CBP's Powerpoint template for scientific posters
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Materials and Methods Satellite signal Each NOOA satellites send to the earth two data streams: high resolution digital BPSK and low resolution analog APT. Our instruments are able to receive the analog stream so called FM-FAX modulation, which has a little shift of about 800 Hz from the main transmission frequency, affordable to be demodulated by a normal receiver of lateral band. NOAA satellites carry among other instruments a radiometer (AVHRR) with APT format transmitted by two channels of 7 pulse each (A, 1040 Hz and B, 832 Hz). Sensors (5) on board of satellites are sensitive to different frequency bands. Band 2 (VIS) and 4 (IR) operate during the daylight and 3 (medium IR) and 4 in the night. IR sensors are special useful to monitoring the night cloudiness. Satellite broadband tuner Data transmitted by satellites carry valuable information on the earth atmosphere physical conditions, such temperature, clouds, vapor content, at different altitudes. Important information to characterize geographical sites. The electronic tuner has an audio frequency demodulator in the FM broadband, the output when a FM signal has been tuned, is processed by the computer sound card and decoded by software to display the images. The control module indicated in the Fig. 4, was made using a last generation microcontroller, to set the tuner to work at the satellite frequency shown on a 2x16 LCD display. The commercial I2C format is employed to communicate with the tuner,. The satellite orbits are simulated by software to estimate the approaching time of the satellite. NOAAs satellites send data at 137 Mhz. with a circular polarization, so a proper antenna was built to receive the signal[4]. A commercial broadband turner also was attached to the system to compare the performance of our instrument. In this case, we are constrained to the frequency step defined for the manufacturer. Low Cost NOAA Satellite Signal Receiver for Characterization of Astronomical Sites Gary Flores 1 , Ericson Lopez 1 , Luis Tituaña 1 , Edwin Mena 1 , Daniel Vera 1 , Jairo Armijos 1 , and Enrique Lascano 2 1 Quito Astronomical Observatory of National Polytechnic School, Quito, Ecuador 2 Ecuadorian Space Institute, Quito, Ecuador Introduction To deploy expensive astronomical instrumentation, in order to guarantee its major utility and benefit, the determination of the astronomical features of the geographic site where it will be installed it is essential, both for radio and optical observations. The historical Quito astronomical observatory (founded in 1873) in the Republic of Ecuador, leads the project for the construction of the New National Astronomical Observatory, where large instruments will be installed and will be operating right on the line equator. As part of this project the physical characterization of the possible sites must be performed. On the basis of meteorological data provided by the network of the National Meteorological and Hydrological Institute of Ecuador (INAMHI), a primary estimation of cloudiness and the number of clear night has been done in the 70`s by a Russian team of collaborators to determine the suitable site for astronomical proposes, in the Ecuadorian territory. The results of these preliminary studies conducted to choose the plain of Jerusalem Park, an ecologic reserve, located in Malchingui parish. The major advantage of this plateau is its localization right over the line equator, making of this site, from the point of view of astronomy, very interesting. Nowadays, we decided to carry out further characterization of the Jerusalem site, using satellite signals. For that, two instruments have been used; a broadband satellite tuner designed in our institution the Astronomical Observatory of Quito (OAQ), and a commercial one, able to sense satellite signals in the Satellite broadband tuner. Results Site radio frequency contamination In this work, our radio system was primary used to study the radio spectra in the ranges of 1-200 MHz and 1300- 1400 MHz.The data were taken in the Jerusalem Park, located 35 Km northward from Quito. The free software RTL SDR SCANNER was used to processing the obtained data. The resulting spectra (Figure 5), show great differences between both frequency ranges. In the 1-200 MHz range we observe many spectral features generated by radio and TV stations (electromagnetic contamination). Whereas, in the 1300-1500 MHz range, there are not radio features and the noise has an amplitude about 2 dB/sqrt (Hz). Research Objective The goal of this study was to validate the operation of an satellite signal receiver built at the Quito Observatory, for further characterization of potential astronomical sites. Fig. 7 Yury Gagarin commemorative satellite pictures Discussion The characterization of astronomical sites is of great importance to determine