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/dokumenty/skolni/diplomka/conclusion.tex
5,3 → 5,7
\sec Possible future improvements
 
Several ADC module imperfections, such as useless separation of FRAME and DCO signal to two connectors, should be mitigated. And this two signals should be merged to one SATA connector. This modification removes one redundant SATA cable between analog to digital converter nest and between computational unit nest.
 
\bibchap
\usebbl/c mybase
 
/dokumenty/skolni/diplomka/description.tex
50,7 → 50,7
 
\secc Frequency synthesis
 
We have used a centralized topology as a basis for frequency synthesis. One precise high-frequency and low-jitter digital oscillator has been used, while other working frequencies have been derived from it by the division of its signal. This central oscillator has a software defined GPS disciplined control loop for frequency stabilization.\fnote{\url{http://wiki.mlab.cz/doku.php?id=en:gpsdo} SDGPSDO design has been developed in parallel to this diploma thesis as a related project, but it is not explicitly required by the diploma thesis.}
We have used a centralized topology as a basis for frequency synthesis. One precise high-frequency and low-jitter digital oscillator has been used \cite[MLAB-GPSDO], while other working frequencies have been derived from it by the division of its signal. This central oscillator has a software defined GPS disciplined control loop for frequency stabilization.\fnote{SDGPSDO design has been developed in parallel to this diploma thesis as a related project, but it is not explicitly required by the diploma thesis.}
We have used methods of frequency monitoring compensation in order to meet modern requirements on radioastronomy equipment which needs precise frequency and phase stability over a wide scale for effective radioastronomy imaging.
Every ADC module will be directly connected to CLKHUB02A module which takes sampling clock signal delivered by FPGA from main local oscillator. This signal should use high quality differential signaling cable -- we should use SATA cable for this purpose.
103,7 → 103,7
* serial LVDS
\enditems
 
Because it uses the smallest number of differential pairs, the choice fell on the serial LVDS format. Small number of differential pairs is an important parameter determining the construction complexity and reliability. \url{http://www.ti.com/lit/pdf/snaa110}
Because it uses the smallest number of differential pairs, the choice fell on the serial LVDS format. Small number of differential pairs is an important parameter determining the construction complexity and reliability\cite[serial-lvds].
 
An ultrasound AFE chip seems to be ideal for this purpose -- the chip has integrated both front-end amplifiers and filters. It has a drawback though - it is incapable of handling differential input signal and has a relatively low dynamic range (as it consists only of 12bit ADC). Because this IO has many ADC channels the scaling is possible only by a factor of 4 receivers (making 8 analogue channels).
 
270,7 → 270,7
\sec Basic interferometer station
 
Interferometry station was selected as most basic setup. We connected the new data acquisition system to two SDRX01B receivers. Block schematic of used setup is shown in image \ref[block-schematic]. Two ground-plane antennas were used and mounted outside of balcony at CTU building at location 50°4'36.102"N, 14°25'4.170"E. Antennas were equipped by LNA01A amplifiers. Coaxial cable length are matched for 5 meters. And antennas were isolated by common mode ferrite bead mounted on cable for minimize signal coupling between antennas. Evaluation system consists SDGPSDO local oscillator subsystem used for tunning local oscillator frequency.
Interferometry station was selected as most basic setup. We connected the new data acquisition system to two SDRX01B receivers. Block schematic of used setup is shown in image \ref[block-schematic]. Two ground-plane antennas were used and mounted outside of balcony at CTU building at location 50$^\circ$4'36.102"N, 14 $^\circ$ 25'4.170" E. Antennas were equipped by LNA01A amplifiers. Coaxial cable length are matched for 5 meters. And antennas were isolated by common mode ferrite bead mounted on cable for minimize signal coupling between antennas. Evaluation system consists SDGPSDO local oscillator subsystem used for tuning local oscillator frequency.
 
\midinsert
\clabel[block-schematic]{Receiver block schematic}
309,7 → 309,7
In the beginning of the project, a custom design of FPGA interface board had been considered. This FPGA board should include PCI express interface and should sell at lower price than trial design. It should be compatible with MLAB which is further backward compatible with the existing or improved design of ADC modules. For a connection of this board to another adapter board with PCIe we expect a use of a host interface.
Thunderbolt technology standard was expected to be used in this PC to PCIe -> FPGA module. Thunderbolt chips are currently available on the market for reasonable prices. However, a problem lies in the accessibility to their specifications, as they are only available for licensed users and Intel has a mass market oriented licensing policy, that makes this technology inaccessible for low quantity production. As a consequence, an external PCI Express cabling and expansion slots should be considered as a better solution.
 
However, these systems and cables are still very expensive. Take (http://www.opalkelly.com/products/xem6110/) as an example, with its price tag reaching 995 USD at time of writing of thesis.
However, these systems and cables are still very expensive. Take Opal Kelly XEM6110 \cite[fpga-pcie] as an example, with its price tag reaching 995 USD at time of writing of thesis.
Therefore, a better solution probably needs to be found.
 
