First Bounds on the Very High Energy γ‐Ray Emission from Arp 220 | 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. A. 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; S. Ciprini | Zendy; J. A. Coarasa | Zendy; S. Commichau | Zendy; J. L. Contreras | Zendy; J. Cortina | Zendy; V. Curtef | Zendy; V. Danielyan | Zendy; F. Dazzi | Zendy; A. De Angelis | 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; M. Garczarczyk | Zendy; M. Gaug | Zendy; M. Giller | Zendy; F. Göebel | Zendy; D. Hakobyan | Zendy; M. Hayashida | Zendy; T. Hengstebeck | Zendy; D. Höhne | Zendy; J. Hose | Zendy; C. C. Hsu | Zendy; P. Jacoń | Zendy; T. Jogler | Zendy; O. Kalekin | Zendy; R. Kosyra | Zendy; D. Kranich | Zendy; R. Kritzer | Zendy; A. Laille | Zendy; P. Liebing | 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; 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; N. Puchades | Zendy; E. Prandini | 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. Sillanpaa | 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; R. Zanin | Zendy; J. Zapatero | Zendy

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First Bounds on the Very High Energy γ‐Ray Emission from Arp 220

Author(s) -

J. Albert,

E. Aliu,

H. Anderhub,

P. Antoranz,

A. Armada,

C. Baixeras,

J. A. Barrio,

H. Bartko,

D. Bastieri,

J. A. 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,

S. Ciprini,

J. A. Coarasa,

S. Commichau,

J. L. Contreras,

J. Cortina,

V. Curtef,

V. Danielyan,

F. Dazzi,

A. De Angelis,

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,

M. Garczarczyk,

M. Gaug,

M. Giller,

F. Göebel,

D. Hakobyan,

M. Hayashida,

T. Hengstebeck,

D. Höhne,

J. Hose,

C. C. Hsu,

P. Jacoń,

T. Jogler,

O. Kalekin,

R. Kosyra,

D. Kranich,

R. Kritzer,

A. Laille,

P. Liebing,

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,

R. Paoletti,

J. M. Paredes,

M. Pasanen,

D. Pascoli,

F. Pauss,

R. Pegna,

M. Persic,

L. Peruzzo,

A. Piccioli,

M. Pöller,

N. Puchades,

E. Prandini,

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. Sillanpaa,

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,

R. Zanin,

J. Zapatero

Publication year - 2007

Publication title -

the astrophysical journal

Language(s) - English

Resource type - Journals

eISSN - 1538-4357

pISSN - 0004-637X

DOI - 10.1086/511173

Subject(s) - magic (telescope) , physics , galaxy , telescope , astrophysics , flux (metallurgy) , infrared , energy (signal processing) , astronomy , chemistry , quantum mechanics , organic chemistry

Using the Major Atmospheric Gamma Imaging Cerenkov Telescope ( MAGIC), we have observed the nearest ultraluminous infrared galaxy, Arp 220, for about 15 hr. No significant signal was detected within the dedicated amount of observation time. The first upper limits to the very high energy gamma-ray flux of Arp 220 are herein reported and compared with theoretical expectations

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