text:
\section{Introduction} \label{sect:intro}

Ultraluminous infrared galaxies (ULIRGs) are advanced mergers of
gas-rich galaxies. They have an infrared luminosity greater than
10$^{12}$~L$_\odot$ in 8-1000 $\mu$m band \citep[e.g.][]{sm96,lfs06}.
Their high infrared luminosity comes from violent starbursts with
significant contribution from active galactic nuclei (AGNs) in some
ULIRGs \citep[e.g.][]{fae03}.

ULIRGs can be classified according to dominance of starburst or AGN
component, namely as the HII-like ULIRGs, LINER ULIRGs, Seyfert-HII
composite ULIRGs, Type 1 ULIRGs and Seyfert 2
ULIRGs. \citet{sse+98,sse+982} proposed an evolutionary scenario of
ULIRGs from cool-ULIRGs to warm-ULIRGs and finally to QSOs. The
cool-ULIRGs have $f_{25}/f_{60} \le 0.2$ and are preferably
star-forming galaxies \citep{ham87}, i.e. the HII-like galaxies. Here
$f_{25}$ and $f_{60}$ are flux densities at 25~$\mu m$ and 60~$\mu m$,
respectively. The warm-ULIRGs have $f_{25}/f_{60} > 0.2$ and
preferably host an AGN \citep{dmlj85,bsh+86}. ULIRGs are important to
understand the evolution of merger galaxies and the possible
connections between the starburst and AGNs.  Further imaging and
spectroscopy studies
\citep[e.g.][]{ssv+98,ss99,sse00,ltd+03,sls+06,nls+07,vrk+09} and
numerical simulations \citep[e.g.][]{ks92,sdh05,njb06} support this
evolutionary scenario. However, this standard evolution sequence is
questioned by \citet{cbb+01,gtr+01,tgl+02,rtg10}.

If the standard evolutionary scenario is true, ULIRGs should
experience the continuing conversion of gas component to stellar
populations in {their} lifetime. ULIRGs in the earlier evolutionary
stage are expected to possess more gas and young stars, less old
stellar populations, smaller stellar mass and larger gas mass fraction,
compared with those of ULIRGs in a later evolutionary stage. There
should be enough gas in early stage ULIRGs to be converted into
stars when they evolve to a later stage for a larger stellar
mass.

The stellar population analysis of ULIRGs can shed light on ULIRG
evolution. Previous such analyses were only carried out on very small
samples \citep[e.g.][]{cs00,cs002,cs01,rhtg07,rtg08,sm10}. A slightly
larger sample of 36 local ULIRGs was studied by
\citet{rtg09,rtg10}. In contrast to the standard evolutionary
scenario, their stellar population analysis based on the optical
spectra exhibits no significant differences of the stellar ages among the
HII-like ULIRGs, LINER, and Seyfert 2 ULIRGs. Note that {the} physical
parameters of ULIRGs are rather scatter \citep[e.g.][]{vrk+09},
{therefore,} the possible evolutionary of ULIRGs can not be revealed
if only a small sample is applied to.

In this work, we {analyse} the spectra of 160 ULIRGs available from
the Sloan Digital Sky Survey \citep[SDSS,][]{aaa+09} for stellar
populations. In Section 2, we introduce our ULIRG sample. The stellar
population analysis of the sample is presented in Section 3.  In
Section 4, we discuss the inferred stellar age, mass and gas for
different types of ULIRGs. {Several} factors which affect our analysis
are discussed in Section 5, and conclusions are given in Section 6.

In this paper, we adopt $H_0$ = 70 km s$^{-1}$ Mpc$^{-1}$,
$\Omega_{\rm m} = 0.3$ and $\Omega_{\rm \Lambda} = 0.7$.

\section{The ULIRG sample}
\label{sect:Obs}

For reliable stellar population analysis, we work on a large sample
of ULIRGs which have optical spectra
covering the wavelength regions of 4000~$\rm \AA$ break and strong
stellar absorptions near 4000~$\rm \AA$.

\begin{figure*}[bt]\centering
\includegraphics[angle=270,width=56mm]{NII_BPT.ps}
\includegraphics[angle=270,width=56mm]{OI_BPT.ps}
\includegraphics[angle=270,width=56mm]{SII_BPT.ps}
\caption{BPT diagrams for line ratios of 185 narrow-line ULIRGs.}
\label{bpt}
\end{figure*}

\begin{figure}[bt]
\centering \includegraphics[angle=270,width=83mm]{dis_sub.ps}
\caption{Redshift distribution of 160 narrow line ULIRGs, after we
  discarded 22 ambiguous objects and 3 Seyfert-HII composite ULIRGs
  with bad pixels from 185 narrow-line ULIRGs.}
\label{disz}
\end{figure}

The SDSS database \citep[DR7,][]{aaa+09} released the spectra of more
than 920,000 galaxies in the range of 3800~$\rm \AA$ to 9200~$\rm \AA$
in the observer frame. Following the procedures described in
\citet{hwh09}, we found 398 ULIRG candidates from the SDSS DR7
spectral catalog \citep{aaa+09} and {\it IRAS} Faint Sources Catalog
\citep{mkc92}. We checked them from NASA/IPAC Extragalactic Database
(NED) and SDSS images. We found that 38 of them are wrong
identifications of ULIRGs due to either the known redshift of a ULIRG
in the NED not consistent with the redshift from the SDSS database or
an obviously nearby large bright galaxy as an IRAS source but with a
mis-matched SDSS redshift. The spectra of 360 identified ULIRGs are
then fitted and classified \citep{hwh09}. Among them, 73 ULIRGs have
broad lines and are of Type 1, and 287 objects are narrow-line ULIRGs.
We will not work on Type 1 ULIRGs for stellar population studies in
this paper because their spectra are dominated by strong AGN features
(e.g. the power-law continuum, the strong and broad emission lines,
the strong {  Fe$_{\rm II}$} features).

Based on the line ratios in {the} BPT diagrams \citep[see
  Figure~\ref{bpt},][]{bpt81,kgkh06}, 185 of 287 narrow-line ULIRGs
are further classified as 32 HII-like ULIRGs, 77 Seyfert-HII composite
ULIRGs, 48 Seyfert 2 ULIRGs, 6 LINER ULIRGs, and 22 ambiguous
objects. We omitted the other 102 narrow-line ULIRGs from stellar
population analysis, because one or more lines either are redshifted
outside the wavelength range or do not have a good signal-to-noise
ratio for the classification in the BPT diagrams. We also discarded 22
ambiguous ULIRGs for our analysis because they are shown as one type
in {one} BPT {diagram} but another type in the other diagram(s). Three
Seyfert-HII composite ULIRGs are further skipped because more than
half of pixels in their SDSS spectra are masked as bad. Therefore, we
will study the stellar populations of 160 well-classified
ULIRGs. Their redshift distribution is shown in Figure~\ref{disz}.

\begin{figure}[tb]
\centering \includegraphics[angle=270,width=85mm]{combin2.ps}
\caption{Combined spectra of {  four types} of narrow-line
ULIRGs.} \label{combin}
\end{figure}

In Figure~\ref{combin} we show the combined spectra for four types of
narrow-line ULIRGs. The spectrum of every ULIRG is first normalized by
the {  median} flux in the wavelength $4010~{\rm \AA}$ -- $4060~{\rm
 \AA}$. The combined spectra are the weighted mean of the normalized
spectra according to their signal-to-noise ratio in the wavelength
range of $5300~{\rm\AA}$ --$5800~{\rm\AA}$ in the rest frame. The
combined spectra clearly show that along the sequence of HII-like,
Seyfert-HII composite, Seyfert 2, and LINER ULIRGs, the normalized
continuum fluxes below 4000 ${\rm \AA}$ decrease and the fluxes above
4000 ${\rm \AA}$ increase, which roughly indicates that the fraction
of old stellar populations increases along the sequence.

\section{Stellar population analysis}

The stellar population analysis is an important tool to study star
formation in galaxies and evolution of galaxies. It has been applied
to various type of galaxies, e.g. HII galaxies \citep[e.g.][]{sbp96,
wctk04}, AGNs \citep[e.g.][]{cgs+04,cgm+04}, infrared selected
galaxies \citep{clh+09,clh+10}, ULIRGs \citep[e.g.][]{rtg10,mwg+10}.
Here, we use it for a large ULIRG sample to study the evolution
sequence of ULIRGs.

We noticed that the fiber diameter of SDSS spectrograph is $3''$,
corresponding to $\sim$~3~kpc for a galaxy at redshift $z\sim0.05$
or $\sim18$~kpc at $z\sim0.25$. For any galaxies with different
redshifts, the observed spectrum comes from central regions of
different size. We use the software,
STARLIGHT \footnote{http://www.starlight.ufsc.br} \citep[{  version
04, }][]{cms+05,msc+06,acs+07}, to analyze the stellar populations of
ULIRGs in the central {  regions}. We will discuss the aperture
effect later.

\begin{figure*}[bth]
\centering
\includegraphics[angle=270,width=140mm]{example_1.ps}
\caption{{  One example} for spectrum fitting. We show the
  normalized observed spectrum ($F_{\lambda}/F_{\lambda4020}$, black)
  and the modeled spectrum (green) {  in the left-upper panel and
  the residual in the left-lower panel}. The key parameters from the
  fitting: $\chi^2$, mean stellar age, stellar mass and extinction
  parameter are given in the right side. The fractional
  contribution to the model flux ($x_j$) and the stellar mass
  ($\mu_j$) of the $j$th SSP are plotted in the right.}
\label{2examp}
\end{figure*}

