Changeset 9188
- Timestamp:
- Dec 4, 2008, 1:30:45 PM (12 years ago)
- Location:
- trunk/Documents/DrivePaper
- Files:
-
- 8 edited
Legend:
- Unmodified
- Added
- Removed
-
trunk/Documents/DrivePaper/elsarticle.cls
r9109 r9188 17 17 %% version 1999/12/01 or later. 18 18 %% 19 %% $Id: elsarticle.cls,v 1. 1 2008-08-07 14:26:10tbretz Exp $19 %% $Id: elsarticle.cls,v 1.2 2008-12-04 13:30:45 tbretz Exp $ 20 20 %% 21 21 \def\RCSfile{elsarticle}% -
trunk/Documents/DrivePaper/paper.bib
r9109 r9188 1 ------------------------------------------------------------------------------2 ------------------------------------------------------------------------------3 Article (author, title, journal, year)4 (volume, numbe,r pages, month, note)5 Book (author/editor, title, publisher, year)6 (volume/number, series, address, edition, month, note)7 Conference (author, title, booktitle, year)8 (editor, volume/number, organization, series, pages, publisher, address, month, note)9 Inproceedings (author, title, booktitle, year)10 (editor, volume/number, organization, series, pages, publisher, address, month, note)11 Manual (title)12 (author, organization, address, edition, month, year, note)13 Masterthesis (author, title, school, year)14 (address, month, note, type)15 phdthesis (author, title, school, year)16 (address, month, note, type)17 unpublished (author, title, note)18 (month, year)19 misc ()20 (author, title, howpublished, month, year, note)21 ------------------------------------------------------------------------------22 23 @MISC{www:fornaxa, key = {{www-01}}, title = {\url{http://www.nrao.edu/imagegallery/}}, year=2006, note={Credit: NRAO/AUI/NSF}}24 @MISC{www:agnartist0, key = {{www-02}}, title = {\url{http://integral.esa.int/integ_pictures.html}}, year=2006}25 @MISC{www:agnartist, key = {{www-03}}, title = {\url{http://www.spacetelescope.org/images/}}, year=2006, note={Credit: ESA/NASA, the AVO Project and Paolo Padovani}}26 @MISC{www:compton, key = {{www-04}}, title = {\url{http://chandra.harvard.edu/resources/illustrations/xlightScatter.html}}, year=2006}27 @MISC{www:shower, key = {{www-05}}, title = {\url{http://www.mpi-hd.mpg.de/hfm/CosmicRay/shower.png}}, year=2006}28 @MISC{www:showerartist, key = {{www-06}}, title = {\url{http://abyss.uoregon.edu/~js/glossary/cosmic_rays.html}}, year=2006}29 @MISC{www:mars, key = {{www-07}}, title = {\url{http://magic.astro.uni-wuerzburg.de/mars/}}, year=2006}30 @MISC{www:google, key = {{www-08}}, title = {\url{http://earth.google.com}}, year=2006}31 @MISC{www:slalib, key = {{www-09}}, title = {\url{http://star-www.rl.ac.uk/star/docs/sun67.htx/sun67.html}}, year=2006}32 @MISC{www:root, key = {{The ROOT System Home Page}}, title = {\url{http://root.cern.ch}}, year=2008}33 @MISC{www:htmldoc, key = {{www-11}}, title = {\url{http://magic.astro.uni-wuerzburg.de/mars/htmldoc/}}, year=2006}34 @MISC{www:mysql, key = {{www-12}}, title = {\url{http://www.mysql.com}}, year=2006}35 @MISC{www:unified, key = {{www-13}}, title = {\url{http://chandra.harvard.edu/resources/illustrations/quasar.html}}, year=2006, note={Credit: NASA/CXC, Melissa Weiss}}36 @MISC{www:asdc, key = {{www-14}}, title = {\url{http://www.asdc.asi.it/blazars/}}, year=2006}37 @MISC{www:kva, key = {{www-15}}, title = {\url{http://tur3.tur.iac.es/}}, year=2006}38 @MISC{www:integral, key = {{www-16}}, title = {\url{http://altamira.asu.cas.cz/iblwg/show.php?id=131}}, year=2006}39 @MISC{www:ned, key = {{www-17}}, title = {\url{http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=1es1218+304}}, year=2006}40 @MISC{www:gcn, key = {{GCN}}, title = {\url{http://gcn.gsfc.nasa.gov}}, year=2008}41 42 %@MISC{www:BH1m, key = {{www-02}}, title = {\url{http://www.gsfc.nasa.gov/gsfc/spacesci/pictures/blackhole/BH1m.jpg}}, year=2006}43 %@MISC{www:hillas, key = {{www-10}}, title = {\url{http://lpnhe-auger.in2p3.fr/slides/hillas.ps}}, year=2006}44 %@MISC{www:agnartist2, key = {{www-03}}, title = {\url{http://upload.wikimedia.org/wikipedia/en/4/40/Galaxies_AGN_Inner-Structure-of.jpg}}, year=2006}45 46 47 @BOOK{Peebles:1983,48 author = {Peebles, Philip~James~Edwin},49 title = {Principles of Physical Cosmology},50 publisher = {Princton Series in Physics},51 year = 198352 }53 54 @BOOK{Weekes:2003,55 author = {Weekes, T.~C.},56 title = {Very high energy gamma-ray astronomy},57 series = {Astronomy and Astrophysics},58 publisher = {Institute of Physics Publishing},59 year = 200360 }61 62 @BOOK{Rybicki:1979,63 author = {{Rybicki}, George B. and {Lightman}, Alan P.},64 title = "Radiative Processes in Astrophysics",65 publisher = { Wiley-Interscience },66 year = 197967 }68 69 @BOOK{Begelman:1995,70 author = {Begelman, M. and Rees, M.},71 title = "{Gravity's Fatal Attraction: Black Holes in the Universe}",72 year = 1995,73 publisher = {Scientific American Library}74 }75 76 @BOOK{Mueller:2005,77 author = {{M\"uller}, A.},78 title = "{Lexikon der Astrophysik}",79 year = 2005,80 month = sep,81 url = {http://www.mpe.mpg.de/~amueller}82 }83 84 @BOOK{Zensus:1987,85 author = {{Pearson}, T.~J. and {Zensus}, J.~A.},86 year = 1987,87 title = {Superluminal radio sources},88 publisher = {Cambridge University Press}89 }90 91 @BOOK{Schlickeiser:2003,92 author = {{Schlickeiser}, Reinhard},93 year = 2003,94 title = {Cosmic Ray Astrophysics},95 publisher = {Springer}96 }97 98 @BOOK{Landau:1971,99 author = {{Landau}, L.~D. and {Lifshitz}, E.~M.},100 title = "{The classical theory of fields}",101 publisher = {Course of theoretical physics - Pergamon International Library of Science, Technology, Engineering and Social Studies, Oxford: Pergamon Press, 1971, 3rd rev.~engl.~edition},102 year = 1971,103 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1971ctf..book.....L&db_key=AST},104 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}105 }106 107 @MANUAL{Corsika,108 author = {{Heck}, D. and {Knapp}, J. and {Capdevielle}, J.~N. and {Schatz}, G. and {Thouw}, T.},109 year = 1998,110 title = {{CORSIKA}: {A} {M}onte {C}arlo {C}ode to {S}imulate {E}xtensive {A}ir {S}howers},111 organization = {Forschungszentrum Karlsruhe, {R}eport {FZKA} 6019},112 note = {\url{http://www-ik.fzk.de/corsika/physics\_description/corsika\_phys.html}}113 }114 115 @MANUAL{slalib,116 author = {{Wallace}, P.~T.},117 year = 2005,118 title = {{SLALIB} -- {P}osition {A}stronomy {L}ibrary 2.5-3, {P}rogrammer's {M}anual},119 organization = {Rutherford Appleton Laboratory},120 note = {\url{http://star-www.rl.ac.uk/star/docs/sun67.htx/sun67.html}}121 }122 123 @MANUAL{tpoint,124 author = {{Wallace}, P.~T.},125 year = 2001,126 month = may,127 title = {{TPOINT} -- {A} {T}elescope {P}ointing {A}nalaysis {S}ystem},128 address = {19 Sutton Wick Lane, Drayton, Abingdon, Oxfordshire, United Kingdom, OX14 4HH},129 note = {\url{http://star-www.rl.ac.uk/star/docs/sun67.htx/sun67.html}}130 }131 132 @MANUAL{Breiman,133 author = {Breiman, Leo},134 title = {Machine Learning 45(1), 5},135 year = 2001136 }137 138 @MASTERSTHESIS{Doro:Diploma,139 author = {Doro, M.},140 title = {The Commissioning and Characterization of the Calibration System of the {MAGIC} Telescope},141 school = {Universit{\'a} di Padova},142 year = {2004},143 note = {\url{http://wwwmagic.mppmu.mpg.de/publications/theses/LaureaMDoro.ps.gz}}144 }145 146 @MASTERSTHESIS{Stefan:Diploma,147 author = {R\"ugamer, S.},148 title = {},149 school = {Bayerische Julius-Maximilians-Universit{\"a}t W{\"u}rzburg},150 year = {2006},151 note = {in preparation}152 }153 154 @MASTERSTHESIS{Hoehne:Diploma,155 author = {H\"ohne, D.},156 title = "{Beobachtung von HESS\,J1813-178 mit dem MAGIC-Teleskop}",157 school = {Bayerische Julius-Maximilians-Universit{\"a}t W{\"u}rzburg},158 month = sep,159 year = {2005},160 }161 162 @MASTERSTHESIS{Dorner:Diploma,163 author = {Dorner, D.},164 title = {{S}ystem zum {A}usrichten und {N}achf\"uhren des {MAGIC}-{T}eleskops},165 school = {Bayerische Julius-Maximilians-Universit{\"a}t W{\"u}rzburg},166 year = {2003}167 }168 169 @MASTERSTHESIS{Riegel:Diploma,170 author = {Riegel, B.},171 title = {{S}ystematische {U}ntersuchung der {B}ildparameter f\"ur das {MAGIC}-{T}eleskop},172 school = {Bayerische Julius-Maximilians-Universit{\"a}t W{\"u}rzburg},173 year = {2005}174 }175 176 @MASTERSTHESIS{Bretz:1999,177 author = {Bretz, T.},178 title = {Magnetfeldeigenschaften des {S}pektrometers {HADES}},179 school = {Technische Universit{\"a}t M{\"u}nchen},180 year = {1999}181 }182 183 %MASTERSTHESIS{Doro:2005,184 % author = {Doro, Michele},185 % year = {2005}186 %187 188 @MISC{Giommi:2006,189 author = { Giommi, P. and others},190 year = 2006,191 howpublished = {in preparation}192 }193 194 @MISC{Giommi:2005,195 author = { Giommi, P.},196 year = 2006,197 howpublished = {private communication}198 }199 200 @ARTICLE{Dondi:1995,201 author = {{Dondi}, L. and {Ghisellini}, G.},202 title = "{Gamma-ray-loud blazars and beaming}",203 journal = {\mnras},204 year = 1995,205 month = apr,206 volume = 273,207 pages = {583-595},208 asdurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1995MNRAS.273..583D&db_key=AST},209 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}210 }211 212 @ARTICLE{Fermi:1954,213 author = {{Fermi}, E.},214 title = "{Galactic Magnetic Fields and the Origin of Cosmic Radiation.}",215 journal = {\apj},216 year = 1954,217 month = jan,218 volume = 119,219 pages = {1-+},220 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1954ApJ...119....1F&db_key=AST},221 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}222 }223 224 @ARTICLE{Fermi:1949,225 author = {{Fermi}, E.},226 journal = {Phys.~Rev.},227 volume = 75,228 pages = 1169,229 year = {1949}230 }231 232 @ARTICLE{Wentzel:1963,233 author = {{Wentzel}, D.~G.},234 title = "{Fermi Acceleration of Charged Particles.}",235 journal = {\apj},236 year = 1963,237 month = jan,238 volume = 137,239 pages = {135-+},240 adsurl = {http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=1963ApJ...137..135W&db_key=AST},241 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}242 }243 244 @BOOK{Spitzer:1956,245 author = {{Spitzer}, L.},246 title = "{Physics of Fully Ionized gases}",247 publisher = {Interscience, New York },248 year = 1956,249 }250 251 @ARTICLE{Einstein:1905,252 author = {{Einstein}, A.},253 title = "{Zur Elektrodynamik bewegter K{\"o}rper}",254 journal = {Annalen der Physik},255 year = 1905,256 volume = 17,257 pages = {891-921},258 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1905AnP....17..891E&db_key=AST},259 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}260 }261 262 @ARTICLE{Einstein:1916,263 author = {{Einstein}, A.},264 title = "{Die Grundlage der allgemeinen Relativit{\"a}tstheorie}",265 journal = {Annalen der Physik},266 year = 1916,267 volume = 49,268 pages = {769-822},269 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1916AnP....49..769E&db_key=AST},270 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}271 }272 273 @ARTICLE{Eddington:1935a,274 author = {{Eddington}, A.~S.},275 title = "{On "relativistic degeneracy,"}",276 journal = {\mnras},277 year = 1935,278 month = jan,279 volume = 95,280 pages = {194-206},281 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1935MNRAS..95..194E&db_key=AST},282 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}283 }284 285 @ARTICLE{Rindler:1956,286 author = {{Rindler}, W.},287 title = "{Visual horizons in world models}",288 journal = {\mnras},289 year = 1956,290 volume = 116,291 pages = {662-+},292 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1956MNRAS.116..662R&db_key=AST},293 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System},294 }295 296 @ARTICLE{Eddington:1935b,297 author = {{Eddington}, A.~S.},298 title = "{Note on "relativistic degeneracy"}",299 journal = {\mnras},300 year = 1935,301 month = nov,302 volume = 96,303 pages = {20-+},304 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1935MNRAS..96...20E&db_key=AST},305 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}306 }307 308 @ARTICLE{Chandrasekhar:1931,309 author = {{Chandrasekhar}, S.},310 title = "{The Maximum Mass of Ideal White Dwarfs}",311 journal = {\apj},312 year = 1931,313 month = jul,314 volume = 74,315 pages = {81-+},316 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1931ApJ....74...81C&db_key=AST},317 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}318 }319 320 @ARTICLE{Oppenheimer:1939,321 author = {{Oppenheimer}, Julius Robert and {Snyder}, Hartland},322 title = {On continued gravitational contraction},323 journal = {Phys.~Rev.},324 volume = 56,325 pages = 455,326 year = {1939}327 }328 329 @ARTICLE{Kerr:1963,330 author = {{Kerr}, Roy Patrick},331 title = {Gravitational field of a spinning mass as an example of algebraically special metrics},332 journal = {\prl},333 volume = 11,334 pages = 237,335 year = {1963}336 }337 338 @ARTICLE{Bolton:1971,339 author = {{Bolton}, C.~T.},340 title = {Identification of {Cyg} {X}-1 with {HDE} 226868},341 journal = {\nat},342 year = 1972,343 volume = 235,344 pages = {271},345 }346 347 @ARTICLE{Shakura:1973,348 author = {{Shakura}, N.~I. and {Sunyaev}, R.~A.},349 title = "{Black holes in binary systems. Observational appearance.}",350 journal = {\aap},351 year = 1973,352 volume = 24,353 pages = {337-355},354 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1973A%26A....24..337S&db_key=AST},355 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}356 }357 358 @ARTICLE{Hasinger:1998,359 author = {{Hasinger}, G. and {Burg}, R. and {Giacconi}, R. and {Schmidt}, M. and360 {Trumper}, J. and {Zamorani}, G.},361 title = "{The ROSAT Deep Survey. I. X-ray sources in the Lockman Field}",362 journal = {\aap},363 year = 1998,364 month = jan,365 volume = 329,366 pages = {482-494},367 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998A%26A...329..482H&db_key=AST},368 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}369 }370 371 @ARTICLE{LyndenBell:1969,372 author = {{Lynden-Bell}, D.},373 title = "{Galactic Nuclei as Collapsed Old Quasars}",374 journal = {\nat},375 year = 1969,376 volume = 223,377 pages = {690-+},378 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1969Natur.223..690L&db_key=AST},379 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}380 }381 382 @ARTICLE{Georga:1988,383 author = {{George}, I.~M. and {Warwick}, R.~S. and {Bromage}, G.~E.},384 title = "{X-ray and ultraviolet observations of Markarian 421}",385 journal = {\mnras},386 year = 1988,387 month = jun,388 volume = 232,389 pages = {793-808},390 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1988MNRAS.232..793G&db_key=AST},391 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}392 }393 394 @ARTICLE{LyndenBell:1971,395 author = {{Lynden-Bell}, D. and {Rees}, M.~J.},396 title = "{On quasars, dust and the galactic centre}",397 journal = {\mnras},398 year = 1971,399 volume = 152,400 pages = {461-+},401 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1971MNRAS.152..461L&db_key=AST},402 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}403 }404 405 @ARTICLE{Hawking:1975,406 author = {{Hawking}, {S}tephen W.},407 title = {Particle creation by black holes},408 journal = {Comm.~Math.~Phys.},409 volume = {43},410 pages = {199},411 year = 1975412 }413 414 @ARTICLE{Penrose:1965,415 author = {{Penrose}, Roger},416 title = {Gravitational collapse and space-time singularities},417 journal = {\prl},418 volume = 14,419 pages = 57,420 year = {1965}421 }422 423 @INPROCEEDINGS{Schwarzschild:1916a,424 author = {Schwarzschild, K.},425 title = {{\"U}ber das {G}ravitationsfeld eines {M}assenpunktes nach der {E}insteinschen {T}heorie},426 booktitle = {Sitzungsberichte der k\"oniglich preu\ss{}ischen {A}kademie der {W}issenschaften zu {B}erlin},427 year = {1916},428 pages = {189-196},429 note = {physics/9905030}430 }431 432 @INPROCEEDINGS{Schwarzschild:1916b,433 author = {Schwarzschild, K.},434 title = {{\"U}ber das {G}ravitationsfeld einer {K}ugel aus inkompressibler {F}l\"ussigkeit nach der {E}insteinschen {T}heorie},435 booktitle = {Sitzungsberichte der k\"oniglich preu\ss{}ischen {A}kademie der {W}issenschaften zu {B}erlin},436 year = {1916},437 pages = {424-434},438 note = {physics/9912033}439 }440 441 @ARTICLE{MAGIC:30GeV,442 author = {{Moralejo}, A. and others},443 title = {The {MAGIC} telescope for gamma-ray astronomy above 30 {GeV}},444 journal = {\cjaa},445 year = 2003,446 month = dec,447 volume = 3,448 pages = {531-538},449 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2003ChJAA...3S.531M&db_key=AST},450 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}451 }452 453 @ARTICLE{MAGIC:LowEnergy,454 author = {{Albert}, J. and others},455 title = {Physics and astrophysics with a ground-based gamma-ray telescope of low energy threshold},456 journal = {Astroparticle Physics},457 year = 2005,458 month = jun,459 volume = 23,460 pages = {493-509},461 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2005APh....23..493F&db_key=AST},462 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}463 }464 465 @ARTICLE{Albert:2006grb,466 author = {{Albert}, J. and others467 },468 title = "{Flux Upper Limit on Gamma-Ray Emission by GRB 050713a from MAGIC Telescope Observations}",469 journal = {\apjl},470 year = 2006,471 month = apr,472 volume = 641,473 pages = {L9-L12},474 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2006ApJ...641L...9A&db_key=AST},475 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}476 }477 478 @ARTICLE{Horan:2004,479 author = {{Horan}, D. and others},480 title = "{Constraints on the Very High Energy Emission from BL Lacertae Objects}",481 journal = {\apj},482 year = 2004,483 month = mar,484 volume = 603,485 pages = {51-61},486 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004ApJ...603...51H&db_key=AST},487 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}488 }489 490 @ARTICLE{Aharonian:1553,491 author = {{Aharonian}, F. and others},492 title = "{Evidence for VHE Gamma-ray Emission from the Distant BL Lac PG\,1553+113}",493 journal = {\aap},494 year = 2006,495 note = {in press}496 }497 498 @ARTICLE{Green:1986,499 author = {{Green}, R.~F. and {Schmidt}, M. and {Liebert}, J.},500 title = "{The Palomar-Green catalog of ultraviolet-excess stellar objects}",501 journal = {\apjs},502 year = 1986,503 month = jun,504 volume = 61,505 pages = {305-352},506 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1986ApJS...61..305G&db_key=AST},507 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}508 }509 510 @ARTICLE{Paciesas:1999,511 author = {{Paciesas}, W.~S. and others},512 title = "{The Fourth BATSE Gamma-Ray Burst Catalog (Revised)}",513 journal = {\apjs},514 year = 1999,515 month = jun,516 volume = 122,517 pages = {465-495},518 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1999ApJS..122..465P&db_key=AST},519 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}520 }521 522 @ARTICLE{Donato:2001,523 author = {{Donato}, D. and {Ghisellini}, G. and {Tagliaferri}, G. and524 {Fossati}, G.},525 title = "{Hard X-ray properties of blazars}",526 journal = {\aap},527 year = 2001,528 month = sep,529 volume = 375,530 pages = {739-751},531 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2001A%26A...375..739D&db_key=AST},532 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}533 }534 535 @ARTICLE{Costamante:2002,536 author = {{Costamante}, L. and {Ghisellini}, G.},537 title = "{TeV candidate BL Lac objects}",538 journal = {\aap},539 year = 2002,540 month = mar,541 volume = 384,542 pages = {56-71},543 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2002A%26A...384...56C&db_key=AST},544 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}545 }546 547 @ARTICLE{Ledden:1985,548 author = {{Ledden}, J.~E. and {Odell}, S.~L.},549 title = "{The radio-optical-X-ray spectral flux distributions of blazars}",550 journal = {\apj},551 year = 1985,552 month = nov,553 volume = 298,554 pages = {630-643},555 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1985ApJ...298..630L&db_key=AST},556 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}557 }558 559 @ARTICLE{Hogg:2002,560 author = {Hogg, D.~W. and Baldry, I.~K. and Blanton, M.~R. and Eisenstein, D.~J. },561 title = {The {K} correction},562 year = 2002,563 month = oct,564 journal = {astro-ph},565 note = {astro-ph/0210394}566 }567 568 @ARTICLE{Holder:2006,569 author = {Holder, J. and others},570 title = "{The First VERITAS Telescope}",571 year = 2006,572 month = apr,573 journal = {submitted},574 note = {astro-ph/0604119}575 }576 577 @ARTICLE{Lorenz:2004,578 author = {{Lorenz}, E.},579 title = "{Status of the 17 m MAGIC telescope}",580 journal = {New Astronomy Review},581 year = 2004,582 month = apr,583 volume = 48,584 pages = {339-344},585 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004NewAR..48..339L&db_key=AST},586 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}587 }588 589 @ARTICLE{Kubo:2004,590 author = {{Kubo}, H. and others},591 title = "{Status of the CANGAROO-III project}",592 journal = {New Astronomy Review},593 year = 2004,594 month = apr,595 volume = 48,596 pages = {323-329},597 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004NewAR..48..323K&db_key=AST},598 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}599 }600 601 @ARTICLE{Weekes:2002,602 author = {{Weekes}, T.