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@ARTICLE{Abe:586739,
author = {Abe, S. and Aguasca-Cabot, A. and Agudo, I. and Crespo, N.
Alvarez and Antonelli, L. A. and Aramo, C. and Arbet-Engels,
A. and Artero, M. and Asano, K. and Aubert, P. and Baktash,
A. and Bamba, A. and Larriva, A. Baquero and Baroncelli, L.
and de Almeida, U. Barres and Barrio, J. A. and Batkovic, I.
and Baxter, J. and González, J. Becerra and Bernardini, E.
and Bernardos, M. I. and Medrano, J. Bernete and Berti, A.
and Bhattacharjee, P. and Biederbeck, N. and Bigongiari, C.
and Bissaldi, E. and Blanch, O. and Bordas, P. and
Bulgarelli, A. and Burelli, I. and Buscemi, M. and Cardillo,
M. and Caroff, S. and Carosi, A. and Cassol, F. and Cauz, D.
and Ceribella, G. and Chai, Y. and Cheng, K. and Chiavassa,
A. and Chikawa, M. and Chytka, L. and Cifuentes, A. and
Contreras, J. L. and Cortina, J. and Costantini, H. and
D'Amico, G. and Dalchenko, M. and De Angelis, A. and de
Lavergne, M. de Bony and De Lotto, B. and de Menezes, R. and
Deleglise, G. and Delgado, C. and Mengual, J. Delgado and
della Volpe, D. and Dellaiera, M. and Depaoli, D. and Di
Piano, A. and Di Pierro, F. and Di Tria, R. and Di Venere,
L. and Díaz, C. and Dominik, R. M. and Dominis Prester, D.
and Donini, A. and Dorner, D. and Doro, M. and Elsässer, D.
and Emery, G. and Escudero, J. and Fallah Ramazani, V. and
Ferrara, G. and Fiasson, A. and Coromina, L. Freixas and
Fröse, S. and Fukami, S. and Fukazawa, Y. and Garcia, E.
and López, R. Garcia and Gasparrini, D. and Geyer, F. and
Paiva, J. Giesbrecht and Giglietto, N. and Giordano, F. and
Giro, E. and Gliwny, P. and Godinovic, N. and Grau, R. and
Green, J. and Green, D. and Gunji, S. and Hackfeld, J. and
Hadasch, D. and Hahn, A. and Hashiyama, K. and Hassan, T.
and Hayashi, K. and Heckmann, L. and Heller, M. and
Llorente, J. Herrera and Hirotani, K. and Hoffmann, D. and
Horns, D. and Houles, J. and Hrabovsky, M. and Hrupec, D.
and Hui, D. and Hütten, M. and Imazawa, R. and Inada, T.
and Inome, Y. and Ioka, K. and Iori, M. and Ishio, K. and
Iwamura, Y. and Jacquemont, M. and Martinez, I. Jimenez and
Jurysek, J. and Kagaya, M. and Karas, V. and Katagiri, H.
and Kataoka, J. and Kerszberg, D. and Kobayashi, Y. and
Kong, A. and Kubo, H. and Kushida, J. and Lainez, M. and
Lamanna, G. and Lamastra, A. and Flour, T. Le and Linhoff,
M. and Longo, F. and López-Coto, R. and López-Moya, M. and
López-Oramas, A. and Loporchio, S. and Lorini, A. and
Luque-Escamilla, P. L. and Majumdar, P. and Makariev, M. and
Mandat, D. and Manganaro, M. and Manicò, G. and Mannheim,
K. and Mariotti, M. and Marquez, P. and Marsella, G. and
Martí, J. and Martinez, O. and Martínez, G. and Martínez,
M. and Marusevec, P. and Mas-Aguilar, A. and Maurin, G. and
Mazin, D. and Guillen, E. Mestre and Micanovic, S. and
Miceli, D. and Miener, T. and Miranda, J. M. and Mirzoyan,
R. and Mizuno, T. and Gonzalez, M. Molero and Molina, E. and
Montaruli, T. and Monteiro, I. and Moralejo, A. and
Morcuende, D. and Morselli, A. and Mrakovcic, K. and Murase,
K. and Nagai, A. and Nakamori, T. and Nickel, L. and Nievas,
M. and Nishijima, K. and Noda, K. and Nosek, D. and Nozaki,
S. and Ohishi, M. and Ohtani, Y. and Okazaki, N. and
Okumura, A. and Orito, R. and Otero-Santos, J. and
Palatiello, M. and Paneque, D. and Pantaleo, F. R. and
Paoletti, R. and Paredes, J. M. and Pavletić, L. and Pech,
M. and Pecimotika, M. and Pérez, A. and Pietropaolo, E. and
Pirola, G. and Plard, C. and Podobnik, F. and Poireau, V.