The STARLIGHT fits an observed galaxy spectrum $O(\lambda)$ with a
combination of $N$ simple stellar populations (SSPs). The intrinsic
extinction due to the foreground dust in the host galaxy is
considered and parameterized by the $V$-band extinction $A_V$. The
line-of-sight stellar motions are modeled by a Gaussian distribution
$G(v_0,\sigma_*)$ centered at the velocity $v_0$ and with the
dispersion $\sigma_*$. The modeled spectrum $M(\lambda)$ is
described by:
\begin{equation}
M(\lambda)=M_{\lambda_0}[\sum_{j=1}^{N}x_jb_{j}(\lambda)\otimes
G(v_0,\sigma_*)]r({\lambda})
\end{equation}
where $M_{\lambda_0}$ is the synthetic flux normalized at
$\lambda_0$, $x_j$ is the fractional contribution of the $j$th SSP
to the model flux at $\lambda_0$, $b_{j}(\lambda)$ is the normalized
spectrum of the $j$th SSP, and
$r(\lambda)=10^{-0.4[A(\lambda)-A_{\lambda_0}]}$ is the reddening
term. The best fitting to search for the minimum
$\chi^2=\sum_{\lambda}[(O(\lambda)-M(\lambda))\cdot w(\lambda)]^2$,
where {  $w(\lambda)$ is the weight factor, and $w(\lambda)^{-1}$ is
  the uncertainty of observed spectrum $O(\lambda)$ given in the
  SDSS database}.
We used a base of $N=45$ SSPs with different ages and metallicities
from the evolution synthesis models of \citet{bc03}, and adopted the
initial mass function from \citet{cha03} and the Padova 1994
evolutionary tracks \citep{abb+93,bfbc93,fbbc94,gbc+96} and STELIB
library \citep{lbp+03}. The base comprises of star population with 15
different ages between 1~Myr to 13~Gyr at each of the three
metallicities: 0.2, 1, and 2.5 Z$_\odot$. Here Z$_\odot$ is the
metallicities of the Sun. The reddening law of \citet{cks94} is
adopted in the fitting.

We obtained the spectra with uncertainties of 160 ULIRGs from SDSS.
We corrected the Galactic reddening effect, and converted each
spectrum to the rest-frame. The STARLIGHT was used to fit the
continuum and absorption features. The emission lines and sky lines
are discarded in the mask file of STARLIGHT. The spectrum pixels
without error measurements or with negative flux values are
excluded. In addition, the Na D doublet, $5870~{\rm \AA}-5905~{\rm
  \AA}$, and other three bands, $6845~{\rm \AA}-6945~{\rm \AA}$,
$7550~{\rm \AA}-7725~{\rm \AA}$, and $7165~{\rm \AA}-7210~{\rm \AA}$
are also masked, due to the bugs in SSP model  {  \citep{lbp+03}}
or the large fitting residual in some regions \citep{msc+06}.
Considering the redshift coverage of our sample, we restricted the
fitting in the wavelength range $3400~{\rm \AA}-6700~{\rm \AA}$ for
each spectrum. A power-law component,
$F(\lambda)\propto\lambda^{\alpha}$, is used in the STARLIGHT to
account the AGN contribution to the observed continuum
\citep{cgm+04, cms+05}, and $\alpha=-1.5$ \citep{rs80,cgm+04} is
adopted. The random Markov Chains method was used in the STARLIGHT,
which needs an input of integer seed. Different seeds slightly
affect the fitting results. Following \citet{mwg+10}, we fit each
spectrum 100 times with different seeds. The final fitted parameters
are the mean values from 100 runs. One example of the spectrum
fitting {  is} shown in Figure~\ref{2examp}.

\begin{deluxetable}{lcccc}[bth]
\tabletypesize{\scriptsize} \tablecolumns{5} \tablewidth{0pt}
\tablecaption{{  Mean fractional contributions of different stellar
  populations} and the power-law component to the model flux at 4020
  $\rm \AA$ for different types of ULIRGs}
\tablehead{
\colhead{Type} & \colhead{young} & \colhead{intermediate-age}
& \colhead{old} & \colhead{power-law} \\
 &($<10^8$ yr) & ($10^8-10^9$ yr)& ($>10^9$ yr) &
}
\startdata
HII-like  & 0.622  & 0.261  & 0.117 &     \\
Composite & 0.355  & 0.408  & 0.138 & 0.099\\
Syefert 2 & 0.177  & 0.500  & 0.198 & 0.125\\
LINER     & 0.112  & 0.579  & 0.261 & ~0.048
\enddata
\label{tab_age}
\end{deluxetable}

\begin{figure}[bth]
\centering
\includegraphics[angle=270,width=85mm]{dis_3.ps}
\caption{Fraction distributions of stellar populations
for different types of ULIRGs from top to bottom.}
\label{frac}
\end{figure}

The stellar populations in a galaxy can be described by the
fractions of young stars of $t_j < 10^8$~yr, intermediate-age stars
of $10^8$~yr~$\le t_j \le 10^9$~yr, and old stars of $t_j > 10^9$~yr
\citep{cms+05}. Here $t_j$ is the age of the $j$th SSP.  We obtain
the fractional contributions of these three stellar populations of
different ages and the power-law contribution to the model {
spectrum} flux at 4020 $\rm \AA$. For each type of ULIRGs, we got
their means as given in Table~\ref{tab_age}. Because there are only
a small number (only 6) of LINER ULIRGs, we will not discuss their
stellar population in the following.

The fractional contributions ({  i.e. $x_j$ in Equation~1}) of these
stellar populations to the total stellar emission are shown in
Figure~\ref{frac}. We found that they are very different for different
types of ULIRGs. The young stellar population is more dominant for the
HII-like ULIRGs than the composite and Seyfert 2 ULIRGs. The stellar
populations of intermediate-age and old stars are more dominant in the
Seyfert 2 ULIRGs than HII-like and composite ULIRGs. The older stellar
populations and the significant power-law component in Seyfert 2 ULIRGs
suggest that they are at a more evolved stage in the evolution track
towards AGNs. The fraction distribution of stellar populations of
composite ULIRGs {  suggests} that they are at the transitional
stage between HII-like and Seyfert 2 ULIRGs.

\section{Physical parameters of different types of ULIRGs}

The results of stellar population analysis of ULIRGs suggest the
possible evolution sequence from HII-like, composite, to Seyfert 2
ULIRGs. The HII-like ULIRGs are at an earlier evolutionary stage, the
composite ULIRGs are at a transitional stage, and the Seyfert 2 ULIRGs
are at a more evolved stage. In this section, we discuss the physical
parameters of ULIRG galaxies, namely, the mean stellar age, stellar
mass, and gas mass, which may be related to the possible
evolutionary sequence.

\subsection{The mean stellar age}

Based on the results of the stellar population analysis, we
can get the light-weighted mean stellar age \citep{cms+05}:
\begin{equation}
\langle \log t_\ast  \rangle_L=\sum_{j=1}^{N} x_j \log t_j,
\end{equation}
which is an indicator of star formation history. The other such an
indicator is D$_n$(4000) obtained by the MPA/JHU
group\footnote{http://www.mpa-garching.mpg.de/SDSS/DR7/}, which is
defined as the average flux density ratio for the bands $3850~ {\rm
 \AA}-3950~ {\rm \AA}$ and $4000~{\rm \AA}-4100~ {\rm \AA}$
\citep{bru83,bmy+99}. We compared them (Figure~\ref{age}) and
found that they are well correlated, with the Spearman Rank-Order
Correlation Coefficient of $r_s=0.90$. The best fitting is
\begin{equation}
D_n(4000)=-(0.24\pm0.06) + (0.18\pm0.01)
\langle \log t_\ast  \rangle_L .
\end{equation}

\begin{figure}[tb]
\centering \includegraphics[angle=270,width=85mm]{l_age3.ps}
\caption{Light-weighted mean stellar ages of ULIRGs estimated by
  the stellar population analysis are compared with the D$_n$(4000)
  obtained by the MPA/JHU group. The solid line is the best fit for
  all ULIRGs.  The distributions of the mean stellar ages for
  each type of ULIRGs are shown in the right panels.}
\label{age}
\end{figure}

The distributions of $\langle log t_\ast \rangle_L$ for HII-like,
composite and Seyfert 2 ULIRGs are shown in the right panels of
Figure~\ref{age}. The mean values of ${\langle log t_\ast \rangle_L}$
for three types of ULIRGs, HII-like, composite, and Seyfert 2, are
7.6, 8.0 and 8.4, with the standard deviations of 0.4, 0.5 and 0.4,
respectively. The increase of these mean values is consistent with the
evolution sequence from HII-like ULIRGs and composite ULIRGs to
Seyfert 2 ULIRGs. The young stellar population ($t_j<10^8$~yr) are
always present in ULIRGs (see Figure~\ref{age}) due to the enhanced star
formation in galaxy merger process. The large deviations of $\langle
log t_\ast \rangle_L$ for these types of ULIRGs are probably caused by
the complex dynamical process and star formation history of merger
systems. Therefore, both $\langle log t_\ast \rangle_L$ and
D$_n$(4000) are only the rough age indicator of ULIRGs.

\subsection{The stellar mass}

ULIRGs experience the continuing conversion of gas to stars.  The
stellar masses in ULIRGs are mostly contributed by intermediate-age
and old stars (see $\mu_j$ distribution in Figure~\ref{2examp}), and
thus are a possible indicator for the ULIRG evolution.

