The Orthogonal Transfer CCD

Tonry, J.; Burke, Barry E.; Schechter, Paul L.

doi:10.1086/133989

Cited by 62 publications

(46 citation statements)

References 10 publications

(11 reference statements)

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“…It features a gigapixel camera (GPC1; 1.44 billion pixels) with a field of view of ∼7 deg 2 , which gives a pixel scale of 0.3". The camera uses a new CCD technology called orthogonal transfer arrays (Tonry et al 1997(Tonry et al , 2006Burke et al 2007) that allow charges to move in both spatial directions in real time to compensate for the image motion caused by the atmosphere and tracking inaccuracies of the telescope. The orthogonal transfer array technology thus provides a tip-tilt correction in the electronics, rather than through manipulation of the secondary mirror, theoretically allowing for subarcsecond seeing over the full field of view, rather than just inside the isoplanatic angle around the center of the field.…”

Section: Introductionmentioning

confidence: 99%

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

Grav

Jedicke

Denneau

et al. 2011

Publications of the Astronomical Society of the Pacific

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ABSTRACT. We present here the Pan-STARRS Moving Object Processing System (MOPS) Synthetic Solar System Model (S3M), the first-ever attempt at building a comprehensive flux-limited model of the major small-body populations in the solar system. The goal of the S3M is to provide a valuable tool in the design and testing of the MOPS software, and will be used in the monitoring of the upcoming Pan-STARRS 1 all-sky survey, which started science operations during late spring of 2010. The model is composed of synthetic populations of near-Earth objects (NEOs with a subpopulation of Earth impactors), the main-belt asteroids (MBAs), Jovian Trojans, Centaurs, trans-Neptunian objects (classical, resonant, and scattered trans-Neptunian objects [TNOs]), Jupiter-family comets (JFCs), long-period comets (LPCs), and interstellar comets. The model reasonably reproduces the true populations to a minimum of V ¼ 24:5, corresponding to approximately the expected limiting magnitude for Pan-STARRS's ability to detect moving objects. The NEO synthetic population has been extended to H < 25 (corresponding to objects of about 50 m in diameter), allowing for close flybys of the Earth to be modeled.

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Section: Introductionmentioning

confidence: 99%

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

Grav

Jedicke

Denneau

et al. 2011

Publications of the Astronomical Society of the Pacific

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“…Anecdotal evidence from other telescopes 9,10 suggests that the isokinetic angle for this type of correction is up to 3 arcmin. We will define three cases: (a) "pessimistic" with an isokinetic angle of 1 arcmin, (b) "neutral" with an angle of 2 arcmin, and (c) "optimistic" with an angle of 3 arcmin.…”

Section: Guide Star Availabilitymentioning

confidence: 98%

COATLI: an all-sky robotic optical imager with 0.3 arcsec image quality

et al. 2016

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COATLI will provide 0.3 arcsec FWHM images from 550 to 900 nm over a large fraction of the sky. It consists of a robotic 50-cm telescope with a diffraction-limited fast-guiding imager. Since the telescope is small, fast guiding will provide diffraction-limited image quality over a field of at least 1 arcmin and with coverage of a large fraction of the sky, even in relatively poor seeing. The COATLI telescope will be installed at the at the Observatorio Astronómico Nacional in Sierra San Pedro Mártir, México, during 2016 and the diffraction-limited imager will follow in 2017.

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“…On short timescales telescope jitter, tracking errors and atmospheric seeing can change the footprint of a beam on the telescope and spectrograph optics and can modulate the detected intensity to create spurious polarization. On long timescales optical coatings oxidize (van Harten et al 2009) making calibrations unstable in time. As non-equatorial telescopes track a target, mirrors rotate with respect to the field to change the properties of the optical system.…”

Section: Spectropolarimetric Instruments Errors and Suppression Tecmentioning

confidence: 99%

Calibrating and stabilizing spectropolarimeters with charge shuffling and daytime sky measurements

Harrington

Kuhn

Nevin

2015

A&A

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Well-calibrated spectropolarimetry studies at resolutions of R > 10 000 with signal-to-noise ratios (S/Ns) better than 0.01% across individual line profiles, are becoming common with larger aperture telescopes. Spectropolarimetric studies require high S/N observations and are often limited by instrument systematic errors. As an example, fiber-fed spectropolarimeters combined with advanced line-combination algorithms can reach statistical error limits of 0.001% in measurements of spectral line profiles referenced to the continuum. Calibration of such observations is often required both for cross-talk and for continuum polarization. This is not straightforward since telescope cross-talk errors are rarely less than ∼1%. In solar instruments like the Daniel K. Inouye Solar Telescope (DKIST), much more stringent calibration is required and the telescope optical design contains substantial intrinsic polarization artifacts. This paper describes some generally useful techniques we have applied to the HiVIS spectropolarimeter at the 3.7 m AEOS Telescope on Haleakala. HiVIS now yields accurate polarized spectral line profiles that are shot-noise limited to 0.01% S/N levels at our full spectral resolution of 10 000 at spectral sampling of ∼100 000. We show line profiles with absolute spectropolarimetric calibration for cross-talk and continuum polarization in a system with polarization cross-talk levels of essentially 100%. In these data the continuum polarization can be recovered to one percent accuracy because of synchronized charge-shuffling model now working with our CCD detector. These techniques can be applied to other spectropolarimeters on other telescopes for both night and daytime applications such as DKIST, TMT, and ELT which have folded non-axially symmetric foci.

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The Orthogonal Transfer CCD

Cited by 62 publications

References 10 publications

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

The Pan-STARRS Synthetic Solar System Model: A Tool for Testing and Efficiency Determination of the Moving Object Processing System

COATLI: an all-sky robotic optical imager with 0.3 arcsec image quality

Calibrating and stabilizing spectropolarimeters with charge shuffling and daytime sky measurements

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