text:
\section{Introduction}

Understanding the evolution of galaxies over cosmic time must include both the amounts and metallicities of gas infall and outflow in order to understand details of stellar evolution (e.g., the `G-dwarf problem') and star formation in galaxy disks as well as the direct observations of these gas flows around galaxies (starburst and AGN winds and infalling high velocity clouds).  Understanding the kinematics and constituency of this `circumgalactic medium' (CGM) is also critical for understanding the more remote `intergalactic medium' (IGM), wherein resides the bulk of the baryons ($> 80\%$) in the local Universe ($ z\leq 0.1$). Until recently our knowledge of gas flows around galaxies has been severely limited to that portion of the CGM (e.g., hot X-ray coronae and optical emission line filaments) that can be seen at high contrast in emission very near some galaxies.

But for several decades large-aperture ground-based optical telescopes have studied in great detail the plethora of absorption lines (several hundreds per unit redshift) in the spectra of distant QSOs and quasars. These absorption lines of \ion{H}{I} (in the Lyman lines) and light metals (mostly in strong resonance lines like \ion{C}{II} 1335~\AA, \ion{C}{III} 977~\AA, \ion{C}{IV} 1548,1551~\AA, \ion{Si}{III} 1206~\AA, \ion{Si}{IV} 1398,1402~\AA, and \ion{O}{VI} 1031,1038~\AA) have allowed us to characterize some of the more basic properties of the CGM and IGM from $z = 1.8$--6. However, optical detections of the strong near-UV \ion{Mg}{II} doublet (2796, 2803~\AA) at $z \geq 0.2$ in conjunction with spectroscopy of the far-UV transitions listed above have also begun to set strong constraints on the nature of the CGM.

The advent of the {\em Hubble Space Telescope} (\hst) and its UV spectrographs has provided a new method for studying these CGM gas flows directly via absorption lines in the spectra of bright AGN targets close on the sky to relatively nearby galaxies. While previous UV spectrographs aboard \hst, including the recently revived Space Telescope Imaging Spectrograph (STIS), have made some progress on this front, the now successfully-deployed, tested, and calibrated Cosmic Origins Spectrograph (COS) will revolutionize studies of galaxy infall/outflow due to its 10--20 times greater sensitivity than STIS at comparable spectral resolution ($R \approx 18\,000$; Froning \& Green 2009). This greatly enhanced sensitivity is already allowing high signal-to-noise (${\rm SNR} \sim 20$--50) spectra to be obtained in only a few orbits for QSOs too faint to have been easily observed with STIS.

While \hst's UV capability opens these studies to the most recent 75\% of a Hubble time ($z<1.8$), the greatest advantages for CGM and IGM studies is at the very lowest redshifts ($z<0.1$). These very nearby absorbers can provide bright, well-resolved prototypes (including absorption from our own Milky Way) whose detailed study yields the necessary baseline parameters for absorption systems already discovered out to nearly the highest redshifts where galaxies have been discovered. Studies of these nearest of all IGM \& CGM \lya\ and metal-line absorbers also profit from recent, large-angle galaxy surveys that are the most complete at the lowest redshifts. Additionally, a host of techniques can be employed at the lowest redshifts (e.g., \ion{H}{I} 21-cm emission line rotation curves and neutral gas distributions; detailed morphological studies of the absorbing galaxy and even the precise location of the sightline through the absorbing galaxy) which are not possible at higher redshifts.

Here we present new results which further illuminate the detailed properties of a very nearby ($cz =1421$~\kms) Lyman-limit system (LLS; the gas is optically-thick at the Lyman-limit; N$_{\rm H\,I}= 2\times10^{17}$ to $2\times10^{20}~{\rm cm^{-2}}$) due to the nearly edge-on spiral galaxy NGC~3067. This absorber is detected in the UV, optical and radio spectra of the bright quasar 3C~232 projected 11~kpc above the galaxy's nucleus. In a previous paper on this system (Keeney et~al. 2005) we showed that the detailed properties of the LLS are identical to the properties of Galactic high-velocity clouds (HVCs) and so had identified this absorber as an HVC near NGC~3067. Although the \ion{H}{I} 21-cm rotation curve for NGC~3067 strongly suggests that the kinematics of the LLS are {\bf infalling} onto the disk of the galaxy, the importance of this inference for understanding HVCs and accretion flows onto normal galaxies requires us to revisit this conclusion using new data. Newly obtained \hst/WFPC2 \Ha\ and continuum images of NGC~3067 allow us to determine the orientation of the galaxy disk in space and to solidify our previous conclusion that the LLS is CGM gas being accreted by NGC~3067. Using this system as a prototype for more distant LLSs found using strong \ion{Mg}{II} absorbers at higher redshifts, we then use this result to place observational constraints on the so-called `cold mode accretion' (CMA) seen to dominate gas accretion onto galaxies in current epoch numerical simulations.

We begin this paper by introducing results on another very nearby QSO/galaxy pair PKS~1327--206/ ESO~1327--2041, which illustrates both the many advantages of studying very nearby absorption systems and also the limitations. In Section~3 we present the new \hst\ images of the 3C~232/NGC~3067 system and the direct inferences it allows for constraining the nature of this absorbing cloud and its status as an HVC in another galaxy. In Section~4 we discuss this result in the context of the significant dataset on \ion{Mg}{II}/LLSs amassed by ground-based studies.  Section~5 discusses the future of this work.

\section{PKS~1327--206/ESO~1327--2041: A Very Nearby Damped \lya\ System}

Figure~1 is a composite {\em B}-, {\em R}-, and {\em I}-band \hst/WFPC2 continuum image with ground-based \Ha\ from the Apache Point 3.5-m overlaid in red, showing the projection of a bright quasar ($z=1.169$) onto an outer spiral arm 14~kpc from the nucleus of a strongly interacting lenticular plus spiral galaxy system ($cz=5340$~\kms). In this paper we summarize some of our conclusions involving the high column density absorption systems detected in the optical/UV and radio spectra of the quasar in order to set the context for our 3C~232 discussion. But this is clearly an unusual system, a `polar-ring' galaxy. In their catalogue of similar systems, Whitmore et~al. (1990) find that only 0.5\% of nearby S0 galaxies exhibit polar ring structures like the one seen in Figure 1. A detailed discussion of this system can be found elsewhere (Keeney et~al. 2010).

