text:
\section{Introduction}
Active galactic nuclei (AGN) are among the most powerful objects in the universe with an extraordinary amount of energy released from their  unresolved nuclei.  Active super-massive black holes (SMBH) in the center of these galaxies are responsible for the tremendous diversity in their observed energy emission \citep[e.g.,][]{1984ARA&A..22..471R,1989ApJ...347...29S,2000ApJ...540L..13P,2004ApJ...613..682P}. Despite the fact that the unified  scheme of AGN has been able to explain the observed type I/II dichotomy \citep[see][for a review]{1993ARA&A..31..473A}, it is clear that by looking at different wave bands there are additional parameters that can complement our current understanding of AGN classification other than to be attributed solely to a viewing angle difference \citep[e.g.,][]{1997ApJ...485..552M,2001ApJ...546..845G,2006AJ....132..401B,2008ApJ...689...95M}. Therefore, in order to unveil and understand the complexity of these sources, ones needs to rely  on multiwavelength studies. In particular,  the radio  and mid-infrared emissions are basically unaffected by  dust extinction which make these energy bands ideal to investigate the nature of the ``hidden" nuclear engine. On the other hand, extended radio emission and low-ionization mid-infrared emission lines  are excellent tracers of star formation activity when properly calibrated \citep[e.g.,][]{1992ARA&A..30..575C,2007ApJ...658..314H}.

 Furthermore,  the strength of the observed radio emission in AGN seems to follow a bimodal distribution falling into  ``radio loud" and ``radio quiet" sources \citep[e.g.,][]{1990MNRAS.244..207M,1999AJ....118.1169X}. Historically, the dividing criterion for the AGN radio loudness was adopted to be the ratio between the radio emission, at the most commonly used frequency of 5~GHz, and the optical continuum at $\sim 4400$~\AA, i.e., the  radio-to-optical parameter, ${\rm R=L_\nu{\rm (6{\rm cm})}/L_\nu({\rm B})}$ \citep[e.g.,][]{1989AJ.....98.1195K,1992ApJ...391..560V}. This convention to quantize the radio loudness of a source is straightforward  when the contribution from the host galaxy does not affect the observed radio and optical components of the AGN, for example in quasars, where the active nucleus overpowers the underlying galaxy. In the case of Seyfert galaxies the quantification  of their radio loudness could be  more subtle.  \citet{2001ApJ...555..650H} found that most Seyfert 1 galaxies, previously classified as radio-quiet, fall  into the radio loud regime when the nuclear component for the radio-to-optical parameter is properly measured. However, even with a resolution of few arcseconds, the nuclear  component of the optical luminosity could be contaminated by star formation and   is strongly affected by dust extinction that may lead to an erroneous AGN characterization.

Previous multiwavelength studies have shown  statistically significant correlations  between the radio core luminosity and purportedly orientation-independent measures of the intrinsic luminosity of the active nuclei, which   suggests a common mechanism at nuclear (subkiloparsec) scales, , e.g., accretion onto the black hole \citep[e.g.,][]{1989MNRAS.240..701R,1999AJ....118.1169X,2002ApJ...564..120H,2009ApJ...698..623D}. On the other hand, the correlations between extra-nuclear radio emission and the far-infrared (FIR) luminosity of the galaxy suggest a circumnuclear starburst as the common cause for these observables \citep[e.g.,][]{1982ApJ...252..102C,1988AJ.....96...30C,1993ApJ...419..553B,1998MNRAS.301.1019R}.  In this regard, early studies suggested two possible scenarios for the origin of the compact radio fluxes observed in radio quiet sources: either the radio emission is associated with a nuclear starburst or generated by relativistic electrons accelerated by a low-power jet (similar to radio loud sources), with high-resolution radio-imaging observations favoring the latter \citep[e.g.,][]{1998MNRAS.299..165B}. More recently, the good correlation between the X-ray and the radio luminosities  raise the possibility  that radio emission in radio quiet sources may  have  a coronal origin \citep{2008MNRAS.390..847L}. All these exemplify that the radio properties of the AGN are diverse and can be intimately  associated with fundamental parameters of the active galaxies, such as the black hole masses, mass accretion rates, and  host galaxy morphology \citep[e.g.,][]{1999AJ....118.1169X,2000ApJ...543L.111L,2001A&A...380...31W}.

Recently,  \citet{2008ApJ...682...94M} found a tight correlation in Seyfert 1 galaxies between the [O~IV]~$\lambda$25.89~$\micron$ and the X-ray 14-195~keV continuum luminosities from  {\it Swift}/BAT observations \citep{2005ApJ...633L..77M,2008ApJ...681..113T}. A weaker correlation was  found in Seyfert 2 galaxies, which was attributed to the effect of Compton scattering  in the 14-195~keV band. These results suggest  that [O~IV] is a truly isotropic property of AGNs, given its high ionization potential and that it is basically unaffected by reddening, meaning that the [O~IV] strength directly measures the AGN power. This result has been later confirmed in more  complete samples \citep[][Weaver et al. submitted to ApJ]{2009ApJ...700.1878R}. Moreover, the strong correlation found between [O~IV] and the high-ionization ($\sim$97~eV) [Ne~V]~$\lambda$14.32/24.32~$\micron$ emission is a further argument for [O~IV] being a good indicator for the intrinsic luminosity of the AGN \citep[e.g.,][Weaver et al. submitted to ApJ]{2009ApJ...691.1501D,2009MNRAS.398.1165G}. It is the primary goal of this paper to examine the physical relationship between the nuclear radio emission and the mid-infrared emission line luminosities in Seyfert galaxies. We use high-resolution radio continuum measurements and the [O~IV]  emission line to investigate  the radio loudness of the Seyfert nuclei  and the black hole mass accretion rate for a sample of Seyfert galaxies.

\section{The Sample}
We have obtained, from the literature, observations with the Very Large Array (VLA) in A-configuration at 8.4-GHz \citep[see][for instrumental details]{1980ApJS...44..151T}, with a resolution of $0.25$$'$$'$ and the largest detectable size of $3.5$$'$$'$, for  the radio quiet sources  in the sample of Seyfert galaxies  presented in \citet{2008ApJ...689...95M}. This sample of Seyfert galaxies includes  compilations from \citet{2007ApJ...671..124D}, \citet{2007arXiv0710.4448T}, \citet{2002A&A...393..821S},  \citet{2005ApJ...633..706W} and from our analysis of archival spectra observed with the Infrared Spectrograph (IRS) on board {\it Spitzer Space Telescope} \citep{2004ApJS..154....1W} (see Appendix). For comparison, we also have obtained from the literature  high resolution  1.4~GHz data  observed with the VLA in B configuration, which has a resolution of $\sim 5$$'$$'$, thus only encompassing the nucleus. Figure~\ref{fig1} shows the good correlation between the 1.4~GHz and 8.4~GHz fluxes and the distribution of their  spectral indices. The good correlation is expected as in high-resolution both fluxes are dominated by the active nucleus. One needs to consider that the spectral indices  may provide a lower limit to the nuclear component, as the  1.4~GHz B-configuration fluxes  could  include some extranuclear emission, thus a possible contamination from star formation. In this regard, and in order to  complete this set of high-resolution 8.4~GHz fluxes, we extrapolated high-resolution observations at different frequencies to 8.4GHz by assuming a conservative $f_\nu \propto \nu^{-0.7}$, as determined  by the spectral indices distribution. Finally, in order to check on the  effect of radio emission regions on scales bigger than that sampled by the VLA in B configuration at 1.4~GHz, we compared these data  with fluxes from the NRAO VLA Sky Survey (NVSS), which has a resolution of $\sim 45$$'$$'$. We found an excellent correlation between VLA in B configuration at 1.4~GHz and NVSS fluxes, $r_s=0.89,~P_r<10^{-6}$, that suggests that, in our sample, compact nuclear regions dominate over large-scale extranuclear emission regions.

\begin{figure}
\includegraphics[width=84mm]{comp1.4_8.4.eps}
    \caption{Correlation between the high-resolution 1.4~GHz and 8.4~GHz. The dashed lines indicate the flux density  relationship expected for different spectral indices in Seyfert~1 ({\it circles}) and Seyfert~2 ({\it triangles}) galaxies.\label{fig1}}
\end{figure}

The  final sample includes  29 Seyfert 1's (i.e., Seyfert 1.0's, 1.2's, and 1.5's)  and 59 Seyfert 2's (i.e., Seyfert 1.8's, 1.9's, and 2.0's), which are listed in Table~\ref{table1}.  There are  six upper limits for the 8.4~GHz emission, two Seyfert 1 galaxies and four  Seyfert 2 galaxies.  Note that it was not possible to find 8.4~GHz  high-resolution fluxes for all the galaxies in the sample first presented by  \citet{2008ApJ...689...95M}. The total radio luminosity, ${\rm L_{8.4GHz}\equiv \nu L_\nu {\rm (8.4GHz)}}$ (ergs/s), and the different mid-infrared emission-line luminosities are calculated from the fluxes assuming $H_o=71{\rm kms^{-1}Mpc^{-1}}$ and  a deceleration parameter $q_o=0$.  At the median redshift for the sample, $z= 0.02$, 1$'$$'$ represents $\sim$400~pc. Furthermore, for a full aperture extraction, {\it Spitzer} short-low (low-resolution, R$\sim 60-127$) and short-high (high-resolution, R$\sim 600$) slits will  sample, in the dispersion direction, a region equivalent to the region sampled by the VLA in B-configuration at 1.4-GHz.

\begin{table*}
 \centering
 \begin{minipage}{140mm}
\caption{The Infrared Sample of Seyfert Galaxies\label{table1}}
 \begin{tabular}{@{}lllccccccccl@{}}
  \hline
Name  &$z$&  Type& ${\rm L_{8.4GHz}}$& ${\rm L_{1.4GHz}}$
& $\log{\rm M_{BH}}$&$\log {\rm L_{bol}/L_{Edd}}$ &$ {\rm R_{[O IV]}}$ &  $ {\rm R_{[Ne III]}}$ &
  $ {\rm R_{[Ne II]}}$ &  MC &  Ref. \\

