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42 results on '"Hudec, R."'

1. Renewed activity from the X-ray transient SAXJ 1810.8-2609 with INTEGRAL

Author

Fiocchi, M., Natalucci, L., Chenevez, J., Bazzano, A., Tarana, A., Ubertini, P., Brandt, S., Beckmann, V., Federici, M., Galis, R., and Hudec, R.

Subjects
Astrophysics
Abstract

We report on the results of INTEGRAL observations of the neutron star low mass X-ray binary SAX J1810.8-2609 during its latest active phase in August 2007. The current outburst is the first one since 1998 and the derived luminosity is 1.1-2.6x10^36 erg s-1 in the 20-100 keV energy range. This low outburst luminosity and the long-term time-average accretion rate of ~5x10^-12Msolar/yr suggest that SAXJ 1810.8-2609 is a faint soft X-ray transient. During the flux increase, spectra are consistent with a thermal Comptonization model with a temperature plasma of ~23-30 keV and an optical depth of ~1.2-1.5, independent from luminosity of the system. This is a typical low hard spectral state for which the X-ray emission is attributed to the upscattering of soft seed photons by a hot, optically thin electron plasma. During the decay, spectra have a different shape, the high energy tail being compatible with a single power law. This confirm similar behavior observed by BeppoSAX during the previous outburst, with absence of visible cutoff in the hard X-ray spectrum. INTEGRAL/JEM-X instrument observed four X-ray bursts in Fall 2007. The first one has the highest peak flux (~3.5Crab in 3--25 keV) giving an upper limit to the distance of the source of about 5.7 kpc, for a LEdd~3.8x10^38 erg s^-1. The observed recurrence time of ~1.2 days and the ratio of the total energy emitted in the persistent flux to that emitted in the bursts (~73) allow us to conclude that the burst fuel was composed by mixed hydrogen and helium with X>0.4., Comment: accepted ApJ

Published
2008
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2. Optical and infrared flares from a transient Galactic soft gamma-ray repeater

Author

Castro-Tirado, A. J., Postigo, A. de Ugarte, Gorosabel, J., Jelinek, M., Fatkhullin, T. A., Sokolov, V. V., Ferrero, P., Kann, D. A., Klose, S., Sluse, D., Bremer, M., Winters, J. M., Nuernberger, D., Perez-Ramirez, D., Guerrero, M. A., French, J., Melady, G., Hanlon, L., McBreen, B., Aceituno, F. J., Cunniffe, R., Kubanek, P., Vitek, S., Schulze, S., Wilson, A. C., Hudec, R., Gonzalez-Perez, J. M., Shahbaz, T., Guziy, S., Pandey, S. B., Pavlenko, L., Sonbas, E., Trushkin, S. A., Bursov, N. N., Nizhelskij, N. A., and Sabau-Graziati, L.

Subjects
Astrophysics
Abstract

Soft gamma-ray repeaters (SGRs) are a rare type of gamma-ray transient sources that are ocasionally detected as bursts in the high-energy sky. They are thought to be produced by magnetars, young neutron stars with very strong magnetic fields of the order of 10^(14-15) G. Only three such objects are known in our Galaxy, and a fourth one is associated with the supernova remnant N49 in the Large Magellanic Cloud. In none of these cases has an optical counterpart to either the gamma-ray flares or the quiescent source been identified. Here we present multi-wavelength observations of a puzzling source, SWIFT J195509+261406, for which we detected more than 40 flaring episodes in the optical band over a time span of 3 days, plus a faint infrared flare 11 days later, after which it returned to quiescence. We propose that SWIFT J195509+261406 is a member of a subgroup of SGRs for which the long-term X-ray emission is transient in nature. Furthermore, it is the first SGR for which bursts have been detected in the optical and near-infrared bands and maybe the link between the "persistent" SGRs and the dim isolated neutron stars., Comment: Version submitted to Nature on 31 Jan 2008. A substantially revised version of this work has been published in Nature, vol. 455 issue 7212 pp 506-509 under the title "Flares from a Galactic magnetar suggest a missing link to dim isolated neutron stars"

Published
2008
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3. Discovery and identification of the very high redshift afterglow of GRB 050904

Author

Haislip, J., Nysewander, M., Reichart, D., Levan, A., Tanvir, N., Cenko, S., Fox, D., Price, P., Castro-Tirado, A., Gorosabel, J., Evans, C., Figueredo, E., MacLeod, C., Kirschbrown, J., Jelinek, M., Guziy, S., Postigo, A. de Ugarte, Cypriano, E., LaCluyze, A., Graham, J., Priddey, R., Chapman, R., Rhoads, J., Fruchter, A., Lamb, D., Kouveliotou, C., Wijers, R., Schmidt, B., Soderberg, A., Kulkarni, S., Harrison, F., Moon, D., Gal-Yam, A., Kasliwal, M., Hudec, R., Vitek, S., Kubanek, P., Crain, J., Foster, A., Bayliss, M., Clemens, J., and Bartelme, J.

Subjects
Astrophysics
Abstract

In 2000, Lamb and Reichart predicted that gamma-ray bursts (GRBs) and their afterglows occur in sufficient numbers and at sufficient brightnesses at very high redshifts (z > 5) to eventually replace quasars as the preferred probe of element formation and reionization in the early universe and to be used to characterize the star-formation history of the early universe, perhaps back to when the first stars formed. Here we report the discovery of the afterglow of GRB 050904 and the identification of GRB 050904 as the first very high redshift GRB. We measure its redshift to be 6.39(+0.11,-0.12), which is consistent with the reported spectroscopic redshift (6.29 +/- 0.01). Furthermore, just redward of Ly-alpha the flux is suppressed by a factor of three on the first night, but returns to expected levels by the fourth night. We propose that this is due to absorption by molecular hydrogen that was excited to rovibrational states by the GRB's prompt emission, but was then overtaken by the jet. Now that very high redshift GRBs have been shown to exist, and at least in this case the afterglow was very bright, observing programs that are designed to capitalize on this science will likely drive a new era of study of the early universe, using GRBs as probes., Comment: Submitted to Nature, 11 pages, 3 figures, LaTeX

Published
2005
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4. Optical replication techniques for image slicers

Author

Schmoll, J., Robertson, D. J., Dubbeldam, C. M., Yao, J., Bortoletto, F., Pina, L., Hudec, R., Prieto, E., Norrie, C., Ramsay-Howat, S., and Preuss, W.

Subjects
Astrophysics
Abstract

The Smart Focal Planes (SmartFP) activity is a European Joint Research Activity funded to develop novel optical technologies for future large telescope instrumentation. In this paper, we will discuss the image slicer developments being carried out as part of this initiative. Image slicing technique s have many applications in the plans for instrumentation on Extremely Large Telescopes and will be central to the delivery of the science case. A study of a virtual "multi-object multi-ifu spectrograph and imager" (MOMSI) for a hypothetical OWL-class telescope reveals the need for focal plane splitting, deployable imagers and very small beam steering elements like deployable IFUs. The image slicer workpackage, lead from Durham University in collaboration with LFM Bremen, TNO Delft, UKATC Edinburgh, CRAL Lyon, LAM Marseille, Padua University and REFLEX Prague, is evaluating technologies for manufacturing micro optics in large numbers to enable multi-object integral field spectroscopy., Comment: To be published in the proceedings of the Durham Integral Field Spectroscopy workshop 2005 July 04-08. REPLACEMENT (Sep 29): Author list updated

Published
2005
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5. GRB 050509b: the elusive optical/nIR/mm afterglow of a short-duration GRB

Author

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

Subjects
Astrophysics
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 magnitudes fainter than a typical type Ia SN., Comment: Accepted for publication in A&A letters

Published
2005
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6. GRB 040403: a faint X-ray rich Gamma-ray Burst discovered by INTEGRAL

Author

Mereghetti, S., Gotz, 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.

Subjects
Astrophysics
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 hours after the burst, indicates a rather faint afterglow, similar to those seen in other relatively soft and faint bursts., Comment: 5 pages, 3 figures, accepted for publication in Astronomy and Astrophysics Letters

Published
2004
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7. Probing a GRB progenitor at a redshift of z=2: a comprehensive observing campaign of the afterglow of GRB 030226

Author

Klose, S., Greiner, J., Rau, A., Henden, A. A., Hartmann, D. H., Zeh, A., Ries, C., Masetti, N., Malesani, D., Guenther, E., Gorosabel, J., Stecklum, B., Antonelli, L. A., Brinkworth, C., Cerón, J. M. Castro, Castro-Tirado, A. J., Covino, S., Fruchter, A., Fynbo, J. P., Ghisellini, G., Hjorth, J., Hudec, R., Jelínek, M., Kaper, L., Kouveliotou, C., Lindsay, K., Maiorano, E., Mannucci, F., Nysewander, M., Palazzi, E., Pedersen, K., Pian, E., Reichart, D., Rhoads, J., Rol, E., Smail, I., Tanvir, N. R., Postigo, A. de Ugarte, Vreeswijk, P. M., Wijers, R. A. M. J., and Heuvel, E. P. J. van den

Subjects
Astrophysics
Abstract

We report results from a comprehensive follow-up observing campaign of the afterglow of GRB 030226, including VLT spectroscopy, VLT polarimetry, and Chandra X-ray observations. In addition, we present BOOTES-1 wide-field observations at the time of the occurrence of the burst. First observations at ESO started 0.2 days after the event when the GRB afterglow was at a magnitude of R~19 and continued until the afterglow had faded below the detection threshold (R>26). No underlying host galaxy was found. The optical light curve shows a break around 0.8 days after the burst, which is achromatic within the observational errors, supporting the view that it was due to a jetted explosion. Close to the break time the degree of linear polarization of the afterglow light was less than 1.1%, which favors a uniform jet model rather than a structured one. VLT spectra show two absorption line systems at redshifts z=1.962+/-0.001 and at z=1.986+/-0.001, placing the lower limit for the redshift of the GRB close to 2. We emphasize that the kinematics and the composition of the absorbing clouds responsible for these line systems is very similar to those observed in the afterglow of GRB 021004. This corroborates the picture in which at least some GRBs are physically related to the explosion of a Wolf-Rayet star., Comment: accepted by Astron. J.; address of two co-authors corrected

Published
2004
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8. The sky behind our galaxy as seen by IBIS on INTEGRAL

Author

Bassani, L., Malizia, A., Stephen, J. B., Gianotti, F., Schiavone, F., Bazzano, A., Bird, A. J., Bouchet, L., Courvoisier, T., Dean, A. J., De Cesare, G., Del Santo, M., De Rosa, A., Hudec, R., Mirabel, F., Laurent, P., Piro, L., Shaw, S., and Zdziarski, A. A.

Subjects
Astrophysics
Abstract

During the Core Programme, INTEGRAL has surveyed a large portion of the sky (around 9000 square degrees); although INTEGRAL is not optimized for extra-galactic studies its observations have nevertheless given us the opportunity to explore the sky behind our Galaxy, something which is impossible in some wavebands due to the presence of strong absorption. Preliminary results from this exploration are presented and compared with the pre-launch expectations. In particular, we detail all extragalactic detections obtained so far: 10 active galaxies and one cluster of galaxies. Of these sources, many have previously been studied at energies above 10-20 keV while a few are new hard X-ray discoveries. Since the number of detections is smaller than estimated on the basis of the IBIS/ISGRI sensitivity, it is likely that some of the new ISGRI sources found in this survey are extragalactic objects; a few of these are likely to be AGN and are described in detail., Comment: 7 pages, 10 figures. Proceedings of the V INTEGRAL Workshop, Munich 16-20 February 2004. ESA SP-552

Published
2004

9. 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., Ticha, J., Tichy, M., Gorosabel, J., Hudec, R., and Simon, V.

