text:
\section{Introduction}
The nature of the absorbing material hiding the central engine of active galactic nuclei (AGN) is crucial to our understanding of
the physics of these objects \citep{2018ARA&A..56..625H}. It is also a key issue in the unified model of AGN \citep{Antonucci_1993, Urry_1995}
which in its simplest version postulates that the diversity of AGN can be largely explained as a viewing angle effect.
The most important ingredient of this orientation-based model is an optically and geometrically thick  torus that obscures the
nuclear regions of an active galaxy (the accretion disk and the hot corona  as well as the broad line region (BLR)).
We optically classify an AGN as type 2 or type 1 depending if our line of sight intercepts or not the obscuring material of the
torus.\\
The validity of the unified model of AGN has largely been tested and confirmed by the presence of high absorption
measured in the X-ray spectra  of type 2  with respect to  lower amounts found in type 1 AGN.
In particular, using  a  sample of 272 AGN observed at high energies ($>$ 20 keV) by INTEGRAL/IBIS we have found that the
standard-based AGN unification scheme is followed by the majority  of bright AGN \citep{Malizia_2012} with only a few exceptions
related to 12--13\% of the objects.
These exceptions are absorbed type 1 and unabsorbed type 2 AGN. The absorption in type 1 AGN is generally  interpreted in terms
of ionised gas located in an accretion disc wind or in the biconical structure associated with the central nucleus
and therefore unrelated to the torus. The lack of  X-ray absorption (N$_{H}<$ 10$^{22}$ cm$^{-2}$) in type 2 AGN could
be explained by the assumption that the torus is either not present (or has disappeared) or the source has been misclassified.
The first case is probably true for  low luminosity objects \citep{Elitzur_2008} while the second case is relevant for the
class of intermediate type 2 Seyfert (type 1.8 -- 1.9).
These intermediate objects have  historically been considered as AGN where the observer's line of  sight intercepts either
the outer edge of the torus or a limited number of clouds, so that the broad line region is still partly visible.
However, in \citet{Malizia_2012} we have also pointed out that these intermediate classifications can  be explained by an  intrinsically
variable ionising continuum or by  the presence of absorption/reddening unrelated to the torus.
For example, a source that would normally appear as a type 1 Seyfert can be classified as an intermediate type if it is in a low
optical flux state \citep{Trippe_2010} or if  its BLR is  obscured (except for the strongest H$_{\alpha}$ line) by dust related to
large-scale structures such as bars, dust lanes and host galaxy material \citep{Malkan_1998, 2000A&A...355L..31M}.\\
Thus absorption in AGN is probably due not only to one component, the torus, but to  multiple  components on very different scales.
\citet{Bianchi_2012} identified 3 such components: the  BLR on the 0.01 pc scale, the torus on a parsec scale and absorption located
in the host galaxy  on a scale of hundreds of parsecs.\\
Evidence  for large scale absorption comes mostly from inclination studies of the host galaxies of AGN.
In one of the first such studies \citet{Keel_1980} found that optically-selected (mostly type 1) Seyferts tend to avoid
edge-on host galaxies.
Using a sample of AGN selected in the soft X-ray band (0.2-3.5 keV), \citet{Simcoe_1997}
subsequently confirmed the  bias against edge-on Seyfert 1 although they were able to recover some of the edge-on AGN missed in UV
and visible surveys, resulting in  30\% incompleteness for type 1's.
However since the soft X-ray band can also be biased in terms of absorption, a definitive test would be provided by the use of
a hard X-ray selected sample.
A preliminary analysis performed on a Swift/BAT sample of around 80 AGN by \citet{winter_2009} showed that objects with low X-ray column
densities were  preferentially found in galaxies with low inclination angles (face-on, $b/a >$ 0.5), while those with higher column
densities were found in galaxies of any inclination  (edge-on and face-on, 0.1 $<$ b/a $<$ 1).
The finding that optically selected AGN samples tend to avoid edge-on systems, has recently  been confirmed and refined with much higher statistics by using the SDSS survey \citep{Lagos_2011}.\\
The first explanations for this result came from \citet{Maiolino_1995}  and \citet{2000A&A...355L..31M}.
\citet{Maiolino_1995} proposed the {\it dual absorber} model which
foresees the existence of a 100 pc scale obscuring material of molecular gas coplanar with the galactic disc and not necessarily
aligned with the torus. On the other hand, taking into account observational evidence, \citet{2000A&A...355L..31M} proposed a scenario where Compton thick Seyfert 2 galaxies
are those sources observed through the torus while Compton thin/intermediate Seyfert galaxies are obscured by dust lanes at larger distances.\\
Focusing on the possible origin of the galactic absorber, a major study is that of \citet{Malkan_1998}, who detected fine-scale
structure in the centres of nearby galaxies using HST images: these structures include dust lanes and patches, bars, rings,
wisps, filaments and  tidal features such as warps and tails. These authors even suggested a new unified model
(the galactic dust model) whereby the obscuration that converts an intrinsic Seyfert 1 nucleus into an apparent Seyfert 2 occurs
in the host galaxy hundreds of parsecs from the nucleus. More recently \citet{Prieto_2014} confirmed these early results of large scale, a few hundred pc, dust filaments and diffuse dust lanes hiding the central region of some AGN. \\
Nowadays the parsec scale environment of AGN can be spatially resolved by high angular resolution observations in the infrared (IR) with VLTI and in the sub-Millimeter by ALMA
(see e.g. \citet{2017ApJ...838L..20H, 2019A&A...623A..79C}) which draws a much more complex picture of multi-phase and multi-component regions.
Recently \citet{2019ApJ...884..171H} has proposed a model which accounts for these new observations wherein  dusty molecular gas flows in from the
host galaxy ($\sim$100 pc) to the sub-parsec environment via a disc with small to moderate height. Due to the radiation pressure, the disc puffs up and unbinds a large amount
of the inflowing gas from the black hole's gravitational potential allowing the creation of dusty molecular winds driven by the radiation pressure from the AGN.
These dusty winds feed back the host galaxy with a rate increasing with the AGN luminosity (or Eddington ratio), and are therefore a mechanism to self-regulate the AGN activity providing a feedback from AGN to host galaxy. Within this picture there are multiple spatial and dynamical components which obscure the
primary emission rather than a single torus.
For local, radio quiet active galaxies, Hoenig's  model  is consistent with the structure proposed by \citet{Ricci_2017}
to explain the X-ray obscuration in AGN.
ALMA observations have revealed the presence of  circumnuclear molecular (CO) gas in many Seyfert galaxies \citep{Schinnerer_1999},
as well as the presence of cold gas and dust at hundreds of pc scales in many AGN host galaxies (e.g. \citealt{Garc_a_Burillo_2005,Garc_a_Burillo_2014}).\\
Finally, we note that large scale absorption may come also from non asymmetric perturbations which provide  a viable way to  channel
gas from the outer part of a galaxy into its central regions. These  perturbations can be of two types: external, such as
galaxy-galaxy interactions or internal, such as due to bars and their gravity torques.
Observations indicate that an AGN becomes heavily obscured behind merger-driven gas and dust, even in the early stages of
galaxy-galaxy interaction, when the galaxies are still well separated \citep{Kocevski_2015}.
Furthermore,  analysis of Swift/BAT AGN indicates that a large fraction (25\%) of these objects  show  disturbed morphologies or are in close
physical pairs  compared to  matched  control  galaxies  or  optically  selected  AGN \citep{Koss_2010}. \\
In this paper we will investigate  the presence/role  of obscuration on large galactic scales and its relation with the X-ray column density,  by examining the axial ratio distribution
 in  a well defined sample of  INTEGRAL selected AGN, listed in \citet{Malizia_2012, Malizia_2016}
and newly reported in this work. This sample, being hard X-ray selected, is the most appropriate to carry out this type of study since it
is  unbiased against obscured objects and therefore free of the limitation  which affects surveys at other frequencies
(i.e. from optical to soft X-rays).

\begin{figure}
	\includegraphics[width=\columnwidth]{fig1.eps}
   \caption{Histogram of the morphological classification following the \citet{DeVaucouleurs_1959} scheme.
Unknown: galaxies which have no host galaxy morphology, E: elliptical galaxies; S0: intermediate systems between ellipticals and spirals; S: spiral galaxies.
Objects are further sub-divided in type 1 and type 2.}
    \label{morph}
\end{figure}