&&& \multicolumn{2}{c}{($\log$~ergs ${\rm s^{-1}}$)}&$(M/M_\odot)$&\\

 \hline

CGCG381-051&0.0307&2&38.02& & & &-2.30&-2.77&-3.53&S &2\\
Circinus&0.0014&2&37.10$^{a}$& &6.23$^{b}$&-0.19&-3.38&-3.08&-3.51&S &8,24\\
ESO012-G021&0.0300&1&$<$39.08$^{a}$& & & &-2.42&-2.03&-2.30&A&9\\
ESO103-G035&0.0133&1&38.79$^{a}$& &7.15&-0.47&-2.34&-2.20&-2.09&A&10,25\\
ESO141-G055&0.0360&1&$<$39.24$^{a}$& &7.10$^{b}$&-0.23&-2.08&-1.97&-1.57&A&9,26\\
ESO541-G012&0.0566&2&38.69& & & &-2.87&-2.48&-2.44&A&2\\
ESO545-G013&0.0337&1&38.65& & & &-2.82&-2.77&-2.76&S &2\\
I Zw 1&0.0611&1&38.78&38.88&7.26$^{d}$&-0.15&-2.77&-3.24&-2.96&S &3,14,27\\
IC4329A&0.0161&1.2&38.86&38.67&7.00$^{e}$&0.32&-2.91&-2.55&-2.20&A&2,13,28\\
IRAS00198-7926&0.0728&2&40.59$^{a}$& &8.44$^{b}$&-0.28&-2.01&-1.64&-1.28&A&11,29\\
IRAS00521-7054&0.0689&2&40.64$^{a}$& &8.45$^{b}$&-0.92&-1.33&-1.30&-1.16&S &11,30\\
IRAS01475-0740&0.0177&2&39.89& &6.09&0.14&-0.79&-1.02&-1.15&S &1,31\\
IRAS04385-0828&0.0151&2&38.50& &8.77$^{b}$&-2.44&-2.27&-2.45&-2.58&S &1,32\\
IRAS15091-2107&0.0446&1&39.46&39.81&7.00$^{d}$&0.69&-2.68&-2.40&-2.25&A&2,16,33\\
IRAS15480-0344&0.0303&2&39.28&39.06&8.22$^{b}$&-0.83&-2.56&-2.20&-1.87&A&1,15,29\\
IRAS22017+0319&0.0611&2&39.15& &8.07$^{b}$&-0.13&-3.24&-2.92&-2.55&A&2,30\\
MCG-2-40-4&0.0252&2&38.54& & & &-2.85&-2.85&-2.74&A&2\\
MCG-2-58-22&0.0469&1.5&39.74$^{a}$& &7.18$^{b}$&0.08&-1.96&-1.95&-1.54&A&4,26\\
MCG-2-8-39&0.0299&2&38.52& &7.85&-0.82&-2.95&-2.77&-2.62&A&1,31\\
MCG-3-58-7&0.0315&2&38.22& & & &-3.20&-3.12&-2.82&A&2\\
MCG-5-13-17&0.0126&1.5&37.86&37.46&7.94&-1.77&-2.76&-2.79&-2.72&A&1,13,31\\
MCG-6-30-15&0.0077&1.2&36.99&36.86&6.81&-0.78&-3.49&-2.74&-2.94&A&13,13,31\\
MRK 3 &0.0140&2&39.45&39.80&8.36&-0.86&-2.50&-2.49&-2.11&A&13,13,31\\
MRK 6&0.0188&1.5&39.41&39.44&7.64$^{b}$&-0.50&-2.18&-2.15&-1.86&A&1,13,26\\
MRK 9&0.0399&1.5&38.38&38.21&7.46$^{b}$&-0.62&-2.92&-2.45&-2.68&A&2,15,26\\
MRK 79&0.0222&1.2&38.26&38.35&7.72$^{e}$&-0.43&-3.48&-3.08&-2.77&A&1,15,28\\
MRK 273&0.0378&2&39.95&39.77&8.22&-0.37&-2.36&-2.18&-2.28&S &2,15,31\\
MRK 334&0.0219&1.8&38.12&38.53&6.51$^{b}$&0.24&-3.08&-3.31&-3.38&S &3,12,34\\
MRK 335 &0.0258&1.2&38.41&38.14&7.15$^{e}$&-0.57&-2.62&-2.13&-2.07&A&3,13,28\\
MRK 348&0.0150&2&40.15&39.32&6.83&-0.21&-0.92&-0.93&-0.65&A&2,13,31\\
MRK 471&0.0342&1.8&38.55$^{a}$&38.16&7.74 &-1.17&-2.47&-2.34&-2.34&A&12,12,35\\
MRK 509&0.0344&1.2&39.17$^{a}$&38.72&8.16$^{e}$&-0.86&-2.58&-2.47&-2.37&A&4,17,28\\
MRK 573&0.0172&2&38.01&38.11&7.28&-0.02&-3.69&-3.18&-2.91&A&3,13,36\\
MRK 609&0.0345&1.8&39.20$^{a}$& &6.80$^{f}$&0.08&-2.13&-2.18&-2.30&S &4,37\\
MRK 622&0.0232&2&38.23&38.00&6.92&-0.30&-2.85&-2.75&-2.62&A&13,13,36\\
MRK 817&0.0315&1.5&38.82& &7.69$^{e}$&-1.02&-2.30&-2.12&-2.22&A&3,28\\
MRK 883&0.0375&1.9&39.43$^{a}$&38.94&8.15&-1.10&-2.06&-1.96&-2.10&S &12,12,25\\
MRK 897&0.0263&2&38.65& &7.42 &-1.89&-1.32&-2.17&-2.91&S &2,25\\
NGC 424&0.0118&2&38.48&38.00&7.54 &-1.26&-2.26&-2.32&-2.18&A&2,13,25\\
NGC 513&0.0195&2&37.92&38.68&7.65&-1.22&-2.95&-2.90&-3.04&S &2,13,36\\
NGC 931&0.0167&1.5&37.78& &7.64 &-0.67&-3.63&-3.34&-2.90&A&1,36\\
NGC 985&0.0431&1&39.11$^{a}$&38.58&8.05$^{d}$&-0.76&-2.63&-2.58&-2.36&A&4,15,38\\
NGC 1068&0.0038&2&39.30&39.24&7.56 &-0.24&-2.47&-2.40&-2.04&A&3,15,25\\
NGC 1125&0.0109&2&38.40& &7.01 &-0.58&-2.47&-2.50&-2.44&A&2,25\\
NGC 1194&0.0136&1&37.48&36.92&7.32$^{b}$&-1.02&-3.27&-3.08&-2.82&A&2,15,39\\
NGC 1320&0.0135&2&37.52&37.31&7.18&-0.52&-3.58&-3.03&-3.03&A&2,13,36\\
NGC 1365&0.0055&1.8&37.70&37.54&7.62$^{g}$&-1.03&-3.34&-2.89&-3.33&S &2,18,40\\
NGC 1667&0.0152&2&37.80&37.41&7.62 &-1.29&-2.98&-3.18&-3.31&S &2,19,25\\
NGC 2639&0.0111&1.9&39.42&38.59&7.94 &-2.48&-0.48&-0.78&-1.05&S &2,19,41\\
NGC 2992&0.0077&2&38.64&38.57&7.87 &-1.19&-2.48&-2.26&-2.21&A&2,20,25\\
NGC 3079&0.0037&2&38.37&38.09&7.97 &-2.39&-1.66&-1.55&-2.28&S &3,15,41\\
NGC 3227&0.0039&1.5&37.51&37.57&7.63$^{e}$&-1.78&-2.77&-2.85&-2.80&A&3,15,28\\
NGC 3516&0.0088&1.5&37.64&37.35&7.63$^{e}$&-1.27&-3.16&-3.00&-2.49&A&3,13,28\\
NGC 3660&0.0123&2&$<$36.92& &6.83 &-1.21&-3.16&-2.77&-3.41&S &2,25\\
NGC 3783&0.0097&1.5&38.14& &7.47$^{e}$&-1.14&-2.65&-2.59&-2.49&A&1,28\\
NGC 3786&0.0089&1.8&37.16&37.46&7.53&-1.46&-3.35&-3.15&-3.12&A&3,20,36\\
NGC 3982&0.0037&2&36.29&36.22&6.37 &-2.05&-2.47&-2.87&-3.38&S &3,15,41\\

\hline
\end{tabular}
\end{minipage}
\end{table*}

\begin{table*}
 \centering
 \begin{minipage}{140mm}
\contcaption{The Infrared Sample of Seyfert Galaxies}
 \begin{tabular}{@{}lllccccccccl@{}}
  \hline
Name  &$z$&  Type& ${\rm L_{8.4GHz}}$& ${\rm L_{1.4GHz}}$
& $\log{\rm M_{BH}}$&$\log {\rm L_{bol}/L_{Edd}}$ &$ {\rm R_{[O IV]}}$ &  $ {\rm R_{[Ne III]}}$ &
  $ {\rm R_{[Ne II]}}$ &  MC &  Ref. \\

&&& \multicolumn{2}{c}{($\log$~ergs ${\rm s^{-1}}$)}&$(M/M_\odot)$&\\

 \hline

NGC 4051&0.0023&1.5&35.77&36.50&6.28$^{e}$&-1.16&-3.80&-3.66&-3.53&A&3,15,28\\
NGC 4151&0.0033&1.5&38.16&38.04&7.12$^{e}$&-0.81&-2.61&-2.61&-2.35&A&3,15,28\\
NGC 4388&0.0084&2&38.08&37.88&7.10 &0.04&-3.50&-3.09&-3.03&A&3,15,25\\
NGC 4501&0.0076&2&$<$36.32&36.67&7.81 &-2.54&-3.40&-3.45&-3.62&S &2,15,41\\
NGC 4507&0.0118&1.9&38.11& &7.56 &-0.94&-2.95&-2.83&-2.90&A&5,25\\
NGC 4748&0.0146&1&37.70& &6.44&0.69&-3.88&-3.16&-2.83&A&5,31\\
NGC 4941&0.0037&2&37.00&36.77&6.88 &-1.46&-2.86&-2.84&-2.63&A&1,19,25\\
NGC 4968&0.0099&2&38.01&37.98&7.25 &-0.90&-2.79&-2.69&-2.69&A&2,13,25\\
NGC 5005&0.0032&2&37.20&37.14&7.87 &-2.73&-2.39&-2.34&-2.91&S &2,15,41\\
NGC 5256&0.0279&2&39.32&39.12&6.92$^{b}$&0.65&-2.70&-2.48&-2.80&S &2,15,26\\
NGC 5347&0.0078&2&37.24&36.79&6.79&-1.30&-2.69&-2.49&-2.59&A&1,19,36\\
NGC 5506&0.0062&1.9&38.86&38.58&6.88 &-0.12&-2.35&-1.93&-1.77&A&1,15,25\\
NGC 5548&0.0172&1.5&38.07&38.31&7.83$^{e}$&-1.29&-2.91&-2.88&-2.34&A&3,13,28\\
NGC 5643&0.0040&2&37.22&37.29&6.79 &-0.64&-3.38&-3.06&-2.97&A&6,21,25\\
NGC 5929&0.0083&2&38.32&38.17&7.22&-1.65&-1.70&-1.80&-2.17&S &3,15,31\\
NGC 5953&0.0066&2&36.93&37.92&6.79 &-0.93&-3.38&-3.36&-4.06&S &2,15,25\\
NGC 6240&0.0245&2&39.77&39.85&9.15 &-1.80&-2.03&-2.14&-2.64&S &7,7,42\\
NGC 6300&0.0037&2&36.82& &6.92 &-1.31&-3.24&-2.84&-2.83&A&6,25\\
NGC 6890&0.0081&2&37.25&37.29&7.07 &-1.37&-2.90&-2.72&-2.95&A&2,19,25\\
NGC 7130&0.0162&2&38.93& &7.52&-0.58&-2.45&-2.39&-2.67&S &2,31\\
NGC 7213&0.0058&1.5&39.06& &7.99&-2.86&-0.51&-0.93&-1.22&S &1,36\\
NGC 7314&0.0048&1.9&36.84& &6.03 &0.02&-3.65&-3.17&-2.84&A&2,25\\
NGC 7469&0.0163&1.5&38.89&39.17&7.09$^{e}$&0.04&-2.69&-2.43&-3.21&S &3,22,28\\
NGC 7582&0.0053&2&38.41&38.14&7.40 &-0.84&-2.60&-2.19&-2.53&A&2,21,25\\
NGC 7590&0.0053&2&$<$36& &6.90 &-1.83&-3.52&-3.32&-3.67&A&2,25\\
NGC 7603&0.0295&1.5&38.73&38.75&8.08&-1.40&-2.40&-2.40&-2.60&S &2,15,36\\
NGC 7674&0.0289&2&39.79&39.70&7.56 &-0.08&-2.14&-2.14&-1.73&A&3,23,36\\
TOL1238-364&0.0109&2&38.32&$\geq$38.45&6.83&-0.79&-2.17&-2.62&-2.68&S &2,19,31\\
UGC 7064&0.0250&1.9&$<$37.36&38.16& & &-4.01&-3.77&-3.62&A&2,15\\
UGC 12138&0.0250&1.8&38.34& &7.16&-0.43&-2.84&-2.70&-2.27&A&5,31\\
UM 146&0.0174&1.9&38.54& &6.19&-0.52&-1.58&-1.89&-1.76&S &3,31\\

\hline
\end{tabular}
\medskip
$^a$ 8.4~GHz High-resolution data was unavailable, thus we extrapolated measurements from other wavelengths assuming, $f_\nu \propto \nu^{-0.7}$ \\
$^b$ Values for the stellar velocity dispersion from the FWHM of [O~III] $\lambda~5007$, $\sigma_{[OIII]}$ \\
$^c$ Maser Kinematics\\
$^d$ Virial Theorem\\
$^e$ Reverbertation Mapping \\
$^f$ From broad ${\rm H_\alpha}$ emission\\
$^g$ $M_{BH}-\sigma_{bulge}$ relationship\\
Note: The luminosities were calculated from the fluxes using  $H_o=71{\rm kms^{-1}Mpc^{-1}}$ and  a deceleration
parameter $q_o=0$ with  redshift values taken from NED. ${\rm R_{[O IV]}}$, $ {\rm R_{[Ne III]}}$ and  $ {\rm R_{[Ne II]}}$ are the 8.4GHz-to-mid-infrared parameters. The last two columns show the main contribution (MC) to the [Ne~II] emission line (A=AGN and S=Star Formation) and the references for the observed  high-resolution 8.4~GHz and 1.4~GHz emission fluxes and black holes masses ${\rm M_{BH}}$, respectively. Most of the values for the BH masses were calculated by using the relationship between the black hole mass and the stellar velocity dispersion \citep{2002ApJ...574..740T}, unless noted.\\
References: (1)  \citet{2001ApJ...555..663S}, (2)  \citet{2000MNRAS.314..573T}, (3)  \citet{1995MNRAS.276.1262K}, (4)  \citet{1984ApJ...278..544U}, (5)  Schmitt et al. 2009, in prep, (6)  \citet{1999A&AS..137..457M}, (7) \citet{1994ApJ...436...89C}, (8)  \citet{1998MNRAS.293..189D}, (9)  \citet{1994ApJ...432..496R}, (10)  \citet{1998MNRAS.300.1111H}, (11)  \citet{1998MNRAS.301.1019R}, (12) \citet{1986ApJ...310..136U}, (13)  \citet{1999ApJS..120..209N}, (14)  \citet{1987AJ.....93..255C}, (15)  \citet{1995ApJ...450..559B}, Faint Images of the Radio Sky at Twenty Centimeters (FIRST) survey, (16)  \citet{1995AJ....109...81U}, (17)  \citet{1987MNRAS.228..521U}, (18)  \citet{1995A&A...295..585S}, (19) \citet{1989ApJ...343..659U}, (20)  \citet{1984ApJ...285..439U}, (21)  \citet{1985MNRAS.216..193M}, (22)  \citet{2006AJ....131..701L}, (23)  \citet{1985ApJ...296...60M}, (24)  \citet{2003ApJ...590..162G}, (25)  \citet{2004MNRAS.355..273C},  (26)  \citet{1992ApJS...79...49W},  (27)  \citet{2007ApJ...661..660K},  (28)  \citet{2004ApJ...613..682P},  (29)  \citet{1991MNRAS.253...19L},  (30)  \citet{1996MNRAS.281.1206Y},  (31)  \citet{2005MNRAS.359..765G},  (32)  \citet{2007ApJ...661L.143W}, (33)  \citet{2007ApJS..169....1O}, (34)  \citet{1988ApJS...67..249D}, (35)  \citet{2007ApJ...668...94H}, (36)  \citet{1995ApJS...99...67N}, (37)  \citet{2007ApJ...667..131G}, (38)  \citet{2005MNRAS.358.1405O}, (39)  \citet{1990AJ.....99.1722K}, (40)  \citet{2009MNRAS.393L...1R},  (41)  \citet{2009ApJS..183....1H},  (42)  \citet{1994ApJ...437L..23D}

