TY - Journal
T1 - Cygnus OB2 region 610MHz sources (Marti+, 2007)
A1 - Marti, J.
A1 - Paredes, J. M.
A1 - Ishwara, C. H. Chandra
A1 - Bosch-Ramon, V.
JO - VizieR Online Data Catalog
VL - 347
Y1 - 2007/11/1
SP - 20557
KW - table3.dat 153x93 Catalogue of GMRT sources detected at 610MHz
UR - http://adsabs.harvard.edu/abs/2007yCat..34720557M
N2 - The observations were carried out at 610MHz (49cm wavelength) on 2005
July 9 and September 1 with the Giant Metrewave Radio Telescope (GMRT).
On 2005 April 29, we observed the field of TeV J2032+4130 in the near
infrared Ks-band (2.2um) using the Calar Alto 3.5m telescope and the
OMEGA2000 camera at CAHA.
(1 data file).
ER -
TY - Journal
T1 - Constraints on the Steady and Pulsed Very High Energy Gamma-Ray Emission from Observations of PSR B1951+32/CTB 80 with the MAGIC Telescope
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Hirotani, K.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C.-C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nieto, D.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 669
Y1 - 2007/11/1
SP - 1143
EP - 1149
KW - Acceleration of Particles/ Gamma Rays: Observations/ pulsars: individual (PSR B1951+32)/ Radiation Mechanisms: Nonthermal
UR - http://adsabs.harvard.edu/abs/2007ApJ...669.1143A
N2 - We report on very high energy gamma-ray observations with the MAGIC
Telescope of the pulsar PSR B1951+32 and its associated nebula, CTB 80.
Our data constrain the cutoff energy of the pulsar to be less than 32
GeV, assuming the pulsed gamma-ray emission to be exponentially cut
off. In the case that the cutoff follows a superexponential behavior,
the cutoff energy can be as high as 60 GeV. The upper limit on the flux
of pulsed gamma-ray emission above 75 GeV is
4.3×10-11 photons cm-2 s-1, and
the upper limit on the flux of steady emission above 140 GeV is
1.5×10-11 photons cm-2 s-1. We
discuss our results in the framework of recent model predictions and
other studies.
ER -
TY - Journal
T1 - Variable Very High Energy gamma-Ray Emission from Markarian 501
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R. J.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hrupec, D.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nieto, D.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Saito, T.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Tavecchio, F.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 669
Y1 - 2007/11/1
SP - 862
EP - 883
KW - BL Lacertae objects: individual (Mrk 501)/ instrumentation: detectors (MAGIC)
UR - http://adsabs.harvard.edu/abs/2007ApJ...669..862A
N2 - The blazar Mrk 501 was observed at energies above 0.10 TeV with the
MAGIC Telescope from 2005 May through July. The high sensitivity of the
instrument enabled the determination of the flux and spectrum of the
source on a night-by-night basis. Throughout our observational campaign,
the flux from Mrk 501 was found to vary by an order of magnitude.
Intranight flux variability with flux-doubling times down to 2 minutes
was observed during the two most active nights, namely, June 30 and July
9. These are the fastest flux variations ever observed in Mrk 501. The
20 minute long flare of July 9 showed an indication of a 4+/-1 minute
time delay between the peaks of F(<0.25 TeV) and F(>1.2 TeV),
which may indicate a progressive acceleration of electrons in the
emitting plasma blob. The flux variability was quantified for several
energy ranges and found to increase with the energy of the gamma-ray
photons. The spectra hardened significantly with increasing flux, and
during the two most active nights, a spectral peak was clearly detected
at 0.43+/-0.06 and 0.25+/-0.07 TeV, respectively, for June 30 and July
9. There is no evidence of such a spectral feature for the other nights
at energies down to 0.10 TeV, thus suggesting that the spectral peak is
correlated with the source luminosity. These observed characteristics
could be accommodated in a synchrotron self-Compton framework in which
the increase in gamma-ray flux is produced by a freshly injected (high
energy) electron population.
ER -
TY - Conference
T1 - Searching for the engine powering the TeV source MGRO J2019+37
A1 - Paredes, Josep Maria
JO - XMM-Newton Proposal ID #05523501
Y1 - 2007/10/1
SP - 79
KW - White Dwarf Binaries/ Neutron Star Binaries/ Cataclysmic Variables/ ULXs/ Black Holes/ MGRO J2019+37/ XMM-Newton Proposal ID #05523501
UR - http://adsabs.harvard.edu/abs/2007xmm..prop...79P
N2 - The MILAGRO Collaboration has recently reported the discovery of a new
extended and unidentified TeV source in the Cygnus region, MGRO
J2019+37. Its location is consistent with two EGRET sources, suggesting
that it could be formed by multiple unresolved sources. To find possible
counterparts, we have conducted a deep radio survey discovering two
jet-like sources which are positionally coincident with each of the
EGRET sources and with the inner box of MGRO J2019+37. One of them has
morphological and spectral characteristics similar to the microquasar 1E
1740.7-2942, the Great Annihilator at the Galactic Center. We propose to
carry out a deep XMM-Newton observation covering the two radio jet
sources to find their keV counterparts and constrain the mechanism
responsible for the TeV emission.