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=0.58, angle=0]{f1.eps}
\caption{\small A composite {\em B}-, {\em R}-, and {\em I}-band \hst/WFPC2 continuum image of the PKS~1327--206/ESO~1327--2041 system with ground-based \Ha\ from the Apache Point 3.5-m overlaid in red. Notice that the QSO sits behind a relatively undisturbed spiral arm (Figure reproduced from Keeney et~al. 2010).}
\end{center}
\end{figure}

All indications are that this is a very strong interaction/merger in progress (note the tidal tail to the north and that the \ion{H}{II} regions are seen both in front of and behind the lenticular starlight component). So while the spiral arm/tidal tail in front of the quasar appears relatively undisturbed, its kinematic relationship to the gaseous spiral disk is uncertain; e.g., note that this outer spiral arm has a different pitch angle than the inner, more tightly-wound spiral arms. The UV and optical spectroscopy detects two absorption components at $cz = 5250$ \& 5500~\kms\ in various low-ionization metals including \ion{Mg}{II}, \ion{Fe}{II}, \ion{Ca}{II} and \ion{Na}{I} (Bergeron et~al. 1987; Keeney et~al. 2010). We also detect two \ion{H}{I} 21-cm absorption components at these same recession velocities (Figure~2). The strength of these two components predicts N$_{\rm H\,I} \geq 2\times10^{20}~{\rm cm^{-2}}$ for $T_{\rm spin} = 300$~K, which suggests that this overall system is a damped-\lya\ absorber (DLA), many of which have been discovered at high-$z$ (Wolfe, Gawiser, \& Prochaska 2005; Prochaska et~al. 2007). The lower velocity absorber is a likely LLS. However, we cannot confirm the DLA/LLS identifications without doubt because the wavelength of the associated \lya\ absorption is blocked by the presence of a higher redshift ($z=0.85$) LLS.

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=0.35, angle=0]{f2.ps}
\caption{\small The redshifted \ion{H}{I} 21-cm spectrum of the quasar PKS~1327--206 showing two components of absorption. The vertical dashed lines identify the velocities of the optical and UV metal-line absorptions from Bergeron et~al. (1987) and Keeney et~al. (2010). The faint \ion{H}{II} regions just NNW of the quasar have velocities similar to the broad \ion{H}{I} absorption (5500~\kms), and so we identify that \ion{H}{I} component with disk gas and the 5250~\kms\ \ion{H}{I} as an HVC.}
\end{center}
\end{figure}

The opportunity to observe a DLA very nearby offers additional insights provided by the high-resolution imaging, ground-based spectroscopy, and \ion{H}{I} VLA imaging spectroscopy only possible to obtain in this detail at very low-$z$. We identify the broad, and potentially multi-component, \ion{H}{I} 21-cm absorption line at 5500~\kms\ with disk gas associated with the outer spiral arm in ESO 1327--2041, which we detect at similar velocities in \ion{H}{I} emission. Additionally, faint \ion{H}{II} regions NNW of the quasar along the spiral arm (seen in Figure~1) have similar velocities to the 5500~\kms\ metals + \ion{H}{I} absorber, confirming our identification of this component as disk absorption. Therefore, we identify the 5250~\kms\ absorber with an HVC, but the kinematic status of the HVC gas is uncertain.

While the orientation of the disk is established by the relationship of the \ion{H}{II} regions to the lenticular bar, the interaction/merger (and tidal tail stream to the north) suggest that significant anomalous gas motion is present in this system. So, while the galaxy orientation (SW edge is closer to us) and blue-shifted HVC gas suggest outflowing gas with respect to the underlying disk, this is far from certain since both the location (in front of or behind the disk from our point of view) and plane of motion of the HVC cloud relative to the disk gas is also uncertain. It seems quite unlikely that there are enough supernovae so far out in this spiral arm to drive a wind of several hundred \kms. Thus, a tidal origin for this high-velocity gas seems more plausible in this case. But we cannot make a strong case that all this HVC gas is infalling; evidently, both a fortuitous orientation and also a simple kinematic (i.e., not strongly interacting) system are required to make an unambiguous determination of an absorber's kinematics relative to a nearby galaxy. This is why the rare opportunity provided by the 3C~232/NGC~3067 system is so important to study in detail.

\section{3C~232/NGC~3067: An HVC Falling into a Nearby Galaxy}

This low redshift system (Figure~3) consists of the very nearby SAB galaxy NGC~3067 ($cz=1465$~\kms) and the quasar 3C~232 ($z=0.53$) projected 11~kpc above the galaxy's nucleus. Due to the proximity of this bright quasar to the galaxy, this system has been the object of several studies over the years (Haschick \& Burke 1975; Boksenberg \& Sargent 1978; Stocke et~al. 1991; Carilli \& van Gorkom 1992; Tumlinson et~al. 1999; Keeney et~al. 2005). Attention to this system was first brought by Burbidge et~al. (1971) who used this and three other examples to argue for the non-cosmological redshift hypothesis. Detections of \ion{H}{I} 21-cm (Haschick \& Burke 1975), \ion{Ca}{II} (Boksenberg \& Sargent 1978) and \ion{Na}{I} (Stocke et~al. 1991) absorption at the redshift of NGC~3067 followed, including the discovery of multiple components in \ion{Na}{I} and \ion{Ca}{II} (Stocke et~al. 1991). The strongest of these three components is coincident with the \ion{H}{I} 21-cm absorber.

An \ion{H}{I} 21-cm VLA image (Carilli \& van Gorkom 1992) of this system shows an \ion{H}{I} emission cloud at the position of the quasar, a large diffuse halo of \ion{H}{I} surrounding the galaxy, and a discrete cloud $\sim\,$5~kpc in size located immediately in front of 3C~232. These VLA observations also provide an accurate \ion{H}{I} rotation curve for the galaxy, including velocities into the low halo. Arecibo, VLA and VLBA \ion{H}{I} absorption spectra in conjunction with a damped \lya\ profile from STIS yield a column density of $N_{\rm H\,I} = 1\times10^{20}~{\rm cm^{-2}}$ (making this absorber a LLS, nearly a DLA) and $T_{\rm spin}=500$~K, consistent with the gas kinetic temperature from the \ion{H}{I} 21-cm linewidth (Keeney et~al. 2005). Other \hst\ UV spectra detect three components in both low- and high-ionization lines including \ion{Si}{IV}, \ion{C}{IV}, \ion{Fe}{II}, \ion{Mn}{II}, \ion{Mg}{II} and \ion{Mg}{I} (Tumlinson et~al. 1999; Keeney et~al. 2005).