\end{minipage}
\end{table*}

In order to confirm that our sample is not biased in terms of luminosities we compared  the different luminosities  for both the mid-infrared emission lines and the radio continuum luminosities for the two groups of galaxies. The histograms of [Ne~II], [Ne~III] and [O~IV]  luminosities and 8.4~GHz continuum luminosities  are presented in  Figure~\ref{hist} with the results from the  Kolmogorov-Smirnov (K-S) test presented in Table~\ref{table2}. This table also includes information about the numbers of Seyfert 1 and Seyfert 2 galaxies, median values and standard deviations of the mean for the measured quantities. For the 8.4~GHz continuum the K-S test  returns a $\sim 82.0\%$ probability of the null hypothesis  (i.e., that there is no difference between Seyfert 1 and Seyfert 2 galaxies), or in other words,  two samples drawn from the same parent population would differ this much $\sim 82.0\%$ of the time\footnote{A probability  value of less than $5\%$ represents a 2$\sigma$ level of significance that two samples drawn from the same population are different. A strong level of significance, at 3$\sigma$ level, is obtained for values smaller than $1\%$ \citep[e.g.,][]{1992nrfa.book.....P,2003drea.book.....B}}. For the [Ne~II], [Ne~III] and [O~IV]  luminosity distributions the K-S test  returns a $\sim 96.9\%$, $\sim 47.9\%$ and $\sim 27.8\%$ probability of the null hypothesis, respectively.

\begin{figure}
\includegraphics[width=84mm]{comp_histograms.eps}
    \caption{Comparison of the [Ne~II], [Ne~III], [O~IV] and 8.4~GHz luminosities (in $ergs~s^{-1}$) in Seyfert 1 ({\it dashed line}) and Seyfert 2 ({\it solid line}) galaxies. This sample includes 29 Seyfert 1 galaxies and 59 Seyfert 2 galaxies for the mid-infrared luminosity  distributions. Upper limits are not included in the 8.4~GHz luminosity distribution. The K-S test for these luminosities  returns a $\sim 96.9\%$, $\sim 47.9\%$,$\sim 27.8\%$ and $\sim 82.0\%$ probability of the null hypothesis for the  [Ne~II], [Ne~III], [O~IV] and 8.4~GHz luminosities, respectively \label{hist}}
\end{figure}

It can be seen that Seyfert 1 and Seyfert 2 galaxies have similar distribution of values. As discussed in  \citet{2008ApJ...689...95M}, there is an apparent  lack of low luminosity Seyfert 1 galaxies in the [O~IV] and [Ne~III] distribution, but we find this difference not to be statistically significant, as shown by the K-S test results. Moreover, the sample presented in this work spans the same range on [O~IV] luminosities as the revised Shapley-Ames sample \citep{2009ApJ...698..623D}. The good agreement between Seyfert 1 and Seyfert 2  galaxies in the radio continuum and mid-infrared emission line  luminosity distributions demonstrates the isotropic properties of these quantities.

\begin{table*}
 \centering
 \begin{minipage}{140mm}
\caption{Statistical Comparison  Between Seyfert 1 and Seyfert 2 Galaxies\label{table2}
}
 \begin{tabular}{@{}lccccccc@{}}
  \hline
& \multicolumn{3}{c}{Seyfert 1}& \multicolumn{3}{c}{Seyfert 2}\\
 \cline{2-4} \cline{5-7}\\
 &  Measurements && Standard & Measurements &&Standard &${\rm P_{K-S}}$\\
 & Available & Median&Deviation &Available&Median&Deviation& (\%)\\
 \hline

{\rm  Log 8.4GHz/[O~IV]} &27&  -2.8  & 0.1  &55&  -2.6   &  0.1 &  8.2   \\
{\rm Log 8.4GHz/[Ne~III]} &27 & -2.6 &  0.1 &55 & -2.5 &  0.1 &  57.3 \\
{\rm Log 8.4GHz/[Ne~II]} & 27 & -2.5 & 0.1  & 55&  -2.6  & 0.1 &  81.6\\

${\rm L_{1.4GHz}}$ & 19  & 38.3 & 0.2 &36 &38.2 &0.1 & 86.8\\
${\rm L_{8.4GHz}}$ &27& 38.4& 0.2& 55  & 38.4& 0.1 & 82.0\\
${\rm L_{[O IV]}}$ & 29& 41.3  &0.1  &59  & 41.0& 0.1 &  27.8\\
${\rm L_{[Ne III]}}$ &29 &41.0& 0.1& 59 & 40.9  & 0.1 & 47.9 \\
${\rm L_{[Ne II]}}$ &29 & 40.9 &0.1 & 59& 41.0 & 0.1 & 96.9  \\

\hline
\end{tabular}
\medskip
Note: The last column, ${\rm P_{K-S}}$,  represents the Kolmogorov-Smirnov (K-S) test null probability. Upper limits for the  8.4~GHz fluxes are not included.
\end{minipage}
\end{table*}

\section{Mid-Infrared and the 8.4~GHz (3.6~cm) Emission}
In order to understand the different contributions to the radio core emission and its interaction with the narrow-line region in Seyfert galaxies we investigated  the  mid-infrared emission line and 8.4~GHz correlations. One should note that, due to redshift effects, luminosity-luminosity  plots will almost always show some correlation. Furthermore, caution must be taken when applying statistical analysis to data sets that contain non-detections (upper limits), or  ``censored" data
 points. In order to deal with these problems we used Astronomy SURVival analysis {\bf ASURV} Rev 1.2 \citep{1990BAAS...22..917I,1992BAAS...24..839L}, which implement the methods presented in  \citet{1986ApJ...306..490I}. We also used a test for partial correlation with censored data \citep{1996MNRAS.278..919A} in order to exclude the redshift effect in the correlations. A detailed comparison between the correlation coefficient for different  radio-to-mid-infrared correlations  is presented in Table~\ref{table3}.

\begin{table*}
 \centering
 \begin{minipage}{140mm}
\caption{Statistical Comparison of the   Relationships Between Radio and Mid-Infrared Emission Lines Luminosities for the  Sample\label{table3}}
 \begin{tabular}{@{}lccccccc@{}}
  \hline
$\log - \log$   & $\rho_s$& $P_\rho$&  $\tau$&  $P_\tau$& $\tau_p$& $\sigma$& $P_{\tau,p}$\\
 \hline

{\bf All The Sample}\\
8.4GHz-[O~IV]&0.66&$<1\times 10^{-6}$&0.50&$<1\times 10^{-6}$&0.35&0.08&$<1\times 10^{-6}$\\
8.4GHz-[Ne~III]&0.75&$<1\times 10^{-6}$&0.57&$<1\times 10^{-6}$&0.44&0.07&$<1\times 10^{-6}$\\
8.4GHz-[Ne~II]&0.74&$<1\times 10^{-6}$&0.54&$<1\times 10^{-6}$&0.40&0.06&$<1\times 10^{-6}$\\

{\bf AGN Dominated Sources}\\
8.4GHz-[O~IV]&0.76&$<1\times 10^{-6}$&0.58&$<1\times 10^{-6}$&0.46&0.09&$<1\times 10^{-6}$\\
8.4GHz-[Ne~III]&0.80&$<1\times 10^{-6}$&0.62&$<1\times 10^{-6}$&0.51&0.09&$<1\times 10^{-6}$\\
8.4GHz-[Ne~II]&0.82&$<1\times 10^{-6}$&0.64&$<1\times 10^{-6}$&0.53&0.09&$<1\times 10^{-6}$\\

{\bf Star Formation Dominated Sources}\\
8.4GHz-[O~IV]&0.59&$1.30\times 10^{-3}$&0.42&$5.00\times 10^{-4}$&0.22&0.12&$6.23\times 10^{-2}$\\
8.4GHz-[Ne~III]&0.68&$1.92\times 10^{-4}$&0.51&$2.80\times 10^{-5}$&0.32&0.12&$8.80\times 10^{-3}$\\
8.4GHz-[Ne~II]&0.64&$5.00\times 10^{-4}$&0.47&$1.00\times 10^{-4}$&0.30&0.11&$6.60\times 10^{-3}$\\

\hline
\end{tabular}
\medskip
Note:  $\rho_s$ is the Spearman rank order correlation coefficient with its associated null probability, $P_\rho$.
$\tau$ represents the generalized Kendall's correlation coefficient for censored data and $\tau_p$ is the  Kendall's  coefficient for partial correlation with censored data. $P_\tau$ and $P_{\tau,p}$ are the  null probabilities for the generalized and partial Kendall's correlation test, respectively. We also show the calculated variance, $\sigma$, for Kendall $\tau_p$. We have used a partial correlation test to exclude the effect of redshift (distance) in the luminosity-luminosity correlations.
\end{minipage}
\end{table*}

 We first considered the ratio between the radio continuum at 8.4~GHz ($L_{8.4GHz}$) and the [O~IV] emission line. The K-S test for this ratio returns a $\sim 8.2\%$ probability of the null hypothesis (see Table~\ref{table2}). Therefore, the radio emission relative to the power of the AGN, as measured by the [O~IV] emission,  is statistically similar in both Seyfert 1 and Seyfert 2 galaxies, suggesting the isotropic property of the radio emission \citep[e.g.,][]{2001MNRAS.325..737T,2009ApJ...698..623D}. This result is expected because the radio emission is expected to be unaffected by the  torus. When using the generalized Spearman correlation test to compare this ratio with the [O~IV] and 8.4~GHz luminosities we find no correlation with the [O~IV] luminosities  ($\rho_s=0.05;~P_\rho=0.64$) and a good correlation with the 8.GHz luminosity ($\rho_s=0.72;~P_\rho<1\times 10^{-6}$), see Figure~\ref{fig5_5}. These results suggest that the radio loudness of the source cannot be associated solely with  the strength of the AGN. In the following section we will elaborate on the implications of this result in view of  the link between radio loudness and the mass accretion rates for the AGN. From the  8.4GHz/[Ne~III] and 8.4GHz/[Ne~II] ratios we found that Seyfert 1 and Seyfert 2 galaxies also have statistically similar distributions. The K-S test returns a  57.3$\%$ and 81.6$\%$ probability of the null hypothesis for the  8.4GHz/[Ne~III] and 8.4GHz/[Ne~II] ratios, respectively (see Table~\ref{table2}). The 8.4GHz-to-mid-infrared ratios are presented in Table~\ref{table1}.

\begin{figure}
\includegraphics[width=84mm]{comp_ratio_8.4_o4_vs_o4_8.4.eps}
    \caption{Correlation between the  ratio {\rm $L_{8.4GHz}/L_{[O IV]}$} and the [O IV] and 8.4~GHz luminosities in Seyfert 1 ({\it circles}) and Seyfert 2 ({\it triangles}) galaxies. \label{fig5_5}}
\end{figure}

Because Seyfert~1 and Seyfert~2 galaxies have statistically similar radio emission, relative to the strength of the AGN, we   separated our sample in two new groups: 1) AGN  and 2) star formation dominated sources, by following our previous  study on the AGN and star formation contribution to the [Ne~II] emission line  \citep{2008ApJ...689...95M}. In this new scheme, sources with more than 50$\%$ contribution from the AGN to the [Ne~II] emission line are considered to be AGN dominated and sources with less than 50$\%$ contribution from the AGN to the [Ne~II] emission line, or alternatively, more than 50$\%$ contribution from stellar activity to the [Ne~II] emission  are star formation dominated. One must note that in active galaxies with strong star formation, the [O~IV] emission could be contaminated by the stellar activity, where the most likely contributor to the [O~IV] emission is from HII regions ionized by  Wolf-Rayet stars \citep[see][for discussion]{2009ApJ...704.1159H}. However, if we correct the [O~IV] emission for stellar contamination in star formation dominated sources, the resulting [O~IV]/[Ne~II] ratio will have even smaller values, thus reinforcing this quantitative classification. Moreover, sources that are well known to harbor massive star formation regions, such as NGC~3079 and NGC~6240 may have an additional complication because of contamination from the adjacent [Fe~II] $\lambda$25.99$\mu {\rm m}$ line from the [O~IV] in low-resolution  IRS spectra. Following the discussion  presented in  \citet{2008ApJ...682...94M} for NGC~3079, we estimated the  starburst contribution to be  $\sim 1.5$ times the uncontaminated [O~IV] emission; similar results are obtained  when comparing our fluxes with high-resolution spectroscopy for NGC~6240 \citep{2006ApJ...640..204A}. Nevertheless, these  extreme cases  have been classified correctly as star formation dominated sources. Moreover, a factor of $\sim 2$ in the [O~IV] flux  represents a dispersion of 0.3~dex, thus within the observed dispersion for the correlations presented in this study.

