arXiv - PHYS - Instrumentation and Methods for Astrophysics最新文献

{"title":"A background-estimation technique for the detection of extended gamma-ray structures with IACTs","authors":"Tina Wach, Alison Mitchell, Lars Mohrmann","doi":"arxiv-2409.02527","DOIUrl":"https://doi.org/arxiv-2409.02527","url":null,"abstract":"Estimation of the amount of cosmic-ray induced background events is a\u0000challenging task for Imaging Atmospheric Cherenkov Telescopes (IACTs). Most\u0000approaches rely on a model of the background signal derived from archival\u0000observations, which is then normalised to the region of interest (ROI) and\u0000respective observation conditions using emission-free regions in the\u0000observation.This is, however, disadvantageous for the analysis of large,\u0000extended $gamma$-ray structures, where no sufficient source free region can be\u0000found. We aim to address this issue by estimating the normalisation of a\u00003-dimensional background model template from separate, matched observations of\u0000emission-free sky regions. As a result, the need for a emission-free region in\u0000the field of view of the observation becomes unnecessary. For this purpose, we\u0000implement an algorithm to identify observation pairs with as close as possible\u0000observation conditions. The open-source analysis package Gammapy is utilized\u0000for estimating the background rate, facilitating seamless adaptation of the\u0000framework to many $gamma$-ray detection facilities. Public data from the High\u0000Energy Stereoscopic System (H.E.S.S.) is employed to validate this methodology.\u0000The analysis demonstrates that employing a background rate estimated through\u0000this run-matching approach yields results consistent with those obtained using\u0000the standard application of the background model template. Furthermore, the\u0000compatibility of the source parameters obtained through this approach with\u0000previous publications and an analysis employing the background model template\u0000approach is confirmed, along with an estimation of the statistical and\u0000systematic uncertainties introduced by this method.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217508","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}

{"title":"An efficient observational strategy for the detection of the Oort cloud","authors":"Eran O. Ofek, Sarah A. Spitzer, Guy Nir","doi":"arxiv-2409.02170","DOIUrl":"https://doi.org/arxiv-2409.02170","url":null,"abstract":"The Oort cloud is presumably a pristine relic of the Solar System formation.\u0000Detection of the Oort cloud may provide information regarding the stellar\u0000environment in which the Sun was born and on the planetesimal population during\u0000the outer planets' formation phase. The best suggested approach for detecting\u0000Oort cloud objects in situ, is by searching for sub-second occultations of\u0000distant stars by these objects. Following Brown & Webster, we discuss the\u0000possibility of detecting Oort cloud objects by observing near the quadrature\u0000direction. Due to the Earth's projected velocity, the occultations are longer\u0000near the quadrature direction and are therefore easier to detect, but have\u0000lower rate. We show that, for <1-m size telescopes, the increased exposure time\u0000will result in about one to three orders of magnitude increase in the number of\u0000detectable stars that have an angular size smaller than the Fresnel scale and\u0000are therefore suitable for an occultation search. We discuss the ability of\u0000this method to detect Oort cloud objects using existing survey telescopes, and\u0000we estimate the detection rate as a function of the power-law index of the size\u0000distribution of the Oort cloud objects and their distance from the Sun. We show\u0000that occultations detected using ~1-s integration by <1-m telescopes at the\u0000optimal region near the quadrature points will be marginally dominated by Oort\u0000cloud objects rather than Kuiper belt objects.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"85 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217515","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}

