SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 1
The Supernova / Acceleration Probe
(SNAP)
Presentation to the Experimental Program Advisory Committee at SLAC.
November 14, 2003
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 2
SLAC Involvement in SNAP
• With the creation of the Kavli Institute for Particle Astrophysics and Cosmology (KIPAC), experiments addressing issues at the interface between particle physics and astrophysics will play an increasingly prominent role in the SLAC research program.
• Of particular interest will be the “dark sector”, the nature of dark energy and dark matter, and the roles they play in the evolution of the Universe.
• Technology development in connection with the SNAP mission has been a cornerstone of the DOE-OS program addressing the mystery of dark energy.
• We believe that SLAC can and should play a prominent and important role in this mission if it goes forward as currently planned.
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 3
SLAC Involvement in SNAP
• The first discussions about SLAC involvement with the leadership of the SNAP collaboration (S. Perlmutter, M. Levi) were held in February 2003.
• At that time, a potential hardware role in the mission associated with the design and development of the Observatory Control Unit (OCU) was identified.
• We also highlighted our science interest in the use of SNAP data for strong lensing investigations.
• A letter of application for institutional membership in the SNAP collaboration on behalf of Stanford and SLAC was submitted in August 2003. That application is currently still under discussion, but the preliminary responses have been very positive.
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 4
Outline of Presentations
• The Science of Dark Energy and the Design of the SNAP Mission – E. Linder
• Strong Lensing Investigations with SNAP – R. Blandford
• The Observatory Control Unit – M. Huffer
• Concluding Comments – S. Kahn
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 5
National priorities
HEPAP: Scientic potential and facility need – absolutely central
Secretary of Energy (11/10/03) – SNAP has very high priority (#3 on list)
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 6
SLAC and SNAP
SLAC/Stanford major strengths include:
• Strong Gravitational Lensing – Blandford
Dark matter / dark energy / cosmology
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 7
SLAC and SNAP
Observatory control unit expertise – Huffer
Technical experience and development resources
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SNAP OBSERVATORY SYSTEM ELECTRICAL BLOCK DIAGRAM21 AUGUST, 2003H HEETDERKS
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SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 8
SLAC and SNAP
SLAC/Stanford major strengths include:
• Space mission experience – Kahn
Extensive design and implementation
Knowledge of NASA culture
• Experience with joint NASA-DOE projects from GLAST
Collaborative agency working relationships
• Dark Energy and High Energy Physics – Existing and ongoing SNAP theory collaboration by Kallosh & Linde
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 9
Revolutions in Physics
Lord Kelvin (1900): Two clouds on the horizon
The horizon is 95% cloudy!
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 10
Mapping our history
The subtle slowing down and speeding up of the expansion, of distances with time: a(t), maps out cosmic history like tree rings map out the Earth’s climate history.
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 11
Accelerating universe
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 12
What is dark energy?
• 70-75% of the energy density of the universe
• Accelerating the expansion, like inflation
• Determining the fate of the universe
But what is it? Einstein’s cosmological constant ? Problems: fine tuning and coincidence
Matter
Dark energy
Today Size=2 Size=4Size=1/2Size=1/4
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 13
Dark energy – discovery!
accelerating
decelerating > 0 at 99% confidence
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 14
Next generation
Supernova/Acceleration Probe: SNAP
Dedicated dark energy probe
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 15
Mission design
• ~2 m aperture telescope
Reach very distant SNe.
• 1 degree mosaic camera, ½ billion pixels
Efficiently study large numbers of SNe.
• 0.35 – 1.7 m spectrograph
Analyze in detail each SN.
Dedicated instrument designed
to repeatedly observe an area of
sky.
Essentially no moving parts.
3+ year operation for experiment
(lifetime open ended).
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 16
Mission design
Spectrograph
GuiderCCD’s
HgCdTe
BITE
Photometry: half-billion pixel mosaic camera, high-resistivity, rad-tolerant p-type CCDs (0.35-1.0 m) and, HgCdTe arrays (0.9-1.7 m).
Field of View Optical ( 36 CCD’s) = 0.34 sq. deg.
Four filters on each 10.5 m pixel CCD detector
Field of View IR (36 HgCdTe’s) = 0.34 sq. deg.
One filter on each 18 m pixel HgCdTe detector
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 17
Mission design
Field beforeslicing
Pseudo-slit
Slicing mirror (S1)
Spectrogram
Pupil mirrors(S2)
To spectrograph
Field optics (slit mirrors S3)
From telescopeand fore-optics
Input port
Slicer
PrismBK7 Prism
CaF2
NIRdetector
VisDetector
Integral field optical and IR spectroscopy:
0.35-1.7 m,
3”x6” FOV,
low resolution,
high throughput.