A summary of the observable properties of the strongest absorber (the \ion{H}{I} 21-cm absorber) in this system made by Keeney et~al. (2005) finds a very striking parallel with the properties of HVCs around our own Galaxy. Specifically, the kinematics, size, temperature, gas density, location and metallicity of this very nearby LLS are consistent with this absorber being an HVC. The other two absorbers could also be HVCs, or possibly the more abundant, lower \ion{H}{I} column density highly-ionized HVCs (Sembach et~al. 2003; Richter et~al. 2009; Shull et~al. 2009).

Tumlinson et~al. (1999) used the non-detection of the \ion{H}{I} 21-cm absorbing cloud (see also Stocke et~al. 1991) in \Ha\ emission and the absorption line strength ratios (particularly \ion{Fe}{II}/\ion{Fe}{I}) to set both upper and lower limits on the intensity of the  $z=0$ extra-galactic ionizing radiation field. This analysis also yielded a limit on the percentage of ionizing radiation escaping upwards from the disk to the location of this cloud ($<2\%$) consistent with other attempts to measure this quantity at low-$z$.  While the limits of Tumlinson et~al. (1999) and Stocke et~al. (1991) are larger than the expected \Ha\ surface brightness of a cloud irradiated by the extragalactic background (Bland-Hawthorn \& Maloney 1999), the discovery of \Ha\ emission associated with the Magellanic Stream has shown that the disruption of clouds moving through a hot galactic halo can enhance \Ha\ emission (Bland-Hawthorn et~al. 2007).  The absence of \Ha\ emission from the \ion{H}{I} cloud projected onto the quasar or between the galaxy and the quasar on the sky suggests that there is no strong outflowing starburst wind or shock heating due to an infalling cloud impacting a hot gaseous halo, and so this non-detection favors neither hypothesis.  But the question about whether these absorbers are infalling or outflowing depends critically upon the orientation on the sky of this galaxy since very accurate radial velocities are available from the \ion{H}{I} 21-cm emission and absorption.

In Keeney et~al. (2005) we concluded that we are viewing the underside of NGC~3067 based upon the observed \ion{H}{I} rotation curve of Carlli \& van Gorkom (1992). This orientation implies that the blueshift of the \ion{H}{I} 21-cm absorber relative to the \ion{H}{I} systemic velocity of NGC~3067 means that the absorbing cloud is {\em infalling} onto the galaxy disk. The simplest model for these three absorbers, in which all total space velocities are perpendicular to the galaxy disk, finds the strongest system to be infalling at $-115$~\kms. The other two systems are one infalling and the other outflowing, although even for the latter the inferred outflow velocity is less than the escape velocity at its location above the disk. Thus, for this rather normal spiral galaxy there is no evidence for outflowing gas from the nucleus that escapes the galaxy's gravitational potential, and two of the three clouds are infalling gas being accreted onto the galaxy disk. By the perpendicular motion assumption, the third system will also return to the galaxy disk as a `galactic fountain'. Therefore, all the observed CGM gas detected in front of 3C~232 is a sampling of the total amount of CGM being accreted by NGC~3067 at this time or in the near future.

Based upon similar UV absorption line spectroscopy with \hst/STIS and {\sl FUSE} of targets above and below our own Galactic Center, Keeney et~al. (2006a) come to similar conclusions for the Milky Way's Galactic wind; i.e., the outflowing gas on either side of the nucleus will not escape from the potential well of our Galaxy, rising to $\approx12.5$~kpc before returning to the disk like a fountain. These two examples are consistent with the Steidel (1995) hypothesis that LLS absorbers are the bound halos of luminous ($\sim {\rm L}^*$) galaxies. If this inference is correct, then these large galaxies are not the primary contributors to metals and energy in the low-$z$ IGM. We can also infer that LLSs are a sampling of the total amount of gas in the CGM that will eventually fall onto large galaxies to stimulate and enrich their star formation. Therefore, it seems worthwhile to confirm that the 3C~232/NGC~3067 LLS is infalling gas.

Figure~3 shows the \hst/WFPC2 {\em I}-band (F791W) image based on 2400~secs of observing time. The pure \Ha\ image shown in Figure~4 is based on 14\,400~secs of integration time in the F658N [\ion{N}{II}] filter minus the scaled {\em I}-band image. The F658N filter has a bandpass of 29~\AA\ FWHM centered at 6591~\AA\ and so contains only \Ha\ at the redshift of NGC~3067. The filter throughput is 79\% (its peak throughput) for \Ha\ throughout the velocity range of the disk of NGC~3067 seen in the \ion{H}{I} 21-cm images of Carlli \& van Gorkom (1992). The limiting fluxes for these two images are: (1) an {\em I}-band limiting magnitude (3$\sigma$) of $I_{\rm limit} = 26.0$ and (2) a 3$\sigma$ \Ha\ flux limit of $F({\rm \Ha})= 2 \times10^{-18}$ ${\rm ergs\,cm^{-2}\,s^{-1}}$. The latter limit corresponds to an \Ha\ luminosity of ${\rm L(\Ha)} = 1\times10^{35}~{\rm ergs\,s^{-1}}$ for an unresolved source ($<15$~pc) at the Hubble-flow distance to NGC~3067, which is about 0.3\% of the luminosity of the Orion Nebula, ${\rm L(\Ha)} \approx 3\times10^{37}~{\rm ergs\,s^{-1}}$. This limit corresponds to a star formation rate of $\sim 10^{-6}~{\rm M_{\odot}\,yr^{-1}}$ (Kennicutt 1998).

Also, there is no indication at all for \Ha\ emission knots between the disk of NGC~3067 and 3C~232 on the sky down to the 3$\sigma$ limit quoted above. The ground-based limits on diffuse \Ha\ from the \ion{H}{I} cloud in front of 3C~232 are exceptionally deep and place excellent limits on the flux of the extragalactic ionizing radiation at $z=0$ of $\Phi(\rm ion) \leq 80\,000~{\rm photons\,cm^{-2}\,s^{-1}}$ (Stocke et~al. 1991; Tumlinson et~al. 1999). But very small-scale emission features associated with extra-planar \ion{H}{II} regions or with gas collisionally-ionized by an outflowing wind from the disk could have been missed. However, we find no such emission knots in our pure \Ha\ image (Figure~4) so that there is no observational evidence supporting the hypothesis that the LLS cloud in front of 3C~232 was expelled by either a very active recent episode of star formation or an AGN, now dormant. If this were the case we would expect to see shock-heated gas above the plane of NGC~3067 on both sides of the nucleus as has been commonly observed in starburst galaxies (Veilleux, Cecil, \& Bland-Hawthorn 2005).

