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+arXiv:1001.0049v1  [astro-ph.CO]  30 Dec 2009Optical Spectral Properties of Swift BAT Hard X-ray Selecte d
+Active Galactic Nuclei Sources
+Lisa M. Winter1,∗, Karen T. Lewis2, Michael Koss3, Sylvain Veilleux3,4, Brian Keeney1,
+Richard F. Mushotzky3,5
+ABSTRACT
+The Swift Burst Alert Telescope (BAT) survey of Active Galac tic Nuclei (AGN) is
+providing an unprecedented view of local AGNs ( < z >≈0.03) and their host galaxy
+properties. In this paper, we present an analysis of the opti cal spectra of a sample of
+64 AGNs from the 9-month survey, detected solely based on the ir 14-195keV ﬂux. Our
+analysis includes both archived spectra from the Sloan Digi tal Sky Survey and our own
+observations from the 2.1-m Kitt Peak National Observatory telescope. Among our
+results, we include line ratio classiﬁcations utilizing st andard emission line diagnostic
+plots, [O III] 5007˚A luminosities, and H βderived black hole masses. As in our X-
+ray study, we ﬁnd the type 2 sources to be less luminous (in [O III] 5007˚A and 14–
+195keV luminosities) with lower accretion rates than the ty pe 1 sources. We ﬁnd that
+the optically classiﬁed LINERs, H II/composite galaxies, and ambiguous sources have
+the lowest luminosities, while both broad line and narrow li ne Seyferts have similar
+luminosities. FromacomparisonofthehardX-ray(14–195ke V)and[O III]luminosities,
+we ﬁnd that both the observed and extinction-corrected [O III] luminosities are weakly
+correlated with X-ray luminosity. In a study of the host gala xy properties from both
+continuum ﬁts and measurements of the stellar absorption in dices, we ﬁnd that the
+hosts of the narrow line sources have properties consistent with late type galaxies.
+Subject headings: X-rays: galaxies, galaxies:active
+1. Introduction
+The Swift Burst Alert Telescope (BAT) provides an unprecede nted opportunity to study
+the optical properties of an unbiased sample of AGN. Conduct ing an all-sky mission in the 14–
+*Hubble Fellow
+1Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO
+2Department of Physics & Astronomy, Dickinson College, Carl isle, PA
+3Department of Astronomy, University of Maryland, College P ark, MD
+4Max-Planck-Institut f¨ ur extraterrestrische Physik, Pos tfach 1312, D-85741 Garching, Germany
+5NASA Goddard Space Flight Center, Greenbelt, MD– 2 –
+195keV band, the BAT survey has detected 153 AGN in the ﬁrst 9- months1(Tueller et al. 2008;
+Baumgartner et al. 2008). Since the sources were detected ba sed on 14–195keV ﬂux, with a ﬂux
+limit of 2–3 ×10−11ergss−1cm−2, selection eﬀects due to obscuring material are minimal. Due
+to the unbiased nature of the Swift BAT survey, Suzaku follow -ups of Swift-detected sources
+led to the identiﬁcation of a new class of “hidden” AGN (Ueda e t al. 2007), heavily obscured
+(NH>1023cm−2) sources that would not likely be identiﬁed as AGN based on th eir optical or
+soft X-ray ( E <3keV) properties alone. This class of “hidden” sources was f ound to comprise
+24% of the 9-month BAT AGNs (Winter et al. 2009a), making an an alysis of the collective optical
+properties an important piece in understanding the propert ies of the Swift BAT-detected AGN.
+Currently, great progress is being made in collecting and an alyzing the multi-wavelength prop-
+erties of this uniquely selected, very hard X-ray, 9-month S wift BAT AGN sample. The collec-
+tive properties of the 0.3–10keV X-ray band have been analyz ed and presented in Winter et al.
+(2009a). A comparison of the IR [O IV], optical [O III], and X-ray 2–10keV luminosity are pre-
+sented in Mel´ endez et al. (2008) for a sample of 40 BAT AGNs. S imultaneous optical-to-X-ray
+spectral energy distributions are analyzed for 26 of the BAT AGNs in Vasudevan et al. (2009).
+Additionally, some details of the optical host properties a re presented in Winter et al. (2009a) as
+well as Schawinski et al. (2009). Further, the results a full analysis of the optical colors and mor-
+phologies are being compiled in Koss et al.(in prep) and the Spitzer-based IR properties will be
+presented in Weaver et al.(submitted).In this paper, we present an analysis of the opt ical spectral
+properties of a sub-sample of the AGN from the BAT 9-month cat alog.
+Since the BAT-detected sources are bright ( mV<16) and nearby ( < z >= 0.03), they are
+easily observable with ground-based facilities. Between p ublished optical spectral analyses, the
+publicly available Sloan Digital Sky Survey (SDSS) spectra , and our own follow-up observations
+with the Kitt Peak National Observatory’s (KPNO) 2.1-m tele scope of sources for which optical
+spectra/analyses were not available, we present the optica l emission line properties of 64/153 of
+the SWIFT BAT AGNs. This sample includes 35 broad line (55%) a nd 29 narrow line (45%)
+sources, the same ratio as in the total sample. All selected s ources were chosen based on positions
+viewable from the Kitt Peak Observatory. In this way, our sam ple represents 81% of the non-blazar
+“northern”BAT AGN sources. As in our X-ray study(Winter et a l. 2009a), we excludethebeamed
+sources due to the diﬀerent physical mechanisms producing th eir spectra (i.e. jets). The missing
+“northern” sources were missed purely due to observation sc heduling and poor weather conditions.
+In the following sections, we describe the observations, da ta analysis, and ﬁnally our results.
+1http://heasarc.gsfc.nasa.gov/docs/swift/results/bs9 mon/– 3 –
+2. Observations and Data Reduction
+For our analysis of the optical spectra of the Swift BAT-dete cted AGN, we ﬁrst obtained
+spectra of our sources that were publicly available from the Sloan Digital Sky Survey (SDSS). We
+supplemented this data set with our own observations at the K itt Peak Observatory. Additionally,
+we included several of the SDSS observed sources as Kitt Peak targets, in order to compare the
+results of our analysis from each observatory.
+Our Kitt Peak observations were obtained on the 2.1-m telesc ope as part of MD-TAC time.
+Over the course of 5 observing trips, from August 2006 – April 2009, we used the GoldCam
+spectrograph to observe the central region of ≈50 objects, including AGN and template galaxies.
+The AGN observed were sources for which we could not ﬁnd archi ved optical spectra or analyses
+of optical lines in the literature. The template galaxies (1 0) were chosen from non-active templates
+listed in Ho et al. (1997). A majority of the sources were obse rved with two 30-minute exposures in
+both the red (grating 35, which covers 4760–7240 ˚A) and blue (grating 26new, which covers 3660–
+6140˚A), through a 2′′slit. Both of these gratings have a spectral resolution of 3. 3˚A, corresponding
+to a velocity width of 200 kms−1at 5007˚A. The exposure times were chosen in order to achieve a
+S/N of≈70 per pixel for the AGN sources and the dispersion relation f or both gratings corresponds
+to≈1.25˚A pixel−1. However, for some of the faintest sources we used a lower dis persion grating,
+grating 32, which covered a larger wavelength range than the higher dispersion gratings (4280–
+9220˚A, at 2.25 ˚A pixel−1and which has a spectral resolution of 6.7 ˚A). We used this grating because
+of the unknown redshift of many of these sources.
+Initial processingof thedataproceededusingthestandard tasks inIRAFtoextract thespectra
+and remove cosmic rays. The spectra were dispersion correct ed using comparison observations of
+the HeNeAr lamp taken at each telescope position. They were t hen ﬂux calibrated using standard
+stars, from the spectrophotometric standards compiled by M assey et al. (1988), observed on the
+same night as the template/AGN. We then added the medium reso lution red and blue spectra
+together to obtain a single medium resolution spectrum for e ach source.
+In addition to the Kitt Peak observations, we include spectr a from the SDSS data release 7
+(Abazajian et al. 2009). Such spectra were publicly availab le for 24 of the non-blazar BAT AGN
+sources. A list of the BAT AGN 9-month sources for which we ana lyzed Kitt Peak/Sloan spectra
+are listed in Table 1. The KPNO observations (with typical to tal exposure times of 1hr in each
+medium resolution grating) were planned such that we would o btain similar signal-to-noise spectra
+as the SDSS spectra (S/N ≈75), to provide an easy comparison between both sets of spect ra. In
+total, our sample consists of 64 sources, including 40 spect ra from our KPNO observations, 24 with
+SDSS spectra (4 sources having both a KPNO and SDSS spectrum) , and 13 with emission line
+properties listed in the literature (9 of which also have eit her a KPNO or SDSS spectrum). Details
+of the KPNO observations, including the extraction apertur e along the slit, are listed in Table 2
+for the target AGN sources and in Table 3 for the galaxy templa te sources. Details of the SDSS
+observations are listed in Table 4. Based on visual inspecti ons of the AGN spectra, we indicate– 4 –
+in the tables which sources display broad lines with a ‘B’. In total, 33 sources (including 3 with
+emission line properties available in the literature), 55% of the sample, exhibit clear broad lines
+(i.e. broad H αand Hβ).
+3. Data Analysis
+Analysis of the spectra consisted of three steps: de-redden ing the spectrum to correct for
+reddening from the Milky Way, continuum subtraction, and ﬁt ting the emission lines. The spectra
+were de-reddenned using the IDL procedure CCMUNREDfrom the Goddard IDL Astronomy User’s
+Library. This procedure uses the reddening curve of Cardell i et al. (1989), with R V= 3.1, and
+the input value of E B−V. The Milky Way E B−Vvalues (listed in Table 1) were obtained for the
+Kitt Peak and SDSS observed sources from the NASA Extragalac tic Database (NED). Following
+this step, the spectra were de-redshifted to their restfram e wavelengths, using the NED redshifts or
+measured redshift from the [OIII] 5007 ˚Aline. Following the continuum ﬁts ( §3.1), we measured
+the emission ( §3.2) and absorption ( §3.3) line parameters for prominent spectral features. We
+then tested forapertureeﬀects by comparingemission linean dstellar absorption line measurements
+with redshift, ﬁnding no correlations.
+3.1. Continuum Modeling
+In order to ﬁt the emission lines as correctly as possible, gr eat care must be taken in modeling
+the continuum. For an AGN source, we expect the continuum to b e a combination of non-thermal
+emissionfromtheAGNandstellarlightfromthehostgalaxy. Tomodelthecontributionfromstellar
+light, we used the population synthesis models from the GALA XEV package2(Bruzual & Charlot
+2003) in the 3200 ˚A–9300˚A range. The spectral resolution of these models ( ≈3˚A) is directly
+comparable to that in the SDSS and KPNO samples. We assume tha t the galaxy light is the
+sum of bursts of formation at diﬀerent ages, using stellar pop ulations at 3 diﬀerent ages (25,
+2500, and 10000 Myr) to determine whether the host is consist ent with a young, intermediate,
+or old population (or any combination of these three). While a three component stellar model
+(young, intermediate, old) does not fully describe the spec tra of all galaxies, we have found (see
+the appendix) that adding more components results in degene rate solutions with diﬀerent sums
+of the 10 spectral models in the Bruzual & Charlot instantane ous burst models. We thus use
+the 3 component models adopted and recognize that this may no t be a fully accurate description
+of the stellar components of the host galaxies. Additionall y, we used 3 metallicity levels: 0.05Z
+(2.5Z⊙), 0.02Z( Z⊙), and 0.004Z (1
+5Z⊙). We usethesame code describedin Tremonti et al. (2004),
+which was used to measure the continuum in a sample of 53,000 S DSS galaxies. As described in
+Tremonti et al. (2004), the best ﬁt is obtained using a nonneg ative least squares ﬁt using the same
+metallicity for all 3 of the ‘age’ groups, attenuated by dust (which is modeled as a free parameter).
+Theχ2values, using diﬀerent metallicity populations, are compar ed to ﬁnd the best ﬁt metallicity– 5 –
+range. We note, however, that these models depend upon neces sary assumptions, such as stellar
+populations created in an instantaneous burst of star forma tion (see Conroy et al. (2009) for a
+discussion of many of the associated uncertainties in singl e stellar population models), which are
+not physical.
+To test the eﬀectiveness of the galaxy continuum ﬁts, we ﬁrst a pplied the models to our set
+of template galaxies obtained at KPNO. The ﬁnal input to the T remonti et al. (2004) code is
+the galaxy’s velocity dispersion, a quantity that is unknow n for many of our AGN host galaxies.
+Therefore, we ﬁt each of the templates with a range of dispers ion values to obtain the best-ﬁt.
+These values were then compared to the known galaxy paramete rs, listed in LEDA3(Paturel et al.
+2003). The galaxy type and velocity dispersion, as well as th e ﬁtted values, are listed in Table 5.
+On average, we ﬁnd that the ﬁtted dispersion velocities (for a Gaussian, FWHM = 2.35×σ) are
+in agreement with the central velocity dispersions listed i n LEDA ( < σM>= 132kms−1, while
+the LEDA values give < vdisp>= 159kms−1). From a comparison of the galaxy type to the light
+fraction (at 5500 ˚A) from the young, intermediate, and old stellar population s, there are no obvious
+contradictions. Our sample includes late spirals through e llipticals and we ﬁnd that the models
+suggest the light is dominated by intermediate to old stella r populations in most of the galaxies
+(this is consistent with the color analysis of the images fou nd by Koss et al.(in preparation)).
+In Figure 1, we plot examples of the results of the stellar con tinuum ﬁtting. We ﬁnd that the
+models are particularly accurate at ﬁtting the blue end (bel ow 5000˚A) of the spectra. While the
+addition of more stellar populations (at diﬀerent ages) woul d provide better ﬁts to the spectra,
+Tremonti et al. (2004) point out that the ﬁts are often degene rate (they use 10 diﬀerent population
+ages). Therefore, in an eﬀort to get a broad understanding of t he stellar properties of the AGN
+host galaxy properties, we conﬁneour ﬁts to the young, inter mediate, and old populations indicated
+above.
+Additionally, we created a grid of test spectra using diﬀeren t combinations of the three stellar
+populations indicated. Random noise was added to the test sp ectra, which were then broadened
+with FWHM = 300kms−1and an instrumental resolution of 75kms−1, and reddened using the
+Charlot & Fall law (Charlot & Fall 2000). The results of conti nuum ﬁts to these test spectra are
+presented in §A. As shown, we ﬁnd that the velocity dispersion is well-dete rmined for our test
+spectra while the metallicities are not. We can clearly dist inguish young stellar populations from
+the intermediate/old populations, however, there is a dege neracy between the intermediate and old
+populations when they are combined with the young populatio ns. These degeneracies are taken
+into account in the following discussions. We also created a grid of test spectra including a power
+law contribution similar to that of our sample along with the stellar populations, from which we
+found no degeneracy between the power law and stellar compon ents (see appendix).
+2http://www2.iap.fr/users/charlot/bc2003/
+3http://leda.univ-lyon1.fr– 6 –
+In order to subtract a continuum from the KPNO and the SDSS spe ctra, we modiﬁed the
+galaxy modeling code to include a non-thermal power law cont ribution from the AGN ( p0×λp1,
+wherep0is constrained to range from 0 to 1 and p1>0). In our model, separate reddening values
+were ﬁtted for both the power law component and the stellar co mponent. Additionally, in our
+ﬁts we masked out regions near prominent emission line posit ions (i.e. H β, [OIII]λ5007˚A) at a
+standard width of 500kms−1and used a larger width of 7000kms−1around H α. For the broad line
+sources (identiﬁed as such by visual inspection of the optic al spectra), we masked a larger region
+with a width of 10000kms−1around prominent hydrogen and helium emission features (H γ, Hδ,
+Hβ, Hα, HeI, and He II). The results of these ﬁts are presented in Table 6. Average v alues of
+p1for our sources were 0.67, very similar to the power law slope s found for luminous quasars by
+Richards et al. (2006), with a range of ﬁtted values from 0 to 2 .89. The average value for p0is 0.47,
+with values ranging from 0 to 1. As listed in the Table 6, p0was calculated for the speciﬁc ﬂux at
+1˚A and has units of 10−17ergss−1cm−2˚A−1.
+As we show in the appendix, we found no statistical degenerac ies between the power law
+component and stellar continua based upon our simulations. However, the issue of separating
+stellar and non-thermal AGN continua is complex. In order to assess the degree of degeneracy
+in our models, we carefully analyzed the results of our model ﬁts. From our models, 37% of the
+narrow line sources (sources in this category tend to be clas siﬁed as Sy 1.8/1.9 sources by other
+authors) and 38% of the broad line sources have contribution s of 50% or greater from a power
+law. We examined the spectra of these sources in the region fr om 3800–4200 ˚A, which includes
+the important stellar diagnostic lines of Ca H and K as well as the Hδabsorption. For broad line
+sources with high power law contributions, we ﬁnd that absor ption lines tend to be weak, while
+[NeIII] (at 3869 and 3968 ˚A) and occasionally weaker hydrogen Balmer (H ζ, Hǫ, Hδ) emission lines
+are comparatively strong. For the narrow line sources, sour ces with strong power law contributions
+tend to have weak to no clearly evident absorption features. Nearly half of these narrow line
+spectra have either poor ﬁts to the data ( χ2>>1) or no spectral coverage at the blue wavelengths
+which include important stellar lines like Ca H and K (making the ﬁts less reliable). Therefore,
+the eﬀects of any degeneracies between power law and stellar p opulation models are likely small
+for our purposes (i.e. rough estimates of the continuum).
+In Figures 2 and 3, we show examples of the continuum results. Both the original and contin-
+uum subtracted spectra are plotted in black with the continu um plotted in blue. For the majority
+of sources, we ﬁnd acceptable ﬁts with the stellar + power law continuum models. Particularly,
+good ﬁts are obtained for the narrow line sources. For the bro ad line sources, the presence of broad
+Balmer lines makes it particularly hard to obtain a good ﬁt to the spectrum below ≈4500˚A (see
+for example the spectrum of MCG +04-22-042).
+To show how the spectra and continuum models for spectra take n at KPNO compare to the
+SDSS spectra, we plot the KPNO and SDSS spectra + continuum ﬁt s for the four sources with
+spectra from both in Figure 4. We chose to show the region from 3700–6200 ˚A, a region which
+includes both prominent emission lines (i.e. H βand [OIII]) and intrinsic absorption features (Ca– 7 –
+H&K, the G-Band, Mg Ib, and Na ID). Both the SDSS and KPNO spectra of Ark 347 are well ﬁt
+with a continuum dominated by an old stellar population at so lar metallicity. The KPNO spectrum
+of Mkn 417 is found to be dominated by a power law, while the SDS S continuum is dominated by
+a solar metallicity old stellar population. For the broad li ne source MCG +04-22-042, neither the
+KPNO or SDSS spectra are ﬁt well at the blue end of the spectrum (due to the hydrogen Balmer
+lines), making it unsurprising that the models do not match.
+Finally, for Mkn 18, diﬀerent metallicities (low in the SDSS s pectrum and high in the KPNO
+spectrum)andgalaxycontributionsarefound. However, aso urtestmodelsshowed, themetallicities
+are not well-determined with the continuum models. The youn g stellar population contributions
+are similar for both the KPNO and SDSS spectra, leaving the di screpancy in the intermediate
+and old contributions as a likely eﬀect of the degeneracy we fo und in our test models between the
+intermediate and old populations. The diﬀerence in the conti nuum ﬂux between the KPNO and
+SDSS spectra of Mkn 18 is an extreme case, likely due to the fac t that Mkn 18 is highly elliptical
+and inclined along the E-W direction of the slit in the KPNO ob servation (15′′), while the circular
+ﬁber of the SDSS (3′′) misses out on this ﬂux.
+3.2. Emission Line Fitting
+To measure the properties of the emission lines in the KPNO an d SDSS spectra (including the
+FWHM and ﬂux of each line), we adopted two separate methods fo r the narrow line and broad line
+spectra. For the narrow line spectra, we ﬁrst measured the pr ominent lines in two distinct regions,
+the regions surrounding H βand Hα. At the blue end of the spectrum, we ﬁxed the positions of the
+Hγ, Hβ, and [O III] lines (λ4959 and λ5007), requiring that the velocity oﬀset and FWHM of the
+lines remain the same for all of the lines measured, and ﬁt for the ﬂux and equivalent width. For
+spectra whose wavelength range includes [O II]λ3727, an important diagnostic for distinguishing
+low-ionization narrow emission-line regions (LINERs) (He ckman 1980), we include this line in the
+ﬁts to the blue end of the spectrum. Additionally, we followe d the same procedure to ﬁt the
+prominent emission lines surrounding and including H α, [OI]λ6300, [N II]λ6548, [N II]λ6584,
+[SII]λ6716, and [S II]λ6731. The intensities of the [N II] lines are ﬁxed such that the λ6548
+line is at a 1:2.98 ratio with the λ6584 line, as dictated by atomic physics. For all of the narro w
+line ﬁts, the FWHM was corrected for the instrumental resolu tion (200kms−1at 5007˚A for the
+KPNO spectra and 75kms−1for the SDSS spectra) and we placed the restriction that the F WHM
+values have a lower limit of 50kms−1and an upper limit of 1000kms−1. The results are recorded
+in Table 7. In Table 8, we include the intensity ratios for add itional weaker lines (i.e. H δ, [NI],
+HeI) measured in the spectra.
+For the broad line sources, two complications arise which pr event us from performing the
+same analysis as for the narrow line sources. Firstly, great er uncertainties exist in the continuum
+measurements. Secondly, the lines can not be ﬁt by simple Gau ssians with the same widths. While
+the hydrogen Balmer lines of many of the broad line sources sh ow asymmetries, we chose to ﬁt– 8 –
+both Hαand Hβwith a combination of narrow and broad Gaussians. To ensure t he uniform
+measurements of the lines in our spectra, we used an automate d process which focused on ﬁtting
+lines in a narrow region surrounding both the H βand Hαlines, separately.
+In the Hβregion, deﬁned as the region from 4600–5200 ˚A, we ﬁt a combination of three narrow
+Gaussians to [O III] 5007˚A. The use of three Gaussians allowed us to reproduce the shap e more
+robustly, since this line often shows extended wings. The na rrow line shape, particularly the widths
+of these lines, were applied to the narrow He II4686˚A, Hβ4861˚A, and [O III] 4959˚A lines. Both
+the ﬂux and velocity oﬀset of each line were allowed to vary. Th e continuum was ﬁt with a linear
+function in a region unaﬀected by the prominent lines. Finall y, these ﬁtted narrow components
+were combined with a broad H βline, which was modeled with a single broad Gaussian compone nt,
+and re-ﬁt. The use of essentially a narrow and broad Gaussian allows us to estimate the ﬂux and
+width of each component, important in estimating the black h ole mass (based on the FWHM in
+the broad component) and emission line ratios (which depend on the ratio of the narrow lines).
+Results of these ﬁts are included in Table 9, including the me asured continuum ﬂux at 5100 ˚A. The
+recorded values of FWHM for the narrow component apply to the strongest narrow line component
+of the three Gaussians used to ﬁt the [O III] 5007˚A line.
+In the Hαregion, deﬁned as the region from 6200–6900 ˚A, we used the narrow [O I] 6300˚A line
+to deﬁne the initial guess for the velocity oﬀset of the measur ed lines and the set FWHM of a
+single Gaussian component. The oﬀset velocities and ﬂuxes of the remaining narrow H αline, [N II]
+lines, and [S II] lines were allowed to vary. However, the intensities of the [NII] lines are ﬁxed
+such that the λ6548 line is at a 1:2.98 ratio with the λ6584 line. A linear continuum was ﬁt in a
+region unaﬀected by the emission lines. The narrow lines were added to a single broad Gaussian
+for broad H αand re-ﬁt. Results from these ﬁts are recorded in Table 10. Ex amples of ﬁts to both
+the Hβand Hαregions are shown in Figure 5. The largest uncertainties inv olved in these ﬁts are
+associated with the measurements of H αand the two [N II] lines, which are blended in our broad
+line spectra, particularly for a source such as MCG +04-22-0 42.
+Additionally, weaker lines that are also present in the spec tra were measured by manually
+selecting a continuum region surrounding the selected emis sion feature. The ﬂux of each of these
+measured lines are included in Table 11. Where broad lines we re present and clearly separable from
+a narrow component, the indicated ﬂux is for the narrow compo nent.
+3.3. Stellar Absorption Features
+As an alternate method of determining ages of the host galaxi es from the stellar continuum
+ﬁts, we measure the strength of stellar absorption features directly from the non-galaxy continuum
+subtracted (both with and without subtraction of the AGN non -thermal component) spectra of our
+sources. This method is analogous to the work measuring Lick -indices by Worthey & Ottaviani
+(1997). However, instead of broadening our spectra to the ve locity dispersion of the Lick/IDS– 9 –
+spectral library (9 ˚A), we follow the procedure outlined in Kauﬀmann et al. (2003b ) for SDSS spec-
+tra, which instead compares the measured indices to the Bruz ual & Charlot (2003) stellar models.
+For further details on the SDSS analysis, along with a compar ison of the measured indices with
+additional high resolution stellar libraries, see the disc ussion in Kauﬀmann et al. (2003b).
+Two particularly important indicators of the age of a stella r population were used extensively
+in galaxy studies using SDSS spectra (Kauﬀmann et al. 2003a,b ; Gallazzi et al. 2005; Kewley et al.
+2006). These are the 4000 ˚A break (measured with Dn(4000)) and the equivalent width of H δ
+absorption (measured with H δA). Among these, the 4000 ˚A break, or Ca IIbreak, is observed as a
+discontinuity in the optical spectrum, caused mainly by the presence of absorption features from
+metals below 4000 ˚A. Since the opacity of metals in young, hot stars is low, this feature is weak in
+young stellar populations and strong in old populations. As a measurement of the Ca IIbreak, we
+use the deﬁnition of Balogh et al. (1999) to compute:
+Dn(4000) =/integraltext4000
+4100fλdλ
+/integraltext3850
+3950fλdλ(1)
+While strong Ca IIbreaks indicate old populations, strong equivalent widths of Hδabsorption
+indicate a recent burst of star formation within 0.1–1Gyr (W orthey & Ottaviani 1997). Therefore,
+we measure
+HδA= (4083.50−4122.25)(1−(FI/FC)), (2)
+whereFIis the ﬂux of the line within the bandpass of the feature (4122 .25 – 4083.50) and FCis
+the ﬂux in a pseudo-continuum. The pseudo-continuum is deﬁn ed as the line drawn through the
+average of the ﬂux in the continuum immediately blueward ( λλ4041.60 – 4079.75 ˚A) and redward
+(λλ4128.50 – 4161.00 ˚A) of the H δabsorption feature.
