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W. A. E. $. 1 km 2 array version: H igh E nergy A ll S ky T ransient R adiation O bservatory HE - ASTRO. By V. Vassiliev, S. Fegan Ground based g-ray Astronomy: Towards the Future. October 20-22, 2005 UCLA. Hardware implementation. Approach Technologies

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1 km 2 array version h igh e nergy a ll s ky t ransient r adiation o bservatory he astro

W

A

E

$

1 km2 array version:High Energy All Sky Transient Radiation ObservatoryHE-ASTRO

By

V. Vassiliev, S. Fegan

Ground based g-ray Astronomy: Towards the Future. October 20-22, 2005 UCLA

hardware implementation

Hardware implementation

Approach

Technologies

Data Rates & Array Trigger

input parameters from simulations
Input parameters (from simulations)
  • To provide “fly’s eye” operation mode (+- 45 deg sky coverage) FoV >=15 deg is required
  • To sustain CR trigger rate at below 100kHz and operate in ~30-50 GeV domain FoV <25 deg must be used
  • To trigger efficiently in this energy regime “effective” trigger pixel size must be in 0.1-0.2 deg range
  • To reconstruct events in “physics of the shower limited regime” image pixel size must be in the range 0.01-0.02 deg.
  • Optimal pixel size for triggering and imaging differ by a factor of ~10. (by 100 in units of number of “effective” pixels in the camera).
cost embarrassment
Cost Embarrassment
  • FoV =15 deg is ~180 deg2
  • This is equivalent to ~104 “trigger pixels” or 106 “image pixels”
  • To have IACT telescope for <=$1M and FP instrument <= a few $100K the cost per trigger pixel must be in the $10-100 range, and the cost per image pixel must be in $0.1-$1.0 range
  • Current MAPMTs and MCP based MAPMTs are in the range $40-$60 per channel. Current PMTs are in the range above a few $100 depending on the size and some other factors.
  • Oups! To be suitable for imaging with required resolution in 10 years from now the MAPMTs must drop in price by a factor of 10 each year. This can only happen if market of these things will increase so much that every family on the planet will need one. This is not going to happen!
fp plate scale mismatch
FP plate scale mismatch
  • Something very inexpensive with very high level of integration is required such as CCD or CMOS image sensors, or perhaps arrays of SiPMs if they are developed and made cheap.
  • Oups! This devices are very small and to be used as FP instrumentation they would require substantial optical processing of the image to change plate scale without further image distortion. This results in prohibitive light loss in many optical elements and to compensate this would require further increase of the telescope aperture thereby increasing plate scale mismatch problem.
  • Before optical image is conditioned to a small CMOS or CCD plate scale it must be amplified!
slide6

Array of

MAPMTs

Wide field of view optics; possibly of RC type

Fine image

resolution

utilizing CMOS

and CCD

technology

Moderate

size primary

(3-7m)

Large aperture II (Electrostatic or MCP(?)) with extremely rapid image decay time

Fast Gated Image Intensifier

to reduce NSB

1963

Japan: Suga

Italy: ?

Russia: ?

slide8

Energy range

> 1 TeV

Readout

Event Rate

< 1kHz

All sky covered with 80 mega pixels in the CMOS sensor arrays

Optimized Baker-Nunn optical system with three corrector normal lenses

made of acrylic resin and 1 m spherical reflector (spot size less than

1 arcmin, 0.016o, for parallel light rays incident at angles less than 25o).

Focal sphere image intensifier, FIIT, of ~60 cm aperture

focal plane instrumentation
Focal Plane Instrumentation

Fast random access CMOS sensor

Image pixel size – 0.0146o

Readout image –128 x 128 pixels

Readout Image size – 1.875o x 1.875o

Readout rate 30-40 kHz

Optical or

II-based delay

Two-mirror

modified

RC

optical

system

X-Y

Optical

Splitter

Gate & Shutter

OR

X = ∑xi

Y = ∑yi

Amplified Image

Gated Image

Intensifier (MCP)

(25-40 mm)

Gate ~20ns

Rep. rate ~40kHz

P-43/P-24 , ~2msec

Star tracker

VETO

Trigger Sensor

~8200 pixels

with 0.146o

Large Aperture

Image Intensifier

(Electrostatic or MCP)

Photon detection

efficiency ~30-50%

Fast decay scintillator output screen ~25 ns

Primary 3-7m

Fov 15o

e.g. Array of rate

compensated

Discriminators

Slow

Control

cmos image sensor
CMOS Image Sensor

HE-ASTRO Image Sensor is not

commercially available yet.

