Event calendar file
21-22 September 2020
Max Planck Institute for Radio Astronomy
Europe/Berlin timezone
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Contribution List
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27
Session:
Session 5
A Compact Triple Band Receiver System working at K-, Q- and W-band for Medicina, Noto and Sardinia Radio Telescopes
Pietro Bolli (Italian National Institute for Astrophysics), Seog-Tae Han (Korea Astronomy and Space Science Institute), Jihoon Choi (Korea Astronomy and Space Science Institute) and Alessandro Orfei (Italian National Institute for Astrophysics)
A compact triple band receiver sy
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Presented by Dr. Pietro BOLLI
on
22 Sep 2020
at
14:00
Session:
Session 3
A 19 feed 33-50GHz receiver under construction for the SRT antenna will be presented. The key modules will be described as well as their measurements in the laboratory.
Presented by Dr. Alessandro ORFEI
on
22 Sep 2020
at
10:15
Session:
Session 3
In the 20th century high end correlators were built with ASICs (VLA, Westerbork, Australia Telescope). 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 network switches for data transport but this imposed a significant extra cost and for
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Presented by Dr. Grant HAMPSON
on
22 Sep 2020
at
09:00
Session:
Session 4
Pulsar studies are generally carried out at centimetre wavelengths and high-energies (X-ray, Gamma-ray), where pulsars are brighter and the available instrumentation is well adapted to fast time-domain science. In the last years, pulsar astronomy in the millimetre band has intensified, supported mainly by large-bandwidth instrumentation with fast-sampling capabilities at the IRAM 30-m telescope. H
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Presented by Dr. Pablo TORNE
on
22 Sep 2020
at
11:45
Session:
Session 2
The BRAND wideband receiver is being developed with support from the European
Union's Horizon 2020 research
and innovation programme as a part of RadioNet.
The project represents a big technological challenge in the entire signal chain from the feed section to the digital
processing. Its continuous frequency range from 1.5 GHz to 15 GHz makes it a scientifically
extremely interesting dev
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Presented by Gino TUCCARI
on
21 Sep 2020
at
15:35
Session:
Session 3
Bluering is the CSIRO name 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 as the MWA telescope), but has grown to be a receiver also capable of L-band radio astronomy (such as Phased Array Feeds). Bluering is not only an array re
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Presented by Dr. Grant HAMPSON
on
22 Sep 2020
at
09:25
Session:
Session 6
Design and Implementation of Remote RFI Monitoring System
Presented by Joseph A. K NSOR
on
22 Sep 2020
at
15:05
Session:
Session 2
The ultra-wideband redshift search receiver (RSR) on Large Millimetre Telescope (LMT), which covers 73 - 110.5 GHz simultaneously, has been built about 10 years ago. Due to the limits in the speed, performance and cost of the high speed sampler when the receiver was designed, the receiver was implemented using analog autocorrelator. As the price-performance rate in digital technologies is constant
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Presented by Dr. Chao LIU
on
21 Sep 2020
at
16:00
Session:
Session 6
In this paper, we describe our efforts towards
the development of a real-time radio imaging correlator for
the Long-Wavelength Array station in Sevilleta, New Mexico.
We briefly discuss the direct-imaging algorithm and present
the architecture of the GPU implementation. We describe the
code-level modifications carried out to some of the modules in
the algorithm that improves GPU-memory manag
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Presented by Dr. Hariharan KRISHNAN
on
22 Sep 2020
at
15:55
Session:
Registration
The 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 connection and testing. As we have more than 100 participants this could take some time.
In case you have problems please contact our moderator Zegeye Kidane under zkidane(at)mpifr.de.
