J/MNRAS/478/4068 BLAGNs and NLS1s characteristics. (Lakicevic+, 2018)
Narrow vs. broad-line Seyfert 1 galaxies:
X-ray, optical, and mid-infrared AGN characteristics.
Lakicevic M., Popovic L.C., Kovacevic-Dojcinovic J.
<Mon. Not. R. Astron. Soc., 478, 4068-4083 (2018)>
=2018MNRAS.478.4068L 2018MNRAS.478.4068L (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; QSOs ; Infrared sources ; X-ray sources ;
Optical
Keywords: galaxies: active - quasars: emission lines
Abstract:
investigated narrow-line Seyfert 1 galaxies (NLS1s) at optical,
mid-infrared (MIR), and X-ray wavelengths, comparing them to the
broad-line active galactic nuclei (BLAGNs). We found that black hole
mass, coronal line luminosities, X-ray hardness ratio and X-ray, and
optical and MIR luminosities are higher for the BLAGNs than for NLS1s,
while policyclic aromatic hydrocarbon (PAH) contribution and the
accretion rates are higher for NLS1s. Furthermore, we found some
trends among spectral parameters that NLS1s have and BLAGNs do not
have. The evolution of FWHM(Hβ) with the luminosities of MIR and
coronal lines, continuum luminosities, PAH contribution, Hβ broad
line luminosity, FWHM[OIII], and EW(HβNLR) are important trends
found for NLS1s. That may contribute to the insight that NLS1s are
developing AGNs, growing their black holes, while their luminosities
and FWHM(Hβ) consequently grow, and that BLAGNs are mature,
larger objects of slower and/or different evolution. Black hole mass
is related to PAH contribution only for NLS1s, which may suggest that
PAHs are more efficiently destroyed in NLS1s.
Description:
We investigated the differences in the optical, X-ray, and MIR
spectral characteristics between NLS1 and BLS1 and/or BLAGN objects.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 239 163 The MIR and optical data for 99 BLAGNs
and 64 NLS1s
table2.dat 99 66 HRs and the luminosities at 0.2-12keV
for 33 BLS1s and 33 NLS1s
table3.dat 87 87 The luminosities of MIR lines for both
NLS1 and BLAGN samples
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Byte-by-byte Description of file: table1.dat table1b.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Sample [BLAGN NLS1] BLAGN or NLS1 sample
7- 30 A24 --- Name Source name
32- 39 F8.6 --- z Redshift
41- 51 F11.7 deg RAdeg Right ascension (J2000)
53- 63 F11.7 deg DEdeg Declination (J2000)
65- 72 F8.6 --- RAGN ?=- Fractional contributions of AGN component
to the integrated MIR luminosity (1)
74- 83 E10.8 --- RPAH ?=- Fractional contributions of PAH component
to the integrated MIR luminosity (1)
85- 94 E10.8 --- RSTR ?=- Fractional contributions of stellar
component to the integrated MIR luminosity (1)
96-101 F6.3 --- SSIL ?=- Silicate strength
103-108 F6.3 --- alpha ?=- Spectral index of the AGN component
110-117 F8.6 --- L6A ?=- L6A parameter
119-126 F8.6 --- L12A ?=- L12A parameter
128-137 E10.8 --- L12S ?=- L12S parameter
139-150 E12.8 10-7W nuLnu6 ?=- Monochromatic luminosity of the source
at 6um
152-163 E12.8 10-7W nuLnu12 ?=- Monochromatic luminosity of the source
at 12um
165-170 F6.1 Mpc LD Luminosity distance
172-182 F11.6 km/s FWHM(Hb) FWHM of broad Hβ component
184-192 F9.6 10-7W LogL5100 ?=- logarithm of AGN luminosity at 5100Å,
multiplied with 5100
194-205 F12.10 [Msun] logMBH ?=- logarithm of black hole mass
207-218 F12.10 --- acr ?=- acr parameter
220-229 A10 --- Refopt Reference for the optical data (2)
231-239 F9.6 10-7W log(LHb) ?=- Luminosity of H{bata} broad line (3)
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Note (1): RAGN + RPAH + RSTR = 1.
Note (2): References as follows:
Sani10 = Sani et al. (2010MNRAS.403.1246S 2010MNRAS.403.1246S)
Laki17 = Lakicevic et al. (2017MNRAS.472..334L 2017MNRAS.472..334L, Cat. J/MNRAS/472/334)
VC06 = Veron-Cetty et al. (2006A&A...455..773V 2006A&A...455..773V, Cat. VII/248)
Jin12 = Jin et al. (2012MNRAS.420.1825J 2012MNRAS.420.1825J)
Rak17 = Rakshit et al. (2017ApJS..229...39R 2017ApJS..229...39R, Cat. J/ApJS/229/39)
Nik09 = Nikolajuk et al. (2009MNRAS.394.2141N 2009MNRAS.394.2141N)
MJ02 = McLure & Jarvis (2002MNRAS.337..109M 2002MNRAS.337..109M)
W06 = Whalen et al. (2006AJ....131.1948W 2006AJ....131.1948W, Cat. J/AJ/131/1948)
Note (3): (ILR+VBLR - see the text) for the sources from
Lakicevic et al. (2017MNRAS.472..334L 2017MNRAS.472..334L, Cat. J/MNRAS/472/334)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Sample [BLAGN NLS1] BLAGN or NLS1 sample
7- 25 A19 --- Name Source name
27- 32 F6.4 --- z Redshift
34- 49 A16 --- IAUname IAU name (JHHMMSS.s+DDMMSS)
51- 57 F7.4 --- HR1 Hardness ratio 1 (0.2-0.5keV, 0.5-1.0keV)
59- 64 F6.3 --- HR2 Hardness ratio 2 (0.5-1.0keV, 1.0-2.0keV)
66- 71 F6.3 --- HR3 Hardness ratio 3 (1.0-2.0keV, 2.0-4.5keV)
73- 78 F6.3 --- HR4 Hardness ratio 4 (2.0-4.5keV, 4.5-12.0keV)
80- 99 E20.15 10-7W L0.2-12keV 0.2-12keV band luminosity
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 24 A24 --- Name Source name
26- 45 E20.15 10-7W L25um ?=- Luminosity of MIR line [OIV] at 25.89um
47- 66 E20.15 10-7W L14um ?=- Luminosity of MIR line [NeV] at 14.32um
68- 87 E20.15 10-7W L15um ?=- Luminosity of MIR line [NeIII] at 15.55um
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 20-Sep-2021