text:
\section{Introduction}
Current research in galaxy evolution is still largely driven by our lack of  understanding of the link
between the two main types of galaxies observed in the sky. Many theories exist to explain the evolution
between star-forming, gas-rich spiral galaxies (``late''-type) and non-star-forming, passively-evolving
spheroid galaxies (``early''-type).
Since this bimodal nature is highly correlated to the stellar age and star formation history of the
individual galaxies, it is likely that we are observing two main stages of galaxy evolution
\citep{strateva01,baldry04,baldry06,kauffmann04,drory09}; and that the transition between these two
types occurs relatively quickly \citep{martin07}.  The colours and brightnesses (as defined by their
observed magnitudes) of all galaxies appear to be concentrated within two well-defined
colour--magnitude regions.  The star-forming galaxies appear to populate a space dubbed the ``blue
cloud'' and the passively-evolving, non star-forming galaxies lie in a region called  the ``red sequence''.
Recent studies argue that local galaxies must migrate
rapidly (within a Gyr) from the ``blue cloud'' to the ``red sequence''\footnote{There are a few cases
where the evolution of individual galaxies moves from the ``red sequence'' to the ``blue cloud''
\citep[e.g.\ ][]{kannappan09,wei10}.  In these cases,  passively-evolving galaxies have accreted more gas
 recently and are in the process of regrowing their stellar disk.  However, this ``red-to-blue'' mode of
evolution is very unlikely to apply to our particular study because our PSGs are defined to  have no
current on-going star formation.} due to the scarcity of galaxies within the intervening parameter space
 \citep[occasionally dubbed the ``green valley''; e.g.][]{schawinski07b}.  Therefore, valuable insights
into galaxy evolution can be obtained by studying galaxies that appear to have intermediate
properties and may be in the act of transitioning between the two main galaxy populations.

Post-starburst galaxies (hereafter PSGs) or post-quenching galaxies \citep{yan09} such as
``E+A'' or ``K+A'' galaxies, are galaxies which appear to have ceased current star formation, but
still exhibit the spectral signature of recently-formed stars. In E+A galaxies, strong Balmer
absorption lines are observed together with $\alpha$-element signatures such as
Mg$_{5175}$, Fe$_{5270}$ and Ca$_{3934,3468}$
\citep{dressler83,dressler92,dressler99, dressler04,couch87,maclaren88,newberry90,fabricant91,abraham96,poggianti99,goto03,goto04,goto05,goto07}. Similar to E+A galaxies, K+A galaxies are PSGs which have a disk-like morphology
 \citep{couch94,dressler94,caldwell97,dressler99}.
Although PSGs such as E+A galaxies are more common at higher redshifts \citep{wild09,tran04},
detailed high-resolution studies are only possible with a local population of PSGs since low redshift
 observations extend to lower surface brightness limits than that at earlier epochs.

Current studies favor the idea that PSGs are formed  via interactions or major mergers
\citep{yamauchi08,blake04, bekki01} which trigger bursts of star formation. However, due to the effects
 of the merger interaction, the gas reservoir (from which stars are formed) is depleted and these PSGs
eventually turn into bulge-dominated early-type galaxies once their star formation fades completely
\citep[e.g.\ ][]{yang08}. \citet{kaviraj07} found that the quenching efficiency of star formation in
 less massive ($< 10^{10}$ M$_{\odot}$) and more massive  E+A galaxies ($> 10^{10}$M$_{\odot}$) is
consistent with supernovae (SNe) and AGN being the main sources of negative feedback, respectively.

Using the Sloan Digital Sky Survey (SDSS), we assemble and analyze one of the largest, and
most complete samples, of local PSGs to date.  This paper investigates the properties of the local PSGs
derived from the visual classifications of the Galaxy Zoo citizen science project \citep{lintott11,lintott08}.

Section 2 describes our sample selection and the sample properties are examined in Section 3.
A discussion of our results and conclusions can be found in Section 4. The AB magnitude system is
used throughout this work.

\section{Our galaxy sample}

In this paper, we obtain the photometric and spectroscopic data from the Sloan Digital Sky Survey (SDSS)
DR7 \citep{york00,abazajian09} for all objects classified as `galaxy' \citep{strauss02}. The main galaxy
emission line measurements are determined from the SDSS spectra using the {\tt{Gandalf}} IDL tool
by \citet{sarzi06}. To minimise the Malmquist bias, and create a volume and magnitude-limited (proxy for
stellar-mass limited) sample of galaxies, we select all the galaxies within $0.02<z<0.05$ with $M_{z,Petro}<-19.5$
magnitudes.  We use the $z$-band since the reddest waveband provides the closest proxy to stellar mass.
It should be noted that the results of this paper remain unchanged if the  $i$-band is used instead.
As we aim to study the properties of all galaxies which have ceased star formation recently,
 we define a PSG to be a galaxy with a recently-truncated star formation history (i.e.\ where the
observed H$\alpha$ emission line is weaker than four times the RMS level), while still exhibiting strong
 balmer absorption lines from recently-formed young stars (where the H$\delta$ equivalent width is wider
 than three Angstroms). Our strict H$\alpha$ criterion may result in the omission of a few PSG known to
emit weak H$\alpha$ emission but the effects from the inclusion of a few H$\alpha$-emitting galaxies do not
change any of the results that we present in Section 3.

Studies such as \citet{balogh99,blake04,goto07}
 select for PSGs at higher redshifts ($0.5<z<1.0$) which exhibit very strong A-type stellar
populations (where the observed H$\delta$ equivalent width is wider than five Angstroms). To include
as many PSGs as possible into our sample, we imposed a more relaxed H$\delta$
equivalent width so we do not bias against galaxies with a low star formation rate (which results in
weaker Balmer equivalent widths) prior to the cessation of star formation.

The [{\sc{Oii}}] forbidden lines were not used in the selection criteria because the H$\alpha$ emission
line is a more accurate tracer of current star formation in the Local Universe.  The luminosity of the
[{\sc{Oii}}] emission lines is not directly linked to the ionizing luminosity and the [{\sc{Oii}}]
excitation is sensitive to the abundance and the ionisation state of the gas \citep{kennicutt98}.
Moreover, the [{\sc{Oii}}]-derived star formation rates (SFRs) is sensitive to systematic errors from
extinction and variations in the diffused gas fraction \citep{kennicutt98}. In starburst galaxies, the
excitation of [{\sc{Oii}}] is much higher in the diffused ionised gas \citep{hunter90,hunter94,martin97},
and is able to double the $L$[{\sc{Oii}}]/SFR ratio in the integrated spectrum \citep{kennicutt92a}.

Of 47,573 galaxies within our selected volume, we find a total of 80 PSGs.  The general properties of our PSGs
are listed in Table~\ref{genprops}. Figure~\ref{egsamp} shows the SDSS
multicolour composite images for 12 random PSGs within our sample.  This figure exhibits the variety of
morphologies and sizes within our PSG  sample.

Using the bootstrap resampling method to approximate the uncertainty, we find that our percentage of PSGs to the
total number of galaxies (within our specified volume out to $z\sim0.05$) is  0.17$^{+0.07}_{-0.05}$ \%. This
assumes that the uncertainty in our spectral line measurements is given by the signal-to-noise ratio (SNR).
  This PSG fraction is comparable to that of previous local PSG studies by \citet{goto05,goto07} and \citet{kaviraj07}.
It should be noted that we do not find many of the E+A galaxies found by  \citet{goto05,goto07} (hereafter
 known as the ``G05'' sample) from the SDSS DR5 catalogue because we detect strong H$\alpha$ emission in these G05
 objects using the SDSS DR7 catalogue. Hence, these E+A galaxies appear to have current, on-going star formation
and is inconsistent with our definition of a PSG.  Of the overlap galaxies between our full galaxy sample and that of
the G05 sample, we find that our method of using the  Balmer absorption line strength finds every galaxy found via
its absorption line equivalent width. This is consistent with the fact that there is a good correlation between the
line strengths and the equivalent widths for galaxies of similar sizes.

\begin{figure*}
\begin{center}
\begin{tabular}{ccc}
\includegraphics[scale=.4]{f1a.eps} & \includegraphics[scale=.4]{f1b.eps}&\includegraphics[scale=.4]{f1c.eps}\\
\end{tabular}
\end{center}
\caption{Example SDSS colour images of 12 PSGs within our sample. Each image frame provides a
48\arcsec$\times$48\arcsec\ field-of-view centered on the galaxy.  The left panel shows four examples of
early-type PSGs, the middle panel shows four examples of intermediate-type PSGs and the right panel
shows four examples of late-type PSGs. The red circles show the SDSS fiber field-of-view where
each spectrum was obtained.}
\label{egsamp}
\end{figure*}