{"title":"CCAT: Nonlinear effects in 280 GHz aluminum kinetic inductance detectors","authors":"Cody J. Duell, Jason Austermann, James R. Burgoyne, Scott C. Chapman, Steve K. Choi, Abigail T. Crites, Rodrigo G. Freundt, Anthony I. Huber, Zachary B. Huber, Johannes Hubmayr, Ben Keller, Lawrence T. Lin, Alicia M. Middleton, Colin C. Murphy, Michael D. Niemack, Thomas Nikola, Darshan Patel, Adrian K. Sinclair, Ema Smith, Gordon J. Stacey, Anna Vaskuri, Eve M. Vavagiakis, Michael Vissers, Samantha Walker, Jordan Wheeler","doi":"arxiv-2409.02271","DOIUrl":"https://doi.org/arxiv-2409.02271","url":null,"abstract":"Prime-Cam, a first-generation science instrument for the Atacama-based Fred\u0000Young Submillimeter Telescope, is being built by the CCAT Collaboration to\u0000observe at millimeter and submillimeter wavelengths using kinetic inductance\u0000detectors (KIDs). Prime-Cam's 280 GHz instrument module will deploy with two\u0000aluminum-based KID arrays and one titanium nitride-based KID array, totaling\u0000approximately 10,000 detectors at the focal plane, all of which have been\u0000fabricated and are currently undergoing testing. One complication of fielding\u0000large arrays of KIDs under dynamic loading conditions is tuning the detector\u0000tone powers to maximize signal-to-noise while avoiding bifurcation due to the\u0000nonlinear kinetic inductance. For aluminum-based KIDs, this is further\u0000complicated by additional nonlinear effects which couple tone power to\u0000resonator quality factors and resonant frequencies. While both nonequilibrium\u0000quasiparticle dynamics and two-level system fluctuations have been shown to\u0000give rise to qualitatively similar distortions, modeling these effects\u0000alongside nonlinear kinetic inductance is inefficient when fitting thousands of\u0000resonators on-sky with existing models. For this reason, it is necessary to\u0000have a detailed understanding of the nonlinear effects across relevant detector\u0000loading conditions, including how they impact on on-sky noise and how to\u0000diagnose the detector's relative performance. We present a study of the\u0000competing nonlinearities seen in Prime-Cam's 280 GHz aluminum KIDs, with a\u0000particular emphasis on the resulting distortions to the resonator line shape\u0000and how these impact detector parameter estimation.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"77 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217513","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}

{"title":"Diffraction Gratings for X-ray Spectroscopy","authors":"Ralf K. Heilmann, David P. Huenemoerder, Jake A. McCoy, Randall L. McEntaffer","doi":"arxiv-2409.02297","DOIUrl":"https://doi.org/arxiv-2409.02297","url":null,"abstract":"X-ray diffraction gratings play an essential role in high-resolution\u0000spectroscopy of astrophysical phenomena. We present some scientific highlights\u0000from the X-ray grating spectrometers (XGS) on board of the Chandra and\u0000XMM/Newton missions, XGS optical design, and the basic physics of grating\u0000diffraction geometry and efficiency. We review design, fabrication, and\u0000performance of the currently orbiting transmission and reflection grating\u0000elements, followed by descriptions of the state-of-the art of more advanced\u0000grating technologies that promise orders-of-magnitude improvements in XGS\u0000performance, especially in combination with advanced X-ray telescope mirrors. A\u0000few key science questions that require new grating technology are posed, and\u0000powerful future mission concepts and recent and approved missions are\u0000presented.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"292 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217512","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}

