FAST IMPLEMENTATION OF COHERENT DISPERSION COMPENSATION
Section: ASTRONOMICAL INSTRUMENTS AND METHODS
Authors:
1.
Lavochkin Association, JSC
2.
Lavochkin Association, JSC
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDK 53 Физика
UDK 52 Астрономия. Геодезия
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
UDK 52 Астрономия. Геодезия
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
Language:
English
Keywords:
pulsars: general; instrumentation: interferometers; methods: numerical
Abstract (English):
The interstellar medium consists of gas and dust components, almost all of which are completely transparent at centimeter wavelengths. The main cause of radio wave scattering in the interstellar medium is ionized gas—plasma. The behavior of radio waves propagating through such a medium is described by the dispersion equation in a rarefied plasma. The plasma frequency is generally a function of position and time, because it depends on the electron density along the line of sight. The dispersion measure physically represents a column of free electrons between a pulsar and the Earth. Thus, the dispersion measure is a value that determines the delay of radiation pulses of cosmic objects. The delay of radio emission is due to the fact that the refractive index of the plasma depends on the wavelength. Long waves propagate more slowly than short ones, so a signal emitted simultaneously at different frequencies arrives to the observer at long waves later than at short ones. One type of astrophysical objects for which the pulse delay can be measured are pulsars. Since observations are always carried out in a certain wavelength band, the presence of a delay interferes with the study of the fine time structure of pulsar pulses. Without dispersion correction, pulsar observations in a wide frequency band become impossible. The presented work considers the implementation of the coherent dispersion compensation method on a heterogeneous computing structure. Processing in the spectral domain allows the simultaneous search for fast radio bursts (giant pulses), radio pulsars, and refinement of the dispersion measure of the found pulses. It is shown that the proposed implementation on modern computing accelerators allows real-time processing in a wide frequency band that meets modern requirements.
The interstellar medium consists of gas and dust components, almost all of which are completely transparent at centimeter wavelengths. The main cause of radio wave scattering in the interstellar medium is ionized gas—plasma. The behavior of radio waves propagating through such a medium is described by the dispersion equation in a rarefied plasma. The plasma frequency is generally a function of position and time, because it depends on the electron density along the line of sight. The dispersion measure physically represents a column of free electrons between a pulsar and the Earth. Thus, the dispersion measure is a value that determines the delay of radiation pulses of cosmic objects. The delay of radio emission is due to the fact that the refractive index of the plasma depends on the wavelength. Long waves propagate more slowly than short ones, so a signal emitted simultaneously at different frequencies arrives to the observer at long waves later than at short ones. One type of astrophysical objects for which the pulse delay can be measured are pulsars. Since observations are always carried out in a certain wavelength band, the presence of a delay interferes with the study of the fine time structure of pulsar pulses. Without dispersion correction, pulsar observations in a wide frequency band become impossible. The presented work considers the implementation of the coherent dispersion compensation method on a heterogeneous computing structure. Processing in the spectral domain allows the simultaneous search for fast radio bursts (giant pulses), radio pulsars, and refinement of the dispersion measure of the found pulses. It is shown that the proposed implementation on modern computing accelerators allows real-time processing in a wide frequency band that meets modern requirements.
Keywords:
pulsars: general; instrumentation: interferometers; methods: numerical
pulsars: general; instrumentation: interferometers; methods: numerical
1. Eatough R.P., Keane E.F., Lyne A.G., 2009, Monthly Notices of the Royal Astronomical Society, 395, p. 410
2. Girin I.A., Likhachev S.F., Andrianov A.S., et al., 2023, Astronomy and Computing, 45, id. 100754
3. Lorimer D.R. and Kramer M., 2005, Handbook of pulsar astronomy, Cambridge (GB): Cambridge University Press