+Half of the spectra show an H δemission line (10 narrow line sources and 16 broad line sourc es),
+while emission from [Ne III] 3869˚A is often present in the pseudo-continuum from which Dn(4000)
+is measured. For the narrow line sources in our sample, we sub tracted the measured narrow lines
+before calculating these age indicators. Such a calculatio n is not straight forward for the broad line
+sources, where broad emission features are often present in the region containing H δA(with Hδ
+emission) and D n(4000) (including [Ne III] + H7λ3968˚A and H δ). In Figure 6, we plot examples
+of spectra for both narrow and broad line sources, where stel lar absorption features are seen.
+In Figure 7, we plot H δAversus D n(4000) for our sources, excluding broad line sources with
+prominent H δemission. We plot the values measured both after subtractin g the power law con-
+tinuum (Table 6; top plot) and from the original dereddened s pectrum (bottom plot). From each
+of these measurements, the D n(4000) break does not change appreciably whether or not the p ower
+law component is subtracted, with a median value of 1.26 for n arrow line sources and 0.91 for broad
+line sources when the power law is subtracted and 1.41 (narro w) and 0.92 (broad) without the sub-
+traction. The H δAvalues are aﬀected, however, for the narrow line sources with median values of
+0.81 (narrow) and -2.15 (broad) with the power law subtracte d and 1.73 (narrow) and -2.15 (broad)– 10 –
+without the subtraction. To test whether any aperture eﬀects inﬂuenced our measurements, we
+plotted each of these diagnostic measurements against reds hift. With no correlation in either H δA
+or Dn(4000) with z, we conclude that there are no obvious aperture eﬀects to be ac counted for in
+our measurements.
+The majority of the narrow line sources occupy the area expec ted from our stellar population
+model tests, discussed in §A and plotted in Figure 19. The broad line sources, however, o ccupy a
+region with considerably lower values of H δA. This is true even for sources where an H δemission
+line is not seen in the spectrum (as for the sources plotted). From visual inspection of the H δ
+region of our sources, we ﬁnd that unlike the narrow line sour ces, we can not clearly identify an H δ
+absorption feature in any of the broad line sources. In most c ases, we see emission features that
+are often broad. The low values of H δAmeasurements for broad line sources are therefore a likely
+eﬀect of emission in this region.
+In addition to these stellar age diagnostics, we measured ad ditional absorption indices for
+common stellar absorption features. These values were meas ured using the same method as used
+for the H δAindex, ﬁrst subtracting the emission line spectra for the na rrow line sources and
+subtracting the power law component for all of the sources. B andpasses and continuum ranges
+are deﬁned in Worthey et al. (1994) and Worthey & Ottaviani (1 997). In Table 12, we present the
+stellar age indicators (D n(4000) and H δA) along with 6 metallicity indicators, chosen to sample
+indices sensitive to several diﬀerent elements (i.e. C, N, Ca , Mg, Fe). Two of these indices are
+combinations of other indices, deﬁned in Gonz´ alez (1993):
+[MgFe] =/radicalbig
+Mgb<Fe>and<Fe>=1
+2(Fe5270 +Fe5335) . (3)
+We use the modiﬁed form of [MgFe]′, deﬁned by Thomas et al. (2003) as:
+[MgFe]′=/radicalbig
+Mgb(0.72 Fe5270+0 .28 Fe5335) . (4)
+Additionally, tobetterunderstandourresults, wealsomea suredthesestellar absorptionindices
+for a sample of test spectra created from the stellar populat ion models used for the continuum ﬁts.
+We discuss these results, where we used diﬀerent combination s of stellar ages and metallicities, in
+§A. Of the additional stellar absorption indices recorded in Table 12, H δemission could aﬀect
+the value measured for CN 1. Additionally, He II4686˚A is within the range of C 24668 and [N I]
+5199˚A is within the range of Mgb. Since [N I] 5199˚A is weak in our broad line sources, we expect
+little error in our Mgb measurements. In Figure 8, we plot var ious metallicity indicators and the
+age indicator D n(4000) versus themetallicity indicator Mgb for our target s ources. Comparingwith
+our results from the test spectra, it appears that C 24668 is the most aﬀected by “contaminating”
+emission features. The narrow line sources should be unaﬀect ed, however, since we have subtracted
+the emission components from their spectra.
+Based on a comparison of the plots in Figure 8 with the test spe ctra values, we ﬁnd that the
+[MgFe]′vs Mgb and <Fe>vs Mgb plots are the best indicators of the metallicity of the stellar– 11 –
+populations. However, the only clear result is that we do not ﬁnd old, high-metallicity (2.5 Z ⊙)
+populations within our sample (all of the old population tes t spectra have Mgb /lessorsimilar2, as determined
+from the D n(4000) vs Mgb plot). Since there is little diﬀerence in the par ameter space occupied by
+solar and low metallicity populations, we can not discern an ything more from our measured stellar
+absorption indices.
+4. Emission Line Classiﬁcation
+Emission line diagnostic plots, utilizing the optical line ratios of [O III]λ5007/Hβ, [NII]
+λ6583/Hα, [SII]λλ6716,6731/Hα, [OIII]λ5007/[O II]λ3727 and [O I]λ6300/Hα, are an em-
+pirical method of separating Seyferts, LINERs, and star-fo rming galaxies (Baldwin et al. 1981;
+Veilleux & Osterbrock 1987). The chosen line ratios (1) have small wavelength separations, so that
+the eﬀects of reddening are minimal, and (2) distinguish betw een photo-ionization from O and B
+stars (H IIobjects) and a non-thermal/power law continuum (AGNs). In o rder to construct these
+diagnostic diagrams for our Swift BAT AGNs, we ﬁrst correcte d the line ratios for reddening.
+To correct our line ratios for extinction, we use the line rat io of the strongest narrow Balmer
+lines (Hα/Hβ) along with the Cardelli et al. (1989) reddening curve. The e ﬀect of reddening is
+represented as
+I(Hα)
+I(Hβ)=F(Hα)
+F(Hβ)10c[f(Hα)−f(Hβ)](5)
+whereI(λ) is the intrinsic ﬂux, F(λ) is the observed ﬂux, and f(λ) is from the reddening curve. We
+assumeanintrinsicH α/Hβratio(I(Hα)
+I(Hβ))of3.1foroursources, assumingthattheyaredominatedby
+the underlying AGN. Additionally, we assume that RV= 3.1 and therefore E(B−V) = (2.5/3.1)c.
+For 11 of the spectrafromKPNO or SDSS,we ﬁndthat the ratio of Hα/Hβis less than the assumed
+intrinsic value, for which we do not apply a reddening correc tion [E(B−V) = 0]. The corrected line
+ratios, along with values found in the literature for an addi tional 13 sources, are shown in Table 13.
+In Figure 9, we plot the distribution of E(B−V) for the narrow and broad line sources.
+Excluding the few outlying observations with measured valu es ofE(B−V)>1.0, we ﬁnd that the
+broad line sources have a lower average value than the narrow line sources and a smaller range of
+values. We ﬁnd the average value of E(B−V) = 0.08 with a standard deviation of 0.11 for broad
+line sources and an average value of E(B−V) = 0.29 with a standard deviation of 0.33 for narrow
+line sources. The results of a Kolmogorov-Smirnov comparis on test show that it is unlikely that the
+values are drawn from the same distribution with the maximum diﬀerence between the cumulative
+distributions ( D) of 0.375 and a corresponding probability of 0.016. This pro bability is less, but
+still low, when the outlying points are included ( D= 0.301 andP= 0.067). Thus, the narrow lines
+in type 2 objects are more extincted.
+We classify our sources as H IIgalaxies, composites (COMPs), Seyferts, or LINERs using th e
+classiﬁcation criteria based on the analysis of the emissio n line properties of 85224 SDSS galaxies– 12 –
+presented in Kewley et al. (2006). These criteria include a t heoretical ’maximum starburst line’
+from Kewley et al. (2001), shown as a solid line in the diagram s in Figure 10, which represents a
+boundary between H IIgalaxies and AGNs. Additionally, in the [O III]/Hβvs. [NII]/Hαdiagram,
+a dashed line shows the empirical division between pure star -forming galaxies and Seyfert-H II
+composites from Kauﬀmann et al. (2003a). Finally, empirical ly derived divisions between LINERs
+and Seyferts, from Kewley et al. (2006), are shown in the [O III]/Hβvs. [SII]/Hα, [OIII]/Hβvs.
+[OI]/Hα, and [O III]/[OII] vs. [O I]/Hαdiagnostic plots. The emission line diagnostic plots are
+shown in Figure 10 and the classiﬁcations are shown in Table 1 4.
+Based on these classiﬁcations of the narrow line sources (ci rcles and a few squares [values from
+the literature] in Figure 10), 25 spectra are consistent wit h Seyferts, 1 spectrum corresponds to an
+HIIobject, 5 spectra are consistent with LINERs, 1 is a composit e, and 6 are ambiguous. Among
+these, we classify the Ark 347 KPNO spectrum as a Seyfert and N GC 4992 as a LINER. For each
+of these sources, the Veilleux & Osterbrock (1987) diagram i ncluding the [S II]/Hαratio is the
+only diagram with a classiﬁcation inconsistent with the oth er classiﬁcation plots. Errors in this
+measurement ([S II]/Hα) could easily place the spectra within the Seyfert or LINER c lassiﬁcation,
+respectively.
+The LINER sources include NGC 788, NGC 2110, NGC 4992, MCG+04 -48-002, and NGC
+7319. Of these, NGC 4992 is classiﬁed as a possible X-ray brig ht optically normal galaxy (XBONG)
+by Masetti et al. (2006), and MCG+04-48-002 was previously c lassiﬁed as a starburst/H IIgalaxy
+with a hidden Sy 2 nucleus (Masetti et al. 2006) (in their spec trum the [O I]λ6300 line was not
+detected). All but one of the classiﬁed LINERs (NGC 4992) hav e ratios of H α/Hβ <3.1.
+The spectra classiﬁed as starburst/H IIgalaxy and composite, respectively, are the SDSS
+spectrum of Mkn 18 and UGC 11871. Finally, the 6 ambiguous sou rces include: 2 spectra with
+COMP/LINER properties (the KPNO spectrum of Mkn 18 and NGC 62 40, a luminous infrared
+galaxy known to show contributions from both the AGN and star bursts (Sanders et al. 1988)), 2
+spectra with Seyfert/H II(both the KPNO and literature spectra of NGC 4102), and 2 spec tra
+with Seyfert/LINER properties (NGC 1275 (which is in the mid dle of a strong emission nebulae
+associated with the cooling ﬂow in the Perseus cluster) and N GC 4138). In general, there is
+good agreement between classiﬁcations of sources with mult iple spectra. Both Mkn 417 and Ark
+347 spectra indicate a Seyfert and the NGC 4102 spectra show a n ambiguous source between
+Seyfert/H II. While the Mkn 18 classiﬁcations are not the same, they both p oint to having at least
+some H II-like emission line ratios (particularly [S II]/Hα).
+While it is clear that broad line sources are Seyfert 1s, it is of interest to examine how they
+would be classiﬁed based on their narrow line ratios. If the p redictions of the uniﬁed model are
+true then, if the broad line region is absorbed out, the narro w line ratios should classify these
+objects as Seyferts also. We ﬁnd, much to our surprise, that a signiﬁcant fraction of the broad line
+objects have narrow line ratios which lie outside the AGN reg ion based on the Kewley et al. (2006)
+classiﬁcations. While the majority (75%) of broad line sour ces have narrow line ratios consistent– 13 –
+with classiﬁcation as Seyferts (30 spectra), some (in parti cular NGC 931, 1RXSJ193347.6+325422,
+UGC 6728, and IGR21247+5058) are not, being classiﬁed as com posites or H IIsources, though H α
+and the [N II] lines were too heavily blended to separate for the latter tw o. Additionally, 7 spectra
+(including the KPNO and SDSS spectra of MCG +04–22–042) have ambiguous classiﬁcations.
+There is good agreement between classiﬁcations of sources w ith multiple spectra (i.e. MCG +04–
+22–042, NGC 4151, NGC 3227, NGC 3516). The source NGC 4051, cl assiﬁed as ambiguous from
+the KPNO spectrum due to the [N II]/Hαdiagram result showing a COMP, should more likely be
+classiﬁed as a Seyfert (as in the spectrum analyzed in the lit erature).
+Therefore, the Swift BAT AGN optical classiﬁcations are mos tly Seyferts. There are a total of
+29 individual narrow line sources represented, and of these , about 66% are Seyferts, 16% LINERs,
+13% ambiguous, 3% composites, and 3% H IIgalaxies. Of the 35 broad line sources, about 75%
+are Seyferts, 14% are ambiguous, and 11% are composites or H IIgalaxies. We ﬁnd no broad line
+sources with narrow emission consistent with LINERs.
+Since we are studying in this paper the optical properties of a hard X-ray detected sample, it is
+useful to make a comparison with optically selected samples , in particular the recent results of the
+SDSS. In this comparison, we ﬁnd that the optically selected emission-line sources from the 85224
+SDSS galaxy sample of Kewley et al. (2006) consist of very diﬀe rent percentages of the various
+classiﬁcation categories than our hard X-ray selected samp le. The SDSS sample consists of 75%
+star-forming/H IIgalaxies, 3% Seyferts, 7% LINERs, 7% composites, and 8% ambi guous. It is no
+surprise, that the majority of our 14–195keV X-ray sample co nsists of the much more energetic
+(across multiple bands) Seyferts. However, comparing the S DSS results solely with our narrow line
+sources, we are ﬁnding far fewer LINERs than we might expect. In the optically selected SDSS
+sample, the LINER class contains more than twice the number o f sources as Seyferts, while we are
+ﬁnding four-times as many Seyferts as LINERs among the narro w line sources.
+There are a few possibilities as to why the hard X-ray sample s elects fewer LINERs. The most
+obvious reason could be that LINERs are less luminous X-ray s ources (we discuss this further in
+§6). Indeed, Kewley et al. (2006) didﬁndthat LINERshadsubst antially lower reddeningcorrected
+[OIII] 5007˚A luminosities than Seyferts. If L [OIII]is an indicator of bolometric luminosity and
+scales with the Swift BAT luminosity, we may simply not be det ecting many LINERs with BAT
+because their X-ray ﬂuxes are below the current detection th reshold. Further, studies such as
+the Chandra snapshot analysis of Terashima & Wilson (2003) a lso ﬁnd LINERs as less luminous
+than Seyferts in X-rays. Also, based on the nuclear X-ray lum inosities of local LINER sources
+determined from the Chandra analysis of Flohic et al. (2006) who used the IR-selected LINER
+sample of Sturm et al. (2006), the typical local LINER would h ave a BAT ﬂux far below the ﬂux
+detection limit of the Swift survey.
+It is also possible that LINERs are more absorbed in the X-ray s. In Winter et al. (2009a), we
+have shown that the more X-ray absorbed (i.e. highest neutra l hydrogen column density) sources
+have lower X-ray luminosities, on average. If this is the cas e, we would expect to ﬁnd a higher– 14 –
+number of LINERs as Swift BAT detects more heavily absorbed a nd less luminous sources. In
+support of this possibility, the average value of the X-ray d erived N H= 6×1023cm−2of our
+LINERs is high (Winter et al. 2009a). This is in contrast, how ever, to the optical reddening, where
+we noted that the ratio H α/Hβis below the accepted value for AGN (3.1) and the theoretical ly
+expected value for case B recombination (2.85) for most of ou r LINERs. Kewley et al. (2006) also
+foundthis in 45% of their LINER sample, which could bethe res ult of a higher nebular temperature
+(Osterbrock 1989) orshocks. Inthesecases, it is unclearho w to relate theoptical Balmer decrement
+to the X-ray derived column density.
+With lower luminosities than typical AGN sources and emissi on line ratios potentially indicat-
+ing a shock origin, it is possible that LINERs are typically n ot powered by accretion processes. As
+Flohic et al. (2006) show, many LINERs do not have any detecte d X-ray emission. Further, recent
+work by the SAURON team (Sarzi et al. 2009) and SEAGAL collabo ration (Cid Fernandes et al.
+2009) indicates that themajority of LINERs are not powered b y AGN but instead by evolved stellar
+populations. Therefore, we would expect to detect few LINER s in the Swift BAT band.
+5. Additional Diagnostic Lines
+Comparisons of the intensities of multiple emission lines f rom the same ion provide important
+diagnostics of the gas in which they are produced. In the opti cal range probed by our spectra, the
+relative population and therefore intensity of [S II]λ6716/λ6731 depends on the density of the gas
+(with only a slight dependence on temperature of the order T1/2
+e). The [O III]λ4363 emission line
+comes from a diﬀerent upper energy level than the λ4959 and λ5007 lines, where the relative rates
+of excitation to these upper levels is strongly dependent on temperature. An equation relating the
+ratio of the [O III] lines to temperature and density is given in (Osterbrock 19 89) as:
+Iλ4959+Iλ5007
+Iλ4363=7.73exp((3 .29×104)/T
+1+4.5×10−4(Ne/T1/2). (6)
+In Figure 11, we plot the reddening corrected ﬂux ratios for b oth of these diagnostics ([S II]
+and [OIII]). While both intensity ratios do not necessarily probe the same regions of the narrow
+line region, this ﬁgure is useful in illustrating the range o f values measured for our sample. One of
+the results of our analysis is that the ratio of [S II]λ6716/λ6731 is similar for both the broad and
+narrow line sources. Using a Kolmogorov-Smirnov compariso n test, we ﬁnd that both distributions
+are likely to be drawn from the same population with D= 0.22 andP= 0.50. The average and
+standard deviations of these values are 1.12 and 0.27 for the narrow line sources and 1.09 and 0.23
+for the broad line sources. These values of the ratio of [S II]λ6716/λ6731 correspond to electron
+densities of Ne≈103cm−3(assuming Te= 104K as in ﬁgure 6.2 of Peterson (1997)). These results
+are consistent with average narrow line region densities of 2000cm−3found by Koski (1978). Thus,
+the hard X-ray detected Swift BAT AGN have the same densities as optically selected AGN in this
+region (which produces the [S II] emission), regardless of whether broad lines are present.– 15 –
+The temperature sensitive diagnostic [O III] (λ4959+λ5007)/λ4363 clearly is not the same for
+the narrow and broad line sources. The Kolmogorov-Smirnov c omparison test yields a P-value of
+0.000. The average and standard deviation of [O III] (λ4959+λ5007)/λ4363 is 166.0 and 193.0 for
+the narrow line sources and 14.53 and 12.71 for the broad line sources. To better illustrate what
+these values mean, in Figure 11 we also plot the relationship of the [O III] temperature diagnostic
+versus electron density for ﬁxed temperatures. The average values of both the narrow and broad
+line sources are indicated with a horizontal line. In the low density limit ( Ne<104cm−3), the
+average temperature of the [O III] emitting gas is approximately 10000K for narrow line sourc es
+and 50000K for broad line sources. Typical temperatures for narrow line regions are between
+10000–25000K, with an average value of 16000K reported in Ko ski (1978).
+If the temperature of the narrow line region in the type 1s and 2s is diﬀerent, this would
+be a violation of the uniﬁed model. However, if the densities are diﬀerent, this might be due to
+geometrical eﬀects wherein the dense regions in type 2s are bl ocked from our view or have very
+high reddening values. However, there is uncertainty in the measurement of [O III] (λ4959 +
+λ5007)/λ4363 associated speciﬁcally with the measurement of the fai nt [OIII]λ4363˚A line, which
+is just 1% of the bright λ4959˚A andλ5007˚A lines. We note that it is particularly hard to measure
+this line in the broad line sources where H γλ4340˚A may be producing a tilted pseudo-continuum.
+The result of broad line sources having lower values of [O III] (λ4959 +λ5007)/λ4363 than
+narrow line sources has been noted before and is attributed t o broad line sources having stronger
+λ4363 emission (Osterbrock 1978). Instead of a higher temper ature in the narrow line regions of
+broad line sources, Osterbrock (1978) suggests densities o f 106–107cm−3in broad line sources and
+/lessorsimilar105cm−3in narrow line sources. To reconcile these high densities wi th lower densities derived in
+the S+emission region, the narrow line region must consist of a ran ge of densities, among which
+low densities are found in low-ionization regions. Under th is interpretation, the temperatures of
+the narrow line region producing O+2are the same for broad and narrow line sources, provided the
+densities diﬀer in this higher ionization region.
+6. [O III] and Hard X-ray Luminosities
+AfundamentalpropertyofanAGN isitspower, measuredthrou ghluminosity. InFigure12, we
+plot the distributions of both the observed and extinction- corrected [O III] 5007˚A luminosities for
+both our narrow line and broad line sources. For sources with multiple measurements, we averaged
+the values together to obtain a single measurement of observ ed and extinction corrected luminosity
+per source (these values are included in Table 15). We ﬁnd tha t the extinction corrections do not
+signiﬁcantly change the luminosity measurements, with the corrected values being on average 1.1
+(broad line sources) and 1.3 (narrow line sources) times lar ger than the observed luminosities.
+Themeanvalueforthedistributionof extinction corrected luminosity forthebroadlinesources
+is logL [OIII]= 41.79 with a standard deviation of 0.90, while the narrow line so urces have a mean– 16 –
+value of logL [OIII]= 40.82 with a standard deviation of 1.16. The results of a Kolmogr ov-Smirnov
+comparison test suggest that these values are not drawn from a single population ( D= 0.49 and
+P= 0.001). Therefore, the broad line sources appear to be more lum inous than the narrow line
+sources, on average. This is also true of the observed lumino sities (the averages and standard
+deviations are 41.76, 0.79 (broad line sources) and 40.87, 1 .08 (narrow line sources)) and therefore
+not an eﬀect of incorrect reddening corrections. If the [O III] 5007˚A emission line is indeed an
+estimator of the AGN power (assuming that the contamination from star formation is not great),
+theseresults agree withour X-ray results fortheBAT AGNs. N amely, Winter et al. (2009a) showed
+that the unobscured X-ray sources (presumably optical broa d line sources) in the sample were also
+intrinsically more luminous.
+In§4, we described that previous optical and X-ray studies ﬁnd L INERs as less luminous
+than Seyferts. Comparing the extinction-corrected [O III] luminosities for the narrow line sources,
+we conﬁrm these results with our unbiased hard X-ray detecte d sample. We ﬁnd Seyferts have an
+average valueoflogL [OIII]= 41.55 withastandarddeviation of0.85, LINERshaveanaverage v alue
+of logL [OIII]= 40.73 with a standard deviation of 0.60, and sources in other cat egories (including
+ambiguousclassiﬁcations, H IIgalaxies, andcomposites) haveanaverage valueoflogL [OIII]= 40.33
+with a standard deviation of 0.65. Of particular importance , we ﬁnd that the narrow line Seyferts
+have luminosities consistent with those of broad line sourc es.
+Further, we ﬁnd that the hard X-ray luminosities (in the 14–1 95keV band) show these same
+trends. To illustrate these results, we plot the distributi on of hard X-ray luminosity for our
+sources in Figure 13. For the narrow line sources, we ﬁnd that the Seyferts have an average
+value of logL 14−195keV= 43.87 with a standard deviation of 0.94, LINERs have an average v alue
+of logL 14−195keV= 43.50 with a standard deviation of 0.16, and sources in other cat egories have
+an average value of logL 14−195keV= 42.69 with a standard deviation of 0.98. Once again, the
+HII/composites/ambiguous sources have the lowest luminositi es while the Seyferts are most lumi-
+nous. Also, the X-ray luminosities of the narrow line Seyfer ts are consistent with those of the broad
+line sources (which have an average value of logL 14−195keV= 43.74 with a standard deviation of
+0.74).
+BasedonX-raysurveys, severalstudieshadfoundthefracti onofobscuredsourcestoincreaseat
+lower 2–10keV luminosities, including those by Ueda et al. ( 2003) and Steﬀen et al. (2003), as well
+as our own study of the Swift sources (Winter et al. 2009a). Ba sed on an optically selected sample,
+Diamond-Stanic et al. (2009) also found diﬀerences in the dis tributions of 2–10keV and [O III]
+λ5007˚A luminosities for Sy 1s andSy 2s in therevised Shapley-Ames sample (Sandage & Tammann
+1987). A clear explanation for the diﬀerences in the X-ray sel ected samples is that the lowest
+luminosity X-ray sources, which tend to be absorbed sources , are not optical Seyferts, as found
+in our current study. In an optically deﬁned sample, we would expect both the obscured and
+unobscured Seyferts to have the same luminosity distributi ons. However, in this same optically-
+selected sample Diamond-Stanic et al. (2009) ﬁnd that the [O IV]λ25.89µm line, an indicator of
+bolometric luminosity (Mel´ endez et al. 2008), does not sho w this diﬀerence in distributionsbetween– 17 –
+Sy1sandSy2s. Itisunclearhowtointerprettheseresults. S incethestudyofDiamond-Stanic et al.
+(2009) consists of only sources for which multi-wavelength luminosity measurements are available
+(18 Seyfert 1s and 71 Seyfert 2s), it is potentially biased (c onsidering that X-ray surveys ﬁnd
+equal numbers of absorbed and unabsorbed sources) compared to the Swift sample. However,
+the Diamond-Stanic et al. (2009) sample also includes a high percentage of Compton-thick sources
+(20%), which the Swift sample is currently not ﬁnding (due to the low X-ray ﬂux in the BAT band
+of Compton thick sources).
+Since the hard X-ray luminosities are at high enough energie s to cut through much of the
+gas and dust around the AGN, they are a good estimate of the bol ometric luminosity. In lieu of
+these measurements, the optical [O III] luminosities are often used as a measurement of the AGN
+total power. Further, in support of using the [O III] luminosities as a proxy for the bolometric
+luminosity, Heckman et al. (2005) found a relationship betw een the observed hard X-ray (3-20keV)
+and observed [O III] luminosities for a sample of AGN in the RXTE slew survey. How ever, the
+results from a sample of Swift BAT AGN dispute the claim that [ OIII] luminosities are good
+estimates ofbolometric luminosity. Mel´ endez et al. (2008 ) foundthat [O III] was notwell-correlated
+with the hard X-ray (14–195keV).
