The variability of 3C 390.3

Barr, P.; Pollard, G. S. G.; Sanford, P. W.; Ives, J. C.; Ward, M. J.; Hine, R. G.; Longair, M. S.; Penston, M. V.; Boksenberg, A.; Lloyd, C.

doi:10.1093/mnras/193.3.549

Cited by 27 publications

(24 citation statements)

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“…A number of possible models have been suggested to explain double-peaked line profiles: supermassive binary black holes (Gaskell 1996), outflowing biconical gas streams (Zheng 1996), or emission from an accretion disk (Perez et al 1988;Rokaki et al 1992). The strong variability of this object, in both continuum and emission lines is well known (Barr et al 1980(Barr et al , 1983Yee & Oke 1981;Netzer 1982;Clavel & Wamsteker 1987;Veilleux & Zheng 1991;Wamsteker et al 1997;O'Brien et al 1998;Dietrich et al 1998;Shapovalova et al 2001;Sergeev et al 2002;Tao et al 2008;Gupta et al 2009). The object is also a highly variable X-ray source, which has a spectrum exhibiting a broad Fe Kα line (Inda et al 1994;Eracleous et al 1996;Wozniak et al 1998).…”

Section: Introductionmentioning

confidence: 78%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Shapovalova¹,

Popovic²,

Буренков³

et al. 2010

A&A

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Context. We present the results of the long-term (1995)(1996)(1997)(1998)(1999)(2000)(2001)(2002)(2003)(2004)(2005)(2006)(2007) spectral monitoring of the broad-line radio galaxy 3C 390.3, a well known AGN with double-peaked broad emission lines, usually assumed to be emitted from an accretion disk. Aims. To explore dimensions and structure of the BLR, we analyze the light curves of the broad Hα and Hβ line fluxes and the continuum flux. To detect variations in the BLR, we analyze the Hα and Hβ line profiles, as well as the change in the line profiles during the monitoring period. Methods. We attempt first to find a periodicity in the continuum and Hβ light curves, finding that there is a high probability of measuring quasi-periodical oscillations. Using the line shapes and their characteristics (such as e.g., peak separation and their intensity ratio, or FWHM) of broad Hβ and Hα lines, we discuss the structure of the BLR. We also cross-correlate the continuum flux with Hβ and Hα lines to determine the dimensions of the BLR. Results. During the monitoring period, we found that the broad emission component of the Hα and Hβ lines, and the continuum flux varied by a factor of ≈4−5. We also detected different structure in the line profiles of Hα and Hβ. An additional central component appears to be present and superimposed on the disk emission. In the period of high activity (after 2002), Hβ became broader than Hα and red wing of Hβ was higher than that of Hα. We detected time lags of ∼95 days between the continuum and Hβ flux, and about 120 days between the continuum and Hα flux. Conclusions. Variations in the line profiles, as well as correlation between the line and continuum flux during the monitoring period, are consistent with a disk origin of the broad lines and the possible contribution of some additional region and/or some kind of perturbation in the disk.

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Section: Introductionmentioning

confidence: 78%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Shapovalova¹,

Popovic²,

Буренков³

et al. 2010

A&A

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“…The strong variability of this object, both in the continuum light and the emission lines is well known (Barr et al 1980;Yee & Oke 1981;Netzer 1982;Barr et al 1983;Penston & Perez 1984;Clavel & Wamsteker 1987;Shapovalova et al 1996;Zheng 1996;Wamsteker et al 1997;Dietrich et al 1998;O'Brien et al 1998). The object is also a highly variable X-ray source, with a spectrum showing a broad Fe Kα line (Inda et al 1994;Eracleous et al 1996;Wozniak et al 1998).…”

Section: Introductionmentioning

confidence: 79%

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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“…Such pro les draw particular attention as they may be the signature of a relativistically rotating disk (P erez et al 1988). The object's high variability in the continuum as well as in the emission lines has been well{known (Barr et al 1980;Yee & Oke 1981;Netzer 1982;Barr, Willis, & Wilson 1983;Penston & P erez 1984). The narrow emission lines in 3C 390.3 are formed in a compact region of moderate density ( 10 6 cm 3 , Osterbrock et al 1975) and { 3 { exhibit considerable variations within several years (Clavel & Wamsteker 1987;Zheng et al 1995).…”

Section: Introductionmentioning

confidence: 92%

Study of Time Varitions of UV Continuum and Emission Lines in 3C 390.3

Zheng¹

1996

The Astronomical Journal

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Based on the IUE SWP spectra obtained between 1978 and 1994, the variations of the UV continuum and the Ly and C iv emission lines of the broad{line radio galaxy 3C 390.3 are studied. The UV continuum between 1220 and 1990 A has varied considerably. In 1991 August, the ux at 1360 A reached a maximum level of 1:3 10 14 erg cm 2 s 1 A 1 , 27 times as high as its minimum level. At 1850 A, the continuum varies by a factor of 12. Signi cant variations are frequently observed in periods as short as one month.

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The variability of 3C 390.3

Cited by 27 publications

References 0 publications

Spectral optical monitoring of 3C 390.3 in 1995–2007

Spectral optical monitoring of 3C 390.3 in 1995–2007

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

Study of Time Varitions of UV Continuum and Emission Lines in 3C 390.3

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