\sec Parralella board computer
/dokumenty/skolni/diplomka/diplomka.pdf
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svn:mime-type = application/octet-stream
/dokumenty/skolni/diplomka/diplomka.ref
8,7 → 8,6
\Xpage{1}
\Xchap{1}{Introduction }{1}
\Xsec{1.1}{Current radioastronomy problems }{1}
\Xfnote
\Xpage{2}
\Xsec{1.2}{Modern Radio astronomy receiver }{2}
\Xfnote
25,75 → 24,89
\Xsecc{1.4.1}{Custom digitalization system }{4}
\Xsecc{1.4.2}{Modular digitalization systems }{4}
\Xpage{5}
\Xchap{2}{Trial design }{5}
\Xsec{2.1}{Required parameters }{5}
\Xsec{2.2}{Sampling frequency }{5}
\Xsec{2.3}{System scalability }{5}
\Xpage{6}
\Xchap{2}{Trial design }{6}
\Xsec{2.1}{Required parameters }{6}
\Xsec{2.2}{Sampling frequency }{6}
\Xsec{2.3}{System scalability }{6}
\Xsecc{2.3.1}{Differential signaling }{6}
\Xsecc{2.3.2}{Phase matching }{6}
\Xsec{2.4}{System description }{6}
\Xsecc{2.4.1}{Frequency synthesis }{6}
\Xfnote
\Xpage{7}
\Xsecc{2.3.1}{Differential signaling }{7}
\Xsecc{2.3.2}{Phase matching }{7}
\Xsec{2.4}{System description }{7}
\Xsecc{2.4.1}{Frequency synthesis }{7}
\Xfnote
\Xsecc{2.4.2}{Signal cable connectors }{7}
\Xsecc{2.4.3}{Signal integrity requirements \immediate \write 16{l.99 OPmac WARNING: duplicated label [diff-signaling], ignored.}\ignorespaces }{7}
\Xlabel{diff-signaling}{2.4.4}
\Xsecc{2.4.4}{ADC modules design }{7}
\Xsecc{2.4.5}{ADC selection }{7}
\Xpage{8}
\Xsecc{2.4.2}{Signal cable connectors }{8}
\Xsecc{2.4.3}{Signal integrity requirements \immediate \write 16{l.99 OPmac WARNING: duplicated label [diff-signaling], ignored.}\ignorespaces }{8}
\Xlabel{diff-signaling}{2.4.4}
\Xsecc{2.4.4}{ADC modules design }{8}
\Xsecc{2.4.5}{ADC selection }{8}
\Xpage{9}
\Xfig{img-miniSAS-cable}{2.1}{Used miniSAS cable}
\Xlabel{img-miniSAS-cable}{2.1}
\Xpage{10}
\Xpage{9}
\Xtab{ADC-types}{2.1}{Available ADC types}
\Xlabel{ADC-types}{2.1}
\Xfig{1-line-out}{2.2}{Single line ADC output signals}
\Xlabel{1-line-out}{2.2}
\Xpage{10}
\Xsecc{2.4.6}{ADC modules interface }{10}
\Xpage{11}
\Xsecc{2.4.6}{ADC modules interface }{11}
\Xpage{12}
\Xfig{VITA57-regions}{2.4}{VITA57 board geometry}
\Xlabel{VITA57-regions}{2.4}
\Xsecc{2.4.7}{Output data format }{12}
\Xsec{2.5}{Achieved parameters }{12}
\Xsecc{2.5.1}{Data reading and recording }{12}
\Xsecc{2.5.2}{ADC module parameters }{12}
\Xsecc{2.4.7}{Output data format }{11}
\Xsec{2.5}{Achieved parameters }{11}
\Xsecc{2.5.1}{Data reading and recording }{11}
\Xsecc{2.5.2}{ADC module parameters }{11}
\Xpage{12}
\Xpage{13}
\Xpage{14}
\Xfig{ADC1-FFT}{2.7}{ADC1 sine test FFT}
\Xlabel{ADC1-FFT}{2.7}
\Xpage{15}
\Xpage{14}
\Xfig{ADC2-FFT}{2.8}{ADC2 sine test FFT}
\Xlabel{ADC2-FFT}{2.8}
\Xpage{16}
\Xchap{3}{Example of usage }{16}
\Xsec{3.1}{Basic interferometer station }{16}
\Xpage{15}
\Xchap{3}{Example of usage }{15}
\Xsec{3.1}{Basic interferometer station }{15}
\Xfig{block-schematic}{3.1}{Receiver block schematic}
\Xlabel{block-schematic}{3.1}
\Xpage{17}
\Xpage{16}
\Xfig{meteor-reflection}{3.2}{Meteor reflection}
\Xlabel{meteor-reflection}{3.2}
\Xfig{phase-phase-difference}{3.3}{Phase difference}
\Xlabel{phase-phase-difference}{3.3}
\Xpage{17}
\Xchap{4}{Proposed final system }{17}
\Xsec{4.1}{Custom design of FPGA board }{17}
\Xsec{4.2}{Parralella board computer }{17}
\Xsec{4.3}{GPU based computational system }{17}
\Xpage{18}
\Xchap{4}{Proposed final system }{18}
\Xsec{4.1}{Custom design of FPGA board }{18}
\Xsec{4.2}{Parralella board computer }{18}
\Xsec{4.3}{GPU based computational system }{18}
\Xpage{19}
\Xfig{img-NVIDIA-K1}{4.1}{NVIDIA Jetson TK1 Development Kit}
\Xlabel{img-NVIDIA-K1}{4.1}
\Xpage{19}
\Xchap{5}{Conclusion }{19}
\Xsec{5.1}{Possible future improvements }{19}
\Xbib{radio-astronomy-frequency}{1}
\Xbib{spectrum-observatory}{2}
\Xbib{lofar}{3}
\Xbib{astron-devices}{4}
\Xbib{casper-project}{5}
\Xpage{20}
\Xchap{5}{Conclusion }{20}
\Xsec{5.1}{Possible future improvements }{20}
\Xchap{!1}{References}{20}
\Xbib{casper-paper}{6}
\Xbib{Z-DOK-connectors}{7}
\Xbib{amateur-fringes}{8}
\Xbib{amateur-sdr}{9}
\Xbib{MLAB-GPSDO}{10}
\Xbib{serial-lvds}{11}
\Xbib{fpga-pcie}{12}
\Xpage{21}
\Xchap{A}{Circuit diagram of ADCdual01A module }{21}
\Xpage{22}
\Xchap{B}{Circuit diagram of FMC2DIFF module }{22}
\Xpage{23}
\Xchap{A}{Circuit diagram of ADCdual01A module }{23}
\Xpage{24}
\Xchap{B}{Circuit diagram of FMC2DIFF module }{24}
\Xpage{25}
\Xpage{26}
\Xpage{27}
\Xchap{C}{Content of enclosed CD }{27}
\Xpage{28}
\Xpage{29}
\Xchap{C}{Content of enclosed CD }{29}
/dokumenty/skolni/diplomka/img/ADC_single_line_output.png
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/dokumenty/skolni/diplomka/introduction.log
1,4 → 1,4
This is pdfTeX, Version 3.1415926-2.5-1.40.14 (TeX Live 2013/Debian) (format=pdfcsplain 2014.4.28) 6 MAY 2014 21:32
This is pdfTeX, Version 3.1415926-2.5-1.40.14 (TeX Live 2013/Debian) (format=pdfcsplain 2014.4.28) 6 MAY 2014 23:39
entering extended mode
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l.73 \caption
l.71 \caption
/t Standard bit depths of ADC and its theoretical dynamic range.
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l.79 \url
{http://observatory.microsoftspectrum.com}
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Current status of receivers digitalization units
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Custom digitalization system
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l.94 ...m developed by Astron in Netherlands. \url
l.92 ...m developed by Astron in Netherlands. \url
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l.98 ...many similarly sophisticated devices. \url
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Modular digitalization systems
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l.102 ...atively high pricing (around 40 USD) \url
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/dokumenty/skolni/diplomka/introduction.tex
6,13 → 6,13
 