ER -
TY - Journal
T1 - Exploring the connection between the stellar wind and the non-thermal emission in LS 5039
A1 - Bosch-Ramon, V.
A1 - Motch, C.
A1 - Ribó, M.
A1 - Lopes de Oliveira, R.
A1 - Janot-Pacheco, E.
A1 - Negueruela, I.
A1 - Paredes, J. M.
A1 - Martocchia, A.
JO - Astronomy and Astrophysics
VL - 473
Y1 - 2007/10/1
SP - 545
EP - 550
KW - X-rays: binaries/ stars: individual: LS 5039/ radiation mechanisms: non-thermal
UR - http://adsabs.harvard.edu/abs/2007A%26A...473..545B
N2 - Context: LS 5039 has been observed with several X-ray instruments so far
showing quite steady emission in the long term and no signatures of
accretion disk. The source also presents X-ray variability at orbital
timescales in flux and photon index. The system harbors an O-type main
sequence star with moderate mass-loss. At present, the link between the
X-rays and the stellar wind is unclear. Aims: We study the X-ray
fluxes, spectra, and absorption properties of LS 5039 at apastron and
periastron passages during an epoch of enhanced stellar mass-loss, and
the long term evolution of the latter in connection with the X-ray
fluxes. Methods: New XMM-Newton observations were performed around
periastron and apastron passages in September 2005, when the stellar
wind activity was apparently higher. April 2005 Chandra observations on
LS 5039 were revisited. Moreover, a compilation of Halpha EW data
obtained since 1992, from which the stellar mass-loss evolution can be
approximately inferred, was carried out. Results: XMM-Newton
observations show higher and harder emission around apastron than around
periastron. No signatures of thermal emission or a reflection iron line
indicating the presence of an accretion disk are found in the spectrum,
and the hydrogen column density (N_H) is compatible with being the same
in both observations and consistent with the interstellar value. 2005
Chandra observations show a hard X-ray spectrum, and possibly high
fluxes, although pileup effects preclude conclusive results from being
obtained. The Halpha EW shows yearly variations of ˜ 10%, and
does not seem to be correlated with X-ray fluxes obtained at similar
phases, unlike what is expected in the wind accretion scenario.
Conclusions: 2005 XMM-Newton and Chandra observations are consistent
with 2003 RXTE/PCA results, namely moderate flux and spectral
variability at different orbital phases. The constancy of the
NH seems to imply that either the X-ray emitter is located at
⪆ 1012 cm from the compact object, or the density in the
system is 3 to 27 times smaller than that predicted by a spherical
symmetric wind model. We suggest that the multiwavelength non-thermal
emission of LS 5039 is related to the observed extended radio jets and
is unlikely to be produced inside the binary system.
The Halpha results presented here are based on observations made with
ESO Telescopes at the La Silla or Paranal Observatories under program
IDs 67.D-0229(A), 69.D-0628(A) and 075.D-0591(A); the Observatoire de
Haute-Provence; the Observatório do Pico dos Dias / LNA, Brazil;
the G. D. Cassini telescope operated at the Loiano Observatory by the
Osservatorio Astronómico di Bologna; and the Nordic Optical
Telescope, operated on the island of La Palma jointly by Denmark,
Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del
Roque de los Muchachos of the Instituto de Astrofisica de Canarias
(those data were taken using ALFOSC, which is owned by the Instituto de
Astrofísica de Andalucía (IAA) and operated at the Nordic
Optical Telescope under agreement between IAA and the NBIfAFG of the
Astronomical Observatory of Copenhagen). Table 2 is only available in
electronic form at http://www.aanda.org
ER -
TY - Preprint
T1 - Observations of microquasars with the MAGIC telescope
A1 - Rico, J.
A1 - Rissi, M.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Cortina, J.
A1 - Paredes, J. M.
A1 - Ribo, M.
A1 - Torres, D. F.
A1 - Zanin, R.
JO - ArXiv e-prints
VL - 0709
Y1 - 2007/9/1
SP - 2288
KW - Astrophysics
UR - http://adsabs.harvard.edu/abs/2007arXiv0709.2288R
N2 - We report on the results from the observations in very high energy band
(VHE, E_gamma > 100GeV) of the black hole X-ray binary (BHXB) Cygnus
X-1. The observations were performed with the MAGIC telescope, for a
total of 40 hours during 26 nights, spanning the period between June and
November 2006. We report on the results of the searches for steady and
variable gamma-ray signals, including the first experimental evidence
for an intense flare, of duration between 1.5 and 24 hours.
