20 research outputs found
Off-disk straylight measurements for the Swedish 1-meter Solar Telescope
Context. Accurate photometry with ground based solar telescopes requires
characterization of straylight. Scattering in Earth's atmosphere and in the
telescope optics are potentially significant sources of straylight, for which
the point spread function (PSF) has wings that reach very far. This kind of
straylight produces an aureola, extending several solar radii off the solar
disk. Aims. We want to measure such straylight using the ordinary science
instrumentation. Methods. We scanned the intensity on and far off the solar
disk by use of the science cameras in several different wavelength bands on a
day with low-dust conditions. We characterized the far wing straylight by
fitting a model to the recorded intensities involving a multi-component
straylight PSF and the limb darkening of the disk. Results. The measured
scattered light adds an approximately constant fraction of the local
granulation intensity to science images at any position on the disk. The
fraction varied over the day but never exceeded a few percent. The PSFs have
weak tails that extend to several solar radii but most of the scattered light
originates within ~1'. Conclusions. Far-wing scattered light contributes only a
small amount of straylight in SST data. Other sources of straylight are
primarily responsible for the reduced contrast in SST images.Comment: Accepted for publication in Astronomy & Astrophysic
SSTRED: A data-processing and metadata-generating pipeline for CHROMIS and CRISP
We present a data pipeline for the newly installed SST/CHROMIS imaging
spectrometer, as well as for the older SST/CRISP spectropolarimeter. The aim is
to provide observers with a user-friendly data pipeline, that delivers
science-ready data with the metadata needed for archival. We generalized the
CRISPRED data pipeline for multiple instruments and added metadata according to
recommendations worked out as part of the SOLARNET project. We made
improvements to several steps in the pipeline, including the MOMFBD image
restoration. A part of that is a new fork of the MOMFBD program called REDUX,
with several new features that are needed in the new pipeline. The CRISPEX data
viewer has been updated to accommodate data cubes stored in this format. The
pipeline code, as well as REDUX and CRISPEX are all freely available through
git repositories or web download. We derive expressions for combining
statistics of individual frames into statistics for a set of frames. We define
a new extension to the World Coordinate System, that allow us to specify cavity
errors as distortions to the spectral coordinate.Comment: Draf
Multi-frame blind deconvolution and phase diversity with statistical inclusion of uncorrected high-order modes
Images collected with ground-based telescopes suffer blurring and distortions
from turbulence in Earth's atmosphere. Adaptive optics (AO) can only partially
compensate for these effects. Neither multi-frame blind deconvolution (MFBD)
nor speckle techniques restore AO compensated images to the correct power
spectrum and contrast. MFBD can only compensate for a finite number of
low-order aberrations, leaving a tail of uncorrected high-order modes. Speckle
restoration of AO-corrected data depends on calibrations of the AO corrections
and assumptions regarding the height distribution of atmospheric turbulence. We
seek to develop an improvement to MFBD that combines speckle's usage of
turbulence statistics to account for high-order modes with the ability of MFBD
to sense low-order modes that can be partially corrected by AO and/or include
fixed or slowly changing instrumental aberrations. We modify the image
formation model, supplementing the fitted low-order wavefront aberrations with
tails of random high-order aberrations that follow Kolmogorov statistics,
scaled to estimated or measured values of Fried's parameter, r0, that
characterize the strength of the seeing at the moment of data collection. We
refer to this as statistical diversity (SD). We test MFBD with SD with
noise-free synthetic data, simulating many different r0 and numbers of
AO-corrected modes. SD improves the contrasts and power spectra of restored
images, both in accuracy and in consistency with varying r0, without penalty in
processing time. With focus diversity (FD), the results are almost perfect. SD
also reduces errors in the fitted wavefront parameters. MFBD with SD and FD
seems robust with respect to several percents of error in r0. Adding SD to MFBD
shows great promise for improving contrasts and power spectra in restored
images. Further studies with real data are motivated.Comment: Submitted to Astronomy & Astrophysics. Abstract is abridge
Two Dual-Wavelength Sequences of High-Resolution Solar Photospheric Images Captured Over Several Hours and Restored By Use of Phase Diversity
. The collection, seeing compensation, and temporal filtering of two high-resolution time-sequences of solar photospheric images are described. 44 80 image sequences of co-spatial and co-temporal 430.5 nm G band and 436.4 nm continuum filtergrams, were obtained with the 47.5 cm Swedish Vacuum Solar Telescope. One data set covers 5 hours of photospheric evolution; the other covers 8 hours. The field-of-view contains both an enhanced network region, a large pore, and in the longer sequence, a pore forming event. The mean time between frames is 40 s. With a few exceptions, the G band frames are partitioned phase-diverse speckle (PPDS) restorations of three realizations of the atmospheric turbulence acquired rapidly in sequence. Due to strict simultaneity and closely spaced wavelengths, the G band wavefronts, compensated for fixed aberration differences, could also be used for deconvolving the corresponding continuum data. For some of the data, collected during periods of particularly bad seeing, restorations made with a related method, joint phase-diverse speckle, were substituted for the PPDS restorations. Key words. Methods: observational -- Techniques: high angular resolution -- Techniques: image processing -- Sun: granulation -- Sun: magnetic fields -- Sun: photosphere 1