Subjects
Astrophysics
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. Pre-discovery 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 catalogued 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 and a distinct red asymmetry. A spectrum obtained 9 months after the outburst is similar to the previous spectra, but the integrated flux in H-alpha 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 eta Carinae and SN 1997bs in NGC 3627. The brightest apparent magnitude implies an absolute magnitude of approximately -12.7 at the distance of NGC 3432, a value which is comparable to eta Carinae during its outburst in the mid-nineteenth century., Comment: 18 pages, 9 figures, PASP, in press

Published
2004
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10. The INTEGRAL Science 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., Martinez, A. Preite, Produit, N., Staubert, R., Strong, A. W., Swings, J. -P., Westergaard, N. J., White, N., Winkler, C., and Zdziarski, A. A.

Subjects
Astrophysics
Abstract

The INTEGRAL Science Data Centre (ISDC) provides the INTEGRAL data 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., Comment: 5 pages, 2 figures. Accepted for publication in A&AL (INTEGRAL issue)

Published
2003
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11. Observation of GRB 030131 with the INTEGRAL satellite

Author

Gotz, 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.

Subjects
Astrophysics
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 $\sim$150 seconds, 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\simeq$1.7 and has a flux of $\sim$2 photons cm$^{-2}$ s$^{-1}$ in 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)., Comment: Accepted for publication in A&A, 5 pages, 4 figures, latex

Published
2003
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12. Time resolved spectroscopy of GRB030501 using INTEGRAL

Author

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

Subjects
Astrophysics
Abstract

The Gamma-ray instruments on-board INTEGRAL offer an unique opportunity to perform time resolved analysis on GRBs. The imager IBIS allows accurate positiioning 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 = 3.5 * 10^-6 erg cm^-2 in the 20-200 keV energy band) 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 photon index of -1.7. 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., Comment: 4 pages, 5 figures, accepted for publication in Astronomy & Astrophysics

Published
2003
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13. Detection of an optical transient following the 13 March 2000 short/hard gamma-ray burst

Author

Castro-Tirado, A. J., Cerón, J. M. Castro, Gorosabel, J., Pata, P., Soldan, J., Hudec, R., Jelinek, M., Topinka, M., Bernas, M., Sanguino, T. J. Mateo, Postigo, A. de Ugarte, Berna, J. A., Henden, A., Vrba, F., Canzian, B., Harris, H., Delfosse, X., de Pontieu, B., Polcar, J., Sanchez-Fernandez, C., de la Morena, B., Mas-Hesse, J., Torres, J., and Barthelmy, S.

Subjects
Astrophysics
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 gamma-ray event, in the I-band. A bright optical transient (OT 000313) with I = 9.4 +/- 0.1 was found in the BOOTES-1 image, close to the error box (3-sigma) provided by BATSE. Late time VRIK'-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 enviroments., Comment: Revised version. Accepted for publication in Astronomy and Astrophysics Letters, 5 pages, 3 figures

Published
2002
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14. Colors and luminosities of the optical afterglows of the gamma-ray bursts

Author

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

Subjects
Astrophysics
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_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 +- 0.13, (R-I)_0 = 0.46 +- 0.18, (B-V)_0 = 0.47 +- 0.17. 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_0)_rest = 0.25 days. This spread of M_(R_0) is not significantly influenced by the shifts of lambda, caused by the different redshift z of 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_0 identical for all OAs, and the light curves of all events are almost parallel, when corrected for the redshift-induced time dilation., Comment: 11 pages, 2 tables, 7 figures; to be published on Astronomy & Astrophysics

Published
2001
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15. 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., Magazzu, 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., Marti, J., Xanthopoulos, E., Kristen, H. E., Smoker, J., and Hurley, H.

Subjects
Astrophysics
Abstract

Observations of the extraordinarily bright optical afterglow (OA) of GRB 991208 started 2.1 d after the event. The flux decay constant of the OA in the R-band is -2.30 +/- 0.07 up to 5 d, which is very likely due to the jet effect, and after that it is followed by a much steeper decay with constant -3.2 +/- 0.2, the fastest one ever seen in a GRB OA. A negative detection in several all-sky films taken simultaneously to the event implies either a previous additional break prior to 2 d after the occurrence of the GRB (as expected from the jet effect). The existence of a second break might indicate a steepening in the electron spectrum or the superposition of two events. Once the afterglow emission vanished, contribution of a bright underlying SN is found, but the light curve is not sufficiently well sampled to rule out a dust echo explanation. Our determination of z = 0.706 indicates that GRB 991208 is at 3.7 Gpc, implying an isotropic energy release of 1.15 x 10E53 erg which may be relaxed by beaming by a factor > 100. Precise astrometry indicates that the GRB coincides within 0.2" with the host galaxy, thus given support to a massive star origin. The absolute magnitude is M_B = -18.2, well below the knee of the galaxy luminosity function and we derive a star-forming rate of 11.5 +/- 7.1 Mo/yr. The quasi-simultaneous broad-band photometric spectral energy distribution of the afterglow is determined 3.5 day after the burst (Dec 12.0) implying a cooling frequency below the optical band, i.e. supporting a jet model with p = -2.30 as the index of the power-law electron distribution., Comment: Accepted for publication in Astronomy and Astrophysics, 9 pages, 6 figures (Fig. 3 and Fig. 4 have been updated)

Published
2001
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16. eXTP: Enhanced X-Ray Timing and Polarimetry Mission

Author

Zhang, S. N, Feroci, M, Santangelo, A, Dong, Y. W, Feng, H, Lu, F. J, Nandra, K, Wang, Z. S, Zhang, S, Bozzo, E, Brandt, S, De Rosa, A, Gou, L. J, Hernanz, M, Van der Klis, M, LI, X. D, Liu, Y, Orleanski, P, Pareschi, G, Pohl, M, Poutanen, J, Qu, J. L, Schanne, S, Stella, L, Uttley, P, Watts, A, Xu, R. X, Yu, W. F, In 't Zand, J. J. M, Zane, S, Alvarez, L, Amati, L, Baldini, L, Bambi, C, Basso, S, Bhattacharyya, S, Bellazzini, R, Belloni, T, Bellutti, P, Bianchi, S, Brez, A, Bursa, M, Burwitz, V, Tagliaferri, G, Budtz-Jorgensen, C, Caiazzo, I, Campana, R, Cao, X. L, Casella, P, Chen, C. Y, Chen, L, Chen, T. X, Chen, Y, Chen, Y. P, Civitani, M, Coti Zelati, F, Cui, W, Cui, W. W, Dai, Z. G, Del Monte, E, De Martino, D, Di Cosimo, S, Diebold, S, Dovciak, M, Donnarumma, I, Doroshenko, V, Esposito, P, Evangelista, Y, Favre, Y, Friedrich, P, Fuschino, F, Galvez, J. L, Gao, Z. L, Ge, M. Y, Gevin, O, Goetz, D, Han, D. W, Heyl, J, Horak, J, Hu, W, Huang, F, Huang, Q. S, Hudec, R, Huppenkothen. D, Israel, G. L, Ingram, A, Karas, V, Karelin, D, Jenke, P. A, Ji, L, Kennedy, T, Korpela, S, Kunneriath, D, Labanti, C, Li, G, Li, X, Li, Z. S, Liang, E. W, Limousin, O, Lin, L, Ling, Z. X, Liu, H. B, Liu, H. W, Liu, Z, Lu, B, Lund, N, Lai, D, Luo, B, Luo, T, Ma, B, Mahmoodifar, S, Marisaldi, M, Martindale, A, Meidinger, N, Men, Y. P, Michalska, M, Mignani, R, Minuti, M, Motta, S, Muleri, F, Neilsen, J, Orlandini, M, Pan, A. T, Patruno, A, Perinati, E, Picciotto, A, Piemonte, C, Pinchera, M, Rachevski, A, Rapisarda, M, Rea, N, Rossi, E. M. R, Rubini, A, Sala, G, Shu, X. W, Sgro, C, Shen, Z. X, Soffitta, P, Song, L. M, Spandre, G, Stratta, G, Strohmayer, T. E, Sun, L, Svoboda, J, Tenzer, C, Tong, H, Taverna, R, Torok, G, Turolla, R, Vacchi, A, Wang, J, Wang, J. X, Walton, D, Wang, K, Wang, J. F, Wang, R. J, Wang, Y. F, Weng, S. S, Wilms, J, Winter, B, Wu, X, Wu, X. F, Xiong, S. L, Xu, Y. P, Xue, Y. Q, Yan, Z, Yang, S, Yang, X, Yang, Y. J, Yuan, F, Yuan, W. M, Yuan, Y. F, Zampa, G, Zampa, N, Zdziarski, A, Zhang, C, Zhang, C. L, Zhang, L, Zhang, X, Zhang, Z, Zhang, W. D, Zheng, S. J, Zhou, P, and Zhou, X. L

Subjects
Astrophysics
Abstract

eXTP is a science mission designed to study the state of matter under extreme conditions of density, gravity and magnetism. Primary goals are the determination of the equation of state of matter at supra-nuclear density, the measurement of QED effects in highly magnetized star, and the study of accretion in the strong-field regime of gravity. Primary targets include isolated and binary neutron stars, strong magnetic field systems like magnetars, and stellar-mass and supermassive black holes. The mission carries a unique and unprecedented suite of state-of-the-art scientific instruments enabling for the first time ever the simultaneous spectral-timing-polarimetry studies of cosmic sources in the energy range from 0.5-30 keV (and beyond). Key elements of the payload are: the Spectroscopic Focusing Array (SFA) - a set of 11 X-ray optics for a total effective area of approx. 0.9 m(exp. 2) and 0.6 m(exp. 2) at 2 keV and 6 keV respectively, equipped with Silicon Drift Detectors offering less than 180 eV spectral resolution; the Large Area Detector (LAD) - a deployable set of 640 Silicon Drift Detectors, for a total effective area of approx. 3.4 m(exp. 2), between 6 and 10 keV, and spectral resolution better than 250 eV; the Polarimetry Focusing Array (PFA) - a set of 2 X-ray telescope, for a total effective area of 250 cm(exp. 2) at 2 keV, equipped with imaging gas pixel photoelectric polarimeters; the Wide Field Monitor (WFM) - a set of 3 coded mask wide field units, equipped with position-sensitive Silicon Drift Detectors, each covering a 90 degrees x 90 degrees field of view. The eXTP international consortium includes major institutions of the Chinese Academy of Sciences and Universities in China, as well as major institutions in several European countries and the United States. The predecessor of eXTP, the XTP mission concept, has been selected and funded as one of the so-called background missions in the Strategic Priority Space Science Program of the Chinese Academy of Sciences since 2011. The strong European participation has significantly enhanced the scientific capabilities of eXTP. The planned launch date of the mission is earlier than 2025.