+With our larger and more uniformly measured extinction-cor rected [O III] sample than in the
+Mel´ endez et al. (2008) sample (drawn from the 3-month Swift catalog (Markwardt et al. 2005)),
+we tested for a correlation between the BAT and [O III] luminosities. In Figure 14a, we plot the
+results of our comparison. We ﬁnd weak linear correlations b etween the 14–195keV and [O III]
+luminosities for the broad and narrow line sources. Using th e ordinary least-squares (OLS) bisector
+method (Isobe et al. 1986)), we found L[OIII](corr)∝L1.16±0.13
+14−195keVandR2= 0.34 (P≈0.005) for the
+broad line sources and L[OIII](corr)∝L1.16±0.24
+14−195keVandR2= 0.42 (P≈0.002) for the narrow line
+sources. Here, R2is the correlation coeﬃcient. As further illustrated in the ratio of optical/hard
+X-ray luminosity in Figure 14b, there is a great deal of scatt er in these relationships (e.g. more
+than 2 magnitudes at log L14−195keV). Our results support those of Mel´ endez et al. (2008), show ing
+that even the reddening corrected L[OIII]is aﬀected by extinction. This eﬀect is most pronounced
+for the narrow line sources, which show the greatest amount o f scatter.
+As shown in Rigby et al. (2009), at high levels of absorption t he luminosities measured in the
+Swift BAT band are aﬀected by extinction. Using models from Ma tt et al. (2000), they show the
+diﬀerence between the emergent and input BAT ﬂux at a variety o f column densities. For column
+densities less than 1023cm−2, this eﬀect is minimal ( ≤4%). Since none of our targets are Compton
+thick (NH<1024cm−2in the Swift sample, see Winter et al. (2009b) for Suzaku obse rvations of
+heavily obscured sources conﬁrming their Compton thin natu re), the eﬀects on our sample are
+conﬁned to a factor of ≈10−20% for the highest column density sources (25% of the narrow line
+sources). Even with this level of scatter introduced in the B AT luminosities, clearly the scatter
+seen in the narrow line sources in Figure 14 is not accounted f or by a 20% underestimate in BAT
+luminosity.– 18 –
+7. Mass and Accretion Rate Estimates
+Foreachofthebroadlinespectra, wewereabletoderivethem assofthecentral blackholeusing
+the FWHM of the broad component of H βand the continuum luminosity at 5100 ˚A. The continuum
+luminosity at 5100 ˚A was computedfromapower law continuumﬁt totheH βregion. We calculated
+the Hβmasses using our measurements in Table 9 and equation 5 from V estergaard & Peterson
+(2006). Thecomputedvaluesofextinctioncorrected λLλ(5100˚A)andM HβareincludedinTable15.
+At the resolution of our spectra, we found that the H βline is often more complicated than a simple
+combination of narrow and broad Gaussian proﬁles. Addition al structure or asymmetries are seen
+in a number of sources, making our measurements an approxima tion of the broad H βline FWHM
+(see Figure 5 for example ﬁts).
+To test how our values of M Hβcompare with other mass estimates, we plot our values versus
+reverberation mapping masses and masses derived from the st ellar K-band light from 2MASS
+photometry in Figure 15. The mass estimates from reverberat ion mapping were obtained for 9
+sources from Peterson et al. (2004) and are listed in Table 15 . As shown, our H βderived masses
+are in good agreement with the reverberation mapping result s (with the exception of NGC 4593).
+There are no systematic oﬀsets between the two methods.
+Not surprisingly, there are larger diﬀerences between the IR derived and H βderived masses.
+The 2MASS K sband derived masses (Mushotzky et al. 2008; Winter et al. 200 9a; Vasudevan et al.
+2009) were calculated by subtractingthe central luminosit y of apoint source(the size of the2MASS
+PSF). This presumed AGN luminosity was subtracted from the i ntegrated luminosity of the galaxy
+to determine the luminosity of the stellar bulge. The relati on deﬁned by Novak et al. (2006) was
+then usedto convert the bulgeluminosity to stellar mass. Ap proximately 40% of themass estimates
+from the 2MASS K s-band and H βare within a factor of 2 of each other. A greater majority of th e
+IR masses are higher (typically, by up to a factor of 10).
+Despitethefactthatthe2MASSK sbandderivedmassesarealessaccuratemassdetermination
+than those using reverberation mapping or the H βFWHM method, we ﬁnd that the 2MASS and
+HβFWHM masses are linearly correlated. Using the OLS bisector method, we ﬁnd
+logM2MASS= (0.91±0.14)×logMHβ+(1.07±1.13), (7)
+withR2= 0.56. This is encouraging since the 2MASS derived measurement s are the only uniform
+estimates that we have for the narrow line and broad line sour ces. Therefore, we use the 2MASS
+derived masses to compare estimated masses, and later accre tion rates, between all of our sources.
+Unlike our comparison of luminosities (log L[OIII]), we ﬁnd that the 2MASS derived masses show a
+great probability (from the K-S test) of the narrow and broad line masses being derived from the
+same population ( D= 0.21 andP= 0.71). The mean and standard deviations of log( MIR/M⊙)
+are 8.07 and 0.83 (narrow line sources) and 8.19 and 0.62 (bro ad line sources). With the more
+accurate H βFWHM method, we ﬁnd that the average mass of our sources (base d on the broad
+line sources) is log M/M⊙= 7.87 with a standard deviation of 0.66. The range of masses, as shown– 19 –
+in Figure 15, is consistent with those found in other AGN surv eys. For example, our values are
+consistent with the range, 106–7×109M⊙, found by Woo & Urry (2002) in a sample of 377 AGNs.
+Our values are also similar to those of nearby PG QSOs derived from H-band host magnitudes
+(Veilleux et al. 2009).
+Since the masses of our narrow and broad line sources are simi lar while the average narrow
+line source luminosities are lower, we expect the values of L [OIII]/LEddto diﬀer. The [O III]
+λ5007˚A luminosity is often used as an estimate of the bolometric lu minosity of AGN, particularly
+for sources detected in the SDSS (see Heckman et al. (2004)). Typical bolometric corrections
+for extinction corrected [O III] luminosities are expected to be between 600–800 for Seyfer t 1s
+(Kauﬀmann & Heckman 2008). There are, however, problems with using L [OIII]as an estimate of
+bolometric luminosity. In the previous section, we showed t hat the hard X-ray luminosities, which
+are less aﬀected by contamination from star formation and ext inction, are not well-correlated with
+L[OIII], particularly for the narrow line sources. Despite these pr oblems, the ratio of L [OIII]/LEdd
+allows us to compare a rough estimate of the accretion rates o f our broad and narrow sources, which
+we can also compare with the more robust values we obtained in our X-ray study. In Figure 16, we
+plot the results (where L Eddis deﬁned as 1 .38×1038(M/M⊙) and the mass is obtained from the
+2MASS measurements). We ﬁnd, as expected, that the ratio of L [OIII]/LEddis lower for the narrow
+line sources, with the average and standard deviations corr esponding to 10−5.25±0.81(narrow) and
+10−4.61±0.85(broad). Since only three LINERs and two H II/composite/ambiguous sources have
+available 2MASS-derived masses, we can not test whether sou rces in these categories have lower
+L[OIII]/LEddvalues than Seyferts.
+For the broad line sources, our estimate of the average accre tion rate ( Lbol/LEdd), assuming a
+bolometric correction of 600, is 0.015 with the 2MASS derive d masses or 0.034 with the H βFWHM
+derived masses. Based on our X-ray analysis (Winter et al. 20 09a), the 2MASS derived masses,
+and an assumed 2–10 keV bolometric correction of 35 for unabs orbed sources (Barger et al. 2005),
+we estimate an X-ray derived accretion rate of 0.040. Theref ore, there is very good agreement
+between the optical and X-ray derived accretion rates, in an average sense. Unfortunately, with
+increased uncertainty in the bolometric corrections, it is more diﬃcult to determine these values
+for the narrow line/Sy 2 sources.
+8. Host Galaxy Properties
+Since the Swift BAT-detected AGN are relatively close ( < z >≈0.03) and bright, intrinsic
+stellar absorption features are seen in the majority of the s pectra we analyzed. This allows us
+to determine some of the properties of the host galaxies of ou r target AGN. To do this, we have
+employed two particular methods to analyze the intrinsic st ellar absorption features – one using
+continuum ﬁts and the other measuring stellar absorption in dices. We note, however, that the
+sampling of the host galaxy populations for the BAT-detecte d AGN is not uniform, but a function
+of the aperture size (2–3′′), distance to the source, and both the size and orientation o f the host– 20 –
+galaxy within the slit. It is our intent, in this paper, to det ermine basic conclusions about the
+stellar populations from the optical spectra. More detaile d information on the host galaxies of
+this sample, including star formation rates from Spitzer fo llow-ups and colors from an analysis of
+ground-based optical imaging data, will be presented by our collaborators.
+The ﬁrst method we used to obtain information about the AGN ho st galaxy populations was
+the continuum model ﬁtting described in §3.1. For each of our sources, we ﬁt the continuum with
+a combination of a power law (representing the non-thermal c ontinuum) and a combination of a
+young, intermediate, and old single stellar population mod el, utilizing three diﬀerent metallicities.
+Wethencreatedagridoftestcasestotesttheabilityofthec ontinuummodelstoaccurately describe
+the host galaxy spectrum, ﬁnding that metallicities could n ot be determined but that young stellar
+populations are clearly distinguished between both the int ermediate and old stellar populations
+(see§A). There is a degree of degeneracy between the intermediate and old populations as well
+which occurs when these populations are in combination with other populations (for example, a
+model of 50% intermediate and 50% young populations can be eq ually well modeled with a best ﬁt
+continuum model that is a combination of young, intermediat e, and old populations).
+The main result of our continuum model ﬁts is that the majorit y of the Swift BAT AGN in our
+sample have either a weak or no contribution from young stell ar populations and are dominated
+by intermediate/old populations. Of the sources with conti nuum light dominated by stellar popu-
+lations, only one source has 50% or more of their light domina ted by a young (25Myr) population
+– NGC 4151, whose host galaxy is a barred spiral (Sab) with a ri ng of star formation. This is in
+contrast with the 15 sources with 50% dominated by intermedi ate (2500Myr) populations and the
+23 with 50% or more dominated by old (10000Myr) populations. To these results, however, we
+must add the caveat that we measured the continua with very si mpliﬁed models. It is also possible
+that degeneracies between the power law and young stellar co mponent exist.
+Still, the result of the BAT AGN hosts being largely composed of intermediate to old popula-
+tions, is supported further through an analysis of the H δAand Dn(4000) stellar absorption indices.
+These age sensitive indicators, the former sensitive to rec ent star bursts and the latter to an indi-
+cator of old populations through measurement of the Ca IIbreak, reveal few sources (6 total) in
+the region of the H δA-Dn(4000) parameter space occupied by systems with signiﬁcant contributions
+from young stellar populations ( /greaterorsimilar30%). Due to contamination of the absorption features from
+AGN emission lines (i.e. [Ne III]λ3869˚A and H δ), this result is based largely on the obscured
+sources.
+Based on an SDSS study by Kauﬀmann et al. (2003a), low luminosi ty narrow line AGN are
+hosted in old galaxies (as indicated by D n(4000)). This is consistent with the results of our study.
+Additionally, we ﬁnd that the distribution of our narrow lin e sources in the H δA–Dn(4000) plot is
+consistent with the location of ‘strong’ AGN in the SDSS samp le (Figure 17 in Kauﬀmann et al.
+(2003a)). Since their deﬁnition of strong (3 .85×1040ergss−1in [OIII]λ5007˚A) includes the
+majority of our sources, this shows that our results are cons istent with the SDSS results. As shown– 21 –
+in Kauﬀmann et al. (2003a), the values of D n(4000) for our narrow line sources are indicative of
+normal late-type galaxies. This is also consistent with our analysis of the morphologies of the
+9-month sample AGNs, as listed in NED. In Winter et al. (2009a ), we had shown that the hosts of
+our sources (both Sy1 and Sy2 sources) were mostly spirals an d irregulars.
+Another result from the Kauﬀmann et al. (2003a) study, is a con nection between the age
+distribution of host galaxies and the [O III] luminosity of the AGN. In Figure 17, we plot each
+of the stellar age indicators (H δAand Dn(4000)) versus the extinction-corrected [O III] luminosity
+and the ratio L [OIII]/LEddfor both the narrow and broad line AGN. The top plots of this ﬁg ure
+are comparable to Figure 12 of Kauﬀmann et al. (2003a) (whose L [OIII]measurements are in units
+of L⊙). We ﬁnd no direct correlation between either of these stell ar absorption indices and either
+[OIII] luminosity or accretion rate ( R2/lessorsimilar0.1). Since our sources include only the equivalents of
+SDSS ‘strong’ AGN, it is not surprising that we do not see a cor relation. Our sample does not
+include weak AGN, which tend to have older populations (asso ciated with early type galaxies).
+Finally, we ﬁnd a possible indication that the host galaxies of broad and narrow line sources
+may be diﬀerent. Namely, we see diﬀerences in the metallicity i ndicator Mgb. Applying the
+Kolmogorov-Smirnov test, we ﬁnd a P-value of 0.01, indicating that the populations are likely
+diﬀerent. For the broad line sources, we ﬁnd an average value o f 0.84 with a standard deviation of
+1.65 in Mgb. The narrow line sources have a much higher averag e Mgb measurement of 1.96 with
+a standard deviation of 2.27. Based on our simulations, lowe r values of Mgb also correspond to
+younger populations (see the top left panel of Figure 20). Th erefore, there is a degeneracy between
+age and metallicity such that the result of broad line source s having lower values of Mgb could
+indicate their hosts as either having a larger contribution from a younger population or from a
+lower metallicity than the hosts of narrow line sources.
+9. Conclusions
+AGN surveys are typically dominated by two selection eﬀects: (1) dilution by starlight from
+the host galaxy and (2) obscuration by dust and gas in the host galaxy and/or the AGN itself (see
+Hewett & Foltz (1994); Mushotzky (2004)). For these reasons , an unbiased AGN sample is diﬃcult
+to deﬁne. The Swift’s BAT AGN survey provides one of the ﬁrst t ruly unbiased (to all but the
+highest column densities) samples of local AGNs.
+Since the BAT-detected sources are nearby, < z >= 0.03 (Tueller et al. 2008), they are ex-
+cellent targets for multi-wavelength follow-ups. In this p aper, we presented the optical spectral
+properties from sources detected in the ﬁrst 9-months of the survey. Our analysis includes both the
+emission line properties of the AGN as well as the host proper ties revealed from intrinsic stellar ab-
+sorption features. The sample includes 40 spectra taken at t he 2.1-m KPNO telescope, 24 archived
+SDSS spectra, and the emission line properties of 13 sources presented in the literature. In total,
+this sample covers 81% of the Swift BAT AGN sources viewable f rom KPNO. It is comprised of– 22 –
+55% broad line sources and 45% narrow line sources, in the sam e ratio as the total Swift sample.
+With our unbiased AGN sample, it is important to compile the f undamental properties of the
+sources both as a test to our current understanding of AGN and as a comparison to more biased
+methods of detection (e.g. optical surveys). Using standar d emission line diagnostic plots, we ﬁnd
+that the majority of our hard X-ray detected sources are opti cally Seyferts (66% of narrow line and
+75% of broad line sources). This contrasts with the opticall y selected SDSS sample examined by
+Kewley et al. (2006), which includes a large (75%) fraction o f HIIgalaxies with few Seyferts (3%).
+Since H IIgalaxies are less luminous than Seyferts in the X-ray band (R analli et al. 2003), it is not
+surprising that our hard X-ray ﬂux limited sample detects th e more luminous local sources, which
+are Seyferts. In the same sense, the optical SDSS sample dete cts more LINERs, which are also less
+luminous sources than Seyferts, than we ﬁnd in the Swift BAT s ample. In particular, we classify
+16% of the narrow line sources as LINERs and none of the broad l ine sources.
+One of the most fundamental properties of a black hole is its m ass. Under the uniﬁed AGN
+model, we expect to ﬁnd no diﬀerence in the mass distribution b etween the broad and narrow line
+sources. Indeed, we ﬁnd the distributions of our 2MASS deriv ed masses statistically consistent
+with being drawn from the same population. Comparing 2MASS d erived masses with a more
+accurate determination from the FWHM of H βin broad line sources, we ﬁnd the masses from
+both methods are well correlated. The average value of our ha rd X-ray detected sources is <
+M/M⊙>= 107.87±0.66, with a range of values consistent with those found in previo us studies of
+AGNs (Woo & Urry 2002) and nearby PG QSOs (Veilleux et al. 2009 ).
+Determinations of the reddening from the ratio of narrow H α/Hβ, as well as gas densities and
+temperatures in the narrow line regions from diagnostic emi ssion lines of the same ion, are also
+consistent with both the uniﬁed model and previous results f rom optical studies. Under the uniﬁed
+model, we expect narrow line sources to have heavier extinct ion (assuming the extinction is on the
+nuclear/galactic scale and not simply from the torus), whil e other narrow line region properties
+like density and temperature to be the same for narrow and bro ad line sources. As expected, we
+ﬁnd the average distribution of reddening values [E(B-V)] h igher in the narrow line sources. In
+our calculations of the gas density in the S+emission region, we ﬁnd the same electron densities
+ofNe≈103cm−3for broad and narrow line sources. Superﬁcially, the O+2region appears at a
+higher temperature for the broad line sources. However, as d iscussed in Osterbrock (1978), a likely
+explanation is that the narrow and broad line sources both ha ve similar temperatures (we ﬁnd
+Te≈10000K), but in the broad line sources we are able to probe [O III]λ4363 emitting gas into
+denser regions of the narrow line region.
+Based on the results of our X-ray study of our unbiased AGN sam ple, we suspect that the
+distributions of luminosities of the Swift AGN conﬂict with the uniﬁed model. Namely, our X-ray
+results (Winter et al. 2009a) showed that the absorbed/type 2 AGNs (X-ray absorbed/optically
+narrow line sources, including optically classiﬁed Sy2s, L INERs, and H IIgalaxies) have lower ab-
+sorption corrected 2–10keV luminosities and accretion rat es. These same trends are found among– 23 –
+the optically derived luminosities and accretion rates. Sp eciﬁcally, we ﬁnd average extinction-
+corrected 5007 ˚A [OIII] luminosities of 1041.74±0.93ergss−1and 1040.94±1.00ergss−1and ratios of
+L[OIII]/LEddof 10−4.61±0.85and 10−5.25±0.81, respectively for broad and narrow line sources. Con-
+trary to the results of Heckman et al. (2005), but in agreemen t with Mel´ endez et al. (2008), we ﬁnd
+that the 14–195keV BAT luminosities are only weakly correla ted with [O III] luminosity for broad
+and narrow line sources.
+Seemingly, the result of narrow line sources having lower lu minosities and possibly accretion
+rates (depending on the bolometric corrections) poses a cha llenge to the uniﬁed model. On closer
+inspection, we ﬁnd that the narrow line sources with optical classiﬁcations as Seyferts have similar
+X-ray and optical luminosities to their broad line, Seyfert 1 counterparts. Instead, it is the sources
+optically classiﬁed as LINERs and H II/composite/ambiguous sources which have lower luminosi-
+ties. While these sources are clearly detected AGN based on t heir X-ray properties, modiﬁcation
+of the uniﬁed model to include a luminosity dependence is cle arly required to link these fainter
+non-Seyfert sources with the Seyfert 1s and 2s.
+Finally, through our continuum model ﬁts and measurements o f stellar absorption indices, we
+can make a few general comments on the host galaxy properties of our sources. We ﬁnd that
+the stellar ages of the hosts include small contributions fr om young populations (0.25Gyr). The
+populations are more consistent with intermediate/old (2. 5–10Gyr) populations. Comparing with
+the results drawn from the SDSS survey, we ﬁnd that our narrow line sources have the same
+properties as the ‘strong’ narrow line AGN from Kauﬀmann et al . (2003a). Therefore, their stellar
+absorption properties (from the Ca IIbreak and H δabsorption) are like those of late type galaxies.
+This is also consistent with the NED morphologies of our sour ces (both Sy 1s and Sy 2s), which
+are mostly spirals and irregulars (Winter et al. 2009a).
+The authors would like to greatly thank Christy Tremonti for use of her analysis codes and
+discussions on how to modifythem for application to our AGN s ources. L.W. acknowledges support
+by NASA grant NNX08AC14G. Also, she acknowledges support th rough NASA grant HST-HF-
+51263.01-A, through a Hubble Fellowship from the Space Tele scope Science Institute, which is
+operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA
+contract NAS5-26555. S.V. acknowledges support from a Seni or Award from the Alexander von
+HumboldtFoundation andthanksthehost institution, MPE Ga rching, wheresomeof this work was
+performed. K.T.L. acknowledges support from the NASA Postd octoral Program Fellowship (NNH
+06CC03B). The Kitt Peak National Observatory observations were obtained using MD-TAC time
+as part of the thesis of L.W. at the University of Maryland (fo r programs 0322 and 0107) and M.K.
+(program 0295). Kitt Peak National Observatory, National O ptical Astronomy Observatory, is
+operated by the Association of Universities for Research in Astronomy (AURA) under cooperative
+agreement with the National Science Foundation.
+Facilities: Swift (), KPNO:2.1m (), Sloan ()– 24 –
+A. Galaxy Continuum Spectral Fits
+In this section, we detail additional tests that we conducte d to test the accuracy of the galaxy
+continuum ﬁts. As explained in §3.1, we used a grid of single stellar age population models
+(Bruzual & Charlot 2003) with 3 diﬀerent ages (25, 2500, and 10 000 Myr) and at 3 diﬀerent metal-
+licities (2.5Z ⊙, Z⊙, and 0.2 Z ⊙) to ﬁt the continua of our AGN and template galaxy spectra. In
+order to test the accuracy of these models, we constructed a g rid of test spectra, broadening the
+sources by assuming FWHM = 300kms−1(σ≈128kms−1) and adding both random noise and
+reddening ( τ= 1.5) to the stellar population models used in the continuum ﬁts . This grid of
+models includes a young, intermediate, and old population, as well as the following combinations:
+50% young + 50% intermediate, 50% young + 50% old, 50% interme diate + 50% old, and 33%
+young + 33% intermediate + 33% old. In Figure 18, we plot sever al of these test spectra.
+Assuming an error of 10% in the ﬂux, we ﬁt each of the test spect ra with the model spectra
+used to ﬁt the continua of our target spectra. The results of t hese ﬁts are shown in Table 16.
+Our results show that the velocity dispersions are accurate ly measured by the models in all cases.
+The metallicities, however, are not since all of our test spe ctra have solar metallicity but a range of
+values are found from the ﬁtting process. We also ﬁnd that the young stellar population component
+is measured well, though its contribution is underestimate d by up to about 20%. Finally, we ﬁnd
+that there is a degeneracy between the intermediate and old p opulations when they are found in
+combination with the young population. This is well illustr ated in Figure 18, where there is little
+diﬀerence between the 50% young + 50% intermediate and 50% you ng + 50% old spectra. We do,
+however, ﬁnd that a 100% intermediate population is disting uishable from a 100% old population.
+Therefore, the main conclusion that we draw from our test spe ctra is that our continuum model
+ﬁts can clearly distinguish between young and intermediate /old populations. See Kauﬀmann et al.
+(2003b) for more detailed investigations used to study the S DSS host galaxies.
+In a similar manner, we also created test spectra to look for d egeneracies between the stellar
+continuum and power law component. To accomplish this, we us ed the same set of test galaxy
+models as above. For each of these test spectra, we added a pow er law component with an index
+(p1) set to the average value determined from ﬁts to our AGN sourc es (0.67). We constrained the
+values such that the light fraction from both the stellar lig ht and power law contributed 50% of
+the light at 5500 ˚A. Results of these ﬁts are presented in Table 17. We ﬁnd that t here is no obvious
+degeneracy between any of the stellar population models and the power law component (at least
+at this power law index). The average ﬁtted power law index, 0 .74, is slightly higher than the true
+value while the ﬁtted fraction of light contributed from the power law tends to be slightly lower
+than the true value (most of the values are between 0.41–0.45 instead of 0.50). Generally, we ﬁnd
+that the ﬁtted values are consistent with the input paramete rs.
+In addition to testing the accuracy of the continuum ﬁts, we a lso used our grid of test galaxy
+spectra (excluding a power law contribution) to interpret t he results of measurements of stellar
+absorption indices in our target spectra. In addition to usi ng the grid of solar models we described– 25 –
+above, we created grids of populations with metallicities 2 .5 and 0.20 times solar abundance. For
+all of these sources, we measured the stellar absorption ind ices in the same manner as for our
+target spectra (see §3.3). In this way, we can use our test spectra, which are of app roximately the
+same signal-to-noise as our target spectra, to understand t he results of an analysis of the stellar
+absorption indices.
+In Figure 19, we plot the H δAindex versus D n(4000) for our test spectra. As we described in
+§3.3, these two indices are commonly used as indicators of the age of stellar populations. As the
+plot shows, metallicity of the stellar population models do es not have a large eﬀect on these stellar
+absorption indices. Further, as expected, there is a clear d ependence on age, where populations
+with a signiﬁcant (33% or higher) contribution from a young p opulation have both the highest
+values of H δA, associated with recent bursts of star formation, and the lo west values of D n(4000),
+which indicates the strength of the Ca IIbreak. We ﬁnd that the populations with signiﬁcant
+contributions of young populations have H δA>2 and D n(4000)<1.2.
+InFigure20,weplotadditionalstellarabsorptionindices oftenusedasmetallicity indicators(as
+wellastheCa IIbreakageindicator)forthetestgalaxyspectra. Eachmetal licity isrepresentedwith
+a diﬀerent color, with the same grid of diﬀerent stellar popula tion components mentioned above.