and Polo, M. and Pons, E. and Prandini, E. and Prast, J. and
Principe, G. and Priyadarshi, C. and Prouza, M. and Rando,
R. and Rhode, W. and Ribó, M. and Rizi, V. and Fernandez,
G. Rodriguez and Saito, T. and Sakurai, S. and Sanchez, D.
A. and Šarić, T. and Saturni, F. G. and Schleicher, B. and
Schmuckermaier, F. and Schubert, J. L. and Schussler, F. and
Schweizer, T. and Arroyo, M. Seglar and Sitarek, J. and
Sliusar, V. and Spolon, A. and Strišković, J. and Strzys,
M. and Suda, Y. and Sunada, Y. and Tajima, H. and Takahashi,
M. and Takahashi, H. and Takata, J. and Takeishi, R. and
Tam, P. H. T. and Tanaka, S. J. and Tateishi, D. and
Tejedor, L. A. and Temnikov, P. and Terada, Y. and Terauchi,
K. and Terzic, T. and Teshima, M. and Tluczykont, M. and
Tokanai, F. and Torres, D. F. and Travnicek, P. and Truzzi,
S. and Tutone, A. and Uhlrich, G. and Vacula, M. and van
Scherpenberg, J. and Vázquez Acosta, M. and Verguilov, V.
and Viale, I. and Vigliano, A. and Vigorito, C. F. and
Vitale, V. and Voutsinas, G. and Vovk, I. and Vuillaume, T.
and Walter, R. and Will, M. and Yamamoto, T. and Yamazaki,
R. and Yoshida, T. and Yoshikoshi, T. and Zywucka, N. and
Bernloehr, K. and Gueta, O. and Kosack, K. and Maier, G. and
Watson, J.},
title = {{O}bservations of the {C}rab {N}ebula and {P}ulsar with the
{L}arge-{S}ized {T}elescope {P}rototype of the {C}herenkov
{T}elescope {A}rray},
reportid = {PUBDB-2023-03977, arXiv:2306.12960},
year = {2023},
note = {Submitted to ApJ. v2: solved issue with acknowledgements},
abstract = {CTA (Cherenkov Telescope Array) is the next generation
ground-based observatory for gamma-ray astronomy at
very-high energies. The Large-Sized Telescope prototype
$(\LST)$ is located at the Northern site of CTA, on the
Canary Island of La Palma. LSTs are designed to provide
optimal performance in the lowest part of the energy range
covered by CTA, down to $\simeq 20$ GeV. \LST started
performing astronomical observations in November 2019,
during its commissioning phase, and it has been taking data
since then. We present the first \LST observations of the
Crab Nebula, the standard candle of very-high energy
gamma-ray astronomy, and use them, together with
simulations, to assess the basic performance parameters of
the telescope. The data sample consists of around 36 hours
of observations at low zenith angles collected between
November 2020 and March 2022. \LST has reached the expected
performance during its commissioning period - only a minor
adjustment of the preexisting simulations was needed to
match the telescope behavior. The energy threshold at
trigger level is estimated to be around 20 GeV, rising to
$\simeq 30$ GeV after data analysis. Performance parameters
depend strongly on energy, and on the strength of the
gamma-ray selection cuts in the analysis: angular resolution
ranges from 0.12 to 0.40 degrees, and energy resolution from
15 to 50\%. Flux sensitivity is around 1.1\% of the Crab
Nebula flux above 250 GeV for a 50-h observation (12\% for
30 minutes). The spectral energy distribution (in the 0.03 -
30 TeV range) and the light curve obtained for the Crab
Nebula agree with previous measurements, considering
statistical and systematic uncertainties. A clear periodic
signal is also detected from the pulsar at the center of the
Nebula.},
keywords = {energy, threshold (INSPIRE) / gamma ray, VHE (INSPIRE) /
Cherenkov Telescope Array (INSPIRE) / GeV (INSPIRE) /
performance (INSPIRE) / flux (INSPIRE) / pulsar (INSPIRE) /
angular resolution (INSPIRE) / observatory (INSPIRE) /
sensitivity (INSPIRE) / energy resolution (INSPIRE) / site
(INSPIRE) / spectral energy distribution (INSPIRE) / trigger
(INSPIRE) / statistical (INSPIRE) / TeV (INSPIRE)},
cin = {$Z_CTAS$},
cid = {$I:(DE-H253)Z_CTAS-20210408$},
pnm = {613 - Matter and Radiation from the Universe (POF4-613)},
pid = {G:(DE-HGF)POF4-613},
experiment = {EXP:(DE-H253)CTA-20150101},
typ = {PUB:(DE-HGF)25},
eprint = {2306.12960},
howpublished = {arXiv:2306.12960},
archivePrefix = {arXiv},
SLACcitation = {$\%\%CITATION$ = $arXiv:2306.12960;\%\%$},
url = {https://bib-pubdb1.desy.de/record/586739},
}
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