text:
\section{Introduction}
\label{sect:intro}
Integral Field Spectroscopy (IFS) makes it possible to derive spatially resolved and continuously sampled
line-of-sight velocity distribution (LOSVD) 2-dimensional (2D) maps, providing a unique view of
the internal structure of galaxies, as well as detailed morphological and dynamical information, which are essential to
fully understand the physical mechanisms that regulate galaxy formation and evolution.

An increasing number of studies have recently derived the integrated and spatially resolved properties
of a statistical sample of nearby  galaxies  using IFS (e.g.  \citealt{Bacon2001,Thatte2006,Rawle2008,Czoske2008,Scott2012,Fogarty2014,Gonzalez2014,Sanchez2014,Walcher2014}).
Among the most successful, the ATLAS$^{\rm 3D}$ (\citealt{Cappellari2011}) data set provides a complete inventory
of the baryon budget and a detailed 2D analysis of stellar and gaseous kinematics, together with resolved stellar populations
of a complete and statistically significant sample of early-type galaxies (ETGs) in the local Universe.

One of the most interesting results of the ATLAS$^{\rm 3D}$\, team is that it is possible to connect
the 2D features of the line-of-sight-velocity distribution (LOSVD) to galaxy formation scenarios
by comparing these to high-resolution simulations (e.g. \citealt{Naab2014}, hereafter N+14).
For the majority of early-type galaxies ($\sim 86$\%), the formation processes result in disk-like objects
that maintain the axisymmetric shape of the progenitors, while only a small fraction of systems
(the most massive ones, $12$\%) rotate slowly with no indication of disks.
Possible processes that can form embedded disk components include minor mergers,
major merger with disk regrowth, gas accretion events and secular evolution (\citealt{Krajnovic2011}).

It is possible, in principle, to discriminate between the different formation scenarios
by accurately analyzing the higher moments of the LOSVD, the Gauss-Hermite coefficients
$h_{3}$ and $h_{4}$ (representing skewness and kurtosis, respectively) and comparing these to
high-resolution simulations.
Gas has a strong impact on the non-Gaussian shapes of the line-of-sight velocity
distributions (LOSVDs) of the merger remnants.
In particular, when the values of $h_{3}$ and $V_{\mathrm{rot}}$ have
opposite signs, the leading (pro-grade) wing is steeper than the trailing (retrograde) wing. This
indicates the presence of an embedded disk (see e.g. \citealt{Bender1994}).
When an anti-correlation between the $h_{3}$ and the $V/\sigma$ values does not exist but the galaxy
shows a fast rotation profile, the rotation could be have caused by a recent gas poor major merger
that typically does not permit re-growth of a significant disk component (\citealt{Barnes1996, Naab2006,Hoffman2009}, hereafter H+09).
The sign of the $h_{4}$ coefficient distinguishes a peaked shape ($h_{4}>0$) from a flat-topped one ($h_{4}<0$), where the peak
is broad and the wings are narrow.

The age and metal content of galaxies can provide additional important information
about the formation mechanism and its time-scale.
To obtain an unbiased and detailed understanding of the star formation
history of ETGs from their integrated light, it is necessary to study carefully their unresolved stellar
populations, and to break the degeneracies existing between age, metallicity and element abundances (e.g. \citealt{Worthey1994}).
The best way to achieve this is to look at as many stellar features as possible (\citealt{Spiniello2014}, hereafter S+14).
Clearly, in this context, the very narrow wavelength coverage of SAURON is not ideal, since stellar population studies would
rely on only a few well known blue-optical absorption lines (H$\beta$, Mg${\it b}$, Fe5015 and Fe5270).

The VIMOS IFU (VIsible Multi-Objects Spectrograph on the VLT) covers a wider wavelength range
(5250-7400 \AA\, using the blue grism and 6450-8600 \AA\, using the red grism, in its high-resolution mode),
with comparable spectral and spatial resolution, and is clearly a better choice.
This point is particularly relevant after the recent finding that the low-mass end of the Initial Mass Function (IMF)
is not universal and might become steeper with increasing stellar mass and stellar velocity dispersion
(\citealt{vandokkum2010, Treu2010, Spiniello2012, Cappellari2012, Cappellari2013, Dutton2013, Spiniello2014,
LaBarbera2013, Tortora2013,Tortora2014a, Tortora2014b}, but see also \citealt{Smith2015}) or with changes in
other galaxy structural parameters (e.g. compactness, stellar density, size, see Spiniello et al. 2015b, submitted).
Indeed, to constrain the low-mass end of the IMF, it is crucial to look at the red part of the optical spectra,
where most of the gravity-sensitive absorption features are. Some of the most promising indices, like the optical TiO molecular lines
(bTiO, aTiO, TiO1; S+14), can be captured with VIMOS but are outside the SAURON coverage.
Moreover, the SWELLS survey (\citealt{Treu2011Swells}) has shown that there could be one universal
normalization of the IMF for disk-like stellar populations (presumably Chabrier-like) and a "heavier" (Salpeter-like) one for the
older and possibly more metal rich stellar populations found in massive bulges and spheroids (\citealt{Dutton2013Swells}).

Furthermore, 2D integral-field spectroscopy is crucial for constraining the low-mass end of the IMF slope, given the
very recent observational evidence that seems to indicate that the IMF normalization varies
within individual galaxies (\citealt{MartinNavarro2014}; Sarzi, Spiniello \& Krajnov\'ic, 2015, in prep.)
following the velocity dispersion profile (but see also \citealt{Smith2015, Spiniello2015b}).
In this context, a strong observational limitation is the small field-of-view (FOV) of IFS instruments,
typically of the order of tens of arcsec, preventing good coverage of the target galaxies on the sky and a proper spatially-resolved
study of the IMF slope.
Only very recently has a new class of integral-field spectrographs with larger field of view been built to achieve the challenging
task of studying the internal structure of galaxies.
Unfortunately most of them still cover a small range of wavelength and therefore are not suitable for constraining the low-mass end of the IMF
normalization (e.g. VIRUS-P, 3600--6800 \AA,  \citealt{Hill2008}, or CALIFA,  3750--7000 \AA, \citealt{Sanchez2012} in its red configuration).
 The VLT Multi Unit Spectroscopic Explorer (MUSE) represents the perfect solution, combining a large field of view ($1\times1$ arcmin)
 and a wide wavelength range (4650--9300 \AA).
Finally, in the  near future the MaNGA (Mapping Nearby Galaxies at APO, \citealt{Law2014}) project will further improve the situation,
covering the wavelength range 3600--10000 \AA\, up to $\sim 1.5$$R_{\rm eff}$\, with a spatial resolution of $\sim 2.5$ arcsec (and a resolution of R$\sim 2000$).
We refer to Table 1 of \citet{Brodie2014} for a detailed comparison between current and future integral-field surveys.

Thus, at the present day, VIMOS remains among the most competitive instruments for galaxy structure and
stellar population studies, provided that the small FOV is compensated for by mosaic observations, i.e. contiguous
IFU pointings astrometrized and stacked together to create a larger final FOV.

This is indeed the approach we decided to follow in order to attempt
to systematically study the stellar population and the kinematics of the whole surface of nearby ETGs up to almost
the effective radius over a large wavelength range and with medium-high spectral resolution.
Given the challenges in the data reduction, calibration and visualization,
with this paper we present the analysis of one of the galaxies observed in a pilot program focusing on the kinematics
and the stellar population analysis of two flattened galaxies (NGC~821 and NGC~4697)\footnote{
Program IDs P079.B-0622A and P085.B-0949 (P.I. N.R. Napolitano).}.
In particular we focus on NGC~4697, for which we have 8 VIMOS pointings
covering  $\sim80''\times60''$ effective area, which allows us to
investigate regions up to $\sim 45''$ from the galaxy center, i.e. $\sim$0.7~$R_{\rm eff}$\,  ($R_{\rm eff}$ $=66"$ from \citealt{deLorenzi2008}).

\subsection{Target selection and outline of the paper}
\label{sect:target}
NGC~4697 is an E6, almost edge-on galaxy located along the Virgo southern extension,
with evidence of substructures (from {\it HST}  ACS images, \citealt{Lauer1995}) and the presence of a
strong streaming motion component (known since the pioneering work of \citealt{Bertola1975}).
The galaxy is representative of the class of disky, fast-rotating elliptical $L_ {*}$
galaxies (\citealt{Bender1994}), which are candidates for having less dark matter
(\citealt{Covone2004,Napolitano2005,Cappellari2006}) than the boxy, slow-rotators of comparable mass.
As such, it is among the sample of elliptical galaxies whose planetary nebula (PN) kinematics show
surprisingly little sign of a massive dark matter halo (\citealt{Mendez2001,Romanowsky2003,Napolitano2005, Douglas2007,Mendez2009}).
Finally, the spheroidal part of NGC~4697 may well be a large bulge (\citealt{Dejonghe1996}) and therefore
this system is an interesting candidate for testing the SWELLS (\citealt{Treu2011Swells}) claim about the different
normalization of the low-mass end of the IMF slope (universal, Milky Way-like IMF for the disks and more bottom-heavy IMF,
possibly steepening with velocity dispersion for bulges, \citealt{Dutton2013Swells}).

Based on the combined information of the 2D kinematical characterization of the system,
and stellar population analysis, we are able to fully characterize the stellar population of the disk and bulge components of NGC~4697.
This is important {\sl per se} in order to investigate the variation of the stellar populations and IMF slope in different structural components
of the system and possibly to infer a formation scenario for it, but it will also allow us to correctly normalize the stellar
mass of the galaxy in forthcoming dynamical analysis.

The paper is organized as follows: in Section \ref{sect:observ} we outline the observations and data reduction, in Section \ref{sect:kin}
we introduce our kinematical technique and we show 2D kinematical maps as well as 1-dimensional (1D)
kinematics profiles along the major axis of the galaxy. We compare the latter with kinematics profiles in literature.
In particular, in this Section, we highlight correlations between the $h_{3}$ and $h_{4}$ parameters and
$V/\sigma$ and try to connect these to  predictions from galaxy formation simulations.
In Section 4, we focus on the stellar population analysis performed
via line-index strengths  measurements  on the 1D spectra of the disk and of the bulge separately.
We also attempt to constrain the IMF normalization of the two components.
Finally, discussion and general findings are presented in Section 5 together with conclusions.

