Tools of Radio Astronomy

Rohlfs, K.

doi:10.1007/978-3-662-02465-2

Cited by 78 publications

(49 citation statements)

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“…The response of a feedhorn to incident radiation is complex and depends on two interrelated factors: the radiation modes that propagate in the horn and circular waveguide, and the coupling of the telescope diffraction pattern to the. feedhorn antenna pattern [83,[116][117][118]. The performance of the feedhorns is currently being investigated by members of the SPIRE consortium; the discussion below summarizes the accepted understanding at the time of publication [5,119].…”

Section: Feedhornsmentioning

confidence: 99%

“…Similar to a radio telescope, each feedhorn produces an antenna pattern with sidelobes and a main beam perpendicular to the plane of the feedhorn aperture [118,121]. To describe the feedhorn's response to incident light, we define the main-beam efficiency, n s , as the fraction of the feedhorn antenna pattern contained in the main beam.…”

Section: Feedhorn Antenna Patternmentioning

confidence: 99%

“…Each of the three interconnected efficiencies (aperture, feedhorn and main-beam) have mode and wavelength dependencies [5,66,83,85,113,114,[118][119][120][121][122]124,126].…”

Section: ----mentioning

confidence: 99%

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SHIFTS: simulator for the Herschel imaging Fourier transform spectrometer

Lindner

Naylor

Swinyard

2006

Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter

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The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments on the European Space Agency's (ESAs) Herschel Space Observatory (HSO). The medium resolution spectroscopic capabilities of SPIRE are provided by an imaging Fourier transform spectrometer (IFTS). A software simulator of the SPIRE IFTS was written to generate realistic data products, making use of available qualification and test data. We present the design and implementation of the simulator. Component and end-to-end simulations were compared to results from the first

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Section: Feedhornsmentioning

confidence: 99%

Section: Feedhorn Antenna Patternmentioning

confidence: 99%

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SHIFTS: simulator for the Herschel imaging Fourier transform spectrometer

Lindner

Naylor

Swinyard

2006

Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter

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“…In this case, the shape of the radio continuum spectrum as it varies from the optically thick (low-frequency) to the optically thin (high-frequency) part provides additional information on physical conditions in the plasma (e.g. Rohlfs 1986, Section 8 · 4). The consequence of the theory outlined above is the prediction of a close relationship between the thermal radio continuum flux density and Hα intensity along a line of sight free from other emission or any absorption processes.…”

Section: Basic Mechanisms Of Thermal Emissionmentioning

confidence: 99%

Relationships between Galactic Radio Continuum and HαEmission

Cram

Green

Bock

1998

Publ. – Astron. Soc. Aust

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Radio continuum emission due to thermal bremsstrahlung and optical Hα spectral line emission arise from processes involving similar atomic entities and physical conditions. The relationship between the flux density of the emission from the two processes is mainly a function of the electron temperature of the emitting region, modified by other factors such as the mode of radiation transfer in the hydrogen spectrum. On the other hand, radio continuum radiation due to non-thermal synchrotron emission is formed by species and processes not involved in thermal emission. As a consequence, differences between the observed radio continuum emission and Hα emission from cosmic sources can provide reliable information on a variety of important physical aspects of the sources, including the relative importance of thermal and non-thermal radio emission and the degree of optical obscuration. This paper reviews the theory of the formation of Hα and the radio continuum in the interstellar medium (ISM), discusses some of the factors that must be considered in comparing observations made in the two frequency regimes, and summarises the properties of some classes of galactic object that emit both optical and radio radiation.

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“…Finally, to achieve a reasonable signal to noise ratio, the IF signal generally has to be integrated over a very long period. The required integration time decreases quadratically 21,22 with lower T N .…”

Section: Introductionmentioning

confidence: 99%

Full characterization and analysis of a terahertz heterodyne receiver based on a NbN hot electron bolometer

Hajenius

Baselmans

Baryshev

et al. 2006

Journal of Applied Physics

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We present a complete experimental characterization of a quasioptical twin-slot antenna coupled small area ͑1.0ϫ 0.15 m 2 ͒ NbN hot electron bolometer ͑HEB͒ mixer compatible with currently available solid state tunable local oscillator ͑LO͒ sources. The required LO power absorbed in the HEB is analyzed in detail and equals only 25 nW. Due to the small HEB volume and wide antenna bandwidth, an unwanted direct detection effect is observed which decreases the apparent sensitivity. Correcting for this effect results in a receiver noise temperature of 700 K at 1.46 THz. The intermediate frequency ͑IF͒ gain bandwidth is 2.3 GHz and the IF noise bandwidth is 4 GHz. The single channel receiver stability is limited to 0.2-0.3 s in a 50 MHz bandwidth.

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Tools of Radio Astronomy

Cited by 78 publications

References 0 publications

SHIFTS: simulator for the Herschel imaging Fourier transform spectrometer

SHIFTS: simulator for the Herschel imaging Fourier transform spectrometer

Relationships between Galactic Radio Continuum and HαEmission

Full characterization and analysis of a terahertz heterodyne receiver based on a NbN hot electron bolometer

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