\section{The sample}
In order to have a well defined hard X-ray selected sample of active galactic nuclei, we have considered all the INTEGRAL Seyferts
listed in  \citet{Malizia_2012, Malizia_2016} plus those reported in  Tables \ref{mere}.2 and \ref{krivo}.3 of the Appendix.
This hard X-ray selected sample of AGN  has been extracted from the INTEGRAL/IBIS all sky surveys performed so far  in the 20-100 keV band (\cite{Bird_2016} and reference therein).
This sample has been updated in this work with the addition of the new  AGN reported by
\citet{Mereminskiy_2016}  in the  deep extragalactic surveys of M81, LMC and 3C 273/Coma regions and those reported by
\citet{Krivonos_2017} in the Galactic Plane Survey (see Appendix and Tables \ref{mere}.2 and \ref{krivo}.3 for details on these new additions).\\
The entire INTEGRAL AGN sample is fully characterised in terms of optical identification/classification
and is also fully studied in terms of  X-ray spectral properties (see \cite{Malizia_2012}).
In particular, the column densities (N$_{H}$) measured in the 2-10 keV band for each AGN, have been collected from the literature (see  \citet{Malizia_2012, Malizia_2016})
or calculated for the new added sources in this work (see Appendix, Tables \ref{mere}.2 and \ref{krivo}.3).
All together, we have gathered a sample of 376 hard X-ray selected active  galaxies, with a well defined set of information.
Objects identified as Blazars in the IBIS surveys have been excluded from the analysis to avoid complication due to the presence of jets pointing towards the observer.
Following our previous works
we divided our AGN into type 1 comprising all the broad line Seyferts of our sample
and including Seyfert 1, 1.2, 1.5 (179 objects) and type 2 objects comprising all the narrow line AGN i.e. Seyfert 1.8, 1.9 and 2
(197 objects).
Twenty-two objects ($\sim$ 6\% of the sample) have an unknown optical classification or belong to non-Seyfert optical classes (liners, XBONG, AGN), therefore they have been assimilated into type 1 or 2 AGN depending if they were absorbed (21 objects) or not in the X-ray band. Performing the complete analysis without these sources does not significantly change the overall results.\\
In order to  investigate the role of absorption in the host galaxy we have collected for the entire sample the  axial ratio $b/a$, used here as
a proxy for the host galaxy inclination (to first order, $cos$ $i = b/a$ where a and  b are the observed major and minor axes of a galaxy and $i$ is its inclination).
These values  have been collected from the Two Micron All Sky Survey\footnote{http://irsa.ipac.caltech.edu/cgi-bin/Gator/nph-dd}, where
information was available for  300 objects out of  376 in the sample (i.e. the largest coverage available in catalogues with b/a informations) and they are reported in columns 5 and 10 of tables \ref{all}.1 and \ref{mere}.2/\ref{krivo}.3 respectively.
It is worth noting that  as described by \citet{2003AJ....125..525J}, the 2MASS  images, co-adding J, H and K bands, have a point spread function
FWHM of 2 - 3 arcsec. This value is  much smaller that the radii of our galaxies (around 20-30 arcsec or more) collected from the same archive,
therefore excluding any possible bias in the $b/a$ measurements used in our work, especially for type 1 objects hosting a bright nucleus.
Furthermore, in order to verify the accuracy of these axial ratios, we have used Pan-STARRS1 database \citep{2016arXiv161205560C} and extracted the  DR1 color (g to z filter) images for a representative
sample of over  30 of our objects ranging in axial ratio from 0.1 to 0.9 and over all optical classes.
Representative set of objects among those with no optical classification has also been checked.
We then fitted ellipses to these images in order to measure their axial ratio values.
In every case these values were consistent with those extracted from the 2MASS surveys and originally used. \\

\begin{figure}
	\includegraphics[width=\columnwidth]{fig2.ps}
  \caption{Distribution of column density in each morphological class; X-ray absorption in AGN hosted in galaxies of unknown class is also shown.
  Filled red bins referred to Galactic or upper limit values of N$_{H}$.}
    \label{morph_nh}
\end{figure}

\begin{figure*}
\centering
\includegraphics[width=12cm]{fig3.ps}
   \caption{Distribution of host galaxy axial ratios of INTEGRAL AGN differentiated into broad lines or type 1 i.e. Sy 1 - 1.2 - 1.5 (upper and lower left panels) and narrow lines or type 2 i.e. Sy 1.8 - 1.9 - 2 (upper and lower right panels).
   In the lower panels the morphological type of our sample sources has been considered; histograms in dotted red lines  refer
    to AGN hosted in late type (Spirals) galaxies, blue dashed lines AGN hosted in early (Elliptical and S0) galaxies and black solid lines refer to host galaxies
   for which no morphological type has been found in the literature.}
    \label{histo1}
\end{figure*}

\section{Absorption and source morphology}
Indications that absorption on a galaxy scale is important in the overall column density budget of an AGN, suggests a possible link  between
galaxy morphology and N$_H$.
We have therefore collected data for both these two parameters.
Data for host galaxy morphological information for all objects come from the Hyperleda catalogue  \citep{Makarov_2014}, the NED archive
and the 2MASS Redshift Survey \citep{Huchra_2012}:  the most quoted classification among these 3 databases has been adopted and reported in tables A1, A2 and A3.
When no information or different classification were available, we have also searched the literature for extra information (\citealt{Maiolino_1999}, \citealt{Madrid_2006}, \citealt{McKernan_2010}, \citealt{Maia_2003}, \citealt{Tsvetanov_1992} and \citealt{Ferruit_2000}).
Data for N$_{H}$ values comes instead from our previous publications and current paper as specified in section 2.\\
All the INTEGRAL AGN have been  divided into  3 broad morphological types following the \citet{DeVaucouleurs_1959} scheme:
E to describe elliptical galaxies; S0 for objects which are intermediate systems between ellipticals and spirals (alternatively called
lenticular galaxies), and S for spiral galaxies.
The distribution of INTEGRAL AGN in each morphological class, including those objects for which the host galaxy morphology is unknown,  is shown in figure \ref{morph},
where  the predominance of spiral/lenticular galaxies over ellipticals is evident.
The greater number of type 2 over  type 1 AGN in both S0 and S classes is also clear.\\
We have been able to obtain morphological host galaxy  information for  228 objects or 61\% of the sample.
This low  fraction is due to the fact that many INTEGRAL AGN are newly discovered galaxies, often located on
the Galactic Plane, i.e. in the zone of avoidance and therefore  their morphology is still poorly studied.
In the nearby Universe, elliptical galaxies are known to have less gas, dust, and ongoing star formation activity
than spiral galaxies (\citet{Hirashita_2017} and refences therein).
Figure \ref{morph_nh} shows the histogram of each morphological class as a function of X-ray column density: while there seem to be no
difference in absorption properties among different classes for column density below LogN$_{H}$ = 24, some difference is evident above,
since no Compton thick AGN is hosted in an elliptical host galaxy.
However, this may be due to low number statistics, given the limited number of ellipticals considered here as they count for only  14\% of the entire INTEGRAL AGN sample.
The fraction of heavily absorbed AGN is around 11\% for both spiral and lenticular galaxies;
if the same fraction is applied to ellipticals, then we would expect 3-4 objects in this class to be Compton thick, while none is observed.\\
The evidence of  a lower  fraction  of  Compton thick  AGN  in hard X-ray radio galaxies, typically hosted in elliptical galaxies,
has already been discussed by \citet{Panessa_2016} and \citet{Ursini_2017} and is definitely an issue that deserves
further investigation. \citet{Ursini_2017} also noted that a significant role in the absorption of  heavily absorbed radio galaxies
could be played by material different from the classical pc-scale torus such as that traced by 21 cm H$_{I}$ absorption, which can
be located much farther away, e.g. at galactic scales.
Hence observational evidence even questions the origin of the X-ray absorption  in ellipticals and hints at a possible
difference between the average properties of ellipticals compared to lenticular/spiral galaxies, especially in terms of Compton thick absorption.

\section{Host galaxies inclination}
Using the large INTEGRAL AGN sample, we explore in this section the axial ratio distribution of broad  and narrow line AGN:
figure \ref{histo1} displays the  histograms of $b/a$ by  galaxy type and within each type divided in morphological classes.
Note that the lack of galaxies with   $b/a <$ 0.2 is  due to the  non zero thickness of the disc which accounts for the fact
that, even when seen edge-on, a galaxy has $b/a$ greater than zero \citep{Hubble_1926}.
Among the 122 type 1 AGN  of  our sample for which we obtained axial ratio information, only 12 ($<$10\%) have a host galaxy axial ratio below
0.5; this percentage is much higher in type 2 AGN where 50 out of  178 type 2 objects (or 28\%) have  $b/a <$ 0.5{\bf\footnote{It is worth noting that the absorbed sources with no optical class considered as type 2, have axial ratio distributed over the whole range of b/a, and the only unclassified source included in the type 1 class, has b/a = 0.58.}}.
By performing a KS test, we find that the axial ratio distributions of type 1 and type 2 AGN are different,
since the probability that the two samples come from the same distribution is rejected at a confidence level of 99.99\%.
In order to quantify the deficit of type 1 AGN at low inclination angles, we compare the two histogram distributions.
Taking the difference between the two histograms, and assuming that above an inclination angle of 0.5 they are from identical distributions, we normalise it  so that the total difference in number of sources above that value is zero. In order to have a difference of zero below that threshold, 38 $\pm$ 11 sources must be missing from the type 1 distribution. This implies that in this sample there is a deficit of about 24\% ($\pm$ 5\%) of type 1 AGN, in agreement with \citet{Simcoe_1997} who found 30\% for an X-ray selected sample.\\
Furthermore, using the information on  the host galaxies morphology  and dividing the objects into early (Ellipticals and S0) and late  (Spirals) types,
we also checked if the bias against edge-on host galaxies of broad line AGN is related to any specific  morphological type or
is present in both types.
Using (here and in the following) a confidence level of 99\% and applying the KS test, we find that
the two distributions (type 1 versus type 2 AGN) are different both for early type as well as late type objects. This is also evident
in figure \ref{histo1} where the different morphology types have been highlighted for type 1 and 2 AGN respectively.
We therefore confirm that, even using AGN selected above 20 keV, the  deficit of type 1 AGN hosted in edge-on galaxies  exists in,
and is  independent of, all morphological types. \\
In addition to this deficit, it is interesting that the type 2 are distributed over the whole range of $b/a$.
This result confirms previous findings but also highlights the fact that this lack of Seyfert 1 in edge-on galaxies is not due to observational bias.
As pointed out by \citet{Gelbord_2006}, if the torus was the only obscuration matter, then two possible scenarios should be taken into consideration:
the first where the torus and the host galaxy plane are aligned and the second
where the two are misaligned. In the first case we should see a distribution of type 1 Seyferts peaked in face-on galaxies  and that of the type 2 Seyferts in edge-on galaxies
while in the second case no correlation  between  Seyfert type and host galaxy inclination would be expected.
From the studies performed so far and confirmed herein, neither of these two scenarios are compatible with the observational evidence since the broad line
AGN have a strong correlation with the host inclination angle while the type 2 are broadly distributed over the whole $b/a$ range.
Our findings indicate that something intervenes  outside the nucleus of the AGN (on hundreds of pc scales), likely in the host galaxy;
this absorbing material, which could be not aligned with the torus, can contribute to the final column density measured in the X-ray band.\\
From recent ALMA observations of some AGN, we have an indication that the molecular discs, or tori, detected at 10 pc scales
are kinematically decoupled from their host galaxy disc and have random orientations  \citep{2019A&A...623A..79C}.
Assuming a simplistic approach, i.e. not considering  the BLR but only the host galaxy and the torus, depending on their relative alignment or misalignment we expect the following 4 configurations.
If the torus is edge-on, the source is always classified as a type 2 AGN and should present X-ray absorption, whether or not the galaxy is seen  edge-on or face-on.
If the torus is seen face-on, then  we should expect a type 1 AGN configuration with no or very mild absorption unless the galaxy is seen edge-on and has absorbing
material on large scale.
In this last case the source could be  wrongly classified as a type 2 AGN although the absorption is not related to the torus.
This is schematically shown in figure \ref{scheme} where the horizontal line represents  the dividing line between face-on and  edge-on host galaxies at b/a = 0.5,
while the first vertical line represents instead the value of N$_{H}$ = 4 $\times$  10$^{21}$ cm$^{-2}$ which has been assumed
as the dividing line between absorbed/unabsorbed objects.
This value has been taken from \citet{Mateos_2016}  and corresponds to the extinction level capable of hiding the BLR.
The dashed region delimited by log N$_{H}$ $\leq$ 23 and b/a $\leq$ 0.5, represents  the area where misclassified type 1 AGN could be located (i.e.
galaxy absorption in an edge-on host is sufficient to hide the broad line region).
With this scheme in mind, we can now investigate the relation between host galaxy inclination and X-ray absorption.

