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9 results on '"Chaoyun Bao"'

1. Intensity-Coupled-Polarization in Instruments with a Continuously Rotating Half-Wave Plate

Author

Chaoyun Bao, Kate Raach, Ilan Sagiv, François Aubin, Shaul Hanany, Christopher Geach, Adrian T. Lee, Kevin MacDermid, Johannes Hubmayr, Britt Reichborn-Kjennerud, Daniel Chapman, Asad M. Aboobaker, Jeff Klein, Enzo Pascale, Bradley R. Johnson, Derek Araujo, Andrei Korotkov, Michele Limon, William F. Grainger, Michael Milligan, Gregory S. Tucker, Benjamin Westbrook, Carole Tucker, Amber Miller, Kyle Helson, Andrew H. Jaffe, Terry Jay Jones, Peter A. R. Ade, Carlo Baccigalupi, Kyle Zilic, Seth Hillbrand, Joy Didier, Matt Dobbs, and Karl Young

Subjects
Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Waveplate, Optics, Settore FIS/05 - Astronomia e Astrofisica, The E and B Experiment, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, polarization, business.industry, Detector, instrumentation: polarimeters, Astronomy and Astrophysics, Polarization (waves), methods: data analysis, Nonlinear system, techniques: polarimetric, Space and Planetary Science, balloons, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We discuss a systematic effect associated with measuring polarization with a continuously rotating half-wave plate. The effect was identified with the data from the E and B Experiment (EBEX), which was a balloon-borne instrument designed to measure the polarization of the CMB as well as that from Galactic dust. The data show polarization fraction larger than 10\% while less than 3\% were expected from instrumental polarization. We give evidence that the excess polarization is due to detector non-linearity in the presence of a continuously rotating HWP. The non-linearity couples intensity signals into polarization. We develop a map-based method to remove the excess polarization. Applying this method for the 150 (250) GHz bands data we find that 81\% (92\%) of the excess polarization was removed. Characterization and mitigation of this effect is important for future experiments aiming to measure the CMB B-modes with a continuously rotating HWP., 43 pages, 12 figures, submitted to the Astrophysical Journal

Published
2017

2. The EBEX Balloon Borne Experiment - Optics, Receiver, and Polarimetry

Author

Kate Raach, Michael Milligan, A. M. Aboobaker, Adrian T. Lee, Daniel Chapman, Christopher Geach, Joy Didier, Tomotake Matsumura, Michele Limon, Johannes Hubmayr, Terry J. Jones, Lorne Levinson, Kevin MacDermid, Ilan Sagiv, Giorgio Savini, William F. Grainger, François Aubin, Andrei Korotkov, Derek Araujo, Jacob Klein, Karl Young, Kyle Zilic, Peter A. R. Ade, Seth Hillbrand, Carlo Baccigalupi, Carole Tucker, Matt Dobbs, Chaoyun Bao, Benjamin Westbrook, Gregory S. Tucker, Amber Miller, Andrew H. Jaffe, Shaul Hanany, Britt Reichborn-Kjennerud, Bradley R. Johnson, Kyle Helson, and Locke D. Spencer

Subjects
Polarimetry, FOS: Physical sciences, cosmic background radiation, 01 natural sciences, law.invention, Optics, Settore FIS/05 - Astronomia e Astrofisica, law, The E and B Experiment, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, polarization, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, instrumentation: polarimeters, Astronomy and Astrophysics, Polarimeter, Lens (optics), Cardinal point, balloons, cosmology: observations, Space and Planetary Science, Achromatic lens, Transition edge sensor, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

The E and B Experiment (EBEX) was a long-duration balloon-borne cosmic microwave background polarimeter that flew over Antarctica in 2013. We describe the experiment's optical system, receiver, and polarimetric approach, and report on their in-flight performance. EBEX had three frequency bands centered on 150, 250, and 410 GHz. To make efficient use of limited mass and space we designed a 115 cm$^{2}$sr high throughput optical system that had two ambient temperature mirrors and four anti-reflection coated polyethylene lenses per focal plane. All frequency bands shared the same optical train. Polarimetry was achieved with a continuously rotating achromatic half-wave plate (AHWP) that was levitated with a superconducting magnetic bearing (SMB). Rotation stability was 0.45 % over a period of 10 hours, and angular position accuracy was 0.01 degrees. This is the first use of a SMB in astrophysics. The measured modulation efficiency was above 90 % for all bands. To our knowledge the 109 % fractional bandwidth of the AHWP was the broadest implemented to date. The receiver that contained one lens and the AHWP at a temperature of 4 K, the polarizing grid and other lenses at 1 K, and the two focal planes at 0.25 K performed according to specifications giving focal plane temperature stability with fluctuation power spectrum that had $1/f$ knee at 2 mHz. EBEX was the first balloon-borne instrument to implement technologies characteristic of modern CMB polarimeters including high throughput optical systems, and large arrays of transition edge sensor bolometric detectors with mutiplexed readouts., Comment: 49 pages, 32 figures, submitted to The Astrophysical Journal Supplement

