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Location SAO RAN

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Location SAO RAN

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  1. V.G. Kurt1, V.V. Sokolov2, V.N. Komarova2, Yu. A. Shibanov3“Optical observations radio pulsars and isolated neutron stars with 6 meters telescope BTA SAO RAN”1 Astro Space Center of the P.N.Lebedev Physical Inst. of the Russian Academy of Sciences, Moscow, Russiavkurt@asc.rssi.ru2 Special Astrophysical Observatory of the Russian Academy of Sciences, Nigniy Arkhiz, Karachavo-Cherkessia, Russia3 S-Petersburgh Physical – Technical Institute name A.F. Ioffe, Russia

  2. Location SAO RAN

  3. 6 meter optical telescope BTA1966 y

  4. Winter view

  5. 6 m telescope BTA inside

  6. Optical schema

  7. Optical corrector SCORPIO in main focus

  8. The main parameters • The main mirror is parabolic shape focal length is 24 m. The diameter of the main mirror is 605 cm. In prime focus cage, where optical devices and the mechanisms of input/output of the lens corrector and hyperbolic secondary focus mirror are located. From the laboratory tests the concentration of energy in a circle 0.8" in diameter is 90%. Under favorable conditions the seeing is limited by atmosphere amounts to FWHM ~1" for 20% of observational nights and 1.8’’ tipical. • The optical scheme of the telescope provides for working at the prime focus (f/4) and two Nasmith foci (f/30). To correct for field aberrations, when working at the prime focus, a Rosse corrector is used, which is made of K type glass (the short-wave bandwidth is 3800A ). The field of view with coma and astigmatism corrected at a level of <0.5" is about 14'.

  9. Some parameters of BTA Telescope • The 6-m telescope (BTA - Big Telescope Alt-azimuthal) The telescope is located near Mt. Pastukhova at an altitude of 2070 m above sea level, the coordinates of the site: longitude N 41o26'30", latitude E +43o 39'12". • Main mirror diameter6 m. Focal length24 m. Light collecting area26 sq.mWavelength range0.3 - 10 mkm. Angular resolution0.6 arcsec- with the application of speckle interferometry techniques0.02 arcsec. Mass of the main mirror42 tonsTotal telescope mass850 tons. TelescopeDome is D= 42 m,H = 53 m, Limiting stellar magnitude near 26m for V, R, I (system)

  10. DETECTORS • CCD-photometer • The Prime Focus CCD-photometer • of 1024 x 1024 pixels cooled with liquid nitrogen to a temperature of -120oC The optical and mechanical design of the photometer contains a weal with 12 filters, a fast section shutter and standard lamp for flat-field calibrating. The size of the registered field of view of the photometer in PF BTA is 210.3" x 210.3", the pixel size is 24x24mkm which correspoded angular size in PF BTA 0.205"x0.205". Readout noise is 2.85e– per sec. • The set of wide-band filters used in photometry is system similar to the Jonson and Cousins BVRI. A set of narrow-band filters in the region of Hα line for the observations of galaxies in the range the redshifts z = 0.000 - 0.033 is available. Soft - MIDAS from ESO. • BandBVRI extinction coefficient0.340; 0.210; 0150; 0.100m Limiting mag Texp = 600s and S/N=4 26.1m25.6m25.1m24.4mSky brightness 22.521.520.819.1m / sq.sec

  11. NEW • New CCD EEV 42-40 with 2048x2048 pixels (equals 6.1' onsky). New photometric soft - instead of MIDAS, now we use IRAF (Image Reduction and Analysis Facility). For astrometry our soft is IRAF.

  12. OUR PHOTOMETRY • log f = - 0.4 mx + log f (0) erg cm-2 s-1A-1 For V logf (0) = - 8.440 • R - 8.760 • I - 9.080 • J -9.497 • K -10.380 • Typical seeing ………………………1.3 - 1.8 ” (!) • VERY BAD! For HST S/N=50 BTA ~ 7 • 10 – 20 weak stars for calibration in field near 30”

  13. Catalog of radio pulsars • http://www.atnf.csiro.au/research/pulsaat/ 1794 Radio pulsars with Δα and Δδ 0.1 – 0.001 ang. sec (except VLBI measurements near 1%). • This is our hard astrometry problem! “Step to step movements “

  14. PSR 0656+14

  15. Search of pulsars • F =4   r2  T4 /4   d2 (erg  cm-2  s-1 ) • Low Interstellar absorptions, |b| > 5-10o • To = T /106 , K • Ro = r /10 km • do = d / 500 pc d < 1000 pc • For T0 =R 0=d 0 = 1 without absorptions • V = 24m it is good! • Very Youngτ =P/(2  dP/dt) < 10 8 y

  16. X-ray and gamma ray emissionfor PSR 0656+14 • ROSAT • Soft BB radiation T= 840 000 K • Hard chanall T = 1 650 000 K • GRO Power law  = -1.8 (±0.3)

  17. CCD picture for PSR 0656+14

  18. Photometry HST and BTA

  19. Spectrum of PSR 0656+14

  20. Two parameters • 1) Raylegh – Jeans parameter G =T6 ( R10 /d500 )2 2)Energy power-low index  By fitting of spectrum 0 < G< 6.2 for 1 level 0.3 <  < 2.6 1 level Exist non-thermal component

  21. Synthetic spectrum

  22. Gamma-Radio pulsar GEMINGA • Multiband photometry of Geminga • Kurt, V.G.; Komarova, V.N.; Sokolov, V.V.; Fatkhullin, T.A.; • Koptsevich, A.B.; Shibanov, Yu.A. • Bulletin of the Special Astrophysical Observatory Vol. 51, p. 21 - 37 (2001) • Abstract • We present the results of the BVRI photometry of the Geminga pulsar based on observations with the 6 m telescope. The Geminga magnitudes in B (26.1m+/-0.5), V (25.3m+/-0.3) and Rc (25.4m+/-0.3) are consistent with results of other studies of its optical emission in these spectral bands. We derive for the first time the magnitude in the Ic band to be 25.1m+/-0.4, which is more than a magnitude higher if compared with the upper limit given in the paper of Mignani et al. (1998). The comparison of the broad-band spectra of this middle-aged isolated neutron star with the results of observations in the X-rays and hard ultraviolet suggests non-thermal origin of the Geminga emission at least in some band of the visible range.