Published
2016
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17. The LOFT Mission Concept - A Status Update

Author

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. R, Baldazzi, G, Baldo, M, Balman, S, Barbera, M, van Baren, C, Barret, D, Baykal, A, Begelman, M, Behar, E, Behar, O, Belloni, T, Belluti, P, Bernardini, F, Bertuccio, G, Bianchini, A, Binko, P, Blay, P, Bocchino, P, Bode, M, Bodin, P, Bombaci, I, Bonnet Bidaud, J. -M, Schnittman, Jeremy David, Borghi, G, Boutloukos, N, Bouyjou, F, Bradley, L, Braga, J, Briggs, M. S, Brown, E, Buballa, M, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jorgensen, C, Cackett, E, Cadoux, F. R, 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, Chateau, F, Chen, C, 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'Ai, A, D'Ammando, J. P. C, 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, Ficorella, F, Finger, M, Finger, M. H, Fraser, G. W, Frericks, N, Fullekrug, M, Fuschino, F, Gabler, M, Galloway, D. K, Galvez 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, Goluchova, K, Gotz, 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, A, 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, Jose, J, Kaaret, P, Kalamkar, M, 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, D, Mangano, V, Manousakis, A, Marelli, M, Margueron, J, Marisaldi, M, Markoff, S. B, Markowitz, A, Marinucci, A, Martindale, A, Martinez, 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, Mulacova, J, Muleri, F, Munoz-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, Paltini, 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, Petersen, B. M, Petracek, V, Picciotto, A, Piemonte, C, Pittori, C, Pons, J, Portell, J, Possenti, A, Postnov, K, Poutanen, J, Prakash, M, Prandoni, I, Provost, H. Le, Psaltis, D, Pye, J, Qu, J, Rambaud, D, Ramon, P, Ramsay, G, Rapisarda, M, Rachevski, A, Rashevskaya, I, Ray, P. S, Rea, N, Reddy, S, Reig, P, Reina, M. Aranda, Remillard, R, Reynolds, C, Rezzolla, L, Ribo, M, Rie, R. de la, 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, Xiao, L, 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, Zorzi, N, and Zwart, F

Subjects
Astrophysics
Abstract

The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, is greater than 8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission.

Published
2016
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18. Full orbital solution for the binary system in the northern Galactic disk microlensing event Gaia16aye

Author

Wyrzykowski, Ł., D’Ago, G., Hanlon, L., van Heerden, H., Ihanec, N., Jovanovic, M., Kopacki, G., Martin-Carrillo, A., Marais, J., Meintjes, P., Murphy, D., Van Soelen, B., Strubble, E., Szegedi, H., Vernet, D., Vince, O., van der Westhuizen, I., Wium, D., Zhuchkov, R. Ya., Wyrzykowski, Łukasz, Mróz, P., Rybicki, K., Gromadzki, M., Kołaczkowski, Z., Zieliński, M., Zieliński, P., Britavskiy, N., Gomboc, A., Sokolovsky, K., Hodgkin, S., Abe, L., Aldi, G., AlMannaei, A., Altavilla, G., Al Qasim, A., Anupama, G., Awiphan, S., Bachelet, E., Bakış, V., Baker, S., Bartlett, S., Bendjoya, P., Benson, K., Bikmaev, I., Birenbaum, G., Blagorodnova, N., Blanco-Cuaresma, S., Boeva, S., Bonanos, A., Bozza, V., Bramich, D., Bruni, I., Burenin, R., Burgaz, U., Butterley, T., Caines, H., Caton, D., Calchi Novati, S., Carrasco, J., Cassan, A., Čepas, V., Cropper, M., Chruślińska, M., Clementini, G., Clerici, A., Conti, D., Conti, M., Cross, S., Cusano, F., Damljanovic, G., Dapergolas, A., D'ago, G, de Bruijne, J., Dennefeld, M., Dhillon, V., Dominik, M., Dziedzic, J., Erece, O., Eselevich, M., Esenoglu, H., Eyer, L., Figuera Jaimes, R., Fossey, S., Galeev, A., Grebenev, S., Gupta, A., Gutaev, A., Hallakoun, N., Hamanowicz, A., Han, C., Handzlik, B., Haislip, J., Hardy, L., Harrison, D., Hoette, V., Horne, K., Hudec, R., Hundertmark, M., Ihanec 35, N, Irtuganov, E., Itoh, R., Iwanek, P., Janulis, R., Jelínek, M., Jensen, E., Kaczmarek, Z., Katz, D., Khamitov, I., Kilic, Y., Klencki, J., Kolb, U., Kouprianov, V., Kruszyńska, K., Kurowski, S., Latev, G., Lee, C.-H., Leonini, S., Leto, G., Lewis, F., Li, Z., Liakos, A., Littlefair, S., Lu, J., Manser, C., Mao, S., Maoz, D., Maskoliūnas, M., Maund, J., Melnikov, S., Ment, K., Mikołajczyk, P., Morrell, M., Mowlavi, N., Moździerski, D., Nazarov, S., Netzel, H., Nesci, R., Ngeow, C.-C., Norton, A., Ofek, E., Pakštienė, E., Palaversa, L., Pandey, A., Paraskeva, E., PAWLAK, M., Penny, M., Penprase, B., Piascik, A., Prieto, J., Qvam, J., Ranc, C., Rebassa-Mansergas, A., Reichart, D., Reig, P., Rhodes, L., Rivet, J.-P., Rixon, G., Roberts, D., Rosi, P., Russell, D., Zanmar Sanchez, R., Scarpetta, G., Seabroke, G., Shappee, B., Schmidt, R., Shvartzvald, Y., Sitek, M., Skowron, J., Śniegowska, M., Snodgrass, C., Soares, P., Spetsieri, Z., Stankevičiūtė, A., Steele, I., Street, R., Strobl, J., Tinjaca Ramirez, L., Tomasella, L., Tsapras, Y., Villanueva, S., 56, O, Wambsganss, J., Wiersema, K., Wilson, R., Yoldas, A., Ya, R, Zhukov, D., Zdanavičius, J., Zoła, S., Zubareva, A., Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Instytut Astronomiczny Uniwersytetu Wrocławskiego, Instituto de Astrofìsica de Canarias, National Science Centre (Poland), European Commission, Ministry of Science and Higher Education (Poland), Science and Technology Facilities Council (UK), Foundation for Polish Science, Slovenian Research Agency, University of Crete, Foundation for Research and Technology, National Research Foundation of Korea, University of Leicester, European Space Agency, National Science Foundation (US), Ministerio de Economía y Competitividad (España), Universidad de Barcelona, Agenzia Spaziale Italiana, Royal Society (UK), Ministry of Science and Technology (Taiwan), The Ohio State University, Chinese Academy of Sciences, Villum Fonden, Research Council of Lithuania, Kazan Federal University, National Aeronautics and Space Administration (US), Ministry of Education, Science and Technological Development (Serbia), W. M. Keck Foundation, Astronomical Observatory [Warsaw], Faculty of Physics [Warsaw] (FUW), University of Warsaw (UW)-University of Warsaw (UW), School of Physics, University College Dublin, Ireland, University of Pretoria [South Africa], Clinical Center of Serbia (KCS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, and Ege Üniversitesi

Subjects
Astronomy, Estels binaris, gravitational lensing: micro, techniques: photometric, binaries: general, stars: individual: Gaia16aye-L, Astrophysics, 01 natural sciences, 7. Clean energy, Gaia16aye-L, Gravitational lenses, Bulge, Fotometria astronòmica, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, QC, QB, Physics, Gravitational lensing micro, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomical photometry, 3rd-DAS, Orbital period, Radial velocity, Orbit, Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Stars: individual: Gaia16aye-L, astro-ph.SR, individual: Gaia16aye [Stars], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, Gravitational lensing: micro, micro [Gravitational lensing], Double stars, 0103 physical sciences, Binaries: general, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Orbital elements, general [Binaries], photometric [Techniques], Binaries, Astronomy and Astrophysics, Light curve, Stars, QC Physics, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Techniques - photometric, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Techniques: photometric, astro-ph.IM
Abstract

