Dr. Robert Ferdman
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Applying Convolutional Neural Networks to Classify Fast Radio Bursts Detected by The CHIME Telescope by Prateek Yadav A THESIS SUBMITTED IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF Master of Science in THE FACULTY OF GRADUATE AND POSTDOCTORAL STUDIES (Physics) The University of British Columbia (Vancouver) April 2020 c Prateek Yadav, 2020 The following individuals certify that they have read, and recommend to the Fac- ulty of Graduate and Postdoctoral Studies for acceptance, the thesis entitled: Applying Convolutional Neural Networks to Classify Fast Radio Bursts Detected by The CHIME Telescope submitted by Prateek Yadav in partial fulfillment of the requirements for the de- gree of Master of Science in Physics. Examining Committee: Dr. Ingrid H. Stairs, Astronomy Supervisor Dr. Gary F. Hinshaw, Astronomy Supervisory Committee Member ii Abstract The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a novel ra- dio telescope that is predicted to detect up to several dozens of Fast Radio Bursts (FRBs) per day. However, CHIME’s FRB detection software pipeline is suscep- tible to a large number of false positive triggers from terrestrial sources of Radio Frequency Interference (RFI). This thesis details the description of intensityML, a software pipeline designed to generate waterfall plots and automatically classify ra- dio bursts detected by CHIME without explicit RFI-masking and DM-refinement. The pipeline uses a convolutional neural network based classifier trained exclu- sively on the events detected by CHIME, and the classifier has an accuracy, preci- sion and recall of over 99%. It has also successfully discovered several FRBs, both in real-time and from archival data. -
Natalia Ewelina Lewandowska
Natalia Ewelina Lewandowska - Curriculum Vitae Haverford College Office Phone: +1 304 940 6801 370 Lancester Avenue, Haverford, PA 19041 Email: [email protected] Research Gate LinkedIn Core Professional Strengths • Correlation searches and simulations of multiwavelength pulsar data • High time resolution polarimetry studies of radio pulsar data • Physics & Astronomy teaching • Undergraduate, graduate mentoring & training • Hands-on learning • Collaboration building & diversity initiatives • Public outreach management Current Position Visiting Assistant Professor of Physics and Astronomy - Haverford College Education 2010/09 - 2015/12 PhD, Physics at the Astronomy Department/University of Wu¨rzburg (A Correlation Study of Radio Giant Pulses and Very High Energy Photons from the Crab pulsar; Advisors: K. Mannheim, D. Els¨asser) 2009/01 - 2010/04 Diploma, Physics at Hamburg Observatory/University of Hamburg (Examination of Flare Stars with the highspeed photo-polarimeter OP- TIMA; Advisors: C. Liefke, J. Schmitt, G. Kanbach) 2007/10 - 2008/10 Student Research Project at Hamburg Observatory/University of Hamburg (The morphological Characteristics of Comet 17/P Holmes; Advisors: C. Liefke, J. Schmitt) 2006/04 - 2008/11 Undergraduate Student at University of Hamburg/Germany (Major: Physics, Minor: Astronomy) 2004/08 - 2006/03 Undergraduate Student at Friedrich Schiller University Jena, Extended Education Thuringia/Germany 2014/04 - 2014/07 Attendance of course “Radio Interferometry: Methods and Science” with hands-on tutorials in AIPS -
Binary and Millisecond Pulsars Are Included in Appendix A
Binary and Millisecond Pulsars Duncan R. Lorimer Department of Physics West Virginia University P.O. Box 6315 Morgantown WV 26506, U.S.A. email: [email protected] http://astro.wvu.edu/people/dunc Abstract We review the main properties, demographics and applications of binary and millisecond radio pulsars. Our knowledge of these exciting objects has greatly increased in recent years, mainly due to successful surveys which have brought the known pulsar population to over 1800. There are now 83 binary and millisecond pulsars associated with the disk of our Galaxy, and a further 140 pulsars in 26 of the Galactic globular clusters. Recent highlights include the discovery of the young relativistic