~C. and others},603 title = "{VERITAS: the Very Energetic Radiation Imaging Telescope Array System}",604 journal = {Astroparticle Physics},605 year = 2002,606 month = may,607 volume = 17,608 pages = {221-243},609 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2002APh....17..221W&db_key=AST},610 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}611 }612 613 @ARTICLE{Aharonian:2005,614 author = {{Aharonian}, F. and others},615 title = "{A New Population of Very High Energy Gamma-Ray Sources in the Milky Way}",616 journal = {Science},617 year = 2005,618 month = mar,619 volume = 307,620 pages = {1938-1942},621 adsurl = 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Their Nature and Implications for the Active Galactic Nucleus Luminosity Function}",665 journal = {\apj},666 year = 1999,667 month = apr,668 volume = 514,669 pages = {746-764},670 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1999ApJ...514..746S&db_key=AST},671 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}672 }673 674 @ARTICLE{Janiuk:2006,675 author = {{Janiuk}, A. and {Czerny}, B. and {Moderski}, R. and {Cline}, D.~B. and676 {Matthey}, C. and {Otwinowski}, S.},677 title = "{On the origin of the bimodal duration distribution of gamma-ray bursts and the subjet model}",678 journal = {\mnras},679 year = 2006,680 month = jan,681 volume = 365,682 pages = {874-884},683 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2006MNRAS.365..874J&db_key=AST},684 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}685 }686 687 @ARTICLE{Klebesadel:1973,688 author = {{Klebesadel}, R.~W. and {Strong}, I.~B. and {Olson}, R.~A.},689 title = "{Observations of Gamma-Ray Bursts of Cosmic Origin}",690 journal = {\apjl},691 year = 1973,692 month = jun,693 volume = 182,694 pages = {L85+},695 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1973ApJ...182L..85K&db_key=AST},696 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}697 }698 699 @ARTICLE{Meszaros:1997,700 author = {{Meszaros}, P. and {Rees}, M.~J.},701 title = "{Optical and Long-Wavelength Afterglow from Gamma-Ray Bursts}",702 journal = {\apj},703 year = 1997,704 month = feb,705 volume = 476,706 pages = {232-+},707 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997ApJ...476..232M&db_key=AST},708 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}709 }710 711 @ARTICLE{Waxman:1995,712 author = {{Waxman}, E.},713 title = "{Cosmological Gamma-Ray Bursts and the Highest Energy Cosmic Rays}",714 journal = {\prl},715 year = 1995,716 month = jul,717 volume = 75,718 pages = 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infrared radiation fields}",826 journal = {\apjl},827 year = 1992,828 month = may,829 volume = 390,830 pages = {L49-L52},831 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992ApJ...390L..49S&db_key=AST},832 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}833 }834 835 @ARTICLE{Ben:2002,836 author = {{Ben-Zhong}, Dai and {Ghunag-Zhong}, Xie and {Ze-Jun}, Jiang},837 title = {Properties of BL Lac Objects with Redshift $\le$ 2},838 journal = {\cjaa},839 year = 2002,840 volume = 2,841 pages = {8-16}842 }843 844 @ARTICLE{LiMa:1983,845 author = {{Li}, T.-P. and {Ma}, Y.-Q.},846 title = "{Analysis methods for results in gamma-ray astronomy}",847 journal = {\apj},848 year = 1983,849 month = sep,850 volume = 272,851 pages = {317-324},852 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1983ApJ...272..317L&db_key=AST},853 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}854 }855 856 @ARTICLE{Bartko:2005pa,857 author = 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Proc.},883 volume = 280,884 year = 1993,885 pages = {533},886 editor = {Gehrels}887 }888 889 @ARTICLE{Kneiske:2004,890 author = {{Kneiske}, T.~M. and {Bretz}, T. and {Mannheim}, K. and {Hartmann}, D.~H.},891 title = {Implications of cosmological gamma-ray absorption. {II}. 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{{Bretz}, T. and Dorner, D.},951 title = {{MARS} - {A} framework for a standard analysis},952 booktitle = {Towards a network of atmospheric Cherenkov detectors VII},953 year = 2005,954 month = Apr955 }956 957 @INPROCEEDINGS{Dorner:2005paris,958 author = {{Dorner}, D. and Bretz, T.},959 title = {A concept for data managment and processing},960 booktitle = {Towards a network of atmospheric Cherenkov detectors VII},961 pages = {571-575},962 year = 2005,963 month = Apr964 }965 966 @INPROCEEDINGS{Bastieri:2005,967 author = {Bastieri, D. and others},968 title = {The mirrors of the {MAGIC} telescope},969 booktitle = {$29^{th}$ International Cosmic Ray Conference},970 year = 2005,971 month = Aug,972 note = {astro-ph/0508274}973 }974 975 @INPROCEEDINGS{Dorner:2005icrc,976 author = {Dorner, D. and Berger, K. and Bretz, T. and Gaug, M. and others},977 title = {Data Managment and Processing for the {MAGIC} telescope},978 booktitle = {$29^{th}$ International Cosmic Ray Conference},979 year = 2005,980 volume = 5,981 pages = 175,982 month = Aug,983 note = {astro-ph/0508274}984 }985 986 @INPROCEEDINGS{Beixeras:2005,987 author = {Beixeras, C. and others},988 title = "{MAGIC II}",989 booktitle = {$29^{th}$ International Cosmic Ray Conference},990 volume = 5,991 pages = {227},992 year = 2005,993 month = Aug,994 note = {astro-ph/0508274}995 }996 997 @INPROCEEDINGS{Cortina:2005,998 author = {Cortina, J. and others},999 title = {Technical performance of the {MAGIC} telescope},1000 booktitle = {$29^{th}$ International Cosmic Ray Conference},1001 year = 2005,1002 month = Aug,1003 note = {astro-ph/0508274}1004 }1005 1006 @INPROCEEDINGS{Bretz:2005mars,1007 author = {Bretz, T.},1008 title = {Standard Analysis for the {MAGIC} Telescope},1009 booktitle = {$29^{th}$ International Cosmic Ray Conference},1010 volume = 4,1011 year = 2005,1012 pages = 315,1013 month = Aug,1014 note = {astro-ph/0508274}1015 }1016 1017 @INPROCEEDINGS{Gaug:2005,1018 author = {Gaug, M. and Bartko, H. and Cortina, J. and Rico, J. and others},1019 title = {Calibration of the {MAGIC} telescope},1020 booktitle = {$29^{th}$ International Cosmic Ray Conference},1021 year = 2005,1022 month = Aug,1023 note = {astro-ph/0508274}1024 }1025 1026 @INPROCEEDINGS{Riegel:2005icrc,1027 author = {{Riegel}, B. and Bretz, T.},1028 title = {A systematic study of the interdependance of the {IACT} image parameters},1029 booktitle = {$29^{th}$ International Cosmic Ray Conference},1030 year = 2005,1031 volume = 5,1032 pages = 215,1033 month = Aug,1034 note = {astro-ph/0508274}1035 }1036 1037 @INPROCEEDINGS{Riegel:2005icrc2,1038 author = {{Riegel}, B. and Bretz, T. and Dorner, D. and Wagner, R.~M.},1039 title = {A tracking monitor for the {MAGIC} telescope},1040 booktitle = {$29^{th}$ International Cosmic Ray Conference},1041 year = 2005,1042 volume = 5,1043 pages = 219,1044 month = Aug,1045 note = {astro-ph/0508274}1046 }1047 1048 @INPROCEEDINGS{Goebel:2005,1049 author = {{Goebel}, F. and Mase, K. and Meyer, M. and Mirzoyan, R. and Shayduk, M. and Teshima, M. and others},1050 title = {Absolute energy scale calibration of the {MAGIC} telescope using muon images},1051 booktitle = {$29^{th}$ International Cosmic Ray Conference},1052 year = 2005,1053 month = Aug,1054 note = {astro-ph/0508274}1055 }1056 1057 @INPROCEEDINGS{Majumdar:2005icrc,1058 author = {{Majumdar}, P. and {Moralejo}, A. and {Bigongiari}, C. and {Blanch}, O. and {Sobczynska}, D.},1059 title = {{M}onte {C}arlo simulation for the {MAGIC} telescope},1060 booktitle = {$29^{th}$ International Cosmic Ray Conference},1061 year = 2005,1062 month = Aug,1063 note = {astro-ph/0508274}1064 }1065 1066 @INPROCEEDINGS{Meyer:2005icrc,1067 author = {{Meyer}, M. and Mannheim, K. and Bretz, T. and Dorner, D. and Riegel, B. and H\"ohne, D. and Berger, K. and others},1068 title = {{MAGIC} observations of high-peaked {BL} {L}ac objects},1069 booktitle = {$28^{th}$ International Cosmic Ray Conference},1070 volume = 4,1071 pages = 335,1072 year = 2005,1073 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the Smithsonian/NASA Astrophysics Data System}1099 }1100 1101 @ARTICLE{Urry:2000,1102 author = {{Urry}, C.~M. and {Scarpa}, R. and {O'Dowd}, M. and {Falomo}, R. and1103 {Pesce}, J.~E. and {Treves}, A.},1104 title = "{The Hubble Space Telescope Survey of BL Lacertae Objects. II. Host Galaxies}",1105 journal = {\apj},1106 year = 2000,1107 month = apr,1108 volume = 532,1109 pages = {816-829},1110 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2000ApJ...532..816U&db_key=AST},1111 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1112 }1113 1114 @ARTICLE{Porter:1960,1115 author = {Hill, D.~A. and Porter, N.~A},1116 title = "{Photography of \v{C}erenkov Light from Extensive Air Showers in the Atmosphere}",1117 month = aug,1118 year = 1960,1119 journal = {\nat},1120 volume = 191,1121 pages = 690,1122 note = {Letters to Editor}1123 }1124 1125 @ARTICLE{Jelley:1963,1126 author = {{Jelley}, J.~V. and {Porter}, N.~A.},1127 title = "{{\v C}erenkov Radiation from the Night Sky, and its Application to {$\gamma$}-Ray Astronomy}",1128 journal = {\qjras},1129 year = 1963,1130 month = sep,1131 volume = 4,1132 pages = {275-+},1133 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1963QJRAS...4..275J&db_key=AST},1134 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1135 }1136 1137 @ARTICLE{Padovani:1995,1138 author = {{Padovani}, P. and {Giommi}, P.},1139 title = "{The connection between x-ray- and radio-selected BL Lacertae objects}",1140 journal = {\apj},1141 year = 1995,1142 month = may,1143 volume = 444,1144 pages = {567-581},1145 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1995ApJ...444..567P&db_key=AST},1146 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1147 }1148 1149 @ARTICLE{Boella:1997,1150 author = {{Boella}, G. and {Butler}, R.~C. and {Perola}, G.~C. and {Piro}, L. and1151 {Scarsi}, L. and {Bleeker}, J.~A.~M.},1152 title = "{BeppoSAX, the wide band mission for X-ray astronomy}",1153 journal = {\aaps},1154 year = 1997,1155 month = apr,1156 volume = 122,1157 pages = {299-307},1158 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997A%26AS..122..299B&db_key=AST},1159 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1160 }1161 1162 @ARTICLE{Catanese:1999,1163 author = {{Catanese}, M. and {Weekes}, T.~C.},1164 title = "{Very High Energy Gamma-Ray Astronomy}",1165 journal = {\pasp},1166 year = 1999,1167 month = oct,1168 volume = 111,1169 pages = {1193-1222},1170 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1999PASP..111.1193C&db_key=AST},1171 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1172 }1173 1174 @ARTICLE{Daum:1997,1175 author = {{Daum}, A. and others},1176 title = "{First results on the performance of the HEGRA IACT array}",1177 journal = {Astroparticle Physics},1178 year = 1997,1179 month = dec,1180 volume = 8,1181 pages = {1-2},1182 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997APh.....8....1D&db_key=AST},1183 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1184 }1185 1186 @ARTICLE{Aharonian:2004,1187 author = {{Aharonian}, F. and others},1188 title = "{Observations of 54 Active Galactic Nuclei with the HEGRA system of Cherenkov telescopes}",1189 journal = {\aap},1190 year = 2004,1191 month = jul,1192 volume = 421,1193 pages = {529-537},1194 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004A%26A...421..529A&db_key=AST},1195 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1196 }1197 1198 @ARTICLE{Pohl:2000,1199 author = {{Pohl}, M. and {Schlickeiser}, R.},1200 title = "{On the conversion of blast wave energy into radiation in active galactic nuclei and gamma-ray bursts}",1201 journal = {\aap},1202 year = 2000,1203 month = feb,1204 volume = 354,1205 pages = {395-410},1206 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2000A%26A...354..395P&db_key=AST},1207 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1208 }1209 1210 @ARTICLE{Mannheim:1993,1211 author = {{Mannheim}, K.},1212 title = "{The proton blazar}",1213 journal = {\aap},1214 year = 1993,1215 month = mar,1216 volume = 269,1217 pages = {67-76},1218 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1993A%26A...269...67M&db_key=AST},1219 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1220 }1221 1222 # CHECK AGAIN!1223 @INPROCEEDINGS{Sikora:2001,1224 author = {{Sikora}, M.},1225 title = "{Jets in Quasars}",1226 booktitle = {ASP Conf. Ser. 227: Blazar Demographics and Physics},1227 year = 2001,1228 pages = {95-+},1229 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2001ASPC..227...95S&db_key=AST},1230 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1231 }1232 1233 @ARTICLE{Sikora:1987,1234 author = {{Sikora}, M. and {Kirk}, J.~G. and {Begelman}, M.~C. and {Schneider}, P.1235 },1236 title = "{Electron injection by relativistic protons in active galactic nuclei}",1237 journal = {\apjl},1238 year = 1987,1239 month = sep,1240 volume = 320,1241 pages = {L81-L85},1242 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1987ApJ...320L..81S&db_key=AST},1243 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1244 }1245 1246 # CHECK AGAIN1247 @ARTICLE{Burns:1982,1248 author = {{Burns}, M.~L. and {Lovelace}, R.~V.~E.},1249 title = "{Theory of electron-positron showers in double radio sources}",1250 journal = {\apj},1251 year = 1982,1252 month = nov,1253 volume = 262,1254 pages = {87-99},1255 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1982ApJ...262...87B&db_key=AST},1256 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1257 }1258 1259 @ARTICLE{Svensson:1987,1260 author = {{Svensson}, R.},1261 title = "{Non-thermal pair production in compact X-ray sources - First-order Compton cascades is soft radiation fields}",1262 journal = {\mnras},1263 year = 1987,1264 month = jul,1265 volume = 227,1266 pages = {403-451},1267 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1987MNRAS.227..403S&db_key=AST},1268 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1269 }1270 1271 @BOOK{Berezinskii:1990,1272 author = {{Berezinskii}, V.~S. and {Bulanov}, S.~V. and {Dogiel}, V.~A. and1273 {Ptuskin}, V.~S.},1274 title = "{Astrophysics of cosmic rays}",1275 publisher = {Amsterdam: North-Holland, 1990, edited by Ginzburg, V.L.},1276 year = 1990,1277 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1990acr..book.....B&db_key=AST},1278 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1279 }1280 1281 @ARTICLE{Mannheim:1991,1282 author = {{Mannheim}, K. and {Biermann}, P.~L. and {Kruells}, W.~M.},1283 title = "{A novel mechanism for nonthermal X-ray emission}",1284 journal = {\aap},1285 year = 1991,1286 month = nov,1287 volume = 251,1288 pages = {723-731},1289 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1991A%26A...251..723M&db_key=AST},1290 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1291 }1292 1293 @INPROCEEDINGS{Mannheim:1997,1294 author = {{Mannheim}, K.},1295 title = "{AGN Models: High-Energy Emission.}",1296 booktitle = {Very High Energy Phenomena in the Universe; Moriond Workshop},1297 year = 1997,1298 pages = {17-+},1299 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997vhep.conf...17M&db_key=AST},1300 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1301 }1302 1303 @ARTICLE{Mannheim:1998,1304 author = {{Mannheim}, K.},1305 title = "{Possible Production of High-Energy Gamma Rays from Proton Acceleration in the Extragalactic Radio Source Markarian 501}",1306 journal = {Science},1307 year = 1998,1308 month = jan,1309 volume = 279,1310 pages = {684-+},1311 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998Sci...279..684M&db_key=AST},1312 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1313 }1314 1315 @ARTICLE{Hauser:2001,1316 author = {{Hauser}, M.~G. and {Dwek}, E.},1317 title = "{The Cosmic Infrared Background: Measurements and Implications}",1318 journal = {\araa},1319 year = 2001,1320 volume = 39,1321 pages = {249-307},1322 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2001ARA%26A..39..249H&db_key=AST},1323 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1324 }1325 1326 # TO BE CHECKED!1327 @ARTICLE{Perlman:1998,1328 author = {{Perlman}, E.~S. and {Padovani}, P. and {Giommi}, P. and {Sambruna}, R. and1329 {Jones}, L.~R. and {Tzioumis}, A. and {Reynolds}, J.},1330 title = "{The Deep X-Ray Radio Blazar Survey. I. Methods and First Results}",1331 journal = {\aj},1332 year = 1998,1333 month = apr,1334 volume = 115,1335 pages = {1253-1294},1336 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998AJ....115.1253P&db_key=AST},1337 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1338 }1339 1340 @INPROCEEDINGS{Laurent-Muehleisen:1998,1341 author = {{Laurent-Muehleisen}, S.~A. and {Kollgaard}, R.~I. and {Feigelson}, E.~D.1342 },1343 title = "{The Rosat-Green Bank Sample of Intermediate BL Lac Objects}",1344 booktitle = {ASP Conf. Ser. 144: IAU Colloq. 164: Radio Emission from Galactic and Extragalactic Compact Sources},1345 year = 1998,1346 pages = {163-+},1347 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998ASPC..144..163L&db_key=AST},1348 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1349 }1350 1351 @ARTICLE{Caccianiga:1999,1352 author = {{Caccianiga}, A. and {Maccacaro}, T. and {Wolter}, A. and {della Ceca}, R. and1353 {Gioia}, I.~M.},1354 title = "{The REX Survey: A Search for Radio-emitting X-Ray Sources}",1355 journal = {\apj},1356 year = 1999,1357 month = mar,1358 volume = 513,1359 pages = {51-68},1360 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1999ApJ...513...51C&db_key=AST},1361 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1362 }1363 1364 @ARTICLE{Caccianiga:2004,1365 author = {{Caccianiga}, A. and {March{\~a}}, M.~J.~M.},1366 title = "{The CLASS blazar survey: testing the blazar sequence}",1367 journal = {\mnras},1368 year = 2004,1369 month = mar,1370 volume = 348,1371 pages = {937-954},1372 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004MNRAS.348..937C&db_key=AST},1373 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1374 }1375 1376 @ARTICLE{Kellermann:1989,1377 author = {{Kellermann}, K.~I. and {Sramek}, R. and {Schmidt}, M. and {Shaffer}, D.~B. and1378 {Green}, R.},1379 title = "{VLA observations of objects in the Palomar Bright Quasar Survey}",1380 journal = {\aj},1381 year = 1989,1382 month = oct,1383 volume = 98,1384 pages = {1195-1207},1385 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1989AJ.....98.1195K&db_key=AST},1386 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1387 }1388 1389 @ARTICLE{Rowan:1977,1390 author = {{Rowan-Robinson}, M.},1391 title = "{On the unity of activity in galaxies}",1392 journal = {\apj},1393 year = 1977,1394 month = may,1395 volume = 213,1396 pages = {635-647},1397 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1977ApJ...213..635R&db_key=AST},1398 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1399 }1400 1401 @ARTICLE{Lawrence:1982,1402 author = {{Lawrence}, A. and {Elvis}, M.},1403 title = "{Obscuration and the various kinds of Seyfert galaxies}",1404 journal = {\apj},1405 year = 1982,1406 month = may,1407 volume = 256,1408 pages = {410-426},1409 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1982ApJ...256..410L&db_key=AST},1410 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1411 }1412 1413 @ARTICLE{Giommi:1994,1414 author = {{Giommi}, P. and {Padovani}, P.},1415 title = "{Bl-Lacertae Reunification}",1416 journal = {\mnras},1417 year = 1994,1418 month = may,1419 volume = 268,1420 pages = {L51+},1421 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1994MNRAS.268L..51G&db_key=AST},1422 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1423 }1424 1425 @ARTICLE{Antonucci:1985,1426 author = {{Antonucci}, R.~R.~J. and {Ulvestad}, J.~S.},1427 title = "{Extended radio emission and the nature of blazars}",1428 journal = {\apj},1429 year = 1985,1430 month = jul,1431 volume = 294,1432 pages = {158-182},1433 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1985ApJ...294..158A&db_key=AST},1434 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1435 }1436 1437 @ARTICLE{Fossati:1998,1438 author = {{Fossati}, G. and {Maraschi}, L. and {Celotti}, A. and {Comastri}, A. and1439 {Ghisellini}, G.},1440 title = "{A unifying view of the spectral energy distributions of blazars}",1441 journal = {\mnras},1442 year = 1998,1443 month = sep,1444 volume = 299,1445 pages = {433-448},1446 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998MNRAS.299..433F&db_key=AST},1447 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1448 }1449 1450 @ARTICLE{Aharonian:2000,1451 author = {{Aharonian}, F.},1452 title = "{TeV gamma rays from BL Lac objects due to synchrotron radiation of extremely high energy protons}",1453 journal = {\na},1454 year = 2000,1455 month = nov,1456 volume = 5,1457 pages = {377-395},1458 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2000NewA....5..377A&db_key=AST},1459 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1460 }1461 1462 @ARTICLE{Muecke:2003,1463 author = {{M{\"u}cke}, A. and {Protheroe}, R.~J. and {Engel}, R. and {Rachen}, J.~P. and1464 {Stanev}, T.