Review of PSF reconstruction methods and application to post-processing

Beltramo-Martin, Olivier; Ragland, Sam; Fétick, Romain; Correia, Carlos; Dupuy, Trent J.; Fiorentino, Giulian; Fusco, Thierry; Jolissaint, Laurent; Kamann, Sebastian; Marasco, Antonino; Massari, D.; Neichel, Benoît; Schreiber, Laura; Wizinowich, Peter

doi:10.1117/12.2560805

Cited by 9 publications

(9 citation statements)

References 52 publications

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“…We then compared the measure EE core;OBS with those computed using Eqs. ( 6) and (7). The results are reported in Fig.…”

Section: Appendix A: a Practical Relation Linking Sr Fwhm And Eementioning

confidence: 87%

“…In other words, we encourage the use of aperture referring to actual, post-AO light distribution that implicitly takes into account the broadening due to residual vibrations. To quantify the limits of applicability of the relation in Equation (7), we performed a simple simulation. We convolved the diffraction limited PSF, oversampled by a factor 5, with a 2D Gaussian functions of varying standard deviations (from 1 to 20 mas).…”

Section: Discussionmentioning

confidence: 99%

“…For comparison, it results from telemetry that the amount of tip-tilt only in the WF residuals sum up to 3.9 mas, indicating that other peak-broadening are likely occurring (i.e., defocusastigmatisms, chromatic dispersion). Equation (7) provides accurate results only under particular conditions. The major requirement is that the low-order aberration effect needs to be smaller than the EE aperture.…”

Section: Appendix A: a Practical Relation Linking Sr Fwhm And Eementioning

confidence: 99%

“…All these methods have been extensively described in Ref. 7. Focal-plane-based methods by default include the non common path aberrations (NCPA) components, which means that imperfections in the optics of the instruments are automatically included in the reconstruction.…”

Section: Introductionmentioning

confidence: 99%

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Point spread function reconstruction for SOUL + LUCI LBT data

Simioni

Arcidiacono

Wagner

et al. 2022

J. Astron. Telesc. Instrum. Syst.

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Here, we present the status of an ongoing project aimed at developing a point spread function (PSF) reconstruction software for adaptive optics (AO) observations. In particular, we test for the first time the implementation of pyramid wave-front sensor data on our algorithms. As a first step in assessing its reliability, we applied the software to bright, on-axis, point-like sources using two independent sets of observations, acquired with the single-conjugated AO upgrade for the Large Binocular Telescope. Using only telemetry data, we reconstructed the PSF by carefully calibrating the instrument response. The accuracy of the results has been first evaluated using the classical metric: specifically, the reconstructed PSFs differ from the observed ones by <2% in Strehl ratio and 4.5% in full-width at half maximum. Moreover, the recovered encircled energy associated with the PSF core is accurate at 4% level in the worst case. The accuracy of the reconstructed PSFs has then been evaluated by considering an idealized scientific test-case consisting in the measurements of the morphological parameters of a compact galaxy. In the future, our project will include the analysis of anisoplanatism, low signal-to-noise ratio regimes, and the application to multi-conjugated AO observations.

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“…We then compared the measure EE core;OBS with those computed using Eqs. ( 6) and (7). The results are reported in Fig.…”

Section: Appendix A: a Practical Relation Linking Sr Fwhm And Eementioning

confidence: 87%

Section: Discussionmentioning

confidence: 99%

Section: Appendix A: a Practical Relation Linking Sr Fwhm And Eementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Point spread function reconstruction for SOUL + LUCI LBT data

Simioni

Arcidiacono

Wagner

et al. 2022

J. Astron. Telesc. Instrum. Syst.

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“…These algorithms generally require a careful characterisation of the system PSF, which can be done following distinct reconstruction approaches (see e.g. Beltramo-Martin et al 2020). That de-blending will inevitably introduce residuals that impact the S/N of the host spectrum and images.…”

Section: Band-filter Images and Host Galaxy Parametersmentioning

confidence: 99%

HARMONI view of the host galaxies of active galactic nuclei around cosmic noon

García-Lorenzo

Monreal-Ibero

Pereira-Santaella

et al. 2022

A&A

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Context. The formation and evolution of galaxies appear linked to the growth of supermassive black holes, as evidenced by empirical scaling relations in nearby galaxies. Understanding this co-evolution over cosmic time requires the revelation of the dynamical state of galaxies and the measurement of the mass of their central black holes (MBH) at a range of cosmic distances. Bright active galactic nuclei (AGNs) are ideal for this purpose. Aims. The High Angular Resolution Monolithic Optical and Near-infrared Integral field spectrograph (HARMONI), the first light integral-field spectrograph for the Extremely Large Telescope, will transform visible and near-infrared ground-based astrophysics thanks to its advances in sensitivity and angular resolution. We aim to analyse the capabilities of HARMONI to reveal the stellar morpho-kinematic properties of the host galaxies of AGNs at about cosmic noon. Methods. We made use of the simulation pipeline for HARMONI (HSIM) to create mock observations of representative AGN host galaxies at redshifts around cosmic noon. We used observations taken with the Multi Unit Spectroscopic Explorer of nearby galaxies showing different morphologies and dynamical stages combined with theoretical AGN spectra to create the target inputs for HSIM. Results. According to our simulations, an on-source integration time of three hours should be enough to measure the MBH and to trace the morphology and stellar kinematics of the brightest host galaxies of AGNs beyond cosmic noon. For host galaxies with stellar masses < 1011 M⊙, longer exposure times are mandatory to spatially resolve the stellar kinematics.

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The Mysterious Lives of Speckles. I. Residual Atmospheric Speckle Lifetimes in Ground-based Coronagraphs

Males

Fitzgerald

Belikov

et al. 2021

PASP

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High-contrast imaging observations are fundamentally limited by the spatially and temporally correlated noise source called speckles. Suppression of speckle noise is the key goal of wavefront control and adaptive optics (AO), coronagraphy, and a host of post-processing techniques. Speckles average at a rate set by the statistical speckle lifetime, and speckle-limited integration time in long exposures is directly proportional to this lifetime. As progress continues in post-coronagraph wavefront control, residual atmospheric speckles will become the limiting noise source in high-contrast imaging, so a complete understanding of their statistical behavior is crucial to optimizing high-contrast imaging instruments. Here we present a novel power spectral density method for calculating the lifetime, and develop a semi-analytic method for predicting intensity PSDs behind a coronagraph. Considering a frozen-flow turbulence model, we analyze the residual atmosphere speckle lifetimes in a MagAO-X-like AO system as well as 25-39 m giant segmented mirror telescope scale systems. We find that standard AO control shortens atmospheric speckle lifetime from ∼130 ms to ∼50 ms, and predictive control will further shorten the lifetime to ∼20 ms on 6.5 m MagAO-X. We find that speckle lifetimes vary with diameter, wind speed, seeing, and location within the AO control region. On bright stars lifetimes remain within a rough range of ∼20 ms to ∼100 ms. Due to control system dynamics there are no simple scaling laws which apply across a wide range of system characteristics. Finally, we use these results to argue that telemetry-based post-processing should enable groundbased telescopes to achieve the photon-noise limit in high-contrast imaging.

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Review of PSF reconstruction methods and application to post-processing

Cited by 9 publications

References 52 publications

Point spread function reconstruction for SOUL + LUCI LBT data

Point spread function reconstruction for SOUL + LUCI LBT data

HARMONI view of the host galaxies of active galactic nuclei around cosmic noon

The Mysterious Lives of Speckles. I. Residual Atmospheric Speckle Lifetimes in Ground-based Coronagraphs

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