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73 results on '"Hudec, R."'

10. Search for gamma-ray burst classes with the RHESSI satellite

Author

Řípa, J., Mészáros, A., Wigger, C., Huja, D., Hudec, R., Hajdas, W., Řípa, J., Mészáros, A., Wigger, C., Huja, D., Hudec, R., and Hajdas, W.

Abstract

Aims. We study a sample of 427 gamma-ray bursts (GRBs), measured by the RHESSI satellite, statistically with respect to duration and hardness ratio.

Published
2009
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11. The bright optical flash from GRB 060117

Author

Jelínek, M., Prouza, M., Kubánek, P., Hudec, R., Nekola, M., Řídký, J., Grygar, J., Boháčová, M., Castro-Tirado, A. J., Gorosabel, J., Hrabovský, M., Mandát, D., Nosek, D., Nožka, L., Palatka, M., Pandey, S. B., Pech, M., Schovánek, P., Šmída, R., Trávníček, P., de Ugarte Postigo, A., Vítek, S., Jelínek, M., Prouza, M., Kubánek, P., Hudec, R., Nekola, M., Řídký, J., Grygar, J., Boháčová, M., Castro-Tirado, A. J., Gorosabel, J., Hrabovský, M., Mandát, D., Nosek, D., Nožka, L., Palatka, M., Pandey, S. B., Pech, M., Schovánek, P., Šmída, R., Trávníček, P., de Ugarte Postigo, A., and Vítek, S.

Abstract

We present a discovery and observation of an extraordinarily bright prompt optical emission of the GRB 060117 obtained by a wide-field camera atop the robotic telescope FRAM of the Pierre Auger Observatory from 2 to 10 min after the GRB. We found rapid average temporal flux decay of $\alpha = -1.7 \pm 0.1$and a peak brightness $R = 10.1$mag. Later observations by other instruments set a strong limit on the optical and radio transient fluxes, unveiling an unexpectedly rapid further decay. We present an interpretation featuring a relatively steep electron-distribution parameter $p \simeq 3.0$and providing a straightforward solution for the overall fast decay of this optical transient as a transition between reverse and forward shock.

Published
2006
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12. The unprecedented optical outburst of the quasar 3C 454.3

Author

Villata, M., Raiteri, C. M., Balonek, T. J., Aller, M. F., Jorstad, S. G., Kurtanidze, O. M., Nicastro, F., Nilsson, K., Aller, H. D., Arai, A., Arkharov, A., Bach, U., Benítez, E., Berdyugin, A., Buemi, C. S., Böttcher, M., Carosati, D., Casas, R., Caulet, A., Chen, W. P., Chiang, P.-S., Chou, Y., Ciprini, S., Coloma, J. M., Di Rico, G., Díaz, C., Efimova, N. V., Forsyth, C., Frasca, A., Fuhrmann, L., Gadway, B., Gupta, S., Hagen-Thorn, V. A., Harvey, J., Heidt, J., Hernandez-Toledo, H., Hroch, F., Hu, C.-P., Hudec, R., Ibrahimov, M. A., Imada, A., Kamata, M., Kato, T., Katsuura, M., Konstantinova, T., Kopatskaya, E., Kotaka, D., Kovalev, Y. Y., Kovalev, Yu. A., Krichbaum, T. P., Kubota, K., Kurosaki, M., Lanteri, L., Larionov, V. M., Larionova, L., Laurikainen, E., Lee, C.-U., Leto, P., Lähteenmäki, A., López-Cruz, O., Marilli, E., Marscher, A. P., McHardy, I. M., Mondal, S., Mullan, B., Napoleone, N., Nikolashvili, M. G., Ohlert, J. M., Postnikov, S., Pursimo, T., Ragni, M., Ros, J. A., Sadakane, K., Sadun, A. C., Savolainen, T., Sergeeva, E. A., Sigua, L. A., Sillanpää, A., Sixtova, L., Sumitomo, N., Takalo, L. O., Teräsranta, H., Tornikoski, M., Trigilio, C., Umana, G., Volvach, A., Voss, B., Wortel, S., Villata, M., Raiteri, C. M., Balonek, T. J., Aller, M. F., Jorstad, S. G., Kurtanidze, O. M., Nicastro, F., Nilsson, K., Aller, H. D., Arai, A., Arkharov, A., Bach, U., Benítez, E., Berdyugin, A., Buemi, C. S., Böttcher, M., Carosati, D., Casas, R., Caulet, A., Chen, W. P., Chiang, P.-S., Chou, Y., Ciprini, S., Coloma, J. M., Di Rico, G., Díaz, C., Efimova, N. V., Forsyth, C., Frasca, A., Fuhrmann, L., Gadway, B., Gupta, S., Hagen-Thorn, V. A., Harvey, J., Heidt, J., Hernandez-Toledo, H., Hroch, F., Hu, C.-P., Hudec, R., Ibrahimov, M. A., Imada, A., Kamata, M., Kato, T., Katsuura, M., Konstantinova, T., Kopatskaya, E., Kotaka, D., Kovalev, Y. Y., Kovalev, Yu. A., Krichbaum, T. P., Kubota, K., Kurosaki, M., Lanteri, L., Larionov, V. M., Larionova, L., Laurikainen, E., Lee, C.-U., Leto, P., Lähteenmäki, A., López-Cruz, O., Marilli, E., Marscher, A. P., McHardy, I. M., Mondal, S., Mullan, B., Napoleone, N., Nikolashvili, M. G., Ohlert, J. M., Postnikov, S., Pursimo, T., Ragni, M., Ros, J. A., Sadakane, K., Sadun, A. C., Savolainen, T., Sergeeva, E. A., Sigua, L. A., Sillanpää, A., Sixtova, L., Sumitomo, N., Takalo, L. O., Teräsranta, H., Tornikoski, M., Trigilio, C., Umana, G., Volvach, A., Voss, B., and Wortel, S.

Abstract

Context.The radio quasar 3C 454.3underwent an exceptional optical outburst lasting more than 1 year and culminating in spring 2005. The maximum brightness detected was $R=12.0$, which represents the most luminous quasar state thus far observed ($M_B \sim -31.4$).

