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Träfflista för sökning "WFRF:(Nyström Olle 1979 ) "

Sökning: WFRF:(Nyström Olle 1979 )

  • Resultat 1-10 av 24
  • [1]23Nästa
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1.
  • Belitsky, Victor, 1955-, et al. (författare)
  • Facility Heterodyne Receiver for the Atacama Pathfinder Experiment Telescope
  • 2007
  • Ingår i: Proceedings of Joint 32nd International Conference on Infrared Millimeter Waves and 15th International conference on Terahertz Electronics, Sept 3-7, 2007, City Hall, Cardiff, Wales, UK. - 1424414303 ; s. 326-328
  • Konferensbidrag (refereegranskat)
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2.
  • Belitsky, Victor, 1955-, et al. (författare)
  • Terahertz Instrumentation For Radio Astronomy
  • 2009
  • Ingår i: International Symposium on Terahertz Science and Technology between Japan and Sweden. ; s. 28-29
  • Konferensbidrag (övrigt vetenskapligt)abstract
    • Radio Astronomy was always a frontrunner in the demand on terahertz technology. Millimetre and sub-millimetre wave receivers operate at ground-based observatories for more than 20 years with real Terahertz instruments making its way to ground-based [1] and space-based observatories, e.g., Herschel HIFI, during last years. In this talk, we will look at the key requirements to the radio astronomy and environmental science terahertz receivers using heterodyne technology. The most promising and established technologies for high-resolution spectroscopy instrumentation will be discussed. Using results of the Group for Advanced Receiver Development for Onsala Space Observatory 20 m telescope, for Atacama Pathfinder Experiment (APEX) telescope and ALMA Project Band 5, we will illustrate the trends and achievements in the terahertz instrumentation for radio astronomy.
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3.
  • Lapkin, Igor, 1963-, et al. (författare)
  • Optics Design and Verification for the APEX Swedish Heterodyne Facility Instrument (SHeFI)
  • 2008
  • Ingår i: In Proceedings of The 19th International Symposium on Space Terahertz Technology, Groningen, 28-30 April, 2008, ed. W. Wild, Space Research Organization of the Netherlands (SRON). ; Part I, s. 351-357
  • Konferensbidrag (refereegranskat)abstract
    • We present the design and verification of the receiver optics for the Single-Pixel Heterodyne Facility Instrument (SHFI) of the APEX telescope [1]. The SHFI is designed to cover the frequency band 211 – 1390 GHz in 6 receiver channels. Four of the receiver channels have been designed, installed and characterized: 211-275 GHz (Band 1); 275-370 GHz (Band 2); 385- 500 GHz (Band 3); 1250-1390 GHz (Band T2). The first three bands employ 2SB SIS mixer technology and Band T2 employs HEB mixers in a waveguide balanced mixer configuration. The entire optics design was driven by the receiver position in the telescope Nasmyth cabin “A” (Fig.1) and the aperture limit of Ø150 mm, introduced by the elevation encoder inside the Nasmyth tube A. This layout and the telescope geometry (~ 6 m distance from the focal plane to the Cabin A) lead us to choose a single-pixel configuration and required using intermediate optics with long focal distances. The common optics path, coupling the receivers to the Cassegrain sub-reflector, consists of the three offset ellipsoidal mirrors, M3, M6, M8s, and three flat mirrors, F4, F5, and F7s. The combination M3 and M6 via flat F4, F5, creates a Gaussian telescope, providing frequency-independent re-imaging of the antenna focal plane from the Cassegrain cabin into the Nasmyth cabin A. Switching between channels is achieved by the precision rotating of the active mirror M8s. The mirror M8s in combination with each channel active mirror M10 provides re-imaging of the secondary onto the feed horn aperture of the selected channel. Such a configuration provides frequency independent illumination of the secondary with the edge taper -12dB. The angular position of the flat mirrors F9 is adjustable and gives additional possibility of fine-tuning of the beam alignment from the common optics to every receiver channels. Verification of the optical design through measurements is essential in order to align the beams from the cryostat windows to the common optics to minimize loss in the quasioptical guiding system. In order to verify the design of the cold optics (corrugated horn + M10) in terms of Gaussian beam parameters, a new wideband vector field measurement system was developed [2]. Vector field measurements were performed for band 1, 2, and 3, and scalar measurements were employed for the THz band.
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4.