The stellar mass of a ULIRG in the central 3$^{\prime\prime}$ for the
SDSS fiber spectrograph, $\mathcal{M}_{fiber}$, in unit of $M_{\odot}$,
can be estimated from the the stellar mass parameter
$\mathcal{M}_{cor\_tot}$ given by
STARLIGHT\footnote{http://www.starlight.ufsc.br/papers/Manual\_StCv04.pdf}:
\begin{equation}
\mathcal{M}_{fiber} =\mathcal{M}_{cor\_tot}\times
 10^{-17} \times4 \pi d^2\times(3.826\times10^{33})^{-1},
\end{equation}
where $d$ is the luminosity distance in cm. The aperture effect must
be corrected by using the SDSS Petrosian magnitude \citep{bde01},
$m_{\rm Petro}$, and fiber magnitude, $m_{\rm fiber}$, so that the estimated
mass can be a constant fraction of the total mass of galaxies,
independent of their positions and redshift. The aperture correction
factor for each SDSS photometric band is roughly given by \citep{hmn+03}:
\begin{equation}
A=10^{-0.4(m_{\rm Petro}-m_{\rm fiber})}.
\label{aper1}
\end{equation}
The spectra of ULIRGs fitted for the stellar population analysis
roughly cover the $u$, $g$, $r$, $i$ and $z$ bands. We take the
average of the correction factors of these bands weighted by
their uncertainty $\delta_A$,
\begin{equation}
\overline{A}=\sum_{j=u,g,r,i,z}\frac{A_j}{\delta_{A_{j}}^2}
/\sum_{j=u,g,r,i,z}\frac{1}{\delta _{A_{j}}^2},
\end{equation}
to correct the aperture effect for each ULIRG. The corrected stellar
mass, $\mathcal{M}_{*}$, in unit of $M_{\odot}$, which is a constant
fraction of the total stellar mass in a ULIRG, then can be estimated
by
\begin{equation}
\log(\mathcal{M}_{*})=\log(\mathcal{M}_{fiber})+\log(\overline{A}).
\end{equation}

\begin{figure}[tb]
\centering
\includegraphics[angle=270,width=75mm]{m_stellar.ps}
\caption{Aperture-corrected stellar masses, $\mathcal{M}_{*}$, of
  ULIRGs calculated from the STARLIGHT parameters are compared with
  the stellar masses estimated from the SDSS photometric data by the
  MPA/JHU group (webpage in footnote No.5). The solid line is the best
  fit for all ULIRGs. The {\it total dynamical masses} of four ULIRGs,
  F09039+0503, F13428+5608, F15250+3609 and F15327+2340, are estimated
  from the central velocity dispersion and plotted as squares with
  error-bar. The distributions of the stellar masses for each type of
  ULIRGs are shown in the lower panels.}
\label{mass}
\end{figure}

We obtained $\mathcal{M}_{*}$ for the ULIRGs in our sample. { To show
  the uncertainty of such corrected mass estimates from the fiber
  spectrum of the central part of ULIRGs, we} compared them with the
total stellar masses of whole galaxies estimated by the MPA/JHU group
from the SDSS photometric data of $u$, $g$, $r$, $i$ and $z$ bands
\citep[see the footnote No.5 on their webpage,][]{src+07}. We found
that they are well correlated (see Figure~\ref{mass}) with the
Spearman Rank-Order Correlation Coefficient $r_s=0.80$, which means
that the aperture-corrected stellar masses calculated from the
STARLIGHT parameters are statistically fine. The data scatter in
Figure~\ref{mass} roughly indicates the uncertainty of the mass
estimates. \footnote{In our sample, the {\it total dynamical masses}
  of four ULIRGs, F09039+0503, F13428+5608, F15250+3609 and
  F15327+2340, can be calculated from the central velocity dispersion
  \citep{dtd+062}. As suggested by the referee, we got $\log \mathcal
        {M}_{dyn} [M_\odot]$ of 10.9, 11.1, 10.9, and 11.2 and plotted
        them in the Figure~\ref{mass} for comparison with the {\it
          total stellar masses} derived by the stellar population
        analysis. Considering the typical gas content of ULIRGs of
        $\sim$~10$^{10}M_\odot$ (see Section 4.3), we think different
        kinds of mass estimates are consistent with each other.}

The most important {feature} in Figure~\ref{mass} {is} the obviously
different distributions of $\log \mathcal{M}_{*}$ for HII-like,
composite and Seyfert 2 ULIRGs, whichever the masses estimated from
either spectral or photometric analysis are used. The mean of the
$\log \mathcal{M}_{*}$ distribution for the mass from the spectral
analysis for three types of ULIRGs, HII-like, composite, and Seyfert
2, are 10.70, 11.17 and 11.40, with the standard deviations of 0.45,
0.38 and 0.25, respectively. Seyfert 2 ULIRGs always have
$\mathcal{M}_{*} \gtrsim 10^{10.6}\; M_\odot$, larger than the masses
in HII-like or composite ULIRGs (see Figure~\ref{mass}). The increase
of the stellar masses along the sequence from HII-like ULIRGs to the
composite ULIRGs and Seyfert 2 ULIRGs is consistent with the standard
evolutionary scenario of ULIRGs.

\subsection{Gas in ULIRGs}

We noticed that Seyfert 2 ULIRGs mostly have $\mathcal{M}_{*}>
10^{10.6}M_\odot$ (see Figure~\ref{mass}). However, many HII-like
ULIRGs or composite ULIRGs have much smaller stellar mass,
$\mathcal{M}_{*} < 10^{10.5}M_\odot$. If the evolutionary sequence
from HII-like ULIRGs to composite ULIRGs and Seyfert ULIRGs is true,
there should be enough gas to be converted to stars. The gas mass in
ULIRGs is a key parameter to verify the standard evolution scenario of
ULIRGs.
\begin{figure}[tb]
\centering \includegraphics[angle=270,width=70mm]{mass_co_ratio.ps}
\caption{The estimated gas mass from the CO measurements (the upper
  panel) and the gas fraction of total mass (gas plus stars) in 10
  ULIRGs (the lower panel) are plotted against the aperture-corrected
  stellar mass $\mathcal{M}_{*}$. The dashed lines are the best
  fittings to the 9 ULIRGs except for the outlier, an HII-like ULIRG
  F08572+3915. We also plotted the gas masses of another 9 HII-like
  ULIRGs which have CO observations available in literature but no
  SDSS spectra for stellar population analysis and hence no stellar
  mass. The mean value for HII-like ULIRGs (
  $\log\mathcal{M}_{*}=10.70$, see Figure~\ref{mass}) is adopted for
  these 9 HII-like ULIRGs.}
\label{gas}
\end{figure}

We collected the CO observations of ULIRGs to study their gas content.
Up to now, $\sim$~60 ULIRGs and LIRGs have measurements of CO(1-0)
\citep{sss91,sdrb97,cny+09}. However, only 10 of them have the optical
spectra available from SDSS, and we have got the relevant mass
estimates. CO observations of 9 ULIRGs were observed by \citet{sdrb97}
using the IRAM 30m telescope, and 1 ULIRG by \citet{cny+09} using
FCRAO 14m telescope. The gas mass (in unit of of $M_\odot$) can be
estimated from the CO luminosity (in unit of K~km~s$^{-1}$~pc$^2$)
\citep{ds98},
\begin{equation}
\mathcal{M}_{H_2} \approx 0.8\times L_{CO}.
\end{equation}
After the CO luminosity is converted to the same cosmology adopted in
this paper, we got the gas masses for these 10 ULIRGs (see
Figure~\ref{gas}). They are between $10^{9.6}-10^{10.2}M_\odot$,
typical for normal gas-rich galaxies, except for the only one HII-like
ULIRG, F08572+3915, which have a much smaller CO luminosity
\citep{sdrb97,cny+09} and hence the smaller gas mass. Clearly, more
gas exists in ULIRGs with a smaller stellar mass. We further collected
CO measurements \citep{sss91,sdrb97,cny+09} of 9 HII-like ULIRGs
\citep{vks99}, which have no SDSS spectra available for stellar
population analysis above. We take the mean $\log \mathcal{M}_{*}$ for
these HII-like ULIRGs, and plotted them in Figure~\ref{gas}.

The gas mass from the CO measurements (the upper panel of
Figure~\ref{gas}) and the gas fraction of total mass (the lower panel
of Figure~\ref{gas}) {  seem} to be anti-correlated with the stellar mass
for the ULIRGs ($r_s=-0.60$ and $r_s=-0.88$), if we do not consider
the outlier F08572+3915. The anti-correlation is only marginally
significant because of the small sample of data available. The
possible anti-correlation is preserved for the gas fraction and the
stellar mass estimated from photometric analysis.

HII-like ULIRGs with a gas fraction $>10\%$ follow the
anti-correlation. Gas in ULIRGs may be eventually converted to
stars. We noticed that about half of HII-like ULIRGs have a stellar
mass less than $10^{10.6}M_\odot$ (see Figure~\ref{mass}). HII-like
ULIRGs in Figure~\ref{gas} have a gas mass less than
$\sim10^{10}M_\odot$ and a gas fraction less than $\sim15\%$. For
those less massive HII-like ULIRGs, there is not enough gas to form
stars, and they are not massive enough in total to evolve to Seyfert 2
ULIRGs ($\mathcal{M}_{*}\sim10^{11}M_\odot$). Only massive HII-like
ULIRGs ($\mathcal{M}_{*}>10^{10.6}M_\odot$) may follow the standard
evolutionary scenario of ULIRGs and have a possible connection between
the starbursts and AGNs.

\section{Discussions}

Stellar population analysis for narrow-line ULIRGs show the
systematical changes of stellar age and mass along the sequence
from the HII-like ULIRGs, to the composite ULIRGs and Seyfert 2
ULIRGs. Here we discuss {several} factors which may affect the results
of stellar population analysis.

\subsection{Power-law AGN contribution for spectral continuum}

During the stellar population analysis with STARLIGHT, we used a
power-law component, $F(\lambda)\propto\lambda^{\alpha}$, with a
fixed $\alpha=-1.5$ to represent the AGN contribution to the
continuum spectrum \citep{cgm+04,cms+05}. The AGN contribution is
significant for composite, Seyfert 2 and LINER ULIRGs, but not for
HII-like ULIGRs. However, the index for the power-law contribution,
$\alpha$, could be $-2.0$ to $-1.0$ \citep[see][]{ngcl98}.  To
evaluate the influence of the power-law index $\alpha$ in the
stellar population analysis, we re-do the fittings to the all
spectra of 160 ULIRG sample with different values of $\alpha$, from
$-1.0$, $-$1.25, $-$1.5, $-$1.75, to $-$2.0, for ten times each with
different random seeds. We found that the change of $\chi^2$ by
different $\alpha$ values is less than $\sim $1\%, which is not
adequate to use $\chi^2$ to judge the best $\alpha$ for fitting. {
Changes of the stellar mass
  and the mean stellar age caused by different $\alpha$ are always
  less than 10\%.} Therefore, the adopted power-law index of
$\alpha=-1.5$ is fine for the stellar population analysis.

