text:
\section{Introduction}
\label{sec:introduction}

In the past decade, supernova (SN) surveys targeting nearby, luminous galaxies
have been immensely successful since the total local starlight searched is significantly
larger than in untargeted pointings of equal area.
The Palomar Transient Factory
(PTF; \citealt{lkd+09,rkl+09}){\footnote{http://www.astro.caltech.edu/ptf/}}
is a  wide-angle
transient survey that has an ongoing Dynamic Cadence experiment that combines the
advantages of both a targeted and an untargeted survey. This experiment searches
wide-angle pointings of local ($d < 200$\,Mpc) galaxy light
concentrations at a 1-day cadence to a median depth of 21\,mag. The depth, cadence, and
choice of pointings allow us to find transients that are fainter, faster, and rarer than supernovae.
Furthermore, these survey design characteristics facilitate the discovery of
intracluster transients as well as transients in the far-flung outskirts of their host galaxies.

While monitoring supernovae from the targeted Lick Observatory Supernova Search \citep[LOSS;][]{lft+00,flt+01} with the Katzman Automatic Imaging Telescope (KAIT),
\citet{fcs+03} noted that there was a subclass of peculiar Type I supernovae
that appeared to be rich in Calcium at an early stage. \citet{pgm+10} presented
extensive observations of one of these events, SN\,2005E.
In addition to the Calcium-richness, SN\,2005E was subluminous and rapidly evolving. Furthermore,
SN\,2005E was located 23\,kpc away from the nucleus of its host galaxy, with no signs
of underlying star formation to deep limits. The physical origin of SN\,2005E
remains a matter of debate.

Motivated thus, and given that the survey design of PTF allows it be to especially
sensitive to find and follow-up such events, we searched the PTF discovery stream.
We find three transients -- PTF\,09dav, PTF\,10iuv and PTF\,11bij -- that share five
distinguishing characteristics with SN\,2005E: (i) peak luminosity intermediate
between that of novae and supernovae, (ii) faster photometric evolution (rise and decline)
than supernovae, (iii) photospheric velocities comparable to supernovae,
(iv) early evolution to the nebular phase, and (v) nebular spectra dominated by
Calcium emission. These five explosion properties define a distinct class of
``Calcium-rich gap'' transients. (We closely scrutinize the choice of this
set of explosion characteristics in \S7.1.)

Remarkably, these three PTF transients were also found in remote locations, more than 30\,kpc
away from the nuclei of their host galaxies. Location was not used as a selection criterion; yet,
we do not see any other PTF supernovae thus far that display the five explosion
characteristics listed above (see \S7.2 for details). Therefore, in \S2 we take a
closer look at the locations of these three transients in the context of locations
of other PTF supernovae.

The rest of the paper is organized as follows.  We present observations of
PTF\,09dav, PTF\,10iuv and PTF\,11bij in \S\ref{sec:09dav}, \S\ref{sec:10iuv}
and \S\ref{sec:11bij} respectively. We show the available data on
the six archival candidates from the past decade in \S\ref{sec:loss}.
We analyze the properties of the combined sample of well-observed
transients in this class in \S\ref{sec:analysis}. We discuss whether this
class has an underlying physical commonality and speculate on its origin
in \S\ref{sec:discussion}, and conclude in \S\ref{sec:conclusion}.

\begin{figure*}[!hbt]
   \centering
   \includegraphics[width=3.5in]{snoffsetsv3.ps}\includegraphics[width=3.5in]{hostmags_offsetv3.ps}
   \caption[Offset Distribution of PTF Supernovae]{\small {\it Left:} Histogram of projected offsets from the host-galaxy nucleus for
the first 520 transients discovered and spectroscopically classified by the Palomar Transient Factory with $z\,<\,$0.1.
Stars denote the locations of PTF\,11bij, PTF\,10iuv and PTF\,09dav.
{\it Right:} Upper limits for an underlying dwarf host ($M_{R}$) for transients with offset greater than 20\,kpc.
}
\label{fig:snoffsets}
\end{figure*}

\section{Offset Distribution of PTF Supernovae}
\label{sec:offsets}
The location of a transient explosion has long been exploited as a clue
to determining its nature. It has been suggested that the classical nova population
is bimodal, with some dependence on whether the nova is located in the Galactic disk or bulge \citep{sdh+11}.
Several studies of supernova host-galaxy properties as well as the site
of the supernova  within the host galaxy have been undertaken
\citep{h01,v97,psb+08,hmp+09,bp09,aj09}.
Subluminous Type Ia supernovae (SN\,Ia) are found preferentially in old environments \citep{h01}
(for a review of spectroscopic classification of supernovae, see \citealt{f97}).
Core-collapse supernovae (SN\,CC) and more luminous SN\,Ia are
preferentially found in late-type galaxies \citep{hps+96}. Type Ic supernovae are not found in dwarfs
\citep{agk+10} and SN\,Ibc are more centrally concentrated than SN\,II \citep{aj09}.
About 15\% of the stellar mass is expected to be in the intergalactic medium in clusters, and a
handful of intracluster supernovae have been discovered \citep{gmg+03,sgb+11}. At higher energies, gamma-ray burst
offsets from host galaxies offered a clue to their progenitors \citep{fls+06,bpp+06}.

In the first two years, PTF
discovered and spectroscopically confirmed over 1300 extragalactic transients. Here, we limit the study
of the offset distribution of PTF supernovae to the first 520 transients which were nearby, with redshift
$z < $0.1. We compute precise projected offsets from the host galaxies for each transient, and
the resulting histogram is shown in Figure~\ref{fig:snoffsets}. The redshift of the host galaxy is
consistent with the redshift of the transient. Note that the offset is projected and hence, only a
lower limit.

We split the population into core-collapse supernovae and thermonuclear supernovae.
We find that the core-collapse and thermonuclear populations
show similar distributions out to a projected offset from the host nucleus
of $\approx$\,9\,kpc suggesting that the average distribution is
proportional to starlight. Beyond 9\,kpc, the thermonuclear population shows a heavily extended
tail suggesting a second parameter governing their rate or perhaps even two progenitor populations
\citep{mdp06}. A cautionary note here is that although this sample is relatively more homogeneous in that it is drawn
from a single survey with extensive follow-up observations, it is not spared the vagaries of
incompleteness due to weather and follow-up bias.

Next, we take a closer look at the population with offsets larger than 20\,kpc.
We co-add available pre-explosion data to derive limiting magnitudes on a
satellite host galaxy at the location of the supernova (see Figure~\ref{fig:snoffsets}, right panel).
The redshift limit constrains the luminosity of underlying host galaxies based on our pre-explosion
co-adds to at least $-$16\,mag.

Focusing on the dozen transients with offsets larger than 30\,kpc, we find
9 SN\,Ia, 0 SN\,CC, and 3 peculiar transients. Five SN\,Ia -- PTF\,09cex,
PTF\,10fjg, PTF\,10xua, PTF\,10xgb, and PTF\,10xgc -- with offsets of
30--36\,kpc have spectroscopically confirmed host redshifts. Three SN\,Ia
-- PTF\,10qnk (101\,kpc), PTF\,10qht (79\,kpc), and PTF\,10qyx (48\,kpc) -- are
possibly intracluster supernovae (Horesh et al., in prep.).
The furthest offset SN\,Ia, PTF10ops (140\,kpc), has peculiar properties
and is the subject of another paper \citep{mst+11}.

The three peculiar transients are the topic of this paper.
PTF\,09dav is offset from a spiral host by 40\,kpc;
PTF\,10iuv is in a galaxy cluster containing early and late-type galaxies,
with the closest being an elliptical galaxy 37\,kpc away; and
PTF\,11bij is in a cluster of early-type galaxies, with the closest
being 33\,kpc away. Note that in units of host-galaxy Petrosian radii,
these offsets correspond to 4.9, 5.9, and 3.8 radii, respectively.
We cannot rule out the possibility of an underlying low-luminosity dwarf host; we can only constrain dwarfs to a limiting $R$-band absolute magnitude of
$-$9.8, $-$12.1, and $-$12.4 for PTF\,09dav, PTF\,10iuv, and PTF\,11bij, respectively.
Finding dwarf satellites at a separation of 40\,kpc would not be unusual
(cf., Andromeda's $-$8.5\,mag satellite at 350\,kpc; \citealt{sbm11}).

\section{Observations: PTF\,09dav}
\label{sec:09dav}
We presented the discovery, light curve, and photospheric
spectra of PTF\,09dav in a previous paper \citep{skn+11}.
We found that PTF\,09dav had a low peak absolute magnitude of $M_{R}\,\approx\,-$16.3
and a short rise-time of 12\,days relative to SN\,Ia (which peak at $-$19\,mag with
a rise-time of 17.5\,days). We also found that the photospheric
spectra resembled those of SN\,1991bg-like \citep{frb+92} subluminous SN\,Ia but with very unusual strong lines of
\ion{Sc}{2}, \ion{Mg}{1} and possibly \ion{Sr}{2}. Photospheric velocities were $\approx\,$6000
km\,s$^{-1}$.
Here, we present late-time imaging and nebular spectroscopy of PTF09dav.

\begin{figure*}[!hbt]
\begin{center}
\includegraphics[width=7.5in]{mosaic2.ps}
\begin{scriptsize}
\caption[Outskirts location of PTF\,09dav, PTF\,10iuv and PTF\,11bij]{\small {\it Left:}
PTF\,09dav is offset from its late-type host (circled) by 40\,kpc. Note that the galaxy
on the western edge is unrelated as it is at a different redshift.
 {\it Center:} PTF\,10iuv is offset from a galaxy group (circled) with early-type
and late-type galaxies; the nearest potential host is 37\,kpc away.
{\it Right:} PTF\,11bij is offset from a group of early-type galaxies (circled);
the nearest is 33\,kpc away.
}
\end{scriptsize}
\end{center}
\label{fig:loc}
\end{figure*}

\subsection{Late-Time Imaging}
We undertook deep imaging in the $g$-band and $R$-band filters at the
position of PTF\,09dav with the Low Resolution Imaging Spectrometer
(LRIS; \citealt{occ+95}) on the Keck I telescope on 2010 May 15.603
and July 9.584 (UT dates are used throughout this paper), 9--11 months after explosion.
We registered these images with a Palomar 60-inch (P60) image of PTF\,09dav.
No source is detected to a  3$\sigma$ limiting magnitude of $R = 26.2$\,mag
(Table~\ref{tab:lrislimits}, Figure~\ref{fig:gR09dav}). This constrains
any satellite, dwarf host to be fainter than $M_R = -9.8$\,mag.