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 18
Mission design
15 sq.deg. Deep Survey ~300 sq.deg. Wide Survey
• 9 filters
• mAB=27.7 every 4 days
• 120 epochs • coadd AB=30.3 (31)
GOODS
HDF
• 9 filters
• mAB=28.1
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 19
SN control of systematics
Images
Spectra
Redshift & SN Properties
Lightcurve & Peak Brightness
data analysis physics
M and
Dark Energy Properties
Each supernova sends a rich stream of information about its physical state.
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 20
High energy physics
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Complementarity
Next generation data will map the acceleration of the universe so precisely that it can probe:
• The nature of dark energy w(z)
• Structure of the vacuum
• w´(z) V´ / V()
• High energy physics
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Fate of the universe
a
t
wa=2w´
w0
tdoom= ()
tdoom > 29 Gyr [95% SNAP]
tdoom > 35 Gyr [95%SNAP+CMB]
tdoom > 40 Gyr [95% SN+CMB+WL]
Kallosh, Kratochvil, Linde, Linder, & Shmakova JCAP 2003; astro-ph/0307185
First and simplest DE model: linear potential (Linde 1986) leads to collapsing universe.
Such models look like in the past, but develop a strong w´.
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SNAP Cosmology and Physics
SN IaWeak Lensing
SN IIStrong LensingWide, Deep and Colorful
• 9000 times the area of Hubble Deep Field
• 10 billion years of detailed history
• 108 galaxies, 105 lenses, 9 wavelength bands
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Strong Lensing Program
• Multiple imaging by galaxies, groups and clusters
• Ancillary program - complementary to:– Supernova cosmography– Weak lensing study of large scale structure– Galaxy-galaxy lensing study of galaxy halos
• Telescope nearly ideal for strong lensing because of– 9 filters– 0.1(0.05)” pixels– 4 day cadence– Deep (15 sq deg) and Wide (300 sq deg) surveys
• Lensing rate 0.001-0.002 => ~300,000 “events”– Quantitative, identification pipeline (cf CLASS)– Emphasize standard elliptical galaxy “scattering” with 0.5<z<1
• Complementary to LSST and Square Kilometer Array
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Scientific Goals
• Source Population
– Study the faintest galaxies – building blocks of normal galaxies• redshift distribution
• luminosities
• star formation rates etc
– AGN microlensing– Rare high magnification events
• Lens Population– Galaxy substructure out to R ~ 10kpc– Cluster substructure
• Cosmography
• Propagation Effects– Time delays Þ small scale dark matter distribution– Quasar absorption lines etc
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Source Population
• Understand empirically where when and how small galaxies merge to form larger galaxies
– ~2 x 105 isolated elliptical galaxy lenses on deep field– total cross section ~ 0.02 sq deg
– 10000 (30000) clean lenses on deep field to IAB
~ 28 (30)
– Use lens colors to measure lens distance– Use color maps to separate source from lens, remove dust– Use Einstein ring radius to measure source distance
• 100 times too faint for spectroscopy
– Infer source properties statistically and test CDM theory
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Simulation
• Massive elliptical lens, I=21.5, at zd=0.7
• Faint blue galaxy, B=29, at higher redshift• Fit 9 images with two “spectral” models to reconstruct lensed
source
• Infer zs from Einstein ring radius
• Input images (true color, different intensity scales!):
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Simulation
Simulated SNAP images:
• 0.12” pixels, 0.14” FWHM PSF, no dither • Deep survey, 1.5 mag fainter than HDF• B, V and I-bands shown for illustration:
B (440nm) V (582nm) I (770nm)
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Simulation
Optimal weighting of 9 filters' images allows lens and source components to be separated
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Simulation
Measuring source redshift with:• Einstein ring radius to ±1/4 pixel• Lens photo-z to ±0.02• Lens velocity dispersion to ±10 km s-1
=> Find 1.2 < zs < 1.5 (1) (true value = 1.3)
Lensing provides vital additional information to photo-z at high redshift
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Scientific Goals
• Source Population
– Study the faintest galaxies – building blocks of normal galaxies• redshift distribution
• luminosities
• star formation rates etc
– AGN microlensing– Rare high magnification events
• Lens Population– Galaxy substructure out to R ~ 10kpc– Cluster substructure
• Cosmography
• Propagation Effects– Time delays => small scale dark matter distribution– Quasar absorption lines etc
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Cluster Arc Images
Multi-colour, high resolution surveying and imaging:
RCS0224 (CFHT): Cl0024 (HST):
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Scientific Goals
• Source Population
– Study the faintest galaxies – building blocks of normal galaxies• redshift distribution
• luminosities
• star formation rates etc
– AGN microlensing– Rare high magnification events
• Lens Population– Galaxy substructure out to R ~ 10kpc– Cluster substructure
• Cosmography
• Propagation Effects– Time delays => small scale dark matter distribution– Quasar absorption lines etc
SNAP OCU Project SLAC EPAC Meeting Nov. 14-15, 2003 34
Time delays
• Lens time delays measure the Hubble constant, age of universe
– Accuracy limited by lens model• Currently lens determinations are competitive with traditional
astronomical methods• By the time SNAP is launched this will probably be settled• Small scale structure along the line of sight causes deviation
from apparent pure Hubble expansion• Can measure statistically and check CDM predictions
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B1608+656 delays
Time delays of 1-2 months, measured to precision of 1-2 days...