\begin{figure}
	\includegraphics[width=\columnwidth]{figure4_new.eps}
  \caption{Scheme of the expected type of absorption in the b/a - N$_{H}$ plane for broad line (left blue side) and narrow line AGN (right side)
  in relation to the torus/host galaxy misalignment. The dashed blue region represents values where a passible type 1 AGN could be classified as type 2 due to
  absorption located in the host galaxy.  }
    \label{scheme}
\end{figure}

\subsection{Possible bias on redshift}
Before drawing any further  conclusions from the observed axial ratio distribution, any possible  bias introduced by the sample redshift distribution
must be checked.
It is important to investigate this issue since there are two considerations that pertain to the use of a non  complete sample of AGN.
The first is that at high redshifts, the sources become point-like and therefore it is  very difficult to estimate the host galaxy
axial ratio. The second concerns the widely known fact that in the local Universe type 2 objects outnumber type 1 sources by a factor
of $\sim$4 and more \citep{2015MNRAS.454.1202S};  whether this  effect comes from  cosmological reasons or not is still  matter of debate.
These two effects are highlighted in figure \ref{ax_zeta} where it is clear that the distributions of type 1 and type 2 galaxies are different
in the $z$ -- $b/a$ plane: there are considerably more type 2 AGN  at low $z$ values than type 1 and  very few objects at high redshifts have
axial ratio measurements.
In order to minimise these  effects, we have decided to analyse a subset of the two AGN populations restricting  both high and low $z$ values.
To do this, we first choose all  sources between a lower and higher limit of redshift. The distribution of type 1 and type 2 objects between these
two limits are then compared and the KS statistic applied to identify if they come  from the same population.
This is done for all possible combinations of the two limits  in $z$. The combination which provides  the highest probability that the
two populations come from the same  $z$ distribution (at 99.9\% confidence) are then further reduced to give the largest total number of objects.
In this manner, we found that allowing the redshift to range from 0.026 to 0.095, we obtained a total number of 133 AGN with $z$ within this range;
of these AGN,  66 are of type 1 and 67 of type 2, with a probability of 99.97\% that they come from the same overall redshift distribution
(top panels of figure \ref{histo_z}).
Next, the distribution of the axial ratio of these 133 sources divided in two optical classes were compared as shown in figure \ref{histo_z}  (lower panels).
Again the two distributions are found to be different,  with type 1 objects mainly located in face-on galaxies and type 2 spread over
the entire range of   $b/a$ values. Using the KS statistic we find that the likelihood that the two populations come from the
same distribution is rejected at a confidence level of 99.75\% implying that no bias in redshift affects our result.

\begin{figure}
	\includegraphics[width=\columnwidth]{fig5.ps}
  \caption{Redshift values of the INTEGRAL AGN plotted against the axial ratios of their host galaxies.
           Filled black circles are type 1 AGN while open red squares are type 2.}
    \label{ax_zeta}
\end{figure}

\begin{figure}
	\includegraphics[width=\columnwidth]{fig6.ps}
  \caption{In the upper panels the distributions of redshift values in type 1 (left)  and type 2 (right) in the bin  0.026 and 0.095, while
  in the bottom panels the distributions of their relative axial ratios.}
    \label{histo_z}
\end{figure}

 \begin{figure*}
 \centering
\includegraphics[width=12cm]{fig7.ps}
   \caption{Upper panels: distribution of host galaxy axial ratios. Panel a) Seyfert 1/1.2 (black line) and intermediate Seyfert 1.5 (red dashed line); panel b): Seyfert 2 (black line) and intermediate Seyfert 1.8/1.9 (blue dashed line).
Lower panels:   axial ratios versus X-ray absorption: c) broad line AGN (black circles Seyfert 1/1.2 and red circles Seyfert 1.5; panel d) narrow line AGN, black squares Seyfert 2 and blue squares Seyfert 1.8/1.9. Open circles refer to N$_{H}$ upper limits or objects with no intrinsic absorption, i.e. only Galactic. Lines are like in figure 4.}
    \label{histo2}
\end{figure*}

\section{Host galaxy inclination  versus X-ray absorption}
In order to investigate  the deficit of type 1 AGN in edge-on galaxies in more detail, we first considered for  each AGN type their optical sub-classes
which is a way to investigate if and how the broad line region is detected.
In figure \ref{histo2} panel a), we compare  the axial ratio distribution of Seyfert  1-1.2 (solid black line ) and Seyfert 1.5 (dashed red line).
As is evident in the figure but also quantified by the KS test, the two distributions are  similar (at a confidence level of 99\%) indicating
that the deficit of broad line AGN in edge-on galaxies is present in  all  subclasses.\\
Equally, in panel b) of figure \ref{histo2}, the distribution of axial ratios in Seyfert 2 (black solid line)
and Seyfert 1.8-1.9 (blue dashed line) are plotted in order to see if they are distributed differently and,  as is clear from the histograms and quantified by the
KS statistics, they are not.
Also including all the sources of intermediate class (1.2, 1.5, 1.8 and 1.9) in the type 1 sample and leaving in the type 2 only the pure Seyfert 2
objects, the two distributions resulted statistically different. The same result has been found considering only the high energy selected AGN belonging to
the INTEGRAL complete sample \citep{2009MNRAS.399..944M}.\\
In figure \ref{histo2} panel c) we plot  the axial ratios of type 1 AGN (Seyfert 1-1.2 black circles and Seyfert 1.5 red circles) versus
the X-ray  absorption, the open circles indicate no intrinsic absorption (i.e. only Galactic) or upper limits.
Note that in  panels  c) and d) of figure \ref{histo2} the horizontal and vertical dashed lines follow the scheme introduced in figure \ref{scheme}.\\
As expected from the scheme of figure \ref{scheme}, type 1 AGN fall mostly in the left, top side of panel c), i.e. correspond to the situation
where the torus and the galaxy are both seen face-on and no or mild X-ray absorption is present.
Regarding those type 1 AGN which, despite having torus and  galaxy both face-on, display X-ray absorption (i.e.
fall in the right upper side of panel c)) we assume that they can be largely explained as objects where the absorbing material
is due to ionised gas located in accretion disc winds or in biconical structures close to the nucleus  \citep{Malizia_2012}.
A more complex interpretation pertain to those type 1 AGN which are hosted in edge-on galaxies and therefore fall
in the bottom parts of panel c).
First we notice that their number is limited  as expected on the basis of the consideration made in section 4.
These low numbers can either be due  to a low probability of having a configuration with a face-on torus in an edge-on
galaxy or a high probability that  absorbing material in a host galaxy viewed edge-on is sufficient  to hide
the BLR and to misclassify the object as a type 2 AGN.
Since there is no reason why each of these possibilities is likely, it is possible that  both  concur to create
the observed low number of type 1 AGN seen  in edge-on galaxies.
In particular we already know of type 1 AGN with absorbing material hosted in edge-on galaxies, which is however not high
enough to hide the BLR. These are the objects located in  the bottom left part of panel  c); one of these AGN is IC 4329A
where the presence of a dust lane observed in the equatorial plane of the host galaxy
has been invoked to explain the source's mild X-ray neutral absorption which is however below our limit of  N$_{H}$ = 4 $\times$ 10$^{21}$ cm$^{-2}$
 \citep{Steenbrugge_2005}.
The most particular  objects are the 3 AGN, IGR J05347-6015, 4C +21.55 and ESO 140-G43,  in the bottom right corner of the panel c).
Although they have a column density Log N$_{H} >$ 21.6 and are hosted in low inclination angle galaxies,  we still see their BLR.
However, these objects are either poorly studied as in the case of IGR J05347-6015 and 4C +21.55
(only Swift-XRT short observations were available to estimate the X-ray column density) or found to be absorbed
by complex and  ionised gas as for ESO 140-G43 (\citealt{Ricci_2010}).
In any case given the uncertainty  on the column  density of  these 3 objects, and given their proximity to the chosen $b/a$
and LogN$_{H}$ boundaries, no firm conclusion can be drawn.\\
In  panel d) of figure \ref{histo2}, the X-ray column density is plotted against  the axial ratio of  Seyfert 2 (black squares)
and Seyfert 1.8-1.9 (blue squares) and,  as for the type 1 AGN,  open symbols indicate no intrinsic absorption or upper limits.
In these objects the torus is by definition seen edge-on independently if the AGN is hosted in a face-on or an edge-on galaxy
and their absorption is high: hence these objects  are expected to spread on the  right side of the diagram over all values of b/a.
Here the unusual objects are those  found in the upper left corner of panel d), which have a column density too  low
to completely hide the BLR. Not considering  Sey1.8-1.9 types where an intrinsically variable ionising continuum or absorption/reddening unrelated
to the torus can explain their intermediate classification, there are 4 objects: NGC 4736, IGR J19260+4136, IGR J03249+4041-SW and
IGR J14515-5542, optically classified as Seyfert 2, which have no absorption in X-rays.
NGC 4736 is a nearby star-forming ring galaxy \citep{van_der_Laan_2015} where the torus is probably not present due to the low
luminosity of the nucleus; star formation could then be responsible for the type 2 optical class.
IGR J03249+4041-SW is one component of a pair of Seyfert 2 in close interaction (pair  distance around 12 Kpc) and it is therefore possible
that its type 2 class  is  simply due to dust associated to the galaxy merging.
The other two AGN are poorly studied, but their column density is well measured and confirmed using XMM-INTEGRAL data for  IGR J14515-5542 \citep{De_Rosa_2012}
and  NuSTAR data for IGR J19260+4136 (our analysis) respectively.
The fact that no prominent iron line is seen at soft X-ray energies excludes that these
are Compton thick AGN (see \citealt{Malizia_2007}); it is  therefore very likely that they belong to the small fraction of
naked Seyfert 2 galaxies where the torus is missing and the optical classification is due to other circumstances \citep{Panessa_2002}.
Otherwise they can be type 1 AGN where the combined effect of a very broadened emission profile and an intrinsic weakness with respect to the host galaxy
conspire to produce  a type 2 spectrum \citep{2019MNRAS.488L...1B}. \\
The objects in the bottom right corner of panel d) are  the most relevant for the aim of this work. Following the scheme of
figure \ref{scheme}, for these type 2 objects we cannot discriminate between absorption due to  material located on large scales and related to the host galaxy,
and that due to the torus.