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=0.2, angle=0]{f3.eps}
\caption{\small \hst/WFPC2 {\em I}-band image of NGC~3067.  The position of the nearby quasar 3C~232 and the orientation of the image have been labelled.  The white circles (1~arcsec radius) mark the two possible nuclear positions (NW position preferred) discussed in the text.  The field of view of the image is approximately $150\times150$~arcsec, which corresponds to $15\times15$~kpc at the redshift of NGC~3067.}
\end{center}
\end{figure}

We can also use the pure \Ha\ image in Figure~4 to support the hypothesis that we are viewing NGC~3067 from underneath its disk; i.e. the southern edge is more distant from us. We have tested this hypothesis in two simple ways, by counting the \ion{H}{II} regions above and below the nucleus of the galaxy and by measuring the integrated \ion{H}{II} region \Ha\ flux on these two sides. We identify the nucleus of NGC~3067 using the dynamical center of the galaxy as inferred from the \ion{H}{I} 21-cm emission map (Carilli, van Gorkom \& Stocke 1989). Carilli et~al. do note that the dynamical location for the nucleus is well west of the apparent isophotal center suggesting that the galaxy's eastern edge has been truncated by a recent interaction.  While there is a large complex of \Ha\ emission and obscuration at that location (see Figure~3), there is no clear nuclear bulge visible to support this identification. The total {\em I}-band luminosity within 1~arcsec of that location is $(6.54\pm0.06)\times10^{7}~{\rm L_{\odot}}$. However, the only plausible alternative to this identification are the semi-stellar knot to the SW and its accompanying \ion{H}{II} region, which have a total {\em I}-band luminosity of $(2.29\pm0.02)\times10^{7}~{\rm L_{\odot}}$. These are also marked in Figure~3.

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=0.2, angle=0]{f4.eps}
\caption{\small \hst/WFPC2 \Ha\ image of NGC~3067.  The orientation of the image has been labelled. The faint dots north of NGC~3067 are the incomplete subtractions of the quasar and a bright field star (see Figure~3) and not \Ha\ emission.}
\end{center}
\end{figure}

Once the nucleus is identified, the interpretation of this image with respect to the galaxy orientation is straightforward; the more distant side suffers greater obscuration so that the numbers of \ion{H}{II} regions and their luminosities are diminished. We place a dividing line between the north and south sides through the nucleus along the major axis of the galaxy as defined by the outer ($>10$~arcsec from the nucleus) isophotes. The results of these measurements are that the ratio of \ion{H}{II} region numbers and integrated luminosities top/bottom are: $2.55\pm0.32$ and $1.44\pm0.01$, where the standard deviations are root-N in numbers and counts in the image. In these determinations we have used only the portion of the galaxy on either side of the major axis for which both the top and the bottom are fully on the CCD image. If we had used the small stellar emission knot to the SW (see above), these ratios would have been substantially larger. Both measurements clearly support the previous conclusion of Keeney et~al. (2005) based upon the \ion{H}{I} rotation curve as well as a visible inspection of Figures~3 \& 4, in which the entire south-west side of the galaxy disk appears truncated by a large-scale swath of obscuration most easily seen in Figure~3. We conclude that we are viewing the underside of NGC~3067 and that the LLS detected in optical/UV lines as well as \ion{H}{I} 21-cm absorption is infalling onto the galaxy disk.

In addition, we use the red starlight in Figure~3 to calculate an improved axial ratio of the galaxy disk. Averaging the ellipticity for all isophotes with semi-major axes $>10$~arcsec from the nucleus yields an axial ratio of $0.35\pm0.01$, corresponding to a disk inclination of $73\pm1$~degrees, slightly larger than the $68^{+4}_{-3}$~degrees advocated by Rubin et~al. (1982) and used by us previously. The full spread of axial ratios seen in the outer disk covers a range of 12 degrees around our measured average, so there is no indication that the \hst\ image provides a much improved inclination angle for NGC~3067.

In any case, the kinematic derivations for the absorbers do not change much at all. At this new inclination angle the derived velocities of the metal-line absorbers (assuming motion only perpendicular to the disk) are: $-330\pm40$, $-160\pm30$ and $+220\pm50$~\kms, somewhat larger than the values we derived earlier based upon the Rubin et~al. (1982) inclination value. This new inclination angle places the absorbers at a minimum height above the plane of NGC~3067 of $11.7\pm0.1$~kpc. Given the revised dynamically-determined mass of NGC~3067 of $(1.3\pm0.2)\times10^{11}~{\rm M_{\odot}}$ yields an escape velocity at 11.7~kpc of $310\pm25$~\kms. Our conclusion remains that given only perpendicular motion for these three clouds, even the outflowing CGM gas does not escape from NGC~3067. Relaxing the perpendicular motion assumption could allow this one gas cloud to escape from the galaxy for a fairly wide range of outflow angles, although at this height above the galaxy's disk we would expect any starburst or AGN wind to become collimated sufficiently so that the velocity vector is quite close to being purely vertical from the disk (e.g., MacLow \& McCray 1988).

\section{Discussion}

For many years it has been suggested that the ultimate promise of QSO absorption-line studies is to extend our detailed knowledge of local galaxies out to $z > 5$, where the highest redshift absorbers are found. The nearly flat selection function of absorption lines with redshift allows absorbers to be counted and their physical conditions assessed at whatever redshift distance they can be observed. In the current instance, the population of \ion{Mg}{II}/LLS absorbers has been studied in some detail by Bergeron \& Boiss\'{e} (1991), Steidel and Sargent (1992), Churchill et~al. (1999, 2000), Steidel et~al. (2002), Churchill, Vogt \& Charlton (2003), Kacprzak et~al. (2010) and others at $z=0.2$--2.0. For the current discussion we assume that the strong (rest-frame ${\mathcal W}_{\lambda} \geq 0.3$~\AA) \ion{Mg}{II} absorbers are synonymous with LLSs.