 From this new classification we found that, star formation and AGN dominated sources are statistically different in their radio emission relative to the AGN. The K-S test for the 8.4GHz/[O~IV] ratio returns a $\sim 0.1\%$ probability of the null hypothesis, i.e., indicating that  star formation and AGN dominated galaxies are from different populations. Figure~\ref{hist_1} shows  the distribution of values for the {\rm $L_{8.4GHz}/L_{[O IV]}$} ratio for Seyfert 1 and Seyfert 2 galaxies, as well as for AGN and star formation dominated sources, where  the differences in distributions can be clearly seen.  On the other hand, the K-S test returns a  11.9$\%$ and 10.2$\%$ probability of the null hypothesis for the  8.4GHz/[Ne~III] and 8.4GHz/[Ne~II] ratios, respectively (see Table~4). Table~4 also includes information about the numbers of AGN and star formation dominated sources, median values and standard deviations of the mean for the measured quantities. One must note that a high stellar contribution to the [Ne~II] emission, based on the [O~IV]/[Ne~II] ratio and typical of  star formation dominated sources, does not always translate into higher SFRs, but  could also indicate a relatively weak AGN \citep[see][]{2008ApJ...689...95M}.

\begin{figure}
\includegraphics[width=84mm]{histogram_r.eps}
    \caption{Comparison of the {\rm $L_{8.4GHz}/L_{[O IV]}$} ratio in Seyfert 1 and Seyfert 2 galaxies  and AGN and star formation dominated sources. This sample includes 53 AGN dominated  Seyfert galaxies and 29 star formation dominated sources for the  distributions. Upper limits for the  8.4~GHz fluxes are not included. The K-S test for these  ratios return  $\sim 8.2\%$ and $\sim 0.1\%$ probability of the null hypothesis between Seyfert 1 and Seyfert 2 galaxies and AGN and star formation dominated galaxies, respectively \label{hist_1}}
\end{figure}

\begin{table*}
 \centering
 \begin{minipage}{140mm}
\caption{Statistical Comparison Between AGN and Star Formation  Dominated Sources\label{table4}}
 \begin{tabular}{@{}lccccccc@{}}
  \hline
& \multicolumn{3}{c}{AGN Dominated }& \multicolumn{3}{c}{STAR Dominated}\\
 \cline{2-4} \cline{5-7}\\
 &  Measurements && Standard & Measurements &&Standard &${\rm P_{K-S}}$\\
 & Available & Median&Deviation &Available&Median&Deviation& (\%)\\
 \hline

{\rm  Log 8.4GHz/[O IV]} &53 &  -2.8  &  0.1  & 29&  -2.4 & 0.1   &  0.3   \\
{\rm Log 8.4GHz/[Ne III]} &53  &-2.7  &   0.1 & 29 & -2.4 &   0.1&   11.9 \\
{\rm Log 8.4GHz/[Ne II]} &  53 &  -2.5   & 0.1   & 29 &   -2.7  &  0.1& 10.2  \\

{\rm  Log 1.4GHz/[O IV]} &27 &  -3.0   &  0.1  & 16&  -2.5& 0.1   &  0.2   \\
{\rm Log 1.4GHz/[Ne III]} &27  &-2.8   &   0.1 & 16 & -2.4 &   0.1&   18.9 \\
{\rm Log 1.4GHz/[Ne II]} &  27 &  -2.8  & 0.1   & 16 &   -2.9  &  0.1& 12.3  \\

\hline
\end{tabular}
\medskip
Note: The last column, ${\rm P_{K-S}}$,  represents the Kolmogorov-Smirnov (K-S) test null probability.  Upper limits for the  8.4~GHz and 1.4~GHz fluxes are not included.
\end{minipage}
\end{table*}

\section{The Radio-to-Mid-Infrared radio loudness diagnostic}

 By looking at the mid-infrared and radio correlations in terms of the dominant source of  the [Ne~II] emission, we can  investigate on the relationship between the radio emission and the nuclear activity. Figures~\ref{fig1_3}-\ref{fig1_5} show the mid-infrared and 8.4~GHz luminosities with AGN and star formation dominated sources indicated.  In particular,  in the [O~IV]-8.4~GHz correlation, Figure~\ref{fig1_3}, the upper region of the plot ($>+\sigma$) contains only AGN dominated sources while star formation dominated sources tend to occupied the lower region ($<-\sigma$). Comparing Figures~\ref{fig1_3}-\ref{fig1_5} one must note how the clear separation between the two groups is lost when decreasing the ionization potential of the emission lines or, alternatively, when the emission line has a stronger starburst component, in agreement with the K-S test results. For the star formation dominated region, the [O~IV] underpredicts the observed 8.4~GHz emission. This suggest two possible scenarios: 1) star formation could enhance the 8.4~GHz emission and/or 2) the AGN in star formation dominated sources  is  more radio loud than estimated via standard radio-to-optical estimates.

\begin{figure*}
\vbox to 174mm{\vfil  \includegraphics[width=174mm]{o4_8.4.eps}
    \caption{Correlation between the [O~IV] and the 8.4~GHz emission. The circles represent the AGN dominated sources and the crosses  represent the star formation dominated sources. The solid line represents the linear regression for the whole sample and the dashed lines represent a $1-\sigma$ dispersion. \label{fig1_3}}
\vfil}
\end{figure*}

\begin{figure}
\includegraphics[width=84mm]{ne3_8.4.eps}
    \caption{Correlation between the [Ne~III] and the 8.4~GHz emission. The circles represent the AGN dominated sources and the crosses  represent the star formation dominated sources. The solid line represents the linear regression for the whole sample and the dashed lines represent a $1-\sigma$ dispersion \label{fig1_4}}
\end{figure}

\begin{figure}
\includegraphics[width=84mm]{ne2_8.4.eps}
    \caption{Correlation between the [Ne~II] and the 8.4~GHz emission.The circles represent the AGN dominated sources and the crosses  represent the star formation dominated sources.  The solid line represents the linear regression for the whole sample and the dashed lines represent a $1-\sigma$ dispersion\label{fig1_5}}
\end{figure}

 In order to determine  if  star formation activity  may contaminate the nuclear 8.4~GHz emission we proceed to estimate the 8.4~GHz emission associated with the star formation rates (SFR). For the SFR we adopted the values derived from  the stellar component of the [Ne~II] emission \citep{2008ApJ...689...95M}. Then  we used  the calibration found by  \citet{2006ApJ...643..173S} between the SFR and the 8.4~GHz emission. This calibration includes both the thermal and non-thermal SFR radio contribution (see Table~\ref{table5}). From this we found that the SFR overpredicts the observed 8.4~GHz luminosities in NGC~3982, NGC~5005 and MRK~897. This result is expected because the VLA in A configuration at 8.4~GHz sample a more compact region than that from the short-low and short-high resolution {\it Spitzer} slits, from which we extracted the [Ne~II] emission. Therefore, the 8.4~GHz emission derived from the [Ne~II] SFRs, represents an    upper limit for the star formation contribution, if any, to the radio emission at 8.4~GHz. On the other hand, the SFR underpredicts the 8.4~GHz emission for 6 out of 9 of the sources in the star formation dominated region. For these six sources, stellar activity cannot be solely responsible for the observed radio excess because it can only account for a contribution as little as $\sim 2\%$ and no greater than $\sim 40 \%$ of the observed flux, even when including the radio contribution from the extended star formation associated with the [Ne~II] emission. One must note that the estimated SFRs  represent a lower-limit as we neglect the stellar [Ne~III] contribution \citep[see][for discussion]{2008ApJ...689...95M}. However, all these sources have  weak [Ne~III], compared to the [Ne~II] emission, hence the SFR will not be significantly affected nor the estimates for the radio emission.

\begin{table}
\caption{Comparison between the observed and predicted 8.4~GHz luminosities for the sources in the star formation dominated  region\label{table5} }
 \begin{tabular}{@{}lll@{}}
  \hline
Name & Obs.& Pred.(SFR)\\
            &\multicolumn{2}{c}{Luminosity (${\rm W~Hz^{-1}}$)}\\
 \hline
IRAS01475-0740&22.96&21.38\\
MRK 897&21.73&22.02\\
NGC 2639&22.50&20.83\\
NGC 3079&21.44&21.02\\
NGC 3982&19.37&20.06\\
NGC 5005&20.27&20.44\\
NGC 5929&21.40&20.84\\
NGC 7213&22.14&20.66\\
UM 146&21.61&20.49\\

\hline
\end{tabular}
\medskip

Note: In order to estimate the predicted 8.4~GHz luminosities  we used the SFR values derived from  the stellar component of the [Ne~II] emission \citep{2008ApJ...689...95M}. We adopted the calibration found by  \citet{2006ApJ...643..173S} between the SFR and the 8.4~GHz emission.
\end{table}

 \citet{2002ApJ...564..120H} found an intriguing anticorrelation between the radio loudness of the galaxies, given by the radio-to-optical parameter, and the Eddington ratios, ${\rm L_{bol}/L_{Edd}}$, where $L_{bol}$ is the bolometric luminosity and $L_{Edd}$ is the Eddington luminosity\footnote{The Eddington luminosity is calculated as $1.26 \times 10^{38} M/M_\odot~{\rm erg~s^{-1}}$}. In general he found that galaxies with Eddington ratios $<10^{-5}$ are in the radio loud territory, while galaxies with Eddington ratios of $>1$ are in the radio quiet regime. In order to investigate this dichotomy    we  first need to estimate ${\rm L_{bol}}$. \citet{2004ApJ...613..109H}  first suggested that  the luminosity of [O~III]~5007\AA \ \ can be use as a proxy for the bolometric luminosity. In this regard, and by extending this analysis into the mid-infrared, \citet{2008ApJ...674L...9D} found that ${\rm L_{[O~IV]}}$ is related to  the 5100\AA \ \  continuum luminosity for a sample of reverberation-mapped AGN. From this and by using an estimate for the  correction between the bolometric luminosity and the optical luminosity, ${\rm L_{bol} \approx 9\lambda L_\lambda(5100)}$ \citep{2000ApJ...533..631K}, they determined  a scaling factor of 4500 between ${\rm L_{bol}}$ and  ${\rm L_{[O~IV]}}$ with a variance of 0.5~dex. Because [O~IV] is less sensitive to reddening corrections and  is less contaminated by star-forming regions, by  using ${\rm L_{[O~IV]}}$ as a bolometric luminosity indicator we can avoid the limitations of the ${\rm L_{[O~III]}}$ method. However, caution must be taken as for any of these methods the assumption is that the luminosity from narrow emission lines represents the same fraction of ${\rm L_{bol}}$ for all AGN. Moreover, the bolometric correction could be a function of the source luminosity and/or redshift \citep{2006A&A...453..525N}.

 In order to calculate the Eddington luminosity we searched the literature for  black hole (BH) masses, and found  81 BH masses for our radio sample. For the sake of uniformity, most of the values for the BH masses were calculated by using the relationship between the black hole mass and the stellar velocity dispersion found  by  \citet{2002ApJ...574..740T}, except when noted in Table~\ref{table1}. Previous studies have suggested  an uncertainty of 0.3~dex for the BH masses \citep[e.g.,][]{2002ApJ...564..120H}, however a more conservative uncertainty of 0.5~dex may be more appropriate for relatively low mass BH ($M_{BH}<10^7 M_\odot$). One must note that the range for the normalized accretion rate, ${\rm L_{bol}/L_{Edd}}$, in our sample is in agreement with the range of values found for the  radio quiet sources presented in  \citet{2002ApJ...564..120H}. The Eddington ratios, ${\rm L_{bol}/L_{Edd}}$,  are presented in Table~\ref{table1}.