\placefigfov

\section{Observation and data reduction}
\label{sect:observ}
The integral-field spectroscopic (IFS) observations have been carried out with VIMOS,
the multi-mode wide-field optical instrument mounted on the ESO VLT,
as part of a proposal carried on in two different runs : May 2007 and March 2010, respectively.

The Integral-field Unit (IFU) head of VIMOS consists of a square array of
$80 \times 80$ micro-lenses with a sampling  of $0.67\arcsec$ per spatial element
('spaxel') at the Nasmyth focus of the telescope.
In its high-resolution mode only the central 1600 lenses are used, resulting in a field-of-view (FOV) of $27" \times 27"$.
The seeing was generally below $0.8\arcsec$ during the observations, so that each fiber of the IFU gives a spectrum
that is essentially independent of its neighbors.
All data sets have been taken with the high-resolution
blue grism, covering a wavelength range between $4100 - 6300$ \AA\,
with a dispersion of $0.51$ \AA/pixel.
The spectral resolution of the HR-Blue grism is $\lambda / \Delta \lambda = 2550$, where
$\Delta \lambda$ is the full width at half-maximum (FWHM) of the instrument profile.

In order to cover the effective radius and to have a high S/N among the whole FOV,  we use a mosaic approach.
During the first observation run, we have obtained 6 different pointings,
each made by six exposures of $\sim 800$ seconds, while for the second run we
have obtained 2 pointings along the major axis of the system,  with 4 exposures of $825$ seconds each.
The Position Angle of all pointings has been fixed to $PA=-20°$.
For accurate measurements of the stellar kinematics, one must properly evaluate the sky background
contamination. Since VIMOS does not have sky-dedicated fibers, and the target galaxy covers the entire
field-of-view, it has been necessary to make separate telescope pointings (of $\sim 300$ seconds) to measure
the sky background for each observing night.

\subsection{Data Reduction}
\label{subsect:datared}
Data reduction has been carried out using the VIMOS pipeline (version 2.1.1) by the ESO
``Data Flow System Group\footnote{N. Devillard, Y. Jung, R. Palsa, C. Izzo, P. Ballester, C. Sabet, K. Banse, M. Kiesgen, L. Lundin,
A. Modigliani, D. J. McKay, N. P. F. McKay, J. Moeller-Larsen, L. de Bilbao}",
via the Gasgano data file organizer developed by ESO.
A schematic representation of the data reduction processes performed within Gasgano is provided by \citet{Zanichelli2005}.
The reduction involves standard steps for fiber-based integral-field spectroscopy:
\textit{(i)} Subtraction of a master bias frame created by averaging all the bias frames
\textit{(ii)} Fiber identification (correct association of a fiber position on the IFU mask to a corresponding position
      on the CCD) and correction of the differences in the fiber-to-fiber transmission
\textit{(iii)} Wavelength calibration
\textit{(iv)} Scientific image combination.

We create a final data cube for each pointing by averaging over the final single-observing block (OB)
flux-calibrated science cubes produced by the pipeline
using the IFU tables, with the correspondence between each row (i.e. each spectrum)
of the extracted spectra and the fiber's position on the IFU head.
The four IFU quadrants  are treated independently up to the combination of all exposures  into a single-pointing datacube.

We subtract the median sky spectrum (extracted directly from the `sky frame') from the `science frame'.
Median combining was needed to ensure that any residual contamination from faint objects was removed.
We are confident that this sky-subtraction procedure is accurate enough but, if prominent sky emission lines are
still present in the spectra after sky subtraction, we mask them out during the the stellar kinematics recovery process.
We also investigate possible effects of the differential atmospheric refraction by checking whether or not the
photometric center of the galaxy changes its position as a function of wavelength in the datacube.
We find that the position does not change by more than 2 pixels ($\sim 1.3$ arcsec) between 4000 and 6200 \AA.
Each single-pointing datacube is astrometrically calibrated independently by matching the position of the
photometric center or of a star (when the center is not visible in that particular pointing)
to an {\it HST} ACS image of the central region of NGC~4697. Subsequently,  the different pointings are
linearly interpolated onto a common 3D grid uniformly sampled,  after normalizing them for exposure times,
using a simple grid interpolation \footnote{We interpolate, shift and rotate each single-pointing datacube
by matching the position of the center and the rotational angle into this datacube-container.} to obtain the final mosaic datacube.
As a further check of the robustness of this mosaic reconstruction,
we re-check the WCS astrometry on our final combined image,
using as reference the same {\it HST}/ACS image.

The results of this comparison are visible in
 Figure~\ref{fig:fov} which shows the final reconstructed mosaic image, obtained by averaging the datacube along
the wavelength direction, as well as the ACS image.  Twenty blue isophotes, derived from the {\it HST} image,
 are shown on both images to check the accuracy of our astrometrical calibration. Although most of the point sources visible in
 the {\it HST} image are too faint to be detected in our VIMOS observations, the positions of the center and of a star (ENE)
 coincide between the two instruments.
On the right side of Figure~\ref{fig:fov} we also plot a 1D spectrum extracted at the photometric
center of the galaxy and another 1D spectrum extracted at $\sim 40"$, in a position which is highlighted in the reconstructed FOV
by a small yellow star.

\section{Kinematics Measurements}
 \label{sect:kin}
To recover the line-of-sight velocity distribution (LOSVD) first,
 we apply a spatial binning method in order to increase the signal-to-noise ratio (S/N)
over the single-fiber spatially resolved spectra of the final datacube (Section 3.1).
Then we measure the LOSVD for the
galaxy using a maximum penalized likelihood approach (Section 3.2).
In this way, we obtain spatially resolved 2D profiles of rotation velocity, V, and  velocity dispersion, $\sigma$,
as well as the higher order Gauss-Hermite moments $h_{3}$ and $h_{4}$,
which quantify the asymmetric and symmetric departures of the LOSVD from a pure
Gaussian (related to the skewness and kurtosis respectively).
In the following sections we describe in more detail the spatial binning procedure and the LOSVD recovery.

\subsection{Voronoi 2D spatial binning}
\label{subsect:voronoi}
We re-bin the data with a fixed final S/N by locally averaging
neighboring fibers (using the Voronoi Adaptive technique IDL code of \citealt{Cappellari2003}).
We use an adaptive binning scheme where the size of the bin is adapted to the
local S/N. Bigger spatial bins are created in the low-S/N regions,
with higher resolution and smaller bins retained in the high-S/N
regions (towards the galaxy center)\footnote{Spaxels are arranged in a regular grid, so the size is a well defined quantity.}.

We tested several values for the final Voronoi fixed S/N, choosing a final threshold of  $S/N=70$.
In this way we are able to obtain a high resolution spectrum for each spaxel, which is fundamental for performing a proper
stellar population analysis based on line-index measurements, while also preserving spatial information
that is crucial for recovering detailed spatially resolved kinematics information up to $\sim 0.7$ effective radius ($R_{\rm eff}$$=66"$).

\subsection{Line-Of-Sight Velocity Distribution (LOSVD) fitting}
\label{subsect:losvd}
We measure rotation velocity, velocity dispersion and higher-order moments (V, $\sigma$, $h_{3}$, $h_{4}$)
for each Voronoi-rebinned spaxel spectrum using the pPXF code of \citet{Cappellari2004}.
This software, working in pixel space, finds the combination of stellar templates which, convolved
with an appropriate line-of-sight-velocity distribution, best reproduces the galaxy spectrum.
The best-fitting parameters of the LOSVD are determined by minimizing $\chi^{2}$, which
measures the agreement between the model and the observed galaxy spectrum, over the set of N good pixels.
We use the MILES Library of Stellar Spectra (\citealt{SanchezBlazquez2006, Falcon-Barroso2011}):
985 well-calibrated stars covering the region from 3525-7500 \AA\,  at a spectral resolution of 2.54 \AA\, (FWHM),
$\sigma \sim 57$ $\rm km\,s^{-1}$\, at the central wavelength, obtained at the 2.5m Isaac Newton Telescope (INT).
The pPXF code also allows the user to mask out noisy regions of the galaxy spectrum.
We mask out sky emission lines, focusing on absorption lines from $4300-5400$ \AA\,
(including in this way H$\beta$, O lines, Mg${\it b}$\, doublet and Fe).
Uncertainties on individual points are obtained via a Monte Carlo simulation.

We follow the approach described in \citet{Cappellari2004},  to recover rotation, velocity dispersion and the higher-order terms
of the Gauss-Hermite series simultaneously.
The method makes use of a penalization factor to the solution, which biases the results to suppress the noise.
Obviously, one would like the penalty to leave the LOSVD virtually unaffected.
Thus, we first  perform the kinematics fit without including any penalty (i.e. setting the keyword BIAS=0 in the pPXF code)
to make sure that our results have not been biased and also to properly estimate the uncertainties on the velocity distribution.
This produces a noisy solution (especially for $\sigma$) but allows us to set a range of values for $h_{3}$ and $h_{4}$
which can be used to estimate the right value for the penalization factor.

In particular, this has been done with the {\sl `ppxf simulation'} procedure (included in the publicly available code).
The routine performs a Monte Carlo simulation of the spectra, which repeats
the full fitting process for a large number of different realizations of the data obtained by randomly adding noise to the original
spectra with a resulting S/N equal to the chosen threshold value (S/N = 70 in our case), and using
as input for [$h_{3}$ , $h_{4}$] the maximum representative values measured in the non-penalized pPXF fit of the previous step ([$-0.3,0.3$]).
At this point, we repeat the fitting procedure while using as penalty the largest value such that the mean difference between the
output and the input [$h_{3}$ , $h_{4}$] is well within the rms scatter of the simulated values (BIAS=1.5).

Finally, we inspect by eye zones of the FOV where we expect to have contamination
(e.g.\ near the brighter stars) and spectra for which the reduced $\chi^{2}$ of the fit was larger than 3.
In particular, we identify  $\sim 30$  ``problematic" Voronoi cells, for which we go back to the
single fiber spectra and re-create the Voronoi cell while excluding
contaminated or noisy spectra. Then we re-run the pPXF procedure, in some cases also
setting by hand the pixel regions where the fit is performed.

