Discovery of Very High Energy γ-Ray Emission from the Low-Frequency-peaked BL Lacertae Object BL Lacertae | Zendy

J. Albert | Zendy; E. Aliu | Zendy; H. Anderhub | Zendy; P. Antoranz | Zendy; A. Armada | Zendy; C. Baixeras | Zendy; J. A. Barrio | Zendy; H. Bartko | Zendy; D. Bastieri | Zendy; J. K. Becker | Zendy; W. Bednarek | Zendy; K. Berger | Zendy; C. Bigongiari | Zendy; A. Biland | Zendy; R. K. Böck | Zendy; P. Bordas | Zendy; V. BoschRamon | Zendy; T. Bretz | Zendy; I. Britvitch | Zendy; Montaña Cámara | Zendy; E. Carmona | Zendy; A. Chilingarian | Zendy; J. A. Coarasa | Zendy; S. Commichau | Zendy; J. L. Contreras | Zendy; J. Cortina | Zendy; M. T. Costado | Zendy; V. Curtef | Zendy; V. Danielyan | Zendy; F. Dazzi | Zendy; A. De Angelis | Zendy; C. Delgado Mendez | Zendy; R. de los Reyes | Zendy; B. De Lotto | Zendy; E. Domingo-Santamaría | Zendy; D. Dorner | Zendy; M. Doro | Zendy; M. Errando | Zendy; M. Fagiolini | Zendy; D. Ferenc | Zendy; E. Fernández | Zendy; R. Firpo | Zendy; J. Flix | Zendy; M. V. Fonseca | Zendy; L. Font | Zendy; M. Fuchs | Zendy; N. Galante | Zendy; R. J. Garcı́a López | Zendy; M. Garczarczyk | Zendy; M. Gaug | Zendy; M. Giller | Zendy; F. Göebel | Zendy; D. Hakobyan | Zendy; M. Hayashida | Zendy; T. Hengstebeck | Zendy; A. Herrero | Zendy; D. Höhne | Zendy; J. Hose | Zendy; C. C. Hsu | Zendy; P. Jacoń | Zendy; T. Jogler | Zendy; R. Kosyra | Zendy; D. Kranich | Zendy; R. Kritzer | Zendy; A. Laille | Zendy; E. Lindfors | Zendy; S. Lombardi | Zendy; F. Longo | Zendy; J. López | Zendy; Marcos López | Zendy; E. Lorenz | Zendy; P. Majumdar | Zendy; G. Maneva | Zendy; K. Mannheim | Zendy; O. Mansutti | Zendy; M. Mariotti | Zendy; M. Martı́nez | Zendy; D. Mazin | Zendy; C. Merck | Zendy; M. Meucci | Zendy; M. Meyer | Zendy; J. M. Miranda | Zendy; R. Mirzoyan | Zendy; S. Mizobuchi | Zendy; A. Moralejo | Zendy; K. Nilsson | Zendy; J. Ninković | Zendy; E. de Oña Wilhelmi | Zendy; A. N. Otte | Zendy; D. Paneque | Zendy; M. Panniello | Zendy; R. Paoletti | Zendy; J. M. Paredes | Zendy; M. Pasanen | Zendy; D. Pascoli | Zendy; F. Pauss | Zendy; R. Pegna | Zendy; M. Persic | Zendy; L. Peruzzo | Zendy; A. Piccioli | Zendy; M. Pöller | Zendy; E. Prandini | Zendy; N. Puchades | Zendy; A. Raymers | Zendy; W. Rhode | Zendy; M. Ribó | Zendy; J. Rico | Zendy; M. Rissi | Zendy; A. Robert | Zendy; S. Rügamer | Zendy; A. Saggion | Zendy; A. Sánchez | Zendy; P. Sartori | Zendy; V. Scalzotto | Zendy; V. Scapin | Zendy; R. Schmitt | Zendy; T. Schweizer | Zendy; M. Shayduk | Zendy; K. Shinozaki | Zendy; S. N. Shore | Zendy; N. Sidro | Zendy; A. Sillanpää | Zendy; D. Sobczyńska | Zendy; A. Stamerra | Zendy; L. S. Stark | Zendy; L. O. Takalo | Zendy; P. Temnikov | Zendy; D. Tescaro | Zendy; M. Teshima | Zendy; N. Tonello | Zendy; D. F. Torres | Zendy; N. Turini | Zendy; H. Vankov | Zendy; V. Vitale | Zendy; Robert Wagner | Zendy; Tadeusz Wibig | Zendy; W. Wittek | Zendy; F. Zandanel | Zendy; R. Zanin | Zendy; J. Zapatero | Zendy