In Figure~\ref{edd_ratio} we show that a number of  star formation dominated sources have smaller Eddington ratios in agreement with the radio excess observed in the star formation  dominated  region in the [O~IV]-8.4~GHz correlation. There is certainly a trend of  the Eddington ratios decreasing with increase radio loudness for star formation dominated sources, but  this correlation is  not statistically significant with this trend been dominated by the   sources  in the star formation dominated region. Also, there is an inherent scatter because of the uncertainties in the  BH mass estimate. Nevertheless, these results show  that star formation dominated sources with the bigger radio contribution, i.e., sources in the star formation dominated region, have smaller mass accretion rates. In this regard we also examined the dependence of the [O~IV] luminosity on black hole mass (see Figure~\ref{comp_o4_BHM}). From this comparison it can be seen that star formation dominated sources tend to have smaller accretion rates. Although the scatter is very large, there is a trend of $L_{[O IV]}$ increasing with $M_{BH}$.

\begin{figure}
\includegraphics[width=84mm]{comp_Edd.eps}
    \caption{Comparison between ${\rm L_{bol}/L_{Edd}}$ and ${\rm L_{8.4GHz}/L_{[O IV]}}$ as a proxy for the AGN radio loudness. The symbols are the same as in Figure~\ref{fig1_3}\label{edd_ratio}}
\end{figure}

\begin{figure}
\includegraphics[width=84mm]{comp_o4_BHM.eps}
    \caption{Dependence of [O~IV] luminosity on black hole mass. The solid and dashed lines represent different values for Eddington accretion rates.  The symbols are the same as in Figure~\ref{fig1_3}\label{comp_o4_BHM}}
\end{figure}

Using the radio-to-mid-infrared  ratio,  8.4GHz/[O~IV],   we found that star formation dominated sources are, on average, $\sim 2.8$ times more radio loud than AGN dominated sources (see Table~\ref{table4}). This ratio has the advantage of classifying galaxy radio loudness without star formation contamination and/or dust extinction in the determination of the optical luminosity. On the other hand, the galaxy radio loudness determined from the 8.4GHz/[Ne~III] and  8.4GHz/[Ne~II] ratios could be a closer match   to the historically  radio loudness parameter, $R$, because these  fine-structure lines of neon could be  affected by star formation contamination, especially in weak or low-luminous AGN. Moreover, in some AGN, the observed   [Ne~V]14.32~$\micron$/[Ne~V]24.32~$\micron$  ratio seems to fall below the low-density limit, implying a wavelength dependent extinction in the mid-infrared, with stronger extinction at shorter wavelengths \citep[e.g.,][]{2007ApJ...664...71D,2009MNRAS.398.1165G}, suggesting that [Ne~III] and  [Ne~II] could be more affected by dust extinction than [O~IV],  attributing  the   statistical differences between radio loudness in AGN and star formation dominated sources observed with  these ratios.

Overall, we found a good correlation between all the mid-infrared lines and the 8.4~GHz luminosities in AGN dominated sources.  On the other hand, the correlations for  star dominated sources seems to be strongly affected by the distance as these correlations are not statistically significant when using a partial correlation test with the effect of redshift excluded (see Table~\ref{table3}). These results suggest that the nuclear 8.4~GHz radio emission cannot be associated directly with the intrinsic power of the AGN, as measured with [O~IV], in sources that are dominated by star formation, or alternatively in low-luminosity AGN,  nor can it be associated with star formation emission, because the SFRs for most of these sources  underpredict the observed 8.4GHz luminosity (see Table~\ref{table5}). This may  argue in favor of an advection dominated accretion flow (ADAF) model   for the accretion disk \citep[e.g.,][]{1994ApJ...428L..13N}. In this model, the low accretion rates for the infalling material may never form a thin disk because of inefficient cooling, with the main  coolant process being cyclo-synchrotron emission, which result in a compact radio emission source that is faint in other wavelengths, providing an alternative to low-power jets models in radio quiet sources. The accretion rates for some   sources in the star formation dominated region are  sufficiently sub-Eddington to support the ADAFs accretion models,e.g.,  low-luminous sources with a bright nuclear radio emission (see Table~\ref{table1}).  Previous studies have suggested ADAF-type accretion flow models to explain the sub-Eddington accretion nature of  two of the more extreme sources  presented in this work, NGC~2639 and NGC~7213 \citep[e.g.,][]{2003ApJ...583..145T,2005MNRAS.356..727S}. Our results support  this scenario in light of the observed radio ``excess", compared to the intrinsic power of the AGN, as these  are the most  radio loud sources  in our sample (see Table~\ref{table1} and Figure~\ref{edd_ratio}). One may consider that star formation dominated sources could have a greater amount of fueling material in their nuclear regions, contrary to the ADAFs accretion models,  but as we have mentioned before, sources with higher star formation contributions to [Ne~II] do not necessarily have high SFR.

\begin{figure}
\includegraphics[width=84mm]{o4_1.4.eps}
    \caption{Correlation between the [O~IV] and the 1.4~GHz emission. The red diamonds represent the AGN dominated sources and the blue squares represent the star formation dominated sources. The solid line represents the linear regression for the whole sample and the dashed lines represent a $1-\sigma$ dispersion\label{fig2_1}}
\end{figure}

Finally, we  compared  the  radio-to-mid-infrared parameter by using VLA B-configuration radio flux densities  at 1.4~GHz and the mid-infrared emission lines, between AGN and star formation dominated sources. As we mentioned before,  to estimate the radio contribution from the AGN one needs to use high angular resolution data, which are less contaminated by star formation from  the host galaxy, except for the nuclear stellar activity. However, caution must been taken because  at 1.4~GHz the region sampled by the VLA B-configuration could be contaminated by star formation in the circumnuclear region (within the inner few kpc). However, when comparing the shape of the SED between  1.4~GHz and 8.4~GHz emission we found that  the K-S test for the spectral indices distribution, between AGN and star formation dominated sources,  returns a $\sim 51.1\%$ probability of the null hypothesis. This result suggest that stellar activity is not the leading effect that drives the radio core  correlation, as we found previously with the 8.4~GHz emission or, in other words, the high-resolution radio images at 1.4~GHz and 8.4~GHz are, on average,  dominated by the active nuclei. Moreover, \citet{2008ApJ...682...94M} suggested that because its high ionization potential the [O~IV] emission is well within the Spitzer aperture on scales of less than a few hundreds of parsecs, typical of the NLR. From  the 1.4GHz/[O~IV] ratios  we  found that star formation and AGN dominated sources are statistically different in their radio loudness. The K-S test for this ratio returns a $\sim 0.2\%$ probability of the null hypothesis with star formation dominated sources more radio loud by a factor $\sim 3$ than AGN dominated sources, in close agreement with our previous finding using the radio core emission at 8.4~GHz. On the other hand, the K-S test returns a  18.9$\%$ and 12.3$\%$ probability of the null hypothesis for the  1.4GHz/[Ne~III] and 1.4GHz/[Ne~II] ratios, respectively (see Table~4). These results corroborate our assumption that the [O~IV] emission is a true indicator of the AGN power, as the [Ne~II] and [Ne~III] emission could have a strong starburst component in weak AGN. Figure~\ref{fig2_1} shows the 1.4GHz-[O~IV] correlation, where one  can see the  separation between AGN and star formation dominated sources, in agreement with the K-S test results and  despite the smaller sample because of the  limited number of high-resolution observations.

\section{Conclusions}
We have investigated the relationship between the radio emission and the ionization state of the emission-line gas in Seyfert galaxies with the aim to understand the connection between the radio loudness and the  ionizing luminosities of the AGN. We used the [O~IV] emission line  to estimate the intrinsic power of the AGN and high-resolution 8.4~GHz emission to characterize the radio core power. From this we defined a radio-to-mid-infrared parameter, 8.4GHz/[O~IV], to identify the radio contribution from the Seyfert nuclei. We found that Seyfert 1 and Seyfert 2  galaxies are statistically similar in their radio emission, relative to the  strength of the AGN. On the other hand, when separated  by  the dominant source of [Ne~II] emission, we found that two groups, AGN and star formation dominated sources, are statistically different in their radio loudness.  We found that sources with strong star formation, relative to the strength of the AGN, or alternatively weak AGNs,  tend to be more radio loud, by a factor of $\sim 2.8$, than AGN dominated sources. Furthermore, in the 8.4GHz-[O~IV] correlation,  sources in the star formation dominated region have lower mass accretion rates than the rest of the sample. This result is in agreement with the anticorrelation found by  \citet{2002ApJ...564..120H} between the radio loudness and Eddington accretion rates. Given the sub-Eddington nature of the more radio loud sources in our sample, sources in the star formation dominated region, one  can invoke advection-dominated accretion  models  to explain their bright compact radio emission and a low-luminous nucleus both consistent with their high radio-to-mid-infrared parameter.

 We also found that high resolution 1.4~GHz emission could also be used as a reasonable proxy for the AGN radio contribution. When using the 1.4GHz/[O~IV] ratios we found that sources in which the [Ne~II] emission is dominated by the stellar activity, or alternatively weak AGNs,  tend to be more radio loud, by a factor of $\sim 3.0$, than AGN dominated sources, in close agreement with the radio loudness characterization using the radio core power at 8.4GHz. When comparing the observed 8.4~GHz and 1.4~GHz high-resolution core emission in our sample of Seyfert galaxies we found a strong  linear correlation, suggesting that the core radio emission is dominated by the active nuclei with a spectral index of $f_\nu \propto \nu^{-0.7}$. We found  the spectral index distribution, between 1.4~GHz and 8.4~GHz, for Seyfert 1 and Seyfert 2 galaxies and for AGN and star formation dominated sources to be statistically similar within the groups.

We suggest that the radio-to-optical parameter, $R$, used to classify  galaxy radio loudness may erroneously quantize  the radio contribution in galaxies with strong star formation or alternatively, weak AGNs, in which the optical luminosity may be contaminated by star formation and/or suffer from dust extinction. Instead, we found that a radio-to-mid-infrared parameter, 8.4GHz/[O~IV], is a better probe for the radio loudness of the galaxy,  as it is basically  unaffected by star formation contamination and is less affected by extinction than optically dependent  diagnostics.

\section*{Acknowledgments}
We thank the referee for a very useful comments that improved
the paper. We would also like to acknowledge  D.M. Crenshaw for valuable comments on the work. This research has made use of NASA's Astrophysics Data System. Also, this research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory,
California Institute of Technology, under contract with the National Aeronautics and Space Administration. The VLA is operated by the US National Radio Astronomy Observatory which is operated by Associated
Universities, Inc., under cooperative agreement with the National Science Foundation. SMART was developed by the IRS Team at Cornell University and is available through the Spitzer Science Center at Caltech. Basic research in astronomy at the NRL is supported by 6.1 base funding.

