LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability...

13
LXO/MagEX Meeting Greenbelt, 24/10/07 lescope Baseline Configuration: maging Capability (Micropore Optic) elescope Field of View ~ 30° x 30° ngular Resolution ~ 1.5 arcminutes etector Pixel Size < 200 μm etector Energy Range ~ 0.2 to 2.0 keV etector Resolution ~ 50 eV FWHM @ 600 eV etector Geometric Area ~ 13 cm x 13 cm otal Instrument Mass ~ 20 – 40 kg nstrument Power ~ 20W operational, 2W standby
  • date post

    19-Dec-2015
  • Category

    Documents

  • view

    217
  • download

    0

Transcript of LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability...

Page 1: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Telescope Baseline Configuration:

• Imaging Capability (Micropore Optic)

• Telescope Field of View ~ 30° x 30°

• Angular Resolution ~ 1.5 arcminutes

• Detector Pixel Size < 200 μm

• Detector Energy Range ~ 0.2 to 2.0 keV

• Detector Resolution ~ 50 eV FWHM @ 600 eV

• Detector Geometric Area ~ 13 cm x 13 cm

• Total Instrument Mass ~ 20 – 40 kg

• Instrument Power ~ 20W operational, 2W standby

Page 2: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Micropore Optics, Leicester Heritage:Optics manufactured to our specification by Photonis (France)

Mercury Imaging X-ray Spectrometer (MIXS) (BepiColombo, ESA)

PI George Fraser (SRC, Leicester)

Status: funded, launch 2013

Wide-Field Auroral Imager (WFAI) (KuaFu, Chinese)

PI Mark Lester (RSPP, Leicester)

Status: proposed, launch ~ 2012

Lobster-Eye Wide-Field Telescope (LWFT) (Spectrum-RG, Russian)

PI George Fraser (SRC, Leicester)

Status: proposed, launch ??

Page 3: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

MIXS-T relatively narrow fov ~ few (TBD) degrees

Page 4: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

LWFT Prototype Support Structure (left)

Page 5: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

LWFT Optic Characteristics

• Focal length = 37.5 cm

• Radius of curvature = 75 cm

• Channel cross-section = 20 µm

• Channel array pitch = 24 µm

• Channel length (MCP thickness) = 1 mm

• MCP size (one plate) = 4 cm x 4 cm

• Channel coating ~ 200 Å Ni

• Support Structure Material = Beryllium Alloy

• Optic Mass ~ < 1 kg

Page 6: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Detector Plane

Detector plane geometric area is half the optic geometric area

Page 7: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Optic

RC FL

20° 30° 40°

50.0 25.0 17.5 26.2 34.9

75.0 37.5 26.2 39.3 52.4

100.0 50.0 34.9 52.4 69.8

50.0 25.0 8.7 13.1 17.5

75.0 37.5 13.1 19.6 26.2

100.0 50.0 17.5 26.2 34.9

~ 170 cm2

Area

~ 380 cm2

Optic

(cm)

Detector

(cm)

Optic and Detector Geometrical Area for FOV & Focal Length

Page 8: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

EPIC-MOS detector plane:

7 x 2.5 cm x 2.5 cm CCDs; Total Geometric Area ~ 44 cm2

Devices, FI MOS CCDs, manufactured by E2V (was EEV)

Page 9: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Large Area focal plane detectors now common in Optical applications

focal plane array (E2V devices)

Gaia (ESA)

Cost ~ 50-100 K Euro/Unit

Page 10: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Large Area Detector (LAD) Program for X-ray Applications

Research joint funded by UK industry (E2V) and PPARC

Application in this case was X-ray macromolecular crystallography

5.5 cm x 4.1 cm active area, 3.2M pixel, 27 µm, 2 MHz pixel readout,

Device is 3-sides buttable

Page 11: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Readout is 130 k pixel s-1 readout, so to read out full frame of 2k x 4k pixels would take ~ 64 s !

On-board binning to 150 µm pixels (~ 2 arc minute on sky) allows

Minimum readout time of 0.64 s (not counting overhead, ~ factor of 2)

Max source count rate ~ 0.8 cts / kilosecond /pixel

Hamamatsu CCD….BI device, 6.69 cm x 3.15 cm, 4-sides buttable

Designed for proposed

HyperSuprime Camera on

Subaru

Focal plane array has 176 CCDs

Page 12: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

PSF Optimum

Centre FOVPSF Optimum

Outer FOV

PSF Optimum

Across FOV

CCD arrangement on Focal Plane ?

Page 13: LXO/MagEX Meeting Greenbelt, 24/10/07 Telescope Baseline Configuration: Imaging Capability (Micropore Optic) Telescope Field of View ~ 30° x 30° Angular.

LXO/MagEX Meeting

Greenbelt, 24/10/07

Technical Issue:

Power

How many CCDs can we operate within

the power budget?

Project Issue (assuming technical solution):

Development Cost

Can we use “off-the-shelf CCDs?”

Bottom-line Detector Issues…to be solved