We take into account all the main systematic uncertainties, mostly caused by template mismatch, and wavelength coverage.
In order to minimize template-mismatch errors, we fit a broad set of stellar templates
together with the kinematics, after convolving both to a common resolution.
We also test the robustness of the kinematic results by changing the spectral region
of the fit and we find results always consistent within $2\sigma$  (not including systematics).
The uncertainties on the final inferred kinematics are estimated by adding in quadrature the formal uncertainty
given by the Monte Carlo simulation and the scatter in the results for different templates and spectral regions.
Typically, we find uncertainties of the order of 5\% for rotation and velocity dispersion and at most of the order of 10\%
for the higher-order LOSVD moments.
For the central bin, we obtain a velocity dispersion of $\sigma_{\star}= 161 \pm 8$ $\rm km\,s^{-1}$\,
perfectly consistent with previously published results (i.e. \citealt{Binney1990, deLorenzi2008}).

\subsection{Two dimensional kinematics maps}
\label{subsect:2Dmaps}
The reconstructed mosaic ($\sim80" \times 60"$ effective area), is among the largest 2D maps
ever measured for an elliptical galaxy and provides a powerful tool to full characterize the internal kinematics of the system
and the spatially-resolved properties of its underlying stellar population, which are necessary ingredients to understand the dynamics
and its connection with formation mechanisms.
Here below, we characterize the 2D behavior of all the relevant kinematical quantities, while in the next sections
we discuss the properties of the stellar populations and try to establish their connection with the kinematical structure.
The full dynamical analysis as well as the derivation of the mass and orbital profile of the galaxy
will be presented in a forthcoming paper.

\placefigmappe

Figure~\ref{fig:mappe} shows 2D maps of rotation velocity, velocity dispersion
and the Gauss-Hermite moments $h_{3}$ and $h_{4}$ of the LOSVD. On the left column, these quantities are
shown as derived from the Voronoi-binning technique discussed in Section \ref{subsect:voronoi}.
Here the small scale features are visible, mainly in the center, while the large scale structure at larger radii looks noisy.
In order to make more evident the large scale pattern of the kinematical quantities, we show on the right column the 2D
quantities smoothed by averaging the Voronoi values over a grid of 15$\times$15 macro bins and then
interpolated. The final average maps have been masked with an ellipse mimicking the orientation and the
axis ratio of the outermost isophote enclosing the VIMOS mosaic.

The galaxy shows a rotation velocity (upper panel) and $h_{3}$  (third panel from above) patterns typical of a
 rotation-supported structure along the major axis of the system. In particular, the $h_{3}$ indicates the presence of a
disk-like structure elongated along the major axis.

The velocity dispersion map (second panel), on the other hand, is rather flat over the full area covered by our observations,
with minimal, statistically insignificant fluctuations.

Finally the $h_4$ parameter map (bottom panel) shows a clear elongated
area along the line of nodes with positive values ($h_{4}\sim 0.01$), which tend to become negative
in the regions off the plane.
which are not common for disk-like structure.
The presence of negative $h_{4}$ off the main rotation axis in the regions where the rotation field
is almost zero indicates tangential orbits, possibly belonging to the bulge component
that starts to dominate outward (see Sec~\ref{sec:bulgedisk}).
The presence of two components along the line of sight might be responsible for the
positive $h_{4}$ parameter aligned along the galaxy major axis by producing a
overall peaked distribution due to the superposition of a cold disk
and hot bulge.

IFS provides a complete and high resolution 2D map of the LOSVD,
allowing the definition and estimation of a number of important parameters that can
be used to better understand the detailed internal structure of the galaxy, a crucial ingredient
for investigating possible formation scenarios.
An interesting quantity that is possible to derive in 2D is the ratio of the ordered
and random motion in a galaxy ($V/\sigma$).

\placefigVsigma

In Figure~\ref{fig:vsig}
we present the first  $V/\sigma$ 2D map of NGC~4697, up to $\sim 0.7$$R_{\rm eff}$ ,which gives a
more quantitative view of the dynamical state of the galaxy
and further confirms the presence of the galaxy sub-components.
One expects that the regions which are bulge-dominated
have smaller $V/\sigma$ values, while the rotation-supported regions where
the disk is dominant have larger $V/\sigma$ values.
This is indeed what we observe in the 2D map and it is further confirmed in the next Section,
where we compare our $h_{3}$--  and $h_{4}$--$V/\sigma$ correlations with those inferred from
hydrodynamical simulations.

We note that none of the previous 3D measurements of galaxies have performed the same kinematical diagnostic as the one above.
However, more standard rotation and dispersion 2D maps of the LOSVD of NGC~4697, like the ones
derived from the ATLAS$^{\rm 3D}$  survey, are fully consistent with the ones presented here,
although  with a lower spatial resolution and over a smaller FOV (ATLAS$^{\rm 3D}$ covers $40\times60$ arcsec, \citealt{Krajnovic2011}).
We do not directly compare our 2D maps to those obtained by ATLAS$^{\rm 3D}$\ because of the different spatial and spectral resolution but
in  Section 3.5 we extract 1D profiles along the major axis and compare our kinematics profiles against the ATLAS$^{\rm 3D}$ ones.

Finally, extended 2D kinematical maps up to  $3.5$ $R_{\rm eff}$\, of this galaxy were recently presented as part of
the SLUGGS Survey (\citealt{Arnold2014}).  Overall there is a fair agreement on the
features observed in the data, both in the velocity field and in the higher-order moments of the LOSVD.
In fact, based on their more spatially-extended kinematic map, the SLUGGS team concluded that the
fast rotation is due to an embedded disk with a rotation amplitude clearly declining with radius.
The presence of a disk  is also found from our detailed analysis of the $h_{3}-$ and $h_{4}$--$V/\sigma$ diagrams.

\subsection{Comparison with simulations}
$h_{3}$--$V/\sigma$ and $h_{4}$--$V/\sigma$ correlations have also been
predicted in simulations of disk merging (\citealt{Naab2006b}, H+09 and N+14).
For instance, N+14 linked the present day central kinematic properties of galaxies
to their individual cosmological formation histories and showed that galaxy mergers (major and minor)
have a significant influence on the rotation properties, resulting in both a spin-down and a spin-up
of the merger remnants, and in a clear anti-correlation between $h_{3}$ and $V/\sigma$.

N+14 have defined six classes (named with letters from A to F)
with different evolutionary paths and histories of mass assembly that can be
directly linked to their 2D kinematic maps and the present day shapes.
The galaxies groupings are based on the 2D kinematic maps and on the
so-called  `spin' parameter ($\lambda_{\rm R}$), a proxy for the projected
angular momentum per unit mass (\citealt{Emsellem2007, Emsellem2011}).

The $\lambda_{\rm R}$\, parameter has been used to show that, within the effective radius,
a dichotomy exists between `fast-' ($\lambda_{\rm R}$$>0.1$) and `slow-' ($\lambda_{\rm R}$$<0.1$)
rotators (\citealt{Emsellem2007}).
The second class of galaxies shows little or no rotation, significant
misalignment between the photometric and the kinematic axes,
and contains kinematically decoupled components,
whereas the first class exhibits regular stellar velocity fields,
consistent with disk-like rotation and sometimes bars.
This version of the `spin' parameter takes the form:
\begin{equation}
\lambda_{R} = \frac{\sum_{i=1}^{N_{p}} F_{i}R_{i} |V_{i}|}{\sum_{i=1}^{N_{p}} F_{i}R_{i} \sqrt{V^{2}_{i}+\sigma^{2}_{i}}}
\label{lambdaR}
\end{equation}
where $F_{i}$, $R_{i}$, $V_{i}$ and $\sigma_{i}$ are the flux, circular radius,
velocity and velocity dispersion of the i-th spatial bin,
with the sum running over the $N_{p}$ bins.

A revised and more accurate separation of these two classes of galaxies
has been proposed  by \citet{Emsellem2011} to include the associated apparent ellipticity:
a higher value of the specific stellar angular
momentum is expected for galaxies which are more flattened or closer to edge-on
if these are all intrinsically fast rotators\footnote{A galaxy with a relatively low value
of $\lambda_{\rm R}$, e.g., of 0.2, may be consistent with a simple spheroidal axisymmetric
system viewed at a high inclination (near face-on), but this is
true only if its ellipticity is correspondingly low (e.g., $\varepsilon \leq 0.3$).
A large ellipticity would instead imply a more extreme object (in terms of orbital
structure or anisotropy).}.

The threshold for $\lambda_{\rm R}$\, was fixed to be
proportional to square-root of  $\varepsilon$ with a scaling parameter
 that depends on the aperture (see Appendix B in \citealt{Emsellem2011} for further details).
For instance, at $R_{\rm eff}/2$

\begin{equation}
\lambda_{R_{\rm eff}/2} = (0.265 \pm 0.01) \times \sqrt(\varepsilon_{eff/2})
\label{lambdaR2}
\end{equation}

Following this classification, NGC~4697 was previously classified as ``fast-rotator''.
This means that, given an ellipticity of $\varepsilon= 0.36$ (\citealt{Peletier1990}),
one expects for this parameter  a value of $\lambda_{\rm R}$$>0.16$ (for $r<R_{\rm eff}/2$).
We find $\lambda_{R_{\rm eff}/2}=0.35 \pm 0.05$, confirming the classification of
this galaxy as a `fast-rotator' and in perfect agreement with the ATLAS$^{\rm 3D}$
result ($\lambda_{R_{\rm eff}/2}=0.322$, \citealt{Emsellem2011}).

Fast-rotators belong to class A, B and D in the N+14 classifications.
However only the first two groups of galaxies will result in $h_{3}$ and $h_{4}$
distributions similar to that we observe in NGC~4697.
Both groups (A and B) of galaxies are rotationally supported, had a significant amount of central in-situ,
dissipative, star formation but, while class A have late assembly histories dominated by minor mergers,
class B galaxies have gone through a late gas-rich major merger.
These two formation scenarios will produce the same $h_{3}$--$V/\sigma$ anti-correlation
that we observe in our maps.

One way to distinguish between the two classes is to look at the  $\lambda_{\rm R}$\, profiles:
class A galaxies show peaked $\lambda_{\rm R}$\, profiles within the effective radius,
originating from the fast rotating central stellar disk, whereas class B galaxies have $\lambda_{\rm R}$\,
profiles constantly rising beyond the effective radius.

