Techniques and Instrumentation for Detection of Exoplanets XI最新文献

Flexible exoplanet observation simulations with psisim 灵活的系外行星观测模拟与psisim

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2677598

Connor Vancil, M. Millar-Blanchaer, Jason Wang, Michael P. Fitzgerald, A. Gibbs, Sofia Hillman, D. Mawet, J. Ruffio

{"title":"Flexible exoplanet observation simulations with psisim","authors":"Connor Vancil, M. Millar-Blanchaer, Jason Wang, Michael P. Fitzgerald, A. Gibbs, Sofia Hillman, D. Mawet, J. Ruffio","doi":"10.1117/12.2677598","DOIUrl":"https://doi.org/10.1117/12.2677598","url":null,"abstract":"Psisim is a software suite that acts as a high-level simulation tool for the development and characterization of instrument performance in stellar and substellar observations. Psisim is capable of modeling science yields, generating simulated spectra, and acting as an exposure time calculator. Its modular framework allows for implementation of various instruments, including imagers and spectrographs. Currently models exist for KPIC, MODHIS, GPI, HISPEC, PSI-Blue and PSI-Red. One of the larger functionalities of psisim is the simulation of exoplanet observations behind adaptive optics systems. Utilizing instrument characteristics, such as Strehl ratio, throughput, etc., and pulling from models generated on the fly or from various common atmospheric grids, psisim is able to return simulated spectra and separate noise components from sky, photon, and thermal sources. We are then able to evaluate instrument performance and perform simulated science programs. We have recently upgraded psisim with a module for observations in polarized light. Manipulation of instrumental Mueller matrices mimics the effect optical components have on incoming light. Inversion of the instrumental Mueller matrices enables recovery of desired Stokes parameters, along with associated observational noise. Here we will provide an overview of psisim, highlighting key features and its adaptability for use with new instruments. We’ll demonstrate how psisim simulates observation with an example, describe a few use cases where it has proved useful, and provide some preliminary results of spectro-polarimetric observations using the new polarimetry mode.","PeriodicalId":222276,"journal":{"name":"Techniques and Instrumentation for Detection of Exoplanets XI","volume":"150 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134288761","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}

引用次数: 0

Coronagraph survey for future exoplanet direct imaging space missions: interim update 未来系外行星直接成像太空任务的日冕调查:临时更新

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2677732

R. Belikov, C. Stark, Pin Chen, K. Fogarty, O. Guyon, R. Juanola-Parramon, J. Krist, D. Mawet, Camilo Mejia Prada, N. Kasdin, B. Mennesson, E. Por, L. Pueyo, S. Redmond, G. Ruane, D. Sirbu, K. Stapelfeldt, J. Trauger, N. Zimmerman, N. Siegler

{"title":"Coronagraph survey for future exoplanet direct imaging space missions: interim update","authors":"R. Belikov, C. Stark, Pin Chen, K. Fogarty, O. Guyon, R. Juanola-Parramon, J. Krist, D. Mawet, Camilo Mejia Prada, N. Kasdin, B. Mennesson, E. Por, L. Pueyo, S. Redmond, G. Ruane, D. Sirbu, K. Stapelfeldt, J. Trauger, N. Zimmerman, N. Siegler","doi":"10.1117/12.2677732","DOIUrl":"https://doi.org/10.1117/12.2677732","url":null,"abstract":"NASA is about to embark on an ambitious program to develop a Habitable Worlds Observatory (HWO) flagship mission to directly image approximately 25 potentially Earth-like planets and spectroscopically characterize them for signs of life, as recommended by the Astro2020 decadal survey. In addition, Astro2020 recommended a new approach for flagship formulation, which involves increasing the scope and depth of early, pre-phase A trades and technology maturation, as part of the new Great Observatories Maturation Program (GOMAP). The critical capability of the HWO mission is starlight suppression. To inform future architecture trades, it is necessary to survey a wide range of technologies, from the relatively mature ones such as the ones described in the LUVOIR and HabEx reports, to the relatively new and emerging ones, which may lead to breakthrough performance. In this paper, we present an interim update on a new effort, initiated by NASA’s Exoplanet Exploration Program (ExEP), to survey coronagraph design options for HWO. We present a preliminary summary of the survey, including: (1) a current list of coronagraph design options; (2) proposed evaluation criteria, such as expected mission yields and feasibility of maturing to TRL5 by 2029; and (3) tools and methods which we are using to quantify evaluations of different designs. While not charged to down-select or prioritize the different coronagraph designs, this survey is expected to be valuable in informing future mission teams of coronagraph design options. All interested coronagraph researchers are welcome to participate in this survey by contacting the first two authors of this paper.","PeriodicalId":222276,"journal":{"name":"Techniques and Instrumentation for Detection of Exoplanets XI","volume":"233 6","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134322983","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}

引用次数: 0

Testbed multi-star wavefront control experiment modeling analysis 试验台多星波前控制实验建模分析