+We point out that, as shown in the D n(4000) versus Mgb plot, that the populations with signiﬁcan t
+contributionsfromyoungstars( <1.2) tendtohavelower valuesofMgb( /lessorsimilar3). Distinctionsbetween
+intermediate/old higher metallicity (Z ⊙and 2.5 Z ⊙) and low metallicity (0.2 Z ⊙) populations are
+seen in the C 24668 vs. Mgb, [MgFe] vs. Mgb and <Fe>vs. Mgb plots – where higher values in
+x and y parameters are seen for the higher metallicity popula tions. For young populations of any
+metallicity, it is more diﬃcult to distinguish between diﬀer ent metallicity populations.
+B. Notes on Individual Spectra
+In this section, we include notes on the emission line spectr a of the sources examined. These
+notes particularly relate to peculiarities in the spectra o r the ﬁtting procedurefor sources indicated.
+For 10 broad line sources (or ≈1/3 of the broad line sources), absorption lines from the Na ID
+doubletλ5890,5896˚A are seen. These absorption features are seen in Mkn 1018, Mk n 590, MCG
+-01-13-025, Mrk 6, SDSS J090432.19+553830.1, NGC 3227, NGC 3516, NGC 4593, MCG +09-21-
+096, NGC 5548, and RX J2135.9+4728. In the spectrum of MCG +09 -21-096, the absorption line
+is embedded in a broad He I(FWHM ≈2270kms−1) emission line. The Na ID doublet was also
+detected (by eye) in 9 narrow line sources: NGC 788, Mkn 18, SD SS J091129.97+452806.0, SDSS
+J091800.25+042506.2, Ark 347, NGC 4102, NGC 6240, UGC 11871 , and NGC 7319.
+Additionally:
+BROAD LINE SOURCES:– 26 –
+LEDA 138501: Hβhas a “red” wing.
+MCG -01-13-025, Mrk 1018, NGC 3227: Strong intrinsic absorption lines are seen in the
+spectra of these broad line sources. He Iis seen in absorption for both sources.
+IRAS 05589+2828: There is a clear broad component to He IIλ4686˚A. Hβhas a red wing.
+MCG +04-22-042: There is a clear broad component to He IIλ4686˚A.
+SBS 1136+594: There is a clear broad component to He IIλ4686˚A.
+UGC 6728: Two narrow emission lines are present for each of the [O III] emission lines (at
+λ4959˚Aandλ5007˚A).
+NGC 4593: Two narrow emission lines are present for each of the [O III] emission lines (at
+λ4959˚Aandλ5007˚A).
+MCG +09-21-096: The proﬁles of the broad Balmer lines are complex, with broad “boxy”
+shapes (including H δ, Hγ, Hβ, and Hα).
+Mrk 813: Hβis blended with the nearby [O III] emission lines.
+4C +74.26 : Hβis extremely broad and blended with the nearby [O III] emission lines at this
+resolution.
+NARROW LINE SOURCES:
+Mkn 18: Both the KPNO and SDSS spectra show an additional broad compo nent to H αof
+approximately 370kms−1.
+Ark 347: The Hαregion is quite complex. Six distinct narrow lines are seen i n the region
+including [N II]λ6548˚A, Hα, and [N II]λ6583˚A. The measured wavelengths of these lines are:
+6546.72±0.17,6555.7±0.34,6563.25±0.19,6570.23±0.08,6582.42±0.20, and 6591 .70±0.09˚A.
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+This preprint was prepared with the AAS L ATEX macros v5.2.– 30 –
+Table 1. SWIFT BAT-detected AGN
+Source RA (h m s) Dec (d m s) Redshift E(B-V)1Type2Host Galaxy2Obs.3
+Mkn 352 00:59:53.3 +31:49:36.8 0.015 0.06 Sy 1 SA0 Lit.
+NGC 788 02:01:06.5 – 06:48:55.8 0.014 0.03 Sy 2 SA(s)0/a KPNO
+Mkn 1018 02:06:16.0 – 00:17:29.2 0.043 0.03 Sy 1.5 S0; merger SDSS
+LEDA 138501 02:09:34.3 +52:26:33.0 0.049 0.16 Sy 1 KPNO
+Mkn 590 02:14:33.6 – 00:46:00.3 0.026 0.04 Sy 1.2 SA(s)a SDSS
+NGC 931 02:28:14.5 +31:18:42.1 0.017 0.10 Sy 1.5 Sbc Lit.
+2MASX J03181899+6829322 03:18:19.0 +68:29:31.6 0.090 0.7 2 Sy 1.9 KPNO
+NGC 1275 03:19:48.2 +41:30:42.1 0.018 0.16 Sy 2 NLRG Lit.
+3C 105 04:07:16.5 +03:42:25.8 0.089 0.48 NLRG KPNO
+3C 111 04:18:21.3 +38:01:35.8 0.049 1.65 Sy 1 N KPNO
+2MASX J04440903+2813003 04:44:09.0 +28:13:01.0 0.011 0.8 5 (Sy2) S KPNO
+MCG -01-13-025 04:51:41.5 – 03:48:33.7 0.016 0.04 Sy 1.2 SAB (s)0+ pec KPNO
+1RXS J045205.0+493248 04:52:05.0 +49:32:45.0 0.029 0.73 S y 1 KPNO
+NGC 2110 05:52:11.4 – 07:27:22.3 0.008 0.38 Sy 2 SAB0- Lit.
+MCG +08-11-011 05:54:53.6 +46:26:22.0 0.021 0.22 Sy 1.5 SB0 KPNO
+IRAS 05589+2828 06:02:10.7 +28:28:22.1 0.033 0.43 Sy 1 KPNO
+Mkn 3 06:15:36.3 +71:02:15.0 0.014 0.19 Sy 2 S0 KPNO
+2MASX J06411806+3249313 06:41:18.0 +32:49:31.4 0.048 0.1 5 Sy 2 KPNO
+Mkn 6 06:52:12.2 +74:25:37.0 0.019 0.14 Sy 1.5 SAB0+ KPNO
+Mkn 79 07:42:32.8 +49:48:34.8 0.022 0.07 Sy 1.2 SBb KPNO
+Mkn 18 09:01:58.4 +60:09:06.2 0.011 0.04 (HII/Ambig.) S? SD SS, KPNO
+SDSS J090432.19+553830.1 09:04:32.2 +55:38:30.3 0.037 0. 02 (Sy1.5) SDSS
+SDSS J091129.97+452806.0 09:11:30.0 +45:28:06.0 0.027 0. 02 (Sy2) SDSS
+SDSS J091800.25+042506.2 09:18:00.3 +04:25:06.2 0.156 0. 04 (Sy2) SDSS
+MCG -01-24-012 09:20:46.3 – 08:03:22.1 0.020 0.03 Sy 2 SAB(r s)c KPNO
+MCG +04-22-042 09:23:43.0 +22:54:32.6 0.033 0.04 Sy 1.2 SDS S, KPNO
+Mkn 110 09:25:12.9 +52:17:10.3 0.035 0.01 Sy 1 Pair? SDSS
+NGC 3227 10:23:30.6 +19:51:54.0 0.004 0.02 Sy 1.5 SAB(s) pec KPNO, Lit.
+Mkn 417 10:49:30.9 +22:57:52.4 0.033 0.03 Sy 2 Sa SDSS, KPNO
+NGC 3516 11:06:47.5 +72:34:07.0 0.009 0.04 Sy 1.5 (R)SB(s) K PNO, Lit.
+1RXS 112716.6+190914 11:27:16.3 +19:09:20.2 0.106 0.02 Sy 1.8 KPNO
+SBS 1136+594 11:39:09.0 +59:11:54.8 0.061 0.01 Sy 1.5 SDSS
+UGC 06728 11:45:16.0 +79:40:53.0 0.007 0.10 Sy 1.2 SB0/a KPN O
+CGCG 041-020 12:00:57.9 +06:48:23.1 0.036 0.02 (Sy2) SDSS
+NGC 4051 12:03:09.6 +44:31:52.7 0.002 0.01 Sy 1.5 SAB(rs)bc KPNO, Lit.
+Ark 347 12:04:29.7 +20:18:58.4 0.022 0.03 Sy 2 S0: pec SDSS, K PNO
+NGC 4102 12:06:23.0 +52:42:39.8 0.003 0.02 LINER SAB(s)b? K PNO, Lit.
+NGC 4138 12:09:29.8 +43:41:07.1 0.003 0.01 Sy 1.9 SA(r)0+ Li t.
+NGC 4151 12:10:32.6 +39:24:20.6 0.003 0.03 Sy 1.5 (R’)SAB(r s)ab KPNO, Lit.
+Mkn 766 12:18:26.5 +29:48:46.3 0.013 0.02 Sy 1.5 (R’)SB(s)a KPNO
+NGC 4388 12:25:46.7 +12:39:42.8 0.009 0.03 Sy 2 SA(s)b SDSS, Lit.
+NGC 4395 12:25:48.9 +33:32:48.7 0.001 0.02 Sy 1.8 SA(s)m SDS S, Lit.
+NGC 4593 12:39:39.4 – 05:20:39.3 0.009 0.03 Sy 1 (R)SB(rs)b K PNO
+MCG +09-21-096 13:03:59.5 +53:47:30.1 0.030 0.02 Sy 1 KPNO
+NGC 4992 13:09:05.6 +11:38:02.9 0.025 0.03 (LINER) Sa SDSS
+NGC 5252 13:38:15.9 +04:32:33.3 0.023 0.03 Sy 1.9 S0 SDSS– 31 –
+Table 1—Continued
+Source RA (h m s) Dec (d m s) Redshift E(B-V)1Type2Host Galaxy2Obs.3
+NGC 5506 14:13:14.9 – 03:12:27.4 0.006 0.06 Sy 1.9 Sa pec SDSS
+NGC 5548 14:17:59.6 +25:08:12.7 0.017 0.02 Sy 1.5 (R’)SA(s) 0/a SDSS, Lit.
+Mkn 813 14:27:25.1 +19:49:51.5 0.111 0.03 Sy 1 KPNO
+Mkn 841 15:04:01.2 +10:26:16.0 0.036 0.03 Sy 1.5 E KPNO
+Mkn 290 15:35:52.4 +57:54:09.5 0.030 0.02 Sy 1 E1? SDSS
+Mkn 1498 16:28:04.0 +51:46:31.0 0.055 0.03 Sy 1.9 KPNO
+NGC 6240 16:52:58.9 +02:24:03.0 0.025 0.08 Sy 2 I0: pec KPNO
+1RXS J174538.1+290823 17:45:38.2 +29:08:22.0 0.111 0.05 ( Sy1) KPNO
+3C 382 18:35:03.4 +32:41:46.8 0.058 0.07 Sy 1 KPNO
+NVSS J193013+341047 19:30:13.3 +34:10:47.0 0.063 0.19 (Sy 1.5) KPNO
+1RXS J193347.6+325422419:33:47.6 +32:54:22.0 0.030 0.27 (BL COMP) KPNO
+3C 403 19:52:15.8 +02:30:24.5 0.059 0.19 NLRG S0 KPNO
+Cygnus A 19:59:28.3 +40:44:02.0 0.056 0.38 Sy 2 S?; Radio gal . KPNO
+MCG +04-48-002 20:28:35.1 +25:44:00.0 0.014 0.45 Sy 2 S KPNO
+4C +74.26 20:42:37.3 +75:08:02.0 0.104 0.44 Sy 1 KPNO
+IGR 21247+5058 21:24:38.1 +50:58:58.0 0.020 2.43 Sy 1 KPNO
+RX J2135.9+4728 21:35:55.0 +47:28:23.2 0.025 0.62 Sy 1 KPNO
+UGC 11871 22:00:41.4 +10:33:08.7 0.027 0.06 Sy 1.9 Sb KPNO
+NGC 7319 22:36:03.5 +33:58:33.0 0.023 0.08 Sy 2 SB(s)bc pec K PNO
+3C 452 22:45:48.8 +39:41:15.7 0.081 0.14 NLRG KPNO
+Mkn 926 23:04:43.5 – 08:41:08.6 0.047 0.04 Sy 1.5 SDSS
+1Milky Way reddening values, E(B-V), obtained from NED.
+2AGN type and host galaxy type from NED, Tueller et al. (2008), and the results of this paper. For AGN types, optical
+identiﬁcations are listed, where available. Values in pare ntheses indicate classiﬁcations from this paper, where ’Sy 1’ is a source
+with broad emission lines and narrow line emission consiste nt with a Seyfert and ’Sy 2’ is a source without broad emission lines and
+with narrow line emission consistent with a Seyfert. Sub-cl assiﬁcations were made (i.e. Sy1.5) following the criteria of Osterbrock
+(1981) (based upon the ratio of the broad to narrow component s of Hαand Hβ. Where “Gal” is indicated, there are no optical
+emission lines indicative of the presence of an AGN. The opti cal spectrum looks like a galaxy spectrum. Additional host g alaxy
+classiﬁcations were obtained from the LEDA database. Where “?” is indicated, there is no available classiﬁcation.
+3Observation type from Sloan Digital Sky Survey archive (SDS S) or our Kitt Peak Observations (KPNO). Sources with line
+ratios that we have obtained in the literature are indicated by (Lit.).
+4This source was initially included in the 9-month catalog ba sed on an earlier method of source selection. However, with
+subsequent analysis it fell below the 4.8 σdetection threshold. It is detected above 5 σand included in the 22-month BAT survey.– 32 –
+Table 2. Details of KPNO Observations
+Source Grating UT Date Exp. (s) x (kpc)†y (kpc)†B?∗
+NGC 788 35 2006-11-20 3600 0.53 4.49
+LEDA 138501 26new 2006-11-17 1800 1.93 5.53 B
+LEDA 138501 35 2006-11-19 1800 1.93 7.53 B
+3C 111 35 2006-11-20 2700 1.90 7.42 B
+2MASX J04440903+2813003 26new 2006-11-17 3380 0.44 2.25
+2MASX J04440903+2813003 35 2006-11-19 3601 0.44 1.71
+MCG -01-13-025 26new 2006-11-18 3600 0.62 2.79 B
+MCG -01-13-025 35 2006-11-19 3601 0.62 2.79 B
+1RXS J045205.0+493248 26new 2006-11-18 3600 1.13 3.21 B
+1RXS J045205.0+493248 35 2006-11-20 3600 1.13 4.27 B
+2MASX J06411806+3249313 35 2006-11-20 5400 1.88 8.71
+Mkn 79 26new 2007-04-14 1200 0.87 3.62 B
+Mkn 79 35 2007-04-15 2401 0.87 3.38 B
+Mkn 18 26new 2006-11-18 3601 0.43 2.87
+Mkn 18 35 2006-11-19 3600 0.43 2.34
+MCG -01-24-012 26new 2007-04-14 1200 0.76 3.77
+MCG -01-24-012 35 2007-04-15 1199 0.76 2.98
+MCG +04-22-042 26new 2007-04-14 1200 1.30 4.32 B
+MCG +04-22-042 35 2007-04-15 1200 1.30 4.16 B
+Mkn 417 35 2006-11-20 3600 1.28 5.00
+1RXS J1127166.6+190914 26new 2007-04-14 1200 4.19 24.62
+1RXS J1127166+190914 35 2007-04-15 2399 4.19 15.32
+UGC06728 26new 2006-11-18 3000 0.25 0.81 B
+UGC06728 35 2006-11-19 3600 0.25 0.89 B
+Ark 347 26new 2007-04-14 1199 0.87 6.05
+Ark 347 35 2007-04-15 1200 0.87 4.45
+NGC 4593 26new 2007-04-14 1200 0.35 1.77 B
+NGC 4593 35 2007-04-15 1200 0.35 2.24 B
+MCG +09-21-096 26new 2007-04-14 2399 1.17 3.90 B
+MGC +09-21-096 35 2007-04-15 2400 1.17 4.56 B
+Mkn 813 26new 2007-06-15 2399 4.40 15.92 B
+Mkn 813 35 2007-06-17 2700 4.40 12.75 B
+Mkn 841 26new 2007-06-15 2399 1.42 5.56 B
+Mkn 841 35 2007-06-17 2700 1.42 4.59 B
+Mrk 1498 26new 2007-06-16 3600 2.15 8.38
+Mrk 1498 35 2007-06-18 3600 2.15 12.31
+NGC 6240 26new 2007-06-15 2400 0.96 3.73
+NGC 6240 35 2007-06-17 2701 0.96 7.65– 33 –
+Table 2—Continued
+Source Grating UT Date Exp. (s) x (kpc)†y (kpc)†B?∗
+1RXS J174538.1+290823 26new 2007-04-14 2400 4.43 17.28 B
+1RXS J174538.1+290823 35 2007-04-15 3601 4.43 17.86 B
+3C 382 26new 2007-06-15 3599 2.28 8.88 B
+3C 382 35 2007-06-17 3601 2.28 27.10 B
+3C 382 35 2007-06-18 2700 2.28 7.31 B
+NVSS J193013+341047 26new 2007-06-16 3600 2.48 8.56 B
+NVSS J193013+341047 35 2007-06-18 3602 2.48 6.60 B
+1RXS J193347.6+325422 26new 2007-06-15 2399 1.17 3.17 B
+1RXS J193347.6+325422 35 2007-06-17 2700 1.17 4.27 B
+3C 403 26new 2006-11-17 3600 2.32 18.93
+3C 403 26new 2006-11-18 1918 2.32 10.21
+3C 403 35 2006-11-19 3599 2.32 9.05
+3C 403 35 2006-11-20 1800 2.32 9.23
+Cyg A 26new 2007-06-16 2401 2.21 8.60
+Cyg A 35 2007-06-18 2699 2.21 13.76
+MCG +04-48-002 26new 2006-11-18 1801 0.54 2.11
+MCG+04-48-002 35 2006-11-19 3601 0.54 2.11
+4C +74.26 26new 2007-06-16 2400 4.13 11.16 B
+4C +74.26 35 2007-06-18 2698 4.13 24.36 B
+IGR 21247+5058 26new 2007-06-15 2400 0.78 3.04 B
+IGR 21247+5058 35 2007-06-17 2701 0.78 2.86 B
+UGC 11871 26new 2006-11-17 1800 1.04 4.73
+UGC 11871 26new 2006-11-18 1800 1.04 4.36
+UGC 11871 35 2006-11-19 1800 1.04 4.84
+UGC 11871 35 2006-11-20 1800 1.04 4.35
+NGC 7319 26new 2007-06-15 1422 0.88 3.42
+NGC 7319 35 2007-06-17 2736 0.88 5.84
+2MASX J03181899+6829322 32 2006-11-21 3599 3.57 15.28
+3C 105 32 2006-11-21 3599 3.53 10.87
+MCG+08-11-011 32 2008-12-04 900 0.80 6.23 B
+IRAS 05589+2828 32 2006-11-21 1800 1.29 1.79 B
+Mkn 3 32 2008-12-04 540 0.53 4.10
+Mkn 6 32 2008-12-04 900 0.73 5.71 B
+NGC 3227 32 2009-04-17 900 0.15 0.46 B
+NGC 3516 32 2009-04-17 900 0.34 1.53 B
+NGC 4051 32 2009-04-17 900 0.09 0.30
+NGC 4102 32 2009-04-17 900 0.11 0.58
+NGC 4151 32 2009-04-17 900 0.13 0.43 B– 34 –
+Table 2—Continued
+Source Grating UT Date Exp. (s) x (kpc)†y (kpc)†B?∗
+Mrk 766 32 2009-04-17 900 0.50 2.29
+NVSS 19013+341047 32 2006-11-21 3600 2.48 11.97 B
+RX J2135.9+4728 32 2006-11-21 3600 0.98 7.31 B
+3C 452 32 2006-11-21 5401 3.21 18.76
+†An estimate of the extraction aperture along the slit in both x and y is given in units
+of kpc. The x value is calculated as the ﬁxed 2′′slit size, converted to kpc using the
+redshift to the source. The y value is obtained from the aperture s ize used to extract the
+individual spectrum.
+∗B indicates the presence of broad lines (particularly H I Balmer lines) f rom a visual
+inspection of the spectra.– 35 –
+Table 3. Details of KPNO Observations of Template Galaxies
+Source Grating UT Date Exp. (s) x (kpc)†y (kpc)†
+NGC 205 26new 2006-11-17 2101 0.03 0.09
+NGC 205 35 2006-11-19 1800 0.03 0.19
+NGC 221 26new 2006-11-18 1800 0.03 0.16
+NGC 221 35 2006-11-20 1799 0.03 0.15
+NGC 628 26new 2006-11-17 3600 0.09 0.65
+NGC 628 35 2006-11-19 1800 0.09 1.01
+NGC 1023 26new 2006-11-17 1799 0.08 0.67
+NGC 1023 35 2006-11-20 1800 0.08 0.68
+NGC 3384 26new 2006-11-17 1799 0.09 0.66
+NGC 3884 35 2006-11-20 1801 0.09 0.82
+NGC 3640 26new 2006-11-17 1800 0.16 1.52
+NGC 3640 35 2006-11-20 1800 0.16 1.91
+NGC 4914 26new 2007-04-14 1200 0.61 3.01
+NGC 4914 35 2007-04-15 1200 0.61 3.71
+NGC 5308 26new 2007-06-16 1801 0.26 1.83
+NGC 5308 35 2007-06-18 1800 0.26 5.50
+NGC 5557 26new 2007-04-14 1200 0.42 3.36
+NGC 5557 35 2007-04-15 1200 0.42 4.21
+NGC 5638 26new 2007-06-16 1800 0.22 1.77
+NGC 5638 35 2007-06-18 1800 0.22 5.57
+NGC 6654 26new 2007-06-16 1800 0.24 1.26
+NGC 6654 35 2007-06-18 1799 0.24 3.53
+†An estimate of the extraction aperture along the slit in both x and
+y is given in units of kpc.– 36 –
+Table 4. Details of SDSS Observations
+Source UT Date Exp. (s) Plate Tile d (kpc)†B?∗
+Mkn 1018 2000-09-25 2700 404 193 2.53 B
+Mkn 590 2003-01-08 4200 1073 9328 1.52 B
+Mkn 18 2007-12-05 4204 1785 1290 0.64
+SDSS J090432.19+553830.1 2000-12-29 9000 450 238 2.17 B
+SDSS J091129.97+452806.0 2002-02-07 4803 832 603 1.58
+SDSS J091800.25+042506.2 2003-03-09 3000 991 763 9.40
+MCG +04-22-042 2005-12-23 4800 2290 1658 1.94 B
+Mkn 110 2001-12-09 4803 767 553 2.05 B
+Mkn 417 2006-12-16 5884 2481 1736 1.94
+SBS 1136+594 2002-05-06 5408 952 724 3.60 B
+CGCG 041-020 2005-01-15 3100 1622 1147 2.11
+Ark 347 2008-01-06 6008 2608 1821 1.29
+NGC 4388 2004-06-10 2400 1615 1140 0.52
+NGC 4395 2006-03-25 3000 2015 1471 0.06
+NGC 4992 2004-04-21 2100 1696 1212 1.46
+NGC 5252 2002-04-10 2701 853 624 1.35
+NGC 5506 2002-04-14 2646 916 688 0.35
+NGC 5548 2006-05-04 2500 2127 1533 0.99 B
+Mkn 290 2002-03-14 3904 615 400 1.76 B
+Mkn 926 2001-12-15 3304 725 503 2.77 B
+†The diameter of the aperture size for SDSS (3′′) in kpc.
