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Ignore whitespace Rev 1108 → Rev 1109

/dokumenty/skolni/diplomka/diplomka.pdf
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/dokumenty/skolni/diplomka/diplomka.ref
21,64 → 21,79
\Xlabel{ADC-dynamic-range}{1.1}
\Xsecc{1.3.3}{Bandwidth }{3}
\Xpage{4}
\Xchap{2}{Trial design }{4}
\Xsec{2.1}{Required parameters }{4}
\Xsec{2.2}{Sampling frequency }{4}
\Xsec{2.3}{System scalability }{4}
\Xsec{1.4}{Current status of receivers digitalization units }{4}
\Xsecc{1.4.1}{Custom digitalization system }{4}
\Xsecc{1.4.2}{Modular digitalization systems }{4}
\Xpage{5}
\Xsecc{2.3.1}{Differential signalling }{5}
\Xsecc{2.3.2}{Phase matching }{5}
\Xsec{2.4}{System description }{5}
\Xsecc{2.4.1}{Frequency synthesis }{5}
\Xfnote
\Xpage{6}
\Xsecc{2.4.2}{Signal cable connectors }{6}
\Xsecc{2.4.3}{Signal integrity requirements }{6}
\Xsecc{2.4.4}{ADC modules design }{6}
\Xchap{2}{Trial design }{6}
\Xsec{2.1}{Required parameters }{6}
\Xsec{2.2}{Sampling frequency }{6}
\Xsec{2.3}{System scalability }{6}
\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
\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}
\Xsecc{2.4.5}{ADC selection }{7}
\Xpage{8}
\Xpage{10}
\Xtab{ADC-types}{2.1}{Available ADC types}
\Xlabel{ADC-types}{2.1}
\Xsecc{2.4.6}{ADC modules interface }{8}
\Xsecc{2.4.7}{Output data format }{8}
\Xsec{2.5}{Achieved parameters }{8}
\Xpage{9}
\Xfig{VITA57-regions}{2.3}{VITA57 board geometry}
\Xlabel{VITA57-regions}{2.3}
\Xsecc{2.5.1}{Data reading and recording }{9}
\Xpage{10}
\Xfig{1-line-out}{2.2}{Single line ADC output signals}
\Xlabel{1-line-out}{2.2}
\Xpage{11}
\Xsecc{2.5.2}{ADC module parameters }{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}
\Xpage{13}
\Xchap{3}{Example of usage }{13}
\Xsec{3.1}{Basic interferometer station }{13}
\Xfig{meteor-reflection}{3.1}{Meteor reflection}
\Xlabel{meteor-reflection}{3.1}
\Xfig{phase-phase-difference}{3.2}{Phase difference}
\Xlabel{phase-phase-difference}{3.2}
\Xpage{14}
\Xfig{block-schematic}{3.3}{Receiver block schematic}
\Xlabel{block-schematic}{3.3}
\Xfig{ADC1-FFT}{2.7}{ADC1 sine test FFT}
\Xlabel{ADC1-FFT}{2.7}
\Xpage{15}
\Xchap{4}{Proposed final system }{15}
\Xsec{4.1}{Custom design of FPGA board }{15}
\Xsec{4.2}{Parralella board computer }{15}
\Xsec{4.3}{GPU based computational system }{15}
\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}
\Xfig{block-schematic}{3.1}{Receiver block schematic}
\Xlabel{block-schematic}{3.1}
\Xpage{17}
\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{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{17}
\Xchap{5}{Conclusion }{17}
\Xsec{5.1}{Possible future improvements }{17}
\Xpage{19}
\Xchap{A}{Circuit diagram of ADCdual01A module }{19}
\Xpage{20}
\Xchap{B}{Circuit diagram of FMC2DIFF module }{20}
\Xchap{5}{Conclusion }{20}
\Xsec{5.1}{Possible future improvements }{20}
\Xpage{21}
\Xchap{A}{Circuit diagram of ADCdual01A module }{21}
\Xpage{22}
\Xchap{B}{Circuit diagram of FMC2DIFF module }{22}
\Xpage{23}
\Xpage{24}
\Xpage{25}
\Xpage{26}
\Xpage{27}
\Xchap{C}{Content of enclosed CD }{27}
/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) 4 MAY 2014 22:50
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
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stronomyobservations:Asaresult; wecannotworkinthesamewayashadtheradioastronomer
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l.25 ...gh for make new astronomy discovery.\fnote
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l.25 ...w astronomical discoveries possible.\fnote
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Observation types
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l.55 \secc
l.54 ... bit depth using a following formula \ref
[dynamic-range]
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l.56 \clabel
[dynamic-range]
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l.61 The formula \ref
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l.61 ...e] gives values shown in table below \ref
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l.63 \midinsert \clabel
[ADC-dynamic-range]{Dynamic range versus bit depth}
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l.64 \ctable
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l.65 \hfil ADC Bits &
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l.73 \caption
/t Standard bit depths of ADC and its theoretical dynamic range.
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l.79 \url
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l.87 \sec
Current status of receivers digitalization units
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l.61 ...uses proprietary digitalisation units \url
l.91 \secc
Custom digitalization system
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l.94 ...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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\teni DOKconnectorsarehighqualitydifferentialpairsconnectors; butpriceoftheseco
nnectorsiscomparablewithvalueofoneADCchannelinourdesigndescribedinfollowingpart
ofdocument:$ |
 
\hbox(6.94444+1.94444)x452.96786
.\teni D
.\kern0.27779
.\teni O
.\kern0.27779
.\teni K
.etc.
 