\begin{table*}
\tiny{
\begin{center}
\caption{General properties of our PSG sample.}
\label{genprops}
\begin{tabular}{lcccccccccccl}
\hline
\hline
SDSS object ID & RA  &Declination  &$m_{\rm{r}}$ & $u-r$ & $EW$(H$\delta$)& $S_{\rm{[\sc{OII}]}}$ & $S_{\rm{H}\alpha}$&log (M$_{\star}$) & $f_m$& $frac_{\rm{dev}}$  & Type & Comments\\
(1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) & (10) &(11) &(12)\\
\hline
  587731513679478898  &  01:14:47.2 & $+$00:37:55.7 &      16.75 &       2.00 &  3.4&$<7.9\times10^{-15}$&---&     9.95 &        0.000 &   0.595   &  I & ---      \\
  587731513681313986  &  01:31:37.9 & $+$00:48:51.7 &      16.52 &       1.37 &  5.0&$<2.4\times10^{-16}$&$<1.3\times10^{-17}$&     9.69 &        0.000 &   0.000   &  I & ---      \\
  587731511533961332  &  01:32:50.2 & $-$00:56:17.6 &      16.86 &       2.11 &  4.7&$<6.4\times10^{-15}$&$<1.5\times10^{-15}$&    10.03 &        0.000 &   1.000   &  I & blob      \\
  587727230522032233  &  01:37:16.4 & $-$09:29:06.5 &      16.63 &       2.25 &  3.7&$<1.2\times10^{-16}$&---&     9.96 &        0.000 &   0.546   &  I & blob       \\
  588015510358524013  &  02:20:38.7 & $+$00:54:09.1 &      15.15 &       0.97 &  4.1&$1.5\times10^{-13}$ &$<6.3\times10^{-15}$&     9.66 &        0.000 &   0.240   &  S & ---     \\
  587731512082956346  &  03:23:33.3 & $-$00:26:18.8 &      14.92 &       2.04 &  4.2&---&$<7.3\times10^{-14}$&     9.99 &        0.000 &   0.770   &  E & ---      \\
  587731514232996008  &  03:47:10.2 & $+$01:04:39.9 &      15.78 &       1.77 &  3.9&$<4.8\times10^{-16}$&$<4.7\times10^{-17}$&     9.97 &        0.000 &   0.007   &  I & ---      \\
  587732053779283987  &  08:43:20.7 & $+$37:13:27.6 &      16.24 &       2.26 &  3.7&$<5.5\times10^{-16}$&$<3.1\times10^{-16}$&    10.23 &        0.000 &   0.926   &  I & blob      \\
  587744874791370929  &  09:01:03.8 & $+$13:36:33.3 &      14.91 &       0.85 &  4.0&$1.7\times10^{-13}$ &$<1.2\times10^{-14}$&     9.82 &        0.188 &   0.505   &  I &  disturbed     \\
  587745403073855572  &  09:11:31.1 & $+$12:08:52.1 &      14.96 &       2.22 &  3.3&$<1.0\times10^{-14}$&$<2.4\times10^{-15}$&    10.43 &        0.047 &   1.000   &  I & disturbed      \\
  587745540514119842  &  09:25:03.2 & $+$13:03:58.0 &      16.56 &       2.06 &  3.0&$<3.5\times10^{-14}$&$<2.2\times10^{-15}$&     9.81 &        0.000 &   1.000   &  I &  blob     \\
  588016891707392070  &  09:29:34.6 & $+$33:47:51.1 &      15.28 &       1.22 &  4.3&$1.1\times10^{-13}$ &$<1.6\times10^{-14}$&     9.70 &        0.115 &   0.000   &  I & disturbed        \\
  587745243626405989  &  09:45:00.0 & $+$15:27:40.0 &      15.79 &       2.10 &  4.0&$<1.2\times10^{-14}$&$<4.2\times10^{-15}$&     10.25 &        0.000 &   0.609   &  I & blob      \\
  587735044693753946  &  09:46:29.9 & $+$39:02:19.7 &      16.72 &       1.34 &  3.9&$1.9\times10^{-13}$ &$<1.2\times10^{-14}$&     9.61 &        0.000 &   0.620   &  I & ---       \\
  587725074458804315  &  09:49:56.4 & $-$00:13:52.9 &      13.89 &       2.36 &  3.4&$<6.5\times10^{-16}$&$<2.7\times10^{-16}$&    11.35 &        0.095 &   1.000   &  I & disturbed    \\
  588848900973789221  &  10:04:29.8 & $+$00:41:20.2 &      16.49 &       2.06 &  3.2&$<1.8\times10^{-16}$&$<2.1\times10^{-16}$&     9.93 &        0.000 &   0.870   &  I& blob      \\
  587726032236183669  &  10:06:50.9 & $+$01:41:34.0 &      16.94 &       2.08 &  5.7&$<2.0\times10^{-16}$&---&     9.84 &        0.074 &   0.613   &  I & blob        \\
  587738948283334792  &  10:12:18.9 & $+$36:07:50.0 &      15.62 &       1.59 &  3.3&$1.1\times10^{-13}$ &$<1.9\times10^{-14}$&     9.96 &        0.000 &   0.964   &  I & blob      \\
  587741828579393617  &  10:21:25.9 & $+$21:32:45.8 &      16.00 &       1.90 &  4.1&---&$<6.2\times10^{-16}$&     9.91 &        0.000 &   0.002   &  S &   ---    \\
  587733080268931236  &  10:30:53.7 & $+$51:19:59.6 &      15.05 &       1.18 &  4.2&$4.9\times10^{-15}$&$<8.3\times10^{-16}$&    10.35 &        0.031 &   0.194   &  S & asymmetric  \\
  587728947978436717  &  10:42:32.3 & $-$00:41:58.3 &      15.83 &       2.07 &  4.3&$<2.9\times10^{-16}$&$<7.5\times10^{-16}$&    10.10 &        0.000 &   0.994   &  I & blob        \\
  587729386611212446  &  10:53:05.4 & $+$57:51:54.2 &      15.60 &       1.10 &  3.8&$3.7\times10^{-16}$&$<1.5\times10^{-16}$&    10.05 &        0.000 &   0.054   &  I & ---        \\
  587734894357381314  &  11:00:48.5 & $+$10:31:19.0 &      16.44 &       2.23 &  4.2&$<6.1\times10^{-15}$&$<1.6\times10^{-15}$&    10.12 &        0.000 &   0.864   &  I &asymmetric      \\
  587741489834754106  &  11:10:33.9 & $+$28:29:33.3 &      15.73 &       2.07 &  4.1&---&$<1.4\times10^{-14}$&     10.00 &        0.000 &   0.985   &  I &  blob     \\
  588848898833842380  &  11:13:28.0 & $-$00:54:09.5 &      16.62 &       2.03 &  4.9&$<2.5\times10^{-14}$&$<3.7\times10^{-15}$&     9.57 &        0.000 &   0.771   &  I & blob      \\
  587732580982521898  &  11:19:07.6 & $+$58:03:14.3 &      14.17 &       2.16 &  4.7&$1.6\times10^{-13}$&$<2.9\times10^{-14}$&    10.74 &        0.000 &   1.000   &  I & asymmetric      \\
  587739405703577638  &  11:26:53.7 & $+$33:07:09.5 &      14.86 &       1.21 &  4.5&$1.3\times10^{-13}$ &$<7.3\times10^{-15}$&     9.92 &        0.108 &   0.190   &  S & --- \\
  587732482746548338  &  11:35:32.0 & $+$48:56:38.5 &      15.99 &       2.19 &  4.0&$<6.5\times10^{-15}$&$<1.3\times10^{-15}$&     9.76 &        0.017 &   0.866   &  I & disturbed      \\
  587741726574444657  &  11:36:55.2 & $+$24:53:25.5 &      14.92 &       1.73 &  5.5&$1.4\times10^{-13}$ &$ <5.0\times10^{-11}$  &   9.98 &        0.027 &   0.200   &  I &  disturbed     \\
  587742573224657026  &  11:43:47.8 & $+$20:21:48.0 &      15.61 &       1.83 &  6.7&$<8.2\times10^{-15}$&---&     9.56 &        0.000 &   0.305   &  S & disturbed   \\
  588017111833182222  &  12:21:05.7 & $+$47:58:51.9 &      16.54 &       2.18 &  3.6&$<7.2\times10^{-14}$&$<2.2\times10^{-15}$&    10.02 &        0.000 &   0.978   &  I &  ---     \\
  588017730836561977  &  12:26:41.6 & $+$08:44:32.2 &      15.42 &       2.45 &  6.5&$<8.9\times10^{-13}$ &$<4.9\times10^{-14}$&    10.38 &        0.000 &   0.906   &  I &  ---     \\
  587726033325850747  &  12:32:18.9 & $+$03:00:09.8 &      16.82 &       2.00 &  3.3&$<6.2\times10^{-14}$&---&    10.10 &        0.000 &   1.000   &  I & blob        \\
  587725816414142618  &  12:32:23.3 & $+$66:25:36.6 &      16.90 &       2.26 &  3.1&$<1.0\times10^{-16}$&---&     9.82 &        0.032 &   0.528   &  I & blob     \\
  587734892220252284  &  12:37:18.0 & $+$09:32:09.0 &      14.55 &       1.89 &  3.0&$<3.4\times10^{-16}$&---&     9.84 &        0.000 &   0.979   &  E & ---      \\
  587739096454332452  &  12:38:52.8 & $+$36:32:05.7 &      15.74 &       2.15 &  3.7&$<1.2\times10^{-16}$&$<1.3\times10^{-17}$&    10.19 &        0.000 &   1.000   &  E & ---     \\
  587741602572599308  &  12:57:17.8 & $+$27:48:39.3 &      15.40 &       1.97 &  3.9&$<1.7\times10^{-15}$&$<4.4\times10^{-18}$&     9.74 &        0.000 &   0.211   &  I &  disturbed     \\
  587741722823557134  &  12:57:21.7 & $+$27:52:49.5 &      15.23 &       2.10 &  3.6&$<5.1\times10^{-15}$&$<1.9\times10^{-17}$&     9.94 &        0.000 &   0.873   &  E &  ---   \\
  587741722286686489  &  12:57:45.7 & $+$27:25:45.6 &      15.92 &       1.94 &  3.9&$<1.3\times10^{-13}$&$<1.1\times10^{-14}$&     9.56 &        0.000 &   0.254   &  S &  ---     \\
  587741721749881039  &  12:58:12.0 & $+$27:07:39.5 &      16.60 &       2.31 &  3.5&$<3.0\times10^{-14}$&---&    10.06 &        0.000 &   0.806   &  S & ---      \\
  587741722823754043  &  12:59:39.5 & $+$27:51:16.6 &      16.57 &       2.20 &  4.2&$<3.7\times10^{-17}$&$<1.1\times10^{-17}$&     9.95 &        0.454 &   0.343   &  I &  disturbed     \\
  587741722823819345  &  13:00:10.2 & $+$27:51:50.2 &      15.85 &       2.22 &  3.4&$<2.8\times10^{-15}$&---&    10.00 &        0.097 &   0.357   &  I &  disturbed    \\
  587741722286948519  &  13:00:29.2 & $+$27:30:53.4 &      15.53 &       1.63 &  8.5&$<1.1\times10^{-15}$&$<9.6\times10^{-17}$&     9.55 &        0.125 &   0.224   &  I &  disturbed     \\
  587739719754514434  &  13:04:22.7 & $+$28:48:38.8 &      14.33 &       0.86 &  4.4&$<2.9\times10^{-12}$&$<4.2\times10^{-14}$&    10.15 &        0.365 &   0.643   &  S & disturbed \\
   587733195160485975  &  13:05:25.8 & $+$53:35:30.3 &      14.29 &       2.15 & 4.6&$<4.8\times10^{-16}$&$<1.4\times10^{-16}$&     10.75 &        0.000 &   1.000   &  E & ---      \\
  587722982822379684  &  13:17:59.6 & $-$00:17:43.2 &      13.29 &       1.22 &  5.2&$<2.1\times10^{-14}$ & $<5.1\times10^{-14}$&   10.44 &        0.139 &   0.477   &  S & asymmetric  \\
  587729773681377291  &  13:37:44.1 & $-$02:10:27.9 &      14.61 &       0.72 &  3.5&---&$<2.5\times10^{-14}$&   10.41 &        0.000 &   0.338   &  S & ---      \\
   587726032797565040  &  13:50:51.0 & $+$02:19:38.5 &      15.62 &       2.11 & 4.7&$<3.2\times10^{-16}$&$<8.7\times10^{-17}$&      9.97 &        0.167 &   1.000   &  I & disturbed        \\
  587730021178867826  &  14:18:51.0 & $+$05:28:14.2 &      15.92 &       2.09 &  3.0&$<7.3\times10^{-15}$&$<2.6\times10^{-15}$&    9.90 &        0.000 &   0.961   &  I &  blob     \\
  587739827130007710  &  14:39:08.5 & $+$22:17:42.4 &      15.42 &       0.84 &  4.5&$2.0\times10^{-14}$&$<1.1\times10^{-15}$&    9.75 &        0.136 &   0.000   &  I & asymmetric      \\
  587739408405626997  &  14:39:30.4 & $+$30:52:49.1 &      16.14 &       1.97 &  4.2&$<5.0\times10^{-14}$&$<1.3\times10^{-15}$&     9.97 &        0.153 &   1.000   &  I & disturbed     \\
  587739379916210254  &  14:54:24.7 & $+$27:39:38.7 &      16.23 &       2.04 &  3.9&$<1.8\times10^{-16}$&$<4.2\times10^{-17}$&     9.98 &        0.000 &   1.000   &  I & blob      \\
 587726032268362094  &  15:01:24.0 & $+$01:39:25.0 &      15.90 &       1.92 &   3.9&---&$<4.5\times10^{-15}$&    9.95 &        0.000 &   0.682   &  I & blob        \\
  588017949366157511  &  15:03:39.4 & $+$35:27:30.5 &      16.14 &       0.94 &  3.9&$1.8\times10^{-13}$ &$<6.4\times10^{-15}$&     9.60 &        0.000 &   0.000   &  I & ---      \\
  587736975271067720  &  15:12:04.1 & $+$28:25:14.1 &      14.26 &       1.20 &  4.2&$1.3\times10^{-15}$&$<4.7\times10^{-15}$&    10.43 &        0.015 &   0.772   &  I & asymmetric      \\
  588017991773978739  &  15:14:29.9 & $+$07:35:46.8 &      15.45 &       1.97 &  4.4&$<4.7\times10^{-14}$&$<5.5\times10^{-15}$&    10.27 &        0.000 &   0.918   &  I & blob      \\
  587736543098568963  &  15:21:08.6 & $+$07:37:53.9 &      16.40 &       2.05 &  4.9&$<1.7\times10^{-14}$&$<2.5\times10^{-15}$&    10.12 &        0.000 &   0.920   &  I & blob      \\
  587742575924805956  &  15:23:22.8 & $+$13:26:19.2 &      15.91 &       1.38 &  3.4&$2.8\times10^{-14}$ &$<7.7\times10^{-15}$&     9.99 &        0.000 &   0.038   &  I &  disturbed     \\
  587736477596975155  &  15:23:43.0 & $+$08:27:29.0 &      15.86 &       2.06 &  3.0&$<5.2\times10^{-16}$&---&     9.81 &        0.000 &   1.000   &  I & ---      \\
  587739810494218509  &  15:24:25.6 & $+$19:42:59.5 &      14.96 &       1.13 &  5.4&$1.2\times10^{-14}$&$<1.4\times10^{-15}$&     9.73 &        0.027 &   0.031   &  S &  L; disturbed   \\
  587733603187556413  &  15:26:21.9 & $+$48:42:14.4 &      15.88 &       1.58 &  3.9&$1.4\times10^{-13}$ &$<5.7\times10^{-14}$&    10.07 &        0.310 &   1.000   &  I & ---      \\
  588017703489634681  &  15:26:53.3 & $+$08:32:07.7 &      16.64 &       2.21 &  4.7&$<1.3\times10^{-13}$&$<5.7\times10^{-15}$&    10.00 &        0.000 &   0.359   &  I &  blob     \\
  587730021724062009  &  15:34:53.4 & $+$04:16:60.0 &      15.66 &       1.43 &  3.5&$1.9\times10^{-15}$&$<7.4\times10^{-16}$&    10.00 &        0.000 &   0.181   &  I &  disturbed      \\
  587739721917595889  &  15:39:19.9 & $+$21:21:30.0 &      16.76 &       2.05 &  3.1&$<3.9\times10^{-15}$&$<8.8\times10^{-16}$&     9.86 &        0.000 &   1.000   &  I &   blob    \\
  588017704565276972  &  15:44:31.7 & $+$08:35:07.4 &      16.52 &       1.93 &  3.6&$<6.4\times10^{-14}$&$<3.3\times10^{-15}$&     9.75 &        0.000 &   0.717   &  S &  ---     \\
 588011101570662666  &  16:00:17.3 & $+$46:51:35.6 &      16.57 &       2.28 &   3.3&$<9.8\times10^{-14}$ &$<8.1\times10^{-15}$&   10.29 &        0.000 &   0.779   &  E & blob      \\
  587739828212793702  &  16:03:15.7 & $+$16:19:07.9 &      15.86 &       2.09 &  3.6&$3.1\times10^{-14}$&$<4.5\times10^{-15}$&    10.07 &        0.044 &   0.814   &  I & disturbed      \\
  587739809961804053  &  16:03:25.9 & $+$15:38:48.2 &      15.43 &       0.84 &  4.0&$5.7\times10^{-14}$ &$<4.2\times10^{-15}$&     9.55 &        0.000 &   0.106   &  S &  L   \\
   587729227152752660  &  16:03:44.5 & $+$52:24:12.6 &      15.57 &       2.23 & 4.3&$<5.8\times10^{-15}$&$<1.2\times10^{-15}$&     10.42 &        0.000 &   1.000   & E &  ---     \\
  587739707420901722  &  16:04:38.6 & $+$17:36:35.0 &      16.61 &       2.00 &  3.8&$<3.3\times10^{-17}$&$<1.5\times10^{-16}$&     9.46 &        0.186 &   0.499   &  I & disturbed      \\
  587725817501712592  &  16:16:52.9 & $+$50:57:04.6 &      14.69 &       2.73 &  4.0&---&$<6.7\times10^{-15}$&    11.47 &        0.000 &   0.734   &  E & ---     \\
  587735666928844900  &  16:25:18.3 & $+$37:56:40.6 &      15.03 &       2.12 &  3.2&$<1.0\times10^{-15}$&$<1.6\times10^{-16}$&    10.15 &        0.000 &   1.000   &  I & ---      \\
  588018090548920817  &  16:41:33.5 & $+$24:42:14.2 &      16.01 &       2.02 &  4.1&$<6.9\times10^{-15}$ &$<2.3\times10^{-15}$&     10.04 &        0.000 &   0.849   &  I & blob      \\
  588018253228408956  &  16:53:14.4 & $+$25:07:59.2 &      14.01 &       1.45 &  4.3&$1.1\times10^{-13}$ & $<9.3\times10^{-14}$&    10.44 &        0.000 &   0.692   &  S &  disturbed     \\
  588018254302609790  &  16:59:33.1 & $+$24:55:59.9 &      16.17 &       2.36 &  3.0&$<7.3\times10^{-16}$&$<2.2\times10^{-16}$&    10.28 &        0.000 &   0.717   &  I &  blob     \\
  587733432998559923  &  17:04:51.3 & $+$25:03:18.4 &      16.51 &       2.51 &  8.3&$<1.1\times10^{-14}$&$<2.4\times10^{-15}$&    10.45 &        0.068 &   1.000   &  I &  blob     \\
  587725503947735340  &  17:14:07.2 & $+$57:28:38.7 &      16.00 &       2.10 &  3.2&$<1.4\times10^{-14}$&$<8.2\times10^{-16}$&     9.83 &        0.000 &   0.129   &  S & ---   \\
  587731174382502294  &  21:19:48.2 & $+$00:40:21.8 &      16.37 &       1.83 &  5.5&$<3.7\times10^{-16}$&$<5.5\times10^{-17}$&     9.91 &        0.000 &   0.880   &  I & ---        \\
  587727213347799419  &  21:33:56.5 & $-$07:54:08.7 &      15.22 &       1.14 &  4.4&$<2.7\times10^{-16}$&$<5.5\times10^{-17}$&     9.75 &        0.000 &   0.000   &  I & ---       \\
  587731185117954089  &  22:08:06.1 & $-$00:54:25.0 &      15.10 &       2.06 &  4.3&$<4.9\times10^{-16}$&$<3.3\times10^{-16}$&    10.54 &        0.036 &   1.000   &  E & disturbed      \\
\hline
\hline
\end{tabular}
\end{center}
\begin{flushleft}
Col.\ (1): SDSS object identification.  Col.\ (2): Galaxy center's right ascension.  Col.\ (3): Galaxy center's declination.
Col.\ (4):  $r$-band magnitude.  Col.\ (5): $u-r$ colour. Col.\ (6): H$\delta$ equivalent width (Angstroms).
Col.\ (7): Measured {\sc[Oii]} flux densities in units of $10^{-17}$ ergs s$^{-1}$ cm$^{-2}$ \AA$^{-1}$.  The  upper limits are defined to be four times the RMS noise.  Col.\ (8): Estimated upper limits for the H$\alpha$ flux densities in
units of $10^{-17}$ ergs s$^{-1}$ cm$^{-2}$ \AA$^{-1}$ as defined to be four times the RMS noise.
Col.\ (9): Log of the stellar mass obtained from \citet{schawinski07b} which were determined by fitting the five SDSS
photometric bands to model star formation histories  from \citet{maraston98, maraston05} stellar models . Col.\ (10): Weighted
merger parameter \citep{darg10}. Col.\ (11): The SDSS parameter  which gives the fraction of light (in the $r$-band) fitted by
a de Vaucouleurs profile. Col.\ (12): Description of galaxy type where `S' represents late-type spiral galaxies, `E' represents
early-type galaxies and `I' represent intermediate-type galaxies.  Col.\ (10): Comments from visual inspection of each galaxy.
A `disturbed' comment indicates that the stellar morphology appears to have been disrupted by tidal interaction with features such
as stellar tails/rings or with neighboring galaxies at close proximities. An `asymmetric' defines an observed asymmetric stellar disk.
A `---' comment represents galaxies whose morphologies appear fairly regular, while a `blob' comment refers to galaxy morphologies
which are small, compact and fairly spherical in appearance. An 'L' indicates that this galaxy exhibits spectral signatures of a LINER.
\end{flushleft}}
\end{table*}

