Issue O4 June 2020 Insights Into the Max Planck Ska Dish Prototype Ska Partners Contribute to Pandemic Response Askap Unveils
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RF Interference Monitoring for the Onsala Space Observatory Master of Science Thesis (Communication Engineering)
RF Interference Monitoring for the Onsala Space Observatory Master of Science Thesis (Communication Engineering) SYED AMEER AHMED GILLANI Department of Earth and Space Sciences, Onsala Space Observatory, CHALMERS UNIVERSITY OF TECHNOLOGY, Göteborg, Sweden, 2010. RF INTERFERENCE MONITORING FOR ONSALA SPACE OBSERVATORY SYED AMEER AHMED GILLANI Department of Earth and Space Sciences, Onsala Space Observatory CHALMERS UNIVERSITY OF TECHNOLOGY Göteborg, Sweden 2010 ii ABSTRACT With the continuous and rapid developments in wireless services and allocation of radio frequency spectrum to these services, huge interferences have been observed in the field of radio astronomy. According to the international regulations, parts of the spectra are reserved for radio-astronomical observations. Man-made signals entering the receiver chain of a radio telescope have much higher power compared to natural or passive signals received at the radio telescopes. Passive signals received at radio telescopes are normally 60 dB below the receiver noise level. Active signals generated by man-made wireless services pollute the natural emissions by completely masking them due to high signal strength. The cosmic radiation is determined by the fundamental laws of physics, thus the frequencies are fixed and cannot be changed. So interferences created by active services lead to wrong interpretations of the astronomical data. The present thesis deals with RF interference monitoring system for the Onsala Space Observatory. As part of the thesis, a software application has been developed, which communicates with different type of digital receivers (spectrum analyzers) attached with antenna controlling hardware to control omnidirectional and steerable antennas. A steerable antenna is used to find the direction of interference source by moving the antenna in azimuth and elevation direction. -
Report on the Radionet3 Networking Activity
REPORT ON THE RADIONET3 NETWORKING ACTIVITY TITLE: LOFAR SCIENCE WEEK 2014 A JOINT MEETING COMBINING THE “2014 LOFAR COMMUNITY SCIENCE WORKSHOP” AND A SEPARATE, RELATED SYMPOSIUM ON “FIRST SCIENCE WITH LOFAR’S FIRST ALL-SKY SURVEY” DATE: 7 APRIL – 11 APRIL 2014 TIME: ALL DAY LOCATION: AMSTERDAM, THE NETHERLANDS MEETING WEBPAGE http://www.astron.nl/lofarscience2014/ HOST INSTITUTE: ASTRON (NETHERLANDS INSTITUTE FOR RADIO ASTRONOMY) PARTICIPANTS NO: 105 (COMMUNITY WORKSHOP) / 62 (SURVEY WORKSHOP) MAIN LEADER: ASTRON Project supported by the European Commission Contract no.: 283393 REPORT: 1. Agenda of the meeting The final programmes for both of the workshops are reproduced in their entirety in Appendix A. The programs and presentations are also available from the conference website. 2. Scientific Summary The LOFAR Science Week for 2014 was held April 7-11, 2014 in Amsterdam, NL and brought together roughly 120 members of the LOFAR science community. The week began on Monday afternoon with a LOFAR Users Meeting, open to the whole LOFAR community, organized by ASTRON and intended to provide a forum for users to both learn about the status of the array as well as provide feedback. Members of ASTRON gave updates on the current operational status, ongoing developments, and plans for the coming year. Representative users from the community were also invited to share their personal experiences from using the system. Robert Pizzo and the Science Support team were on hand to answer questions and gathered a lot of good feedback that they will use to improve the user experience for LOFAR. The User’s Meeting was followed on Tuesday by a two day LOFAR Community Science Workshop where nearly 120 members of the LOFAR collaboration came together to present their latest science results and share ideas and experiences about doing science with LOFAR. -
Planck 2011 Conference the Millimeter And