However, it is due to these artificial signals, that the current radioastronomy faces a disturbing problem. The problem arises from the fact, that there are so many terrestrial transmitters currently active and all of them are sources of a dense signal mixture which can cause trouble not only to radioastronomers.
 
As a consequence, there already exist effort to control the radiofrequency spectrum. As result of attempts to control the radiofrequency spectrum, the frequency allocation table was created. \fnote{\url{http://www.ukaranet.org.uk/basics/frequency_allocation.htm}} Radio-frequency allocation table table contains special bands allocated to radioastronomy use. However, for many reasons these bands are not clean enough to be used directly in radioastronomy observations. As a result, we cannot work in the same way as had the radioastronomers in the very beginnings of radioastronomy. Many experiments, namely Cosmic microwave background detection or pulsar detection, cannot be nowadays realised in their original forms with satisfactory results.
As a consequence, there already exist effort to control the radiofrequency spectrum. As result of attempts to control the radiofrequency spectrum, the frequency allocation table was created \cite[radio-astronomy-frequency]. Radio-frequency allocation table table contains special bands allocated to radioastronomy use. However, for many reasons these bands are not clean enough to be used directly in radioastronomy observations. As a result, we cannot work in the same way as had the radioastronomers in the very beginnings of radioastronomy. Many experiments, namely Cosmic microwave background detection or pulsar detection, cannot be nowadays realised in their original forms with satisfactory results.
 
Supporting evidence of such effect is RadioJOVE project. NASA engineers who originally created the RadioJOVE project had a great idea. The RadioJOVE project brought an opportunity for creating a publicly available, cheap radioastronomy receiver. However, they used an old-fashioned construction design which, on one hand, can operate in harsh environments like deserts, but on the other it simply did not meet the criteria that would make it possible to be used in modern civilisation, as we know it in Europe.
The source of its dysfunction is a presence of strong radiofrequency interferences. These interferences are orders of magnitude stronger than Jupiter decametric emissions, whose detection was the main aim of the RadioJOVE project.
From what we have already seen in the light pollution mitigation pursuit, there is only a small chance to radically improve the situation in radiofrequency spectrum.
 