We undertook imaging in the $K^{\prime}$ band with Laser Guide Star Adaptive Optics
(LGS-AO; \citealt{wcj+06,vbl+06}) on the Keck II telescope with the Near Infrared Camera 2
(NIRC2). On 2010 June 17.568, we obtained 10 images of 10\,s co-added integrations.
The zeropoint was derived relative to the 2MASS catalog \citep{scs+06}. No source was detected
to a 3$\sigma$ limit of $K^{\prime} = 21.1$\,mag.

\begin{figure}[htbp]
   \centering
   \includegraphics[height=2.7in]{ptf09dav_g.ps}
   \caption[Deep limit on dwarf host for PTF\,09dav]{\small Deep late-time $g$-band imaging
with Keck I/LRIS  showing no host galaxy
at the position of PTF\,09dav brighter than 26\,mag. The registration accuracy is
0.241$\arcsec$. We denote the position of PTF\,09dav with a 5$\sigma$ position error circle.
}
\label{fig:gR09dav}
\end{figure}

\begin{deluxetable*}{llllll
  \tabletypesize{\footnotesize}
  \tablecaption{Late-Time Photometry of PTF\,09dav}
  \tablecolumns{6}
  \tablewidth{0pc}
 \tablehead{\colhead{Date} & \colhead{Phase} & \colhead{Facility} & \colhead{Exposure} & \colhead{Filter} & \colhead{Magnitude}\\
\colhead{(UT 2010)} & \colhead{(day)} & \colhead{} & \colhead{(s)} & \colhead{} & \colhead{}
}
 \startdata
May 15.612 & 279.7 & Keck I/LRIS   & 1230 & $g$ & $>$26.0 \\
May 15.614 & 279.7 & Keck I/LRIS   & 1030 & $R$ & $>$24.8 \\
June 17.568 & 313.7 & Keck II/NIRC2 &  100  & $K^{\prime}$ & $>$21.1           \\
July 9.584 & 334.7 & Keck I/LRIS   & 1450 & $g$ & $>$25.4  \\
July 9.584 & 334.7 & Keck I/LRIS   & 1200 & $R$ & $>$26.2
 \enddata
\label{tab:lrislimits}
\end{deluxetable*}

\subsection{Nebular Spectroscopy}
On 2009 November 11, only three months after maximum light, a spectrum
taken with LRIS on Keck I revealed that PTF\,09dav had become nebular. The
time scale to become nebular was surprising as it was faster
than that of typical supernovae by a factor of a few.
Furthermore, only two emission features are seen -- H$\alpha$ and [Ca~II] $\lambda\lambda$\,7291, 7324). The width,
redshift, and flux of the lines are summarized in Table~\ref{tab:nebular}.
The absence of the Ca~II near-infrared (IR) triplet ($\lambda\lambda$\,8498, 8542, 8662) is indicative
of a low circumstellar density. No H$\alpha$ was seen in the photospheric spectra presented
by \citet{skn+11}. The presence of H$\alpha$ emission is usually
interpreted as the interaction of a massive star wind with the circumstellar
environment.  Neither oxygen (prominent in SN\,CC) nor
iron lines (prominent in SN\,Ia) are seen in the nebular phase.
These characteristics of the nebular spectrum were unprecedented
and no match could be found in supernova libraries.

\begin{figure*}[htbp]
   \centering
   \includegraphics[width=5in]{nebspec.ps}
   \caption[Peculiar Nebular Spectra of PTF\,09dav, PTF\,10iuv, and SN\,2005E]{\small Nebular spectra of PTF\,09dav, PTF\,10iuv, and SN\,2005E. All three are very Calcium-rich.
Also shown for comparison, nebular spectra of a SN\,Ia (SN\,1986G, +257\,day; Asiago Catalog),
a SN\,Ib (SN\,2007C, +165\,day; \citealt{tvb+09}), a SN\,Ic (SN\,2002ap, +249\,day; \citealt{gos+02}) and
a SN\,IIP (SN\,2004et, +454\,day; \citealt{sas+06}). The nebular spectra of SN\,Ia
are dominated by [Fe~II], [Fe~III], and  [Co~III] emission lines. The nebular spectra of
SN\,CC have a much lower ratio of Calcium to Oxygen.
}
\label{fig:nebspec}
\end{figure*}

\section{Observations: PTF\,10iuv}
\label{sec:10iuv}
\subsection{Discovery and Light Curve}
On 2010 May 31.241, PTF discovered a new transient,
PTF\,10iuv, at $\alpha$(J2000) = 17$^h$16$^m$54.27$^s$ and
$\delta$(J2000) = $+31^\circ 33' 51.7''$.
It was initially found at $R = 21.2$\,mag, and we monitored its brightness
with the P60 in the $Bgriz$ filters for three
months \citep{cfm+06}. Late-time photometric observations were taken with the Large Format Camera
(LFC) on the Palomar 200-inch telescope and LRIS on the Keck I telescope.

Data were reduced following standard procedures and aperture photometry was performed.
Photometric calibration was done relative to photometry of field stars from the
Sloan Digital Sky Survey \citep{aaa+09}. A common set of calibration stars was chosen for the
P48, P60, LFC and LRIS data for consistency. Conversion from $ugriz$ to the $B$ band was done
following \citet{jga06}.

The light curve is summarized in Figure~\ref{fig:10iuvlc}.
PTF\,10iuv peaked on June 10 with $R = 19.0$\,mag. It rapidly rose by 3\,mag in 12\,days,
followed by a rapid decline at the rate of 1\,mag in 12\,days for one month. Subsequently, PTF\,10iuv
evolved slowly at the rate of 0.02 mag day$^{-1}$ for three months followed by 0.005 mag day$^{-1}$.
The color was neither extremely red nor blue. It evolved from $g-i \approx 0.4$ near maximum
to $g-i \approx 0.7$ one month later.

\begin{figure}[!htbp]
   \centering
   \includegraphics[width=3.0in]{lczoom.ps}
   \caption[Light Curve of PTF\,10iuv]{\small Light curves of PTF\,10iuv. Note the rapid rise of 3\,mag in 12\,days,
followed by the rapid decline at the rate of 1\,mag in 12\,days.
}
\label{fig:10iuvlc}
\end{figure}

\subsection{Spectroscopy}
On June 7, we obtained a classification spectrum using ISIS on the William Herschel  Telescope (WHT). Subsequently,
we continued to monitor the evolution with the Keck I (+LRIS) and Keck II (+DEIMOS) telescopes
until the spectra became completely nebular (Figure~\ref{fig:spec10iuv}).

The spectra evolved to show prominent Helium features, resembling Type Ib spectra. The Calcium
lines become stronger with time, especially [Ca~II] relative to O~I. We identify major lines
both pre-maximum and post-maximum using SYNOW (Figure~\ref{fig:synow}).

As with PTF\,09dav, the spectrum of PTF\,10iuv became nebular in only 3 months. Both showed
prominent Calcium emission (Table~\ref{tab:nebular}, Figure~\ref{fig:nebspec}). Unlike
PTF\,09dav, PTF10\,iuv showed O~I emission and did not exhibit H$\alpha$ emission in the nebular phase.

\begin{figure}[!htbp]
   \centering
   \includegraphics[width=3.5in]{spec_series.ps}
   \caption[Spectral Evolution of PTF10iuv]{\small Spectral evolution of PTF\,10iuv.
}
\label{fig:spec10iuv}
\end{figure}

\begin{figure}[!htbp]
   \centering
   \includegraphics[width=3.0in]{synowfit_10iuv_20100607.eps} \\
   \includegraphics[width=3.0in]{synowfit_10iuv_20100612.eps}
   \caption[SYNOW fits to PTF10iuv]{\small SYNOW fits to photospheric spectra of PTF\,10iuv.
{\it Top:} SYNOW fit of a pre-maximum spectrum ($T\,\approx\,$8500\,K, $v\,\approx\,$10,000\,km\,s$^{-1}$) with
prominent Magnesium, Silicon and Oxygen lines.
{\it Bottom:} SYNOW fit of post-maximum photospheric spectrum of PTF\,10iuv ($T\,\approx\,$6500\,K, $v\,\approx\,$9000\,km\,s$^{-1}$).
The most prominent features are Helium, Oxygen, Calcium and Titanium.
}
\label{fig:synow}
\end{figure}

\subsection{Radio Observations}
We observed PTF\,10iuv with the Expanded Very Large Array twice, once on
2010 August 25.06 and again on 2011 May 12.20. We observed in the X-band (8.46\,GHz)
and added together two adjacent 128\,MHz subbands with full polarization to maximize continuum
sensitivity. Amplitude and bandpass calibration was achieved using
the archival flux value of J1721+3542. Phase calibration was carried
out every 10\,min by switching between the target field and the
point source J1721+3542. The visibility data were calibrated and imaged
in the {\it AIPS} package following standard practice.

The transient was not detected with a 3$\sigma$ upper limit of 189\,$\mu$Jy during
the first epoch and 96\,$\mu$Jy during the second epoch.
This corresponds to $L_{\nu} < 1.0 \times 10^{27}$\,erg\,s$^{-1}$\,Hz$^{-1}$.

\begin{deluxetable*}{lllllll
  \tabletypesize{\footnotesize}
  \tablecaption{Lines in Nebular Spectra}
  \tablecolumns{7}
  \tablewidth{0pc}
 \tablehead{\colhead{Transient} & \colhead{Ion} & \colhead{Line Center} & \colhead{Shift$^{a}$} & \colhead{Flux} & \colhead{Width$^{b}$} & \colhead{Velocity Width} \\
\colhead{} & \colhead{} & \colhead{\AA\ } & \colhead{km\,s$^{-1}$} & \colhead{erg\,cm$^{-2}$\,s$^{-1}$} & \colhead{\AA\ } & \colhead{km\,s$^{-1}$}
}
 \startdata
SN\,2005E  & O~I       & 6360.6 & $-$1120 & 2.0$\times$10$^{-15}$ & 107.8  & 5110  \\
SN\,2005E  & [Ca~II]   & 7367.0 & $-$17   & 1.5$\times$10$^{-14}$ & 127.6  & 5240  \\
SN\,2005E  & Ca~II     & 8710.4 & 2530    & 2.7$\times$10$^{-14}$ & 299.0  & 10470 \\
PTF\,09dav & H$\alpha$ & 6820.4 & 840     & 7.6$\times$10$^{-17}$ & 23.5   & 1000  \\
PTF\,09dav & [Ca~II]   & 7579.1 & 250     & 2.0$\times$10$^{-15}$ & 166.1  & 6600  \\
PTF\,10iuv & O~I       & 6467.7 & $-$460  & 1.7$\times$10$^{-16}$ & 170.8  & 8090  \\
PTF\,10iuv & [Ca~II]   & 7465.4 & $-$410  & 8.0$\times$10$^{-16}$ & 134.2  & 5510  \\
PTF\,10iuv & Ca~II     & 8827.3 & 2150    & 9.4$\times$10$^{-16}$ & 312.8  & 10950 \\
PTF\,11bij & O~I       & 6531.5 & $-$1010 & 8.6$\times$10$^{-17}$ & 98.8   & 4680  \\
PTF\,11bij & [Ca~II]   & 7573.5 & 406     & 5.8$\times$10$^{-16}$ & 136.9  & 5620  \\
PTF\,11bij & Ca~II     & 8960.0 & 3140    & 1.3$\times$10$^{-15}$ & 257.0  & 9000
 \enddata
\tablecomments{$^{a}$ Shift is computed relative to the velocity of the putative host galaxy.}
\label{tab:nebular}
\end{deluxetable*}

\section{Observations: PTF\,11bij}
\label{sec:11bij}
On 2011 March 13.187, PTF discovered a new transient,
PTF\,11bij, at $\alpha$(J2000) = 12$^h$58$^m$58.39$^s$ and
$\delta$(J2000) = $+37^\circ 23' 12.0''$.
It was initially found at $R = 19.9$\,mag, and we monitored its brightness
with the P60 in the $gri$ filters.
Similar to PTF\,09dav and PTF\,10iuv, the light curve showed a peak luminosity
in the gap between novae and supernovae, and it evolved rapidly (see Figure~\ref{fig:lcall}).

