➡ 2:1 Resonance
➡ 90° Phasing
TESS Orbit is Stable for Decades (no station keeping req’d)
15
“Special” Orbit Enables and Simplifies TESS 1) Extended & Unbroken Observa4ons: >300 hrs per orbit
2) Thermal Stability: <40 mK/hr (passive control only)
3) Earth/Moon Stray Light Tolerance: 10-‐6 (vs 10-‐12 in LEO) 4) Low Radia4on Levels: No SAA, No Outer Belt Electrons
5) Frequent Launch Windows: 5 of 27 days per lunar month
6) High Data Rates: 100 Mbit/s (300 GB in 5 hr at TESS Perigee)
[1/R2 advantage: ~200x Earth-‐Sun L2; ~10,000x Kepler-‐type Orbit]
7) Excellent Poin4ng Stability: No Drag, No Gravity Gradient
8) Simple opera4ons: Single 5-‐7 hr Downlink & Repoint every ~2 wks
9) Long Orbit Life4me: ~Several Decades with Perigee > 6.6 RE
Gangestad et al. 2013 (astro-‐ph 1306.5333)
16
MIT-‐LL Deep Deple:on CCDs
Ricker et al. (2014)
17
Quantum Efficiency of BI CCID-‐80
Quantum Efficiency
CCID-‐80
Thickness = 100µm
Reference CCD
Thickness = 36 µm
Ion-‐implant, Laser anneal back surface
Wavelength (nm)
18
ude of 6 . Figure 1 shows the hemispherical coverage r
ing from this arrangement.
TESS Filter Passband
1
V
IC
R
z
Spectral SpectralResponse
response
T ESS
0.8
0.6
0.4
0.2
0
500
600
700
800
900
Wavelength
[nm] Wavelength [nm] G.
1000
1100
Ricker et al. 2014
(astro-‐ph 1406.0151)
product
of the
2.— The TESS spectral response, which is the
CC
tum efficiency and the longpass filter curve. Shown for comparison
19
TESS Camera (1 of 4)
TESS Lens Design
– Hybrid Petzval design
– 600-‐1000 nm optimized – 24˚ x 24˚ FOV
– 7 elements – 146 mm f/1.4 lens
– 2 aspheric surfaces
20
TESS Engineering Model Camera at MKI
21
TESS Wide FOV CCD Camera Prototype
22
Full Size Replica of TESS
23
σ [pp
5
102
Photometric Noise in 1 Hour
l Aperture
Pixels in Optimal
σ [ppm Aperture
hr1/2 ]
10
Star noise
Zodiacal noise
Read noise
Sys. noise
Saturation
4
101
10
30
3
10
20
2
10
10
1
100
30
4
6
8
10
12
14
16
Apparent Magnitude [IC ]
Ricker et al. (2014)
σ [pp
5
102
l Aperture
Pixels in Optimal
σ [ppm Aperture
hr1/2 ]
10
Star noise
Zodiacal noise
Read noise
Sys. noise
th
Saturation
200 ppm
4
101
10
for 10 mag.
30
3
10
20
2
10
10
1
100
30
4
6
8
10
12
14
16
Ricker et al. (2014); Sullivan et al. (submitted), both includingRicker
Berta-Thompson
et al. (2014)
σ [pp
5
102
l Aperture
Pixels in Optimal
σ [ppm Aperture
hr1/2 ]
10
Star noise
Zodiacal noise
Read noise
Sys. noise
Saturation
th
1%
4
101
10
30
3
for 16 mag.
10
20
2
10
10
1
100
30
4
6
8
10
12
14
16
Ricker et al. (2014); Sullivan et al. (submitted), both includingRicker
Berta-Thompson
et al. (2014)
TESS: Simulated Detections
T ESS
Planet Detections
Simulated
TESS
detections
Ecliptic
Coordinates
Sullivan et al. (arXiv:1506.08845)
Full-Frame Images
2x105 Target Stars
Detectable planets around 200,000 preselected stars
Detectable planets around
20,000,000 stars in full images
The Predicted TESS Yield
TESS: Simulated