The only way to overcome this problem is to search for new methods of radioastronomy observations. New methods which allows us to work without completely clear radiofrequency bands and which allow us to see the surrounding universe even despite the existence of man-made radiofrequency interference mixture. One solution is to use already known natural radio frequency signals parameters. Natural signals usually have different signal properties than local interference. Natural objects do not have problems with transmission in bandwidths of tens of megahertz in sub 100 MHz bands. These objects are usually far away and the same signal could be received at almost half of the Earth globe without any significant differences. On the other hand, it is obvious that signals with such parameters have some drawbacks, namely in the reception power. The reception power of radioastronomical object is 1e9 smaller than signal power received from a typical broadband radio transmitter.
The only way to overcome this problem is to search for new methods of radioastronomy observations. New methods which allows us to work without completely clear radiofrequency bands and which allow us to see the surrounding universe even despite the existence of man-made radiofrequency interference mixture. One solution is to use already known natural radio frequency signals parameters. Natural signals usually have different signal properties than local interference. Natural objects do not have problems with transmission in bandwidths of tens of megahertz in sub 100 MHz bands. These objects are usually far away and the same signal could be received at almost half of the Earth globe without any significant differences. On the other hand, it is obvious that signals with such parameters have some drawbacks, namely in the reception power. The reception power of radioastronomical object is $1*10^9$ smaller than signal power received from a typical broadband radio transmitter.
 
From the above mentioned facts concerning the natural radio signals we can conclude that modern requirements imposed on a radioastronomy receiver are completely different from the requirements existing back in the history. Radioastronomy is no longer limited by an access to electronic components, today it is rather limited by the everywhere presence of electronic.
73,9 → 73,8
 
% dopsat cast o minimalnim dynamickem rozsahu ADC.
 
If we look at actual spectrum occupancy in Europe (measured in power spectral density) we see that signal dynamic range in spectra
\url{http://observatory.microsoftspectrum.com}
easily reaches more than 80 dB above natural noise levels. If we don't want to deal with receiver saturation or poor sensitivity we need a receiver and digitalization unit which has comparable dynamical range of with received signals. This imply use of least 14 bit ADC without any spare of range.
If we look at actual spectrum occupancy in Europe (measured in power spectral density) we see that signal dynamic range in spectra
easily reaches more than 80 dB above natural noise levels \cite[spectrum-observatory]. If we don't want to deal with receiver saturation or poor sensitivity we need a receiver and digitalization unit which has comparable dynamical range of with received signals. This imply use of least 14 bit ADC without any spare of range.
 
 
\secc Bandwidth
84,22 → 83,22
 
\sec Current status of receivers digitalization units
 
Only few digitalization systems dedicated for radioastronomy exists nowadays. Currently existing systems use either custom design of the entire receiver or they are constructed from commercially available components. The attempts to use open-source solutions in the radioastronomical field are still rather scarce.
Only few digitalization systems dedicated for radioastronomy currently exists. Currently existing systems uses either custom design of whole receiver or they are constructed from commercially available components. Open-source principle attempts are very rare in radioastronomy field.
 
\secc Custom digitalization system
 
Custom designs usually use non-recurring engineering techniques for the development of specific solutions for observational projects. Thus the costs of these instruments are mostly very high as long as they are not produced in larger quantities. A typical example of an instrument developed and manufactured in one piece with enormous founding drawn is Arecibo ALFA survey multi beam feed Array.
Another example illustrating the opposite of custom receiver and digitalization unit design is LOFAR system developed by Astron in Netherlands. \url{http://arxiv.org/abs/1305.3550}
Custom designs usually uses non-recurring engineering for development specific solution for observation project thus costs of this instruments are very high if developed instrument are not reproduced many times. Typical example of instrument developed and manufactured in one piece with enormous founding resources draws is Arecibo ALFA survey multi beam feed Array.
Another opposite example for custom receiver and digitalization unit design is LOFAR system developed by Astron in Netherlands \cite[lofar].
LOFAR is an innovative radioastronomical system which uses the phased antenna array approach in extensive scale with thousands (around $2*10^4$) of antennas manufactured an deployed on the field. The centre of LOFAR system is situated in Netherlands and peripheral antennas and connection network are extended to other European countries.
LOFAR is innovative radioastronomy system which uses the phased antenna array approach in enormous scale and thousands (around $2*10^4$) of antennas are manufactured an deployed on field. The centrer of LOFAR system is situated in Netherlands and peripheral antennas and connection network are extended to other European countries.
 
LOFAR project must use low cost hardware due to its large scale. Special construction techniques are used to keep the overall project budget at an acceptable level (take the specially designed polystyrene supporting blocks for HBA antennas as an example). Many of the components used are manufactured in mass scale for other than scientific purposes. LBA antennas masts are made of standard PVC plastic waste pipes and LOFAR uses low cost direct sampling receivers. The whole project has been designed by Netherlands Institute for Radio Astronomy, which produces many similarly sophisticated devices. \url{http://www.astron.nl/other/desp/competences_DesApp.htm}
LOFAR project must use low cost hardware due to systems scale. Special construction techniques are used to keep overall project budget at acceptable levels (specially designed polystyrene supporting blocks for HBA antennas for example). Many of used components are manufactured in mass scale for other than scientific use LBA antennas masts are made from standard PVC plastic waste pipes and LOFAR uses low cost direct sampling receiver. Whole project has been designed by Netherlands Institute for Radio Astronomy, which produces many similarly sophisticated devices\cite[astron-devices].
 
