Transcript Recompetition - National Optical Astronomy Observatory (NOAO)

Exploring the time domain
• Gamma ray bursters
• Supernovae
• accretion disk instabilities
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galactic to stellar scales
• planetary transits
• moving objects
LSST
LSST, a digital
survey of the
sky each week
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Weak lensing mass
map of the Universe
100,000 supernovae
per year z < 1
Earth crossing asteroids
10,000 primordial transNeptunian objects
View of the LSST telescope structure in the Steward Observatory straw
man design. The primary mirror is at the center, and the secondary and
tertiary are almost equidistant from the primary. The detectors are just
ahead of the central hole in the primary (see: http://dmtelescope.org/
design.html)
LSST Weak Lensing survey
Low z WL
LSST Supernovae
Scan mode
1000’s/yr
Deep Mode
1000’s/yr
Need
IR too
w
MULTIPLE PROBES:
TEST FOUNDATIONS
LSST SN
LSST Lensing
Solar System Objects
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Increase inventory of solar system x100
10,000 NEAs, 90% complete >250m
Over 10 million MBAs
Cometary nuclei >15km @ Saturn
Extend size-n of comets to <100m
TNOs beyond 100AU
rare new objects
NEO Hazard
LSST science working group
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Andy Connolly
Fiona Harrison
Tony Tyson
Michael Strauss chair
Kem Cook
Gary Bernstein
Dave Jewitt
Chris Stubbs
Alan Harris
Dave Monet
 David Morrison
 Nick Kaiser
 Peter Garnavich
 Dennis Zaritsky
 Mike Shara
 Steve Larson
 Alan Stern
 Dan Eisenstein
 Zeljko Ivesic
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LSST SWG Charge
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Develop science case and priorities for LSST
Flowdown to engineering goals & requirements
Identify key instrumentation capabilities
Prepare 10 year Design Reference Mission
Establish the relationship with other facilities
– SNAP, Gemini, VISTA, PanStarrs, Lowell 4 m, VST
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Prioritize key technology developments
Assess design concepts science performance
Assemble community wide partnerships for
proposals to NSF and NASA
Technology Development
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Large field of view telescope
– 8 meter primary
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Detector development
Large filters
Gigapixel camera
Data acquisition system
10-20 petabyte database
National Virtual Observatory
Data mining
Systems engineering
Simulations and theory
Figure of Merit
Area surveyed (number of objects found)
to some SNR at some magnitude limit,
per unit time:
Apparatus & Eff.
Science goals
N φ A Ω QE 
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2
t (SNR) φsky (δΩ)
2
obj
site & optics
A – aperture
 – observing eff.
W – camera FOV
Fsky – sky flux
QE – det. Eff.
dW – seeing footprint
8.4 meter Primary Mirror
3.5 meter Secondary
Trapped Focus
4.2 meter
Tertiary
Primary Mirror Cell is
integral part of Structure
C Ring
The Large Synoptic Survey Telescope
DATA PUBLIC. Simultaneously address:
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Solar System Probes: Earth-crossing asteroids, Comets, TNOs
Space assets & space junk to 1 cm
Dark matter/dark energy via weak lensing
Dark matter/dark energy via supernovae
Galactic Structure encompassing local group
Dense astrometry over 10000 sq.deg -> deep proper motion science
Gamma Ray Bursts and transients to high z
Gravitational mlensing
Variable stars/galaxies
QSO time delays vs z
Transients to 27 mag: the unknown
5-band 28 mag photometric survey
Unprecedented many Pbyte time-tagged photometric database
http://lssto.org
GSMT
Top
optical
infrared
priority
ground
based
of the
McKee
Taylor
decadal
survey
“21st century
astronomy is uniquely
positioned to study the
evolution of the
universe in order to
relate causally the
physical conditions
during the Big Bang to
the development of
RNA & DNA” –
Riccardo Giacconi
Connecting recombination to the formation of planets
Kinematics of Individual Galaxies
out to z ~3
• Determine the gas and
mass dynamics within
individual Galaxies
 Multiple IFU
spectroscopy
R ~ 5,000 – 10,000
GSMT 3 hour, 3s limit
at R=5,000
0.1”x0.1” IFU pixel
(sub-kpc scale structures)
J
26.5
H
25.5
K
24.0
Probing Planet Formation with High
Resolution Infrared Spectroscopy
Planet formation studies in the infrared (5-30µm):
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Planets forming at small distances (< few AU) in warm region of the disk
Spectroscopic studies:
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Residual gas in cleared region
emissions
Rotation separates disk radii in velocity
High spectral resolution
high spatial resolution
S/N=100, R=100,000, >4mm
Gemini
GSMT
JWST
out to 0.2kpc sample ~ 10s
1.5kpc
~100s
X
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8-10m telescopes with high resolution
(R~100,000) spectrographs can detect
the formation of Jupiter-mass planets in
disks around nearby stars (d~100pc).
