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J/A+A/376/775 UBVRI and H-beta observations of 3C 390.3 (Shapovalova+ 2001)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table2.dat table4.dat table5.dat
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Query from: http://vizier.cds.unistra.fr/cgi-bin/VizieR?-source=J/A+A/376/775
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drwxr-xr-x 2 cats archive 4096 Jan 12 2023 [TAR file]
-rw-r--r-- 1 cats archive 493 Dec 19 2022 .message
-r--r--r-- 1 cats archive 7549 Sep 16 2001 ReadMe
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-r--r--r-- 1 cats archive 1745 Aug 15 2001 table2.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 922 Aug 15 2001 table4.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 720 Sep 14 2001 table5.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 10622 Aug 15 2001 tables.ps.gz [Uncompressed]
-r--r--r-- 1 cats archive 3301 Aug 15 2001 tables.tex.gz [Uncompressed]
Beginning of ReadMe :J/A+A/376/775 UBVRI and H-beta observations of 3C 390.3 (Shapovalova+ 2001)
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Intermediate resolution H-beta spectroscopy and photometric monitoring
of 3C 390.3. I. Further evidence of a nuclear accretion disk.
Shapovalova A.I., Burenkov A.N., Carrasco L., Chavushyan V.H.,
Doroshenko V.T., Dumont A.M., Lyuty V.M., Valdes J.R., Vlasuyk V.V.,
Bochkarev N.G., Collin S., Legrand F., Mikhailov V.P., Spiridonova O.I.,
Kurtanidze O., Nikolashvili M.G.
<Astron. Astrophys. 376, 775 (2001)>
=2001A&A...376..775S
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ADC_Keywords: Active gal. nuclei ; Photometry, UBVRI ; Photometry, Cousins
Keywords: galaxies: active - galaxies: Seyfert -
galaxies: individual (3C 390.3) - line: profiles
Abstract:
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 Hbeta emission
and the continuum flux varied by a factor of 3. Two large amplitude
outbursts, of different duration, in continuum and light were observed
i.e.: 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 i.e. 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 Hbeta wings and line core vary simultaneously, a behavior
indicative of predominantly circular motions in the broad line region.
Important changes of the Hbeta emission profiles were detected: at
times, we found profiles with prominent asymmetric wings, like those
normaly seen in Sy1s, while at other times, we observe profiles with
weak, almost symmetrical wings, similar to those of Sy1.8s.
Objects:
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RA (2000) DE Designation(s)
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18 42 09.0 +79 46 17 3C 390.3 = QSO 1845+796
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