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Picture of the Week

Plasma Jet Machining on strongly curved off axis parabolic SiC mirrors

Credit: TNO/IOM/Fred Kamphues

TNO Science and Industry and the Leibniz Institute of Surface Modification (IOM) are developing processes for finishing strongly curved off axis parabolic SiC mirrors. The mirrors form a crucial part of the cryogenic fibre collimators for the Gaia Basic Angle Monitoring Opto-Mechanical Assembly (BAM OMA).

The Gaia BAM OMA is a double Michelson interferometer which measures the basic angle between the two telescopes with an accuracy of better than 0.5 microarcseconds. The Gaia BAM OMA consists of two SiC optical benches with fibre collimators, beam splitters and a large number of folding mirrors.

The off axis parabolic SiC mirrors are designed by TNO in close cooperation with Astrium and were manufactured by Boostec. TNO and IOM use a combination of 3D robot polishing and Plasma Jet Machining (PJM). Plasma enhanced chemical etching is a non-conventional technology for surface machining. The method is based on a microwave or RF excited plasma jet under normal atmospheric pressure or in rough vacuum yielding a high flux of reactive radicals. Material removal is obtained by chemical reactions between the radicals and surface atoms.

Different plasma jet sources have been developed to do deterministic surface shaping and surface figure error correction over a wide spatial range with nanometre accuracy. The half-width of the almost nearly Gaussian like shaped removal functions reaches from about 0.1 mm to about 10 mm. Maximum volume removal rates of about 50mm³/min have been achieved for fused silica and ULE™. Surface machining is accomplished using the dwell time algorithm on CNC controlled multi-axes systems. Far developed mathematical de-convolution routines are used for creating the machining files.

During plasma jet treatment no sub-surface damage occurs in contrast to abrasive methods. This advantage makes the plasma jet technology very attractive for the precise manufacturing of especially spherical and free-form optics. On the other hand the chemical removal mechanism leads to an increase of surface roughness depending on the material and the removal depth. But at the same time potential subsurface damage is removed. A low surface roughness is achieved with a post polishing run on the Zeeko polishing robot at TNO.

The parabolic mirror is made of silicon carbide (SiC) and needs to be polished to a surface error of less than 12.5 nm RMS. The main difficulty of this mirror is its small radius of curvature (R = 50.17 mm) over an effective aperture of 10 mm. During trial runs by IOM and TNO a surface error of 8 nm RMS was achieved. Production of the flight mirrors has started.

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[Published: 19/06/2009]

