Pulsars with NenuFAR: backend and pipelines. (arXiv:2009.02076v2 [astro-ph.IM] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Bondonneau_L/0/1/0/all/0/1">L. Bondonneau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Griessmeier_J/0/1/0/all/0/1">J.-M. Grie&#xdf;meier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Theureau_G/0/1/0/all/0/1">G. Theureau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cognard_I/0/1/0/all/0/1">I. Cognard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brionne_M/0/1/0/all/0/1">M. Brionne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kondratiev_V/0/1/0/all/0/1">V. Kondratiev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bilous_A/0/1/0/all/0/1">A.Bilous</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McKee_J/0/1/0/all/0/1">J. W. McKee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zarka_P/0/1/0/all/0/1">P. Zarka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Viou_C/0/1/0/all/0/1">C. Viou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guillemot_L/0/1/0/all/0/1">L. Guillemot</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_S/0/1/0/all/0/1">S. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Main_R/0/1/0/all/0/1">R. Main</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pilia_M/0/1/0/all/0/1">M. Pilia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Possenti_A/0/1/0/all/0/1">A. Possenti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serylak_M/0/1/0/all/0/1">M. Serylak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shaifullah_G/0/1/0/all/0/1">G. Shaifullah</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tiburzi_C/0/1/0/all/0/1">C. Tiburzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Verbiest_J/0/1/0/all/0/1">J. P. W. Verbiest</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wu_Z/0/1/0/all/0/1">Z. Wu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wucknitz_O/0/1/0/all/0/1">O. Wucknitz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yerin_S/0/1/0/all/0/1">S. Yerin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Briand_C/0/1/0/all/0/1">C.Briand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cecconi_B/0/1/0/all/0/1">B. Cecconi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Corbel_S/0/1/0/all/0/1">S. Corbel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dallier_R/0/1/0/all/0/1">R. Dallier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loh_A/0/1/0/all/0/1">A. Loh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Martin_L/0/1/0/all/0/1">L. Martin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girard_J/0/1/0/all/0/1">J. N. Girard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tasse_C/0/1/0/all/0/1">C.Tasse</a>

NenuFAR (New extension in Nanc{c}ay upgrading LoFAR) is a new radio
telescope developed and built on the site of the Nanc{c}ay Radio Observatory.
It is designed to observe the largely unexplored frequency window from 10 to
85,MHz, offering a high sensitivity across its full bandwidth. NenuFAR has
started its “early science” operation in July 2019, with 58% of its final
collecting area being available. Pulsars are one of the major topics for the
scientific exploitation of this frequency range and represent an important
challenge in terms of instrumentation. Designing instrumentation at these
frequencies is complicated by the need to compensate for the effects of both
the interstellar medium and the ionosphere on the observed signal. Our
real-time pipeline LUPPI (Low frequency Ultimate Pulsar Processing
Instrumentation) is able to cope with a high data rate and to provide real-time
coherent de-dispersion down to the lowest frequencies reached by NenuFAR
(10,MHz). The full backend functionality is described, as well as the main
pulsar observing modes (folded, single-pulse, waveform, and dynamic spectrum).
This instrumentation allowed us to detect 172 pulsars in our first targeted
search below 85,MHz, including 10 millisecond pulsars (6 of which detected for
the first time below 100 MHz). We also present some of the “early science”
results of NenuFAR on pulsars: a high frequency resolution mapping of PSR
B1919$+$21’s emission profile and a detailed observation of single-pulse
sub-structures from PSR~B0809$+$74 down to 16,MHz, the high rate of
giant-pulse emission from the Crab pulsar detected at 68.7,MHz (43
events/min), and the illustration of the very good timing performance of the
instrumentation, allowing us to study dispersion measure variations in great
detail.

NenuFAR (New extension in Nanc{c}ay upgrading LoFAR) is a new radio
telescope developed and built on the site of the Nanc{c}ay Radio Observatory.
It is designed to observe the largely unexplored frequency window from 10 to
85,MHz, offering a high sensitivity across its full bandwidth. NenuFAR has
started its “early science” operation in July 2019, with 58% of its final
collecting area being available. Pulsars are one of the major topics for the
scientific exploitation of this frequency range and represent an important
challenge in terms of instrumentation. Designing instrumentation at these
frequencies is complicated by the need to compensate for the effects of both
the interstellar medium and the ionosphere on the observed signal. Our
real-time pipeline LUPPI (Low frequency Ultimate Pulsar Processing
Instrumentation) is able to cope with a high data rate and to provide real-time
coherent de-dispersion down to the lowest frequencies reached by NenuFAR
(10,MHz). The full backend functionality is described, as well as the main
pulsar observing modes (folded, single-pulse, waveform, and dynamic spectrum).
This instrumentation allowed us to detect 172 pulsars in our first targeted
search below 85,MHz, including 10 millisecond pulsars (6 of which detected for
the first time below 100 MHz). We also present some of the “early science”
results of NenuFAR on pulsars: a high frequency resolution mapping of PSR
B1919$+$21’s emission profile and a detailed observation of single-pulse
sub-structures from PSR~B0809$+$74 down to 16,MHz, the high rate of
giant-pulse emission from the Crab pulsar detected at 68.7,MHz (43
events/min), and the illustration of the very good timing performance of the
instrumentation, allowing us to study dispersion measure variations in great
detail.

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