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).