ER -
TY - Journal
T1 - Discovery of Very High Energy gamma-Rays from 1ES 1011+496 at z = 0.212
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R. J.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nieto, D.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Perlman, E.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Saito, T.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Tavecchio, F.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 667
Y1 - 2007/9/1
SP - L21
EP - L24
KW - Gamma Rays: Observations/ quasars: individual (1ES 1011+496)
UR - http://adsabs.harvard.edu/abs/2007ApJ...667L..21A
N2 - We report on the discovery of very high energy (VHE) gamma-ray
emission from the BL Lacertae object 1ES 1011+496. The observation was
triggered by an optical outburst in 2007 March and the source was
observed with the MAGIC telescope from 2007 March to May. Observing for
18.7 hr, we find an excess of 6.2 sigma with an integrated flux above
200 GeV of (1.58 +/- 0.32) × 10-11 photons
cm-2 s-1. The VHE gamma-ray flux is >40%
higher than in 2006 March-April (reported elsewhere), indicating that
the VHE emission state may be related to the optical emission state. We
have also determined the redshift of 1ES 1011+496 based on an optical
spectrum that reveals the absorption lines of the host galaxy. The
redshift of z=0.212 makes 1ES 1011+496 the most distant source observed
to emit VHE gamma-rays to date.
ER -
TY - Journal
T1 - MAGIC Upper Limits on the Very High Energy Emission from Gamma-Ray Bursts
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Ciprini, S.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kalekin, O.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lenisa, T.
A1 - Liebing, P.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 667
Y1 - 2007/9/1
SP - 358
EP - 366
KW - Gamma Rays: Bursts/ Gamma Rays: Observations
UR - http://adsabs.harvard.edu/abs/2007ApJ...667..358A
N2 - During its first data cycle, between 2005 and the beginning of 2006, the
fast repositioning system of the MAGIC telescope allowed the observation
of nine different gamma-ray bursts as possible sources of very high
energy gamma-rays. These observations were triggered by alerts from
Swift, HETE-2, and INTEGRAL; they started as quickly as possible after
the alerts and lasted for several minutes, with an energy threshold
varying between 80 and 200 GeV, depending on the zenith angle of the
burst. No evidence for gamma signals was found, and upper limits for the
flux were derived for all events using the standard analysis chain of
MAGIC. For the bursts with measured redshifts, the upper limits are
compatible with a power-law extrapolation, when the intrinsic fluxes are
evaluated taking into account the attenuation due to the scattering in
the metagalactic radiation field.
ER -
TY - Journal
T1 - Discovery of Very High Energy gamma-Ray Emission from the Low-Frequency-peaked BL Lacertae Object BL Lacertae
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 666
Y1 - 2007/9/1
SP - L17
EP - L20
KW - Galaxies: BL Lacertae Objects: Individual: Name: BL Lacertae/ Gamma Rays: Observations
UR - http://adsabs.harvard.edu/abs/2007ApJ...666L..17A
N2 - The MAGIC collaboration observed BL Lacertae for 22.2 hr during 2005
August to December and for 26 hr during 2006 July to September. The
source is the historical 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 a 5.1 sigma excess in the 2005
data. Above 200 GeV, an integral flux of
(0.6+/-0.2)×10-11 cm-2 s-1 was
measured, corresponding to approximately 3% of the Crab flux. The
differential spectrum between 150 and 900 GeV is rather steep with a
photon index of -3.6 +/- 0.5. The light curve shows no significant
variability during the observations in 2005. For the first time a clear
detection of VHE gamma-ray emission from an LBL object was obtained
with a signal below previous upper limits. The 2006 data show no
significant excess. This drop in flux follows the observed trend in
optical activity.
ER -
TY - Journal
T1 - Deep radio images of the HEGRA and Whipple TeV sources in the Cygnus OB2 region
A1 - Martí, J.
A1 - Paredes, J. M.
A1 - Ishwara Chandra, C. H.
A1 - Bosch-Ramon, V.
