Zeren Lin, T. Kumar, Xun Chen, Jessica R. Lu, P. Wizinowich, S. Lilley, E. Wetherell, N. McConnell
{"title":"Design of a precision calibration unit for Keck NIRC2 AO instrument","authors":"Zeren Lin, T. Kumar, Xun Chen, Jessica R. Lu, P. Wizinowich, S. Lilley, E. Wetherell, N. McConnell","doi":"10.1117/12.2561958","DOIUrl":"https://doi.org/10.1117/12.2561958","url":null,"abstract":"","PeriodicalId":231205,"journal":{"name":"Adaptive Optics Systems VII","volume":"95 2 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"130721701","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
This paper provides a status update on the Natural Guidestar (NGS) Adaptive Optics (AO) system being built for Castor, the meter class telescope at the Starfire Optical Range. We present a radiometric case study for a range of variable parameters such as source brightness, number of Shack-Hartmann sub-apertures, AO and Track loop frame rate and bandwidth. We gauge system performance by contrast and adapt the error budget to allow detection of a dim object near a bright star. We present wave band splits between the different AO components such as track sensor, wavefront sensor, scoring camera, and science camera. We show the different configurations that allow to switch between dim object and bright object tracking. The opto-mechanical design of the AO system is also presented.
{"title":"High contrast adaptive optics system for meter class telescopes","authors":"M. Mateen, O. Reynolds, M. Eickhoff","doi":"10.1117/12.2563214","DOIUrl":"https://doi.org/10.1117/12.2563214","url":null,"abstract":"This paper provides a status update on the Natural Guidestar (NGS) Adaptive Optics (AO)\u0000system being built for Castor, the meter class telescope at the Starfire Optical Range. We present a radiometric case study for a range of variable parameters such as source brightness, number of Shack-Hartmann sub-apertures, AO and Track loop frame rate and bandwidth. We gauge system performance by contrast and adapt the error budget\u0000to allow detection of a dim object near a bright star. We present wave band splits between the different AO components such as track sensor, wavefront sensor, scoring camera, and science camera. We show the different configurations that allow to switch between dim object and bright object tracking. The opto-mechanical design of the AO system is\u0000also presented.","PeriodicalId":231205,"journal":{"name":"Adaptive Optics Systems VII","volume":"134 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131012497","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
S. Hippler, W. Brandner, S. Scheithauer, M. Kulas, J. Panduro, P. Bizenberger, H. Bonnet, C. Deen, F. Delplancke-Ströbele, F. Eisenhauer, G. Finger, Z. Hubert, J. Kolb, E. Müller, L. Pallanca, J. Woillez, G. Zins
We describe the operation of the infrared wavefront sensing based Adaptive Optics system CIAO. The Coude Infrared Adaptive Optics (CIAO) system is a central auxiliary component of the Very Large Telescope interferometer (VLTI). It enables in particular Galactic Center observations using the GRAVITY interferometric instrument. CIAO compensates for phase disturbances caused by atmospheric turbulence, which all four 8 m Unit Telescopes (UT) experience during observation. Each of the four CIAO units generates an almost diffraction-limited image quality at its UT, which ensures that maximum flux of the observed stellar object enters the input fibers of GRAVITY. We present CIAO performance data obtained in the first 3 years of operation. We describe how CIAO is configured and used for observations with GRAVITY. We focus on the outstanding features of the infrared sensitive Saphira detector, which is used for the first time on Paranal, and show how it works as a wavefront sensor detector.