H0 = 75±6 km s-1 Mpc
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Research underway and planned
• Simulations using Hubble images and projected SNAP resolution (including dithering) and sky/detector noise (Marshall)
– Establish procedure for data analysis pipeline to find clean and dirty lenses
– Establish procedure for refining elliptical potentials– Use Hubble Ultradeep Field to describe source population– Estimate accuracy for determining source properties
• Work with weak lensing group to develop strategy to combine strong and weak lensing studies of galaxy structure (Koopmans)
• Study rare, higher order catastrophes as (Baltz):– highly magnifying telescopes– probes of granularity of dark matter– surveying instruments
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What instrument deliverable does SLAC propose?
• The Observatory Control Unit (OCU)
• Both a hardware (electronics) and software system
• Supervises and manages (on-station) observatory operation
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Electrical Block Diagram
FilterWheel
Mass store
Primary
OCURedundant
Mass store
Redundant
Ka xmtPrimary
Ka xmtRedundant
Power
CD&H
ACS
S-bandTransponde
rPrimary
S-bandTransponde
rRedundant
Focal
Plane
Assembly
OCUPrimary
Shutter
Focus
Thermal
Power
1553 BusAfter H. Heetderks
200 GBytes
Spectrograph
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Functional requirements
• Executes instrument’s observation plan– Transfer pointing requests to ACS– Controls CCD array parameterization and readout
• Science data management– Manage mass store– Route real-time and stored data to downlink transmitters
• Mechanism management, control, and operation– Telescope cover, optical shutter, stepper coils, etc…
• Power distribution and management
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Functional requirements…
• Thermal management– Manage heater elements
• Primary, Secondary mirrors, telescope structure, etc…
– Survival heaters– Monitor and trend temperatures
– Housekeeping» Monitor instrument environment» Packetize and route as telemetry
• Data (Event) readout and acquisition• Command processing and distribution
– Command database definition and maintenance– Decoding, distribution, and execution
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What is the scope of the OCU within the observatory?
• OCU performs electronic supervision of entire instrument
• Encompasses design, specification and implementation of…– The bulk of instrument’s digital electronics – A modest amount of analog electronics– The entire Flight Software System
• Executes the science mission …
• Natural consequence is significant role in defining….– instrument architecture– translation of science objectives to operational program
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How does it fit within SLAC’s current program?
• OCU development requires a unique blend of skills…– Data Acquisition– Detector Monitoring and Control
• SLAC has extensive experience in these areas…– Successful, lead role within 2 major HEP experiments:
• SLD• BaBar
• SLAC has space heritage…– Lead role in both Electronics and Flight Software for GLAST– Demonstrated collaboration with NASA based labs
• SLAC has long history of successful collaboration with LBL– We enjoy a physical proximity…
• Phases well with GLAST and BaBar program– BaBar no longer in development – GLAST moving out of design/development stage
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Concluding Comments
• In October 2003, NASA and DOE announced the results of a year-long discussion regarding the possibility for cooperation in a space-based mission devoted to exploring the nature of dark energy.
• The plan involves the development of a Joint Dark Energy Mission (JDEM).
• NASA/DOE will issue a single AO soliciting a dark energy science investigation requiring a space-based observatory. The science investigation will be PI-led and will be selected via open competition.
• The present schedule shows selection of the science investigation one year after the onset of new funding, leading to launch of the mission eight years later.
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Organization of JDEM
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Concluding Comments
• The proposed plan is for the SLAC team to participate in an LBNL-led proposal for a JDEM science investigation based on the SNAP concept.
• SLAC and LBNL have a long history of close cooperation in high energy physics experiments.
• The differences in culture between the NASA and DOE communities will introduce some challenges in making the JDEM concept work.
• SLAC’s extensive experience working with both agencies in the GLAST program should prove to be a key asset to the SNAP collaboration.
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