In the large survey by Steidel \& Sargent (1992) DLAs comprise $<10\%$ of their strong \ion{Mg}{II} sample; the remainder are LLSs. Steidel (1995, 1998) found that 55 of his 58 absorbers with rest-frame Mg II equivalent widths $\geq0.3$~\AA\ in his sample at $0.2 \leq z \leq 1$ were associated with bright (${\rm L} \geq 0.1 {\rm L}^*$) galaxies at the same redshift within a projected distance of 50$\,h^{-1}$ kpc. The few absorbers without bright galaxy associations have been found to be DLAs, probably due to the sightline directly penetrating the disk of both luminous and dwarf galaxies so that the background QSO continuum makes the foreground galaxy hard to spot. The LLSs, being offset from the galaxy disk and being associated with luminous galaxies, means that the associated $\sim {\rm L}^*$ galaxies are much easier to detect.

So, while the prima facie evidence is that LLSs are exclusively due to gas in the halos of luminous galaxies, McLin, Giroux \& Stocke (1998) used the Steidel (1995, 1998) statistic that 55 \ion{Mg}{II} absorbers in his sample are associated with $\geq 0.1 {\rm L}^*$ galaxies to conclude that LLSs could not be associated with dwarf galaxies {\bf at all}. Physically, the gas giving rise to a LLS is likely within a gravitationally-bound halo because the ionization energy of \ion{Mg}{II} is so close to that of \ion{H}{I} (15.0~eV compared with 13.6~eV). This means that any high column density \ion{Mg}{II} absorber must be successfully shielded from the extragalactic ionizing radiation field. An outflowing wind that smoothly varies in density (i.e., no clumps) will rapidly expand, lose its self-shielding and \ion{Mg}{II} ions will be quickly ionized to become \ion{Mg}{III}. This simple picture suggests that massive galaxies have bound gaseous halos and dwarf galaxies possess unbound winds, but these ideas need to be tested by observing other examples of LLSs and more highly-ionized metal-line systems associated with dwarfs and ${\rm L}^*$ galaxies at low-$z$ with \hst.

In the most recent work on \ion{Mg}{II}/LLSs, Kacprzak et~al. (2010) come to quite similar conclusions as we do here from the 3C~232/NGC~3067 system alone. Based on their \hst\ imaging and beautiful ground-based spectroscopy of $\sim {\rm L}^*$ galaxies nearby to low-$z$ LLSs (but at significantly higher redshifts than our prototype system NGC~3067), Kacprzak et~al. find:
\begin{enumerate}
\item The \ion{Mg}{II} absorption almost always falls on one side or the other of the galaxy's velocity centroid. This requires that almost all of the \ion{Mg}{II}/LLS absorption is either infalling or outflowing and is rarely a combination of both.
\item These authors also show that the absorbing clouds seen as strong \ion{Mg}{II} absorbers are HVCs in the sense that their velocities exceed the velocity of the disk gas `beneath them' (see also, Steidel et al. 2002).
\end{enumerate}
Further, the vector from the galaxy to the QSO (and thus to the absorbers) is rather randomly oriented with respect to the galaxy disk. It seems unlikely that an outflowing wind would be spherically symmetric around a large disk galaxy given the strong density gradients which orient an outflowing wind rather quickly into a perpendicular wind (e.g., MacLow \& McCray 1988).

Therefore, we conclude that the Kacprzak et~al. results are suggestive that LLSs are dominated by infalling gas. However, lacking either detailed \ion{H}{I} 21-cm rotation curves or imaging with high enough physical resolution to determine galaxy orientation in the Kacprzak et~al. sample without doubt, it cannot be proven as yet whether the gas is infalling or outflowing in these cases. Despite these limitations, we note that the Kacprzak et~al. results are fully consistent with our interpretations of the nearby example of 3C~232/ NGC~3067.

It has been known for some time that the number of strong \ion{Mg}{II} absorbers per unit redshift is relatively constant with redshift ($dN/dz \approx 1$ per unit redshift; although the very strongest \ion{Mg}{II} absorbers do appear to exhibit significant cosmological evolution; Steidel \& Sargent 1992; Rao \& Turnshek 2000), requiring that the product of the number of sites for these absorbers, their area on the sky and their covering factor within that area does not vary significantly from $z=0.2$--1.0. If luminous galaxies are the sites for these absorbers, it is reasonable to expect that the numbers of sites for strong \ion{Mg}{II} systems would be relatively constant with look-back-time since these galaxies are already in-place by redshifts of one or higher. A constant number of strong \ion{Mg}{II} absorbers and a constant number of sites requires that the area on the sky $\times$ the covering factor of these absorbers is also constant over the time interval from $z=0$--1. This suggests that massive galaxy halos have seen little change in the last few Gyrs.

Theoretical modelling of massive galaxy halos and cold gas clouds within them have the clouds forming either by cooling instabilities in a pre-existing hot halo (Kere\u{s} \& Hernquist 2009) or near the transition between an ionizing background dominated by extra-galactic sources and one dominated by local sources (Giroux \& Shull 1997). In either case, the radius at which these transitions/instabilities occur is not expected to change dramatically with redshift, in agreement with the \ion{Mg}{II}/LLS absorber statistics. But, what does change somewhat is the number of absorbers per LLS.

\ion{Mg}{II} absorptions are so highly saturated that their equivalent width is increased not by an increasing optical depth but by an increased velocity spread within the absorption. This effect has been used by Churchill, Vogt \& Charlton (2003) to estimate the numbers of absorbers as a function of equivalent width. Although there is signficant scatter, these authors find that: $(N/17) \approx {\mathcal W}_{\lambda}$, where $N$ is the estimated number of individual absorption components within any one \ion{Mg}{II} absorption system and ${\mathcal W}_{\lambda}$ is the rest-frame equivalent width (in \AA) of the 2796~\AA\ \ion{Mg}{II} line. And the trend is for there to be more components in \ion{Mg}{II} absorbers at higher redshift by a factor of, $N \propto (1+z)^{0.6}$, not a very strong evolution at all (Nestor, Turnshek, \& Rao 2005). In the context of the results presented here for the LLS prototype 3C~232/NGC~3067, the size of the bound halo and the covering factor of the halo gas in NGC~3067 have not changed significantly but the number of HVC-like clouds either being accreted or as part of a galactic fountain has decreased modestly by a factor of at most 2--3 over the last few Gyrs.

If most \ion{Mg}{II}/LLSs are composed of primarily infalling gas and bound galactic fountain gas like we find for the 3C~232/NGC~3067 system and for our own Galaxy, this helps to explain the \ion{Mg}{II} absorption line velocities seen by Kapcrzak et~al. (2010). This identification also suggests that \ion{Mg}{II}/LLSs are a sampling of the CMA gas rate falling onto these normal, $\sim {\rm L}^*$ galaxies.