\section{Results}

\subsection{Morphological properties}

\subsubsection{Morphological classification using Galaxy Zoo}
Galaxy morphologies are derived from the Galaxy Zoo 1 project  \citep{lintott11}.  From the multiple independent
 inspections (and classifications) made for each galaxy, the accuracy of the classifications for individual galaxies
can be determined by imposing a required level of agreement among the classifiers.  Following the definition
of the {\tt{clean}} sample from \citet{land08}, we require a minimum of an 80\% majority agreement on the
morphology for each object.  Spiral galaxies (from an Sa to an Sd morphology) are classified as {\em{late-type}}
objects, while all spheroids  (including lenticular  galaxies) are classed as {\em{early-type}}.    Galaxy
 morphologies which are neither ``early''- nor ``late'' are classed as {\em{intermediate-type}} which include
galaxies with irregular/disturbed and merging morphologies.

\begin{table}
\begin{center}
\caption{Distributions of galaxy morphologies and star formation properties of our entire
local volume sample and that of the PSG sample. The distributions are listed as percentages
and the number of galaxies are given in parentheses. }
\label{morph1}
\scriptsize{
\begin{tabular}{lcccc}
\hline
\hline
\multicolumn{4}{c}{Entire Galaxy Sample} & PSG sample \\
 & Non-SF & SF & Total & \\
\hline
Early-type &     50\% (5148)   &   10\% (3770)     &     19\% (8918)   & 16\% (13) \\
Intermediate &   46\% (4841)   &   47\% (17589)    &             47\% (22430)   & 74\% (59)\\
Late-type  &   4\% (388)    &   43\% (15837)     &              34\% (16225)    & 10\% (8) \\
Total &     100\% (10377)      &   100\% (37196)     &               100\% (47573)  & 100\% (80)\\
\hline
\hline
\end{tabular}}
\end{center}
\end{table}

Relative to the entire local volume sample, there is a smaller fraction of PSGs with spiral or late-type
morphologies. We find that 74 ($\pm10)$\% of our PSG sample appear to have intermediate morphologies, while
16 ($\pm 5$)\%  and 10 ($\pm 4$)\% of our PSGs are classed as early- and late-types, respectively. It should
 be noted that a colour bias in morphology votes (by the Galaxy Zoo citizen scientists) is unlikely to occur
 since our PSG sample is dominated by intermediate-type morphologies.  In addition, investigations by
\citet{lintott08} found colour bias to not be a significant effect on the final morphological classifications.

Similar to the results of \citet{baldry04,driver06,bamford09}, we find that the majority of the spheroidal/elliptical
galaxies within our local volume sample exhibit non-star-forming (non-SF) properties, while, the star-forming
(SF) galaxies tended to have spiral morphologies. In this paper, we classify a galaxy as star-forming if its
 H$\alpha$ emission line is stronger than four times the RMS level.  As expected from our PSG selection criteria
of galaxies with recently-truncated star formation, we find that the PSGs appear to have a morphology distribution
which appears intermediate to that of SF and non-SF galaxies within the control sample.
Table~\ref{morph1} lists the distribution of morphologies and star-forming properties  of both the local volume
control sample and the PSG sample.

In addition to the Galaxy Zoo classifications, we visually inspected each PSG to confirm the morphologies.
Consistent with the fact that a majority of the PSGs have intermediate-type morphologies, we find disturbed galaxy
morphologies which resemble neither early- nor late-type galaxies.      Depending on the size
of the galaxy, the 3\arcsec\ fibers (from which the SDSS spectra are obtained) may only correspond to the central
1.2--2.9 kpc of galaxies within our redshift range. In our sample, the observed spectral properties may not be
representative for approximately 5\% of our sample where the outer
galaxy regions are much  greater than 3\arcsec\ and appear to be bluer than the central region.

