J/A+A/591/A88 [OIII] of radio-emitting narrow-line Seyfert 1 (Berton+, 2016)
[O III] line properties in two samples of radio-emitting narrow-line
Seyfert 1 galaxies.
Berton M., Foschini L., Ciroi S., Cracco V., La Mura G., Di Mille F.,
Rafanelli P.
<Astron. Astrophys., 591, A88 (2016)>
=2016A&A...591A..88B 2016A&A...591A..88B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, Seyfert ; QSOs ; Galaxies, radio
Keywords: galaxies: Seyfert - galaxies: jets - quasars: emission lines
Abstract:
The [OIII] λλ 4959, 5007 lines are a useful proxy to
test the kinematic of the narrow-line region (NLR) in active galactic
nuclei (AGN). In AGN, and particularly in narrow-line Seyfert 1
galaxies (NLS1s) these lines often show few peculiar features, such as
blue wings, often interpreted as outflowing component, and a shift -
typically toward lower wavelengths - of the whole spectroscopic
feature in some exceptional sources, the so-called blue outliers,
which are often associated to strong winds. We investigated the
incidence of these peculiarities in two samples of radio-emitting
NLS1s, one radio-loud and one radio-quiet. We also studied a few
correlations between the observational properties of the [OIII] lines
and those of the AGN. Our aim was to understand the difference between
radio-quiet and radio-loud NLS1s, which may in turn provide useful
information on the jet formation mechanism. We find that the NLR gas
is much more perturbed in radio-loud than in radio-quiet NLS1s. In
particular the NLR dynamics in γ-ray emitting NLS1s appears to
be highly disturbed, and this might be a consequence of interaction
with the relativistic jet. The less frequently perturbed NLR in
radio-quiet NLS1s suggests instead that these sources likely do not
harbor a fully developed relativistic jet. Nonetheless blue-outliers
in radio-quiet NLS1s are observed, and we interpret them as a product
of strong winds.
Description:
We decided to use the sample created by Cracco et al. (2016, MNRAS,
submitted) to have a uniformly selected sample of RQNLS1s that is not
contaminated by any spurious source. They found 9 RLNLS1s, which we
included in our second sample, and 59 RQNLS1s. To further increase the
number of sources, we decided to add also the RQNLS1s from Berton et
al. (2015A&A...578A..28B 2015A&A...578A..28B), which were not already included in their
sample because of the selection criteria and had a suitable spectra to
analyze. Our RQNLS1s sample in conclusion is made of 68 RQNLS1s.
For the RLNLS1s sample, besides the nine sources we already found with
the previous selection, we decided to use all the sources analyzed by
Foschini et al. (2015A&A...575A..13F 2015A&A...575A..13F) and Berton et al.
(2015A&A...578A..28B 2015A&A...578A..28B) for which an optical spectrum was available in
SDSS DR12, in the NED archive, or observable with the Asiago 1.22m
telescope (Sect. 3.1). Our sample is comprised of 56 RLNLS1s.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 62 68 Summary of the sources intrinsic properties in
radio-quiet narrow-line Seyfert 1 sample, RQNLS1s
tablea2.dat 62 56 Summary of the sources intrinsic properties in
radio-loud narrow-line Seyfert 1 sample, RLNLS1s
tablea3.dat 103 68 Summary of the [OIII] line properties for RQNLS1s
tablea4.dat 103 56 Summary of the [OIII] line properties for RLNLS1s
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Byte-by-byte Description of file: tablea1.dat tablea2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Short name (JHHMM+DDMM)
12- 13 I2 h RAh Right ascension (J2000)
15- 16 I2 min RAm Right ascension (J2000)
18- 22 F5.2 s RAs Right ascension (J2000)
24 A1 --- DE- Declination sign (J2000)
25- 26 I2 deg DEd Declination (J2000)
28- 29 I2 arcmin DEm Declination (J2000)
31- 34 F4.1 arcsec DEs Declination (J2000)
36- 40 F5.3 --- z Redshift
42- 45 F4.2 [Msun] logMBH logarithm of the black hole mass
47- 50 F4.2 --- Edd Eddington ratio
52- 56 F5.2 [10-7W] logL(Hb) logarithm of the Hβ luminosity
58- 62 F5.2 [10-7W] logLrad logarithm of the radio luminosity at 1.4GHz
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Byte-by-byte Description of file: tablea3.dat tablea4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Short name (JHHMM+DDMM)
11 A1 --- n_Name [*] Note on Name (1)
13- 17 F5.2 [10-7W] logL[OIII] logarithm of the [OIII] luminosity
19- 25 F7.2 0.1nm lambdac Wavelength of the [O III] core component
27- 30 F4.2 0.1nm e_lambdac rms uncertainty on lambdac
32- 38 F7.2 km/s Vc Shift of the [OIII] core with respect to
the rest-frame wavelength
40- 44 F5.2 km/s e_Vc rms uncertainty on vc
46- 52 F7.2 km/s FWHMc FWHM of the [OIII] core component
54- 59 F6.2 km/s e_FWHMc rms uncertainty on FWHMc
61- 67 F7.2 0.1nm lambdaw ?=- Wavelength of the [OIII] wing component
69- 72 F4.2 0.1nm e_lambdaw ? rms uncertainty on lambdaw
74- 81 F8.2 km/s Vw ?=- Velocity of the [O III] wing component
with respect to the core
83- 88 F6.2 km/s e_Vw ? rms uncertainty on Vw
90- 96 F7.2 km/s FWHMw ?=- FWHM of the wing component
98-103 F6.2 km/s e_FWHMw ? rms uncertainty on FWHMw
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Note (1): Sources marked with an asterisk are those where the redshift is
calculated with respect to Hβ narrow component.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Aug-2016