\section{Discussion}
It is a well known effect that optically selected type 1 Seyfert tend to avoid edge-on host galaxies.
Extensive studies have been performed in different wavebands in order to explain this bias \citep{Keel_1980,Simcoe_1997,Lagos_2011} and although some
objects missed in UV and optical surveys have been recovered going at higher energies, the deficit of type 1 hosted in edge-on galaxies still remains. A definitive test is that provided by the use of a hard X-ray selected sample which is less biased against obscured objects and therefore free of the limitation which affects surveys at other frequencies (i.e. from optical to soft X-rays). The first test at high energies was performed by \citet{winter_2009} on a limited Swift/BAT sample of around 80 AGN and also with this selection, they found that edge-on galaxies only host the more absorbed AGN, finding that from the 11 edge-on sources in their sample, only one is associated with a Sey 1.\\
In this work using the INTEGRAL high energy selected sample of AGN (376 Seyferts), we have confirmed that there is a deficit  of around 24\% ($\pm$ 5\%) of type 1 objects hosted in edge-on galaxies.
Since this bias is not observational, i.e. due to the particular selection of the AGN sample, we deem that this effect
is most likely physical and presumably due to the presence of absorption located in the large scale structure of the host galaxy.
This extra absorption that we called for simplicity galactic, contributes to the total column density observed in X-rays and, even alone, could be sufficient to hide
the broad line region providing a type 2 classification.
The observed axial ratio distribution found in the present analysis can only  be  explained by considering a galactic absorption
lying on the galaxy plane (e.g. inner bars, rings, dust lanes) in addition  to  the nuclear absorber.\\
In this picture, the role played by the orientation  of the two absorbing structures (large and small scale) is obviously more complicated than
in the more conventional unified picture where only the orientation of the torus determines if a source  is classified as a type 1 or 2.
Within this scenario either absorber is capable of attenuating the BLR flux, and so not only the orientation of each with respect to
the line of sight is important but also their relative location and orientation.
Following this scenario, when the torus and the galactic absorber
are both edge-on, much of the absorbing material lies in the shadow of the torus leaving a wide range of angles which provide a direct view
of the nucleus and therefore a type 1 classification.
On the contrary, if the two absorbers are severely  misaligned,  then the absorbing
material, either due to the torus or the galactic absorber, covers a much larger fraction of the nucleus, substantially increasing the
probability that a randomly oriented observer will see a type 2 AGN.
In this case we can have 3 configurations that provide a type 2 classification:
one in which only the torus  is detected, one  where both absorbing structures lie along the line of sight and, finally, one where only a thick layer of galactic absorber is intercepted.
In the first two cases the classification is that of a classical (torus hidden) type 2 AGN where the galactic absorption can eventually
enhance the X-ray column density due to the torus.
In the last case the source is formally not a type 2 AGN according  to the classical unified theory, since the torus is not along the line of sight, but
if  LogN$_{H}>$21.6 and the host galaxy is edge-on, the BLR becomes hidden and the source is optically classified as a type 2 AGN.
In other words, if it were  not for the host galaxy, these would be classified as type 1, i.e. it is the host galaxy that makes them appear as type 2.
Given their relevance, it is important to find some examples of these AGN within our large data-set.
If we assumed that the parsec scale tori are  always Compton thick or nearly so,  i.e. have column density above a few
10$^{23}$ cm$^{-2}$,  then objects with absorption much lower are probably hidden behind galactic material.
Therefore in order to search for {\it "misclassified"} type 1 Seyferts, we  focus on those
Seyfert 1.8, 1.9 and 2 hosted in edge-on galaxies (i.e. having  $b/a$ below 0.5) and have mild X-ray absorption
(below 10$^{23}$ at cm$^{-2}$), i.e. those located in the dashed region of figure \ref{scheme}.
There are 22 such objects in our sample of INTEGRAL AGN, most of which are newly discovered and therefore poorly studied.
For 9 of them broad band information could be gathered and analysed to verify their classification.
These objects are shown in Table 1 where we list their name, presence of bar or dust lanes as  reported in
the literature and evidence, from the near infrared spectroscopy (NIR), for the presence of broad emission lines.
The NIR regime is particularly useful from this purpose since, being less affected by dust extinction, is more likely  to
show a BLR otherwise hidden in the optical band.
The  sources listed in Table 1 are clear examples of how a type 1 nucleus can hide behind absorbing structures
that are located in the host galaxy.
Some objects  like NGC 7172 \citep{Smaji__2012}, NGC 2992 \citep{Trippe_2008}, NGC 5252 \citep{Kotilainen_1995}  and
NGC 5506 \citep{Nagar_2002} have already been discussed in the literature as examples of how a Seyfert 1 can be
disguised as a Seyfert 2 due to galactic obscuration, while the other examples are  suggested here for the first time.
Although with the available observations their number is small (these objects represent 40\% of the sample) and not yet sufficient  to compensate
for the lack of type 1 AGN in edge-on galaxies, their existence indicates this kind of {\it "misclassification"} due to galactic absorption can take place and, if extended to a large
number of objects, might explain  the difference in the  axial ratio distributions of type 1 and 2 AGN.
On the other hand the existence of such objects gives support to the idea
that an absorption located at larger scales is at work within a large fraction of local AGN.\\
As said, now that the co-evolution of galaxies and black holes is well established (e.g. see \citet{2014ARA&A..52..589H}  and references therein)
and the advent of the ALMA observations  probe and image the gas within 100 pc of the AGN, there is beginning to accumulate evidence of multi absorption components.
Mass and gas concentrations in host galaxies which are responsible for the
feeding mechanism in AGN, can also contribute to the obscuration of  their nuclei.
The mechanism appears to be that of kinematically decoupled embedded bars, i.e. the combination of a slowly rotating kpc-scale
stellar bar and a kinematically decoupled nuclear bar, with overlapping dynamical resonances \citep{Combes_2013}.
Such resonances and kinematic decoupling are fostered by a large central mass concentration and high gas fraction.
The gas is first halted in a nuclear ring (a few 100 pc scale), and then driven inward under the influence
of the decoupled nuclear bar obscuring the central engine.
This has been observed in ESO 428-G14, where the measured kinematics is consistent with a nuclear inflow, or inner bar,
which feeds the AGN \citep{2020ApJ...890...29F}.\\
Therefore the picture emerging from recent observations is that this galactic absorption may reside in different structures present in the host galaxy
which include dust lanes, bars, rings etc. In this paper  we focus on their contribution to the  obscuration of the direct radiation from the AGN
especially when the host galaxy is seen edge-on.
With this in mind also Compton thick AGN could be explained as sources in which the two
absorbers on galactic and nuclear scales  are both aligned and seen edge on.
A similar result was also obtained by \citet{Goulding_2012}, studying the deep silicate absorption features seen in many
Compton-thick AGN. \citet{Goulding_2012} found that an important  contribution to the observed mid-IR  extinction in these objects is dust located
in the host galaxy, i.e. due to disturbed morphologies, dust lanes or galaxy inclination angles.
However, these authors  considered these  two absorbers, galactic versus torus, as two alternative absorbing structures while
here we assume that they could be both present in the same object and possibly aligned to enhance the nuclear obscuration.
To produce Compton thick absorption our line of sight intercepts an edge-on torus and the  galactic absorber (like for example an inner bar) can intervene or not
depending if it is  present or not in the host galaxy.
The other possible geometry, i.e. that of a face on torus, either  aligned or not with the galactic absorber,  will always produce a Compton thin source \citep{2019arXiv190713137B}.
Therefore we can say that a Compton thick AGN can have two flavours: one in which our line of sight intercepts
only the torus and one in which both the torus and the galactic structure are seen edge-on.
This last configuration produces objects like ESO 428-G14 and those  discussed by \citet{Goulding_2012}.
We note  that the deep silicate absorption features observed in \citet{Goulding_2012} sample, cannot be explained
in terms of torus absorption models (see for example \citet{Garc_a_Gonz_lez_2017} ) and can only be produced by dust on
galactic scales.