JO - Astronomy and Astrophysics
VL - 472
Y1 - 2007/9/1
SP - 557
EP - 564
KW - radio continuum: stars/ X-rays: binaries/ galaxies: active/ gamma rays: observations
UR - http://adsabs.harvard.edu/abs/2007A%26A...472..557M
N2 - Context: The modern generation of Cherenkov telescopes has revealed a
new population of gamma-ray sources in the Galaxy. Some of them have
been identified with previously known X-ray binary systems while other
remain without clear counterparts a lower energies. Our initial goal
here was reporting on extensive radio observations of the first extended
and yet unidentified source, namely TeV J2032+4130. This object was
originally detected by the HEGRA telescope in the direction of the
Cygnus OB2 region and its nature has been a matter of debate during the
latest years. The situation has become more complex with the Whipple and
MILAGRO telescopes new TeV detections in the same field which could be
consistent with the historic HEGRA source, although a different origin
cannot be ruled out. Aims: We aim to pursue our radio exploration of
the TeV J2032+4130 position that we initiated in a previous paper but
taking now into account the latest results from new Whipple and MILAGRO
TeV telescopes. The data presented here are an extended follow up of our
previous work. Methods: Our investigation is mostly based on
interferometric radio observations with the Giant Metre Wave Radio
Telescope (GMRT) close to Pune (India) and the Very Large Array (VLA) in
New Mexico (USA). We also conducted near infrared observations with the
3.5 m telescope and the OMEGA2000 camera at the Centro
Astronómico Hispano Alemán (CAHA) in Almería
(Spain). Results: We present deep radio maps centered on the TeV
J2032+4130 position at different wavelengths. In particular, our 49 and
20 cm maps cover a field of view larger than half a degree that fully
includes the Whipple position and the peak of MILAGRO emission. Our most
important result here is a catalogue of 153 radio sources detected at 49
cm within the GMRT antennae primary beam with a full width half maximum
(FWHM) of 43 arc-minute. Among them, peculiar sources inside the Whipple
error ellipse are discussed in detail, including a likely double-double
radio galaxy and a one-sided jet source of possible blazar nature. This
last object adds another alternative counterpart possibility to be
considered for both the HEGRA, Whipple and MILAGRO emission. Moreover,
our multi-configuration VLA images reveal the non-thermal extended
emission previously reported by us with improved angular resolution. Its
non-thermal spectral index is also confirmed thanks to matching beam
observations at the 20 and 6 cm wavelengths.
Table 3 is only available in electronic form at http://www.aanda.org
ER -
TY - Journal
T1 - Very High Energy Gamma-Ray Radiation from the Stellar Mass Black Hole Binary Cygnus X-1
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R. J.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nieto, D.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Saito, T.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 665
Y1 - 2007/8/1
SP - L51
EP - L54
KW - Acceleration of Particles/ Stars: Binaries: General/ Gamma Rays: Observations/ X-Rays: Individual: Constellation Name: Cygnus X-1
UR - http://adsabs.harvard.edu/abs/2007ApJ...665L..51A
N2 - We report on the results from the observations in the very high energy
band (VHE; Egamma>=100 GeV) of the black hole X-ray
binary (BHXB) Cygnus X-1. The observations were performed with the MAGIC
telescope, for a total of 40 hr during 26 nights, spanning the period
between 2006 June and November. Searches for steady gamma-ray signals
yielded no positive result, and upper limits to the integral flux
ranging between 1% and 2% of the Crab Nebula flux, depending on the
energy, have been established. We also analyzed each observation night
independently, obtaining evidence of gamma-ray signals at the 4.0
sigma significance level (3.2 sigma after trial correction) for 154
minutes of effective on-time (EOT) on September 24 between 20:58 and
23:41 UTC, coinciding with an X-ray flare seen by RXTE, Swift, and
INTEGRAL. A search for faster-varying signals within a night resulted in
an excess with a significance of 4.9 sigma (4.1 sigma after trial
correction) for 79 minutes EOT between 22:17 and 23:41 UTC. The measured
excess is compatible with a pointlike source at the position of Cygnus
X-1 and excludes the nearby radio nebula powered by its relativistic
jet. The differential energy spectrum is well fitted by an unbroken
power law described as
dN/(dAdtdE)=(2.3+/-0.6)×10-12(E/1
TeV)-3.2+/-0.6. This is the first experimental evidence of
VHE emission from a stellar mass black hole and therefore from a
confirmed accreting X-ray binary.
ER -
TY - Journal
T1 - Discovery of Very High Energy Gamma Radiation from IC 443 with the MAGIC Telescope
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R. J.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nieto, D.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Saito, T.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 664
Y1 - 2007/8/1
SP - L87
EP - L90
KW - Gamma Rays: Observations/ ISM: Individual: Alphanumeric: IC 443/ ISM: individual (MAGIC J0616+225)/ ISM: Supernova Remnants
UR - http://adsabs.harvard.edu/abs/2007ApJ...664L..87A
N2 - We report the detection of a new source of very high energy (VHE;
Egamma>=100 GeV) gamma-ray emission located close to
the Galactic plane, MAGIC J0616+225, which is spatially coincident with
supernova remnant IC 443. The observations were carried out with the
MAGIC telescope in the periods 2005 December-2006 January and 2006
December-2007 January. Here we present results from this source, leading
to a VHE gamma-ray signal with a statistical significance of 5.7
sigma in the 2006/2007 data and a measured differential gamma-ray
flux consistent with a power law, described as
dNgamma/(dAdtdE)=(1.0+/-0.2)×10-11(E/0.4
TeV)-3.1+/-0.3 cm-2 s-1
TeV-1. We briefly discuss the observational technique used
and the procedure implemented for the data analysis. The results are
placed in the context of the multiwavelength emission and the molecular
environment found in the region of IC 443.
