Transcript Advanced Technology Large-Aperture Space Telescope

ATLAST:
Advanced
Technology
Large-Aperture
Space Telescope
Marc Postman
STScI
A NASA Astrophysics
Strategic Mission
Concept Study of the
Science Cases &
Technology
Developments needed to
build an AFFORDABLE
8m - 16m UV/Optical
Filled-Aperture Space
Telescope
Advanced Technology Large-Aperture Space Telescope (ATLAST)
Concept Study Team
Ball Aerospace:
Vic Argabright
Paul Atcheson
Morley Blouke
Dennis Ebbets
Teri Hanson
Leela Hill
Steve Kilston
JPL:
Peter Eisenhardt
Greg Hickey
Bob Korechoff
John Krist
Jeff Booth
STScI:
Dave Redding
Karl Stapelfeldt
Wes Traub
Steve Unwin
Michael Werner
Goddard Space Flight Center:
David Aronstein
Lisa Callahan
Mark Clampin
David Content
Qian Gong
Ted Gull
Tupper Hyde
Dave Leckrone
Rick Lyon
Gary Mosier
Bill Oegerle
Bert Pasquale
George Sonneborn
Richard Wesenberg
Jennifer Wiseman
Bruce Woodgate
Johnson Space Flight Center:
Tom Brown
Rodger Doxsey
Andrew Fruchter
Ian Jordan
Anton Koekemoer
Peter McCullough
Matt Mountain
Marc Postman, P.I.
Neill Reid
Kailash Sahu
Babak Saif
Ken Sembach
Jeff Valenti
John Grunsfeld
University of Colorado:
Marshall Space Flight Center:
Bill Arnold
Randall Hopkins
John Hraba
Phil Stahl
Gary Thronton
Scott Smith
Northrop Grumman:
Dean Dailey
Cecelia Penera
Rolf Danner
Chuck Lillie
Ron Polidan
Amy Lo
Princeton University:
Jeremy Kasdin
David Spergel
Robert Vanderbei
Webster Cash
Mike Shull
Jim Green
University of Massachusetts:
Daniela Calzetti
Mauro Giavalisco
Is There Life Elsewhere in the Galaxy?
Why istoa multiply
large UVOIR
space
telescope
required
Need
these
values
by Earth
x fB
to get
answer
question?
to
the this
number
of potentially life-bearing
planets detected by a space telescope.
Zones (HZ) of nearby stars subtend
Habitable
Earth = fraction of stars with Earth-mass planets in HZ
smallofangles
(<200 mas)
fBvery
= fraction
the Earth-mass
planets that have
detectable biosignatures
Earth-mass planets within these HZ will be very
faint
AB mag)
If:
(>29
then DTel ~ 4m
Earth x fB ~1
Earthhigh-contrast
x fB < 1
then DTel ~ to8m
Requires
(10-10) imaging
see
Earth
x fBachieve
<< 1 this
then
Dthe
16m
planet.
Cannot
from
ground.
Tel ~
Number of nearby stars capable of hosting
potentially habitable planets is not large (e.g.,
To maximize
chance
for a successful
non-binary,
solarthe
type
or later).
searchsize
for 
lifeD3in the solar neighborhood
Sample
requires a space telescope with an
Planets aperture
with detectable
biosignatures
may be
of at least
8-meters
rare. May need to search many systems to find
even a handful. Sample size  D3
Number of FGK stars for which
SNR=10, R=70 spectrum of Earthtwin could be obtained in <500 ksec
1000
100
10
1
2-m
4-m
8-m
16-m
Green bars show the number of
FGK stars that could be observed
3x each in a 5-year mission without
exceeding 20% of total observing
time available to community.
Re-tracing the Star Formation History
of Galaxies in High Definition
Map of Nearby
Galaxies,
centered on
Milky Way
Resolved Stellar Populations: An 8-m to 16-m
space telescope will bring about a major revolution in
the study of stars, enabling observations of solarluminosity stars outside the Local Group of galaxies.
Observations of solar-luminosity stars on the main
sequence are essential to reconstructing the star
formation history over the entire lifetime of a galaxy.
HST
Increasing
distance
from Earth
T. Brown, 2006
1 Egal
10 Egals Virgo Clstr
Diffraction limited imaging in V-band (500 nm) of
faint point sources over 5 arcmin FOV. Medium to
high resolution spectroscopy of faint point sources in
UV/Optical passband.