  • Nyström, Olle, 1979-, et al. (författare)
  • Optics Design and Verificatgion for the APEX Swedish Heterodyne Facility Instrument (SHeFI)
  • 2009
  • Ingår i: Journal of Infrared, Millimeter and Terahertz Waves. - 1866-6892. ; 30:7, s. 746-761
  • Tidskriftsartikel (refereegranskat)abstract
    • In this paper, we present the design and verification of the optics of the Swedish Heterodyne Facility Instrument (SHeFI) receiver installed in the Atacama Pathfinder EXperiment (APEX) telescope during spring 2008. SHeFI is located in the Nasmyth instrumentation Cabin A (NCA). The receiver has been designed to have 6 frequency channels, of which four receiver channels have been built, and characterized: 211-275 GHz(Band 1), 275-370 GHz (Band 2), 385-500 GHz (Band 3), and 1250-1390 GHz (Band T2). Bands 1, 2, and T2 are installed at the telescope and are currently in operation. The optical design is driven by the requirement of frequency independent illumination of the secondary with -12 dB edge taper for each frequency channel and the limitation (beam clearance through the Nasmyth tube and the elevation encoder) imposed by the receiver position in the NCA. This paper describes the design approach, optimization, and verification of the optical system, coupling each individual receiving beam to the common optics of the telescope.
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5.
  • Vassilev, Vessen, 1969-, et al. (författare)
  • A Swedish heterodyne facility instrument for the APEX telescope
  • 2008
  • Ingår i: Astronomy & Astrophysics. - 0004-6361. ; 490:3, s. 1157-1163
  • Tidskriftsartikel (refereegranskat)abstract
    • In March 2008, the APEX facility instrument was installed on the telescope at the site of Lliano Chajnantor in northern Chile. The main objective of the paper is to introduce the new instrument to the radio astronomical community. It describes the hardware configuration and presents some initial results from the on-sky commissioning. The heterodyne instrument covers frequencies between 211 GHz and 1390 GHz divided into four bands. The first three bands are sideband-separating mixers operating in a single sideband mode and based on superconductor-insulator-superconductor (SIS) tunnel junctions. The fourth band is a hot-electron bolometer, waveguide balanced mixer. All bands are integrated in a closedcycle temperature-stabilized cryostat and are cooled to 4 K. We present results from noise temperature, sideband separation ratios, beam, and stability measurements performed on the telescope as a part of the receiver technical commissioning. Examples of broad extragalactic lines are also included.
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6.
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7.
  • Belitsky, Victor, 1955-, et al. (författare)
  • Design and performance of ALMA band 5 receiver cartridge
  • 2010
  • Ingår i: 35th International Conference on Infrared Millimeter and Terahertz Waves (IRMMW-THz), 2010. - 978-1-4244-6655-9 ; s. 1-2
  • Konferensbidrag (refereegranskat)abstract
    • ALMA, Atacama Large Millimetre Array, covers the frequency band from 30 GHz to 960 GHz in ten separate frequency bands. We present here the design and performance of the ALMA Band 5 receiver cartridge that covers 163–211 GHz. The Band 5 receiver shows the state-of-the-art performance with the noise temperature below 65K (SSB) and sideband rejection above 12 dB over 80% of the RF band.
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8.
  • Belitsky, Victor, 1955-, et al. (författare)
  • Prototype ALMA Band 5 Cartridge:Design and Performance
  • 2009
  • Ingår i: Proceedings of the 20TH INTERNATIONAL SYMPOSIUM ON SPACE TERAHERTZ TECHNOLOGY, Charlottesville, VA, USA, April 20-22, 2009, s. 2-5.
  • Konferensbidrag (refereegranskat)abstract
    • The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of East Asia, Europe and North America in cooperation with the Republic of Chile and aims to build an interferometer radio telescope consisting of more than 60 antennas. The instrument is under construction at the Llano de Chajnantor, about 50 km east of San Pedro de Atacama, Chile. This work presents a part of ALMA frontend, the development, design and performance of one of the frequency channels of the ALMA receiver, the Band 5 prototype cartridge for 163 – 211 GHz frequency band.
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9.
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10.
  • Billade, Bhushan, 1982-, et al. (författare)
  • Performance of the First ALMA Band 5 Production Cartridge
  • 2012
  • Ingår i: IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY. - 2156-342X. ; 2:2, s. 208-214
  • Tidskriftsartikel (refereegranskat)abstract
    • We present performance of the first ALMA Band 5 production cartridge, covering frequencies from 163 GHz to 211 GHz. ALMA Band 5 is a dual polarization, sideband separation (2SB) receiver based on all Niobium (Nb) Superconductor-Insulator-Superconductor (SIS) tunnel junction mixers, providing 16 GHz of instantaneous RF bandwidth for astronomy observations. The 2SB mixer for each polarization employs a quadrature configuration. The sideband separation occurs at the output of the IF hybrid that has integrated bias-T for biasing the mixers, and is produced using superconducting thin film technology. Experimental verification of the Band 5 cold cartridge performed together with warm cartridge assembly, confirms that the system noise temperature is below 45 K over most of the RF band, which is less than five photon noise (5 hf/k). This is to our knowledge, the best results reported at these frequencies. The measurement of the sideband rejection indicates that the sideband rejection better than 10 dB over 90% of the observational band.
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  • Resultat 1-10 av 24
  • [1]23Nästa
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