Radioastron broke all records for the angular resolution

  • Radioastron.  Spektr-R
  • Radioastron. Spektr-R

In the early part of the scientific program of the mission, "RadioAstron" studied three groups of space objects: quasars — nuclei of distant galaxies, pulsars — neutron stars in our galaxy, masers — the education of stars in our galaxy. At the beginning of 2013 provided new important results.

 


"RadioAstron" and records

With the help of the "RadioAstron" managed to break all the world records on the angular resolution by implementing the most keen eye for history. Interference signals from distant galaxies, ultra-confident registered on the basis of Earth-Space to 20 diameters of the Earth! In particular, it was possible to beat the record set in 2012 at ground interferometer observations at a wavelength of 1.3 mm. Achieved an angular resolution of 40 microseconds of arc.

  • Fig.  1 Record for detecting ultra nuclei of active galaxies in the project "RadioAstron."  In traditional response diagram shows the value depending on the delay (delay) and frequency interference (fringe rate).  Left - the quasar 3C273, range 18 cm, base diameter 13.5 interferometer Earth RadioAstron-Aresibo/SShA, January 20, 2013 In the center - the active galaxy BL Lacertae, the range of 6 cm, the base of the interferometer 19 Earth diameters, РадиоАстрон-Эффельсберг/Германия, November 28, 2012 Right - quasar 3C273, the range of 1.3 cm, the base of the interferometer 8 diameter of the Earth, RadioAstron-GBT/SShA, February 2, 2013
  • Fig. 1 Record for detecting ultra nuclei of active galaxies in the project "RadioAstron." In traditional response diagram shows the value depending on the delay (delay) and frequency interference (fringe rate). Left — the quasar 3C273, range 18 cm, base diameter 13.5 interferometer Earth RadioAstron-Aresibo/SShA, January 20, 2013 In the center — the active galaxy BL Lacertae, the range of 6 cm, the base of the interferometer 19 Earth diameters, РадиоАстрон-Эффельсберг/Германия, November 28, 2012 Right — quasar 3C273, the range of 1.3 cm, the base of the interferometer 8 diameter of the Earth, RadioAstron-GBT/SShA, February 2, 2013


"RadioAstron" and the interstellar medium

The modern theory of the interstellar plasma in our galaxy predicted that the long-wavelength radio emission from pulsars and quasars will be eroded and, as a result, "RadioAstron" will not be able to enroll their signals over large ground-space bases for wavelengths 18 and 92 cm results are totally refuted this prediction (see Figures 1 and 2), broke up with the theory in 10100 times!

This discovery completely changes the existing understanding of the structure of the interstellar plasma in our galaxy.

 

  • Fig.  2: Structure of the interference response distant pulsar V0329 +55 at a distance of 6000 light years.  For the source, not subjected to the effects of scattering on this diagram should be a single peak.  In fact, there is a close band interference responses, each of which corresponds to the peak of the interference of the rays passing through its combination of refraction by plasma inhomogeneities.
  • Fig. 2: Structure of the interference response distant pulsar V0329 +55 at a distance of 6000 light years. For the source, not subjected to the effects of scattering on this diagram should be a single peak. In fact, there is a close band interference responses, each of which corresponds to the peak of the interference of the rays passing through its combination of refraction by plasma inhomogeneities.


"RadioAstron" and galactic water

Detected water maser emission from an ultra-compact clouds of 8 diameters of the Sun, in the formation of massive stars W3IRS5, located at a distance of 5.5 thousand light-years in the Perseus spiral arm of our galaxy (see Figures 3 and 4).

This result will allow scientists to better understand the formation of massive stars.

 

  • Fig.  3: Interference response from the star-forming region W3IRS5 Observations RadioAstron with Spanish telescope Yebes.  On the vertical axis: the amplitude of the correlated signal.  Horizontal axis: the residual value of the frequency and spectral frequency interference.
  • Fig. 3: Interference response from the star-forming region W3IRS5 Observations RadioAstron with Spanish telescope Yebes. On the vertical axis: the amplitude of the correlated signal. Horizontal axis: the residual value of the frequency and spectral frequency interference.

Press Service of the Russian Federal Space Agency and the Physical Institute Astro Space Center. Lebedev, Russian Academy of Sciences (ASC FIAN)

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