J/MNRAS/422/3268 Relation between X-ray and optical spectra (Jin+, 2012)
A combined optical and X-ray study of unobscured type 1 active galactic nuclei.
II. Relation between X-ray emission and optical spectra.
Jin C., Ward M., Done C.
<Mon. Not. R. Astron. Soc., 422, 3268-3284 (2012)>
=2012MNRAS.422.3268J 2012MNRAS.422.3268J
ADC_Keywords: Active gal. nuclei ; X-ray sources
Keywords: accretion, accretion discs - galaxies: active - galaxies: nuclei
Abstract:
In this second paper in a series of three, we study the properties of
the various emission features and underlying continuum in the optical
spectra of type 1 active galactic nuclei (AGNs) by using the
unobscured hard X-ray emission as a diagnostic. We introduce the use
of the "correlation spectrum technique" (CST) for the first time. We
use this to show the strength of the correlation between the hard
X-ray luminosity and each wavelength of the optical spectrum. This
shows that for broad-line Seyfert 1 galaxies all the strong emission
lines (the broad component of Hα and Hβ, [NeIII]
λλ3869/3967, [OI] λλ6300/6364, [OII]
λλ3726/3729 and [OIII] λλ4959/5007) and
the optical underlying continuum all strongly correlate with the hard
X-ray emission. In contrast, the narrow-line Seyfert 1 galaxies show a
stronger correlation in the optical continuum but a weaker correlation
in the lines.
Description:
The sample used in this paper is a nearby unobscured type 1 AGN sample
derived from the cross-correlation of the 2XMMi and SDSS DR7
catalogues.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 135 36 Spearman's Rank Correlation Coefficients of SED
components vs. Hα, Hβ and [OIII]5007
line parameters.
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Param Line parameter designation
18- 23 A6 --- Comp Component (1)
25- 29 F5.2 --- Disc1r Spearman's rank correlation coefficient,
Disc composant, SED component luminosity
31- 32 I2 --- Disc1d Logarithm of the significance level of being
random distribution, Disc composant,
SED component luminosity (2)
34- 38 F5.2 --- Comp1r Spearman's rank correlation coefficient,
soft X-ray Comptonisation component,
SED component luminosity
40- 41 I2 --- Comp1d Logarithm of the significance level of being
random distribution, soft X-ray Comptonisation
component, SED component luminosity (2)
43- 47 F5.2 --- PL1d Spearman's rank correlation coefficient,
hard X-ray Comptonisation component composant,
SED component luminosity
49- 51 I3 --- PL1r Logarithm of the significance level of being
random distribution, hard X-ray Comptonisation
component composant, SED component luminosity (2)
53- 57 F5.2 --- C+P1d Spearman's rank correlation coefficient,
sum of soft and hard X-ray Comptonisation
emission (i.e. corona emission),
SED component luminosity
59- 61 I3 --- C+P1r Logarithm of the significance level of being
random distribution, sum of soft and hard
X-ray Comptonisation emission (i.e. corona
emission), SED component luminosity (2)
63- 67 F5.2 --- Bol1d Spearman's rank correlation coefficient,
Bolometric composant, SED component luminosity
69- 71 I3 --- Bol1r Logarithm of the significance level of being
random distribution, Bolometric composant,
SED component luminosity (2)
73- 77 F5.2 --- Disc2r Spearman's rank correlation coefficient,
Disc composant, SED component fraction
(fraction of each component in the bolometric
luminosity)
79- 80 I2 --- Disc2d Logarithm of the significance level of being
random distribution, Disc composant,
SED component fraction (fraction of each
component in the bolometric luminosity) (2)
82- 86 F5.2 --- Comp2r Spearman's rank correlation coefficient,
soft X-ray Comptonisation component,
SED component fraction (fraction of each
component in the bolometric luminosity)
88- 89 I2 --- Comp2d Logarithm of the significance level of being
random distribution, soft X-ray Comptonisation
component, SED component fraction (fraction of
each component in the bolometric luminosity) (2)
91- 95 F5.2 --- PL2d Spearman's rank correlation coefficient,
hard X-ray Comptonisation component composant,
SED component fraction (fraction of each
component in the bolometric luminosity)
97- 98 I2 --- PL2r Logarithm of the significance level of being
random distribution, hard X-ray Comptonisation
component composant, SED component fraction
(fraction of each component in the bolometric
luminosity) (2)
100-104 F5.2 --- C+P2d Spearman's rank correlation coefficient,
sum of soft and hard X-ray Comptonisation
emission (i.e. corona emission), SED component
fraction (fraction of each component in the
bolometric luminosity)
106-107 I2 --- C+P2r Logarithm of the significance level of being
random distribution, sum of soft and hard
X-ray Comptonisation emission (i.e. corona
emission), SED component fraction (fraction of
each component in the bolometric luminosity) (2)
109-113 F5.2 --- Gammar Spearman's rank correlation coefficient,
Γ2-10keV, 2-10keV energy band
115-116 I2 --- Gammad Logarithm of the significance level of being
random distribution, Γ2-10keV,
2-10keV energy band (2)
118-122 F5.2 --- Luminr Spearman's rank correlation coefficient,
Luminosity, 2-10keV energy band
124-126 I3 --- Lumind Logarithm of the significance level of being
random distribution, Luminosity,
2-10keV energy band (2)
128-132 F5.2 --- fracd Spearman's rank correlation coefficient,
fraction of 2-10keV luminosity related to
bolometric luminosity, 2-10keV energy band
134-135 I2 --- fracr Logarithm of the significance level of being
random distribution, fraction of 2-10keV
luminosity related to bolometric luminosity,
2-10keV energy band (2)
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Note (1): Component signification as follows:
NC = narrow component
IC = intermediate component
BC = broad component
IC+BC = intermediate plus broad component
(i.e. narrow component subtracted)
Whole = whole emission line
Centre = central lower velocity shift component (for [OIII]5007)
Blue = higher velocity shift component (often shows blue shift)
(for [OIII]5007)
Note (2): significance of being random means that a strong correlation
is represented by a small value of the significance level.
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History:
From electronic version of the journal
References:
Jin et al., Paper I 2012MNRAS.420.1825J 2012MNRAS.420.1825J
Jin et al., Paper III 2012MNRAS.425..907J 2012MNRAS.425..907J
(End) Patricia Vannier [CDS] 23-Jan-2013