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2676172

Hanying Zhou, D. Marx, C. Prada, D. Sirbu, R. Belikov

{"title":"Testbed multi-star wavefront control experiment modeling analysis","authors":"Hanying Zhou, D. Marx, C. Prada, D. Sirbu, R. Belikov","doi":"10.1117/12.2676172","DOIUrl":"https://doi.org/10.1117/12.2676172","url":null,"abstract":"The Astro2020 Decadal Survey calls for a mission yield goal of 25 or more habitable zone planets detection and characterization in its recommendation of next NASA flagship mission, the Habitable World Observatory (HWO). Multi-Star Wavefront Control (MSWC) is a technique that enables simultaneous star light suppression of a binary or more star system. It has the potential to help achieve the goal by substantially increasing viable target samples to beyond single star systems. Technology development for MSWC has been ongoing for a number of years. Recently a better than 1e-7 monochromatic contrast was demonstrated at JPL’s High Contrast Imaging Testbed (HCIT) with a true binary source having similar Alpha Centauri star system separation for the first time. Here we present (High Order) Wavefront Sensing and Control (HOWFSC) modeling analysis of the testbed experiments for improving future performance. Our model is a modified extension of the HOWFSC engineering model that has proven to be a valuable tool for Roman Coronagraph Instrument (CGI) and was validated on the HCIT. It includes crucial engineering features and factors relevant to testbed (while omitting CGI specific elements) such as probing and sensing with detector noise and finite bandwidth used. The analysis provides important insight into and understanding of MSWC testbed experiments and identifies key performance-limiting factors that were not previously considered. Adjustments in both hardware and WFSC strategy and algorithm are discussed for next round testbed experiments to improve performance necessary for both Roman and HWO.","PeriodicalId":222276,"journal":{"name":"Techniques and Instrumentation for Detection of Exoplanets XI","volume":"48 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"117139798","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}

引用次数: 0

Reflective Lyot-stop low-order wavefront control for future large space telescope coronagraphs 未来大型空间望远镜日冕仪的反射式Lyot-stop低阶波前控制

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2677654

Christopher Mendillo, Jaren Ashcraft, Kevin Z. Derby, Ewan S Douglas, Daewook Kim, J. Males

引用次数: 0

The diffractive interfero coronagraph exoplanet resolver (DICER) 衍射干涉日冕仪系外行星解析器(DICER)

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2678557

H. Newberg, Leaf A. Swordy, Thomas D. Ditto, Richard K. Barry, L. Deming, F. Ravizza

引用次数: 0

Optics testing for SCALES 天平光学测试

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2677808

Aditi Gangadharan, D. Dillon, I. Kain, A. Skemer, R. Kupke, D. Stelter, Pavl Zachary, Nick MacDonald

引用次数: 1

First laboratory demonstration of real-time multi-wavefront sensor adaptive optics 实时多波前传感器自适应光学的首次实验室演示

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2676559

B. Gerard, D. Dillon, S. Cetre, R. Jensen-Clem

{"title":"First laboratory demonstration of real-time multi-wavefront sensor adaptive optics","authors":"B. Gerard, D. Dillon, S. Cetre, R. Jensen-Clem","doi":"10.1117/12.2676559","DOIUrl":"https://doi.org/10.1117/12.2676559","url":null,"abstract":"Exoplanet imaging has thus far enabled studies of wide-orbit (⪆10 AU) giant planet (⪆2 Jupiter masses) formation and giant planet atmospheres, with future 30 meter-class Extremely Large Telescopes (ELTs) needed to image and characterize terrestrial exoplanets. However, current state-of-the-art exoplanet imaging technologies placed on ELTs would still miss the contrast required for imaging Earth-mass habitable-zone exoplanets around low-mass stars by 100x due to speckle noise–scattered starlight in the science image due to a combination of aberrations from the atmosphere after an Adaptive Optics (AO) correction and internal to the telescope and instrument. We have been developing a focal plane wavefront sensing technology called the Fast Atmospheric Self-coherent camera Technique (FAST) to address both of these issues; in this work we present the first results of simultaneous first and second stage AO wavefront sensing and control with a Shack Hartmann Wavefront Sensor (SHWFS) and FAST, respectively, using two common path deformable mirrors. We demonstrate this “multi-WFS single conjugate AO” real-time control at up to 200 Hz loop speeds on the Santa Cruz Extreme AO Laboratory (SEAL) testbed, showing a promising potential for both FAST and similar high-speed diffraction-limited second-stage wavefront sensing technologies to be deployed on current and future observatories, helping to remove speckle noise as the main limitation to ELT habitable exoplanet imaging.","PeriodicalId":222276,"journal":{"name":"Techniques and Instrumentation for Detection of Exoplanets XI","volume":"53 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"128775499","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}