},1465 title = "{BL Lac objects in the synchrotron proton blazar model}",1466 journal = {Astroparticle Physics},1467 year = 2003,1468 month = mar,1469 volume = 18,1470 pages = {593-613},1471 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2003APh....18..593M&db_key=AST},1472 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1473 }1474 1475 @ARTICLE{Schlickeiser:2000,1476 author = {{Pohl}, M. and {Schlickeiser}, R.},1477 title = "{On the conversion of blast wave energy into radiation in active galactic nuclei and gamma-ray bursts}",1478 journal = {\aap},1479 year = 2000,1480 month = feb,1481 volume = 354,1482 pages = {395-410},1483 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2000A%26A...354..395P&db_key=AST},1484 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1485 }1486 1487 @ARTICLE{Lyutikov:2005,1488 author = {{Lyutikov}, M.},1489 title = "{Composition of ultra-relativistic jets}",1490 journal = {American Astronomical Society Meeting Abstracts},1491 year = 2005,1492 month = may,1493 volume = 206,1494 pages = {-+},1495 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2005AAS...206.3008L&db_key=AST},1496 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1497 }1498 1499 @ARTICLE{Sikora:2005,1500 author = {{Sikora}, M. and {Begelman}, M.~C. and {Madejski}, G.~M. and1501 {Lasota}, J.-P.},1502 title = "{Are Quasar Jets Dominated by Poynting Flux?}",1503 journal = {\apj},1504 year = 2005,1505 month = may,1506 volume = 625,1507 pages = {72-77},1508 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2005ApJ...625...72S&db_key=AST},1509 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1510 }1511 1512 @ARTICLE{Montigny:1995,1513 author = {{von Montigny}, C. and others},1514 title = "{High-Energy Gamma-Ray Emission from Active Galaxies: EGRET Observations and Their Implications}",1515 journal = {\apj},1516 year = 1995,1517 month = feb,1518 volume = 440,1519 pages = {525-+},1520 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1995ApJ...440..525V&db_key=AST},1521 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1522 }1523 1524 @ARTICLE{Fichtel:1994,1525 author = {{Fichtel}, C.~E. and others},1526 title = "{The first energetic gamma-ray experiment telescope (EGRET) source catalog}",1527 journal = {\apjs},1528 year = 1994,1529 month = oct,1530 volume = 94,1531 pages = {551-581},1532 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1994ApJS...94..551F&db_key=AST},1533 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1534 }1535 1536 @ARTICLE{Thompson:1995,1537 author = {{Thompson}, D.~J. and others},1538 title = "{The Second EGRET Catalog of High-Energy Gamma-Ray Sources}",1539 journal = {\apjs},1540 year = 1995,1541 month = dec,1542 volume = 101,1543 pages = {259-+},1544 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1995ApJS..101..259T&db_key=AST},1545 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1546 }1547 1548 @ARTICLE{Ghisellini:1989,1549 author = {{Ghisellini}, G. and {Maraschi}, L.},1550 title = "{Bulk acceleration in relativistic jets and the spectral properties of blazars}",1551 journal = {\apj},1552 year = 1989,1553 month = may,1554 volume = 340,1555 pages = {181-189},1556 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1989ApJ...340..181G&db_key=AST},1557 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1558 }1559 1560 @ARTICLE{Weekes:1996,1561 author = {{Weekes}, T.~C. and others},1562 title = "{Observations of gamma-ray sources at energies $>$300GeV.}",1563 journal = {\aaps},1564 year = 1996,1565 month = dec,1566 volume = 120,1567 pages = {C603+},1568 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996A%26AS..120C.603W&db_key=AST},1569 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1570 }1571 1572 @ARTICLE{Petry:1996,1573 author = {{Petry}, D. and others},1574 title = "{Detection of VHE {$\gamma$}-rays from MKN 421 with the HEGRA Cherenkov Telescopes.}",1575 journal = {\aap},1576 year = 1996,1577 month = jul,1578 volume = 311,1579 pages = {L13-L16},1580 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996A%26A...311L..13P&db_key=AST},1581 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1582 }1583 1584 @ARTICLE{Tavecchio:1998,1585 author = {{Tavecchio}, F. and {Maraschi}, L. and {Ghisellini}, G.},1586 title = "{Constraints on the Physical Parameters of TeV Blazars}",1587 journal = {\apj},1588 year = 1998,1589 month = dec,1590 volume = 509,1591 pages = {608-619},1592 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998ApJ...509..608T&db_key=AST},1593 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1594 }1595 1596 @ARTICLE{Bloom:1993,1597 author = {{Bloom}, S.~D. and {Marscher}, A.~P. and {Gear}, W.~K.},1598 title = "{Multiwavelength Observations of Flat Radio Spectrum Quasars and Active Galaxies}",1599 journal = {\baas},1600 year = 1993,1601 month = may,1602 volume = 25,1603 pages = {920-+},1604 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1993AAS...182.7007B&db_key=AST},1605 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1606 }1607 1608 @ARTICLE{Schmidt:1963,1609 author = {{Schmidt}, M.},1610 title = "{3C 273: a star-like object with large red-shift.}",1611 journal = {\nat},1612 year = 1963,1613 volume = 197,1614 pages = {1040-1040},1615 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1963Natur.197.1040S&db_key=AST},1616 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1617 }1618 1619 @ARTICLE{Ghisellini:1994,1620 author = {Ghisellini, G. and Maraschi, L.},1621 title = {Are $\gamma$-rays from {HPQ}s and {BL} {L}acs due to the same process?},1622 booktitle = {Proceedings of the Second Compton Symposium},1623 journal = {AIP Conf. Proc.},1624 pages = 616,1625 year = 1994,1626 volume = 304,1627 }1628 1629 @ARTICLE{Dermer:1993,1630 author = {{Dermer}, C.~D. and {Schlickeiser}, R.},1631 title = "{Model for the High-Energy Emission from Blazars}",1632 journal = {\apj},1633 year = 1993,1634 month = oct,1635 volume = 416,1636 pages = {458-+},1637 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1993ApJ...416..458D&db_key=AST},1638 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1639 }1640 1641 @ARTICLE{Dermer:2002,1642 author = {{Dermer}, C.~D.},1643 title = "{Neutrino, Neutron, and Cosmic-Ray Production in the External Shock Model of Gamma-Ray Bursts}",1644 journal = {\apj},1645 year = 2002,1646 month = jul,1647 volume = 574,1648 pages = {65-87},1649 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2002ApJ...574...65D&db_key=AST},1650 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1651 }1652 1653 @ARTICLE{Sikora:1994,1654 author = {{Sikora}, M. and {Begelman}, M.~C. and {Rees}, M.~J.},1655 title = "{Comptonization of diffuse ambient radiation by a relativistic jet: The source of gamma rays from blazars?}",1656 journal = {\apj},1657 year = 1994,1658 month = jan,1659 volume = 421,1660 pages = {153-162},1661 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1994ApJ...421..153S&db_key=AST},1662 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1663 }1664 1665 @ARTICLE{Blandford:1995,1666 author = {{Blandford}, R.~D. and {Levinson}, A.},1667 title = "{Pair cascades in extragalactic jets. 1: Gamma rays}",1668 journal = {\apj},1669 year = 1995,1670 month = mar,1671 volume = 441,1672 pages = {79-95},1673 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1995ApJ...441...79B&db_key=AST},1674 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1675 }1676 1677 @ARTICLE{Wagner:1995,1678 author = {{Wagner}, S.~J. and others},1679 title = "{High-Energy Gamma Rays from PKS 1406-076 and the Observation of Correlated Gamma-Ray and Optical Emission}",1680 journal = {\apjl},1681 year = 1995,1682 month = dec,1683 volume = 454,1684 pages = {L97+},1685 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1995ApJ...454L..97W&db_key=AST},1686 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1687 }1688 1689 @INPROCEEDINGS{Blandford:1978,1690 author = {{Blandford}, R.~D. and {Rees}, M.~J.},1691 title = "{Some comments on radiation mechanisms in Lacertids}",1692 booktitle = {Pittsburgh Conference on BL Lac Objects, Pittsburgh, Pa., April 24-26, 1978, Proceedings. (A79-30026 11-90) Pittsburgh, Pa., University of Pittsburgh, 1978, p. 328-341; Discussion, p. 341-347. NATO-supported research},1693 year = 1978,1694 pages = {328-341},1695 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1978bllo.conf..328B&db_key=AST},1696 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1697 }1698 1699 @ARTICLE{Bradbury:1997,1700 author = {{Bradbury}, S.~M. and others},1701 title = "{Detection of {$\gamma$}-rays above 1.5TeV from MKN 501.}",1702 journal = {\aap},1703 year = 1997,1704 month = apr,1705 volume = 320,1706 pages = {L5-L8},1707 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997A%26A...320L...5B&db_key=AST},1708 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1709 }1710 1711 @ARTICLE{Browne:1983,1712 author = {{Browne}, I.~W.~A.},1713 title = "{Is it possible to turn an elliptical radio galaxy into a BL Lac object?}",1714 journal = {\mnras},1715 year = 1983,1716 month = jul,1717 volume = 204,1718 pages = {23P-27P},1719 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1983MNRAS.204P..23B&db_key=AST},1720 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1721 }1722 1723 @ARTICLE{Celotti:2003,1724 author = {{Celotti}, A.},1725 title = "{On the energetics and composition of jets}",1726 journal = {\nar},1727 year = 2003,1728 month = oct,1729 volume = 47,1730 pages = {525-528},1731 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2003NewAR..47..525C&db_key=AST},1732 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1733 }1734 1735 @ARTICLE{Wardle:1984,1736 author = {{Wardle}, J.~F.~C. and {Moore}, R.~L. and {Angel}, J.~R.~P.},1737 title = "{The radio morphology of blazars and relationships to optical polarization and to normal radio galaxies}",1738 journal = {\apj},1739 year = 1984,1740 month = apr,1741 volume = 279,1742 pages = {93-98},1743 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1984ApJ...279...93W&db_key=AST},1744 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1745 }1746 1747 @ARTICLE{Lind:1985,1748 author = {{Lind}, K.~R. and {Blandford}, R.~D.},1749 title = "{Semidynamical models of radio jets - Relativistic beaming and source counts}",1750 journal = {\apj},1751 year = 1985,1752 month = aug,1753 volume = 295,1754 pages = {358-367},1755 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1985ApJ...295..358L&db_key=AST},1756 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1757 }1758 1759 @ARTICLE{Phinney:1986,1760 author = {{Phinney}},1761 title = {Astrophysics of {A}ctive {G}alaxies and {QSO}s},1762 publisher = {Oxford University Press},1763 editor = {R.W.Miller},1764 year = 1986,1765 page = 453,1766 }1767 1768 @ARTICLE{Fazio:1979,1769 author = {{Fazio}, G.~G. and {Stecker}, F.~W.},1770 year = 1979,1771 volume = 226,1772 pages = {135-+},1773 title = {Predicted High Energy Break in the Isotropic Gamma Ray Spectrum: a Test of Cosmological Origin},1774 journal = {\nat}1775 }1776 1777 @ARTICLE{Punch:1992,1778 author = {{Punch}, M. and others},1779 title = "{Detection of TeV photons from the active galaxy Markarian 421}",1780 journal = {\nat},1781 year = 1992,1782 month = aug,1783 volume = 358,1784 pages = {477-+},1785 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992Natur.358..477P&db_key=AST},1786 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1787 }1788 1789 @ARTICLE{Fanaroff:1974,1790 author = {{Fanaroff}, B.~L. and {Riley}, J.~M.},1791 title = "{The morphology of extragalactic radio sources of high and low luminosity}",1792 journal = {\mnras},1793 year = 1974,1794 month = may,1795 volume = 167,1796 pages = {31P-36P},1797 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1974MNRAS.167P..31F&db_key=AST},1798 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1799 }1800 1801 @ARTICLE{Odell:1974,1802 author = {{Jones}, T.~W. and {O'dell}, S.~L. and {Stein}, W.~A.},1803 title = "{Physics of Compact Nonthermal Sources. Theory of Radiation Processes}",1804 journal = {\apj},1805 year = 1974,1806 month = mar,1807 volume = 188,1808 pages = {353-368},1809 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1974ApJ...188..353J&db_key=AST},1810 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1811 }1812 1813 @ARTICLE{Ghisellini:1993,1814 author = {{Ghisellini}, G. and {Padovani}, P. and {Celotti}, A. and {Maraschi}, L.1815 },1816 title = "{Relativistic bulk motion in active galactic nuclei}",1817 journal = {\apj},1818 year = 1993,1819 month = apr,1820 volume = 407,1821 pages = {65-82},1822 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1993ApJ...407...65G&db_key=AST},1823 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1824 }1825 1826 @ARTICLE{Ghisellini:1998,1827 author = {{Ghisellini}, G. and {Celotti}, A. and {Fossati}, G. and {Maraschi}, L. and1828 {Comastri}, A.},1829 title = "{A theoretical unifying scheme for gamma-ray bright blazars}",1830 journal = {\mnras},1831 year = 1998,1832 month = dec,1833 volume = 301,1834 pages = {451-468},1835 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998MNRAS.301..451G&db_key=AST},1836 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1837 }1838 1839 @ARTICLE{Hillas:1984,1840 author = {{Hillas}, A.~M.},1841 title = "{The Origin of Ultra-High-Energy Cosmic Rays}",1842 journal = {\araa},1843 year = 1984,1844 volume = 22,1845 pages = {425-444},1846 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1984ARA%26A..22..425H&db_key=AST},1847 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1848 }1849 1850 @ARTICLE{Hoyle:1966,1851 author = {{Hoyle}, F. and {Burbidge}, G.~R. and {Sargent}, W.~L.~W.},1852 title = "{On the Nature of Quasi-Stellar Sources}",1853 journal = {\nat},1854 year = 1966,1855 volume = 209,1856 pages = {751-+},1857 adsurl = 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Astrophysics Data System}1882 }1883 1884 @ARTICLE{Kirk:1987,1885 author = {{Kirk}, J.~G. and {Schneider}, P.},1886 title = "{On the acceleration of charged particles at relativistic shock fronts}",1887 journal = {\apj},1888 year = 1987,1889 month = apr,1890 volume = 315,1891 pages = {425-433},1892 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1987ApJ...315..425K&db_key=AST},1893 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1894 }1895 1896 @ARTICLE{Kirk:1998,1897 author = {{Kirk}, J.~G. and {Rieger}, F.~M. and {Mastichiadis}, A.},1898 title = "{Particle acceleration and synchrotron emission in blazar jets}",1899 journal = {\aap},1900 year = 1998,1901 month = may,1902 volume = 333,1903 pages = {452-458},1904 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998A%26A...333..452K&db_key=AST},1905 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1906 }1907 1908 @ARTICLE{Lawrence:1987,1909 author = {{Lawrence}, A.},1910 title = "{Classification of active galaxies and the prospect of a unified phenomenology}",1911 journal = {\pasp},1912 year = 1987,1913 month = may,1914 volume = 99,1915 pages = {309-334},1916 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1987PASP...99..309L&db_key=AST},1917 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1918 }1919 1920 @ARTICLE{Padovani:1993,1921 author = {{Padovani}, P.},1922 title = "{The Radio Loud Fraction of QSOs and its Dependence on Magnitude and Redshift}",1923 journal = {\mnras},1924 year = 1993,1925 month = jul,1926 volume = 263,1927 pages = {461-+},1928 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1993MNRAS.263..461P&db_key=AST},1929 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1930 }1931 1932 @ARTICLE{LaFranca:1994,1933 author = {{La Franca}, F. and {Gregorini}, L. and {Cristiani}, S. and1934 {de Ruiter}, H. and {Owen}, F.},1935 title = "{Deep VLA observations of an optically selected sample of intermediate redshift QSOs and the optical luminosity function of the radio loud QSOs}",1936 journal = {\aj},1937 year = 1994,1938 month = nov,1939 volume = 108,1940 pages = {1548-1556},1941 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1994AJ....108.1548L&db_key=AST},1942 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1943 }1944 1945 @ARTICLE{DellaCeca:1994,1946 author = {{della Ceca}, R. and {Lamorani}, G. and {Maccacaro}, T. and1947 {Wolter}, A. and {Griffiths}, R. and {Stocke}, J.~T. and {Setti}, G.1948 },1949 title = "{The properties of X-ray selected active galactic nuclei. 3: The radio-quiet versus radio-loud samples}",1950 journal = {\apj},1951 year = 1994,1952 month = aug,1953 volume = 430,1954 pages = {533-544},1955 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1994ApJ...430..533D&db_key=AST},1956 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1957 }1958 1959 @ARTICLE{Pier:1992,1960 author = {{Pier}, E.~A. and {Krolik}, J.~H.},1961 title = "{Radiation-pressure-supported obscuring tori around active galactic nuclei}",1962 journal = {\apjl},1963 year = 1992,1964 month = nov,1965 volume = 399,1966 pages = {L23-L26},1967 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992ApJ...399L..23P&db_key=AST},1968 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1969 }1970 1971 @ARTICLE{Pier:1993,1972 author = {{Pier}, E.~A. and {Krolik}, J.~H.},1973 title = "{Infrared Spectra of Obscuring Dust Tori around Active Galactic Nuclei. II. Comparison with Observations}",1974 journal = {\apj},1975 year = 1993,1976 month = dec,1977 volume = 418,1978 pages = {673-+},1979 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1993ApJ...418..673P&db_key=AST},1980 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1981 }1982 1983 @ARTICLE{Sanders:1989,1984 author = {{Sanders}, D.~B. and {Phinney}, E.~S. and {Neugebauer}, G. and1985 {Soifer}, B.~T. and {Matthews}, K.},1986 title = "{Continuum energy distribution of quasars - Shapes and origins}",1987 journal = {\apj},1988 year = 1989,1989 month = dec,1990 volume = 347,1991 pages = {29-51},1992 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1989ApJ...347...29S&db_key=AST},1993 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}1994 }1995 1996 @ARTICLE{Ghisellini:1996a,1997 author = {{Ghisellini}, G. and {Madau}, P.},1998 title = "{On the origin of the gamma-ray emission in blazars}",1999 journal = {\mnras},2000 year = 1996,2001 month = may,2002 volume = 280,2003 pages = {67-76},2004 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996MNRAS.280...67G&db_key=AST},2005 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2006 }2007 2008 @ARTICLE{Costamante:2001,2009 author = {{Costamante}, L. and {Ghisellini}, G. and {Giommi}, P. and {Tagliaferri}, G. and2010 {Celotti}, A. and {Chiaberge}, M. and {Fossati}, G. and {Maraschi}, L. and2011 {Tavecchio}, F. and {Treves}, A. and {Wolter}, A.},2012 title = "{Extreme synchrotron BL Lac objects. Stretching the blazar sequence}",2013 journal = {\aap},2014 year = 2001,2015 month = may,2016 volume = 371,2017 pages = {512-526},2018 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2001A%26A...371..512C&db_key=AST},2019 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2020 }2021 2022 2023 @ARTICLE{Blandford:1979,2024 author = {{Blandford}, R.~D. and {K\"onigl}, A.},2025 title = "{Relativistic jets as compact radio sources}",2026 journal = {\apj},2027 year = 1979,2028 month = aug,2029 volume = 232,2030 pages = {34-48},2031 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1979ApJ...232...34B&db_key=AST},2032 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2033 }2034 2035 @ARTICLE{Ghisellini:1996b,2036 author = {{Ghisellini}, G. and {Maraschi}, L. and {Dondi}, L.},2037 title = "{Diagnostics of Inverse-Compton models for the {$\gamma$}-ray emission of 3C~279 and MKN 421.}",2038 journal = {\aaps},2039 year = 1996,2040 month = dec,2041 volume = 120,2042 pages = {C503+},2043 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996A%26AS..120C.503G&db_key=AST},2044 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2045 }2046 2047 @ARTICLE{Lamer:1996,2048 author = {{Lamer}, G. and {Brunner}, H. and {Staubert}, R.},2049 title = "{ROSAT observations of BL Lacertae objects.}",2050 journal = {\aap},2051 year = 1996,2052 month = jul,2053 volume = 311,2054 pages = {384-392},2055 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996A%26A...311..384L&db_key=AST},2056 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2057 }2058 2059 @ARTICLE{Blustin:2004,2060 author = {{Blustin}, A.~J. and {Page}, M.~J. and {Branduardi-Raymont}, G.2061 },2062 title = "{Intrinsic absorbers in BL Lac objects: The XMM-Newton view}",2063 journal = {\aap},2064 year = 2004,2065 month = apr,2066 volume = 417,2067 pages = {61-70},2068 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2004A%26A...417...61B&db_key=AST},2069 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2070 }2071 2072 @ARTICLE{Spergel:2006,2073 author = {{Spergel}, D.~N. and others},2074 title = "{Three Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Implications for cosmology}",2075 journal = {in preparation},2076 year = 2006,2077 note= {\url{http://lambda.gsfc.nasa.gov/product/map/dr2/map_bibliography.cfm}}2078 }2079 2080 @ARTICLE{Weekes:1989,2081 author = {{Weekes}, T.~C. and {Cawley}, M.~F. and {Fegan}, D.~J. and {Gibbs}, K.~G. and2082 {Hillas}, A.~M. and {Kowk}, P.~W. and {Lamb}, R.~C. and {Lewis}, D.