Presented by LOC
on
21 Sep 2020
at
12:00
Session:
Session 6
I investigate the idea that VLBI might be done between one antenna
and itself as it moves along the Earth's orbit, provided the bandwidth
is sufficiently small that the coherence time is longer than the time
needed for the antenna to sweep out the baseline. Such a technique
offers the tantalizing prospect of synthesizing space-VLBI-like
baselines without needing a satellite, or the ability t
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Presented by Alan ROY
on
22 Sep 2020
at
16:20
Session:
Session 6
The enigmatic Fast Radio Bursts (FRBs) are motivating new instruments to monitor large areas of the sky with 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 continuous monitoring of even wider areas. Regular antenna arrays can be combined
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Presented by Olaf WUCKNITZ
on
22 Sep 2020
at
15:30
Session:
Session 1:
IRAM operates two millimetre observatories on two sites: the NOEMA interferometer located in the French Alps at 2500m altitude with currently 11 antennas of 15m diameter and the 30m telescope in southern Spain, Pico Veleta (3000m). They observe in the 70-373 GHz frequency range. We'll summarise the current receivers status and performance, and present the plans for the near and far future. In part
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Presented by Dr. christophe RISACHER
on
21 Sep 2020
at
13:25
Session:
Session 1:
ASTRON operates the pan-European Low -Frequency Array (LOFAR), a unique
instrument that will complement phase one of the Square Kilometre Array
(SKA), planned for construction in the coming three to five years. After
nearly a decade of scientific operations, LOFAR science output is still
ramping up. However, to keep the telescope at the forefront of science,
a staged upgrade programme LO
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Presented by Dr. Albert-Jan BOONSTRA
on
21 Sep 2020
at
13:50
Session:
Session 4
QUBIC is an experiment dedicated to the measurement of the B-mode polarization from
the Cosmic Microwave Background (CMB), using a novel technology: Bolometric
Interferometry. The instrument will have 2 focal planes at 150 GHz and 220 GHz. Thanks
to its unique spectroimaging capabilities, QUBIC will also be a powerful instrument to
constrain foreground contamination (thermal galaxy dust emissi
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Presented by Louise MOUSSET
on
22 Sep 2020
at
10:55
Session:
Session 5
The 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 signals 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 work in progress.
Presented by Dr. Alessandro ORFEI
on
22 Sep 2020
at
13:35
Session:
Session 1:
It is universally recognised that a well-funded and carefully targeted development programme is essential to maintain the scientific competitiveness of any observatory. The purpose of the SKA Observatory Development Programme (SODP) is to enhance the scientific productivity of the Observatory by: adapting to changes in the scientific landscape and priorities, enabling new science, restoring descop
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Presented by Mr. Luca STRINGHETTI
on
21 Sep 2020
at
13:00
Session:
Session 5
The technological developments pioneered at the Korean VLBI Network
for designing and implementing simultaneous multfiband (SMB) receivers
paved the way to extending phase calibration and phase referencing
techniques to the frequency space. Numerous advantages of this
extension have been convincingly demonstrated at the KVN, and the time
is now right to explore them on a larger scale. This wo
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Presented by Andrei LOBANOV
on
22 Sep 2020
at
14:25
Session:
Session 4
We present the analysis of the optical system of the STRIP instrument, the ground-based telescope of the Large Scale Polarization (LSPE) experiment, which aims at polarization measurements of the Cosmic Microwave Background on large angular scales.
STRIP will observe the polarized emission from the "Observatorio del Teide" in Tenerife, starting in late 2021. The instrument consists of an array of
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Presented by Ms. Sabrina REALINI
on
22 Sep 2020
at
11:20
Session:
Session 2
Most radio telescopes can have greatly expended survey speed and imaging capability by utilizing multiple receivers either as feed clusters, phased-array feeds, or a larger number of individual antennas. The number of receivers is often limited by the cost of the cryogenic cooling required for sensitivity at frequencies > 1 GHz. This paper will describe a new class of LNAs for the low microwa
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Presented by Dr. Sander WEINREB
on
21 Sep 2020
at
16:25
Session:
Session 4
We have presented the idea at past meetings to use the mirror arrays of concentrating solar power stations as vast collecting areas for high-sensitivity radio astronomy. Since the signals do not combine coherently they will produce an extended speckle pattern over the focal region that requires a large phased array feed to collect and combine in-phase. The 4000 element EMBRACE array developed un
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Presented by Alan ROY, Olaf WUCKNITZ
on
22 Sep 2020
at
12:10
Session:
Session 2
Recent developments in high-speed networking and PCIe-mounted accelerator
cards have made possible new backend designs that provide vastly improved
flexibility and capability in signal processing for radio astronomy.
While direct digitization close to the receiver improves the quality of the
physical signal by reducing analog transmission and filtering losses, it also
enables the building of
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Presented by Dr. Tobias WINCHEN
on
21 Sep 2020
at
15:10
Session:
Session 1:
A new digital back-end architecture for the Very Long Baseline Array (VLBA) is being developed at NRAO. The system will consist of several main components that are interconnected through a 100 Gbps Ethernet switch. 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 "di
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Presented by Dr. Walter BRISKEN
on
21 Sep 2020
at
14:15
Session:
Session 3
The Hydrogen maser is required 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 headers to allow playback at a correlator. These necessities however don't come cheap.
White Rabbit is an open standard for time and frequency distribution
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Presented by Mr. Paul BOVEN
on
22 Sep 2020
at
09:50
Session:
Welcome
Some technical/administrative 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 want to make a group photo.
Presented by Dr. Reinhard KELLER
on
21 Sep 2020
at
12:30