Published
2017
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3. Maximum Likelihood Foreground Cleaning for Cosmic Microwave Background Polarimeters in the Presence of Systematic Effects

Author

B. Gold, Shaul Hanany, Radek Stompor, Carlo Baccigalupi, Andrew H. Jaffe, Chaoyun Bao, School of Physics and Astronomy [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Hamline University, Imperial College London, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Frequency band, 0306 Physical Chemistry (Incl. Structural), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Astronomy & Astrophysics, 01 natural sciences, 0305 Organic Chemistry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, The E and B Experiment, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Physics, Spectral index, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, instrumentation: polarimeters, Astronomy and Astrophysics, Polarization (waves), methods: data analysis, Computational physics, 0201 Astronomical And Space Sciences, Space and Planetary Science, Measurement uncertainty, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We extend a general maximum likelihood foreground estimation for cosmic microwave background polarization data to include estimation of instrumental systematic effects. We focus on two particular effects: frequency band measurement uncertainty, and instrumentally induced frequency dependent polarization rotation. We assess the bias induced on the estimation of the $B$-mode polarization signal by these two systematic effects in the presence of instrumental noise and uncertainties in the polarization and spectral index of Galactic dust. Degeneracies between uncertainties in the band and polarization angle calibration measurements and in the dust spectral index and polarization increase the uncertainty in the extracted CMB $B$-mode power, and may give rise to a biased estimate. We provide a quantitative assessment of the potential bias and increased uncertainty in an example experimental configuration. For example, we find that with 10\% polarized dust, tensor to scalar ratio of $r=0.05$, and the instrumental configuration of the EBEX balloon payload, the estimated CMB $B$-mode power spectrum is recovered without bias when the frequency band measurement has 5% uncertainty or less, and the polarization angle calibration has an uncertainty of up to 4$^{\circ}$., Comment: Accepted for publication in The Astrophysical Journal

Published
2016
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4. The performance of the bolometer array and readout system during the 2012/2013 flight of the E and B experiment (EBEX)

Author

Julien Grain, Ted Kisner, Matt Dobbs, Kent D. Irwin, Gene C. Hilton, Adrian T. Lee, Bradley R. Johnson, Ilan Sagiv, Michael Milligan, Joy Didier, Matthieu Tristram, François Aubin, Kyle Zilic, L. J. Levinson, Seth Hillbrand, Radek Stompor, Peter A. R. Ade, Daniel Chapman, Jeff Klein, Kate Raach, Asad M. Aboobaker, Carl D. Reintsema, Enzo Pascale, Amber Miller, Terry Jay Jones, Ben Westbrook, Andrei Korotkov, Hannes Hubmayr, Kevin MacDermid, Kevin Bandura, Carlo Baccigalupi, Britt Reichborn-Kjennerud, Shaul Hanany, Graeme Smecher, Gregory S. Tucker, Julian Borrill, Chaoyun Bao, Kyle Helson, Andrew H. Jaffe, Michele Limon, and William F. Grainger

Subjects
Physics::Instrumentation and Detectors, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, SQUID, law.invention, Telescope, Optics, bolometer, The E and B Experiment, law, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, multiplexing, business.industry, balloon-borne, TES, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Amplifier, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Polarization (waves), Transition edge sensor, business, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

EBEX is a balloon-borne telescope designed to measure the polarization of the cosmic microwave background radiation. During its eleven day science flight in the Austral Summer of 2012, it operated 955 spider-web transition edge sensor (TES) bolometers separated into bands at 150, 250 and 410 GHz. This is the first time that an array of TES bolometers has been used on a balloon platform to conduct science observations. Polarization sensitivity was provided by a wire grid and continuously rotating half-wave plate. The balloon implementation of the bolometer array and readout electronics presented unique development requirements. Here we present an outline of the readout system, the remote tuning of the bolometers and Superconducting QUantum Interference Device (SQUID) amplifiers, and preliminary current noise of the bolometer array and readout system., Comment: 15 pages, 12 figures, SPIE conference proceedings

Published
2014
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5. The Impact of the Spectral Response of an Achromatic Half-Wave Plate on the Measurement of the Cosmic Microwave Background Polarization