PLANCK 2011 CONFERENCE THE MILLIMETER AND SUBMILLIMETER SKY IN THE PLANCK MISSION ERA 10-14 January 2011 Paris, Cité des Sciences Monday, January 10th 2011 13:00 Registration 14:00 Claudie Haigneré (Présidente of Universcience) Welcome Planck mission status, Performances, Cross-calibration Jan Tauber (ESA) - Jean-Loup Puget (IAS Orsay) - Reno Mandolesi (INAF/IASF Bologna) Introduction Session chair: François Pajot 14:20 François Bouchet (Institut d'Astrophysique de Paris) 30+5' HFI data and performance (invited on Planck early paper) 14:55 Marco Bersanelli (University of Milano) 30+5' LFI data and performance (invited on Planck early paper) 15:30 Ranga Chary (IPAC Caltech) 30+5' Planck Early Release Compact Source Catalogue (invited on Planck early paper) 16:05 Coffee break 16:30 Goran Pilbratt (European Space Agency) 20+5' The Herschel observatory (invited) Radio sources 16:55 Bruce Partridge (Haverford College) 25+5' Overview (invited) 17:25 Luigi Tofolatti (Universidad de Oviedo) 20+5' Planck radio sources statistics (invited on Planck early paper) 17:50 Francisco Argueso (Universidad de Oviedo) 15+5' A Bayesian technique to detect point sources in CMB maps 18:10 Anna Scaife (Dublin Institute for Advanced Studies) 15+5' The 10C survey of Radio Sources - First Results 18:30 End of day 1 19:00 Welcome reception at the Conference Center Tuesday, January 11th 2011 Radio sources (continued) Session chair: Bruce Partridge 9:00 Anne Lahteenmaki (Aalto University Metsahovi Radio Observatory) 20+5' Planck observations of extragalactic radio -
Radio Galaxy Zoo: Compact and Extended Radio Source Classification with Deep Learning
MNRAS 476, 246–260 (2018) doi:10.1093/mnras/sty163 Advance Access publication 2018 January 26 Radio Galaxy Zoo: compact and extended radio source classification with deep learning V. Lukic,1‹ M. Bruggen,¨ 1‹ J. K. Banfield,2,3 O. I. Wong,3,4 L. Rudnick,5 R. P. Norris6,7 and B. Simmons8,9 1Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany 2Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia 3ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), Building A28, School of Physics, The University of Sydney, NSW 2006, Australia 4International Centre for Radio Astronomy Research-M468, The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia Downloaded from https://academic.oup.com/mnras/article/476/1/246/4826039 by guest on 23 September 2021 5University of Minnesota, 116 Church St SE, Minneapolis, MN 55455, USA 6Western Sydney University, Locked Bag 1797, Penrith South, NSW 1797, Australia 7CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia 8Oxford Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK 9Center for Astrophysics and Space Sciences, Department of Physics, University of California, San Diego, CA 92093, USA Accepted 2018 January 15. Received 2018 January 9; in original form 2017 September 24 ABSTRACT Machine learning techniques have been increasingly useful in astronomical applications over the last few years, for example in the morphological classification of galaxies. Convolutional neural networks have proven to be highly effective in classifying objects in image data. In the context of radio-interferometric imaging in astronomy, we looked for ways to identify multiple components of individual sources. -
GCSE Astronomy Scheme of Work
Scheme of Work GCSE (9-1) Astronomy Pearson Edexcel Level 1/Level 2 GCSE (9-1) in Astronomy (1AS0) GCSE Astronomy Scheme of Work Topic 1 Planet Earth Week 1 1.1 The Earth’s structure Specification Maths Related practical Exemplar activities Exemplar resources points skills activities 1.1 Starter: Teacher shows images of the Earth showing its Find useful information in chapter 1 2a 1.2 many diverse surface features and asks the class to of GCSE Astronomy – A Guide for 2b 1.3 a-d share what they know about its shape, size and internal Pupils and Teachers (5th ed.) by structure. Marshall, N. (Mickledore). Pupils study the shape and mean diameter of the Earth (13 000 km). Further useful information in chapter Pupils study the Earth’s interior, its main divisions and 3 of The Planets by Aderin-Pocock, their properties (approximate size, state of matter, M. et al (DK). temperature etc.): o crust o mantle o outer core o inner core. © Pearson Education Ltd 2016 1 GCSE Astronomy Scheme of Work Topic 1 Planet Earth Week 2 1.2 Latitude and longitude Specification Maths Related practical Exemplar activities Exemplar resources points skills activities 1.4 Teacher demonstrates latitude and longitude on a globe Find useful information in chapter 1 5a 1.5 a-h of the Earth. of GCSE Astronomy – A Guide for 5d Pupils and Teachers (5th ed.) by Pupils use globes, maps and/or an atlas to study Marshall, N. (Mickledore). latitude and longitude. Model globes and atlases are Pupils learn that in addition to being simply lines on a available from many retail outlets or map, latitude and longitude are actually angles. -