引用次数: 1

Testing and performance of IFS upgrades for GPI 2.0 GPI 2.0的IFS升级测试和性能

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2677675

Dillon H. Peng, J. Chilcote, Q. Konopacky, R. Hamper, Brian Sands, Joel Burke, M. Engstrom, Abigail Karaszewski, Rebecca Boyle, M. Limbach, Alexa Rizika, S. Perera, C. Do Ó, Jayke S. Nguyen, B. Macintosh, J. Fitzsimmons, C. Marois, F. Rantakyrö, Arlene Aleman, J. Maire, R. D. de Rosa, E. Por, D. Savransky, M. Nguyen, M. Perrin, R. Soummer, L. Pueyo, B. Nickson, E. Spalding

引用次数: 0

The telescope simulator for the Fraunhofer telescope Wendelstein 弗劳恩霍夫温德尔施泰因望远镜模拟器

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2676662

F. Grupp, H. Kellermann, F. Lang, C. Gössl, Felix Kummer, Felix Langgaßner, U. Hopp, R. Bender, Juliana F. Erhardt

{"title":"The telescope simulator for the Fraunhofer telescope Wendelstein","authors":"F. Grupp, H. Kellermann, F. Lang, C. Gössl, Felix Kummer, Felix Langgaßner, U. Hopp, R. Bender, Juliana F. Erhardt","doi":"10.1117/12.2676662","DOIUrl":"https://doi.org/10.1117/12.2676662","url":null,"abstract":"The 2.1 m-telescope at Mt.Wendelstein in the German Alps will be equipped with an upgraded multi-focal station, distributing the telescope light of one of the Nasmyth ports to either a high-resolution radial velocity instrument, a Shack-Hartmann wavefront sensor or a three-channel-imager. For feeding calibration light to both, the Shack-Hartmann Sensor and the fiber-fed high-resolution spectrograph, a diffraction-limited telescope simulator is used. This simulator mimics the angular distribution of light (secondary mirror vignetting) of the telescope in order to excite the same modes in the fiber feed as the” real” telescope. This is necessary to allow for m/s calibration by means of an astro frequency comb. As 1 m/s corresponds to about 1/2000 of a 13.5 μm pixel on the R=60000 spectrograph, modal effects are crucial and small changes in the illumination of the fiber have an imprint on the calibration accuracy that can be achieved in simultaneous calibration mode. With this paper we introduce the optical layout of the telescope simulator and its opto-mechanical design, taking into account the space constraints at one of our Nasmyth ports of the telescope. The wavefront performance is verified utilizing a Shack-Hartmann sensor. And it is verified that the system is tolerant to small alignment inaccuracies allowing for a relatively relaxed co-alignment of the telescope simulator and the telescope. Our tests in the laboratory prior to installation of the telescope simulator show small wavefront errors and prove that the optical system of the telescope simulator meets all requirements, including a performance that is diffraction limited (Marechal limit: RMS ⪅ λ/14).","PeriodicalId":222276,"journal":{"name":"Techniques and Instrumentation for Detection of Exoplanets XI","volume":"21 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"121014365","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}

引用次数: 0

SHIMM as an atmospheric profiler on the Nickel telescope 作为镍望远镜上的大气分析器

Techniques and Instrumentation for Detection of Exoplanets XI Pub Date : 2023-10-06 DOI: 10.1117/12.2677510

Ollie Jackson, M. V. Kooten, S. Perera, R. Jensen-Clem, P. Hinz

{"title":"SHIMM as an atmospheric profiler on the Nickel telescope","authors":"Ollie Jackson, M. V. Kooten, S. Perera, R. Jensen-Clem, P. Hinz","doi":"10.1117/12.2677510","DOIUrl":"https://doi.org/10.1117/12.2677510","url":null,"abstract":"Optimal atmospheric conditions are beneficial for detecting exoplanets via high contrast imaging (HCI), as speckles from adaptive optics' (AO's) residuals can make it difficult to identify exoplanets. While AO systems greatly improve our image quality, having access to real-time estimates of atmospheric conditions could also help astronomers use their telescope time more efficiently in the search for exoplanets as well as aid in the data reduction process. The Shack-Hartmann Imaging Motion Monitor (SHIMM) is an atmospheric profiler that utilizes a Shack-Hartmann wavefront sensor to create spot images of a single star in order to reconstruct important atmospheric parameters such as the Fried parameter ($r_0$), $C_n^2$ profile and coherence time. Due to its simplicity, the SHIMM can be directly used on a telescope to get in situ measurements while observing. We present our implementation of the Nickel-SHIMM design for the one meter Nickel Telescope at Lick Observatory. We utilize an HCIPy simulation of turbulence propagating across a telescope aperture to verify the SHIMM data reduction pipeline as we begin on-sky testing. We also used on-sky data from the AO system on the Shane Telescope to further validate our analysis, finding that both our simulation and data reduction pipeline are consistent with previously determined results for the Fried parameter at the Lick Observatory. Finally, we present first light results from commissioning of the Nickel-SHIMM.","PeriodicalId":222276,"journal":{"name":"Techniques and Instrumentation for Detection of Exoplanets XI","volume":"24 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"116279749","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}

引用次数: 0