\secc Modular digitalization systems
Due to the cost restrictions in science and astronomy instruments' development, a reuse of engineering work turns out to be very useful. There is only one modular digitalization and data processing system currently in existence - it is called CASPER and it is under development at Berkley university since around 2005. \url{https://casper.berkeley.edu/wiki/Main_Page} as CASPER's designers an engineers remarkably noticed a lack of such hardware in radioastronomy. Their ideas are summarised in the following paper \url{https://casper.berkeley.edu/papers/200509URSI.pdf}. Unfortunately they use proprietary connector standard and technology and develop modular system based purely on Tyco Z-DOK+ connectors family. Z-DOK connectors are high quality differential pairs connectors, but price of these connectors (around 40 USD) is comparable with the cost of one ADC channel in the design described in our thesis. \url{http://www.digikey.com/product-detail/en/6367550-5/6367550-5-ND/2259130}.
Due to cost restrictions in science and astronomy instruments development, an reuse of engineering work should be useful. One modular digitalization and data processing system currently exit. It is being developed at Berkley\cite[casper-project]. CASPER is in development from around 2005. CASPER's designers an engineers remarkably noticed a lack of such hardware in radioastronomy science, theirs ideas are summarised in paper \cite[casper-paper]. Unfortunately they use proprietary connector standard and technology and develops modular system based purely on Tyco Z-DOK+ connectors family. Z-DOK connectors have relatively high pricing (around 40 USD) \cite[Z-DOK-connectors]. Z-DOK connectors are high quality differential pairs connectors, but price of these connectors is comparable with value of one ADC channel in our design described in following part of document.
 
In contrast to professional astronomers which use proprietary digitalization units, amateur radioastronomers currently use multichannel sound cards \url{http://fringes.org/} or self designed digitalisation units. Devices constructed by amateurs are usually non-reproducible \url{http://wwwhome.cs.utwente.nl/~ptdeboer/ham/sdr/} . It is evident that current radioastronomy lacks a proper hardware which could be used by both communities - professionals and amateurs. Optimal solution for this situation would be an open-source hardware.
In opposite to professional astronomers which uses proprietary digitalization units, amateur radioastronomers currently uses multichannel sound cards \cite[amateur-fringes] or self designed digitalisation units. Devices constructed by amateurs are usually non reproducible \cite[amateur-sdr] . It is evident that current radioastronomy lacks of proper hardware which could be used on both communities - professionals and amateurs. Optimal solution for this situation should be open-source hardware.
 
 
 
/dokumenty/skolni/diplomka/mybase.bbl
1,181 → 1,95
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9,294 → 9,114
URLDATE= {2012-12-13},
}
 
@MISC{ CVUT-FEL:smernice,
AUTHOR = {ČVUT FEL},
TITLE = {Směrnice děkana pro magisterské státní
závěrečné zkoušky na {ČVUT FEL}},
@MISC{spectrum-observatory,
AUTHOR = {Microsoft},
TITLE = {Microsoft Spectrum Observatory},
YEAR = {2012},
NOTE = {\url{http://www.fel.cvut.cz/rozvoj/smerniceMSZZ.html}},
URLDATE= {2012-12-13},
NOTE = {\url{http://observatory.microsoftspectrum.com/}},
URLDATE= {2014-5-3},
}
 
@MISC{ CSN:016910,
AUTHOR = {{ČSN} 01 6910},
TITLE = {Úprava písemností zpracovaných textovými editory},
YEAR = {2007},
MONTH = apr,
NOTE = {\url{http://typotypo.wz.cz/csn016910.pdf}},
@MISC{radio-astronomy-frequency,
AUTHOR = {UKARANet},
TITLE = {RADIO ASTRONOMY FREQUENCY ALLOCATIONS},
YEAR = {2014},
MONTH = May,
NOTE = {\url{http://www.ukaranet.org.uk/basics/frequency_allocation.htm}},
}
 