Cutting-Edge Engineering for the World's Largest Radio Telescope
SKAO Cutting-edge engineering for the world’s largest radio telescope Cutting-edge engineering for the world’s largest radio telescope Approaching a technological challenge on the scale of the SKA is formidable... while building on 60 years of radio- astronomy developments, the huge increase in scale from existing facilities demands a revolutionary break from traditional radio telescope design and radical developments in processing, computer speeds and the supporting technological infrastructure. To answer this challenge the SKA has been broken down into various elements that will form the final SKA telescope. Each element is managed by an international consortium comprising world leading experts in their fields. The SKA Office, staffed with engineering domain experts, systems engineers, scientists and managers, centralises the project management and system design. SKAO The design work was awarded through the SKA Office to these Consortia, made up of over 100 of some of the world’s top research institutions and companies, drawn primarily from the SKA Member countries but also beyond. Following the delivery of a detailed design package in 2016, in 2018 nine consortia are having their Critical Design Reviews (CDR) to deliver the final design documentation to prepare a construction proposal for government approval. The other three consortia are part of the SKA’s Advanced Instrumentation Programme, which develops future instrumention for the SKA. The 2018 SKA CalenDaR aims to recognise the immense work conducted by these hundreds of dedicated engineers and project managers from around the world over the past five years. Without their crucial work, the SKA’s ambitious science programme would not be possible. -
All the Things That Back to the Future Got Right (And Wrong)
All the things that Back to the Future got right (and wrong) Posted 7 days ago by i100 staff in ents Upvote Wednesday 21st October 2015 marks the date that Marty McFly and Doc Brown flew through time to visit in the 1989 classic Back to the Future II. While the film, directed by Robert Zemeckis and starring Michael J Fox and Christopher Lloyd, made many fanciful predictions which we're still waiting for, it was surprisingly correct in some aspects. Here's what it got right and what it got wrong about the world we live in, in 2015: Right Fingerprint scanners Fingerprint recognition, like that used to pay for a taxi in the film, can be found on the latest iPhones and at US passport control. Fuelling cars on rubbish While you can't exactly scavenge through a wheelie-bin and force feed it through your car's petrol cap (as Doc does to the DeLorean), using waste as a fuel - in the form of biogas, is something we use in 2015. There's even a bus in Bristol that runs entirely on human and food waste. Hoverboard transportation The kind with wheels may be banned on British streets, but inventors in the US have managed to create a real hoverboard using powerful electromagnets and a metal course. The Hendo II, fronted by renowned skateboarder Tony Hawk will be launched on Wednesday. Hands-free games A young Elijah Wood and his pal denounce Marty for using a video game that needs a handset in the film, suggesting that by 2015 hands-free computer games would be mainstream. -
A Study of Giant Radio Galaxies at Ratan-600 173
