Optical Monitoring of NGC4151 During 110 Yearsтезисы доклада

Дата последнего поиска статьи во внешних источниках: 8 февраля 2017 г.

Работа с тезисами доклада


[1] Optical monitoring of ngc4151 during 110 years / В. Л. Окнянский, Н. В. Метлова, Н. А. Гусейнов, В. М. Лютый // 1 6 - th Odessa International Astronomical Gamow Conference - School “Astronomy and beyond: Astr o physics, Cosmology and Gravitation, Cosmomicrophysics, Radio - astronomy and Astrobiology” (Ukraine, Odessa, Chernomorka, 14 - 2 0 August, 20 16 ). — Одесская астрономическая обсерватория, ОНУ Одесса, Украина, 2016. — P. 19–19. We present the historical light curve of NGC 4151 for 1906 - 2016. The light curve (Oknyanskij and Lyuty, 2007) is primarily based on our published photoelectric data (1968 - 2007, about 1040 nightly mean measurements) and photographic estimates (mostly Odessa and Moscow plates taken in 1906 – 1982 (Oknyanskij, 1978, 1983), about 350 measurements). Additionally, we include all data obtained prior to 1968 (de Vaucouleurs and de Vaucouleurs, 1968; Sandage, 1967; Wisniewski and Kleinmann, 1968; Fitch et al., 1967) in total, 19 photoelectric observations from 1958 - 1967, reduced by us to the same diaphragm aperture as that used in our measurements) as well as photographic data (. Pacholczyk et al., 1983) (Harvard and Steward observatories' patrol plates taken in 1910 - 1968, about 210 measurements). The light curve includes our new photoelectrical and CCD data obtained during last 10 years at SAI and ShAO as well as other published data. All these data were reduced to an uniform photometric system. Applying Fourier (CLEAN algorithm) we have found periodic component ∼16 years in the 100 years light curve. 40 years ago about the same "period" was firstly reviled from Odessa's photometrical data (Oknyanskij, 1977,1978). This “period” seen in the light curve was then found independently in the spectral variability and interpreted as a case of the supermassive binary black hole (Bon et al. 2012). We interpret these circles as some accretion dynamic time.

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