ATLAST will open up the entire Hubble sequence of
elliptical
and spiralS/N
galaxies
study, revealing
We require
= 5 tophotometry
oftheir
detailed star formation histories. These histories hold
~thousands of 33 - 35 mv stars. about
fundamental (but as yet unknown) information
We also
require
galaxy
formation.
JWST high-resolution
will observe the integrated
populations
of stars capabilities
at high redshiftinbut
spectroscopic
thewill not
reconstruct their detailed star formation histories. We
near
- opticalofto
study
the
will
need UV
the capabilities
ATLAST
to understand
the
detailed
evolutionary
history of
nearby galaxies
to
distribution
of stellar
masses
in
obtain a comprehensive understanding of how stars
nearby galaxies.
form.
Many astrophysical investigations require the
capabilities of a large UVOIR space telescope
Direct detection & verification
of the hierarchical assembly of
structure & the processes that
govern the interactions
between the IGM and galaxies
UV / optical R~1000-2000 absorption spectroscopy
of faint galaxies (>26 mag) and QSO’s (>22 mag).
Core of M31 as seen with
16m space telescope
Direct measurement of the
proper motions of galaxies in
the Local Group: direct
constraints on the kinematics
and distribution of Dark Matter
Very stable and well-calibrated imaging (PSF,
distortion, pixel scale) on time scales of up to 5
years.
If we want to pursue the compelling scientific issues we imagine today (and the
many we cannot imagine), we will need a large UV/optical space telescope as
part of our astronomical tool kit. Making it affordable is the strong motivation for
a focused technology development program for the coming decade.
Pathways to a Large UVOIR
Space Telescope
If Ares V is built by 2019 …
8-m monolithic
mirror Telescope
in ~2025
and/or
16-m segmented
mirror Telescope
in ~2030+
If Ares V is not built …
9.2-m segmented
mirror Telescope
in ~2028
or
Elliptical (lightweight) monolithic
mirror Telescope
in ~2028
Delta IV HLV
Ares V payload to L2 = 65 mT, Delta IV HLV payload to L2 = 16 mT
ATLAST Concepts
8-m Monolithic Primary
(shown with on-axis SM configuration)
9.2-m Segmented Telescope
36 1.3-m hexagonal mirror segments
16.8-m Segmented Telescope
36 2.4-m hexagonal mirror segments
Common Features for all Designs
•
•
•
•
Diffraction limited @ 500 nm
Designed for SE-L2 environment
Non-cryogenic OTA at ~290o K
Heaters stabilize PM temperature to ±
0.1o K
• OTA provides two simultaneously
available foci - narrow FOV Cassegrain
(2 bounce) for Exoplanet & UV
instruments and wide FOV TMA
channel for Gigapixel imager and MOS
• Designed to permit (but not require) onorbit instrument replacement and
propellant replenishment
Technology Development Needed for ATLAST
Technology Development for:
8-m
9.2-m
• Starlight Suppression Systems:
Hi-contrast Coronagraph -orExternal Occulter
• Gigapixel Detector Arrays
Photon-counting Detectors
High Efficiency Dichroics
High Efficiency UV coatings
• Optical Telescope Assembly
Advanced WF Sensing & Control
Fully Active Optics
Lightweight Mirror Materials
Lightweight Mirror Fabrication
Milli-arcsecond pointing control
Flight qualif. of monolithic mirror
Requires engineering,
but no new tech.
• Systems Modeling & Verification
• Autonomous Rendezvous & Docking
TRL6 or higher
TRL4 or higher
TRL3 or lower
16.8-m
Key Objective of Technology Development: Break the Cost Curve
FY08 Cost =$2.44B (Mass/10000 kg)0.654 x (1.555Difficulty
FY2008 Billions (Phase A-D)
$12
Low (-1)
Average (0)
High (1)
Very High (2)
HST
JWST
Kepler
GALEX
Spitzer
Herschel
$10
$8
$6
$4
$2
ATLAST Mass Range
9.2m
$0
0
10000
16.8m
20000
Delta IV HLV
30000
40000
8m
50000
60000
Mass (kg)
Ares V Cargo LV