Bull. Spec. Astrophys. Obs., 2011, 66, 171–182 c Special Astrophysical Observatory of the Russian AS, 2018 A Study of Giant Radio Galaxies at RATAN-600 M.L. Khabibullinaa, O.V. Verkhodanova, M. Singhb, A. Piryab, S. Nandib, N.V. Verkhodanovaa a Special Astrophysical Observatory of the Russian AS, Nizhnij Arkhyz 369167, Russia; b Aryabhatta Research Institute of Observational Sciences, Manora Park, Nainital 263 129, India Received July 28, 2010; accepted September 15, 2010. We report the results of flux density measurements in the extended components of thirteen giant radio galaxies, made with the RATAN-600 in the centimeter range. Supplementing them with the WENSS, NVSS and GB6 survey data we constructed the spectra of the studied galaxy components. We computed the spectral indices in the studied frequency range and demonstrate the need for a detailed account of the integral contribution of such objects into the background radiation. Key words: Radio lines: galaxies—techniques: radar astronomy 1. INTRODUCTION than the one, expected from the evolutional models. As noted in [8], such radio galaxies may affect the According to the generally accepted definition, gi- processes of galaxy formation, since the pressure of ant radio galaxies (GRGs) are the radio sources with gas, outflowing from the radio source, may compress linear sizes greater than 1 Mpc, i.e. the largest ra- the cold gas clouds thus initiating the development dio sources in the Universe. They mostly belong to of stars on the one hand, and stop the formation of the morphological type FR II [1] and are identified galaxies on the other hand. -
Machine Learning in Large Radio Astronomy Surveys (How to Do Science with Petabytes)
Machine Learning in Large Radio Astronomy Surveys (How to do Science with Petabytes) Ray Norris, Western Sydney University & CSIRO Astronomy & Space Science, ASKAP: Australian Square Kilometre Array Pathfinder ▪ $185m telescope built by CSIRO, approaching completion ▪ Mission: to solve fundamental problems in astrophysics ▪ “EMU” = Evolutionary Map of the Universe PAFs -> Big Data Data Rate to correlator = 100 Tbit/s = 3000 Blu-ray disks/second = 62km tall stack of disks per day = world internet bandwidth in June 2012 Processed data volume = 70 PB/yr (only store 4 PB/yr) EMU: Evolutionary Map of the Universe ▪ PI Ray Norris ▪ Will survey the whole sky for radio continuum ▪ Will discover ~ 70 million galaxies, ▪ compared to 2.5 million currently known ▪ Will revolutionize our view of the Universe ▪ Will revolutionize the way we do astronomy ▪ “large-n astronomy” ASKAP Radio Continuum survey: EMU = 70 million NVSS=1.8 million current total=2.5 million From Norris, 2017, Nature Astronomy, 1,671 1940 1980 2020 EMU Team: ~300 scientists in 21 countries Key Title Project Leader project KP1. EMU Value-Added Catalogue Nick Seymour (Curtin) KP2. Characterising the Radio Sky Ian Heywood (Oxford) KP3. EMU Cosmology David Parkinson (KASA, Korea) KP4. Cosmic Web Shea Brown (Iowa) KP5. Clusters of Galaxies Melanie Johnston-Hollitt (NZ) KP6. cosmic star formation history Andrew Hopkins (AAO) KP7. Evolution of radio-loud AGN Anna Kapinska (UWA) KP8. Radio AGN in the EoR Jose Afonso (Lisbon) KP9. Radio-quiet AGN Isabella Prandoni (Bologna) KP10. Binary super-massive black holes Roger Deane (Cape Town) KP11. Local Universe Josh Marvil (NRAO) KP12. The Galactic Plane Roland Kothes (Canada) KP13. -
Essential Radio Astronomy
February 2, 2016 Time: 09:25am chapter1.tex © Copyright, Princeton University Press. No part of this book may be distributed, posted, or reproduced in any form by digital or mechanical means without prior written permission of the publisher. 1 Introduction 1.1 AN INTRODUCTION TO RADIO ASTRONOMY 1.1.1 What Is Radio Astronomy? Radio astronomy is the study of natural radio emission from celestial sources. The range of radio frequencies or wavelengths is loosely defined by atmospheric opacity and by quantum noise in coherent amplifiers. Together they place the boundary be- tween radio and far-infrared astronomy at frequency ν ∼ 1 THz (1 THz ≡ 1012 Hz) or wavelength λ = c/ν ∼ 0.3 mm, where c ≈ 3 × 1010 cm s−1 is the vacuum speed of light. The Earth’s ionosphere sets a low-frequency limit to ground-based radio astronomy by reflecting extraterrestrial radio waves with frequencies below ν ∼ 10 MHz (λ ∼ 30 m), and the ionized interstellar medium of our own Galaxy absorbs extragalactic radio signals below ν ∼ 2 MHz. The radio band is very