\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


text:
EU launches conference to debate its future with citizens
PARIS — French President Emmanuel Macron on Sunday expressed hope that Europe would rediscover the path of "great projects, great ambitions and great dreams" as the European Union launched a wide consultation process meant to design the shape of the bloc's future.
Macron spoke as part of Europe Day, the inaugural event of the Conference on the Future of Europe in the French city of Strasbourg.
"What Europe do we want in 10 years, 15 years from now?," Macron asked in his opening speech, calling on people to debate all major issues, from the bloc's borders to new institutions, cultural projects, education and the fight against climate change.
The process also aims at bringing the EU's complex decision-making closer to its 450 million citizens.
While advocating for Europe's democratic model, based on solidarity, Macron acknowledged that "we've seen that sometimes Europe didn't go fast enough and maybe didn't have enough ambition."
He called on Europeans to get inspired by the United States to rediscover ways to "shape the future and move fast."
The pandemic has shown that the EU lacked the effective tools to react quickly to a continent-wide emergency. The bloc was notably criticized at the beginning of the year for its vaccination campaign starting slower compared to the U.S. and the United Kingdom.
"The pandemic has been traumatic … and like all trauma we need to find a way of talk about it if we want to move beyond it," European Commission President Ursula von der Leyen said. "And there's no better way to do that than by offering prospective, hope and the ability to change things for the better."
The process is meant to allow "young people in particular to have their say" about Europe's future, she said.
A digital platform and series of conference-related events will enable people to share their views on changes and improvements they wish for the EU.
The conference's plenary will be composed of representatives from the European Parliament, member states, the European Commission, as well as representatives from all national parliaments, social partners, the civil society and panels of citizens.
European Parliament President David Sassoli said "as we are about to rebuild our economies and our societies on new foundations … it is even more crucial and urgent to listen to our fellow citizens, to feel their needs, their expectations in terms of assistance, jobs, dignity, security and prosperity."
The conference is expected to reach conclusions to provide guidance on the future of Europe by spring 2022.
Meanwhile, Macron hoped the European Parliament will be able to hold its next plenary session in June in Strasbourg, its official seat. European lawmakers didn't return to the French city since February last year because of the virus crisis.
France government

redpajama_set_name: RedPajamaCommonCrawl


text:
High Court of Gujarat Driver Result, Answer Key & Question Paper 2021
High Court of Gujarat has published an Advertisement for the below-mentioned Posts. Eligible Candidates advised to refer to the official advertisement and apply for this post. You can find other details like age limit, educational qualification, selection process, application fee, and how to apply are given below.
C Recruitment 2020 Job Details:
Advertisement No.: RC/B.1304/2020
Posts: Driver
Please read Official Notification for Educational Qualification details.
Candidates have to pay Rs. /- + Charges through challan.
Candidates will be selected based on competitive written exam & computer proficiency test.
How to Apply ?:
Interested Candidates may Apply Online Through the official Website.
Starting Date of Online Application: 17-03-2021
High Court of Gujarat Driver Call Letter 2021 Out
Posts Name: Driver [No.RC/B.1304/2020(Driver)-86/202021]
Elimination Test (Objective Type-MCQs) Date: 26-09-2021
Shortlisted candidates for Driving/Skill Test: Click Here
Download Answer Key: Click here
High Court Of Gujarat Driver Question Paper 2021: Download Here
More Details: Click Here
Gujarat High Court Recruitment 2021 Free Job alert for both Fresher and Experienced Candidates updated on March 10, 2021. Get a Direct Official Link for applying for Gujarat High Court Recruitment 2021 along with the current Gujarat High Court Recruitment official Notification 2021 here. Find all recent Gujarat High Court Vacancies 2021 across India and check all the latest Gujarat High Court 2021 job openings instantly here, Know upcoming Gujarat High Court Recruitment 2021 immediately here.
The Gujarat High Court is the High Court of the state of Gujarat. This high court was established on 1 May 1960 as a result of the bifurcation of the former State of Bombay into two States of Maharashtra and Gujarat. The High Court started functioning near Akashwani, Navrangpura, Ahmedabad. The High Court has later shifted to the new building at Sola, Ahmedabad, from 16 January 1999. The Gujarat High Court has jurisdiction over the entire state of Gujarat. It has jurisdiction over all district, administrative and other courts in Gujarat. This high court is a Court of record and empowered to punish anyone for contempt of court.


text:
ABOUT ARTIST
VIP ART INVESTMENT
YAROSLAV LEVCHENKO
Artwork can be precious not just because it resists through the years, but also because it has owned it's value since its birth.
Miraslav Gornichek
Yaroslav Levchenko's ambitious paintings seduce, repel, surprise, and puzzle. His masterful technique is achieved through the scrutiny and emulation of the compositional devices, graphic rhythms and refined surfaces of sixteenth and seventeenth century Northern European paintings, while his subjects exist at odds with the popular dialogue and politics of contemporary art. Consistent throughout his oeuvre is his search for the point at which the beautiful and the grotesque are held in perfect balance.Yaroslav Levchnko (b.1987, USSR) received his PHD from the Academy of Fine Arts in Saint-Petersburg. He lives and works in Athens Greece. Levchenko's work is represented in museum collections worldwide, including the State Hermitage Museum. Major museum exhibitions include "Yaroslav Levchenko: CHRISTMAS SUITE," State Complex "Palace of Congress, Saint-Petersburg, Russia (2010); "Yaroslav Levchenko: ITALIAN CYCLE," State Hermitage Museum (2011); "Yaroslav Levchenko: TOTALLY CONTEMPO/CONTEMPORARY ANATOMY" Vyborg Castle State Museum (2011/2014); and "Yaroslav Levchenko: SACRED ESSENCE," Kiev National Museum of Russian Art (2015).
Mikhail Anikin*
* Art critic and main partner of St Petersburg's Hermitage, specialized in Italian art and,
in particular, in Leonardo da Vinci's painting.
ART INVESTMENT
COPYRIGHT © YAROSLAV LEVCHENKO 2015. Please do not reproduce without the expressed written consent of Yaroslav Levchenko.by levgallery.com


