Home > Publications database > Observations of the Crab Nebula and Pulsar with the Large-Sized Telescope Prototype of the Cherenkov Telescope Array > print

001     586739
005     20240114021242.0
024 7 _ |a CTA-LSTProject:2023haa
|2 INSPIRETeX
024 7 _ |a inspire:2670948
|2 inspire
024 7 _ |a arXiv:2306.12960
|2 arXiv
024 7 _ |a altmetric:150475495
|2 altmetric
037 _ _ |a PUBDB-2023-03977
041 _ _ |a English
088 _ _ |a arXiv:2306.12960
|2 arXiv
100 1 _ |a Abe, S.
|b 0
245 _ _ |a Observations of the Crab Nebula and Pulsar with the Large-Sized Telescope Prototype of the Cherenkov Telescope Array
260 _ _ |c 2023
336 7 _ |a Preprint
|b preprint
|m preprint
|0 PUB:(DE-HGF)25
|s 1689939208_647181
|2 PUB:(DE-HGF)
336 7 _ |a WORKING_PAPER
|2 ORCID
336 7 _ |a Electronic Article
|0 28
|2 EndNote
336 7 _ |a preprint
|2 DRIVER
336 7 _ |a ARTICLE
|2 BibTeX
336 7 _ |a Output Types/Working Paper
|2 DataCite
500 _ _ |a Submitted to ApJ. v2: solved issue with acknowledgements
520 _ _ |a 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.
536 _ _ |a 613 - Matter and Radiation from the Universe (POF4-613)
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|c POF4-613
|f POF IV
|x 0
588 _ _ |a Dataset connected to INSPIRE
650 _ 7 |a energy, threshold
|2 INSPIRE
650 _ 7 |a gamma ray, VHE
|2 INSPIRE
650 _ 7 |a Cherenkov Telescope Array
|2 INSPIRE
650 _ 7 |a GeV
|2 INSPIRE
650 _ 7 |a performance
|2 INSPIRE
650 _ 7 |a flux
|2 INSPIRE
650 _ 7 |a pulsar
|2 INSPIRE
650 _ 7 |a angular resolution
|2 INSPIRE
650 _ 7 |a observatory
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650 _ 7 |a sensitivity
|2 INSPIRE
650 _ 7 |a energy resolution
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650 _ 7 |a site
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650 _ 7 |a spectral energy distribution
|2 INSPIRE
650 _ 7 |a trigger
|2 INSPIRE
650 _ 7 |a statistical
|2 INSPIRE
650 _ 7 |a TeV
|2 INSPIRE
693 _ _ |0 EXP:(DE-H253)CTA-20150101
|5 EXP:(DE-H253)CTA-20150101
|e Cherenkov Telescope Array
|x 0
700 1 _ |a Aguasca-Cabot, A.
|b 1
700 1 _ |a Agudo, I.
|b 2
700 1 _ |a Crespo, N. Alvarez
|b 3
700 1 _ |a Antonelli, L. A.
|b 4
700 1 _ |a Aramo, C.
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700 1 _ |a Arbet-Engels, A.
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700 1 _ |a Asano, K.
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700 1 _ |a Bamba, A.
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700 1 _ |a Larriva, A. Baquero
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700 1 _ |a Baroncelli, L.
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700 1 _ |a de Almeida, U. Barres
|b 14
700 1 _ |a Barrio, J. A.
|b 15
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|b 16
700 1 _ |a Baxter, J.
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700 1 _ |a González, J. Becerra
|b 18
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700 1 _ |a Bernardos, M. I.
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700 1 _ |a Biederbeck, N.
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700 1 _ |a Blanch, O.
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700 1 _ |a Bulgarelli, A.
|b 29
700 1 _ |a Burelli, I.
|b 30
700 1 _ |a Buscemi, M.
|b 31
700 1 _ |a Cardillo, M.
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700 1 _ |a Caroff, S.
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700 1 _ |a Cauz, D.
|b 36
700 1 _ |a Ceribella, G.
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700 1 _ |a Chai, Y.
|b 38
700 1 _ |a Cheng, K.
|b 39
700 1 _ |a Chiavassa, A.
|b 40
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|b 41
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|b 44
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|b 46
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|b 47
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|b 48
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|b 50
700 1 _ |a De Lotto, B.
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700 1 _ |a de Menezes, R.
|b 52
700 1 _ |a Deleglise, G.
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700 1 _ |a Delgado, C.
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|b 55
700 1 _ |a della Volpe, D.
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700 1 _ |a Dellaiera, M.
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700 1 _ |a Di Piano, A.
|b 59
700 1 _ |a Di Pierro, F.
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700 1 _ |a Martinez, I. Jimenez
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|b 122
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|b 131
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|b 134
700 1 _ |a López-Coto, R.
|b 135
700 1 _ |a López-Moya, M.
|b 136
700 1 _ |a López-Oramas, A.
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700 1 _ |a Loporchio, S.
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700 1 _ |a Lorini, A.
|b 139
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700 1 _ |a Makariev, M.
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700 1 _ |a Marsella, G.