Published
2006
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13. Search for correlations between BATSE gamma-ray bursts and supernovae

Author

Polcar, J., Topinka, M., Nečas, D., Hudec, R., Hudcová, V., Hroch, F., Masetti, N., Pizzichini, G., Palazzi, E., Polcar, J., Topinka, M., Nečas, D., Hudec, R., Hudcová, V., Hroch, F., Masetti, N., Pizzichini, G., and Palazzi, E.

Abstract

We report on our statistical research of space-time correlated supernovae and CGRO-BATSE gamma-ray bursts. There exists a significantly higher abundance of core-collapse supernovae among the correlated supernovae, but the subset of all correlated objects does not seem to be physically different from the whole set. The upper limit of the fraction of possibly correlated GRBs and SNe is of order of a few percent.

Published
2006
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14. INTEGRALobservations of the blazar 3C 454.3 in outburst

Author

Pian, E., Foschini, L., Beckmann, V., Soldi, S., Türler, M., Gehrels, N., Ghisellini, G., Giommi, P., Maraschi, L., Pursimo, T., Raiteri, C. M., Tagliaferri, G., Tornikoski, M., Tosti, G., Treves, A., Villata, M., Barr, P., Courvoisier, T. J.-L., Di Cocco, G., Hudec, R., Fuhrmann, L., Malaguti, G., Persic, M., Tavecchio, F., Walter, R., Pian, E., Foschini, L., Beckmann, V., Soldi, S., Türler, M., Gehrels, N., Ghisellini, G., Giommi, P., Maraschi, L., Pursimo, T., Raiteri, C. M., Tagliaferri, G., Tornikoski, M., Tosti, G., Treves, A., Villata, M., Barr, P., Courvoisier, T. J.-L., Di Cocco, G., Hudec, R., Fuhrmann, L., Malaguti, G., Persic, M., Tavecchio, F., and Walter, R.

Abstract

In Spring 2005, the blazar 3C 454.3 underwent a dramatic outburst at all wavelengths from mm to X-rays. This prompted INTEGRALobservations, accomplished in 15-18 May 2005. The source was detected by the INTEGRALinstruments from 3 to 200 keV in a bright state (${\sim} 5 \times 10^{-10}$erg s-1cm-2), at least a factor of 2-3 higher than previously observed. This is one of the brightest blazar detections achieved by INTEGRAL. During the 2.5 days of INTEGRALmonitoring, we detected a ~20% decrease in the hard X-rays (20-40 keV), indicating that we have sampled the decaying part of the flare. The decrease is less apparent in the soft X-rays (5-15 keV). The simultaneous optical variations are weakly correlated with those at soft X-rays, and not clearly correlated with those at hard X-rays. The spectral energy distribution exhibits two components, as typically seen in blazars, which can be modeled with synchrotron radiation and inverse Compton scattering occurring in a region external to the broad line region.

Published
2006
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15. GRB 050509b: the elusive optical/nIR/mm afterglow of a short-duration GRB

Author

Castro-Tirado, A. J., Postigo, A. de Ugarte, Gorosabel, J., Fathkullin, T., Sokolov, V., Bremer, M., Márquez, I., Marín, A. J., Guziy, S., Jelínek, M., Kubánek, P., Hudec, R., Vitek, S., Mateo Sanguino, T. J., Eigenbrod, A., Pérez-Ramírez, M. D., Sota, A., Masegosa, J., Prada, F., Moles, M., Castro-Tirado, A. J., Postigo, A. de Ugarte, Gorosabel, J., Fathkullin, T., Sokolov, V., Bremer, M., Márquez, I., Marín, A. J., Guziy, S., Jelínek, M., Kubánek, P., Hudec, R., Vitek, S., Mateo Sanguino, T. J., Eigenbrod, A., Pérez-Ramírez, M. D., Sota, A., Masegosa, J., Prada, F., and Moles, M.

Abstract

We present multiwavelength (optical/near infrared/millimetre) observations of a short duration gamma-ray burst detected by Swift(GRB 050509b) collected between 0 seconds and ~18.8 days after the event. No optical, near infrared or millimetre emission has been detected in spite of the well localised X-ray afterglow, confirming the elusiveness of the short duration events. We also discuss the possibility of the burst being located in a cluster of galaxies at $z = 0.225$or beyond. In the former case, the spectral energy distribution of the neighbouring, potential host galaxy, favours a system harbouring an evolved dominant stellar population (age ~360 Myr), unlike most long duration GRB host galaxies observed so far, i.e. thus giving support to a compact binary merger origin. Any underlying supernova that could be associated with this particular event should have been at least 3 magnitudes fainter than the type Ib/c SN 1998bw and 2.3 mag fainter than a typical type Ia SN.

Published
2005
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16. GRB 040403: A faint X-ray rich gamma-ray burst discovered by INTEGRAL*

Author

Mereghetti, S., Götz, D., Andersen, M. I., Castro-Tirado, A., Frontera, F., Gorosabel, J., Hartmann, D. H., Hjorth, J., Hudec, R., Hurley, K., Pizzichini, G., Produit, N., Tarana, A., Topinka, M., Ubertini, P., de Ugarte, A., Mereghetti, S., Götz, D., Andersen, M. I., Castro-Tirado, A., Frontera, F., Gorosabel, J., Hartmann, D. H., Hjorth, J., Hudec, R., Hurley, K., Pizzichini, G., Produit, N., Tarana, A., Topinka, M., Ubertini, P., and de Ugarte, A.

Abstract

GRB 040403 is one of the faintest gamma-ray bursts for which a rapid and accurate localization has been obtained. Here we report on the gamma-ray properties of this burst, based on observations with the IBIS instrument aboard INTEGRAL, and the results of searches for its optical afterglow. The steep spectrum (power law photon index = 1.9 in the 20–200 keV range) implies that GRB 040403 is most likely an X-ray rich burst. Our optical limit of R> 24.2 at 16.5 h after the burst, indicates a rather faint afterglow, similar to those seen in other relatively soft and faint bursts.