\subsection{Different bases of simple stellar populations}

The evolutionary population synthesis method is mainly based on the
stellar evolution model. We have used a base of 45 simple stellar
populations (SSPs) for the stellar population analysis. The
different bases of SSPs may affect the fitting results. Following
the same procedures described in Section 3, we re-do the fittings to
the spectra for 160 ULIRGs with a base of 150 SSPs (25 ages and 6
metallicities) and a base of 15 SSPs (15 ages and 1 metallicity)
extracted from \citet{bc03}.  {Although} the fractional contribution
of each stellar population component does not remain the same and
may vary about 20\%, the mean stellar age and stellar mass do not
change {  significantly, less than $\sim$10\%. Their distributions} are
consistent with those shown in Section 4 for different types of
ULIRGs.

\begin{figure}[tb]
\centering \includegraphics[angle=270,width=83mm]{l_age_bias.ps}
\caption{Same as Figure~\ref{age} but only for ULIRGs in the
redshift range of 0.20$-$0.24.}
\label{age_z}
\end{figure}

\subsection{The aperture effect}

We made stellar population analysis for the SDSS spectrum of the
central $3''$ region. The aperture effect has been corrected for the
mass estimates, but not for the mean stellar age.  To evaluate the
aperture effect, we divided the ULIRG sample to several redshift
bins, and re-do the analysis. In each redshift bin, the linear size
of the aperture is almost the same for all ULIRGs, and the aperture
effect is almost the same.  Here we take the redshift bin of
$0.20<z<0.24$ as the example which has the largest number of ULIRGs
in the bin.  As shown in Figure~\ref{age_z}, the correlation between
$D_n$(4000) and $\langle log t_\ast \rangle_L$ keeps the same as the
whole sample of ULIRGs. The distributions of $\langle log t_\ast
\rangle_L$ for HII-like, composite and Seyfert 2 ULIRGs in the right
panel of Figure~\ref{age_z} also show {  similar offsets as the
whole
  sample. So do for other redshift bins.} Therefore, we believe that
the aperture effect does not influence our results.

\subsection{Extinction}

In the stellar population synthesis model of STARLIGHT
\citep{cms+05,msc+06}, the extinction was considered as a foreground
screen and fitted by one parameter, the $V$-band extinction $A_V$. But
the young, intermediate and old stellar populations have different
extinctions in a galaxy. Particularly the young stellar population was
more extinguished than the others, being in places very dust obscured.
Different $A_V$ should be assumed for the different populations.
However, this can not be achieved in the model.

\begin{figure}[bt]
\centering \includegraphics[angle=270,width=85mm]{a_v.ps}
\caption{Distribution of the extinction parameter $A_V$ given by
  the STARLIGHT model for HII-like ULIRGs, composite ULIRGs and
  Seyfert 2 ULIRGs.}
\label{extinc}
\end{figure}

From the stellar population analysis to ULIRGs, the distributions of
extinction parameter $A_V$ given by the STARLIGHT model for HII-like
ULIRGs, composite ULIRGs and Seyfert 2 ULIRGs are very similar, as
shown in Figure~\ref{extinc}. The means of $A_V$ for three types of
ULIRGs are 0.91, 1.09 and 0.92 with the standard deviations of 0.28,
0.39 and 0.36, respectively. The extinction parameters $A_V$ of
HII-like and Seyfert 2 ULIRGs on average are {  slightly} smaller
than that of composite ULIRGs, which is consistent with
\citet{vrk+09}.

The distributions of the mean stellar age for different ULIRGs
discussed in Section~4 are probably not influenced by the
simplified treatment of extinction in the model. The mean stellar age
given by the stellar population synthesis model are well correlated
with results of D$_n$(4000) (see Figure~\ref{age}), which verifies the
mean age. On the other hand, in ULIRGs, the stellar mass is dominant
by old stellar populations (see the right panels of
Figure~\ref{2examp}), which are expected to suffer less from
extinction than young stellar populations. Therefore, the simplified
extinction in the model probably does not affect our conclusions for
ULIRGs.

\section{Conclusions}

We analyse the stellar populations for a sample of 160 narrow-line
ULIRGs. They are optically classified as 32 HII-like ULIRGs, 74
Seyfert-HII composite ULIRGs, 6 LINER ULIRGs and 48 Seyfert 2
ULIRGs. We found that that along the sequence of HII-like, composite
and Seyfert 2 ULIRGs, both the mean stellar age and the
aperture-corrected stellar mass increase. This supports the standard
evolutionary scenario of ULIRGs in which the Seyfert 2 ULIRGs are in a
late stage of ULIRG evolution with a large mean stellar age and a
large stellar mass ($\sim10^{11} M_{\odot}$) while HII-like ULIRGs are
in an early stage with a young stellar age and a small stellar mass on
average.

Whether HII-like ULIRGs have enough gas for starburst, so that they
can evolve to Seyfert 2 ULIRGs? We collected CO measurements of 10
ULIRGs which have the SDSS spectra for the stellar population
analysis. The gas mass fractions seem to be anti-correlated with the
stellar masses for massive ULIRGs. All ULIRGs in our sample with CO
measurements have a gas mass less than $\sim10^{10} M_{\odot}$.
HII-like ULIRGs with a small stellar mass ($\mathcal{M}_{*} <
10^{10.4}M_\odot$) do not possess enough gases for starburst, and
therefore have no evolution connections with massive Seyfert 2
ULIRGs. We conclude that only massive HII-like ULIRGs and
composite ULIRGs may follow the evolution sequence toward AGNs.

\bigskip

\begin{acknowledgments}
  {We thank the referee for helpful comments, and} Dr. XiaoYan Chen,
 XianMin Meng and Ran Wang for discussions and suggestions.
  The authors are supported by the National Natural Science Foundation
  of China (10821061, 10833003 and 11033001), and the National Key
  Basic Research Science Foundation of China (2007CB815403,
  2007CB815405).
  The STARLIGHT project is supported by the Brazilian agencies CNPq,
  CAPES and FAPESP and by the France-Brazil CAPES/Cofecub program.
  Funding for the SDSS has been provided by the Alfred P. Sloan
  Foundation, the Participating Institutions, the National Science
  Foundation, the Department of Energy, the National Aeronautics and
  Space Administration, the Japanese Monbukagakusho, the Max Planck
  Society, and the Higher Education Funding Council for England. The
  SDSS Web Site is http://www.sdss.org.
\end{acknowledgments}

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


text:
Hotline Miami 2: Wrong Number: news and videos
UpdatesReviewPhotos
from our Community Blogs
What Hotline Miami 2: Wrong Number taught me about death
[I hold both Hotline Miami games in high regards as they are prime examples of doing a lot with so little in terms of gameplay. The games make you take an introspective look at yourself and question whether or not you may be a bad person be...
Hotline Miami 2's level editor is ready at last
The level editor for Hotline Miami 2 is no longer in beta, and to celebrate, I think a Carpenter Brut playlist is in order. If it seems like this rollout has taken its sweet time, I agree -- the game is over a year old and, initially, I tho...
You can now make your own Hotline Miami 2 levels
At long last, Dennaton has finally released an early beta of the mod tools for Hotline Miami 2: Wrong Number. It's only available for Window, but you're now able to make your own custom maps. A tutorial released by Dennaton show...
Hotline Miami 2 level editor beta hitting next month
It's been a little while since we last heard about the "almost ready" level editor for Hotline Miami 2: Wrong Number. But good things come to masked murderers who lie in wait and our patience has finally been rewarded. Developer...
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One of the common complaints for Hotline Miami 2: Wrong Number is its large levels. Were they too large? I didn't mind them. Sure, it felt bad to die from the last guy on the floor after pulling off a miraculous string of executions, but th...
The Hotline Miami Story covers the making of this trippy series
I still remember how the original Hotline Miami suddenly came out of nowhere and left an incredible impression on those who took a chance on it. It was such an unusual title. Its bright, vivid visuals, along with the overhead view of the e...
Download this free track off the Hotline Miami 2 OST
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Get both Hotline Miami games in a brutal physical box set
Rejoice Hotline Miami fans who still like physical boxed releases, there's a Hotline Miami and Hotline Miami 2 physical collectors edition in the works. The $60 (£40) box set, due to ship out in August 2015, comes with DVD and Steam c...
I'm going to play the Hotline Miami 2 soundtrack on repeat until I'm utterly sick of it
If there's one thing we can all agree upon re: Hotline Miami 2: Wrong Number, it's that Dennaton Games did an exceptional job matching songs with the tone and feel of specific levels. This series wouldn't be what it is -- a brutal, gory, a...
There's a fun little Easter egg at the end of Hotline Miami 2
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For some, Hotline Miami was an existential look at the current macro-state of videogames. You were told to commit random acts of murder seemingly without remorse, and at the end, you get a bit of interesting commentary on the culture of vio...
Answer Hotline Miami 2's call on March 10, 2015
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Hotline Miami 2 digital comic series free on Steam
Devolver Digital and Dennaton Games have teamed up with Italian art collective Dayjob Studio to bring you an early taste of Hotline Miami 2: Wrong Number in delicious, digital comic book form. The free, five-part comic series digs...
Hotline Miami dev suggests piracy as an alternative to Australia 'ban'
Devolver Digital and Dennaton Games' forthcoming title Hotline Miami 2: Wrong Number made headlines yesterday after the Australian Classification Board made the decision to refuse the game classification, effectively banning ...
Hotline Miami 2 refused classification in Australia (Update)
Hotline Miami 2 has been refused classification in Australia, primarily due to a rape scene. Before we dig into the meat of the news, be warned this article contains a pretty graphic description of rape. With that out the way, yes, Hot...
Grab some headphones and listen to this Hotline Miami 2 song
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Holy crap, this Hotline Miami 2 vinyl is cool
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Hero worship gone wrong in Hotline Miami 2
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redpajama_set_name: RedPajamaCommonCrawl


