PRIME: PSF Reconstruction and Identification for Multiple-source characterization Enhancement – application to Keck NIRC2 imager

Beltramo-Martin, Olivier; Correia, Carlos; Ragland, Sam; Jolissaint, Laurent; Neichel, Benoît; Fusco, Thierry; Wizinowich, Peter

doi:10.1093/mnras/stz1667

Cited by 20 publications

(21 citation statements)

References 37 publications

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“…Although PSF-reconstruction algorithms have been in existence for a long time (Véran et al 1997;Gendron, E. et al 2006;Gilles et al 2012;Ragland et al 2016;Beltramo-Martin et al 2019), most of them are too complex to implement and are not robust enough to be used blindly in normal operations. The fact that AO techniques have also evolved rapidly in parallel giving birth to a large number of species (e.g.…”

Section: Introductionmentioning

confidence: 99%

Reconstruction of the ground-layer adaptive-optics point spread function for MUSE wide field mode observations

Fusco

Bacon

Kamann

et al. 2020

A&A

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Context. Here we describe a simple, efficient, and most importantly fully operational point-spread-function(PSF)-reconstruction approach for laser-assisted ground layer adaptive optics (GLAO) in the frame of the Multi Unit Spectroscopic Explorer (MUSE) Wide Field Mode. Aims. Based on clear astrophysical requirements derived by the MUSE team and using the functionality of the current ESO Adaptive Optics Facility we aim to develop an operational PSF-reconstruction (PSFR) algorithm and test it both in simulations and using on-sky data.Methods. The PSFR approach is based on a Fourier description of the GLAO correction to which the specific instrumental effects of MUSE Wide Field Mode (pixel size, internal aberrations, etc.) have been added. It was first thoroughly validated with full end-to-end simulations. Sensitivity to the main atmospheric and AO system parameters was analysed and the code was re-optimised to account for the sensitivity found. Finally, the optimised algorithm was tested and commissioned using more than one year of on-sky MUSE data. Results. We demonstrate with an on-sky data analysis that our algorithm meets all the requirements imposed by the MUSE scientists, namely an accuracy better than a few percent on the critical PSF parameters including full width at half maximum and global PSF shape through the kurtosis parameter of a Moffat function. Conclusions. The PSFR algorithm is publicly available and is used routinely to assess the MUSE image quality for each observation. It can be included in any post-processing activity which requires knowledge of the PSF.

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Section: Introductionmentioning

confidence: 99%

Reconstruction of the ground-layer adaptive-optics point spread function for MUSE wide field mode observations

Fusco

Bacon

Kamann

et al. 2020

A&A

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“…Methodology for calculating BAO from WFS measurements is highly spread in the literature (Beltramo-Martin et al 2019;Ragland et al 2018;Jolissaint et al 2015;Gilles et al 2012;Veran et al 1997); practically we used the Vii algorithm proposed by (Gendron et al 2006) where…”

Section: Reconstruction Of Tip-tilt Excluded Modesmentioning

confidence: 99%

“…New approaches must be envisioned to step into the next level of PSF-R. We have introduced the so-called method PRIME (Beltramo- Martin et al 2019) that yields a builtin parametric PSF model using AO measurements. As discussed, the reconstruction relies usually on fudge factors which are learned by comparing PSF-R to on-sky images and set up as constants afterwards.…”

Section: Introduction To Primementioning

confidence: 99%

“…For a given AO data set, we calculate BAO, BTT and BAL, while B ⊥ is computed for once. Contrary to the model presented in Beltramo- Martin et al (2019), we have introduced the gain g al to calibrate the aliasing model. The use of g al allows us to account for fluctuations in the wind speed profile, which enters the computation of the aliasing mode via Eq.…”

Section: Introduction To Primementioning

confidence: 99%

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Pushing point-spread function reconstruction to the next level: application to SPHERE/ZIMPOL

Beltramo-Martin

Marasco

Fusco

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Point spread function (PSF) reconstruction (PSF-R) is a well established technique to determine reliably and accurately the PSF from Adaptive Optics (AO) control loop data. We have successfully applied this technique to improve the precision on photometry and astrometry to observation of NGC6121 obtained with SPHERE/ZIMPOL as it will be presented in a forthcoming letter. Firstly, we present the methodology we followed to reconstruct the PSF combining pupil-plane and focal-plane measurements using using our PSF-R method PRIME (Beltramo-Martin et al. 2019), with upgrade of both the model and best-fitting steps compared to previous papers. Secondly, we highlight that PRIME allows to maintain the PSF fitting residual below 0.2% over 2 hours of observation and using only 30 s of AO telemetry, which may have important consequences for telemetry storage for PSF-R purpose on future 30-40 m class telescopes. Finally, we deploy PRIME in a more realistic regime using faint stars so as to identify the precision needed on the initial guess parameters to ensure the convergence towards the optimal solution.

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“…In this Letter, we exploit a new hybrid technique known as PRIME (Beltramo-Martin et al 2019), which combines PSF-R with image fitting to perform a photometric and astrometric analysis of a small stellar field in the Galactic globular cluster NGC 6121 observed with SPHERE/ZIMPOL (Schmid et al 2018). While the theoretical background has been provided in Beltramo-Martin et al (2020;hereafter BMS), here we focus on the results in terms of the photometric and astrometric precision achieved on these real data.…”

Section: Introductionmentioning

confidence: 99%

Successful application of PSF-R techniques to the case of the globular cluster NGC 6121 (M 4)

Massari

Marasco

Beltramo-Martin

et al. 2020

A&A

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Context. Precise photometric and astrometric measurements on astronomical images require an accurate knowledge of the Point Spread Function (PSF). When the PSF cannot be modelled directly from the image, PSF-reconstruction techniques become the only viable solution. So far, however, their performance on real observations has rarely been quantified. Aims. In this Letter, we test the performance of a novel hybrid technique, called PRIME, on Adaptive Optics-assisted SPHERE/ZIMPOL observations of the Galactic globular cluster NGC 6121. Methods. PRIME couples PSF-reconstruction techniques, based on control-loop data and direct image fitting performed on the only bright point-like source available in the field of view of the ZIMPOL exposures, with the aim of building the PSF model. Results. By exploiting this model, the magnitudes and positions of the stars in the field can be measured with an unprecedented precision, which surpasses that obtained by more standard methods by at least a factor of four for on-axis stars and by up to a factor of two on fainter, off-axis stars.Conclusions. Our results demonstrate the power of PRIME in recovering precise magnitudes and positions when the information directly coming from astronomical images is limited to only a few point-like sources and, thus, paving the way for a proper analysis of future Extremely Large Telescope observations of sparse stellar fields or individual extragalactic objects.

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PRIME: PSF Reconstruction and Identification for Multiple-source characterization Enhancement – application to Keck NIRC2 imager

Cited by 20 publications

References 37 publications

Reconstruction of the ground-layer adaptive-optics point spread function for MUSE wide field mode observations

Reconstruction of the ground-layer adaptive-optics point spread function for MUSE wide field mode observations

Pushing point-spread function reconstruction to the next level: application to SPHERE/ZIMPOL

Successful application of PSF-R techniques to the case of the globular cluster NGC 6121 (M 4)

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