Published
2005
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17. INTEGRALobservations of the field of the BL Lacertae object S5 0716+714*

Author

Pian, E., Foschini, L., Beckmann, V., Sillanpää, A., Soldi, S., Tagliaferri, G., Takalo, L., Barr, P., Ghisellini, G., Malaguti, G., Maraschi, L., Palumbo, G. G. C., Treves, A., Courvoisier, T. J.-L., Di Cocco, G., Gehrels, N., Giommi, P., Hudec, R., Lindfors, E., Marcowith, A., Nilsson, K., Pasanen, M., Pursimo, T., Raiteri, C. M., Savolainen, T., Sikora, M., Tornikoski, M., Tosti, G., Türler, M., Valtaoja, E., Villata, M., Walter, R., Pian, E., Foschini, L., Beckmann, V., Sillanpää, A., Soldi, S., Tagliaferri, G., Takalo, L., Barr, P., Ghisellini, G., Malaguti, G., Maraschi, L., Palumbo, G. G. C., Treves, A., Courvoisier, T. J.-L., Di Cocco, G., Gehrels, N., Giommi, P., Hudec, R., Lindfors, E., Marcowith, A., Nilsson, K., Pasanen, M., Pursimo, T., Raiteri, C. M., Savolainen, T., Sikora, M., Tornikoski, M., Tosti, G., Türler, M., Valtaoja, E., Villata, M., and Walter, R.

Abstract

We have performed observations of the blazar S5 0716+714 with INTEGRALon 2-6 April 2004. In the first months of 2004, the source had increased steadily in optical brightness and had undergone two outbursts. During the latter outburst, that occurred in March, it reached the extreme level of $R = 12.1$mag, which triggered our INTEGRALprogram. The target has been detected with IBIS/ISGRI up to 60 keV, with a flux of ∼$3 \times 10^{-11}$erg s-1cm-2in the 30–60 keV interval, a factor of ~2 higher than observed by the BeppoSAXPDS in October 2000. In the field of S5 0716+714 we have also detected the Flat Spectrum Radio Quasar S5 0836+710 and the two Seyfert galaxies Mkn 3 and Mkn 6. Their IBIS/ISGRI spectra are rather flat, albeit consistent with those measured by BeppoSAX. In the spectrum of Mkn 3 we find some evidence of a break between ~60 and ~100 keV, reminiscent of the high energy cut-offs observed in other Seyfert galaxies. This is the first report of INTEGRALspectra of weak Active Galactic Nuclei.

Published
2005
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18. The color evolution of the optical afterglow of GRB 030329 and the implications for the underlying supernova SN 2003dh

Author

Šimon, V., Hudec, R., Pizzichini, G., Šimon, V., Hudec, R., and Pizzichini, G.

Abstract

We find that the color indices $(B-V)_{0}$, $(V-R)_{0}$, $(R-I)_{0}$, $(I-J)_{0}$in the observer frame of the optical afterglow (OA) of GRB 030329 during $t-T_{0}<10$days are consistent with those of a uniform group of 25 OAs of GRBs, previously analyzed by Šimon et al. ([CITE]; [CITE]a). The synchrotron component with parameters similar to those of the other 25 OAs was thus initially dominant in the optical and IR spectrum of the OA of GRB 030329. Following the arguments of Šimon et al. ([CITE]), it also appears that either GRB 030329 was not located deep inside a star-forming region or that the local dust was destroyed by the intense initial flash. The absolute Rmagnitude of this event $M_{R_0}\approx -26.6$mag in the rest frame at $(t-T_{\rm 0})_{\rm rest}= 0.25$days is in good agreement with the typical brightness of the OAs analyzed by Šimon et al. ([CITE]). We detected large color variations of the OA of GRB 030329 only for $t-T_{0}>12$days, which suggest a rapid evolution of the spectrum of the underlying SN 2003dh. We compare it with the individual type Ic SNe and find that its color evolution is plausibly matched only by that of SN 1998bw although the indices still reveal spectral differences between the two objects. The agreement is particularly good only at $t-T_{0}= 26$and 27 days. The evolution of SN 2003dh becomes faster than that of SN 1998bw later on and SN 2003dh develops an excess light in the red/IR spectral region. We also emphasize the discordance with other type Ic SNe which are not associated with GRBs.

Published
2004
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19. Time resolved spectroscopy of GRB 030501 using INTEGRAL*

Author

Beckmann, V., Borkowski, J., Courvoisier, T. J.-L., Götz, D., Hudec, R., Hroch, F., Lund, N., Mereghetti, S., Shaw, S. E., von Kienlin, A., Wigger, C., Beckmann, V., Borkowski, J., Courvoisier, T. J.-L., Götz, D., Hudec, R., Hroch, F., Lund, N., Mereghetti, S., Shaw, S. E., von Kienlin, A., and Wigger, C.

Abstract

The gamma-ray instruments on-board INTEGRAL offer an unique opportunity to perform time resolved analysis on GRBs. The imager IBIS allows accurate positioning of GRBs and broad band spectral analysis, while SPI provides high resolution spectroscopy. GRB 030501 was discovered by the INTEGRAL Burst Alert System in the ISGRI field of view. Although the burst was fairly weak (fluence $F_{20-200 \,{\rm keV} } \simeq 3.5 \times 10^{-6}\,\rm{erg\,cm}^{-2})$it was possible to perform time resolved spectroscopy with a resolution of a few seconds. The GRB shows a spectrum in the 20–400 keV range which is consistent with a spectral index $\Gamma = -1.8$. No emission line or spectral break was detectable in the spectrum. Although the flux seems to be correlated with the hardness of the GRB spectrum, there is no clear soft to hard evolution seen over the duration of the burst. The INTEGRAL data have been compared with results from the Ulysses and RHESSI experiments.

Published
2003
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20. The Input Catalogue for the OMC camera onboard INTEGRAL

Author

Domingo, A., Caballero, M. D., Figueras, F., Jordi, C., Torra, J., Mas-Hesse, J. M., Giménez, A., Hudcova, V., Hudec, R., Domingo, A., Caballero, M. D., Figueras, F., Jordi, C., Torra, J., Mas-Hesse, J. M., Giménez, A., Hudcova, V., and Hudec, R.

Abstract

The Optical Monitoring Camera (OMC) onboard INTEGRAL (launched on October 17, 2002) has been designed to obtain V-Johnson photometry simultaneously with high energy observations at X-ray (3–35 keV) and (15 keV–10 MeV) performed by the main instruments onboard INTEGRAL. Due to technical limitations on the data processing electronics and the available telemetry, it is necessary to know, a priori, the objects to be monitored within the field of view (FOV) of the OMC. The OMC Input Catalogue – and subsequent provides this information: astrometric and photometric reference stars for calibration and scientific targets for accurate photometric variability studies.