The $f_{\rm{m}}$ parameter is a quantification of the merger properties of Galaxy Zoo 1 and is defined to be the
 weighted-merger-vote fraction where the fraction of merger votes is multiplied by a weighting factor
\citep[$W$; ][]{lintott08} to account for the quality of the particular voters who have assessed each galaxy
\citep{darg10}. Assuming that $f_{\rm{m}} > 0.4$ describes a merger \citep{darg10}, we do not find many mergers within our PSG sample even though a large number of the PSGs
appear asymmetrical or disturbed.  A comparison of the distribution of $f_{\rm{m}}$ parameters of our PSG sample
 to those of the early- and late-types of the entire galaxy sample yields Kolmogorov-Smirnov (KS) probabilities
which indicate that there are no significant differences between any of the $f_{\rm{m}}$ distributions. Figure~\ref{fmdist}
shows the normalized cumulative distributions of $f_{\rm{m}}$ for the different galaxy types.

\begin{figure}
\begin{flushleft}
\includegraphics[scale=0.43]{f2.ps}
\end{flushleft}
\caption{Peak-normalized cumulative distributions of $f_{\rm{m}}$ for our PSG sample (black solid line) and
the different types of galaxies within the control sample. }
\label{fmdist}
\end{figure}

\subsubsection{Concentration}

As the majority of our PSG sample consists of intermediate-type morphologies, further investigation of the stellar
structure will reveal quantitatively whether these PSGs truly have intermediate-type morphologies (possibly due to past interactions) or are
 similar in structure to the early- or late-type galaxies within the same volume.  We measure the  concentration
index  using the ratio between the $R90$ and $R50$ parameters which are the radii where 90\% and
50\% of the total Petrosian\footnote{A Petrosian radius is where the mean local surface brightness (within the local
annulus) is equal to a constant fraction of the mean surface brightness within that radius \citep{strauss02}.} flux have
been measured in the $i$-band.  Therefore bulge-dominated galaxies will have greater $R90/R50$  ratios, while
disk-dominated galaxies will have smaller values.

To determine the end-products of our PSG sample, we compare the peak-normalised distributions of concentration
 indices for our population of  PSGs  to the early- and late-type population of galaxies with
log (M$_{\star}$) $<10.5$ M$_{\odot}$.  In agreement with \citet{strateva01}, we find that the division between
early- and late-type galaxies is where the $R90$ is approximately 2.6 times greater than the $R50$.
The distribution of concentration indices for our PSG sample is very similar  to that of the early-type galaxies.

On the other hand, \citet{masters10} showed that early-type galaxies classified in such a manner may be
contaminated by up to 50\% by edge-on spirals and that the SDSS {\tt{fracDev}} parameter ({\tt{fracDev}}; which
gives the fraction of light  fitted by a de Vaucouleurs profile) provides a better differentiation between the early-
and late-type galaxies as typical early-type elliptical galaxies are traditionally characterised by a de Vaucouleurs
profile and as such have an {\tt{fracDev}} $ > 0.5$.  As such, we show the distribution of {\tt{fracDev}} for our
``green'' PSGs and low-mass early- and late-type sample in Figure~\ref{fracdevfig}.  The PSG distribution is shown
by the gray-shaded histogram, while the striped histogram in the left-panel represents the distribution for the
early-types and the distribution for late-types are represented by the striped histogram in the right panel.
A quantitative comparison using the KS test yields a KS probability of 0.68 that the {\tt{fracDev}} distributions of
PSGs and early-types are derived from the same parent sample, while  the {\tt{fracDev}} distributions of PSGs and
late-types yield a KS probability of $<$0.001.

\begin{figure}
\begin{center}
\includegraphics[scale=0.45]{f3.eps}
\end{center}
\caption{Peak-normalised distributions of {\tt{fracDev}} (which describes the fraction of light from a fit to a
de Vaucouleurs profile). The gray shaded histograms show the {\tt{fracDev}} distribution for PSGs.  The
striped histogram show the {\tt{fracDev}} distribution for the early-type galaxies (in the left panel) and
the distribution for the late-type galaxies (in the right panel).}
\label{fracdevfig}
\end{figure}

Therefore, we find that the structural stellar morphologies of the PSGs within the ``green valley'' appear to be
more closely related to the morphologies of low-mass early-type galaxies even though star formation has only been
truncated recently.

\subsection{Colour and stellar mass}

We derive the $u-r$ colours of our sample using the {\tt{modelMags}} \citep[from SDSS DR7; ][]{abazajian09}
which are determined from the best fit of each galaxy profile to the linear combination of the exponential and the
de Vaucouleurs profiles.
In addition, these magnitude measurements are corrected for dust attenuation using the models of \citet{calzetti00}.
The ``green valley'' of our sample's colour distribution is defined to be within the nominal colour range of $1.8<u-r<2.3$.
The stellar mass estimates for each galaxy are measured by fitting the five optical wavebands from SDSS to star formation
history libraries generated from stellar models of \citet{maraston98,maraston05}. The uncertainties in our derived
stellar masses are dominated by the inherent uncertainties within the stellar models used. More details on the
parameterization of the star formation histories  and the fitting process can be found in \citet{schawinski10a} and
references within.

\begin{figure*}
\raggedright{
\includegraphics[angle=90,scale=0.535]{f4.eps}
\caption{The $u-r$ colour versus stellar mass distribution of our the SDSS galaxy sample are shown by the contours.
The top row shows PSG sample (solid red circles) overplotted onto the distribution of SDSS galaxies of a particular
type (demarcated by the solid line contours). The panels from left to right show the distributions: for all galaxy types,
for early-type galaxies, for intermediate-type galaxies and for late-type galaxies.
Within the top row, the distribution of SDSS galaxies for all galaxy types
are also shown as a comparison by dotted-lined contours within the early-, intermediate and late-type galaxy panels.
The bottom row shows the number fraction of our PSG sample to the galaxy sample of a particular type in a given
colour--mass bin as a solid orange contour map overlaid onto the contours marking the distribution of SDSS galaxies.
The maximum number fractions for all galaxy types, early-types, intermediate-types, late-types are 3.0\%, 2.6\%,
3.0\% and 1.9\%; respectively.  }
\label{colourmass}
}
\end{figure*}

The top row of panels in Figure ~\ref{colourmass} shows the colour--stellar mass distribution of our PSG sample as red
solid circles and the SDSS galaxy sample of a particular type is represented by the black solid contours. Black
dotted-lined contours represent the distribution of the entire sample regardless of galaxy-type and are shown for
comparison purposes.  The bottom row of panels in Figure~\ref{colourmass} shows the distribution of the fraction of PSGs
to the number of galaxies (of a particular type) in a given colour--stellar mass bin as a solid orange-shaded
contour map overlaid on the solid contours showing the distribution of the SDSS galaxies of  a particular type.

As can be seen from the top row panels of Figure~\ref{colourmass}, our PSG sample appears to be spread over a fairly
large $u-r$ colour range even though a majority (94\%) of the PSGs have stellar masses below the transition mass of
log $M_{\star} <$ 10.5 M$_{\odot}$ which separate the low-mass star-forming galaxies from the high-mass passively-evolving
bulge-dominated galaxies \citep{kauffmann03}. In fact, we do not find any PSG with a log $M_{\star} >$  11.5 M$_{\odot}$.
Such a stellar mass limit in our PSG sample is more clearly illustrated by the number fractions of PSGs to
the number of galaxies within a particular colour--stellar mass range (see the bottom panels of Figure~\ref{colourmass}).
  Figure~\ref{fracerrsmassbin} shows the percentage of PSGs per 10$^{0.5}$ M$_{\odot}$  bins. The average
percentage of PSGs in the log $M_{\star}$ bins between  9.5 and 10.5 M$_{\odot}$  is $\sim8$ times greater than that
between the log $M_{\star}$ bins between 10.5 and 11.5 M$_{\odot}$ (with a 3$\sigma$ significance). The uncertainties in the stellar
masses are dominated by the uncertainties in the stellar population models and can be up to 10$^{0.3}$ M$_{\odot}$  in
stellar masses \citep[e.g.\ ][]{conroy09}.

\begin{figure}
\begin{center}
\includegraphics[scale=0.5]{f5.eps}
\end{center}
\caption{Percentage of PSGs as a function of stellar mass. The uncertainties are given by the 10$^{\rm{th}}$ and 90$^{\rm{th}}$ percentile
values derived from bootstrap resampling of our data. }
\label{fracerrsmassbin}
\end{figure}

One possible reason for the lack of high mass PSGs is likely to be because our sample is restricted to a very
 local volume. As such, the probability of finding massive galaxies in such a local volume is much less than at
higher redshifts. Galaxies with log stellar masses greater than 11.5  account for only 3.8\% of the entire galaxy
sample. In addition, high-redshift surveys of E+A galaxies are not as sensitive to smaller (and fainter) galaxies.
As such, the E+A galaxies found at $z\sim0.1$ are most likely the biggest and brightest types of post-starburst
galaxies. For example, the PSG sample at $z=0.8$ in \citet{yan09} have stellar masses greater than
$10^{10.6}$ M$_{\odot}$. In addition, low redshift PSGs are also more closely associated to less massive blue
galaxies than high redshift PSGs which are more similar to massive red galaxies \citep[e.g.\ ][]{yan09}. Therefore,
it is not surprising that our local sample of PSGs is dominated by low mass objects.

In addition to the apparent stellar mass limit of  our PSG population, the bottom panels of  Figure~\ref{colourmass}
also show that a significant fraction (61\%) of our PSG sample reside within the ``green valley'', while 31\%
and 8\% reside in the ``blue cloud'' ($u-r < 1.8$) and the ``red sequence'', respectively.  Similarly, we find that
the percentage of  PSGs within the ``green valley'' (0.6\%) is 17 times and 6 times greater than the fraction
of PSGs within the ``red sequence'' and the ``blue cloud'', respectively. Hence, we propose that local PSGs occupy
a well-defined position in the low-mass end of the ``green valley''.   Consistent with the idea of galaxy formation
 downsizing, we postulate that local PSGs  will transform into passively-evolving ``red'' galaxies
 and contribute towards the build-up of  the low-mass end of the ``red sequence'' if star formation has indeed ceased.

