2024A&A...690A.167A

Query : 2024A&A...690A.167A

2024A&A...690A.167A - Astronomy and Astrophysics, volume 690A167 (2024/10-1)

A detailed study of the very high-energy Crab pulsar emission with the LST-1.

ABE K., ABE S., ABHISHEK A., ACERO F., AGUASCA-CABOT A., AGUDO I., ALVAREZ CRESPO N., ANTONELLI L.A., ARAMO C., ARBET-ENGELS A., ARCARO C., ARTERO M., ASANO K., AUBERT P., BAKTASH A., BAMBA A., BAQUERO LARRIVA A., BARONCELLI L., BARRES DE ALMEIDA U., BARRIO J.A., BATKOVIC I., BAXTER J., BECERRA GONZAILEZ J., BERNARDINI E., BERNETE MEDRANO J., BERTI A., BHATTACHARJEE P., BIGONGIARI C., BISSALDI E., BLANCH O., BONNOLI G., BORDAS P., BRUNELLI G., BULGARELLI A., BURELLI I., BURMISTROV L., BUSCEMI M., CARDILLO M., CAROFF S., CAROSI A., CARRASCO M.S., CASSOL F., CASTREJON N., CAUZ D., CERASOLE D., CERIBELLA G., CHAI Y., CHENG K., CHIAVASSA A., CHIKAWA M., CHON G., CHYTKA L., CICCIARI G.M., CIFUENTES A., CONTRERAS J.L., CORTINA J., COSTANTINI H., DA VELA P., DALCHENKO M., DAZZI F., DE ANGELIS A., DE BONY DE LAVERGNE M., DE LOTTO B., DE MENEZES R., DEL PERAL L., DELGADO C., DELGADO MENGUAL J., DELLA VOLPE D., DELLAIERA M., DI PIANO A., DI PIERRO F., DI TRIA R., DI VENERE L., DIAZ C., DOMINIK R.M., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., EISENBERGER L., ELSASSER D., EMERY G., ESCUDERO J., FALLAH RAMAZANI V., FERRAROTTO F., FIASSON A., FOFFANO L., FREIXAS COROMINA L., FROSE S., FUKAZAWA Y., GARCIA LOPEZ R., GASBARRA C., GASPARRINI D., GAVIRA L., GEYER D., GIESBRECHT PAIVA J., GIGLIETTO N., GIORDANO F., GLIWNY P., GODINOVIC N., GRAU R., GREEN D., GREEN J., GUNJI S., GUNTHER P., HACKFELD J., HADASCH D., HAHN A., HASSAN T., HAYASHI K., HECKMANN L., HELLER M., HERRERA LLORENTE J., HIROTANI K., HOFFMANN D., HORNS D., HOULES J., HRABOVSKY M., HRUPEC D., HUI D., IARLORI M., IMAZAWA R., INADA T., INOME Y., IOKA K., IORI M., JIMENEZ MARTINEZ I., JIMENEZ QUILES J., JURYSEK J., KAGAYA M., KARAS V., KATAGIRI H., KATAOKA J., KERSZBERG D., KOBAYASHI Y., KOHRI K., KONG A., KUBO H., KUSHIDA J., LAINEZ M., LAMANNA G., LAMASTRA A., LEMOIGNE L., LINHOFF M., LONGO F., LOPEZ-COTO R., LOPEZ-MOYA M., LOPEZ-ORAMAS A., LOPORCHIO S., LORINI A., LOZANO BAHILO J., LUQUE-ESCAMILLA P.L., MAJUMDAR P., MAKARIEV M., MALLAMACI M., MANDAT D., MANGANARO M., MANICO G., MANNHEIM K., MARCHESI S., MARIOTTI M., MARQUEZ P., MARSELLA G., MARTI J., MARTINEZ O., MARTINEZ G., MARTINEZ M., MAS-AGUILAR A., MAURIN G., MAZIN D., MESTRE GUILLEN E., MICANOVIC S., MICELI D., MIENER T., MIRANDA J.M., MIRZOYAN R., MIZUNO T., MOLERO GONZALEZ M., MOLINA E., MONTARULI T., MORALEJO A., MORCUENDE D., MORSELLI A., MOYA V., MURAISHI H., NAGATAKI S., NAKAMORI T., NERONOV A., NICKEL L., NIEVAS ROSILLO M., NIKOLIC L., NISHIJIMA K., NODA K., NOSEK D., NOVOTNY V., NOZAKI S., OHISHI M., OHTANI Y., OKA T., OKUMURA A., ORITO R., OTERO-SANTOS J., OTTANELLI P., OWEN E., PALATIELLO M., PANEQUE D., PANTALEO F.R., PAOLETTI R., PAREDES J.M., PECH M., PECIMOTIKA M., PERESANO M., PFEIFFLE F., PIETROPAOLO E., PIHET M., PIROLA G., PLARD C., PODOBNIK F., PONS E., PRANDINI E., PRIYADARSHI C., PROUZA M., RANDO R., RHODE W., RIBO M., RIGHI C., RIZI V., RODRIGUEZ FERNANDEZ G., RODRIGUEZ FRIAS M.D., SAITO T., SAKURAI S., SANCHEZ D.A., SANO H., SARIC T., SATO Y., SATURNI F.G., SAVCHENKO V., SCHIAVONE F., SCHLEICHER B., SCHMUCKERMAIER F., SCHUBERT J.L., SCHUSSLER F., SCHWEIZER T., SEGLAR ARROYO M., SIEGERT T., SILVIA R., SITAREK J., SLIUSAR V., STRISKOVIC J., STRZYS M., SUDA Y., TAJIMA H., TAKAHASHI H., TAKAHASHI M., TAKATA J., TAKEISHI R., TAM P.H.T., TANAKA S.J., TATEISHI D., TAVERNIER T., TEMNIKOV P., TERADA Y., TERAUCHI K., TERZIC T., TESHIMA M., TLUCZYKONT M., TOKANAI F., TORRES D.F., TRAVNICEK P., TRUZZI S., TUTONE A., VACULA M., VALLANIA P., VAN SCHERPENBERG J., VAZQUEZ ACOSTA M., VERNA G., VIALE I., VIGLIANO A., VIGORITO C.F., VISENTIN E., VITALE V., VOITSEKHOVSKYI V., VOUTSINAS G., VOVK I., VUILLAUME T., WALTER R., WAN L., WILL M., YAMAMOTO T., YAMAZAKI R., YEUNG P.K.H., YOSHIDA T., YOSHIKOSHI T., ZHANG W. and ZYWUCKA N.