Published
2003
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21. OMC: An Optical Monitoring Camera for INTEGRAL

Author

Mas-Hesse, J. M., Giménez, A., Culhane, J. L., Jamar, C., McBreen, B., Torra, J., Hudec, R., Fabregat, J., Meurs, E., Swings, J. P., Alcacera, M. A., Balado, A., Beiztegui, R., Belenguer, T., Bradley, L., Caballero, M. D., Cabo, P., Defise, J. M., Díaz, E., Domingo, A., Figueras, F., Figueroa, I., Hanlon, L., Hroch, F., Hudcova, V., García, T., Jordan, B., Jordi, C., Kretschmar, P., Laviada, C., March, M., Martín, E., Mazy, E., Menéndez, M., Mi, J. M., de Miguel, E., Muñoz, T., Nolan, K., Olmedo, R., Plesseria, J. Y., Polcar, J., Reina, M., Renotte, E., Rochus, P., Sánchez, A., San Martín, J. C., Smith, A., Soldan, J., Thomas, P., Timón, V., Walton, D., Mas-Hesse, J. M., Giménez, A., Culhane, J. L., Jamar, C., McBreen, B., Torra, J., Hudec, R., Fabregat, J., Meurs, E., Swings, J. P., Alcacera, M. A., Balado, A., Beiztegui, R., Belenguer, T., Bradley, L., Caballero, M. D., Cabo, P., Defise, J. M., Díaz, E., Domingo, A., Figueras, F., Figueroa, I., Hanlon, L., Hroch, F., Hudcova, V., García, T., Jordan, B., Jordi, C., Kretschmar, P., Laviada, C., March, M., Martín, E., Mazy, E., Menéndez, M., Mi, J. M., de Miguel, E., Muñoz, T., Nolan, K., Olmedo, R., Plesseria, J. Y., Polcar, J., Reina, M., Renotte, E., Rochus, P., Sánchez, A., San Martín, J. C., Smith, A., Soldan, J., Thomas, P., Timón, V., and Walton, D.

Abstract

The Optical Monitoring Camera (OMC) will observe the optical emission from the prime targets of the gamma-ray instruments onboard the ESA mission INTEGRAL, with the support of the JEM-X monitor in the X-ray domain. This capability will provide invaluable diagnostic information on the nature and the physics of the sources over a broad wavelength range. Its main scientific objectives are: (1) to monitor the optical emission from the sources observed by the gamma- and X-ray instruments, measuring the time and intensity structure of the optical emission for comparison with variability at high energies, and (2) to provide the brightness and position of the optical counterpart of any gamma- or X-ray transient taking place within its field of view. The OMC is based on a refractive optics with an aperture of 50 mm focused onto a large format CCD ($1024 \times 2048$pixels) working in frame transfer mode ($1024 \times 1024$pixels imaging area). With a field of view of $5^\circ\times5^\circ$it will be able to monitor sources down to magnitude $V = 18$. Typical observations will perform a sequence of different integration times, allowing for photometric uncertainties below 0.1 mag for objects with $V\le16$.

Published
2003
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22. The INTEGRALScience Data Centre (ISDC)

Author

Courvoisier, T. J.-L., Walter, R., Beckmann, V., Dean, A. J., Dubath, P., Hudec, R., Kretschmar, P., Mereghetti, S., Montmerle, T., Mowlavi, N., Paltani, S., Preite Martinez, A., Produit, N., Staubert, R., Strong, A. W., Swings, J.-P., Westergaard, N. J., White, N., Winkler, C., Zdziarski, A. A., Courvoisier, T. J.-L., Walter, R., Beckmann, V., Dean, A. J., Dubath, P., Hudec, R., Kretschmar, P., Mereghetti, S., Montmerle, T., Mowlavi, N., Paltani, S., Preite Martinez, A., Produit, N., Staubert, R., Strong, A. W., Swings, J.-P., Westergaard, N. J., White, N., Winkler, C., and Zdziarski, A. A.

Abstract

The INTEGRALScience Data Centre (ISDC) provides the INTEGRALdata and means to analyse them to the scientific community. The ISDC runs a gamma ray burst alert system that provides the position of gamma ray bursts on the sky within seconds to the community. It operates a quick-look analysis of the data within few hours that detects new and unexpected sources as well as it monitors the instruments. The ISDC processes the data through a standard analysis the results of which are provided to the observers together with their data.

Published
2003
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23. Observation of GRB 030131 with the INTEGRAL satellite *

Author

Götz, D., Mereghetti, S., Hurley, K., Deluit, S., Feroci, M., Frontera, F., Fruchter, A., Gorosabel, J., Hartmann, D. H., Hjorth, J., Hudec, R., Mirabel, I. F., Pian, E., Pizzichini, G., Ubertini, P., Winkler, C., Götz, D., Mereghetti, S., Hurley, K., Deluit, S., Feroci, M., Frontera, F., Fruchter, A., Gorosabel, J., Hartmann, D. H., Hjorth, J., Hudec, R., Mirabel, I. F., Pian, E., Pizzichini, G., Ubertini, P., and Winkler, C.

Abstract

A long Gamma-Ray Burst (GRB) was detected with the instruments on board the INTEGRAL satellite on January 31 2003. Although most of the GRB, which lasted ~150 s, occurred during a satellite slew, the automatic software of the INTEGRAL Burst Alert System was able to detect it in near-real time. Here we report the results obtained with the IBIS instrument, which detected GRB 030131 in the 15 keV–200 keV energy range, and ESO/VLT observations of its optical transient. The burst displays a complex time profile with numerous peaks. The peak spectrum can be described by a single power law with photon index $\Gamma\simeq1.7$and has a flux of ~2 photons cm-2s-1in the 20–200 keV energy band. The high sensitivity of IBIS has made it possible for the first time to perform detailed time-resolved spectroscopy of a GRB with a fluence of $7\times10^{-6}$erg cm-2(20–200 keV).