+∗B indicates the presence of broad lines (particularly H I Balmer lines) f rom a visual
+inspection of the spectra.– 37 –
+Table 5. Stellar Light Fits to the Galaxy Templates
+Galaxy Type∗vdisp∗FWHM†Z†Lfyoung†Lfinterm†Lfold†
+NGC 205 E5 pec 40.8 300 0 .2Z⊙0.02 0.98 –
+NGC 221 cE2 71.8 170 Z⊙ 0.05 – 0.95
+NGC 628 SA(s)c 72.2 270 Z⊙ 0.07 0.40 0.53
+NGC 1023 SB(rs)0- 204.5 300 2 .5Z⊙– 0.02 0.98
+NGC 3384 SB(s)0- 148.4 300 Z⊙ – – 1.00
+NGC 3640 E3 181.6 430 2 .5Z⊙– 0.10 0.90
+NGC 4914 E+ 223.6 330 2 .5Z⊙– 0.46 0.53
+NGC 5308 S0- 227.2 370 Z⊙ – – 1.00
+NGC 5557 E1 253.0 400 2 .5Z⊙– 0.27 0.73
+NGC 5638 E1 165.0 270 Z⊙ – – 1.00
+NGC 6654 (R’)SB(s)0/a 157.8 270 Z⊙ – 0.05 0.95
+∗The galaxy type was obtained from NED while the central velocity disp ersion was found
+in LEDA. Typical errors on the central velocity dispersion are of th e order 5kms−1. These
+templates were selected from the non-active galaxy templates liste d in Ho et al. (1997)
+†TheﬁttedvaluesusingthestellarpopulationmodelsofBruzual & Cha rlot(2003)include
+the FWHM (kms−1), metallicity ( Z), and light fractions ( Lf) at 5500 ˚A using populations
+at 25 (young), 2500 (interm), and 10000 (old) Myr. A dash indicate s no contribution from
+the indicated component.– 38 –
+Table 6. Stellar Light Fits to the AGN Sources
+Source FWHM†Z†p0†p1†Lfpow†Lfyoung†Lfinterm†Lfold†χ2/dof
+KPNO Spectra
+NGC 788 200 2.5 Z⊙1.00 0.77 0.73 0.05 0.09 0.12 10.3
+LEDA 138501 400 0.2 Z⊙0.56 0.37 1.00 – – – 1.0
+2MASX J03181899+6829322 200 0.2 Z⊙– – – – 1.00 – 17.9
+3C 105 170 0.2 Z⊙– – – – 1.00 – 25.3
+3C 111 200 2.5 Z⊙0.32 0.96 1.00 – – – 2840
+2MASX J04440903+2813003 460 2.5 Z⊙0.01 1.58 1.00 – – – 101
+MCG -01-13-025 330 2.5 Z⊙– – – 0.06 – 0.94 3.0
+MCG +04-22-042 260 0.2 Z⊙– – – – – 1.00 4.9
+1RXS J045205.0+493248 460 Z⊙0.26 0.75 1.00 – – – 107
+MCG +08-11-011 50 0.2 Z⊙– – – 0.25 0.75 – 60.1
+IRAS 05589+2828 400 2.5 Z⊙0.00‡1.43 0.78 0.22 – – 30.3
+Mkn 3 50 0.2 Z⊙– – – – 1.00 – 85.8
+2MASX J06411806+3249313 200 0.2 Z⊙0.53 0.83 1.00 – – – 2.7
+Mkn 6 430 0.2 Z⊙1.00 0.44 0.16 – 0.84 – 95.6
+Mkn 79 460 Z⊙1.00 0.51 1.00 – – – 3.4
+Mkn 18 460 2.5 Z⊙– – – 0.35 0.58 0.08 4.7
+MCG -01-24-012 400 Z⊙1.00 0.02 0.02 – – 0.98 2.5
+MCG +04-22-042 260 0.2 Z⊙– – – – – 1.00 4.9
+NGC 3227 50 0.2 Z⊙– – – 0.46 0.26 0.28 15.2
+Mkn 417 200 2.5 Z⊙0.11 1.09 0.98 – 0.01 0.01 2.8
+NGC 3516 50 0.2 Z⊙– – – – 0.32 0.68 21.9
+1RXS J1127166+190914 270 2.5 Z⊙0.22 1.06 0.99 – 0.01 – 5.0
+UGC 6728 460 2.5 Z⊙1.00 0.32 0.33 – – 0.67 6.1
+NGC 4051 300 0.2 Z⊙1.00 0.54 0.39 – – 0.61 12.5
+Ark 347 300 Z⊙– – – – – 1.00 1.7
+NGC 4102 50 0.2 Z⊙– – – – 0.28 0.72 21.9
+NGC 4151 50 0.2 Z⊙– – – 0.71 – 0.29 92.7
+Mkn 766 360 0.2 Z⊙1.00 0.45 0.39 – – 0.61 15.4
+NGC 4593 460 Z⊙– – – 0.19 – 0.81 8.2
+MCG +09-21-096 230 0.2 Z⊙– – – – – 1.00 0.8
+Mkn 813 460 2.5 Z⊙1.00 0.19 0.17 0.15 – 0.68 1.1
+Mkn 841 400 Z⊙0.08 0.62 1.00 – – – 2.9
+Mkn 1498 460 Z⊙– – – – – 1.00 1.7
+NGC 6240 460 Z⊙1.00 0.23 0.01 – – 0.99 8.1
+1RXS J174538.1+290823 400 0.2 Z⊙0.00‡2.89 0.94 0.06 – – 3.7
+3C 382 460 2.5 Z⊙0.56 0.00 0.08 – 0.92 – 0.3– 39 –
+Table 6—Continued
+Source FWHM†Z†p0†p1†Lfpow†Lfyoung†Lfinterm†Lfold†χ2/dof
+NVSS J193013+341047 130 0.2 Z⊙1.00 0.45 0.44 – 0.10 0.45 2.2
+1RXS J193347.6+325422 460 Z⊙0.00 2.01 1.00 – – – 12.9
+3C 403 270 2.5 Z⊙1.00 0.53 0.72 – 0.09 0.19 1.8
+Cygnus A 270 Z⊙0.56 0.00 0.01 – – 0.99 6.3
+MCG +04-48-002 400 2.5 Z⊙– – – 0.29 0.53 0.18 17.3
+4C +74.26 430 0.2 Z⊙1.00 0.52 0.07 – – 0.93 90.6
+IGR 21247+5058 230 2.5 Z⊙1.00 0.61 0.22 – 0.78 – 0.4
+RX J2135.9+4728 460 0.2 Z⊙– – – – 1.00 – 1.5
+UGC 11871 430 0.2 Z⊙0.00‡1.73 0.77 0.11 0.11 – 1.1
+NGC 7319 460 Z⊙0.01 1.42 0.93 – – 0.07 0.8
+3C 452 200 0.2 Z⊙– – – – 1.00 – 6.1
+SDSS Spectra
+Mkn 1018 50 0.2 Z⊙0.02 0.51 0.01 – – 0.99 1.4
+Mkn 590 50 2.5 Z⊙0.17 0.46 0.02 – 0.98 – 3.6
+Mkn 18 50 0.2 Z⊙– – – 0.22 0.26 0.52 1.4
+SDSS J090432.19+553830.1 200 0.2 Z⊙1.00 0.39 1.00 – – – 3.0
+SDSS J091129.97+452806.0 50 0.2 Z⊙0.53 0.70 0.63 0.06 – 0.31 1.4
+SDSS J091800.25+042506.2 330 2.5 Z⊙1.00 0.09 0.12 – 0.88 – 2.4
+MCG +04-22-042 460 0.2 Z⊙0.62 0.51 1.00 – – – 7.4
+Mkn 110 50 0.2 Z⊙0.03 0.53 0.03 – – 0.97 11.1
+Mkn 417 50 Z⊙1.00 0.32 0.18 0.03 – 0.79 2.9
+SBS 1136+594 400 0.2 Z⊙1.00 0.27 1.00 – – – 4.9
+CGCG 041-020 50 0.2 Z⊙1.00 0.12 0.01 0.01 0.30 0.67 1.7
+Ark 347 50 Z⊙1.00 0.40 0.12 – – 0.88 6.0
+NGC 4388 50 0.2 Z⊙0.82 0.21 0.01 – – 0.99 19.5
+NGC 4395 50 0.2 Z⊙1.00 0.20 0.23 – 0.77 – 15.5
+NGC 4992 50 Z⊙1.00 0.31 0.10 – – 0.90 2.59
+NGC 5252 50 Z⊙1.00 0.37 0.13 – – 0.87 5.2
+NGC 5506 50 2.5 Z⊙0.00‡2.28 0.96 – 0.04 – 31.8
+NGC 5548 330 Z⊙1.00 0.54 1.00 – – – 4.9
+Mkn 290 50 0.2 Z⊙1.00 0.36 1.00 – – – 2.9
+Mkn 926 400 Z⊙1.00 0.41 1.00 – – – 14.9
+†The ﬁtted values using the stellar population models of Bruzual & Cha rlot (2003) include FWHM (kms−1), metal-
+licity (Z), and light fractions ( Lf) at 5500 ˚A using both a power law and stellar population models with ages of:
+25 (young), 2500 (interm), and 10000 (old) Myr. The values p0andp1are the power law components, deﬁned as
+p0×λp1. The constant factor, p0, is constrained to range from 0 to 1 and is the speciﬁc ﬂux at 1 ˚Awith units of– 40 –
+10−17ergss−1cm−2˚A−1. Where a component’s contribution (e.g. power law) was not require d in the best-ﬁt, a dash
+is indicated.
+‡For the indicated sources, the value of p0<0.01 but non-negligible. The parameter p0for the marked sources is:
+9.9×10−5(IRAS 05589+2828), 4 .2×10−12(1RXS J174538.1+290823), 2 ×10−4(UGC 11871), and 1 .6×10−7(NGC
+5506).– 41 –Table 7. Emission Line Properties For Strong Lines (Narrow L ine Sources)
+Source FWHM blue†[OII]λ3727∗Hγ λ4340∗Hβ λ4861.3∗[OIII]λ4959∗[OIII]λ5007∗
+FWHM red†[OI]λ6300∗[NII]λ6548∗[NII]λ6583∗[SII]λ6716∗[SII]λ6731∗log F(Hα)
+KPNO Spectra
+NGC 788 674.2 ±30.6··· ··· 1.82±0.65 2.31 ±0.76 3.79 ±1.53
+177.7±5.0 0.81 ±0.22 0.44 1.33 0.95 0.92 -13.29
+2MASX J03181899+6829322 144.8 ±1.5··· 0.14±0.01 0.37 ±0.01 1.06 ±0.01 2.93 ±0.03
+50.0‡0.09±0.01 0.14 0.43 ±0.01 0.35 ±0.02 0.26 ±0.02 -14.09
+3C 105 243.6 ±2.1··· ··· 0.13±0.01 0.74 ±0.01 2.49 ±0.04
+50.0‡0.22±0.01 0.57 ±0.01 1.71 ±0.03 0.34 ±0.02 0.57 ±0.02 -14.10
+2MASX J04440903+2813003 299.4 ±1.4··· 0.05 0.15 0.21 0.60
+160.5±0.5 -0.13 0.45 1.34 0.52 0.47 -13.17
+Mkn 3 410.5 ±0.5··· 0.08 0.15 0.69 2.21 ±0.01
+153.5±2.8 0.24 0.40 1.20 ±0.01 0.27 0.35 -11.65
+2MASX J06411806+3249313 216.0 ±1.8··· 0.18±0.04 0.32 ±0.01 1.25 ±0.02 3.65 ±0.05
+233.9±5.2 0.24 ±0.01 0.13 0.40 ±0.01 0.26 ±0.01 0.22 ±0.01 -13.97
+Mkn18 478.0 ±31.7 1.79 ±0.99 0.23 ±0.02 0.55 ±0.11 0.41 ±0.06 0.69 ±0.18
+33.3±24.8 0.10 0.33 ±0.05 0.45 ±0.08 0.18 ±0.03 0.19 ±0.02 -12.72
+MCG -01-24-012 541.7 ±23.6 0.64 ±0.02 0.07 0.48 ±0.05 1.05 ±0.13 2.02 ±0.35
+301.9±10.4 0.19 0.31 ±0.01 0.67 ±0.02 0.34 0.17 ±0.07 -13.14
+Mkn 417 107.8 ±3.1··· 0.10±0.05 0.27 ±0.01 0.83 ±0.01 1.97 ±0.02
+50.0‡0.23±0.01 0.27 0.83 ±0.01 0.32 ±0.01 0.31 ±0.01 -13.76
+1RXS J1127166+190914 169.3 ±1.5··· ··· 0.41±0.03 1.35 ±0.13 3.99 ±1.00
+442.5±21.0 0.25 0.42 ±0.02 0.86 ±0.02 0.37 0.21 ±0.01 -13.03
+Ark 347 166.3 ±9.4 0.56 ±0.03 0.14 ±0.00 0.59 ±0.05 1.49 ±0.28 3.60 ±1.58
+355.4±5.1 0.3 ±0.01 0.22 ±0.12 1.11 ±0.45 0.54 ±0.03 0.54 ±0.05 -13.08– 42 –Table 7—Continued
+Source FWHM blue†[OII]λ3727∗Hγ λ4340∗Hβ λ4861.3∗[OIII]λ4959∗[OIII]λ5007∗
+FWHM red†[OI]λ6300∗[NII]λ6548∗[NII]λ6583∗[SII]λ6716∗[SII]λ6731∗log F(Hα)
+NGC 4102 262.2 ±50.5··· ··· 0.29±1.96 0.14 ±1.77 0.39 ±2.21
+334.6±4.6 0.09 ±0.17 0.41 ±0.14 0.93 ±0.02 0.15 ±0.14 0.16 ±0.15 -12.25
+Mkn 1498 321.3 ±16.8 1.14 ±0.08 0.50 ±0.02 1.35 ±0.25 2.47 ±0.47 5.69 ±2.62
+256.3±18.3 0.05 0.19 0.26 ±0.10 0.14 0.11 ±0.00 -13.18
+NGC 6240 425.1 ±23.8 0.35 ±0.01 0.02 0.11 ±0.01 0.06 ±0.01 0.20 ±0.01
+377.4±1.4 0.27 0.33 1.00 0.36 0.52 -12.73
+3C 403 134.6 ±4.2 0.21 ±0.03 0.10 ±0.02 0.32 ±0.02 1.30 ±0.03 3.69 ±0.05
+50.0‡0.16 0.32 0.96 ±0.01 0.30 ±0.01 0.29 ±0.01 -13.87
+Cygnus A 115.8 ±3.1 0.98 ±0.01 0.12 0.27 ±0.01 0.92 ±0.01 2.68 ±0.03
+320.4±6.5 0.26 0.59 1.77 ±0.01 0.51 0.43 -13.04
+MCG +04-48-002 186.0 ±5.9 1.05 ±0.05 0.18 0.60 ±0.02 0.27 ±0.00 0.72 ±0.02
+197.6±16.0 0.19 0.57 ±0.03 0.85 ±0.28 1.00 ±0.06 0.76 ±0.03 -12.99
+UGC 11871 50.0‡0.22 0.05 0.14 0.16 0.31 ±0.01
+279.1±6.7 0.08 0.24 0.67 0.22 0.20 -12.25
+NGC 7319 285.0 ±20.1 2.34 ±0.09 0.17 ±0.03 0.66 ±0.10 1.21 ±0.10 2.18 ±0.16
+239.9±3.6 0.42 ±0.04 0.60 ±0.01 1.81 ±0.03 0.80 ±0.02 0.55 ±0.02 -13.68
+3C 452 235.1 ±7.3··· ··· 0.14±0.01 0.36 ±0.02 0.98 ±0.03
+50.0‡0.21±0.01 0.32 ±0.01 0.95 ±0.03 0.27 ±0.02 0.20 ±0.03 -14.22
+SDSS Spectra
+Mkn 18 91.8 ±1.1··· 0.08 0.20 0.09 0.29
+117.2±0.7 0.05 0.15 0.44 ±0.01 0.20 0.16 -12.98
+SDSS J091129.97+452806.0 140.9 ±3.4··· 0.05±0.01 0.12 ±0.01 0.29 ±0.01 0.90 ±0.02
+118.0±2.3 0.10 ±0.01 0.24 ±0.00 0.72 ±0.02 0.29 ±0.01 0.23 ±0.01 -14.49– 43 –Table 7—Continued
+Source FWHM blue†[OII]λ3727∗Hγ λ4340∗Hβ λ4861.3∗[OIII]λ4959∗[OIII]λ5007∗
+FWHM red†[OI]λ6300∗[NII]λ6548∗[NII]λ6583∗[SII]λ6716∗[SII]λ6731∗log F(Hα)
+SDSS J091800.25+042506.2 176.2 ±0.8 0.56 ±0.01 0.08 0.25 1.00 ±0.01 3.02 ±0.03
+187.7±1.4 0.18 0.22 0.66 ±0.01 0.22 ±0.01 0.20 -14.08
+Mkn 417 196.3 ±6.4 0.43 ±0.02 0.07 ±0.00 0.24 ±0.01 1.08 ±0.18 2.95 ±1.19
+228.8±7.2 0.20 0.20 0.62 ±0.05 0.23 ±0.01 0.23 ±0.01 -13.02
+CGCG 041-020 133.9 ±2.0 0.25 ±0.01 0.07 0.18 ±0.01 0.26 ±0.01 0.73 ±0.01
+120.5±1.4 0.09 ±0.01 0.23 0.68 ±0.01 0.25 ±0.01 0.22 ±0.01 -13.96
+Ark 347 225.6 ±5.0 0.5 0.07 0.27 0.91 ±0.03 2.46 ±0.07
+171.7±0.7 0.11 0.39 1.18 0.30 0.28 -13.27
+NGC 4388 188.3 ±0.4··· 0.10 0.34 ±0.02 1.12 ±0.16 2.67 ±0.66
+280.7±3.8 0.12 ±0.01 0.11 ±0.03 0.53 ±0.10 0.19 ±0.05 0.26 ±0.03 -12.33
+NGC 4395 270.7 ±0.5··· 0.11 0.31 0.74 ±0.01 2.07 ±0.03
+248.2±0.6 0.19 0.07 0.21 0.13 0.16 -12.81
+NGC 4992 113.5 ±5.1 1.42 ±0.70 0.34 ±0.04 0.28 ±0.11 0.31 ±0.48 1.30 ±2.15
+106.9±4.0 0.87 ±0.39 0.86 ±0.31 2.06 ±2.96 0.59 ±0.60 0.30 ±0.22 -14.32
+NGC 5252 186.0 ±0.9··· 0.10 0.24 0.52 ±0.01 1.57 ±0.02
+211.9±1.0 0.34 ±0.01 0.32 0.95 ±0.01 0.45 ±0.01 0.41 ±0.01 -13.32
+NGC 5506 289.1 ±0.6··· 0.04 0.17 ±0.01 0.43 ±0.03 1.24 ±0.24
+333.8±7.0 0.12 0.27 ±0.01 0.70 ±0.06 0.14 ±0.02 0.12 ±0.03 -11.99
+†The FWHM of the lines, in kms−1, are tied together for all of the narrow emission lines liste d in this table.
+∗Ratio of the intensity of the indicated line to the intensity of Hα. The units of the H αﬂux are ergss−1cm−2. Where errors are not indicated,
+the errors are on the order of 10−3.
+‡Indicated FWHM of the lines was ﬁxed to the narrow velocity va lue of 50kms−1.– 44 –
+Table 8. Emission Line Fluxes For Weaker Lines (Narrow Line S ources)
+Source [Ne III]λ3869∗Hδ [OIII]λ4363∗HeIIλ4686∗[NI]λ5199∗
+HeIλ5876∗[FeVII]λ6087∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+NGC 788 ··· ··· ··· -14.13±0.16 -14.09 ±0.12
+-14.28±0.14 -14.72 ±0.22 -15.03 ±0.31 ··· -14.71±0.24
+2MASX J03181899+6829322 ··· -14.02±0.16 -14.87 ±0.18 -15.69 ±0.34 -15.75 ±0.39
+··· -15.62±0.32 -16.50 ±0.78 -14.96 ±0.20 -15.87 ±0.54
+3C 105 ··· ··· ··· ··· -15.84±0.43
+··· -15.29±0.24 ··· -15.24±0.27 -14.60 ±0.15
+2MASX J04440903+2813003 ··· ··· ··· -14.71±0.15 -13.85 ±0.06
+··· ··· ··· ··· ···
+Mkn 3 ··· ··· -13.22±0.22 ··· -13.17±0.14
+-13.40±0.16 -13.55 ±0.19 -12.82 ±0.10 -13.83 ±0.29 -12.75 ±0.09
+2MASX J06411806+3249313 ··· ··· -14.64±0.26 -15.37 ±0.33 -15.71 ±0.39
+-15.46±0.29 -15.37 ±0.27 -15.08 ±0.22 -15.65 ±0.39 -15.14 ±0.28
+Mkn 18 -14.19 ±0.17 -14.29 ±0.16 -15.14 ±0.37 -14.84 ±0.25 -14.32 ±0.20
+-14.40±0.21 ··· ··· ··· -14.33±0.13
+MCG -01-24-012 -14.27 ±0.16 -15.46 ±0.55 -14.85 ±0.24 -14.90 ±0.23 -14.98 ±0.31
+-14.82±0.27 -15.31 ±0.46 -15.06 ±0.26 -15.13 ±0.28 ···
+Mkn 417 ··· ··· ··· -15.77±0.54 -15.08 ±0.23
+-14.99±0.20 ··· -15.01±0.20 -16.35 ±0.70 -15.10 ±0.26
+1RXS J1127166+190914 ··· ··· ··· -14.66±0.18 -14.69 ±0.17
+··· -14.82±0.19 -14.67 ±0.17 -14.68 ±0.18 ···
+Ark 347 -14.02 ±0.16 -14.74 ±0.30 -14.83 ±0.31 -14.51 ±0.20 -14.44 ±0.26
+-14.25±0.24 -14.39 ±0.28 -14.68 ±0.23 -15.56 ±0.54 -14.49 ±0.18
+NGC 4102 ··· ··· -13.76±0.25 ··· -13.82±0.20
+··· -16.20±1.17 ··· -15.04±0.68 -14.05 ±0.27
+Mkn 1498 -13.78 ±0.09 -14.36 ±0.15 -14.15 ±0.11 -14.21 ±0.12 -15.01 ±0.36
+-14.87±0.41 -15.35 ±0.66 -15.23 ±0.37 -15.54 ±0.49 -14.61 ±0.23
+NGC 6240 -14.24 ±0.26 -14.46 ±0.29 -15.27 ±0.54 ··· -13.82±0.19
+··· ··· -13.86±0.11 ··· ···
+3C 403 -14.56 ±0.23 -16.38 ±0.92 -15.31 ±0.39 -14.91 ±0.25 -14.87 ±0.23
+-15.07±0.20 -15.07 ±0.17 -15.19 ±0.19 -15.16 ±0.19 -14.52 ±0.18– 45 –
+Table 8—Continued
+Source [Ne III]λ3869∗Hδ [OIII]λ4363∗HeIIλ4686∗[NI]λ5199∗
+HeIλ5876∗[FeVII]λ6087∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+Cygnus A -13.55 ±0.10 -14.20 ±0.17 -14.24 ±0.15 -14.11 ±0.12 -14.01 ±0.17
+-14.74±0.39 -14.87 ±0.42 -14.12 ±0.11 -14.79 ±0.22 -14.14 ±0.13
+MCG +04-48-002 ··· -15.03±0.37 -14.82 ±0.26 ··· -14.32±0.14
+-14.40±0.14 ··· ··· ··· -14.95±0.22
+UGC 11871 -14.06 ±0.14 -14.68 ±0.24 -14.90 ±0.29 -14.63 ±0.20 -14.31 ±0.32
+-14.44±0.32 -15.89 ±0.90 -14.43 ±0.15 ··· -14.60±0.23
+NGC 7319 -13.98 ±0.22 -14.45 ±0.31 -14.87 ±0.42 -14.83 ±0.37 -14.29 ±0.30
+-14.68±0.42 -14.88 ±0.47 -14.52 ±0.18 -15.69 ±0.57 -14.76 ±0.25
+3C 452 ··· ··· ··· ··· ···
+··· ··· ··· ··· -14.79±0.20
+Mkn 18 -14.64 ±0.15 -14.43 ±0.12 -15.23 ±0.28 -15.35 ±0.32 -14.99 ±0.23
+-14.50±0.14 ··· -15.04±0.27 -16.29 ±0.79 -14.85 ±0.24
+SDSS J091129.97+452806.0 -15.53 ±0.24 -16.02 ±0.36 -16.44 ±0.53 -16.11 ±0.40 -16.31 ±0.48
+-15.75±0.27 -16.52 ±0.57 ··· ··· -16.20±0.48
+SDSS J091800.25+042506.2 -14.70 ±0.08 -15.50 ±0.18 -15.35 ±0.16 -15.27 ±0.15 -15.57 ±0.20
+-15.73±0.24 -15.96 ±0.30 -15.36 ±0.17 -16.22 ±0.43 -15.36 ±0.18
+Mkn 417 -14.26 ±0.08 -15.10 ±0.16 -14.93 ±0.14 -14.82 ±0.13 -15.30 ±0.22
+-15.25±0.20 -15.37 ±0.25 -14.80 ±0.13 -15.76 ±0.36 -14.88 ±0.15
+CGCG 041-020 -15.30 ±0.20 -15.47 ±0.23 -15.78 ±0.33 -15.79 ±0.34 -15.84 ±0.37
+-15.79±0.36 -16.00 ±0.45 ··· -15.95±0.44 ···
+Ark 347 -14.00 ±0.07 -14.69 ±0.12 -14.73 ±0.13 -14.38 ±0.10 -14.88 ±0.17
+-14.65±0.14 -14.34 ±0.11 -14.73 ±0.16 -15.28 ±0.29 -14.26 ±0.11
+NGC 4388 -13.65 ±0.06 -14.18 ±0.08 -14.30 ±0.08 -14.06 ±0.07 -14.55 ±0.11
+-14.28±0.09 -14.55 ±0.12 -14.07 ±0.08 -15.30 ±0.25 -13.86 ±0.07
+NGC 4395 -13.55 ±0.07 -14.04 ±0.08 -14.05 ±0.08 -14.10 ±0.08 -14.74 ±0.12
+-14.37±0.09 -15.19 ±0.17 -14.07 ±0.08 -15.61 ±0.26 -14.18 ±0.08
+NGC 4992 -15.43 ±0.25 -15.75 ±0.34 ··· -15.78±0.38 -15.81 ±0.42
+-16.89±0.90 -15.94 ±0.49 -15.82 ±0.44 ··· ···
+NGC 5252 -13.98 ±0.08 -14.67 ±0.13 -14.81 ±0.17 -14.77 ±0.16 -14.72 ±0.16– 46 –
+Table 8—Continued
+Source [Ne III]λ3869∗Hδ [OIII]λ4363∗HeIIλ4686∗[NI]λ5199∗
+HeIλ5876∗[FeVII]λ6087∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+-15.08±0.24 -15.40 ±0.37 -14.28 ±0.12 -15.18 ±0.30 -14.74 ±0.19
+NGC 5506 -13.81 ±0.07 ··· -14.57±0.11 -14.19 ±0.08 -14.31 ±0.09
+-14.12±0.07 -14.74 ±0.14 -14.00 ±0.07 -15.82 ±0.44 -13.74 ±0.07
+∗Logarithm of the intensity of the indicated line.– 47 –Table 9. Emission Line Properties For Strong Blue Lines (Bro ad Line Sources)
+Source FWHM (km s−1) H βN∗[OIII]λ4959∗[OIII]λ5007∗HβBFWHM (km s−1) H βB∗F5100˚A
+KPNO Spectra
+3C 111 214.6 ±0.4 -12.70 -11.97 -11.54 4960.5 ±1.6 -11.55 -13.90 ±0.05
+MCG -01-13-025 656.3 ±666.1 -13.76 -13.32 -13.02 8162.8 ±288.6 -13.11 ±0.01 -14.63 ±0.02
+1RXS J045205.0+493248 374.1 ±4.8 -13.01 ±0.01 -12.48 ±0.01 -12.04 ±0.01 7402.1 ±21.7 -12.36 -14.33 ±0.01
+MCG +08-11-011 986.1 ±20.5 -12.15 ±0.07 -11.71 ±0.07 -11.24 ±0.07 3762.3 ±28.6 -11.61 -13.60 ±0.02
+IRAS 05589+2828 563.2 ±33.5 -12.87 ±0.33 -12.81 ±0.33 -12.36 ±0.33 5564.9 ±15.1 -12.34 -14.40 ±0.01
+Mkn 6 750.1 ±212.0 -12.41 ±0.53 -11.97 -11.52 ±0.00 4757.8 ±69.5 -12.19 ±0.01 -13.89 ±0.02
+Mkn 79 1078.6 ±96.9 -13.11 ±0.04 -12.56 ±0.02 -12.09 ±0.02 3940.9 ±54.4 -12.55 ±0.01 -14.66 ±0.03
+MCG +04-22-042 1486.6 -12.72 ±0.20 -12.73 ±0.20 -12.26 ±0.20 2951.4 ±62.5 -12.43 ±0.01 -14.49 ±0.02
+NGC 3227 1445.1 -12.67 ±0.57 -12.11 -11.64 3737.2 ±61.2 -12.17 ±0.01 -13.98 ±0.01
+NGC 3516 315.4 ±57.7 -13.53 -12.48 -12.04 5294.9 ±100.3 -12.18 ±0.01 -13.88 ±0.01
+UGC 6728 327.9 ±612.0 -12.80 -13.13 -12.75 2308.3 ±79.6 -12.68 ±0.02 -14.47 ±0.01
+NGC 4051 1445.1 -12.52 ±0.18 -12.36 ±0.18 -11.87 ±0.18 1498.9 ±35.3 -12.29 ±0.02 -14.05 ±0.01
+NGC 4151 626.3 ±26.5 -11.40 ±0.08 -11.00 -10.51 2653.5 -13.41 ±0.04
+Mkn 766 939.1 ±24.5 -12.66 ±0.02 -12.26 ±0.02 -11.78 ±0.02 2422.6 ±59.0 -12.68 ±0.01 -14.43 ±0.02
+NGC 4593 1486.6 -13.12 ±0.55 -12.71 ±0.54 -12.48 ±0.54 5966.3 ±390.7 -12.40 ±0.04 -14.15 ±0.01
+MCG +09-21-096 485.5 ±351.2 -13.87 ±0.00 -13.51 -13.06 ±0.00 5412.3 ±115.8 -12.93 ±0.01 -14.94 ±0.01
+Mkn 813 1486.6 -13.82 ±0.25 -13.51 ±0.24 -13.15 ±0.24 7072.1 ±207.9 -12.98 ±0.01 -14.94 ±0.01
+Mkn 841 1486.6 -13.23 ±0.96 -12.68 -12.24 ±0.00 4957.7 ±87.3 -12.47 ±0.01 -14.61 ±0.02
+1RXS J174538.1+290823 1001.7 ±36.4 -13.71 ±0.03 -13.19 ±0.03 -12.75 ±0.03 9998.0 -13.68 ±0.01 -15.52 ±0.02
+3C 382 361.6 ±259.8 0.00 -14.63 ±0.76 -14.19 ±0.84 9998.0 -14.02 ±0.08 -15.62 ±0.02
+NVSS J193013+341047 1366.4 ±579.9 -13.43 ±0.74 -12.81 ±0.74 -12.35 4999.5 ±204.5 -13.32 ±0.02 -15.17 ±0.30
+1RXS J193347.6+325422 157.4 ±36.0 -13.08 -12.93 ±0.98 -12.40 ±0.99 3979.2 ±32.3 -12.36 -14.51 ±0.04
+4C+74.26 1428.6 ±814.2 -13.39 ±0.20 -12.66 ±0.17 -12.31 ±0.17 9099.9 ±108.5 -11.90 -13.80
+IGR 21247+5058 734.2 ±356.9 -14.22 ±0.41 -13.93 ±0.41 -13.40 ±0.41 2322.7 ±162.1 -13.66 ±0.04 -15.72 ±0.02
+RX J2135.9+4728 1486.6 -14.58 ±0.74 -14.05 ±0.74 -13.54 ±0.74 5047.7 ±385.9 -14.11 ±0.03 -15.71 ±0.01
+SDSS Spectra
+Mkn 1018 693.8 ±100.3 -13.91 ±0.09 -13.39 ±0.09 -12.91 ±0.09 5857.6 ±130.7 -13.19 ±0.01 -14.64 ±0.01
+Mkn 590 779.9 ±137.8 -13.59 ±0.04 -12.91 ±0.04 -12.46 ±0.04 5402.8 ±130.3 -13.40 ±0.01 -14.70 ±0.01
+SDSS J090432.19+553830.1 200.2 ±5.8 -13.52 ±0.03 -13.35 ±0.03 -12.87 ±0.03 5694.8 ±44.1 -13.25 -15.15 ±0.01
+MCG+04-22-042 318.7 ±7.3 -12.56 ±0.01 -12.67 ±0.01 -12.21 ±0.01 3780.2 ±23.5 -12.41 -14.41 ±0.02
+Mkn 110 483.3 ±11.50 -13.09 ±0.19 -12.64 ±0.19 -12.17 ±0.19 3332.8 ±21.1 -13.21 -15.28 ±0.03
+SBS 1136+594 1498.1 -13.45 ±0.02 -12.87 ±0.01 -12.39 3955.4 ±24.9 -12.76 -14.79 ±0.01
+NGC 5548 247.1 ±15.1 -12.74 ±0.02 -12.14 ±0.02 -11.69 ±0.02 7736.2 ±76.3 -12.45 -14.39 ±0.01
+Mkn 290 659.8 ±24.0 -13.18 ±0.58 -12.60 ±0.58 -12.13 4343.8 ±37.0 -12.61 -14.54 ±0.02– 48 –Table 9—Continued
+Source FWHM (km s−1) H βN∗[OIII]λ4959∗[OIII]λ5007∗HβBFWHM (km s−1) H βB∗F5100˚A
+Mkn 926 1331.7 ±30.3 -13.05 ±0.01 -12.53 ±0.01 -12.05 ±0.01 6993.6 ±93.4 -13.11 ±0.01 -14.83 ±0.01
+∗
+The logarithm of the indicated lines are given in ergss−1cm−2, where H βNindicates the narrow component of H βand HβBindicates the broad component.
