Zobrazeno 1 - 10
of 28
pro vyhledávání: '"V. S. Tamazian"'
Publikováno v:
Astrophysics. 43:162-169
Autor:
V. S. Tamazian
Publikováno v:
Astronomy and Astrophysics Supplement Series. 139:537-543
Several H I related astrophysical parameters such as neutral hydrogen total mass and hydrogen mean projected density, indicative total mass as well as usual ratios , and for 23 galaxies from Kazarian lists are derived. Their variation ranges are rath
Publikováno v:
Astronomy and Astrophysics Supplement Series. 126:471-478
The 21-cm neutral hydrogen line has been measured for the rst time in 39 non-Seyfert type galax- ies from Kazarian list, with the Nan cay radiotelescope. The line proles, widths at 20% and 50% of the peak in- tensity, radial velocities as well as tot
Publikováno v:
AIP Conference Proceedings.
Publikováno v:
AIP Conference Proceedings.
Publikováno v:
Astrophysics. 37:1-5
The results of new spectral observations of the Seyfert component of the close binary galaxy with UV excess Kaz 163 are presented. Two new spectra have been obtained: with the 3-m telescope of Lick Observatory in 1986 and with the 1.8-m telescope of
Autor:
M. A. Kazarian, V. S. Tamazian
Publikováno v:
Astrophysics. 36:222-228
Autor:
N. D. Melikian, V. S. Tamazian, J. A. Docobo, A. A. Karapetian, G. S. Kostandyan, A. L. Samsonyan, Y. Y. Balega
Publikováno v:
AIP Conference Proceedings.
Results of spectral observations of the eclipsing binary star RY Sct carried out in 2005 and 2009 with the 2.6 m telescope of V.A. Ambartsumian Byurakan Astrophysical Observatory are presented. While RY Sct needs a further detailed study, some import
Publikováno v:
AIP Conference Proceedings.
We performed exhaustive work during the past 30 years in the Astronomical Observatory of the University of Santiago de Compostela (called Ramon Maria Aller since 1981). In this communication, I explain all the necessary efforts made to obtain the cur
Publikováno v:
AIP Conference Proceedings.
The WIYN Observatory speckle program has been in operation since 1997, taking data mainly with a large‐format, low‐noise CCD detector. However, new instrumentation, first used in 2008, has created the possibility to use two detectors simultaneous