~A. and2083 {Macomb}, D. and {Porter}, N.~A. and {Reynolds}, P.~T. and {Vacanti}, G.2084 },2085 title = "{Observation of TeV gamma rays from the Crab nebula using the atmospheric Cerenkov imaging technique}",2086 journal = {\apj},2087 year = 1989,2088 month = jul,2089 volume = 342,2090 pages = {379-395},2091 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1989ApJ...342..379W&db_key=AST},2092 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2093 }2094 2095 @ARTICLE{Morrison:1958,2096 author = {Morrison, P.},2097 title = {On Gamma-Ray Astronomy},2098 journal = {Il nuovo cimento},2099 year = 1958,2100 volume = {Vol.\,VII, N.\,6},2101 }2102 2103 @ARTICLE{Blasi:2005,2104 author = {{Blasi}, P. and {Vietri}, M.},2105 title = "{On Particle Acceleration around Shocks. II. A Fully General Method for Arbitrary Shock Velocities and Scattering Media}",2106 journal = {\apj},2107 year = 2005,2108 month = jun,2109 volume = 626,2110 pages = {877-886},2111 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2005ApJ...626..877B&db_key=AST},2112 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2113 }2114 2115 @ARTICLE{Blandford:1982,2116 author = {{Blandford}, R.~D. and {Payne}, D.~G.},2117 title = "{Hydromagnetic flows from accretion discs and the production of radio jets}",2118 journal = {\mnras},2119 year = 1982,2120 month = jun,2121 volume = 199,2122 pages = {883-903},2123 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1982MNRAS.199..883B&db_key=AST},2124 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2125 }2126 2127 @INPROCEEDINGS{Hillas:1983,2128 author = {{Hillas}, A.~M.},2129 title = "{Ultra high energy cosmic rays}",2130 booktitle = {NATO ASIC Proc. 107: Composition and Origin of Cosmic Rays},2131 year = 1983,2132 pages = {125-148},2133 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1983cocr.proc..125H&db_key=AST},2134 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2135 }2136 2137 @PROCEEDINGS{Holt:1992,2138 editor = {{Holt}, S.~S. and {Neff}, S.~G. and {Urry}, C.~M.},2139 title = "{Testing the AGN paradigm; Proceedings of the 2nd Annual Topical Astrophysics Conference, Univ. of Maryland, College Park, Oct. 14-16, 1991}",2140 booktitle = {American Institute of Physics Conference Series},2141 year = 1992,2142 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992AIPC..254.....H&db_key=AST},2143 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2144 }2145 2146 @BOOK{Heitler:1957,2147 author = {{Heitler}, W.},2148 title = "{Quantum theory of radiation}",2149 publisher = {International Series of Monographs on Physics, Oxford: Clarendon, 1954, 3rd ed.},2150 year = 1954,2151 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1954qtr..book.....H&db_key=AST},2152 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2153 }2154 2155 @ARTICLE{Halzen:1992b,2156 author = {{Halzen}, F.},2157 title = "{Gamma-Ray Astronomy - Catching Photons from Hell}",2158 journal = {\nat},2159 year = 1992,2160 month = aug,2161 volume = 358,2162 pages = {452-+},2163 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992Natur.358..452H&db_key=AST},2164 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2165 }2166 2167 @ARTICLE{Halzen:1991,2168 author = {{Halzen}, F. and {Zas}, E. and {MacGibbon}, J.~H. and {Weekes}, T.~C.2169 },2170 title = "{Gamma rays and energetic particles from primordial black holes}",2171 journal = {\nat},2172 year = 1991,2173 month = oct,2174 volume = 353,2175 pages = {807-815},2176 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1991Natur.353..807H&db_key=AST},2177 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2178 }2179 2180 @ARTICLE{Halzen:1992,2181 author = {{Halzen}, F. and {Zas}, E.},2182 title = "{Giant horizontal air showers. Implications for AGN neutrino fluxes}",2183 journal = {Physics Letters B},2184 year = 1992,2185 month = sep,2186 volume = 289,2187 pages = {184-188},2188 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992PhLB..289..184H&db_key=PHY},2189 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2190 }2191 2192 @PROCEEDINGS{Stenger:1992,2193 editor = {{Stenger}, V.~J. and {Learned}, J.~G. and {Pakvasa}, S. and2194 {Tata}, X.},2195 title = "{High Energy Neutrino Astrophysics}",2196 booktitle = {High Energy Neutrino Astrophysics},2197 year = 1992,2198 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992hena.conf.....S&db_key=AST},2199 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2200 }2201 2202 @INPROCEEDINGS{Cassiday:1989,2203 author = {{Cassiday}, G.~L. and {et al.}},2204 title = "{Neutrino Detection with the High Resolution Eye}",2205 booktitle = {Particle Astrophysics: Forefront Experimental Issues},2206 year = 1989,2207 pages = {259-+},2208 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1989pafe.conf..259C&db_key=AST},2209 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2210 }2211 2212 @INPROCEEDINGS{Pian:1997,2213 author = {{Pian}, E. and {Vacanti}, G. and {Tagliaferri}, G. and {Ghisellini}, G. and2214 {Maraschi}, L. and {Treves}, A. and {Urry}, C.~M. and {Fiore}, F. and2215 {Giommi}, P. and {Palazzi}, E. and {Chiappetti}, L. and {Sambruna}, R.~M.2216 },2217 title = "{BeppoSAX Monitoring of the BL Lac MKN 501}",2218 booktitle = {Proceedings of the Fourth Compton Symposium},2219 journal = {AIP Conf. Proc.},2220 year = 1997,2221 volume = 410,2222 pages = {1412-+},2223 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997AIPC..410.1412P&db_key=AST},2224 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2225 }2226 2227 @ARTICLE{Giommi:2000,2228 author = {{Giommi}, P. and {Padovani}, P. and {Perlman}, E.},2229 title = "{Detection of exceptional X-ray spectral variability in the TeV BL Lac 1ES 2344+514}",2230 journal = {\mnras},2231 year = 2000,2232 month = oct,2233 volume = 317,2234 pages = {743-749},2235 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2000MNRAS.317..743G&db_key=AST},2236 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2237 }2238 2239 @ARTICLE{Hartman:1999,2240 author = {{Hartman}, R.~C. and others},2241 title = "{The Third EGRET Catalog of High-Energy Gamma-Ray Sources}",2242 journal = {\apjs},2243 year = 1999,2244 month = jul,2245 volume = 123,2246 pages = {79-202},2247 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1999ApJS..123...79H&db_key=AST},2248 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2249 }2250 2251 @ARTICLE{Feldman:1998,2252 author = {{Feldman}, G.~J. and {Cousins}, R.~D.},2253 title = "{Unified approach to the classical statistical analysis of small signals}",2254 journal = {\prd},2255 year = 1998,2256 month = apr,2257 volume = 57,2258 pages = {3873-3889},2259 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998PhRvD..57.3873F&db_key=PHY},2260 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2261 }2262 2263 @ARTICLE{Inoue:1996,2264 author = {{Inoue}, S. and {Takahara}, F.},2265 title = "{Electron Acceleration and Gamma-Ray Emission from Blazars}",2266 journal = {\apj},2267 year = 1996,2268 month = jun,2269 volume = 463,2270 pages = {555-+},2271 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996ApJ...463..555I&db_key=AST},2272 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2273 }2274 2275 @ARTICLE{Chiaberge:1997,2276 author = {{Chiaberge}, M. and {Ghisellini}, G.},2277 title = "{Time dependent spectra of blazars}",2278 journal = {Memorie della Societa Astronomica Italiana},2279 year = 1997,2280 volume = 68,2281 pages = {191-+},2282 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997MmSAI..68..191C&db_key=AST},2283 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2284 }2285 2286 @ARTICLE{Mastichiadis:1997,2287 author = {{Mastichiadis}, A. and {Kirk}, J.~G.},2288 title = "{Variability in the synchrotron self-Compton model of blazar emission.}",2289 journal = {\aap},2290 year = 1997,2291 month = apr,2292 volume = 320,2293 pages = {19-25},2294 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997A%26A...320...19M&db_key=AST},2295 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2296 }2297 2298 @INPROCEEDINGS{Marscher:1996a,2299 author = {{Marscher}, A.~P.},2300 title = "{The Inner Jets of Blazars}",2301 booktitle = {ASP Conf. Ser. 100: Energy Transport in Radio Galaxies and Quasars},2302 year = 1996,2303 editor = {{Hardee}, P.~E. and {Bridle}, A.~H. and {Zensus}, J.~A.},2304 pages = {45-+},2305 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996ASPC..100...45M&db_key=AST},2306 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2307 }2308 2309 @ARTICLE{Marscher:1996b,2310 author = {{Marscher}, A.~P. and {Travis}, J.~P.},2311 title = "{Synchrotron self-Compton interpretation of multiwaveband observations of gamma-ray bright blazars.}",2312 journal = {\aaps},2313 year = 1996,2314 month = dec,2315 volume = 120,2316 pages = {C537+},2317 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1996A%26AS..120C.537M&db_key=AST},2318 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2319 }2320 2321 @ARTICLE{Maraschi:1992,2322 author = {{Maraschi}, L. and {Ghisellini}, G. and {Celotti}, A.},2323 title = "{A jet model for the gamma-ray emitting blazar 3C~279}",2324 journal = {\apjl},2325 year = 1992,2326 month = sep,2327 volume = 397,2328 pages = {L5-L9},2329 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1992ApJ...397L...5M&db_key=AST},2330 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2331 }2332 2333 @ARTICLE{Giommi:1999,2334 author = {{Giommi}, P. and {Menna}, M.~T. and {Padovani}, P.},2335 title = "{The sedentary multifrequency survey - I. Statistical identification and cosmological properties of high-energy peaked BL Lacs}",2336 journal = {\mnras},2337 year = 1999,2338 month = dec,2339 volume = 310,2340 pages = {465-475},2341 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1999MNRAS.310..465G&db_key=AST},2342 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2343 }2344 2345 @ARTICLE{Padovani:2003,2346 author = {{Padovani}, P. and {Perlman}, E.~S. and {Landt}, H. and {Giommi}, P. and2347 {Perri}, M.},2348 title = "{What Types of Jets Does Nature Make? A New Population of Radio Quasars}",2349 journal = {\apj},2350 year = 2003,2351 month = may,2352 volume = 588,2353 pages = {128-142},2354 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2003ApJ...588..128P&db_key=AST},2355 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2356 }2357 2358 @ARTICLE{Giommi:2005b,2359 author = {{Giommi}, P. and {Piranomonte}, S. and {Perri}, M. and {Padovani},P.2360 },2361 title = "{The sedentary survey of extreme high energy peaked BL Lacs}",2362 journal = {\aap},2363 year = 2005,2364 month = apr,2365 volume = 434,2366 pages = {385-396},2367 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2005A%26A...434..385G&db_key=AST},2368 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2369 }2370 2371 @ARTICLE{Nieppola:2006,2372 author = {{Nieppola}, E. and {Tornikoski}, M. and {Valtaoja}, E.},2373 title = "{Spectral energy distributions of a large sample of BL Lacertae objects}",2374 journal = {\aap},2375 year = 2006,2376 month = jan,2377 volume = 445,2378 pages = {441-450},2379 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=2006A%26A...445..441N&db_key=AST},2380 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2381 }2382 2383 @ARTICLE{Gould:1965,2384 author = {{Gould}, R.~J.},2385 title = "{High-Energy Photons from the Compton-Synchrotron Process in the Crab Nebula}",2386 journal = {\prl},2387 year = 1965,2388 month = oct,2389 volume = 15,2390 pages = {577-579},2391 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1965PhRvL..15..577G&db_key=PHY},2392 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2393 }2394 2395 @ARTICLE{Lamb:1997,2396 author = {{Lamb}, R.~C. and {Macomb}, D.~J.},2397 title = "{Point Sources of GeV Gamma Rays}",2398 journal = {\apj},2399 year = 1997,2400 month = oct,2401 volume = 488,2402 pages = {872-+},2403 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1997ApJ...488..872L&db_key=AST},2404 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2405 }2406 2407 @ARTICLE{Buckley:1998,2408 author = {{Buckley}, J.~H.},2409 title = "{ASTROPHYSICS: What the Wild Things Are}",2410 journal = {Science},2411 year = 1998,2412 month = jan,2413 volume = 279,2414 pages = {676-+},2415 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1998Sci...279..676B&db_key=AST},2416 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2417 }2418 2419 @INPROCEEDINGS{Dermer:1994,2420 author = {Dermer, C.~D.},2421 booktitle = "{NATO Advanced Study Institute: The Gamma-Ray Sky}",2422 year = 1994,2423 publisher = {Dodrecht: Kluwer Academic},2424 pages = {39}2425 }2426 2427 @ARTICLE{Rees:1966,2428 author = {{Rees}, M.~J.},2429 title = "{Appearance of Relativistically Expanding Radio Sources}",2430 journal = {\nat},2431 year = 1966,2432 volume = 211,2433 pages = {468-+},2434 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1966Natur.211..468R&db_key=AST},2435 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2436 }2437 2438 @ARTICLE{Rees:1966b,2439 author = {{Rees}, M.~J. and {Sciama}, D.~W.},2440 title = "{Inverse Compton Effect in Quasars}",2441 journal = {\nat},2442 year = 1966,2443 volume = 211,2444 pages = {805-+},2445 adsurl = {http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?bibcode=1966Natur.211..805R&db_key=AST},2446 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2447 }2448 2449 @ARTICLE{n/a,2450 author = {n/a},2451 title = {n/a},2452 journal = {n/a},2453 year = 02454 }2455 2456 ----------------------------------------------------------------------------------2457 2458 \bibitem{Magic-PMT}2459 A.~Ostankov et~al.,2460 \newblock {\em A study of the new hemispherical 6-dynodes PMT from electron2461 tubes},2462 \newblock Nucl. 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Sci. {\bf 49} (2002) 2497.2486 2487 \bibitem{MC_timing_Indians}2488 V.~R. {Chitnis} and P.~N. {Bhat},2489 \newblock {\em {Possible discrimination between gamma rays and hadrons using2490 {\v C}erenkov photon timing measurements}},2491 \newblock Astroparticle Physics {\bf 15} (2001) 29.2492 2493 -----------------------------------------------------------------------------------2494 2495 @ARTICLE{Aharonian:2006,2496 author = {{Aharonian}, F. and others},2497 title = "{The H.E.S.S.\ Survey of the Inner Galaxy in Very High Energy Gamma Rays}",2498 journal = {\apj},2499 year = 2006,2500 month = jan,2501 volume = 636,2502 pages = {777-797},2503 adsurl = {http://cdsads.u-strasbg.fr/abs/2006ApJ...636..777A},2504 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2505 }2506 2507 @ARTICLE{Paneque:2004,2508 author = {{Paneque}, D. and {Gebauer}, H.~J. and {Lorenz}, E. and {Mirzoyan}, R.2509 },2510 title = "{A method to enhance the sensitivity of photomultipliers for Air Cherenkov Telescopes by applying a lacquer that scatters light}",2511 journal = {Nuclear Instruments and Methods in Physics Research A},2512 year = 2004,2513 month = feb,2514 volume = 518,2515 pages = {619-621},2516 adsurl = {http://cdsads.u-strasbg.fr/abs/2004NIMPA.518..619P},2517 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2518 }2519 2520 @ARTICLE{Milagro:2007,2521 author = {{Abdo}, A.~A. and others},2522 title = "{TeV Gamma-Ray Sources from a Survey of the Galactic Plane with Milagro}",2523 journal = {ArXiv e-prints},2524 eprint = {0705.0707},2525 year = 2007,2526 month = may,2527 volume = 705,2528 adsurl = {http://cdsads.u-strasbg.fr/abs/2007arXiv0705.0707A},2529 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2530 }2531 2532 @ARTICLE{Rieger:2000,2533 author = {{Rieger}, F.~M. and {Mannheim}, K.},2534 title = "{Implications of a possible 23 day periodicity for binary black hole models in Mkn 501}",2535 journal = {\aap},2536 eprint = {arXiv:astro-ph/0005478},2537 year = 2000,2538 month = jul,2539 volume = 359,2540 pages = {948-952},2541 adsurl = {http://cdsads.u-strasbg.fr/abs/2000A%26A...359..948R},2542 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2543 }2544 2545 @INPROCEEDINGS{Rieger:2001,2546 author = {{Rieger}, F.~M. and {Mannheim}, K.},2547 title = "{A Possible Black Hole Binary in Mkn 501}",2548 booktitle = {American Institute of Physics Conference Series},2549 year = 2001,2550 volume = 558,2551 editor = {{Aharonian}, F.~A. and {V{\"o}lk}, H.~J.},2552 pages = {716-+},2553 adsurl = {http://cdsads.u-strasbg.fr/abs/2001AIPC..558..716R},2554 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2555 }2556 2557 @ARTICLE{Rieger:2003,2558 author = {{Rieger}, F.~M. and {Mannheim}, K.},2559 title = "{On the central black hole mass in Mkn 501}",2560 journal = {\aap},2561 eprint = {arXiv:astro-ph/0210326},2562 year = 2003,2563 month = jan,2564 volume = 397,2565 pages = {121-125},2566 adsurl = {http://cdsads.u-strasbg.fr/abs/2003A%26A...397..121R},2567 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2568 }2569 2570 @ARTICLE{Blandford,2571 author = {{Blandford}, R.~D. and {K\"onigl}, A.},2572 title = {Relativistic jets as compact radio sources},2573 journal = {\apj},2574 year = 1979,2575 month = aug,2576 volume = 232,2577 pages = {34-48},2578 adsurl = {http://cdsads.u-strasbg.fr/abs/1979ApJ...232...34B},2579 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2580 }2581 2582 @ARTICLE{Dermer,2583 author = {{Dermer}, C.~D. and {Schlickeiser}, R. and {Mastichiadis}, A.},2584 title = {High-energy gamma radiation from extragalactic radio sources},2585 journal = {\aap},2586 year = 1992,2587 month = mar,2588 volume = 256,2589 pages = {L27-L30},2590 adsurl = {http://cdsads.u-strasbg.fr/abs/1992A%26A...256L..27D},2591 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2592 }2593 2594 @ARTICLE{Begelman,2595 author = {{Begelman}, M.~C. and {Fabian}, A.~C. and {Rees}, M.~J.},2596 title = "{Implications of very rapid TeV variability in blazars}",2597 journal = {ArXiv e-prints},2598 eprint = {0709.0540},2599 year = 2007,2600 month = sep,2601 volume = 709,2602 adsurl = {http://cdsads.u-strasbg.fr/abs/2007arXiv0709.0540B},2603 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2604 }2605 2606 @ARTICLE{Meszaros,2607 author = {{Meszaros}, P. and {Rees}, M.~J.},2608 title = {Gamma-Ray Bursts: Multiwaveband Spectral Predictions for Blast Wave Models},2609 journal = {\apjl},2610 eprint = {arXiv:astro-ph/9309011},2611 year = 1993,2612 month = dec,2613 volume = 418,2614 pages = {L59+},2615 adsurl = {http://cdsads.u-strasbg.fr/abs/1993ApJ...418L..59M},2616 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2617 }2618 2619 @ARTICLE{Rachen,2620 author = {{Rachen}, J.~P. and {Biermann}, P.~L.},2621 title = {{E}xtragalactic {U}ltra-{H}igh {E}nergy {C}osmic-{R}ays - {P}art {O}ne - {C}ontribution from {H}ot {S}pots in {Fr-II} {R}adio {G}alaxies},2622 journal = {\aap},2623 eprint = {arXiv:astro-ph/9301010},2624 year = 1993,2625 month = may,2626 volume = 272,2627 pages = {161-+},2628 adsurl = {http://cdsads.u-strasbg.fr/abs/1993A%26A...272..161R},2629 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2630 }2631 2632 @INPROCEEDINGS{Mannheim:1999,2633 author = {{Mannheim}, K.},2634 title = {Frontiers in High-Energy Astroparticle Physics},2635 booktitle = {Reviews in Modern Astronomy},2636 year = 1999,2637 volume = 12,2638 editor = {{Schielicke}, R.~E.},2639 pages = {167-+},2640 adsurl = {http://cdsads.u-strasbg.fr/abs/1999RvMA...12..167M},2641 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2642 }2643 2644 @ARTICLE{Blazejowski,2645 author = {{B{\l}a{\.z}ejowski}, M. and others},2646 title = "{A Multiwavelength View of the TeV Blazar Markarian 421: Correlated Variability, Flaring, and Spectral Evolution}",2647 journal = {\apj},2648 eprint = {arXiv:astro-ph/0505325},2649 year = 2005,2650 month = sep,2651 volume = 630,2652 pages = {130-141},2653 adsurl = {http://cdsads.u-strasbg.fr/abs/2005ApJ...630..130B},2654 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2655 }2656 2657 @ARTICLE{Rieger:2007,2658 author = {{Rieger}, F.~M.},2659 title = {Supermassive binary black holes among cosmic gamma-ray sources},2660 journal = {\apss},2661 eprint = {arXiv:astro-ph/0611224},2662 year = 2007,2663 month = jun,2664 volume = 309,2665 pages = {271-275},2666 adsurl = {http://cdsads.u-strasbg.fr/abs/2007Ap%26SS.309..271R},2667 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2668 }2669 2670 @INPROCEEDINGS{Kranich,2671 author = {{Kranich}, D.},2672 title = {Evidence for a {QPO} structure in the {TeV} and X-ray light curve during the 1997 high state {$\gamma$} emission of {Mkn}\,501},2673 booktitle = {International Cosmic Ray Conference},2674 year = 1999,2675 volume = 3,2676 month = aug,2677 pages = {358-+},2678 adsurl = {http://cdsads.u-strasbg.fr/abs/1999ICRC....3..358K},2679 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2680 }2681 2682 @ARTICLE{Osone,2683 author = {{Osone}, S.},2684 title = "{Study of 23 day periodicity of Blazar Mkn501 in 1997}",2685 journal = {Astroparticle Physics},2686 eprint = {arXiv:astro-ph/0506328},2687 year = 2006,2688 month = oct,2689 volume = 26,2690 pages = {209-218},2691 adsurl = {http://cdsads.u-strasbg.fr/abs/2006APh....26..209O},2692 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2693 }2694 2695 @ARTICLE{Rieger:2003,2696 author = {{Rieger}, F.~M. and {Mannheim}, K.