However, industry is very close

to meet specification. High-speed

readout is achieved with pipeline

and parallel technologies.

Parallel processing macro-cell of

32x32 pixels (1024) can be readout

with > 500 kHz, and 128 x 128 pixel

image (16 macro-cells) with > 30 kHz

Micron-MT9M413

1.3-Megapixel CMOS

Active Pixel Digital

Image Sensor

Image pixel size – 0.0146o

Readout image –128 x 128 pixels

Readout Image size – 1.875o x 1.875o

NSB per pixel – 0.032 (20 nsec gate)

ADC – 8 bit (S/N improved, 10–>8)

Pixel dimension 12mm x 12mm

Sensor area – 12.3 mm x 12.3 mm

Shutter exposure – a few msec

ashra cmos image sensor
Ashra CMOS image sensor
  • Ashra collaboration had worked with FillFactory to develop Ashra Fine Sensor (2048x2048 pixels, 2D control of shutter/exposure and readout).
  • Prototyping from existing LUPA 4000M
  • Readout module is being developed by Toshiba
  • Ultimate goal 128x128 macrocells with 24x24 pixels
  • Status … unknown

IBIS4

1.3 Megapixel

Rolling Shutter

Image Sensor

(LUPA 4000M)

Read out rate is probably a factor of a few x 10 lower than required

ultrafast imaging
Ultrafast Imaging

DRS technologies Inc.

Variety of Ultrafast Cameras

for Military applications

CCD based

500fps to 100,000,000fps

e.g. 350 KHz at 250 x 250 Pixel

exposures from 5 nsec

limited number of frames

120mm tank gun projectile

Photron CMOS based high speed cameras

Ultima APX-RS one of the fastest video cameras with

3,000 mega pixel frames per second (fps) or 250,000 fps

at reduced resolution

FASTCAM-X 1024 PCI is the first system to bring mega-pixel

CMOS to your personal computer at usable speeds; capable

of operating as fast as 1,000 fps at full 1,024 by 1,024 pixel

resolution, or 109,500 fps through ‘windowing‘.

Ultima APX-i2 uses a 25mm MCP Gen II image intensifier,

directly bonded onto the APX's mega pixel sensor to provide

unmatched image quality with 20ns gating.

airgun pellet impacting a matchstick

gated image intensifiers
Gated Image Intensifiers

Left : C9016-2x Series & Controller Center : C9546 Series Right : C9547 Series

Hamamatsu products

Commercial products which

almost satisfy requirements

of resolution, repetition rate,

and fast gating exist.

trigger sensor
Trigger Sensor

Hamamatsu H9500

Flat Panel

52mm square

Bialkali Photocathode

16 x 16 Multianode

12 stage

FoV: 15o

Trigger pixel size: 0.146o

Number of MAPMTs: 32

Effective Area Ratio : 89%

Size: 312 mm

trigger sensor1
Trigger Sensor

Hamamatsu H8500

Flat Panel

52mm square

Bialkali Photocathode

8 x 8 Multianode

12 stage

FoV: 15o

Trigger pixel size: 0.205o

Number of MAPMTs: 69

Effective Area Ratio : 89%

Size: 468 mm

trigger sensor alternatives
Trigger Sensor (alternatives)

Courtesy of

R. Mirzoyan

BURLE85011-501 PLANACON™

71 mm square ( 51.2 mm active)

Bialkali Photocathode

MCP-PMT8 x 8 pixels

Nice single pe pulse

FoV: 15o

Trigger pixel size: >0.135o

Number of MCP-PMTs: 91

Effective Area Ratio : ~52%

Size: 710 mm

Front illuminated SiPMs

(Avalanche Geiger discharge)

3x3 mm2square

5625 pixels of 40µ x 40µ each

FoV: 15o

Trigger pixel size: 0.2o

Number of SiPMs: 1

Effective Area Ratio : ~80%

Size: 3 mm

optical system ritchey chr tien configuration

II

To trigger

To single

camera

Increase of telescope aperture could be achieved by combining several midsize telescopes on the same mount and utilizing optical mixing (single camera) or digital mixing (multiple cameras – possibly more expensive). Various multiplexing options could be explored.

Optical SystemRitchey-Chrétien configuration

FP plate scale is matched with telescope aperture

Field curvature coupled II

For modified RC optical system the field curvature is convex toward the sky.

Primary 3-4 m

Fov 15o

focal plane image intensifier
Focal Plane Image Intensifier

Electrostatic Image Intensifiers

MCP Image Intensifiers

Photek manufactures a range

of 18, 25, 40, 75 and 150 mm

active diameter image intensifiers

(too expensive and too small)

SIEMENS image intensifiers. Large

aperture units (>40cm) are developed

for X-ray imaging.