\subsection{Environment}
Using the adaptive Gaussian environment parameter, $\rho_{\rm{g}}$ \citep[which provides a measure of
the number and proximity of galaxies around a point in space, see][]{schawinski07a},  we study the
environment properties of our PSG sample.  Low, medium and  high density environments are
described by $\rho_{\rm{g}} < 0.21$, $ 0.21 <\rho_{\rm{g}} < 0.58$  and $\rho_{\rm{g}} > 0.58$ respectively
\citep{schawinski07a}.
The low density class of environment can be likened to the galaxy field environment.  Similarly,  the
medium and high density classes can be compared to the group (or cluster outskirts) and cluster
environments, respectively.

\begin{table}
\begin{center}
\caption{Fractions of galaxies in three different environment classes for different types of galaxies.  }
\label{envtab}
\footnotesize{
\begin{tabular}{lccc}
\hline
\hline
 Galaxy type & $\rho_{\rm{g}} < 0.21$ & $ 0.21 <\rho_{\rm{g}} < 0.58$  &$\rho_{\rm{g}} > 0.58$\\
\hline
Early-type & 45\% (4034) & 29\% (2561) & 26\% (2333)\\
Intermediate & 53\% (11866) & 27\% (6022) & 20\% (4592)\\
Late-type  & 56\% (9124) & 28\% (4555) & 16\% (2566)\\
PSG & 50\% (40) & 26\% (21) & 24\% (19) \\
\hline
\hline
\end{tabular}}
\end{center}
\end{table}

We find that 50\% of our sample reside in the low density environment, while 26\% and 24\% reside in
the medium and high density environments, respectively.   In high density environments, the fraction of
PSGs is similar to that of early-types, while in low density environments, the fraction of PSGs is in
between that of intermediate- and early-type galaxies. As can be seen from Table~\ref{envtab},
the number fractions of early- and late-type galaxies in the low and high density environments differ by
$\sim$10\% whereby a greater fraction of early-types are found in high density environments and a greater
fraction of late-types are found in low density environments.  This greater fraction of early-type
galaxies at higher densities recapitulates the well-known morphology--density relation found by
\citet{dressler80} and more recent studies such as \citet{bamford09}. Similar to the PSG sample, the
intermediate-type galaxies appear to have fractions which are in between those found for early- and late-types.
In addition, the fractions of galaxies residing in medium density environments are roughly the same
regardless of galaxy types
It should be noted that KS tests comparing the $\rho_{\rm{g}}$ distributions of different galaxy types
confirm these results.  Hence, we find that the PSG distributions across all three environment
classes are similar to those of the early- and intermediate-type galaxies. This is consistent with the
fact that $\sim90$\% of the PSG sample consists of galaxies classified as early- or intermediate-type
galaxies.  Our results are also consistent with those of \citet{blake04} who found that the local
environments of E+A galaxies follow that of the general galaxy population.

\section{Discussion}

Our results show that local post-starburst galaxies represent one population of galaxies which
currently occupies a well-defined position in the low-stellar-mass end of the ``green valley''
and is rapidly transitioning onto the low-mass end of the ``red sequence'' unless star formation
resumes within the  transitioning period of $\sim1$ Gyr.  The duration within which the individual
PSG spends in the ``green valley'' is probably only on the order of $\sim1$ Gyr (the timescale for
the fading of the Lyman continuum from the current generation of young stars) because structurally,
 the stellar concentration of the PSGs within the ``green valley'' already closely resemble those
 of low-mass early-type galaxies even though star formation has only been truncated recently.
Our transition timescale concurs with recent findings of transition times on the order of $\sim1$
Gyr between the ``blue cloud'' and the ``red sequence'' \citep[e.g.\ ][]{kaviraj11,kaviraj07, schawinski07b}.
These results are  consistent with the idea of downsizing in the sense that larger objects have mostly
been formed at earlier epochs, while smaller objects are still being formed at later epochs.
Our results are therefore comparable to those of \citet{wild09} who found the mass density of PSGs to be
 230 times lower at $z\sim 0.07$ than at $z\sim 0.7$.

Current galaxy evolution models often suggest that feedback from an active galactic nuclei (AGN) could
provide the means to quench and truncate the star formation history of a massive galaxy
\citep[e.g. ][]{silk98, kaviraj05,croton06}.
Incidentally, our observation of a stellar mass limit in our PSG sample coincides with the findings of
\citet{schawinski10a} who found that the AGN duty cycle peaks at the low mass-end of the ``green valley''
and that the low-mass early-type AGN hosts appear to have post-starburst properties.  However, apart from two
PSGs which exhibit spectral properties of LINERs, we do not observe any spectral signatures of AGN within
our PSG sample.

The connection between AGN and merger/interactions have been discussed in the context of mergers
inducing in-flows of gas that fuel star formation and the black hole \citep[in the central regions; e.g.\ ][]{canalizo06},
 while feedback from the AGN is predicted to quench star formation by re-heating the cold gas and expelling
much of it in AGN-driven winds \citep[e.g.\ ][]{dimatteo05,thacker06}.  \citet{tremonti07} found evidence for
these winds in 10 out of 14 PSGs at $z=0.6$.  They hypothesised that the observed gas outflows in these
galaxies suggest that AGN feedback may play a role in quenching star formation in PSGs.
Compared to the PSG sample of \citet{tremonti07}, our local PSGs are redder and not as massive.
Therefore, following the results of \citet{yan09} and \citet{wild09}, we hypothesise that the evolution of our
local PSG sample is likely to be different to that of PSGs at higher redshifts. Consistent with the results of
\citet{kaviraj07}, it is unlikely that AGN feedback will be a dominant quenching process for star formation
in local PSGs.

\section{Summary}
In this paper, we have presented a study of local post-starburst galaxies (PSGs) using the photometric and spectroscopic
observations from SDSS in conjunction with the results from the Galaxy Zoo 1 project. We find that:

\begin{itemize}
\item The local population of PSGs occupy a well-defined space on the colour--stellar mass diagram, most notably in the
low-mass end of the green valley below the transition mass \citep[log $M_{\star} <$ 10.5 M$_{\odot}$; ][]{kauffmann03}
 thought to be the mass division between low-mass star-forming galaxies and high-mass passively-evolving bulge-dominated
galaxies.  Consistent with the idea of galaxy formation downsizing where smaller galaxies form at later epochs, we think
that the local PSGs  will contribute to the build-up of the low-mass end of the red sequence if star formation has indeed
ceased in these galaxies.

\item Consistent with previous studies \citep[e.g. ][]{blake04}, we find that local environment of local PSGs follow that
of the general galaxy population within the same volume.

\item Using the morphological classifications from Galaxy Zoo, we are able to study the distributions
of morphologies in our PSG sample in comparison to those of 47,573 galaxies in our full galaxy sample within the same
 local volume. Although a majority of our local PSG sample appears to have intermediate-type morphologies which
are neither early- nor late-type morphologies, we find that  the stellar structural morphology (as described by {\tt{fracDev}})
of the local ``green valley'' PSGs to be very similar to that of low-mass early-type galaxies in the ``red sequence'' even
though star formation has only recently ceased.  Therefore, unless star formation resumes, we hypothesize that the
local PSGs  will evolve out of the ``green valley'' in  $\sim1$ Gyr  onto the ``red sequence'' as soon as the young stellar
population from the most recent episode of star formation fades.

\end{itemize}

\vspace{1cm}

\chapter{\bf{Acknowledgments.}}
Galaxy Zoo acknowledges support from The Leverhulme Trust.
OIW is the recipient of a Super Science Fellowship from the Australian
Research Council.  Support for the work of KS was provided by NASA through
Einstein Postdoctoral Fellowship grant number PF9-00069 issued by the Chandra
X-ray Observatory Center, which is operated by the Smithsonian Astrophysical
Observatory for and on behalf of NASA under contract NAS8-03060.
KLM acknowledges funding from the Peter and Patricia Gruber Foundation
as the 2008 Peter and Patricia Gruber Foundation International
Astronomical Union Fellow, from a 2010 Leverhulme Trust Early Career
Fellowship and from the University of Portsmouth and SEPnet
(www.sepnet.ac.uk). The authors also thank the anonymous referee
 for the constructive comments which has improved this paper.

\bibliographystyle{mn2e}

redpajama_set_name: RedPajamaArXiv


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Starbucks Corp. has launched an aggressive plan to ensure coffee sold in its stores comes from environmentally friendly farms paying workers a fair wage, Chief Executive Orin Smith said in an interview.
By 2007, Starbucks expects that 60 percent of its coffee will come from farmers following strict rules on everything from forestation to pesticides to labor practices. About 10 percent of Starbucks' coffee is bought from suppliers following such rules now. "It's very aggressive," Smith told Reuters in an interview on Thursday.
Starbucks hopes the move will protect its growing empire of 8,500 coffee shops from boycotts and bad publicity.
"If you are tapped as a bad corporate citizen, the penalty is large," Smith said. Starbucks recently lost business in the U.K. during a campaign by the charity Oxfam showcasing the global coffee crisis.
"We got hit hard," Smith said. The company has since entered into a partnership with Oxfam to work on a rural development program in a coffee-growing region of Ethiopia.
In 1999, a Starbucks store was trashed by protesters at the World Trade Organization meeting in Seattle.
Smith said the program should not raise costs because the premium Starbucks already pays provides coffee growers from Latin America to Asia with incentive to plant trees; limit pesticide use; and raise wages.
Starbucks has long paid above-market prices for coffee, averaging about $1.20 a pound for the last three years. On the New York Board of Trade, December arabica coffee closed on Thursday at 77.7 cents a pound.
"These high prices we pay made us the company that everybody wants to do business with," Smith said. "We are able to leverage that and say if you want to do business with us, here is what you have to do."
Starbucks sells several varieties of shade-grown, Fair Trade, and organic coffees in one-pound bags, sometimes as its "coffee of the day." Smith said the company's new guidelines are more comprehensive than any of those individual labels.
Seattle-based Starbucks received help in developing the guidelines, called the Coffee and Farmer Equity (C.A.F.E.) Practices Program, from environmental nonprofit Conservation International (CI) and other nongovernmental organizations. Scientific Certification Systems, an independent environmental and food safety evaluation and certification firm, will audit growers participating in the program.
Protesters have targeted global companies like Wal-Mart Stores Inc. and McDonald's Corp., charging them with squeezing out local businesses and exploiting workers. CI CEO Peter Seligman said Starbucks has set a high standard, and some other U.S. companies are following suit.
"There has been a ripple effect," said Seligman, who added that CI is working with McDonald's on the fishing practices of suppliers so fish stocks will survive over time.
Starbucks hopes to keep increasing the amount of coffee it buys under C.A.F.E. Practices after it hits the 60 percent goal, Smith said.
But he said the figure probably would not reach 100 percent, noting that Starbucks has had difficulty in countries like Kenya, where the government controls coffee supplies.


text:
DRE may refer to:

 Dre (album), 2010 by American rapper Soulja Boy Tell 'Em, 2010
 Dre (name)
Dr. Dre, American rapper and producer
 DRE voting machine
 Digital rectal examination, in medicine
 Director of religious education; for example,
 Directorio Revolucionario Estudiantil, CIA backed anti-Castro group based in Miami
 Drug Recognition Expert
 Drug resistant epilepsy, in neurology
 Dense-rock equivalent in geology/volcanolgy

redpajama_set_name: RedPajamaWikipedia


text:
Emmanuel Renaut creates typical Savoyard dishes for Air France's La Première menu
From November 2019 to February 2020, for the first time, Emmanuel Renaut will be creating dishes for the Air France La Première menu. Awarded the title of meilleur ouvrier de France and a triple Michelin-starred chef, Emmanuel Renaut belongs to a new generation of chefs who are reinventing Savoyard cuisine. His refined, vibrant and colourful cuisine features surprising and harmonious compositions.
In collaboration with the Servair Culinary Studio, onboard the company's most exclusive cabin, the chef is signing two appetizers, seven main dishes and one dessert that customers can discover over the next four months.
Emmanuel Renaut's dishes on Air France's La Première menu:
Two appetizers:
Langoustine tartar and caviar with lemon and gentian
Royal celery and chestnut soup
Seven dishes:
Venison steak, celery and chestnut purée
Scallops quenelle, lemon sauce, root vegetable risotto
Spinach gratin, mushroom polenta
American lobster royale and mini vegetable balls
Root vegetable risotto with beaufort, crispy vegetable muesli
Veal shank blanquette-style
Farm chicken wing and thigh, scalloped potatoes and mushrooms
One dessert:
Much more than a creator of recipes, Emmanuel approaches his profession as a messenger. Transmission lies at the heart of his mission. Respect for nature, respect for the soil, animals and humans are the messages he wants to convey through each of his creations.
French chef born in 1968 in Soisy-sous-Montmorency, Emmanuel Renaut is part of a new generation of chefs who are reinventing local dishes by using local produce in inventful ways.
After training in Paris, he began his career at the hotel Crillon restaurant, with Christian Constant. He then joined Marc Veyrat at the Auberge de l'Eridan, where he was second in command to him for seven years. This experience was interrupted by a spell with chef Yves Thuriès.
After a period in London, where he was in charge of the kitchens at Claridge's, he returned to the mountains and settled in Megève, in the heart of the French Alps, in 1997, where he opened his gastronomic restaurant Flocons de Sel. Strongly inspired by Savoyard cuisine, he creates a gourmet, vibrant, colourful and resolutely modern cuisine featuring surprising and harmonious compositions.
In 2017, while back in his native Haute Savoie between trips, Emmanuel returned to the alpine pastures where he opened his alpine restaurant, Le Forestier, in Megève.
Emmanuel Renaut has since accumulated a list of accomplishments, holding the title of Meilleur Ouvrier de France (Best Craftsman of France), Compagnon du Tour de France (Companion of the Tour de France) and earning three stars in the Michelin Guide.
Written by Jason Published 18:08
Tags: Air France, News
Chief Aviation Correspondent. Jason has many years experience of the aviation and media industries. He has written numerous articles, reports and features for various publications and is the author of a number of both nonfiction and fiction books.