ER -
TY - Journal
T1 - Chandra Observations of the Gamma-Ray Binary LS I +61 303: Extended X-Ray Structure?
A1 - Paredes, Josep M.
A1 - Ribó, Marc
A1 - Bosch-Ramon, Valentí
A1 - West, Jennifer R.
A1 - Butt, Yousaf M.
A1 - Torres, Diego F.
A1 - Martí, Josep
JO - Astrophysical Journal
VL - 664
Y1 - 2007/7/1
SP - L39
EP - L42
KW - Stars: Emission-Line/ Be/ stars: individual (LS I +61 303)/ X-Rays: Binaries/ X-Rays: General/ X-rays: individual (LS I +61 303)/ X-Rays: ISM
UR - http://adsabs.harvard.edu/abs/2007ApJ...664L..39P
N2 - We present a 50 ks observation of the gamma-ray binary LS I +61 303
carried out with the ACIS-I array aboard the Chandra X-Ray Observatory.
This is the highest resolution X-ray observation of the source conducted
so far. Possible evidence of an extended structure at a distance between
5" and 12" toward the north of LS I +61 303 has been found at a
significance level of 3.2 sigma. The asymmetry of the extended
emission excludes an interpretation in the context of a dust-scattered
halo, suggesting an intrinsic nature. On the other hand, while the
obtained source flux of
F0.3-10keV=7.1+1.8-1.4×10-12
ergs cm-2 s-1 and hydrogen column density
NH=(0.70+/-0.06)×1022 cm-2 are
compatible with previous results, the photon index Gamma=1.25+/-0.09
is the hardest ever found. In light of these new results, we briefly
discuss the physics behind the X-ray emission, the location of the
emitter, and the possible origin of the extended emission 0.1 pc away
from LS I +61 303.
ER -
TY - Journal
T1 - Observations of Markarian 421 with the MAGIC Telescope
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Asensio, M.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Ciprini, S.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kalekin, O.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laatiaoui, M.
A1 - Laille, A.
A1 - Liebing, P.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Orduña, R.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Prandini, E.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, A.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 663
Y1 - 2007/7/1
SP - 125
EP - 138
KW - Galaxies: BL Lacertae Objects: Individual: Name: Markarian 421/ Gamma Rays: Observations
UR - http://adsabs.harvard.edu/abs/2007ApJ...663..125A
N2 - The MAGIC telescope took data of very high energy gamma-ray emission
from the blazar Markarian 421 (Mrk 421) between 2004 November and 2005
April. We present a combined analysis of data samples recorded under
different observational conditions, down to gamma-ray energies of 100
GeV. The flux was found to vary between 0.5 and 2 crab (integrated above
200 GeV), considered a low state when compared to known data. Although
the flux varied day by day, no short-term variability was observed,
although there is some indication that not all nights show an equally
quiescent state. The results at higher energies were found to be
consistent with previous observations. A clear correlation is observed
between gamma-ray and X-ray fluxes, whereas no significant correlation
between gamma-ray and optical data is seen. The spectral energy
distribution between 100 GeV and 3 TeV shows a clear deviation from a
power law, more clearly and at lower flux than previous observations at
higher energies. The deviation persists after correcting for the effect
of attenuation by the extragalactic background light, and most likely is
source-inherent. There is a rather clear indication of an inverse
Compton peak around 100 GeV. The spectral energy distribution of Mrk 421
can be fitted by a one-zone synchrotron self-Compton model, suggesting
once again a leptonic origin of the very high energy gamma-ray
emission from this blazar.
ER -
TY - Journal
T1 - Results of two observation cycles of LS I+61°303 with the MAGIC telescope
A1 - Berger, Karsten
A1 - Sidro, Nuria
A1 - Bosch-Ramon, Valentí
A1 - Cortina, Juan
A1 - Jogler, Tobias
A1 - Paredes, Joseph M.
A1 - Perez Torres, Mighel
A1 - Ribó, Marc
A1 - Rico, Javier
A1 - Torres, Diego F.
A1 - MAGIC Collaboration
JO - Astronomische Nachrichten
VL - 328
Y1 - 2007/7/1
SP - 623
UR - http://adsabs.harvard.edu/abs/2007AN....328..623B
N2 - Not Available
ER -
TY - Journal
T1 - Observation of Very High Energy gamma-Rays from the AGN 1ES 2344+514 in a Low Emission State with the MAGIC Telescope
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J. K.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Ciprini, S.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Costado, M. T.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - Delgado, C.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - De Angelis
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - García-López, R.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Herrero, A.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kalekin, O.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Liebing, P.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Onña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Panniello, M.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Prandini, E.