},2697 title = {On the central black hole mass in Mkn 501},2698 journal = {\aap},2699 eprint = {arXiv:astro-ph/0210326},2700 year = 2003,2701 month = jan,2702 volume = 397,2703 pages = {121-125},2704 adsurl = {http://cdsads.u-strasbg.fr/abs/2003A%26A...397..121R},2705 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2706 }2707 2708 @ARTICLE{Hong,2709 author = {{Hong}, X.~Y. and others},2710 title = "{A relativistic helical jet in the {$\gamma$}-ray AGN 1156+295}",2711 journal = {\aap},2712 eprint = {arXiv:astro-ph/0401627},2713 year = 2004,2714 month = apr,2715 volume = 417,2716 pages = {887-904},2717 adsurl = {http://cdsads.u-strasbg.fr/abs/2004A%26A...417..887H},2718 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2719 }2720 2721 @ARTICLE{Aharonian:2006,2722 author = {{Aharonian}, F. and others},2723 title = "{The H.E.S.S.\ Survey of the Inner Galaxy in Very High Energy Gamma Rays}",2724 journal = {\apj},2725 year = 2006,2726 month = jan,2727 volume = 636,2728 pages = {777-797},2729 adsurl = {http://cdsads.u-strasbg.fr/abs/2006ApJ...636..777A},2730 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2731 }2732 2733 @MASTERSTHESIS{Meyer:Diploma,2734 author = {Meyer, M.},2735 title = {{K}alibrierung des {MAGIC}-{T}eleskops mit {M}yonen},2736 school = {Bayerische Julius-Maximilians-Universit{\"a}t W{\"u}rzburg},2737 year = {2004}2738 }2739 2740 @INPROCEEDINGS{Bretz:2003drive,2741 author = {Bretz, T. and Dorner, D. and Wagner, R. M.},2742 title = "{The tracking system of the MAGIC telescope}",2743 booktitle = {$28^{th}$ International Cosmic Ray Conference},2744 year = 2003,2745 }2746 2747 @MASTERSTHESIS{Riegel:Diploma,2748 author = {Riegel, B.},2749 title = {{S}ystematische {U}ntersuchung der {B}ildparameter f\"ur das {MAGIC}-{T}eleskop},2750 school = {Bayerische Julius-Maximilians-Universit{\"a}t W{\"u}rzburg},2751 year = {2005}2752 }2753 2754 2755 @ARTICLE{Milagro:2007,2756 author = {{Abdo}, A.~A. and others},2757 title = "{TeV Gamma-Ray Sources from a Survey of the Galactic Plane with Milagro}",2758 journal = {ArXiv e-prints},2759 eprint = {0705.0707},2760 year = 2007,2761 month = may,2762 volume = 705,2763 adsurl = {http://cdsads.u-strasbg.fr/abs/2007arXiv0705.0707A},2764 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2765 }2766 2767 @ARTICLE{Curtef:CM,2768 author = {{Curtef}, V. and {Backes}, M. and {Hadasch}, D.},2769 title = "{Improvements of the energy reconstruction for the MAGIC telescope by means of analysis and Monte Carlo techniques}",2770 journal = {Astronomische Nachrichten},2771 eprint = {0711.2256},2772 year = 2007,2773 volume = 328,2774 number = 7,2775 }2776 2777 @INPROCEEDINGS{Rieger:2001,2778 author = {{Rieger}, F.~M. and {Mannheim}, K.},2779 title = "{A Possible Black Hole Binary in Mkn 501}",2780 booktitle = {American Institute of Physics Conference Series},2781 year = 2001,2782 volume = 558,2783 editor = {{Aharonian}, F.~A. and {V{\"o}lk}, H.~J.},2784 pages = {716-+},2785 adsurl = {http://cdsads.u-strasbg.fr/abs/2001AIPC..558..716R},2786 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2787 }2788 2789 @ARTICLE{Rieger:2003,2790 author = {{Rieger}, F.~M. and {Mannheim}, K.},2791 title = "{On the central black hole mass in Mkn 501}",2792 journal = {\aap},2793 eprint = {arXiv:astro-ph/0210326},2794 year = 2003,2795 month = jan,2796 volume = 397,2797 pages = {121-125},2798 adsurl = {http://cdsads.u-strasbg.fr/abs/2003A%26A...397..121R},2799 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2800 }2801 2802 @ARTICLE{Aharonian:2007pks,2803 author = {{Aharonian}, F. and others},2804 title = "{An Exceptional Very High Energy Gamma-Ray Flare of PKS 2155-304}",2805 journal = {\apjl},2806 eprint = {arXiv:0706.0797},2807 year = 2007,2808 month = aug,2809 volume = 664,2810 pages = {L71-L74},2811 adsurl = {http://cdsads.u-strasbg.fr/abs/2007ApJ...664L..71A},2812 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2813 }2814 2815 @MASTERSTHESIS{Haffke:Dipl,2816 author = {Haffke, M.},2817 title = "{Berechnung und Implementierung neuer Atmosph\"arenmodelle in die MAGIC-Monte-Carlo-Kette}",2818 school = {Universit{\"a}t Dortmund},2819 month = {Mar},2820 year = {2007}2821 }2822 2823 @MASTERSTHESIS{Dreyer:Dipl,2824 author = {Dreyer, J.},2825 title = {Hard- und {S}oftwareentwicklung im {R}ahmen der {E}xperimente {AMANDA} und {IceCube}},2826 school = {Universit{\"a}t Dortmund},2827 month = {Nov},2828 year = {2005}2829 }2830 2831 @MASTERSTHESIS{Refflinghaus:Dipl,2832 author = {Refflinghaus, F.},2833 title = "{Datenkompression der Photomultiplier-Signale des AMANDA-Neutrinodetektors}",2834 school = {Universit{\"a}t Dortmund},2835 month = {Nov},2836 year = {2005}2837 }2838 2839 @MASTERSTHESIS{Bartelt:Dipl,2840 author = {Bartelt, M.},2841 title = "{Test von alternativen Konzepten zur Hochspannungsversorgung des IceCube-Detektors}",2842 school = {Universit{\"a}t Dortmund},2843 month = {Dez},2844 year = {2004}2845 }2846 2847 @MASTERSTHESIS{Deeg:Dipl,2848 author = {Deeg, M.},2849 title = "{Prototypenentwicklung eines Detektorsystems f\"ur ultrahochenergetische Kosmische Strahlung}",2850 school = {Universit{\"a}t Dortmund},2851 month = {Feb},2852 year = {2003}2853 }2854 2855 @PHDTHESIS{Messarius:PhD,2856 author = {Messarius, T.},2857 title = {Entwurf und Realisation des AMANDA Softwaretriggers f\"ur das TWR Datenauslese System},2858 school = {Universit{\"a}t Dortmund},2859 month = {Aug},2860 year = {2003}2861 }2862 2863 @PHDTHESIS{Wagner:PhD,2864 author = {Wagner, W.},2865 title = "{Design and Realisation of a new AMANDA Data Aquisition System with Transient Waveform Recorders}",2866 school = {Universit{\"a}t Dortmund},2867 month = {Oct},2868 year = {2003}2869 }2870 2871 @PHDTHESIS{Schroeder:PhD,2872 author = {Schroeder, F.},2873 title = "{Simulation und Beobachtung von Luftschauern unter großen Zenitwinkeln}",2874 school = {Bergische Universit{\"a}t Wuppertal},2875 year = {2001}2876 }2877 2878 @ARTICLE{hepph0407075,2879 author = {{Albert}, J.},2880 title = "{Implementation of the Random Forest Method for the Imaging Atmospheric Cherenkov Telescope MAGIC}",2881 journal = {ArXiv e-prints},2882 eprint = {0709.3719},2883 year = {2007},2884 month = {Sep},2885 volume = {709},2886 adsurl = {http://cdsads.u-strasbg.fr/abs/2007arXiv0709.3719A},2887 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2888 }2889 2890 @INPROCEEDINGS{Curtef:CDM,2891 author = {Curtef, V. and Backes, M. and Hadasch, D.},2892 title = {Improvements of the energy reconstruction for the MAGIC telescope by means of analysis and Monte Carlo techniques},2893 booktitle = {Astronomische Nachrichten},2894 volume = 328,2895 year = 2007,2896 }2897 2898 @INPROCEEDINGS{Rueger,2899 author = {R\"{u}ger, M. and Spanier, F.},2900 booktitle = {Astronomische Nachrichten},2901 volume = 328,2902 year = 2007,2903 }2904 2905 @INPROCEEDINGS{Burkart,2906 author = {Burkart, T. and Spanier, F.},2907 booktitle = {Astronomische Nachrichten},2908 volume = 328,2909 year = 2007,2910 }2911 2912 @INPROCEEDINGS{Ruegamer,2913 author = {R\"{u}gamer, S. and others},2914 title = {Wide Range Multifrequency Observations of Northern TeV Blazars},2915 booktitle = {Astronomische Nachrichten},2916 volume = 328,2917 year = 2007,2918 }2919 2920 @ARTICLE{Kneiske,2921 author = {{Kneiske}, T.~M. and {Bretz}, T. and {Mannheim}, K. and {Hartmann}, D.~H.},2922 title = {Implications of cosmological gamma-ray absorption. {II}. Modification of gamma-ray spectra},2923 journal = {\aap},2924 year = 2004,2925 month = jan,2926 volume = 413,2927 pages = {807-815},2928 adsurl = {http://adsabs.harvard.edu/cgi-bin/nph-bib_query?bibcode=2004A%26A...413..807K&db_key=AST},2929 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2930 }2931 2932 @INPROCEEDINGS{Mannheim:1995,2933 author = {{Mannheim}, K.},2934 title = "{Gamma Rays from Compact Objects. (Ludwig Biermann Award Lecture 1995)}",2935 booktitle = {Reviews in Modern Astronomy},2936 year = 1996,2937 volume = 9,2938 editor = {{Schielicke}, R.~E.},2939 pages = {17-48}2940 }2941 2942 @ARTICLE{Albert:501,2943 author = {{Albert}, J. and others },2944 title = "{Variable Very High Energy {$\gamma$}-Ray Emission from Markarian 501}",2945 journal = {\apj},2946 eprint = {arXiv:astro-ph/0702008},2947 year = 2007,2948 month = nov,2949 volume = 669,2950 pages = {862-883},2951 adsurl = {http://adsabs.harvard.edu/abs/2007ApJ...669..862A},2952 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2953 }2954 2955 @INPROCEEDINGS{Muenich:Icrc,2956 author = {M\"{u}nich, K. and L\"{u}nemann, J.},2957 title = {Measurement of the atmospheric lepton energy spectra with {AMANDA-II}},2958 booktitle = {$30^{th}$ International Cosmic Ray Conference},2959 year = 2007,2960 }2961 2962 @INPROCEEDINGS{Bretz:2005drive,2963 author = {Bretz, T. and Dorner, D. and Wagner, R.M. and Riegel, B.},2964 title = {A Scalable Drive System Concept for Future Projects},2965 booktitle = {Towards a network of atmospheric Cherenkov detectors VII},2966 year = 2005,2967 month = Apr2968 }2969 2970 @ARTICLE{Moralejo:2004,2971 author = {{Moralejo}, A. and others},2972 title = "{Monte Carlo estimate of flux sensitivity of MAGIC for point-like sources}",2973 journal = {Internal MAGIC report},2974 year = 2004,2975 month = {Dec},2976 }2977 2978 @ARTICLE{MAGICsensi,2979 author = {{MAGIC website}},2980 title = "{MAGIC sensitivity at \url{http://magic.mppmu.mpg.de/physics/results/}}",2981 journal = {Official MAGIC website},2982 eprint = {http://magic.mppmu.mpg.de/physics/results/released/sensit.jpg},2983 }2984 2985 @ARTICLE{Magnussen:1998,2986 author = {{Magnussen}, N.},2987 title = "{The MAGIC Telescope Project for Gamma Astronomy above 10 GeV}",2988 journal = {ArXiv Astrophysics e-prints},2989 eprint = {astro-ph/9805184},2990 year = 1998,2991 month = may,2992 adsurl = {http://adsabs.harvard.edu/abs/1998astro.ph..5184M},2993 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}2994 }2995 2996 @INPROCEEDINGS{Vassiliev:1999,2997 author = {{Vassiliev}, V.~V.},2998 title = "{VERITAS: Performance characteristics (baseline design)}",2999 booktitle = {International Cosmic Ray Conference},3000 year = 1999,3001 volume = 5,3002 pages = {299-+},3003 adsurl = {http://adsabs.harvard.edu/abs/1999ICRC....5..299V},3004 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}3005 }3006 3007 @ARTICLE{Leier:2006,3008 author = {{Leier}, D. and {Becker}, J.~K. and {Groß}, A. and {Rhode}, W.},3009 title = "{Coincident observations between Neutrino- and TeV-Cherenkov-Telescopes}",3010 journal = {Internal IceCube report},3011 year = 2006,3012 month = {Apr},3013 }3014 3015 @ARTICLE{Chirkin:2004,3016 author = {{Chirkin}, D. and {Rhode}, W.},3017 title = "{Muon Monte Carlo: a high-precision tool for muon propagation through matter}",3018 journal = {ArXiv High Energy Physics - 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Suppl.},3103 editor = {{Medina}, J.},3104 }3105 3106 @ARTICLE{Meli,3107 author = {{Meli}, A. and {Becker}, J.~K. and {Quenby}, J.~J.},3108 title = "{Cosmic ray acceleration in subluminal and superluminal relativistic shock environments}",3109 journal = {ArXiv e-prints},3110 eprint = {0709.3031},3111 year = 2007,3112 month = sep,3113 volume = 709,3114 adsurl = {http://adsabs.harvard.edu/abs/2007arXiv0709.3031M},3115 adsnote = {Provided by the Smithsonian/NASA Astrophysics Data System}3116 }3117 3118 @ARTICLE{2006ApJ...642L.119A,3119 author = {{Albert}, J. and others},3120 title = "{Discovery of Very High Energy Gamma Rays from 1ES\,1218+30.4}",3121 journal = {\apjl},3122 eprint = {arXiv:astro-ph/0603529},3123 keywords = {BL Lacertae objects: individual (1ES 1218+30.4), Gamma Rays: Observations},3124 year = 2006,3125 month = may,3126 volume = 642,3127 pages = {L119-L122},3128 doi = {10.1086/504845},3129 adsurl = {http://cdsads.u-strasbg.fr/abs/2006ApJ...642L.119A},3130 adsnote = {Provided by the SAO/NASA Astrophysics Data System}3131 }3132 3133 @ARTICLE{2007ApJ...667L..21A,3134 author = {{Albert}, J. and others},3135 title = "{Discovery of Very High Energy {$\gamma$}-Rays from 1ES\,1011+496 at z\,=\,0.212}",3136 journal = {\apjl},3137 eprint = {arXiv:0706.4435},3138 keywords = {Gamma Rays: Observations, quasars: individual (1ES 1011+496)},3139 year = 2007,3140 month = sep,3141 volume = 667,3142 pages = {L21-L24},3143 doi = {10.1086/521982},3144 adsurl = {http://cdsads.u-strasbg.fr/abs/2007ApJ...667L..21A},3145 adsnote = {Provided by the SAO/NASA Astrophysics Data System}3146 }3147 3148 @ARTICLE{2001MNRAS.320..504S,3149 author = {{Somerville}, R.~S. and {Primack}, J.~R. and {Faber}, S.~M.},3150 title = "{The nature of high-redshift galaxies}",3151 journal = {\mnras},3152 eprint = {arXiv:astro-ph/9806228},3153 year = 2001,3154 month = feb,3155 volume = 320,3156 pages = {504-528},3157 adsurl = {http://cdsads.u-strasbg.fr/abs/2001MNRAS.320..504S},3158 adsnote = {Provided by the SAO/NASA Astrophysics Data System}3159 }3160 3161 @ARTICLE{2007arXiv0707.2915K,3162 author = {{Kneiske}, T.~M.},3163 title = "{Gamma-ray background: a review}",3164 journal = {ArXiv e-prints},3165 eprint = {0707.2915},3166 keywords = {Astrophysics},3167 year = 2007,3168 month = jul,3169 volume = 707,3170 adsurl = {http://cdsads.u-strasbg.fr/abs/2007arXiv0707.2915K},3171 adsnote = {Provided by the SAO/NASA Astrophysics Data System}3172 }3173 3174 @ARTICLE{1996ApJ...467..532M,3175 author = {{Mannheim}, K. and {Hartmann}, D. and {Funk}, B.},3176 title = "{The Gamma-Ray Burst Rate at High Photon Energies}",3177 journal = {\apj},3178 eprint = {arXiv:astro-ph/9605108},3179 keywords = {COSMOLOGY: DIFFUSE RADIATION, GAMMA RAYS: BURSTS, GALAXIES: INTERGALACTIC MEDIUM},3180 year = 1996,3181 month = aug,3182 volume = 467,3183 pages = {532-+},3184 doi = {10.1086/177629},3185 adsurl = {http://cdsads.u-strasbg.fr/abs/1996ApJ...467..532M},3186 adsnote = {Provided by the SAO/NASA Astrophysics Data System}3187 }3188 3189 @ARTICLE{1988VeARI..32....1F,3190 author = {{Fricke}, W. and {Schwan}, H. and {Lederle}, T. and others},3191 title = "{Fifth fundamental catalogue (FK5). 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trunk/Documents/DrivePaper/paper.tex
r9109 r9188 5 5 %\documentclass[authoryear,preprint,12pt]{elsarticle} 6 6 % 7 %\documentclass[preprint,5p,twocolumn,12pt]{elsarticle}8 \documentclass[12pt,final]{elsart5p}7 \documentclass[5p,twocolumn,12pt]{elsarticle} 8 %\documentclass[12pt,final]{elsart5p} 9 9 10 10 % Use the option review to obtain double line spacing … … 36 36 % \begin{linenumbers}, end it with \end{linenumbers}. Or switch it on 37 37 % for the whole article with \linenumbers. 38 \usepackage{lineno}38 %\usepackage{lineno} 39 39 %\linenumbers 40 40 41 \usepackage[numbers]{natbib}41 %\usepackage[numbers]{natbib} 42 42 43 43 \usepackage{textcomp,graphicx,times,wrapfig,xspace,url,amssymb,amsmath,wasysym,stmaryrd} … … 57 57 \title{The drive system of the\\Major Atmospheric Gamma-ray Imaging Cherenkov Telescope} 58 58 59 \newcommand{\corref}{\thanksref} 60 \newcommand{\cortext}{\thanks} 61 62 %\tnotetext[t1]{This document is collaborative effort} 63 %\tnotetext[t2]{This document is collaborative effort more} 64 59 %\newcommand{\corref}{\thanksref} 60 %\newcommand{\cortext}{\thanks} 65 61 \author[tb]{T.~Bretz\corref{cor1}} 66 \address[tb]{Universit\"{a}t W\"{urzburg}, Am Hubland, D-97074 W\"{u}rzburg, Germany} 67 %\ead{tbretz@astro.uni-wuerzburg.de} 68 %\fntext[fn1]{My name is Thomas Bretz} 69 70 \author[tb]{D.~Dorner},\author[rw]{R.~M.~Wagner} 71 %\address[dd]{Integral Science Data Center} 72 %\ead{dorner@astro.uni-wuerzburg.de} 73 74 75 %\ead[rw]{robert.wagner@mpp.mpg.de} 76 \address[rw]{Max-Planck-Institut f\"ur Physik, F\"ohringer Ring 6, D-80805 M\"{u}nchen, Germany} 77 62 \author[tb]{D.~Dorner} 63 \author[rw]{R.~M.~Wagner} 64 \author[rw]{P.~Sawallisch} 65 \address[tb]{Universit\"{a}t W\"{u}rzburg, Am Hubland, 97074 W\"{u}rzburg, Germany} 66 \address[rw]{Max-Planck-Institut f\"ur Physik, F\"ohringer Ring 6, 80805 M\"{u}nchen, Germany} 78 67 \cortext[cor1]{Corresponding author: tbretz@astro.uni-wuerzburg.de} 79 68 … … 86 75 \begin{abstract} 87 76 The MAGIC telescope is an imaging atmospheric Cherenkov telescope, 88 designed to observe very high energy gamma-rays achieving a low energy89 threshold. One of the key science goals is thefast follow-up of the77 designed to observe very high energy gamma-rays while achieving a low 78 energy threshold. One of the key science goals is fast follow-up of the 90 79 enigmatic and short lived gamma-ray bursts. The drive system for the 91 80 telescope has to meet two basic demands: (1)~During normal 92 observations, the 64-ton telescope has to be repositioned accurately,93 andhas to track a given sky position with high precision at a typical81 observations, the 72-ton telescope has to be positioned accurately, and 82 has to track a given sky position with high precision at a typical 94 83 rotational speed in the order of one revolution per day. (2)~For 95 84 successfully observing GRB prompt emission and afterglows, it has to be 96 powerful enough to reposition the telescope to an arbitrary point on 97 the sky within a few ten seconds and commence normal tracking immediately 98 thereafter. To meet these requirements, the implementation and 99 realization of the drive system relies strongly on standard industry 100 components to ensure robustness and reliability. In this paper, we 101 describe the mechanical setup, the drive control and the calibration of 102 the pointing, as well as present measurements of the accuracy of the 103 system. We show that within the limits of the mount the drive system is 104 mechanically able to operate with an accuracy even better than the 105 feedback values from the axes. In the context of future projects, 106 envisaging telescope arrays comprising about 100 individual 107 instruments, the robustness and scalability of the concept is 108 emphasized. 85 powerful enough to position to an arbitrary point on the sky within a 86 few ten seconds and commence normal tracking immediately thereafter. To 87 meet these requirements, the implementation and realization of the 88 drive system relies strongly on standard industry components to ensure 89 robustness and reliability. In this paper, we describe the mechanical 90 setup, the drive control and the calibration of the pointing, as well 91 as present measurements of the accuracy of the system. We show that the 92 drive system is mechanically able to operate the motors with an 93 accuracy even better than the feedback values from the axes. In the 94 context of future projects, envisaging telescope arrays comprising 95 about 100 individual instruments, the robustness and scalability of the 96 concept is emphasized. 109 97 \end{abstract} 110 98 111 99 \begin{keyword} 112 MAGIC\sep drive system\sep IACT\sep scalability\sep calibration\sep fast repositioning100 MAGIC\sep drive system\sep IACT\sep scalability\sep calibration\sep fast positioning 113 101 \end{keyword} 114 102 … … 120 108 121 109 The MAGIC telescope on the Canary Island of La~Palma, located 2200\,m 122 above sea level at 28\textdegree{}45 '\,N and 17\textdegree{}54'\,W, is an123 imaging atmospheric Cherenkov telescope designed to achieve a low124 energy threshold, fast repositioning, and high tracking accuracy,125 e.g.~\cite{Lorenz:2004, Cortina:2005}. The MAGIC design, and the110 above sea level at 28\textdegree{}45$^\prime$\,N and 17\textdegree{}54$^\prime$\,W, is 111 an imaging atmospheric Cherenkov telescope designed to achieve a low 112 energy threshold, fast positioning, and high tracking 113 accuracy~\cite{Lorenz:2004, Cortina:2005}. The MAGIC design, and the 126 114 currently ongoing construction of a second telescope 127 (MAGIC\,II;~\cite{Goebel:2007}), pave the way to theground-based115 (MAGIC\,II;~\cite{Goebel:2007}), pave the way for ground-based 128 116 detection of gamma-ray sources at cosmological distances down to less 129 than 80\,GeV. After the discovery of the distant blazars 1ES\,1218+304117 than 25\,GeV~\cite{Sci}. After the discovery of the distant blazars 1ES\,1218+304 130 118 at a redshift of $z$\,=\,0.182~\citep{2006ApJ...642L.119A} and 131 119 1ES\,1011+496 at $z$\,=\,0.212~\citep{2007ApJ...667L..21A}, the most … … 136 124 in the mid-infrared to near-infrared wavelength range was believed to 137 125 be strong enough to inhibit propagation of gamma-rays across 138 cosmological distances~\citep{2001MNRAS.320..504S}. However, it could 139 be shown that the results of deep galaxy surveys with the Hubble and 140 Spitzer Space telescopes are consistent with these findings, if the 141 spurious feature at one micron is attributed to a foreground effect 142 resulting from an inaccurate subtraction of zodiacal 143 light~\citep{Hauser:2001, 2007arXiv0707.2915K, Kneiske:2004}. The low 144 level of pair attenuation of gamma-rays greatly improves the prospects 145 of searching for very high energy gamma-rays from gamma-ray bursts 146 (GRBs). Their remarkable similarities with blazar flares, albeit at 147 much shorter timescales, presumably arise from the scaling behavior of 148 relativistic jets, the common physical cause of these phenomena. Since 149 most GRBs reside at large redshifts, their detection relies on the low 150 level of absorption at very high energies~\citep{1996ApJ...467..532M}. 