their potential to decide on the investment for the acquisition of astronomical instruments. Recently, it has been demonstrated the utility of satellite databases for these kind of studies [2], supplementing the information obtained from meteorological studies with ground stations and from the local inspection at the site of interest. The electronic system developed at the Quito Astronomical Observatory, is able both receive radio signals emitted by artificial satellite or terrestrial sources. These signals are processed to characterize the site of interest for astronomical observations. At this early stage of site characterization, our broadband tuner has been used to determine the degree of electromagnetic pollution of the potential astronomical site. In later stages the project considered a more thorough study to be conducted on key parameters retrieved from remote sensing techniques and climate diagnostic archives, for astronomical site characterization and for selecting the best sites for hosting large telescopes. References 1. Munoz-Tun´on C., Vernin J., Sarazin M., 2004, Proc. SPIE Vol. 5382, 2nd BackaskogWorkshop on Extremely Large Telescopes. Bellingham, p. 607 2. Soden , B. J. and Bretherton, F. P., 1993, in Upper tropospheric relative humidity from the GOES 6.7 um channel: Method and climatology for July 1987. J. Geophys. Res. 96, 16669. 3. Varela A. M., Bertolin C., Mu˜noz-Tu˜n´on C., Fuensalida J. J., Ortolani S., 2007, Proc. SPIE Vol. 6745, Remote Sensing of Clouds and the Atmosphere XII. SPIE, Bellingham, 674508-1 4. Alvarez Carlo W., 2012, Thesis”Diseño y construcción de una antena Double Cross para recepción de imágenes procedentes de satélites de órbita polar”, Universidad Politécnica de Cataluña. Fig. 5 Radio spectra at Jerusalem Park site: 1-200 MHz range (up) and 1300-1400 MHz (down) Poster # 3.59 Consequently, radio emission from astrophysical sources in the 1300-1500 MHz range, is expected to be not affected by artificial electromagnetic radiation. Whereas radio waves in the 1-200 MHz range might be biased. The 1300-1500 MHz range is used for spectroscopic studies of astrophysical sources since several molecular lines are expected. NOAAS Satellite Maps Since the tuner was implemented (January 2015), the first satellite imagines were received (Fig. 6). There appear clear enough to see the variability of the Earth atmospheric conditions over Ecuador and surrounding region. The resolution of our data (4 km/pixel)) lets us to be able to follow the variability of meteorological parameters over the place of interest. A long term project to study the variability of local conditions over the astronomical site is taking place. In the figure 7 commemorative imagines for the 80th Anniversary of Yuri Gagarin's birthday are shown. These were recently transmitted by Russia from the International Space Station (ISS), and received by QAO tuner.. Fig. 6 QAO Receiver Satellite maps Fig,4 Satellite Anttena Fig 3 .Control module
Transcript of CBP's Powerpoint template for scientific posters
Materials and MethodsSatellite signalEach NOOA satellites send to the earth two data streams: high resolution digital BPSK and low resolution analog APT. Our instruments are able to receive the analog stream so called FM-FAX modulation, which has a little shift of about 800 Hz from the main transmission frequency, affordable to be demodulated by a normal receiver of lateral band. NOAA satellites carry among other instruments a radiometer (AVHRR) with APT format transmitted by two channels of 7 pulse each (A, 1040 Hz and B, 832 Hz). Sensors (5) on board of satellites are sensitive to different frequency bands. Band 2 (VIS) and 4 (IR) operate during the daylight and 3 (medium IR) and 4 in the night. IR sensors are special useful to monitoring the night cloudiness.
Satellite broadband tunerData transmitted by satellites carry valuable information on the earth atmosphere physical conditions, such temperature, clouds, vapor content, at different altitudes. Important information to characterize geographical sites.The electronic tuner has an audio frequency demodulator in the FM broadband, the output when a FM signal has been tuned, is processed by the computer sound card and decoded by software to display the images. The control module indicated in the Fig. 4, was made using a last generation microcontroller, to set the tuner to work at the satellite frequency shown on a 2x16 LCD display. The commercial I2C format is employed to communicate with the tuner,.The satellite orbits are simulated by software to estimate the approaching time of the satellite. NOAAs satellites send data at 137 Mhz. with a circular polarization, so a proper antenna was built to receive the signal[4].A commercial broadband turner also was attached to the system to compare the performance of our instrument. In this case, we are constrained to the frequency step defined for the manufacturer.