A1 - Puchades, N.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zandanel, F.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 662
Y1 - 2007/6/1
SP - 892
EP - 899
KW - Galaxies: BL Lacertae Objects: Individual: Alphanumeric: 1ES 2344+514/ Gamma Rays: Observations
UR - http://adsabs.harvard.edu/abs/2007ApJ...662..892A
N2 - The MAGIC collaboration has observed very high energy gamma-ray emission
from the AGN 1ES 2344+514. A gamma-ray signal corresponding to an 11
sigma excess and an integral flux of
(2.38+/-0.30stat+/-0.70syst)×10-11
cm-2 s-1 above 200 GeV has been obtained from 23.1
hr of data taking between 2005 August 3 and 2006 January 1. The data
confirm the previously detected gamma-ray emission from this object
during a flare seen by the Whipple collaboration in 1995 and the
evidence (below 5 sigma significance level) from long-term
observations conducted by the Whipple and HEGRA groups. The MAGIC
observations show a relatively steep differential photon spectrum that
can be described by a power law with a photon index of
alpha=-2.95+/-0.12stat+/-0.2syst between 140 GeV
and 5.4 TeV. The observations reveal a low-flux state, about 6 times
below the 1995 flare seen by Whipple and comparable with the previous
Whipple and HEGRA long-term measurements. During the MAGIC observations
no significant time variability was observed.
ER -
TY - Journal
T1 - The search for hot spots associated with the Cygnus X-3 relativistic jet
A1 - Martí, J.
A1 - Pérez-Ramírez, D.
A1 - Luque-Escamilla, P.
A1 - Garrido, J. L.
A1 - Paredes, J. M.
A1 - Muñoz-Arjonilla, A.
A1 - Sánchez-Sutil, J. R.
JO - Astrophysics and Space Science
VL - 309
Y1 - 2007/6/1
SP - 309
EP - 313
KW - Stars: individual: Cygnus X-3/ Radio continuum: steps/ X-rays: binaries
UR - http://adsabs.harvard.edu/abs/2007Ap%26SS.309..309M
N2 - We report and shortly discuss here the observational work carried out in
order to test the possibility that two previously detected radio
sources, in the vicinity of the well known microquasar Cygnus X-3, could
be hot spot tracers of interaction between its relativistic jet and the
interstellar medium (ISM). The motivation behind this search is in part
justified considering recent theoretical models of high energy
gamma-ray emission which strongly rely on the interaction sites of
galactic relativistic jets with nearby ISM clouds. The results presented
in this paper include an improved radio exploration of the several
arc-minute field around Cygnus X-3 using the Very Large Array (VLA), as
well as deep near infrared (NIR) imaging with the Calar Alto 3.5 m
telescope. We anticipate here that our observations do not appear to
support the initial hot spot hypothesis. Instead, the resulting images
suggest that the two radio sources, originally believed to be hot spot
candidates, are most likely background or foreground objects.
ER -
TY - Journal
T1 - INTEGRAL serendipitous detection of the gamma-ray microquasar LS 5039
A1 - Goldoni, P.
A1 - Ribó, M.
A1 - di Salvo, T.
A1 - Paredes, J. M.
A1 - Bosch-Ramon, V.
A1 - Rupen, M.
JO - Astrophysics and Space Science
VL - 309
Y1 - 2007/6/1
SP - 293
EP - 297
KW - X-ray binaries/ Microquasars/ X-rays/ Gamma-rays
UR - http://adsabs.harvard.edu/abs/2007Ap%26SS.309..293G
N2 - LS 5039 is the only X-ray binary persistently detected at TeV energies
by the Cherenkov HESS telescope. It is moreover a gamma-ray emitter in
the GeV and possibly MeV energy ranges. To understand important aspects
of jet physics, like the magnetic field content or particle
acceleration, and emission processes, such as synchrotron and inverse
Compton (IC), a complete modeling of the multiwavelength data is
necessary. LS 5039 has been detected along almost all the
electromagnetic spectrum thanks to several radio, infrared, optical and
soft X-ray detections. However, hard X-ray detections above 20 keV have
been so far elusive and/or doubtful, partly due to source confusion for
the poor spatial resolution of hard X-ray instruments. We report here on
deep (˜300 ks) serendipitous INTEGRAL hard X-ray observations of
LS 5039, coupled with simultaneous VLA radio observations. We obtain a
20 40 keV flux of 1.1±0.3 mCrab (5.9 (±1.6)
×10-12 erg cm-2
s-1), a 40 100 keV upper limit of 1.5 mCrab
(9.5×10-12 erg cm-2
s-1), and typical radio flux densities of ˜25 mJy
at 5 GHz. These hard X-ray fluxes are significantly lower than previous
estimates obtained with BATSE in the same energy range but, in the lower
interval, agree with extrapolation of previous RXTE measurements. The
INTEGRAL observations also hint to a break in the spectral behavior at
hard X-rays. A more sensitive characterization of the hard X-ray
spectrum of LS 5039 from 20 to 100 keV could therefore constrain key
aspects of the jet physics, like the relativistic particle spectrum and
the magnetic field strength. Future multiwavelength observations would
allow to establish whether such hard X-ray synchrotron emission is
produced by the same population of relativistic electrons as those
presumably producing TeV emission through IC.