We obtained a Target Of Opportunity spectrum
on 2011 April 3.40 and a nebular spectrum on April 27.40,
both with  LRIS on the Keck I telescope (Figure~\ref{fig:nebspec}).
The spectra were Calcium-rich, similar to PTF\,10iuv and PTF\,09dav,
and the redshift of 0.035 is consistent with a group of early-type galaxies
(the nearest galaxy is offset by 33\,kpc).

\begin{figure*}[!htbp]
   \centering
   \includegraphics[width=5in]{lc_fullsample.ps}
   \caption[Light Curves of Full Sample]{\small Light curves of all five members of the class of
Calcium-rich gap transients. Note the lower peak luminosities and faster evolution relative to normal
supernovae.
}
\label{fig:lcall}
\end{figure*}

\begin{figure*}[!htbp]
   \centering
   \includegraphics[width=5.5in]{CarichKAIT.eps}
   \caption[Finder Charts for KAIT Sample]{\small Locations of Calcium-rich supernovae from the KAIT Lick Observatory
Supernova Search sample. From {\it Top Left} to {\it Bottom Right}: SN\,2000ds, SN\,2003H, SN\,2003dg, SN\,2003dr, SN\,2005E, and SN\,2007ke.
Unfortunately, adequate photometric data are available only for SN\,2005E and SN\,2007ke to confirm
their similarity to PTF\,09dav, PTF\,10iuv, and PTF\,11bij. Note that the locations are atypical:
elliptical host, interacting galaxy pair environment, off the disk of an edge-on galaxy,
large projected offset from isolated host, and galaxy group environment.
}
\label{fig:lossfinders}
\end{figure*}

\section{Observations: Archival Candidates}
\label{sec:loss}
Here, we present archival data on candidate transients from
other surveys noted for their Calcium-rich spectra
\citep{fcs+03}. Specifically, \citet{pgm+10} suggest that
the following six supernovae resemble SN\,2005E:
SN\,2000ds (IAUC\#7507), SN\,2001co (IAUC\#7643),
SN\,2003dg (IAUC\#8113), SN\,2003dr (IAUC\#8117),
SN\,2003H (IAUC\#8045), and SN\,2007ke (CBET\#1084).
SN\,2000ds was discovered by T. Puckett. SN\,2001co, SN\,2003dg, SN\,2003H, and SN\,2007ke were
discovered by LOSS. SN\,2003dr was discovered independently
by both T. Puckett and LOSS.

Here, we review the available data for these supernovae. In Figure~\ref{fig:lossfinders}, we display
the environments of these candidate members of the Calcium-rich class. Next, in Figure~\ref{fig:specloss}, we plot their spectra
(at the latest phase available) and compare them to those of PTF\,10iuv.
The strength of [Ca~II] relative to Oxygen is a distinguishing
spectroscopic feature of this class; it is common to SN\,2000ds, SN\,2003dg, SN\,2003dr,
SN\,2007ke, and SN\,2003H.
The case for SN\,2001co is less clear due to the noisy spectrum and we exclude it from further analysis.

Unfortunately, the photometry is extremely sparse for this sample ---
only one of the five supernovae has more than two points on the light curve.
SN\,2007ke has a peak absolute magnitude of $-$16.3, a rise-time of 15\,days, and a decline
rate of 0.1 mag day$^{-1}$ (Figure~\ref{fig:lcall}). Therefore, SN\,2007ke satisfies all of the
photometric and spectroscopic properties of the class of ``Calcium-rich gap"  transients
as outlined in \S1. Note that the location of SN\,2007ke is ``off-galaxy'' (Figure~\ref{fig:lossfinders},
bottom-right panel). In view of the paucity of photometric data for the other four supernovae,
we do not discuss them further.

\begin{figure}[!htbp]
   \centering
   \includegraphics[width=3.5in]{kait_spec_compare.ps}
   \caption[Spectra of KAIT Sample]{Spectra of the KAIT/LOSS sample of Calcium-rich supernovae compared to PTF\,10iuv.
Except for SN\,2007ke, as the photometry is not available to constrain the maximum-light epoch, the phase is
relative to discovery and not maximum.
}
\label{fig:specloss}
\end{figure}

\section{Analysis}
\label{sec:analysis}

\subsection{The Sample}
To summarize, the five distinguishing characteristics of our
peculiar new class of transients are (i) peak luminosity intermediate between that of
novae and most supernovae, (ii) faster photometric evolution (rise and decline)
than that of normal supernovae, (iii) photospheric velocities comparable to those of normal supernovae,
(iv) early evolution to the nebular phase, and (v) nebular spectra dominated by
Calcium emission.

Based on available observations, the objects that satisfy the defining
characteristics of this class of ``Calcium-rich gap'' transients are
SN\,2005E, SN\,2007ke, PTF\,09dav, PTF\,10iuv, and
PTF\,11bij. Their light curves are shown in Figure~\ref{fig:lcall} and nebular
spectra in Figure~\ref{fig:nebspec}. Observed properties of these events are
summarized in Table~\ref{tab:summary}.

Our choice of these five characteristics is motivated by choosing the maximum
set of characteristics that gives the largest number of related transients.
Evidently, if we add characteristics to this list, the family size becomes smaller
and we may overlook a unifying explanation. If we remove characteristics from
this list, the family becomes larger but we may inadvertently introduce a diversity
of progenitor channels. We discuss examples of each case below.

If we require an additional sixth property of a photospheric spectrum with prominent Helium
lines, only PTF\,10iuv and SN\,2005E would be members of the family. It is not clear whether
the photospheric spectra of PTF\,09dav exhibit Helium (see discussion in \citealt{skn+11}). The
earliest spectra of SN\,2007ke and PTF\,11bij are not until +19\,d and +21\,d after maximum light.
These two spectra already show the nebular features of prominent [\ion{Ca}{2}] emission common to
the class, but we cannot confirm Helium. Therefore, we allow a photospheric diversity but require
a nebular uniformity in the class.

If in addition to Calcium, we also require Oxygen emission in the nebular spectrum, only PTF\,10iuv,
SN\,2005E, and PTF\,11bij would be members of this class. PTF\,09dav does not show Oxygen emission
and SN\,2007ke does not have spectra at a sufficiently late epoch to test this.

On the other hand, if we require the absence of Hydrogen emission from this class, we would exclude
PTF\,09dav. It is the only member of this class that showed Hydrogen, albeit only at late times.

It is pertinent here to discuss the case of SN\,2008ha \citep{vpc+09,fcf+09,fbr+09}, a peculiar transient
found in the disk of an irregular galaxy. This transient satisfies four out of the five properties of this class.
The only difference is that it showed extremely low photospheric
velocities of $\approx$\,2000\,km\,s$^{-1}$. The photospheric spectra of SN\,2008ha have been
compared to those of the SN\,2002cx family of supernovae, and it has been suggested that SN\,2008ha is a lower velocity
and lower luminosity analog of this family. The SN\,2002cx family has starkly different late-time
spectra dominated by permitted iron lines (it has been argued that these spectra are not nebular even
at +400\,d, e.g., \citealt{jbc+06,sta+08}) and no evidence of Calcium-richness. Therefore, the 2002cx-family is likely unrelated to
the class of transients discussed here.

The membership of SN\,2008ha in either the SN\,2002cx family or in the ``Calcium-rich gap"  class
of transients is unclear. On grounds that the extremely low velocities may be diagnostic
of a different explosion mechanism, we tentatively exclude SN\,2008ha as a member of the
class of ``Calcium-rich gap"  transients.

Originally, \citet{fcs+03} suggested that there was a class defined by only one property:
prominence of Calcium relative to supernovae of Type Ib. This property alone would suggest
that SN\,2000ds, SN\,2003dg, SN\,2003dr and SN\,2003H are also members
of this class. As discussed in \S\ref{sec:loss}, these events were not monitored photometrically.
Additionally, SN\,2005cz \citep{kmn+10,pgc+11}, which also has a similar nebular spectrum
but an extremely sparse light curve, would become a member of this class.
Without a light curve, the ejecta mass in this classification
would remain ambiguous. As discussed below, low ejecta mass is a crucial clue to distinguish
this class from variants of normal SN\,CC as well as SN\,Ia. We note here that even
if light curves were available and consistent with the properties
of this class, it would not alleviate the challenge posed to many progenitor scenarios
by the strong preference for remote locations. Specifically, SN\,2005cz is in an old environment
\citep{pgc+11}, SN\,2003H is amidst interacting galaxies, SN\,2000ds is in an elliptical galaxy,
and SN\,2003dr is offset from an edge-on galaxy.

\begin{deluxetable*}{llllll
  \tabletypesize{\footnotesize}
  \tablecaption{Summary of properties of ``Ca-rich gap'' transients}
  \tablecolumns{6}
  \tablewidth{0pc}
 \tablehead{\colhead{} & \colhead{SN\,2005E} & \colhead{SN\,2007ke} & \colhead{PTF\,09dav} & \colhead{PTF\,10iuv} & \colhead{PTF\,11bij}
}
 \startdata
Peak absolute mag. ($M_{r}$)         & $-$15.5    &  $-$16.3   & $-$16.4    & $-$16      &  $-$15.9         \\
Rise-time (days)                      & $>$9   &  15     & 12      & 12      &  \nodata         \\
Decay time (days)                     & 14     &  15     & 12      & 12      &  10           \\
Photospheric velocity  (km\,s$^{-1}$)  & 11,000    & 11,000     & 6000      & 10,000    & \nodata         \\
Helium in photospheric spectra?       & Yes       &  Yes       & Maybe      & Yes        & \nodata         \\
Calcium in nebular spectra?           & Yes       & Yes        & Yes        & Yes        & Yes             \\
Hydrogen in nebular spectra?          & No        & No         & Yes        & No         & No              \\
Limiting magnitude of host galaxy & $-$7.5    & \nodata    & $-$9.8    & $-$12.1       & $-$12.4         \\
Offset from nearest host galaxy (kpc)       & 23   & 8.5   & 40    & 37     & 33         \\
Galaxy group environment?             & No        & Yes        & No         & Yes         & Yes
 \enddata
\label{tab:summary}
\end{deluxetable*}

\begin{figure}[!htbp]
   \centering
   \includegraphics[width=3.5in]{spec_compare.ps}
   \caption[Spectral Evolution of PTF10iuv]{\small Comparison of PTF\,10iuv
to other SN\,Ib about a month after maximum light. Note the strength of the [Ca~II] line
relative to O~I.
}
\label{fig:specIb}
\end{figure}