If this is the case, the available LLS statistics gathered by Bergeron \& Boiss\'{e} (1991), Steidel \& Sargent (1992), Rao \& Turnshek (2000), Churchill, Vogt \& Charlton (2003), and others can then be used to measure the amount of the CMA (although the simulators call this infalling gas `cold' because it is well below the virial temperature of the massive halo into which it is falling, observers call this `warm gas' because it has both a neutral and an ionized component). Extrapolated down to the current epoch, the \ion{Mg}{II} $dN/dz$ absorber densities account for only about 1/3 to 1/2 of the total CMA predicted by numerical simulations (e.g., Kere\u{s} et~al. 2009).

So, if there is a connection between the observed LLSs and the simulated CMA, the total CMA infall rate must also include more highly-ionized gas than can be observed easily in \ion{Mg}{II}. This more highly-ionized gas recently has been shown to comprise a large fraction of the total accretion onto the Milky Way, $\sim 1~{\rm M}_{\odot}$ per year in ionized gas as traced by \ion{Si}{III} (Shull et~al. 2009) and other ions (Richter et~al. 2009). Furthermore, the predicted increase of the CMA with redshift, i.e., $\dot{\rm M} \propto (1+z)^{2.5}$ (Kere\u{s} et al. 2009), is a much steeper dependence on redshift than the observed \ion{Mg}{II} statistics alone support (see above).

We conclude that the ionized fraction of the CMA must increase rapidly with redshift in order to bring the observations and the results of numerical simulations into even rough agreement. This seems quite reasonable since the intensity of the ambient ionizing radiation field around these clouds is increasing with redshift at a similar rate to the predicted CMA rate. This is true regardless of whether the ambient ionizing radiation is due to the extragalactic ionizing flux or the ionizing flux leaking upward from young stars in the nearby galaxy disk. Given a constant leakage factor ($f_{\rm esc}$) with redshift, the ionizing flux leaking up from the disk is also expected to increase at a similarly rapid rate [i.e., $(1+z)^{2.5}$] because the cosmic star formation rate also increases dramatically between $z=0$--1. This more highly-ionized CMA can be found only by detecting species like \ion{Si}{III}, \ion{Si}{IV}, \ion{C}{IV} and \ion{O}{VI} which are at UV wavelengths for absorbers at $z \leq 1.4$. Thus, UV spectroscopy with \hst\ is required.

\section{The Future is Now}

If big galaxies do not provide most of the metals to enrich the IGM at low-$z$, then dwarf galaxies must be the primary contributors. There is some, but not overwhelming, support for this hypothesis (Stocke et~al. 2004; Keeney et~al. 2006b). But, there also is significant evidence that the much more massive `Lyman-break galaxies' at $z\approx2$--4 have enormous starburst winds that escape into the IGM where nearby metal-line absorbers have been found (Adelberger et~al. 2003). So we expect any conclusions involving the source of IGM metals to remain controverisal and a topic for on-going research. Likewise the types of galaxies which possess bound gaseous halos will also remain controversial. While large-aperture, ground-based spectroscopy can address questions of IGM enrichment and galaxy halos and winds at $z\geq2$ directly, only \hst\ UV spectroscopy can study the low-$z$ IGM and its gas suppliers.

\begin{figure}[!t]
\begin{center}
\includegraphics[scale=0.4, angle=0]{f5.ps}
\caption{\small A comparison between the STIS E140M echelle spectrum (${\rm SNR} \sim 12$) of PKS 0405--123 (bottom spectrum) and a shorter exposure of the same target with COS (${\rm SNR} \sim 50$) on top.  The two spectra have been offset in the y-coordinate for display purposes.  The COS spectrum is a portion of the `Early Release Observations' taken this past summer.  GTO and GO observations with COS are now well underway.}
\end{center}
\end{figure}

This is where the road ahead is quite bright due to the successful deployment of COS on \hst\ this last May. In \hst's Cycle 17 alone there will be $>$ 300 \hst\ orbits of COS observations made by 5 separate proposers (COS GTO Team $+$ 4 GOs) investigating QSO/galaxy pairs to study gas infall and outflow in and around a diverse set of low-$z$ galaxies. These chance projections of QSOs near foreground galaxies will probe the physical condition and kinematics of gas around M~31, around nearby and distant  starburst galaxies, and around normal luminous and dwarf galaxies in the local Universe.  We expect that these new observations will revolutionize this field and give us a much clearer picture of galaxy/gas interactions in the local Universe. We also expect that these and other COS observations will allow the assertions made in this paper based on the observational evidence of a very small number of low-$z$ absorbers to be thoroughly tested.

As a preview of what is to come, Figure~5 shows a pair of spectra of the same target, the bright $z=0.573$ quasar PKS~0405--123. The STIS spectrum has a resolution of 35\,000 and a ${\rm SNR} \sim 12$ based on 27~ksecs of observation. The COS spectrum has $R=18\,000$ and ${\rm SNR} \sim 50$ based on 17~ksecs of observation. Based upon the nominal in-orbit performance of the COS instrument, the next few years should see a substantial change in our understanding of the local IGM, wherein most of the baryons are still lurking. Interesting topics in local IGM studies which will be addressed by COS observations include: which types of galaxies possess outflowing winds that escape into
the IGM, the extent of the spread of metals away from galaxies into the IGM, the metallicity of gas in cosmic voids and the amount of baryons in the shock-heated `warm-hot IGM' (WHIM). The present authors look forward to using \hst/COS to contribute to our better understanding of these topics.

\section*{Acknowledgments} The authors acknowledge the support of an \hst\ guest observing grant GO-10925.01-A and the Cosmic Origins Spectrograph project through NASA's Goddard Space Flight Center (grant \#NNX08AC14G) and the Space Telescope Science Institute.

