J/MNRAS/448/2900 Emission lines for SDSS Coronal-Line Forest AGNs (Rose+, 2015)
Coronal-Line Forest AGN: the best view of the inner edge of the AGN torus?
Rose M., Elvis M., Tadhunter C.N.
<Mon. Not. R. Astron. Soc., 448, 2900-2920 (2015)>
=2015MNRAS.448.2900R 2015MNRAS.448.2900R (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Spectroscopy ; Equivalent widths
Keywords: galaxies: active - quasars: emission lines - quasars: general -
galaxies: Seyfert
Abstract:
We introduce Coronal-Line Forest active galactic nuclei (CLiF AGN),
AGN which have a rich spectrum of forbidden high-ionization lines
(FHILs, e.g. [FeVII], [FeX] and [NeV]), as well as relatively strong
narrow (∼300 km/s) Hα emission when compared to the other Balmer
transition lines. We find that the kinematics of the CLiF emitting
region are similar to those of the forbidden low-ionization
emission-line (FLIL) region. We compare emission line strengths of
both FHILs and FLILs to cloudy photoionization results and find that
the CLiF emitting region has higher densities (104.5<nH<107.5/cm3)
when compared to the FLIL emitting region (103.0<nH<104.5/cm3).
We use the photoionization results to calculate the CLiF regions
radial distances (0.04<RCLiF<32.5 pc) and find that they are
comparable to the dust grain sublimation distances (0.10<RSUB<4.3 pc).
As a result, we suggest that the inner torus wall is the most likely
location of the CLiF region, and the unusual strength of the FHILs is
due to a specific viewing angle giving a maximal view of the far wall
of the torus without the continuum being revealed.
Description:
In this paper, we make use of SDSS spectra. The basic properties of
the CLiF AGN sample studied in this paper are given in Table 1. Note
that the outputs of the SDSS pipeline are used only for the sample
selection. Detailed measurements of emission line parameters such as
the flux and velocity widths are measured using our own methods
(Section 4). The redshifts were determined using single Gaussian fits
to the [O III] λ5007 emission line. This line was chosen
because it is the most prominent emission line in the optical spectra
of these and most other AGN.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 69 4 Basic properties of the CLiF AGN sample
tablea1.dat 76 62 Line identifications for the SDSS spectrum
of Mrk 1388
tablea2.dat 76 51 Line identifications for the SDSS spectrum
of III Zw 77
tablea3.dat 76 34 Line identifications for the SDSS spectrum
of J1241+44
tablea4.dat 76 28 Line identifications for the SDSS spectrum
of J1641+43
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See also:
VII/270 : SDSS quasar catalog: tenth data release (Paris+, 2014)
J/ApJS/143/257 : AGN emission line properties (Kuraszkiewicz+, 2002)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name CLiF AGN name
11- 12 I2 h RAh Hour of Right Ascension (J2000)
14- 15 I2 min RAm Minute of Right Ascension (J2000)
17- 21 F5.2 s RAs Second of Right Ascension (J2000)
22 A1 --- DE- Sign of the Declination (J2000)
23- 24 I2 deg DEd Degree of Declination (J2000)
26- 27 I2 arcmin DEm Arcminute of Declination (J2000)
29- 33 F5.2 arcsec DEs Arcsecond of Declination (J2000)
35- 40 F6.4 --- z Redshift (1)
42- 46 F5.2 mag rmag SDSS r model magnitude (2)
48- 51 A4 --- Spec [SDSS] Origin of the spectrum
53- 69 A17 --- Ref Reference (3)
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Note (1): Determined by single Gaussian fits to the prominent [O III]
λ5007 emission line.
Note (2): We choose model magnitudes because these objects are type 2 AGN and
therefore the photometry will be dominated by the host galaxy.
(see https://www.sdss3.org/dr10/algorithms/magnitudes.php)
Note (3): Refers to the first publication that discusses the optical spectrum
of the CLiF AGN candidate.
Reference as follows:
Osterbrock (1981) = 1981ApJ...249..462O 1981ApJ...249..462O;
Osterbrock (1985) = 1985PASP...97...25O 1985PASP...97...25O.
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Byte-by-byte Description of file: tablea[1234].dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Line Line identifier (1)
10- 14 F5.1 eV IP ? Ionization potential for the securely
identified emission species
16- 21 F6.1 0.1nm lambda ? Wavelength (Å)
23- 28 F6.1 0.1nm lambdaS SDSS Wavelength (Å)
30- 32 F3.1 0.1nm e_lambdaS Uncertainty in lambdaS
34- 37 F4.2 --- F/FHb ? Flux relative to Hβ and not corrected
for reddening (2)
39- 42 F4.2 --- e_F/FHb ? Uncertainty in F/FHb (2)
44- 48 F5.1 0.1 EW Equivalent width (Å)
50- 55 F6.1 km/s Deltav ? Velocity shift Δv (1)
57- 61 F5.1 km/s e_Deltav ? Uncertainty in Deltav (1)
63- 68 F6.1 km/s FWHM Full width at half maximum (1)
70- 74 F5.1 km/s e_FWHM Uncertainty in FWHM (1)
76 I1 --- NGauss [1/2] Number of Gaussians required to fit
the profile of the emission line
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Note (1): Columns "Line", "DeltaV" and "FWHM" are determined by fitting a single
Gaussian to the emission lines.
Note (2): Note that the fluxes presented here are from the double-Gaussian
fitting model.
The total flux of the Hβ emission line is:
(2.65±0.19)x10-15 erg/s/cm2/Å in tablea1;
(2.52±0.09)x10-14 erg/s/cm2/Å in tablea2;
(4.96±0.30)x10-16 erg/s/cm2/Å in tablea3;
(2.26±0.10)x10-15 erg/s/cm2/Å in tablea4.
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History:
From electronic version of the journal
(End) Tiphaine Pouvreau [CDS] 29-Nov-2017