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Discovery of Very High Energy γ-Ray Emission from the Low-Frequency-peaked BL Lacertae Object BL Lacertae

Author(s) -

J. Albert,

E. Aliu,

H. Anderhub,

P. Antoranz,

A. Armada,

C. Baixeras,

J. A. Barrio,

H. Bartko,

D. Bastieri,

J. K. Becker,

W. Bednarek,

K. Berger,

C. Bigongiari,

A. Biland,

R. K. Böck,

P. Bordas,

V. BoschRamon,

T. Bretz,

I. Britvitch,

Montaña Cámara,

E. Carmona,

A. Chilingarian,

J. A. Coarasa,

S. Commichau,

J. L. Contreras,

J. Cortina,

M. T. Costado,

V. Curtef,

V. Danielyan,

F. Dazzi,

A. De Angelis,

C. Delgado Mendez,

R. de los Reyes,

B. De Lotto,

E. Domingo-Santamaría,

D. Dorner,

M. Doro,

M. Errando,

M. Fagiolini,

D. Ferenc,

E. Fernández,

R. Firpo,

J. Flix,

M. V. Fonseca,

L. Font,

M. Fuchs,

N. Galante,

R. J. Garcı́a López,

M. Garczarczyk,

M. Gaug,

M. Giller,

F. Göebel,

D. Hakobyan,

M. Hayashida,

T. Hengstebeck,

A. Herrero,

D. Höhne,

J. Hose,

C. C. Hsu,

P. Jacoń,

T. Jogler,

R. Kosyra,

D. Kranich,

R. Kritzer,

A. Laille,

E. Lindfors,

S. Lombardi,

F. Longo,

J. López,

Marcos López,

E. Lorenz,

P. Majumdar,

G. Maneva,

K. Mannheim,

O. Mansutti,

M. Mariotti,

M. Martı́nez,

D. Mazin,

C. Merck,

M. Meucci,

M. Meyer,

J. M. Miranda,

R. Mirzoyan,

S. Mizobuchi,

A. Moralejo,

K. Nilsson,

J. Ninković,

E. de Oña Wilhelmi,

A. N. Otte,

D. Paneque,

M. Panniello,

R. Paoletti,

J. M. Paredes,

M. Pasanen,

D. Pascoli,

F. Pauss,

R. Pegna,

M. Persic,

L. Peruzzo,

A. Piccioli,

M. Pöller,

E. Prandini,

N. Puchades,

A. Raymers,

W. Rhode,

M. Ribó,

J. Rico,

M. Rissi,

A. Robert,

S. Rügamer,

A. Saggion,

A. Sánchez,

P. Sartori,

V. Scalzotto,

V. Scapin,

R. Schmitt,

T. Schweizer,

M. Shayduk,

K. Shinozaki,

S. N. Shore,

N. Sidro,

A. Sillanpää,

D. Sobczyńska,

A. Stamerra,

L. S. Stark,

L. O. Takalo,

P. Temnikov,

D. Tescaro,

M. Teshima,

N. Tonello,

D. F. Torres,

N. Turini,

H. Vankov,

V. Vitale,

Robert Wagner,

Tadeusz Wibig,

W. Wittek,

F. Zandanel,

R. Zanin,

J. Zapatero

Publication year - 2007

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.376

H-Index - 489

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/521550

Subject(s) - bl lac object , physics , astrophysics , flux (metallurgy) , light curve , magic (telescope) , astronomy , blazar , gamma ray , materials science , metallurgy

The MAGIC collaboration observed BL Lacertae for 22.2 hr during 2005 Augustto December and for 26 hr during 2006 July to September. The source is thehistorical prototype and eponym of a class of low-frequency peaked BL Lacertae(LBL) objects. A very high energy (VHE) gamma-ray signal was discovered with a5.1 sigma excess in the 2005 data. Above 200 GeV, an integral flux of 0.6+-0.2x 10^(-11) cm^(-2) s^(-1) was measured, corresponding to approximately 3% ofthe Crab flux. The differential spectrum between 150 and 900 GeV is rathersteep with a photon index of -3.6+-0.5. The light curve shows no significantvariability during the observations in 2005. For the first time a cleardetection of VHE gamma-ray emission from an LBL object was obtained with asignal below previous upper limits. The 2006 data show no significant excess.This drop in flux follows the observed trend in optical activity.Comment: Accepted for publication in ApJ Letters, 4 pages, 5 figures, Figure-5 revised, Minor corrections following the referee repor

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