+The limits on the velocity oﬀsets of the lines were ±1000kms−1. Where error-bars are not listed, they are on the order of 10−3.– 49 –Table 10. Emission Line Properties For Strong Red Lines (Bro ad Line Sources)
+Source FWHM (km s−1) H αN∗[NII]λ6583∗[SII]λ6716∗[SII]λ6731∗HαBFWHM (km s−1) H αB∗
+KPNO Spectra
+3C111 481.1 ±2.4 -12.14 -12.81 -12.93 -12.98 4589.8 ±0.5 -11.23
+MCG-01-13-025 888.8 ±70.9 -13.21 ±0.01 -13.20 -13.58 ±0.03 -13.48 ±0.02 6381.7 ±27.7 -12.55
+1RXS J045205.0+493248 310.2 ±2.0 -12.48 -12.68 -13.08 -13.09 5706.2 ±2.1 -11.88
+MCG +08-11-011 766.1 ±19.6 -11.51 -11.60 -12.35 -12.19 4214.3 ±9.3 -11.20
+IRAS 05589+2828 785.1 ±67.6 -12.49 -12.85 -13.85 ±0.02 -13.86 ±0.03 5416.2 ±7.1 -12.11
+Mkn 6 848.2 ±25.5 -11.97 -12.26 -12.60 -12.45 6800.9 ±15.1 -11.51
+Mkn 79 395.5 ±38.5 -12.66 -12.74 -13.36 ±0.01 -13.45 ±0.01 3660.3 ±5.5 -12.08
+MCG +04-22-042 365.4 ±30.9 -12.57 -13.84 -13.48 -13.54 2328.1 ±3.1 -11.90
+NGC 3227 601.4 ±26.7 -12.04 ±0.01 -11.93 -12.55 ±0.01 -12.55 ±0.01 3452.9 ±16.4 -11.73
+NGC 3516 528.1 ±182.4 -12.46 ±0.59 -11.27 ±0.93 -13.62 ±0.97 -13.70 ±0.97 4418.8 ±11.2 -11.56
+UGC 6728 207.2 ±55.8 -12.34 0.00 -13.92 -13.88 1288.1 ±1.7 -12.00
+NGC 4051 227.5 ±42.5 -11.97 -12.59 -12.91 -12.93 1627.3 ±8.3 -11.80
+NGC 4151 488.3 ±5.8 -11.12 -11.22 -11.80 -11.73 4745.8 ±7.8 -11.06
+Mkn 766 511.1 ±35.8 -12.10 ±0.04 -12.46 ±0.04 -13.17 ±0.05 -13.15 ±0.05 2327.3 ±13.2 -12.17 ±0.01
+NGC 4593 427.8 ±198.5 -13.34 ±0.71 -13.17 ±0.71 -13.28 ±0.71 -13.27 ±0.71 8259.5 ±62.3 -12.41
+MCG +09-21-096 394.0 ±39.5 -13.54 ±0.07 0.00 -13.79 ±0.07 -13.83 ±0.07 5104.7 ±15.8 -12.42
+Mkn 813 0.0 -13.77 ±0.03 0.00 -14.39 ±0.06 -14.35 ±0.06 6495.0 ±21.9 -12.50
+Mkn 841 120.2 ±19.6 -12.8 -13.20 -13.41 ±0.01 -13.55 ±0.01 4190.3 ±7.8 -12.12
+1RXS J174538.1+290823 590.2 ±72.2 -14.46 ±0.19 -14.22 ±0.19 -13.83 ±0.05 -14.07 ±0.07 7303.9 ±48.7 -12.93
+3C382 0.0 -15.34 ±0.79 -15.01 ±0.77 -15.01 ±0.77 -15.14 ±0.78 1315.8 ±996.1 -14.84 ±0.21
+NVSS J193013+341047 624.9 ±28.4 -12.87 ±0.02 -13.15 ±0.02 -13.71†-13.79†5282.8±15.7 -12.50
+1RXS J193347.6+325422 789.8 ±23.9 -12.11 ±0.83 -12.36 ±0.83 -14.09 ±0.94 -14.39 ±0.93 3269.9 ±3.5 -11.97
+4C+74.26 1486.6 ±0.0 -12.83 ±0.01 -12.56 -13.25 ±0.13 -13.24 ±0.12 9998.0 -11.44
+IGR 21247+5058 295.1 ±292.0 -13.28 ±0.99 0.00 -14.62 ±0.99 -14.69 ±0.99 2122.0 ±9.0 -12.69
+RX J2135.9+4728 620.0 ±99.8 -13.59 ±0.17 -13.72 ±0.17 -14.53 ±0.17 -14.58 ±0.18 4475.1 ±33.2 -13.19
+SDSS Spectra
+Mkn 1018 457.0 ±69.7 -13.46 ±0.20 -13.24 ±0.20 -13.87 ±0.20 -13.91 ±0.20 4847.3 ±28.2 -12.67
+Mkn 590 566.0 ±22.7 -13.00 -12.99†-13.76†-13.75†6850.3±43.0 -12.79
+SDSS J090432.19+553830.1 342.8 ±12.7 -12.95 -13.25 -13.71 -13.77 5190.9 ±10.4 -12.71
+MCG +04-22-042 354.1 ±21.4 -12.21 ±0.01 -12.81 -13.36 ±0.01 -13.42 ±0.01 3059.7 ±8.0 -11.94
+Mkn 110 362.1 ±3.2 -12.47 -13.05 -13.41 -13.46 3069.7 ±6.8 -12.47
+SBS 1136+594 245.6 ±10.0 -12.92 -14.06 -13.84 -13.92 3846.5 ±8.7 -12.35
+NGC 5548 587.4 ±14.3 -12.37†-12.61†-13.07†-13.13†6736.0±18.5 -11.92
+Mkn 290 349.2 ±24.1 -12.70 ±0.01 -13.11 -13.59 ±0.01 -13.65 ±0.01 4480.0 ±13.9 -12.21– 50 –Table 10—Continued
+Source FWHM (km s−1) HαN∗[NII]λ6583∗[SII]λ6716∗[SII]λ6731∗HαBFWHM (km s−1) HαB∗
+Mkn 926 529.8 ±6.6 -12.68 -12.75†-13.14†-13.14†8292.8±20.3 -12.33
+∗
+The logarithm of the indicated lines are given in ergss−1cm−2, where H αNindicates the narrow component of H αand HαBindicates the broad component.
+The [NII]λ6548 line, not shown in the table, was ﬁxed to a ratio of 1:2.98 with [NII]λ6583. Where error-bars are not included, they are on the orde r of 10−3.
+†The indicated value is a lower limit.– 51 –Table 11. Emission Line Properties For Weaker Narrow Lines ( Broad Line Sources)
+Source [O II]λ3727∗[NeIII]λ3869∗[NeIII]λ3968∗Hδ4101∗Hγ4340∗[OIII]λ4363∗HeIIλ4686∗
+[NI]λ5199∗HeIλ5876∗[FeVII]λ6087∗[OI]λ6300∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+KPNO Spectra
+LEDA 138501 -13.86 ±0.08 -13.57 ±0.08 -13.66 ±0.12 -12.76 ±0.10 -13.39 ±0.06 -13.36 ±0.05 -13.96 ±0.09
+··· ··· ··· ··· ··· ··· ···
+3C 111 ··· ··· ··· ··· ··· ··· ······ ··· -12.85±0.14 -13.01 ±0.17 -13.78 ±0.18 ···
+MCG -01-13-025 -13.23 ±0.17 ··· ··· ··· ··· ··· ··· ···
+-14.44±0.19 ··· ··· -13.49±0.05 -13.74 ±0.05 ··· ···
+1RXS J045205.0+493248 -12.37 ±0.07 -12.59 ±0.12 ··· ··· -13.19±0.10 -12.48 ±0.08 -14.12 ±0.18
+-14.46±0.09 ··· ··· -13.05±0.04 -13.60 ±0.07 ··· -14.21±0.07
+MCG +08-11-011 ··· ··· ··· ··· -11.61±0.03 -12.40 ±0.05 -13.03 ±0.06
+-13.32±0.08 -12.32 ±0.04 -13.32 ±0.10 -12.41 ±0.04 -12.69 ±0.05 ··· -13.13±0.10
+IRAS 05589+2828 ··· ··· ··· ··· -12.49±0.10 -12.84 ±0.15 -13.58 ±0.06
+··· -14.00±0.03 ··· -14.15±0.06 -14.08 ±0.07 -15.83 ±0.18 ···
+Mkn 6 ··· ··· ··· ··· -12.49±0.09 -13.00 ±0.11 -13.66 ±0.10
+-14.19±0.09 ··· ··· -12.61±0.05 -13.39 ±0.10 ··· -13.92±0.15
+Mkn 79 -12.87 ±0.11 -12.97 ±0.14 -13.11 ±0.23 -12.63 ±0.21 -12.72 ±0.07 -13.02 ±0.09 -13.36 ±0.11
+-14.25±0.19 -13.77 ±0.06 -13.71 ±0.05 -13.41 ±0.03 -13.87 ±0.06 -13.87 ±0.05 -13.86 ±0.08
+MCG +04-22-042 -12.95 ±0.10 -13.06 ±0.10 -12.79 ±0.12 -12.35 ±0.11 -12.29 ±0.06 -12.90 ±0.08 -12.59 ±0.07
+··· -12.77±0.04 -13.74 ±0.05 -13.76 ±0.05 -13.46 ±0.06 ··· -14.32±0.08
+NGC 3227 ··· ··· ··· ··· -12.19±0.06 -13.01 ±0.09 -13.69 ±0.11
+-13.79±0.07 ··· ··· -12.66±0.04 -12.87 ±0.07 ··· -12.98±0.08
+NGC 3516 ··· ··· ··· ··· -12.07±0.12 ··· ··· ···
+··· ··· ··· ··· ··· ··· ···– 52 –Table 11—Continued
+Source [O II]λ3727∗[NeIII]λ3869∗[NeIII]λ3968∗Hδ4101∗Hγ4340∗[OIII]λ4363∗HeIIλ4686∗
+[NI]λ5199∗HeIλ5876∗[FeVII]λ6087∗[OI]λ6300∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+UGC 6728 -13.35 ±0.15 -13.49 ±0.14 -13.13 ±0.15 -12.88 ±0.13 -12.64 ±0.08 -13.43 ±0.12 -13.36 ±0.11
+··· -13.42±0.07 ··· -14.02±0.04 -14.65 ±0.07 ··· ···
+NGC 4051 ··· ··· ··· ··· -12.54±0.11 -13.41 ±0.17 -13.55 ±0.10
+··· -13.18±0.07 -13.75 ±0.08 -13.05 ±0.06 -12.93 ±0.07 ··· -14.04±0.06
+NGC 4151 ··· ··· ··· ··· -11.64±0.06 -11.86 ±0.06 -12.60 ±0.07
+-12.63±0.06 -12.35 ±0.08 -12.22 ±0.06 -11.67 ±0.03 -12.04 ±0.05 ··· -12.17±0.03
+Mkn 766 ··· ··· ··· ··· -13.06±0.14 ··· ··· -13.92±0.10
+··· -13.37±0.09 -13.83 ±0.10 -13.42 ±0.08 -13.58 ±0.12 ··· -13.90±0.06
+NGC 4593 -12.85 ±0.15 -12.99 ±0.14 ··· -12.26±0.21 -12.21 ±0.11 -12.55 ±0.11 ···
+··· -12.10±0.08 -13.10 ±0.12 -13.75 ±0.08 -13.31 ±0.07 ··· ···
+MCG +09-21-096 -13.23 ±0.07 -13.64 ±0.12 ··· ··· -13.35±0.15 -12.69 ±0.12 ···
+··· -12.62±0.05 ··· -13.88±0.06 -14.14 ±0.10 ··· ···
+Mkn 813 -14.39 ±0.16 -13.69 ±0.14 -14.33 ±0.15 -12.88 ±0.06 -13.23 ±0.06 -13.50 ±0.07 -14.62 ±0.12
+··· -12.54±0.06 ··· -13.88±0.05 -14.15 ±0.10 ··· ···
+Mkn 841 -13.06 ±0.08 -13.06 ±0.09 -13.44 ±0.15 -12.79 ±0.15 -13.16 ±0.08 -12.90 ±0.08 -13.52 ±0.11
+-14.35±0.14 -12.52 ±0.08 -14.23 ±0.17 -14.30 ±0.07 ··· ··· -13.97±0.16
+1RXS J174538.1+290823 -13.26 ±0.06 -13.62 ±0.09 -14.06 ±0.09 -14.37 ±0.13 -13.90 ±0.10 -13.92 ±0.10 -14.66 ±0.09
+-15.11±0.09
+NVSS J193013+341047 -13.10 ±0.10 -13.18 ±0.13 -13.63 ±0.24 -13.79 ±0.25 -13.59 ±0.13 -13.37 ±0.11 -14.03 ±0.14
+···
+1RXS J193347.6+325422 ··· -12.77±0.13 -12.68 ±0.12 -12.40 ±0.10 -12.37 ±0.04 -12.81 ±0.05 ···
+-14.68±0.05 -14.63 ±0.10 -14.81 ±0.13 -13.75 ±0.06 -14.41 ±0.10 ··· ···
+4C +74.26 ··· ··· ··· ··· -11.97±0.07 ··· ···– 53 –Table 11—Continued
+Source [O II]λ3727∗[NeIII]λ3869∗[NeIII]λ3968∗Hδ4101∗Hγ4340∗[OIII]λ4363∗HeIIλ4686∗
+[NI]λ5199∗HeIλ5876∗[FeVII]λ6087∗[OI]λ6300∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+··· ··· ··· ··· ··· ··· ···
+IGR 21247+5058 ··· ··· ··· -14.01±0.24 -13.87 ±0.19 ··· ··· ···
+··· -13.73±0.19 -14.68 ±0.10 -14.84 ±0.12 -14.58 ±0.10 -15.26 ±0.15 ···
+RX J2135.9+4728 ··· ··· ··· ··· ··· ··· ··· -15.26±0.10
+··· -14.61±0.11 -14.09 ±0.10 -14.72 ±0.08 -15.48 ±0.12 -15.65 ±0.18 ···
+SDSS Spectra
+Mkn 1018 -13.61 ±0.06 -14.48 ±0.09 ··· ··· ··· ··· ··· ···
+··· ··· ··· -14.57±0.08 ··· ··· ···
+Mkn 590 -13.42 ±0.16 -13.28 ±0.15 ··· ··· -13.30±0.18 -13.62 ±0.13 ···
+··· ··· -13.97±0.12 -13.54 ±0.06 -14.24 ±0.13 ··· -14.53±0.07
+SDSS J090432.19+553830.1 -13.23 ±0.04 -13.87 ±0.10 ··· -14.67±0.09 -14.03 ±0.06 -13.68 ±0.09 -14.91 ±0.08
+-15.35±0.12 -14.17 ±0.10 ··· -14.16±0.05 -14.66 ±0.10 ··· -14.88±0.07
+MCG +04-22-042 -13.01 ±0.02 -12.99 ±0.08 -12.68 ±0.11 -12.25 ±0.06 -12.25 ±0.05 -12.88 ±0.07 -13.55 ±0.12
+··· -12.63±0.06 -13.58 ±0.07 -13.76 ±0.06 -14.89 ±0.12 -13.51 ±0.07 -14.51 ±0.07
+Mkn 110 -12.87 ±0.04 -13.16 ±0.05 -13.42 ±0.08 -13.53 ±0.12 -13.29 ±0.10 -13.24 ±0.09 -14.03 ±0.07
+-14.44±0.12 -14.03 ±0.06 -14.45 ±0.06 -13.25 ±0.02 -13.66 ±0.03 ··· -14.28±0.04
+SBS 1136+594 -13.17 ±0.06 -13.32 ±0.05 -13.46 ±0.09 -13.84 ±0.09 -13.48 ±0.05 -13.02 ±0.04 -14.02 ±0.09
+··· -13.11±0.03 -15.07 ±0.10 -14.05 ±0.03 -14.55 ±0.06 -14.68 ±0.09 -15.09 ±0.09
+NGC 5548 ··· -12.50±0.05 -13.05 ±0.10 -13.43 ±0.08 -12.91 ±0.08 -12.67 ±0.07 -13.57 ±0.09
+··· -13.59±0.07 -13.17 ±0.05 -12.98 ±0.03 -13.52 ±0.06 ··· -14.24±0.06
+Mkn 290 -13.35 ±0.07 -13.14 ±0.07 -13.42 ±0.12 -14.09 ±0.06 -13.72 ±0.07 -13.45 ±0.06 -13.86 ±0.07
+··· -12.66±0.06 -13.87 ±0.06 -13.85 ±0.05 -14.47 ±0.09 -15.02 ±0.14 -14.62 ±0.07– 54 –Table 11—Continued
+Source [O II]λ3727∗[NeIII]λ3869∗[NeIII]λ3968∗Hδ4101∗Hγ4340∗[OIII]λ4363∗HeIIλ4686∗
+[NI]λ5199∗HeIλ5876∗[FeVII]λ6087∗[OI]λ6300∗[OI]λ6363∗[FeX]λ6375∗[ArIII]λ7136∗
+Mkn 926 -12.55 ±0.03 -13.01 ±0.05 -13.48 ±0.08 -13.52 ±0.11 -13.20 ±0.08 -13.35 ±0.11 -13.90 ±0.14
+-13.77±0.07 -14.20 ±0.10 ··· -13.06±0.03 -13.84 ±0.06 ··· -14.22±0.05
+∗The logarithm of the ﬂux for each indicated line is given in un its of ergss−1cm−2.– 55 –Table 12. Measurements of Intrinsic Stellar Absorption
+Source D n(4000) H δA(˚A) CN 1(mag) Ca 4227 ( ˚A) C2 4668 ( ˚A) Mgb ( ˚A) [MgFe]′(˚A) <Fe>(˚A)
+KPNO Spectra
+NGC 788 ··· ··· ··· ··· -24.12±0.80 -8.50 ±0.14 13.61 ±0.06 -7.05 ±0.11
+LEDA 138501 0.88 ±0.00 -3.25 ±0.16 0.11 ±0.00 0.24 ±0.09 -2.62 ±0.19 -0.09 ±0.12 0.69 ±0.17 -0.25 ±0.09
+2MASX J03181899+6829322 ··· ··· -0.52±0.02 -0.36 ±0.68 -4.64 ±0.45 2.33 ±0.30 ··· 2.19±0.20
+3C 105 ··· ··· ··· ··· 3.63±0.48 3.89 ±0.26 3.66 ±0.16 3.52 ±0.18
+3C 111 ··· ··· ··· ··· 21.49±0.08 -210.88 ±92.86 ··· -98.29±46.43
+2MASX J04440903+2813003 ··· -0.22±0.00 0.00 ±0.00 0.04 ±0.00 -0.21 ±0.00 -0.14 ±0.00 0.16 -0.10 ±0.00
+MCG -01-13-025 1.51 ±0.01 -2.15 ±0.25 0.09 ±0.01 1.05 ±0.12 5.14 ±0.17 4.21 ±0.17 4.32 ±0.09 3.20 ±0.13
+MCG +04-22-042 0.86 ±0.00 -12.30 ±0.18 0.21 ±0.00 0.02 ±0.09 -10.97 ±0.20 -1.49 ±0.33 2.96 ±0.47 -0.26 ±0.23
+1RXS J045205.0+493248 0.78 ±0.00 -0.30 ±0.06 0.12 ±0.00 -0.28 ±0.04 0.08 ±0.09 1.25 ±0.05 0.30 ±0.16 1.17 ±0.04
+MCG +08-11-011 ··· -10.93±0.83 -0.05 ±0.01 0.09 ±0.19 -5.44 ±0.25 0.71 ±0.13 ··· 0.37±0.09
+IRAS 05589+2828 ··· ··· ··· 0.51±0.12 -5.46 ±0.08 -0.06 ±0.06 ··· 0.07±0.04
+Mkn 3 ··· ··· 0.32±0.23 -3.18 ±2.17 -7.11 ±0.84 8.09 ±0.26 ··· 4.24±0.22
+2MASX J06411806+3249313 ··· ··· ··· ··· -0.09±0.05 -0.12 ±0.02 0.10 -0.09 ±0.01
+Mkn 6 ··· -6.79±1.60 -0.00 ±0.02 -0.18 ±0.26 -1.34 ±0.29 0.88 ±0.13 ··· 0.18±0.10
+Mkn 79 0.84 ±0.01 -14.85 ±0.30 0.32 ±0.01 0.48 ±0.15 -8.12 ±0.30 1.85 ±0.43 ··· 1.73±0.32
+Mkn 18 1.10 ±0.01 2.14 ±0.20 -0.02 ±0.01 0.39 ±0.10 2.11 ±0.18 2.15 ±0.21 2.03 ±0.11 1.80 ±0.15
+MCG -01-24-012 1.37 ±0.04 0.09 ±0.99 -0.03 ±0.02 1.50 ±0.36 1.99 ±0.49 3.66 ±0.45 2.52 ±0.22 2.81 ±0.32
+MCG +04-22-042 0.86 ±0.00 -12.30 ±0.18 0.21 ±0.00 0.02 ±0.09 -10.97 ±0.20 -1.49 ±0.33 2.96 ±0.47 -0.26 ±0.23
+NGC 3227 ··· ··· ··· -0.52±0.38 -3.08 ±0.37 1.50 ±0.17 ··· 1.20±0.13
+Mkn 417 ··· ··· ··· ··· -0.41±0.04 -0.26 ±0.01 0.30 -0.20 ±0.01
+NGC 3516 ··· ··· -0.18±0.04 -0.32 ±0.39 2.92 ±0.34 1.99 ±0.16 2.40 ±0.12 1.97 ±0.12
+1RXS J1127166+190914 ··· 0.16±0.07 0.01 ±0.00 -0.08 ±0.02 -0.03 ±0.03 -0.16 ±0.01 0.07 -0.14 ±0.01
+UGC 6728 0.91 ±0.01 -9.14 ±0.26 0.16 ±0.01 0.52 ±0.12 -8.25 ±0.24 -1.08 ±0.28 2.58 ±0.34 -0.59 ±0.20
+NGC 4051 ··· ··· ··· -0.58±0.47 -2.30 ±0.44 0.12 ±0.21 ··· 0.71±0.15
+Ark 347 1.63 ±0.04 -3.75 ±0.62 0.09 ±0.02 0.13 ±0.28 5.35 ±0.36 3.64 ±0.39 4.25 ±0.21 3.16 ±0.28
+NGC 4102 ··· ··· ··· 0.44±0.50 1.96 ±0.44 2.19 ±0.19 1.97 ±0.17 1.82 ±0.14
+NGC 4151 ··· ··· ··· -0.33±0.15 -8.56 ±0.20 2.17 ±0.09 ··· 0.83±0.07
+Mkn 766 ··· ··· 0.16±0.04 -1.20 ±0.54 -8.12 ±0.57 -0.34 ±0.26 0.54 ±1.56 0.20 ±0.20
+NGC 4593 0.91 ±0.01 -5.95 ±0.38 0.17 ±0.01 -0.32 ±0.21 -0.38 ±0.42 1.13 ±0.63 ··· 1.40±0.45