151 Moreover, the cosmological absorption decreases with photon energy, 152 favoring MAGIC to discover GRBs due to its low energy threshold. 153 154 Due to the short life time of GRBs and the limited field of view of 126 cosmological distances~\citep{2001MNRAS.320..504S, 2007arXiv0707.2915K, Hauser:2001}. 127 %However, it could 128 %be shown that the results of deep galaxy surveys with the Hubble and 129 %Spitzer Space telescopes are consistent with these findings, if the 130 %spurious feature at one micron is attributed to a foreground effect 131 %resulting from an inaccurate subtraction of zodiacal 132 %light~\citep{Hauser:2001, 2007arXiv0707.2915K, Kneiske:2004}. 133 The 134 apparent low level of pair attenuation of gamma-rays greatly improves 135 the prospects of searching for very high energy gamma-rays from 136 gamma-ray bursts (GRBs), cf.~\citep{Kneiske:2004}. Their remarkable similarities with blazar 137 flares, albeit at much shorter timescales, presumably arise from the 138 scaling behavior of relativistic jets, the common physical cause of 139 these phenomena. Since most GRBs reside at large redshifts, their 140 detection at very high energies relies on the low level of 141 absorption~\citep{1996ApJ...467..532M}. Moreover, the cosmological 142 absorption decreases with photon energy, favoring MAGIC to discover 143 GRBs due to its low energy threshold. 144 145 Due to the short life times of GRBs and the limited field of view of 155 146 imaging atmospheric Cherenkov telescopes, the drive system of the MAGIC 156 147 telescope has to meet two basic demands: during normal observations, 157 the 64-ton telescope has to be repositioned accurately, and has to148 the 72-ton telescope has to be positioned accurately, and has to 158 149 track a given sky position, i.e., counteract the apparent rotation of 159 150 the celestial sphere, with high precision at a typical rotational speed 160 151 in the order of one revolution per day. For catching the GRB prompt 161 emission and afterglows, it has to be powerful enough to reposition the152 emission and afterglows, it has to be powerful enough to position the 162 153 telescope to an arbitrary point on the sky within a very short time 163 ($\apprle$\,60\,s) and commence normal tracking immediately 154 %($\apprle$\,60\,s) 155 and commence normal tracking immediately 164 156 thereafter. To keep the system simple, i.e., robust, both requirements 165 157 should be achieved without an indexing gear. The telescope's total 166 weight of 64~tons is a comparatively low measure, reflecting the167 construction principle of usinglow-weight materials whenever possible.158 weight of 72~tons is comparatively low, reflecting the 159 use of low-weight materials whenever possible. 168 160 For example, the mount consists of a space frame of carbon-fiber 169 161 reinforced plastic tubes, and the mirrors are made of polished … … 174 166 setup of the drive system are outlined. The control loops and 175 167 performance goals are described in section~\ref{sec3}, while the 176 implementation of the repositioning and tracking algorithms and the168 implementation of the positioning and tracking algorithms and the 177 169 calibration of the drive system are explained in section~\ref{sec4}. 178 170 The system can be scaled to meet the demands of other telescope designs 179 as shown in section~\ref{sec5}. Finally, in section~\ref{ conclusions}180 we draw conclusions from our experience of operating the MAGIC 181 telescope with this drive system for four years.182 183 \section{General design considerations} 171 as shown in section~\ref{sec5}. Finally, in section~\ref{outlook} and 172 section~\ref{conclusions} we draw conclusions from our experience of 173 operating the MAGIC telescope with this drive system for four years. 174 175 \section{General design considerations}\label{design} 184 176 185 177 The drive system of the MAGIC telescope is quite similar to that of … … 187 179 quite a few aspects that influenced the design of the MAGIC drive 188 180 system in comparison to optical telescopes and small-diameter Imaging 189 Atmospheric Cherenkov telescope (IACT). 190 191 The tracking and stability requirements for IACTs are much less 192 demanding than for optical telescopes. Although IACTs, like optical 193 telescopes, track celestial objects, they observe quite different 194 phenomena: Optical telescopes observe visible light, which originates 195 at infinity and is parallel. The best-possible optical resolution is 196 required and in turn, equal tracking precision due to comparably long 197 integration times, i.e., seconds to hours. In ground-based astronomy at 198 very high gamma-ray energies, IACTs record the Cherenkov light produced 199 by an electromagnetic air-shower in the atmosphere, induced by a 200 primary gamma-ray, i.e., from a close by (5\,km\,-\,20\,km) and 201 extended event with a diffuse transverse extension and a typical 202 extension of a few km. Due to the stochastic nature of the shower 203 development, the detected light will have an inherent limitation in 204 explanatory power, improving normally with the energy, i.e., 205 shower-particle multiplicity. As, in this case, the Cherenkov light is 206 emitted with under a small angle off the particle tracks, these photons 207 do not even point directly to the source like in optical astronomy. 208 Nevertheless, the shower points towards the direction of the incoming 209 gamma-ray and thus towards its source on the sky, and for this reason 210 its origin can be reconstructed analyzing its image. Modern IACTs 211 achieve an energy-dependent pointing resolution for individual showers 212 of 0.1\textdegree\,-\,0.01\textdegree. These are the predictions from 213 Monte Carlo simulations assuming, amongst other things, ideal tracking. 214 This sets the limits achievable in practical cases. Consequently, the 215 required tracking precision must be at least of the same order or even 216 better. Although the short integration times, on the order of a few 217 nanoseconds, would allow for an offline correction, this should be 218 avoided since it may give rise to an additional systematic error. 219 220 MAGIC, as other large IACTs, has no protective dome. It is constantly 221 exposed to daily changing weather conditions and intense sunlight, and 222 therefore suffers much more material aging than optical telescopes. A 223 much simpler mechanical mount had to be used, resulting in a design of 224 considerably less stiffness, long-term irreversible deformations, and 225 small unpredictable deformations due to varying wind pressure. The 226 tracking system does not need to be more precise than the mechanical 227 structure and, consequently, can be much simpler and hence cheaper as 228 compared to that of large optical telescopes. 181 Atmospheric Cherenkov telescopes (IACT). 182 183 Although IACTs have optical components, the tracking and stability 184 requirements for IACTs are much less demanding than for optical 185 telescopes. Like optical telescopes, IACTs track celestial 186 objects, but observe quite different phenomena: Optical telescopes 187 observe visible light, which originates at infinity and is parallel. 188 Consequently, the best-possible optical resolution is required and in 189 turn, equal tracking precision due to comparably long integration 190 times, i.e., seconds to hours. In contrast, IACTs record the Cherenkov 191 light produced by an electromagnetic air-shower in the atmosphere, 192 induced by a primary gamma-ray, i.e., from a close by 193 (5\,km\,-\,20\,km) and extended event with a diffuse transverse 194 extension and a typical extension of a few hundred meters. Due to the 195 stochastic nature of the shower development, the detected light will 196 have an inherent limitation in explanatory power, improving normally 197 with the energy, i.e., shower-particle multiplicity. As 198 the Cherenkov light is emitted under a small angle off the particle 199 tracks, these photons do not even point directly to the source like in 200 optical astronomy. Nevertheless, the shower points towards the 201 direction of the incoming gamma-ray and thus towards its source on the 202 sky. For this reason its origin can be reconstructed analyzing its 203 image. Modern IACTs achieve an energy-dependent pointing resolution for 204 individual showers of 6$^\prime$\,-\,0.6$^\prime$. These are the 205 predictions from Monte Carlo simulations assuming, amongst other 206 things, ideal tracking. This sets the limits achievable in practical 207 cases. Consequently, the required tracking precision must be at least 208 of the same order or even better. Although the short integration times, 209 on the order of a few nanoseconds, would allow for an offline 210 correction, this should be avoided since it may give rise to an 211 additional systematic error. 212 213 %MAGIC, as other large IACTs, has no protective dome. It is constantly 214 %exposed to daily changing weather conditions and intense sunlight, and 215 %therefore suffers much more material aging than optical telescopes. A 216 %much simpler mechanical mount had to be used, resulting in a design of 217 %considerably less stiffness, long-term irreversible deformations, and 218 %small unpredictable deformations due to varying wind pressure. The 219 %tracking system does not need to be more precise than the mechanical 220 %structure and, consequently, can be much simpler and hence cheaper as 221 %compared to that of large optical telescopes. 229 222 230 223 To meet one of the main physics goals, the observation of prompt and 231 afterglow emission of GRBs, repositioning of the telescope to their224 afterglow emission of GRBs, positioning of the telescope to their 232 225 assumed sky position is required in a time as short as possible. 233 226 Alerts, provided by satellites, arrive at the MAGIC site typically 234 within 10\,s after the outburst~\citep{2007ApJ...667..358A}. To achieve 235 a positioning time to any position on the sky within less than a minute 236 requires a very light-weight but sturdy telescope and a fast-acting and 237 powerful drive system. 238 \begin{figure*}[htb] 227 within 10\,s after the outburst~\citep{2007ApJ...667..358A}. 228 Since the life times of GRBs show a bimodal distribution~\cite{Paciesas:1999} 229 with a peak between 10\,s and 100\,s. To achieve 230 a positioning time to any position on the sky within a reasonable 231 time inside this window, i.e. less than a minute, 232 a very light-weight but sturdy telescope and a fast-acting and 233 powerful drive system is required. 234 \begin{figure*}[htbp] 239 235 \begin{center} 240 \includegraphics*[width=0.48\textwidth,angle=0,clip]{figure1a.eps} 241 \hfill 242 \includegraphics*[width=0.48\textwidth,angle=0,clip]{figure1b.eps} 243 \caption{{\em Left}: One of the bogeys with its two railway rails. The 244 motor is encapsulated in the grey box on the yellow drive unit. It drives 245 the tooth double-toothed wheel gearing into the chain through a gear 246 and a clutch. {\em Right}: The drive unit driving the elevation axis 247 from the back side. Visible is the actuator of the safety holding brake 248 and its corresponding brake disc mounted on the motor-driven axis. The 249 motor is attached on the opposite side. } 236 \includegraphics*[width=0.91\textwidth,angle=0,clip]{figure1.eps} 237 \caption{The top picture shows the MAGIC\,I telescope with the major 238 components of the drive system. The elevation drive unit, from its back 239 side, is enlarged in the bottom left picture. Visible is the actuator 240 of the safety holding brake and its corresponding brake disk mounted on 241 the motor-driven axis. The motor is attached on the opposite side. The 242 picture on the bottom right shows one of the azimuth bogeys with its 243 two railway rails. The motor is housed in the grey box on the 244 yellow drive unit. It drives the tooth double-toothed wheel gearing 245 into the chain through a gear and a clutch.} 246 % \includegraphics*[width=0.48\textwidth,angle=0,clip]{figure1a.eps} 247 % \hfill 248 % \includegraphics*[width=0.48\textwidth,angle=0,clip]{figure1b.eps} 249 %\caption{{\em Left}: One of the bogeys with its two railway rails. The 250 %motor is encapsulated in the grey box on the yellow drive unit. It drives 251 %%the tooth double-toothed wheel gearing into the chain through a gear 252 %and a clutch. {\em Right}: The drive unit driving the elevation axis 253 %from the back side. Visible is the actuator of the safety holding brake 254 %and its corresponding brake disk mounted on the motor-driven axis. The 255 %motor is attached on the opposite side. } 250 256 \label{figure1} 251 257 \end{center} … … 256 262 The implementation of the drive system relies strongly on standard 257 263 industry components to ensure robustness, reliability and proper 258 support. The azimuth drive ring of 21\,m diameter is made from a normal 259 railway rail, which was delivered in pre-bent sections and welded on 260 site. The fixing onto the concrete foundation uses standard rail-fixing 261 elements, and allows for movements caused by temperature changes. The 262 maximum allowable deviation from the horizontal plane as well as 263 deviation from flatness is $\pm 2$\,mm, and from the ideal circle it is 264 1\,cm. Each of the six bogeys holds two standard crane wheels of 60\,cm 265 diameter with a rather broad wheel tread. This allows for deviations in 266 the 11.5\,m-distance to the central axis due to extreme temperature 267 changes, which can even be asymmetric in case of different exposure to 268 sunlight on either side. The central bearing of the azimuth axis is a 269 high-quality ball bearing, while for the elevation axis, due to lower 270 weight, a less expensive sliding bearing with a teflon layer was 271 installed. These sliding bearings have a slightly spherical surface to 272 allow for small misalignments during installation and some bending of 273 the elevation axis stubs under load. 264 technical support. Its major drive components, described hereafter, are 265 shown on the pictures in fig.~\ref{figure2}. 266 267 The azimuth drive ring of 20\,m diameter is made from a normal railway 268 rail, which was delivered in pre-bent sections and welded on site. Its 269 head is only about 74\,mm broad and has a bent profile. The fixing onto 270 the concrete foundation uses standard rail-fixing elements, and allows 271 for movements caused by temperature changes. The maximum allowable 272 deviation from the horizontal plane as well as deviation from flatness 273 is $\pm 2$\,mm, and from the ideal circle it is $\Delta$r\,=\,8\,mm. 274 The rail support was leveled with a theodolite every 60\,cm 275 with an overall tolerance of $\pm 1.5$\,mm every 60\,cm. In between the 276 deviation is negligible. Each of the six bogeys holds two standard 277 crane wheels of 60\,cm diameter with a rather broad wheel tread of 278 110\,mm. This allows for deviations in the 11.5\,m-distance to the 279 central axis due to extreme temperature changes, which can even be 280 asymmetric in case of different exposure to sunlight on either side. 281 For the central bearing of the azimuth axis, a high-quality ball 282 bearing was installed fairly assuming that the axis is vertically 283 stable. For the elevation axis, due to lower weight, a less expensive 284 sliding bearing with a teflon layer was used. These sliding bearings 285 have a slightly spherical surface to allow for small misalignments 286 during installation and some bending of the elevation axis stubs under 287 load. 274 288 275 289 The drive mechanism is based on duplex roller chains and sprocket 276 290 wheels in a rack-and-pinion mounting. The chains have a breaking 277 strength of 1 7~tons and a chain-link spacing of 2.5\,cm. The initial291 strength of 19~tons and a chain-link spacing of 2.5\,cm. The initial 278 292 play between the chain links and the sprocket-wheel teeth is about 279 293 3\,mm\,-\,5\,mm, according to the data sheet, corresponding to much 280 294 less than an arcsecond on the telescope axes. The azimuth drive chain 281 295 is fixed on a dedicated ring on the concrete foundation, but has quite 282 some radial distance variation of up to 3\,cm. The elevation drive296 some radial distance variation of up to 5\,mm. The elevation drive 283 297 chain is mounted on a slightly oval ring below the mirror dish, because 284 298 the ring forms an integral part of the camera support mast structure. 285 299 286 Commercial synchronous motors (type designation Bosch Rexroth 287 MHD\,112C-058) are used together with low-play planetary gears linked 300 % Bosch Rexroth AG, 970816 Lohr am Main, Germany 301 % www.boschrexroth.de 302 303 % Wittenstein alpha GmbH, Walter-Wittenstein-Stra"se 1, D-97999 Igersheim 304 % www.wittenstein-alpha.de 305 306 % updated 307 Commercial synchronous motors (type designation Bosch 308 Rexroth\footnote{\url{http://www.boschrexroth.de}\\Bosch Rexroth AG, 309 97816 Lohr am Main, Germany} MHD\,112C-058) are used together with 310 low-play planetary gears (type designation 311 alpha\footnote{\url{http://www.wittenstein-alpha.de}\\Wittenstein alpha 312 GmbH, 97999 Igersheim, Germany} GTS\,210-M02-020\,B09, ratio 20) linked 288 313 to the sprocket wheels. These motors intrinsically allow for a 289 314 positional accuracy better than one arcsecond of the motor axis. Having … … 292 317 installation height of more than 2200\,m a.s.l., due to lower air 293 318 pressure and consequently less efficient cooling, the nominal values 294 given must be reduced by about 25\%. The azimuth motors are mounted on 295 small lever arms. In order to follow the small radial irregularities of 296 the azimuthal drive chain, the motors are pressed against it by 297 springs. The elevation-drive motor is mounted on a nearly 1\,m long 319 given must be reduced by about 20\%. Deceleration is done operating the 320 motors as generator which is as powerful as acceleration. The motors 321 contain 70\,Nm holding brakes which are not meant to be used as driving 322 brake. The azimuth motors are mounted on small lever arms. In order to 323 follow the small irregularities of the azimuthal drive chain, the units 324 are forced to follow the drive chain, horizontally and vertically, by 325 guide rolls. The elevation-drive motor is mounted on a nearly 1\,m long 298 326 lever arm to be able to compensate the oval shape of the chain and the 299 327 fact that the center of the circle defined by the drive chain is 300 shifted 50\,cm away from the axis towards the camera. 328 shifted 356\,mm away from the axis towards the camera. The elevation 329 drive is also equipped with an additional brake, operated only as 330 holding brake, for safety reasons in case of extremely strong wind 331 pressure. No further brake are installed on the telescope. 301 332 302 333 The design of the drive system control, c.f.~\citet{Bretz:2003drive}, … … 319 350 $\theta$\,=\,+100\textdegree{} to $\theta$\,=\,-70\textdegree{} where 320 351 the change of sign implies a movement {\em across the zenith}. This 321 so-called {\it reverse mode} is currently not in use, as it might imply322 hysteresis effects of the active mirror control system, still under352 so-called {\it reverse mode} is currently not in use, as it might result 353 in hysteresis effects of the active mirror control system, still under 323 354 investigation, due to shifting of weight at zenith. The accessible 324 355 range in both directions and on both axes is limited by software to the … … 334 365 \section{Setup of the motion control system}\label{sec3} 335 366 336 Like for the mechanical drive system, also for the motion-control system 337 standard industry components were used. The drive is controlled bythe338 feedback of encoders measuring the angular positions of the motors and 339 the telescope axes. The encoders on the motor axes provide340 information to microcontrollers dedicated for motion control, 341 initiating and monitoring every movement. Professional build-in servo 342 loops take over the suppression of oscillations. The correct pointing 343 p osition of the system is ensured by a computer program evaluating the344 feedback from the telescope axes and initiating the motion executed by 345 the micro controllers. Additionally, the motor-axis encoders are also 346 evaluated to increase accuracy. The details of this system, as shown in 347 figure~\ref{figure2}, are discussedbelow.367 The motion control system similarly uses standard industry components. 368 The drive is controlled by the feedback of encoders measuring the 369 angular positions of the motors and the telescope axes. The encoders on 370 the motor axes provide information to micro controllers dedicated for 371 motion control, initiating and monitoring every movement. Professional 372 built-in servo loops take over the suppression of oscillations. The 373 correct pointing position of the system is ensured by a computer 374 program evaluating the feedback from the telescope axes and initiating 375 the motion executed by the micro controllers. Additionally, the 376 motor-axis encoders are also evaluated to increase accuracy. The 377 details of this system, as shown in figure~\ref{figure2}, are discussed 378 below. 