The imaging performance of the Hubble Space Telescope

Burrows, Christopher J.; Holtzman, Jon A.; Faber, S. M.; Bély, Pierre Y.; Hasan, H.; Lynds, C. R.; Schroeder, Daniel J.

doi:10.1086/185950

Cited by 82 publications

(55 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…HST suffers from 0.25 µm RMS of spherical aberration caused by an improperly figured primary mirror, preventing the telescope from achieving proper focus 7 . Prior to the 1 st servicing mission in December 1993, when corrective optics were installed, HST was set to be near paraxial focus, so that rays from the center of the primary were in focus but those from the outer (marginal) regions of the mirror were not.…”

Section: Simulation Of Aberrated (Pre-correction) Camera Psfsmentioning

confidence: 99%

20 years of Hubble Space Telescope optical modeling using Tiny Tim

Krist¹,

Hook²,

Stoehr³

2011

SPIE Proceedings

364

184

View full text Add to dashboard Cite

Point spread function (PSF) models are critical to Hubble Space Telescope (HST) data analysis. Astronomers unfamiliar with optical simulation techniques need access to PSF models that properly match the conditions of their observations, so any HST modeling software needs to be both easy-to-use and have detailed information on the telescope and instruments. The Tiny Tim PSF simulation software package has been the standard HST modeling software since its release in early 1992. We discuss the evolution of Tiny Tim over the years as new instruments and optical properties have been incorporated. We also demonstrate how Tiny Tim PSF models have been used for HST data analysis. Tiny Tim is freely available from tinytim.stsci.edu.

show abstract

Section: Simulation Of Aberrated (Pre-correction) Camera Psfsmentioning

confidence: 99%

20 years of Hubble Space Telescope optical modeling using Tiny Tim

Krist¹,

Hook²,

Stoehr³

2011

SPIE Proceedings

364

184

View full text Add to dashboard Cite

show abstract

“…Prior to this operation, the HST PSF contained a sharp core of about 0.1 arcsec FWHM, surrounded by a very broad halo (Burrows et al 1991). The PSF was dependant upon the camera, the position in the field, and also upon time.…”

Section: Experiments With "Hst-like" Psf'smentioning

confidence: 99%

“…the PSF phst0 was built from a series of 4 gaussians, and is intended to approximate the mean radial profile of the HST PSF as given by Burrows et al (1991). It was truncated at a radius of 60 pixels or 2.58 arcsec.…”

Section: Experiments With "Hst-like" Psf'smentioning

confidence: 99%

Artefacts in the deconvolution of images of E-S0 galaxies

Michard

1996

Astron. Astrophys. Suppl. Ser.

View full text Add to dashboard Cite

Abstract. -Unexpected circumnuclear isophotal structures were observed during tests of Lucy's deconvolution technique, performed upon high resolution CFHT frames. They contain an enhanced nuclear disk surrounded by a "boxy" ring; an upward hump in ellipticity corresponds with this ring. Such structures are produced in the deconvolution of synthetic images having large enough surface brightness gradients and ellipticities, as is the case for two of our test galaxies. Similar stuctures occur in convolving and deconvolving model galaxies with a model of the HST's PSF prior to the telescope renovation, but they are limited in radial extent up to less than 1 arcsec of isophotal major axis. If the deconvolution is performed with a PSF differing somewhat from the one used in the convolution, large and far extending artefacts can occur.

show abstract

“…Algorithmically deblurring single telescope images has had a long history. At first during the 1970s, when Richardson [23] and Lucy [19] independently introduced a Poisson-based iterative deconvolution method, generally known as the Richardson-Lucy, and then during the early days of the Hubble Space Telescope when researchers rushed to remove the blur induced by the misaligned optics Burrows et al [5], Cunningham & Anthony [8], Krist & Hasan [16], Lucy & Hook [18], Nunez & Llacer [22]. Most of these techniques rely on a variation of an iterative deconvolution using a known point spread function (PSF).…”

Section: Introductionmentioning

confidence: 99%

Robust statistics for image deconvolution

Lee

Budavàri

White

et al. 2017

Astronomy and Computing

View full text Add to dashboard Cite

We present a blind multiframe image-deconvolution method based on robust statistics. The usual shortcomings of iterative optimization of the likelihood function are alleviated by minimizing the M -scale of the residuals, which achieves more uniform convergence across the image. We focus on the deconvolution of astronomical images, which are among the most challenging due to their huge dynamic ranges and the frequent presence of large noise-dominated regions in the images. We show that high-quality image reconstruction is possible even in super-resolution and without the use of traditional regularization terms. Using a robust ρ-function is straightforward to implement in a streaming setting and, hence our method is applicable to the large volumes of astronomy images. The power of our method is demonstrated on observations from the Sloan Digital Sky Survey (Stripe 82) and we briefly discuss the feasibility of a pipeline based on Graphical Processing Units for the next generation of telescope surveys.

show abstract

The imaging performance of the Hubble Space Telescope

Cited by 82 publications

References 0 publications

20 years of Hubble Space Telescope optical modeling using Tiny Tim

20 years of Hubble Space Telescope optical modeling using Tiny Tim

Artefacts in the deconvolution of images of E-S0 galaxies

Robust statistics for image deconvolution

Contact Info

Product

Resources

About