Published
2003
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24. The LOFT mission concept: a status update

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Feroci, M., Bozzo, E., Brandt, S., Hernanz, M., van der Klis, M., Liu, L.-P., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Zhang, S.-N., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J.-L., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, E., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, P., Bombaci, I., Bonnet Bidaud, J.-M., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M. S., Brown, E., Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz-Jørgensen, C., Cackett, E., Cadoux, F., Cais, P., Caliandro, G. A., Campana, R., Campana, S., Cao, X., Capitanio, F., Casares, J., Casella, P., Castro-Tirado, A. J., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda-Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, C., Chen, Y., Chen, Y., Chenevez, J., Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Z., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J. W., Diebold, S., Di Salvo, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S. A., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M. H., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, H., Ferrari, V., Ferrigno, C., Finger, M., Finger, M. H., Fraser, G. W., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D. K., Gálvez Sanchez, J. L., Gandhi, P., Gao, Z., Garcia-Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A. B., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, F., Hartmann, D. H., Haswell, C. A., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S. C., Ingram, A., In't Zand, J. J. M., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H. M., Jetter, F., Johannsen, T., Jenke, P. A., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A. F., Kreykenbohm, I., Kuiper, L. M., Kunneriath, D., Kurkela, A., Kuvvetli, I., La Franca, F., Labanti, C., Lai, D., Lamb, F. K., Lachaud, C., Laubert, P. P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, N., Maccarone, T. J., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S. B., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., McHardy, I. M., Medina-Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, M. C., Miller, J. M., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz-Darias, T., Negueruela, I., Neilsen, J., Neubert, T., Norton, A. J., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, P. E. H., Orienti, M., Orio, M., Orlandini, M., Osborne, J. P., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J. M., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A. V., Peretz, U., Perez, M. A., Perez-Torres, M., Peterson, B. M., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, J., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P. S., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D. H., Rodríguez-Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E. M. R., Rozanska, A., Rousseau, A., Rudak, B., Russell, D. M., Ryde, F., Sabau-Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner-Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J. D., Schneider, R., Schwenk, A., Schwope, A. D., Sedrakian, A., Seyler, J.-Y., Shearer, A., Slowikowska, A., Sims, M., Smith, A., Smith, D. M., Smith, P. J., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A. W., Stergioulas, N., Stevens, A. L., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F. K., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J. M., Torres, D. F., Torresi, E., Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F. H., Vrba, V., Walton, D., Wang, J., Wang, Z., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson-Hodge, C. A., Winter, B., Walk, S. J., Wood, K., Woosley, S. E., Wu, X., Xu, R., Yu, W., Yuan, F., Yuan, W., Yuan, Y., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, B., Zhang, C., Zhang, S., Zingale, M., and Zwart, F.

Published
2016
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25. Detection of an optical transient following the 13 March 2000 short/hard gamma-ray burst*

Author

Castro-Tirado, A. J., Castro Cerón, J. M., Gorosabel, J., Páta, P., Soldán, J., Hudec, R., Jelinek, M., Topinka, M., Bernas, M., Mateo Sanguino, T. J., Postigo, A. de Ugarte, Berná, J. Á., Henden, A., Vrba, F., Canzian, B., Harris, H., Delfosse, X., de Pontieu, B., Polcar, J., Sánchez-Fernández, C., de la Morena, B. A., Más-Hesse, J. M., Torres Riera, J., Barthelmy, S., Castro-Tirado, A. J., Castro Cerón, J. M., Gorosabel, J., Páta, P., Soldán, J., Hudec, R., Jelinek, M., Topinka, M., Bernas, M., Mateo Sanguino, T. J., Postigo, A. de Ugarte, Berná, J. Á., Henden, A., Vrba, F., Canzian, B., Harris, H., Delfosse, X., de Pontieu, B., Polcar, J., Sánchez-Fernández, C., de la Morena, B. A., Más-Hesse, J. M., Torres Riera, J., and Barthelmy, S.

Abstract

We imaged the error box of a gamma-ray burst of the short (0.5 s), hard type (GRB 000313), with the BOOTES-1 experiment in southern Spain, starting 4 min after the γ–ray event, in the I-band. A bright optical transient (OT 000313) with $I = 9.4 \pm 0.1$was found in the BOOTES-1 image, close to the error box (3σ) provided by BATSE. Late time $VRIK^\prime$-band deep observations failed to reveal an underlying host galaxy. If the OT 000313 is related to the short, hard GRB 000313, this would be the first optical counterpart ever found for this kind of events (all counterparts to date have been found for bursts of the long, soft type). The fact that only prompt optical emission has been detected (but no afterglow emission at all, as supported by theoretical models) might explain why no optical counterparts have ever been found for short, hard GRBs. This fact suggests that most short bursts might occur in a low-density medium and favours the models that relate them to binary mergers in very low-density environments.

Published
2002
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26. Colors and luminosities of the optical afterglows of the γ-ray bursts

Author

Šimon, V., Hudec, R., Pizzichini, G., Masetti, N., Šimon, V., Hudec, R., Pizzichini, G., and Masetti, N.

Abstract

Results of the study of the color indices and luminosities of 17 optical afterglows (OAs) of GRBs are presented. We show that the color variations during the decline of OAs (except for GRB000131) are relatively small during $t-T_{\rm 0}< 10$days and allow a comparison among them, even for the less densely sampled OAs. The colors in the observer frame, corrected for the Galactic reddening, concentrate at $(V-R)_0= 0.40\pm0.13$, $(R-I)_0= 0.46\pm0.18$, $(B-V)_0= 0.47\pm0.17$. The color evolution of the OAs is negligible although their brightness declines by several magnitudes during the considered time interval. Such a strong concentration of the color indices also suggests that the intrinsic reddening (inside their host galaxies) must be quite similar and relatively small for all these events. The absolute brightness of OAs in the observer frame, corrected for the host galaxy, lies within $M_{R_0}= -26.5$to -22.2 for $(t-T_{\rm 0})_{\rm rest}=0.25$days. This spread of $M_{R_0}$is not significantly influenced by the shifts of λ, caused by the different redshift zof the respective OAs. The general decline rate of the OA sample considered here seems to be independent of the absolute optical brightness of the OA, measured at some $t-T_{\rm 0}$identical for all OAs, and the light curves of all events are almost parallel, when corrected for the redshift-induced time dilation.

