MAXIM Periscope Module

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MAXIM Periscope Module

• Science Liaison
• H. John Wood
• (Read by Jennifer Bracken)
• 25 April 2003

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Structure and Evolution of the Universe

• In order to study the structure and evolution of
  the universe micro arc-second imaging will be
  required
• X-ray imaging can pierce the dusty centers of
  galaxies in order to study some of the most
  energetic events in creation
• What can you see with micro arc-second imaging in
  the x-ray region of the spectrum?
• accretion disks of black holes
• stellar coronae and interacting binaries
• Cataclysmic variables and X-ray binaries
• Distant Active Galactic Nuclei

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Two globular clusters
These globular clusters both have giant black
holes at their centers
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The Event Horizon can be Imaged by MAXIM
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Purpose of the Study

• An optics oriented study
• Are the mirrors impossible to make?
• Are actuators available to move the mirrors by nm
  steps over microns of range?
• Can the thermal and structural environment be
  benign enough to maintain mirror figure and
  stability?
• Is internal metrology needed if so how to
  implement?
• What would the alignment procedures be?
• Trade study on the mirror sizes and the impact on
  the number and sizes of the spacecrafts
• What are the cost, mass and power inputs?

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The Collecting Area of Chandra for 1/10 The Cost

• Chandra has 0.5 arc sec resolution and its
  mirrors cost 400M
• This study has shown that it is possible to build
  a microarcsec imaging telescope with the same
  collecting area as the current Chandra for 1/10
  its cost
• The study has also shown how the engineering can
  be done to allow X-ray imaging and spectroscopy
  in formation flying
• The nature of the detector allows imaging over a
  large range of energies simultaneously

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Full MAXIM Design Overview

• Configuration at L2
• Hub and 25 free-flyers form an objective over a
  one-kilometer diameter area
• 4-mirror grazing-incidence periscopes in each
  spacecraft reflect x-rays to a detector ship
  20,000 km away
• Alignment of the optical beams and phasing of
  them on the detector allows formation of an image
• Collecting area is 1000 square centimeters the
  entrance aperture is 18.25 by 0.489 cm for each
  periscope
• Thus, each of the 25 free flyers will have 4
  periscopes and the hub will have 12 periscopes
  for a total of 112 periscopes

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Full MAXIM Design Overview cont

• Optical design
• 4-mirror grazing-incidence periscope design
  simulates the properties of a thin lens optical
  tolerances are relaxed in comparison to a typical
  two-mirror X-ray design
• In the periscope, each flat mirror is used at 1
  degree angle of incidence
• Mirrors are known by their numbers in sequence
  they are hit by X-rays (1 entrance, 2, 3 and
  4 exit)
• Flat mirrors are 30 x 20 x 5 cm with the optical
  reflection on the 30 x 20 face (gold coat)
• Graze direction is in the 30 cm direction and
  requires figure quality of lambda/300 (633nm)
• Orthogonal direction only requires lambda/10
• Beam steering with roll and pitch of the exit
  mirror (4)
• Optical path length phasing by motion of a
  daughter bench carrying mirrors 2 and 3
  relative to the main optical bench which hold 1
  and 4 with its actuators

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Side View of a Periscope Module
Mirrors in lilac bench in fuchsia daughter
bench in orange with its actuator in gold
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A Dual-Periscope Module
Note the entrance slots right with one shutter
open one closed
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Up Next

• The Systems Engineering Report will be presented
  by Deborah Amato