\subsection{Comparison to Type Ia and Type Ib Supernovae}
\label{sec:Iab}
In \citet{skn+11}, we discussed that although the photospheric spectra of PTF\,09dav
share some similarities to those of SN\,Ia, there are several differences as follows.
(i) PTF\,09dav does not obey the Phillips relation \citep{p93}. There is a break in the slope of
the relation for subluminous SN\,Ia, but this is obeyed by all SN\,1991bg-like supernovae
including the faintest member, SN\,2007ax \citep{kog+08}.
(ii) The photospheric spectra of PTF\,09dav show Scandium and Strontium
(elements usually seen only in spectra of SN\,CC).
(iii) The nebular spectrum of PTF\,09dav does not show any Fe-peak elements,
which is inconsistent with nebular spectra of all SN\,Ia (Figure~\ref{fig:nebspec}).

The photospheric spectra of PTF\,10iuv around maximum light resemble those of SN\,Ib.
However, a distinguishing characteristic is that a month after maximum, Calcium emission
starts to become prominent. We checked spectra of 26 SN\,Ib from PTF for
Calcium-richness. In Figure~\ref{fig:spec10iuv}, we show seven spectra of SN\,Ib.
While the Calcium near-IR triplet becomes prominent in all of the SN\,Ib as they evolve,
the [Ca~II] doublet is especially prominent in PTF\,10iuv. PTF\,10vnv and PTF\,10inj also show
[Ca~II], but the relative flux ratio of [Ca~II] to O~I is much lower than that
seen in PTF\,10iuv. The case of PTF\,10hcw is less clear, as [Ca~II] is more prominent
than O~I but the supernova set soon after discovery and the photometric coverage stops
before it reached maximum. In the nebular phase, the flux ratio of [Ca~II] to [O~I] is also
much lower in SN\,Ib relative to PTF\,10iuv (Figure~\ref{fig:nebspec}).
Furthermore, the light curves of SN\,Ib are typically more luminous by about
2\,mag and evolve more slowly by at least a factor of 2.

\subsection{Modeling the Light Curve: Ejecta Mass and Radioactivity}
\label{sec:modellc}

\begin{figure}[htbp]
   \centering
   \includegraphics[width=3.5in]{bollc.ps}
   \caption[Modeling the light curve of PTF10iuv]{\small Modeling the light curve
(circles; $\nu\,F_{\nu}$ in the $r$ band) of PTF\,10iuv with radioactive $^{56}$Ni decay. The
dotted line assumes that the last two data points are due to host-galaxy light contamination and
subtracts $r=23.8$\,mag from the rest of the light curve. The model (dashed line) is based on an
ejecta mass of 0.46\,M$_{\odot}$ and a $^{56}$Ni mass of 0.016\,M$_{\odot}$.}
\label{fig:bollc}
\end{figure}

The light curve of PTF\,10iuv is very well-sampled.
The rising portion of the light curve can constrain
the ejecta mass and the late-time decay can constrain the radioactive mass.
Therefore, we can test the hypothesis of whether this
explosion is radioactively powered by $^{56}$Ni as in SN\,Ia.

For supernovae with photospheric velocity, $v$, and rise-time, $t_{\rm r}$,
the ejecta mass is $M_{\rm ej} \propto v\,t_{\rm r}^2$ \citep{a82}.
Therefore, assuming the same opacity, we can derive an ejecta mass by scaling
relative to a normal SN\,Ia with parameters
1.4\,M$_{\odot}$, 11,000\,km\,s$^{-1}$, and 17.4\,days.
PTF\,10iuv has a rise-time of 12\,days and an average
photospheric velocity of 7600\,km\,s$^{-1}$; hence, it has
an ejecta mass of 0.46\,M$_{\odot}$. PTF\,09dav has
the same rise-time but a lower velocity of 6000\,km\,s$^{-1}$,
giving an ejecta mass of 0.36\,M$_{\odot}$ \citep{skn+11}. There are no data to
constrain the rise-time of SN\,2005E. Assuming it was also 12\,days
and using its photospheric velocity of 11,000\,km\,s$^{-1}$, we
get an ejecta mass of 0.67\,M$_{\odot}$. Note that this is a factor
of two higher than the total ejecta mass estimated by \citet{pgm+10}
based on the nebular spectrum. This may not be surprising
given that the nebular spectrum analysis may not have accounted
for all of the Helium. Moreover, higher ejecta mass for SN\,2005E was
expected based on light-curve modeling as well \citep{wsl+10}.

For PTF\,10iuv, given the peak luminosity of $4.6\, \times \,10^{41}$\,erg\,s$^{-1}$ and a 12\,day rise,
we can derive a $^{56}$Ni mass of 0.016\,M$_{\odot}$. However, we find that
the late-time photometry is brighter than what is expected
from radioactive decay of $^{56}$Ni (Figure~\ref{fig:bollc}).
A possible caveat here is that there is some light from an underlying dwarf
host galaxy. The last photometric point is fainter than the depth of our pre-explosion co-add.
It is possible that there is some contamination in the light curve due to the
flux of such a host. Therefore, we plot the dotted line in Figure~\ref{fig:bollc}
which subtracts the last two data points from the rest of the light curve. We are
continuing to obtain even later time imaging to further test this caveat.

Should further observations rule out host contamination,
this may suggest either a radioactive species other than $^{56}$Ni
or an additional source powering the light curve.
For example, a larger contribution by $^{44}$Ti, which has a long half-life
of 60\,yr, may seem a promising candidate to explain the late-time slow evolution.
However, if all of the high luminosity at late times were attributed to this element, it
would require too large a quantity of $^{44}$Ti ($\sim$\,2\,M$_{\odot}$).
Modeling of different
combinations of other additional radioactive species ($^{44}$Cr, $^{44}$Ti,
and $^{52}$Fe) in the context of Helium-shell detonations
on small \citep{wsl+10} and large CO white dwarf cores \citep{skw+10} has been
undertaken. These efforts were limited by the missing light-curve
data in the rising and very late phase of SN\,2005E. The well-sampled
light curve of PTF\,10iuv should be able  to better constrain these models.

\subsection{Constraint on Electron Density}
Using the flux ratio between [Ca~II] and the Ca~II near-IR triplet,
we can constrain the density given a temperature. For PTF\,10iuv,
the nebular spectrum at +87\,day gives a ratio of 0.86 and the
spectrum at +115\,day gives a ratio of 1.8. For PTF\,09dav,
the nebular spectrum at +94\,day gives a ratio of $>$2.2
(assumed width of 300\,\AA, 3$\sigma$ limit is
$3 \times 10^{-18}$\,erg\,cm$^{-2}$\,s$^{-1}$\,\AA$^{-1}$).
For SN\,2005E, the ratio at +65\,d is 0.55 \citep{pgm+10}.
SYNOW fits to late-time spectra suggest a temperature
roughly in the range 4500--5000\,K.
Following Figure~2 of \citet{fp89}, assuming a temperature
around 4500\,K, the electron density is on the order of $10^9$\,cm$^{-3}$
and decreases by a factor of a few in a couple of months.

\subsection{Modeling the Nebular Spectra}
Next, we estimate the mass of the dominant species in the
ejecta using the nebular spectrum.

We estimate the Oxygen mass based on the luminosity of the [O~I] line in
the nebular phase. We can assume the high-density limit holds ($>10^{6}$\,cm$^{-3}$)
and estimate the oxygen mass as $$M_{O} = 10^{8}f_{\rm [O~I]} D_{\rm Mpc}^{2} e^{(2.28/T_4)} {\rm M}_{\odot},$$ following \citet{u86}.
Assuming a temperature of 4500\,K, we get 0.025\,M$_{\odot}$ of Oxygen
for PTF\,10iuv and 0.037\,M$_{\odot}$ for SN\,2005E. Note that the oxygen
mass is consistent with the mass derived by \citet{pgm+10}. A cautionary note
here is that this calculation is extremely sensitive to temperature;
a difference of only 500\,K in temperature changes this estimate by a factor of 2.

Two months after maximum brightness, the luminosity in [Ca~II] nebular
emission for SN\,2005E was $2 \times 10^{39}$\,erg\,s$^{-1}$ and the derived ejecta mass was
0.135\,M$_{\odot}$ \citep{pgm+10}. The [Ca~II] nebular luminosity is a factor of 2.5 smaller for
PTF\,10iuv and factor of 2.6 larger for PTF\,09dav relative to SN\,2005E.
Under similar conditions, this may be representative of the range in Calcium mass
for these events.

\section{Discussion}
\label{sec:discussion}

We are struck by the remote ``off-galaxy'' locations of all five confirmed
members of the class of ``Calcium-rich gap"  transients (Figure~\ref{fig:loc}) and
Figure~\ref{fig:lossfinders}). While five may still be considered small-number
statistics, location can be a powerful diagnostic of the physical origin.
Below, we discuss the pros and cons of two broad classes of possible
progenitor scenarios: a white dwarf and a massive star.

\subsection{A White Dwarf?}

The white dwarf scenario has tremendous appeal to explain ``Calcium-rich
gap'' transients for two reasons.
First, the remote galactic locations, intracluster environments,
and constraints on star formation of the observed members of this family
point to an old population. Second, the low ejecta masses derived from
the light curves and nebular spectra are in the range of what is
derived from white dwarf explosions and not massive star explosions.

The family of transients presented here is not the standard thermonuclear explosion
of a white dwarf as seen in SN\,Ia. There are two major
differences. First, none of these transients obey the \citet{p93} relation. The
inferred ejected masses are smaller than in SN\,Ia.
Second, Fe-group elements seen in all SN\,Ia are absent in the nebular spectra of these explosions.

