# Presentation: 004269

## Instrumentation, Technologies, R&DCost & Schedule

- Talk Outline:
- Requirements (throughout)
- CCD Technology
- GigaCAM
- Spectroscopy
- Optics
- Trade-Study/Orbit
- R&D Plan
- Cost
- Schedule

- GigaCAM, a billion pixel CCD array

- SuperNova /Acceleration Probe

- Presented by:  Michael Levi
- December 1, 1999

## Instrumentation Requirements

- Need consistent uniform data set where selection criteria can be applied and systematic sources can be analyzed and factored.
- Minimum data set criteria:
- 1) discovery within 2 days of explosion (peak + 3.8 magnitude),
- 2) 10 high S/N photometry points on lightcurve,
- 3) lightcurve out to plateau (2.5 magnitude from peak),
- 4) high quality spectrophotometry,
- 5) minimize color corrections,
- 6) multiple spectra on lightcurve,
- 7) IR spectra.
- How to obtain both data quantity AND data quality?
- Batch processing techniques -- large multiplex advantage,
- Mostly preprogrammed observations, fixed fields / spin filter wheel
- Wide field imager sensitive to 30th magnitude
- Well calibrated photometry and spectroscopy

## Typical CCD’s

## Fully-Depleted CCD’s

## CCD Technology

- Photoactive region of standard CCD’s are 10-20 microns thick
- Photoactive region of LBNL CCD’s are 300 microns thick

## Quantum Efficiency

- Better overall response than more costly “thinned” devices in use
- High-purity silicon has better radiation tolerance for space applications
- Measured Quantum Efficiency at Lick Observatory (R. Stover):

## Portrait Gallery from Lick ObservatoryLBNL CCD’s

- 2k x 2k

- 2k x 2k

- 200x200
- Lick Obs.
- Orion
- Left: R band
- Rgt: Z band

## Mosaic Packaging

## Imager Technology

## CCD Status

- 2k x 2k (15 m pixels) design successful, meets SNAP performance requirements
- Commercialization at Mitel Corp, Bromont Canada
- Fabricating 2k x 2k (15 m pixels)
- Two separate processing runs (1) Mitel “standard”; (2) LBNL modified process recipe
- Current run of 25 wafers; will be followed by another run when this finishes (January)
- LBNL current fabrication
- 2k x 4k (15 m pixels) for Eschellette Spectrograph and Imager (Keck)
- 2k x 4k (12 m pixels)
- 2k x 4k (10.5 m pixels) for SNAP

- NSF grant to develop technology for astronomy
- Requires further radiation testing (already tested at LBNL 88” cyclotron to 20% of SNAP lifetime exposure w/o degradation)
- Complete commercialization

## GigaCAM

- GigaCAM, a one billion pixel array
- Depending on pixel scale approximately 1 billion pixels (28k x 28k imager)
- ~200 Large format CCD detectors required
- 150K operation
- Issues: detectors, electronics, metrology
- Looks like the SLD vertex detector in Si area (0.1 m2)
- Larger than SDSS camera, smaller than BaBar Vertex Detector (1 m2)

## Optical Photometry Requirements

## IR Photometry Requirements

## Observatory Requirements

## Telescope

- Fully corrected image over one square-degree field.
- Examined two-mirror Ritchey-Chretien & three mirror designs
- Sloane
- Paul-Baker
- Korsch
- Dark Matter Telescope
- New Planetary Telescope (off-axis design)
- Looking for design with intermediate
- waist to facilitate filters & fast steering
- mirror.

- S Sloan

- S Korsch

- Designs that achieve a diffraction-limited 10 FOV in a 2-m aperture:

## S New Planetary Telescope

- S New Planetary Telescope

- S

- S Dark Matter Telescope

- Designs that achieve a diffraction-limited 10 FOV in a 2-m aperture:

## Telescope in Fairing

- Ball concept study

- Off-axis design

## Optics

- HST (2.4m) light-weighted glass 770 kg, for SNAP expect 450 kg light-weighted glass; Delta III lift to orbit > 2800 kg.
**We also have the luxury of considering NGST technology:**
- Rigid mirrors (15 kg/m2)
- Beryllium
- Composite w/ glass face sheet
- C:SiC
- Flexible mirrors (15 kg/m2)
- Glass

## Spectroscopy Technology

- MicroLens Array
- Reflective Image Slicer (e.g. Palomar 200”, NGST IFMOS)

## Spectroscopy w/ fibers

- MicroLens Array:

- From Haynes, astro-ph/9909017

## Integral Field Spectrograph for NGST

- From LAS-NGST-IFMOS-004
- O. Le Fevre, et.al  - Laboratoire d’Astronomie Spatiale in Marseilles

## Integral Field/Multi-Object Spectrograph for NGST

- From LAS-NGST-IFMOS-004
- O. Le Fevre, et.al  - Laboratoire d’Astronomie Spatiale in Marseilles

## Optical Spectrograph Requirements

## IR Spectrograph Requirements

## Trade-Study

- Ball Aerospace Trade-Study

- Selected Lunar Assist “Prometheus” Orbit
- 14 day orbit: 19Re Perigee/57Re Apogee
- 7 day orbit: 8Re Perigee/40Re Apogee

## Orbit

- Lunar Assist “ Prometheus” Orbit
- Direct lunar insertion (two stage Delta III), two mid-course corrections
- Lunar swingby to increase perigee above radiation belts
- At perigee small rocket burn to lower apogee
- Orbit Parameters
- High inclination (up to 70 degrees), high angle of perigee
- 7 day (8/40 Re) or 14 day (19/57 Re) period to avoid lunar perturbations

## Telemetry

- High northern hemisphere orbit has excellent telemetry: ~50 Mbit/s for 19/57 orbit, >50 Mbit/s for 8/40 orbit
- 8 Gbit image every 200s  40 Mbit/s  (no image stacking required)

## Electronics

- GigaCAM Readout looks like high density vertex detector readout with 400 readout channels (two per CCD)
- Design from J.F. Genat (Univ. Paris):

## Electronics

- Custom Readout - Correlated Double Sampler
- Already in development (LBNL/Univ. Paris)

## R&D Cost Plan Estimate

## Preliminary Schedule

## Preliminary Schedule

## Organization

## Depleted Silicon