Bibcode
Aleksić, J.; Alvarez, E. A.; Antonelli, L. A.; Antoranz, P.; Asensio, M.; Backes, M.; Barrio, J. A.; Bastieri, D.; Becerra-González, J.; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Bock, R. K.; Boller, A.; Bonnoli, G.; Bordas, P.; Borla Tridon, D.; Bosch-Ramon, V.; Braun, I.; Bretz, T.; Cañellas, A.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Cossio, L.; Covino, S.; Dazzi, F.; De Angelis, A.; De Cea del Pozo, E.; De Lotto, B.; Delgado-Méndez, C.; Diago-Ortega, A.; Doert, M.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Elsaesser, D.; Ferenc, D.; Fonseca, M. V.; Font, L.; Fruck, C.; García-López, R. J.; Garczarczyk, M.; Garrido, D.; Giavitto, G.; Godinović, N.; Hadasch, D.; Häfner, D.; Herrero, A.; Hildebrand, D.; Höhne-Mönch, D.; Hose, J.; Hrupec, D.; Huber, B.; Jogler, T.; Klepser, S.; Krähenbühl, T.; Krause, J.; La Barbera, A.; Lelas, D.; Leonardo, E.; Lindfors, E.; Lombardi, S.; López, M.; Lorenz, E.; Makariev, M.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martínez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Miyamoto, H.; Moldón, J.; Moralejo, A.; Munar-Adrover, P.; Nieto, D.; Nilsson, K.; Orito, R.; Oya, I.; Paneque, D.; Paoletti, R.; Pardo, S.; Paredes, J. M.; Partini, S.; Pasanen, M.; Pauss, F.; Perez-Torres, M. A.; Persic, M. et al.
Bibliographical reference
The Astrophysical Journal Letters, Volume 735, Issue 1, article id. L5 (2011).
Advertised on:
7
2011
Citations
13
Refereed citations
8
Description
The acceleration of particles up to GeV or higher energies in
microquasars has been the subject of considerable theoretical and
observational efforts in the past few years. Sco X-1 is a microquasar
from which evidence of highly energetic particles in the jet has been
found when it is in the so-called Horizontal Branch (HB), a state when
the radio and hard X-ray fluxes are higher and a powerful relativistic
jet is present. Here we present the first very high energy gamma-ray
observations of Sco X-1, obtained with the MAGIC telescopes. An analysis
of the whole data set does not yield a significant signal, with 95% CL
flux upper limits above 300 GeV at the level of 2.4 ×
10-12 cm-2 s-1. Simultaneous RXTE
observations were conducted to provide the X-ray state of the source. A
selection of the gamma-ray data obtained during the HB based on the
X-ray colors did not yield a signal either, with an upper limit of 3.4
× 10-12 cm-2 s-1. These upper
limits place a constraint on the maximum TeV luminosity to non-thermal
X-ray luminosity of L VHE/L ntX <~ 0.02 that
can be related to a maximum TeV luminosity to jet power ratio of L
VHE/L j <~ 10-3. Our upper limits
indicate that the underlying high-energy emission physics in Sco X-1
must be inherently different from that of the hitherto detected
gamma-ray binaries.