\section{Summary and Conclusions}
Using the hard X-ray selected sample of AGN detected by INTEGRAL/IBIS, in this work we have investigated  the possible
contribution of  absorbing material located on a scale of hundreds of parsecs, i.e. in the host galaxies, to the total amount of
N$_{H}$ measured in the X-ray band.
By collecting  the axial ratios  ($b/a$) of the host galaxies  for all our sample sources,
we have verified that also within our hard X-ray selection sample there is a deficiency of around 24\% ($\pm$ 5\%) of type 1 AGN hosted in edge-on
galaxies (those with $b/a < $0.5).
We have investigated the distribution of the host galaxies axial ratios in type 1 and type 2 AGN and further highlighted
the optical Seyfert subclasses (type 1.5 for the unabsorbed and type 1.8 and 1.9 for absorbed AGN) to check whether there
is a trend of the optical class with the inclination of the galaxy, in other words, we checked for the presence of
absorption able to hide the BLR, or part of it, in the different galaxy axial ratios, and we found none.
Possible bias in redshift has been excluded. We found the same effect in a well determined range of
$z$ (0.026 $< z <$ 0.095) where the number and the distributions of the two classes are statistically
the same (at 99.9\% confidence).
Clearly this indicates that some material located in the host galaxy on scales of hundreds of parsec and not aligned
with the putative absorbing torus of the AGN can contribute to the column density measured in the X-ray band.
In particular we have developed a scheme of the expected AGN type as a function of X-ray absorption and axial ratio
in the different configuration of torus and galaxy inclinations: when the torus is seen edge-on, we always have a type 2 absorbed
AGN independently of the host galaxy orientation; when the torus is seen face-on we may have a  type 1 AGN unabsorbed or mildly
absorbed or  "misclassified type 2 objects where the absorption is on galactic scales.
Plotting the axial ratio versus the column density for type 1 and type 2 we have highlighted peculiar sources and  in particular have been able to
identify a set of possible "misclassified type 2 AGN", i.e those which are absorbed (type 2) and located in edge-on
galaxies.
Our conclusion is that these absorptions, galactic versus torus, are not alternative but  could be both present in the same object
and possibly aligned to enhance the nuclear obscuration.
Within this scenario a Compton thick AGN can come in  two flavours: one in
which our line of sight intercepts only the torus and one in which
both the torus and the galactic structure are seen edge-on.

\begin{table*}
\begin{center}
\caption{Possible Misclassified type 1.9/2 AGN}
\begin{tabular}{lcccc}
\hline
{\bf name}                                      &  {\bf dust$^{\dagger}$/bar}  &   {\bf ref} & {\bf NIR BLR } &  {\bf ref}   \\
\hline
IGR J02343+3229= NGC 973       & DC/N               &      1       &      --          &                 \\
IGR J09025-6814=UGC11397      &  --/Y                 &      --       &      --          &                \\
NGC 2992                                     & DC/N               &       2       &     Y           &        3       \\
NGC 5506                                     & D-S/Y              &       4       &     Y            &       5       \\
NGC 5252                                     & R-I/N               &        2       &     Y           &        5       \\
IGR J19039+3344=NGC2788A    &  D/Y                 &        6       &    -              &                \\
NGC 7172                                     & DC/N               &       2        &    Y             &       7       \\
NGC 7314                                     & DC/Y                &       2        &   Y             &       5, 3   \\
IGR J22367-1231=MKN 915        & DC/N                &       2        &    Y            &       5       \\
\hline
\end{tabular}
\end{center}
($\dagger$) Same nomenclature as used by \citet{Malkan_1998}.
Ref: (1) \citealt{Verstappen_2013}; (2) \citealt{Malkan_1998}; (3) \citealt{Onori_2016};  (4) \citealt{Martini_2003}; (5) \citealt{Lamperti_2017}; (6) NED; (7) \citealt{Smaji__2012}.
\label{tab1}
\end{table*}

\section*{Acknowledgements}
The authors acknowledge financial support from ASI under contract n.  2019-35-HH.0.
We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr).
This research has made use of the NASA/IPAC Extragalactic Database (NED) and NASA/ IPAC Infrared Science Archive, which are operated by
the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
Acknowledgements go to Rick White at Pan-STARRS database for his help in finding/interpreting  PS1 tables.
We thank Chiara Feruglio for worthwhile discussion. The authors  also thank Marco Mignoli for useful discussion on
AGN/host galaxy characteristics in optical/IR band, Eliana Palazzi and Andrea Rossi for imaging analysis in optical/IR band.\\
We thank the anonymous referee for useful remarks which helped us to improve the quality of this paper.

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


UTRECHT, Netherlands (AP) — The Latest on the tram attack in the Netherlands (all times local): 10:45 p.m. Dutch police say they have arrested another man on suspicion of involvement in the deadly tram shooting in Utrecht.
Dutch police stand guard outside a house where the suspect of a shooting incident in a tram was arrested in Utrecht, Netherlands, Monday, March 18, 2019. A gunman killed three people and wounded nine others on a tram in the central Dutch city of Utrecht.
A forensic expert looks for clues in a house where the suspect of a shooting incident was arrested in Utrecht, Netherlands, Monday, March 18, 2019. A gunman killed three people and wounded nine others on a tram in the central Dutch city of Utrecht.
Police said in a statement late Tuesday that the 40-year-old man was arrested in the afternoon by heavily armed officers in Utrecht. They say the man "is suspected of involvement in the shooting. His role is under further investigation."
Police say that two other men arrested following Monday's shooting that left three people dead and three seriously wounded have been released and are no longer considered suspects. The main suspect, 37-year-old Gokmen Tanis, remains in custody.


text:
El Niño Update: Chances for weak to moderate El Niño move higher
There is an approximately 65% chance that El Niño conditions will be present during the Northern Hemisphere winter and last into the Northern Hemisphere spring 2015, NOAA\'s latest El Niño climate predictions show. This is up from 58% predicted in the November report. Australian authorities say there is at least a 70% chance that El Niño will be declared in the coming months.
There is an approximately 65% chance that El Niño conditions will be present during the Northern Hemisphere winter and last into the Northern Hemisphere spring 2015, NOAA\'s latest El Niño climate predictions show. This is up from 58% predicted in the November report.
Similar to last month, most models predict sea surface temperature anomalies to be at weak El Niño levels during November-January 2014-15 and to continue above the El Niño threshold into early 2015 (Fig. 6). Assuming that El Niño fully emerges, the forecaster consensus favors a weak event. In summary, there is an approximately 65% chance of El Niño conditions during the Northern Hemisphere winter, which are expected to last into the Northern Hemisphere spring 2015 (click CPC/IRI consensus forecast for the chance of each outcome).
Meanwhile, the Australian Bureau of Meteorology said many climate indicators remain close to El Niño thresholds, with climate model outlooks suggesting further intensification of conditions remains likely. The Bureau's ENSO Tracker status is currently at ALERT, indicating at least a 70% chance that El Niño will be declared in the coming months. Whether or not an El Niño fully develops, a number of El Niño-like impacts have already emerged.
Several ENSO indicators are currently close to, or exceed, El Niño thresholds. These include tropical Pacific Ocean temperatures, which have now exceeded El Niño levels for a month, and the Southern Oscillation Index, which has remained at or near El Niño levels for three months. Other indicators, such as tropical cloud, trade winds and rainfall patterns, have either remained near average or only temporarily approached thresholds. This indicates a typical El Niño ocean–atmosphere interaction may not be fully locked in.
The majority of international climate models surveyed by the Bureau suggest further warming of the tropical Pacific Ocean is likely, so it also remains possible that the ocean and atmosphere will fully couple in the coming weeks to months. If an El Niño is established, models suggest it will be weak, or moderate at most. Some El Niño-like impacts have already been seen this spring in Australia and several regions around the globe, including Asia, South America and southern Africa.
AFRICA - Insect feed among joint Australian and Canadian research projects to address food insecurity
MALAYSIA - AwF makes Asian connection to professionalize the aquaculture supply chain

redpajama_set_name: RedPajamaCommonCrawl


High in the hills of Echo Park, Blackbirds is a micro-neighborhood inspired by the architectural heritage of its surrounding community. Designed by renowned Eastside architect, Barbara Bestor, Blackbirds appeals to those looking for a timeless, modernist home. Interiors feature custom lighting by Brendan Ravenhill, polished concrete and white oak flooring, custom cabinetry and floor-to-ceiling bookshelves.
Rooftop decks, private yards and expansive windows take full advantage of sweeping canyon views while still being mindful of privacy. Landscape design by Mia Lehrer + Assoc enhances a central living street – and features Afghan pine and honey locust trees, Mexican elderberry, lavender and feather grass. Singular in design and intent, these carefully crafted homes offer a living experience like no other.
For more information about this beautiful home or to schedule a private showing, call or email Grant Linscott at 323-333-6222. You can also email me for details about other development and properties in the Echo Park area. If you or someone you know is looking to buy or sell, I'd love to help you with any of your Real Estate needs!
Previous PostPrevious 1417 Kellam Ave.