Published
2001
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27. The extraordinarily bright optical afterglow of GRB 991208 and its host galaxy

Author

Castro-Tirado, A. J., Sokolov, V. V., Gorosabel, J., Cerón, J. M. Castro, Greiner, J., Wijers, R. A. M. J., Jensen, B. L., Hjorth, J., Toft, S., Pedersen, H., Palazzi, E., Pian, E., Masetti, N., Sagar, R., Mohan, V., Pandey, A. K., Pandey, S. B., Dodonov, S. N., Fatkhullin, T. A., Afanasiev, V. L., Komarova, V. N., Moiseev, A. V., Hudec, R., Simon, V., Vreeswijk, P., Rol, E., Klose, S., Stecklum, B., Zapatero-Osorio, M. R., Caon, N., Blake, C., Wall, J., Heinlein, D., Henden, A., Benetti, S., Magazzù, A., Ghinassi, F., Tommasi, L., Bremer, M., Kouveliotou, C., Guziy, S., Shlyapnikov, A., Hopp, U., Feulner, G., Dreizler, S., Hartmann, D., Boehnhardt, H., Paredes, J. M., Martí, J., Xanthopoulos, E., Kristen, H. E., Smoker, J., Hurley, K., Castro-Tirado, A. J., Sokolov, V. V., Gorosabel, J., Cerón, J. M. Castro, Greiner, J., Wijers, R. A. M. J., Jensen, B. L., Hjorth, J., Toft, S., Pedersen, H., Palazzi, E., Pian, E., Masetti, N., Sagar, R., Mohan, V., Pandey, A. K., Pandey, S. B., Dodonov, S. N., Fatkhullin, T. A., Afanasiev, V. L., Komarova, V. N., Moiseev, A. V., Hudec, R., Simon, V., Vreeswijk, P., Rol, E., Klose, S., Stecklum, B., Zapatero-Osorio, M. R., Caon, N., Blake, C., Wall, J., Heinlein, D., Henden, A., Benetti, S., Magazzù, A., Ghinassi, F., Tommasi, L., Bremer, M., Kouveliotou, C., Guziy, S., Shlyapnikov, A., Hopp, U., Feulner, G., Dreizler, S., Hartmann, D., Boehnhardt, H., Paredes, J. M., Martí, J., Xanthopoulos, E., Kristen, H. E., Smoker, J., and Hurley, K.

Abstract

Broad-band optical observations of the extraordinarily bright optical afterglow of the intense gamma-ray burst GRB 991208 started ~2.1 days after the event and continued until 4 Apr. 2000. The flux decay constant of the optical afterglow in the R-band is -2.30 ±0.07 up to ~5 days, which is very likely due to the jet e ffect, and it is followed by a much steeper decay with constant -3.2 ±0.2, the fastest one ever seen in a GRB optical afterglow. A negative detection in several all-sky films taken simultaneously with the event, that otherwise would have reached naked eye brightness, implies either a previous additional break prior to ~2 days after the occurrence of the GRB (as expected from the jet effect) or a maximum, as observed in GRB 970508. The existence of a se cond break might indicate a steepening in the electron spectrum or the superposition of two events, resembling GRB 000301C. Once the afterglow emission vanished, contribution of a bright underlying supernova was found on the basis of the late-time R-band measurements, but the light curve is not sufficiently well sampled to rule out a dust echo explanation. Our redshift determination of $z = 0.706$indicates that GRB 991208 is at 3.7 Gpc (for $H_{0}= 60$km s-1Mpc-1, $\Omega_{0}= 1$and $\Lambda_{0}= 0$), implying an isotropic energy release of 1.15 1053erg which may be relaxed by beaming by a factor >102. Precise astrometry indicates that the GRB coincides within 0.2″ with the host galaxy, thus supporting a massive star origin. The absolute magnitude of the galaxy is MB= -18.2, well below the knee of the galaxy luminosity function and we derive a star-forming rate of ($11.5 \pm 7.1$) $M_{\odot}$yr-1, which is much larger than the present-day rate in our Galaxy. The quasi-simultaneous broad-band photometric spectral energy distribution of the afterglow was determined ~3.5 day after the burst (Dec. 12.0) implying a cooling frequency $\nu_{\rm c}$below the optical band, i.e. supporting a jet model with $p = -$2.30 as the index of the power-law electron distribution.

Published
2001
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29. The Large Observatory for x-ray timing

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Feroci, M., den Herder, J. W., Bozzo, E., Barret, D., Brandt, S., Hernanz, M., van der Klis, M., Pohl, M., Santangelo, A., Stella, L., Watts, A., Wilms, J., Zane, S., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J.-L., Azzarello, P., Bakala, P., Baldazzi, G., Balman, S., Barbera, M., van Baren, C., Bhattacharyya, S., Baykal, A., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bodin, P., Bombaci, I., Bonnet Bidaud, J.-M., Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz-Jørgensen, C., Cackett, E., Cadoux, F. R., Caïs, P., Caliandro, G. A., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro-Tirado, A. J., Cavazzuti, E., Cerda-Duran, P., Chakrabarty, D., Château, F., Chenevez, J., Coker, J., Cole, R., Collura, A., Cornelisse, R., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Ai, A., D'Elia, V., Del Monte, E., de Luca, A., de Martino, D., Dercksen, J. P. C., de Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Diebold, S., Di Salvo, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Erkut, M. H., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Finger, M. H., Fraser, G. W., Frericks, M., Fuschino, F., Gabler, M., Galloway, D. K., Galvez Sanchez, J. L., Garcia-Berro, E., Gendre, B., Gezari, S., Giles, A. B., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Gschwender, M., Gualtieri, L., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hansen, F., Hartmann, D. H., Haswell, C. A., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J. J. M., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H. M., Jetter, F., Johannsen, T., Jonker, P., Josè, J., Kaaret, P., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Kokkotas, K., Korpela, S., Kouveliotou, C., Kreykenbohm, I., Kuiper, L. M., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F. K., Laubert, P. P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T. J., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Mandel, I., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., McHardy, I. M., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M. C., Miller, J. M., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz-Darias, T., Negueruela, I., Neilsen, J., Norton, A. J., Nowak, M., O'Brien, P., Olsen, P. E. H., Orienti, M., Orio, M., Orlandini, M., Orleański, P., Osborne, J. P., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J. M., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A. V., Perez, M. A., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Poutanen, J., Prakash, M., Le Provost, P., Psaltis, D., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rachevski, A., Rashevskaya, I., Ray, P. S., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rodríguez-Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E. M. R., Rozanska, A., Rousseau, A., Ryde, F., Sabau-Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Sandberg, J., Scaringi, S., Schanne, S., Schee, J., Schmid, C., Shore, S., Schneider, R., Schwenk, A., Schwope, A. D., Seyler, J.-Y., Shearer, A., Smith, A., Smith, D. M., Smith, P. J., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A. W., Stergioulas, N., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J. M., Torres, D. F., Tramacere, A., Trois, A., Turolla, R., Turriziani, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vrba, V., Walton, D., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson-Hodge, C. A., Winter, B., Wood, K., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zhang, B., Zwart, F., Ayre, M., Boenke, T., Corral van Damme, C., Kuulkers, Erik, and Lumb, D.