text:
#0021: Willa Cather to Mariel C. Gere, Ellen B. Gere, Frances C. Gere, Mary Ames, and Althea Roberts, January 2, 1896
Siberia2
Jan 2/96 Mariel3,
Ellen5,
Frances6,
Allie7,
and Maysie8;
My Dear Push9,
I address you thus in a bunch because I dare not address Mariel singly as I do not feel equal to discussing Love and Live and Death and Alvary10 and German opera11 with her by mail. My spirit is willing but my pen is weak12. When I see her I will consent to talk it however. I wonder if it would diminish Mariel's adoration to know that all Alvary's real name is Max Achenbach and that he has nine charming little Achenbachs and a Frau who weighs three hundred.
I had a fine time in Beatrice13, the fascinating Katharine14 is just as fascinating as ever and Bertie's15 charms grow apace. He and I used to sit around and quote Ella Wheeler Wilcox16 untilltil we wellnigh drove Katharine crazy. He was very nice and I dont blame Katharine for liking him, I do and he is not my brother either.
Well, girls, I must tell you about a New Year's dance Douglas17 and I went to last night. Douglas made me go, for about sixteen girls wanted him and expected him to ask them and he thought it would be nice to make them all furious. He sent to Lincoln4 for a lot of flowers for me and so on and I really had to go with them. And of all rough-house affairs, of all cake walks! The hall was big and the floor might have been good, but they had the floor heaped with shavings and chunks of wax, chunks which you had to leap and mount and clamber over with an alpenstock. For seats they had big rough planks on resting on chairs. The boys and girls had the same dressing room. The refreshments consisted of ice water in a wooden pail, coffee and ham sandwitches which they passed in a bushel basket, a potato basket. But this is only the setting, the environment, the dance was the thing! The men caught your arm just as high as your sleeve would permit, fortunately they could not get up any farther than my elbow, and they hugged you like ten thousand Oury18s. I had a terrible feeling that they were likely to lay hands upon my bare neck at any moment and wished for a high neck. yet this The men fell down every now and then and you had to help them up. Yet this was a dance of the elite and bon ton of Red Cloud2. Mary19 and Margie20 and Hughie21 and my fair cousin22 were there. One thing was a comfort, Douglas did splendidly and he certainly was the most civilized looking object in the crowd.
Say girls, you remember our handsome preacher Putnam23 whose bible Maril3 returned two years go, well he is pastor of the First Christian Church of Denver24 now. He was in town yesterday and he is better looking than ever.
I suppose poor Ned5 and Frances6 are getting the best out of their vacation ere their period of servitude begins again. Smile sweetly on Mr. Oury for me, Neddy. I send him some literature on Virginia25 today. Have you heard any th thing from John Charles26 or from the sister of John Charles?
Say Mariel, I am going to ask a favor of you and if you hate to do it, why just dont. Sarah Harris27 has a little book of mine, "Sapho28", by Alphonse Daudet29, which I am very fond of as it is illustrated by Rossi30 and every picture is a whole French novel. Now considering the existing relations it would be snippy of me to write and demand it from Sarah, and alas I know too well her habit of forgetting to return things. Would you please tell her sometime that you want to read it and I asked told you to ask her for it? I really want the thing awfully and I dont want to ask Mrs. Imhoff31 to get it for me as I am afraid it the book might corrupt her morals or dispel her illusions or something, but you see I have confidence in Mariel.
I dont know when I will appear in Lincoln next, nor do I much care. One of the charms of the Province32 is that one gets indifferend toward everything, even suicide. "Then think of me as one already dead, and laid withing the the bottom of a tomb." Please let me know the university and "social" news from time to time, you know I really am interested in all those complicated matters. When you next see "all my friends" give them my love, unqualified and unmodified.
Farewell, O Maids,
"And when like her, O Saki! you shall pass, Among the guests star scattered on the grass, And reach the spot where I myself made one, Forget me33 and turn down an empty glass."
Thats poetry34, I quote it to Jack35 and the cats now that I have not Allie and Bert Weston anymore.
Farewell all of ye Willa
Love to your Papa36 & Mamma37.
Miss Mariel Gere3 D & 9th Str Lincoln4 Neb. RED CLOUD NEBR.2 2 JAN 1896 8 PM Jan 3 1896Letter to the push LINCOLN N4 JAN 3 830 AM
Document is six leaves, handwritten on recto and verso of each leaf. Includes one envelope, handwritten.
Mariel C. Gere, Ellen B. Gere, Frances C. Gere, Mary Ames, and Althea Roberts1
Red Cloud, Nebraska, United States2
Cather's nickname for her college friends, including the Gere sisters, Allie Roberts, and Maysie Ames.
The Damrosch Opera Company performed in Omaha December 26 to 28, 1895.
Matthew 26:41 reads, "for the spirit indeed is willing, but the flesh is weak."
Cather's nickname for Red Cloud, NE.
Cather misquotes the third line of Edward Fitzgerald's 1879 version of the last quatrain and adds the phrase "Forget me."
Gere, Ellen Bladen (1875-1941) ("Ned" or "Neddums"). Cather's friend. Ellen Gere, the second daughter of Charles H. and Mariel C. Gere, was born in Lincoln, NE. She visited Cather in Red Cloud, NE, with her sisters, and Cather included her in her correspondence in the 1890s. Ellen Gere entered the University of Nebraska in Lincoln around 1892, but graduated with the class of 1899. In the 1920s she adopted two children, believing, with her friend Dorothy Canfield, that women who wanted to be mothers did not have to be married.
Gere, Frances C. (1877-1965). Cather's friend. Frances Gere, the youngest child of Charles H. and Mariel C. Gere, was born in Lincoln, NE. She entered the University of Nebraska in 1894 and graduated in 1898. Like her sisters, Mariel and Ellen, she joined the Kappa Kappa Gamma sorority and lived in Lincoln the remainder of her life.
Haggard, Althea B. Roberts (1874-1960) ("Allie"). Cather's university friend. Althea Roberts was the second of the four daughters of Aurelius and Lizzie Roberts of Rising City, NE. She entered the University of Nebraska in Lincoln in 1890, joined the Kappa Gamma sorority, and graduated with Willa Cather in the class of 1895. She married Corwin R. Haggard around 1897; their first child, born in 1897, died in infancy. The couple moved to Tulsa, OK, after 1910, where they were still living in 1940.
Ames, Mary ("Maysie," "Mayzie") Henderson (1874-mid 1920s). Friend and classmate of Cather; librarian. Maysie Ames was born in Illinois to John A. and Elizabeth Ames. The family moved to Lincoln, NE, in the early 1880s; by 1891 they were living at 1020 H Street, across the street from Cather's rooming-house at 1019 H. Ames and Cather were both members of the Union Literary Society from their first year at the University of Nebraska, and she was part of the circle of friends that included Cather, the Geres, the Broadys, Althea Roberts, and Olivia Pound. Ames became a member of the Fem Bot, the women students' answer to Roscoe Pound and the Sem Bot, the all-male Botanical Seminar. She and classmates Flora Bullock and Mariel Gere were among the first students in the library cataloging courses offered by university librarians Mary L. Jones and Mary Esther Robbins in 1895, and she became assistant librarian at the university, with special responsibility for the engineering and scientific books. She resigned in 1904 to become librarian of the Grand Island city library from 1905-1909. By 1923 the university's alumni association had lost touch with her, although she was reported as deceased in their 1927 alumni directory.
Alvary, Max (1856-1898). German opera singer. Born Maximilian Achenbach in Germany, Max Alvary performed as a tenor in Wagnerian opera in Germany, England, and the United States. He was a member of the Damrosch Opera Company when it performed in Omaha in December 1895; Willa Cather did not attend any of these performances.
Wing, Katherine Weston (1871-1903) ("Kit"). Cather's friend. Born in Nebraska, Katherine was the third of four children born to J.B. and Helen Weston, who became well-to-do residents of Beatrice, NE, thirty miles south of Lincoln, NE. She entered the University of Nebraska in 1887, but withdrew for several years due to poor health. When she returned in 1891, she met Cather. She visited Cather in Red Cloud in the summers of 1891, 1894, and 1895, and Cather visited Weston in Beatrice in June, July, and December 1895, where Cather also enjoyed the company of Katherine's younger brother Herbert (Bert). Katherine attended the library school of the University of Illinois as a member of the class of 1898 but withdrew in 1897. She then remained at home until her June 1902 marriage to Thomas E. Wing, a fellow 1894 University of Nebraska graduate. She moved with him to Scarsdale, NY, where she died of pneumonia in 1903.
Weston, Herbert Towle (1876-1951) ("Bert"). Cather's Nebraska acquaintance. Born in Lincoln, NE, Bert Weston was raised in Beatrice, NE, by his father, J.B. Weston, one of the town's founding settlers and most prominent citizens, and mother Helen Towle Weston. His sister Katherine was Cather's University of Nebraska classmate, and Cather met Bert when she visited her friend in Beatrice. After graduating from Beatrice High School, Bert Weston's parents sent him to the Michigan Military Academy in Orchard Lake, MI, in 1893. After graduating from MMA in 1895, Weston was admitted to the Sheffield Scientific School at Yale University. In 1898 he joined the First Connecticut Light Infantry in hopes of fighting in the Spanish-American War but never saw action. He returned to Beatrice at the war's end and married Margaret Collins of Brooklyn, NY, in 1903. They raised three sons in Beatrice, where Bert worked for the family business, the Beatrice National Bank, established his own business, Nebraska Corn Mills, and managed the Western business interests of his wife's family.
Wilcox, Ella Wheeler (1850-1919). American poet. Born in Wisconsin, Ella Wheeler began writing poetry at an early age; her poems were published in newspapers, earning her a state-wide reputation while in her teens. Her Drops of Water (1872), a book of temperance poems, and Maurine (1875) appeared before her first great success, Poems of Passion (1883). Attacks on the supposed immorality of that volume and ridicule of its naïve versification and sentiments were almost as widespread as its popularity, with Cather being among the scoffers. Wheeler married Robert Wilcox in 1884; they had one child, who died at birth. She continued to publish prolifically; as she became interested in theosophy and spiritualism, she also wrote on those topics.
Cather, Charles Douglas (1880-1938) ("Douglass"). Cather's brother. Born in Virginia and raised in Red Cloud, NE, Charles was third child and second son of Charles and Virginia Cather. As an adolescent, Douglass Cather helped his father supervise rented farm properties and worked as a messenger for the local Burlington & Missouri Railroad office. In 1897 he left Red Cloud for a position in Sterling, CO, and then took a position with at the Cheyenne, WY, office of the Burlington Railroad. In 1908 he traveled to Mexico, an experience that his sister gave to Emil Bergson in O Pioneers! (1913). By 1910 he was living in Winslow, AZ, still working for the Burlington, where Willa Cather visited him in 1912. He later achieved success in the oil business in California. Although he never married, Cather notes that during the last six or seven years of his life he had a relationship with Dorothy Rogers. Douglass visited Cather in New York City in December of 1937. His death in June 1938 left her devastated. Douglass served as a prototype for one of the twin brothers in the Templeton family in "Old Mrs. Harris" (1932) and Hector the messenger boy brother in "The Best Years" (1948). His years working for the Burlington also inspired Cather's many railroad worker characters in her novels, including Song of the Lark (1915) and The Professor's House (1925). Few letters from this important sibling relationship have survived.
Oury, William H. (1872-after 1939). American Army officer. Born in Virginia, Oury graduated from the University of Nebraska in 1897. While there he played on the football team and with William and Louis Westerman was a member of Phi Delta Theta. In his senior year a humorous table of the attributes of class members noted that his deficiency was "Girls," although Cather's references to him suggest he pursued girls somewhat aggressively. A captain of Company A of the university's cadet corps, he joined the U.S. Army after graduation, serving as a captain in the Spanish American War and as a colonel under his college cadet commander, General John J. Pershing in World War I. From 1930 to 1939 he was commandant of cadets at the University of Nebraska.
Creighton, Mary S. Miner (1873-1968). Clubwoman; Cather's friend from childhood. Born in Iowa, Mary Miner was the second daughter of James and Julia Miner, neighbors of the Cather family in Red Cloud, NE. Willa Cather later recalled that when she first moved into town with her family and enrolled in school in 1885, "Margie Miner was so jolly I wanted awfully to know her." They became lifelong friends and correspondents, and Mary's sisters Irene and Carrie were equally close to Cather. Mary Miner wed local physician E. A. Creighton in 1900 and lived the rest of her life in Red Cloud. She was the prototype for Julia Harling in My Ántonia (1918).
Gund, Margaret Miner (1875-1936). Cather's childhood friend; iris breeder. Born in Iowa, the third surviving daughter of James L. and Julia Erickson Miner, Margaret grew up in Red Cloud, NE, where she was one of Cather's close friends. She played the role of Beauty in the children's play Beauty and the Beast in 1888, while Cather played the merchant, her father; she also sang and played the violin in various local musical performances. In 1896 she met bank cashier Frederick Gund at a dance in Blue Hill, NE; they were married in December 1900. The couple lived in Blue Hill, where their four children were born and she cultivated iris plants. When the bank closed in 1932, the couple—their children grown—moved to Crawford, NE. Margaret Miner Gund died in Chicago, IL, and is buried in Lincoln, NE. Cather portrayed her as Sally Harling, the tomboy, in My Ántonia (1918).
Miner, Charles Hugh (1871-1954) ("Hugh," "Hughie"). Red Cloud businessman and postmaster. Born in Iowa, eldest and only surviving son of James L. and Julia Erickson Miner, Charles Hugh Miner was named for his uncle Hugh Miner and came with his family to Red Cloud, NE, in 1878. Hugh was educated in Red Cloud and at a business college in Notre Dame, IN. He married Cather's cousin Alfretta "Retta" Ayre in 1896, and they had four children, Jennie, Margaret, James, and Charles Hugh. In 1917 Hugh sold the Miner Bros. store and concentrated on farming and ranching. In 1936 he was appointed postmaster of Red Cloud. Cather portrayed the Miner family in My Ántonia (1918) as the Harlings, whose only son is Charley Harling.
Miner, Alfaretta Ayre (1874-1951) ("Retta"). Cather's cousin. Retta Ayre was born in Virginia, daughter of John and Jennie Cather Ayre. Orphaned at a young age, Retta and another cousin, Kyd Clutter, made their homes with grandparents William and Caroline Cather in Red Cloud, NE. Retta married Charles Hugh Miner in 1896; Willa Cather arranged the wedding breakfast. The couple had four children. When her grandmother died in 1900, Retta Ayre Miner inherited much of her estate, and later bought more land near Trenton, NE.
Putnam, Melvin (1869-1937). Canadian-American minister. Born in Ontario, Canada, Melvin Putnam came to the United States in 1888. In 1890 he married Lillian Miller; their one son, Glen Putnam, was born in Ohio in 1891. Melvin Putnam became a minister of the Christian Church, serving the congregation in Red Cloud, NE, in 1893-94, where Willa Cather and some of her friends knew him. Later he served in churches in Colorado, Utah, Missouri, Oklahoma, Washington, and Oregon, where he died.
John Charles. No further information is available about this person.
Dorris, Sarah Harris (1862-1918). American newspaper editor. Born in Massachusetts, Sarah came to Lincoln, NE, in 1870 with her parents, railroad land agent George B. Harris and his wife Sarah. She graduated from the University of Nebraska in 1888. After several years in Lincoln's social scene, she became associated with the Lincoln Courier, a weekly newspaper. Cather, who knew Harris socially, was briefly Harris's coeditor in the fall of 1895. After Cather moved to Pittsburgh, PA, in 1896, she contributed reviews, columns, and stories to the Courier, and she stopped in Lincoln to visit Harris occasionally on her way to and from Red Cloud. In August 1903, Cather met Edith Lewis, who also wrote for the Courier, at Harris's house. Sarah Harris married retired surgeon Alvah H. Dorris in 1907, several years after she sold the newspaper.
Daudet, Alphonse (1840-1897). French writer. Born in Nîmes in the south of France. Daudet was educated in Lyon. He taught briefly before joining his elder brother in Paris in 1857, where he worked as a journalist while writing poetry and plays. His Letters from My Windmill (1866), set in Provence, established his literary career. Other important works were the Tatarin books, Artists' Wives (1874), Kings in Exile (1879), Sapho (1884), and a play, The Arlesienne Girl (1872), for which Georges Bizet wrote the incidental music. Daudet married writer Julia Allard in 1867; like Baudelaire and Manet, he suffered from syphilis. Cather refers to Daudet frequently in her newspaper criticism, and in 1891 Cather and her female friends in Lincoln, NE, were sharing a copy of Daudet's scandalous novel Sapho (1884); in "Coming Aphrodite" (1920), Cather has Eden Bower read the same book as a teenager in Illinois.
Rossi, Luigi (1853–1923). Swiss painter. Born in Cassarate, Switzerland, Luigi Rossi studied at the Brera Academy of Fine Arts in Milan, Italy, under the tutelage of Giuseppe Bertini. From 1885 to 1888 Rossi lived in Paris, France, painting and illustrating works by Alphonse Daudet, Pierre Loti, and others.
Imhoff, Grace Douglas (1860-1945). Cather's Lincoln acquaintance. Born in New York, Grace and her family moved to Iowa in the late 1860s; in the 1870s, she moved to Lincoln, NE, living with her sister Elizabeth Douglas Raymond. She attended Lincoln High School, where she met her future husband, Charles Hudson Imhoff. They married in 1887 and had three children. After her husband's bank closed in the 1890s, the family moved to New Jersey in 1899. She was widowed in 1929, and moved to Long Beach, CA, where she died. According to Grace's sister-in-law, Mary Baird Raymond, the two women took fiction-writing lessons from Cather in the 1890s.
Cather, John (1892-1959) ("Jack"). Cather's brother. Born and raised in Red Cloud, NE, Jack was the seventh child and fourth son of Charles and Virginia Cather. He was nearly two decades younger than Willa Cather, and she was a doting older sister when he was a small boy. Because she missed him after her 1896 move to Pittsburgh, PA, she wrote several poems about him and the story "Jack-a-Boy" (1901). After graduating from Red Cloud High School in 1912, Jack studied for two years at University of Nebraska in Lincoln. With Willa Cather's encouragement, in 1914 he enrolled at the Carnegie Institute of Technology in Pittsburgh to study engineering. Willa Cather was then living in New York City but traveled to Pittsburgh to help him settle in and enjoyed visiting him and supported his decision to change his major to theater. It is not clear whether he graduated from Carnegie Tech but the British government trained him as a chemist so he could inspect munitions factories. While working in Smethport, PA, he met Irma Wells, and they married in 1918. They had two children, Catherine and Ella Faye. After World War I, he worked as a chemical engineer in the oil industry in Cincinnati, OH, Casper, WY, and Bradford, PA. In 1936 he moved to Whittier, CA, and became a business partner with his brothers Douglass and James in an oil production company. He died in Long Beach, CA. Willa Cather mentions him frequently in letters, but she seems to have had little contact with him and his family in later years, and no letters from her to him have surfaced.
Gere, Charles Henry (1838-1904). Newspaper publisher; Cather's employer during college. Charles H. Gere, born in New York, graduated from Dickinson College in Carlisle, PA, in 1861 and joined the Union army. In 1865 he moved to Nebraska, where his family had moved. Politically active in the Republican Party, he moved to Lincoln, NE, and founded the city's first newspaper, the Nebraska State Journal. He married Mariel E. Clapham of Washington, D.C., in 1871. While serving as a representative in the first state legislature, he helped found the University of Nebraska, for which he served as regent from 1882 to 1892. Cather wrote for his newspaper when she was a university student, and became a friend of Charles and Mariel Gere's three daughters, Mariel, Ellen, and Frances. She remembered Charles Gere's "kindness, his easy wit, the ease and charm of his personality."
Gere, Mariel E. Clapham (1838-1912). Cather's friend; mother of her friends, the Gere sisters. Mariel Elizabeth Clapham was born in Washington, D.C., the daughter of Captain John Clapham and Mariel Goodwin Clapham. She corresponded with Charles Gere for several years before their marriage in 1871, when she came to Lincoln, NE. When Cather became friends with their daughters Mariel, Ellen, and Frances, she welcomed her to their home at 8th and D streets. Mrs. Gere, according to Cather, persuaded her to grow out her close-cropped hair.
Red Cloud, Nebraska, United States
Lincoln, Nebraska, United States
Beatrice, Nebraska, United States
Virginia, United States
Sapho (1884) by Alphonse Daudet
Rubáiyát of Omar Khayyám (1859) by Edward FitzGerald


A versatile, stylish, and exceptional piece of furniture, the Calvin Heights XL sectional brings a classic contemporary feel that has just the right amount of upscale elegance. Covered in durable Microfiber that offers comfortable, deep seating for you and your guests, the bold slate color lends fantastic eye appeal. Perfect for larger spaces, this expansive sectional can comfortably seat your whole family and easily turns your living area or den into the perfect place to mingle with guests and friends.. Quality constructed on a hardwood frame for strength and stability, the sinuous wire seating system provides additional support for an enduring and solid foundation. Premium design features such as welting details, track arms, and elegant tufting on the bench-style seat cushions maintain a tailored silhouette and afford a long life and beautiful appearance. Matching pillows and bold, free-flowing wave patterned pillows included.


