BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:The Effelsberg Direct Digitizaion Project DTSTART;VALUE=DATE-TIME:20200921T131000Z DTEND;VALUE=DATE-TIME:20200921T133500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-24@cern.ch DESCRIPTION:Speakers: Dr. WINCHEN\, Tobias (Max Planck Institute for Radio Astronomy)\nRecent developments in high-speed networking and PCIe-mounted accelerator\ncards have made possible new backend designs that provide va stly improved\nflexibility and capability in signal processing for radio a stronomy.\nWhile direct digitization close to the receiver improves the qu ality of the\nphysical signal by reducing analog transmission and filterin g losses\, it also\nenables the building of a backend based on commercial- off-the-shelf (COTS)\nhardware that is able to exploit modern cloud comput ing paradigms. In the\nEffelsberg Direct Digitization (EDD) project we are developing a versatile\nbackend that takes advantage of these benefits. The EDD backend orchestrates\ndata processing on COTS computing systems ho sting GPUs as well as FPGA that can\nbe rapidly and easily adapted to a wi de range of observing use cases\, e.g.\nspectroscopy\, polarimetry\, pulsa r timing\, etc. The highly modular system uses\na unified interface for t he control of its subsystems. This interface abstracts\nthe telescope into well defined components which allows for a universal design\nsuitable for deployment at any radio observatory only minimal customisation.\n\nhttps: //events.mpifr-bonn.mpg.de/indico/event/154/session/4/contribution/24 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/4/contributi on/24 END:VEVENT BEGIN:VEVENT SUMMARY:Science applications of multiband receivers and frequency-phase tr ansfer DTSTART;VALUE=DATE-TIME:20200922T122500Z DTEND;VALUE=DATE-TIME:20200922T125000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-25@cern.ch DESCRIPTION:Speakers: LOBANOV\, Andrei ()\nThe technological developments pioneered at the Korean VLBI Network\nfor designing and implementing simul taneous multfiband (SMB) receivers\npaved the way to extending phase calib ration and phase referencing\ntechniques to the frequency space. Numerous advantages of this\nextension have been convincingly demonstrated at the K VN\, and the time\nis now right to explore them on a larger scale. This wo uld enable\nreaching an astrometric accuracy of ~10 microarcseconds\, perf orming\nrelative astrometric measurements at multiple frequencies\, and\ni ncreasing the dynamic range of mm-VLBI observations by factors of\n20-50. A possible extension of the frequency-phase transfer (FPT) to\n230 GHz is likely to bring a critically needed improvement of the\nquality of EHT ima ging. Scientific potentials of implementing the SMB\nfor mm- and sumnn-VLB I on a global scale will be discussed in this\npresentation.\n\nhttps://ev ents.mpifr-bonn.mpg.de/indico/event/154/session/8/contribution/25 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/8/contributi on/25 END:VEVENT BEGIN:VEVENT SUMMARY:LOFAR2.0: extending LOFAR observational capabilities for the comin g decade DTSTART;VALUE=DATE-TIME:20200921T115000Z DTEND;VALUE=DATE-TIME:20200921T121500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-26@cern.ch DESCRIPTION:Speakers: Dr. BOONSTRA\, Albert-Jan (ASTRON)\nASTRON operates the pan-European Low -Frequency Array (LOFAR)\, a unique \ninstrument that will complement phase one of the Square Kilometre Array \n(SKA)\, planned for construction in the coming three to five years. After \nnearly a deca de of scientific operations\, LOFAR science output is still \nramping up. However\, to keep the telescope at the forefront of science\, \na staged u pgrade programme LOFAR2.0 was set in motion. This programme \nincludes upg rading LOFAR phased-array stations by increasing the number \nof connected antennas\, and by jointly observing the low-band and \nhigh-band frequenc ies. This will greatly increase the sensitivity\, \nespecially at the lowe st frequencies where ionospheric effects are most \nsevere. Simultaneous o bservations with both bands will allow to \ncalibrate out these effects at the low band by using the ionospheric \ncalibration solutions at the high band. The presentation will describe \nthe new station architecture\, sho w the first laboratory tests\, and will \nalso highlight the new design me thodology.