Gaia16aye was a binary microlensing event discovered in the direction towards the northern Galactic disc and was one of the first microlensing events detected and alerted to by the Gaia space mission. Its light curve exhibited five distinct brightening episodes, reaching up to I = 12 mag, and it was covered in great detail with almost 25 000 data points gathered by a network of telescopes. We present the photometric and spectroscopic follow-up covering 500 days of the event evolution. We employed a full Keplerian binary orbit microlensing model combined with the motion of Earth and Gaia around the Sun to reproduce the complex light curve. The photometric data allowed us to solve the microlensing event entirely and to derive the complete and unique set of orbital parameters of the binary lensing system. We also report on the detection of the first-ever microlensing space-parallax between the Earth and Gaia located at L2. The properties of the binary system were derived from microlensing parameters, and we found that the system is composed of two main-sequence stars with masses 0.57 +/- 0.05 M-circle dot and 0.36 +/- 0.03 M-circle dot at 780 pc, with an orbital period of 2.88 years and an eccentricity of 0.30. We also predict the astrometric microlensing signal for this binary lens as it will be seen by Gaia as well as the radial velocity curve for the binary system. Events such as Gaia16aye indicate the potential for the microlensing method of probing the mass function of dark objects, including black holes, in directions other than that of the Galactic bulge. This case also emphasises the importance of long-term time-domain coordinated observations that can be made with a network of heterogeneous telescopes., Polish National Sci-ence Centre (NCN): HARMONIA NCN grant [2015/18/M/ST9/00544]; Polish National Sci-ence Centre (NCN): OPUS NCN grant [2015/17/B/ST9/03167]; Polish National Sci-ence Centre (NCN): DAINA NCN grant [2017/27/L/ST9/03221]; European CommissionEuropean CommissionEuropean Commission Joint Research Centre [312430, 730890]; Polish Ministry of Higher EducationMinistry of Science and Higher Education, Poland [3040/7.PR/2014/2, DIR/WK/2018/12]; MAESTRO NCN grant [2014/14/A/ST9/00121]; DDT programmes [SW2016b12, A34DDT3]; UK Science and Technology Facilities CouncilUK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC); Foundation for Polish Science (Program START); National Science Center, PolandNational Science Centre, Poland [ETIUDA 2018/28/T/ST9/00096]; Slovenian Research AgencySlovenian Research Agency - Slovenia [P1-0031, J1-8136]; COST Action GWverseEuropean Cooperation in Science and Technology (COST) [CA16104]; National Research Foundation of KoreaNational Research Foundation of Korea [2017R1A4A1015178]; STFCUK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC); European Space Agency under the NELIOTA program [4000112943]; GROWTH project - National Science Foundation [1545949]; MINECO (Spanish Ministry of Economy) [ESP2016-80079-C2-1-R, ESP2014-55996-C2-1-R, RTI2018-095076B-C21]; ICCUB (Unidad de Excelencia a Maria de Maeztu) [MDM-2014-0369]; Agenzia Spaziale Italiana (ASI)Agenzia Spaziale Italiana (ASI) [ASI I/058/10/0, ASI 2014-025-R.1.2015]; Royal Society Research GrantRoyal Society of London [RG170230]; Ministry of Science and Technology (Taiwan)Ministry of Science and Technology, Taiwan [104-2112-M-008-012MY3, 104-2923-M-008-004-MY5]; European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant [320964]; Gordon and Betty Moore FoundationGordon and Betty Moore Foundation [GBMF5490]; NSFNational Science Foundation (NSF) [AST-1515927, AST-0908816, AST-1412587]; Mt. Cuba Astronomical Foundation; Center for Cosmology and AstroParticle Physics at the Ohio State UniversityOhio State University; Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA); Villum Foundation; MINECO under the Ramon y Cajal programme [RYC-2016-20254]; MINECO [AYA2017-86274-P]; AGAUR grantAgencia de Gestio D'Ajuts Universitaris de Recerca Agaur (AGAUR) [SGR-661/2017]; Science and Technology Facilities CouncilUK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC) [ST/P000541/1]; STFC consolidated grant [ST/M001296/1]; Research Council of LithuaniaResearch Council of Lithuania (LMTLT) [S-LL-19-2]; TUB.ITAKTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK); IKI; KFU; AST; National Science Fund (Bulgaria)National Science Fund of Bulgaria [DN 18/13-12.12.2017]; Institute of Astronomy via research project "Study of ICRF radio-sources and fast variable astronomical objects"; NAO Rozhen, BAS, via research project "Study of ICRF radio-sources and fast variable astronomical objects"; Ministry of Education, Science and Technological Development of the Republic of Serbia [176011, 176004, 176021]; DFGGerman Research Foundation (DFG)European Commission [SPP 1992, WA 1074/11-1]; NCN [2016/21/B/ST9/01126]; MINECO Ramon y Cajal programme [AYA2017-86274-P, RYJ-2016-20254]; Robert Martin Ayers Sciences Fund; National Aeronautics and Space AdministrationNational Aeronautics & Space Administration (NASA) [NNX08AR22G]; National Science FoundationNational Science Foundation (NSF) [AST-1238877]; W. M. Keck FoundationW.M. Keck Foundation; ICCUB (Unidad de Excelencia 'Maria de Maeztu') [MDM-2014-0369]; [3.6714.2017/8.9], This work relies on the results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia Multi-Lateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia.In particular we acknowledge Gaia Photomet-ric Science Alerts Team, website http://gsaweb.ast.cam.ac.uk/alerts.We thank the members of the OGLE team for discussions and support. We also would like to thank the Polish Children Fund (KFnRD) for support of an internship of their pupils in Ostrowik Observatory of the Warsaw Univ-ersity, during which some of the data were collected, in particular we thank: Robert Nowicki, Michal Por.ebski and Karol Niczyj. The work presented here has been supported by the following grants from the Polish National Sci-ence Centre (NCN): HARMONIA NCN grant 2015/18/M/ST9/00544, OPUS NCN grant 2015/17/B/ST9/03167, DAINA NCN grant 2017/27/L/ST9/03221, as well as European Commission's FP7 and H2020 OPTICON grants (312430 and 730890), Polish Ministry of Higher Education support for OPTICON FP7, 3040/7.PR/2014/2, MNiSW grant DIR/WK/2018/12. PMr and JS acknowledge support from MAESTRO NCN grant 2014/14/A/ST9/00121 to Andrzej Udal-ski. We would like to thank the following members of the AAVSO for their amazing work with collecting vast amounts of data: Teofilo Arranz, James Boardman, Stephen Brincat, Geoff Chaplin, Emery Erdelyi, Rafael Farfan, William Goff, Franklin Guenther, Kevin Hills, Jens Jacobsen, Raymond Kneip, David Lane, Fernando Limon Martinez, Gianpiero Locatelli, Andrea Mantero, Attila Madai, Peter Meadows, Otmar Nickel, Arto Oksanen, Luis Perez, Roger Pieri, Ulisse Quadri, Diego Rodriguez Perez, Frank Schorr, George Sjoberg, Andras Timar, Ray Tomlin, Tonny Vanmunster, Klaus Wenzel, Thomas Wikander. We also thank the amateur observers from around the world, in particular, Pietro Capuozzo, Leone Trascianelli, Igor Zharkov from Ardingly College and Angelo Tomassini, Karl-Ludwig Bath. We also thank Roger Pickard from the British Astronomical Association and Matthias Penselin from the German Haus der Astronomie association for their contributions. KS thanks Dr. Dmitry Chulkov and Dr. Panagiotis Gavras for the interesting discussion of stellar multiplicity. We acknowledge support of DDT programmes SW2016b12 (WHT) and A34DDT3 (TNG). The INT, TNG and WHT are operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. SJF would like to thank the UCL students who assisted with the collection and checking of UCLO data for the observing campaign: Martina Aghopian, Ashleigh Arendt, Artem Barinov, Luke Barrett, Jasper Berry-Gair, Arjun Bhogal, Charles Bowesman, William Boyd, Andrei Cuceu, Michael Davies, Max Freedman, Gabriel Fu, Abirami Govindaraju, Iandeep Hothi, Clara Matthews Torres, Darius Modirrousta-Galian, Petru Neague, George Pattinson, Xiaoxi Song, and Brian Yu. P.Mr. acknowledges support from the Foundation for Polish Science (Program START) and the National Science Center, Poland (grant ETIUDA 2018/28/T/ST9/00096).; r r AC, AG and NI acknowledge the financial support from the Slovenian Research Agency (research core funding No. P1-0031 and project grant No. J1-8136)and networking support by the COST Action GWverse CA16104. Skinakas Observatory is a collaborative project of the University of Crete and the Foundation for Research and Technology-Hellas. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. KW acknowledges funding from STFC, and thanks the University of Lei-cester for the investment in instrumentation. We gratefully acknowledge financial support by the European Space Agency under the NELIOTA program, contract No. 4000112943. This work has made use of data obtained with the Kryoneri Prime Focus Instrument, developed by the European Space Agency NELIOTA project on the 1.2 m Kryoneri telescope, which is operated by IAASARS, National Observatory of Athens, Greece. The Aristarchos tele-scope is operated on Helmos Observatory by the IAASARS of the National Observatory of Athens. This work was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. This work was supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R (MINECO/FEDER, UE) and ESP2014-55996-C2-1-R (MINECO/FEDER, UE) and MDM-2014-0369 of ICCUB (Unidad de Excelencia a Maria de Maeztu). This work was supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R and RTI2018-095076B-C21 (MINECO/FEDER, UE), and MDM-2014-0369 of ICCUB (Unidad de Excelencia 'Maria de Maeztu'). The Joan Oro Telescope (TJO) of the Montsec Astronomical Observatory (OAdM) is owned by the Catalan Government and is operated by the Institute for Space Studies of Catalonia (IEEC). Support to this study has been provided by Agenzia Spaziale Italiana (ASI) through grants ASI I/058/10/0 and ASI 2014-025-R.1.2015. KW thanks Dipali Thanki and Ray McErlean for their technical support of the scientific programme of the University of Leicester observatory. This work was supported by Royal Society Research Grant RG170230. CCN thanks the funding from Ministry of Science and Technology (Taiwan) under the contracts 104-2112-M-008-012MY3 and 104-2923-M-008-004-MY5. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 320964 (WDTracer). We thank the Las Cumbres Observatory and its sta ff for its continuing support of the project. ASAS-SN is supported by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University and NSF grant AST-1515927. Development of ASAS-SN has been supported by NSF grant AST-0908816, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA), the Villum Foundation, and George Skestos. ARM acknowledges support from the MINECO under the Ramon y Cajal programme (RYC-2016-20254) and the AYA2017-86274-P grant, and the AGAUR grant SGR-661/2017. We acknowledge support from the Science and Technology Facilities Council (TB and RWW; ST/P000541/1). K.Horne acknowledges support from STFC consolidated grant ST/M001296/1. This work was partly supported by the Research Council of Lithuania, grant No. S-LL-19-2 Authors thank to TUB.ITAK, IKI, KFU, and AST for partial supports in using RTT150 (Russian-Turkish 1.5-m telescope in Antalya).; r r This work was partially funded by the subsidy 3.6714.2017/8.9 allocated to Kazan Federal University for the state assignment in the sphere of scientific activities. This research was partially supported by contract DN 18/13-12.12.2017 with the National Science Fund (Bulgaria). Work by YS was supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, California Institute of Technology, administered by Uni-versities Space Research Associ-ation through a contract with NASA. GD gratefully acknowledges the obser-ving grant support from the Institute of Astronomy and NAO Rozhen, BAS, via bilateral joint research project "Study of ICRF radio-sources and fast variable astronomical objects" (PI:G.Damljanovic). This work is a part of the Projects no. 176011 "Dynamics and kinematics of celestial bodies and systems", no. 176004 "Stellar physics" and no. 176021 "Visible and invisible matter in nearby galaxies: theory and observations" supported by the Ministry of Education, Science and Technological Development of the Republic of Serbia. YT acknowledges the support of DFG priority program SPP 1992 "Exploring the diversity of Extrasolar Planets" (WA 1074/11-1). This work of PMi, DM and ZK was supported by the NCN grant no. 2016/21/B/ST9/01126. ARM acknowledges support from the MINECO Ramon y Cajal programme RYJ-2016-20254 and grant AYA2017-86274-P and from the AGAUR grant SGR-661/2017. The work by C. R. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA. The Faulkes Telescope Project is an education partner of Las Cumbres Observatory (LCO). The Faulkes Telescopes are maintained and operated by LCO. This research was made possible through the use of the AAVSO Photomet-ric All-Sky Survey (APASS), funded by the Robert Martin Ayers Sciences Fund and NSF AST-1412587. The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project O ffice, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incor-porated, the National Central University of Taiwan, the Space Telescope Sci-ence Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Ins-titute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.

Published
2020

19. Astrophysics with digitized astronomical plate archives.

Author

Hudec, R.

Subjects
*ASTRONOMICAL photography, *DIGITAL cameras, *DIGITIZATION, *ASTROPHYSICS, *ASTRONOMICAL photometry
Abstract

We discuss the recent status of astrophysical analyses with digitized astronomical plate archives with emphasis on high‐energy and transient astrophysics. These data represent huge scientific, historical, and cultural value, but only the recent digitization has enabled their effective use in astrophysics. [ABSTRACT FROM AUTHOR]

Published
2018
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20. Digitization and astrophysical use of Hewitt Camera Archive.

Author

Hudec, R., Hudec, L., and Howarth, J.

Subjects
*DIGITIZATION, *ASTROPHYSICS, *ASTRONOMICAL photometry, *ARTIFICIAL satellite tracking, *TELESCOPES
Abstract

We briefly present the status of digitization and astrophysical use of the Hewitt Camera Archive, UK. These wide‐field images, so far little used for astrophysical work, cover both northern as well as southern sky down to limiting mag 13. We also discuss the potential of photographic images taken by satellite tracking cameras for recent astrophysics in general. [ABSTRACT FROM AUTHOR]

Published
2018
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21. Low‐dispersion spectroscopy with cubesats and photographic plates.

Author

Hudec, R.

Subjects
*CUBESATS (Artificial satellites), *PHOTOGRAPHIC plates, *X-ray telescopes, *MINIATURE electronic equipment, *ASTROPHYSICS
Abstract

We will briefly present the proposal for the UV experiment based on low‐dispersion spectroscopy (LDS) of stars for cubesat mission, as well as the potential of LDS with digitized photographic plates taken mostly by Schmidt telescopes. Extended databases of these records are available at numerous observatories, mainly in the United States, with the total estimated number exceeding 100,000. They represent a valuable source of astrophysical information, especially for automated searches for objects with peculiar spectra as well as for (prominent) spectral changes. [ABSTRACT FROM AUTHOR]

Published
2018
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22. INTEGRAL observations 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., Malaguri, G., Maraschi, L., Palumbo, G. G. C., Treves, A., J-L Courvoisier, T., Di Cocco, G., Gehrels, N., Giommi, P., Hudec, R., Lindfors, E., Marcowith, A., Nilsson, K., Pasanen, M., Pursimo, T., Raiteri, C. M., Tuomas Savolainen, Sikor, M., Tornikoski, M., Tosti, G., Türler, M., Valtaoja, E., Villata, M., Walter, R., E.Pian, L.Foschini, V. Beckmann, A. Sillanpaa, S. Soldi, G. Tagliaferro, L. Takalo, P. Barr, G. Ghibellini, G. Malaguti, L. Maraschi, G.G.C. Palumbo, A. Treve, T.J.-L. Courvoisier, G. Di Cocco, N. Gehrel, P. Giommi, R. Hudec, E. Lindfor, A. Marcowith, K. Nilsson, M. Pasanen, T. Pursimo, C.M. Raiteri, T. Savolainen, M. Sikora, M. Tornikoski, G. Tosti, M. Turler, E. Valaoja, M. Villata, and R. Walter.

