An ultra-wide bandwidth (704 to 4032 MHz) receiver for the Parkes radio telescope. (arXiv:1911.00656v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Hobbs_G/0/1/0/all/0/1">G. Hobbs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manchester_R/0/1/0/all/0/1">R. N. Manchester</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunning_A/0/1/0/all/0/1">A. Dunning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jameson_A/0/1/0/all/0/1">A. Jameson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roberts_P/0/1/0/all/0/1">P. Roberts</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+George_D/0/1/0/all/0/1">D. George</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Green_J/0/1/0/all/0/1">J. A. Green</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tuthill_J/0/1/0/all/0/1">J. Tuthill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Toomey_L/0/1/0/all/0/1">L. Toomey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaczmarek_J/0/1/0/all/0/1">J. F. Kaczmarek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mader_S/0/1/0/all/0/1">S. Mader</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marquarding_M/0/1/0/all/0/1">M. Marquarding</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ahmed_A/0/1/0/all/0/1">A. Ahmed</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amy_S/0/1/0/all/0/1">S. W. Amy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bailes_M/0/1/0/all/0/1">M. Bailes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beresford_R/0/1/0/all/0/1">R. Beresford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bhat_N/0/1/0/all/0/1">N. D. R. Bhat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bock_D/0/1/0/all/0/1">D. C.-J. Bock</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bourne_M/0/1/0/all/0/1">M. Bourne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bowen_M/0/1/0/all/0/1">M. Bowen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brothers_M/0/1/0/all/0/1">M. Brothers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cameron_A/0/1/0/all/0/1">A. D. Cameron</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretti_E/0/1/0/all/0/1">E. Carretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carter_N/0/1/0/all/0/1">N. Carter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castillo_S/0/1/0/all/0/1">S. Castillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chekkala_R/0/1/0/all/0/1">R. Chekkala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheng_W/0/1/0/all/0/1">W. Cheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chung_Y/0/1/0/all/0/1">Y. Chung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Craig_D/0/1/0/all/0/1">D. A. Craig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_S/0/1/0/all/0/1">S. Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dawson_J/0/1/0/all/0/1">J. R. Dawson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dempsey_J/0/1/0/all/0/1">J. Dempsey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doherty_P/0/1/0/all/0/1">P. Doherty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dong_B/0/1/0/all/0/1">B. Dong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edwards_P/0/1/0/all/0/1">P. G. Edwards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ergesh_T/0/1/0/all/0/1">T. Ergesh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gao_X/0/1/0/all/0/1">X. Y. Gao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_J/0/1/0/all/0/1">J. L. Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hayman_D/0/1/0/all/0/1">D. B. Hayman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Indermuehle_B/0/1/0/all/0/1">B. T. Indermuehle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jeganathan_K/0/1/0/all/0/1">K. Jeganathan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnston_S/0/1/0/all/0/1">S. Johnston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kanoniuk_H/0/1/0/all/0/1">H. Kanoniuk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kesteven_M/0/1/0/all/0/1">M. Kesteven</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kramer_M/0/1/0/all/0/1">M. Kramer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leach_M/0/1/0/all/0/1">M. Leach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mcintyre_V/0/1/0/all/0/1">V. J. Mcintyre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moss_V/0/1/0/all/0/1">V. A. Moss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oslowski_S/0/1/0/all/0/1">S. Oslowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Phillips_C/0/1/0/all/0/1">C. J. Phillips</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pope_N/0/1/0/all/0/1">N. C. Pope</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Preisig_B/0/1/0/all/0/1">B. Preisig</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Price_D/0/1/0/all/0/1">D. C. Price</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reeves_K/0/1/0/all/0/1">K. Reeves</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reilly_L/0/1/0/all/0/1">L. Reilly</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reynolds_J/0/1/0/all/0/1">J. E. Reynolds</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robishaw_T/0/1/0/all/0/1">T. Robishaw</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Roush_P/0/1/0/all/0/1">P. Roush</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruckley_T/0/1/0/all/0/1">T. Ruckley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sadler_E/0/1/0/all/0/1">E. M. Sadler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarkissian_J/0/1/0/all/0/1">J. Sarkissian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Severs_S/0/1/0/all/0/1">S. Severs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shannon_R/0/1/0/all/0/1">R. M. Shannon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smart_K/0/1/0/all/0/1">K. W. Smart</a>, et al. (8 additional authors not shown)

We describe an ultra-wide-bandwidth, low-frequency receiver (“UWL”) recently
installed on the Parkes radio telescope. The receiver system provides
continuous frequency coverage from 704 to 4032 MHz. For much of the band (~60%)
the system temperature is approximately 22K and the receiver system remains in
a linear regime even in the presence of strong mobile phone transmissions. We
discuss the scientific and technical aspects of the new receiver including its
astronomical objectives, as well as the feed, receiver, digitiser and
signal-processor design. We describe the pipeline routines that form the
archive-ready data products and how those data files can be accessed from the
archives. The system performance is quantified including the system noise and
linearity, beam shape, antenna efficiency, polarisation calibration and timing
stability.

We describe an ultra-wide-bandwidth, low-frequency receiver (“UWL”) recently
installed on the Parkes radio telescope. The receiver system provides
continuous frequency coverage from 704 to 4032 MHz. For much of the band (~60%)
the system temperature is approximately 22K and the receiver system remains in
a linear regime even in the presence of strong mobile phone transmissions. We
discuss the scientific and technical aspects of the new receiver including its
astronomical objectives, as well as the feed, receiver, digitiser and
signal-processor design. We describe the pipeline routines that form the
archive-ready data products and how those data files can be accessed from the
archives. The system performance is quantified including the system noise and
linearity, beam shape, antenna efficiency, polarisation calibration and timing
stability.

http://arxiv.org/icons/sfx.gif