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/0/ contribution/26 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/0/contributi on/26 END:VEVENT BEGIN:VEVENT SUMMARY:Smart Ambient-Temperature Very Low Noise LNAs for Radio Astronomy Arrays DTSTART;VALUE=DATE-TIME:20200921T142500Z DTEND;VALUE=DATE-TIME:20200921T145000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-27@cern.ch DESCRIPTION:Speakers: Dr. WEINREB\, Sander (Caltech)\nMost radio telescope s can have greatly expended survey speed and imaging capability by utilizi ng multiple receivers either as feed clusters\, phased-array feeds\, or a larger number of individual antennas. The number of receivers is often l imited by the cost of the cryogenic cooling required for sensitivity at f requencies > 1 GHz. This paper will describe a new class of LNAs for the low microwave range that operate at ambient temperature and are “smart ” in that they include functions such as noise calibration\, tuning\, s witching\, and monitoring within the LNA package. In addition\, the LNAs are powered and controlled by just one wire\, the output coaxial cable. A first generation of this new class of LNAs has been developed for detec tion and location of fast radio bursts (FRBs) in a 110 x 5m array at the Caltech Radio Observatory in Owens Valley\, CA. These DSA110 LNAs have n oise temperature in the 7 to 9 K range to realize system noise temperature s in the 22 to 25 K range in the frequency band of 1.28 to 1.53 GHz. Ove r 40 of the LNAs have now been completed and have internal\, temperature-c ompensated\, noise calibration signals so they can be directly attached to the dual -linear polarized feed without the directional coupler usually required for calibration. Further development of this LNA for a proposed DSA2000 array is in process and will include internal cooling to -40C of the InP HEMT input transistor utilizing a Peltier micro-cooler. This coo ling is motivated by the large decrease in noise temperature with physical temperature measured for the DSA110 LNAs\; the noise decreases by approx imately a factor of two upon cooling from +40C to -40C\, a much greater fa ctor than the change in absolute temperature\, 313K to 233K. This change is believed to be due to a large decrease in the transistor hot-electron n oise\, an effect not noted in previous studies and a subject of a theoreti cal study at Caltech.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154 /session/4/contribution/27 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/4/contributi on/27 END:VEVENT BEGIN:VEVENT SUMMARY:Director's welcome address DTSTART;VALUE=DATE-TIME:20200921T104000Z DTEND;VALUE=DATE-TIME:20200921T110000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-20@cern.ch DESCRIPTION:Speakers: Prof. ZENSUS\, Anton (MPIfR\, RadioNet Coordinator)\ nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/6/contribution/ 20 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/6/contributi on/20 END:VEVENT BEGIN:VEVENT SUMMARY:Open discussion\, workshop summary\, and closure DTSTART;VALUE=DATE-TIME:20200922T144500Z DTEND;VALUE=DATE-TIME:20200922T151500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-21@cern.ch DESCRIPTION:Speakers: Dr. KELLER\, Reinhard (MPIfR)\nhttps://events.mpifr- bonn.mpg.de/indico/event/154/session/10/contribution/21 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/10/contribut ion/21 END:VEVENT BEGIN:VEVENT SUMMARY:Simulations of the Optical System of the LSPE‐STRIP Instrument DTSTART;VALUE=DATE-TIME:20200922T092000Z DTEND;VALUE=DATE-TIME:20200922T094500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-22@cern.ch DESCRIPTION:Speakers: Ms. REALINI\, Sabrina (Università degli Studi di Mi lano)\nWe present the analysis of the optical system of the STRIP instrume nt\, the ground-based telescope of the Large Scale Polarization (LSPE) exp eriment\, which aims at polarization measurements of the Cosmic Microwave Background on large angular scales.\nSTRIP will observe the polarized emis sion from the "Observatorio del Teide" in Tenerife\, starting in late 2021 . The instrument consists of an array of forty-nine coherent polarimeters at 43 GHz (Q-band)\, coupled to a 1.5 m fully rotating crossed-Dragone tel escope. An additional frequency channel with six-elements at 95 GHz (W-ban d) will be exploited as an atmospheric monitor. \nWe modelled and characte rized the STRIP optics by means of electromagnetic simulations. The model includes the two nominal reflectors\, forty-nine Q-band feedhorns\, six W- band feedhorns\, and the shielding structures. We present the results of t he optical simulations of both main beam and sidelobes\, including the eff ects of the infrared filters and the dielectric window of the cryostat. An analysis of the mirrors imperfections and deformations completes our unde rstanding of the LSPE-STRIP optical response in its real configuration.