\placefiglambdar

In Figure~\ref{fig:lambdaR} we plot the  $\lambda_{\rm R}$\, profile as a function of radius calculated from circular apertures.
The profile has a strong peak around $0.2$$R_{\rm eff}$\, and then it rises until $\sim$$R_{\rm eff}$, which
suggests that the mass assembly of NGC~4697 has involved significant in-situ star formation,
 that NGC~4697 has experienced several gas-rich minor mergers
(like simulated galaxies of class A)  and possibly a late gas-rich major merger
leaving a previously rapidly rotating system unchanged (like simulated galaxies of class B).
However given the poor resolution of the simulations this interpretation should be taken with caution (Fig.5 in N+15
shows the $\lambda_{\rm R}$\, profiles of the simulated galaxies in the six classes and  only one galaxy of class A shows
a peak, which is at $\sim 0.95$$R_{\rm eff}$. On the other hand we observe
that in Fig.5 of \citealt{Emsellem2011}, showing  $\lambda_{\rm R}$\,
for the full ATLAS$^{\rm 3D}$\, sample,  several fast-rotators show a profile similar to what we derive for NGC~4697).
Moreover, \citet{Coccato2009} derived the $\lambda_{\rm R}$\, profile for NGC~4697 out to $\sim 3.5$$R_{\rm eff}$\, based
on planetary nebulae (PNe) and showed that it flattens out at  $\sim 1$$R_{\rm eff}$\, which supports the idea that
NGC~4697 should be compared with simulated galaxies of class A.
We also note that \citet{Arnold2014} concluded that galaxies like NGC~4697 formed through
rapid, dissipative processes, which formed the central regions, followed by a prolonged period of dry minor mergers.
We cannot exclude the scenario of gas-rich late major mergers, but independent lines of evidence point toward
a scenario where the mass assembly of NGC~4697 is dominated by minor mergers and gradual dissipation.

\placefigsimul

In Figure~\ref{fig:simulh3h4} we show the $h_{3}$--  and $h_{4}$--$V/\sigma$
correlations derived from the 2D kinematic maps (left panels), and we compare them to
luminosity contours derived by H+09 for a 1:1 disk--disk merger with 30\% gas fraction (middle panels)
and from  the cosmological hydrodynamical simulations of N+14 (class A and class B, right panels).
 A  good agreement, at least on a qualitative level, is found between data and simulations,
although we caution that H+09 only considered the case of equal-mass mergers.

VIMOS data-points are color coded in accord with their value of $|Cos[\theta]|$,
calculated with respect to the galaxy minor kinematical axis.
We find a clear correlation between the $|Cos[\theta]|$ values and the regions where
the disk component is elongated.
Points oriented near the major axis (i.e., $|Cos[\theta]| \sim 0$) have also
higher absolute values of $h_{3}$ and therefore are associated with the rotation-supported structure.
Similarly, points with higher values of $|Cos[\theta]|$ have lower $h_{3}$ and roughly
correspond to the bulge region.
The $h_{4}$ does not show a similar (anti-)correlation with $V/\sigma$.

The $h_{3}$--$V/\sigma$ anti-correlation generically tracse cold disks.
It is a feature that naturally emerges in
 disk-disk gas-rich mergers, and tends to produce large asymmetric deviations
 from Gaussianity because of the presence of sub-components that retain a memory
of the disk-star streaming, and because of gas that settles down through dissipation to form a thin embedded disk.
This $h_{3}$--$V/\sigma$  correlation is generally negative when the dominant orbit population tends to stream
(e.g. z-tube orbits, see also \citealt{Rottgers2014}), and positive when the rotation is caused by sub-dominant
streaming population (e.g. x-tube orbits)
superimposed on the tail of the dominant streaming orbits (e.g z-tubes which still contribute  some rotation along
the minor axis; see also the discussion in H+09).
The same features are not found in second generations of major (re-)mergers
(mergers at lower redshift, where less cold gas is present and with elliptical-morphology progenitors), in which case
 the features are more mixed and look more concentrated around the center of the diagram.

The $h_{4}$--$V/\sigma$ correlation of NGC~4697 in Figure~\ref{fig:simulh3h4} shows a V-shaped distribution
with a double peak at $|V/\sigma|\sim0.5$.
This distribution is very similar to  the predictions from simulations of N+14 (right, bottom panel)
and it also agree with H+09 (middle, bottom panel), although there is a significant
offset between the data and the H+09 predictions.
The peaked population could correspond to a late-formed disk stars (note the correspondence to the extreme
$h_{3}$ values and $|Cos[\theta]| \sim 0$ indicating the alignment along the major axis) which tend to produce a positive
$h_{4}$ in superposition with the more isotropic component (differences in ages of the two components
are discussed in Sec.~\ref{sect:stellpop}).
In the simulations of H+09 the re-mergers would look more concentrated around the origin and would
tend to have LOSVDs with positive $h_{4}$, similarly to expectations from violent relaxation,
which generally results in a radially-biased distribution function (\citealt{Binney2008}). \\
\indent To conclude,  the high-order moments of the LOSVD provide kinematical evidence
for a two-component system:
the largest absolute values of $h_{3}$ and $h_{4}$
indicate an area of the galaxy with the dominance of x-tube over z-tube orbits, which are produced in
collisionless mergers and trace the presence of a (later) streaming structure,
these are also the regions around $|Cos[\theta]| \sim 0$ (minor axis).
Values with $h_3\sim 0$ and $h_4\sim 0$ indicate instead the presence of a non rotating subsystem
that dominates in the regions where the values of $|Cos[\theta]|$ are higher.
The $h_{3}$--$V/\sigma$ and the peaked $\lambda_{\rm R}$\, profile suggest that gas-rich minor mergers
dominate the mass assembly of NGC~4697, although we cannot completely exclude the possibility of a
major merger event that happened at redshift $z \geq 1$.

We make use of this evidence in Section \ref{sec:bulgedisk} where, based on the photometry
of NGC~4697, we separate the disk from the bulge and study the ages and metal
abundances of the stellar populations of these two components.

The details of the gas accretion leading to the formation of the central disk may be somewhat
different than the one investigated in the simulation of disk merging and it might be useful to have
LOSVD predictions from simulations of cold accretions as an alternative high dissipative process forming the disk.
It seems evident, though, from H+09 and N+14 that dry mergers is not able
to produce the  kinematical substructures we see in the $h3$-- $h4$--$V/\sigma$ diagrams.
In fact, in a merger without a dissipative gas component, the remnant galaxies are axisymmetric and
do not show a population of stars with high angular momentum tube orbits nor the re-growth
of a significant disk component (e.g.\ class D in N+14).

\subsection{One dimensional spatially resolved kinematics profiles}
\label{subsect:onedprof}

\placefigoneDprof

To compare our results against published results based on long-slit data
and IFS with different FOV and resolution, we extract from the 2D kinematics maps the information along the major axis.
Specifically, we extract and sum all the spectra positioned in a rectangle with width of $1.34''$ (2 pixels) oriented along
the major axis of the galaxy and centered on our kinematic center (to be as close as possible to the configuration of slit-based studies).
We perform the same extraction for the IFU ATLAS$^{\rm 3D}$ observations (publicly available on the Survey Webpage)
in order to perform a simple comparison of the two sets of data with different spatial and spectral sampling.
In Figure~\ref{fig:delor} we compare our profiles (black points) with the ATLAS$^{\rm 3D}$ ones (green points) and with the ones published in
de Lorenzi et al. (2008, hereafter DL08), derived from high S/N integrated absorption line spectra obtained by \citet{Mendez2005} with
FORS2 at the VLT, a slit width of 1 arcsec and seeing 1 -- 1.5 arcsec (blue points).
For the major axis inclination, we assume the value PA = 63 degrees from \citet{Binney1990}, slightly different
from the one assumed by DL08 but providing the best symmetry and maximum rotation for our extracted 1D profiles.
We do not worry about this small PA discrepancy that could be caused by the fact that the slit in DL08 was not
exactly on-center or could be related to the offset we found between kinematic and photometric center, most
probably caused by a small effect of  atmospheric refraction.
For the ATLAS$^{\rm 3D}$\, data we use the same inclination of PA = 63 degrees and extract the major
axis profiles with the same procedure applied to our VIMOS data.
We found an overall good agreement between the three 1D kinematical profiles which
 nicely demonstrates the robustness of our mosaic approach and the validity of our results.

\section{2D Stellar Population Analysis}
\label{sect:stellpop}
In this section we study the stellar population of the disk and of the bulge of NGC~4697 separately,
to put constraints on the age, $[\alpha/\mathrm{Fe}]$, metallicity and IMF normalization
of the stellar population of the different morphological components of the galaxy.

To constrain the stellar population parameters, we focus on line-index measurements rather than full
spectral fitting, which avoids issues with spectral calibration when
comparing to observations that might have been poorly calibrated and
we assume a simple stellar population (SSP), rather than an extended star formation history,
which is still a strong assumption and will be properly addressed in future work.

We measure equivalent widths (EWs) of several stellar absorption features in each of the Voronoi-rebinned 1D
spectra, after convolving them to a common resolution of $350$ $\rm km\,s^{-1}$\, to correct for kinematic
broadening\footnote{This final resolution has been chosen for practical reasons:
the version of the simple stellar population models used in this paper was created and used in S+14
with a resolution of  $350$ $\rm km\,s^{-1}$. To save computer power, we did not perform again the EW measurements
and simply smoothed our data to the resolution of the models. We are confident that this did not cause any
loss of information, and we check (by eye-inspection) that contamination from sky line residuals do not affect the spectral features.}.
We compared these EWs to those measured from an extended version of the SSP models of  Conroy \& van Dokkum
(2012a, hereafter CvD12) with the same common resolution, obtained in Spiniello, Trager \& Koopmans (2014b).