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}
 
@MISC{ bibtex,
AUTHOR = {Feder, Alexander},
TITLE = {{Bib\TeX}},
NOTE = {\url{http://www.bibtex.org/}},
URLDATE= {2012-12-13},
@MANUAL{lofar,
AUTHOR = {M. P. van Haarlem, M. W. Wise, A. W. Gunst, G. Heald, J. P. McKean, J. W. T. Hessels, A. G. de Bruyn, R. Nijboer, J. Swinbank, R. Fallows, M. Brentjens, A. Nelles, R. Beck, H. Falcke, R. Fender, J. Hörandel, L. V. E. Koopmans, G. Mann, G. Miley, H. Röttgering, B. W. Stappers, R. A. M. J. Wijers, S. Zaroubi, M. van den Akker, A. Alexov, J. Anderson, K. Anderson, A. van Ardenne, M. Arts, A. Asgekar, I. M. Avruch, F. Batejat, L. Bähren, M. E. Bell, M. R. Bell, I. van Bemmel, P. Bennema, M. J. Bentum, G. Bernardi, P. Best, L. Bîrzan, A. Bonafede, A.-J. Boonstra, R. Braun, J. Bregman, F. Breitling, R. H. van de Brink, J. Broderick, P. C. Broekema, W. N. Brouw, M. Brüggen, H. R. Butcher, W. van Cappellen, B. Ciardi, T. Coenen, J. Conway, A. Coolen, A. Corstanje, S. Damstra,
O. Davies, A. T. Deller, R.-J. Dettmar, G. van Diepen, K. Dijkstra, P. Donker, A. Doorduin, J. Dromer, M. Drost, A. van Duin, J. Eislöffel, J. van Enst, C. Ferrari, W. Frieswijk, H. Gankema, M. A. Garrett, F. de Gasperin, M. Gerbers, E. de Geus, J.-M. Grießmeier, T. Grit, P. Gruppen, J. P. Hamaker, T. Hassall, M. Hoeft, H. Holties, A. Horneffer, A. van der Horst, A. van Houwelingen, A. Huijgen, M. Iacobelli, H. Intema, N. Jackson, V. Jelic, A. de Jong, E. Juette, D. Kant, A. Karastergiou, A. Koers, H. Kollen, V. I. Kondratiev, E. Kooistra, Y. Koopman, A. Koster, M. Kuniyoshi, M. Kramer, G. Kuper, P. Lambropoulos, C. Law, J. van Leeuwen, J. Lemaitre, M. Loose, P. Maat, G. Macario, S. Markoff, J. Masters, D. McKay-Bukowski, H. Meijering, H. Meulman, M. Mevius, E. Middelberg, R. Millenaar, J. C. A. Miller-Jones, R. N. Mohan, J. D. Mol, J. Morawietz, R. Morganti, D. D. Mulcahy, E. Mulder, H. Munk, L. Nieuwenhuis, R. van Nieuwpoort, J. E. Noordam, M. Norden, A. Noutsos, A. R. Offringa, H. Olofsson, A. Omar, E. Orrú, R. Overeem, H. Paas, M. Pandey-Pommier, V. N. Pandey, R. Pizzo, A. Polatidis, D. Rafferty, S. Rawlings, W. Reich, J.-P. de Reijer, J. Reitsma, A. Renting, P. Riemers, E. Rol, J. W. Romein, J. Roosjen, M. Ruiter, A. Scaife, K. van der Schaaf, B. Scheers, P. Schellart, A. Schoenmakers, G. Schoonderbeek, M. Serylak, A. Shulevski, J. Sluman, O. Smirnov, C. Sobey, H. Spreeuw, M. Steinmetz, C. G. M. Sterks, H.-J. Stiepel, K. Stuurwold, M. Tagger, Y. Tang, C. Tasse, I. Thomas, S. Thoudam, M. C. Toribio, B. van der Tol, O. Usov, M. van Veelen, A.-J. van der Veen, S. ter Veen, J. P. W. Verbiest, R. Vermeulen, N. Vermaas, C. Vocks, C. Vogt, M. de Vos, E. van der Wal, R. van Weeren, H. Weggemans, P. Weltevrede, S. White, S. J. Wijnholds, T. Wilhelmsson, O. Wucknitz, S. Yatawatta, P. Zarka, A. Zensus, J. van Zwieten},
TITLE = { LOFAR: The LOw-Frequency ARray},
YEAR = {2013},
MONTH = May,
NOTE = {\url{http://arxiv.org/abs/1305.3550}},
}
 
@MISC{ csbibtex,
AUTHOR = {Novotný, Petr},
TITLE = {{CSBib\TeX}},
YEAR = {1994},
NOTE = {\url{http://math.feld.cvut.cz/olsak/cstex/csbibtex.txt}},
@MISC{astron-devices,
AUTHOR = {Astron},
TITLE = {Design and development},
YEAR = {2014},
MONTH = May,
NOTE = {\url{http://www.astron.nl/other/desp/competences_DesApp.htm}},
URLDATE= {2014-5-3},
}
 
@MISC{ bibtex8,
AUTHOR = {Kempson, Niel and Aguilar-Sierra, Alejandro},
TITLE = {{Bib\TeX 8}},
YEAR = {1996},
NOTE = {\url{http://www.ctan.org/tex-archive/biblio/bibtex/8-bit}},
URLDATE= {2012-12-13},
@MISC{casper-project,
AUTHOR = {Univeristy of California Berkeley},
TITLE = {Center for Astronomy Signal Processing and Electronics Research},
YEAR = {2014},
MONTH = May,
NOTE = {\url{https://casper.berkeley.edu/}},
URLDATE= {2014-5-3},
}
 
@MISC{ biber,
AUTHOR = {Charette, Fran\c{c}ois and Kime, Philip},
TITLE = {{Biber}},
NOTE = {\url{http://biblatex-biber.sourceforge.net/}},
URLDATE= {2012-12-13},
@MISC{casper-paper,
AUTHOR = {Univeristy of California Berkeley},
TITLE = {A new Approach to Radioastronomy Signal Processing},
YEAR = {2014},
MONTH = May,
NOTE = {\url{https://casper.berkeley.edu/papers/200509URSI.pdf}},
URLDATE= {2014-5-3},
}
 
@MISC{ biblatex,
AUTHOR = {Lehman, Philipp},
TITLE = {{Bib\LaTeX}},
YEAR = {2012},
NOTE = {\url{http://ftp.cstug.cz/pub/tex/CTAN/help/Catalogue/entries/biblatex.html}},
URLDATE= {2012-12-13},
@MISC{Z-DOK-connectors,
AUTHOR = {Digikey},
TITLE = {6367550-5-ND},
YEAR = {2014},
MONTH = May,
NOTE = {\url{http://www.digikey.com/product-detail/en/6367550-5/6367550-5-ND/2259130}},
URLDATE= {2014-5-3},
}
 