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700 1 _ |a Martinez, O.
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|b 155
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|b 166
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|b 167
700 1 _ |a Monteiro, I.
|b 168
700 1 _ |a Moralejo, A.
|0 P:(DE-HGF)0
|b 169
|e Corresponding author
700 1 _ |a Morcuende, D.
|b 170
700 1 _ |a Morselli, A.
|b 171
700 1 _ |a Mrakovcic, K.
|b 172
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|b 175
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|b 176
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|b 177
700 1 _ |a Nishijima, K.
|b 178
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|b 179
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|b 180
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|b 181
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|b 182
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|b 183
700 1 _ |a Okazaki, N.
|b 184
700 1 _ |a Okumura, A.
|b 185
700 1 _ |a Orito, R.
|b 186
700 1 _ |a Otero-Santos, J.
|b 187
700 1 _ |a Palatiello, M.
|b 188
700 1 _ |a Paneque, D.
|b 189
700 1 _ |a Pantaleo, F. R.
|b 190
700 1 _ |a Paoletti, R.
|b 191
700 1 _ |a Paredes, J. M.
|b 192
700 1 _ |a Pavletić, L.
|b 193
700 1 _ |a Pech, M.
|b 194
700 1 _ |a Pecimotika, M.
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700 1 _ |a Pérez, A.
|b 196
700 1 _ |a Pietropaolo, E.
|b 197
700 1 _ |a Pirola, G.
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700 1 _ |a Podobnik, F.
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700 1 _ |a Poireau, V.
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700 1 _ |a Polo, M.
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700 1 _ |a Prandini, E.
|b 204
700 1 _ |a Prast, J.
|b 205
700 1 _ |a Principe, G.
|b 206
700 1 _ |a Priyadarshi, C.
|b 207
700 1 _ |a Prouza, M.
|b 208
700 1 _ |a Rando, R.
|b 209
700 1 _ |a Rhode, W.
|b 210
700 1 _ |a Ribó, M.
|b 211
700 1 _ |a Rizi, V.
|b 212
700 1 _ |a Fernandez, G. Rodriguez
|b 213
700 1 _ |a Saito, T.
|b 214
700 1 _ |a Sakurai, S.
|b 215
700 1 _ |a Sanchez, D. A.
|b 216
700 1 _ |a Šarić, T.
|b 217
700 1 _ |a Saturni, F. G.
|b 218
700 1 _ |a Schleicher, B.
|b 219
700 1 _ |a Schmuckermaier, F.
|b 220
700 1 _ |a Schubert, J. L.
|b 221
700 1 _ |a Schussler, F.
|b 222
700 1 _ |a Schweizer, T.
|b 223
700 1 _ |a Arroyo, M. Seglar
|b 224
700 1 _ |a Sitarek, J.
|b 225
700 1 _ |a Sliusar, V.
|b 226
700 1 _ |a Spolon, A.
|b 227
700 1 _ |a Strišković, J.
|b 228
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|b 229
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|b 230
700 1 _ |a Sunada, Y.
|b 231
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|b 232
700 1 _ |a Takahashi, M.
|b 233
700 1 _ |a Takahashi, H.
|b 234
700 1 _ |a Takata, J.
|b 235
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|b 236
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|b 237
700 1 _ |a Tanaka, S. J.
|b 238
700 1 _ |a Tateishi, D.
|b 239
700 1 _ |a Tejedor, L. A.
|b 240
700 1 _ |a Temnikov, P.
|b 241
700 1 _ |a Terada, Y.
|b 242
700 1 _ |a Terauchi, K.
|b 243
700 1 _ |a Terzic, T.
|b 244
700 1 _ |a Teshima, M.
|b 245
700 1 _ |a Tluczykont, M.
|b 246
700 1 _ |a Tokanai, F.
|b 247
700 1 _ |a Torres, D. F.
|b 248
700 1 _ |a Travnicek, P.
|b 249
700 1 _ |a Truzzi, S.
|b 250
700 1 _ |a Tutone, A.
|b 251
700 1 _ |a Uhlrich, G.
|b 252
700 1 _ |a Vacula, M.
|b 253
700 1 _ |a van Scherpenberg, J.
|b 254
700 1 _ |a Vázquez Acosta, M.
|b 255
700 1 _ |a Verguilov, V.
|b 256
700 1 _ |a Viale, I.
|b 257
700 1 _ |a Vigliano, A.
|b 258
700 1 _ |a Vigorito, C. F.
|b 259
700 1 _ |a Vitale, V.
|b 260
700 1 _ |a Voutsinas, G.
|b 261
700 1 _ |a Vovk, I.
|b 262
700 1 _ |a Vuillaume, T.
|b 263
700 1 _ |a Walter, R.
|b 264
700 1 _ |a Will, M.
|b 265
700 1 _ |a Yamamoto, T.
|b 266
700 1 _ |a Yamazaki, R.
|b 267
700 1 _ |a Yoshida, T.
|b 268
700 1 _ |a Yoshikoshi, T.
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700 1 _ |a Zywucka, N.
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