Author

Andrew H. Jaffe, Bradley R. Johnson, Joy Didier, D. O'Dea, Carlo Baccigalupi, S. Leach, B. Gold, Tomotake Matsumura, Amber Miller, Chaoyun Bao, and Shaul Hanany

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, cosmic background radiation, Astrophysics::Cosmology and Extragalactic Astrophysics, Waveplate, law.invention, Optics, Settore FIS/05 - Astronomia e Astrofisica, law, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, Spectral index, business.industry, Gravitational wave, Linear polarization, Astrophysics::Instrumentation and Methods for Astrophysics, instrumentation: polarimeters, Astronomy and Astrophysics, Polarization (waves), methods: data analysis, techniques: polarimetric, Space and Planetary Science, Achromatic lens, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the impact of the spectral dependence of the linear polarization rotation induced by an achromatic half-wave plate on measurements of cosmic microwave background polarization in the presence of astrophysical foregrounds. We focus on the systematic effects induced on the measurement of inflationary gravitational waves by uncertainties in the polarization and spectral index of Galactic dust. We find that for the experimental configuration and noise levels of the balloon-borne EBEX experiment, which has three frequency bands centered at 150, 250, and 410 GHz, a crude dust subtraction process mitigates systematic effects to below detectable levels for 10% polarized dust and tensor to scalar ratio of as low as r = 0.01. We also study the impact of uncertainties in the spectral response of the instrument. With a top-hat model of the spectral response for each band, characterized by band-center and band-width, and with the same crude dust subtraction process, we find that these parameters need to be determined to within 1 and 0.8 GHz at 150 GHz; 9 and 2.0 GHz at 250 GHz; and 20 and 14 GHz at 410 GHz, respectively. The approach presented in this paper is applicable to other optical elements that exhibit polarization rotation as a function of frequency., 6 pages, 7 figures, accepted for publication by Astrophysical Journal

Published
2011

6. EBEX: A balloon-borne CMB polarization experiment

Author

S. Leach, F. Stivoli, Graeme Smecher, Huan Tran, Theodore Kisner, Enzo Pascale, Amber Miller, Shaul Hanany, Andrei Korotkov, Radek Stompor, X. Meng, Johannes Hubmayr, Carlo Baccigalupi, Julian Borrill, Daniel Chapman, Asad M. Aboobaker, Michael Milligan, Matthieu Tristram, Kyle Zilic, Michele Limon, Seth Hillbrand, Kevin MacDermid, Britt Reichborn-Kjennerud, Bradley R. Johnson, Peter A. R. Ade, Terry J. Jones, William F. Grainger, Christopher Cantalupo, Adrian T. Lee, Ilan Sagiv, Amit P. S. Yadav, Kate Raach, François Aubin, Matias Zaldarriaga, Matt Dobbs, Jacob Klein, Nicolas Ponthieu, L. J. Levinson, Yury Vinokurov, Chaoyun Bao, Julien Grain, Tomotake Matsumura, Joy Didier, Andrew H. Jaffe, Gregory S. Tucker, Daniel Polsgrove, Columbia University [New York], University of Minnesota [Twin Cities] (UMN), University of Minnesota System, Cardiff University, McGill University = Université McGill [Montréal, Canada], Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National Institute of Standards and Technology [Gaithersburg] (NIST), Imperial College London, Brown University, Weizmann Institute of Science [Rehovot, Israël], California Institute of Technology (CALTECH), Global parallel and distributed computing (GRAND-LARGE), Centre National de la Recherche Scientifique (CNRS)-Inria Saclay - Ile de France, Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université Paris-Sud - Paris 11 (UP11)-Laboratoire d'Informatique Fondamentale de Lille (LIFL), Université de Lille, Sciences et Technologies-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Lille, Sciences Humaines et Sociales-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Sciences et Technologies-Université de Lille, Sciences Humaines et Sociales-Centre National de la Recherche Scientifique (CNRS)-Laboratoire de Recherche en Informatique (LRI), Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-CentraleSupélec, APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institute for Advanced Study [Princeton] (IAS), Holland, Wayne S., Zmuidzinas, Jonas, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Recherche en Informatique (LRI), Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Informatique Fondamentale de Lille (LIFL), Université de Lille, Sciences et Technologies-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Lille, Sciences Humaines et Sociales-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Sciences et Technologies-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Lille, Sciences Humaines et Sociales-Centre National de la Recherche Scientifique (CNRS)-Inria Saclay - Ile de France, Institut National de Recherche en Informatique et en Automatique (Inria), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Minnesota [Twin Cities], McGill University, Weizmann Institute of Science, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Waveplate, Radio spectrum, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, 0103 physical sciences, 010303 astronomy & astrophysics, media_common, Physics, 010308 nuclear & particles physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Polarization (waves), Sky, Transition edge sensor, business, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