redpajama_set_name: RedPajamaCommonCrawl


The past seven days of racing have seen profits galore. For two pro punters in particular, it has been a week they won't be forgetting in a hurry. This dynamic duo of Tezzaraki and Rowdylegend combined for a ridiculous $25k* profit between them.
First up is Tezzaraki, a veteran punter who hails from the Moreton Bay area in Queensland. And didn't his experience pay off, picking up just shy of fifteen grand in cash from $100 win bets. This extraordinary profit came from the crazy value he found from his winners which averaged odds of $26.26.
Tezzaraki's phenomenal week finished with an enormous 371% profit on turnover (POT) rocketing him right to the top of the November Tipping competition leaderboard with 84% POT posted over the entire month.
The other Pro punter who cleaned up deluxe was Rowdylegend. This bloke picked up just shy of $10k* in profit from his racing tips with his winners also averaging huge odds of $28.60.
That effort is just typical of what the Shepparton punter has served up over the past 30 days. At close of business Monday night he had amassed $12,050* profit over the extended period. With 62% POT achieved from almost 200 tips in November, the pro punter has put himself well in contention to share in the $1,000 cash on offer in the November tipping competition.
If you're searching for a media tipster who can't stop tipping winners, then look no further than Richard Callander. Big Richie has recorded the second highest POT over the past seven days, notching up a whopping 273% POT.
Richie's Sydney tips have been on fire. At Rosehill on Saturday he tipped 5 of the 8 winners on the card, including the roughie Kool Vinnie in Race 6, which saluted at odds of $18.80.
Richie's tipping performance over the past 7 days is by no means a flash in the pan. The popular racing identity has notched up 7 profitable days from his last 9 tipping days and over the past 30 days, he has found his army of followers more than three and a half grand in profit*.
That pours plenty more gas on the #BringBackRitchie to broadcasting fire that is burning amongst Aussie punters on social media.
Another tipping hot streak that is well under way comes from Sky Racing analyst Michael Charge. The North Queensland racing expert has knocked up 5 palings in his 'profitable days' picket fence and looks like he's got plenty more in him.
With $1,950* in profit at 93% POT, Charge has also had a stellar tipping week and month with his November POT sitting at 79% and earning him second place in the tip comp, just behind Tezzaraki with just three days to go.
*Profit calculated from $100 win bets on each tip.


Hi I'm using a command line script to upload a file to a 3rd party SMTP site using the sync command. The file is renames to filename.FILEPART when the upload completes successfully it renames back to filename. The 3rd party have something which picks the file up really quickly but their mark is set up for files with FILEPART as the extension. How can I leave it with this extension?


text:
https://www.thehour.com/nation/article/Iraq-attacks-kill-106-in-deadliest-day-in-2-years-8227447.php
Iraq attacks kill 106 in deadliest day in 2 years
BUSHRA JUHI SINAN SALAHEDDIN
Published 9:15 am EDT, Monday, July 23, 2012
People inspect the aftermath of a car bomb attack in Baghdad's Shiite enclave of Sadr City, Iraq, Monday, July 23, 2012. An onslaught of bombings and shootings killed scores of people across Iraq on Monday, in the nation's deadliest day so far this year. The attacks come days after the leader of al-Qaida in Iraq declared a new offensive seeking to re-assert its might in the security vacuum left by the departing Americans. (AP Photo/Karim Kadim)
People inspect the aftermath of a car bomb attack in Baghdad's Shiite enclave of Sadr City, Iraq, Monday, July 23, 2012. An onslaught of bombings and shootings killed scores of people across Iraq on Monday, in
BAGHDAD (AP) -- Bombings and shootings ripped across Iraq on Monday, killing at least 106 people in the deadliest day in more than two years. The coordinated attacks in 15 cities sent a chilling warning that al-Qaida is slowly resurging in the security vacuum created by a weak government in Baghdad and the departure of the U.S. military seven months ago.
Though there was no immediate claim of responsibility, the leader of al-Qaida in Iraq declared last week a new offensive aimed at sowing instability across the country.
Iraqi militants have kept up a steady drumbeat of deadly attacks since the U.S. pulled out in December, ending nearly a decade of war. They have sought to increase the chaos created by the deepening sectarian political crisis that pits Sunni and Kurdish leaders against Shiite political powers.
"Al-Qaida is trying to send a message that it is still strong and can choose the time and places to attack," said Shiite lawmaker Hakim al-Zamili, a member of parliament's security and defense committee. He said weaknesses in Iraq's ability to gather intelligence about terror plots, or stop them despite security checkpoints has shown how toothless the government is in protecting its people.
Al-Zamili also raised the specter of al-Qaida infiltrating security forces. If these gaps are not closed quickly, he said, "the attacks and explosions will continue and al-Qaida will be stronger."
In one brazen assault on Monday, three carloads of gunmen pulled up at an Iraqi army base early Monday near the northeastern town of Udaim and opened fire, killing 13 soldiers before escaping, two senior police officials said.
The deadliest attack, however, took place just north of Baghdad in the town of Taji, where a double bombing killed at least 41 people. The blasts were timed to hit as police rushed to help victims from a series of five explosions minutes earlier.
Monday's violence bore most of the hallmarks of al-Qaida: the bombings and shootings all took place within a few hours of each other and struck mostly at security forces and government offices -- favorite targets of the predominantly Sunni militants. And most of it happened in the capital and in northern areas the terror group used to control and where they now stand the best chance of regaining a foothold.
More than 200 people also were wounded in the onslaught Monday, Iraq's bloodiest day since a string of nationwide attacks on May 10, 2010, killed at least 119 people. Spokesmen for Iraq's government and Shiite Prime Minister Nouri al-Maliki could not be immediately reached for comment.
Iraq's Interior Ministry, which oversees the country's security, condemned the attacks, calling them a "flagrant violation" of the ongoing Muslim holy month of Ramadan. It said security officials now planned to devise a new strategy to protect the public, but said complaints about the security gaps were "not useful."
For years, al-Qaida in Iraq has been seeking to re-assert its might, although U.S. and Iraqi officials insist it is nowhere as strong as it was when the nation came to the brink of civil war between 2006 and 2008.
The militant group made a series of missteps shortly afterward -- targeting civilians, imposing overly strict Islamic discipline, alienating tribal leaders -- that undercut its support in Iraq's Sunni communities and helped lead to the widespread defection of fighters to groups allied with the U.S. The flow of funding, arms and fighters slowed to a trickle, and al-Qaida in Iraq since has struggled, but failed, to command much power.
But the militant group's local wing -- known as the Islamic State of Iraq -- is now seizing on the vacuum left by the Americans and Baghdad's fragmented government.
Baghdad political analyst Hadi Jalo said al-Qaida in Iraq, as a Sunni group, feels emboldened by the success of the Sunni-dominated uprising in neighboring Syria against Damascus' Alawite rulers. The Alawites are an offshoot of Shiite Islam.
"It is leading a sectarian war and Iraq is part of its war and ideology in this region," Jalo said.
In a statement issued Saturday, the leader of al-Qaida's affiliate in Iraq warned that the militant network is returning to strongholds from which it was driven from while the American military was here.
"The majority of the Sunnis in Iraq support al-Qaida and are waiting for its return," Islamic State of Iraq leader Abu Bakr al-Baghdadi said in the statement that was posted on a militant website.
The local wing of al-Qaida, known as the Islamic State of Iraq, has long been at odds with al-Qaida's central leadership. The global network's current leader, Ayman al-Zawahri, has in the past criticized Iraq's movement for targeting civilians. But earlier this year, al-Zawahri softened his stance, and included ISI militants in a network plea for fighters to join the Syrian uprising.
Previous al-Qaida offensives have failed to push the country into civil war, largely because Shiite militias in recent years have refused to be lured into the kind of tit-for-tat killings that marked Iraq's descent six years ago. Additionally, for all its weaknesses, the Iraqi government now holds more authority than it did during those dark years, and, by and large, citizens have no desire to return down that path.
Still, the militant group appears to be banking on Iraq's fragility in its campaign to throw it into permanent chaos. Sectarian tensions have risen due to a political crisis stemming from terror charges the Shiite-led government has filed against one of the country's vice presidents, who is one of Iraq's top Sunni officials. He says they are politically inspired.
Mohammed Munim, 35, was working at an Interior Ministry office that issues government ID cards to residents in Baghdad's Shiite Sadr City neighborhood when a car exploded outside, killing 16 people.
"It was a thunderous explosion," Munim said from his bed in the emergency room at Sadr City hospital. He was hit by shrapnel in his neck and back. "The only thing I remember was the smoke and fire, which was everywhere."
Most of the cities and towns pounded by bombs Monday are located in Sunni-dominated areas that nonetheless include sizable pockets of ethnically- and religiously-mixed populations.
Attacks struck the Baghdad suburb of Hussainiya, northeastern Diyala province, five towns around Kirkuk and in the oil-rich city itself as well as the northern city of Mosul -- a former al-Qaida stronghold, police said.
Only one of Monday's attacks occurred in undisputed Shiite territory: a bomb in the southern town of Diwaniyah that police said killed three people and wounded 25.
All of the casualties were confirmed by police and health officials who spoke on condition of anonymity because they were not authorized to release the information.
Associated Press Writer Lara Jakes in Baghdad and Yahya Barzanji in Sulaimaniyah, Iraq, contributed to this report.


The launch marks the start of the X-37 B programme's second space mission. The OTV was designed to examine how highly complex technologies will perform in space before they are made operational. OTV was the first vehicle since NASA's shuttle orbiter capable of returning experiments to Earth for further inspection and analysis. The air force's other X-37B plane, known as OTV-1, returned to Earth in December 2010 after a similarly mysterious seven-month maiden mission. This is a classified mission.