CvD12  optimized models over the wavelength interval $0.35\, \mu m \,< \lambda < 2.4\,\mu m$
at a resolving power of R $\sim 2000$, specifically for the purpose
of studying old, metal-rich stellar populations.  The models are built combining two
empirical stellar libraries (MILES, \citealt{SanchezBlazquez2006}; and IRTF, \citealt{Cushing2005})
and three sets of isochrones to measure the IMF slope down
to $\sim 0.1\, {M}_{\odot}$. The CvD12 models explore variations in age in the range 3--13.5 Gyr,
$\alpha-$enhancement of 0--0.4 dex, and four different single-slope IMFs:
a bottom-light single-slope power law with $x=1.8$ (where $x$ is the IMF slope,
using $dN/dm \propto m^{-x}$) that produces a stellar mass-to-light ratio comparable to the one
obtained from a standard Chabrier IMF (\citealt{Chabrier2003}), a Salpeter (1955) IMF
with a slope of $x=2.35$, and two bottom-heavy (dwarf-rich) IMFs with slopes of $x=3.0$ and $x=3.5$.

The CvD12 models also allow for variations in the $[\alpha/$Fe] ratio as well as variations in
the abundance pattern of 11 different single elements.  This is enough to decouple
IMF variations from abundance variations.
However, all of the CvD12 models use {\sl solar} metallicity isochrones, even when synthesizing
with different abundance patterns or different $[\alpha/$Fe].
The abundance variations of single elements are implemented at fixed [Fe/H], which implies  that the total metallicity
$Z$ cannot be easily controlled.  This is restrictive, if one aims to disentangle elemental enhancements,
metallicity changes and IMF variations, especially in the case of  massive ETGs, which have star formation histories
different from the solar neighborhood (e.g., \citealt{Peterson1976,Peletier1989,Worthey1992, Trager2000b, Arrigoni2010}).

To resolve this issue, we follow the approach presented in \citet{Spiniello2015}, hereafter S+15
of extending the parameter space of the SSP models using response functions.
We construct a metallicity-response function for each given age and IMF slope
taking the ratio between two spectra of the MIUSCAT SSP models (\citealt{Vazdekis2012})\footnote{The MIUSCAT SSP has
instead  a fixed total metallicity and covers six metallicity bins
$Z=0.0004, 0.001, 0.004,0.008,0.019$ and $0.03$, where $0.019$ represents the solar value.}
with the same age and IMF slope but different total $Z$.
We then multiply this response function with the spectrum of a CvD12 model with fixed age and IMF
to build a new model (SSP) that extrapolates the latter model to a new part of parameter space
(i.e. covering super-solar $Z$).
These modified SSP models combine the flexibility  of both the MIUSCAT and CvD12 models
to predict spectra in a part of parameter space that neither of them reaches separately
(MIUSCAT models use different total metallicities but do not allow one to change the
abundances which are fixed to solar).
As pointed out in S+14 and S+15, selecting IMF-dependent features that are age- and metallicity-independent
and combining them with indices that depend mainly on age or mainly on element abundance
is important for breaking the age-metallicity-IMF degeneracy when using
SSP models to infer the stellar populations from unresolved galaxies spectra.

We measure some of the classical blue Lick indices (e.g. H$\beta$, Mg${\it b}$, Fe5270, Fe5335, [MgFe]:
\citealt{Gonzalez1993, Worthey1994, Trager2000}) that have been extensively and successfully used in the literature to
constrain the age and metallicity of galaxies, together with some of the bluer
IMF-sensitive features defined and used in S+14 and S+15.
Unfortunately  this paper makes use of data taken with the HR-blue grism, and therefore only covers
the bluer IMF-features of S+14 (specifically bTiO, aTiO, TiO1)
while in the future we plan to obtain new data using the HR-red grism which will cover also
TiO2, CaH1, TiO3 and TiO4, allowing a more detailed analysis and a more secure inference on the low-mass end of the IMF slope.

Before measuring EWs, we convolved galaxy and model spectra to an effective velocity dispersion of
$\sigma = 350\,\mathrm{km}\,\mathrm{s}^{-1}$ to correct for kinematic broadening.
Indices in both the galaxy and the model spectra have been measured
with the same definitions and methods\footnote{We use the code SPINDEX from \citet{Trager2008}.}.
We do not place our indices on the zero-point system of the Lick indices and quote them
as index strengths in units of angstrom (if atomic) or magnitudes (if molecular, like the TiO lines).

\placefigelemmaps

The great advantage of integral field spectroscopy is the simultaneous availability of spatial and spectral information.
This allows us to generate 2D spatial maps of spectral features of interest, like the one in Figure~\ref{fig:element_maps},
showing  the [MgFe]\footnote{[MgFe] = $\sqrt{(\mathrm{Fe5270} +\mathrm{Fe5335})/2 \times \mathrm{Mg b}}$, (\citealt{Gonzalez1993})}
index that has been widely used to constrain the metallicity.
The 2D map suggests different stellar populations in the bulge and in the disk: specifically,
the [MgFe] EWs are systematically higher in the Voronoi cells within the disk.
Therefore, the 2D element maps indicate that the stars in the disk are more
metal-rich than the stars in the bulge. However, we caution the reader that it is not possible to directly infer
the total metallicity by looking at a single-element map, because of the degeneracies present between the stellar
population parameters. For instance, in this case the [MgFe] values could be higher due to an increase of age and/or could
increase of total metallicity. This is an example of the so-called age-metallicity degeneracy which can be broken by
using more than one indicator.
This motivates us to decompose the bulge and disk components and to extract a 1D spectrum
of each of them in order to study their stellar populations separately through a  more quantitative,
proper SSP analysis.

\placefigoneDspec

\subsection{Disk-Bulge decomposition}
\label{sec:bulgedisk}
We perform a two-component fit to the HST V-band image of NGC~4697 obtained by \citet{Tal2009}, driven by the
correlations in the $h_{3}$ and $h_{4}$ parameters versus $V/\sigma$ that clearly indicate the presence of a disk.
We use the latest version of GALFIT (\citealt{Peng2010}) to fit two ellipsoid models (`sersic' for the bulge and `expdisk' for the disk)
to the light profiles of the galaxy image.
We obtain a similar position angle (PA $\sim 64$ deg, confirming previous findings)
but very different axis-ratios for the two components: $(b/a)_{disk}=0.297$,  $(b/a)_{bulge}=0.7512$.
We use those to spectroscopically separate the bulge from the disk.
We note that a more rigorous spectroscopic separation, following the approach
of  \citet{Coccato2011} and \citet{Coccato2014}, will be performed in future studies to fully separate these two components.

First, we extract and sum together all the spectra in the datacube with $r < $$R_{\rm eff}$$/8$.
In this central region we expect bulge and disk to both contribute substantially.
Second, we select and sum the spectra belonging to an elliptical anulus centered
on the kinematics center with the axis-ratio and PA found by GALFIT for the disk: $(b/a)_{disk}=0.297$, $PA=65.47$deg
and with $r > $$R_{\rm eff}$$/8$ (to exclude the central region).
Finally, we sum up the remaining spectra where the contribution of the bulge is dominant.
The resulting 1D spectra have very high S/N ($S/N = [450, 320,280]$ for center, disk and bulge respectively).

In Figure~\ref{fig:1dspectra} we show the extracted 1D spectra of the disk and
bulge, as well as of the mixed (disk$+$bulge) population of the central region of NGC~4697 for comparison.
Shaded yellow bands show some of the line indices used in this work, along with continuum side-bands (blue and red colored bands).
Some small differences are visible already from the spectra: the disk spectrum shows stronger Mg and Fe lines,
which confirms what have already seen from the [MgFe] 2D map and gives hints of a more metal-rich population.
The NaD absorption line, the narrow strong line around 5900 \AA is stronger in the bulge than in the disk,
consistent with the hypothesis that bulges could be Na-enhanced (e.g. in the bulge of the Milky Way, on average [Na/Fe] $\sim 0.2$,
\citealt{Fulbright2007}). However, we do not use this particular line in the following analysis because
its blue band is heavily contaminated from emission sky-lines and because of the recent finding presented in
S+15 showing that the NaD lines are model dependent and therefore must be interpreted with caution.
The aTiO index has also been excluded from the analysis because it is contaminated from emission sky-lines.

\placefigstelpop

In Figure~\ref{fig:index-index} we show index-index plots of the selected optical indicators
to provide qualitative constraints on the stellar population parameters. In panels a) and b) the IMF dependence is minimal
and the age and abundances of the galaxy can be inferred.
The IMF normalization of the galaxy can be instead inferred from panels c) and d),
using SSP models with the metallicity and age previously determined.

\subsection{Age and metallicity of the stellar population}
\label{subsect:agemetal}
In the upper panel of Figure~\ref{fig:index-index} we show index-index diagrams
of some of the classical Lick-indices.
These diagrams are widely used to constrain age and metallicity of
integrated stellar populations.
The average indices extracted from the different regions are plotted
on top of grids of CvD12 SSP models with varying ages (blue lines, [7,9,11,13.5] Gyr),
$[\alpha/\mathrm{Fe}]$\, (red lines, [0.0, 0.2, 0.4] dex) and total metallicity
(green lines, [-0.22, 0.0, +0.22]). All plotted models have a
Chabrier-like IMF, but for these indicators (H$\beta$, Mg${\it b}$,
Fe5270, Fe5335) the dependency on IMF is minimal.

Panel a) of Figure~\ref{fig:index-index} shows the H$\beta$--[MgFe] diagram.
The H$\beta$\, index is one of the most used age-indicators in the optical, and allows one to
break the age-metallicity degeneracy,  when combined with the
commonly-used [MgFe] index.
However, this diagram alone does not allow one to also break degeneracies with $[\alpha/\mathrm{Fe}]$.
This is clear for instance in the case of the disk component. From panel a) it is inferred that
the bulge has an old population with solar $[\alpha/\mathrm{Fe}]$\, and slightly sub-solar metallicity. The central
region is also old but has super-solar abundances.
For the disk the interpretation is somewhat more difficult. In fact, the disk spectrum matches a model
with age $=11 \pm 2$ Gyr, slightly super-solar metallicity and solar $[\alpha/\mathrm{Fe}]$\, but also a
model with older age, lower metallicity and $\alpha$-enhanced.
To discriminate between these two possibilities, the reader should refer to the results plotted in panel b).
Panel b) shows  ${\mathrm{Mg}b}$ versus $<Fe>$, which is the mean of Fe5270 and Fe5335.
Here the disk matches only with a model with age $=11 \pm 1$ Gyr, solar metallicity and solar  $[\alpha/\mathrm{Fe}]$.