\n\ nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/2/contribution/ 22 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/2/contributi on/22 END:VEVENT BEGIN:VEVENT SUMMARY:A Q-band 19 pixel multifeed receiver for the Sardinia radio telesc ope DTSTART;VALUE=DATE-TIME:20200922T081500Z DTEND;VALUE=DATE-TIME:20200922T084000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-1@cern.ch DESCRIPTION:Speakers: Dr. ORFEI\, Alessandro (INAF-IRA)\nA 19 feed 33-50GH z receiver under construction for the SRT antenna will be presented. The k ey modules will be described as well as their measurements in the laborato ry.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/1/contrib ution/1 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/1/contributi on/1 END:VEVENT BEGIN:VEVENT SUMMARY:Dial In DTSTART;VALUE=DATE-TIME:20200921T100000Z DTEND;VALUE=DATE-TIME:20200921T102000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-0@cern.ch DESCRIPTION:Speakers: LOC ()\nThe zoom link including the password will be distributed shortly before the workshop by e-mail. We will give you 30min to open your connection to the workshop so please use the time for connec tion and testing. As we have more than 100 participants this could take so me time.\nIn case you have problems please contact our moderator Zegeye Ki dane under zkidane(at)mpifr.de.\n\nhttps://events.mpifr-bonn.mpg.de/indico /event/154/session/11/contribution/0 LOCATION:your home URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/11/contribut ion/0 END:VEVENT BEGIN:VEVENT SUMMARY:SKA1 Observatory Developement Plan DTSTART;VALUE=DATE-TIME:20200921T110000Z DTEND;VALUE=DATE-TIME:20200921T112500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-3@cern.ch DESCRIPTION:Speakers: Mr. STRINGHETTI\, Luca (SKA Organisation)\nIt is uni versally recognised that a well-funded and carefully targeted development programme is essential to maintain the scientific competitiveness of any o bservatory. The purpose of the SKA Observatory Development Programme (SODP ) is to enhance the scientific productivity of the Observatory by: adaptin g to changes in the scientific landscape and priorities\, enabling new sci ence\, restoring descoped functionality\, improving output and reliabilit y and reducing operational cost.\n\nThe SODP is divided into Projects\, wh ich deliver major improvements\, and Studies\, which are intended to evalu ate new ideas and bring them to an adequate Technology and Manufacturing R eadiness Level (TRL/MRL) to become potential projects. The process require s prioritisation of research and development in the context of science and technology roadmaps.\nThe present discussion is restricted to SKA1 and co ncentrates on the initiation of the SODP and its evolution as the Observat ory transitions from the Construction phase into the operational phase.\nT he talk will present the current plan for the SKA observatory development program as part of the SKA Operation. It will present the organization of the SKA1 roadmaps (science Roadmap and Technological Roadmap) how they are organized and how they will work together to realize the SODP objectives. It will also show the current schedule and the funding mechanism for the programme.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/0/ contribution/3 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/0/contributi on/3 END:VEVENT BEGIN:VEVENT SUMMARY:Managing hundreds of wideband receiving signals at the SRT DTSTART;VALUE=DATE-TIME:20200922T113500Z DTEND;VALUE=DATE-TIME:20200922T120000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-2@cern.ch DESCRIPTION:Speakers: Dr. ORFEI\, Alessandro (INAF-IRA)\nThe completion of the receiver suite up to 116 GHz at the Sardinia radio telescope asks for a completely new infrastructure for routing hundreds of large bandwidth s ignals to several back-ends of different type. In this talk I'll describe how these signals is thought to be handled as well as the status of the wo rk in progress.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/sessi on/8/contribution/2 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/8/contributi on/2 END:VEVENT BEGIN:VEVENT SUMMARY:The VLBA New Digital Architecture DTSTART;VALUE=DATE-TIME:20200921T121500Z DTEND;VALUE=DATE-TIME:20200921T124000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-5@cern.ch DESCRIPTION:Speakers: Dr. BRISKEN\, Walter (National Radio Astronomy Obser vatory)\nA new digital back-end architecture for the Very Long Baseline Ar ray (VLBA) is being developed at NRAO. The system will consist of several main components that are interconnected through a 100 Gbps Ethernet switc h. A pair of dual-channel IF samplers will be placed in the VLBA receiver cabin\, producing four VDIF streams at 2048 Gsps and with greater than 8 bits per sample quanitzation. These "digital IFs" are to be injected into the 100 Gbps switch as VDIF packets over multicast UDP\, allowing one or more "consumer" modules to perform further processing. For the VLBI use c ase\, a module that channelizes and requantizes the data will feed Mark6 r ecorders. the architecture will allow other commensal uses of the digital IF streams such as transient searching\, pulsar timing\, or spectroscopy. In this talk\, I will discuss the overall system architecture\, the stat us of the project\, and the motivations that led to this particular design choice.