{"title":"Infrared wavefront sensing for adaptive optics assisted galactic center observations with GRAVITY","authors":"S. Hippler, W. Brandner, S. Scheithauer, M. Kulas, J. Panduro, P. Bizenberger, H. Bonnet, C. Deen, F. Delplancke-Ströbele, F. Eisenhauer, G. Finger, Z. Hubert, J. Kolb, E. Müller, L. Pallanca, J. Woillez, G. Zins","doi":"10.1117/12.2560222","DOIUrl":"https://doi.org/10.1117/12.2560222","url":null,"abstract":"We describe the operation of the infrared wavefront sensing based Adaptive Optics system CIAO. The Coude Infrared Adaptive Optics (CIAO) system is a central auxiliary component of the Very Large Telescope interferometer (VLTI). It enables in particular Galactic Center observations using the GRAVITY interferometric instrument. CIAO compensates for phase disturbances caused by atmospheric turbulence, which all four 8 m Unit Telescopes (UT) experience during observation. Each of the four CIAO units generates an almost diffraction-limited image quality at its UT, which ensures that maximum flux of the observed stellar object enters the input fibers of GRAVITY. We present CIAO performance data obtained in the first 3 years of operation. We describe how CIAO is configured and used for observations with GRAVITY. We focus on the outstanding features of the infrared sensitive Saphira detector, which is used for the first time on Paranal, and show how it works as a wavefront sensor detector.","PeriodicalId":231205,"journal":{"name":"Adaptive Optics Systems VII","volume":"111 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"117177160","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
In 2013, Frazin introduced a statistical inference algorithm that uses simultaneous millisecond exposures in the science camera (SC) and wavefront sensor (WFS) to jointly estimate this NCPA, as well as the exoplanetary image. Here, we provide an update on the advancement of the method, with a focus on the ability to compensate NCPA in real time, and an evaluation of the effect of readout noise on the contrast. Finally, we make conclusions about the practicality of implementing the algorithm on modern and future telescopes, discussing factors such as real time computational requirements and high fidelity model calibrations.
{"title":"Joint estimation of NCPA and exoplanetary image in stationary atmospheric turbulence using millisecond telemetry from the WFS and science camera","authors":"A. Rodack, R. Frazin, J. Males","doi":"10.1117/12.2562890","DOIUrl":"https://doi.org/10.1117/12.2562890","url":null,"abstract":"In 2013, Frazin introduced a statistical inference algorithm that uses simultaneous millisecond exposures in the science camera (SC) and wavefront sensor (WFS) to jointly estimate this NCPA, as well as the exoplanetary image. Here, we provide an update on the advancement of the method, with a focus on the ability to compensate NCPA in real time, and an evaluation of the effect of readout noise on the contrast. Finally, we make conclusions about the practicality of implementing the algorithm on modern and future telescopes, discussing factors such as real time computational requirements and high fidelity model calibrations.","PeriodicalId":231205,"journal":{"name":"Adaptive Optics Systems VII","volume":"6 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"122105906","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Esther Soria Hernández, R. López López, Alejandro Oscoz Abad, Carlos Colodro Conde
Adaptive optics (AO) systems correct atmospheric turbulence in real time and they are normally used in large and medium telescopes but not in modest telescopes due to their size and cost. Here we propose a portable AO instrument capable of being installed in different medium and small-sized telescopes. The novelty of this new instrument is that it is based on the modularization of its components: simulator/calibrator, Wavefront Corrector (WFC) with a deformable mirror (DM) and Wavefront sensor (WFS) modules. This modular concept allows great flexibility in the design, being possible to easily adapt the instrument to the working telescope or instrument by adjusting each module independently. This concept also makes possible the comparison between different types of WFS such as Shack-Hartmann (S-H), Two Pupil Plane Position (TP3) or Pyramidal. Here we present the optical design and expected performance of the three WFS for 1.52m, Carlos Sanchez Telescope (TCS), and the preliminary results of the S-H sensor in laboratory and the first on-sky test.
{"title":"ALIOLI: presentation and first steps","authors":"Esther Soria Hernández, R. López López, Alejandro Oscoz Abad, Carlos Colodro Conde","doi":"10.1117/12.2562277","DOIUrl":"https://doi.org/10.1117/12.2562277","url":null,"abstract":"Adaptive optics (AO) systems correct atmospheric turbulence in real time and they are normally used in large and medium telescopes but not in modest telescopes due to their size and cost. Here we propose a portable AO instrument capable of being installed in different medium and small-sized telescopes. The novelty of this new instrument is that it is based on the modularization of its components: simulator/calibrator, Wavefront Corrector (WFC) with a deformable mirror (DM) and Wavefront sensor (WFS) modules. This modular concept allows great flexibility in the design, being possible to easily adapt the instrument to the working telescope or instrument by adjusting each module independently. This concept also makes possible the comparison between different types of WFS such as Shack-Hartmann (S-H), Two Pupil Plane Position (TP3) or Pyramidal. Here we present the optical design and expected performance of the three WFS for 1.52m, Carlos Sanchez Telescope (TCS), and the preliminary results of the S-H sensor in laboratory and the first on-sky test.","PeriodicalId":231205,"journal":{"name":"Adaptive Optics Systems VII","volume":"9 2","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2020-12-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"120881359","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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