text:
Seattle Asian Art Museum Reopens
By Madeleine Porter | February 20, 2020
Photos courtesy SAM via Facebook
The Seattle Asian Art Museum reopened to the public this month after being closed since February of 2017 due to issues relating to infrastructure, accessibility complications, and lack of program space.
Modernizing while simultaneously preserving the historic building, Seattle-based LMN Architects, along with landscape artist Walker Macy, did a beautiful job reviving the Art Deco style museum. Some of the new features include a beautiful new presentation of Asian art never seen before, a special exhibitions gallery, an Asian Paintings Conservation Center, a new education space, and numerous other amenities.
Over the past three years, SAM has put immense focus on reworking the exhibits for the reopening in a way that will influence and inspire visitors and their vision for Asian art. Continuing to feature pieces from the museum's permanent collection of Chinese, Korean, Japanese, Indian, Himalayan, and Southeast Asian art, the museum has also acquired ten new works of Asian art within the last year. With the reopening of the museum, SAM is looking to continue to focus on growing its collection of art centered around historic, modern, and contemporary Asian Pacific Islander as well as Southeast Asian art, specifically collecting different works created by local Asian Pacific Islander artists within the Seattle area.
Boundless: Stories of Asian Art was the museum's initial exhibit to be installed, featuring a collection spanning across 13 of the galleries. The exhibit is comprised of art connected to material life held within the northern wing galleries and art connected to spiritual life within the southern wings galleries. Be/longing: Contemporary Asian Art is an exhibition featured in the eastern wing of the building, exploring works from 12 featured artists portraying their diverse experiences as well as their unique Asian and international perspectives.
Other new features to look forward to with the new reopening of the museum include: the Fuller Garden Court's beautiful new LED-light canopy installation titled Gather, as well as the new Asian Paintings Conservation Center, the first of its kind in the western United States. The museum also features a newly renovated and expanded community learning gallery, where visitors K-12 can get creative and become artists themselves. Interactive experiences, smartphone-enabled multimedia tours, and in-gallery video content have also been integrated throughout the different galleries and educational spaces. A full list of the rest of the Seattle Asian Art Museum's highlights can be found here.
The museum is now operating at its regularly scheduled hours: Tuesday through Sunday from 10 a.m. to 5 p.m. and on Saturdays from 9 a.m. to 5 p.m. SAM will also be offering four new free days each month. Visit this website for more information on free days, ticket pricing, memberships, and more.
Tags: Asian Art, museum, SAM, Seattle Asian Art Museum
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If you would like to file a complaint with the Division of Consumer Protection, you may do so through the U.S. mail or by facsimile. Your complaint will be screened to determine whether it is a matter that can be handled by us. If it is something that we handle, your complaint will be assigned to an investigator who will determine what further action, if any, should be taken. Please let us know if you do not get a response from us within thirty (30) days of our receipt of your complaint.
You may also use the Consumers "Who Do I Contact?" Resource Guide to help determine the appropriate contact for a complaint.
Please contact the Department of Real Estate regarding any loan modification complaints.
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At the end of last year, I began to loo k afresh into the lifestyle of Jesus and having taught and written on the subject of lifestyle for many years, was surprised at how challenging His life was.
Now we know of course that Jesus is a lot more to us than a role model and an example, He is Saviour, Redeemer, Creator, Lord and King. In John 1.1 It says, 'In the beginning was the Word (Capital W- in other words Jesus), and the Word was with God and the Word was God.' Jesus is God.
But He is indeed also our role model. There are many people and groups, who may not even believe in God, but are so impressed and influenced by His alternative lifestyle that they seek to emulate Him, if not as God, then as an exceptional teacher and life example.
One of my first observations was how impartial Jesus was and how He treated everyone equally, He was no 'respecter of persons'.(1 Peter 1.17) At a time of great inequality, Jesus was impartial and treated all the same, the rich, the poor, the old, children, the sick, the sinner, the leper, women and strangers and foreigners.
But she was more than a woman; she was a Samaritan woman, with historical animosity between the Jews and the Samaritans. Then the third strike against this woman was she was a woman with questionable morals, who had had five husbands and the man she was now living with, was not her husband!
We have to be truthful here and say how easy and even understandable it would have been for Jesus to avert his eyes, to give a tiny non-committal smile and a nod, He was after all tired from His journey, but Jesus got right in there and had a deep, meaningful, revealing and relationship building conversation with her.
Even in those days of massive inequality and discrimination, Jesus cut through it all. He refused the norm and even the customs of His generation and was not sexist, racist or judgmental.


text:
Andy "Frank" Wright  is an Australian supervising sound editor. He is known for his work on the war-drama film Hacksaw Ridge directed by Mel Gibson, for which he received two Academy Award nominations at the 89th Academy Awards, Best Sound Editing and winning Best Sound Mixing (both shared with Robert Mackenzie).

Awards

 Won: Academy Award for Best Sound Mixing
 Won: Satellite Award for Best Sound
 Nominated: Academy Award for Best Sound Editing
 Nominated: BAFTA Award for Best Sound
 Nominated: Cinema Audio Society Award for Outstanding Achievement in Sound Mixing for a Motion Picture – Live Action

References

External links
 Andy Wright at Sound Firm

Living people
Australian audio engineers
Year of birth missing (living people)
Australian sound editors
Best Sound Mixing Academy Award winners

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It's still unclear how or why the scrappy, apricot-colored dog with pointy ears showed up to the starting line of the 155-mile ultramarathon in June. The closest village was several miles away, and all that lay ahead was the vast, unforgiving Gobi Desert.
Dion Leonard, a distance runner from Scotland, noticed the pup scampering alongside a group of American runners, but didn't think she would last long - much less through most of the six stages of a grueling, week-long endurance race.
Until she reappeared by his side at the start line on the morning of Day 2.
"This little dog's sort of sitting next to me, looking up like, 'Are we going to run together today?'" Leonard told The Washington Post. "I didn't really think that much of it. I thought, let's see how long this dog lasts."
The dog, whom he soon nicknamed Gobi, followed him through all 23 miles that day, climbing nearly 20,000 feet in elevation as they crossed the Tian Shan range and journeyed into the Gobi Desert. At times, she would charge ahead of Leonard, motivating him to run faster. At other points, he stopped to give her beef jerky and water from his own pack.
At their campsite that night, Gobi lay down next to him in his sleeping pad, wedging herself against his armpit to snuggle.
Ultra runner Dion Leonard talks about adopting Gobi, a stray dog who followed him for multiple days as he competed in an ultra marathon.
"She literally stayed with me all day," said Leonard, 41, an Edinburgh resident who has competed in numerous multistage ultramarathons. It's still a mystery why Gobi followed him, of all the 101 competitors in this year's Gobi March. "I didn't do anything in particular to gain her attention. She chose me. I was the one that she was going to stick to."
Over Day 3, Gobi continued to follow Leonard, this time over increasingly harsh terrain. Leonard picked her up and carried her over multiple river crossings up to 21 yards long, with rushing water up to his stomach.
"I started to realize then that we were really close," he said. "I wasn't going to leave her behind."
In all, Leonard estimates Gobi accompanied him for 105 miles of the seven-day race, through stages 2, 3 and 6. Because of the heat - temperatures peaked around 125 degrees Fahrenheit around the middle of the course - Gobi wasn't allowed to run stages 4 and 5. However, race organizers drove her to the finish lines on those days, where she waited faithfully for Leonard to cross.
"Day 5 is actually 80 kilometers. You're obviously pretty tired. It's a big day. It's very hot," he said. "To come in to the finish line and to see her wagging her tail . . . was just amazing."
Ultimately, Leonard took second place in the race. At the final finish line, event organizers produced a matching medal for Gobi, too.
By then, he knew they shared a special, inexplicable bond. Leonard began researching what it would take to bring Gobi back to the United Kingdom: a host of medical examinations, paperwork and quarantines, at a cost of more than $6,500.
He and his wife started a crowdfunding campaign online. Within days, it surpassed its fundraising goal, attracting donations from all over the world.
"We're really thankful," he said. "I think everyone's been keen to seeing good news."
He doesn't know Gobi's age, breed or medical history - just that they now are incomprehensibly connected. Leonard has since returned to Scotland and estimates that the process for Gobi to make it to the U.K. could take up to four months.
"We're looking at having her here for Christmas in an ideal world," he said. His wife is thrilled. Their cat remains unaware she will be getting a "sister" soon, Leonard said.
While they wait, Leonard is preparing for his next ultramarathon in October, a similar 155-mile trek across the Atacama Desert in Chile that, like the Gobi March, is part of the 4 Deserts Race Series.
"I'm hoping a horse or an alpaca doesn't follow me there," he said, laughing. "I may not get away with bringing that back."