Next, we discuss several alternate explosions of white dwarfs that have been
discussed in the literature to explain intermediate luminosity and fast
evolving transients. First, we consider a ``.Ia'' explosion following the final Helium flash in an ultracompact
white-dwarf white-dwarf  binary \citep{bsw+07,skw+10}. The observed rise-time of ``Calcium-rich gap"
transients is too slow for a ``.Ia'' explosion. The observed ejecta masses are too large for a
shell detonation \citep{wsl+10} and suggest that the core also participated in the explosion.

\citet{wk11} derive several models for explosions of sub-Chandrashekhar white dwarfs.
However, the peak absolute magnitude and rise-time range observed for ``Calcium-rich gap''
transients is not predicted by any of these models.

Another proposed theoretical model is accretion induced collapse (AIC) of a rapidly rotating
white dwarf into a neutron star \citep{mpq+09}. However, AIC predicts a spectrum dominated
by intermediate-mass elements, much higher velocities (0.1\,$c$), and much more rapid rise
(1\,day) and decline (4--5\,days) than what is observed for Ca-rich gap transients.

Another possibility is deflagration of a sub-Chandrashekhar mass white dwarf \citep{ww94},
as it is also expected to have lower luminosity than a SN\,Ia. However, the late-time light curve
and absence of Fe-peak elements in the nebular spectra are inconsistent with this model.

The presence of Helium in SN\,2005E and PTF\,10iuv can be explained for some
white dwarf models. But, the presence of hydrogen in PTF\,09dav poses a major challenge to all white dwarf explosions.
One possible scenario to explain late-time hydrogen in a white-dwarf explosion is as follows:
Consider a binary where mass-transfer is from a hydrogen rich companion star onto a white dwarf.
This accretion initially proceeded at a low rate, resulting in a series of nova eruptions prior to
the sub-Chandrashekhar explosion or Helium-shell detonation. The photons from the final explosion would
eventually reach one of the previously ejected nova shells and the interaction would give H$\alpha$ emission.

Quantitatively, if the shell was photo-ionized,
the distance to this nova shell would be the speed of light multiplied
by 95\,days, or $2.5 \times 10^{17}$\,cm. Given the velocity of 1000\,km\,s$^{-1}$
to traverse this distance, the nova eruption would then have occurred 78\,yr
prior to the supernova. Given the absence of Hydrogen in early-time spectra, we consider instead
collisional ionization when the shock front itself reaches the shell. The
distance to the shell would then be $8.2 \times 10^{15}$\,cm and the nova shell would
have to be ejected $\sim$\,950\,days before the supernova.  The mass of Hydrogen needed to sustain the observed
luminosity for an hour is $\frac{4}{n}\,\times\,$10$^{-4}$\,M$_{\odot}$, where $n$
is the number of times the same Hydrogen atom gets excited in one hour.

Yet another scenario was recently proposed by \citet{m11} that can  potentially
explain a trace amount of Hydrogen -- tidal disruption of a white dwarf by a neutron star
or stellar mass black hole.  However, several other observables (e.g., velocities)
are inconsistent with this model.

While the presence of five transients in remote locations is a strong clue in favor
of the white dwarf scenario, the absence of any events in disks of galaxies is quite
problematic. Studies of white dwarf binaries have shown that the number of white dwarfs
in halos relative to that in the disk is nearly a third, larger than expected from
the ratio of the overall mass or light \citep{rbb+07}. However, that is not sufficient
to explain why there is a strong preference for remote locations.

If the progenitor is indeed a white dwarf, then there must be a characteristic of white
dwarfs which can be attributed to location and affects the explosion signature.
For example, the age of the white dwarf (e.g., if the time scale for evolution
in a multiple star system were longer), the composition of the white dwarf (e.g., if
Helium white dwarfs were preferentially found in remote locations), environmental characteristics
(e.g., if metallicity/density affected the explosion or progenitor evolution time scale).
One scenario that remains to be tested with detailed modeling is that
at lower metallicity, even relatively lower mass stars can evolve to become
white dwarfs in a Hubble time. Perhaps, explosions of these relatively
lower mass white dwarfs are subluminous, fast evolving, and Calcium-rich.

\subsection{A Massive Star?}
Given that none of the above white dwarf models easily explain all of the observed
clues of ``Calcium-rich gap'' transients, we briefly consider the massive star option. There are
some explosion properties which are reminiscent of core-collapse supernovae: similarity of nebular spectra
albeit with enhanced Calcium, similarity of photospheric
spectra to SN\,Ib in the case of PTF\,10iuv and SN\,2005E,
and the presence of Hydrogen in the case of PTF\,09dav.

\subsubsection{Massive Star in the Outskirts?}
\citet{pgm+10} convincingly argue against the progenitors being hypervelocity
massive stars formed in the disk. A more feasible option that allows massive stars
to traverse large distances is tidal stripping during galaxy interactions.
This is especially intriguing given the galaxy group surrounding the locations
of PTF\,10iuv, PTF\,11bij and SN\,2007ke.

Studies of intracluster environments show evidence for a dominant old component as well
as a young component, particularly in tidal tails of interacting gas-rich galaxies
\citep{mkk+11,wcd+07}. It has been shown that roughly 15\% of the
cluster's mass is in the intracluster medium.
Sivanandam et al. (2009) show that 50\% of metals come
from intracluster supernovae. \citet{mkk+11} present a study of tidal tails
of interacting galaxies and find that young star clusters formed {\it in situ} in half the sample.
Another possibility is that there is some low-level star formation in remote locations.
Recent systematic surveys  \citep{wpm+10,wpm+08} show star formation in the far outskirts
of noninteracting galaxies. About 10\% of the galaxies
in this study had outlying H~II regions with offsets between 20\,kpc and 40\,kpc.

Our deep ground-based limits show neither any evidence of tidal tails nor
H~II regions. However, given the distance to these supernovae, they are not
sensitive to a significant fraction of the luminosity function of H~II regions
and young star clusters. So, we cannot completely rule out the possibility of a massive
star origin. Deep narrow-band imaging will provide better constraints.

\subsubsection{Fallback Supernova?}
Assuming there was a small amount of {\it in situ} star formation below our
detection limits, one would expect regular core-collapse supernovae
in the outskirts as well. However, the absence of regular SN\,CC
with offsets larger than 30\,kpc in the PTF sample appears to
be at odds with the progenitors being massive stars (see Figure~\ref{fig:snoffsets}).

A possible partial resolution is if the fate of
massive stars in very low-metallicity environments is very different.
Specifically, the lower metallicity in the outskirts lowers the
mass-loss rate, and it has been suggested that a larger fraction of massive stars
collapse directly to a black hole (e.g., \citealt{hfw+03}, \citealt{oo11}).
Such a collapse results in a subluminous explosion or no explosion at all.
This could explain both the small numbers of SN\,CC
in the outskirts and the dearth of regular SN\,Ib/c
in low-metallicity environments. This is also consistent with studies that
show that regular SN\,Ib/c are more centrally concentrated relative
to SN\,II \citep{aj09}. Some of the missing Type Ib/c explosions in
low-metallicity environments (outer parts of galaxies) could perhaps be
subluminous and short-lived fallback events. Fallback of some ejecta onto the proto-neutron star
to form the black hole could explain the low ejecta mass, fast evolution,
and absence of heavy elements observed in this class. It would not be surprising,
then, that the first fallback events observed are located in the outskirts of their hosts.

There are three important caveats to this scenario. First, since the initial mass function is
quite universal and varies little over a wide range of metallicity (e.g., \citealt{mkkm11}),
we expect to see a significant population of normal SN\,II-P from the lower
mass range of SN\,CC unaffected by metallicity. But, current transient surveys
have not found any SN\,II-P in such remote galactic outskirts.
Second, PTF\,10iuv and SN\,2005E were Hydrogen-free. Therefore, mass loss
would have to be finely tuned to be high enough to expel the Hydrogen, low enough such that
there is fallback onto the core, yet not too low such that there is no explosion at all.
\citet{kmn+10} proposed an alternate scenario where the Hydrogen was removed by close
binary interaction. Third, some galaxies have shown
that the metallicity gradient flattens beyond a certain radius and doesn't continue to decrease.
For example, metallicity measurements of the H~II regions in the outskirts
show that they are not exceptionally low metallicity (roughly 0.4 solar; \citealt{wpm+11}).
To the extent that metallicity is diagnostic of line-driven mass loss,
this presents another challenge to the massive star scenario.

\section{Conclusions}
\label{sec:conclusion}

Five transients (SN\,2005E, SN\,2007ke, PTF\,09dav, PTF\,10iuv
and PTF\,11bij) share the following common properties:
low peak luminosity, fast photometric evolution, large photospheric
velocities, early evolution to the nebular phase, and Calcium-dominated ejecta.
Furthermore, all five members of this class of ``Calcium-rich gap'' transients
are located in the outskirts of their
putative host galaxies. This set of properties, in conjunction with peculiarities
specific to each of them (e.g., the presence of Hydrogen, Scandium,
and Strontium in PTF\,09dav, strong constraints against star
formation in SN\,2005E, intracluster environment of PTF\,10iuv, PTF\,11bij, and SN\,2007ke),
warrants a creative modification of standard thermonuclear
or standard core-collapse scenarios.

We can estimate a lower limit on the rate of this class of ``Calcium-rich gap''
events by comparing to the rate of SN\,Ia discovered by PTF in the same volume in the
same time. Within 200\,Mpc, we found 128 SN\,Ia and 3 such events.
Therefore, a lower limit on the rate is $>7 \times 10^{-7}$\,Mpc$^{-3}$\,yr$^{-1}$
(we used the SN\,Ia rate from \citealt{lcl+11}). We emphasize that this
is a lower limit, as a few days of bad weather would be much more detrimental for
finding these short-lived and lower luminosity transients compared to SN\,Ia.
This rate of $>$2.3\% relative to SN\,Ia is consistent with the
relative rate of 7$\pm$5\% estimated by \citet{pgm+10}.

The key to solving the mystery of the origin of ``Calcium-rich gap''
transients is their location. The remote locations can either be
a red herring (due to small numbers) or the most important clue. Parenthetically, we
remark that the two Type Ia supernovae (SN\,2006bt -- \citealt{fnc+10};
PTF\,10ops -- \citealt{mst+11}) found farthest outside the main body
of their host galaxies are also peculiar.
Extremely deep late-time observations (e.g., with the {\it Hubble Space Telescope})
are needed to serve as a litmus test: detection of a dwarf satellite,
super star cluster, or globular cluster would provide a direct clue
about the environment, and nondetection would require a phoenix
transient that rose from the ashes.

\bigskip
\smallskip
\noindent{\bf Acknowledgments} \\
We thank Chuck Steidel and Ryan Trainor for Target of Opportunity
observations of PTF\,11bij with Keck I. We are grateful to the staff of
the Expanded Very Large Array for efficiently executing Target Of
Opportunity triggers. Excellent assistance was provided by the staffs
of the various observatories where we obtained data (Lick, Keck, Palomar,
WHT, EVLA).