Low Cost NOAA Satellite Signal Receiver for Characterization of Astronomical Sites
Gary Flores 1, Ericson Lopez 1, Luis Tituaña 1, Edwin Mena 1, Daniel Vera 1, Jairo Armijos 1, and Enrique Lascano2
1 Quito Astronomical Observatory of National Polytechnic School, Quito, Ecuador 2 Ecuadorian Space Institute, Quito, Ecuador
IntroductionTo deploy expensive astronomical instrumentation, in order to guarantee its major utility and benefit, the determination of the astronomical features of the geographic site where it will be installed it is essential, both for radio and optical observations. The historical Quito astronomical observatory (founded in 1873) in the Republic of Ecuador, leads the project for the construction of the New National Astronomical Observatory, where large instruments will be installed and will be operating right on the line equator. As part of this project the physical characterization of the possible sites must be performed. On the basis of meteorological data provided by the network of the National Meteorological and Hydrological Institute of Ecuador (INAMHI), a primary estimation of cloudiness and the number of clear night has been done in the 70`s by a Russian team of collaborators to determine the suitable site for astronomical proposes, in the Ecuadorian territory. The results of these preliminary studies conducted to choose the plain of Jerusalem Park, an ecologic reserve, located in Malchingui parish. The major advantage of this plateau is its localization right over the line equator, making of this site, from the point of view of astronomy, very interesting.Nowadays, we decided to carry out further characterization of the Jerusalem site, using satellite signals. For that, two instruments have been used; a broadband satellite tuner designed in our institution the Astronomical Observatory of Quito (OAQ), and a commercial one, able to sense satellite signals in the range of 54 MHz to 1.3 GHz. Within this range, there are a number of frequencies used to transmit images and data by educational and meteorological research satellites [1].
Satellite broadband tuner.
ResultsSite radio frequency contaminationIn this work, our radio system was primary used to study the radio spectra in the ranges of 1-200 MHz and 1300-1400 MHz.The data were taken in the Jerusalem Park, located 35 Km northward from Quito. The free software RTL SDR SCANNER was used to processing the obtained data.
The resulting spectra (Figure 5), show great differences between both frequency ranges. In the 1-200 MHz range we observe many spectral features generated by radio and TV stations (electromagnetic contamination). Whereas, in the 1300-1500 MHz range, there are not radio features and the noise has an amplitude about 2 dB/sqrt (Hz).
Research ObjectiveThe goal of this study was to validate the operation of an satellite signal receiver built at the Quito Observatory, for further characterization of potential astronomical sites.
Fig. 7 Yury Gagarin commemorative satellite pictures
DiscussionThe characterization of astronomical sites is of great importance to determine their potential to decide on the investment for the acquisition of astronomical instruments.
Recently, it has been demonstrated the utility of satellite databases for these kind of studies [2], supplementing the information obtained from meteorological studies with ground stations and from the local inspection at the site of interest.
The electronic system developed at the Quito Astronomical Observatory, is able both receive radio signals emitted by artificial satellite or terrestrial sources. These signals are processed to characterize the site of interest for astronomical observations. At this early stage of site characterization, our broadband tuner has been used to determine the degree of electromagnetic pollution of the potential astronomical site. In later stages the project considered a more thorough study to be conducted on key parameters retrieved from remote sensing techniques and climate diagnostic archives, for astronomical site characterization and for selecting the best sites for hosting large telescopes.
References1. Munoz-Tun´on C., Vernin J., Sarazin M., 2004, Proc. SPIE Vol. 5382, 2nd BackaskogWorkshop
on Extremely Large Telescopes. Bellingham, p. 607 2. Soden , B. J. and Bretherton, F. P., 1993, in Upper tropospheric relative humidity from the GOES
6.7 um channel: Method and climatology for July 1987. J. Geophys. Res. 96, 16669.3. Varela A. M., Bertolin C., Mu˜noz-Tu˜n´on C., Fuensalida J. J., Ortolani S., 2007, Proc. SPIE Vol.
6745, Remote Sensing of Clouds and the Atmosphere XII. SPIE, Bellingham, 674508-14. Alvarez Carlo W., 2012, Thesis”Diseño y construcción de una antena Double Cross para
recepción de imágenes procedentes de satélites de órbita polar”, Universidad Politécnica de Cataluña.
Fig. 5 Radio spectra at Jerusalem Park site: 1-200 MHz range (up) and 1300-1400 MHz (down)
Poster # 3.59
Consequently, radio emission from astrophysical sources in the 1300-1500 MHz range, is expected to be not affected by artificial electromagnetic radiation. Whereas radio waves in the 1-200 MHz range might be biased.
The 1300-1500 MHz range is used for spectroscopic studies of astrophysical sources since several molecular lines are expected.
NOAAS Satellite MapsSince the tuner was implemented (January 2015), the first satellite imagines were received (Fig. 6). There appear clear enough to see the variability of the Earth atmospheric conditions over Ecuador and surrounding region. The resolution of our data (4 km/pixel)) lets us to be able to follow the variability of meteorological parameters over the place of interest.
A long term project to study the variability of local conditions over the astronomical site is taking place.
In the figure 7 commemorative imagines for the 80th Anniversary of Yuri Gagarin's birthday are shown. These were recently transmitted by Russia from the International Space Station (ISS), and received by QAO tuner..
Fig. 6 QAO Receiver Satellite maps Fig,4 Satellite Anttena Fig 3 .Control module