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text:
WVU study reveals falsification issues in higher education hiring processes
When concerns are expressed about distrust in science, they often focus on whether the public trusts research findings.
A new study from West Virginia University, however, explores a different dimension of trust.
Two researchers in WVU's Eberly College of Arts and Sciences examined whether and how frequently researchers misrepresent their research accomplishments when applying for faculty jobs.
The research team, led by Associate Professor of Political Science Trisha Phillips and Department of Sociology and Anthropology chair Lynne Cossman, collected all vitae submitted for faculty positions at a large research university for one year. The institution was intentionally unidentified to maintain confidentiality.
After reviewing a 10 percent sample for accuracy, they discovered that of the 180 applicants whose vitae were analyzed, 141, or 78 percent, claimed to have at least one publication. Of these applicants with publications, 79, or 56 percent, listed at least one publication that was unverifiable or inaccurate in a self-promoting way.
"We were initially trying to determine whether and how frequently people were lying. You can't truly know that without intent," Phillips said. "So, we looked for other indicators. We considered any inaccuracies that were not self-promoting to just be accidents. We found 27 of those mistakes. But in the end, we found that more than half of the inaccuracies were self-promoting. That's nowhere near as equal as it needs to be to think that there is no lying going on."
The falsifications were not limited to any particular disciplines or subject areas.
"People often think that the integrity of the person will translate into the integrity of the profession or the integrity of the field. It's important to show that a number of the problems that affect business and industry and other non-academic disciplines may also be a problem in higher education," Phillips said. "In being aware that higher education may have misconduct, we shouldn't assume that we are any better than what our non-academic peers might be experiencing. We always need to be vigilant."
The research team was motivated by several cases of high-profile professional misrepresentation in higher education as well as in their own experiences serving on hiring committees.
"These high-profile cases of professional misrepresentation in academia generate news, but they do not reveal the frequency or severity of the problem," Phillips said. "Instead, they raise concerns about the truthfulness of academic vitae and questions about how often academics falsify their credentials and accomplishments when applying for jobs."
Because this study reflects the vitae of applicants at one institution, the research team aspires to replicate the study at more colleges and universities in the future.
"We have to keep in mind that this study was done at a single institution, so it could just be a problem there. However, it's not like all the applicants graduated from that institution," Cossman said. "The sample of applicants included recent Ph.D. grads from institutions located all over the nation and world applying for all different kinds of tenure-track jobs at that institution."
Phillips and Cossman hope the findings can inform recommendations for journal editors, graduate student advisers and human resources offices. One idea is making the publication process more consistent.
"Journal editors need to be careful about how they communicate with authors about where their manuscript is in the process. What does it mean to be accepted versus forthcoming versus in print versus published?" Cossman said. "In larger conversations, I've realized those terms mean different things in different disciplines and that the timeframes can vary. We need to identify those inconsistencies and discuss them rather than letting graduate students and new faculty figure it out on their own."
Ultimately, the researchers aspire to change the culture of the academic hiring process.
"It's important because there's something about the culture of faculty in higher education that is encouraging this behavior or implicitly influencing it in some way. We need to find this type of misconduct when it's happening. We need to be aware that it might be happening, look for it, find it and address it," Phillips said. "But we also need to think long and hard about why it's happening and look at the upstream factors that are influencing culture and these decisions to engage in this type of behavior. We hope our findings will start a larger discussion in academia in general about what we should all be more aware of and more vigilant in doing."
Title: Assessing Trustworthiness in Research: A Pilot Study on CV Verification
Link: https://journals.sagepub.com/doi/10.1177/1556264619857843
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text:
@interface BirdSprite : CCSprite{
    CCLayer* gLayer;

}

@property ccVertex2F vel; //速度
@property ccVertex2F acc; //加速度

@property (nonatomic,retain) CCParticleSystem* trick_particles;

@property (nonatomic,retain) CCAction* normalAction;
@property (nonatomic,retain) CCAction* upAction;
@property (nonatomic,retain) CCAction* downAction;
@property (nonatomic,retain) GameLayer* layer;
//当前主角等级,从1开始
@property  int currentGrade;
+ (id) BirdWithinLayer:(CCLayer *)layer;

-(void)upgradeBird;

- (void)birdEmitterInit;
-(void)changeMoveDirection:(bool)isUp;

-(void)resetParticleSystem;
-(void)stopParticleSystem;

+(void)initSpriteSheet:(CCNode*)layer;
- (void) changePositon:(CCLayer *)layer xStep:(float)xStep yStep:(float)yStep;
@end

redpajama_set_name: RedPajamaGithub


RF Silicon on Insulator (SOI) technology focused chip company Peregrine Semiconductor announced industry's first RF SOI technology built on GLOBALFOUNDRIES' 130 nm 300 mm RF technology platform. This process technology platform called UltraCMOS 11 uses a custom fabrication flow from GLOBALFOUNDRIES' Fab 7 facility in Singapore.
300mm helps in achieving manufacturing scale of RF SOI chips in applications including mobile devices and high-volume RF communication applications. Peregrine's 40 GHz switch which is an RF silicon-on-insulator (SOI) performs as good as gallium arsenide (GaAs) switches in applications such as test-and-measurement, microwave backhaul, radar and military communications applications.
In another SOI semiconductor fab related news, X-FAB Silicon foundries announced 180nm SOI technology for automotive and industrial applications. X-FAB says its XT018 180-nanometer SOI platform outperforms bulk CMOS technologies and provides cost savings of up to 30-percent. XT018 process is suggested for advanced automotive applications such as monolithic motor controllers and physical layer transceivers including integrated or stand-alone LIN/CAN transceivers.
The XT018 platform targeted at automotive, industrial and medical applications with up to 200V operating voltage and an operating temperature up to 175°C.
"The X-FAB XT018 180nm modular high-voltage SOI CMOS technology combines the benefits of SOI wafers with Deep Trench Isolation (DTI) plus those of a state-of-the-art six-metal-layer 180nm bulk CMOS process. Using SOI wafers as the starting material, in combination with trench isolation instead of the more commonly used junction isolation techniques in CMOS, simplifies the design concept. The SOI wafers eliminate the parasitic bipolar effects to substrate, reducing latch-up risk. They also enable the development of devices such as truly isolated diodes, allowing reverse supply voltage protection that is difficult to achieve with bulk CMOS or BCD technologies. " explains X-FAB in its release.
The new process helps in fabricating a low on resistance 40V NMOS transistor with on resistance of 26 milli-ohm-mm², 40V and 60V ESD enhanced devices and matching PMOS and depletion transistors.
The enhanced XT018 foundry platform is available immediately including full PDK support.


Why UA – Ursuline Academy – Celebrating 125 Years!
Since our founding in 1893, Ursuline Academy has been dedicated to educating young women and men in the spirit of St. Angela Merici. Our rigorous academic curriculum coupled with our relentless commitment to balanced and individualized programming for every student provides the greatest opportunities, support and success.
At Ursuline, we are inspired by a deep sense of mission, a bold vision for the future and a constant drive to explore and excel. What does this mean for your child? It means they will grow in faith and friendship and they will seize extraordinary opportunities in Academics, Arts, Athletics, and Christian Service. It means they will be both the learner and the teacher, broadening their horizons and stepping outside of their comfort zone.


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onlinecasinoselite.org › Games › Scratch Games › Rock Paper Scissors
Play at Rock Paper Scissors Online Casino Game
4.7 out of 5 - from 25 votes
What do you like of this game?
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Graphic 0%
Gameplay 0%
Involvement 0%
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Developed by Playtech, Rock-paper-scissors is a simple experience that lets players wager on the classic game: rock beats scissors, where scissors beat paper and paper beats rocks.
Bet amounts in Rock-paper-scissors ranges from $0.10 to $1. The object is to choose either rock, paper or scissors and hope that the computer, which chooses randomly, makes an inferior selection. Each round, there is only a 33 percent chance that the player wins, but since ties are a push, there is also only a 33 percent chance that he or she loses. Single-game wins pay out 1.9, and the stake is returned. Therefore, if a player bet a $1 and won, he would get his dollar back and an additional $1.90.
Rock-paper-scissors also allows players to bet on a winning streak rather than a single game. The available streak lengths are two, three and four. Betting on a streak does not increase the commitment, so bet amounts still range from $0.10 to $1. What changes, however, is the payout. The payout is 8.7 at two games, 26 at three games and 78 at four games. Therefore, on a $1 wager, a two-game streak pays out $8.70, a three-game steak pays out $26 and a four-game streak pays out $78.
Graphics & Audio
When it comes to slot machines, Playtech is known for its unique style and great attention to detail. That isn't really the case here, and it does feel as if maybe the developers mailed this one in to some degree because Rock-paper-scissors won't likely ever be a high-profile game for the company. The user interface is certainly serviceable, but the design is uninspired, and the gong sound and looping background music had us hunting for the mute option on our second bet.
The jackpot for the standard game is a $1.90, and a player can win as much as $78 on a four-game winning streak. Playing four games at a time is the ideal way to play Rock-paper-scissors, and even at the minimum $0.10, it will pay out $7.80, which isn't bad at all.
Rock-paper-scissors is exactly what most players will expect it to be, and it may be worth trying as a brief diversion, but there probably isn't enough here to maintain a player's attention for long. That said, for a no-skill game, one could do a lot worse than having a chance at $78 for a $1 at these odds. Do you want to play at more scratch cards games? Point your cursor here to visit our dedicated page.
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Rock Paper ScissorsRock-paper-scissors is a simple experience that lets players wager on the classic game: rock beats scissors, where scissors beat paper and paper beats rocks. - Review by OnlineCasinosElite
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Google Faces Antitrust Probe in Europe
Douglas McIntyre
Google's (GOOG) search market share is about 80% in the U.K., Germany, and France, according to Comscore. That compares to about 66% of the U.S. market. The No.1 search company's dominance has sparked a European Commission anti-trust investigation. According toThe Telegraph, "The Commission has written to Google with a series of questions over how its search functions operate and also questioned the way it sells advertising." The companies that have filed the complaints that the the E.C. has acted on are U.K. search site Foundem, a shopping price comparison site, Ciao, which is owned by Microsoft (MSFT), and ejustice.fr, a French site for browsing legal content.


