1 / 14

Astrometric Goals of RadioAstron Mission in Moscow, November 2003

Explore astrophysics and astrometry breakthroughs via RadioAstron Mission in Moscow. Study black holes, cosmology, pulsars, and more with high-resolution technology.

jgermany
Download Presentation

Astrometric Goals of RadioAstron Mission in Moscow, November 2003

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. International Conference on RadioAstron MissionNovember 2003, MoscowASTROMETRIC GOALS OF THE RADIOASTRON MISSION V.E.ZHAROV1, A.E.RODIN2 , I.A.GERASIMOV1, Yu.P.ILYASOV2, K.V.KUIMOV1 1 Sternberg State Astronomical Institute, Russia 2 Puschino Radio Astronomical Observatory of Lebedev Physical Institute, Russia

  2. RADIOASTRON MISSION Orbital parameters • Orbital period p = 9.5 days • Semi-major axis a = 189 000 km • Eccentricity e = 0.853 • Perigee height H = 2000 km • Optimized launch date is March 15, 2006.

  3. The fringe sizes (in micro arc seconds) for the apogee

  4. Main scientific goals of the mission Astrophysics problems: • Study of radio galaxies, quasars, black holes, neutron stars with very high angular resolution; • cosmological evolution of compact extragalactic radio sources; • determination of fundamental cosmological parameters and study of gravitational lenses and the nature of dark matter. Astrometry problems: • Precise astrometry on level of several microarcseconds, determinations of the distances to pulsars as well as evaluations of their velocities by the measurements of parallax and proper motion; • link of kinematical and dynamical celestial reference frames; • measurements of secular aberration (motion of the Solar system in Galaxy); • search of the weak microlensing events – study of apparent motions of compact extragalactic radio sources; • direct measurements of distances using spherical wave front.

  5. Modern and future radio and optical catalogsRadio Optical

  6. Defining sources for improved ICRF and its distributionS/N=10 Smin~ 30 mJy • Defining sources with S>1 Ju S/N>30 st300 ps • Each source will be observed more than 100 times • Uncertainty of coordinate will be < 10 mas

  7. Weak Microlensing • Sazhin M.V., Zharov V.E., et al., Microarcsecond instability of the celestial reference frame. Monthly Notices of Roy. Astron. Soc., 300, p. 287-291 (1998)

  8. Pulsar list B0329+5403h 32 m 59.3816s±0.0005s 54o 34 ' 43.486 ' '±0.004 ' ' B0355+5403h 58m 53.713s±0.003s 54o13' 13.75 ' ' ±0.1' ' B0950+0809h 53m 09 .30s ±0.01s 07o55' 36.154 ' ‘±0.07 ' ' B1933+1619h 35m 47.824s±0.006s 16o 16 ' 40.07' ' ±0.27' ' B2021+51 20h 22m 49 .866s±0.005s 51o54 ' 50.302 ' ' ±0.01' ' Eulerian angles Link of the celestial frames DE200 and ICRFby pulsar positions VLBI Timing B0329+54 (Rodin, Sekido, 2000) (Downs, Reichly, 1983) B1257+12 (Bartel, Nunes, 1996) (Wolszczan, 1999) B1937+21 (Bartel, et.al, 1996) (Kaspi, et. al, 1994) B2021+51 (Campbell, et.al, 1996) (Downs, Reichly, 1983) Eulerian angles (mas) from DE200 to ICRF Finger, Folkner, Folkner et al., Rodin, Sekido, 1992 1994 2001 LLR & VLBI LLR & VLBI Pulsar VLBI & timing (TDA Progr. Report (A&A, 287, (AP–RASC Conf. Digest, 42–109, JPL, CA) p. 279–289) Chuo Univ., Tokyo, p.388) Ax 1 ± 3 – 2 ± 2 – 4 ± 2 Ay –10 ± 3–12 ± 3 –13 ± 2 Az – 4 ± 5 – 6 ± 3 –17 ± 6 List of reference pulsars