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/0/co ntribution/5 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/0/contributi on/5 END:VEVENT BEGIN:VEVENT SUMMARY:Design and Implementation of Remote RFI Monitoring System DTSTART;VALUE=DATE-TIME:20200922T130500Z DTEND;VALUE=DATE-TIME:20200922T133000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-4@cern.ch DESCRIPTION:Speakers: NSOR\, Joseph A. K (Ghana Space Science & Technology Inst.)\nDesign and Implementation of Remote RFI Monitoring System\n\nhttp s://events.mpifr-bonn.mpg.de/indico/event/154/session/3/contribution/4 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/3/contributi on/4 END:VEVENT BEGIN:VEVENT SUMMARY:Bluering Prototype System Results DTSTART;VALUE=DATE-TIME:20200922T072500Z DTEND;VALUE=DATE-TIME:20200922T075000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-7@cern.ch DESCRIPTION:Speakers: Dr. HAMPSON\, Grant (CSIRO)\nBluering is the CSIRO n ame given to a new generation of radio astronomy array receivers based on Xilinx’s Radio Frequency System on Chip (RFSOC) technology. Bluering was initially designed for low frequency radio astronomy applications (such a s the MWA telescope)\, but has grown to be a receiver also capable of L-ba nd radio astronomy (such as Phased Array Feeds). Bluering is not only an array receiver\; the spare FPGA resources can be used to form multiple wid eband beams\, compute the array covariance matrix\, RFI mitigation\, and e ven pulsar timing. \n\nTo enable many types of astronomy receiver applicat ions an RF daughter board\, called Taipan\, can be customised to have coax ial and fibre inputs. Available to each Taipan is a tuneable LO signal (wh ich can double the number of RF inputs for some frequencies)\, attenuator control bits as well as a calibration signal. With all these features it i s possible to customise the Taipan to most astronomy applications.\n\nCSIR O has developed a prototype Bluering system based around the 16 input 2GSP S 12-bit ADC version of the RFSOC. This paper presents some of the design details\, including liquid cooling\, RFI shielding\, optical timing\, embe dded control system\, as well as signal processing and communications firm ware. Prototyping results are also presented - in particular RFI shielding \, power\, weight\, SNR\, etc. will be shown. Following the development an d testing of this initial version CSIRO is planning on building a second v ersion (without some of the bugs!) and aims to improve the general perform ance of the system.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/s ession/1/contribution/7 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/1/contributi on/7 END:VEVENT BEGIN:VEVENT SUMMARY:Accelerating astronomy using Atomic COTS DTSTART;VALUE=DATE-TIME:20200922T070000Z DTEND;VALUE=DATE-TIME:20200922T072500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-6@cern.ch DESCRIPTION:Speakers: Dr. HAMPSON\, Grant (CSIRO)\nIn the 20th century hig h end correlators were built with ASICs (VLA\, Westerbork\, Australia Tele scope). As we entered the 21st century FPGAs came to the fore (eVLA\, CABB \, etc.) but due to the huge data flows they needed massive dedicated data transport systems. The CASPER group followed a different path and used n etwork switches for data transport but this imposed a significant extra co st and for large systems such as MeerKAT with considerable effort and inte raction with the switch vendor to get the system to work. The last 5 years has seen the appearance of a new generation of Ethernet switches (In-Netw ork Processors) where the data plane is fully programmable using languages such as P4 and OpenFlow. These languages not only allow precise routing o f packets based on metadata within the Ethernet packets but also open the door to a precise monitoring of the data flow. Thus\, the designer now has the control available with older designs but without the complexity and w ith more advanced features. \n\nThe second revolution was the combination of FPGAs and High Bandwidth (attached) Memory (HBM). HBM memory has an I/0 bandwidth that is more than 30 times that of a 100GbE link. This allows t he full data to be buffered to memory multiple times. Each stage of proces sing can now operate independently of any other\, effectively independent asynchronous subroutines (whereas all early correlator designs were synchr onous). The multiple “subroutines” can now implement end-to-end proces sing. These FPGAs are now available as COTS hardware ready to plug into a standard server and have 100GbE ports that can connect to the In-Network P rocessor.