A possible verification of Arp's hypothesis

Babadzhanyants, M. K.

doi:10.1007/bf01002580

Cited by 1 publication

(2 citation statements)

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“…The image reduction process included bias, flat-field corrections, cosmic ray removal, 2D wavelength linearization, background subtraction, stacking of the spectra for every set up, and flux calibration. Neizvestny (1986); large filled circles -photometry (present paper); open squares - Yee & Oke (1981); small filled circles - Babadzhanyants et al (1973Babadzhanyants et al ( , 1974Babadzhanyants et al ( , 1975Babadzhanyants et al ( , 1976Babadzhanyants et al ( , 1984; crosses - Cannon et al (1971), Scott et al (1976), Selmes et al (1975), Pica et al (1980); plusses -spectral continuum (present paper); open triangles - Dietrich et al (1998); filled trianglesspectral cont. from Perez et al (1988) and Lawrence et al (1996).…”

Section: Observationsmentioning

confidence: 85%

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Intermediate Resolution Hβ Spectroscopy and Photometric Monitoring of 3C 390.3. I. Further Evidence of a Nuclear Accretion Disk

Shapovalova¹,

Буренков²,

Spiridonova³

et al. 2002

International Astronomical Union Colloquium

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We have monitored the AGN 3C 390.3 between 1995 and 2000. A historical B-Band light curve dating back to 1966, shows a large increase in brightness during 1970 -1971, followed by a gradual decrease down to a minimum in 1982. During the 1995-2000 lapse the broad Hβ emission and the continuum flux varied by a factor of ≈ 3. Two large amplitude outbursts, of different duration, in continuum and Hβ light were observed ie.: in October 1994 a brighter flare that lasted ≈1000 days and in July 1997 another one that lasted ≈ 700 days were detected. The response time lag of the emission lines relative to flux changes of the continuum, has been found to vary with time ie. during 1995-1997 a lag of about 100 days is evident, while during 1998-1999 a double valued lag of ≈ 100 days and ≈ 35 days is present in our data. The flux in the Hβ wings and line core vary simultaneously, a behavior indicative of predominantly circular motions in the BLR. Important changes of the Hβ emission profiles were detected: at times, we found profiles with prominent asymmetric wings, as those normaly seen in Sy1s, while at other times, we observe profiles with weak almost symmetrical wings, similar to those of Sy1.8s. We further dismiss the hypothesis that the double peaked Hβ profiles in this object originate in a massive binary BH. Instead, we found that the radial velocity difference between the red and blue bumps is anticorrelated with the light curves of Hβ and continuum radiation. This implies that the zone that contributes with most of the energy to the emitted line, changes in radius within the disk. The velocity difference increases, corresponding to smaller radii, as the continuum flux decreases. When the continuum flux increases the hump velocity difference decreases. These transient phenomena are expected to result from the variable accretion rate close to the central source. The optical continuum and the Hβ flux variations might be related to changes in X-ray emission modulated by a variable accretion rate, changing the surface temperature of the disk, as a result of a variable X-ray irradiation ( Ulrich, 2000). Theoretical Hβ profiles were computed for an accretion disk, the observed profiles are best reproduced by an inclined disk (25 • ) whose region of maximum emission is located roughly at 200 Rg. The mass of the black hole in 3C 390.3, estimated from the reverberation analysis is Mrev ≈ 2.1 × 10 9 M ⊙ , 5 times larger than previous estimates (Wandel et al.1999).

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Section: Observationsmentioning

confidence: 85%

“…We also make use of the photographic photometry available, ie. 1967-1980 from Cannon et al (1971); Babadzhanyants et al (1973;1974;1975;1984); Selmes et al (1975); Scott et al (1976); Pica et al (1980). In order to increase their accuracy, the photographic observations were averaged in 5 day bins.…”

Section: A Historical B Light Curvementioning

confidence: 99%