broad logarithmically: it spans the five decades between 10 MHz and 1 THz at the low-frequency end of the electromagnetic spectrum. Nearly everything emits radio waves at some level, via a wide variety of emission mechanisms. Few astronomical radio sources are obscured because radio waves can penetrate interstellar dust clouds and Compton-thick layers of neutral gas. Because only optical and radio observations can be made from the ground, pioneering radio astronomers had the first opportunity to explore a “parallel universe” containing unexpected new objects such as radio galaxies, quasars, and pulsars, plus very cold sources such as interstellar molecular clouds and the cosmic microwave background radiation from the big bang itself. -
Event Horizon Telescope Observations of the Jet Launching and Collimation in Centaurus A
https://doi.org/10.1038/s41550-021-01417-w Supplementary information Event Horizon Telescope observations of the jet launching and collimation in Centaurus A In the format provided by the authors and unedited Draft version May 26, 2021 Typeset using LATEX preprint style in AASTeX63 Event Horizon Telescope observations of the jet launching and collimation in Centaurus A: Supplementary Information Michael Janssen ,1, 2 Heino Falcke ,2 Matthias Kadler ,3 Eduardo Ros ,1 Maciek Wielgus ,4, 5 Kazunori Akiyama ,6, 7, 4 Mislav Balokovic´ ,8, 9 Lindy Blackburn ,4, 5 Katherine L. Bouman ,4, 5, 10 Andrew Chael ,11, 12 Chi-kwan Chan ,13, 14 Koushik Chatterjee ,15 Jordy Davelaar ,16, 17, 2 Philip G. Edwards ,18 Christian M. Fromm,4, 5, 19 Jose´ L. Gomez´ ,20 Ciriaco Goddi ,2, 21 Sara Issaoun ,2 Michael D. Johnson ,4, 5 Junhan Kim ,13, 10 Jun Yi Koay ,22 Thomas P. Krichbaum ,1 Jun Liu (刘Ê ) ,1 Elisabetta Liuzzo ,23 Sera Markoff ,15, 24 Alex Markowitz,25 Daniel P. Marrone ,13 Yosuke Mizuno ,26, 19 Cornelia Muller¨ ,1, 2 Chunchong Ni ,27, 28 Dominic W. Pesce ,4, 5 Venkatessh Ramakrishnan ,29 Freek Roelofs ,5, 2 Kazi L. J. Rygl ,23 Ilse van Bemmel ,30 Antxon Alberdi ,20 Walter Alef,1 Juan Carlos Algaba ,31 Richard Anantua ,4, 5, 17 Keiichi Asada,22 Rebecca Azulay ,32, 33, 1 Anne-Kathrin Baczko ,1 David Ball,13 John Barrett ,6 Bradford A. Benson ,34, 35 Dan Bintley,36 Raymond Blundell ,5 Wilfred Boland,37 Geoffrey C. Bower ,38 Hope Boyce ,39, 40 Michael Bremer,41 Christiaan D. -
Probing Galaxy Halos Using Background Polarized Radio Sources
Probing galaxy halos using background polarized radio sources Master’s thesis in Physics and Astronomy ANTON NILSSON Department of Earth and Space Sciences CHALMERS UNIVERSITY OF TECHNOLOGY Gothenburg, Sweden 2016 Probing galaxy halos using background polarized radio sources Anton Nilsson Department of Earth and Space Sciences Radio Astronomy and Astrophysics group Chalmers University of Technology Gothenburg, Sweden 2016 Probing galaxy halos using background polarized radio sources Anton Nilsson © Anton Nilsson, 2016. Supervisor: Cathy Horellou, Department of Earth and Space Sciences Examiner: Cathy Horellou, Department of Earth and Space Sciences Department of Earth and Space Sciences Radio Astronomy and Astrophysics group Chalmers University of Technology SE-412 96 Gothenburg Telephone +46 31 772 1000 Cover: Polarized emission of the radio source J133920+464115 at Faraday depth +20.75 rad m−2 in grayscale. The contours show the total intensity. Typeset in LATEX Printed by Chalmers Reproservice Gothenburg, Sweden 2016 iv Probing galaxy halos using background polarized radio sources Anton Nilsson Department of Earth and Space Sciences Chalmers University of Technology Abstract Linearly polarized radio emission from synchrotron sources undergoes Faraday ro- tation when passing through a magneto-ionized medium. This might be used to search for evidence of ionized halos around galaxies, using polarized radio sources as a probe. In this thesis I analyze the polarization properties of background radio sources from the Taylor et al. (2009) catalog based on observations with the Very Large Array, and correlate these to the angular separation between the radio sources and foreground galaxies. I find a decrease in the amount of polarized radio sources near the galaxies, interpreting this as radio sources being depolarized by galaxy halos.