J/ApJ/832/67 Double-peaked narrow lines in AGN. II. z<0.1 (Nevin+, 2016)
The origin of double-peaked narrow lines in active galactic nuclei.
II. Kinematic classifications for the population at z < 0.1.
Nevin R., Comerford J., Muller-Sanchez F., Barrows R., Cooper M.
<Astrophys. J., 832, 67-67 (2016)>
=2016ApJ...832...67N 2016ApJ...832...67N (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Spectroscopy ; Redshifts
Keywords: galaxies: active; galaxies: interactions;
galaxies: kinematics and dynamics; galaxies: nuclei
Abstract:
We present optical long-slit observations of the complete sample of 71
Type 2 active galactic nuclei (AGNs) with double-peaked narrow
emission lines at z<0.1 in the Sloan Digital Sky Survey. Double-peaked
emission lines are produced by a variety of mechanisms including disk
rotation, kiloparsec-scale dual AGNs, and narrow-line region (NLR)
kinematics (outflows or inflows). We develop a novel kinematic
classification technique to determine the nature of these objects
using long-slit spectroscopy alone. We determine that 86% of the
double-peaked profiles are produced by moderate-luminosity AGN
outflows, 6% are produced by rotation, and 8% are ambiguous. While we
are unable to directly identify dual AGNs with long-slit data alone,
we explore their potential kinematic classifications with this method.
We also find a positive correlation between the NLR size and
luminosity of the AGN NLRs (RNLR∝L[OIII]0.21±0.05),
indicating a clumpy two-zone ionization model for the NLR.
Description:
To determine the nature of 71 Type 2 AGNs with double-peaked [OIII]
emission lines in SDSS that are at z<0.1 and further characterize
their properties, we observe them using two complementary follow-up
methods: optical long-slit spectroscopy and Jansky Very Large Array
(VLA) radio observations.
We use various spectrographs with similar pixel scales (Lick Kast
Spectrograph; Palomar Double Spectrograph; MMT Blue Channel
Spectrograph; APO Dual Imaging Spectrograph and Keck DEep Imaging
Multi-Object Spectrograph. We use a 1200 lines/mm grating for all
spectrographs; see table 1.
In future work, we will combine our long-slit observations with the
VLA data for the full sample of 71 galaxies (O. Muller-Sanchez+ 2016,
in preparation).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 64 71 Summary of longslit observations
table2.dat 91 71 Measured luminosities
table3.dat 79 142 Values for the parameters for quantitative
classification for both observed position angles
table4.dat 76 71 Official kinematic classification for each galaxy
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See also:
V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012)
VII/258 : Quasars and Active Galactic Nuclei (13th Ed.) (Veron+ 2010)
II/294 : The SDSS Photometric Catalog, Release 7 (Adelman-McCarthy+, 2009)
J/ApJ/777/64 : A search for double-peaked AGNs in AGES (Comerford+, 2013)
J/ApJ/769/95 : [NeV] or [NeIII] double peaked SDSS quasars (Barrows+, 2013)
J/AJ/144/125 : Photometry & spectroscopy of Markarian 266 (Mazzarella+, 2012)
J/ApJS/201/31 : Emission-line galaxies from SDSS. I. (Ge+, 2012)
J/ApJ/753/42 : Double-peaked AGN. I. Dual AGN candidates (Comerford+, 2012)
J/ApJ/746/L22 : Dual AGNs in the nearby Universe (Koss+, 2012)
J/ApJ/716/866 : SDSS search for binary AGN (Smith+, 2010)
J/ApJ/708/427 : Type 2 AGNs with double-peaked [OIII] lines (Liu+, 2010)
J/ApJ/705/L76 : AGNs with double-peaked [OIII] lines (Wang+, 2009)
J/AJ/137/42 : Matched SDSS and FIRST Sample (Rafter+, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 19 A19 --- SDSS SDSS ID (JHHMMSS.ss+DDMMSS.s) (1)
21- 30 A10 --- Name Galaxy Name (JHHMM+DDMM)
32- 39 F8.6 --- z [0.008/0.098] Redshift determined from the
velocity of the stellar absorption lines
41- 47 E7.1 --- e_z [0.000006/0.00004] Uncertainty in z
49- 64 A16 --- Tel Observatory and spectrograph (2)
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Note (1): J101836.77+512753.0 is very likely a misprint for J101835.77+512753.0
(see Liu+, 2010, J/ApJ/708/427); corrected at CDS.
Note (2): Observatory and spectrograph used:
APO/DIS = APO Dual Imaging Spectrograph, 0.42"/pixel in the
blue channel, 0.4"/pixel in the red channel;
Keck/DEIMOS = Keck DEep Imaging Multi-Object Spectrograph, 0.12"/pixel;
Lick/Kast = Lick Kast Spectrograph, 0.78"/pixel;
MMT/Blue Channel = MMT Blue Channel Spectrograph, 0.29"/pixel;
Palomar/DBSP = Palomar Double Spectrograph, 0.39"/pixel.