MMK acknowledges support from the Hubble Fellowship and Carnegie-Princeton
Fellowship. EOO is supported by an Einstein Fellowship. HBP is a
CfA and Bikura prize fellow.
The Weizmann Institute's participation in PTF is supported by grants
to AGY from the Israel Science Foundation and the US-Israel Binational
Science Foundation. AVF and his group at UC Berkeley acknowledge generous financial
assistance from Gary \& Cynthia Bengier, the Richard \& Rhoda
Goldman Fund,
the TABASGO Foundation, and National Science Foundation (NSF) grant AST-0908886.
KAIT was constructed and supported by donations from Sun
Microsystems, Inc., the Hewlett-Packard Company, AutoScope
Corporation, Lick Observatory, the NSF,
the University of California, the Sylvia \& Jim Katzman
Foundation, and the TABASGO Foundation.
Computational resources and data storage were contributed by NERSC, supported by
U.S. DoE contract DE-AC02-05CH11231. PEN acknowledges support from the US DoE
contract DE-FG02-06ER06-04. JSB acknowledges support of an NSF-CDI grant 0941742,
``Real-time Classification of Massive Time-series Data Streams.''
MS acknowledges support from the Royal Society. LB acknowledges NSF grants
PHY-0551164 and AST-0707633. DCL acknowledges NSF grant AST-1009571.

Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated
as a scientific partnership among the California Institute of Technology, the University
of California and the National Aeronautics and Space Administration;
it was made possible by the generous financial support of the W. M. Keck Foundation.
The Expanded Very Large Array is operated by the National Radio Astronomy
Observatory, a facility of the NSF operated
under cooperative agreement by Associated Universities, Inc.
The WHT is operated on the island of La Palma by the Isaac Newton Group in the Spanish
Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.

\bibliographystyle{apj}

redpajama_set_name: RedPajamaArXiv


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Demonstrate knowledge and understanding of engineering and management principles as a member and/or leader in a team to manage projects and in multidisciplinary environments.
The BS Electrical Engineering Program of Mariano Marcos State University has been awarded a Level III status by the Accrediting Agency of State Colleges and Universities in the Philippines (AACUP) Inc.


404 whoops page not found, cushions for timber kitchen chairs, wood counter bar, 404 whoops page not found. Cushions for timber kitchen chairs, wood counter bar. High quality vinyl wooden swivel bar stool 29 inch seat.


Social media giant Facebook has taken the wraps off a plan aimed to bring more great content to its iOS app, according to a report from Re/code. Dubbed "Instant Articles," the new feature will bring articles from the likes of The New York Times, National Geographic, BuzzFeed, and NBC News to your mobile timeline. The Guardian, BBC News, Spiegel, and Bild will be coming soon. For now, the Instant Articles are only available from within the iOS Facebook app.
Facebook's mobile platform boasts 1.25 billion users, so most publishers are going to jump at the opportunity to get their content in front of that many pairs of eyeballs. The core terms of the program are very friendly to publishers, so Facebook is likely to see a great deal of interest from content producers. BuzzFeed president Greg Coleman pointed out that Facebook has truly taken the needs of the publisher to heart in developing the program.
Facebook really understood what would be important to us. So instead of acting like someone who would dictate, they came to us and asked us what would be great for BuzzFeed.
Facebook's Instant Articles are designed to load instantly on the social media site's iOS app. Publishers use their own tools to create the posts, and Facebook automatically converts those stories into a format that works on the iOS app. Content producers can take advantage of some cool bells and whistles, like the photo and video-panning feature from Facebook's almost extinct Paper app.
Publishers get to keep 100 percent of the ad revenue they earn from their Instant Articles. For stories that don't make it into Instant Articles, Facebook will sell the unsold inventory through its own ad network and give publishers 70 percent of that revenue. Instant Article publishers will get access to performance data on their stories, provided by Google Analytics and Adobe's Omniture, and ComScore will give full credit for each post to the actual content producer.
If it all seems too good to be true, it very well might be. Facebook has such a proven track record of changing its mind and the terms and conditions for its services that such revision is almost considered standard operating procedure for the social media giant. Facebook is already so hugely important to many publishers that it has even surpassed Google as those sites' chief referral source. Is it such a great idea to give Facebook even more power?
If Facebook is truly doing this to give users a better experience of reading stories on mobile phones, then publishers should have little to worry about. On the other hand, if Facebook is initiating this program out of a desire to gain more ownership over publishing, Instant Articles might not be such a hot idea.


Melrose has never had it easier.
The garage is one of the most underused rooms in a home. Mostly because homeowners don't know how to make complete use of the space they have there. Monkey Bar Storage creates customized garage storage in Melrose to get your storage organized. With customized products like shelving, overhead storage, and durable cabinets, you will be surprised you ever lived without it!
Without a storage plan in place, chaos can quickly arise in a garage. Monkey Bar Storage provides a plan and system for your garage, so it can stay organized for years to come.
Affordable: We offer top of the line products at an affordable price, so you can stay within your budget.
Accessories: We offer multiple accessories to complete our organization system. For example, we offer ski racks, bike racks, ball bags, shoe racks, and much more!
Adjustable: Our system was created to be easy to adjust, so whenever your storage needs change your storage system can too.
Garage Shelving: Unique shelving that provides multiple storage options.
Garage Cabinets: lockable cabinets that hold up to 100 lbs per shelf.
Overhead Garage Storage: Storage and safe overhead storage racks.
Garage Flooring: Durable, waterproof, and protective flooring that looks great!


A: In it's simplest terms, gum disease is an infection in your mouth. It can range from a minor infection, on the scale of a canker sore, to a severe infection that affects your whole body. The technical term for gum disease is periodontal disease, though some people call it pyria, but since this isn't a text book we'll just call it gum disease here.
Q: What are the symptoms of gum disease?
A: Gum disease in it's early stages is a silent disease. In fact, you may not even know you have gum disease until your dental hygienist mentions it during a routine cleaning. If left unchecked the infection will continue to worsen and become symptomatic.
Bad Breath – Yikes! This isn't the kind of bad breath a mint, quick rinse with mouth wash, or regular brushing will clear up. We're sorry to say the smell is coming from the infection that's lurking beneath your gum line.
Tooth sensitivity – The newly exposed areas of the tooth can be quite sensitive.
Q: What can happen from gum disease?
A: It's all bad news, sorry.
Gum recession – As the infection progresses the gums pull away from the tooth and start to recede. Once the gum recedes it will never reattach on it's own, even after the infection is cleared up.
Bone Loss – Chronic gum disease eventually affects the jaw or cranial bone it covers and causes the bone to break down. In some cases the dentist can do a bone graft to help build up and replace lost bone, but bone grafts aren't always successful or sometimes only have marginal improvement so it's best not to let the gum disease get that far.
Tooth Loss – Without the support of healthy gums and bone the teeth eventually become loose and fall out. To make matters worse, tooth loss due to gum disease will mean you're probably not a good candidate for a dental implant (because there won't be good, strong, healthy bone to anchor the implant into).
Increased risk for cardiovascular disease, heart attack, and stroke. Research shows a connection between periodontal disease (gum disease) and cardiovascular disease. You're welcome to read a tidy summary of current findings on WebMD.
Additionally, diabetics are especially susceptible to complications of gum disease, and studies have shown that management of gum disease in diabetics can improve patient blood sugars.
That's all pretty awful stuff. We'd really rather you never have to go down that road, or if you have, give us a call and let our gentle and friendly dental hygienists and dentists get you on the road to oral health. Did we mention our hygienists are gentle? You're gonna love them, we promise!
Q: Ok, I know gum disease can cause sore gums, but is there anything else that can cause sore or bleeding gums?
A: Yes, there are a few other things that could be causing you gum trouble.
Trauma caused by brushing your teeth too hard or cutting your gums accidentally with dental floss. (Please buy toothbrushes with the extra soft bristles and don't scrub your teeth with a vengeance).
Gently floss to be sure there is no food or other item stuck between the teeth or in the gums. (Popcorn hulls are a common culprit for this type of sore gums).
Swish and rinse your mouth with lukewarm saline solution (spit the saline out after rinsing, don't swallow it). See recipe for homemade saline solution below. Swishing with hydrogen peroxide is a common home remedy for gum disease, but it won't cure periodontal disease.
Be a little more gentle when brushing your teeth in the affected area for the next few days. If your sore gums were caused by using a toothbrush with very stiff bristles or brushing too hard the soreness should go away in three to four days.
If you continue to have swollen and sore gums for more than one week please call the office to schedule and examination to determine what the problem is. If your sore swollen gums are caused by gum disease it is important to treat it as soon as possible.
Ask one of our doctors to prescribe you a prescription mouthwash called Peridex. It is a special mouthwash for people with gum disease that helps kill the infection and with proper hygiene will help keep it from coming back. We consider it the best mouthwash for gum disease patients.
Mix the salt and water until salt is dissolved.


Epworth Knowledge Bank: The incidence and natural history of dasatinib complications in the treatment of chronic myeloid leukemia.
Title: The incidence and natural history of dasatinib complications in the treatment of chronic myeloid leukemia.
Abstract: Dasatinib has shown superiority over imatinib in achieving molecular responses (MRs) in chronic phase chronic myeloid leukemia but with a different toxicity profile, which may impact its overall benefit. Reported toxicities include pleural effusions and pulmonary hypertension, and although the incidence of these events is well described, response to therapy and impact of dose modifications on toxicity has not been comprehensively characterized in a real-world setting. We retrospectively reviewed the incidence of dasatinib adverse events in 212 chronic phase chronic myeloid leukemia patients at 17 Australian institutions. Adverse events were reported in 116 patients (55%), most commonly pleural effusions (53 patients, 25%), which was the predominant cause of permanent drug cessation. Age and dose were risk factors for pleural effusion (P < .01 and .047, respectively). Recurrence rates were higher in those who remained on 100 mg compared with those who dose reduced (P = .041); however, recurrence still occurred at 50 mg. Patients who developed pleural effusions were more likely to have achieved MR4.5 after 6 months of dasatinib than those without effusions (P = .008). Pulmonary hypertension occurred in 5% of patients, frequently in association with pleural effusion, and was reversible upon dasatinib cessation in 6 of 7 patients. Dose reductions and temporary cessations had minimal impact on MR rates. Our observations suggest that by using the lowest effective dose in older patients to minimize the effusion risk, dose modification for cytopenias, and care with concomitant antiplatelet therapy, the necessity for permanent dasatinib cessation due to toxicity is likely to be minimal in immunologically competent patients.
Affiliated Organisations: Austin Hospital, Melbourne, Australia.
Baker IDI Heart and Diabetes Institute, Melbourne, Australia.
Princess Alexandra Hospital, Brisbane, Australia.
Monash Health, Clayton, Melbourne, Australia.
School of Clinical Sciences at Monash Health, Monash University, Clayton, Melbourne, Australia.
Hollywood Medical Centre, Perth, Australia.
Box Hill Hospital, Melbourne, Australia.
Royal Hobart Hospital, Hobart, Australia.
Royal Melbourne Hospital, Melbourne, Australia.
St Vincent's Hospital, Melbourne, Australia.
Royal Prince Alfred Hospital, Sydney, Australia.
Calvary Mater Hospital, Newcastle, Australia.