Subjects
Physics, Brightness, Active galactic nucleus, Astrophysics (astro-ph), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Quasar, Astrophysics, Galaxy, Spectral line, Space and Planetary Science, Blazar, BL Lac object
Abstract

We have performed observations of the blazar S5 0716+714 with INTEGRAL on 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, occurred in March, it reached the extreme level of R = 12.1 mag, which triggered our INTEGRAL program. The target has been detected with IBIS/ISGRI up to 60 keV, with a flux of ~3 x 10e-11 erg/s/cm2 in the 30-60 keV interval, a factor of ~2 higher than observed by the BeppoSAX PDS 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 INTEGRAL spectra of weak Active Galactic Nuclei., 5 pages, 5 figures, in press in A&A

Published
2005

23. The Possibility of GRB Investigations by ESA Satellite Gaia.

Author

Hudec, R. and Hudec, L.

Subjects
*GAMMA ray bursts, *ARTIFICIAL satellites, *AFTERGLOW (Physics), *ELECTRIC transients, *ASTROMETRY, *PHOTOMETRY, *ASTROPHYSICS
Abstract

We refer on further studies on possibility to investigate the Optical Afterglows and Optical Transients of GRBs by the ESA satellite Gaia to be launched in 2012, The satellite will focus on highly precise astrometry of stars and all objects down to limiting magnitude 20. Albeit focusing on astrometry related matters, the satellite will also provide photometric and spectral information and hence important inputs for various branches of astrophysics. Within the Gaia Variability Unit CU7 and related work package Specific Object Studies there has been a sub-work package accepted for optical counterparts to celestial high-energy sources, a category which includes the optical counterparts (i.e. optical transients and optical afterglows, including counterparts of XRFs and yet hypothetical orphan afterglows) of GRBs. Although the sampling of photometric data will not be optimal for this type of work, the strength of Gaia in such analyses is the fine spectral resolution (spectro-photometry) which will allow the correct classification of related triggers. The possibilities to detect and to analyze optical transients and optical afterglows of GRBs by Gaia will be presented and discussed. [ABSTRACT FROM AUTHOR]

Published
2011
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24. GRB Astrophysics with LOBSTER.

Author

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

Subjects
*GAMMA ray bursts, *ASTROPHYSICS, *GAMMA ray detectors, *ELECTROMAGNETIC waves, *ASTRONOMY, *PHYSICS
Abstract

We refer on the recent developments of LOBSTER project suggesting novel wide-field Lobster-Eye type of X-ray All Sky Monitor to detect and to analyze GRBs including XRF and X-ray rich GRBs. The triggers can be detected and localized by their X-ray emission in the 0.1 – 8 keV energy range. The system exhibits fine detecting sensitivities of order of 10–12 ergcm-2s-1 and the localization accuracy is of order of a few arcmin. The LOBSTER is expected to contribute significantly to analyses of GRBs and especially the XRFs. © 2006 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2006
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25. GRB Optical Prompt Emission: The Role of Monitors.

Author

Hudec, R.

Subjects
*GAMMA ray bursts, *OPTICS, *SPECTRUM analysis, *ASTROPHYSICS, *ASTRONOMY
Abstract

The prompt optical emission of Gamma Ray Bursts was detected only in one case so far. We discuss the possibility to detect this type of optical emission, which is still difficult to record by follow-up experiments, by wide-field optical monitors. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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26. The KLENOT Telescope and GRBs.

Author

Tichý, M., Tichá, J., Kočer, M., Hudec, R., and Šimon, V.

Subjects
GAMMA ray bursts, X-ray bursts, GAMMA ray astronomy, ASTROPHYSICS, ASTRONOMY, PHYSICS, PHYSICS instruments, TELESCOPES
Abstract

The new 1.06-m KLENOT telescope equipped with a CCD camera is now in routine operation at the Klet’ Observatory, with the primary goal to investigate the near-earth objects (NEOs) and other unusual objects. We describe this new telescope and the related systems and discuss the use of the telescope in GRB optical follow-up observations. The KLENOT Project website is http://klenot.klet.org. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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27. Digitized astronomical plates: Optical data for X-ray astronomy.

Author

Hudec, R.

Subjects
*X-ray astronomy, *ASTROPHYSICS
Abstract

The worlds astronomical plate archives count nearly 3 million plates, some of them of very high quality with limiting magnitudes up to 22-23. The recent digitization of astronomical plates enables their wide use as data source in many areas of astronomy and astrophysics. I review the worlds major plate collections and discuss their impact on various regions of X-ray astronomy and astrophysics including long-term studies and monitoring of flaxes and active states of both galactic and extragalactic X-ray sources. [ABSTRACT FROM AUTHOR]

Published
2001

28. The Role of Ground-Based Robotic Observatories in Satellite Projects.

Author

Hudec, R.

Subjects
*OBSERVATORIES, *SPACE telescopes, *ARTIFICIAL satellites, *ASTROPHYSICS, *PHOTOMETRY, *PARTICLES (Nuclear physics), *ROBOTICS, *MULTISPECTRAL imaging, *WAVELENGTHS
Abstract

We discuss the role of robotic telescopes in satellite projects, as well as related strategies. Most satellite projects in space astrophysics focus on high-energy astrophysics from X-rays to gamma-rays. A large fraction of objects of high-energy astrophysics emit also optical light, which is, in many cases, variable. The observation of these sources at optical wavelengths can provide valuable inputs for multispectral analysis of various categories of celestial high-energy (HE) sources. As the magnitudes of numerous objects are bright and can be hence accessed by robotic ground-based observatories, these observations can contribute to investigations and analyses of HE sources. We discuss in detail this possible contribution, with emphasis on the ESA INTEGRAL mission. In addition to this, there are also satellite projects outside the high-energy astronomy, in which the robotic telescopes can also play an important role. We will illustrate this on the example of the ESA satellite Gaia. In this project, robotic telescopes are expected not only to verify the triggers detected by satellite (such as transients and flares) but also to provide additional (mostly photometric) data for better scientific cases. [ABSTRACT FROM AUTHOR]

Published
2010
Full Text
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29. The GRB Investigations by ESA Satellite Gaia.

Author

Hudec, R., Šimon, V., and Hudec, L.

Subjects
*ARTIFICIAL satellites, *ASTROMETRY, *PHOTOMETRY, *ASTROPHYSICS, *AFTERGLOW (Physics)
Abstract

The ESA satellite in development Gaia to be launched in 2011 will focus on highly precise astrometry of stars and all objects down to limiting magnitude 20. Albeit focusing on astrometry related matters, the satellite will also provide photometric and spectral information and hence important inputs for various branches of astrophysics. Within the Gaia Variability UnitCU7 and related work package Specific Object Studies there has been a sub-work package accepted for optical counterparts to celestial high-energy sources, a category which includes the optical counterparts (i.e. optical transients and optical afterglows, including counterparts of XRFs and yet hypothetical orphan afterglows) of GRBs, and also microquasars. Although the sampling of photometric data will not be optimal for this type of work, the strength of Gaia in such analyses is the fine spectral resolution (spectro-photometry) which will allow the correct classification of related triggers. The possibilities to detect and to analyze optical transients and optical afterglows of GRBs and microquasars by Gaia will be presented and discussed. [ABSTRACT FROM AUTHOR]

Published
2009
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30. OPTICAL TRANSIENTS.

Author

Hudec, R. and Wenzel, W.

Subjects
*GAMMA ray bursts, *ASTROPHYSICS
Abstract

ABSTRACT The recent detections of optical afterglows of gamma ray burst detected by the BeppoSAX satellite confirm the existence of optical transients related to GRB phenomenon. We discus the category of optical transients (OTs) in more detail including archival OTs found before SAX as well as statistical issues and conlude that random GRB/OTs coincidences cannot be excluded at present. [ABSTRACT FROM AUTHOR]

Published
1999

31. Secondary Science with ROTSE Data.

Author

Štrobl, J., Hudec, R., Jelínek, M., Šimon, V., Hroch, F., and Akerlof, C.

Subjects
*GAMMA ray bursts, *ASTRONOMY, *ASTROPHYSICS
Abstract

The ROTSE optical GRB follow-up instrument offers an excellent possibility for a secondary science with the data obtained within the sky monitoring. We present and discuss the results of a project of analysing two selected ROTSE monitoring fields with the goal to study the long-term behaviour of the objects located inside. The method developed and tested can be applied in a general way to study light changes of astrophysical objects of various types within the limiting magnitude of the ROTSE device. [ABSTRACT FROM AUTHOR]

Published
2003

32. Recent Developments in the BOOTES Experiment.

Author

de Ugarte Postigo, A., Mateo Sanguino, T. J., Castro Cerón, J. M., Páta, P., Bernas, M., Jelinek, M., Hudec, R., McBreen, S., Berná, J. Á., García Dabó, C. E., Gorosabel, J., Más-Hesse, J. M., Soria, T., de la Morena, B. A., Torres Riera, J., and Castro-Tirado, A. J.

Subjects
GAMMA ray bursts, GAMMA ray astronomy, ASTROPHYSICS
Abstract

BOOTES, the Burst Observer and Optical Transient Exploring System, is mostly a Spanish-Czech international collaboration that works to fill the space that there actually exists in the rapid variability Astronomy. It is specially aimed towards the detection and study of the optical transients that are generated in conjunction with the elusive GRBs (Gamma Ray Bursts). Since 1998 BOOTES has provided follow ups for more than 60 of these phenomena with the first of its observatories; the most important results obtained so far are the detection of an OT (Optical Transient) in the GRB 000313 error box and the non detection of optical emission simultaneous to the GRB 010220 event. With the recent inauguration of a second observatory BOOTES multiplies its science capabilities. [ABSTRACT FROM AUTHOR]

Published
2003

33. 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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34. Preface.

Author

Hudec, R., Urban, M., and Nentvich, O.

Subjects
*ASTROPHYSICS, *WORKSHOPS (Facilities), *SPACE exploration, *IMAGE processing
Abstract

The fifteenth of a series of successful workshops on high‐energy astrophysics and related ground experiments was held in Karlovy Vary from April 16 to 20, 2018. The INTEGRAL/BART Workshop (IBWS) was a working meeting of experts (with strong participation of young research fellows and students) in the field of space exploration with the help of satellites observing in the γ‐ and X‐ray regions and the related ground‐based experiments using, e.g., robotic telescopes. [ABSTRACT FROM AUTHOR]

Published
2018
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35. The Sky Behind Our Galaxy as Seen by IBIS on INTEGRAL

Author

Bassani, L., Malizia, A., Stephen, J. B., Gianotti, F., Schiavone, F., Bazzano, A., Bird, A. J., Bouchet, L., Courvoisier, T., Dean, A. J., Giovanni De Cesare, Del Santo, M., Rosa, A., Hudec, R., Mirabel, F., Laurent, P., Piro, L., Shaw, S., and Zdziarski, A. A.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

During the Core Programme, INTEGRAL has surveyed a large portion of the sky (around 9000 square degrees); although INTEGRAL is not optimized for extra-galactic studies its observations have nevertheless given us the opportunity to explore the sky behind our Galaxy, something which is impossible in some wavebands due to the presence of strong absorption. Preliminary results from this exploration are presented and compared with the pre-launch expectations. In particular, we detail all extragalactic detections obtained so far: 10 active galaxies and one cluster of galaxies. Of these sources, many have previously been studied at energies above 10-20 keV while a few are new hard X-ray discoveries. Since the number of detections is smaller than estimated on the basis of the IBIS/ISGRI sensitivity, it is likely that some of the new ISGRI sources found in this survey are extragalactic objects; a few of these are likely to be AGN and are described in detail., Comment: 7 pages, 10 figures. Proceedings of the V INTEGRAL Workshop, Munich 16-20 February 2004. ESA SP-552

36. Colors of the Optical Afterglow of GRB030329/SN 2003dh.

Author

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

Subjects
*AFTERGLOW (Physics), *ELECTRIC discharges, *SUPERNOVAE, *SPECTRUM analysis, *ASTRONOMY, *ASTROPHYSICS
Abstract