I'm still reeling from the beauty of our tiny holiday to Ponza. You know how it goes: you're sitting in a bar, or maybe a restaurant, with friends. It's an early summer evening, but that back-note of Rome's high summer mugginess is already beginning to wisp tendrils round your neck, presaging the hot soupy air of dog days and August nights. But that's all in the future. A summer of work beckons, but with the vitality of term's end bubbling, a couple of hard months of research look retrospectively like a vacation for the spirit.
Talk turns to holidays, for people who can live the Roman style and get out of town for ferragosto and beyond. Talk turns to sea breezes, and sailing. Talk turns to the Pontine Islands.
Ponza has been simmering in my mind for years, but only this summer took centre stage. That warm Roman night in early July we heard how magical it was, how easy to get to, how our summer shouldn't end this year again without a trip. Getting home and small-hours googling ferries meant suddenly we'd wrested a few days annual leave from the dying days of summer, and were Ponza-bound in early September.
We started from (Nero's) Anzio. It's one of my favourite seaside port towns (evoking childhood trips to Bray, but that's stories for other days), and we spent an especially gilded day there last summer with two close friends. Our B&B was simple but friendly, and while the room was old-world in various ways, it was large, opposite the archaeological museum, and five mins or so either way to Station and Port. I was determined on a genuine holiday — none of the buswoman's business that illuminated Abruzzo in July. Just fun. But we'd been attempting to visit Anzio's archaeological park and imperial villa remains for years; this seemed a moment to seize.
The little archaeological museum (free entry) is charming, and has lovely and evocative pieces. I felt sad for its loss of much that's really substantial of Anzio's 'finds' to Rome (Palazzo Massimo in the main), but the politics of heritage and its presentation are complex. We had time for a quick dash round the under-the-same-roof Anzio Landings museum: chock full of donated ephemera, uniforms, equipment it's a bit of a lucky dip, but in its confusion, oddly, there's a compelling sense of history.
Next, a dash across town to the archaeological park. The road is lined with tamarisks; lovely creatures, but very imperially minded and minimally donative of shade. We were hot and slightly scratchy in temper by the time we got to the park, and believe me it's only because it was so meagrely an experience, so stunningly unimpressive, that we were able to laugh a great deal about it. Especially when we fled down to the beach for a reflective paddle.
and to view the (much more visible down below!) remains.
Late and multi-platter lunch at the harbour, at La Fraschetta del Mare, left us a little dozy, so despite the wake-up candy-colours of Anzio architecture an early-ish night beckoned; depositing us awake and zipping down to the hydrofoil in our B&B host's car at 0730. About 90mins after leaving Anzio with Vetor Aliscafi we were strolling up through Ponza's Bourbon-flavour streets to our hotel.
Breakfast #2 was irresistible; the view from the breakfast terrace a jewel box of hot colour and straw-gold light. It seemed churlish not to change directly into swimmery and after unpacking, catch a water-taxi from the harbour to Frontone beach. It's a shingle strand, a narrow stretch between deeply shelving waves and dramatic cliffs. I'm such a pale-face — lettoni and ombrelloni are always required.
Thus commenced a four-day step out-of-time. Dinner across the water that first night drifted into a morning trip to the harbour to collect our rental boat, after which we were mostly afloat until finally reaching Anzio again on Thursday evening last. Salt cracked and caked everywhere, lending a briny tang to fruit we greedily ate in between snorkelling epics through tiny cove-kingdoms. Pizza al taglio (tomato and mint, aubergine, cicoria and caper) and the breeze of open water were excellent appetite whetters.
For the final two days, after an evening gazing across sunset-illuminated Palmarola from Le Forna, we made the crossing to Ponza's next sibling along. The helpful boatman suggested various coves, sail-throughs and delights we should be alert for. Our first Palmarola crossing took us over some higher seas that our 15hp engine was wholly happy with, and we were glad to ease into a restful few hours in a secluded cove where water-line caves made for shady respite from swimming in the glittering sun. A quick circumnavigation before making our way home suggested there was much more to investigate, and ensconced in a 25hp upgrade the next day we explored just about every inlet, and in-and-out-let.
Our first day making the Palmarola crossing we saw a dolphin; hoped it was fortunate not an indication of dufferish unseaworthiness. The second day it was a hurly burly of flying fish, flittering and skimming just above the kissing waves.
The magical and otherworldly aspect didn't fully come home to us until we tried to revisit our lingering cove of the previous day. Try as we might, casting a churning wake up and down well out from coast, then slowing to make closer and closer approaches, that cove entrance was just impossible to recapture. Did we dream it? There was a languor and haze to to the first of the Palmarola days which makes me think that perhaps it was a carpe diem shot, a one-off, rewarding the ambition of our nervous open-water crossing, the water we shipped, the odd elevator-wave. Who knows? the last day had its own bitter-sweet end of summer charms, and after four days of island-hopping life I felt ready to contemplate home with the promise of Pontine delights waiting on another summer. The return to term-life has been rather more brutal than I'd expected, so the memory of Ponza and Palmarola now all the more cherished.


text:
Victor Crowley (also known as Hatchet IV) is a 2017 American slasher comedy film written and directed by Adam Green. It is the fourth installment in Green's Hatchet film series, and a sequel to Hatchet III. Kane Hodder returns to the role of the titular killer Victor Crowley. Critical reaction for the film was generally mixed.

Plot
A decade after the events of the first three films, survivor of the Honey Island Swamp massacre Andrew Yong is told by his publicist Kathleen that he has been offered a special interview for a true-crime TV series, but that that the producers have insisted that his interview take place in the Honey Island Swamp. Andrew initially refuses to go due to his trauma from his experience with Victor Crowler, but is convinced when Kathleen tells him they have offered him $600,000, and she got them to go up to $1,000,000.

Andrew and Kathleen head out on a private charter plane, where Andrew learns that his interview will be hosted by his ex-wife Sabrina and her crew: audio technician Austin, his videographer girlfriend Casey, makeup artist Jay, and production assistant Zach. Suddenly, one of the plane's engines explodes during flight, and Jay and Zach are killed as the plane starts plummeting to the ground.

Meanwhile at the swamp, Chloe, her boyfriend Alex, and her best friend Rose are preparing to film a trailer for a movie they are creating based on the Crowley massacre, alongside eccentric swamp tour guide/local actor Dillon. For the sake of research, Rose begins searching YouTube for videos of people attempting to recite the voodoo curse that originally brought Crowley back to life, when Zach's charred corpse suddenly flies from the plane and lands in front of them. Rose and Dillion overhear the plane crashing, and so go off to investigate while Alex stays behind to calm Chloe down. However, Rose drops her phone while it is playing videos of people trying to recite the curse, and fails to realise.

At the plane wreckage, Dillon and Rose find that everyone aside from Jay, Zach and the pilots have managed to survive the crash, but that Casey is trapped under the seats and has water slowly rising around her due to the plane being partially submerged in the swamp. Meanwhile, Rose's phone autoplays a video of Reverend Zombie reciting the voodoo curse, and Victor Crowley is resurrected from the swamp, following which he kills Alex. Chloe flees and nearly makes it to the plane wreckage, but is severely wounded by Crowley, who then disappears into the fog.

With the survivors having witnessed the attack, Kathleen begins to suffer from a panic attack and flees the plane. Austin attempts to stop her, but he and Kathleen are both killed by Crowley, who then finishes Chloe off and attacks the plane, making it sink further and causing Casey to drown.

As Dillon locks himself in the pilot's cabin, hoping to radio for help, Andrew, Sabrina and Rose all flee in separate directions. Sabrina tries to escape on Dillon's boat, but Crowley appears and kills her. Meanwhile, Dillon manages to get the plane's engine working, and he, Andrew and Rose have a standoff with Crowley beside the plane, which sees Dillon sacrificing himself by tackling Crowley into the plane turbine, shredding them both to pieces.

Marybeth Dunston watches a news report on the crash and the discovery of several mutilated bodies. Realizing Crowley has returned, she grabs a shotgun, saying "I've been waiting for you, motherfucker."

Cast

Production

In November 2015, reports emerged that a fourth entry in the Hatchet series was in development. Simultaneously, various outlets alleged that a New Nightmare-esque premise was proposed by series creator Adam Green, but was rejected by the studio. However, Dread Central debunked these claims and instead revealed that Green opted not to move forward with the pitch. Green would later become disenchanted in continuing the franchise and was adamant there wouldn't be another installment. It wasn't until George A. Romero convinced Green to finally make the film at the Rock and Shock convention. Green immediately began work on the script, under the title Arwen's Fancy Dinner.

Principal photography began in secret under the working title Arwen's Revenge. Production spanned eleven days, while an entire day of filming was lost due to a set collapsing. Cast members Kane Hodder, Parry Shen, Laura Ortiz, Dave Sheridan, and Brian Quinn were officially revealed in August 2017.

In July 2017, it was announced that an official '10th Anniversary Event' screening of the original Hatchet film would be playing at the FrightFest Film Festival of 2017, featuring newly released footage. The same event, which took place on August 22, 2017 in Los Angeles, brought forth the announcement that it was actually the premiere of a secretly filmed Hatchet sequel titled Victor Crowley. Green said on the matter, "I couldn't be happier to partner with Dark Sky Films and bring Victor Crowley back to horror fans around the world. Resurrecting the series for its tenth anniversary was our way of saying thank you to everyone in The Hatchet Army and beyond who have supported this series since its inception. This bloodbath is for all of you."

Release

Theatrical
Victor Crowley debuted on August 22, 2017 in Los Angeles, California The film began screening in select theatres across the United States on October 5, 2017 on special one night events featuring Adam Green collectively known as the "Victor Crowley Road Show".

Home media
The film was released on blu-ray and DVD on February 6, 2018.

Reception

On Rotten Tomatoes, Victor Crowley holds an approval rating of 67% based on 15 reviews, with an average rating of 6.7/10.

The film was met with mixed reviews. Steve Barton of Dread Central awarded the film a quality rating of 4 out of 5, stating that "Victor Crowley is a smartly written, outrageously funny, and incredibly gory affair that's nothing short of a gift for slasher fans who appreciate their films wrapped in viscera with gallons of blood to spare." JoBlo.com said of the film "VICTOR CROWLEY may be the best of the sequels to HATCHET, perhaps the best in the series." Kalyn Corrigan of Bloody Disgusting called it "the Gory Slasher Film You're Craving!", while critiquing "Sure, they spend a little too much time on the plane, and it would've been nice to see some of the more human characters last a bit longer during the runtime, but... in all honesty, it's just nice to have a series in the same iconic style that we can count on to carry us through the years of big studio films and over produced predictable cash grabs." Alternately, Brad Miska also reviewing for Bloody Disgusting said "While Hatchet has since become an iconic franchise, none of the sequels have been able to recreate the magic of the first film. The latest, Victor Crowley, is easily the worst of the bunch."

Potential sequel
In October 2019, Danielle Harris revealed that two more films were planned by the studio, with the intention of shooting both back-to-back. In May 2020, Green said that a fifth film was a "safe bet" due to the financial success of Victor Crowley.

References

External links

2017 films
2010s comedy horror films
2017 horror films
2017 independent films
2010s serial killer films
2010s slasher films
American independent films
American sequel films
American slasher films
American splatter films
Slasher comedy films
Films set in Louisiana
Films shot in New Orleans
Hatchet (film series)
Parodies of horror
2017 comedy films
2010s English-language films
Films directed by Adam Green
2010s American films

redpajama_set_name: RedPajamaWikipedia


Wollzelle pioneered the concept of web applications back in the early 2000s. Developing rich and powerful platforms has long been part of our DNA.
Besides operating as a full-service agency, we have successfully bootstrapped three large-scale SaaS products. Fluxiom and Maiko empower both professionals and corporations. Our unique Store Locator is backed by a dedicated B2B support team.
Companies large and small work in our cloud every day, including household names like Fox, Steinway & Sons, and TNT. Designing and deploying rich applications is second nature to our development team.
If the web is your platform, Wollzelle is your partner!
fly out at blazing speeds.
If it involves files, Fluxiom will make it simpler. Since 2006, our collaborative assets manager has helped thousands cut through the clutter of modern life. From its breakthrough desktop-like interface (a first on the web) to its advanced content-processing engine, Fluxiom keeps pushing the boundaries of online file management. Our first product, it kick-started the web application revolution and remains a strong platform for innovation today.
High-profile brands entrust our Store Locator platform with delivering happy clients to their doorstep. Fully multi-lingual up to nine languages, location-aware and search-enabled, this cloud-based solution integrates with almost any site and back-end to transparently direct clients to your nearest location. It comes fully serviced and supported, and our dedicated migration assistance gets you started quickly.