J/MNRAS/509/831 NLS1s and BLAGNs PAH (Lakicevic+, 2022)
AGN orientation through the spectroscopic correlations and
model of dusty cone shell.
Lakicevic M., Kovacevic-Dojcinovic J., Popovic L.C.
<Mon. Not. R. Astron. Soc., 509, 831-843>
=2022MNRAS.509..831L 2022MNRAS.509..831L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Spectroscopy ; Photometry, H-beta ;
Infrared sources
Keywords: galaxy: structure - galaxies: active - quasars: emission lines -
galaxies: Seyfert
Abstract:
The differences between Narrow Line Seyfert 1 galaxies (NLS1s) and
Broad Line AGNs (BLAGNs) are not completely understood; it is thought
that they may have different inclinations and/or physical
characteristics. The FWHM(Hβ)-luminosities correlations are found
for NLS1s and their origin is the matter of debate. Here we
investigated the spectroscopic parameters and their correlations
considering a dusty, cone model of AGN. We apply a simple conical dust
distribution (spreading out of broad line region, BLR), assuming that
the observed surface of the model is in a good correlation with MIR
emission. The dusty cone model in combination with a BLR provides the
possibility to estimate luminosity dependence on the cone inclination.
The FWHM(Hβ)-luminosities correlations obtained from model in
comparison with observational data show similarities which may
indicate the influence of AGN inclination and structure to this
correlation. An alternative explanation for FWHM(Hβ)-luminosities
correlations is the selection effect by the black hole mass. These
FWHM(Hβ)-luminosities correlations may be related to the
starburst in AGNs, as well. The distinction between spectral
properties of the NLS1s and BLAGNs could be caused by multiple
effects: beside physical differences between NLS1s and BLAGNs (NLS1s
have lighter black hole mass than BLAGNs), inclination of the conical
AGN geometry may have important role as well, where NLS1s may be seen
in lower inclination angles.
Description:
We explored the influence of calculated inclination (i) to the
luminosities of the Type 1 AGNs using (1) a sample model of dusty cone
shells, and/or (2) the selection effect by the BH mass. Inclinations
of AGNs are found from optical data.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 80 56 Name of object, coordinates, and redshifts,
FWHM(Hβ) and equivalent width of PAH
at 7.7um
tablea2.dat 109 56 Name of object, PAH fraction, L6, L12
and log(MBH)
tablea3.dat 96 56 Name of object, RBLR, δRBLR, calculated
inclination and luminosity at the peak of
the 7.7um feature
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Name of object
16- 25 F10.6 deg RAdeg Right ascension (J2000)
27- 36 F10.6 deg DEdeg Declination (J2000)
38- 42 F5.3 --- z Redshift
44- 48 I5 km/s FWHMHb Hβ FWHM
50- 52 A3 --- r_FWHMHb Reference for FWHMHb (G1)
54- 59 F6.2 km/s dFWHMHb Hβ FWHM dispersion
61- 63 A3 --- r_dFWHMHb Reference for dFWHMHb (G1)
65- 69 F5.1 nm EW7.7 ?=- Equivalent width of PAH at 7.7um
71- 80 F10.7 nm e_EW7.7 ?=- Equivalent width of PAH at 7.7um error
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Name of object
16- 25 E10.8 --- RPAH PAH fraction
27- 36 F10.8 --- e_RPAH PAH fraction error
38- 50 E13.9 10-7W nuLnu6 ?=- Luminosity at 6um
52- 64 E13.9 10-7W e_nuLnu6 ?=- Luminosity at 6um error
66- 78 E13.9 10-7W nuLnu12 Luminosity at 12um
80- 92 E13.9 10-7W e_nuLnu12 Luminosity at 12um error
94- 97 F4.2 [Msun] log(MBH) Black hole mass
99-105 F7.5 [Msun] e_log(MBH) Black hole mass error
107-109 A3 --- r_log(MBH) Reference for log(MBH) (G1)
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Name of object
16- 20 F5.1 --- Rblr BLR radius (in day light unit)
22- 24 A3 --- r_Rblr Reference for Rblr (G1)
26- 30 F5.2 --- dRblr BLR radius error (in day light unit)
32- 34 A3 --- r_dRblr Reference for dRblr (G1)
36- 52 F17.14 deg i Inclination
54- 64 F11.9 deg e_i Inclination error
66- 70 A5 --- Type Type
72- 76 A5 --- r_Type Reference for Type
78- 86 F9.6 [10-7W] log(nuL7.7) ?=- Luminosity at the peak of
the 7.7um feature
88- 96 F9.6 [10-7W] e_log(nuL7.7) ?=- Luminosity at the peak of
the 7.7um feature error
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Global notes:
Note (G1): References as follows:
A19 = Afanasiev et al. (2019MNRAS.482.4985A 2019MNRAS.482.4985A)
Z02 = Zhang & Wu (2002ChJAA...2..487Z 2002ChJAA...2..487Z)
S12 = Shapovalova et al. (2012ApJS..202...10S 2012ApJS..202...10S)
B10 = Bian et al., 2010ApJ...718..460B 2010ApJ...718..460B
B15 = Berton et al., 2015A&A...578A..28B 2015A&A...578A..28B
G99 = Goncalves et al., 1999A&A...341..662G 1999A&A...341..662G
K04 = Klimek et al., 2004ApJ...609...69K 2004ApJ...609...69K
M16 = Marinello et al., 2016ApJ...820..116M 2016ApJ...820..116M
M93 = Marziani et al., 1993ApJ...410...56M 1993ApJ...410...56M
Mar14 = Markowitz et al., 2014MNRAS.439.1403M 2014MNRAS.439.1403M
N09 = Nikolajuk et al., 2009MNRAS.394.2141N 2009MNRAS.394.2141N
S10 = Sani et al., 2010MNRAS.403.1246S 2010MNRAS.403.1246S
VC10 = Veron-Cetty & Veron, 2010A&A...518A..10V 2010A&A...518A..10V, Cat. VII/258
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Aug-2024