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Draft Scout College Football Player News: Howard
10/08/21 - Quinton Williams, Jr/2023, Howard, 6-3, 178 (DS#999 QB) + More +
Quinton Williams threw for 337 yards and two touchdowns, including a 97-yarder, Faraji Woodson added a pair of field goals and Howard blanked Morgan State 27-0 on Friday night. The Bison (2-4, 1-0 Mid-Eastern Athletic Conference) are on a two-game win streak for the first time since the 2018 season. Morgan State (0-5, 0-1) had an apparent 76-yard touchdown run by Alonzo Graham in the first half negated by a holding penalty and also saw a 41-yard field goal attempt miss. Woodson, a sophomore, surpassed 300 yards passing for the second time in his career. He racked up 357 in a loss to Hampton last month.
The Bison broke an otherwise scoreless first half with a 35-yard field goal by Woodso n with 13 seconds left on the clock. Five minutes into the second half, Woodson found Antoine Murray on the 97-yarder. Early in the fourth quarter, Woodson hit Richie Ilaraza from the 9. Ian Wheeler completed the scoring with a 20-yard touchdown run, capping a 13-play, 55-yard drive. Murray had four catches for 171 yards. - AP College Football
(DS#999 QB) Jr/2023 QB Quinton Williams, Howard
Quinton Williams threw three touchdown passes including a 38-yarder to Kasey Hawthorne with just over two minutes remaining to lift Howard to its first win of the season, 22-17 over Sacred Heart on Saturday. Hawthorne leaped to make the catch against tight coverage at the 5-yard line then stumbled backward into the end zone. The Bison (1-4) failed on a two-point conversion try but their defense held off the Pioneers (2-3). Faraji Woodson's field goal gave Howard an early lead but Sacred Heart scored the next 17 points before Williams threw an 18-yard pass to Matthew McDonald for a touchdown. The PAT failed and Sacred Heart led 17-9 at halftime. Williams threw a 29-yard score to McDonald to cut the deficit to two in the third quarter. Sacred Heart's points came on short touchdown runs by Marquez McCray and Jalen Madison plus a field goal by Ricky Lancaster. - AP College Football
08/06/20 - Ray Williams, Jr/2023, Howard, 5-10, 183 (DS#999 FS) + More +
2020 PHIL STEELE/DRAFTSCOUT PRESEASON ALL-MEAC SECOND TEAM: Ray Williams, Howard, Soph.,...Darrien Brokenburr and Ray Williams earned a spot on the second team after receiving sufficient playing time in their freshman campaign. Last season, Brokenburr saw action in all 12 games where he racked up 31 tackles (25 solo) with a team-leading 3.5 sacks. For Williams, the Detroit product led HU with 61 tackles (48 solo) in 12 contests. - Howard Football
(DS#999 FS) Jr/2023 FS Ray Williams, Howard
News Source: Howard Football
08/06/20 - Darrien Brokenburr, Jr/2023, Howard, 6-2, 240 (DS#999 DE) + More +
2020 PHIL STEELE/DRAFTSCOUT PRESEASON ALL-MEAC SECOND TEAM: Darrien Brokenburr, Howard, Soph.,...Darrien Brokenburr and Ray Williams earned a spot on the second team after receiving sufficient playing time in their freshman campaign. Last season, Brokenburr saw action in all 12 games where he racked up 31 tackles (25 solo) with a team-leading 3.5 sacks. For Williams, the Detroit product led HU with 61 tackles (48 solo) in 12 contests. - Howard Football
(DS#999 DE) Jr/2023 DE Darrien Brokenburr, Howard
08/06/20 - Aaron Walker, rSr/2022, Howard, 5-10, 190 (DS#999 SS) + More +
2020 PHIL STEELE/DRAFTSCOUT PRESEASON ALL-MEAC THIRD TEAM: Aaron Walker, Howard, Sr.,...The trio of Quinton Hill, Aaron Walker and Christian White made Steele's Third Team with each Bison playing all 12 games. Hill and Walker had 56 (35 solo) and 47 (33 solo) tackles, respectively, which ranked second and third on the club. White wrapped up his rookie campaign with 44 tackles (32 solo) and a pair of sacks. - Howard Football
(DS#999 SS) rSr/2022 SS Aaron Walker, Howard
08/06/20 - Quinton Hill, rSr/2022, Howard, 5-11, 200 (DS#999 OLB) + More +
2020 PHIL STEELE/DRAFTSCOUT PRESEASON ALL-MEAC THIRD TEAM: Quinton Hill, Howard, Sr.,...The trio of Quinton Hill, Aaron Walker and Christian White made Steele's Third Team with each Bison playing all 12 games. Hill and Walker had 56 (35 solo) and 47 (33 solo) tackles, respectively, which ranked second and third on the club. White wrapped up his rookie campaign with 44 tackles (32 solo) and a pair of sacks. - Howard Football
(DS#999 OLB) rSr/2022 OLB Quinton Hill, Howard
08/06/20 - Christian White, Jr/2023, Howard, 5-11, 200 (DS#999 OLB) + More +
2020 PHIL STEELE/DRAFTSCOUT PRESEASON ALL-MEAC THIRD TEAM: Christian White, Howard, Soph.,...The trio of Quinton Hill, Aaron Walker and Christian White made Steele's Third Team with each Bison playing all 12 games. Hill and Walker had 56 (35 solo) and 47 (33 solo) tackles, respectively, which ranked second and third on the club. White wrapped up his rookie campaign with 44 tackles (32 solo) and a pair of sacks. - Howard Football
(DS#999 OLB) Jr/2023 OLB Christian White, Howard
12/30/19 - Michael Cornwell, rSr/2020, Howard, 6-3, 223 (DS#999 FB) + More +
2019 ALL-MEAC THIRD TEAM (COACHES): TE Michael Cornwell, r-Sr., Howard,...Howard's Cronwell (tight end - 6'3 - 230 lbs - Owen Mills, Md.) - a graduate student, in his lone season as a Bison, he grabbed 28 receptions for 415 yards and four touchdowns. He recorded a season-best, five catches versus Delaware State University on Sept. 21 in Dover, Del. - Howard Football
(DS#999 FB) rSr/2020 FB Michael Cornwell, Howard
12/30/19 - Kyle Anthony, Sr/2020, Howard, 6-2, 207 (DS#117 WR) + More +
2019 ALL-MEAC THIRD TEAM (COACHES): WR Kyle Anthony, Sr., Howard,...HU's Anthony (wide receiver - 6'3 - 205 lbs - Miramar, Fla.) - a graduating senior, finished his career as Howard's all-time career reception leader. Anthony amassed 70 receptions for 786 yards and seven touchdowns. He recorded a career-high 12-receptions versus Hampton University on Sept. 14 in Chicago, Ill. - Howard Football
(DS#117 WR) Sr/2020 WR Kyle Anthony, Howard
NOV 25 MEAC TOP PERFORMER: Ray Williams (HOW) had seven tackles, a half sack, a force fumble and a blocked field goal attempt in Howard's 20-15 win over Morgan State. - Mid-Eastern Athletic Conference Football
News Source: Mid-Eastern Athletic Conference Football
Quinton Williams hit Michael Cornwell on an 8-yard touchdown toss in the final seconds of the game and Howard then held off a Morgan State charge to claim a 20-15 victory on Saturday. Cornwell scored with 39 seconds remaining in the game. The Bears then drove to Howard's 30 with three seconds left. DeAndre Harris threw into the end zone where the ball was batted down on the final play of the game, allowing Howard to escape with just its second victory of the season.
Williams threw for 202 yards and two touchdowns and Dedrick Parson rushed for 170 yards and another score for Howard (2-10, 2-6 Mid-Eastern Athletic Conference). The Bison had lost seven straight coming into the season finale for both teams. Howard took its first lead when Williams hit Kyle Anthony from the 6 for a 14-8 advantage with 7:24 left in the third. The Bears answered to retake the lead 15-14 when E'Munn Parker ran it from the 7 with 3:16 remaining in the game. The Bears (3-9, 2-6) were led by Harris who threw for 245 yards and one touchdown. Wesley Wolfolk hauled in four passes for 116 yards and a score. - AP College Football
SEPT 30/WEEK 5 MEAC ROOKIE OF THE WEEK: Howard freshman Quinton Williams (QB, 6-4, 178, Fr., Upper Marlboro, Md.) was 21-for-35 for 179 yards passing to go along with three touchdowns, while also rushing for 25 yards and a touchdown in the Bison's home opener. - Mid-Eastern Athletic Conference Football
SEPT 9/WEEK 2 MEAC TOP PERFORMERS: Quinton Williams (HOW) was 5-for-5 with 40 yards passing along with his first career touchdown. - Mid-Eastern Athletic Conference Football
SEPT 9/WEEK 2 MEAC TOP PERFORMERS: Kyle Anthony (HOW) had 10 receptions for 146 yards with three touchdowns for the Bison against Youngstown State. - Mid-Eastern Athletic Conference Football
2019 PRESEASON PHIL STEELE/DRAFT SCOUT ALL-FCS THIRD TEAM: Kyle Anthony, Howard, Sr.,...Anthony was elected to the 2018 Mid-Eastern Athletic Conference (MEAC) All-Conference First Team in 2018...played in all 10 games...recorded 659 yards on 53 catches with six receiving TDs. - Howard Football
Howard Football Videos


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Spirituality & Beliefs > Philosophy > History of Western philosophy > Western philosophy: Ancient to 500 AD
Socrates, Ironist and Moral Philosopher - Cornell Studies in Classical Philology (Paperback)
Gregory Vlastos (author)
This vivid and compelling study of Socrates's moral philosophy and, more generally, of his moral outlook and his attitude toward religion and society, reclaims the remarkable originality of his thought. Gregory Vlastos shows us a Socrates who, though he has been long overshadowed by his successors, Plato and Aristotle, represented the true turning point in Greek attitude toward philosophy, religion, and ethics. In his quest for the historical Socrates, Vlastos focuses on Plato's earlier dialogues, setting the Socrates we find there in sharp contrast to the Socrates of later dialogues, in which he is used as a mouthpiece for Plato's own doctrines, many of them anti-Socratic in nature.
At the heart of the book is Vlastos's perception of the paradoxical nature of Socratic thought. But Vlastos explains the paradoxes rather than explaining them away, and he highlights the tensions in the Socratic search for the answer to the question: How should we live? The magnetic quality of Socrates' personality emerges throughout his book. Clearly and elegantly written, subtle in its arguments yet entirely accessible to non-specialists, this is major work in ancient philosophy and the history of Western thought.
Publisher: Cornell University Press
"This is the best book available on its subject. No other book written by someone with such deep knowledge can speak with so much authority to scholars and still be so enjoyable for general readers. Philosophical writing now tends to be excessively technical and academic. Socrates, Ironist and Moral Philosopher is not; it can take many different kinds of people to the heart of the most puzzling and important features of Socrates."-Julia Annas, New York Times Book Review
"Gregory Vlastos's book begins from the conviction that Socrates' strangeness is 'the key to his philosophy.' It is a marvelous book, in which no major aspect of Socrates' career is eclipsed. The rigor of his arguments, the depth of his moral commitment and understanding, his complex relationship to Athenian ethical traditions, his rational religion: all this comes to life in writing whose vigor and lucidity put the challenge of Socrates squarely before the reader. . . . It deserves as much honor as any work of scholarship in Greek philosophy in this century."-Martha C. Nussbaum, The New Republic
"What can be surmised about this extraordinary and arresting figure has been brilliantly presented and argued in this closely reasoned book, for which we are all greatly in Gregory Vlastas's debt."-Charles Taylor, Times Literary Supplement
A Monk's Guide to a Clean House and Mind
Shoukei Matsumoto
Outgrowing God
Utopia for Realists
How the World Thinks
Julian Baggini
A Little History of Philosophy
Nigel Warburton
Sarah Harvey
Josh Cohen
Paul Dolan