\n\nThe combination of these two technology advances allows a new approach to radio astronomy correlators and beamformers - what we have ca lled “Atomic COTS”. This is a design that uses COTS In-Network Process ors to route data to COTS FPGA cards such that each card receives part of the total bandwidth for all receiving elements. The FPGA then completes al l processing to implement a correlator or beamformer independent of any ot her FPGA (an Atomic operation). The resulting astronomy data products can be routed back through the In-Network Processors to the next stage of pro cessing such as imaging with visibilities and searches for FRBs on tied ar ray beams. An Atomic COTS architecture will enable astronomy backends to u pgrade and deploy incrementally.\n\nhttps://events.mpifr-bonn.mpg.de/indic o/event/154/session/1/contribution/6 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/1/contributi on/6 END:VEVENT BEGIN:VEVENT SUMMARY:Solar power mirror arrays for radio astronomy - towards a test wit h the Juelich Solar Power Tower DTSTART;VALUE=DATE-TIME:20200922T101000Z DTEND;VALUE=DATE-TIME:20200922T103500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-9@cern.ch DESCRIPTION:Speakers: ROY\, Alan ()\, WUCKNITZ\, Olaf ()\nWe have presente d the idea at past meetings to use the mirror arrays of concentrating sola r power stations as vast collecting areas for high-sensitivity radio astro nomy. Since the signals do not combine coherently they will produce an ex tended speckle pattern over the focal region that requires a large phased array feed to collect and combine in-phase. The 4000 element EMBRACE arra y developed under the RadioNet SKADS project is such array feed and might conceivably be re-purposed for this application. We will give an update o n the idea and the plans for a proof-of-concept experiment on the Juelich experimental solar array. For simplicity these start with a two-pixel rec eiver before scaling up.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/ 154/session/2/contribution/9 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/2/contributi on/9 END:VEVENT BEGIN:VEVENT SUMMARY:Developing Digital Receiver for Radio Astronomy Receiver using RFS oC DTSTART;VALUE=DATE-TIME:20200921T140000Z DTEND;VALUE=DATE-TIME:20200921T142500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-8@cern.ch DESCRIPTION:Speakers: Dr. LIU\, Chao (Oxford University)\nThe ultra-wideba nd redshift search receiver (RSR) on Large Millimetre Telescope (LMT)\, wh ich covers 73 - 110.5 GHz simultaneously\, has been built about 10 years a go. Due to the limits in the speed\, performance and cost of the high spee d sampler when the receiver was designed\, the receiver was implemented us ing analog autocorrelator. As the price-performance rate in digital techno logies is constantly improving\, replacing the analog RSR receiver by a di gital one becomes feasible. The digital system could offer higher frequenc y resolution and more system flexibility for more advanced science cases. This project was aimed to design and implement digital backend system for RSR. \nThe RFSoC from Xilinx caught the attention of radio astronomy commu nity when first released. RFSoC device has been selected as a core platfor m for the RSR receiver\, as it offer 8x4G ADCs\, large amount of programma ble logic resources and powerful processor with multiple cores. Therefore\ , the RFSoC can integrate signal sampling\, data processing and transmissi on and control functions in a single IC\, which will be beneficial in both system design and costing perspectives. The talk will be focused on the d igital backend system built for RSR and general radio astronomy receivers based on the RFSoC. The system at the present stage is fully functional as a spectrometer and can be extended in any shape base on system requiremen t of different telescopes and science cases. The experimental ADC characte rization demonstrates around 80 dB Spurious Free Dynamic Range (SFDR) over the spectrum from DC to 2.048 GHz. The evaluation results of the RFSoC ba sed spectrometer performs with high level of stability and dynamic range w ith hundreds of seconds’ real-time integration time. The results give us solid confidence in using RFSoC for radio astronomy receivers. It is a cr itical milestone of the RSR receiver project and we can carry on by just s caling the system up. \nThe RFSoC based receiver modules will be extend to CBASS\, Goonhilly GHY3 and other receiver platforms under development in Oxford. The system is not only suitable for high bandwidth signal but also hugely beneficial for systems with high channel counts\, such as SKA\, AT A and other interferometry radio astronomy telescopes. The RFSoC data conv erters can digitize as many as 16 channels simultaneously\, the programmab le logic can handle the channelization and beamforming and the control and communication can be managed by the applications on ARM processors. It ca n largely save the system cost and development effort in both hardware and software perspectives.