{"title":"Development of the 220/270 GHz Receiver of BICEP Array","authors":"The BICEP/Keck CollaborationStanford University, :Stanford University, Y. NakatoStanford University, P. A. R. AdeCardiff University, Z. AhmedKIPAC/SLAC, M. AmiriUniversity of British Columbia, D. BarkatsHarvard/CfA, R. Basu ThakurCaltechNASA JPL, C. A. BischoffUniversity of Cincinnati, D. BeckStanford UniversityKIPAC/SLAC, J. J. BockCaltechNASA JPL, V. BuzaUniversity of Chicago, B. CantrallStanford University, J. R. Cheshire IVMinnesota Institute for Astrophysics, J. CornelisonHarvard/CfA, M. CrumrineUniversity of Minnesota, A. J. CukiermanCaltech, E. DenisonNIST, M. DierickxHarvard/CfA, L. DubandSBT Grenoble, M. EibenHarvard/CfA, B. D. ElwoodHarvard/CfAHarvard University, S. FatigoniUniversity of British ColumbiaCaltech, J. P. FilippiniUniversity of Illinois Urbana-ChampaignUniversity of Illinois Urbana-Champaign, A. FortesStanford University, M. GaoCaltech, C. GiannakopoulosUniversity of Cincinnati, N. Goeckner-WaldStanford University, D. C. GoldfingerKIPAC/SLAC, J. A. GraysonStanford University, P. K. GrimesHarvard/CfA, G. HallUniversity of Minnesota, G. HalalStanford University, M. HalpernUniversity of British Columbia, E. HandUniversity of Cincinnati, S. HarrisonUniversity of British Columbia, S. HendersonKIPAC/SLAC, J. HubmayrNIST, H. HuiCaltech, K. D. IrwinStanford UniversityKIPAC/SLACNIST, J. KangStanford UniversityCaltech, K. S. KarkareKIPAC/SLAC, E. KarpelStanford University, S. KefeliCaltech, J. M. KovacHarvard/CfAHarvard University, C. L. KuoStanford UniversityKIPAC/SLAC, K. LauCaltech, M. LautzenhiserUniversity of Cincinnati, A. LennoxUniversity of Illinois Urbana-Champaign, T. LiuStanford University, K. G. MegerianNASA JPL, M. MillerHarvard/CfA, L. MinutoloCaltech, L. MoncelsiCaltech, H. T. NguyenNASA JPL, R. O'BrientCaltechNASA JPL, A. PatelCaltech, M. PetroffHarvard/CfA, A. R. PolishHarvard/CfAHarvard University, T. ProuveSBT Grenoble, C. PrykeMinnesota Institute for AstrophysicsUniversity of Minnesota, C. D. ReintsemaNIST, T. RomandCaltech, M. SalatinoStanford University, A. SchillaciCaltech, B. L. SchmittHarvard/CfAUniversity of Pennsylvania, B. SingariMinnesota Institute for Astrophysics, A. SolimanCaltechNASA JPL, T. St. GermaineHarvard/CfAHarvard University, A. SteigerCaltech, B. SteinbachCaltech, R. SudiwalaCardiff University, K. L. ThompsonStanford UniversityKIPAC/SLAC, C. TuckerCardiff University, A. D. TurnerNASA JPL, C. VergèsHarvard/CfA, A. WanduiCaltech, A. C. WeberNASA JPL, J. WillmertUniversity of Minnesota, W. L. K. WuKIPAC/SLAC, H. YangStanford University, E. YoungStanford UniversityKIPAC/SLAC, C. YuStanford University, L. ZengHarvard/CfA, C. ZhangStanford UniversityCaltech, S. ZhangCaltech","doi":"arxiv-2409.02296","DOIUrl":"https://doi.org/arxiv-2409.02296","url":null,"abstract":"Measurements of B-mode polarization in the CMB sourced from primordial\u0000gravitational waves would provide information on the energy scale of inflation\u0000and its potential form. To achieve these goals, one must carefully characterize\u0000the Galactic foregrounds, which can be distinguished from the CMB by conducting\u0000measurements at multiple frequencies. BICEP Array is the latest-generation\u0000multi-frequency instrument of the BICEP/Keck program, which specifically\u0000targets degree-scale primordial B-modes in the CMB. In its final configuration,\u0000this telescope will consist of four small-aperture receivers, spanning\u0000frequency bands from 30 to 270 GHz. The 220/270 GHz receiver designed to\u0000characterize Galactic dust is currently undergoing commissioning at Stanford\u0000University and is scheduled to deploy to the South Pole during the 2024--2025\u0000austral summer. Here, we will provide an overview of this high-frequency\u0000receiver and discuss the integration status and test results as it is being\u0000commissioned.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217511","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}