EBEX is a NASA-funded balloon-borne experiment designed to measure the polarization of the cosmic microwave background (CMB). Observations will be made using 1432 transition edge sensor (TES) bolometric detectors read out with frequency multiplexed SQuIDs. EBEX will observe in three frequency bands centered at 150, 250, and 410 GHz, with 768, 384, and 280 detectors in each band, respectively. This broad frequency coverage is designed to provide valuable information about polarized foreground signals from dust. The polarized sky signals will be modulated with an achromatic half wave plate (AHWP) rotating on a superconducting magnetic bearing (SMB) and analyzed with a fixed wire grid polarizer. EBEX will observe a patch covering ~1% of the sky with 8' resolution, allowing for observation of the angular power spectrum from \ell = 20 to 1000. This will allow EBEX to search for both the primordial B-mode signal predicted by inflation and the anticipated lensing B-mode signal. Calculations to predict EBEX constraints on r using expected noise levels show that, for a likelihood centered around zero and with negligible foregrounds, 99% of the area falls below r = 0.035. This value increases by a factor of 1.6 after a process of foreground subtraction. This estimate does not include systematic uncertainties. An engineering flight was launched in June, 2009, from Ft. Sumner, NM, and the long duration science flight in Antarctica is planned for 2011. These proceedings describe the EBEX instrument and the North American engineering flight., 12 pages, 9 figures, Conference proceedings for SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V (2010)

Published
2010
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7. Software systems for operation, control, and monitoring of the EBEX instrument

Author

Michael Milligan, Peter Ade, François Aubin, Carlo Baccigalupi, Chaoyun Bao, Julian Borrill, Christopher Cantalupo, Daniel Chapman, Joy Didier, Matt Dobbs, Will Grainger, Shaul Hanany, Seth Hillbrand, Johannes Hubmayr, Peter Hyland, Andrew Jaffe, Bradley Johnson, Theodore Kisner, Jeff Klein, Andrei Korotkov, Sam Leach, Adrian Lee, Lorne Levinson, Michele Limon, Kevin MacDermid, Tomotake Matsumura, Amber Miller, Enzo Pascale, Daniel Polsgrove, Nicolas Ponthieu, Kate Raach, Britt Reichborn-Kjennerud, Ilan Sagiv, Huan Tran, Gregory S. Tucker, Yury Vinokurov, Amit Yadav, Matias Zaldarriaga, Kyle Zilic, Radziwill, Nicole M., and Bridger, Alan

Subjects
Schedule, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, business.industry, Payload, Computer science, Real-time computing, Housekeeping (computing), FOS: Physical sciences, 01 natural sciences, Front and back ends, Software, 0103 physical sciences, Disk storage, Software system, Ground segment, Astrophysics - Instrumentation and Methods for Astrophysics, business, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the hardware and software systems implementing autonomous operation, distributed real-time monitoring, and control for the EBEX instrument. EBEX is a NASA-funded balloon-borne microwave polarimeter designed for a 14 day Antarctic flight that circumnavigates the pole. To meet its science goals the EBEX instrument autonomously executes several tasks in parallel: it collects attitude data and maintains pointing control in order to adhere to an observing schedule; tunes and operates up to 1920 TES bolometers and 120 SQUID amplifiers controlled by as many as 30 embedded computers; coordinates and dispatches jobs across an onboard computer network to manage this detector readout system; logs over 3~GiB/hour of science and housekeeping data to an onboard disk storage array; responds to a variety of commands and exogenous events; and downlinks multiple heterogeneous data streams representing a selected subset of the total logged data. Most of the systems implementing these functions have been tested during a recent engineering flight of the payload, and have proven to meet the target requirements. The EBEX ground segment couples uplink and downlink hardware to a client-server software stack, enabling real-time monitoring and command responsibility to be distributed across the public internet or other standard computer networks. Using the emerging dirfile standard as a uniform intermediate data format, a variety of front end programs provide access to different components and views of the downlinked data products. This distributed architecture was demonstrated operating across multiple widely dispersed sites prior to and during the EBEX engineering flight., Comment: 11 pages, to appear in Proceedings of SPIE Astronomical Telescopes and Instrumentation 2010; adjusted metadata for arXiv submission