@MANUAL{ Lamport87,
AUTHOR = {Lamport, Leslie},
TITLE = {{MakeIndex}: An Index Processor For \LaTeX{}},
YEAR = {1987},
MONTH = feb,
}
 
@MANUAL{ Chen86,
AUTHOR = {Chen, Pehong},
TITLE = {Index Preparation and Processing},
YEAR = {1986},
}
 
@MANUAL{ Wagner92,
AUTHOR = {Wagner, Zdeněk},
TITLE = {{CsIndex} v.2.11 czech/slovak implementation of -- česká slovenská implementace programu {MakeIndex}},
YEAR = {1992},
MONTH = aug,
NOTE = {\url{http://mi21.vsb.cz/sites/mi21.vsb.cz/files/csindex.pdf}},
}
 
@MISC{ xindy,
AUTHOR = {Schrod, Joachim},
TITLE = {{Xindy}},
NOTE = {\url{http://xindy.sourceforge.net/}},
URLDATE= {2012-12-13},
}
 
@MISC{ CVUT-FEL-rocenka11,
AUTHOR = {ČVUT v~Praze, FEL},
TITLE = {Výroční zpráva za rok 2011},
YEAR = {2012},
NOTE = {\url{http://www.fel.cvut.cz/rozvoj/vyrocni-zprava2011.pdf}},
}
 
@MANUAL{ longtable,
AUTHOR = {Carlisle, David},
TITLE = {The longtable package},
@MISC{amateur-fringes,
AUTHOR = {Fringe Dwellers},
TITLE = {Simple Interferometer},
YEAR = {2004},
MONTH = feb,
NOTE = {\url{http://mirrors.ctan.org/macros/latex/required/tools/longtable.pdf}},
MONTH = May,
NOTE = {\url{http://fringes.org/}},
URLDATE= {2014-5-3},
}
 
@MANUAL{ epslatex,
AUTHOR = {Reckdahl, Keith},
TITLE = {Using Imported Graphics in {\LaTeX} and {pdf\LaTeX}},
YEAR = {2006},
MONTH = jan,
NOTE = {\url{http://mirrors.ctan.org/info/epslatex/english/epslatex.pdf}},
}
 
@MANUAL{ amsmath,
AUTHOR = {American Mathematical Society},
TITLE = {User's Guide for the amsmath Package},
YEAR = {1999},
MONTH = dec,
NOTE = {\url{ftp://ftp.ams.org/pub/tex/doc/amsmath/amsldoc.pdf}},
@MISC{amateur-sdr,
AUTHOR = {Pieter-Tjerk de Boer},
TITLE = {PA3FWM's software defined radio page},
YEAR = {2013},
MONTH = Apr,
NOTE = {\url{http://wwwhome.cs.utwente.nl/~ptdeboer/ham/sdr/}},
URLDATE= {2014-5-3},
}
 
@MISC{ texniccenter,
TITLE = {{\TeX{}nicCenter}},
NOTE = {\url{http://www.texniccenter.org/}},
URLDATE= {2012-12-13},
KEY = {texniccenter},
@MISC{MLAB-GPSDO,
AUTHOR = {J. Kakona, M. Kakona},
TITLE = {Software Defined GPS disciplined oscillator - GPSDO01A},
YEAR = {2014},
MONTH = Jan,
NOTE = {\url{http://wiki.mlab.cz/doku.php?id=en:gpsdo}},
URLDATE= {2014-5-3},
}
 
@MISC{ xemacs,
TITLE = {{XEmacs}},
NOTE = {\url{http://www.xemacs.org/}},
URLDATE= {2012-12-13},
KEY = {xemac},
@MISC{serial-lvds,
AUTHOR = {Robert LeBoeuf},
TITLE = {Data Converter Serial LVDS Interface Improves Board Routing, SNAA110},
YEAR = {2011},
MONTH = Jan,
NOTE = {\url{http://www.ti.com/lit/wp/snaa110/snaa110.pdf}},
URLDATE= {2014-5-3},
}
 
@MISC{ texworks,
TITLE = {{\TeX{}works}},
NOTE = {\url{http://www.tug.org/texworks/}},
URLDATE= {2012-12-13},
KEY = {texworks},
@MISC{fpga-pcie,
AUTHOR = {Opal Kelly},
TITLE = {Opal Kelly XEM6110},
YEAR = {2011},
MONTH = Jan,
NOTE = {\url{http://www.opalkelly.com/products/xem6110/}},
URLDATE= {2014-5-3},
}
 
@BOOK{ Rybicka02,
AUTHOR = { Rybička, Jiří },
TITLE = { {\LaTeX} pro začátečníky },
PUBLISHER = { Konvoj },
YEAR = { 2002 },
KEYWORDS = { LaTeX, TeX, document preparation },
ISBN = {80-7302-049-1},
EDITION = {Edition 3},
}
 
@BOOK{ Kopka04,
AUTHOR = {Kopka, Helmut and Daly, Patrick W.},
TITLE = {Guide to {\LaTeX}},
PUBLISHER = {Addison-Wesley},
YEAR = {2003},
MONTH = nov,
EDITION = {Edition 4},
PAGES = {624},
ISBN = {0-321-17385-6},
}
 
