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1781. http://hea.iki.rssi.ru/integral06/travel~
h2>Travel Info</h2> <p>Most international flights arrive at Sheremetyevo II Airport (SVO) (phone: +7 495/956-4666 or 495/578-0101) and <a href="http://www.eastline.ru/domodedovo">Domodedovo</a> Airport (DME) (phone: +7 495/323-8565).</p> <strong>Transfers Between the Airport & Town</strong><br> <i>Bus & Train</i> <p>City transitions are serviced by municipal buses from Sheremetyevo II airport to subway station Rechnoy Vokzal with buses leaving every 15-20 minutes. ...
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Ссылки http://hea.iki.rssi.ru/integral06/travel~ -- 4.1 Кб -- 21.03.2007
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1782. http://hea.iki.rssi.ru/integral06/ttt
email ={ sergei@hea.iki.rssi.ru }, email ={sizun@cea.fr}, email ={st@hea.iki.rssi.ru}, email ={sizun@cea.fr}, email ={mikej@hea.iki.rssi.ru}, email ={chelovekov@hea.iki.rssi.ru}, email ={Sandrine.Deluit@cesr.fr}, email ={olivia.tsang@mpi-hd.mpg.de}, email ={pierre.jean@cesr.fr}, email ={malzac@cesr.fr}, email ={askar.ibragimov@oulu.fi}, email ={jean@cesr.fr}, email ={nguessoum@aus.edu}, email ={lonjou@cesr.fr}, ...
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Ссылки http://hea.iki.rssi.ru/integral06/ttt -- 5.7 Кб -- 21.03.2007
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1783. http://hea.iki.rssi.ru/integral06/visa
TABLE WIDTH=100%><TR><TD><h2>Obtaining Russian Visa</h2></TD><TD align=right><IMG SRC="images/ru5.gif" width=80pt></TD></TR></TABLE> <p>All foreigners are required to obtain visas to enter Russia. If you travel alone, the cheapest option (saves you $30) is to obtain a "business visa" using an official invitation from IKI. This takes about 45 days. The ESA representatives can obtain an official invitation for a "business visa" from the ESA Office in Moscow. ...
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Ссылки http://hea.iki.rssi.ru/integral06/visa -- 5.6 Кб -- 21.03.2007
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1784. http://hea.iki.rssi.ru/integral06/visanew
TABLE WIDTH=100%><TR><TD><h2>Obtaining Russian Visa</h2></TD><TD align=right><IMG SRC="images/ru5.gif" width=80pt></TD></TR></TABLE> <p>All foreigners are required to obtain visas to enter Russia. If you travel alone, the cheapest option (saves you $30) is to obtain a "business visa" using an official invitation from IKI or (for representatives of ESA) from the ESA Office in Moscow. This takes about 45 days. ... Visa is issued in 10 days or so. ...
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Ссылки http://hea.iki.rssi.ru/integral06/visanew -- 5.5 Кб -- 21.03.2007
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1785. http://hea.iki.rssi.ru/integral06/visaold
TABLE WIDTH=100%><TR><TD><h2>Obtaining Russian Visa</h2></TD><TD align=right><IMG SRC="images/ru5.gif" width=80pt></TD></TR></TABLE> <p>All foreigners are required to obtain visas to enter Russia. If you travel alone, the cheapest option (saves you $30) is to obtain a "business visa" using an official invitation from IKI. This takes about 45 days. ... The consular fee in the US is $100 plus postage.</p> <p>Some hotel reservations services in Moscow send invitations free of extra charge. ...
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Ссылки http://hea.iki.rssi.ru/integral06/visaold -- 4.9 Кб -- 21.03.2007
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1786. http://hea.iki.rssi.ru/integral06/visa~
TABLE WIDTH=100%><TR><TD><h2>Obtaining Russian Visa</h2></TD><TD align=right><IMG SRC="ru5.gif" width=80pt></TD></TR></TABLE> <p>Short summary: All foreigners are required to obtain visas to enter Russia. If you travel alone, the cheapest option (saves you $30) is to obtain a "business visa" using invitation from IKI. This takes about 45 days. ... The consular fee in the US is $100 plus postage.</p> <p>Some hotel reservations services in Moscow send invitations free of extra charge. ...