Abstract (from CDS):

Context. To date, three pulsars have been firmly detected by imaging atmospheric Cherenkov telescopes (IACTs). Two of them reached the TeV energy range, challenging models of very high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the large-sized telescopes, which will be part of the Cherenkov Telescope Array Observatory (CTAO). Its improved performance over previous IACTs makes it well suited for studying pulsars.
Aims. In this work we study the Crab pulsar emission with the LST-1, improving upon and complementing the results from other telescopes. Crab pulsar observations can also be used to characterize the potential of the LST-1 to study other pulsars and detect new ones.
Methods. We analyzed a total of ∼103 hours of gamma-ray observations of the Crab pulsar conducted with the LST-1 in the period from September 2020 to January 2023. The observations were carried out at zenith angles of less than 50 degrees. To characterize the Crab pulsar emission over a broader energy range, a new analysis of the Fermi/LAT data, including ∼14 years of observations, was also performed.
Results. The Crab pulsar phaseogram, long-term light curve, and phase-resolved spectra are reconstructed with the LST-1 from 20 GeV to 450 GeV for the first peak and up to 700 GeV for the second peak The pulsed emission is detected with a significance level of 15.2σ. The two characteristic emission peaks of the Crab pulsar are clearly detected (> 10σ), as is the so-called bridge emission between them (5.7σ). We find that both peaks are described well by power laws, with spectral indices of ∼3.44 and ∼3.03, respectively. The joint analysis of Fermi/LAT and LST-1 data shows a good agreement between the two instruments in their overlapping energy range. The detailed results obtained from the first observations of the Crab pulsar with the LST-1 show the potential that CTAO will have to study this type of source.

Abstract Copyright: © The Authors 2024

Journal keyword(s): astroparticle physics - stars: neutron - pulsars: general - pulsars: individual: Crab pulsar - gamma rays: stars

Simbad objects: 5

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Number of rows : 5
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 3FGL J0534.5+2201s Psr 05 34 31.1993408 +22 01 12.001648           ~ 11 1
2 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
3 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
4 PSR J0633+1746 Psr 06 33 54.153 +17 46 12.91           ~ 1308 0
5 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545     15.10     ~ 2446 1

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