@BOOK{ jemny,
AUTHOR = {Michael Doob},
TITLE = {Jemný úvod do \TeX{}u},
PUBLISHER = {CSTUG},
YEAR = {1997},
NOTE = {\url{ftp://math.feld.cvut.cz/pub/cstex/doc/jemny.tar.gz}},
}
@BOOK{ latexcompanion2nd,
AUTHOR = {Frank Mittelbach and Michel Goossens and Johannes Braams
and David Carlisle and Chris Rowley},
TITLE = {{\LaTeX} Companion},
PUBLISHER = {Addison-Wesley},
YEAR = {2004},
MONTH = apr,
EDITION = {Edition 2},
PAGES = {1120},
ISBN = {0-201-36299-6},
}
 
@BOOK{ latexgraphicscompanion2nd,
AUTHOR = {Michel Goossens and Frank Mittelbach and Sebastian Rahtz
and Denis Roegel and Herbert Voss},
TITLE = {{\LaTeX} Graphics Companion},
PUBLISHER = {Addison-Wesley},
YEAR = {2007},
MONTH = aug,
EDITION = {Edition 2},
PAGES = {976},
ISBN = {0-321-50892-0},
}
 
@MANUAL{ Oetiker11,
TITLE = {The not so short introduction to {\LaTeX2e}},
AUTHOR = {Tobias Oetiker and Hubert Partl and Irene Hyna and Elisabeth Schlegl},
YEAR = {2011},
NOTE= {\url{http://tobi.oetiker.ch/lshort/lshort.pdf}},
}
 
@MANUAL{ nestrucLaTeX,
TITLE = {Nepříliš stručný úvod do systému {\LaTeX}},
AUTHOR = {Tobias Oetiker and Hubert Partl and Irene Hyna
and Elisabeth Schlegl and Michal Kočer and Pavel Sýkora},
YEAR = {1998},
NOTE= {\url{www.penguin.cz/~kocer/texty/lshort2e/lshort2e-cz.pdf}},
}
 
@BOOK{ texbook,
AUTHOR = { Knuth, Donald Ervin },
TITLE = { Computer \& Typesetting A: The~{\TeX}book },
PUBLISHER = { Addison Wesley },
YEAR = { 1994 },
}
 
@BOOK{ tbn,
AUTHOR = {Olšák, Petr},
TITLE = {{\TeX}book naruby},
PUBLISHER = {Konvoj Brno},
YEAR = {2001},
ISBN = {80-7302-007-6},
NOTE = {\url{http://petr.olsak.net/tbn.html}},
}
 
@BOOK{ tst,
AUTHOR = {Olšák, Petr},
TITLE = {Typografický systém {\TeX}},
PUBLISHER = {Konvoj Brno},
YEAR = {1998},
NOTE = {\url{http://petr.olsak.net/tst.html}},
}
 
@BOOK{ prvni,
AUTHOR = {Olšák, Petr},
TITLE = {První setkání s \TeX{}em},
PUBLISHER = {Konvoj Brno},
YEAR = {1999, 2012},
NOTE = {\url{http://petr.olsak.net/ftp/cstex/doc/prvni.pdf}},
}
 
@MISC{ texlive,
TITLE = {{\TeX{}Live}},
YEAR = {2012},
NOTE = {\url{http://www.tug.org/texlive/}},
URLDATE= {2012-12-13},
KEY = {TeXLive},
}
 
@MISC{ csplain,
AUTHOR = {Olšák, Petr},
TITLE = {{\csplain}},
YEAR = {1992--2013},
NOTE = {\url{http://petr.olsak.net/csplain.html}},
URLDATE= {2012-12-13},
}
 
@MISC{ opmac,
AUTHOR = {Olšák, Petr},
TITLE = {{OPmac}},
YEAR = {2012},
NOTE = {\url{http://petr.olsak.net/opmac.html}},
URLDATE= {2012-12-13},
}
 
@MISC{ LatinModern,
TITLE = {{Latin Modern} font family},
AUTHOR = {Jackowski, Bogusław and Nowacki, Janusz M.},
NOTE = {\url{http://oldwww.gust.org.pl/projects/e-foundry/latin-modern}},
URLDATE= {2012-12-13},
}
 
@MISC{ vlna,
TITLE = {Program vlna},
AUTHOR = {Olšák, Petr},
NOTE = {\url{ftp://math.feld.cvut.cz/olsak/vlna/}},
}
 
@MANUAL{ grafman,
TITLE = {Grafický manuál identity Českého vysokého učení technického v Praze},
NOTE= {Reklamní a umělecká agentura Klubko 55.
\url{http://www.cvut.cz/informace-pro-media/graficky-manual}},
KEY = {grafman},
}
 
@MANUAL{ zyka,
TITLE = {FELthesis -- \LaTeX{} templates for thesis on CTU FEL},
AUTHOR = {Vít Zýka},
YEAR = {2012},
NOTE = {\url{http://zyka.net/felthesis/felthesis.zip}},
}
 
/dokumenty/skolni/diplomka/mybase.tex
0,0 → 1,2
\input opmac
\genbbl{mybase}{plain} \end