Published
2014
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30. The large area detector of LOFT: the Large Observatory for X-ray Timing

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Zane, S., Walton, D., Kennedy, T., Feroci, M., Den Herder, J.-W, Ahangarianabhari, M., Argan, A., Azzarello, P., Baldazzi, G., Barbera, M., Barret, D., Bertuccio, G., Bodin, P., Bozzo, E., Bradley, L., Cadoux, F., Cais, P, Campana, R., Coker, J., Cros, A., Del Monte, E., De Rosa, A., Di Cosimo, S., Donnarumma, I., Evangelista, Y., Favre, Y., Feldman, C., Fraser, G., Fuschino, F., Grassi, M., Hailey, M. R., Hudec, R., Labanti, C., Malcovati, P., Macera, D., Marisaldi, M., Martindale, A., Mineo, T., Muleri, F., Nowak, M., Orlandini, M., Pacciani, L., Perinati, E., Petracek, V., Pohl, M., Rachevski, A., Smith, P., Santangelo, A., Seyler, J.-Y., Schmid, C., Soffitta, P., Suchy, S., Tenzer, C., Uttley, P., Vacchi, A., Zampa, G., Zampa, N., Wilms, J., and Winter, B.

Published
2014
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31. The design of the wide field monitor for the LOFT mission

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Brandt, S., Hernanz, M., Alvarez, L., Argan, A., Artigues, B., Azzarello, P., Barret, D., Bozzo, E., Budtz-Jørgensen, C., Campana, R., Cros, A., del Monte, E., Donnarumma, I., Evangelista, Y., Feroci, M., Galvez Sanchez, J. L., Götz, D., Hansen, F., den Herder, J. W., Hudec, R., Huovelin, J., Karelin, D., Korpela, S., Lund, N., Michalska, M., Olsen, P., Orleanski, P., Pedersen, S., Pohl, M., Rachevski, A., Santangelo, A., Schanne, S., Schmid, C., Suchy, S., Tenzer, C., Vacchi, A., Walton, D., Wilms, J., Zampa, G., Zampa, N., in't Zand, J., Zane, S., Zdziarski, A., and Zwart, F.

Published
2014
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33. Slumping of Si wafers at high temperature

Author

Juha, Libor, Bajt, Saša, London, Richard, Hudec, René, Pina, Ladislav, Mika, M., Jankovsky, O., Simek, P., Lutyakov, O., Havlikova, R., Sofer, Z., Hudec, R., Pina, L., Inneman, A., Sveda, L., and Marsikova, V.

Published
2013
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34. Si and Glass - Novel Technologies for Space

Author

Hudec, R., Pina, L., Semencova, V., Inneman, A., Skulinova, M., Sveda, L., Mika, M., Brozek, V., Kacerovsky, R., Prokop, J., and Sik, J.

Subjects
*TECHNOLOGY, *SPACE sciences, *X-ray telescopes, *NUCLEAR physics
Abstract

The thermally formed thin glass foils and optically shaped Si wafers are considered to belong to the most promising technologies for future large space X-ray telescopes. We present and discuss the recent progress in these technologies, as well as properties of test mirrors produced and tested. [Copyright &y& Elsevier]

Published
2007
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35. LOBSTER – New Space X–Ray telescopes

Author

Hudec, R., Pina, L., Šimon, V., Švéda, L., Inneman, A., Semencová, V., and Skulinová, M.

Subjects
*X-ray telescopes, *SPACE telescopes, *GAMMA ray bursts, *NUCLEAR physics
Abstract

We discuss the technological and scientific aspects of fully innovative very wide–field X–ray telescopes with high sensitivity. The prototypes of Lobster telescopes designed, developed and tested are very promising, allowing the proposals for space projects with very wide–field Lobster Eye X–ray optics to be considered for the first time. The novel telescopes will monitor the sky with unprecedented sensitivity and angular resolution of order of 1 arcmin. They are expected to contribute essentially to study of various astrophysical objects such as AGN, SNe, Gamma-ray bursts (GRBs), X–ray flashes (XRFs), galactic binary sources, stars, CVs, X-ray novae, various transient sources, etc. For example, the Lobster optics based X-ray All Sky Monitor is capable to detect around 20 GRBs and 8 XRFs yearly and this will surely significantly contribute to the related science. [Copyright &y& Elsevier]

Published
2007
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36. Variable X–ray sky with Lobster Eye Telescopes

Author

Hudec, R., Pína, L., Inneman, A., and Švéda, L.

Subjects
*X-rays, *ELECTROMAGNETIC waves, *ASTROPHYSICS, *ASTRONOMY
Abstract

The variable X-ray sky requires wide–field monitoring with high sensitivity. We refer on novel X–ray telescopes with high sensitivity as well as large field of view. The results are very promising, allowing the proposals for space projects with very wide–field Lobster–eye X–ray optics to be considered. The novel telescopes will monitor the sky with unprecedented sensitivity and angular resolution of order of 1 arcmin. They are expected to contribute essentially to study and to understand various astrophysical objects such as AGN, SNe, GRBs, X–ray flashes, galactic binary sources, stars, CVs, X-ray novae, various transient sources, etc. [Copyright &y& Elsevier]

Published
2004
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37. Discovery and Evolution of an Unusual Luminous Variable Star in NGC 3432 (Supernova 2000ch)

Author

Wagner, R. M., Vrba, F. J., Henden, A. A., Canzian, B., Luginbuhl, C. B., Filippenko, A. V., Chornock, R., Li, W., Coil, A. L., Schmidt, G. D., Smith, P. S., Starrfield, S., Klose, S., Tichá, J., Tichý, M., Gorosabel, J., Hudec, R., and Simon, V.