  9. Secular aberration • Solar system velocity V= 220 km/s, orbit radius R= 8,5 kpc maximum secular aberration = 2.5 min of arc • Annual change of the direction of the Solar system velocity = 50 mas (secular aberration per year = 4 mas )

  10. Name R.A. Dec. Gal. b Gal. l 1954+513 D 19 55 42.738273 51 31 48.54623 11.7568385.29847 2005+642 O 20 6 17.694616 64 24 45.41805 16.73457 97.64550 2021+614 O 20 22 6.681695 61 36 58.80479 13.77531 96.08284 2030+547 D 20 31 47.958562 54 55 3.14060 8.98830 91.12945 2037+511 D 20 38 37.034755 51 19 12.66269 6.04010 88.80853 2100+468 C 21 2 17.056050 47 2 16.25468 0.33862 87.94161 2200+420 O 22 2 43.291381 42 16 39.97998 -10.44116 92.58958 2201+315 O 22 3 14.975796 31 45 38.27004 -18.77888 85.95683 2214+350 C 22 16 20.009936 35 18 14.18072 -17.62088 90.50210 0809-493 C 08 11 8.802530 -49 29 43.50928 -8.60913 -95.20763 0823-500 C 08 25 26.869117 -50 10 38.48735 -7.06041 -93.35106 0831-445 C 08 33 22.315631 -44 41 38.71463 -2.77977 -97.04408 0833-450 C 08 35 20.655289 -45 10 35.15391 -2.78726 -96.44804 0920-397 C 09 22 46.418275 -39 59 35.06753 7.19027 -94.64841 0959-443 C 10 1 59.907283 -44 38 0.60564 8.48927 -86.06662 1004-500 C 10 6 14.009559 -50 18 13.47089 4.37000 -82.07913 Name R.A. Dec. Gal. b Gal. l 0008-264 C 0 11 1.246752 -26 12 33.37686 -80.92652 36.45592 0104-408 O 1 6 45.107969 -40 34 19.96036 -76.18917 -69.33453 0118-272 C 1 20 31.663311 -27 1 24.65133 -83.52463 -146.33661 0135-247 D 1 37 38.346378 -24 30 53.88526 -79.28429 -158.60686 0150-334 C 1 53 10.121676 -33 10 25.86226 -75.37042 -118.93763 1147+245 D 11 50 19.212173 24 17 53.83503 75.95562 -138.85148 1155+251 D 11 58 25.787505 24 50 17.96369 77.87572 -139.14904 1156+295 C 11 59 31.833914 29 14 43.82693 78.37433 -160.58637 1213+350 D 12 15 55.601049 34 48 15.22053 79.19912 165.48024 1215+303 D 12 17 52.081987 30 7 0.63625 82.05288 -171.12516 1219+285 C 12 21 31.690512 28 13 58.50014 83.28802 -158.26477 1226+373 D 12 28 47.423662 37 6 12.09578 78.93803 147.14245 1240+381 C 12 42 51.369079 37 51 0.02510 79.12757 131.94832 1257+145 D 13 0 20.918799 14 17 18.53107 76.99325 -47.43343 1308+326 D 13 10 28.663845 32 20 43.78295 83.34593 85.70205 1315+346 C 13 17 36.494181 34 25 15.93257 80.79743 86.93673 1323+321 C 13 26 16.511396 31 54 9.51991 81.04764 67.23374 1324+224 D 13 27 0.861311 22 10 50.16306 80.52740 3.38099 1328+307 C 13 31 8.288145 30 30 32.95986 80.67466 56.52436 1338+381 C 13 40 22.951763 37 54 43.83468 75.10274 82.35931 List of Sources for the Secular Aberration Measurement

  11. CONCLUSION • Generation of precise fundamental celestial reference frame • Link of kinematical and dynamical celestial reference frames • Precise measurement of radio telescopes positionsin geocentric terrestrial reference frame • Parallax and proper motion measurements of pulsars • Tests of Theory of Relativity • measurements of secular aberration (motion of the Solar system).

More Related