Aplicación práctica transceptor BGT24MTR11 : radar Doppler

En los últimos tiempos, los radares han dejado de ser instrumentos utilizados únicamente en aviación, defensa y detección de velocidad. El avance de la tecnología de radiofrecuencia ha permitido la reducción de coste, tamaño y consumo de los componentes radar. Esto ha permitido que cada sea más frecuente el uso del radar en elementos de nuestra vida cotidiana tales como la automoción, la seguridad, la medida de líquidos… Este proyecto se basa en uno de estos nuevos componentes de bajo coste y pequeño tamaño, el transceptor BGT24MTR11. El BGTR24MTR11 integra transmisor, VCO y receptor, los elementos principales para la creación de un radar Doppler en la banda de frecuencia ISM 24-24,25 GHz. A partir de la placa de evaluación de ese transceptor, se aborda el diseño de un prototipo/demostrador de radar Doppler CW en la banda de 24 GHz. Para la generación de frecuencia se utiliza la placa de evaluación del PLL HMC702 y se ha diseñado un PCB a medida cuyas funciones son las de alimentación, programación y amplificación de las señales recibidas por el prototipo. Por último, se comprueba el correcto funcionamiento del prototipo y se verifica su funcionamiento mediante la simulación de dos escenarios de prueba. ABSTRACT. In the recent times, radar systems have changed of being tools used only in aviation, defence and speed detection. Radiofrequency technology improvements have allowed a cost, size and power consumption of the radar components. This is the reason because each time is more frequent the use of radar in elements of our daily life such as automotive, security, liquid measurements… This Project is base don one of this low power and size components, the MMIC transceptor BGT24MTR11. This transceptor integrates the main components needed to make a Doppler radar in the ISM Band (24-24 GHz), the transmitter, the receiver with the low noise amplifier and the VCO. Using the evaluation board of this transceptor, this Project approach the design of a CW Doppler radar prototype/demonstrator in the frequency band of 24 GHz. The frequency generation is based on the use of the HMC702 PLL evaluation board. Moreover, it has been designed a custom PCB whose funcionts are the power supply, programation and amplification of the signals received by the prototype. At the end, the correct operation of the prototype is verified and it is tested simulating two different test scenarios.

The first extrasolar planet discovered with a new-generation high-throughput Doppler instrument

We report the detection of the first extrasolar planet, ET-1 (HD 102195b), using the Exoplanet Tracker (ET), a new-generation Doppler instrument. The planet orbits HD 102195, a young star with solar metallicity that may be part of the local association. The planet imparts radial velocity variability to the star with a semiamplitude of 63.4 ± 2.0 m s^-1 and a period of 4.11 days. The planetary minimum mass (m sin i) is 0.488MJ ± 0.015M_J. The planet was initially detected in the spring of 2005 with the Kitt Peak National Observatory (KPNO) 0.9 m coudé feed telescope. The detection was confirmed by radial velocity observations with the ET at the KPNO 2.1 m telescope and also at the 9 m Hobby-Eberly Telescope (HET) with its High Resolution Spectrograph. This planetary discovery with a 0.9 m telescope around a V = 8.05 magnitude star was made possible by the high throughput of the instrument: 49% measured from the fiber output to the detector. The ET's interferometer-based approach is an effective method for planet detection. In addition, the ET concept is adaptable to multiple-object Doppler observations or very high precision observations with a cross-dispersed echelle spectrograph to separate stellar fringes over a broad wavelength band. In addition to spectroscopic observations of HD 102195, we obtained brightness measurements with one of the automated photometric telescopes at Fairborn Observatory. Those observations reveal that HD 102195 is a spotted variable star with an amplitude of ~0.015 mag and a 12.3 ± 0.3 day period. This is consistent with spectroscopically observed Ca II H and K emission levels and line-broadening measurements but inconsistent with rotational modulation of surface activity as the cause of the radial velocity variability. Our photometric observations rule out transits of the planetary companion.