+MCG +09-21-096 0.97 ±0.01 -2.84 ±0.29 0.03 ±0.01 0.52 ±0.17 -3.00 ±0.31 1.74 ±0.40 ··· 1.39±0.30
+Mkn 813 0.86 ±0.01 -1.16 ±0.26 0.06 ±0.01 0.17 ±0.14 0.93 ±0.33 0.37 ±0.45 0.43 ±0.42 0.07 ±0.36
+Mkn 841 0.83 ±0.00 -6.04 ±0.27 0.19 ±0.01 -0.07 ±0.17 -5.94 ±0.29 0.54 ±0.50 ··· 0.60±0.36
+Mkn 1498 0.92 ±0.02 -9.97 ±0.72 0.20 ±0.02 0.26 ±0.34 -7.18 ±0.61 2.34 ±0.72 ··· 1.70±0.63
+NGC 6240 1.40 ±0.06 -0.85 ±1.18 0.04 ±0.03 1.10 ±0.58 2.55 ±0.72 6.07 ±0.76 3.39 ±0.32 3.26 ±0.57– 56 –Table 12—Continued
+Source D n(4000) H δA(˚A) CN 1(mag) Ca 4227 ( ˚A) C2 4668 ( ˚A) Mgb ( ˚A) [MgFe]′(˚A)<Fe>(˚A)
+1RXS J174538.1+290823 0.79 ±0.01 -3.20 ±0.32 0.15 ±0.01 0.18 ±0.17 3.18 ±0.38 0.59 ±0.31 0.86 ±0.47 -0.05 ±0.25
+3C 382 1.11 ±0.04 -0.99 ±1.56 0.09 ±0.05 -0.88 ±0.86 2.24 ±1.15 1.45 ±1.65 1.33 ±1.30 0.28 ±1.79
+NVSS J193013+341047 0.51 ±0.03 -28.46 ±3.36 0.38 ±0.08 3.40 ±1.29 -19.33 ±2.24 -2.59 ±1.76 9.52 ±1.61 -6.34 ±1.97
+1RXS J193347.6+325422 0.84 ±0.00 -6.62 ±0.09 0.19 ±0.00 -0.12 ±0.05 -2.95 ±0.30 0.06 ±0.16 ··· -0.01±0.16
+3C 403 0.72 ±0.02 3.35 ±1.19 -0.25 ±0.03 0.55 ±0.68 -14.05 ±3.19 -22.14 ±1.97 17.25 ±1.38 -20.44 ±5.88
+Cygnus A 0.95 ±0.03 -5.58 ±1.22 0.14 ±0.04 -0.68 ±0.58 -4.52 ±0.72 10.01 ±0.86 ··· 5.46±1.58
+MCG +04-48-002 1.14 ±0.01 4.75 ±0.31 -0.09 ±0.01 0.39 ±0.14 1.65 ±0.22 2.44 ±0.12 1.89 ±0.10 1.93 ±0.09
+4C +74.26 0.86 ±0.00 -0.75 ±0.04 0.05 ±0.00 0.11 ±0.03 1.14 ±0.06 -0.14 ±0.20 ··· -0.20±0.15
+IGR 21247+5058 1.02 ±0.01 1.02 ±0.26 -0.01 ±0.01 0.11 ±0.12 1.12 ±0.19 0.10 ±0.15 0.21 ±0.33 -0.01 ±0.11
+RX J2135.9+4728 ··· ··· 0.35±0.90 2.56 ±5.61 -1.30 ±1.42 0.59 ±0.99 ··· 0.97±0.56
+UGC 11871 1.08 ±0.00 -0.75 ±0.06 0.01 ±0.00 -0.07 ±0.03 -0.03 ±0.05 -0.41 ±0.13 0.11 -0.28 ±0.09
+NGC 7319 1.03 ±0.01 0.40 ±0.19 -0.02 ±0.01 0.07 ±0.09 -0.52 ±0.14 -0.71 ±0.14 0.55 -0.47 ±0.10
+3C 452 ··· ··· ··· ··· 5.30±0.54 1.20 ±0.41 2.83 ±0.31 1.75 ±0.26
+SDSS Spectra
+Mkn 1018 0.96 ±0.00 -1.92 ±0.12 0.05 ±0.00 0.33 ±0.07 1.93 ±0.18 1.98 ±0.11 1.86 ±0.08 1.65 ±0.09
+Mkn 590 1.17 ±0.00 -3.76 ±0.13 0.17 ±0.00 0.88 ±0.06 5.25 ±0.16 3.77 ±0.10 4.20 ±0.06 3.05 ±0.07
+Mkn 18 1.20 ±0.00 3.08 ±0.16 -0.03 ±0.00 0.58 ±0.09 2.64 ±0.22 2.11 ±0.13 2.32 ±0.09 1.98 ±0.10
+SDSS J090432.19+553830.1 0.88 ±0.00 -4.24 ±0.20 0.15 ±0.01 0.59 ±0.11 0.98 ±0.27 2.43 ±0.18 1.50 ±0.14 2.19 ±0.14
+SDSS J091129.97+452806.0 0.99 ±0.00 -0.30 ±0.05 0.01 ±0.00 -0.13 ±0.03 -0.72 ±0.06 -0.39 ±0.03 0.53 -0.38 ±0.02
+SDSS J091800.25+042506.2 1.52 ±0.02 0.32 ±0.47 0.06 ±0.01 0.69 ±0.27 4.51 ±0.48 4.55 ±0.28 4.22 ±0.16 3.46 ±0.20
+MCG +04-22-042 0.78 ±0.00 -11.76 ±0.12 0.21 ±0.00 -0.30 ±0.06 -9.96 ±0.18 -1.13 ±0.11 2.33 ±0.19 -0.09 ±0.08
+Mkn 110 0.72 ±0.00 -15.51 ±0.21 0.34 ±0.01 0.47 ±0.10 -8.30 ±0.26 0.60 ±0.14 0.54 ±0.87 -0.53 ±0.11
+Mkn 417 1.69 ±0.02 0.64 ±0.28 0.05 ±0.01 1.22 ±0.14 7.15 ±0.27 5.53 ±0.17 5.88 ±0.09 4.30 ±0.12
+SBS 1136+594 0.85 ±0.00 -6.08 ±0.13 0.15 ±0.00 0.13 ±0.07 -9.36 ±0.20 -0.48 ±0.12 2.00 ±0.24 -0.39 ±0.11
+CGCG 041-020 1.48 ±0.01 0.91 ±0.25 -0.02 ±0.01 1.08 ±0.13 5.05 ±0.27 3.36 ±0.16 3.99 ±0.10 2.98 ±0.12
+Ark 347 2.24 ±0.02 -1.51 ±0.27 0.11 ±0.01 1.33 ±0.12 7.42 ±0.24 4.86 ±0.14 5.79 ±0.08 4.27 ±0.10
+NGC 4388 1.11 ±0.01 2.97 ±0.35 0.07 ±0.01 -2.10 ±0.19 -3.03 ±0.38 3.83 ±0.18 ··· 2.41±0.13
+NGC 4395 0.92 ±0.01 4.20 ±0.33 0.08 ±0.01 -0.19 ±0.17 -10.31 ±0.46 1.10 ±0.22 ··· 0.08±0.17
+NGC 4992 -1.25 ±0.51 4.54 ··· ··· ··· ··· ··· ···
+NGC 5252 2.06 ±0.02 -0.14 ±0.27 0.13 ±0.01 1.48 ±0.13 7.47 ±0.26 5.85 ±0.15 6.05 ±0.09 4.14 ±0.12
+NGC 5506 1.27 ±0.01 -1.54 ±0.14 0.18 ±0.01 -0.54 ±0.15 -4.09 ±0.32 3.11 ±0.15 ··· 1.17±0.12
+NGC 5548 0.80 ±0.00 -1.42 ±0.17 0.14 ±0.01 0.47 ±0.10 -2.45 ±0.26 2.63 ±0.16 ··· 0.95±0.12
+Mkn 290 0.86 ±0.00 -3.98 ±0.14 0.11 ±0.00 0.16 ±0.08 -4.78 ±0.21 0.06 ±0.13 ··· 0.19±0.10
+Mkn 926 0.79 ±0.00 -4.54 ±0.16 0.25 ±0.00 0.18 ±0.09 2.80 ±0.24 5.02 ±0.14 3.26 ±0.09 2.85 ±0.12– 57 –– 58 –
+Table 13. De-reddened Emission Line Properties
+Source∗Hα/HβE(B - V) int[OIII]/Hβ[OI]/Hα[NII]/Hα[SII]/Hα[OIII]/[OII]
+KPNO Spectra
+NGC 788 0.55 ··· 2.08 0.81 1.33 1.87 ···
+2MASX J03181899+6829322 2.70 ··· 7.92 0.09 0.43 0.61 ···
+3C 105 7.69 0.92 17.07 0.11 0.77 0.39 ···
+3C 111 (B) 3.60 0.15 14.01 0.10 0.19 0.27 ···
+2MASX J04440903+2813003 6.67 0.77 3.63 -0.07 0.68 0.48 ···
+MCG -01-13-025 (B) 3.50 0.12 5.38 0.43 0.93 0.86 1.39
+1RXS J045205.0+493248 (B) 3.43 0.10 9.22 0.17 0.57 0.45 1.89
+MCG +08-11-011 (B) 4.38 0.35 7.72 0.07 0.59 0.25 ···
+IRAS 05589+2828 (B) 2.42 ··· 3.26 0.01 0.43 0.09 ···
+Mkn 3 6.67 0.77 13.37 0.13 0.61 0.30 ···
+2MASX J06411806+3249313 3.12 0.01 11.39 0.24 0.40 0.48 ···
+Mkn 6 (B) 2.74 ··· 7.82 0.17 0.51 0.57 ···
+Mkn 79 (B) 2.80 ··· 10.58 0.08 0.83 0.36 6.10
+Mkn 18 1.82 ··· 1.25 0.10 0.45 0.37 0.39
+MCG -01-24-012 2.08 ··· 4.21 0.19 0.67 0.51 3.16
+MCG +04-22-042 (B) 1.42 ··· 2.89 0.02 0.05 0.23 5.57
+NGC 3227 (B) 4.21 0.31 10.19 0.13 1.00 0.46 ···
+Mkn 417 3.70 0.18 7.13 0.20 0.71 0.53 ···
+NGC 3516 (B) 11.66 1.34 25.72 ··· 4.81 0.04 ···
+1RXS J1127166+190914 2.44 ··· 9.73 0.25 0.86 0.58 ···
+UGC 6728 (B) 2.89 ··· 1.13 0.01 ··· 0.06 3.96
+NGC 4051 (B) 3.50 0.12 4.35 0.07 0.22 0.20 ···
+Ark 347 1.69 ··· 6.10 0.25 1.11 1.08 6.43
+NGC 4102 3.45 0.11 1.33 0.08 0.85 0.28 ···
+NGC 4151 (B) 1.90 ··· 7.70 0.18 0.80 0.46 ···
+Mkn 766 (B) 3.67 0.17 7.45 0.04 0.37 0.15 ···
+NGC 4593 (B) 0.60 ··· 4.33 0.39 1.46 2.30 2.33
+MCG +09-21-096 (B) 2.14 ··· 6.57 0.38 ··· 1.08 1.49
+Mkn 813 (B) 1.13 ··· 4.74 0.07 ··· 0.50 17.55
+Mkn 841 (B) 2.99 ··· 9.86 0.09 0.36 ··· 6.67
+Mkn 1498 0.74 ··· 4.21 0.05 0.26 0.25 4.99
+NGC 6240 9.09 1.09 1.59 0.12 0.39 0.32 0.16
+1RXS J174538.1+290823 (B) 0.18 ··· 9.23 0.33 1.73 6.72 3.28
+3C 382 (B) ··· ··· ··· 0.41 2.13 3.70 ···
+NVSS J193013+341047 (B) 3.63 0.16 11.74 0.09 0.46 0.23 4.72
+1RXS J193347.6+325422 (B) 9.33 1.11 4.16 ··· 0.21 0.01 ···
+3C 403 3.12 0.01 11.52 0.16 0.95 0.59 17.40
+Cygnus A 3.70 0.18 9.70 0.23 1.51 0.79 2.20
+MCG +04-48-002 1.67 ··· 1.20 0.19 0.85 1.76 0.69
+4C +74.26 (B) 3.63 0.16 11.53 0.41 1.62 ··· ···
+IGR 21247+5058 (B) 8.80 1.06 5.81 ··· ··· 0.03 ···
+RX J2135.9+4728 (B) 9.82 1.17 9.64 0.04 0.27 0.07 ···
+UGC 11871 7.14 0.84 1.99 0.04 0.32 0.19 0.51
+NGC 7319 1.52 ··· 3.30 0.42 1.81 1.35 0.93
+3C 452 7.14 0.84 6.30 0.11 0.45 0.21 ···– 59 –
+Table 13—Continued
+Source∗Hα/HβE(B - V) int[OIII]/Hβ[OI]/Hα[NII]/Hα[SII]/Hα[OIII]/[OII]
+SDSS Spectra
+Mkn 1018 (B) 2.82 ··· 9.91 0.12 1.66 0.74 5.00
+Mkn 590 (B) 3.97 0.25 13.10 0.18 0.81 0.28 6.68
+Mkn 18 5.00 0.48 1.36 0.03 0.29 0.23 ···
+SDSS J090432.19+553830.1 (B) 3.75 0.19 4.34 0.05 0.42 0.27 1 .83
+SDSS J091129.97+452806.0 8.33 1.00 6.62 0.05 0.30 0.20 ···
+SDSS J091800.25+042506.2 4.00 0.26 11.70 0.15 0.53 0.33 3.9 6
+MCG +04-22-042 (B) 2.25 ··· 2.22 0.02 0.25 0.13 6.22
+Mkn 110 (B) 4.10 0.28 7.98 0.12 0.21 0.17 3.61
+Mkn 417 4.17 0.30 11.84 0.18 0.64 0.48 4.80
+SBS 1136+594 (B) 3.38 0.09 11.42 0.10 0.07 0.20 5.53
+CGCG 041-020 5.56 0.59 3.77 0.06 0.41 0.27 1.44
+Ark 347 3.70 0.18 8.91 0.10 1.01 0.49 4.05
+NGC 4388 2.94 ··· 7.85 0.12 0.53 0.45 ···
+NGC 4395 3.23 0.04 6.64 0.18 0.20 0.28 ···
+NGC 4992 3.57 0.14 4.56 0.78 1.82 0.78 0.77
+NGC 5252 4.17 0.30 6.30 0.27 0.73 0.65 ···
+NGC 5506 5.88 0.65 6.73 0.07 0.40 0.14 ···
+NGC 5548 (B) 2.34 ··· 11.23 0.20 0.57 0.38 ···
+Mkn 290 (B) 3.02 ··· 11.15 0.07 0.39 0.24 16.56
+Mkn 926 (B) 2.37 ··· 10.08 0.30 0.85 0.69 3.17
+Spectra from the Literature
+MRK 3521(B) 0.95 ··· 18.25 0.007 0.28 0.007 ···
+NGC 9312(B) 6.17 0.70 2.29 0.04 0.21 0.32 ···
+NGC 127514.16b 0.30 14.88b 1.37 1.36 1.38 ···
+NGC 211033.24 0.04 4.79 0.37 1.29 1.12 ···
+NGC 32271(B) 2.90b ··· 5.91b 0.23 1.33 0.68 ···
+NGC 35161(B) 2.31 ··· 9.28 0.15 1.31 0.70 ···
+NGC 40511(B) 3.30 0.06 4.50 0.14 0.64 0.36 ···
+NGC 410218.33 1.00 0.99 0.041 0.92 0.31 ···
+NGC 413813.66 0.17 5.94 0.33 1.47 1.32 ···
+NGC 41511(B) 3.40 0.09 11.56 0.22 0.68 0.54 ···
+NGC 438815.69 0.61 11.15 0.16 0.57 0.61 ···
+NGC 439512.12 ··· 6.22 0.36 0.44 0.96 ···
+NGC 55481(B) 1.28 ··· 10.09 0.36 0.88 0.66 ···
+∗Sources with broad lines (approximately Sy 1 – Sy 1.5) are ind icated with a (B).
+1Reference: Ho et al. (1997)
+2Reference: Veilleux & Osterbrock (1987)
+3Reference: Kewley et al. (2001)– 60 –
+Table 14. Classiﬁcation
+Source [N II]/Hα[SII]/Hα[OI]/Hα[OIII]/[OII] Class
+KPNO Spectra
+NGC 788 AGN LINER LINER ··· LINER
+2MASX J03181899+6829322 AGN Seyfert Seyfert ··· Seyfert
+3C 105 AGN Seyfert Seyfert ··· Seyfert
+3C 111 (B) AGN Seyfert Seyfert ··· Seyfert
+2MASX J04440903+2813003 AGN Seyfert Seyfert ··· Seyfert
+MCG -01-13-025 (B) AGN Seyfert LINER LINER Ambig.
+1RXS J045205.0+493248 (B) AGN Seyfert Seyfert Seyfert Seyf ert
+MCG +08-11-011 (B) AGN Seyfert Seyfert ··· Seyfert
+IRAS 05589+2828 (B) AGN HII HII ··· Ambig.
+Mkn 3 AGN Seyfert Seyfert ··· Seyfert
+2MASX J06411806+3249313 AGN Seyfert Seyfert ··· Seyfert
+Mkn 6 (B) AGN Seyfert Seyfert ··· Seyfert
+Mkn 79 (B) AGN Seyfert Seyfert Seyfert Seyfert
+Mkn 18 COMP HII LINER LINER Ambig.
+MCG -01-24-012 AGN Seyfert Seyfert Seyfert Seyfert
+MCG +04-22-042 (B) HII HII HII Seyfert Ambig.
+NGC 3227 (B) AGN Seyfert Seyfert ··· Seyfert
+Mkn 417 AGN Seyfert Seyfert ··· Seyfert
+NGC 3516 (B) AGN Seyfert ··· ··· Seyfert
+1RXS J1127166+190914 AGN Seyfert Seyfert ··· Seyfert
+UGC 6728 (B) ··· HII HII HII HII
+NGC 4051 (B) COMP Seyfert Seyfert ··· Ambig.
+Ark 347 AGN LINER Seyfert Seyfert (Seyfert)
+NGC 4102 AGN HII Seyfert ··· Ambig.
+NGC 4151 (B) AGN Seyfert Seyfert ··· Seyfert
+Mkn 766 (B) AGN Seyfert Seyfert ··· Seyfert
+NGC 4593 (B) AGN Seyfert LINER Seyfert Ambig.
+MCG +09-21-096 (B) ··· LINER Seyfert LINER Ambig.
+Mkn 813 (B) ··· Seyfert Seyfert Seyfert Seyfert
+Mkn 841 (B) AGN ··· Seyfert Seyfert Seyfert
+Mkn 1498 AGN Seyfert Seyfert Seyfert Seyfert
+NGC 6240 COMP HII LINER HII Ambig.
+1RXS J174538.1+290823 (B) AGN Seyfert Seyfert Seyfert Seyf ert
+3C 382 (B) ··· ··· ··· ··· ···
+NVSS J193013+341047 (B) AGN Seyfert Seyfert Seyfert Seyfer t
+1RXS J193347.6+325422 (B) COMP HII ··· ··· COMP
+3C 403 AGN Seyfert Seyfert Seyfert Seyfert
+Cygnus A AGN Seyfert Seyfert Seyfert Seyfert
+MCG +04-48-002 AGN LINER LINER LINER LINER
+4C +74.26 (B) AGN ··· Seyfert ··· Seyfert
+IGR 21247+5058 (B) ··· HII ··· ··· HII (?)
+RX J2135.9+4728 (B) AGN Seyfert Seyfert ··· Seyfert
+UGC 11871 COMP HII HII HII COMP
+NGC 7319 AGN LINER LINER LINER LINER
+3C 452 AGN Seyfert Seyfert ··· Seyfert– 61 –
+Table 14—Continued
+Source [N II]/Hα[SII]/Hα[OI]/Hα[OIII]/[OII] Class
+SDSS spectra
+Mkn 1018 (B) AGN Seyfert Seyfert Seyfert Seyfert
+Mkn 590 (B) AGN Seyfert Seyfert Seyfert Seyfert
+Mkn 18 HII HII HII ··· HII
+SDSS J090432.19+553830.1 (B) AGN Seyfert Seyfert Seyfert S eyfert
+SDSS J091129.97+452806.0 AGN Seyfert Seyfert ��·· Seyfert
+SDSS J091800.25+042506.2 AGN Seyfert Seyfert Seyfert Seyf ert
+MCG +04-22-042 (B) HII HII HII Seyfert Ambig.
+Mkn110 (B) AGN Seyfert Seyfert Seyfert Seyfert
+Mkn 417 AGN Seyfert Seyfert Seyfert Seyfert
+SBS 1136+594 (B) AGN Seyfert Seyfert Seyfert Seyfert
+CGCG 041-020 AGN Seyfert Seyfert Seyfert Seyfert
+Ark 347 AGN Seyfert Seyfert Seyfert Seyfert
+NGC 4388 AGN Seyfert Seyfert ··· Seyfert
+NGC 4395 AGN Seyfert Seyfert ··· Seyfert
+NGC 4992 AGN Seyfert LINER LINER (LINER)
+NGC 5252 AGN Seyfert Seyfert ··· Seyfert
+NGC 5506 AGN Seyfert Seyfert ··· Seyfert
+NGC 5548 (B) AGN Seyfert Seyfert ··· Seyfert
+Mkn 290 (B) AGN Seyfert Seyfert Seyfert Seyfert
+Mkn 926 (B) AGN Seyfert Seyfert Seyfert Seyfert
+Spectra from the Literature
+MRK 3521(B) AGN Seyfert Seyfert ··· Seyfert
+NGC 9312(B) HII HII HII ··· HII
+NGC 12751AGN Seyfert LINER ··· Ambig.
+NGC 21103AGN LINER LINER ··· LINER
+NGC 32271(B) AGN Seyfert Seyfert ··· Seyfert
+NGC 35161(B) AGN Seyfert Seyfert ··· Seyfert
+NGC 40511(B) AGN Seyfert Seyfert ··· Seyfert
+NGC 41021AGN HII HII ··· Ambig.
+NGC 41381AGN LINER Seyfert ··· Ambig.
+NGC 41511(B) AGN Seyfert Seyfert ··· Seyfert
+NGC 43881AGN Seyfert Seyfert ··· Seyfert
+NGC 43951AGN Seyfert Seyfert ··· Seyfert
+NGC 55481(B) AGN Seyfert Seyfert ··· Seyfert
+Parenthesis are placed around classiﬁcations where the pro bable class is noted despite the fact that not all of the crite ria point
+to the same class. This is discussed within the text. The symb ol (B) indicates broad line sources (i.e. approximately Sy 1 –1.5).