Published
2010

8. The EBEX Cryostat and Supporting Electronics

Author

ILAN SAGIV, ASAD M. ABOOBAKER, CHAOYUN BAO, SHAUL HANANY, TERRY JONES, JEFFREY KLEIN, MICHAEL MILLIGAN, DANIEL E. POLSGROVE, KATE RAACH, KYLE ZILIC, ANDREI KOROTKOV, GREGORY S. TUCKER, YURY VINOKUROV, TOMOTAKE MATSUMURA, PETER ADE, WILL GRAINGER, ENZO PASCALE, DANIEL CHAPMAN, JOY DIDIER, SETH HILLBRAND, BRITT REICHBORN-KJENNERUD, MICHELE LIMON, AMBER MILLER, ANDREW JAFFE, AMIT YADAV, MATIAS ZALDARRIAGA, NICOLAS PONTHIEU, MATTHIEU TRISTRAM, JULIAN BORRILL, CHRISTOPHER CANTALUPO, TED KISNER, FRANÇOIS AUBIN, MATT DOBBS, KEVIN MACDERMID, GENE HILTON, JOHANNES HUBMAYR, KENT IRWIN, CARL REINTSEMA, CARLO BACCIGALUPI, SAM LEACH, BRADLEY JOHNSON, ADRIAN LEE, HUAN TRAN, and LORNE LEVINSON

Subjects
Cryostat, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), business.industry, Computer file, Cosmic microwave background, Electrical engineering, FOS: Physical sciences, Astrophysics, Electronics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the cryostat and supporting electronics for the EBEX experiment. EBEX is a balloon-borne polarimeter designed to measure the B-mode polarization of the cosmic microwave background radiation. The instrument includes a 1.5 meter Gregorian-type telescope and 1432 bolometric transition edge sensor detectors operating at 0.3 K. Electronics for monitoring temperatures and controlling cryostat refrigerators is read out over CANbus. A timing system ensures the data from all subsystems is accurately synchronized. EBEX completed an engineering test flight in June 2009 during which the cryogenics and supporting electronics performed according to predictions. The temperatures of the cryostat were stable, and an analysis of a subset of the data finds no scan synchronous signal in the cryostat temperatures. Preparations are underway for an Antarctic flight., Comment: 11 pages, 6 figures, Proceedings of the 12th Marcel Grossman Conference

Published
2010
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9. Temperature calibration of the E and B experiment

Author

Stephen M. Feeney, Jacob Klein, Michele Limon, Gene C. Hilton, Bradley R. Johnson, Terry J. Jones, Carl D. Reintsema, Valerie Marchenko, Karl Young, Britt Reichborn-Kjennerud, Andrei Korotkov, Chaoyun Bao, Amber Miller, Giuseppe Puglisi, Christopher Geach, Radek Stompor, Ilan Sagiv, François Aubin, Andrew H. Jaffe, Joy Didier, Shaul Hanany, Gregory S. Tucker, Kyle Helson, Peter A. R. Ade, Julian Borrill, Graeme Smecher, Matt Dobbs, Theodore Kisner, Adrian T. Lee, Johannes Hubmayr, Kate Raach, Kyle Zilic, Seth Hillbrand, Lorne Levinson, Michael Milligan, Matthieu Tristram, Enzo Pascale, Ben Westbrook, Daniel Chapman, Asad M. Aboobaker, Kevin MacDermid, Derek Araujo, Carlo Baccigalupi, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de l'Accélérateur Linéaire ( LAL ), and Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Radio spectrum, law.invention, Optics, The E and B Experiment, law, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Temperature calibration, Physics, Settore FIS/05, business.industry, Detector, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimeter, Polarization (waves), Achromatic lens, business, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The E and B Experiment (EBEX) is a balloon-borne polarimeter designed to measure the polarization of the cosmic microwave background radiation and to characterize the polarization of galactic dust. EBEX was launched December 29, 2012 and circumnavigated Antarctica observing $\sim$6,000 square degrees of sky during 11 days at three frequency bands centered around 150, 250 and 410 GHz. EBEX was the first experiment to operate a kilo-pixel array of transition-edge sensor bolometers and a continuously rotating achromatic half-wave plate aboard a balloon platform. It also pioneered the use of detector readout based on digital frequency domain multiplexing. We describe the temperature calibration of the experiment. The gain response of the experiment is calibrated using a two-step iterative process. We use signals measured on passes across the Galactic plane to convert from readout-system counts to power. The effective smoothing scale of the EBEX optics and the star camera-to-detector offset angles are determined through \c{hi}2 minimization using the compact HII region RCW 38. This two-step process is initially performed with parameters measured before the EBEX 2013 flight and then repeated until the calibration factor and parameters converge., 6 pages, 3 figures, Proceedings of the 14th Marcel Grossman Conference

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