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/1 54/session/4/contribution/8 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/4/contributi on/8 END:VEVENT BEGIN:VEVENT SUMMARY:A Compact Triple Band Receiver System working at K-\, Q- and W-ban d for Medicina\, Noto and Sardinia Radio Telescopes DTSTART;VALUE=DATE-TIME:20200922T120000Z DTEND;VALUE=DATE-TIME:20200922T122500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-11@cern.ch DESCRIPTION:Speakers: Dr. BOLLI\, Pietro (INAF)\nA Compact Triple Band Rec eiver System working at K-\, Q- and W-band for Medicina\, Noto and Sardini a Radio Telescopes\n\nPietro Bolli (Italian National Institute for Astroph ysics)\, Seog-Tae Han (Korea Astronomy and Space Science Institute)\, Jiho on Choi (Korea Astronomy and Space Science Institute) and Alessandro Orfei (Italian National Institute for Astrophysics)\n\nA compact triple band re ceiver system is under development by a mutual collaboration between INAF\ , Italy and KASI\, Korea. Three receivers will be fabricated and installed on the 64 m Sardinia radio telescope\, 32 m Noto and Medicina radio teles copes respectively. \nEach receiver enables simultaneous observations in t he three frequency intervals: K-band (18–26 GHz/8 GHz IF bandwidth)\, Q- band (34–50 GHz/16 GHz IF bandwidth) and W-band (85–116GHz/32 GHz IF b andwidth). An integrated quasi-optical circuit plus a compact triple-band receiver located in a single cryostat is chosen in order to circumvent dif ficulties in installation and beam alignment. A frequency-independent quas i-optical circuit for each band is adopted to obtain constant aperture eff iciency as a function of the observed frequencies. The simulation results show that total aperture efficiency of each recommended frequency band is maintained almost constant within 1%. \nWe present the design details of t he compact wideband quasi-optical circuit and the properties of the triple -band receiver optimized for simultaneous multi-frequency observations. It is expected that it will be dedicated to conduct millimeter wave VLBI and Sun observations.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/se ssion/8/contribution/11 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/8/contributi on/11 END:VEVENT BEGIN:VEVENT SUMMARY:IRAM telescope instrumentation overview and future plans DTSTART;VALUE=DATE-TIME:20200921T112500Z DTEND;VALUE=DATE-TIME:20200921T115000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-10@cern.ch DESCRIPTION:Speakers: Dr. RISACHER\, christophe (IRAM)\nIRAM operates two millimetre observatories on two sites: the NOEMA interferometer located in the French Alps at 2500m altitude with currently 11 antennas of 15m diame ter and the 30m telescope in southern Spain\, Pico Veleta (3000m). They ob serve in the 70-373 GHz frequency range. We'll summarise the current recei vers status and performance\, and present the plans for the near and far f uture. In particular\, we are starting an upgrade of the current NOEMA rec eivers to allow interferometric dual frequency observations. On the longer term\, new generation of SIS mixers will allow extending the RF and IF ba ndwidths. Very large heterodyne array receivers are also under development \, at 3 mm and 1.3 mm for the 30m Telescope.\n\nhttps://events.mpifr-bonn. mpg.de/indico/event/154/session/0/contribution/10 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/0/contributi on/10 END:VEVENT BEGIN:VEVENT SUMMARY:Earth-Orbit Aperture Synthesis DTSTART;VALUE=DATE-TIME:20200922T142000Z DTEND;VALUE=DATE-TIME:20200922T144500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-13@cern.ch DESCRIPTION:Speakers: ROY\, Alan ()\nI investigate the idea that VLBI migh t be done between one antenna\nand itself as it moves along the Earth's or bit\, provided the bandwidth\nis sufficiently small that the coherence tim e is longer than the time\nneeded for the antenna to sweep out the baselin e. Such a technique\noffers the tantalizing prospect of synthesizing spac e-VLBI-like\nbaselines without needing a satellite\, or the ability to fil l in\nmissing short baselines in EVN. However the initial result from a\n numerical model is that it does not work\, at least for uniform linear\nmo tion\, for an interesting reason.