J/MNRAS/448/2879 Spectropolarimetry of active galaxy 3C 390.3 (Afanasiev+, 2015)
Spectropolarimetric monitoring of active galaxy 3C 390.3 with 6-m telescope
SAO RAS in the period 2009-2014.
Afanasiev V.L., Shapovalova A.I., Popovic L.C., Borisov N.V.
<Mon. Not. R. Astron. Soc., 448, 2879-2889 (2015)>
=2015MNRAS.448.2879A 2015MNRAS.448.2879A (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Galaxies, Seyfert ; Spectroscopy ;
Balmer lines ; Polarization
Keywords: line: profiles - galaxies: active - quasars: individual: 3C 390.3
Abstract:
Here we present the spectropolarimetric observations of the radio-loud
active galaxy 3C 390.3 in the period 2009-2014 (24 epochs). The galaxy
has been observed with the 6-m telescope of Special Astrophysical
Observatory of the Russian Academy of Science (SAO RAS) using the
Spectral Camera with Optical Reducer for Photometric and
Interferometric Observations (SCORPIO) spectropolarimeter. We explore
the variability and lags in the polarized light of the continuum and
broad Hα line. We give the Stokes parameters Q, U, degree of
linear polarization P and the position angle of the polarization
plane, φ, for 24 epochs. We find a small lag (10-40 d) between the
unpolarized and polarized continuum that is significantly smaller than
the estimated lags for the unpolarized broad emission lines
(lag(Hα) ∼138-186 and lag(Hβ) ∼60-79 d). This shows that
the region of the variable polarized continuum is significantly
smaller than the broad line region, indicating that a part of the
polarized continuum is coming from the jet. The lag of the polarized
light in the Hα line (89-156 d) indicates an additional
component to the disc one that has an outflowing velocity of ~-1200 km/s.
This region seems to depolarize the polarized broad Hα line
emitted from the disc and scattered in the inner part of the torus.
Description:
In the period 2009-2014 we performed spectropolarimetric monitoring
of the broad line radio galaxy 3C 390.3 (24 epochs) with the 6-m
telescope of SAO RAS using the modified spectrograph Spectral Camera
with Optical Reducer for Photometric and Interferometric Observations
(SCORPIO; Afanasiev & Moiseev 2005AstL...31..194A 2005AstL...31..194A; 2011BaltA..20..363A 2011BaltA..20..363A)
in the mode of the spectropolarimetry and polarimetry in the spectral
range 4000-8000Å with the spectral resolution 4-10Å.
Objects:
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RA (ICRS) DE Designation(s)
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18 42 08.99 +79 46 17.1 3C 390.3 = ICRF J184208.9+794617
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 97 24 *Spectropolarimetric observation
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Note on table2.dat:
Observed Stokes parameters Q and U of the continuum, degree of polarization and
polarization angle, fluxes in continuum, broad lines Hβ and Hα,
polarized broad Hα and its shift.
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See also:
J/ApJS/115/185 : 3C 390.3 BVRI and H photometry (Dietrich+, 1998)
J/A+A/376/775 : UBVRI and H-beta observations of 3C 390.3 (Shapovalova+ 2001)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- JD Julian Date (JD+240000)
7- 11 F5.2 % Q5500 Q Stoke parameter
13- 16 F4.2 % e_Q5500 Uncertainty in Q5500
18- 22 F5.2 % U5500 U Stoke parameter
24- 27 F4.2 % e_U5500 Uncertainty in U5500
29- 32 F4.2 % P5500 Degree of linear polarization at 5500Å
(1)
34- 37 F4.2 % e_P5500 Uncertainty in P5500
39- 43 F5.1 deg PA Polarization angle at 5500Å (1)
45- 47 F3.1 deg e_PA Uncertainty in PA
49- 52 F4.2 10-17W/m2/nm F5100 Continuum flux at 5100Å
(in 10-15erg/cm2/s/Å)
54- 57 F4.2 10-17W/m2/nm e_F5100 Uncertainty in F5100
59- 62 F4.2 10-16W/m2 FHb Broad Hβ line flux
(in 10-13erg/cm2/s)
64- 67 F4.2 10-16W/m2 e_FHb Uncertainty in FHb
69- 72 F4.2 10-15W/m2 FHa Broad Hα line flux
(in 10-12erg/cm2/s)
74- 77 F4.2 10-15W/m2 e_FHa Uncertainty in FHa
79- 82 F4.2 10-17W/m2 FHapol Polarized Hα flux
(in 10-14erg/cm2/s)
84- 87 F4.2 10-17W/m2 e_FHapol Uncertainty in FHapol
89- 93 I5 km/s DeltaV Difference between the systematic and
polarized line velocity (Vsys-Vpol)
for the broad Hα line
95- 97 I3 km/s e_DeltaV Uncertainty in DeltaV
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Note (1): The polarization parameters have been corrected for the ISM
polarization.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 29-Nov-2017