We show that the color indices (B - V)0, (V - R)0, (R - I)0 of the optical afterglow of GRB030329 were consistent with those of the other OAs during t - T0 < 10 days. This suggests that the synchrotron component was initially dominant in the spectrum. Large color variations emerge only for t - T0 > 20 days and suggest a rapid spectral evolution of the underlying supernova SN 2003dh. © 2004 American Institute of Physics [ABSTRACT FROM AUTHOR]

Published
2004
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37. THESEUS: A key space mission concept for Multi-Messenger Astrophysics

Author

F. Fuschino, Ruben Salvaterra, F. Frontera, M. Branchesi, Bruce Gendre, U. Maio, Stefano Covino, Tomaz Rodic, Giancarlo Ghirlanda, Serena Vinciguerra, D. Mereghetti, Andrea Rossi, Lorenzo Amati, Diego Götz, M. H. P. M. van Putten, Monica Colpi, Roberto Mignani, P. D'Avanzo, Riccardo Campana, Eliana Palazzi, Andrea Bulgarelli, M. G. Bernardini, Valerio D'Elia, Jochen Greiner, Elisabetta Maiorano, Enzo Brocato, Joseph Caruana, Piero Rosati, R. L. C. Starling, Nial Tanvir, Riccardo Ciolfi, G. Stratta, S. D. Vergani, S. Colafrancesco, Claudio Labanti, Bing Zhang, Dorottya Szécsi, M. Razzano, Enrico Bozzo, Antonio Stamerra, D. Malesani, René Hudec, Francesco Longo, Luciano Rezzolla, S. Piranomonte, M. de Pasquale, Richard Willingale, B. Patricelli, J. P. Osborne, P. T. O'Brien, Peter G. Jonker, Luciano Nicastro, C. Guidorzi, Aniello Grado, M. Boer, Alessandro Drago, Maria Giovanna Dainotti, Carole Mundell, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Brera (OAB), University of Ferrara [Ferrara], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Physics and Astronomy [Leicester], University of Leicester, Max-Planck-Institut für Extraterrestrische Physik (MPE), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), INAF - Osservatorio Astronomico di Roma (OAR), INAF-IASF Milano, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), ASI-Science Data Center, Rome, Laboratori Nazionali di Frascati (LNF), National Institute for Nuclear Physics (INFN), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), CNR Institute of Atmospheric Sciences and Climate (ISAC), Consiglio Nazionale delle Ricerche (CNR), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Università degli Studi di Ferrara = University of Ferrara (UniFE), Istituto Nazionale di Fisica Nucleare (INFN), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Radboud University [Nijmegen]-Radboud University [Nijmegen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), THESEUS, Stratta, G., Ciolfi, R., Amati, L., Bozzo, E., Ghirlanda, G., Maiorano, E., Nicastro, L., Rossi, A., Vinciguerra, S., Frontera, F., Götz, D., Guidorzi, C., O'Brien, P., Osborne, J. P., Tanvir, N., Branchesi, M., Brocato, E., Dainotti, M. G., De Pasquale, M., Grado, A., Greiner, J., Longo, F., Maio, U., Mereghetti, D., Mignani, R., Piranomonte, S., Rezzolla, L., Salvaterra, R., Starling, R., Willingale, R., Böer, M., Bulgarelli, A., Caruana, J., Colafrancesco, S., Colpi, M., Covino, S., D'Avanzo, P., D'Elia, V., Drago, A., Fuschino, F., Gendre, B., Hudec, R., Jonker, P., Labanti, C., Malesani, D., Mundell, C. G., Palazzi, E., Patricelli, B., Razzano, M., Campana, R., Rosati, P., Rodic, T., Szécsi, D., Stamerra, A., van Putten, M., Vergani, S., Zhang, B., Bernardini, M., Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Ferrara (UniFE), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Stratta, G, Ciolfi, R, Amati, L, Bozzo, E, Ghirlanda, G, Maiorano, E, Nicastro, L, Rossi, A, Vinciguerra, S, Frontera, F, Götz, D, Guidorzi, C, O'Brien, P, Osborne, J, Tanvir, N, Branchesi, M, Brocato, E, Dainotti, M, De Pasquale, M, Grado, A, Greiner, J, Longo, F, Maio, U, Mereghetti, D, Mignani, R, Piranomonte, S, Rezzolla, L, Salvaterra, R, Starling, R, Willingale, R, Böer, M, Bulgarelli, A, Caruana, J, Colafrancesco, S, Colpi, M, Covino, S, D'Avanzo, P, D'Elia, V, Drago, A, Fuschino, F, Gendre, B, Hudec, R, Jonker, P, Labanti, C, Malesani, D, Mundell, C, Palazzi, E, Patricelli, B, Razzano, M, Campana, R, Rosati, P, Rodic, T, Szécsi, D, Stamerra, A, van Putten, M, Vergani, S, Zhang, B, and Bernardini, M

Subjects
Atmospheric Science, Computer science, Astronomy, Astronomical and space-research instrumentation, Gamma-ray bursts, Gamma-ray sources, X-ray bursts, X-ray sources, Aerospace Engineering, Space and Planetary Science, Astrophysics, 01 natural sciences, Economica, astronomical and space-research instrumentation, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], energy: high, gamma-ray bursts, Gamma-ray source, neutrino: detector, Geophysics, Upgrade, Neutrino detector, upgrade, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Cosmic Vision, media_common.quotation_subject, FOS: Physical sciences, Context (language use), frequency: high, X-ray source, 0103 physical sciences, gravitational radiation: frequency, Gamma-ray burst, X-ray burst, gamma-ray sources, 010308 nuclear & particles physics, Gravitational wave, family: 3, Astronomy and Astrophysics, gravitational radiation detector, Universe, messenger, electromagnetic, General Earth and Planetary Sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The recent discovery of the electromagnetic counterpart of the gravitational wave source GW170817, has demonstrated the huge informative power of multi-messenger observations. During the next decade the nascent field of multi-messenger astronomy will mature significantly. Around 2030, third generation gravitational wave detectors will be roughly ten times more sensitive than the current ones. At the same time, neutrino detectors currently upgrading to multi km^3 telescopes, will include a 10 km^3 facility in the Southern hemisphere that is expected to be operational around 2030. In this review, we describe the most promising high frequency gravitational wave and neutrino sources that will be detected in the next two decades. In this context, we show the important role of the Transient High Energy Sky and Early Universe Surveyor (THESEUS), a mission concept proposed to ESA by a large international collaboration in response to the call for the Cosmic Vision Programme M5 missions. THESEUS aims at providing a substantial advancement in early Universe science as well as playing a fundamental role in multi-messenger and time-domain astrophysics, operating in strong synergy with future gravitational wave and neutrino detectors as well as major ground- and space-based telescopes. This review is an extension of the THESEUS white paper (Amati et al. 2017), also in light of the discovery of GW170817/GRB170817A that was announced on October 16th, 2017., Comment: 25 pages, 13 figures, accepted to Advances in Space Research with minor revisions. Details on the THESEUS instrumentation, science case and expected performances can also be found in Amati et al. 2017 (arXiv:1710.04638) and in the presentations of the THESEUS Workshop 2017 (http://www.isdc.unige.ch/theseus/workshop2017-programme.html). v2 few typos corrected

Published
2018

38. The THESEUS space mission concept: science case, design and expected performances.

Author

Amati, L., O’Brien, P., Götz, D., Bozzo, E., Tenzer, C., Frontera, F., Ghirlanda, G., Labanti, C., Osborne, J.P., Stratta, G., Tanvir, N., Willingale, R., Attina, P., Campana, R., Castro-Tirado, A.J., Contini, C., Fuschino, F., Gomboc, A., Hudec, R., and Orleanski, P.

Subjects
*GAMMA ray bursts, *ASTROPHYSICS, *SPECTROSCOPIC imaging, *LUMINOSITY, *WAVELENGTHS
Abstract

THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1sr) with 0.5–1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift ∼ 10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late ’20s/early ’30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA). [ABSTRACT FROM AUTHOR]

Published
2018
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39. LOFT: the Large Observatory For X-ray Timing