  23. OTHER SOURCES • Optical studies of neutron stars and their surroundings • at the 6m telescope of SAO RAS} • V.N. Komarova, T.A. Fatkhullin, V.G. Kurt, Yu.A. Shibanov • Physics of Neutron Stars-2005 • The results of the on-going program for study of optical counterparts of pulsars and candidates to isolated neutron stars (NS) and search for pulsar wind nebulae (PWNe) in the H line at the 6m telescope SAO RAS are presented. Broad- and narrow-band observations have been carried out with the prime focus photometer and the focal reducer SCORPIO in image mode. There are close and/or high energetic (high velocity) NSs and pulsars, such as RX J0007+7302, AXP 4U0142+61, PSR B0823+26, PSR B1951+32, RBS 1774, PSRB2334+61 and others, in a target list. Upper limits on the level of detection and flux estimates of the objects under investigation have been obtained.

  24. Comparison pulsars with different ages 9500A 3 mkm 9500A 9500A 9500 A 3000 A

  25. AGE of OUR Pulsars • Crab 1 103 years • VELA 1.13 104 • GEMINGA 1.5 103 • B 0656+14 1.1 105 • B 0540 - 69 1.67 103

  26. The Isolated, Radio-Quiet Neutron Star RXJ 185635-3754 Two backbody fit: T1=64 eV T2=30 eV Rinf=12-26 km Pure H model Walter & Lattimer (2002)

  27. LITERATURE • Bibliography • for report V. G. Kurt at Conference “Frontiers of Space Astrophysics: Neutron Stars and Gamma Ray Bursts” • 1). Optical Observations of the Nearby Isolated Pulsar PSR 0656+14 at the SAO 6-meter Telescope. • Kurt, V. G., Komberg B. V., Sokolov, V. V., Zharykov S. V. • Astrophysics and Space Science, v. 252, Issue 1/2, p. 451-460. • 2). BVRI observations of PSR B0656+14 with the 6-meter telescope • Kurt, V.G., Sokolov V.V., Zharikov S.V., Pavlov G.G., Komberg, B.V. • Astronomy and Astrophysics, v.333, p.547-556 (1998) • 3). Optical Observations of the Nearby Isolated Pulsars With the 6 Meter Telescope • Sokolov V.V., Kurt, V.G., Zharikov S.V., Shibanov Yu.A., Koptsevich A.B. • Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and • Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.: J.Paul, T.Montmerle, • and E. Aubourg (CEA Saclay) • 4). Photometric study of fields of nearby pulsars with the 6m telescope. • Kurt V.G., Komarova V.N., Fatkhullin T.A., Sokolov, V.V., • Koptsevich A.B., Shibanov Y.A. • Bulletin. Special Astrophys. Obs., 49, 5-13 (2000) • 5). Multiband photometry of Geminga • Kurt, V.G., Komarova V.N., Sokolov V.V., Fatkhullin T.A., • Koptsevich A.B., Shibanov Yu.A. • Bulletin of the Special Astrophysical Observatory Vol. 51, p. 21 - 37 (2001)

  28. 6). Optical photometry of the PSR B0656+14 and its neighborhood • Koptsevich A.B., Pavlov G.G., Zharikov S.V., Sokolov, V.V., • Shibanov Yu.A., Kurt V.G. • Astronomy and Astrophysics, v.370, p.1004-1016 (2001) • 7)."Фотометрические исследования центральной области CTB 80", • В.Н. Комарова, В.Г. Курт, В.В. Соколов, Ю.А. Шибанов, • 2001, Тезисы докладов ВАК-2001, 94 • 8). Фотометрические исследования оптического излучения пульсаров • В.Н. Комарова, В.Г. Курт, В.В. Соколов, Ю.А. Шибанов • Всеpоссийская Конфеpенция Астpофизика Высоких Энеpгий Сегодня и Завтpа • HEA-2003 • 9). Окрестности пульсара B1951+32 в оптике • В.Н. Комарова, В.Г. Курт, В.В. Соколов, Ю.А. Шибанов • Всеpоссийская Конфеpенция Астpофизика Высоких Энеpгий Сегодня и Завтpа • HEA-2003 • 10). Optical studies of neutron stars and their surroundings • at the 6m telescope of SAO RAS} • V.N. Komarova, T.A. Fatkhullin, V.G. Kurt, Yu.A. Shibanov • Physics of Neutron Stars-2005 • 11). OPTICAL SEARCH FOR COUNTERPARTS TO ISOLATED NEUTRON STARS AT THE 6METER TELESCOPE OF SAO RAS • V.N. Komarova, V.G. Kurt, Yu.A. Shibanov • Physics of Neutron Stars-2008

  29. We are asking! • We want to find anybody who want to study South Sky ! • Many thanks for your attention!

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