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
{"title":"开发 BICEP 阵列 220/270 千兆赫接收器","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":null,"url":null,"abstract":"Measurements of B-mode polarization in the CMB sourced from primordial\ngravitational waves would provide information on the energy scale of inflation\nand its potential form. To achieve these goals, one must carefully characterize\nthe Galactic foregrounds, which can be distinguished from the CMB by conducting\nmeasurements at multiple frequencies. BICEP Array is the latest-generation\nmulti-frequency instrument of the BICEP/Keck program, which specifically\ntargets degree-scale primordial B-modes in the CMB. In its final configuration,\nthis telescope will consist of four small-aperture receivers, spanning\nfrequency bands from 30 to 270 GHz. The 220/270 GHz receiver designed to\ncharacterize Galactic dust is currently undergoing commissioning at Stanford\nUniversity and is scheduled to deploy to the South Pole during the 2024--2025\naustral summer. Here, we will provide an overview of this high-frequency\nreceiver and discuss the integration status and test results as it is being\ncommissioned.","PeriodicalId":501163,"journal":{"name":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","volume":"8 1","pages":""},"PeriodicalIF":0.0000,"publicationDate":"2024-09-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":"0","resultStr":"{\"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\":null,\"url\":null,\"abstract\":\"Measurements of B-mode polarization in the CMB sourced from primordial\\ngravitational waves would provide information on the energy scale of inflation\\nand its potential form. To achieve these goals, one must carefully characterize\\nthe Galactic foregrounds, which can be distinguished from the CMB by conducting\\nmeasurements at multiple frequencies. BICEP Array is the latest-generation\\nmulti-frequency instrument of the BICEP/Keck program, which specifically\\ntargets degree-scale primordial B-modes in the CMB. In its final configuration,\\nthis telescope will consist of four small-aperture receivers, spanning\\nfrequency bands from 30 to 270 GHz. The 220/270 GHz receiver designed to\\ncharacterize Galactic dust is currently undergoing commissioning at Stanford\\nUniversity and is scheduled to deploy to the South Pole during the 2024--2025\\naustral summer. Here, we will provide an overview of this high-frequency\\nreceiver and discuss the integration status and test results as it is being\\ncommissioned.\",\"PeriodicalId\":501163,\"journal\":{\"name\":\"arXiv - PHYS - Instrumentation and Methods for Astrophysics\",\"volume\":\"8 1\",\"pages\":\"\"},\"PeriodicalIF\":0.0000,\"publicationDate\":\"2024-09-03\",\"publicationTypes\":\"Journal Article\",\"fieldsOfStudy\":null,\"isOpenAccess\":false,\"openAccessPdf\":\"\",\"citationCount\":\"0\",\"resultStr\":null,\"platform\":\"Semanticscholar\",\"paperid\":null,\"PeriodicalName\":\"arXiv - PHYS - Instrumentation and Methods for Astrophysics\",\"FirstCategoryId\":\"1085\",\"ListUrlMain\":\"https://doi.org/arxiv-2409.02296\",\"RegionNum\":0,\"RegionCategory\":null,\"ArticlePicture\":[],\"TitleCN\":null,\"AbstractTextCN\":null,\"PMCID\":null,\"EPubDate\":\"\",\"PubModel\":\"\",\"JCR\":\"\",\"JCRName\":\"\",\"Score\":null,\"Total\":0}","platform":"Semanticscholar","paperid":null,"PeriodicalName":"arXiv - PHYS - Instrumentation and Methods for Astrophysics","FirstCategoryId":"1085","ListUrlMain":"https://doi.org/arxiv-2409.02296","RegionNum":0,"RegionCategory":null,"ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":null,"EPubDate":"","PubModel":"","JCR":"","JCRName":"","Score":null,"Total":0}
Development of the 220/270 GHz Receiver of BICEP Array
Measurements of B-mode polarization in the CMB sourced from primordial
gravitational waves would provide information on the energy scale of inflation
and its potential form. To achieve these goals, one must carefully characterize
the Galactic foregrounds, which can be distinguished from the CMB by conducting
measurements at multiple frequencies. BICEP Array is the latest-generation
multi-frequency instrument of the BICEP/Keck program, which specifically
targets degree-scale primordial B-modes in the CMB. In its final configuration,
this telescope will consist of four small-aperture receivers, spanning
frequency bands from 30 to 270 GHz. The 220/270 GHz receiver designed to
characterize Galactic dust is currently undergoing commissioning at Stanford
University and is scheduled to deploy to the South Pole during the 2024--2025
austral summer. Here, we will provide an overview of this high-frequency
receiver and discuss the integration status and test results as it is being
commissioned.
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