348 379 349 380 \begin{figure*}[htb] … … 365 396 366 397 The angular telescope positions are measured by three shaft-encoders 367 (Hengstler AC61/1214EQ.72OLZ). These absolute multi-turn encoders have 368 a resolution of 4\,096 (10\,bit) revolutions and 16\,384 (14\,bit) 369 steps per revolution, corresponding to an intrinsic angular resolution 370 of 1.3\,arcmin per step. One shaft encoder is located on the azimuth 371 axis, while two more encoders are fixed on either side of the elevation 372 axis, increasing the resolution and allowing for measurements of the 373 twisting of the dish (fig.~\ref{figure3}). All shaft encoders used are 374 watertight (IP\,67) to withstand the extreme weather conditions 375 occasionally encountered at the telescope site. The motor positions are 376 read out at a frequency of 1\,kHz from 10\,bit relative rotary encoders 377 fixed on the motor axes. Due to the gear ratio of more than one 378 thousand between motor and load, the 14\,bit resolution of the shaft 379 encoder system on the axes can be interpolated further using the 380 position readout of the motors. For communication with the axis 381 encoders, a CANbus interface with the CANopen protocol is in use 382 (operated at 125\,kbps). The motor encoders are directly connected by 383 an analog interface. 398 (type designation Hengstler\footnote{\url{http://www.hengstler.de}\\Hengstler GmbH, 399 78554 Aldingen, Germany} AC61/1214EQ.72OLZ). These absolute multi-turn 400 encoders have a resolution of 4\,096 (10\,bit) revolutions and 16\,384 401 (14\,bit) steps per revolution, corresponding to an intrinsic angular 402 resolution of 1.3$^\prime$ per step. One shaft encoder is located on 403 the azimuth axis, while two more encoders are fixed on either side of 404 the elevation axis, increasing the resolution and allowing for 405 measurements of the twisting of the dish (fig.~\ref{figure3}). All 406 shaft encoders used are watertight (IP\,67) to withstand the extreme 407 weather conditions occasionally encountered at the telescope site. The 408 motor positions are read out at a frequency of 1\,kHz from 10\,bit 409 relative rotary encoders fixed on the motor axes. Due to the gear ratio 410 of more than one thousand between motor and load, the 14\,bit 411 resolution of the shaft encoder system on the axes can be interpolated 412 further using the position readout of the motors. For communication 413 with the axis encoders, a CANbus interface with the CANopen protocol is 414 in use (operated at 125\,kbps). The motor encoders are directly 415 connected by an analog interface. 384 416 385 417 \subsection{Motor control} … … 388 420 units ({\em DKC}, type designation Bosch Rexroth, 389 421 DKC~ECODRIVE\,03.3-200-7-FW), serving as intelligent frequency 390 converters and power supplies. An input value, given either analog or422 converters. An input value, given either analog or 391 423 digital, is converted to a predefined output, e.g., command position, 392 424 velocity or torque. All command values are processed through a chain of 393 buil d-in controllers, cf. fig.~\ref{figure4}, resulting in a final425 built-in controllers, cf. fig.~\ref{figure4}, resulting in a final 394 426 command current applied to the motor. This internal chain of control 395 loops, maintaining the movement of the motors , worksat a frequency of396 1\,kHz fed back by the rotary encoders on the corresponding motor axes.427 loops, maintaining the movement of the motors at a frequency of 428 1\,kHz, fed back by the rotary encoders on the corresponding motor axes. 397 429 Several safety limits ensure damage-free operation of the system even 398 430 under unexpected operation conditions. These safety limits are, e.g., … … 404 436 slave is driven by the command torque output of the master. This 405 437 operation mode ensures that both motors can apply their combined force 406 to the telescope structure without oscillations. 438 to the telescope structure without oscillations. In principle it is 439 possible to use a bias torque to eliminate play. This feature 440 was not used because the play is negligible anyhow. 407 441 408 442 \begin{figure}[htb] … … 414 448 position to the opposite side. The average offset from zero 415 449 corresponds to a the twist of the two shaft encoders with respect to 416 each other. Under normal conditions the torsion between both ends of 450 each other. The error bars denote the spread of several measurements. 451 Under normal conditions the torsion between both ends of 417 452 the axis is less than the shaft-encoder resolution.} 418 453 \label{figure3} … … 423 458 \begin{figure*}[htb] 424 459 \begin{center} 425 \includegraphics*[width=0. 6\textwidth,angle=0,clip]{figure4.eps}460 \includegraphics*[width=0.78\textwidth,angle=0,clip]{figure4.eps} 426 461 \caption{The internal flow control between the individual controllers 427 462 inside the drive control unit. Depending on the type of the command … … 433 468 \end{figure*} 434 469 435 The master DKC for each axis is controlled by presetting a rotational 470 % zub machine control AG, Kastaniensteif 7, CH-6047 Kastanienbaum 471 % www.zub.de 472 473 The master for each axis is controlled by presetting a rotational 436 474 speed defined by $\pm$10\,V on its analog input. The input voltage is 437 produced by a programmable micro controller dedicated to analog motion438 control, produced by Z\&B ({\em MACS}, type designation MACS). The439 feedback is realized through a 500-step emulation of the motor's rotary 440 encoders by the DKCs for each axis seperately. Elevation and azimuth 441 movement is regulated by individual MACSs. The MACS controller itself 442 communicates with the control software (see below) through a CANbus 443 connection.475 produced by a programmable micro controller dedicated to analog motion 476 control, produced by Z\&B\footnote{\url{http://www.zub.de}\\zub machine control AG, 6074 477 Kastanienbaum, Switzerland} ({\em MACS}, type 478 designation MACS). The feedback is realized through a 500-step 479 emulation of the motor's rotary encoders by the DKCs. Elevation and azimuth movement is regulated by individual 480 MACSs. The MACS controller itself communicates with the control 481 software (see below) through a CANbus connection. 444 482 445 483 It turned out that in particular the azimuth motor system seems to be 446 484 limited by the large moment of inertia of the telescope 447 ($J_{\mathrm{az}} \approx4400$\,tm$^2$, for comparison448 $J_{\mathrm{el}} \approx850$\,tm$^2$; note that the exact numbers depend485 ($J_{\mathrm{az}}$\,$\approx$\,4400\,tm$^2$, for comparison 486 $J_{\mathrm{el}}$\,$\approx$\,850\,tm$^2$; note that the exact numbers depend 449 487 on the current orientation of the telescope). At the same time, the 450 488 requirements on the elevation drive are much less demanding.\\ 451 489 452 \noindent {\em MAGIC\,II}\quad For the drive system currently under commissioning for453 MAGIC\,II, several improvements have been provided:\\ 490 \noindent {\em MAGIC\,II}\quad For the drive system 491 several improvements have been provided:\\\vspace{-2ex} 454 492 \begin{itemize} 455 \item 13\,bit absolute shaft-encoders (type designation Heidenhain 493 \item 13\,bit absolute shaft-encoders (type designation Heidenhain\footnote{\url{http://www.heidenhain.de}\\Dr.~Johannes Heidenhain GmbH, 83301 Traunreut, Germany} 456 494 ROQ\,425) are installed, providing an additional sine-shaped 457 495 $\pm$1\,Vss output within each step. This allows for a more accurate … … 465 503 better motion control of the system. 466 504 \item The analog transmission of the master's command torque to the 467 slave is substituted by a direct digital bi-directional communication 468 of the DKCs. 505 slave is replaced by a direct digital communication (EcoX) 506 of the DKCs. This allows for more robust and precise slave control. 507 Furthermore the motors could be coupled with relative angular synchronism 508 allowing to suppress deformations of the structure by keeping the 509 axis connecting both motors stable. 469 510 \item A single professional programmable logic controller (PLC), in German: 470 511 {\em Speicherprogammierbare Steuerung} (SPS, type designation Rexroth … … 491 532 \subsubsection{Positioning} 492 533 493 Whenever the telescope has to be repositioned, the relative distance to534 Whenever the telescope has to be positioned, the relative distance to 494 535 the new position is calculated in telescope coordinates and then 495 converted to motor revolutions. Then, the micro -controllers are536 converted to motor revolutions. Then, the micro controllers are 496 537 instructed to move the motors accordingly. Since the motion is 497 538 controlled by the feedback of the encoders on the motor axes, not on … … 534 575 i.e., the movement of the axis is stopped. 535 576 536 \subsection{Fast repositioning}577 \subsection{Fast positioning} 537 578 538 579 The observation of GRBs and their afterglows in very-high energy … … 541 582 after their outburst via the {\em Gamma-ray Burst Coordination 542 583 Network}~\cite{www:gcn}, typical burst durations of 10\,s to 543 100\,s~\cite{Paciesas:1999} demand a fast repositioning of the584 100\,s~\cite{Paciesas:1999} demand a fast positioning of the 544 585 telescope. The current best value for the acceleration has been set to 545 586 11.7\,mrad\,s$^{-2}$. It is constrained by the maximum constant force … … 556 597 ignoring all other control elements. 557 598 558 Currently, automatic repositioning by599 Currently, automatic positioning by 559 600 $\Delta\varphi$\,=\,180\textdegree{} in azimuth to the target position 560 is achieved within 45\,s. The repositioning time in elevation is not601 is achieved within 45\,s. The positioning time in elevation is not 561 602 critical in the sense that the probability to move a longer path in 562 603 elevation than in azimuth is negligible. Allowing the telescope drive … … 570 611 the telescope structure. 571 612 613 With the upgraded MAGIC\,II drive system, during commissioning in 2008 August, a 614 maximum acceleration and deceleration of $a_{az}$\,=\,30\,mrad\,s$^{-2}$ 615 and $a_{zd}$\,=\,90\,mrad/s$^{-2}$ and a maximum velocity of 616 $v_{az}$\,=\,290\,mrad\,s$^{-1}$ and $v_{zd}$\,=\,330\,mrad\,s$^{-1}$ 617 could be reached. With these values the limits of the motor power are 618 exhausted. This allowed a movement of 619 $\Delta\varphi$\,=\,180\textdegree/360\textdegree{} in azimuth within 20\,s\,/\,33\,s. 620 572 621 \subsection{Tracking precision} 573 622 … … 586 635 axes into account. In almost all cases it is well below the resolution 587 636 of the shaft encoders, and in 80\% of the time it does not exceed 1/8 588 of this value ($ sim$10\,arcsec). This means that the accuracy of the637 of this value ($\sim$10$^{\prime\prime}$). This means that the accuracy of the 589 638 motion control, based on the encoder feedback, is much better than 590 1\,arcmin on the sky, which is roughly a fifth of the diameter of a 591 pixel in the MAGIC photomultiplier (PM) camera (0.1\textdegree{}, 592 c.f.~\cite{Beixeras:2005}). 593 594 In the case of a real telescope ultimate limits of the tracking 595 precision are given by the precision with which the correct command 596 value is known. Its calibration is discussed in the following. 597 639 1$^\prime$ on the sky, which is roughly a fifth of the diameter of a 640 pixel in the MAGIC camera (6$^\prime$, c.f.~\cite{Beixeras:2005}). 598 641 \begin{figure}[htb] 599 642 \begin{center} … … 604 647 deviation is shown as absolute control deviation projected on the sky. 605 648 The blue lines correspond to fractions of the shaft-encoder resolution. 649 The peak at half of the shaft-encoder resolution results from cases 650 in which one of the two averaged elevation encoders is off by one step. 606 651 } 607 652 \label{figure5} … … 609 654 \end{figure} 610 655 656 In the case of a real telescope ultimate limits of the tracking 657 precision are given by the precision with which the correct command 658 value is known. Its calibration is discussed hereafter. 659 611 660 \section{Calibration}\label{sec4} 612 661 613 To calibrate the position , command value-astrometric corrections,662 To calibrate the position command value, astrometric corrections 614 663 (converting the celestial target position into the target position of 615 664 an ideal telescope) and misalignment corrections (converting it further … … 627 676 into the position as seen from Earth's center (apparent position) -- 628 677 take into account precession and nutation of the Earth and annual 678 \begin{figure}[htb] 679 \begin{center} % Goldener Schnitt 680 \includegraphics*[width=0.185\textwidth,angle=0,clip]{figure6.eps} 681 \caption{The transformation applied to a given set of catalog source 682 coordinates to real-telescope coordinates. These corrections include 683 all necessary astrometric corrections, as well as the pointing 684 correction to transform from an ideal-telescope frame to the frame of a 685 real telescope. 686 %A detailed description of all corrections and the 687 %calibration of the pointing model is given in section~\ref{sec4}. 688 } 689 \label{figure6} 690 \end{center} 691 \end{figure} 629 692 aberration, i.e., apparent displacements caused by the finite speed of 630 693 light combined with the motion of the observer around the Sun during … … 637 700 misalignment correction, all these effects are taken into account. 638 701 639 \begin{figure}[htb]640 \begin{center} % Goldener Schnitt641 \includegraphics*[width=0.185\textwidth,angle=0,clip]{figure6.eps}642 \caption{The transformation applied to a given set of catalog source643 coordinates to real-telescope coordinates. These corrections include644 all necessary astrometric corrections, as well as the pointing645 correction to transform from an ideal-telescope frame to the frame of a646 real telescope. A detailed description of all corrections and the647 calibration of the pointing model is given in section~\ref{sec4}.}648 \label{figure6}649 \end{center}650 \end{figure}651 652 702 \subsection{Pointing model} 653 703 654 704 Imperfections and deformations of the mechanical construction lead to 655 deviations from an ideal telescope. These deviations include the non-exact 656 alignment of axes, and deformations of the telescope structure. To 657 assure reliable pointing and tracking accuracy, such effects have to be 658 taken into account. Therefore the tracking software employs an 659 analytical pointing model based on the {\rm TPOINT}\texttrademark{} 660 telescope modeling software~\cite{tpoint}, also used for 661 optical telescopes. This model, called {\em pointing model}, 662 parameterizes deviations from the ideal telescope. Calibrating the 663 pointing model by mispointing measurements of bright stars, which 664 allows to determine the necessary corrections, is a standard procedure. 665 Once calibrated, the model is applied online. Since an analytical model 666 is used, the source of any deviation can be identified and traced back 667 to components of the telescope mount.\\ 705 deviations from an ideal telescope, including the non-exact 706 alignment of axes, and deformations of the telescope structure. 707 708 %new 709 In the case of the MAGIC telescopes the optical axis of the mirror is 710 defined by an automatic alignment system. This active mirror control 711 is programmed not to change the optical axis once defined, but only 712 controls the optical point spread function of the mirror, i.e., it does 713 not change the center of gravity of the light distribution. 714 This procedure is applied whenever the telescope is observing including 715 any kind of calibration measurement for the drive system. The precision 716 of the axis alignment of the mirrors is better than 0.2$^\prime$ and can 717 therefor be neglected. 718 %new 719 720 %To assure reliable pointing and tracking accuracy, such effects have to 721 %be taken into account. 722 Consequently, to assure reliable pointing and tracking accuracy, 723 mainly the mechanical effects have to be taken into account. 724 Therefore the tracking software employs an analytical pointing model 725 based on the {\rm TPOINT}\texttrademark{} telescope modeling 726 software~\cite{tpoint}, also used for optical telescopes. This model, 727 called {\em pointing model}, parameterizes deviations from the ideal 728 telescope. Calibrating the pointing model by mispointing measurements 729 of bright stars, which allows to determine the necessary corrections, 730 is a standard procedure. Once calibrated, the model is applied online. 731 Since an analytical model is used, the source of any deviation can be 732 identified and traced back to components of the telescope mount.\\ 668 733 669 734 Corrections are parameterized by alt-azimuthal terms~\cite{tpoint}, 670 735 i.e., derived from vector transformations within the proper coordinate 671 system. The following possible misalignments are taken into account:\\ 672 736 system. The following possible misalignments are taken into account:\\\vspace{-2ex} 673 737 \begin{description} 674 738 \item[Zero point corrections ({\em index errors})] Trivial offsets … … 700 764 the encoders, has such a high static friction that in case of reversing 701 765 the direction of the movement, the shaft-encoder will not indicate any 702 movement, even though the telescope is rotating. 766 movement for a small and stable rotation angle, even though the 767 telescope is rotating. Since this offset is stable, it can easily 768 be corrected after it is fully passed. The passage of the hysteresis 769 is currently corrected offline only. 703 770 \end{itemize} 704 771 \vspace{1em} … … 708 775 unnecessary. Another class of deformations of the telescope-support 709 776 frame and the mirrors are non-deterministic and, consequently, pose an 710 ultimate limit of the precision of the pointing correction. 711 712 As discussed below, the size of the total correction (excluding the 713 index error) is on the order of 0.1\textdegree{}. Therefore all individual 714 correction terms are smaller or of similar size. 777 ultimate limit of the precision of the pointing. 778 779 % Moved to results 715 780 716 781 \subsection{Determination} … … 719 784 720 785 To determine the coefficients of a pointing model, calibration 721 data is recorded , consistingof mispointing measurements depending786 data is recorded. It consists of mispointing measurements depending 722 787 on altitude and azimuth angle. Bright stars are tracked with the 723 788 telescope at positions uniformly distributed in local coordinates, 724 i.e. \, in altitude and azimuth angle. To measure the real pointing725 position of the telescope, the reflection of a bright star on a726 s creen in front of the MAGIC PM camera is determined. The center789 i.e., in altitude and azimuth angle. The real pointing 790 position is derived from the position of the reflection of a bright 791 star on a screen in front of the MAGIC camera. The center 727 792 of the camera is defined by LEDs mounted on an ideal ($\pm$1\,mm) 728 793 circle around the camera center, cf.~\citet{Riegel:2005icrc}. … … 735 800 736 801 A 0.0003\,lux, 1/2\(^{\prime\prime}\) high-sensitivity standard PAL CCD 737 camera (\mbox{Watec}~WAT-902\,H, technical details given in 738 table~\ref{table}) equipped with a zoom lens (type: Computar) is used 802 camera (type designation \mbox{Watec}~WAT-902\,H) equipped with a zoom lens (type: Computar) is used 739 803 for the mispointing measurements. The camera is read out at a rate of 740 25\,frames per second using a framer-grabber card in a standard PC. The 741 tradeoff for the high sensitivity of the camera is its high noise level 742 in each single frame recorded. Since there are no rapidly moving 743 objects within the field of view, a high picture quality can be 804 25\,frames per second using a standard frame-grabber card in a standard 805 PC. The camera has been chosen providing adequate performance and 806 easy readout, due to the use of standard components, for a very cheap price 807 ($<$\,500\,Euro). The tradeoff for the high sensitivity of the camera is its high 808 noise level in each single frame recorded. Since there are no rapidly 809 moving objects within the field of view, a high picture quality can be 744 810 achieved by averaging typically 125\,frames (corresponding to 5\,s). An 745 example is shown in figure~\ref{figure7}. This example also 746 illustrates the high sensitivity of the camera, since both pictures of 747 t he telescope structure have been taken with the residual light of less811 example is shown in figure~\ref{figure7}. This example also illustrates 812 the high sensitivity of the camera, since both pictures of the 813 telescope structure have been taken with the residual light of less 748 814 than a half-moon. In the background individual stars can be seen. 749 815 Depending on the installed optics, stars up to 12$^\mathrm{m}$ are … … 753 819 images of stars on the screen. 