text:
Wise Aesthetics – Carmel
The Wise Choice
Delivering Excellence in Medical Aesthetics & an Exceptional Customer Experience
Photography Provided by Abbie Gowen
Whenever anyone asks Crissy Wiseman, NP-C what she does for a living, she tells them that she has the best job in the world.
"I get to make women feel better about themselves so when they wake up in the morning, they like what they see in the mirror," Crissy says. "Nothing is better than helping boost someone's self-esteem and confidence."
Crissy has been a registered nurse for 23 years, a nurse practitioner for 13 years and has worked in the aesthetics industry for many years alongside some of the top plastic surgeons in the nation. Now, Crissy is the proud owner of Wise Aesthetics, a premier medical spa that offers clinical facials, laser treatments, hair reduction, skin tightening, cellulite treatment, and every quality injectable on the market.
"We do CO2 laser peels, chemical peels, radiofrequency microneedling, hydrafacials, HALO and photofacials with Intensed Pulsed Light (IPL) and BroadBand Light (BBL), which are great treatments for everyone to get in the fall to correct sun damage," Crissy says.
Wise Aesthetics' services also include PDO thread lifts, a minimally invasive alternative to a surgical face and neck lift, often used in combination with other therapies like laser treatments, RF microneedling, dermal fillers and chemical peels. They also offer Kybella/deoxycholic acid to treat double chin and Laser Genesis, which stimulates new skin cells and collagen growth.
Everything they do is clinical, but that doesn't mean the atmosphere is sterile. At Wise Aesthetics, clients enjoy a luxury experience with professionally trained, friendly staff.
"There are a lot of nurses and nurse practitioners breaking into the industry, which is saturating the market, but many have very little experience," Crissy says,"Our three aestheticians and nurse have a significant amount of experience and are highly trained."
Crissy is keen on keeping herself and her staff skilled in all the latest techniques and procedures by regularly attending training and conferences. Crissy has and continues to train with experts from all over the world.
The first thing Crissy does when a client comes to see her is develop a plan based on their individual concerns or frustrations. No one client is the same. No one appointment is the same.
"We develop an interdisciplinary plan," Crissy says, "We may start with skin care by prescribing medical-grade skin care products and laser resurfacing. The patient then may require injectables to treat their specific concern. Everything we do is customized to the patient with the intention to achieve the desired result."
And those results are all nonsurgical.
"That's our big focus because most people we see don't want to have surgery," Crissy says. What's more, most of these treatments have little to no downtime, which is important because people want to go about their daily lives.
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"I'm 45 – I know what it feels like to age, " she says with a chuckle. "But the great thing is that there are non-surgical treatments that we can do to help, if not turn back the clock, to at least slow down the process by using the tools we have to stimulate collagen production and other techniques that complement the aging process."
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"It's crazy how often I hear, 'I don't want to look like my mom,'" says Crissy, who specializes in what she calls a "global face rejuvenation." For instance, if somebody comes to her and asks her to make their lips bigger or fuller, Crissy knows that making that change will cause other features of their face to look different. Therefore, she looks at the face holistically and treats the areas that need to be treated in a natural way. This is precisely why her clients call her an artist.
"I'm so thankful for Crissy's artistic eye and knowledgeable mind," says client Elizabeth Wyeth. "Crissy has a vision and a plan. I love the symmetry, balance and natural look that she creates."
"It takes a certain eye to do what we do and be good at it," says Crissy, who couldn't be prouder of the team she has assembled.
"We're like a family," she says. "The fact that I've been able to attract these highly experienced people to come work with me is a dream come true."
Crissy is currently working with a designer to renovate their current space to add four more treatment rooms, administrative offices and a luxurious and cozy reception area for patients. Down the road she hopes to expand her practice and hire additional experienced medical professionals and aestheticians.
Her clients are thrilled to get a chance to see Crissy and her team. As client Jenny Ferree says, "My face isn't something I want to find the cheapest injector or product. I want someone who is educated, experienced and treats her clients like friends. I love my lips and love that my eyes no longer have that tired-mom look."
Wise Aesthetics is located at 2325 Pointe Parkway, Suite 110 in Carmel.
For more information, call (317)569-6448, email info@wise-aesthetics.com, or visit www.wise-aesthetics.com.
Wise Aesthetics, Pointe Parkway, Carmel, IN, USA
https://wise-aesthetics.com/