Index-index plots are a useful tool to give qualitative inference
on the stellar population parameters, but it is sometimes hard to break degeneracies
and quantitatively constrain age, metal abundance and IMF slope at the same time.
Therefore, in order to give more quantitative constraints on the stellar population parameters of the three components, we perform a
$\chi^{2}$ minimization comparing the 1D spectrum of each component with grids of linearly interpolated SSPs spanning a range of ages
(between 7 and 13.5 Gyr with steps of 1  Gyr,), $[\alpha/\mathrm{Fe}]$\, (between −0.2 and +0.4 dex, with a step of 0.1 dex), and total metallicity
([M/H]=[-0.22,0.0,+0.22])  for a Chabrier IMF (we note that a moderate change in the IMF slope has only a
negligible effect on  these blue features).
We find that the disk is slightly younger and more metal-rich than the bulge, consistent with a SSP model of $\sim 10.5_{-2.0}^{+1.6}$ Gyr, solar
total metallicity ([M/H]=$-0.03^{+0.02}_{-0.1}$) and solar $[\alpha/\mathrm{Fe}]$ ($[\alpha/\mathrm{Fe}]$$=+0.04^{+0.02}_{-0.01}$).
The bulge fits better with a $13.5^{+1.4}_{-1.4}$ Gyr model with sub-solar metallicity
([M/H]$=-0.17^{+0.12}_{-0.1}$) and solar $[\alpha/\mathrm{Fe}]$ ($[\alpha/\mathrm{Fe}]$$=+0.03^{+0.03}_{-0.01}$).
The central region shows stellar population properties  in between those of the disk and
those of the bulge, as expected. It is as old as the bulge ($12.9^{+1.5}_{-1.8}$ Gyr),
shows a solar or slightly super solar $[\alpha/\mathrm{Fe}]$\, ($[\alpha/\mathrm{Fe}]$$=+0.09^{+0.03}_{-0.01}$)
and it is even more metal enriched ([M/H]=$+0.23^{+0.08}_{-0.05}$).
These SSP results nicely confirm the qualitative picture obtained via index-index plots in the upper
row of Figure~\ref{fig:index-index}, and are summarized in Tab.~\ref{tab:SSP}.
However, we note that since the 1D spectra of bulge and disk are composite spectra where
the contributions of the two components are not perfectly disentangled, the true stellar population differences are likely
to be even greater.

\placetab
Finally we consider NGC~4697 as whole and calculate gradients in its stellar populations.
Following the approach of \citet{Tortora2010b},  we define the stellar  population gradient
as the dimensionless coefficient of the relation
\begin{equation}
\log X -- \log R/R_{\rm eff}(\nabla_{X} = \frac{\delta (\log X)}{\delta \log (R/R_{\rm eff})}),
\end{equation}
where X represents the age or the total  metallicity expressed in terms of [M/H].
We find a non negligible but very small age gradient and a  negative metallicity
gradient in the sense that NGC~4697 is more metal-rich and older in the center.
These gradients are consistent with the measured gradients in old early-type galaxies
(\citealt{Kuntschner2010, Tortora2010b})  and with remnants of gas-rich major mergers
from simulations (e.g. \citealt{Hopkins2009}, H+09).

\subsection{The IMF normalization}
Using the metallicity and age constraints obtained from the Lick blue indices via the $\chi^{2}$ minimization, we focus now on two
of the IMF-sensitive optical indicators that fall in the VIMOS wavelength range, the bTiO and the TiO1.
We plot them against the [Mg/Fe] index in the lower panels of Figure~\ref{fig:index-index}. The combination of the latter indicator with
IMF-sensitive features breaks the degeneracies between the $[\alpha/\mathrm{Fe}]$, total metallicity and IMF slope variations.

For each component,  we use SSP models with varying IMF slope (x between 1.8 and 2.5) and  $[\alpha/\mathrm{Fe}]$, and with the other stellar population
parameters as close as possible to the ones derived from the $\chi^{2}$ fit to the blue indices. For the bulge, we use SSP
models with 13.5 Gyr and [M/H] = -0.22, for the disk we use a SSP models with 11.0 Gyr and [M/H] = 0.0 (solar).
Finally, for the mixed, central population we use SSP  models with 13.5 Gyr
and [M/H] =+0.22 (super-solar).

In Figure~\ref{fig:index-index} black lines show models with different IMF slopes and red lines show models with varying  $[\alpha/\mathrm{Fe}]$.
No detectable variation in the IMF normalization between bulge and disk is visible from the two panels.
Both components of NGC~4697, as well as the  central region, are consistent with a normalization of $x=2.0 \pm 0.2$,
slightly dwarf richer than a Chabrier IMF (x=1.8, still consistent within 1-sigma) but shallower than a Salpeter (x=2.35),
which is perfectly consistent with the slope predicted from the IMF--$\sigma_{\star}$ relation (e.g.,
\citealt{LaBarbera2013, Tortora2013}; S+14) for an ETG with $\sigma_{\star} = 160$ $\rm km\,s^{-1}$.
IMF normalization does not change with radius for this galaxy is consistent with the results found in  \citet{MartinNavarro2014}.
The lack of IMF spatial gradient is also consistent with the results on the low-mass system in
\citet{MartinNavarro2014} that shows an IMF normalization constant with radius and consistent with a Kroupa-like profile.

\subsection{Linking kinematics and stellar populations }
The main conclusion from the stellar population analysis is that the inner region (typically $\sim $$R_{\rm eff}$$/8$)
looks coeval (or a bit older) and more metal-rich than the regions farther out,
which suggests that this central region has been formed early via rapid
collapse.
However, from the stellar population analysis alone, we cannot exclude minor or major merging of
late-type disk galaxies, which have destroyed spiral arm features
and left a younger disk component. It is therefore necessary to connect and
correlate the stellar population results with those on the
spatially resolved kinematics.

The SAURON team (\citealt{Kuntschner2006, Krajnovic2008}) have found that
the fast-rotating component almost always features a higher metallicity compared to the galaxy as a whole.
They have attributed this to the presence of a later-forming stellar population in a rotating structure with disk-like
kinematics (\citealt{Kuntschner2010}).
From the NGC~4697 2D maps as well as from the stellar population analysis
presented in this study, we infer the same scenario.
This is demonstrated inFigure~\ref{fig:h4hbeta}, which shows the
correlation between the $h_{3}$ (top panels) and the $h_{4}$ (bottom panels) parameters
and the H$\beta$\, (left) and Mg${\it b}$\, (middle) values obtained from the smoothed 2D maps.
We run a Spearman test on these relations to better quantify the statistical dependence
between the high-order moments of the LOSVD  and  H$\beta$\ and Mg${\it b}$\, respectively.
The resulting  Spearman rank correlation coefficients are $\rho=0.36$ ($0.2$) and $\rho=0.32$
($0.36$) for $h_{4}$ ($h_{3}$) and H$\beta$\, and Mg${\it b}$\, respectively. Given the big sample size
(more than 100 points), these values of $\rho$ all exceed the critical value ($\rho_{crit} (n>100) =0.165$)
and therefore the relations are statistically significant, although not strong.

The right panels of Figure~\ref{fig:h4hbeta} shows the H$\beta$\, --$h_{3}$ (top panel)
and --$h_{4}$ (bottom panel) diagrams
with the points color-coded according to the Mg${\it b}$\, values.
Although the discussion must be kept on a qualitative level because
of the well-known age-metallicity degeneracy (\citealt{Worthey1994}),
we can simplify the situation and say that
larger H$\beta$\, values indicate younger ages and larger Mg${\it b}$\, values indicate higher total metallicity.
Thus we can conclude that points with $h_4>0$, tracing the later-formed disk,
are slightly younger and more metal rich, while points with $h_4<0$, roughly tracing the bulge component
because they are along the minor axis of NGC~4697,  all have generally older age and lower metallicity.
The same holds also for points with larger $|h_{3}|$, although in this case the relations are less robust.

Remarkably, the spatially resolved stellar population results perfectly agree (on a qualitative level at least)
with the spatially resolved kinematics results.
Unfortunately none of the hydrodynamical simulations derive 2D detailed stellar population properties.
In the future, it might be extremely useful to have predictions from simulations on the ages and metal abundances
of the remnant of different mergers scenarios.

In the SAURON ETGs of low to intermediate mass ($\sigma =100$--$160$ $\rm km\,s^{-1}$), the region of increased metallicity is
connected to a mild decrease of the $[\alpha/\mathrm{Fe}]$, whereas in more massive galaxies ($\sigma > 160$ $\rm km\,s^{-1}$) the disk formation and
increased metallicity is typically constrained to a central location involving only a minor fraction of the total mass of the
galaxy and only in about 25 per cent of the cases also a central depression in $[\alpha/\mathrm{Fe}]$\, can be seen.

In the case of NGC~4697, we find that the central region is
slightly $\alpha-$enhanced with respect to the bulge, whereas the disk shows roughly the same [$\alpha$/Fe] as the bulge.
A larger metallicity associated with the fast rotating component, seems to point toward
a formation scenario where fast rotator galaxies have undergone one or multiple periods of secondary star-formation
at a later stage and over longer timescales and therefore resulted in an increased metallicity and a decrease of the abundance ratio
in a disk-like structure (\citealt{Kuntschner2010}).

A younger and more metal-rich disk is also well
consistent with the scenario suggested by the gas-rich merger (e.g. H+09), as the younger disk would arise when the gas, retaining
its angular momentum during the merger, is fueled in the center of the remnant and eventually turns into stars.
In Section \ref{subsect:2Dmaps} we have demonstrated that this same scenario is also perfectly able to explain the kinematical
substructures.

We note here that the disk merging scenario does not necessarily imply major merging, as also merging with lower mass
fraction can produce similar kinematical features.
In fact, simulations in N+14 have shown that  correlations similar to the ones we observe in the $h_{3}$ and $h_{4}$
parameters of NGC~4697 can originate from two galaxy formation scenarios: a late gas-rich major merger
or in situ star formation plus minor merging.