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What Can You Do If You Are A Philosophy Graduate?
Why should a student study philosophy at the university and obtain a degree? Here you can read the information on what you should study at a philosophy faculty at the university, and what career you do after graduation.
Philosophy at universities gives us the answers to the most fundamental and important questions about the problems of who we are and what are we living for. It examines our lives through the history.
What will you study for a degree?
If you are a university student of the philosophy faculty, a obtaining a degree during the first year you will study common disciplines and wide modules. It will give you a solid background in different fundamental areas, and it will help you to study successfully in the future. And only from the second or even the third year, students start to study special courses or modules that are necessary for them.
Undergraduate courses usually take three or four years. The university student will study philosophy of mind, logic, ethics, metaphysics, political philosophy, philosophy of science, etc. Many modules demand a hard working and writing numerous essays and research papers.
When you study philosophy, you obtain such important skills as critical thinking, logic and effective communication. Studying at the university will give you an ability to analyze all perspectives of the issue and to make a conclusion. So will be able to answer existential question, but where can a graduate with a philosophy degree work.
What kind of jobs are you qualified for?
If you have a university degree, you definitely have mastered the skill of critical thinking after the graduation from the university. This skill along with analytical ability are valued in a great number of business fields. This skill helps to find effective solutions to many problems so it may ensure your career growth after the graduation. Someone may think that there is nothing to do with a philosophy university degree. But this is misleading. If you are a university graduate and have a philosophy degree, there is a great number of careers which are available for you.
Philosophy university graduates may get a job in a great variety of fields with their degree. University graduates are able to work in teaching, politics and public relations. And it's not the end. Students with a philosophy degree after their graduation from the university can be employed in communications, publishing, HR, advertising. Philosophy graduates also may work in business, civil service, scientific projects, banking and even the law. Graduates also can continue further philosophy study and research. Let's talk about the most attractive careers a philosophy graduate can apply for.
Many graduates have built their careers in law. Their skill of analytical thinking and the ability to express thoughts clearly as well as the ability to analyze arguments and distinguish the most important facts help them much in their career. All of these skills are highly valued in this field, and philosophy graduates are welcomed in many law schools. Graduates with philosophy degree are those who have one of the highest rates during acceptance to different law schools.
Careers in this field involve such areas as book publishing, newspapers, and magazine production. The graduates can also be employed in many other media forms. Graduates are not limited in their choices. And due to globalization, information and digital revolution, traditional publishing has to struggle for its existing. The dramatic growth of digital media has worsened the business condition of traditional media, but at the same time has expanded job opportunities of university philosophy graduates. A student with a degree can also get a job in journalism and writing. They can be employed in research work, editing, etc. He can also become a professional writer.
University students have the opportunity to apply for a great variety of reliable positions in different government agencies. It can be the Environmental Protections Agency, the Department of Transportation, and even the Goddard Space Center, etc. Philosophy faculties provide a great number of opportunities for government internships.
In fact, a university degree provides for the graduates a great background and basis for the successful career in teaching at all levels. Graduates can use their skills such as good communication, logic and critical thinking in their teaching career. These skills help them to teach students to develop the same skills which make them successful.
In many countries, you have to obtain a special teaching degree in order to build your career in teaching. But there are some cases in which your philosophy degree will be enough. For example. You can work at private schools.
It is known that graduates with the university degree are well-represented in the medical area as well. They can be employed as administrators and practitioners. It has become a tradition for medical schools to look for candidates with an arts degree. And they prefer graduates from philosophy departments. Philosophy students can make their career in orthopedics, psychiatry, ophthalmology, neurology, dentistry and the ability of analytical thinking five them an opportunity to take part in the cancer research. There are many graduates who work in the health administration.
In fact, business and philosophy seem to be so different and even opposite. But according to the practice, many successful businessmen started their careers with a philosophy degree. If you study this subject after the graduation, you can become a venture capitalist, manager, real-estate broker or stockbroker.
So if you have a philosophy degree, you can choose so many careers in numerous fields with your university degree. Just chose the one which is the most interesting to you. Many doors are open to you.


Many long books are fine, of course, but folks don't like books that just go on and on.
So it wasn't just me.
This fall, I wrote a Bookmark column for Star Tribune books editor Laurie Hertzel, complaining about the too long books that the publishing industry has been churning out lately.
I wasn't dissing all long books. Like most of us, I've read my share of 500- and even 800-plus pagers, and enjoyed them.
What I was whining about was the slew of new, so-called "epic" novels that, while not bad, seemed bloated, as if their authors were stretching to make it to the 500-page mark.
Lots of you, it seems, share my literary dismay.
"When I look at an 800-page book these days, my heart sinks," Francine Marie Tolf wrote in an e-mail. "I can't even open it, no matter how much it has been raved about.
Mary Carolyn Youngquist took aim at publishers who seem to be putting sales ahead of quality.
"A good story just doesn't quite cut it anymore," she wrote. "Today's formula writing, highly influenced by 'what sells,' has worked for some time. Well-crafted stories have helped readers unpack family baggage, deal with the ravages of war and murder, revisit social issues, re-examine political and religious philosophies and 'discover' diversity.
For her part, Kathy Jursik pleaded for tighter editing.
"Books don't need to be 450 to 500 pages!" she wrote. "Like you, I am a devoted reader, but I am also a fan of good editing. I have gotten to the point where I check the page count of a book that interests me, and if it is over 450 pages I dismiss it out of hand.
Shirley Bunde also chimed in about her disdain for big, fat, sweeping novels that don't have the writing power to sustain their lengths.
"Bloated is an accurate description of so many books where, as you say, length seems to be the point," she wrote.
It's the rare book that makes it to the friends-for-life status for most of us. But I'm pretty sure that the ones that do earn the moniker "epic" on the strength of their storytelling, not their length.
Connie Nelson is a features editor at the Star Tribune.
Connie Nelson is the senior editor for lifestyles for the Star Tribune.
Here's where to enjoy quiche, shakshuka, toast "flights" and more.


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Home News stories Names proposed for new elements
Names proposed for new elements
Jennifer Carpenter December 16, 2011	 January 27, 2018
Venue: BBC
Scientists have put forward their suggested names for the newest additions to the Periodic Table.
If the names are accepted, element 114 will become Flerovium (Fl) in honour of the physicist Georgiy Flerov.
While element 116 will become Livermorium (Lv), after the Californian laboratory where it was discovered.
The table's governing body will officially endorse the names in five month's time, 10 years after the elements were discovered.
The newest elements were among a handful of elements put forward for inclusion in the table in recent years.
They were accredited in June this year after a three year review by the International Union of Pure and Applied Chemistry (IUPAC) and the International Union of Pure and Applied Physics (IUPAP).
The other putative heavy elements, 113, 115, and 118, are still under review.
Scientists at Lawrence Livermore National Laboratory (LLNL), in collaboration with a team at the Flerov Laboratory of Nuclear Reactions in Dubna, Russia, discovered the newest additions to the periodic table by smashing calcium ions into the element curium to create element 116, which quickly decays to element 114.
The teams also created element 114 separately by replacing curium with a plutonium target.
IUPAC will officially accept the proposed names after giving the public time to comment on the discoverers' choice.
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The powerhouse vocalist proves yet again there's no song she can't crush.
Whitney Houston's greatness is hard to beat, but Ariana Grande's soaring vocals seem to be a close match for the late R&B queen's talent. Ariana appeared on the ABC concert series Greatest Hits on Thursday and she slayed two iconic songs from Whitney's legendary catalog.
Taking the stage in all black everything, paired with sky-high silver boots just for an added bit of sparkle, the powerhouse vocalist first busted out Whitney's signature track "How Will I Know." Once she wrapped up the flirty single, she kicked up the diva dial all the way by performing "Queen Of The Night" which was featured on The Bodyguard soundtrack.
Actually after watching Ariana perform that medley, she's officially the queen of our weekend playlist. Take a bow, girl. You deserve it.