binary system PSR J1906+0746, a rejuvination in globular cluster pulsar research including growing numbers of pulsars with masses in excess of 1.5 M⊙, a precise measurement of relativistic spin precession in the double pulsar system and a Galactic millisecond pulsar in an eccentric (e = 0.44) orbit around an unevolved companion. arXiv:0811.0762v1 [astro-ph] 5 Nov 2008 1 1 Preamble Pulsars – rapidly rotating highly magnetised neutron stars – have many applications in physics and astronomy. Striking examples include the confirmation of the existence of gravitational ra- diation [366, 367, 368], the first extra-solar planetary system [404, 293] and the first detection of gas in a globular cluster [116]. The diverse zoo of radio pulsars currently known is summarized in Figure 1. 1527 solitary pulsars SMC Globular Binary 1 4 Cluster 1 5 8 80 LMC 531 72 14 1 Planets 1 ~20 15 Supernova Recycled Remnant Figure 1: Venn diagram showing the numbers and locations of the various types of radio pulsars known as of September 2008. -
Arxiv:1908.05356V2 [Astro-Ph.IM] 16 Aug 2019 Gravitational Waves, Extreme Astrophysics, and Fundamental Physics with Precision Pulsar Timing, J
Astro2020 Project White Paper The NANOGrav Program for Gravitational Waves and Fundamental Physics The North American Nanohertz Observatory for Gravitational Waves 15 July 2019 Thematic areas: Multi-messenger astronomy and astrophysics; Cosmology and fundamental physics; Formation and evolution of compact objects. Contact author: Scott Ransom (NANOGrav Chair), NRAO, [email protected] Authors: A. Brazier (Cornell), S. Chatterjee (Cornell), T. Cohen (NMT), J. M. Cordes (Cornell), M. E. DeCesar (Lafayette), P. B. Demorest (NRAO), J. S. Hazboun (UW Bothell), M. T. Lam (WVU, RIT), R. S. Lynch (GBO), M. A. McLaughlin (WVU), S. M. Ransom (NRAO), X. Siemens (OSU, UWM), S. R. Taylor (Caltech/JPL, Vanderbilt), and S. J. Vigeland (UWM) for the NANOGrav Collaboration ( 50 institutions, 100+ individuals) ∼ Related NANOGrav Science White Papers arXiv:1908.05356v2 [astro-ph.IM] 16 Aug 2019 Gravitational Waves, Extreme Astrophysics, and Fundamental Physics with Precision Pulsar Timing, J. Cordes et al. · Supermassive Black-hole Demographics & Environments with Pulsar Timing Arrays, S. Taylor et al. · Fundamental Physics with Radio Millisecond Pulsars, E. Fonseca et al. · Physics Beyond the Standard Model with Pulsar Timing Arrays, X. Siemens et al. · Multi-messenger Astrophysics with Pulsar Timing Arrays, L. Kelley et al. · The Virtues of Time and Cadence for Pulsars and Fast Transients, R. Lynch et al. · Twelve Decades: Probing the ISM from kiloparsec to sub-AU scales, D. Stinebring et al. · About the cover image: Characteristic GW strain across the full spectrum. Binary black hole sources are shown in each frequency band, probed by current (PTA and ground-based) and planned (LISA) detectors. The allowed range of the stochastic background is scaled to be compatible with the NANOGrav 2018 upper limit. -
The Advanced GBT (A-GBT)1
Astro2020 APC White Paper Advanced Capabilities for the Green Bank Telescope Type of Activity: Ground Based Project Space Based Project Infrastructure Activity Technology Development Activity State of the Profession Consideration Other Summary: We describe projects to advance the capabilities of the GBT in survey speed, bandwidth, interference mitigation, preservation of legacy data, and community access. These upgrades will impact the study of GW and MM astronomy, fundamental physics, FRBs, cosmology, star formation, astrochemistry, distant galaxies, and searches for technosignatures. Principal Author: Ryan S. Lynch Institution: Green Bank Observatory Email: [email protected] Phone: (304) 456-2357 Co-authors: William P. Armentrout (GBO), Amber Bonsall (GBO), Natalie Butterfield (GBO), David T. Frayer (GBO), Frank Ghigo (GBO), Tapasi Ghosh (GBO), Felix J. Lockman (GBO), Ronald J. Maddalena (GBO), Anthony Minter (GBO), Larry Morgan (GBO), Karen L. O’Neil (GBO), Christopher Salter (GBO), Andrew Seymour (GBO), Joy Skipper (GBO) Endorsers: Esteban D. Araya (Western Illinois University), Hector´ G. Arce (Yale University), Filippo D’Ammando (INAF), Trisha Ashley (Caltech; Vanderbilt University), Tracy Becker (Southwest Research Institute), Robert Benjamin (University of Wisconsin-Whitewater), Sara Cazzoli (Instituto de Astrofisica de Andalucia), Tzu-Ching Chang (JPL), Suchetana Chatterjee (Presidency University), Claudia Cicone (University of Oslo), Mark J. Claussen (NRAO), Jim Cordes (Cornell University), Martin Cordiner (NASA Goddard Space Flight Center), Filippo D’Ammando (INAF-IRA Bologna), Jeremy Darling (University of Colorado), Simon Dicker (University of Pennsylvania), James Di Francesco (National Research Council of Canada), Chuanfei Dong (Princeton University), Olivier Dore´ (JPL/Caltech), Andrew Fox (STScI), Andrew Harris (University of Maryland), Jeffrey S. Hazboun (University of Washington Bothell), Ian M. -
Natalia Ewelina Lewandowska
Natalia Ewelina Lewandowska - Curriculum Vitae Swarthmore College Office Phone: +1 304 940 6801 500 College Ave, Swarthmore, PA 19081 Email: [email protected] Research Gate LinkedIn Core Professional Strengths • Correlation searches and simulations of multiwavelength pulsar data • High time resolution polarimetry studies of radio pulsar data • Physics & Astronomy teaching • Undergraduate, graduate mentoring & training • Hands-on learning • Collaboration building & diversity initiatives • Public outreach management Current Position Visiting Assistant Professor of Physics - Swarthmore College Adjunct Professor of Physics and Astronomy - West Virginia University Education 2010/09 - 2015/12 PhD, Physics at the Astronomy Department/University of W¨urzburg (A Correlation Study of Radio Giant Pulses and Very High Energy Photons from the Crab pulsar; Advisors: K. Mannheim, D. Els¨asser) 2009/01 - 2010/04 Diploma, Physics at Hamburg Observatory/University of Hamburg (Examination of Flare Stars with the highspeed photo-polarimeter OP- TIMA; Advisors: C. Liefke, J. Schmitt, G. Kanbach) 2007/10 - 2008/10 Student Research Project at Hamburg Observatory/University of Hamburg (The morphological Characteristics of Comet 17/P Holmes; Advisors: C. Liefke, J. Schmitt) 2006/04 - 2008/11 Undergraduate Student at University of Hamburg/Germany (Ma- jor: Physics, Minor: Astronomy) 2004/08 - 2006/03 Undergraduate Student at Friedrich Schiller University Jena, Thuringia/Germany Extended Education 2014/04 - 2014/07 Attendance of course \Radio Interferometry: -
Binary and Millisecond Pulsars Are Included in Appendix A
Binary and Millisecond Pulsars Duncan R. Lorimer University of Manchester Jodrell Bank Observatory Macclesfield Cheshire, SK11 9DL, U.K. email: [email protected] http://www.jb.man.ac.uk/~drl Abstract We review the main properties, demographics and applications of binary and millisecond radio pulsars. Our knowledge of these exciting objects has greatly increased in recent years, mainly due to successful surveys which have brought the known pulsar population to over 1700. There are now 80 binary and millisecond pulsars associated with the disk of our Galaxy, and a further 103 pulsars in 24 of the Galactic globular clusters. Recent highlights have been the discovery of the first ever double pulsar system and a recent flurry of discoveries in globular clusters, in particular Terzan 5. arXiv:astro-ph/0511258v1 9 Nov 2005 1 1 Introduction and Overview Pulsars – rapidly rotating highly magnetised neutron stars – have resulted in many applications in physics and astronomy. Striking examples include the confirmation of the existence of gravitational radiation [314] as predicted by general relativity [312, 313], the first detection of an extra-solar planetary system [346, 244] and the discovery of the first double-pulsar binary system [44, 198]. The diverse zoo of radio pulsars currently known is summarized in Figure 1. ~ 1700 Radio Pulsars SMC Globular Binary 1 1 Cluster 1 5 6 76 LMC 181 49 4 1 Planets 1 ~20 15 Supernova ``Recycled'' Remnant Figure 1: Venn diagram showing the numbers and locations of the various types of radio pulsars known as of January 2005. The large and small Magellanic clouds are denoted by LMC and SMC.