ER -
TY - Journal
T1 - INTEGRAL/XMM views on the MeV source GRO J1411-64
A1 - Torres, Diego F.
A1 - Zhang, Shu
A1 - Reimer, Olaf
A1 - Barcons, Xavier
A1 - Corral, Amalia
A1 - Bosch-Ramon, Valentí
A1 - Paredes, Josep M.
A1 - Romero, Gustavo E.
A1 - Qu, Jin
A1 - Collmar, Werner
A1 - Schönfelder, Volker
A1 - Butt, Yousaf
JO - Astrophysics and Space Science
VL - 309
Y1 - 2007/6/1
SP - 17
EP - 21
UR - http://adsabs.harvard.edu/abs/2007Ap%26SS.309...17T
N2 - The COMPTEL unidentified source GRO J 1411-64 was observed by INTEGRAL
and XMM-Newton in 2005. The Circinus Galaxy is the only source detected
within the 4sigma location error of GRO J1411-64, but in here excluded
as the possible counterpart. At soft X-rays, 22 reliable and
statistically significant sources (likelihood >10) were extracted and
analyzed from XMM-Newton data. Only one of these sources, XMMU
J141255.6-635932, is spectrally compatible with GRO J1411-64 although
the fact the soft X-ray observations do not cover the full extent of the
COMPTEL source position uncertainty make an association hard to quantify
and thus risky. At the best location of the source, detections at hard
X-rays show only upper limits, which, together with MeV results obtained
by COMPTEL suggest the existence of a peak in power output located
somewhere between 300 700 keV for the so-called low state. Such a
spectrum resembles those in blazars or microquasars, and might suggest
at work by the models accordingly. However, an analysis using a
microquasar model consisting on a magnetized conical jet filled with
relativistic electrons, shows that it is hard to comply with all
observational constrains. This fact and the non-detection at hard X-rays
introduce an a-posteriori question mark upon the physical reality of
this source, what is discussed here.
ER -
TY - Journal
T1 - Preface
A1 - Paredes, Josep M.
A1 - Reimer, Olaf
A1 - Torres, Diego F.
JO - Astrophysics and Space Science
VL - 309
Y1 - 2007/6/1
SP - 1
EP - 4
UR - http://adsabs.harvard.edu/abs/2007Ap%26SS.309....1P
N2 - Not Available
ER -
TY - Journal
T1 - First Bounds on the Very High Energy gamma-Ray Emission from Arp 220
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Ciprini, S.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kalekin, O.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Liebing, P.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Puchades, N.
A1 - Prandini, E.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Shore, S. N.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 658
Y1 - 2007/3/1
SP - 245
EP - 248
KW - Gamma Rays: Observations
UR - http://adsabs.harvard.edu/abs/2007ApJ...658..245A
N2 - 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.
ER -
TY - Journal
T1 - The Population of Radio Sources in the Field of the Unidentified Gamma-Ray Source TeV J2032+4130
A1 - Paredes, Josep M.
A1 - Martí, Josep
A1 - Ishwara Chandra, C. H.
A1 - Bosch-Ramon, Valentí
JO - Astrophysical Journal
VL - 654
Y1 - 2007/1/1
SP - L135
EP - L138
KW - Gamma Rays: Observations/ Radio Continuum: ISM/ Radio Continuum: Stars/ X-Rays: Stars
UR - http://adsabs.harvard.edu/abs/2007ApJ...654L.135P
N2 - TeV J2032+4130 is the first extended very high energy gamma-ray source
and has remained enigmatic since its discovery because of the lack of
identification. We report here deep radio observations covering the TeV
J2032+4130 field and revealing for the first time an extended and
diffuse radio emission, as well as a remarkable population of compact
radio sources. Some of these radio sources are in positional coincidence
with X-ray and optical/IR sources. Future follow-up studies of these new
radio sources will likely contribute to solving the mystery of this
extended unidentified TeV source.
ER -
TY - Journal
T1 - Detection of Very High Energy Radiation from the BL Lacertae Object PG 1553+113 with the MAGIC Telescope
A1 - Albert, J.
A1 - Aliu, E.
A1 - Anderhub, H.
A1 - Antoranz, P.
A1 - Armada, A.
A1 - Baixeras, C.
A1 - Barrio, J. A.
A1 - Bartko, H.
A1 - Bastieri, D.
A1 - Becker, J.
A1 - Bednarek, W.
A1 - Berger, K.