Phosphor Scintillator P-47 - 80 ns <10%> decay time

Lanthanum Bromide Scintillator, LaBr3 / LaCl3 - 25 ns <10%> decay time

High QE photocathode in 200-400 nm, >25%, continues to be an issue

telescope data pipeline
Telescope data pipeline

~80Mb/s

TD &

Veto

Stars

Trigger

Sensor

Disk

Retrieve

Image to disk

L1

Position encoding

X = ∑xi, Y = ∑yi

Timing T

Array trigger

&

L2 Broadcast

10 ms

Memory Ring

Buffer of

Images

Indexed by

local trigger

timestamp

T

II (int. ~20ns)

OR

L1i

X,Y

delay

Timing

Event

Identification

L2

Telescope

Trigger ~40 kHz

Gated

Image

Intensifier

P-43 ~2msec

Gate 20 ns

~2.3kb

per image

Shatter 2msec

Zero

suppression

~20kb per image

1024x1024

pixels

Readout

128x128 Pixels

1.9o x 1.9o

ADC 10 bits/pixel, 16384 pixels

~600 non-zero pixels (mostly NSB)

Bitmask 20 bits

ADC 10 bits

~1.0 Mpixel CMOS

Image Sensor

(1000-500 fps

full frame)

15o x 15o

SDSS 34 Mb/s

LSST 10 Gb/s= 36 Tb/h

Data rate = 80 Mb/s x 3600 s/h x 217 telescopes= ~62.5 Tb / array / hour

array trigger
Array Trigger
  • Telescope Trigger decision (~30 kHz)
  • Local trigger → convert to GPS timestamp (good to 100ns)
  • Buffer timestamp locally
  • Broadcast “trigger packet” of timestamp and node identifier (~5 bytes) to all nearest and next-nearest neighbors (max. 2Mbps outflow rate)

Distributed →Every node acts as its own array trigger

  • Local trigger together with any trigger of two telescopes from all neighbors and next nearest-neighbors is recognized as array trigger
  • Local processing at node
    • Receive trigger timestamps
    • Buffer trigger timestamps (10-20 μs)
    • Search for a coincidence (compensate for relative delays due to pointing)
    • Coincidence → retrieve pixel data, write to disk (~80 Mb/s)

Data rate to center node

~24 Mbps @ 30 kHz

he astro specs
HE-ASTRO (specs)
  • Image pixel size – 0.0146o
  • Readout image – 128 x 128 pixels
  • Readout Image size –

1.875o x 1.875o

  • NSB per pixel – 0.032 (20 nsec gate)
  • ADC – 8 bit (S/N improved,

10– >8)

  • Pixel dimension 12mm x 12mm
  • Sensor area – 12.3 mm x 12.3 mm
  • Shutter exposure – a few msec
  • Image integration time - 20 ns
  • Optical system TBD
  • Array trigger protocol TBD
  • Data Rates ~80 Mb/secper node
  • Online data processing TBD
  • Array of 217 telescopes
  • Elevation 3.5km
  • Telescopes’ coupling distance 80m
  • Area ~1.0km2 (~1.6km2)
  • Single Telescope Field of View ~15o
  • FoV area ~177 deg2
  • Reflector Diameter ~7m
  • Reflector Area ~40 m2
  • QE 50% (200-400 nm)
  • Trigger sensor pixel size 0.146o
  • Trigger Sensor Size ~31.2cm
  • NSB rate per Trigger pixel ~3.2 pe

per 20 ns

  • Single Telescope NSB Trigger Rate 1KHz
  • Energy Range 20–200 GeV
  • Differential Detection Rate Peak

~30 GeV

  • Single Telescope CR trigger rate

~30 kHz

conclusions
Conclusions
  • Large array of moderate size telescopes may provide a viable cost effective solution to the problem of required large collecting area, large field of view, and low energy threshold at the same time, by combining new and reviving old ideas, e.g. using image intensifiers, but based on the contemporary technology.
  • Design of FP instrumentation requires innovative approach to resolution of a number of challenges. For example, cost vs # of pixels, large telescope aperture vs small imaging sensors (extremely light limited regime), large FoV vs high data rates.
  • Initial feasibility study of a possible implementation of FP instrument indicates that all critical to the project problems might be resolvable already in the next few years since the current state of technology is not too far from achieving required specifications.
  • Detailed feasibility study of proposed FP implementation concept as well as possible alternatives is required