Picture of the Week archive
2013
04/04: DPCC (CNES)
03/26: Gaia artist impression
02/11: Gaia payload testing
01/04: Space flyby with Gaia-like data
2012
12/10: DPAC OR#2. Testing with Planck
11/05: Galaxy detection with Gaia
10/09: Plot of part of the GUMS-10 catalogue
07/23: "Gaia" meets at Gaia
06/29: The Sky as seen by Gaia
05/31: Panorama of BAM clean room
03/29: GREAT school results
03/12: Scanning-law movie
02/21: Astrometric microlensing and Gaia
02/03: BAM with PMTS
01/12: FPA with all the CCDs and WFSs
2011
12/14: Deployable sunshield
11/10: Earth Trojan search
10/21: First Soyuz liftoff from the French Guiana
09/20: Fast 2D image reconstruction algorithm
09/05: RVS OMA
08/10: 3D distribution of the Gaia catalogue
07/13: Dynamical Attitude Model
06/22: Gaia's view of open clusters
05/27: Accuracy of the stellar transverse velocity
05/13: Vibration test of BAM mirrors
04/18: L. Lindegren, Dr. Honoris Causa of the Observatory of Paris
01/19: Detectability of stars close to Jupiter
01/05: Delivery of the WFS flight models
2010
12/21: The 100th member of CU3
11/17: Nano-JASMINE and AGIS
10/27: Eclipsing binary light curves fitted with DPAC code
10/13: Gaia broad band photometry
09/28: Measuring stellar parameters and interstellar extinction
09/14: M1 mirror
08/27: Quest for Sun siblings
07/23: Surprising finding in the coverage of Gaia
07/09: Binarity of Cepheids
06/25: Honorary doctorate for M. Perryman
06/03: Observing Planck
04/23: M4 mirror
03/15: Hyper-Runaway Candidate
02/26: Auto Collimating Flat Mirror Assembly
01/29: Complete Gaia Torus
2009
12/17: Soyuz launch pad
11/27: M2 mirror
10/23: BAM OMA mirror
09/30: SVN reached the 100000 commit
06/19: Plasma Jet Machining on mirrors
06/03: Gaia Torus Segments
05/15: Variability tree
04/21: Siblings of the Sun
03/27: CTI Effects Models for Gaia
03/11: Global astrometric solution
02/24: Combining Geneva with Hipparcos
02/10: BAM OMA mirror type A
01/27: Astrophysical parameter estimation with Ilium
01/08: Bulge with Gaia
2008
12/05: CCD Support Structure
10/21: RVS Fery Prism Breadboard
10/07: Discrete Source Classifier
09/23: Standard stars for RVS
09/09: MareNostrum
07/25: Wavefront Sensor
07/09: Sky-like mask
06/25: Data Compression Study
06/11: Video Processing Unit
05/22: New CCD test bench
04/25: WMAP and Gaia
03/10: New AGIS results
02/18: M5 mirror
02/04: PLM torus
01/21: Solar Cycle 24
2007
12/17: DPAC cycles
11/12: Thermal Vacuum Facility for FPA
07/02: Gaia Payload
06/11: Launch & Operations
04/05: New e2v test facility
02/26: The Ring Solution verified
2006
11/13: AGIS test results
09/25: Gaia Focal Plane
08/02: GUMS release
04/24: RP spectra
03/27: Gaia telescopes
02/27: First data from RAVE
02/06: L3CCD life tests
01/23: AGIS result
2005
12/19: GAREX
11/14: Variable stars
10/24: Ice Age Epoch
10/03: Asteroid orbits, J2, b
09/05: Milky Way bar
08/22: Detecting MBOs & NEOs
08/08: RGO 1995
07/25: Galaxy remnants
06/27: Cebreros
06/13: EODM testing
05/30: Bulge visibility
05/09: First Look: ODIS
04/25: Radiation testing
04/04: CCD Packaging
03/21: Gaia imaging
03/07: Working Groups
02/21: Gaia logo
02/14: MBP devices
01/31: Proton irradiation
01/24: Asteroids
01/17: MBP filters
01/10: BBP filters
2004
12/20: Astro CCD tests
12/06: FPA baseplate
11/22: Interconnection module
11/08: PE Modules
10/25: Scanning law II
10/11: Reference frame
09/20: Testing L3CCDs
08/30: CCD metrology
08/23: Gaia Symposium
06/28: PoW - first year
06/21: CCD evaluation
06/14: Artistic spacecraft
06/07: Star tracking
05/31: Spectralib
05/24: Digital Universe
05/17: Gaia M1 mirror
05/10: v_t CMD
04/26: Gaia parameter database
04/19: RVS optics design
04/12: Supercomputer
04/05: CCD depletion
03/29: Giant planets
03/22: KBO's
03/01: GS visibility
02/16: Halo accretion
02/09: Filter Design
01/19: Sunshield
01/12: Lund Map
01/05: The ICRF
2003
12/15: Nice meeting
12/08: Scanning law
11/24: Microlensing
11/17: Planet discovery
11/10: Optics test bench
11/03: RVS calibration
10/27: ESTEC
10/20: Baade's window
10/13: Quasars
09/29: First Gaia CCDs
09/22: Cannibal galaxy
09/15: All-sky transits
09/08: Monte Rosa II
09/01: EADS-Astrium
08/25: HD70642
08/18: Catalogues
08/11: Hipparcos
08/04: ESOC
07/28: Light bending
07/21: NEO 1994 XM1
07/14: Monte Rosa I
07/07: SiC facilities
06/30: CCD centroiding
06/23: Soyuz launchers
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