A1 - Bigongiari, C.
A1 - Biland, A.
A1 - Bock, R. K.
A1 - Bordas, P.
A1 - Bosch-Ramon, V.
A1 - Bretz, T.
A1 - Britvitch, I.
A1 - Camara, M.
A1 - Carmona, E.
A1 - Chilingarian, A.
A1 - Ciprini, S.
A1 - Coarasa, J. A.
A1 - Commichau, S.
A1 - Contreras, J. L.
A1 - Cortina, J.
A1 - Curtef, V.
A1 - Danielyan, V.
A1 - Dazzi, F.
A1 - De Angelis, A.
A1 - de los Reyes, R.
A1 - De Lotto, B.
A1 - Domingo-Santamaría, E.
A1 - Dorner, D.
A1 - Doro, M.
A1 - Errando, M.
A1 - Fagiolini, M.
A1 - Ferenc, D.
A1 - Fernández, E.
A1 - Firpo, R.
A1 - Flix, J.
A1 - Fonseca, M. V.
A1 - Font, L.
A1 - Fuchs, M.
A1 - Galante, N.
A1 - Garczarczyk, M.
A1 - Gaug, M.
A1 - Giller, M.
A1 - Goebel, F.
A1 - Hakobyan, D.
A1 - Hayashida, M.
A1 - Hengstebeck, T.
A1 - Höhne, D.
A1 - Hose, J.
A1 - Hsu, C. C.
A1 - Jacon, P.
A1 - Jogler, T.
A1 - Kalekin, O.
A1 - Kosyra, R.
A1 - Kranich, D.
A1 - Kritzer, R.
A1 - Laille, A.
A1 - Liebing, P.
A1 - Lindfors, E.
A1 - Lombardi, S.
A1 - Longo, F.
A1 - López, J.
A1 - López, M.
A1 - Lorenz, E.
A1 - Majumdar, P.
A1 - Maneva, G.
A1 - Mannheim, K.
A1 - Mansutti, O.
A1 - Mariotti, M.
A1 - Martínez, M.
A1 - Mazin, D.
A1 - Merck, C.
A1 - Meucci, M.
A1 - Meyer, M.
A1 - Miranda, J. M.
A1 - Mirzoyan, R.
A1 - Mizobuchi, S.
A1 - Moralejo, A.
A1 - Nilsson, K.
A1 - Ninkovic, J.
A1 - Oña-Wilhelmi, E.
A1 - Otte, N.
A1 - Oya, I.
A1 - Paneque, D.
A1 - Paoletti, R.
A1 - Paredes, J. M.
A1 - Pasanen, M.
A1 - Pascoli, D.
A1 - Pauss, F.
A1 - Pegna, R.
A1 - Persic, M.
A1 - Peruzzo, L.
A1 - Piccioli, A.
A1 - Poller, M.
A1 - Puchades, N.
A1 - Prandini, E.
A1 - Raymers, A.
A1 - Rhode, W.
A1 - Ribó, M.
A1 - Rico, J.
A1 - Rissi, M.
A1 - Robert, A.
A1 - Rügamer, S.
A1 - Saggion, A.
A1 - Sánchez, A.
A1 - Sartori, P.
A1 - Scalzotto, V.
A1 - Scapin, V.
A1 - Schmitt, R.
A1 - Schweizer, T.
A1 - Shayduk, M.
A1 - Shinozaki, K.
A1 - Sidro, N.
A1 - Sillanpää, A.
A1 - Sobczynska, D.
A1 - Stamerra, A.
A1 - Stark, L. S.
A1 - Takalo, L.
A1 - Temnikov, P.
A1 - Tescaro, D.
A1 - Teshima, M.
A1 - Tonello, N.
A1 - Torres, D. F.
A1 - Turini, N.
A1 - Vankov, H.
A1 - Vitale, V.
A1 - Wagner, R. M.
A1 - Wibig, T.
A1 - Wittek, W.
A1 - Zanin, R.
A1 - Zapatero, J.
JO - Astrophysical Journal
VL - 654
Y1 - 2007/1/1
SP - L119
EP - L122
KW - BL Lacertae objects: individual (PG 1553+113)/ Gamma Rays: Observations
UR - http://adsabs.harvard.edu/abs/2007ApJ...654L.119A
N2 - In 2005 and 2006, the MAGIC telescope observed very high energy
gamma-ray emission from the distant BL Lac object PG 1553+113. The
overall significance of the signal was 8.8 sigma for 18.8 hr of
observation time. The light curve shows no significant flux variations
on a daily timescale; the flux level during 2005 was, however,
significantly higher compared to 2006. The differential energy spectrum
between 90 and 500 GeV is well described by a power law with photon
index Gamma=4.2+/-0.3. The combined 2005 and 2006 energy spectrum
provides an upper limit of z=0.74 on the redshift of the object.
ER -