Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT)

O. Citterio, M. M. Civitani, J. Arnold, S. Campana, H. Combrinck, P. Conconi, V. Cotroneo, R. Freeman, E. Mattaini, R. Morton, G. Motta, G. Pareschi, G. Parodi, L. Proserpio, S. Schuler, P. Simpson, G. Tagliaferri, D. Walker

Research output: Chapter in Book/Report/Conference proceedingConference contribution

10 Citations (Scopus)

Abstract

The next generation wide-field X-ray telescope (WFXT) will require an angular resolution of ∼5-10 arcsec almost constant across a wide field of view (∼1 deg2 diameter). To achieve this goal, the design of the optical system has to be based on mirrors characterized by short length and polynomial profiles, as well as focal plane curvature and plate scale corrections. These concepts guarantee an improved angular resolution at large off-axis angle with respect to the normally used Wolter-I configuration. These telescopes are therefore optimal for survey purposes. A significant increase of effective area and grasp with respect to previous missions must also be achieved. This is possible with high precision but at the same time thin (2-3 mm thickness for mirror diameters of 30-110 cm) glass mirror shells. To achieve the goal of 5 arcsec and improve further the technology, we are considering different materials. Fused silica, a well-known material with good thermo-mechanical and polishability characteristics provide the best choice. To bring the mirror shells to the needed accuracy, we are adopting a deterministic direct polishing method (already used for past missions as Einstein, Rosat, Chandra). The technological challenge now is to apply it for almost ten times thinner shells.

LanguageEnglish
Title of host publicationOptics for EUV, X-Ray, and Gamma-Ray Astronomy V
Volume8147
DOIs
Publication statusPublished - 8 Nov 2011
Externally publishedYes
EventOptics for EUV, X-Ray, and Gamma-Ray Astronomy V - San Diego, United States
Duration: 23 Aug 201125 Aug 2011
Conference number: V
https://spie.org/OP11O/conferencedetails/optics-for-euv-x-ray-gamma-ray-astronomy?SSO=1 (Link to Conference Details )

Conference

ConferenceOptics for EUV, X-Ray, and Gamma-Ray Astronomy V
CountryUnited States
CitySan Diego
Period23/08/1125/08/11
Internet address

Fingerprint

X-ray Telescopes
Polishing
Grinding
Wide-field
grinding
polishing
Telescopes
Shell
Mirror
Mirrors
telescopes
mirrors
X rays
Glass
glass
angular resolution
x rays
Fused silica
Optical systems
Fused Silica

Cite this

Citterio, O., Civitani, M. M., Arnold, J., Campana, S., Combrinck, H., Conconi, P., ... Walker, D. (2011). Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT). In Optics for EUV, X-Ray, and Gamma-Ray Astronomy V (Vol. 8147). [814714] https://doi.org/10.1117/12.895309
Citterio, O. ; Civitani, M. M. ; Arnold, J. ; Campana, S. ; Combrinck, H. ; Conconi, P. ; Cotroneo, V. ; Freeman, R. ; Mattaini, E. ; Morton, R. ; Motta, G. ; Pareschi, G. ; Parodi, G. ; Proserpio, L. ; Schuler, S. ; Simpson, P. ; Tagliaferri, G. ; Walker, D. / Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT). Optics for EUV, X-Ray, and Gamma-Ray Astronomy V. Vol. 8147 2011.
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abstract = "The next generation wide-field X-ray telescope (WFXT) will require an angular resolution of ∼5-10 arcsec almost constant across a wide field of view (∼1 deg2 diameter). To achieve this goal, the design of the optical system has to be based on mirrors characterized by short length and polynomial profiles, as well as focal plane curvature and plate scale corrections. These concepts guarantee an improved angular resolution at large off-axis angle with respect to the normally used Wolter-I configuration. These telescopes are therefore optimal for survey purposes. A significant increase of effective area and grasp with respect to previous missions must also be achieved. This is possible with high precision but at the same time thin (2-3 mm thickness for mirror diameters of 30-110 cm) glass mirror shells. To achieve the goal of 5 arcsec and improve further the technology, we are considering different materials. Fused silica, a well-known material with good thermo-mechanical and polishability characteristics provide the best choice. To bring the mirror shells to the needed accuracy, we are adopting a deterministic direct polishing method (already used for past missions as Einstein, Rosat, Chandra). The technological challenge now is to apply it for almost ten times thinner shells.",
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Citterio, O, Civitani, MM, Arnold, J, Campana, S, Combrinck, H, Conconi, P, Cotroneo, V, Freeman, R, Mattaini, E, Morton, R, Motta, G, Pareschi, G, Parodi, G, Proserpio, L, Schuler, S, Simpson, P, Tagliaferri, G & Walker, D 2011, Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT). in Optics for EUV, X-Ray, and Gamma-Ray Astronomy V. vol. 8147, 814714, Optics for EUV, X-Ray, and Gamma-Ray Astronomy V, San Diego, United States, 23/08/11. https://doi.org/10.1117/12.895309

Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT). / Citterio, O.; Civitani, M. M.; Arnold, J.; Campana, S.; Combrinck, H.; Conconi, P.; Cotroneo, V.; Freeman, R.; Mattaini, E.; Morton, R.; Motta, G.; Pareschi, G.; Parodi, G.; Proserpio, L.; Schuler, S.; Simpson, P.; Tagliaferri, G.; Walker, D.

Optics for EUV, X-Ray, and Gamma-Ray Astronomy V. Vol. 8147 2011. 814714.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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AU - Civitani, M. M.

AU - Arnold, J.

AU - Campana, S.

AU - Combrinck, H.

AU - Conconi, P.

AU - Cotroneo, V.

AU - Freeman, R.

AU - Mattaini, E.

AU - Morton, R.

AU - Motta, G.

AU - Pareschi, G.

AU - Parodi, G.

AU - Proserpio, L.

AU - Schuler, S.

AU - Simpson, P.

AU - Tagliaferri, G.

AU - Walker, D.

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AB - The next generation wide-field X-ray telescope (WFXT) will require an angular resolution of ∼5-10 arcsec almost constant across a wide field of view (∼1 deg2 diameter). To achieve this goal, the design of the optical system has to be based on mirrors characterized by short length and polynomial profiles, as well as focal plane curvature and plate scale corrections. These concepts guarantee an improved angular resolution at large off-axis angle with respect to the normally used Wolter-I configuration. These telescopes are therefore optimal for survey purposes. A significant increase of effective area and grasp with respect to previous missions must also be achieved. This is possible with high precision but at the same time thin (2-3 mm thickness for mirror diameters of 30-110 cm) glass mirror shells. To achieve the goal of 5 arcsec and improve further the technology, we are considering different materials. Fused silica, a well-known material with good thermo-mechanical and polishability characteristics provide the best choice. To bring the mirror shells to the needed accuracy, we are adopting a deterministic direct polishing method (already used for past missions as Einstein, Rosat, Chandra). The technological challenge now is to apply it for almost ten times thinner shells.

KW - Deterministic Polishing

KW - Grazing-Incidence

KW - Mirror Shells

KW - Wolter

KW - X-Ray Shells

KW - X-Ray Telescopes

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SN - 9780819487575

VL - 8147

BT - Optics for EUV, X-Ray, and Gamma-Ray Astronomy V

ER -

Citterio O, Civitani MM, Arnold J, Campana S, Combrinck H, Conconi P et al. Progress on precise grinding and polishing of thin glass monolithic shell (towards WFXT). In Optics for EUV, X-Ray, and Gamma-Ray Astronomy V. Vol. 8147. 2011. 814714 https://doi.org/10.1117/12.895309