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The Royal Society of Medicine is committed to environmental sustainability and tackling climate change by:
Understanding environmental issues and sharing this information
Developing innovative and flexible solutions to bring about change
Sourcing products and services which are produced and distributed in a responsible fashion
Recognising that managed social responsibility is essential to our future
Investing the Society's funds in a responsible manner
Encouraging all our suppliers and partners to share in our aims
Monitoring and measuring our progress
Through our primary charitable purpose, which is to provide education for doctors and other healthcare professionals, we highlight key health issues such as the impact of climate change within our education programmes.
The RSM is a founding member of the UK Health Alliance on Climate Change which brings together healthcare professionals to advocate for better responses to climate change that protect and promote public health.
We have implemented an effective environmental system throughout our operations in 1 Wimpole Street, which not only reduces the impact of our activities on the environment, but also increases our efficiency and effectiveness.
Thoughtful and considerate staff
The RSM recognises the responsibility our staff have in contributing to good environmental management. We seek to harness and channel the enthusiasm and interest shown by our employees and provide the appropriate training and support to ensure all staff exercise their environmental responsibility.
Responsible suppliers and partners
The RSM promotes and encourages good environmental practice to the organisations we work with, including suppliers and partners. We seek to do business with those who share our vision.
In our Club, hotel and hospitality operations, we source our food ingredients from suppliers who can demonstrate that they are promoting sustainability and minimising food miles. This means using butchers who can trace every link in their supply chain back to the farm, using fruit and vegetables from British growers and serving tea and coffee from importers who are as committed to the welfare of the growers as they are to the quality of the product.
A commitment to recycling
We recycle:
Reducing our environmental footprint
Within 1 Wimpole Street we:
Manage our energy consumption by turning off unnecessary light and climate control to our rooms through a computerised Building Management System (BMS)
Procure electricity from 100% renewable energy sources: wind, biomass and solar
Reduce electrical load on aircon chilling plant by using fresh air only when the weather is below 19 degrees and by not using any re-circulation function
Use low energy light bulbs wherever possible
Send all waste food to Veolia UK | Leeming Biogas gas-to-grid anaerobic digestion
Buy from small independent suppliers and have seasonal produce tailored to our conference menus
Minimise cardboard packaging on deliveries where possible, for example our vegetable supplier uses returnable crates
Have an on-site water purification system which has saved annually an estimated 92,000 1 litre glass bottles from being transported and saves an estimated 7,200 tonnes of carbon emissions
Have signed up to the Meeting Industry Association's 20% less campaign in our commitment against single-use plastic
Use environmentally friendly cleaning products
Use electronic documentation and files where possible to limit paper consumption
Use meeting room notepads made from FSC-certified paper
Promote the use of hybrid events to reach domestic and overseas delegates, in order to reduce their carbon footprint
Encourage the streaming of events so fringe delegates can access events at a time that suits them
Encourage the use of video conferencing in all meetings allowing potential overseas attendees to reduce their carbon footprint by accessing the event remotely
Encourage hotel guests to reuse towels, and reduce linen use during their stay which in turn uses less water and detergent
Have aerators on taps and showers in the bedrooms to reduce water usage
Within 1 Wimpole Street we don't:
Use air freight transport wherever possible, allowing us to limit "food miles".
Use disposable or non-recyclable packaging.
Use aerosols as all our cleaning materials are held within reusable containers.
Believe in waste.
The RSM's Council is aware of its need to invest the Society's funds in a responsible manner and to have a positive impact on people and the planet. This is done by investing in funds that adopt screening policies that exclude areas of significant social or environmental harm and integrate ESG (Environmental, Social and Governance) factors within the investment selection process. One such exclusion is the direct holding of investments whose primary business is in fossil fuels (thermal coal and tar sands), screened at more than 10% of revenue. We are in the process of extending this exclusion to cover the extraction, production and refining of coal, oil and gas.


This set features images of extinct birds. There are 50 cards, two each of 25 different birds.
The cards measure 5.5x8.4cm (2.2x3.25") and are professionally printed on 100% recycled cardstock, high in post consumer paper.
The cards come packed in a simple muslin bag, tucked in a box to keep them safe for travel.
Haven't played Pairs before? It's a simple memory game, that you can play by yourself or with others. Shuffle and lay all the cards bird-side down on a table, and taking turns, flip over a card to see the bird underneath. Flip a second card to see if it is the same bird. If it is, you get to go again, if not, turn the cards over again, and it's the next persons turn.


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Spearpoint Rocky Mtn Elk
Edition of 25 pieces
B12 ROCKY MTN ELK
The Spearpoint 'Rocky Mtn Elk' features mesmerizing hand-engraved bolsters with 24K gold inlays by Bottega Incisioni, inlaid with a stunning piece of 10,000 year-old fossil Woolly Mammoth tooth. The blade is hand-forged 'Hornet's Nest' damascus by Mike Norris; the one-hand button lock and the thumb stud are set with smoky quartz gemstones.
A remarkable design that gives you an instrument with a full-size secure grip, and a versatile deep-belly blade, the Spearpoint epitomizes William Henry's core philosophy – that superlative function deserves to be elevated to superlative art.
The 'Rocky Mtn Elk' features some of the most exotic materials, artistry and forged metals that are the hallmark of William Henry's collections.
One-hand button lock system
Blade 3.06" (77.7mm)
Handle 4.13" (104.9.5mm)
Overall open 7.19" (182.6mm)
All William Henry knives feature a unique serial number which is engraved into the blade to assure the authenticity and lifetime traceability of the product
This knife is shipped in an elegant wood presentation box, and it comes with a pocket clipcase made from soft, high-grade leather, with an integrated stainless steel pocket clip
'Hornet's Nest' damascus
Damascus steel was a term used by several Western cultures from the Medieval period onward to describe a type of steel created in India and used in swordmaking from about 300 BC to 1700 AD. These swords were characterized by distinctive patterns of banding and mottling reminiscent of flowing water. Such blades were reputed to be not only tough and resistant to shattering, but capable of being honed to a sharp and resilient edge. William Henry's damascus is made from several types of steel welded together to form a billet.
The patterns vary depending on how the damascus artist works the billet. The billet is drawn out and folded until the desired number of layers are formed. William Henry damascus billets are forged with a minimum of 300 layers. William Henry works with a handful of the very best damascus artists/forgers in the U.S.Link to damascus Page
Fossil Mammoth tooth
From a Woolly Mammoth that walked the Earth at least 10,000 years ago.
Modern humans coexisted with woolly mammoths during the Upper Paleolithic period when they entered Europe from Africa between 30,000 and 40,000 years ago. Prior to this, Neanderthals had coexisted with mammoths during the Middle Paleolithic and up to that time. Woolly mammoths were very important to Ice Age humans, and their survival may have depended on these animals in some areas.
The woolly mammoth is the next most depicted animal in Ice Age art after horses and bisons, and these images were produced up to 11,500 years ago. Today, more than five hundred depictions of woolly mammoths are known, in media ranging from carvings and cave paintings located in 46 caves in Russia, France and Spain, to sculptures and engravings made from different materials.
William Henry's fossil Mammoth tooth is harvested in Alaska and Siberia. It is a rare and mesmerizing material, a living testimony of the dawn of Mankind.
Smoky quartz is a grey, translucent variety of quartz. It ranges in clarity from almost complete transparency to a brownish-gray crystal that is almost opaque.
Smoky Quartz was known as a Stone of Power. To the ancient Druids, it was sacred and signified the potent dark power of Earth gods and goddesses.
Spearpoint Amber Butte $2,150.00
Spearpoint Blue Burl $1,650.00
Spearpoint Round Up $48,000.00
Spearpoint Glade $1,750.00
Spearpoint Majestic $1,850.00
Spearpoint Jerome $2,500.00
Spearpoint Spatial $3,750.00
Spearpoint Queensland $1,150.00
Spearpoint Burns $650.00
Spearpoint Soar $3,000.00
Spearpoint Jasmine $9,000.00
Spearpoint Synergy $25,000.00


TORONTO, March 18, 2015 /CNW/ - Triax Diversified High-Yield Trust (the "Fund") (TSX: "TRH.UN") announced today acceptance by the Toronto Stock Exchange (the "TSX") of the Fund's Notice of Intention to make a Normal Course Issuer Bid (the "NCIB").
Pursuant to the NCIB, the Fund proposes to purchase through the facilities of the TSX, from time to time, if it is considered advisable, up to 127,545 Units of the Fund, representing approximately 10% of the public float, being 1,275,458 Units as of the close of business of March 12, 2015. The Fund will not purchase in any given 30-day period, in the aggregate, more than 31,163 Units, representing approximately 2% of the issued and outstanding Units, being 1,558,176 Units as of the close of business of March 12, 2015. Purchases of Units under the NCIB may commence on March 20, 2015. First Asset Investment Management Inc., the manager of the Fund, believes that such purchases are in the best interests of the Fund and are a desirable use of the Fund's resources. All purchases will be made through the facilities of the TSX in accordance with its rules and policies. All Units purchased by the Fund pursuant to the NCIB will not be cancelled and will be held for resale. The NCIB will expire on March 19, 2016.
On March 10, 2014, the Fund announced that it was making a Normal Course Issuer Bid, which commenced March 12, 2014, to purchase up to 148,313 Units through the facilities of the TSX. No purchases were made under the Fund's prior Normal Course Issuer Bid.
First Asset is an independent investment firm, focused on providing smart, low cost solutions that address the real-world investment needs of Canadians - capital appreciation, income generation and risk mitigation. Rooted in strong fundamentals, First Asset's smart solutions strive to deliver better risk-adjusted returns than the broad market while helping investors achieve their personal financial goals.
For further information please contact Investor Relations, First Asset at 416-642-1289 or 1-877-642-1289 or visit www.firstasset.com.