{"title":"NEW-MUSIC: The Next-generation Extended-Wavelength Multiband Sub/millimeter Inductance Camera","authors":"Sunil R. Golwala, Andrew D. Beyer, Daniel Cunnane, Peter K. Day, Fabien Defrance, Clifford F. Frez, Xiaolan Huang, Junhan Kim, Jean-Marc Martin, Jack Sayers, Shibo Shu, Shiling Yu","doi":"arxiv-2409.02307","DOIUrl":"https://doi.org/arxiv-2409.02307","url":null,"abstract":"The Next-generation Extended Wavelength-MUltiband Sub/millimeter Inductance\u0000Camera (NEW-MUSIC) on the Leighton Chajnantor Telescope (LCT) will be a\u0000first-of-its-kind, six-band, transmillimeter-wave (\"trans-mm\") polarimeter\u0000covering 2.4 octaves of spectral bandwidth to open a new window on the trans-mm\u0000time-domain frontier, in particular new frontiers in energy, density, time, and\u0000magnetic field. NEW-MUSIC's broad spectral coverage will also enable the use of\u0000the Sunyaev-Zeldovich effects to study accretion, feedback, and dust content in\u0000the hot gaseous haloes of galaxies and galaxy clusters. Six-band spectral\u0000energy distributions, with polarization information, will yield new insights\u0000into stellar and planetary nurseries. NEW-MUSIC will employ hierarchical,\u0000phased arrays of polarization-sensitive superconducting slot-dipole antennas,\u0000coupled to photolithographic bandpass filters, to nearly optimally populate\u0000LCT's 14' field-of-view with six spectral bands over 80-420 GHz (1:5.25\u0000spectral dynamic range; 2.4 octaves). Light will be routed to Al or AlMn\u0000microstripline-coupled, parallel-plate capacitor, lumped-element kinetic\u0000inductance detectors (MS-PPC-LEKIDs), an entirely new KID architecture that\u0000substantially enhances design flexibility while providing background-limited\u0000performance. Innovative, wide-bandwidth, etched silicon structures will be used\u0000to antireflection-treat the back-illuminated focal plane. NEW-MUSIC will\u0000cost-effectively reuse much of the MUSIC instrument, initially deploying a\u0000quarter-scale focal plane capable of the bulk of NEW-MUSIC science followed\u0000later by a full-FoV focal plane needed for NEW-MUSIC wide-area survey science.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"33 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142217509","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}

{"title":"Predicting RSO Populations Using a Neighbouring Orbits Technique","authors":"Benjamin F. CookeCentre for Space Domain Awareness, University of Warwick, UKDepartment of Physics, University of Warwick, UK, James A. BlakeCentre for Space Domain Awareness, University of Warwick, UKDepartment of Physics, University of Warwick, UK, Paul ChoteCentre for Space Domain Awareness, University of Warwick, UKDepartment of Physics, University of Warwick, UK, James McCormacCentre for Space Domain Awareness, University of Warwick, UKDepartment of Physics, University of Warwick, UK, Don PollaccoCentre for Space Domain Awareness, University of Warwick, UKDepartment of Physics, University of Warwick, UK","doi":"arxiv-2408.04966","DOIUrl":"https://doi.org/arxiv-2408.04966","url":null,"abstract":"The determination of the full population of Resident Space Objects (RSOs) in\u0000Low Earth Orbit (LEO) is a key issue in the field of space situational\u0000awareness that will only increase in importance in the coming years. We\u0000endeavour to describe a novel method of inferring the population of RSOs as a\u0000function of orbital height and inclination for a range of magnitudes. The\u0000method described uses observations of an orbit of known height and inclination\u0000to detect RSOs on neighbouring orbits. These neighbouring orbit targets move\u0000slowly relative to our tracked orbit, and are thus detectable down to faint\u0000magnitudes. We conduct simulations to show that, by observing multiple passes\u0000of a known orbit, we can infer the population of RSOs within a defined region\u0000of orbital parameter space. Observing a range of orbits from different orbital\u0000sites will allow for the inference of a population of LEO RSOs as a function of\u0000their orbital parameters and object magnitude.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947737","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}

{"title":"A Method of Rapidly Deriving Late-type Contact Binary Parameters and Its Application in the Catalina Sky Survey","authors":"JinLiang Wang, Xu Ding, JiaJia Li, JianPing Xiong, Qiyuan Cheng, KaiFan Ji","doi":"arxiv-2408.04896","DOIUrl":"https://doi.org/arxiv-2408.04896","url":null,"abstract":"With the continuous development of large optical surveys, a large number of\u0000light curves of late-type contact binary systems (CBs) have been released.\u0000Deriving parameters for CBs using the the WD program and the PHOEBE program\u0000poses a challenge. Therefore, this study developed a method for rapidly\u0000deriving light curves based on the Neural Networks (NN) model combined with the\u0000Hamiltonian Monte Carlo (HMC) algorithm (NNHMC). The neural network was\u0000employed to establish the mapping relationship between the parameters and the\u0000pregenerated light curves by the PHOEBE program, and the HMC algorithm was used\u0000to obtain the posterior distribution of the parameters. The NNHMC method was\u0000applied to a large contact binary sample from the Catalina Sky Survey, and a\u0000total of 19,104 late-type contact binary parameters were derived. Among them,\u00005172 have an inclination greater than 70 deg and a temperature difference less\u0000than 400 K. The obtained results were compared with the previous studies for 30\u0000CBs, and there was an essentially consistent goodness-of-fit (R2) distribution\u0000between them. The NNHMC method possesses the capability to simultaneously\u0000derive parameters for a vast number of targets. Furthermore, it can provide an\u0000extremely efficient tool for rapid derivation of parameters in future sky\u0000surveys involving large samples of CBs.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"59 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947738","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}