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<*> introduction.tex
/dokumenty/skolni/diplomka/introduction.tex
53,10 → 53,8
Dynamic range represents a huge problem of current radioastronomical receivers. This parameter is enforced by everywhere present humans made EMI radiation on RF frequencies. The modern radio astronomy receiver must not be saturated by this high levels of signals but still needs to have enough sensitivity to see faint signals from natural sources. Dynamic range is limited either by the construction of analogue circuitry in receiver or by the digitalisation unit.
The maximal theoretical dynamic range of ADC could be estimated from ADC bit depth using a following formula \ref[dynamic-range]
 
%\clabel[dynamic-range]
$$
D.R. (dB) = 20 * log(2^n)
$$
\label[dynamic-range]
$$ D.R. (dB) = 20 * log(2^n) $$
 
The formula \ref[dynamic-range] gives values shown in table below \ref[ADC-dynamic-range].
 
63,12 → 61,12
\midinsert \clabel[ADC-dynamic-range]{Dynamic range versus bit depth}
\ctable{cc}{
\hfil ADC Bits & Dynamic range [dB] \cr
8 & 48 \cr
10 & 60 \cr
12 & 72 \cr
14 & 84 \cr
16 & 96 \cr
24 & 144 \cr
8 & 48 \cr
10 & 60 \cr
12 & 72 \cr
14 & 84 \cr
16 & 96 \cr
24 & 144 \cr
}
\caption/t Standard bit depths of ADC and its theoretical dynamic range.
\endinsert
77,7 → 75,7
 
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 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.
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.
 
 
\secc Bandwidth
84,52 → 82,25
 
Historically, the parameter of bandwidth in radioastronomical receiver used to be within the kilohertz range. Small bandwidth was acceptable because observations were processed directly by listening or by paper chart intensity recorder. Chart recorder integrated energy of signal over defined small bandwidth which was suitable for detecting the intensity variance of microwave background. No wide-band transmitters existed in that era (except for TV transmitters) and tuning to other neighbouring frequency was easy as they were mostly vacant. Parallel observations from several places were unnecessary as well because the electromagnetic conditions were nearly same at all locations.
 
 
 
\sec Current status of receivers digitalization units
 
% dopsat navaznost na aktualne pouzivane digitalizacni jednotky
 
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 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 instrument developed in one piece with leads to enormous founding resources draws is Arecibo ALFA survey multi beam feed Array.
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. \url{http://arxiv.org/abs/1305.3550}
LOFAR is innovative radioastronomy system which uses the phased antenna array approach in enormous scale and thousands of antennas are manufactured an deployed on field. The center of LOFAR system is situated in Netherlands and periferal antennas and 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 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. \url{http://www.astron.nl/other/desp/competences_DesApp.htm}
 
LOFAR project must use low cost hardware due to project scale to keep overall project budget at acceptable levels. LOFAR in order of thisuses direct sampling receiver technology
 
 
 
 
 
 
 
 
ASTRON ADCs
http://www.astron.nl/other/desp/competences_DesApp.htm
 
 
\secc Modular digitalization systems
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 \url{https://casper.berkeley.edu/wiki/Main_Page}. 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 \url{https://casper.berkeley.edu/papers/200509URSI.pdf}. 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) \url{http://www.digikey.com/product-detail/en/6367550-5/6367550-5-ND/2259130}. 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.
 
One modular digitalization system currently exit. It is beaing developed at Berkley
In opposite to professional astronomers which uses proprietary digitalization units, amateur radioastronomers currently uses 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 of proper hardware which could be used on both communities - professionals and amateurs. Optimal solution for this situation should be open-source hardware.
 
\url{https://casper.berkeley.edu/wiki/Main_Page}
 
Z-DOK connectors have relatively high pricing around 40 USD http://www.digikey.com/product-detail/en/6367550-5/6367550-5-ND/2259130
This price is comparable with value of one ADC channel in our design described in following part of document.
 
 
Mudular radioastronomy hardware: https://casper.berkeley.edu/papers/200509URSI.pdf
 
In opposite of professional astronomers which uses proprietary digitalization units, amateur radioastronomers currently uses multichannel sound cards \url{http://fringes.org/}
 
It is evident that current radioastronomy lacks of proper hardware which could be used on both communities professionals and amateurs. In addition open-source hardware