754 820 755 \begin{table}[htb] 756 \begin{center} 757 \small 758 \begin{tabular}{|l|l|}\hline 759 Model&Watec WAT-902H (CCIR)\\\hline\hline 760 Pick-up Element&1/2" CCD image sensor\\ 761 &(interline transfer)\\\hline 762 Number of total pixels&795(H)x596(V)\\\hline 763 Minimum Illumination&0.0003\,lx. F/1.4 (AGC Hi)\\ 764 &0.002\,lx. F/1.4 (AGC Lo)\\\hline 765 Automatic gain&High: 5\,dB\,-\,50\,dB\\ 766 &Low: 5\,dB\,-\,32\,dB\\\hline 767 S/N&46\,dB (AGC off)\\\hline 768 Shutter Speed&On: 1/50\,-\,1/100\,000\,s\\ (electronic iris)&Off: 1/50\,s\\\hline 769 Backlight compensation&On\\\hline 770 Power Supply&DC +10.8\,V\,-\,13.2\,V\\\hline 771 Weight&Approx. 90\,g\\\hline 772 \end{tabular} 773 \end{center} 774 \caption{Technical specifications of the CCD camera used for 775 measuring of the position of the calibration stars on the PM camera lid.} 776 \label{table} 777 \end{table} 778 821 %\begin{table}[htb] 822 %\begin{center} 823 %\small 824 %\begin{tabular}{|l|l|}\hline 825 %Model&Watec WAT-902H (CCIR)\\\hline\hline 826 %Pick-up Element&1/2" CCD image sensor\\ 827 %&(interline transfer)\\\hline 828 %Number of total pixels&795(H)x596(V)\\\hline 829 %Minimum Illumination&0.0003\,lx. F/1.4 (AGC Hi)\\ 830 %&0.002\,lx. F/1.4 (AGC Lo)\\\hline 831 %Automatic gain&High: 5\,dB\,-\,50\,dB\\ 832 %&Low: 5\,dB\,-\,32\,dB\\\hline 833 %S/N&46\,dB (AGC off)\\\hline 834 %Shutter Speed&On: 1/50\,-\,1/100\,000\,s\\ (electronic iris)&Off: 1/50\,s\\\hline 835 %Backlight compensation&On\\\hline 836 %Power Supply&DC +10.8\,V\,-\,13.2\,V\\\hline 837 %Weight&Approx. 90\,g\\\hline 838 %\end{tabular} 839 %\end{center} 840 %\caption{Technical specifications of the CCD camera used for 841 %measuring of the position of the calibration stars on the PM camera lid.} 842 %\label{table} 843 %\end{table} 779 844 \begin{figure*}[htb] 780 845 \begin{center} … … 795 860 figure~\ref{figure8}. Using the seven LEDs mounted on a circle around 796 861 the camera center, the position of the camera center is determined. 797 Only the upper half of the area instrumented with PMsis visible, since862 Only the upper half of the area instrumented is visible, since 798 863 the lower half is covered by the lower lid, holding a special 799 864 reflecting surface in the center of the camera. The LED positions are 800 865 evaluated by a simple cluster-finding algorithm looking at pixels more 801 866 than three standard deviations above the noise level. The LED position 802 is defined as the center of gravity of its light distribution . The803 search region is defined by the surrounding black-coloured boxes. For867 is defined as the center of gravity of its light distribution, its 868 search region by the surrounding black-colored boxes. For 804 869 simplicity the noise level is determined just by calculating the mean 805 870 and the root-mean-square within the individual search regions below a … … 813 878 gravity, as well as the reconstructed circle on which the LEDs are 814 879 located. The LEDs on the bottom part are hidden by the lower lid, 815 holding a screen in front of the PM camera. For calibration, the center 816 of gravity of the measured star, as visible in the center, is compared 817 to the center of the circle given by the LEDs, coinciding with the 818 center of the PM camera. The black regions are the search regions for 880 holding a screen in front of the camera. 881 %For calibration, the center 882 %of gravity of the measured star, as visible in the center, is compared 883 %to the center of the circle given by the LEDs, coinciding with the 884 %center of the PM camera. 885 The black regions are the search regions for 819 886 the LEDs and the calibration star. A few dead pixels in the CCD camera 820 can also be recognized. 887 can also be recognized.} 821 888 \label{figure8} 822 889 \end{center} … … 831 898 determination can be improved further by applying small offsets of 832 899 the non-ideal LED positions. The radius distribution is Gaussian 833 and its resolution is $\sigma \,\apprle$\,1\,mm900 and its resolution is $\sigma$\,$\apprle$\,1\,mm 834 901 ($\mathrm{d}r/r\approx0.3$\textperthousand) on the camera plane 835 corresponding to $\sim$1 \,arcsec.836 837 The center of the LEDring is calculated as the average of all circle838 centers after quality cuts. The resolution of the centeris839 $\sim$2 \,arcsec. In this setup, the large number of LEDs guarantees840 operation even in case one LED is damaged or could not be detected due841 toscattered light.902 corresponding to $\sim$1$^{\prime\prime}$. 903 904 The center of the ring is calculated as the average of all circle 905 centers after quality cuts. Its resolution is 906 $\sim$2$^{\prime\prime}$. In this setup, the large number of LEDs guarantees 907 operation even in case one LED could not be detected due to damage or 908 scattered light. 842 909 843 910 To find the spot of the reflected star itself, the same cluster-finder … … 866 933 be improved to a value below the intrinsic resolution of the system, 867 934 i.e., below shaft-encoder resolution. In more than 83\% of all cases the 868 tracking accuracy is better than 0.02\textdegree{} ($\sim$1.3\,arcmin)869 and it hardly ever exceeds 0.04\textdegree. The few datasets exceeding870 0.04\textdegree{}are very likely due to imperfect measurement of the871 real pointing position of the telescope, i.e. \, the center of gravity of935 tracking accuracy is better than 1.3$^\prime$ 936 and it hardly ever exceeds 2.5$^\prime$. The few datasets exceeding 937 2.5$^\prime$ are very likely due to imperfect measurement of the 938 real pointing position of the telescope, i.e., the center of gravity of 872 939 the star light. 940 941 The average absolute correction applied (excluding the index error) is on 942 the order of 4$^\prime$. Given the size, weight and structure of 943 the telescope this proves a very good alignment and low sagging of the 944 structure. The elevation hysteresis, which is intrinsic to the 945 structure, the non-perpendicularity and non-centricity of the axes are 946 all in the order of 3$^\prime$, while the azimuth axis 947 misalignment is $<$\,0.6$^\prime$. These numbers are well in agreement 948 with the design tolerances of the telescope. 873 949 874 950 \begin{figure}[htb] … … 890 966 \subsubsection{Limitations} 891 967 892 The ultimate limit on the achievable tracking precision are effects,968 The ultimate limit on the achievable pointing precision are effects, 893 969 which are difficult to correlate or measure, and non-deterministic 894 970 deformations of the structure or mirrors. For example, the azimuth … … 899 975 deformations. Other deformations are caused by temperature changes and 900 976 wind loads which are difficult to control for telescopes without dome, 901 and which cannot be model led. It should be noted that the azimuth structure977 and which cannot be modeled. It should be noted that the azimuth structure 902 978 can change its diameter by up to 3\,cm due to day-night temperature 903 979 differences, indicating that thermal effects have a non-negligible and 904 980 non-deterministic influence. 905 981 982 Like every two axis mount, also an alt-azimuth mount has a blind spot 983 near its upward position resulting from misalignments of the axis which 984 are impossible to correct by moving one axis or the other. From the 985 size of the applied correction it can be derived that the blind spot 986 must be on the order of $\lesssim$\,6$^\prime$ around zenith. 987 Although the MAGIC drive system is powerful enough to keep on track 988 pointing about 6$^\prime$ away from zenith, for safety reasons, i.e., 989 to avoid fast movment under normal observation conditions, the observation 990 limit has been set to $\theta$\,$<$\,30$^\prime$. Such fast movements 991 are necessary to change the azimuth position from moving the telescope 992 upwards in the East to downwards in the South. In the case of an ideal 993 telescope, pointing at zenith, even an infinitely fast movement would 994 be required. 995 906 996 \subsubsection{Stability} 907 997 908 With each measurement of a calibration-star also the present tracking909 uncertainty is recorded. This allows for monitoring of the tracking998 With each measurement of a calibration-star also the present pointing 999 uncertainty is recorded. This allows for monitoring of the pointing 910 1000 quality and for offline correction. In figure~\ref{figure10} the 911 evolution of the measured residuals over the years are shown. The912 continuous monitoring has been started in March 2005 and is still913 ongoing. Quantiles are shown since the distribution can be highly914 asymmetric. The points have been grouped, where the grouping reflects915 data taken under the same conditions (pointing model, mirror alignment,916 etc.) It should be noted, that the measured residuals depend on zenith917 and azimuth angle, i.e., the distributions shown are biased due to918 inhomogeneous distributions on the sky in case of low statistics.919 Therefore the available statistics is given in table~\ref{table2}.920 %, for convenience, together with the average measured mispointing.921 922 1001 \begin{figure}[htb] 923 1002 \begin{center} 924 1003 \includegraphics*[width=0.48\textwidth,angle=0,clip]{figure10.eps} 925 \caption{The distribution of mispointing measurements, which is an 926 exact measure of accuracy of the command values send to the drive 927 system. The plot shows its time-evolution. Details on the separation 928 and the available statistics is given in the caption of 929 table~\ref{table2}. Since the distribution is highly asymmetric, 930 quantiles are shown, from bottom to top, at 5\%, 13\%, 32\%, 68\%, 87\% 931 and 95\%. The dark grey region belong to the region between quantiles 932 32\% and 68\%. 933 } 1004 \caption{The distribution of mispointing measurements. The 1005 measurement is a direct measurement of the pointing accuracy. The plot 1006 shows its time-evolution. Details on the bin edges and the available 1007 statistics is given in the caption of table~\ref{table2}. Since the 1008 distribution is asymmetric, quantiles are shown, from bottom to top, at 1009 5\%, 13\%, 32\%, 68\%, 87\% and 95\%. The dark grey region belong to 1010 the region between quantiles 32\% and 68\%. } 934 1011 \label{figure10} 935 \end{center} 1012 \end{center} 936 1013 \end{figure} 937 938 The mirror focusing can influence the alignment of the optical axis of 939 the telescope, i.e., it can modify the pointing model. Therefore a mirror 940 refocusing can worsen the tracking accuracy, later corrected by a new 941 pointing model. Also the determination of the pointing model relies on 942 a good statistical basis, because the measured residuals are of a 943 similar magnitude as the accuracy of a single calibration-star 944 measurement. The visible improvements and deterioration are mainly a 945 consequence of new mirror focusing and following implementations of new 946 pointing models. The improvement over the past year is explained by the 947 gain in statistics. 948 949 On average the systematic pointing uncertainty was always better than 950 three shaft-encoder steps (corresponding to 4\,arcmin), most of the 951 time better than 2.6\,arcmin and well below one shaft-encoder step, 952 i.e.\ 1.3\,arcmin, in the past year. Except changes to the pointing 953 model or the optical axis, as indicated by the bin edges, no 954 degradation or change with time of the pointing model could be found. 955 956 \section{Scalability}\label{sec5} 957 958 With the aim to reach lower energy thresholds the next generation of 959 Cherenkov telescopes will become larger and heavier. Therefore more 960 powerful drive systems will be needed. The scalable drive system of the 961 MAGIC telescope is suited to meet this challenge. With its synchronous 962 motors and their master-slave setup it can easily be extended to larger 963 telescopes at moderate costs or even scaled down using less powerful 964 components. A motion accuracy at least of the order of the 965 shaft-encoder resolution is guaranteed. Real tracking accuracy -- 966 already including all possible pointing corrections -- is dominated by 967 dynamic and unpredictable deformations of the mount, e.g., temperature 968 expansion. 969 1014 evolution of the measured residuals over the years are shown. The 1015 continuous monitoring has been started in March 2005 and is still 1016 ongoing. Quantiles are shown since the distribution can be 1017 asymmetric depending on how the residuals are distributed on the sky. The 1018 points have been grouped, where the grouping reflects data taken under 1019 the same conditions (pointing model, mirror alignment, etc.). It should 1020 be noted, that the measured residuals depend on zenith and azimuth 1021 angle, i.e., the distributions shown are biased due to inhomogeneous 1022 distributions on the sky in case of low statistics. Therefore the 1023 available statistics is given in table~\ref{table2}. 970 1024 \begin{table}[htb] 971 1025 \begin{center} 972 1026 \begin{tabular}{|l|c|}\hline 973 1027 Begin&Counts\\\hline\hline 974 2005/03/20&29\\ 975 2005/04/29&43\\ 976 2005/05/25&30\\ 977 2005/06/08&26\\ 978 2005/08/15&160\\ 979 2005/09/12&22\\ 1028 2005/03/20&29\\%& 2005/11/24&38\\ 1029 2005/04/29&43\\%& 2006/03/19&502\\ 1030 2005/05/25&30\\%& 2006/10/17&827\\ 1031 2005/06/08&26\\%& 2007/07/31&87\\ 1032 2005/08/15&160\\%& 2008/01/14&542\\ 1033 2005/09/12&22\\\hline%& 2008/06/18&128\\\hline 1034 \end{tabular} 1035 \hfill 1036 \begin{tabular}{|l|c|}\hline 1037 Begin&Counts\\\hline\hline 980 1038 2005/11/24&38\\ 981 1039 2006/03/19&502\\ … … 984 1042 2008/01/14&542\\ 985 1043 2008/06/18&128\\\hline 986 \end{tabular} 1044 \end{tabular}\hfill 987 1045 \end{center} 988 1046 \caption{Available statistics corresponding to the distributions … … 995 1053 \end{table} 996 1054 997 \section{Outlook} 1055 The mirror focusing can influence the alignment of the optical axis of 1056 the telescope, i.e., it can modify the pointing model. Therefore a 1057 calibration of the mirror refocusing can worsen the tracking accuracy, 1058 later corrected by a new pointing model. Although the automatic mirror 1059 control is programmed such that a new calibration should not change the 1060 center of gravity of the light distribution, it happened sometimes in 1061 the past due to software errors. 1062 1063 The determination of the pointing model also relies on a good 1064 statistical basis, because the measured residuals are of a similar 1065 magnitude as the accuracy of a single calibration-star measurement. The 1066 visible improvements and deterioration are mainly a consequence of new 1067 mirror focusing and following implementations of new pointing models. 1068 The improvement over the past year is explained by the gain in 1069 statistics. 1070 1071 On average the systematic pointing uncertainty was always better than 1072 three shaft-encoder steps (corresponding to 4$^\prime$), most of the 1073 time better than 2.6$^\prime$ and well below one shaft-encoder step, 1074 i.e.\ 1.3$^\prime$, in the past year. Except changes to the pointing 1075 model or the optical axis, as indicated by the bin edges, no 1076 degradation or change with time of the pointing model or 1077 a worsening of the limit given by the telescope mechanics could be found. 1078 1079 \section{Scalability}\label{sec5} 1080 1081 With the aim to reach lower energy thresholds, the next generation of 1082 Cherenkov telescopes will also include larger and heavier ones. 1083 Therefore more powerful drive systems will be needed. The scalable 1084 drive system of the MAGIC telescope is suited to meet this challenge. 1085 With its synchronous motors and their master-slave setup, it can easily 1086 be extended to larger telescopes at moderate costs, or even scaled down 1087 to smaller ones using less powerful components. Consequently, 1088 telescopes in future projects, with presumably different sizes, can be 1089 driven by similar components resulting in a major 1090 simplification of maintenance. With the current setup, a tracking 1091 accuracy at least of the order of the shaft-encoder resolution is 1092 guaranteed. Pointing accuracy -- already including all possible 1093 pointing corrections -- is dominated by dynamic and unpredictable 1094 deformations of the mount, e.g., temperature expansion. 1095 1096 \section{Outlook}\label{outlook} 998 1097 999 1098 Currently, efforts are ongoing to implement the astrometric subroutines … … 1018 1117 without influencing the general functionality of the system. 1019 1118 1119 An upgrade of the MAGIC\,I drive system according to the improvements 1120 applied for MAGIC\,II is ongoing. 1121 1020 1122 \section{Conclusions}\label{conclusions} 1021 1123 … … 1023 1125 system for the MAGIC telescope. From its hardware installation and 1024 1126 software implementation, the installed drive system exceeds its design 1025 specifications. At the same time the system performs reliably and 1026 stably, showing no deterioration after five years of routine operation. 1027 The mechanical precision of the motor movement is almost ten times 1028 better than the readout on the telescope axes. The tracking accuracy is 1029 dominated by random deformations and hysteresis effects of the mount, 1030 but still within limits within which the position of the telescope axes 1031 can be measured. The system features integrated tools, like an 1032 analytical pointing model. Fast repositioning for gamma-ray bursts 1033 followup is achieved on average within less than 45 seconds, or, if 1034 movements {\em across the zenith} are allowed, within less than 30 1035 seconds. Thus, the drive system makes MAGIC the best suited telescope 1036 for observations of gamma-ray burst at very high energies. 1127 specifications as given in section~\ref{design}. At the same time the 1128 system performs reliably and stably, showing no deterioration after 1129 five years of routine operation. The mechanical precision of the motor 1130 movement is almost ten times better than the readout on the telescope 1131 axes. The tracking accuracy is dominated by random deformations and 1132 hysteresis effects of the mount, but still negligible 1133 compared to the measurement of the position of the telescope axes. The 1134 system features integrated tools, like an analytical pointing model. 1135 Fast positioning for gamma-ray burst followup is achieved on average 1136 within less than 45 seconds, or, if movements {\em across the zenith} 1137 are allowed, 30 seconds. Thus, the drive system makes 1138 MAGIC the best suited telescope for observations of these phenomena at 1139 very high energies. 1037 1140 1038 1141 For the second phase of the MAGIC project and particularly for the 1039 second telescope, the system has been further improved by replacing the 1040 partially analog communication with a completely digital one. 1142 second telescope, the drive system has been further improved. 1041 1143 By design, the drive system is easily scalable from its current 1042 1144 dimensions to larger and heavier telescope installations as required 1043 1145 for future projects. The improved stability is also expected to meet 1044 1146 the stability requirements, necessary when operating a larger number of 1045 tele copes.1147 telescopes. 1046 1148 1047 1149 \section[]{Acknowledgments} 1048 1150 The authors acknowledge the support of the MAGIC collaboration, and 1049 thank the IAC for providing excellent working conditions at the Roque 1050 de los Muchachos Observatory in La Palma. The MAGIC telescope project 1051 is mainly supported by BMBF (Germany), MCI-NN (Spain), INFN and MUR 1052 (Italy). We thank the construction department of the MPI for Physics, 1053 particularly Peter Sawallisch, for their help in the design and 1054 installation of the drive system. We are grateful for Eckart Lorenz's 1055 help with the hardware installations and also for some important 1056 comments concerning this manuscript. R.M.W.\ acknowledges financial 1057 support by the Max Planck Society. His research is also supported in 1058 part by the DFG Cluster of Excellence ``Origin and Structure of the 1059 Universe''. 1151 thank the IAC for providing excellent working conditions at the 1152 Observatorio del Roque de los Muchachos. The MAGIC project is mainly 1153 supported by BMBF (Germany), MCI (Spain), INFN (Italy). We thank the 1154 construction department of the MPI for Physics, for their help in the 1155 design and installation of the drive system as well as Eckart Lorenz, 1156 for some important comments concerning this manuscript. R.M.W.\ 1157 acknowledges financial support by the MPG. His research is also 1158 supported by the DFG Cluster of Excellence ``Origin and Structure of 1159 the Universe''. 1060 1160 1061 1161 \begin{thebibliography}{00} … … 1069 1169 \bibitem[Cortina et~al.(2005)]{Cortina:2005} J.~Cortina et~al. (MAGIC Collab.), in: Proc. 29th Int. Cosm. 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