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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 (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:
FileName Lrecl Records Explanations
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
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
Bytes Format Units Label Explanations
1- 19 A19 --- SDSS SDSS ID ( (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)
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.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
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 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
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). 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.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
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
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.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 10 A10 --- Name Galaxy Name (1) 12 A1 --- l_NG Limit flag on NG 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")
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.
History: From electronic version of the journal References: Muller-Sanchez et al. Paper I. 2015ApJ...813..103M
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Feb-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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