\placefiglast

In conclusion, the combination of the kinematical features and the stellar population properties seem to point to the scenario where
some fast rotating and disky ellipticals can have formed from dissipative (wet) mergers of disk galaxies.

\section{Discussion and conclusions}
In this paper, we have presented high S/N integral field kinematics and stellar population
combined analysis of the elliptical galaxy NGC~4697,
an almost edge-on, intermediate luminosity ($L_ {*}$) isolated elliptical galaxy.
We used a mosaic approach,  the first of its kind with VIMOS IFU data, obtaining
2D maps of stellar kinematics and absorption lines up to 0.7$R_{\rm eff}$.
The final effective field-of-view of $\sim 80"\times 60"$ allowed up to obtain one among the largest
2D kinematical maps ever measured for a single early-type galaxy (in terms of arcsec)
 providing a unique view on the internal structure of the system, as well as crucial morphological
and dynamical information.

Our main scientific findings are the following:
\begin{itemize}
\item[i)] We have measured the 2D velocity moments of the galaxy's stellar population finding
clear evidence for a rotation-supported structure along the major axis from the rotation
velocity and the third Gauss-Hermite coefficient $h_{3}$ (representing the skewness).
We have  measured the ``spin-parameter" ($\lambda_{\rm R}$) confirming the classification
of this system as `fast-rotator'.
\item[ii)] We have analyzed the correlations between the  $h_{3}$ and  $h_{4}$ parameters
with $V/\sigma$ (Fig.~\ref{fig:vsig}), together with the $\lambda_{\rm R}$\, spatial profile, demonstrating how these characterize the
different kinematical components (bulge and disk) of the galaxy.
\item[iii)] We have directly compared these correlations with those predicted by hydrodynamical
simulations of  \citet{Hoffman2009} from gas-rich disk-disk major mergers with a 30\% gas fraction and of
\citet{Naab2014} for gas-rich minor and major mergers (class A and B).
The correlations we presented  closely resemble the theoretical predictions and indicate that the mass assembly of NGC~4697
is dominated by gas-rich minor mergers, gradual dissipation plus possibly a late gas-rich major merger.
\item[iv)] A direct comparison with 1D long-slit spectroscopy (\citealt{deLorenzi2008})
shows an overall good agreement between the different kinematics results along the major axis.
\item[v)] We extracted 1D spectra of the disk and the bulge of NGC~4697, using
a two-components fit to a deep V-band image.
\item[vi)] We studied the stellar populations of these two components using SSP models.
We find indications  that the stars in the disk are $\sim 2-3$ Gyr younger and
more metal rich that the stars in the bulge.
\item[vii)] We linked the stellar population analysis and the internal kinematics of the system by correlating
age and metallicity of the stellar populations of the two components with the $h_{3}$ and
the $h_{4}$ kinematic parameters, finding further evidence for a  significant in-situ formation of stars since $z\sim 2$
with additional gas-rich minor mergers (although we do not exclude the possibility of a late major-merger that
left a previously rapidly rotating system unchanged).
\item[viii)] From the two bluer IMF-sensitive optical indicators of  S+14, which fall in the VIMOS wavelength range,
we do not detect any difference in the IMF slope between the bulge and the disk.
Both components are consistent with an IMF with a single power slope of $x$=2.0, consistent with a
Kroupa IMF and slightly lighter than a Salpeter-like IMF. The inferred IMF slope is perfectly consistent with
the one predicted from the IMF--$\sigma_{\star}$ relation for an  ETG with $\sigma_{\star} = 160$ $\rm km\,s^{-1}$, such as
NGC~4697 (\citealt{Conroy2012b, LaBarbera2013, Treu2010, Tortora2013, Tortora2014a}, S+14).
\end{itemize}

The absolute novelty of this work resides: i) on the depth and width of the data acquired as we have very high $S/N$
spectra over a  an effective area of the sky of $80''\times60''$ (e.g. larger than MUSE FOV); ii) on the presentation of a detailed spatially
resolved kinematical and population 2D analysis within the central effective radius, which has allowed us to cross-correlate LOSVD
 information (i.e. $h_3$ and $h_4$) with relevant line indices (e.g. $h_4$ vs. H$\beta$\, and Mg${\it b}$\, in  Figure~\ref{fig:h4hbeta}), showing that points
 with $h_4>0$, associate mainly to the later-formed disk,  are younger and more metal rich, while
 points with $h_4<0$, roughly tracing the bulge component because aligned with the minor axis of NGC~4697,
 all have generally a  smaller H$\beta$\, and smaller [M/H].

The emerging picture is that a later formed disk has been built from pre-enriched gas that formed stars after having
dissipatively sunk into the center. This is well consistent with the scenario suggested by
gas-rich disk merging simulations (e.g. H+09), as the younger disk would arise when the gas,
retaining its angular momentum during the merger, is fueled in the center of the remnant and eventually turns into stars.
It is remarkable that within this scenario, photometry, stellar population features and kinematical features like
the $h_3$- and $h_4$-$V/\sigma$ correlations are
all qualitatively correctly predicted.  We stress again that H+09 only considers 1:1 disk-disk merger but that also
merging with lower mass fraction (minor mergers) can produce similar kinematical features (e.g. N+14).
Furthermore other mechanisms involving a rapid dissipative collapse of enriched gas
(clumpy disks, violent relaxation, cold accretion), might have produced a similar galaxy component.

This paper is intended as a pilot program for a large project that
aims at the study of internal structure, mass distribution and stellar population of a sample of nearby $L_ {*}$ ETGs.
With medium-high signal-to-noise spatially resolved spectra, we will perform a detailed 2D study
of the stellar population via line-index measurements and try to further test possible variation in the IMF normalization.
We will attempt to characterize the low-mass end of  Initial Mass Function normalization in the bulge and in the disk components
by measuring EWs of the IMF-sensitive features defined in S+14. In order to achieve this result we plan to change
the configuration of VIMOS in the new observations, choosing a redder filter (HR-red) to cover the proper wavelength range\footnote{We are aware that
moving to the red filter will cause the loss of some of the blue indices covered in this paper, making age determination more complex. We therefore plan to select
ETGs where measurements of age and metallicity are available from the literature and mainly focus on measuring gravity-sensitive features
to study the possible spatially variation of the IMF slope, with particular regard on bulge versus disk dominated zones.}.
In addition to a direct measurement  of the stellar mass-to-light ratios (M$^{\star}$/L), thanks to the 2D IF coverage,
we will be able to study age and metallicity  radial gradients for our systems.
Moreover, where spatial gradients in the stellar population parameters are present, the assumption of a spatially-constant (M$^{\star}$/L)
clearly does not work. Consequently, the 2D coverage, allowing a more accurate measure of the (M$^{\star}$/L), also permits a more accurate and
complete dynamical analysis (e.g., \citealt{Tortora2010,Tortora2011}).

A quantitative dynamical model to fit the whole 2D maps for the rotation
and the velocity dispersion, is out of the purpose of this paper but will be performed in future work.
Only with a complete 2D kinematical map of a galaxy (up to at least $1$$R_{\rm eff}$) as well as a robust dynamical model it
will be possible to measure the DM fraction, trace its radial distribution as a function of the mass of the halo,
and test plausible environment dependencies.
In future work we therefore plan to perform a detailed study of the stellar content of ETGs to
combine spatially resolved stellar information on the central region with planetary nebula
data on the outskirts (up to $\sim 5'$) with the final purpose of obtaining the complete rotation curve and
distribution of dark matter (e.g. \citealt{Napolitano2009,Napolitano2011}).

Moreover, thanks to a complete and detailed dynamical analysis, we will have a completely independent measurement of the IMF slope that
we will compare to the one obtained by stellar population modeling. If both methods agree on the resulting IMF, this will be
a strong test of the absence of hidden systematics.

Finally another possible interesting follow-up will be studying the dynamics and the IMF normalization of this galaxy in the phenomenological
framework of  the Modified Newtonian Dynamics theory (MOND, \citealt{Milgrom1983a,Milgrom1983b}, following the approach presented in \citealt{Tortora2014a}).

\section*{Acknowledgments}
The use of the Penalized Pixel Fitting developed by Cappellari \& Emsellem is gratefully acknowledged.
Data were reduced using EsoRex and XSH pipeline by ESO Data Flow System Group.
C.S. thanks S.C. Trager for the use of the code SPINDEX2 and C. Conroy for the precious help in
understanding and using his stellar population models.
C.T. has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement n. 267251.
We thank the referee for very constructive comments

redpajama_set_name: RedPajamaArXiv


iPad Best utility to view hidden files on iPad?
Discussion in 'Jailbreaks and iOS Hacks' started by patent10021, Feb 8, 2014.
I bought a book from an online store that has an app so you can view the books in the app and in the app without internet in online viewing mode. When you choose to download the book for offline viewing you can see the book being downloaded into the app with a progress bar. Whether or not the book is in ePub, PDF format or made up of hundreds of JPEG pages I don't know but the book is definitely in the app's or iPhone's documents folder. Using iFunBox and iExplorer I found hundreds of jpegs of fig.1 fig.2 fig.3 etc images that the book uses. Problem is I never found the main book pages. I suspect the pages are in the same location but hidden or somewhere else on the phone.
Where could the book be and what JB utility do you recommend?


I wrote this when I just discovered Blog Engage and My Guest Blog and reaslised how powerful guest blogging/posting can be. Although it's sad I haven't been able to do as much guest blogging as I would like I'm going to try and revive that for 2011 (one of my resolutions...) because it's such a great opportunity to meet new readers and network.
This was an updated article on using the Google Webmaster Tool for keyword research, the first article can be found here. The first article was more basic plus GWT was updated with more information which I found very useful for keyword research, so I decided to blog about it and give it an update.
Facebook Pages Vs Accounts, which do you prefer?
This was actually written in response to a question related to this topic which a friend of mine over at Techsling asked me. I figured since I had done so much research into it and was quite happy with my results I'll publish it as blog post, which I did! Glad that I did, turns out it was helpful for people.
This was a guest post written by Ben Hook from Navaro which touched a topic which was quite popular at the time of publish. It talks about the benefits of setting up 301 Redirects but also noted that they don't pass on the full pagerank to the redirected page. It lastly talked about what the alternative to redirects were if you had to redirect pages.
This was similar to the keyword research using Google Webmaster Tool but instead talks about keyword research with the Keyword Tool. I had a lot of fun writing this as well because I was just learning how to use it myself so it was literally fresh in my head and exciting.
This article which seems to be one of the favorites of most people (and mine too) seeing as it came in second talks about internal link builidng, which is something I believe is highly undermined. It can go a long way in helping internal pages by getting it to rank on search engines and letting the search engines know the hieracrhy of your website.
That's the round up of top posts for 2010. Hopefully there will be better and more insighful posts in 2011. In the mean time I hope to get my blogging juice back and resume blogging as normal next week.