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Ссылки http://hea.iki.rssi.ru/integral06/visa~ -- 4.8 Кб -- 21.03.2007
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1787. http://hea.iki.rssi.ru/integral06/wether~
efeffe
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Ссылки http://hea.iki.rssi.ru/integral06/wether~ -- 1.0 Кб -- 21.03.2007
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1788. http://hea.iki.rssi.ru/integral06/papers/D34_Bottacini01-12Mar07_13:28:35.pdf
INTEGRAL OBSERVATIONS OF THE GAMMA-RAY BLAZAR 3C 279 DURING THE `DEEP EXTRAGALACTIC SURVEY' E. Bottacini(1), W. Collmar(1), T. Courvoisier (1 ) (2 ), (3 ) (3 ) Max Planck Institut fЭr extraterrestrische Physik , Giessenbachstraъe, 85748 Garching, Germany (2 ) INTEGRAL Science Data Centre, Chemin d'Ecogia 16, 1290 Versoix, Swiss Observatoire Astronomique de l'UniversitИ de GenХve, Chemin des Maillettes 51, 1290 ... We have studied the hard X-ray emission of 3C 279 during the INTEGRAL mission. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/D34_Bottacini01-12Mar07_13:28:35.pdf -- 130.0 Кб -- 12.03.2007
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1789. http://hea.iki.rssi.ru/integral06/papers/G30_Balman01-05Mar07_11:54:53.pdf
TIME-AVERAGED BROAD-BAND SPECTRA OF THE DIPPING LOW-MASS X-RAY BINARIES OBSERVED WITH INTEGRAL S. Balman1 , A. N. Parmar1 , L. Sidoli2 , A. Paizis2 , M. Diaz Trigo3 , and T. Oosterbroek 1 4 Astrophysics Missions Division, Research and Scientific Support Department of ESA, ESTEC, Postbus 299, NL-2200 AG Noordwijk, Netherlands 2 Istituto di astrofisica Spaziale e Fisica Cosmica-Sezione, di Milano-IASF/INAF, I-20133 Milano, Italy 3 ESA, ESAC, Urb. ... 11] Hua X-M. and Titarchuk L., ApJ 449, 188, 1995. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/G30_Balman01-05Mar07_11:54:53.pdf -- 149.1 Кб -- 05.03.2007
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1790. http://hea.iki.rssi.ru/integral06/papers/F40_Ziolkowski01-03Mar07_22:49:23.pdf
PHOTOMETRIC SEARCH FOR BLACK HOLES IN DORMANT X-RAY TRANSIENTS Є Є Aleksander Sadowski1 , Janusz Ziolkowski2 , and Krzysztof Belczynski3 ? Astronomical Observatory of Warsaw University, Al. ... Such definition means that our statistics for the number of expected BH X-ray binaries include both transient and persistent systems. ... If this value is 2 M , then, according to our calculations, Galaxy contains some 15 000 to 40 000 of BH X-ray binaries (and some 30 000 to 250 000 of NS X-ray binaries). ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/F40_Ziolkowski01-03Mar07_22:49:23.pdf -- 1545.4 Кб -- 03.03.2007
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1791. http://hea.iki.rssi.ru/integral06/papers/I08_McBreen01-02Mar07_22:32:44.pdf
... The intense burst occurred about 250 s after the precursor and the long delay enabled optical and near infrared telescopes to observe the prompt emission. ... We avail of multi-wavelength data to generate broadband spectra of GRB 041219a and afterglow. ... Broadband spectra of the prompt emission were generated in 7 time intervals using -ray, x-ray, optical and near-infrared data and these were compared to the high-redshift burst GRB 050904. ... There is no measured redshift available for this burst...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/I08_McBreen01-02Mar07_22:32:44.pdf -- 254.6 Кб -- 02.03.2007
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1792. http://hea.iki.rssi.ru/integral06/papers/B31_Martin01-01Mar07_11:05:37.pdf