Author

M. Feroci, JW den Herder, JW 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. Alpar, A. Altamirano, D. Alvarez, L. Amati, L. Amoros, C. Andersson, N. Antonelli, A. Argan, A. Artigue R, Azzarello P, Balman, S. Barbera, M. Belloni, T. Bertuccio, G. Bianchi, S. Bianchini, A. Bodin, P. Bidaud, JMB Boutloukos, S. Braga, J. Brown, E. Bucciantini, N. Burderi, L. Bursa, M. Budtz Jorgensen, C. Cackett, E. Cadoux, FR Cais, P. Caliandro, GA Campana, R. Campana, S. Casella, P. Chakrabarty, D. Chenevez, J. Coker, J. Cole, R. Collura, A. Courvoisier, T. Cros, A. Cumming, A. Cusumano, G. D'Ai, A. D'Elia, V. Del Monte, E. De Martino, D. De Rosa, A. Di Cosimo, S. Diebold, S. Di Salvo, T. Donnarumma, I. Drago, A. Durant, M. Emmanoulopoulos, D. Evangelista, Y. Fabian, A. Falanga, M. Favre, Y. Feldman, C. Ferrigno, C. Finger, MH Fraser, GW Fuschino, F. Galloway, DK Sanchez, JLG Garcia Berro, E. Gendre, B. Gezari, S. Giles, AB Gilfanov, M. Giommi, P. Giovannini, G. Giroletti, M. Goldwurm, A. Gotz, D. Gouiffes, C. Grassi, M. Groot, P. Guidorzi, C. Haas, D. Hansen, F. Hartmann, DH Haswell, CA Heger, A. Homan, J. Hornstrup, A. Hudec, R. Huovelin, J. Ingram, A. in't Zand, JJM Isern, J. Israel, G. Izzo, L. Jonker, P. Kaaret, P. Karas, V. Karelin, D. Kataria, D. Keek, L. Kennedy, T. Klochkov, D. Kluzniak, W. Kokkotas, K. Korpela, S. Kouveliotou, C. Kreykenbohm, I. Kuiper, LM Kuvvetli, I. Labanti, C. Lai, D. Lamb, FK Lebrun, F. Lin, D. Linder, D. Lodato, G. Longo, F. Lund, N. Maccarone, TJ Macera, D. Maier, D. Malcovati, P. Mangano, V. Manousakis, A. Marisaldi, M. Markowitz, A. Martindale, A. Matt, G. McHardy, IM Melatos, A. Mendez, M. Migliari, S. Mignani, R. Miller, MC Miller, JM Mineo, T. Miniutti, G. Morsink, S. Motch, C. Motta, S. Mouchet, M. Muleri, F. Norton, AJ Nowak, M. O'Brien, P. Orienti, M. Orio, M. Orlandini, M. Orleanski, P. Osborne, JP Osten, R. Ozel, F. Pacciani, L. Papitto, A. Paul, B. Perinati, E. Petracek, V. Portell, J. Poutanen, J. Psaltis, D. Rambaud, D. Ramsay, G. Rapisarda, M. Rachevski, A. Ray, PS Rea, N. Reddy, S. Reig, P. Aranda, MR Remillard, R. Reynolds, C. Rodriuez Gil, P. Rodriguez, J. Romano, P. Rossi, EMR Ryde, F. Sabau Graziati, L. Sala, G. Salvaterra, R. Sanna, A. Schanne, S. Schee, J. Schmid, C. Schwenk, A. Schwope, AD Seyler, JY Shearer, A. Smith, DM Smith, PJ Sochora, V. Soffitta, P. Soleri, P. Stappers, B. Stelzer, B. Stergioulas, N. Stratta, G. Strohmayer, TE Stuchlik, Z. Suchy, S. Sulemainov, V. Takahashi, T. Tamburini, F. Tenzer, C. Tolos, L. Torok, G. Torrejon, JM Torres, DF Tramacere, A. Trois, A. 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, CA Winter, B. Wood, K. Zampa, G. Zampa, N. Zampieri, L. Zdziarski, A. Zhang, BALDAZZI, GIUSEPPE, FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), PCAS, APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), NOAA Geophysical Fluid Dynamics Laboratory (GFDL), National Oceanic and Atmospheric Administration (NOAA), Departamento de Biología Animal (Universidad de Granada), Universidad de Granada (UGR), Estación Experimental de Zonas Áridas (CSIC), Universitat Politècnica de Catalunya [Barcelona] (UPC), INAF-IASF Milano, Groupe d'Etudes des Matériaux Hétérogènes (GEMH), Université de Limoges (UNILIM)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM), Institute of Geology, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Tadayuki Takahashi, Stephen S. Murray, Jan-Willem A. den Herder, Shiro Ueno, LOFT, Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Universidad de Granada = University of Granada (UGR), Feroci, M, den Herder, JW, 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, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Azzarello, P, Baldazzi, G, Balman, S, Barbera, M, Belloni, T, Bertuccio, G, Bianchi, S, Bianchini, A, Bodin, P, Bonnet Bidaud, J-M, Boutloukos, S, Braga, J, Brown, E, Bucciantini, N, Burderi, L, Bursa, M, Budtz-Jørgensen, C, Cackett, E, Cadoux, F R, Cais, P, Caliandro, G A, Campana, R, Campana, S, Casella, P, Chakrabarty, D, Chenevez, J, Coker, J, Cole, R, Collura, A, Courvoisier, T, Cros, A, Cumming, A, Cusumano, G, D'Ai, A, D'Elia, V, Del Monte, E, de Martino, D, De Rosa, A, Di Cosimo, S, Diebold, S, Di Salvo, T, Donnarumma, I, Drago, A, Durant, M, Emmanoulopoulos, D, Evangelista, Y, Fabian, A, Falanga, M, Favre, Y, Feldman, C, Ferrigno, C, Finger, M H, Fraser, GW, Fuschino, F, Galloway, DK, Galvez Sanchez, JL, Garcia-Berro, E, Gendre, B, Gezari, S, Giles, AB, Gilfanov, M, Giommi, P, Giovannini, G, Giroletti, M, Goldwurm, A, Götz, D, Gouiffes, C, Grassi, M, Groot, P, Guidorzi, C, Haas, D, Hansen, F, Hartmann, D H, Haswell, C A, Heger, A, Homan, J, Hornstrup, A, Hudec, R, Huovelin, J, Ingram, A, In't Zand, J J M, Isern, J, Israel, G, Izzo, L, Jonker, P, Kaaret, P, 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, Lebrun, F, Lin, D, Linder, D, Lodato, G, Longo, F, Lund, N, Maccarone, TJ, Macera, D, Maier, D, Malcovati, P, Mangano, V, Manousakis, A, Marisaldi, M, Markowitz, A, Martindale, A, Matt, G, McHardy, IM, Melatos, A, Mendez, M, Migliari, S, Mignani, R, Miller, M C, Miller, J M, Mineo, T, Miniutti, G, Morsink, S, Motch, C, Motta, S, Mouchet, M, Muleri, F, Norton, AJ, Nowak, M, O'Brien, P, Orienti, M, Orio, M, Orlandini, M, Orleanski, P, Osborne, J P, Osten, R, Ozel, F, Pacciani, L, Papitto, A, Paul, B, Perinati, E, Petracek, V, Portell, J, Poutanen, J, Psaltis, D, Rambaud, D, Ramsay, G, Rapisarda, M, Rachevski, A, Ray, P S, Rea, N, Reddy, S, Reig, P, Reina Aranda, M, Remillard, R, Reynolds, C, Rodríguez-Gil, P, Rodriguez, J, Romano, P, Rossi, E M R, Ryde, F, Sabau-Graziati, L, Sala, G, Salvaterra, R, Sanna, A, Schanne, S, Schee, J, Schmid, C, Schwenk, A, Schwope, A D, Seyler, J-Y, Shearer, A, Smith, A, Smith, D M, Smith, P J, Sochora, V, Soffitta, P, Soleri, P, Stappers, B, Steltzer, B, Stergioulas, N, Stratta, G, Strohmayer, T E, Stuchlik, Z, Suchy, S, Sulemainov, V, Takahashi, T, Tamburini, F, Tenzer, C, Tolos, L, Torok, G, Torrejon, J M, Torres, D F, Tramacere, A, Trois, A, 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, Zdziarski, A, Zhang, B, High Energy Astrophys. & Astropart. Phys (API, FNWI), 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., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Azzarello, P., Baldazzi, G., Balman, S., Barbera, M., Belloni, T., Bertuccio, G., Bianchi, S., Bianchini, A., Bodin, P., Bonnet Bidaud, J. M., Boutloukos, S., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F. R., Cais, P., Caliandro, G. A., Campana, R., Campana, S., Casella, P., Chakrabarty, D., Chenevez, J., Coker, J., Cole, R., Collura, A., Courvoisier, T., Cros, A., Cumming, A., Cusumano, G., D'Ai, A., D'Elia, V., Del Monte, E., de Martino, D., De Rosa, A., Di Cosimo, S., Diebold, S., Di Salvo, T., Donnarumma, I., Drago, A., Durant, M., Emmanoulopoulos, D., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrigno, C., Finger, M. H., Fraser, G. W., Fuschino, F., 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., Goldwurm, A., Götz, D., Gouiffes, C., Grassi, M., Groot, P., Guidorzi, C., Haas, D., Hansen, F., Hartmann, D. H., Haswell, C. A., Heger, A., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J. J. M., Isern, J., Israel, G., Izzo, L., Jonker, P., Kaaret, P., 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., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, Francesco, Lund, N., Maccarone, T. J., Macera, D., Maier, D., Malcovati, P., Mangano, V., Manousakis, A., Marisaldi, M., Markowitz, A., Martindale, A., Matt, G., Mchardy, I. M., Melatos, A., Mendez, M., Migliari, S., Mignani, R., Miller, M. C., Miller, J. M., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Muleri, F., Norton, A. J., Nowak, M., O'Brien, P., Orienti, M., Orio, M., Orlandini, M., Orleanski, P., Osborne, J. P., Osten, R., Ozel, F., Pacciani, L., Papitto, A., Paul, B., Perinati, E., Petracek, V., Portell, J., Poutanen, J., Psaltis, D., Rambaud, D., Ramsay, G., Rapisarda, M., Rachevski, A., Ray, P. S., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rodríguez Gil, P., Rodriguez, J., Romano, P., Rossi, E. M. R., Ryde, F., Sabau Graziati, L., Sala, G., Salvaterra, R., Sanna, A., Schanne, S., Schee, J., Schmid, C., Schwenk, A., Schwope, A. D., Seyler, J. Y., Shearer, A., Smith, A., Smith, D. M., Smith, P. J., Sochora, V., Soffitta, P., Soleri, P., Stappers, B., Steltzer, B., Stergioulas, N., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tenzer, C., Tolos, L., Torok, G., Torrejon, J. M., Torres, D. F., Tramacere, A., Trois, A., 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., Zdziarski, A., Zhang, B., Astronomy, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), SPIE-INT SOC OPTICAL ENGINEERING, 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA, M Feroci, JW den Herder, JW Bozzo, E Barret, D Brandt, S Hernanz, M van der Kli, M Pohl, M Santangelo, A Stella, L Watt, A Wilm, J Zane, S Ahangarianabhari, M Alpar, A Altamirano, D Alvarez, L Amati, L Amoro, C Andersson, N Antonelli, A Argan, A Artigue R, Azzarello P, G Baldazzi, Balman, S Barbera, M Belloni, T Bertuccio, G Bianchi, S Bianchini, A Bodin, P Bidaud, JMB Boutlouko, S Braga, J Brown, E Bucciantini, N Burderi, L Bursa, M Budtz-Jorgensen, C Cackett, E Cadoux, FR Cai, P Caliandro, GA Campana, R Campana, S Casella, P Chakrabarty, D Chenevez, J Coker, J Cole, R Collura, A Courvoisier, T Cro, A Cumming, A Cusumano, G D'Ai, A D'Elia, V Del Monte, E De Martino, D De Rosa, A Di Cosimo, S Diebold, S Di Salvo, T Donnarumma, I Drago, A Durant, M Emmanoulopoulo, D Evangelista, Y Fabian, A Falanga, M Favre, Y Feldman, C Ferrigno, C Finger, MH Fraser, GW Fuschino, F Galloway, DK Sanchez, JLG Garcia-Berro, E Gendre, B Gezari, S Gile, AB Gilfanov, M Giommi, P Giovannini, G Giroletti, M Goldwurm, A Gotz, D Gouiffe, C Grassi, M Groot, P Guidorzi, C Haa, D Hansen, F Hartmann, DH Haswell, CA Heger, A Homan, J Hornstrup, A Hudec, R Huovelin, J Ingram, A in't Zand, JJM Isern, J Israel, G Izzo, L Jonker, P Kaaret, P Kara, V Karelin, D Kataria, D Keek, L Kennedy, T Klochkov, D Kluzniak, W Kokkota, K Korpela, S Kouveliotou, C Kreykenbohm, I Kuiper, LM Kuvvetli, I Labanti, C Lai, D Lamb, FK Lebrun, F Lin, D Linder, D Lodato, G Longo, F Lund, N Maccarone, TJ Macera, D Maier, D Malcovati, P Mangano, V Manousaki, A Marisaldi, M Markowitz, A Martindale, A Matt, G McHardy, IM Melato, A Mendez, M Migliari, S Mignani, R Miller, MC Miller, JM Mineo, T Miniutti, G Morsink, S Motch, C Motta, S Mouchet, M Muleri, F Norton, AJ Nowak, M O'Brien, P Orienti, M Orio, M Orlandini, M Orleanski, P Osborne, JP Osten, R Ozel, F Pacciani, L Papitto, A Paul, B Perinati, E Petracek, V Portell, J Poutanen, J Psalti, D Rambaud, D Ramsay, G Rapisarda, M Rachevski, A Ray, PS Rea, N Reddy, S Reig, P Aranda, MR Remillard, R Reynold, C Rodriuez-Gil, P Rodriguez, J Romano, P Rossi, EMR Ryde, F Sabau-Graziati, L Sala, G Salvaterra, R Sanna, A Schanne, S Schee, J Schmid, C Schwenk, A Schwope, AD Seyler, JY Shearer, A Smith, DM Smith, PJ Sochora, V Soffitta, P Soleri, P Stapper, B Stelzer, B Stergioula, N Stratta, G Strohmayer, TE Stuchlik, Z Suchy, S Sulemainov, V Takahashi, T Tamburini, F Tenzer, C Tolo, L Torok, G Torrejon, JM Torre, DF Tramacere, A Troi, A 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 Wijer, R Wijnand, R Wille, M Wilson-Hodge, CA Winter, B Wood, K Zampa, G Zampa, N Zampieri, L Zdziarski, A Zhang, Pohl, Martin, Cadoux, Franck, and Favre, Yannick