Not sure if anyone has addressed this before but couldn't find anything. Really trying to get my hear around the whole nodal thing, but it's tough. I've been working on a tree that uses the occlusion node to put texture (or color) into the nooks and crannies of a model without using weight maps (the old way I did it) My question is: Does the Occlusion node cheat the shading once (like I hope) or does it update in some way? The documentation wasn't clear. I suspect it dosen't react like real occlusion (if it did my textures would move across the surface depending ol lights and such, right?) Anyway, thanks if you can help!
Hi there - lights don't affect it only geometry does. It fires rays out from the point being rendered to see if they hit anything. If you moved an object near the surface the occlusion would be affected but moving lights shouldn't matter.
So using it for animation probably wouldn't work, hu? Poo. Hey, Simon, didn't you do the metal Grider surface? I found the thread but the pst isn't on it anymore for download anymore, is there another place I can get it?
Yes if you used it in an animation and the geometry changed so would the surface probably. I would use the surface baking camera perhaps to bake onto a UV and keep it constant?


Hope Heals. – Hope is Hard.
There was a season when big life altering decisions were around the corner and I was stuck. I couldn't sleep. I couldn't eat. I couldn't make a decision. A very-bad-no-good-ugly-thing had happened to me and I was afraid of taking a risk on hope. I felt broken, with no hope of repair.
So at night, I would lay awake with my mind racing. I couldn't stop making a list of all the pro's and con's, the potential hurts, the what-if's. I was so driven by fear that eventually due to lack of sleep, I started getting heart palpitations and had to go visit my doctor. Physically, my body was experiencing a surge in stress driven by hurt and fear, and it started to alter how I responded to the world. The typically laid back Brittany became anxious. I had irrational fears. My ability to accurately assess a situation went out the door. And as for hope, it wasn't dead, but there wasn't much room for it to breath around my suffocating anxiety.
Praise the Lord for godly counselors and doctors! Because of their wisdom, my body started sleeping again. And after we got that sorted out, I was able to start processing life through a healthier filter, not a fear-based one.
Hope finally had room to grow, but fear had to die in order for hope to breathe again. So how did I get there? It wasn't a quick fix, but here are my 3 tips to anyone wrestling with the physical effects of hopelessness.
1. Talk to a Biblical counselor and potentially medical doctor. I remember sitting in my counselor's office talking about the tightening of my chest and the rapid beating of my heart. My hands fiddled with a tissue, while I confessed my body's shortcomings. I was so embarrassed that my body couldn't handle the stress I was under. With kind eyes, he looked at me and gave me the best advice I could have ever received. His wisdom was God's grace to me in a very dark season. He helped me see that I wasn't "less-than" for asking for help, that it was ok to go see a doctor to address my lack of sleep. Perhaps if we focused on me getting physically healthy, we could deal with the emotional trauma later.
I saw a counselor for almost two years, and it was in the hard work done in those sessions and at home that lead me to hope again. If you have experienced trauma or brokenness and are trapped by fear, let me plead with you to ask people into those broken spaces. There is no shame in getting help from licensed professionals. They are God's gift to a broken world; please utilize them.
2. Take care of your physical needs. Sometimes, triage is necessary. It doesn't mean we ignore the broken leg, rather it simply means we take a moment to fix the gaping wound in our hearts before we address the other hurts. If you aren't sleeping, eating, drinking lots of water, or exercising, may I suggest you start there. If your body is physically drained by a lack of hope or the physical drain of trauma, start with making sure you are taking care of your body. Go for a walk, stay away from alcohol and caffeine, get some rest, and choose foods that fuel and heal.
3. Hope, even when the world tells you not to. As believers, we have access to a holy God who is in the business of redeeming. It literally is his name. Jehovah-Rapha, Our God is healer. There will always be brokenness this side of glory, but our hope isn't in a pain-free existence. Our hope is in a God who is big and loving enough to offer redemption to a broken world. And if He's big enough to offer salvation to all of mankind, there's nothing in your life so royally screwed up that He is unable to redeem it. There is nothing too broken, no person too far gone, no wound too ugly. Never stop hoping. And if you do, look to Jesus and remember what He has done for you and let it be enough for that day, that moment.
My dear friend, never lose hope. He shines brightly on our darkest nights.
You should know that not all stories have happy endings, but mine does. When I physically got healthy, I was able to make a decision rooted in hope instead of fear. I tossed "What-if's" to the side and chose to love and forgive BIG. God restored some broken places in my life that the world would tell me could never be whole again. And it all started by choosing to hope again, choosing that my life decisions wouldn't be rooted in fear, but in love.
And I feel propelled to tell you this, even if I get hurt again, even if my worst "what-if's" come true, I'm so glad I chose hope. There are no regrets when you choose to fight fear and live basking in light of redeeming love.
Previous Post Deafening Anxiety to Stillness of Soul.


Mums Wine HQ: A House Move That Won't Leave Your Wallet Empty!
A House Move That Won't Leave Your Wallet Empty!
Keeping a tight reign on the family budget isn't easy at the best of times, but during a home move, things can get out of hand pretty quickly. This is because there is always so much to pay for including fees, items for the new place, and all those other things like cleaning and removal crews. This makes it seem like saving money while moving is an impossibility, but that just isn't the case. Especially if you handle the move carefully. Read on to find out more.
One of the biggest costs involved with moving house is that we end up paying out for professional services connected with the industry. This can include real estate agents, builders, gardeners, cleaners and removal firms. However, it's important to assess your financial situation and the need for outside services when you are trying move while saving money. Yes, it's like that you will need a real estate agent unless you plan to sell your home privately, but look at the online options too. As they take a flat fee, something that can save you a lot of money in the long run.
Similarly, unless you have a particular issue that you need a deep clean for in you new home, do you need to employ a professional cleaning crew? Probably not. In fact, it's going to be a lot cheaper to grab a bottle of cleaning fluid and a cloth and get done to it yourself. Perhaps the only fee that is it consistently worth paying out for is a company like Two Men professional mover's. This is because the sheer physical and organisational effort that goes into moving an entire house full of items from one place to another is a mammoth job. One that it is always easier to give it over to someone else, so you can focus on more important things like settling in the new place and ensuring that the family adapts to the move well.
So, apart from the professional mover's exception, we can see that in many cases it is possible to save money when moving. Especially if we don't spend on professional services for every single job that needs to get done.
Next, a good rule for saving some money when you are moving home is to not buy anything for the new house, at least until you have moved in and unpacked. This works because it does two things. The first is that it stops you getting carried away with the new place being perfect, something that can see you spending a lot of money on new items just because they are new rather than because they are needed. The second is that you may actually have things that will fit well in the new home, but you don't really that until you get there and try them out. Also even if you do decide on some new items, look out for sales and bargains, so you aren't paying full price!
That is why you should always wait until you have your stuff from the old place unpacked before you start buying new stuff. As you could be shelling out money that you just don't need to.


text:
The Impact upon a Family of Having a Disabled Child
Williams, G. 2021. The Impact upon a Family of Having a Disabled Child. Research in Teacher Education. 11 (2), pp. 18-23. https://doi.org/10.15123/uel.8q583
Williams, G.
This research seeks to explore the impact of having a disabled sibling, with a focus on autism. This impact has often been overlooked, meaning there is a lack of research focused on siblings despite the challenges they face. The sample comprises five individuals from different families; four of the participants have a sibling with autism, and one participant has a sibling with Down syndrome. The study has taken an interpretivist approach using interviews and open-ended questionnaires to collect qualitative data. The chosen paradigm was the most appropriate when collecting and analysing experiences of individuals with disabled siblings. It employed mixed methods: semi-structured interviews were conducted, and each participant completed an open-ended questionnaire. The data were analysed using a thematic approach to identify six themes. The results showed that all the respondents agreed that their disabled sibling has impacted their life, but the overall impact was mixed, showing positives and negatives, although, more negatives were found. There was a detailed discussion on the participants' experiences. It is recommended that there should be further research conducted on siblings and more support given.
Research in Teacher Education
11 (2), pp. 18-23
The School of Education and Communities, University of East London
File Access Level
https://doi.org/10.15123/uel.8q583
© 2021 The Author
https://repository.uel.ac.uk/item/8q583
License: All rights reserved
File access level: Anyone
Garby-Czerniawski, G. 2021. Editorial. Research in Teacher Education. 11 (2), p. 5. https://doi.org/10.15123/uel.8q580
Transitioning to Online Teaching and Learning: A Discussion of Barriers Faced by Educators and Students in Higher Education during a Global Pandemic
Brown-Wilsher, P. 2021. Transitioning to Online Teaching and Learning: A Discussion of Barriers Faced by Educators and Students in Higher Education during a Global Pandemic. Research in Teacher Education. 11 (2), pp. 6-11. https://doi.org/10.15123/uel.8q581
Addressing the Attainment Gap through Early Intervention: Assessment of the First of a Multi-Year Project
Ahmed, F. 2021. Addressing the Attainment Gap through Early Intervention: Assessment of the First of a Multi-Year Project. Research in Teacher Education. 11 (2), pp. 12-17. https://doi.org/10.15123/uel.8q582
A Four-Phase Working Methodological Model for Conducting Action Research
Balmforth, N. 2021. A Four-Phase Working Methodological Model for Conducting Action Research. Research in Teacher Education. 11 (2), pp. 24-28. https://doi.org/10.15123/uel.8q584
Teachers' Perceptions of Creativity and How It Relates to Primary School Science: A Reflection
Stephens, K. 2021. Teachers' Perceptions of Creativity and How It Relates to Primary School Science: A Reflection. Research in Teacher Education. 11 (2), pp. 29-34. https://doi.org/10.15123/uel.8q585
Where Have All the Flowers Gone? A Case for Community Gardening for Education
James, M. 2021. Where Have All the Flowers Gone? A Case for Community Gardening for Education. Research in Teacher Education. 11 (2), pp. 35-38. https://doi.org/10.15123/uel.8q586