Abstract

We present photometric and spectroscopic observations of SN 2000ch, an unusual and extremely luminous variable star located in the galaxy NGC 3432. The object was discovered on 2000 May 3.2 during the course of the Lick Observatory Supernova Search, at an unfiltered magnitude of about 17.4. Prediscovery images obtained in 1997, 1998, and 2000 April show the object with R = 19.2-19.5 mag. Optical spectra obtained beginning on 2000 May 6 show a smooth, flat continuum and strong, broad hydrogen Balmer emission lines at wavelengths consistent with the cataloged redshift of NGC 3432, strengthening the association of the variable with the galaxy. Photometric monitoring reveals a complex and erratic light curve over a time span of ?10 days. Subsequent optical spectra over the next ?3 months continued to show strong Balmer emission lines with a mean full width at half-maximum intensity ?1550 km s?1and a distinct red asymmetry. A spectrum obtained 9 months after the outburst is similar to the previous spectra, but the integrated flux in H? is nearly half that observed during the outburst. The object's photometric behavior, spectrum, and luminosity suggest that it is a very massive and luminous variable star and might be related to some luminous blue variable stars such as ? Carinae and SN 1997bs in NGC 3627. The brightest apparent magnitude implies an absolute magnitude of MV? - 12.7 at the distance of NGC 3432, a value that is comparable to ? Car during its outburst in the mid-19th century.

Published
2004
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39. The Burst Observer and Optical Transient Exploring System (BOOTES)

Author

Castro-Tirado, A. J., Soldán, J., Bernas, M., Páta, P., Rezek, T., Hudec, R., Sanguino, T. M., de la Morena, B., Berná, J. A., Rodríguez, J., Peña, A., Gorosabel, J., Más-Hesse, J. M., Giménez, A., Castro-Tirado, A. J., Soldán, J., Bernas, M., Páta, P., Rezek, T., Hudec, R., Sanguino, T. M., de la Morena, B., Berná, J. A., Rodríguez, J., Peña, A., Gorosabel, J., Más-Hesse, J. M., and Giménez, A.

Abstract

The Burst Observer and Optical Transient Explo ring System (BOOTES) is considered as a part of the preparations for the ESA's satellite INTEGRAL, and is currently being developed in Spain, in collaboration with two Czech institutions. It makes use of two sets of wide-field cameras 240 kms apart, and two robotic 0.3-m telescopes. The first obser ving station (BOOTES-1) is located in Huelva (Spain) and the first light was obtained in July 1998. During the test phase, it has provided rapid follow-up observations for 5 GRBs detected by the BATSE aboard the CGRO. The system will fully operate in late 1999.

Published
1999
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41. Operational testing of the SBIG ST-6 CCD camera

Author

Pravec, P., Hudec, R., Soldán, J., Sommer, M., and Schenkl, K. H.

Abstract

The SBIG Model ST-6 CCD Imaging Camera was tested and found suitable for various kinds of astronomical observations on telescopes with apertures from 6 mm to 0.6 m. We discuss different noise sources, linearity, sensitivity, and other detector characteristics. Limits, which they set to the observations and accuracy of data evaluation process, are also discussed. Detection, accurate astrometry, and VR photometry limiting magnitudes are about 21, 20, and 17.5, respectively, with the 0.6-m telescope and 10-min integration time. Detection of 5th magnitude 1-second optical transients is possible with the 6-mm wide-field lens.

Published
1994
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42. Preliminary results of optical searches of IPN3 localizations

Author

Luginbuhl, C. B., Vrba, F. J., Hudec, R., Hartmann, D., Hurley, K., Boër, M., Niel, M., Sommer, M., Kouveliotou, C., Meegan, C., and Fishman, G.

Abstract

We present preliminary results from deep optical searches of small (=~5 arcmin2) GRB error boxes determined using the Third Interplanetary Network (IPN3). Two of these fields also have been found to have historical OT events located within the IPN3 error boxes. We compare the preliminary results of these searches to those reported for the larger IPN1 error boxes. The small size of the IPN3 error boxes should allow a test of the hypothesis suggested by the IPN1 study that there are excess QSOs associated with the GRB fields.

Published
1995
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43. A simultaneous X-ray and optical study of TT Arietis

Author

Hudec, R., Valnícek, B., Peřesty, R., Wenzel, W., Richter, G. A., Goetz, W., Hacke, G., Hutch, H., Schult, R., Pfau, W., Reimann, G. -H., Stecklum, B., Tremko, J., Mrkos, A., Schpitshka, I. V., Kojevnikov, V. P., Kumshiashvili, M. I., Oprescu, G., Dumitrescu, A., Cristescu, C., Bojack, W., Patkós, L., Toth, I., and Olah, K.

Abstract

Prelimary results of an extended program of coordinated X-ray and optical observations of TT Ari are presented. The object was observed on August 21/22 1985 both in X-rays (EXOSAT) and optical range, about 100 days after the return to the active state. The first detailed simultaneous study of TT Ari in active state indicates the presence of strongly absorbing structure in the system.

Published
1987
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44. X-Ray and optical observations of the X-ray source EX0020528+1454.8

Author

Hudec, R., Wenzel, W., Goetz, W., Valníček, B., Peřestý, R., Richter, G. A., Hacke, G., Huth, H., Mrkos, A., and Tremko, J.

Abstract

We present preliminary results of the EXOSAT X-ray observations and quasisimultaneous and simultaneous optical photometry of the X-ray source EX0020528+1454.8=1E0205+149 found independently as an serendipitous source both with Einstein and EXOSAT satellites. The optical counterpart is a pair of dMe stars. Our results indicate that the object is variable both in X-rays and optical wavelenghts, and probably belongs to dMe flare stars.

Published
1987
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45. Investigation of blazars with the INTEGRAL satellite

Author

Hudec, R., Kubánek, P., Munz, F., and Pian, E.

Subjects
*BL Lacertae objects, *ARTIFICIAL satellites, *RADIO sources (Astronomy), *NUCLEAR physics
Abstract

We discuss the ESA INTEGRAL satellite data for specific class of active galactic nuclei - blazars. These objects represent promising sources to be observed by INTEGRAL, especially during their active states. Suitable strategy for the future analysis is also proposed and discussed. [Copyright &y& Elsevier]

Published
2007
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