TY - GEN
T1 - DiskFM
T2 - Ground-Based and Airborne Instrumentation for Astronomy VIII 2020
AU - Mazoyer, Johan
AU - Arriaga, Pauline
AU - Hom, Justin
AU - Millar-Blanchaer, Maxwell A.
AU - Chen, Christine
AU - Wang, Jason
AU - Duchêne, Gaspard
AU - Patience, Jennifer
AU - Pueyo, Laurent
N1 - Funding Information:
This material is based upon work supported by the National Science Foundation under Astronomy and Astrophysics Grant No. 1616097 (JM). JM acknowledges support for part of this work was provided by NASA through the NASA Hubble Fellowship grant #HST -HF2-51414 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. This work uses observations obtained at the Gemini Observatory.
Publisher Copyright:
© 2020 SPIE
PY - 2020
Y1 - 2020
N2 - Because of bright starlight leakage in coronagraphic raw images, faint astrophysical objects such as exoplanets can only be detected using powerful point spread function (PSF) subtraction algorithms. However, these algorithms have strong effects on faint objects of interest, and often prevent precise spectroscopic analysis and scattering property measurements of circumstellar disks. For this reason, PSF-subtraction effects is currently the main limitations to the precise characterization of exoplanetary dust with scattered-light imaging. Forward modeling techniques have long been developed for point source objects (Pueyo 2016). However, Forward Modeling with disks is complicated by the fact that the disk cannot be simplified using a simple point source convolved by the PSF as the astrophysical model; all hypothetical disk morphologies must be explored to understand the subtle and non-linear effects of the PSF subtraction algorithm on the shape and local geometry of these systems. Because of their complex geometries, the forward-modeling process has to be repeated tens or hundred of thousands of times on disks with slightly different physical properties. All of these geometries are then compared to the PSF-subtracted image of the data, within an MCMC or a Chi-square wrapper. In this paper, we present here DiskFM, a new open-source algorithm included in the PSF subtraction algorithms package pyKLIP. This code allows to produce fast forward-modeling for a variety of observation strategies (ADI, SDI, ADI+SDI, RDI). pyKLIP has already been used for SPHERE/IRDIS and GPI data. It is readily available on all instruments supported by pyKLIP (SPHERE/IFS, SCExAO/CHARIS), and can be quickly adapted for other coronagraphic instruments.
AB - Because of bright starlight leakage in coronagraphic raw images, faint astrophysical objects such as exoplanets can only be detected using powerful point spread function (PSF) subtraction algorithms. However, these algorithms have strong effects on faint objects of interest, and often prevent precise spectroscopic analysis and scattering property measurements of circumstellar disks. For this reason, PSF-subtraction effects is currently the main limitations to the precise characterization of exoplanetary dust with scattered-light imaging. Forward modeling techniques have long been developed for point source objects (Pueyo 2016). However, Forward Modeling with disks is complicated by the fact that the disk cannot be simplified using a simple point source convolved by the PSF as the astrophysical model; all hypothetical disk morphologies must be explored to understand the subtle and non-linear effects of the PSF subtraction algorithm on the shape and local geometry of these systems. Because of their complex geometries, the forward-modeling process has to be repeated tens or hundred of thousands of times on disks with slightly different physical properties. All of these geometries are then compared to the PSF-subtracted image of the data, within an MCMC or a Chi-square wrapper. In this paper, we present here DiskFM, a new open-source algorithm included in the PSF subtraction algorithms package pyKLIP. This code allows to produce fast forward-modeling for a variety of observation strategies (ADI, SDI, ADI+SDI, RDI). pyKLIP has already been used for SPHERE/IRDIS and GPI data. It is readily available on all instruments supported by pyKLIP (SPHERE/IFS, SCExAO/CHARIS), and can be quickly adapted for other coronagraphic instruments.
KW - Data analysis
KW - Differential imaging
KW - High-contrast imaging
KW - Software
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U2 - 10.1117/12.2560091
DO - 10.1117/12.2560091
M3 - Conference contribution
AN - SCOPUS:85107488296
T3 - Proceedings of SPIE - The International Society for Optical Engineering
BT - Ground-Based and Airborne Instrumentation for Astronomy VIII
A2 - Evans, Christopher J.
A2 - Bryant, Julia J.
A2 - Motohara, Kentaro
PB - SPIE
Y2 - 14 December 2020 through 22 December 2020
ER -