redpajama_set_name: RedPajamaCommonCrawl


My apologies for the delay in this post! This months giving blocks are improv stripes!
These blocks are pretty easy and quick! Make 1 make 10! It's up to you!
Block size to be 12.5″ x 12.5″ or 12.5″ x 24.5″.
Colors are to be warm colors. As in red, orange, pink, yellow.
Colors are preferred to be solids, but prints that are color on color that read as a solid will work as well.
Are you as excited as I am to see how ours turns out?? Make some and bring to the November meeting!!
It's time for a new giving quilt plan! And this time around, there's no need to rummage through your stash becuase our local Clothworks has generously donated beautiful American Made Brand solids for our next giving quilt.
The colors chosen are the same as the logo for Homeward Pet Adoption Center, our intended recipient for this quilt. Specifically, they are (top to bottom in photo below) dark eggplant, dark blue, brown, and white. Bundles will be available at the August meeting, with each consisting of 1/16 yard of each of the colors, and 1/8 yard of white.
Your assignment if you choose to accept it is to make as many original improv blocks as you like using the fabrics in the bundle only. You can use some or all of the colors, with blocks being in one of three sizes: 6 1/2″ square, 6 1/2″ x 12 1/2″, or 12 1/2″ square. Please return all blocks along with any fabric you don't use to the September meeting.
We'd love to see your progress on Instagram using the hashtags #seamqggiving and #seamqg. And feel free to thank @clothworks for their #americanmadebrand fabrics! Enjoy the freedom of doing your own thing for good!
With our first 2016 giving quilt complete and the second in the finishing stages, it's time to start another! This month, let's make "Little Tent" blocks, inspired by Daisy/Ants to Sugar.
Let's make unfinished blocks that are 6.5″, 12.5″, or 18.5″ on any side. That means any shape with those sizes, so squares, tall rectangles, or long rectangles. Make yellow triangles, aqua strips, and navy or dark blue 'background,' and a mix of prints and solids is just fine. Here are some sample blocks to give you an idea of what we're after!
Return your blocks by the July meeting. Thank you!
First off, a big thanks to everyone that contributed blocks to the black and white Quarter Log Cabin that is being put together as we speak! It's going to be great!
Next up, our next Giving Committee quilt! X Marks the Improv!
This block was designed by Debbie, originally for her do.Good Stitches Group. But we love it so much we thought we needed to do it for our Giving Committee as well. You might recognize it from the blogging world! Her original quilt was done in blues with different color accents, but we're switching things up and doing it in reds with yellow accents.
Make blocks that measure 12.5 inches by 24.5 inches. That should be the size they are when you hand them over. These dimensions includes seam allowances.
Please keep the fabric solids.
Like I mentioned above, we're doing reds with yellow accents.
Please return blocks at the May meeting.
Feel free to make 1 or as many as you like!
The size might seem daunting, but it's not time consuming! I made my block in about an hour. I can't wait to see how our guild pulls this one together. It's going to be fantastic! Thank you!
For our first charity block of the year, we thought we'd make use of some fabric contributed last year. Even though packets of fabric will be available at our February meeting, we're posting the block instructions now in case any of you would like to sew from stash. Either way, we'd like to have all completed blocks or unused packets returned by the March meeting.
The block for this first giving project is the Improv Quarter Log Cabin, made with black and white prints and a true white solid.The final block size should be 12 1/2″ square. When you square it up, though, feel free to give it some wonk – even more than the sample block is great.
See the post here for full directions!
In an effort to see who wants to participate and how, we have a short survey. Seriously, it'll only take you a very few minutes. Just indicate how you'd like to participate this year, and leave us your contact info so we can be in touch if needed. Thanks for taking the time, and we definitely look forward to sewing for good with you this year!


text:
Битка код Кустоце вођена је 23-25. јула 1848. године између војске Аустријског царства са једне и војске Сардиније са друге стране. Део је Италијанских ратова за независност, а завршена је победом Аустријанаца.

Увод

После заузећа Виченце и добијених појачања, аустријски фелдмаршал Радецки је 22. јула поново кренуо у офанзиву. Сардинска војска под краљем Карлом Албертом је средином јула била развучена од Говернола на Поу до Риволија. Четири дивизије под генералом Бавом стајале су пред Мантовом; 2. корпус под генералом Де Сонацом код Сомакампање; коњица и Тосканци јужно од Вилафранке, а ломбардијске трупе на предделима Минча. Са трупама (око 4000 људи) у горњој долини Кијеза и у Валтелини сардинска војска бројала је укупно око 77.000 људи. Радецки је решио да пробије непријатељску средину код Соне и Сомакампање. Аустријанци су 23. јула код ових места ударили на делове сардинског 2. корпуса и освојили ивичне висове брежуљкастог земљишта. Де Сонац је свој корпус повео на десну обалу Минча. Аустријски 2. корпус је увече био код Кастелнуова, 1. корпус у простору Олиози, Салионце, Кустоца, а 1. резервни корпус генерала Вохера код Сан Ђорђа. Аустријска бригада генерала Зимбшена новообразованог 4. корпуса стигла је са југоистока у Бутапијетру. Радецки је намеравао да настави пробој и да са 2. корпусом пређе Минчо, а 1. корпус да штити јужни блок. На другој страни, сардински 1. корпус није прешао Минчо да би се спојио са 2. корпусом, па је краљ код Вилафранке прикупио 4 бригаде и коњичку дивизију да би напао непријатеља у бок. Сардински напад од Вилафранке према ивичних висова Кустоца-Сомакампања 24. јула погодио је бригаду Зимбшен, која је од Бутапијетре наставила марш према североистоку, и одбацио је према северу. Увече су Сардинци били за леђима аустријских главних снага. У међувремену је Радецки 24. јула код Салионца форсирао Минчо и пребацио укупно четири бригаде 1. и 1. резервног корпуса на западну обалу. Оне су се осигурале према Пескијери и пошле за сардинским 2. корпусом који је са главнином кренуо према Волти. Остале бригаде аустријског 1. и 1. резервног корпуса биле су 24. јула увече у Валеђу и Олиозију. Армија Радецког се дакле налазила на обема обалама Минча, али у једној групи, док је сардинска била аустријском армијом поцепана на два дела, а трећи се налазио код Мантове.

Битка

Успехом Сардинаца против бригаде Зимбшен аустријска армија је угрожена с бока и леђа, а веза са Вероном ила је у опасности. Радецки је очекивао да ће пораз сардинског 2. корпуса привући остале сардинске снаге да се повуку на западну обалу Минча. Међутим, краљ је предузео успешан противудар у опасном правцу и Радецки је одустао од надирања према западу. Задржавајући запоседнуте делове преко Минча, решио је да са главнином нападне противника код Кустоце и Сомакампање. Карло Алберт, не знајући ништа о догађајима на Минчу западно од њега, решио је да идућег дана настави напад у бок и леђа Аустријанаца. На појачања није могао рачунати. Своју резерву оставио је у Вилафранки, а 1. корпус је требало да наступа према Валеђу.

Ове обостране одлуке довеле су 25. јула до наставка битке. Сардинске бригаде које су нападале на линију Валеђо-Кустоца-Сомакампања бачене су убрзо у одбрану. Аустријанци, затим, прелазе у напад. Уздрмали су цео сардински фронт. Сардинци се повлаче у току ноћи. Губици: Аустријанци: 2838, Сардинци 1139 људи. Већи губици Аустријанаца објашњавају се поразом бригаде Зимбшен.

Види још
 Италијански ратови за независност
 Битка код Кустоце
 Револуције 1848-1849

Извори

 Војна енциклопедија, том 5 (99—100)

Револуционарна 1848.
1848.

redpajama_set_name: RedPajamaWikipedia


text:
Golf is booming because of the pandemic
At the beginning of 2020, golf courses were seeing business as usual. There was no big nationwide increase in the number of rounds of golf played, according to data from Golf DataTech. There was no indication that this would be the biggest year yet for the recreational sport.
But when everything came to a standstill because of the pandemic, things changed.
When states started reopening in late April and May, sprawling, socially distanced golf courses were one of the first "safe" spaces that were able to get back to business. Interest in the sport quickly followed.
In May, the number of reported rounds of golf in the US — defined by Golf Datatech as a single authorized "start" at a self-reporting club or facility — rebounded from a 42.2% decline during lockdowns to a 6.2% increase over last year.
Then, rounds began to surge. Since June there have been over 50 million incremental rounds of gold played, according to the National Golf Foundation. October's year-over-year numbers are the greatest yet adding just over 11 million additional rounds for the month than in 2019.
In fact, the NGF reports there's only been one other year that saw a bigger rise in interest in the sport: 1997, the year Tiger Woods became a massive sensation.
Equipment sales are surging
But rounds played is not the only indicator of growth in the golf industry. Equipment sales also surge. The industry hit an all time high of $388.6 million in sales in July, according to Golf Datatech.
"It's amazing to see the growth the sport has experienced — even in the face of a global pandemic. The fact that people can play safely, get outdoors, social distance, etc. is certainly positive. Although retail has experienced an uphill battle this year, we've seen tremendous demand in our online channels," Adidas Golf President Jeff Lienhart told the NGF.
Mike Jakob, CEO of Swing King, a tech company that sets up automatic hole-in-one contests at golf courses, said his company saw sales increases of 20% to 50% for some regions and an overall market growth of 50% to 300%.
July and August saw the two best months for golf sales since Golf Datatech started recording equipment data in 1997.
"We have never seen a surge like what has happened in the summer of 2020, coming out of the worldwide shutdown from COVID-19," said John Krzynowek, Partner, Golf Datatech in a news release.
"The August sales record, which followed an all-time record month in July, is great news for the industry moving forward. It indicates how popular golf is today, especially as an ideal social distancing activity. Newcomers are coming into the game, existing golfers are playing much more, and those who once played but left for a while are returning, which is the perfect combination to drive rounds played and spike equipment sales at retail."
Viewership is some of the best in years
In addition to actual play, 2020 also saw a big boost in golf viewing.
In August, ESPN announced that the ratings for the 2020 PGA Championship were the best they had been in five years.
The first round of the tournament averaged 1,246,000 viewers, making it the event's most viewed first round telecast since 2015, and the second best opening round in the last 10 years. The second day of broadcast, viewership rose another 42%.
Even ESPN's College Gameday broadcast from the Masters for the first time ever, and gained a 31% increase in viewership from all of its other shows in 2020, according to ESPN's Bill Hofmeier.
If one had to pinpoint the moment the current golf renaissance truly began, they might look to early May, when golf greats Tiger Woods and Phil Mickelson teamed up with NFL greats Peyton Manning and Tom Brady for "The Match II," a special charity golf event at at Shadow Creek Golf Course in Las Vegas. (The original "Match," between Woods and Mickelson, was held in 2018.)
For many people, it was the first live sports event they had seen in months, and it showed. "The Match II" automatically became a major topic of discussion online and in living rooms across the country. Content related to the event trended on Twitter all day as people bonded over a moment of familiarity in an increasingly unfamiliar and tragic age.
The numbers just drove home the win. All in all, "The Match" brought in an average of 5.8 million TV viewers — the most-viewed golf event ever.
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