The consensus of those who follow these elections most closely is that the Democrats will win. The most recent evidence comes from the ultra-narrow victory of Republican State Sen. Troy Balderson in the special election for Ohio's 12th Congressional District.
Balderson beat Democrat Danny O'Connor 50 to 49 percent, only a 1 percent margin, in a district that gave President Trump an 11 percent margin in 2016 and Mitt Romney a 10 percent margin in 2012.
Ohio 12 is one of those hybrid districts, about half suburban and half urban, about half rural and half small-town. It includes part of the Ohio State University campus and affluent northern suburbs of Columbus, the Midwest's fastest-growing major metro area.
Romney carried both suburbs and small counties by modest margins. Trump got whacked in the affluent suburbs but won the small counties by overwhelming margins. Recently, and even more in early voting, Democrat O'Connor carried upscale suburban precincts by robust 2-1 margins. Republican Balderson ran well but not as far ahead as Trump, amid lower turnout in the small counties.
Another way to put it: Republicans get the worst showings of both of their last two nominees, losing even further ground among white college graduates while failing to duplicate Trump's gains among whites non-college graduates.
That pattern was discernible in earlier special elections and makes it easy to see how Democrats could win a House majority. It's widely attributed to Trump's combative and provocative style.
There's something to that, of course, but not everything. The voter shifts from Romney 2012 to Trump 2016 were actually small by historic standards, and the steadiness of Republican and Democratic percentages in the two-plus decades since 1994 have been historically small, with a steady increase in straight-ticket voting till 2016.
What we've also seen in congressional elections since the middle 1990s is resistance to one-party control. With close presidential elections, only a few voters need defect in the off year to produce this result, and except for the contests just after 9/11, they have.
Former President Bill Clinton faced Republican Houses and Senates for six of his eight years in office. Then-President George W. Bush's Republicans gained seats in 2002, but he faced a Democratic House for two years and a Democratic Senate for three and a half. Former President Barack Obama faced a Republican House for six of eight years and a Republican Senate for two.
You can ascribe the losses of each president's party as the predictable result of some combination of extremist overreach, legislative fecklessness, personal scandals and suspicion of insiders. But for one reason or another, they keep happening and could again this year, when Republicans could lose their House majority and might conceivably, despite their advantage in seats, lose the Senate, too.
But there's reason to be cautious about predictions. Republicans' big gains weren't visible at this point in the 1994 cycle (I wrote the first article predicting they might win a majority, in July), nor were Democrats' big gains in 2006 or Republicans' sweep of Senate seats in 2014.
Nor are area polls this far out always a reliable guide to November. Except in early June, Democrats have had a 6 to 8 percent lead all year in the RealClearPolitics generic congressional vote poll average. But it's suddenly down to the lower end of that range, numbers that could produce a Republican majority in the House (because Democratic voters are demographically clustered in relatively few districts).
Does that signal a genuine shift in sentiment, or is it just statistical noise? No one knows. Corporate America seems to be joining with affluent Trump haters to give Democrats a significant money edge in key races. But then, smart money was overwhelmingly on the side of Hillary Clinton two years ago.
In that race, like the House races this year, Democrats started off ahead in turnout, but Republicans managed to squeak out just enough votes in the right places to win — as they did in Ohio 12 this week, and may or may not in November.


Magic has a thick, heavy rear to balance out his deep wide chest . When you look at "Magic" you can see he has balance and great proportion.
Magic is wonderful with our calves and all the bull calves live with Magic after weaning. Like a long time breeder told me "The best way to make a calm, respectful bull calf, is to raise him with a calm, respectful Bull". Magic gently teaches the calves there is a power greater than they are, and that calm and quiet is good.
Regardless of whether Magic is stacked like a show dog,( above at 22 mo. old, after finishing breeding our herd) or standing lazy in the pasture or grazing, He exhibits the proud traits of the Scottish Highland Cattle Standard. Magic is a calm bull with Correct and Excellent Level and Straight top line, strong Muscular neck, Low Wide horn set, Broad short head, Bushy Forelock down to his muzzle, And a Thick Slightly Wavy coat. Magic was a planned breeding of ours for the purpose of spreading the incredible Maternal traits of his dams line and superior maternal traits of his sire throughout our herd. We have owned 3 generations of Magic's Dam's line that have tight udders, small teats, have 50-60 pound calves unaided, and their calves nurse unassisted almost immediately. Magic has been producing beautiful structurally correct Black and red calves for us. We Just love his calves!
Haydn was a gentle bull that added incredible spring of rib and depth to his calves. As you can see in the picture with Haydn sharing his feed with the tallest cow in our herd, Haydn was only a couple inches taller, but was twice as wide and one and a half times as deep as Flicka's 1100+ pound frame. Haydn's Forelock, horns, Huge head, and large bone also passed on to his calves along with that wonderful Level Straight Top Line!


text:
Q: Why does read's timeout break my console? I have a script that is causing an issue, I've boiled it down to this;
#/bin/bash
read -t 1 -p 'Wanna continue?'
less +F readTimeout.sh
echo 'Wont get printed'

The original script operated by prompting the user to continue, but after waiting for five seconds (in this case, one) it will continue on its own.
It then proceeds to tail from a log file (in this case, itself, for demonstrative purposes).
Then it should execute the rest of the commands after the user closes less.
Well, when less is in tail mode, you need to hit ctrl+c to stop it from following the file (then you can scroll/search on what's in less so far, or shift+f to follow again, or Q to quit).
The problem for this script is, when you ^C it kills less, takes you back to prompt (i.e. the rest of the commands aren't ran) and stops anything you type from being echoed (if you hit enter your commands are actually being written to the console, though)!
Without the -t switch on read (or if you respond before the timeout) it works fine.
Any ideas why this happens &/or how to combat this? So far I've resorted to just forcing the user to respond to the prompt (i.e. removing the timeout flag from read)
P.S.
This is terminal emulator independent (tested konsole and xterm).
And I've tried placing stty sane after the read line in case it would fix it.

redpajama_set_name: RedPajamaStackExchange


TBQ'S Book Palace: [ARC Review]: "Inescapable"
Kai doesn't like living in Mercy, but because that's where his business is located, he can't completely run away from the small town. He'd prefer the anonymity of a big city to the gossip-heavy curiosity of Mercy. Especially when he and Flick decide to hook up. It's supposed to be just the one night, as he's heading out of town for a few months on a job. When one of his best friends (and business partner) is called away to handle a family emergency, Kai's plans of escaping the awkward morning after is ruined. The town's all abuzz about their tryst, and worse the temptation to continue it is far too strong for either of them to resist.
I have to say, I did like this book. Quite a bit actually. There's not really anything that stands out as "bad" about Inescapable and overall I enjoyed quite a bit of it. That being said, I was easily able to put the book down and go about my day, and it took me 4 days to finish this 200-page book. For me, that's slow, and it does say something about my reading experience with this one. However, I'm not sure if it was due to my reading mood at the time or if there was something in the writing style that just didn't completely pull me in.
Mercy has all the makings for a nice small-town – nosy neighbors, somewhat quirky characters here and there, a bakery (being run by Flick, of course) and so on. I liked Mercy enough that I'd revisit it.
On his knees now, Kai rested his forehead on her stomach, his hands holding her sides.
Flick pushed a hand into his hair. "Why are you stopping?"
"I'm taking a break, trying to slow things down."
"Don't bother on my account," Flick told him. "Throw a condom on and slide on home."
Kai looked up at her, his expression mischievous. "Not a chance in hell. This first time I want to watch you fall apart. I want to see you wild and crazy. I want to see if you're as beautiful coming as you are every other second."
"You're looking at me," she said softly, feeling self-conscious.
"Because you are definitely as beautiful, possibly more so, when you come."
"I'd sit down quickly unless you want to show the people coming up the path exactly how long six inches is."
"Seven." Kai dropped to the rock next to her and lifted his shoulders at her rolling eyes. "What?"
"You measured it?"Flick hissed as the approaching voices got louder.
Flick gripped the bridge of her nose and shook her head. "Men are weird."
Again, I don't really have anything to complain about as far as the story goes. Except, perhaps, to mention that Gina (Flick's aunt) annoyed the hell out of me, as she stubbornly refused to tell her "secret" to her own daughter, instead putting Flick in the horrible position of trying to handle it while lying to her cousin (and best friend), all because Gina made her promise not to tell.
All in all, I liked Inescapable, and nearly gave it 4 stars. But because it didn't hold my attention as thoroughly as I would have liked – and I still can't pinpoint why – I'm lowering it down to a still very respectable 3 1/2. I'm curious enough about some of the other characters – Kai's business partners, Axl and Sawyer in particular – that I'll keep me eye out for the rest of the series. I'll also recommend this book to anyone looking for a new small town to enjoy.
*Note: The quotes used belong to Joss Wood; TBQ's Book Palace does not claim them. Any mistakes or typos in the quotes are my own fault.
Have you had this happen before? Where there was nothing technically wrong with the book, and you liked it, but it just didn't have your attention 100%?


text:
LA Personal Injury Attorneys
Brain Injury Accidents
e-Scooter Accidents
Marc Lazarus
Attorney in Family, Employment Law & Car Accident
by LosAngelesAutoCarAccidentJuly 10, 20200 comments
For more than twelve years prior to becoming a plaintiff personal injury attorney, Mr. Lazarus worked as a paralegal with several plaintiff personal injury law firms, and he has extensive experience in working with individuals who have been injured in automobile collisions, motorcycle collisions, bus accidents, slip and falls, trip and falls, falls from ladders, product-related injuries, medical malpractice claims, and work-related claims.
He specializes in cases resulting in traumatic brain injuries, spinal cord injuries, shoulder injuries, wrist and hand injuries, knee injuries, and ankle injuries. Mr. Lazarus' knowledge in the area of medicine has served to greatly improve the value of his clients' cases throughout his career.
Consulting 68%
Car Accident Law 79%
Personal Injury Law 85%
Membership and Activities
Mr. Lazarus has served as lead counsel on hundreds of litigated actions in which he has taken and/or defended over a thousand depositions of parties, witnesses, and experts. He has also represented clients as lead counsel on approximately five bench trials, approximately twenty jury trials, approximately one hundred binding arbitrations, more than a hundred judicial arbitrations, and over two hundred mediations, mandatory settlement conferences, and voluntary settlement conferences.
Marc Lazarus obtained his Bachelor of Arts degree in English Literature with an emphasis in Technical Writing from the California State University at Northridge in 1992. He obtained his Juris Doctorate degree from Chapman University School of Law as a member of its first graduating class in 1998 and served as an editor of the law journal.
Your Tel (required)
LA-Personal Injury Attorneys
Represents clients throughout Los Angeles County, California.
355 S Grand Ave,
Email: info@la-personalinjuryattorneys.com
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At Grace, we've embraced the Rotation Model of Sunday morning education. We're having fun! We cover less of the Bible, but in greater depth. The leadership team chooses stories from scripture. On Sunday mornings, we spend several weeks dwelling within a story—through drama, art, story-telling, cooking, game-playing. The classes visit a different room each Sunday morning: the drama room, the movement room, the craft room, and the story-telling room. Each unit begins and ends with a celebration. This plan enables us to use the full range of diverse gifts of the congregation. It also allows for different learning styles, with different "rooms" engaging children in different ways.