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Vision, X-ray timing, Astronomy, SPIE Proceedings, Observatories, X-ray timing, X-ray spectroscopy, X-ray imaging, compact objects, Silicon Drift Chambers, FOS: Physical sciences, ddc:500.2, X-ray missions, Space (mathematics), Astrophysics, 01 natural sciences, 7. Clean energy, Settore FIS/05 - Astronomia E Astrofisica, X-rays, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Instrumentation (computer programming), Electrical and Electronic Engineering, Aerospace engineering, Diagnostics, Compact objects, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Spatial resolution, sezele, Sensors, 010308 nuclear & particles physics, business.industry, Applied Mathematics, X-ray imaging, Silicon Drift Chamber, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, X-ray spectroscopy, Electronic, Optical and Magnetic Materials, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Instrumentation and Methods for Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, business
Abstract

The LOFT mission concept is one of four candidates selected by ESA for the M3 launch opportunity as Medium Size missions of the Cosmic Vision programme. The launch window is currently planned for between 2022 and 2024. LOFT is designed to exploit the diagnostics of rapid X-ray flux and spectral variability that directly probe the motion of matter down to distances very close to black holes and neutron stars, as well as the physical state of ultra-dense matter. These primary science goals will be addressed by a payload composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a collimated (, Proceedings of SPIE, Vol. 8443, Paper No. 8443-85, 2012

Published
2012

40. An active state of the BL Lac Object Markarian 421 detected by INTEGRAL in April 2013

Author

A. Stamerra, A. Bazzano, Aldo Treves, P. Romano, M. Villata, Simona Soldi, L. Maraschi, Carlo Ferrigno, S. Vercellone, M. Fiocchi, T. Pursimo, Gianluca Castignani, Filippo D'Ammando, Elena Pian, René Hudec, C. M. Raiteri, Fabrizio Tavecchio, P. Ubertini, Luigi Foschini, Volker Beckmann, R. Walter, Giuseppe Malaguti, R. Boissay, V. Bianchin, Marc Türler, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Brera (OAB), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Nordic Optical Telescope (NOT), Instituto de Astrofisica de Canarias (IAC), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Pian E, Turler M, Fiocchi M, Boissay R, Bazzano A, Foschini L, Tavecchio F, Bianchin V, Castignani G, Ferrigno C, Raiteri CM, Villata M, Beckmann V, DAmmando F, Hudec R, Malaguti G, Maraschi L, Pursimo T, Romano P, Soldi S, Stamerra A, Treves A, Ubertini P, Vercellone S, Walter R, Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), INAF-OAB, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Population, galaxies: active, FOS: Physical sciences, Synchrotron radiation, Astrophysics, law.invention, Apparent magnitude, law, gamma rays: galaxies, education, Blazar, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, education.field_of_study, Astronomy and Astrophysics, radiation mechanisms: non-thermal, Light curve, X-rays: galaxies, Space and Planetary Science, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, galaxies: active / X-rays: galaxies / radiation mechanisms: non-thermal / gamma rays: galaxies, Fermi Gamma-ray Space Telescope, BL Lac object, Flare
Abstract

Multiwavelength variability of blazars offers indirect insight into their powerful engines and on the mechanisms through which energy is propagated from the centre down the jet. The BL Lac object Mkn 421 is a TeV emitter, a bright blazar at all wavelengths, and therefore an excellent target for variability studies. Mkn 421 was observed by INTEGRAL and Fermi-LAT in an active state on 16-21 April 2013. Well sampled optical, soft, and hard X-ray light curves show the presence of two flares. The average flux in the 20-100 keV range is 9.1e-11 erg/s/cm2 (~4.5 mCrab) and the nuclear average apparent magnitude, corrected for Galactic extinction, is V ~12.2. In the time-resolved X-ray spectra (3.5-60 keV), which are described by broken power laws and, marginally better, by log-parabolic laws, we see a hardening that correlates with flux increase, as expected in refreshed energy injections in a population of electrons that later cool via synchrotron radiation. The hardness ratios between the JEM-X fluxes in two different bands and between the JEM-X and IBIS/ISGRI fluxes confirm this trend. During the observation, the variability level increases monotonically from the optical to the hard X-rays, while the large LAT errors do not allow a significant assessment of the MeV-GeV variability. The cross-correlation analysis during the onset of the most prominent flare suggests a monotonically increasing delay of the lower frequency emission with respect to that at higher frequency, with a maximum time-lag of about 70 minutes, that is however not well constrained. The spectral energy distributions from the optical to the TeV domain are satisfactorily described by homogeneous models of blazar emission based on synchrotron radiation and synchrotron self-Compton scattering, except in the state corresponding to the LAT softest spectrum and highest flux., Comment: 11 pages, 6 figures, in press in A&A

Published
2014

41. A large area detector proposed for the Large Observatory for X-ray Timing (LOFT)

Author

I. Donnarumma, Y. Evangelista, Phil Uttley, Christian Schmid, D. Macera, L. Pacciani, Paul S. Smith, T. Kennedy, J.-Y. Seyler, J. W. den Herder, Martino Marisaldi, Michael A. Nowak, A. de Rosa, Berend Winter, Dom Walton, E. Bozzo, A. Argan, Miriam Grassi, C. Tenzer, M. Ahangarianabhari, G. Zampa, Andrea Santangelo, Jörn Wilms, A. Vacchi, P. Bodini, Riccardo Campana, Claudio Labanti, Slawomir Suchy, Silvia Zane, P. Soffitta, F. Fuschino, Fabio Muleri, M. Hailey, S. Di Cosimo, Adrian Martindale, V. Petracek, P. Cais, Giuseppe Baldazzi, Yannick Favre, Mauro Orlandini, E. Del Monte, Didier Barret, Alain Cros, Emanuele Perinati, C. Feldman, M. Pohl, Franck Cadoux, J. Coker, Piero Malcovati, M. Feroci, René Hudec, P. Azzarello, Teresa Mineo, A. Rachevski, G.W. Fraser, Giuseppe Bertuccio, N. Zampa, SPIE, Takahashi, Tadayuki, Zane S., Walton D., Kennedy T., Feroci M., Den Herder J.-W., Ahangarianabhari M., Argan A., Azzarello P., Baldazzi G., Barret D., Bertuccio G., Bodin P., Bozzo E., 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., Macera D., Malcovati P., 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., Winter B., High Energy Astrophys. & Astropart. Phys (API, FNWI), FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Mullard Space Science Laboratory (MSSL), and University College of London [London] (UCL)

Subjects
Silicon, Photon, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Observatories, Collimators, FOS: Physical sciences, ddc:500.2, Astrophysics, 7. Clean energy, 01 natural sciences, Optics, Observatory, 0103 physical sciences, X-rays, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Compact objects, Physics, Millisecond, Photons, Equipment and services, sezele, 010308 nuclear & particles physics, Payload, business.industry, Sensors, Applied Mathematics, Detector, Antenna aperture, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, Capillaries, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, X-ray Timing, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Energy (signal processing), Compact object
Abstract

The Large Observatory for X-ray Timing (LOFT) is one of the four candidate ESA M3 missions considered for launch in the 2022 time-frame. It is specifically designed to perform fast X-ray timing and probe the status of the matter near black holes and neutron stars. The LOFT scientific payload is composed of a Large Area Detector (LAD) and a Wide Field Monitor (WFM). The LAD is a 10 m2-class pointed instrument with 20 times the collecting area of the best past timing missions (such as RXTE) over the 2-30 keV range, which holds the capability to revolutionize studies of X-ray variability down to the millisecond time scales. Its ground-breaking characteristic is a low mass per unit surface, enabling an effective area of ~10 m^2 (@10 keV) at a reasonable weight. The development of such large but light experiment, with low mass and power per unit area, is now made possible by the recent advancements in the field of large-area silicon detectors - able to time tag an X-ray photon with an accuracy, Proceedings of SPIE, Vo. 8443, Paper No. 8443-87

Published
2012

42. Gamma-ray burst investigation via polarimetry and spectroscopy (GRIPS)

Author

R. Bellazini, Andreas Zoglauer, M. I. Panasyuk, René Hudec, L. G. Balasz, R. Marcinkowski, V. M. Lipunov, Mark Pearce, Felix Ryde, Andrei M. Bykov, Elena Pian, D. Hartmann, Guido Barbiellini, Andrew W. Strong, A. Majczyna, Zsolt Bagoly, Sandra Savaglio, J. Kiener, István T. Horváth, B. K. Lubsandorgiev, R. V. Poleschuk, Sheila McBreen, Vincent Tatischeff, Karl Mannheim, G. Wrochna, A. M. Chernenko, Martino Marisaldi, G. Bisnovaty-Kogan, A. Pollo, Attila Mészáros, A. F. Iyudin, A. G. Zabrodskij, J. Uvarov, S. Larsson, W. Dröge, S. E. Boggs, A. M. Cherepashuk, Gottfried Kanbach, Andreas von Kienlin, Norbert Langer, S. I. Svertilov, Dmitry Bisikalo, L. M. Zeleny, G. Dicocco, Jochen Greiner, Werner Collmar, Roland Diehl, B. McBreen, Lorraine Hanlon, Claudio Labanti, Cornelia B. Wunderer, Boris Shustov, E. Orlando, Marco Ajello, M. Gierlik, D. A. Varshalovich, Alexei Pozanenko, G. G. Lichti, L. B. Bezrukov, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Greiner, J., Iyudin, A., Kanbach, G., Zoglauer, A., Diehl, R., Ryde, F., Hartmann, D., v. Kienlin, A., Mcbreen, S., Ajello, M., Bagoly, Z., Balasz, L. G., Barbiellini, G., Bellazini, R., Bezrukov, L., Bisikalo, D. V., Bisnovaty-Kogan, G., Boggs, S., Bykov, A., Cherepashuk, A. M., Chernenko, A., Collmar, W., Dicocco, G., Droege, W., Gierlik, M., Hanlon, L., Horvath, I., Hudec, R., Kiener, J., Labanti, C., Langer, N., Larsson, S., Lichti, G., Lipunov, V. M., Lubsandorgiev, B. K., Majczyna, A., Mannheim, K., Marcinkowski, R., Marisaldi, M., Mcbreen, B., Meszaros, A., Orlando, E, Panasyuk, M. I., Pearce, M., Pian, E., Poleschuk, R. V., Pollo, A., Pozanenko, A., Savaglio, S., Shustov, B., Strong, A., Svertilov, S., Tatischeff, V., Uvarov, J., Varshalovich, D. A., Wunderer, C. B., Wrochna, G., Zabrodskij, A. G., and Zeleny, L. M.

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, education, Early universe, ComputingMethodologies_IMAGEPROCESSINGANDCOMPUTERVISION, Polarimetry, Astrophysics, Compton and pair creation telescope, 7. Clean energy, 01 natural sciences, Primary (astronomy), Nucleosynthesis, Observatory, 0103 physical sciences, Nuclear astrophysics, Hardware_ARITHMETICANDLOGICSTRUCTURES, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, health care economics and organizations, ComputingMethodologies_COMPUTERGRAPHICS, media_common, Physics, 010308 nuclear & particles physics, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, nucleosynthesis, Astronomy, Astronomy and Astrophysics, social sciences, early universe, Universe, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 95.55.Ka * 98.70.Rz * 26.30.-k, Space and Planetary Science, Compton and Pair creation telescope, Gamma-ray bursts, Gamma-ray burst
Abstract

The primary scientific goal of the GRIPS mission is to revolutionize our understanding of the early universe using gamma-ray bursts. We propose a new generation gamma-ray observatory capable of unprecedented spectroscopy over a wide range of gamma-ray energies (200 keV-50 MeV) and of polarimetry (200-1000 keV). The gamma-ray sensitivity to nuclear absorption features enables the measurement of column densities as high as 10(28)cm (-aEuro parts per thousand 2). Secondary goals achievable by this mission include direct measurements of all types of supernova interiors through gamma-rays from radioactive decays, nuclear astrophysics with massive stars and novae, and studies of particle acceleration near compact stars, interstellar shocks, and clusters of galaxies.

Published
2009

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