+1Reference: Ho et al. (1997)
+2Reference: Veilleux & Osterbrock (1987)
+3Reference: Kewley et al. (2001)– 62 –
+Table 15. Mass and Luminosity
+Source λLλ1MHβ2L[OIII](obs)3L[OIII](corr)3Mreverb2M2MASS2
+NGC 788 40.84±0.15 41.50 ±0.15 8.51
+Mkn 1018 43.61 ±0.01 8.25 ±0.02 41.64 ±0.09 41.68 ±0.09 8.94
+Mkn 590 43.12 ±0.01 7.94 ±0.03 41.66 ±0.04 41.66 ±0.04 7.68 ±0.06 8.87
+2MASX J03181899+6829322 41.59 41.64
+3C 105 41.50±0.01 41.50 ±0.01 7.79
+3C 111 44.47 ±0.05 8.54 ±0.03 43.12 43.12
+2MASX J04440903+2813003 40.00 40.00
+MCG -01-13-025 42.77 ±0.02 8.12 ±0.04 40.67 40.67 8.06
+1RXS J045205.0+493248 43.59 ±0.01 8.45 ±0.01 42.17 ±0.01 42.17 ±0.01
+MCG +08-11-011 44.02 ±0.02 8.07 ±0.02 42.67 ±0.07 42.67 ±0.07
+IRAS 05589+2828 43.63 ±0.01 8.22 ±0.01 41.97 ±0.33 42.06 ±0.33
+Mkn 3 42.24 42.24 8.48
+2MASX J06411806+3249313 41.24 ±0.01 41.24 ±0.01
+Mkn 6 43.66 ±0.02 8.09 ±0.02 42.31 42.36 8.24
+Mkn 79 43.03 ±0.03 7.62 ±0.03 41.89 ±0.02 41.93 ±0.02 7 .72±0.10 8.42
+Mkn 18 40.18±0.05 40.19 ±0.05 7.45
+SDSS J090432.19+553830.1 42.99 ±0.01 7.91 ±0.01 41.56 ±0.03 41.56 ±0.03 7.70
+SDSS J091129.97+452806.0 39.61 ±0.01 39.61 ±0.01 7.53
+SDSS J091800.25+042506.2 42.10 42.10 8.57
+MCG -01-24-012 41.04±0.07 41.19 ±0.07 7.16
+MCG +04-22-042 43.63 ±0.02 7.88 ±0.01 42.07 ±0.20 42.37 ±0.20 8.49
+Mkn 110 42.81 ±0.03 7.36 ±0.02 42.22 ±0.19 42.22 ±0.19 7.40 ±0.09 7.80
+NGC 3227 42.19 ±0.01 7.15 ±0.02 40.83 40.83 7 .63±0.17 7.83
+Mkn 417 41.32±0.08 41.32 ±0.08 8.04
+NGC 3516 43.00 ±0.01 7.86 ±0.02 41.13 41.13 7 .63±0.13 8.13
+1RXS J1127166+190914 42.92±0.10 43.01 ±0.10 9.00
+SBS 1136+594 43.78 ±0.01 8.00 ±0.01 42.48 42.48 7.53
+UGC 6728 42.15 ±0.01 6.71 ±0.03 40.16 40.19 6.81
+CGCG 041-020 40.30±0.01 40.30 ±0.01 8.46
+NGC 4051 41.67 ±0.01 6.10 ±0.03 40.14 ±0.18 40.14 ±0.18 6 .28±0.15 7.27
+Ark 347 41.29±0.09 41.37 ±0.09 8.12
+NGC 4102 39.52±0.82 39.52 ±0.82
+NGC 4151 42.62 ±0.04 7.07 ±0.02 41.81 41.99 7 .12±0.13 7.69
+Mkn 766 42.78 ±0.02 7.06 ±0.03 41.73 ±0.02 41.73 ±0.02 7.85
+NGC 4388 41.24±0.10 41.26 ±0.10 8.53
+NGC 4395 38.79±0.01 38.79 ±0.01 5.30
+NGC 4593 42.75 ±0.01 7.83 ±0.07 40.71 ±0.54 41.33 ±0.54 6 .99±0.06 8.61
+MCG +09-21-096 43.01 ±0.01 7.88 ±0.02 41.18 41.32
+NGC 4992 39.88±0.42 39.88 ±0.42 8.56
+NGC 5252 40.89±0.01 40.89 ±0.01 8.64
+NGC 5506 40.96±0.08 40.96 ±0.08 7.77
+NGC 5548 43.04 ±0.01 8.21 ±0.02 42.03 ±0.02 42.14 ±0.02 7 .83±0.01 8.42
+Mkn 813 44.16 ±0.01 8.69 ±0.03 42.24 ±0.24 42.63 ±0.24
+Mkn 841 43.51 ±0.02 8.05 ±0.02 42.17 42.19 8.15
+Mkn 290 43.42 ±0.02 7.90 ±0.02 42.12 42.13 7.68
+Mkn 1498 42.34±0.16 42.89 ±0.16 8.59– 63 –
+Table 15—Continued
+Source λLλ1MHβ2L[OIII](obs)3L[OIII](corr)3Mreverb2M2MASS2
+NGC 6240 40.64±0.02 40.64 ±0.02
+1RXS J174538.1+290823 43.59 ±0.02 8.70 ±0.01 42.65 ±0.03 43.73 ±0.03 8.75
+3C 382 42.91 ±0.02 8.36 ±0.01 40.63 ±0.84 40.63 ±0.84 9.22
+NVSS J193013+341047 43.43 ±0.30 8.02 ±0.19 42.54 42.54
+1RXS J193347.6+325422 43.44 ±0.04 7.83 ±0.03 41.84 ±0.99 41.84 ±0.99
+3C 403 41.53±0.01 41.53 ±0.01
+Cyg A 42.18 42.18
+MCG +04-48-002 40.44±0.01 40.67 ±0.01
+4C +74.26 45.25 ±0.00 9.45 ±0.01 43.03 ±0.17 43.03 ±0.17 9.00
+IGR 21247+5058 41.88 ±0.02 6.58 ±0.07 40.49 ±0.41 40.49 ±0.41
+RX J2135.9+4728 42.08 ±0.01 7.35 ±0.08 40.54 ±0.74 40.54 ±0.74
+UGC 11871 41.38±0.01 41.38 ±0.01 8.34
+NGC 7319 40.65±0.03 40.92 ±0.03 8.54
+3C 452 40.89±0.01 40.89 ±0.01 8.54
+Mkn 926 43.51 ±0.01 8.36 ±0.02 42.58 ±0.01 42.69 ±0.01 8.95
+1λLλis derived from the power law continuum ﬂux at 5100 ˚A and is the logarithm of the luminosity in units of
+ergss−1.
+2Indicated masses are the logarithm of the mass in solar masse s.
+3The logarithm of [O III]5007˚A luminosity is in units of ergss−1, including the observed luminosity (obs) and
+the extinction corrected values (corr) using values of E(B- V) recorded in Table 13. Where errors are not indicated,
+they are of the order of 10−3.– 64 –
+3500 4000 4500 5000 5500 6000 6500 7000
+Wavelength (
+ A)2000400060008000100001200014000Flux (
+10
+17 ergs s
+1 cm
+2)NGC 221
+3500 4000 4500 5000 5500 6000 6500 7000
+Wavelength (
+A)5001000150020002500300035004000Flux (
+10
+17 ergs s
+1 cm
+	2)NGC 1023
+3500 4000 4500 5000 5500 6000 6500 7000
+Wavelength (
+
+A)400600800100012001400160018002000Flux (
+10
+17 ergs s
+1 cm
+2)NGC 3640
+3500 4000 4500 5000 5500 6000 6500 7000
+Wavelength (
+A)2004006008001000120014001600Flux (
+10
+17 ergs s
+1 cm
+2)NGC 5308
+Fig. 1.— Plotted are the KPNO spectra of 4 template galaxies ( black) with the best-ﬁt continuum
+model (blue) described in Table 5. Using three simple stella r population models (young, inter-
+mediate, old), we ﬁnd that we can replicate the spectra well, particularly in the blue end of the
+spectrum. Using additional populations at intervening age s, we could better replicate the spectra.
+However, such ﬁts are degenerate (Tremonti et al. 2004) and w e would lose information about the
+host galaxy, when ﬁtting to our AGN sources (for which the hos t properties are not well-deﬁned).– 65 –
+Fig. 2.— Plotted are the SDSS spectra of 4 AGN, two narrow line sources (top) and two broad
+line sources (bottom), before and after the continnum subtr action (black). The best-ﬁt continuum
+model is plotted in blue (described in Table 6). The continuu m model utilizes three simple stellar
+population models (young, intermediate, old) along with a p ower law model to account for AGN
+emission.– 66 –
+Fig. 3.— Plotted are the best-ﬁt individual components (pow er law and stellar components, mod-
+ulated by reddening) ﬁtted to the spectra shown in Figure 2. T he ﬂux is shown in units of
+10−17ergss−1cm−2˚A−1. The sources shown include NGC 4992 (top left), Mrk 417 (top r ight),
+Mkn 1018 (bottom left), and MCG +04–22–042 (bottom right). T he combined ﬁt is shown in red,
+while individual stellar components and the power law are ea ch shown in blue. Masked regions
+are shown in green. The ﬁrst three sources have strong galaxy contributions, each dominated by a
+contribution from an old population. The ﬁnal source is best -ﬁt with a pure reddened power law
+model.– 67 –
+Fig. 4.— Plotted are the SDSS spectra (blue) and KPNO spectra (black) of the 4 AGN sources
+with spectra from both sources, focusing on a region (3700–6 200˚A) which shows both emission
+(i.e. Hβand [O III]) and intrinsic absorption features. The ﬁtted continuum f or each spectrum
+is shown with the dotted lines. Comparison of the two sets of s pectra for each source show good
+agreement between the ﬂux measurements and spectral shape.– 68 –
+Fig. 5.— Plotted are ﬁts to the H βand Hαregions of the broad line spectra of SDSS
+J090432.19+553830.1 (top), Mkn 841 (middle), and MCG +04-2 2-042 (bottom). The narrow com-
+ponents are shown in blue, while the total ﬁt (broad + narrow l ines) is shown in red.– 69 –
+3850 3900 3950 4000 4050 4100
+Wavelength (
+A)51015202530Flux (
+10
+17 ergs s
+1 cm
+2)Dn(4000) =0 .99SDSS J091129.97+452806.0
+3850 3900 3950 4000 4050 4100
+Wavelength (
+A)10152025303540455055Flux (
+10
+17 ergs s
+1 cm
+2)Dn(4000) =1 .48CGCG 041-020
+3850 3900 3950 4000 4050 4100
+Wavelength (
+A)1020304050607080Flux (
+10
+ 17 ergs s
+!1 cm
+"2)Dn(4000) =#1.25NGC 4992
+4040 4060 4080 4100 4120 4140 4160
+Wavelength (
+$A)1015202530Flux (
+%10
+&17 ergs s
+'1 cm
+(2) H)A=*0.30SDSS J091129.97+452806.0
+4040 4060 4080 4100 4120 4140 4160
+Wavelength (
++A)303540455055Flux (
+,10
+-17 ergs s
+.1 cm
+/2)H 0A=0.91CGCG 041-020
+4040 4060 4080 4100 4120 4140 4160
+Wavelength (
+1A)45505560657075Flux (
+210
+317 ergs s
+41 cm
+52)H 6A=4.5NGC 4992
+3850 3900 3950 4000 4050 4100
+Wavelength (
+7A)406080100120140160180Flux (
+810
+917 ergs s
+:1 cm
+;2)Dn(4000) =1 .51MGC -01-13-025
+3850 3900 3950 4000 4050 4100
+Wavelength (
+<A)260280300320340Flux (
+=10
+>17 ergs s
+?1 cm
+@2)Dn(4000) =0 .96Mkn 1018
+3850 3900 3950 4000 4050 4100
+Wavelength (
+AA)8009001000110012001300140015001600Flux (
+B10
+C17 ergs s
+D1 cm
+E2)Dn(4000) =0 .91NGC 4593
+4040 4060 4080 4100 4120 4140 4160
+Wavelength (
+FA)120130140150160170Flux (
+G10
+H17 ergs s
+I1 cm
+J2)H KA= L2.15MGC -01-13-025
+4040 4060 4080 4100 4120 4140 4160
+Wavelength (
+MA)260265270275280285290295300305Flux (
+N10
+O17 ergs s
+P1 cm
+Q2)HRA=S1.92Mkn 1018
+4040 4060 4080 4100 4120 4140 4160
+Wavelength (
+TA)850900950100010501100115012001250Flux (
+U10
+V17 ergs s
+W1 cm
+X2)HYA=Z1.92NGC 4593
+Fig. 6.— Plotted are the spectra, with errors, in the regions whereDn(4000) and H δAare mea-
+sured for representative narrow line (top two panels) and br oad line (bottom two panels) sources.
+Absorption lines of Ca IIH&K and H δare indicated with dashed lines. For the narrow line sources ,
+emission lines in the spectra were subtracted.– 70 –
+0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0
+Dn(4000)
+[8
+\6
+]4
+^20246H
+_A
+0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0
+Dn(4000)
+`8
+a6
+b4
+c20246H
+dA
+Fig. 7.— Plotted are two age indicators, H δAwhich measures recent bursts of star formation and
+Dn(4000) which measures the Ca IIbreak and is sensitive to old stellar populations. The circl es
+represent narrow line sources and the triangles represent b road line sources. In the top plot, we
+show the values measured after subtracting out the power law components (Table 6). The bottom
+plot shows the values measured directly from the spectra. In both plots, the box in the upper left
+hand corner shows the area where young stellar populations h ad signiﬁcant ( /greaterorsimilar30%) contributions
+in our test galaxy spectra (see §A, Figure 19).– 71 –
+Mgb0.81.21.62.0Dn(4000)
+Mgb
+e0.40.20.81.4CN1
+Mgb
+f4048Ca 4227
+Mgb
+g10
+h505C2 4668i4j20 2 4 6 8
+Mgb
+k226[MgFe]
+lm4n20 2 4 6 8
+Mgb
+o226<Fe>
+Fig. 8.— Plotted are a selection of stellar absorption indic es indicating stellar age (D n(4000))
+or metallicity of the populations vs. the metallicity indic ator Mgb. The circles represent narrow
+line sources and the triangles represent broad line sources . In the top left plot, we show a line
+representing the division in D n(4000) between populations with a signiﬁcant contribution from
+young stars ( /greaterorsimilar30%), as determined in Figure 19.– 72 –
+0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6
+E(B-V)051015202530 No. of Narrow Line Sources
+0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6
+E(B-V)051015202530 No. of Broad Line Sources
+Fig. 9.— Plotted are the distributions of E(B-V) for the narr ow line (left) and broad line (right)
+sources. The average value and standard deviation are much s maller for the broad line sources, as
+expected from the uniﬁed model.– 73 –
+10-210-1100
+[NII]/Hp10-1100101[OIII]/H
+qAGN
+HIIAGN
+HIIAGN
+HII
+10-210-1100
+[SII]/Hr10-1100101[OIII]/H
+sSeyfert
+HII
+LINERSeyfert
+HII
+LINERSeyfert
+HII
+LINER
+10-210-1100
+[OI]/Ht10-1100101[OIII]/H
+uSeyfert
+HII
+LINERSeyfert
+HII
+LINERSeyfert
+HII
+LINER
+10-210-1100
+[OI]/Hv10-210-1100101102[OIII]/[OII]Seyfert
+HII LINERSeyfert
+HII LINER
+Fig. 10.— Plotted are the emission line diagrams showing nar row line (circles) and broad line
+(triangles) sources from the KPNO or SDSS spectra that we hav e analyzed, as well as values
+extracted from the literature (square). The diagnostic lin es separating H IIgalaxies from AGNs
+are shown in red (Kewley et al. 2001). In the [O III]/Hβversus [N II]/Hαdiagnostic plot, the
+dashedbluelinerepresentsthedivisionbetween H IIgalaxies andcompositesfromKauﬀmann et al.
+(2003a). The blue dashed lines on the remaining plots repres ent the division between Seyferts and
+LINERs from Kewley et al. (2006).– 74 –
+10-1100101102103
+(I4959+I5007)/I43630.60.81.01.21.41.61.82.02.2I6716/I6731
+103104105106107108
+Ne (cm
+w3)100101102103(I4959+I5007)/I436310000 K
+12500 K
+15000 K
+20000 K
+50000 K
+Fig. 11.— Plotted at the top is a comparison of the ratio of int ensities of [S II]λ6716/λ6731 versus
+the ratio of [O III] (λ4959 +λ5007)/λ4363 for the narrow line (circle) and broad line (triangle)
+sources. A K-S test shows that the ratios of [S II] (an indicator of density) are likely from the
+same population, while the [O III]-temperature diagnostic is not. In the bottom plot, we show the
+average diagnostic value for the narrow (horizontal blue li ne) and broad (horizontal red line) line
+sources versus density for values of constant temperature. This diagnostic points to a much higher
+temperature for the broad line sources, if the densities are low. If the densities are high in this O+2
+emission region for broad line sources (106cm−3/lessorsimilarNe/lessorsimilar107cm−3) and low ( Ne/lessorsimilar104cm−3) for
+narrow line sources, the temperatures are similar.– 75 –
+37 38 39 40 41 42 43 44
+log L[OIII ](obs)0246810 No. of Narrow Line Sources
+37 38 39 40 41 42 43 44
+log L[OIII ](obs)05101520 No. of Broad Line Sources
+37 38 39 40 41 42 43 44
+log L[OIII ](corr)0246810 No. of Narrow Line Sources
+37 38 39 40 41 42 43 44
+log L[OIII ](corr)05101520 No. of Broad Line Sources
+Fig. 12.— Plotted are histograms of the [O III] 5007˚A emission line luminosity for the narrow line
+(Seyferts = blue, LINERs = green, others = hatched) and broad line (red) sources, showing both
+the observed (obs, top plots) and extiction-corrected (cor r, bottom plots) luminosities. The broad
+line sources are more luminous on average than the narrow lin e sources, in both the observed and
+extinction-corrected luminosities. The mean value for the extinction-corrected luminosity distribu-
+tion of broad line sources is logL [OIII]= 41.79, while the narrow line sources have a mean value of
+logL[OIII]= 40.82.– 76 –
+40 41 42 43 44 45 46
+log L14x195keV02468101214 No. of Broad Line Sources
+40 41 42 43 44 45 46
+log L14y195keV024681012 No. of Narrow Line Sources
+Fig. 13.— Plotted are the distributions of the 14–195keV lum inosity for broad line (left) and
+narrow line (right) sources. The narrow line classiﬁcation s are represented as Seyferts (white),
+LINERs (black), and either ambiguous/H IIgalaxies/composites (hatched). The Seyferts are the
+most luminous of the narrow line sources, both in the hard X-r ay band and the optical (indicated
+by the [OIII] 5007 ˚A luminosities). While the broad line sources have an averag e X-ray luminosity
+higher than the narrow line sources, the distribution of lum inosities for narrow line Seyferts is the
+same as for the broad line sources as a whole.– 77 –
+1040104110421043104410451046
+L14z195keV (ergs s
+{1)1038103910401041104210431044L[OIII ] (obs) (ergs s
+|1)
+1040104110421043104410451046
+L14 }195keV10-510-410-310-210-1100L[OIII ] (obs)/L14
+~195keV
+1040104110421043104410451046
+L14 195keV (ergs s
+1)1038103910401041104210431044L[OIII ] (corr) (ergs s
+1)
+1040104110421043104410451046
+L14195keV10-510-410-310-210-1100L[OIII ] (corr)/L14
+195keV
+Fig. 14.— Plotted is the relationship between observed (top ) and reddening corrected (bottom)
+[OIII] 5007 ˚A luminosities and the 14–195keV Swift BAT luminosities (le ft) and the ratio of these
+luminosities versus the Swift BAT luminosity (right). In th e plots, broad line sources are indicated
+with red triangles, while the narrow line sources are indica ted with blue circles. As the left plots
+show, L [OIII]is not well correlated with the hard X-ray luminosity. The li nes indicate the weak
+correlations seen for the Seyfert 1s ((corrected) R2= 0.35) and narrow line sources ((corrected)
+R2= 0.38). In the right-hand plots, it is clear that there is a great deal of scatter in the optical/X-
+ray ratio for a given X-ray luminosity.– 78 –
+106107108109
+MH (M)106107108109Mreverb (M
+)
+106107108109
+MH  (M)106107108109M2MASS (M
+)
+Fig. 15.— Plotted are comparisons of the H βderived masses from the FWHM of the broad
+component of H βandλLλ(5100˚A) and two additional mass estimates. The ﬁrst comparison is
+with reverberation mapping masses, largely from Peterson e t al. (2004). We ﬁnd good agreement
+between the H βmasses and this more direct mass measurement. The second com parison is with
+masses derived from the 2MASS K-band stellar magnitudes (Mu shotzky et al. 2008; Winter et al.
+2009a). We also ﬁnd a correlation between these two mass meas urements (IR and H βderived),
+indicated by the bolder dashed line. The additional dashed l ines on the second plot represent
+values with (from the top to bottom most line) 10 ×diﬀerence, 2 ×diﬀerence, 1:1 correspondence,
+1/2 diﬀerence, or 1/10 diﬀerence.– 79 –765432
+Log L[OIII ]/LEdd024681012 No. of Narrow Line Sources765432
+Log L[OIII ]/LEdd024681012 No. of Broad Line Sources
+Fig. 16.—Plotted arethedistributionsofL [OIII]/LEddforthenarrowline(Seyferts=blue, LINERs
+= green) and broad line (red) sources. The [O III] 5007˚A luminosity scales with the bolometric
+luminosity, making the ratio L [OIII]/LEddan indicator of the accretion rate. While the ratio of
+L[OIII]/LEddislower forthenarrowlinesources, acomparisonoftheaccr etion ratesdependsgreatly
+on the bolometric corrections, which are determined from th e spectral energy distributions and are
+not well known, particularly for the narrow line sources. On ly two of the H II/ambiguous/other
+sources have masses available to calculate L [OIII]/LEdd. The average value for these sources is low,
+with logL [OIII]/LEdd=−5.4, but not as low as the value for the three LINERs with availab le mass
+measurements (-5.9).– 80 –
+0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 2.2
+Dn(4000)1038103910401041104210431044Log L[OIII ]86 42 0 2 4 6
+HA1038103910401041104210431044Log L[OIII ]
+0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 2.2
+Dn(4000)10-710-610-510-410-3Log L[OIII ]/LEdd8 6 42 0 2 4 6
+HA10-710-610-510-410-3Log L[OIII ]/LEdd
+Fig. 17.— Plotted are two age indicators, H δAwhich measures recent bursts of star formation
+and Dn(4000) which measures the Ca IIbreak and is sensitive to old stellar populations versus the
+reddening corrected [O III] 5007˚A luminosity and L [OIII]/LEddfor the narrow line (circles) and
+broad line (triangles) sources.– 81 –
+Table 16. Stellar Light Fits to the Test Spectra
+Test Spectrum FWHM†Z†Lfyoung†Lfinterm†Lfold†
+25 Myr (Y) 300 0 .2Z⊙0.89 0.00 0.11
+2500 Myr (I) 330 2.5 Z⊙0.00 1.00 0.00
+10000 Myr (O) 300 Z⊙0.00 0.00 1.00
+0.5×(Y + I ) 300 0 .2Z⊙0.41 0.28 0.30
+0.5×(Y + O ) 300 Z⊙0.32 0.68 0.00
+0.5×(I + O) 330 2.5 Z⊙0.00 1.00 0.00
+0.33×(Y + I + O) 300 Z⊙0.19 0.81 0.00
+†The ﬁtted values using the stellar population models of Bruzual & Cha rlot
+(2003) include FWHM (kms−1), metallicity ( Z), and light fractions ( Lf) at
+5500˚Ausing populations at 25 (young or Y), 2500 (interm or I), and 1000 0
+(old or O) Myr.
+Table 17. Best-ﬁt Power law + Stellar Light Fits to the Test Sp ectra
+Source FWHM†Z†p0†p1†Lfpow†Lfyoung†Lfinterm†Lfold†
+25 Myr (Y) + pow 300 Z⊙9.3×10−40.77 0.42 0.58 0.00 0.00
+2500 Myr (I) + pow 300 Z⊙3.3×10−30.66 0.44 0.00 0.56 0.00
+10000 Myr (O) + pow 300 Z⊙4.6×10−40.87 0.45 0.00 0.09 0.46
+0.5×(Y + I ) + pow 300 Z⊙8.5×10−40.79 0.41 0.30 0.24 0.05
+0.5×(Y + O ) + pow 300 Z⊙4.2×10−20.41 0.61 0.20 0.00 0.19
+0.5×(I + O) + pow 300 Z⊙6.2×10−40.83 0.44 0.00 0.29 0.28
+0.33×(Y + I + O) + pow 300 Z⊙3.8×10−40.87 0.41 0.19 0.20 0.20
+†The ﬁtted values using the stellar population models of Bruzual & Cha rlot (2003) include FWHM (kms−1),
+metallicity ( Z), and light fractions ( Lf) at 5500 ˚A using both a power law and stellar population models with
+ages of: 25 (young), 2500 (interm), and 10000 (old) Myr. The valu esp0andp1are the power law components,
+deﬁned as p0×λp1. The constant factor, p0, is constrained to range from 0 to 1.– 82 –
+Fig. 18.— Plotted are several of the test spectra created by b roadening combinations of the stellar
+population models to a velocity dispersion of 300 km s−1, adding random noise, and the eﬀects of
+reddening. From top to bottom, plotted are a young, 50% young + 50% intermediate, 50% young +
+50% old, 33% young + 33% intermediate + 33% old, and 50% interm ediate + 50% old population.
+Notice, there is very little diﬀerence between the 50% young + 50% intermediate and 50% young
++ 50% old populations. We speciﬁcally plot the region surrou nding the 4000 ˚Abreak, a region with
+prominent intrinsic absorption features.– 83 –
+0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0
+Dn (4000)
+ 8
+¡6
+¢4
+£20246H
+¤AYoung
+Fig. 19.— Plotted isthestellar absorptionindexH δAversustheD n(4000) indexforthetest spectra.
+Both are commonly used as age indicators of a stellar populat ion. In the plot, our test spectra,
+consisting of combinations of single stellar population mo dels, are shown for three metallicities:
+0.2Z⊙(triangle), Z ⊙(circle), and 2.5 Z ⊙(square). We ﬁnd that metallicity has little eﬀect on the
+values of thesestellar absorption indices, as expected. We also ﬁndthat populations withsigniﬁcant
+contributions from young populations (33% or higher) fall w ithin a small parameter space on the
+plot, towards the upper left hand corner.– 84 –
+Mgb1.01.41.82.2Dn(4000)
+Mgb
+¥0.6
+¦0.20.20.6CN1
+Mgb
+§1258Ca 4227
+Mgb0510C2 4668¨4©20 2 4 6 8
+Mgb
+ª1258[MgFe]«4¬20 2 4 6 8
+Mgb
+­1258<Fe>
+Fig. 20.— Plotted are measured stellar absorption indices v ersus the Mgb stellar absorption index
+for the test spectra. With the exception of D n(4000), which is an age indicator, the remaining
+plotted indices are sensitive to abundancesof metals inthe population. Inthe plot, our test spectra,
+consisting of combinations of single stellar population mo dels, are shown for three metallicities:
+0.2Z⊙(yellow), Z ⊙(black), and 2.5 Z ⊙(green). The line in the top left plot indicates the division
+between young populations (below the line) and older popula tions (see Figure 19).
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