SEARCH FOR THE 44TI LINES IN CASSIOPEIA A WITH INTEGRAL/SPI Pierrick Ma rtin(1), JЭrg en KnЖdlseder(2), Jacco Vink (1) (2 ) (3) (3) CESR - 9, a venue du Co lonel Ro che ґ BP4346 ґ 31028 Toulouse Ced ex 4 ґ France ґ martin @cesr.fr CESR - 9, a venue du Co lonel Ro che ґ BP4346 ґ 31028 Toulouse Ced ex 4 ґ France ґ knodlsed er@ cesr.fr Astronomical Institu te Utrech t ґ P.O . ... As can be seen, the 67.9 keV line is shrouded in an intense background line complex and is therefore hardly accessible. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/B31_Martin01-01Mar07_11:05:37.pdf -- 721.6 Кб -- 01.03.2007
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1793. http://hea.iki.rssi.ru/integral06/papers/J37_Wunderer02-28Feb07_04:09:11_bandw.pdf
... For the first balloon flight of the Nuclear Compton Telescope (NCT) we have simultaneously reduced lowenergy background and enabled hard X-ray imaging by enshrouding the top of the instrument in a tin shield (bottom had BGO shielding), with part of the shield having strategically placed holes -- a 10% open coded aperture mask working up to 80 keV in conjunction with the finely pixellated double-sided Ge strip detectors. ... Key words: Compton telescope, coded mask, hard X-ray imaging, NCT. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/J37_Wunderer02-28Feb07_04:09:11_bandw.pdf -- 1747.1 Кб -- 28.02.2007
[ Текст ] Ссылки http://hea.iki.rssi.ru/integral06/papers/J37_Wunderer02-28Feb07_04:09:11_color.pdf -- 1747.1 Кб -- 28.02.2007
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[ Текст ] Ссылки http://hea.iki.rssi.ru/integral06/papers/J37_Wunderer02-28Feb07_04:09:11_color.pdf -- 1747.1 Кб -- 28.02.2007
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1794. http://hea.iki.rssi.ru/integral06/papers/I37_Wunderer01-28Feb07_20:33:11.pdf
SEARCHING FOR MILLISECOND FLARES IN INTEGRAL GRBS -- TOWARDS PROBING QUANTUM GRAVITY WITH INTEGRAL GAMMA-RAY BURSTS Cornelia B. Wunderer1 , Steven E. Boggs1 , Wayne Coburn1 , and Kevin Hurley 1 1 Space Sciences Laboratory, UC Berkeley, CA 94720, USA ABSTRACT Since the discovery of the cosmological origin of GRBs there has been growing interest in using these transient events to probe the Quantum Gravity energy scale in the range 1016 ґ1019 GeV, up to the Planck mass scale. ... SPI electronic noise. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/I37_Wunderer01-28Feb07_20:33:11.pdf -- 527.8 Кб -- 28.02.2007
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1795. http://hea.iki.rssi.ru/integral06/papers/E39_Deluit01-28Feb07_19:42:02.pdf
... In particular, with the spectrometer SPI (20 keV-8 MeV), we detect in three observations an emission extending above 200 keV and for the first time even up to 350 keV for a neutron star LMXRB, GS 1826-24. ... The additional component above 200 keV is most probably of non-thermal origin. ... Figure 1. ... We reveal with SPI a hard tail up to 220 keV for 4U 1812-12 (Figure 1) and even up to 350 keV for GS 1826-24 (Figure 2), representing the hardest emission ever detected for a Neutron Star LMXRB. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/E39_Deluit01-28Feb07_19:42:02.pdf -- 1090.1 Кб -- 28.02.2007
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1796. http://hea.iki.rssi.ru/integral06/papers/I35_Marcinkowski01-28Feb07_19:28:29.pdf
