Multi-Spectral Solar Telescope Array

Walker, Arthur B. C.; Lindblom, Joakim F.; O'Neal, Ray H.; Allen, Maxwell J.; Barbee, Troy W.; Hoover, Richard B.

doi:10.1117/12.55640

Cited by 26 publications

(5 citation statements)

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“…Two filters-one situated at the telescope aperture (the entrancefilter) and the other (focal-plane filter) located in front of the focal plane-block off-band light. The wavelength of interest is selected by narrow-passband multilayer mirrors (e.g., Walker et al 1990) for the three EUV telescopes. The fourth telescope views FUV and contains a selector mechanism to choose the wavelength.…”

Section: Instrument and Datamentioning

confidence: 99%

POINT-SPREAD FUNCTIONS FOR THE EXTREME-ULTRAVIOLET CHANNELS OFSDO/AIA TELESCOPES

Poduval

DeForest

Schmelz

et al. 2013

ApJ

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We present the stray-light point-spread functions (PSFs) and their inverses we characterized for the Atmospheric Imaging Assembly (AIA) EUV telescopes on board the Solar Dynamics Observatory (SDO) spacecraft. The inverse kernels are approximate inverses under convolution. Convolving the original Level 1 images with them produces images with improved stray-light characteristics. We demonstrate the usefulness of these PSFs by applying them to two specific cases: photometry and differential emission measure (DEM) analysis. The PSFs consist of a narrow Gaussian core, a diffraction component, and a diffuse component represented by the sum of a Gaussian-truncated Lorentzian and a shoulder Gaussian. We determined the diffraction term using the measured geometry of the diffraction pattern identified in flare images and the theoretically computed intensities of the principal maxima of the first few diffraction orders. To determine the diffuse component, we fitted its parameterized model using iterative forward-modeling of the lunar interior in the SDO/AIA images from the 2011 March 4 lunar transit. We find that deconvolution significantly improves the contrast in dark features such as miniature coronal holes, though the effect was marginal in bright features. On a percentage-scattering basis, the PSFs for SDO/AIA are better by a factor of two than that of the EUV telescope on board the Transition Region And Coronal Explorer mission. A preliminary analysis suggests that deconvolution alone does not affect DEM analysis of small coronal loop segments with suitable background subtraction. We include the derived PSFs and their inverses as supplementary digital materials.

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Section: Instrument and Datamentioning

confidence: 99%

POINT-SPREAD FUNCTIONS FOR THE EXTREME-ULTRAVIOLET CHANNELS OFSDO/AIA TELESCOPES

Poduval

DeForest

Schmelz

et al. 2013

ApJ

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“…Cassegrainian (MSSTA [102][103][104], TRACE [105,106], HiLiTE [107], XDT [108], AIA [27,46,109], and SUVI [110] telescopes) and Ritchey−Chrétien systems (EIT [111], MSSTA [100,[102][103][104], EUVI [112], SPIRIT [113,114], SWAP [115,116]; ARKA [117,118], TESIS [39,62,119], and Hi−C [120] telescopes) are the ones used most often in astrophysics. Herschelian (MSSTA [102][103][104], SPIRIT [113,114], Solar Orbiter EUI [121,122]) and Gregorian (Solar Orbiter EUI [121,122]) systems are used less frequently.…”

Section: Designs Of Normal Incidence Telescopesmentioning

confidence: 99%

Focusing diffraction optics for orbital telescopes

Лидер

2022

Optics and Spectroscopy

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The review is devoted to the principles, state of the art and problems of diffractive optics used to focus X-ray and γ-radiation in telescopes at orbital stations. Various multilayer structures for normal incidence telescopes, supermirrors for Wolter optics, Laue lens as a soft γ-radiation concentrator, as well as modified Fresnel zone plates for focusing radiation in a wide energy range with an unprecedented high angular resolution (10-1-10-3''). Keywords: X-ray and γ-radiation, X-ray and γ-telescopes, diffraction, multilayer structures, Laue lens, Fresnel zone plates.

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“…The telescope structure has been designed to fit inside the existing Multi-Spectral Solar Telescope Array (MSSTA) rocket truss, which flew three times between 1991 and 2002 7,8 . We conducted finite element analysis of the design in this configuration in order to assess the instrument's performance in a rocket flight; see Figure 2.…”

Section: Figurementioning

confidence: 99%

The high-resolution lightweight telescope for the EUV (HiLiTE)

Martinez-Galarce

Boerner

Soufli

et al. 2008

Space Telescopes and Instrumentation 2008: Ultraviolet to Gamma Ray

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The High-resolution Lightweight Telescope for the EUV (HiLiTE) is a Cassegrain telescope that will be made entirely of Silicon Carbide (SiC), optical substrates and metering structure alike. Using multilayer coatings, this instrument will be tuned to operate at the 465 Å Ne VII emission line, formed in solar transition region plasma at ~500,000 K. HiLiTE will have an aperture of 30 cm, angular resolution of ~0.2 arc seconds and operate at a cadence of ~5 seconds or less, having a mass that is about ¼ that of one of the 20 cm aperture telescopes on the Atmospheric Imaging Assembly (AIA) instrument aboard NASA's Solar Dynamics Observatory (SDO). This new instrument technology thus serves as a path finder to a post-AIA, Explorer-class missions.

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Multi-Spectral Solar Telescope Array

Cited by 26 publications

References 0 publications

POINT-SPREAD FUNCTIONS FOR THE EXTREME-ULTRAVIOLET CHANNELS OFSDO/AIA TELESCOPES

POINT-SPREAD FUNCTIONS FOR THE EXTREME-ULTRAVIOLET CHANNELS OFSDO/AIA TELESCOPES

Focusing diffraction optics for orbital telescopes

The high-resolution lightweight telescope for the EUV (HiLiTE)

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