\n\nhttps://events.mpifr-bonn.mpg.de/indi co/event/154/session/3/contribution/13 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/3/contributi on/13 END:VEVENT BEGIN:VEVENT SUMMARY:Latest calibration results from QUBIC: The Q&U Bolometric Interfer ometer for Cosmology DTSTART;VALUE=DATE-TIME:20200922T085500Z DTEND;VALUE=DATE-TIME:20200922T092000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-12@cern.ch DESCRIPTION:Speakers: MOUSSET\, Louise (obsparis)\nQUBIC is an experiment dedicated to the measurement of the B-mode polarization from\nthe Cosmic M icrowave Background (CMB)\, using a novel technology: Bolometric\nInterfer ometry. The instrument will have 2 focal planes at 150 GHz and 220 GHz. Th anks\nto its unique spectroimaging capabilities\, QUBIC will also be a pow erful instrument to\nconstrain foreground contamination (thermal galaxy du st emission\, synchrotron\nemission\, ...). The technical demonstrator has been tested and the concept of this new\ninstrument has been validated.\n In this talk\, I will 1rst explain the instrument architecture\, focussin g on the optical\n design. Some of the calibration results will be present ed\, showing that we actually have\n a working bolometric interferometer.\ n The unique design of QUBIC brings new possibilities to CMB polarization mapping\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/2/con tribution/12 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/2/contributi on/12 END:VEVENT BEGIN:VEVENT SUMMARY:BRAND EVN Broadband Receiver - a technological challenge DTSTART;VALUE=DATE-TIME:20200921T133500Z DTEND;VALUE=DATE-TIME:20200921T140000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-15@cern.ch DESCRIPTION:Speakers: TUCCARI\, Gino ()\nThe BRAND wideband receiver is be ing developed with support from the European \nUnion's Horizon 2020 resear ch \nand innovation programme as a part of RadioNet. \nThe project represe nts a big technological challenge in the entire signal chain from the feed section to the digital \nprocessing. Its continuous frequency range from 1.5 GHz to 15 GHz makes it a scientifically \nextremely interesting develo pment \nfor the EVN network and radio astronomy in general. It also covers the \nVGOS frequencies and even extends them to \nlower and higher freque ncies. It will allow to retrofit \ntraditional prime focus antennas to bec ome compatible with VGOS \nantennas in terms of frequency coverage\, with a much greater output data rate. \nThe status of the project is reported w ith the goals achieved and the items still under way.\n\nhttps://events.mp ifr-bonn.mpg.de/indico/event/154/session/4/contribution/15 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/4/contributi on/15 END:VEVENT BEGIN:VEVENT SUMMARY:Efficient wide-area sky monitoring DTSTART;VALUE=DATE-TIME:20200922T133000Z DTEND;VALUE=DATE-TIME:20200922T135500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-14@cern.ch DESCRIPTION:Speakers: WUCKNITZ\, Olaf ()\nThe enigmatic Fast Radio Bursts (FRBs) are motivating new instruments to monitor large areas of the sky wi th high time resolution. With a field of view of about 200 square degrees\ , CHIME is currently finding several per day. Gravitationally lensed FRBs could be used as a new cosmological probe\, but this requires the continuo us monitoring of even wider areas. Regular antenna arrays can be combined with extremely efficient Fast-Fourier-Transform beamformers to map good fr actions of the sky with full time resolution. We discuss some options\, in cluding the (mis-)use of existing phased-array-feed receivers as aperture arrays.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/3/con tribution/14 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/3/contributi on/14 END:VEVENT BEGIN:VEVENT SUMMARY:VLBI with a remote maser and a COTS formatter DTSTART;VALUE=DATE-TIME:20200922T075000Z DTEND;VALUE=DATE-TIME:20200922T081500Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-17@cern.ch DESCRIPTION:Speakers: Mr. BOVEN\, Paul (JIVE)\nThe Hydrogen maser is requi red equipment for any VLBI station\, and so is a formatter such as a DBBC( 1\,2 or 3) or DBE. Together\, these ensure that the received spectrum gets digitized\, timestamped with sufficient stability\, and provided with hea ders to allow playback at a correlator. These necessities however don't co me cheap.\n\nWhite Rabbit is an open standard for time and frequency distr ibution over fiber. It was originally intended to synchronize and control the experiments at the LHC\, but we show that it is possible to extend its reach and frequency stability in such a way that it can be used to transp ort a reference clock for VLBI.