The VST secondary mirror support system

Schipani, P.; Perrotta, Francesco; Molfese, C.; Caputi, O.; Ferragina, L.; Marty, Laurent; Capaccioli, M.; Gallieni, Daniele; Fumi, Pierluigi; Anaclerio, Enzo; Lazzarini, Paolo; Paris, G. De

doi:10.1117/12.787925

Cited by 14 publications

(7 citation statements)

References 11 publications

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“…The another type of astronomical applications of hexapod robots is the support of the secondary mirror of large telescopes (having a diameter of a few meters). See, for instance Geijo et al (2006) for such applications in the VISTA telescope or Schipani et al (2008) for the VST telescope. The hexapod for supporting the secondary mirror of this telescope is also displayed in Figure 1.6.…”

Section: Motivation For Our Instrument Design: the Hexapodmentioning

confidence: 99%

Instrumentation developments in the aspects of time-domain all-sky surveying autonomous telescopes

Mészáros¹

2019

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Section: Motivation For Our Instrument Design: the Hexapodmentioning

confidence: 99%

Instrumentation developments in the aspects of time-domain all-sky surveying autonomous telescopes

Mészáros¹

2019

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“…It can be tilted for alignment purposes by modifying the positions of three fixed points on the third ring at angles of 120 • . The rigid-body position of the convex hyperbolic secondary mirror can be controlled by a hexapod in 5 degrees of freedom [9][10][11][12]. Additional details on the active optics system can be found in [13][14][15][16].…”

Section: The Telescopementioning

confidence: 99%

Software and control system for the VLT Survey Telescope

et al. 2013

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The VLT Survey Telescope (VST) has started the regular operations in 2011 after a successful commissioning at Cerro Paranal (Chile), the site which hosts the best facilities for optical astronomy operated by the European Southern Observatory (ESO). After a short description of the instrument, this paper mainly focuses on the telescope control software, which is in charge of the real-time control of the hardware and of the overall coordination of the operations, including pointing and tracking, active optics and presets. We describe the main features of the software implementation in the context of the ESO observatory standards, and the goals reached during the commissioning phase and in the first year of operations.

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“…The camera provides an alternative curvature wavefront sensor and a guiding system based on four additional CCDs at the outer edge of the mosaic. Further details on VST subsystems are discussed in [18][19][20][21][22][23][24][25][26].…”

Section: Telescope Overviewmentioning

confidence: 99%

Removing static aberrations from the active optics system of a wide-field telescope

et al. 2012

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The wavefront sensor in active and adaptive telescopes is usually not in the optical path toward the scientific detector. It may generate additional wavefront aberrations, which have to be separated from the errors due to the telescope optics. The aberrations that are not rotationally symmetric can be disentangled from the telescope aberrations by a series of measurements taken in the center of the field, with the wavefront sensor at different orientation angles with respect to the focal plane. This method has been applied at the VLT Survey Telescope on the ESO Paranal observatory.

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The VST secondary mirror support system

Cited by 14 publications

References 11 publications

Instrumentation developments in the aspects of time-domain all-sky surveying autonomous telescopes

Instrumentation developments in the aspects of time-domain all-sky surveying autonomous telescopes

Software and control system for the VLT Survey Telescope

Removing static aberrations from the active optics system of a wide-field telescope

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