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text:
"THE HOUR OF TEMPTATION"
IS IT in vain that the Lord instructed His people that the closing time of this Gospel Age would be an "hour of temptation" coming upon the whole world? (Revelation 3:10.) Surely we have not been taught of the Lord in vain! and so, all loyal to Him are buckling on the breastplate, the helmet and the sandals, and are taking the sword and the shield. If we have not yet entered into fierce conflicts, we know that we are to expect them; and we should be prepared, and have such practise and experience as would enable us to acquit ourselves valiantly in "the hour of temptation."
Since we are instructed that this "hour of temptation" cometh upon the whole world, as well as upon the Church, we perceive that it must be something in the air, as it were, that would affect everybody. We believe that this temptation is a thing spreading itself gradually in every direction; and the Master assured us that unless these days would be cut short by the establishment of His Kingdom in the hands of the Elect, no flesh would survive.
We understand this to mean that the spirit of selfishness and ambition, which is already operating among the nations and driving them insanely to war for commercial supremacy, is the spirit which will increase more and more, and will involve everybody, everywhere. This spirit is seen in the strikes, etc., of our own land—everybody anxious to serve self, and willing to fight for honors, privileges, positions, etc.
But we are more interested in the Church and in seeing how this "hour of temptation" will involve the Lord's people. What we are about to write is far from what we would prefer, but it seems to be our duty as respects the Lord's Cause and people. We believe that a great crisis is upon the Bible students; and that the sooner it is discerned, the more successfully it may be passed. It may mean divisions; but as the Apostle remarked, divisions are sometimes necessary that the approved course and the approved doctrines and the approved methods may be discerned, and that the true teachers be the more fully appreciated.—1 Corinthians 11:18,19.
Before mentioning the sad feature, we mention one for general encouragement; namely, that, so far as we can discern, through intercourse with the friends at conventions, etc., there was never a time when the rank and file of Bible Students possessed such a spirit of meekness, gentleness, patience, love, intelligence, faith, joy, as now.
"TAKE HEED TO YOURSELVES"
It causes real grief to write that much of the difficulty and danger to the Church seems to lie at the door of the Elders and Deacons—not all, thank God, but apparently a small minority of them, judging from the queries which come to the Office from time to time from the bewildered sheep, who seek advice as to their proper course. The [R5981 : page 328] true, loyal servants in the Church should be all the more appreciated by the Lord's people in proportion as they realize the difference between true Elders and Deacons and those who are untrue. Nor are we writing with a view to the discouragement of the unfaithful, but rather to open their eyes to the true situation, that perchance they may be recovered out of the snare of the Adversary and become helpers of the Lord's Flock, instead of hinderers.
So far as we are able to judge, the same conditions prevail today amongst Bible Students which the Apostle pointed out to the Elders of the Church of Ephesus when he charged them: "Take, therefore, heed unto yourselves and all the Flock, over which the Holy Spirit hath made you overseers, to feed the Church of God which He hath purchased with the blood of His own [Son]." (Acts 20:28.) St. Paul's prophecy came true: "After my departing shall grievous wolves enter in among you, not sparing the Flock. Also of your own selves shall men arise, speaking perverse things, to draw away disciples after them. Therefore watch, and remember that by the space of three years I ceased not to warn every one night and day with tears. And now, Brethren, I commend you to God, and to the Word of His grace."—Acts 20:29-32.
COURSE OF TWO OF GOD'S SERVANTS CONTRASTED
As it was ambition which first misled Lucifer, and converted a glorious servant of God into an adversary, so it is his spirit that has been dangerous all the way down. The spirit of our Master was the very reverse of this. "He humbled Himself, even unto death," in the doing of the will of the Father. We see nothing of the spirit of pride or ambition or self-seeking of any sort in our Master. We are warned by the Apostle to humble ourselves after His example, if we desire to be exalted with Him in His Kingdom.
But how many seem to forget entirely these Scriptures, which we so frequently bring to the attention of the Lord's people as essential to our attaining to any position in the Kingdom! From reports given us, a horrible state of affairs prevails in some Classes when an election is to be held. The servants of the Church attempt to be rulers, dictators—sometimes even holding the chairmanship of the meeting with the apparent object of seeing that they and their special friends shall be elected as Elders and Deacons. We have heard of cases in which an Elder refused to speak to one of the Congregation because the latter had not voted for him. Yet doubtless that very Elder would think himself the personification of modesty, humility and meekness.
Oh, for shame that such a spirit should have any place amongst those who have any knowledge of the teachings of God's Word and of the conditions upon which we may hope for joint-heirship with the Master! Of course, there are various degrees of brazen-facedness in such matters. Some quietly try to take advantage of the Class by having the election at some time which is especially favorable to them and their friends. Others seek to pack the meeting with their friends, bringing in comparative strangers, who have no thought of being regular in attendance at the Class, but come merely as an act of friendship to vote for one of their friends.
Additionally, it may generally be expected that such as manifest an ambition of this kind to be leaders and teachers and to ignore the principles of the Golden Rule, as well as the special instructions for the New Creation, are generally the ones who bring in false doctrines. The same ambitious spirit of the Adversary which leads them to strive for honor in the Class seems to lead them on to pose as great teachers—bringers forth of new light. This also, the Apostle explains, is a characteristic of Satan. He says, "What wonder if he transforms himself into an angel of light"—makes himself to appear a leader amongst the children of light.—2 Corinthians 11:14.
In many cases, the Classes are solely to blame, according to their own statement. In some instances, persons have been elected to Eldership who had not even made a profession of consecration to the Lord or who had not symbolized their consecration. Why? Because the Class happened to be without any special talent, and the one who was not a Brother at all, not a New Creature in Christ, was chosen because he had some speaking talent. What could we expect from such a one being exalted to the position of a teacher amongst Bible Students? We could expect only injury to the Cause and injury to the person thus pushed forward contrary to the directions of the Lord's Word. If the natural man cannot receive the things of the Spirit himself, how could he communicate things of the Spirit to the Lord's consecrated ones? How could we expect the Lord to guide such a one, who had not given over his life to be a footstep-follower of the Lord and to be instructed by His Word?
The selection of improper leaders is evidently a sin, and quite a reflection against the Classes who have the improper leaders. How could such get into positions to represent the Lord's people, except by the latter's votes? When will the Lord's people learn that ability to talk in public is only one of the qualifications of an Elder? Time and again we have noted how the Lord's Cause has been hindered, and spirituality amongst the brethren has been stifled, by attempts to imitate the nominal church in putting forward persons glib of tongue, lacking in spirituality.
In such a case, is it not pride on the part of the Class—a desire to make a fair show in the flesh before the world? If not, why do they elect such persons? If they have made a mistake, why do they not at once rectify it in a quiet and positive manner? When Elders seek to bring the Class under their power and control and succeed, does it not show that the Class lacks the very quality that the Lord tells us He desires to see—courage, overcoming? And does the Class not injure such a would-be ruler, as well as itself, by permitting him to succeed in his unscriptural methods?
"DECEIVING AND BEING DECEIVED"
We have already alluded to the ambitious and selfish spirit in the world leading on to anarchy; and we have just pointed out how the same selfish, ambitious spirit is leading on to anarchy in the Church. We foresee a Time of Trouble for the world upon this score, and a Time of Trouble also for the Church. The world cannot purge itself of this class; for the leaders and the led have the worldly spirit, which is sure to wax worse and worse. But not so in the Church of Christ. Ours is the spirit of the Master, the spirit of loyalty to Truth, the spirit of the Golden Rule, the spirit of brotherly love, the spirit of liberty and helpfulness, the spirit of fidelity to what we believe to be the Truth. It is inexcusable for the Church, possessed of this spirit, to continue under the domination of ambitious men (and sometimes ambitious women). If they have not been conducting their Class affairs along proper lines, should they not begin at once? We believe that this is the time in which to set the House of the Lord in order.
But some one will say, "We would have a great disturbance if we attempted to do anything contrary to the wishes of those who have fastened themselves upon us as our leaders and rulers. To make a move at all, would endanger a division of the Class, and how could we think of anything which would result in that catastrophe?"
But, we inquire, which would be the better, to have a [R5982 : page 329] smaller Class operating along the lines which the Lord has indicated, or a larger Class upholding principles contrary to the Lord's provision, injuring themselves, hindering their influence, and encouraging as a leader one who is either a "wolf" or else a "sheep" which has been mistakenly misled into the wolf spirit? We encourage all the dear Brethren who are in such trouble to be very heroic; to see that they do nothing from strife or vain-glory, but everything in the spirit of meekness and love, that they may get back again to the liberty wherewith Christ made free, and be not again entangled in any human bondage.
REMEMBER DOCTRINAL TESTS ALSO
Repeatedly Bible Students write us that their Elders try to hinder them from the use of the WATCH TOWER SOCIETY'S publications as textbooks in Bible Study. Some of these Elders go so far as to tell the classes that they are out of harmony with many of the things in these textbooks. Sometimes, as rulers, they forbid the use of these in the classes. We are asked what should be done under such circumstances.
We reply, Let those who wish to follow such leaders do so—that is their right. We shall wish them well. But let us not follow with them nor submit for a moment to such arrangements. It is the height of impertinence for such a leader to intrude himself in such a manner, and attempt to tell the Church what they shall and what they shall not do. As the power of election is in the hands of the Church, so the power of dismission is in their hands. We recommend that such Classes vote to dismiss such an Elder from his position of service, telling him kindly that his services are no longer desired. Perhaps with a back seat for a while, and an opportunity for thinking over the matter, he may be benefited himself, and the Class also be greatly helped forward by taking such a stand—no matter whether there be no other person in the Class able to address a public meeting or accustomed to leading Classes. Far better would it be to appoint any one of your number to act as chairman, or to take turns in the matter of opening and closing meetings—anything to preserve your liberty and to continue the work of worship and study along proper lines.
Let us make a discrimination between the positive teachings of the Bible—the doctrines of Christ—and the slightly variant ways of expressing those doctrines. We are not to expect any two persons to use exactly the same words; but there are certain doctrines which are fast and immovable from the viewpoint of the majority of Bible Students. Any one not in good harmony with those presentations should not be encouraged in the slightest degree, but, on the contrary, should be discouraged. If he has different views, do not persecute him—do not follow the style of the Dark Ages, but follow the proper course of letting him "flock to himself," or with as many as prefer to view matters as he views them.
We have not given such strong advice heretofore; but we perceive that many of the dear sheep are being troubled, hindered of development and imposed upon. We see that proportionately such Elders and Deacons are growing more bold, and hence the need is the greater that all who do have the right spirit, and who realize that, under the Lord's guidance in our study of the Divine Plan of the Ages, we have not been following "cunningly devised fables," should now take a positive stand for the good of themselves, for the good of the leaders who manifest a wrong spirit, and for the good of the public, who are inquiring for the way of the Lord as never before.
While we are encouraging positiveness and courage, we are not wishing to encourage a spirit of strife, or of nagging and fault-finding amongst the faithful servants of the Lord who do manifest the humble spirit and who do accord the Class its rights and liberties and who seek to "serve well." Again we repeat, "Let nothing be done through strife or vain-glory, but all to the glory of God," and with the sole object in view of purging the Church of the influence of those who never should have been chosen, or having been chosen in proper condition, have since manifested a perverted and ambitious spirit. Again we counsel for these positiveness, but kindness and, if they repent, mercy—with a view possibly to restoring them to confidence later on. The Apostle wrote, "I hear that there are divisions among you; and I partly believe it. For there must also be heresies among you, that they which are approved may be made manifest among you." (1 Corinthians 11:18,19.) Here the division evidently must come; and evidently the sooner it comes, the better it will be for the Truth and for all who love it.
"BY MY SPIRIT, SAITH THE LORD"
We should never forget the Apostle's instruction, "The natural man receiveth not the things of the Spirit of God, neither can he know them, because they are spiritually discerned." (1 Corinthians 2:14.) Additionally, experience demonstrates to us that even after we have been begotten of the Holy Spirit, our ability to understand spiritual things depends, not only upon our study of the Scriptures, which are able to make us wise, but also upon the measure of the Holy Spirit which we possess. Hence the Apostle's exhortation, "Be ye filled with the Spirit!"—Ephesians 5:18.
This means that only the spirit-begotten may understand the deep things of God at all; and that their understanding would be in proportion as they attain more and more a filling, a saturation with the spirit of holiness, the spirit of God, the spirit of Christ, the spirit of Truth. Every Bible Student should realize that if, as a New Creature, he walks after the flesh and not after the Spirit, his mind will become more or less darkened, and not only will his ability to understand the deep things of God decrease, but even his recollection of the Lord's Word will decrease; and that, on the contrary, when he is living near to the Lord—walking after the Spirit and not after the flesh—his memory of the Divine Word and his ability to appreciate its Spirit are increased.
Additionally, let us remember that a correct understanding of the Lord's Word is not enjoyed by all the educated and talented, but comes to those who are of a meek and teachable heart, who study the Lord's Word and who live it and absorb its spirit. Thus we have illustrated to us the Divine declaration, "Not by might [greatness], nor by power, but by My Spirit, saith the Lord of Hosts."—Zechariah 4:6.
The lesson to us is that no matter how great, no matter how able any brother or sister may be, this will not make such fit to be a leader of the Lord's people unless he have additionally the all-important items—first, a knowledge of the Lord's Word; and second, the possession of a good degree of the spirit of Truth—one who always dare be trusted as an ambassador of the Lord. None others should be recognized as teachers or leaders amongst the Lord's people. It is the thought of Churchianity that only the great, the learned, the talented, should be the ministers of the Lord's Word; but the Bible's presentation is to the contrary of this. "The spirit of the Lord God is upon Me, because He hath anointed Me to preach the Good Tidings to the meek."—Isaiah 61:1.
It is in view of these things that we feel justified in urging upon the Classes of Bible Students everywhere that they esteem with double honor such Elder brethren as manifest the Spirit of the Lord, the spirit of meekness, the spirit of gentleness, the spirit of patience, the spirit of long-suffering, the spirit of brotherly-kindness, and the spirit of love—those who have a good knowledge of the Word of God and of the Divine Plan, and who manifest an appreciation of the Spirit of Truth, the Spirit of holiness, and who have an aptness to teach; and that on the contrary, all others be refused.
THE V.D.M. QUESTIONS
Long ago we called attention to the fact that many of the titles applied by the nominal church to their ministers are wholly un-Scriptural—Reverend, Most Reverend, Doctor of Divinity, etc. They are not only opposed to the letter, but also to the spirit of the Scriptures. We called attention to the fact that the words Elder, Deacon and Pastor are Scriptural terms. We also called attention to the Latin title, Verbi Dei Minister (V.D.M.), and stated that this expresses exactly the Bible thought that every representative of Christ who preaches in public is a Minister of the Divine Word—not a minister of human creeds or of self. All Bible Students approved of God and of His people are of necessity Ministers of the Divine Word—each according to his talents, opportunities and restrictions, as set forth in the Bible.
In view of the fact that quite a good many Classes of Bible Students seem to be not sufficiently particular in respect to the qualifications of those whom they choose as their representatives, we formulated a number of questions styled, V.D.M. Questions, believing that the study of these questions would be helpful to everybody, and that the answers of them would help to mark out such as have a reasonable knowledge of the Divine Word, and whose ministries, therefore, it might be hoped would be profitable and not injurious. These questions are not sectarian, but would be proper for any minister of any denomination. Neither are they catch questions, intended to trip up the unwary. They are simple bona fide queries, the answering of which should be helpful to each individual, and especially helpful in designating those fit to be teachers and leaders amongst the Lord's people.
These we prepared and sent to the Pilgrims—the traveling preachers sent forth under the auspices of the WATCH TOWER BIBLE AND TRACT SOCIETY, and to all representatives of the Society in any capacity everywhere. Next came applications from Elders and Deacons in [R5983 : page 330] various quarters, and from others of the Bible Students. Then we advised that the questions be studied and answered, as formulated, by all Bible Students. We received many applications, and many of these have been filled out and returned. It is our recommendation to all the Classes that any brother not able to answer these questions in a reasonable way be not considered a suitable representative.
In order that all Bible Students may have these questions and note their simplicity, we publish them below. Brothers Sturgeon, Burgess and Stephenson have been appointed a committee to examine the answers sent in by the Pilgrims. We have no doubt that every one of their answers will be found satisfactory as a whole. None will be rejected except for good cause, and this will be duly pointed out. By vote the New York City Class decided that none should serve it as Elders or Deacons who could not give a reasonably satisfactory reply to these questions. We suggest a somewhat similar course in all the Classes. The examiners of the answers could either be a committee from the Class or, if desired, the Society's representatives above mentioned, to examine the answers and give their criticisms upon request.
V.D.M. QUESTIONS FOR ADVANCED BIBLE STUDENTS
(1) What was the first creative act of God?
(2) What is the meaning of the word "Logos," as associated with the Son of God? and what is signified by the words Father and Son?
(3) When and how did sin enter the world?
(4) What is the Divine penalty for sin upon the sinners? and who are the sinners?
(5) Why was it necessary for the "Logos" to be made flesh? and was He "incarnated"?
(6) Of what nature was the Man Christ Jesus from infancy to death?
(7) Of what nature is Jesus since the resurrection; and what is His official relation to Jehovah?
(8) What is the work of Jesus during this Gospel Age—during the time from Pentecost until now?
(9) What has thus far been done for the world of mankind by Jehovah God? and what by Jesus?
(10) What is the Divine purpose in respect to the Church when completed?
(11) What is the Divine purpose in respect to the world of mankind?
(12) What will be the fate of the finally incorrigible?
(13) What will be the reward or blessings which will come to the world of mankind through obedience to Messiah's Kingdom?
(14) By what steps may a sinner come into vital relationship with Christ and with the Heavenly Father?
(15) After a Christian has been begotten of the Holy Spirit, what is his course, as directed in the Word of God?
(16) Have you turned from sin to serve the living God?
(17) Have you made a full consecration of your life and all your powers and talents to the Lord and His service?
(18) Have you symbolized this consecration by water immersion?
(19) Have you taken the I.B.S.A. Vow of holiness of life?
(20) Have you read thoroughly and carefully the six volumes of STUDIES IN THE SCRIPTURES?
(21) Have you derived much enlightenment and benefit therefrom?
(22) Do you believe you have a substantial and permanent knowledge of the Bible which will render you more efficient as a servant of the Lord throughout the remainder of your life?
Note: It is, of course, expected that each person filling out one of these reports will do so from his own knowledge and not by inquiring for or copying the answers of others. The BIBLE, STUDIES IN THE SCRIPTURES and TABERNACLE SHADOWS may be consulted, however, and citations given.
SUPPOSED OBJECTIONS ANSWERED
One, and only one, objection was raised to the foregoing—a fear that it is Babylonish, Sectarian. Ah! it is wonderful how the great Adversary strives always to make out that the right is wrong, that the light is darkness. Babylon's method is to take all power and authority out of the hands of the people of God and put it into the hands of one person or a clique of preachers or bishops or elders. Our aim continually is to preserve the liberty of each ecclesia and have each recognize its own authority and responsibility.
Our reply to the objecting Brother may be of interest to all of our readers, and so we present it below:
DEAR BROTHER:—I am glad to see you scrupulously careful of all of the rights and liberties of the Church of God, and careful to oppose anything that would seem to savor of sectarianism.
I remind you that sectarianism is an attempt on the part of many companies or classes to control each other in matters of doctrine and practise. We are suggesting nothing of this kind, but feel as much opposed to it as you do. We are not attempting to establish any law or rule which must govern all the classes of the Lord's people, but merely suggesting to them the establishment of law and order in their own midst, by themselves.
For instance, each member of every class in voting for Elders and Deacons should certainly consider before voting the qualifications of those for whom he votes: (1) What [R5983 : page 331] are his religious professions as respects faith in the teachings of the Bible on the fundamental points; (2) Whether or not the one to be voted for is clear in his understanding of the Truth so as to be apt at teaching it to others; (3) Whether or not the individual has made a consecration of himself to the Lord and has symbolized it; (4) Whether or not the individual manifests a high standard of morals in his deportment, and whether or not he is in sympathy with high ideals such as are represented in the Vow.
Heretofore, the classes have been obliged to surmise on these subjects, and our proposal now is that they do not surmise, but ask the brethren our list of V.D.M. Questions or any other set of questions which the class may prefer, and have their answers to these questions before deciding that they are suitable representatives of the class as its honored servants. This maintains the authority of the class, the Ecclesia, as no sectarian system does, and makes the class the judges of the qualifications of its representatives as the Bible directs should be shown by the stretching forth of the hand and the ordaining or authorizing of the individual to serve as a representative of the class.
Your letter intimates a query as to the propriety of appointing three brethren to examine the answers to the V.D.M. Questions.
I reply that each class certainly has the right to recognize or appoint certain brethren in whose judgment they would have confidence to examine the answers given to the questions, and to report if any of them were answered unsatisfactorily in their judgment—so that the class could have the final decision. This seems to be an easier way than to have each member of the class read over the answers to the questions before voting. However, the matter is one for the class to decide. In the case of the New York City congregation, the vote was unanimous that all would have confidence in the broad-minded decision of the three brethren approved as a committee of examiners.
In respect to the Vow: Your letter seems to intimate that you have some opposition to it, and think an acknowledgment of its principles should not be required. Instead of saying what there is in the Vow that you object to, you hide behind the proposition that the expressions of the Vow are not found in that particular form in the Scriptures. I remind you that nothing in the English language is found in the Scriptures, because they were written in another language; and furthermore, that our hymns are not found in the Scriptures, and that what we believe to be clear statements of our faith are not found in the Scriptures in the very terms in which we would express them today. The Scriptures lay down for us the general principles of righteous living, and the true foundations of the faith once delivered unto the saints. We are to see to it that all that we sing and preach and pray and write and do is in line with these fundamental principles which the Bible sets forth. The great mass of THE WATCH TOWER readers have informed us that they believe that the phraseology of the Vow is in full harmony with the essence and spirit of the Word of God. If it is, and any brother finds himself in opposition to it, is he not finding himself in opposition to the spirit of God's Word? and if so, would he be a suitable representative of any class of Bible Students, as its Elder or Deacon? We think not. If any fault can be found with the Vow—if it can be shown to be in any sense or degree antagonistic to or out of harmony with the letter and essence of the Word of God we want to know it in no uncertain terms—all Bible Students would want to know this. But no one has yet shown any antagonism nor any deflections in the letter and spirit of the Vow from the letter and spirit of the Bible. We therefore advise all classes that anybody unwilling to assent to the Vow, unwilling to make it his own, has something the matter with him—either his head or his heart, in our judgment, must be out of harmony with the letter and spirit of God's Word and he would not be a suitable Elder or Deacon.
I trust, dear Brother, that as you read this over and ponder [R5984 : page 331] it and pray about it, you will realize that you have erred in your first judgment; or if you think of any points that I have not covered and thoroughly answered, it will afford me pleasure to have you state those points.
I here remind you that this Vow is unto the Lord, and not unto the brethren! We hold therefore that any one who declares that he has taken the Vow, has not brought himself thereby under bondage to any of the brethren; but merely declared to the brethren the obligation he has recognized and declared to the Lord—hence it would not be the province of the brethren to investigate the affairs of the brother who declares he has taken the Vow, any more after his declaration than before it. The keeping of that Vow is between the individual and the Lord. It neither adds to nor diminishes his responsibility to the brethren and the class. His declaration that he has taken the Vow merely informs the brethren of the high standard of moral living which he recognizes and is seeking to follow.