Comparative performance of a 30m
GSMT with a 6.5m JWST
10
R = 10,000
R = 1,000
R= 5
1
NGST advantage
S/N Gain (GSMT / NGST)
R =
5
= 1
R
,0 0
R =
1 0
, 0
GSMT
advantage
Assuming a detected S/N of 10 for NGST on
a point source,
with
Comparative
performance
of a4x1000s
30m GSTM integration
with a 6.5m NGST
0.1
0.01
1E-3
1
10
Wavelength (microns)
NOAO’s role in GSMT
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partnering with ACURA, UC & Caltech on TMT
Design and Development Phase
site testing
community input on:
• science drivers for a 30m
• complementarities to other
facilities (e.g. JWST, ALMA)
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technology development
• e.g. AODP
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instrumentation
operations role
GSMT Site Evaluation
NIO collaborating with Carnegie, CELT,
Cornell, ESO, UNAM; to test:
• Chajnantor
• One or two additional Chilean Sites
• Mauna Kea ELT site
• Las Campanas
• San Pedro de Martir
Las Campanas Peak 2
Turbulent Kinetic Energy
500 m
CFD Tools available for any proposed ELT site
Giant Segmented Mirror Telescope
Science Working Group
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NSF AST Division authorized NOAO to maintain
the Science Working Group for GSMT
community based body to develop the science
case and justification for any federal investment
by NSF or other agencies in GSMT.
represent US community in assembling relevant
partnerships for describing and advocating the
appropriate federal role in this project.
this guidance is intended to be a product of all
public, private and international groups that
expect to play a role in the GSMT.
GSMT SWG first report June 2003
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Claire Max
Doug Simons
Terry Herter
Irene Cruz Gonzales
Betsy Barton
Francois Rigaut
Michael Bolte
Observer: Tetsuo
Nishimura
Email [email protected] if you’d like a copy
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Paul Ho
Matthew Colless
Jill Bechtold
Rolf Kudritzki chair
Chris McKee
Alan Dressler
Ray Carlberg
Two Studies, One Result
Results from 2 x 2 years of studies:
 It is feasible to build a 30m Telescope that
will fulfill the science objectives of the
AASC, on a time scale comparable to
JWST
– The optics for a ~700m2 mirror can be
manufactured, polished and assembled
– Wind buffeting effects can be managed
– The technologies exist or can be developed to
enable diffraction limited imaging and
spectroscopy in at least the IR
– The instrumentation, though challenging, is
within the capabilities of major institutions and
industry
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The cost for telescope construction,
adaptive optics, initial instrumentation
and including 30% contingency is
between $600M - $700M
GMT Consortium
Giant Magellan
Telescope
 Magellan partners
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– Carnegie, CfA,
– U of A
– Michigan, MIT
GSMT will complement ALMA & JWST
Explore the cosmic era of
reionization and galaxy
assembly
Understand star
formation, now and in the
early Universe
10
mas
at
1.6m