\n\nGNU Radio is a "free and open-source so ftware development toolkit that provides signal processing blocks to imple ment software defined radios". Using this software\, I've designed a VLBI receiver and formatter using an off the shelf software-defined radio. It g enerates standard compliant VDIF data\, which can be processed by the EVN SFXC correlator\, and many others. Our first experiments were not able to be processed in real-time and only provided two subbands\, but work is ong oing to develop this into a 1024 Mb/s capable VLBI formatter.\n\nUsing the se two methods\, and the H-maser at the WSRT\, we have successfully demons trated VLBI fringes between the historical 25m Dwingeloo telescope and man y EVN stations.\n\nThese developments showcase that off-the-shelf hardware and (open source) software are starting to become viable technologies for our signal processing needs. This will help lower the cost to outfit a st ation for VLBI\, which in turn could help with increasing the UV coverage for VLBI arrays.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/sess ion/1/contribution/17 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/1/contributi on/17 END:VEVENT BEGIN:VEVENT SUMMARY:Development of an Optimized Real-Time Radio Transient Imager for L WA-SV DTSTART;VALUE=DATE-TIME:20200922T135500Z DTEND;VALUE=DATE-TIME:20200922T142000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-16@cern.ch DESCRIPTION:Speakers: Dr. KRISHNAN\, Hariharan (Arizona State University)\ nIn this paper\, we describe our efforts towards\nthe development of a rea l-time radio imaging correlator for\nthe Long-Wavelength Array station in Sevilleta\, New Mexico.\nWe briefly discuss the direct-imaging algorithm a nd present\nthe architecture of the GPU implementation. We describe the\nc ode-level modifications carried out to some of the modules in\nthe algorit hm that improves GPU-memory management and\nhighlight the performance impr ovements achieved through it.\nWe emphasize our ongoing efforts in tuning the overall run-time\nduration of the correlator which in turn is expected to increase\nthe operating bandwidth in order to address the demands of\n wide-band capability for radio transient science.\n\nhttps://events.mpifr- bonn.mpg.de/indico/event/154/session/3/contribution/16 LOCATION:Max Planck Institute for Radio Astronomy URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/3/contributi on/16 END:VEVENT BEGIN:VEVENT SUMMARY:Welcome and technical issues DTSTART;VALUE=DATE-TIME:20200921T103000Z DTEND;VALUE=DATE-TIME:20200921T104000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-19@cern.ch DESCRIPTION:Speakers: Dr. KELLER\, Reinhard ()\nSome technical/administrat ive issues will be explained: how to use zoom with screen sharing and the chat function for questions\, how the trivia evening is working\, how we w ant to make a group photo.\n\nhttps://events.mpifr-bonn.mpg.de/indico/even t/154/session/6/contribution/19 LOCATION: URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/6/contributi on/19 END:VEVENT BEGIN:VEVENT SUMMARY:Application of TES bolometers and KID cameras to pulsar observatio ns DTSTART;VALUE=DATE-TIME:20200922T094500Z DTEND;VALUE=DATE-TIME:20200922T101000Z DTSTAMP;VALUE=DATE-TIME:20260416T114733Z UID:indico-contribution-154-18@cern.ch DESCRIPTION:Speakers: Dr. TORNE\, Pablo (Instituto de Radioastronomia Mili metrica (IRAM))\nPulsar studies are generally carried out at centimetre wa velengths and high-energies (X-ray\, Gamma-ray)\, where pulsars are bright er and the available instrumentation is well adapted to fast time-domain s cience. In the last years\, pulsar astronomy in the millimetre band has in tensified\, supported mainly by large-bandwidth instrumentation with fast- sampling capabilities at the IRAM 30-m telescope. However\, receiver and b ackend combinations suitable for pulsar observations at (sub)millimetre fa cilities are rare. In this contribution\, we will discuss a novel applicat ion of continuum cameras to pulsar astronomy in the (sub)millimetre range\ , which offers a new possibility to enable pulsar observations with high s ensitivity at observatories where these type of receivers are (or will be) available. This promises to extend the spectral window in which pulsars c an be studied\, often with minimal or no extra modifications to the origin al hardware. Two proof-of-concept experiments will be presented\, showing detections of a radio magnetar with the NIKA2 KID camera on the IRAM 30-m Telescope\, and the SCUBA2 TES bolometer on the James Clerk Maxwell Telesc ope.\n\nhttps://events.mpifr-bonn.mpg.de/indico/event/154/session/2/contri bution/18 LOCATION:Max Planck Institute for Radio Astronomy Lecture Hall 0.02 URL:https://events.mpifr-bonn.mpg.de/indico/event/154/session/2/contributi on/18 END:VEVENT END:VCALENDAR