We're saluting magnificent Mexican food from all around the country starting with Alton Brown's favorite homemade salsa in Columbus, Ohio. Ali Khan then serves up a true Mexican original with beef carnitas tacos in Austin, Texas, and Alex Guarnaschelli's favorite Al Pastor at Lene Brave in Chicago is so good, it has customers begging for more. Plus, more best bite revelations from Jeff Mauro, Simon Majumdar, Patricia Jinich, and Beau MacMillan.
See some of the best-ever ice creams, pizzas, burgers and more from The Best Thing I Ever Ate, here.


text:
VR Goggles For More Than Typical Gaming
Oculus VR, an Irvine, California-based company, started shipping their $300 goggles to software developers in March. What's so great about these goggles? They allow a gamer to actually put themselves in a virtual world created by a computer.
The cool part, however, is that these particular Oculus Rift goggles are starting to make their way into applications that are not just for gamers.
NASA believes scientists and the public alike, could explore Mars' surface through virtual reality; rather than via spaceship travel. An Indiana manufacturer researches ways to save money by using VR to demonstrate products. Michigan architects can visualize a home that hasn't had any construction started yet.
The goggles are not finished; they're still a work-in-progress. People still experience motion sickness due to the lack of ability to track the full-range of our motions.
Walt Scacchi, University of California-Irvine's Institute for Virtual Environments and Computer Games' research director, believes that people prefer something better than "wandering around with a head-mounted display in a 3-D stereoscopic world." However, he is also confident that technology will improve for VR including less delay and improved screen resolution, which will empower the immersiveness we can experience in virtual reality environments.
Getting On Top of the Problems
The company is already trying to solve the problems above and others not fully made aware yet. In June, Oculus raised $16 million in venture capital, and they're using those funds to hire VR experts to tackle these issues. They take the feedback from users very seriously and have sold over 35,000 developer kits.
The Orange County Register actually requested some feedback from many people that have tried using the Oculus Rift in different industries, to get an idea of how they're using VR in their industry, as well as what they feel is holding the technology back.
Matterport is a Mountain View, California-based firm. The firm has raised ten million dollars to build a camera that will make 3-D room models (as well as other interior spaces) with accuracy and that can be shared online. In other words, envision being able to redecorate your home virtually before actually taking the first step to do so. The CEO of the firm, Matt Bell, provided some feedback and insight.
Matt Bell, the CEO, said that one of his favorite experiences with Rift was the preschool. He had the user height set to 3 feet so he could explore the preschool as if he was a preschooler. He said it brought back a lot of memories including posters high on the walls, countertops that were unreachable, and toys all over the ground. He also said that he has never actually been to that preschool, only through Rift. They captured images of the entire school which included many large rooms. Bell stated that it took approximately 90 minutes to capture the whole building and that processing it into a 3D model took half an hour and was a fully automatic process.
Walking on Mars
A lab with a focus on projects that alter the way humans control and interact with spacecraft, is the Missions Operations Innovation Office at NASA's Jet Propulsion Laboratory based in Pasadena, California. The leading computer scientist heading this mission is Jeff Norris. Prior to this position he actually worked on the development and uplink system to command the Mars Curiosity Rover.
Norris stated:
"One of the things we're investigating is the use of immersive displays for looking at data returned from spacecraft. We're looking at virtual reality technology as a way for our scientists and engineers to better understand the environment around a spacecraft and then better control that spacecraft."
He also said that they are going to look at using the technology to share the missions with people of the public and that devices such as Rift which are inexpensive are making it easier to reach a much more broad audience.
Norris also said that it is not hard to imagine that in the near future the majority of the public will have access to this technology and will be able to experience the journeys right alongside them. He said it is now possible to put devices such as Rift into the hands of mission science teams.
One NASA demo takes information from the Curiosity Rover on Mars and turns it into panoramic views, as if you were sitting on the vehicle looking around. Another lets you move around the International Space Station, in 3-D, using an Xbox controller.
"If we put humans on Mars someday, we should have millions of people there with them standing beside them in this holodeck-like way. In 1969, the television was the most engaging and effective medium for bringing the world along. It was the perfect choice at the time. It's not the perfect choice now."
Lose the Tanks
A company located near Indianapolis makes pressure vessels; Wessels Co. These pressure vessels are huge containers (up to 12 feet across) that are costly to buy (thousands) and may end up being used as part of a water-heating or drinking-water system. Jay Fuller works for the company and provided his feedback on VR in their industry.
Fuller stated that they do a few large industry tradeshows every year and that it involves shipping some very large tanks between the convention halls which can get to be expensive. He thought it would be a better idea to use virtual reality to showcase their larger tanks in a demo at these tradeshows.
They model all of their tanks using SolidWorks. SolidWorks is a 3D modeling software program. Fuller said it was relatively a painless process to convert the tanks into meshes that were suitable for the game engine. They are planning on premiering their finished demo at the biggest tradeshow in January. That tradeshow is in New York and called the AHR Expo.
The Virtual Architect
Wisconsin-based consultancy firm, Arch Virtual, is spearheaded by the lead developer, Jon Brouchoud who possesses a master's degree in architecture. Brouchoud was hired to create 3D walk-throughs of buildings for web browsers. That was before the Oculus Rift came to be. Now he maintains a steady stream of work for a variety of clients that includes universities, architects, corporations and real estate developers, and ports the work to the Oculus gear.
"We've been focusing on short and sweet experiences. We're finding that just putting an Oculus Rift on someone is enough all by itself to just blow people away. There's a bit of overhyping in terms of game development. It might just be because I'm not a game developer. I don't see people wearing this for extended periods of time playing long game experiences - first-person shooters, where they're running around.
Brouchoud said that most of the people that they are showing their projects to have never used the Oculus Rift before. He said that they are typically not prepared and can only handle a few minutes of walking around but that is all that they need. He said you can stand inside the lobby of a building about to be constructed and walk around and really experience it.
Brouchoud also stated that most people who experience this are in awe. He said that possibly 1 in 30 people do not understand the experience. They tried out this demo on a hundred architects around San Fransisco and Chicago and most of them were blown away.
vr,

redpajama_set_name: RedPajamaCommonCrawl


text:
Sam Pittman Excited Razorbacks Land in Outback Bowl
by: Otis Kirk
Photos Courtesy: University of Arkansas Athletics
FAYETTEVILLE — Arkansas' Sam Pittman held a Zoom presser about the No. 21 Hogs landing in the Outback Bowl.
Arkansas (8-4) and Penn State (7-5) will meet for the first on the football field New Year's Day at 11 a.m. (Central) and televised on ESPN2. Since the bowl announcements were just released Pittman didn't know much about Penn State at this time as far as indepth scouting.
"Just want to say we're so excited to play in a New Year's Day bowl against a great opponent in Penn State University," Pittman said. "It's been an exciting day for us, the University of Arkansas and our program. Can't wait to get down to the sunshine of Tampa, Florida and eat a couple of Bloomin' Onions."
Former Vanderbilt head coach James Franklin is at Penn State. Pittman was asked how much he has crossed paths with Franklin?
"No, I haven't," Pittman said. "I've met Coach Franklin, but I don't know him much better than that. Just a lot of really positive things that people who have worked with him have said about him. Highly successful guy. Highly intelligent guy. Great football mind. Certainly, Penn State is one of the storied programs in the country. Coach (Dowell) Loggains worked up there before the summer as an analyst before we were able to hire him back. He probably would know a little bit more and be able to answer your question better."
How much will you pick Loggains' brain on the Nittany Lions?
"I haven't seen Dowell since, well, that's not true," Pittman said. "He came in and was excited about the bowl and I was walking out to do a home visit. That would certainly be something we talk to him about to see, might be more personnel driven than anything, but certainly we would ask him about. We have 12 videos, 12 films,12 games as well, but he might know something a little bit more about personnel."
Franklin has led Penn State to a 67-32 record in eight seasons, including a 2016 Big Ten championship, just the second outright Big Ten title for the team since the Nittany Lions joined the league in 1993.
As far as his own team Pittman feels they will be excited and very motivated to play this game.
"I think they're unbelievably excited," Pittman said. "There's not many of them in there that's been to a bowl. So, to get to a New Year's Day bowl, and one as prestigious as the Outback Bowl, they'll be ready and they'll be excited. It'll make practice a little bit easier for them I would say."
Pittman said he didn't get a chance to talk to the team about the bowl selection since it was already on social media.
"I wish I had the opportunity to do some of those things," Pittman said. "I think Twitter and Google, or whatever, had it out before I found out about it. It was out. Hunter (Yurachek) called me and told me we were going to get the invite to the Outback Bowl, and they'd be calling in a few minutes. I said 'That's awesome.'
"We'd had several official visits in. They were wrapping up and getting ready to leave. I just came out of a home visit now. So, I haven't had a lot of time. I was able to talk to the officials at the Outback Bowl. They extended the offer. Of course, Mr. (Greg) Sankey called from the SEC and extended that. Whenever they said Outback Bowl, I was proud of that. I'm proud of our football team, our coaches, our assistant coaches. I'm very happy. We didn't send anything out to the team because Lord knows we know they look at their phones all the time, so I'm sure they already knew it."
As noted this will be the first time Arkansas has not only played Penn State, but the initial time to be in the Outback Bowl.
"I think it's something the kids have accomplished, the assistant coaches have accomplished," Pittman said. "I mean, I don't know if they accomplished us playing Penn State, you know, but I think that just happened. We're excited to play a team like Penn State. A lot of tradition there, good football coach, good players. I'm happy for the state of Arkansas, happy to get down there and get us some nice weather. I heard it's 82 or something today. Get down there, have a little fun."
The first practice for Arkansas will be on Friday.
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