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Alan W. Tompkins
Alan Tompkins is the founder and president of the Foundation. A native of western Kentucky, he's an avid bluegrass fan and an established banjo and acoustic bass player. His solo album, No Part of Nothin', was released in 2012. His love of music began at an early age, and he played southern gospel and country music extensively before and during his college years. With Gerald Jones, Alan co-founded the Frisco Bluegrass Festival (in Frisco, Texas; 2006-07) and Acoustic Music Camp, an annual instructional institute for traditional and acoustic musicians. In 2010, together with the City of Farmers Branch, Texas, Alan created the Bloomin' Bluegrass Festival & Chili Cook-Off, the largest bluegrass event in north Texas, which was nominated for the International Bluegrass Music Association's (IBMA) Bluegrass Event of the Year Award in 2014, 2017, 2019, and 2020.
Alan holds a bachelor's degree in bluegrass music from Glenville State College as well as an associate degree in bluegrass and certificate in audio recording from the Kentucky School of Bluegrass & Traditional Music. He is a graduate of the IBMA Leadership Bluegrass class of 2009, served on the Leadership Bluegrass Planning Committee from 2010-2018, and served as Committee Chair from 2011-2014. Alan received the IBMA Momentum Award for Industry Involvement in 2015, is a four-time nominee for IBMA's Bluegrass Broadcaster of the Year Award, and served on the IBMA board of directors from 2015-2019. He presently serves on the board of directors of the IBMA Foundation and the Professional Advisory Committee of the Kentucky School of Bluegrass & Traditional Music. For more, see AlanTompkins.com.
Alan is also Vice President & General Counsel of Unity Hunt, Inc. in Dallas where he manages legal matters for the Lamar Hunt family and affiliated entities. He moved to Texas from Kentucky in 1983 to earn an MBA from SMU and went on to become licensed as both an attorney and CPA in Texas. He has served on the boards of several charitable organizations including the National Soccer Hall of Fame Museum, AFI-Dallas International Film Festival, USA Film Festival, FC Dallas Foundation, Pegasus Theatre, Dallas Christian Leadership, and For The Love Of The Lake Foundation. Alan is a former chair of the State Bar of Texas Entertainment & Sports Law Section.
The Bluegrass Heritage Foundation is a non-profit organization, run by volunteers,
promoting bluegrass music in Texas. While it's free to get in the door to many of our events,
keeping the doors open isn't free. All contributions are greatly appreciated.
Click the donate button to donate online.
YOUR INQUIRIES AND DONATIONS ARE WELCOMED!
© 2021 Bluegrass Heritage Foundation P. O. Box 25032, Dallas, Texas 75225 (972) 306-0321
Bluegrass Heritage Foundation ("BHF") and BHF instrument designs, Making Bluegrass Happen, Play It Forward!,
Bluegrass Star Award, Bluegrass Heritage Festival, Lone Star Fest, and Lone Star Fest banner designs
are trademarks of Bluegrass Heritage Foundation, Reg. U.S. Pat. & Tm. Office.


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The CPS' decision on election expenses shows that big money, not people power, rules our politics
The CPS has announced that no charges will be brought against Conservative party candidates or agents relating to election expenses during the 2015 General Election campaign. The CPS accepted that local returns were inaccurate due to the omission of candidate spending on the 'Battle Bus' but concluded there was insufficient evidence to prove that persons involved acted dishonestly. Allegations in relation to South Thanet remain under consideration.
In contrast to the view taken by the CPS the Electoral Commission noted in their report on their investigation into Conservative electoral expenses that the spending in relation to the battle bus was targeted at marginal seats. They concluded that candidate campaigning by battle bus activists was foreseeable and that evidence from social media demonstrates that it did take place across a number of constituencies. Furthermore the report stated that "there was a realistic prospect that this enabled its candidates to gain a financial advantage over opponents."
Responding to the CPS' decision not to take any action on allegations of election expenses fraud, Unlock Democracy's Director Alexandra Runswick said:
"As with the expenses scandal voters are left feeling that there is one rule for politicians and another for the rest of us. This case raises serious questions about whether electoral law can stand up to the influence of big money dominating our politics.
Free and fair elections underpin our democracy, and when there is the perception that the outcome is determined by who can spend the most money, public trust in our political system is critically undermined.
Overall, there have been paltry repercussions for those who have flagrantly disregarded the law. Earlier this year the Electoral Commission handed out the largest fine in its history to the Conservatives for violating election expenses rules, but this fine paled in comparison to the millions they receive in donations and spend in elections. It is deeply concerning that political parties may see breaking the law as a price worth paying to win an election.
"We also urge those in affected constituencies to use their victim's' right to review to call on the CPS to reconsider its decision to drop some of its cases."
To organise an extended interview or comment with Unlock Democracy's Director, please contact Alexandra Runswick on 07739586666 or alex.runswick@unlockdemocracy.org.uk.
Samuel Ellis May 10, 2017 Comment
Fraud will flourish under the Conservative's plans for the SFO
Samuel Ellis May 23, 2017
"Toothless" revolving doors watchdog needs greater powers
Samuel Ellis April 24, 2017 Revolving Doors


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Tasmosalpingus promiscuus is een keversoort uit de familie Tasmosalpingidae. De wetenschappelijke naam van de soort is voor het eerst geldig gepubliceerd in 1919 door Lea.

Tasmosalpingidae


- Interconnection of different databases where information is stored.
- Development of new efficient methods of digitalization .
The need of unified access and commercial exploitation is an imperative for our country, given the expected enormous purchasing demand for cultural digital content before, during and after the 2004 Olympic Games.
Metadata and cultural content description . In order to make possible the interconnection of different remote databases and the unified access to the content, the use of common description of data (metadata) is required. Generally, the XML description language (Extensible Markup Language) will be used from the content providers (museums etc).
Ontologies for cultural heritage content . Ontologies provide the structure for efficient description of objects, ideas, processes as well as relations between them. In this project ontologies will be developed that will allow the description and organisation of content of cultural heritage based on metadata, and also the search based on the content. The ontology system that will be developed will be based on the philosophy of Topic Maps (in HTM form).


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Online Books by
H. Grattan Guinness
(Guinness, H. Grattan (Henry Grattan), 1835-1910)
A Wikipedia article about this author is available.
Guinness, H. Grattan (Henry Grattan), 1835-1910, contrib.: Bokwala: The Story of a Congo Victim (London: Religious Tract Society, 1910), by A Congo Resident (multiple formats at archive.org)
Guinness, H. Grattan (Henry Grattan), 1835-1910, contrib.: For Christ and Cuzco: A Memorial of W.H. Newell, Missionary to Cuzco, Peru (London: Regions Beyond Missionary Union, ca. 1905), by Martha Newell (page images at HathiTrust; US access only)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Romanism and the Reformation, From the Standpoint of Prophecy (Toronto: S. R. Briggs, ca. 1887) (multiple formats at archive.org)
Additional books from the extended shelves:
Guinness, H. Grattan (Henry Grattan), 1835-1910: The approaching end of the age viewed in the light of history, prophecy, and science. (London : Hodder and Stoughton, 1880) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: The city of the seven hills. (London, J. Nisbet, [1891]) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Creation centred in Christ, (London, Hodder & Stoughton, 1896) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: The divine programme of the world's history / (London ; Hodder and Stoughton, 1888), also by Mrs. H. Grattan Guinness (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: The duty of Christians in the present crisis : a letter to a Christian brother / (Philadelphia : Collins, printer, 1861) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Grammar of the Congo language, : as spoken in the Cataract region below Stanley Pool. (London : Hodder and Stoughton, 27, Paternoster Row, 1882) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Grammar of the Congo language as spoken two hundred years ago, (London, Hodder & Stoughton, [1882]), also by Giacinto Brusciotto and James Mew (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910, trans.: Leta yantete ya Yoani. (Philadelphia, American Baptist Publication Society, [1889]) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Light for the last days : a study historic and prophetic / (London : Hodder and Stoughton, 1888), also by Mrs. H. Grattan Guinness (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: The new world of Central Africa. With a history of the first Christian mission on the Congo. (London, Hodder and Stoughton, 1890) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: The Revival in Ireland : letters from ministers and medical men in Ulster on the revival of religion in the north of Ireland addressed to the Rev. H. Grattan Guinness. (Philadelphia : W.S. & A. Martien, 1860) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Romanism and the reformation; from the standpoint of prophecy, (New York, A.C. Armstrong, [1887]) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Romanism and the reformation from the standpoint of prophecy ... (Boston, Mass., 1893) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Romanism and the reformation : from the standpoint of prophecy / (London : Hodder and Stoughton, 1887) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: Romanism and the reformation from the standpoint of prophecy [electronic resource] / (Toronto : S.R. Briggs, [1887?]) (page images at HathiTrust)
Guinness, H. Grattan (Henry Grattan), 1835-1910: The second advent: will it be before the millennium? Affirmative, (New York, J. Pott and Co., [1887]), also by David Brown, Thomas Charles Edwards, Joseph Agar Beet, Frédéric Louis Godet, Mrs. H. Grattan Guinness, and A. R. Fausset (page images at HathiTrust)
See also what's at your library, or elsewhere.


Food safety is paramount to our business practices. It is a total supply chain responsibility with strict requirements, guidelines and standards for our industry partners. Food safety touches all components and ingredients in all products sold.
We know and understand the concerns of customers. Our commitment to providing consumers with high quality, safe food extends to holding processors, handlers and shippers to those rigorous requirements. From traceability and documentation to cold chain and clear communication, our dedication to food safety runs deep.
We maintain established, trusted relationships with major growers and shippers, and as one of the largest and most respected wholesale fruit and vegetable distributors in California, General Produce has proven access to critical supply — delivering consistent quality and service to you.
We set and maintain high standards which continue to evolve with improved industry guidelines, procedures and protocols. General Produce values these established, stringent food safety policies with a company culture that elevates food safety to top priority.


You know those Chevy commercials with Howie Long? The ones that take place in the dealership pitting Howie against a small mob referred to in the third person as "Everybody"? Well in those commercials, there seems to be a key person missing – the dealer.
And with good reason. The dealer, along with the general manager and the dealership are irrelevant in my opinion. How irrelevant? Enough that I've bypassed all dealership interaction through vehicles I've owned over the past 5 years.
Yet sometimes, a dealer may get a product so tempting to check out, that you can't help but pull into the lot while their open.
This was my experience on Thursday, when a 2010 Camaro LT with the RS package caught my eye. Pressing on the break, I turned in and parked my car in plain view of the salesman. Now let me preface, I drive a pretty nice sedan that returns the favor when I turn it on (car buffs will get the clues). I'm in no way looking to trade, sell, or give away my vehicle. I was curious however as to how the new Camaro looked in real life because given the extreme value of the car ($22,000 for 300 horsepower and 29 mpg!!!) I couldn't help but stop and ponder what I'd buy next when my lease is up in a year.
So of course, like clockwork, the salesman asks if I wanted to see anything. I kindly explained I just wanted to see the new Camaro. Checking out my current car through the window he slyly suggests he could buy me out of my lease and put me in a new Camaro for the same price I'm paying now.
Only one issue. He's talking to me about car payments instead of price of the car.
Now again let me pause for a moment. For those who know me, I'm a car geek. I know all the marketing speak, all the upsell touchpoints, and all the costs associated with them (30 years of Car & Driver magazine will do that to you.). So just eyeballing the Camaro on their lot, I knew that a loaded to the brim V6 with the RS package (20″ rims, halo light effects) would come in around 28 with leather.
I lol'd. Correction, I LMAO'd.
I explained that there was no way I was going to pay a penny over 27. In fact when I buy a Camaro, or a Mustang, or a Charger, I fully expect to pay $500 below invoice. If not they don't get my business.
So the salesman explains to me in calm slow speak – he is only getting 12 a year in his dealership. The "market adjustment" as he referred to it, was meant to keep demand high to balance his lack of supply.
Easily this was the most asanine argument I've heard.
I explained that I was not willing to pay $6000 over MSRP sticker for the honor of driving a Camaro. If there was a level of exclusivity, maybe. If this was some limited edition variant, say a Z28, then maybe I could see a premium to get my hands on one, but this one I called like I saw it.
And in trimes of recessionary pain, greed is not good my friends. I asked the salesman how many Camaros he'd be receiving again. He said 12. I retorted that in a year I'll have 12 to choose from since he won't move a single one off his lot with that mark up.
I'm not the only one who experienced this though. A number of bloggers walked into their Chevy dealerships, probably for the first time in years, only to be slapped in the face with an on average $5000 price tag over MSRP.
1. Customers driving around in their cars vs. keeping one on the lot collecting interest.