Sullivan Dete
et al.
18
NB: Log Scale on Y Axis
66
10
10
Full-Frame Images
Full-Frame
Images
5
2x10 5Target Stars
55
10
10
2x10 Target Stars
17k
17k
44
Detections
Detections
10
10
1.4k
3
10
10
3
300
486
290
2
10
2
10
1
10
3.0k
1910
1111
690
±122
±22
140
45
45
70
67
±9
±8
1
10
Earths Super-Earths Sub-Neptunes Giants
Earths Sup er-Earths Sub-Neptunes Giants
> 4R⊕
< 1.25R⊕ 1.25 − 2R⊕ 2 − 4R⊕
< 1.25R⊕
1.25 − 2R⊕
2 − 4R⊕
> 4R⊕
F IG . 18.— Mean numbers
planets
eclipsing
binaries
that that
areare
detected
inthetheTESS
TE
TESS —of
DMean
iscovering N
ew Earths and
and of
Super-‐Earths in the Solar N
eighborhood
F IG . 18.—
numbers
planets
and
eclipsing
binaries
detected in
18
Sullivan et al.
6
10
Full-Frame Images
2x10 5 Target Stars
5
500 planets smaller
than 2R⊕
10
mass measurements
could resolve the rocky
planet transition
Detections
10
17k
4
3.0k
1.4k
3
10
1111
486
±122
±22
2
10
70
67
±9
±8
1
10
< 1.25R⊕
1.25 − 2R⊕
2 − 4R⊕
> 4R⊕
TESS — DMean
iscovering N
ew Earths and of
eighborhood binaries that are detected in the TESS
F IG . 18.—
numbers
planets
and
eclipsing
18
Sullivan et al.
6
10
Full-Frame Images
2x10 5 Target Stars
5
10
17k
Detections
1500 planets 10
smaller than 4R⊕
atmospheric studies will
be possible for many of
these
4
3.0k
1.4k
3
10
1111
486
±122
±22
2
10
70
67
±9
±8
1
10
< 1.25R⊕
1.25 − 2R⊕
2 − 4R⊕
> 4R⊕
TESS — DMean
iscovering N
ew Earths and of
eighborhood binaries that are detected in the TESS
F IG . 18.—
numbers
planets
and
eclipsing
Timeline for TESS Mission
TESS
Selected
Launch
Commisioning
Begin
Sky
Survey
CDR
PDR
NOW
Flt HW/SW & TesYng
2013
2014
2015
2016
2017
Hemi #1
2018
Sr Review 2018
End
Yr 1
End
Yr 3
End
Yr 2
Hemi #2
2019
“Bonus Yr”*
2020
Sr Review
2020
* 3rd “Bonus Year” of Survey: Con:ngent on residual funds remaining from TESS mission reserves
** TESS itself (and the orbit) should be operable for more than a decade
31
Next Steps in TESS Science Planning
u
InteracYng with Other IniYaYves and Missions:
§ Providing for Non-‐Exoplanet Targets in TESS FFIs
§ CoordinaEng with Gnd Followup
§ Providing Prime Followup Targets (JWST, ELTs)
u
Providing for Asteroseismology:
~15,000 targets @ 2 min cadence
§ ~1000 targets @ 20 sec cadence (special mode)
§
u
Planning for Extended Mission(s):
§ Repeat survey in a single hemisphere?
§ Concentrate on an eclipEc pole?
§ Concentrate on the eclipEc plane?
•
~5 x 72 day duraEons; comparable to ~ 100 K2 poinEngs
32
Prospects for a TESS EclipEc Plane One Year Survey
11/24/13
1000px-MessierStarChart.svg.png (1000×500)
Equatorial Coordinates
Kepler
Field
(100 deg2)
Poin
/ng
and #4
B
g
n
/
Poin
#3
d
n
Ba
g
n
n/
Poi
Ban
d #1
Band #2
g
n
/
n
i
o
P
Poin
/ng
Ban
d #5
24°
Tc
p
i
l
Ec
Each PoinYng Band covers: 24° x 96° = 2304 deg2 for 72 days Total Coverage @ 72 days/poinYng: 5 x 2304 = 11,520 deg2 ( equiv to ~100 K2 campaigns )
33

The TESS Project

Transcription

Similar documents