{"title":"Artemis-enabled Stellar Imager (AeSI): A Lunar Long-Baseline UV/Optical Imaging Interferometer","authors":"Gioia Rau, Kenneth G. Carpenter, Tabitha Boyajian, Michelle Creech-Eakman, Julianne Foster, Margarita Karovska, David Leisawitz, Jon A. Morse, David Mozurkewich, Sarah Peacock, Noah Petro, Paul Scowen, Breann Sitarski, Gerard van Belle, Erik Wilkinson","doi":"arxiv-2408.04699","DOIUrl":"https://doi.org/arxiv-2408.04699","url":null,"abstract":"NASA's return to the Moon presents unparalleled opportunities to advance\u0000high-impact scientific capabilities. At the cutting edge of these possibilities\u0000are extremely high-resolution interferometric observations at visible and\u0000ultraviolet wavelengths. Such technology can resolve the surfaces of stars,\u0000explore the inner accretion disks of nascent stars and black holes, and\u0000eventually enable us to observe surface features and weather patterns on nearby\u0000exoplanets. We have been awarded Phase 1 support from NASA's Innovative\u0000Advanced Concepts (NIAC) program to explore the feasibility of constructing a\u0000high-resolution, long-baseline UV/optical imaging interferometer on the lunar\u0000surface, in conjunction with the Artemis Program. A 1996 study comparing\u0000interferometers on the Moon versus free-flyers in space concluded that, without\u0000pre-existing lunar infrastructure, free-flyers were preferable. However, with\u0000the advent of the Artemis Program, it is now crucial to revisit the potential\u0000of building lunar interferometers. Our objective is to conduct a study with the\u0000same level of rigor applied to large baseline, free-flying interferometers\u0000during the 2003-2005 NASA Vision Missions Studies. This preparation is\u0000essential for timely and effective utilization of the forthcoming lunar\u0000infrastructure. In this paper, we highlight the groundbreaking potential of a\u0000lunar surface-based interferometer. This concept study will be a huge step\u0000forward to larger arrays on both the moon and free-flying in space, over a wide\u0000variety of wavelengths and science topics. Our Phase 1 study began in April\u00002024, and here we present a concise overview of our vision and the progress\u0000made so far.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947739","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}

{"title":"Bright Star Subtraction Pipeline for LSST: Phase one report","authors":"Amir E. Bazkiaei, Lee S. Kelvin, Sarah Brough, Simon J. O'Toole, Aaron Watkins, Morgan A. Schmitz","doi":"arxiv-2408.04387","DOIUrl":"https://doi.org/arxiv-2408.04387","url":null,"abstract":"We present the phase one report of the Bright Star Subtraction (BSS) pipeline\u0000for the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST).\u0000This pipeline is designed to create an extended PSF model by utilizing observed\u0000stars, followed by subtracting this model from the bright stars present in LSST\u0000data. Running the pipeline on Hyper Suprime-Cam (HSC) data shows a correlation\u0000between the shape of the extended PSF model and the position of the detector\u0000within the camera's focal plane. Specifically, detectors positioned closer to\u0000the focal plane's edge exhibit reduced circular symmetry in the extended PSF\u0000model. To mitigate this effect, we present an algorithm that enables users to\u0000account for the location dependency of the model. Our analysis also indicates\u0000that the choice of normalization annulus is crucial for modeling the extended\u0000PSF. Smaller annuli can exclude stars due to overlap with saturated regions,\u0000while larger annuli may compromise data quality because of lower\u0000signal-to-noise ratios. This makes finding the optimal annulus size a\u0000challenging but essential task for the BSS pipeline. Applying the BSS pipeline\u0000to HSC exposures allows for the subtraction of, on average, 100 to 700 stars\u0000brighter than 12th magnitude measured in g-band across a full exposure, with a\u0000full HSC exposure comprising ~100 detectors.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-08-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141947741","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}