Resources for researchers and hints or guides

  • Radar astronomy with the XC crosscorrelators

    The XC crosscorrelators offer various opportunities for research and study.

    One of these opportunities is to turn a radio antenna or a radio antennas array to a single or multichannel radar to study the moon or other NEOs.

    To do this there are two possible configurations: one is to connect a transmitter to the external sampling rate output, the second is to connect the transmitter to the frame end output.

    The transmitter will then emit a pulse each frame end or each sampling pulse synchronized with the readout clock of each antenna input.

    The auto and cross correlation degree will then be relative to the reflection of the transmitted pulses from the object observed.

    Using a single antenna will be very useful to determine the distance of the target of the observations, whilst in interferometer configuration there’s the possibility to draw a detailed map of the surface of the moon, for example or the shape of a smaller NEO like an asteroid or a meteor field during starfalling crossing dates.

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  • Superetherodyne reception with an XC correlator

    The XC correlators offer reception bandwidths up to 200MHz. This feature allows them to obtain spectra and crosscorrelations with greater accuracy in comparison with other products.

    A special feature of the XC correlators is the capability to work in superetherodyne mode by applying an oscillation signal to the external amplifier.

    The superetherodyne mode can be used in radio quantum receivers, photomultiplier tubes, avalanche photodiodes, silicon photomultipliers, nanowire superconducting detectors and any quantum detectors connected to an XC correlator.

    The standard oscillation frequency is set to 400MHz. The intermediate frequency remains the same as their normal bandwidth but the observed frequency is in offset by 400MHz, reaching out 600MHz and 1.67 nanoseconds timing resolutions on products like the XC8.

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  • Hint: observe an exoplanet with an XC correlator using reflex motion

    Exoplanets orbiting around a star are observable in various ways.

    Schematic example of a reflex motion observation

    Typically astronomers use techniques like photometry to determine if a planet transits in front of a star by observing the light curve of a variable star.

    An instant drop-off of the luminosity of the star, and a drop-on of the self, mostly indicate that a planet transits in front of the observed star, expecially if this is observed periodically during an amount of time.

    Another technique is called “reflex motion”:

    This technique is often used on pulsars in radio astronomy. A pulsar emits very strong magnetic emissions in the radio wavelength regime.

    A planet orbiting around a pulsar, when this is in the opposite side of the star (that means the pulsar is in middle way between the planet and Earth), reflects parts of the radiation of the pulsar.

    These reflected radiations arrive delayed to an earth observer.

    This event can be observed by an autocorrelator.

    The XC series crosscorrelators can work in three modes: quantum counters, quantum autocorrelators and quantum crosscorrelators

    An autocorrelator like the XC series cross-correlators in autocorrelation mode can reach temporal precisions down to 5 nanoseconds.

    The XC series crosscorrelators can decrease the temporal resolution time up to 65µs each step, so to coarse precision but acceptable in astronomy.

    Light and radio emissions travel at the speed of light and each 3 nanoseconds travels to around 1m.

    The autocorrelator shows the total emissions during an offset time, so if a planet reflects the light or radio emissions from a star, you can grab the actual perspective distance from the star itself to the planet with an extreme precision.

    This obviously isn’t restricted to radio astronomy: a measurement can be done with optical sensors like photomultiplier tubes, avalanche photodiodes or silicon photomultipliers.

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