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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- 10 A10 --- Name Galaxy Name
12- 21 E10.4 10-7W LOIII Observed [OIII] luminosity
23- 30 E8.2 10-7W e_LOIII Uncertainty in LOIII
32- 40 E9.3 10-7W LOIIIc Dereddened [OIII] luminosity
42- 49 E8.2 10-7W e_LOIIIc Uncertainty in LOIIIc
51- 60 E10.4 10-7W Lbol ? Bolometric luminosity
62- 70 E9.3 10-7W e_Lbol ? Uncertainty in Lbol
72- 75 F4.2 kpc/arcsec scale [0.1/1.9] Conversion from arcsec to kpc
for Galaxy
77- 78 I2 pix ak [4/55] Akaike width of the narrow-line
region (2)
80- 80 I1 pix e_ak [1/8] Uncertainty in ak
82- 86 I5 pc Rad [950/10650] Radius of the narrow-line region
88- 91 I4 pc e_Rad [80/1850] Uncertainty in Rad
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Note (2): The Akaike Information Criterion (AIC) is a least squares statistic
that introduces a penalty for additional parameters, defined by
Akaike (1974ITAC...19..716A 1974ITAC...19..716A). Numerically, AIC=χ2+2k,
where k is the number of parameters and χ2 is the
chi-square statistic. See section 2.3 for further explanations.
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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- 10 A10 --- Name Galaxy Name (1)
12- 14 I3 deg PAobs [0/252] Observation position angle
16- 20 A5 --- Nrow Number of Rows with >2 Gaussian components (2)
22- 26 F5.1 km/s Vr [16.6/664.4] Line of sight velocity from the
single Gaussian centroid
28- 32 F5.1 km/s e_Vr [0.1/266] Uncertainty in Vr
34- 39 F6.1 km/s sigma [114/1039] Dispersion of Single Gauss fit
41- 45 F5.1 km/s e_sigma [0.8/507] Uncertainty in sigma
47- 52 F6.1 km/s sigma1 [122/1202] Dispersion of Double Gauss fit,
component 1
54- 58 F5.1 km/s e_sigma1 [0.9/564] Uncertainty in sigma1
60- 65 F6.1 km/s sigma2 [61/1051] Dispersion of Double Gauss fit,
component 2
67- 71 F5.1 km/s e_sigma2 [0.5/450] Uncertainty in sigma2
73- 75 I3 deg PAgal [3/173] Galaxy photometric major axis position
angle from SDSS r band photometry
77- 79 I3 deg PAOIII [5/176] Galaxy [OIII] major axis position angle
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Note (1): J0731+4258 is very likely a misprint for J0731+4528 and
J1350+3211 is very likely a misprint for J1350+2311; corrected at CDS.
Note (2): The number of rows that are best fit by >2 Gaussians within the
resolved center of emission (FWHM_cont ±1 row). For instance, in
row one, 5/9 indicates that out of the nine rows of the resolved
center of emission, 5 rows are better fit by 3 Gaussians.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Galaxy Name (1)
12- 12 A1 --- l_NG Limit flag on NG
14- 14 I1 --- NG [2] Number of Gaussian components (2)
16- 17 A2 --- l_Vr [ ≤>] Limit flag on Vr
19- 21 I3 km/s Vr [400] Maximum line of sight radial velocity
measured from the single Gaussian fit
for both PA
23- 24 A2 --- l_sigma [ ≤>] Limit flag on sigma
26- 28 I3 km/s sigma [500] Largest dispersion of the single Gaussian
fit from both observed PA
32- 33 A2 --- l_sigma12 [ ≤>] Limit flag on sigma12
35- 37 I3 km/s sigma12 [500] Largest dispersion of either of the two
Gaussian fit from both PA
41- 43 A3 --- Align Alignment flag: yes=PAOIII equal PAgal (3)
45- 76 A32 --- Class Classification (includes 35 "Outflow" and
26 "outflow Composite")
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Note (1): The 1σ error on the measured value straddles the classification
cutoff for some objects, e.g. J0135+1435. However, as the measured
value of J0135+1435 is greater than 500 km/s we classify this galaxy
accordingly as Outflow Composite. For all other galaxies in our sample
in which the measured value straddles a given classification cutoff
within error are classified according to the measured value.
Note (2): The number of components is >2 if at either position angle, more
than half the rows within the spatial center of the galaxy have >2
components as the best fit.
Note (3): Alignment is determined from PA[OIII] and PAgal. If these two
measurements are within 20° of one another, the galaxy is aligned.
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History:
From electronic version of the journal
References:
Muller-Sanchez et al. Paper I. 2015ApJ...813..103M 2015ApJ...813..103M
Nevin et al. Paper II. 2016ApJ...832...67N 2016ApJ...832...67N This catalog
Nevin et al. Paper III. 2018MNRAS.473.2160N 2018MNRAS.473.2160N
Comerford et al. Paper IV. 2018ApJ...867...66C 2018ApJ...867...66C Cat. J/ApJ/867/66
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Feb-2017