While many people are aware of the first time home buyer's tax credit of up to $8,000 and that it was extended recently. What most people aren't aware of is a tax credit for homeowners who currently own a home now. A credit for 10% of the purchase price, up to $6,500.
A few caveats: You must have lived in your current home for five out of the last eight years, and there are income qualifications- up to $225,000 for a couple of their adjusted gross income and $125,000 for single filers. You also must be in contract by April 30th and close by the deadline of June 30th of this year.
If you or a friend are considering selling this year, it may make sense for you to sell now and take advantage of keeping some major money in your hands.


text:
Q: numpy csv import problem I am having some difficulty with importing data from a .csv file. I am simply trying to import the data and print the max value. Here is my code:
>>> x, y = numpy.loadtxt('data.csv', delimiter=',', usecols=(4,5), unpack=True)
>>> print 'max =', max(x)

When I enter the above code, I get the following error message:
TypeError: 'numpy.float64' object is not iterable

I tried to change the data type using the dtype=int argument, but it threw the same error. Does anyone have any idea what could be the problem? Thanks in advance for your help!

A: The output of loadtxt() is unfortunately a bit inconistent:  If there is only one line in your file, x and y will be scalars, but for more than one line, they will be arrays.  The Python built-in max() only works for iterables, so it only works in the latter case.
Using the Python built-in max() function instead of numpy.max() is inefficient for NumPy arrays anyway.  So a solution is to use
print x.max()

or
print numpy.max(x)

in the second line.

redpajama_set_name: RedPajamaStackExchange


Jessica Earhart (pronouns she/they) is a multidisciplinary artist based in Pittsburgh, PA. Collage is her primary medium, where she finds satisfaction in its impulsivity, limitations, and as an expressive way to problem solve. She creates art as a means to understand the human experience addressing feminist themes through surrealism. Her work has consisted of both stand-alone pieces and series, as well as zines and comics. She has exhibited at the Cleveland Museum of Contemporary Art, Short Run in Seattle, and the Chicago Zine Fest.
Her ongoing project, Khloris, is a fantasy comic series made with both analogue and digital collage art. The story is about the goddess of flowers and her demi-goddess friends who all possess the power of Chroma, a positive force in the universe that makes everything beautiful and bright. They use this power to smash the patriarchy and make the galaxy a better place! Issue 3 was released in November, 2017. Issue 2 was included in The Best American Comics 2018 Notable Comics list.
Jessica is passionate about mindfulness and self care. When she doesn't have an x-acto knife in her hand, she can be found practicing yoga, making bath products, or baking up a storm.
Her work can be found at: themedialuna.com.


We started in 2007 as an independent design studio. Our goal is the pursuit of new design proposals. Throughout the last years our selection has evolved, becoming a well-edited range of contemporary designs. We look forward to continue envisioning novel design ideas and crafting exciting concepts.