... We have taken into account: dead-times of detectors, data gaps, VETO, detectors signal thresholds, precursor normalized counts/sec/ keV 10-4 10-3 0.01 0.1 1 peak normalized counts/sec/ keV 10-4 10-3 0.01 0.1 1 normalized counts/sec/ keV 10-4 10-3 0.01 0.1 1 tail peak SPI ACS 120000 100000 80000 1800 [counts/s] 1400 1000 600 200 500 400 300 200 100 0 precursor 140000 tail 2 2 0 0 ISGRI -2 10 100 1000 energy channel [ ... GRB 031111A 10 100 1000 energy channel [keV] Figure 2. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/I35_Marcinkowski01-28Feb07_19:28:29.pdf -- 85.8 Кб -- 28.02.2007
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1797. http://hea.iki.rssi.ru/integral06/papers/D35_Collmar01-27Feb07_19:21:51.pdf
MULTIFREQUENCY OBSERVATIONS OF THE BLAZAR 3C 279 IN JANUARY 2006 и W. Collmar1 , M. Bottcher2 , T. Krichbaum3 , E. Bottacini1 , V. Burwitz1 , A. Cucchiara4 , D. Grupe4 , M. Gurwell5 , P. Kretschmar6 ... Center, ASDC c/o ESRIN, via G. Galilei, 00044 Frascati, Italy 1 6 ABSTRACT We report first results of a multifrequency campaign from radio to hard X-ray energies of the prominent -ray blazar 3C 279 , which was organised around an ... 10 Energy (keV) be measured (Fig. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/D35_Collmar01-27Feb07_19:21:51.pdf -- 260.7 Кб -- 27.02.2007
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1798. http://hea.iki.rssi.ru/integral06/papers/G40_Enoto01-27Feb07_08:17:04.pdf
WIDE-BAND STUDY OF X-RAY PULSARS WITH SUZAKU T. Enoto1 , R. Miyawaki1 , M. Kokubun1 , K. Makishima1 , Y. Terada2 , T. Mihara2 , M. Nakajima2 , M. Suzuki2 , A. Bamba2 , A. Senda2 ... Department of Physics, Kanazawa University 11 Department of Technology, Miyazaki Univerity 1 7 ABSTRACT A summary is given on the timing accuracy verifications of the Hard X-ray Detector ( HXD ) on board the Suzaku satellite ... Key words: Suzaku, HXD, Crab pulsar, PSR1509-58, A0535+26,. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/G40_Enoto01-27Feb07_08:17:04.pdf -- 196.5 Кб -- 27.02.2007
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1799. http://hea.iki.rssi.ru/integral06/papers/B32_Cordier01-26Feb07_18:49:16.pdf
... 0.015 0.01 0.005 0 -0.005 -0.01 -150 -100 -50 0 GLON [deg] 50 100 150 4. ... 0 GLON [ deg ] 50 100 150 ей ж и ей ж и зж 1 -1 -3 1 0 -1 -2 Residuals OFF 0.006 0.004 0.002 count rate [cpscorr] 0 -0.002 -0.004 -0.006 -0.008 -0.01 -0.012 - 150 - 100 -50 0 GLON [ deg ] 50 2 / ndf p0 61.04 / 58 -1.206e-06 ? 1.595e-04 Residuals OFF 0.006 0.004 count rate [cpscorr] 0.002 0 -0.002 -0.004 -0.006 -0.008 -0.01 2 / ndf p0 67.73 / 58 8.599e-06 ? 1.596e-04 100 150 - 150 - 100 -50 0 GLON [ ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/B32_Cordier01-26Feb07_18:49:16.pdf -- 246.3 Кб -- 26.02.2007
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1800. http://hea.iki.rssi.ru/integral06/papers/I07_Ruffini01-23Feb07_22:27:02.pdf
... The concept of the dyadosphere [39, 37] is the only attempt, as far 2 10 50 Theoretical fit in 15-350 keV band Theoretical fit in 0.2-10 keV band XRT observation in 0.2-10 keV band 10 -7 10 Source Luminosity (erg/(s*strad)) 49 10 -8 10 47 10 -10 10 46 10 -11 10 45 10 -12 10 44 10 -13 10 43 10 -1 -14 10 10 0 10 1 10 10 Detector arrival time (s) 2 3 10 4 10 5 10 6 Figure 2. Our theoretical fit (dotted line) of the XRT observations of GRB 050315 in the 0.2-10 keV energy band [61]. ...
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Ссылки http://hea.iki.rssi.ru/integral06/papers/I07_Ruffini01-23Feb07_22:27:02.pdf -- 1376.2 Кб -- 23.02.2007
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