Love is in the air and the dusitD2 Kenz Hotel in Barsha Heights has devised a truly romantic ensemble of Valentine's Day experiences for you to explore.
Lovers can retreat and forget the hustle and bustle of everyday life – feast with a delicious dinner, relax and unwind with complimentary wellbeing treatments or simply be together in comfort and style at the dusitD2 Kenz Hotel.
Whether it is to celebrate decades of togetherness or newfound love, dusitD2 Kenz presents a tempting offer exclusively tailored for couples that will surprise and delight at every moment of their valentine's experience. Couples are offered to stay in the hotel's luxurious D'Light Rooms for at least two days to enjoy forthcoming offerings including rose water éclairs or Macaroons upon arrival to mark the amorous occasion.
After spending the first night at the hotel, guests will wake up to a delicious room-served breakfast. With the taste buds initially indulged, ladies can then ease into a steamy recluse at the D'Stress Spa, taking the opportunity to unwind and be pampered from head to toe whilst enjoying an indulgent break from the hectic outside world, leaving with a feeling of complete rejuvenation and relaxation. Breakfast the following day will be served in the bright and elegant surroundings of Ostro, their signature dining locale where guests can satisfy their palate on an extensive repertoire of dishes. A return in the evening will also find an opportunity to feast at dinner with a beautifully prepared three-course menu and signature mocktails by Ostro.
The menu is a perfect culinary remedy to settle in lovers and is designed purely with the romantic occasion in mind.
Offering: Minimum two-night stay for two people in the signature "D'Light Room" accommodation with a room-served breakfast on the first day and breakfast buffet on the second. Offer also includes a three-course dinner for two people at Ostro; complimentary WiFi and spa treatment available for the ladies and a gym session for the men. Rose water éclairs or Macaroons will also be gifted upon arrival.
For more luxury events in Dubai and Abu Dhabi click here or to read more about Ostro, click here.
Vida Downtown's Urban Picnic goes Latin this Season!
The World Of Hublot Journeys Through Dubai!


1. After sending two invoices for payment, I sent another and called the client when the receipt that they had received it came back.
CLIENT: Why are you calling me?
ME: You haven't paid and this is the third invoice I've sent.
CLIENT: It's even more than the last one!
ME: Yes. The contract you signed stated that I would add a late fee for payment.
CLIENT: You mean I have to actually pay you? I thought you were joking!
ME: What on earth made you think that?
CLIENT: Well, you work for free! If you were supposed to be paid, you'd be called a paidlancer or something!
13. Client: Hey, just one final question before I send the deposit. Do you use a PC or a MAC?
14. The client sent me two word documents with the same content, for me to use on the website.
ME: Both the documents have the same content. Am I missing something?
CLIENT: Um… can you click faster?
CLIENT: Can you put some cool reds in there?
ME: Red is usually considered very warm.
ME: Any colour can be cool, with the right attitude.
18. CLIENT: Should I send the logo as jpg or jpeg?
ME: I'm joking with you, send it as a png.
CLIENT: Nice try, but I'm not that stupid.
20. CLIENT: Can our customers visit our website while they're in our restaurant?
ME: Of course, they can visit the website on their smartphone or laptop. Does your restaurant have WiFi available for customers?
CLIENT: No, not yet. But maybe you can put WiFi on our website?


The Laser design rights have reverted back to Bruce Kirby from Global Sailing. And Bruce hopes to work to get the builders back on track and resolve the dispute that arose around these design rights. It remains to be seen whether this really does resolve the issue, but best of luck to Bruce.
Our own Canterbury Master Radial Sailor Hamish Atkinson has won the 2010/2011 Mader Trust Canterbury dinghy sailor of the year, and gone on to win the major trophy of Mander Trust Canterbury Yachtie of the year.
Nice job Hamish - great to have a Laser sailor winning overall.
Andy Maloney won 5 of 9 races for a clear win at the 2011 Cork OCR regatta in Kingston Canada. He 8 net points clear of 2nd place Chris Dold (CAN) and 19 point ahead of Andys travelling partner Clay Dold (USA). He had no races outside the top 10 in the 47 boat fleet at the ISAF Grade 1 event.
Andys trip continues on to San Francisco for some training before the Perth Worlds at the end of the year.
The 2011 Laser Masters Worlds has finished up in San Francisco with New Zealanders Scott Leith and Ed Tam first and second in the Apprentice Radials, and James Quinn and Mark Page also getting cubes.
The Masters were hosted by a very up market but friendly and well organised St Francis Yacht club on the city shoreline between the CBD and the Golden Gate Bridge. Naturally the backdrop was stunning. But while the sailors enjoyed the famous San Francisco sea breeze it was really all about the tide.
With a 9 and 2 on the penultimate day Andrew Murdoch lead into the final days medal race at the Olympic test event in Weymouth, just one point ahead of Australian Tom Slingsby. But the double points format meant a 7th in the medal race dropped Andrew to 4th behind Tom Slingsby, Rutger van Scaardenburg and Paul Goodison.
A frustrating end for Andrew, but his performance across the regatta looks like it's just where he wants it a year out from the Olympics.
Sara Winther finished 22nd in the radial.
Sailing a Laser on the last day of the Laser 4.7 Worlds was a bit like hitting yourself on the head with a hammer ......it felt so good when you stopped!
This Postcard comes by way of Munich as we head for the Splash Worlds in Czech.


Madonna's 'Truth or Dare' shoe collection arrived in Selfridge's shoe galleries on Monday, just in time as the Queen of Pop kicks off her tour in London's Hyde Park this week.
Created to showcase Madonna's dichotomy as 'both powerful icon and feminine beauty', the line was created with the help of Madonna's longtime stylist Arianne Phillips and features a lot of studs, zips and gold accents.
Produced by high-street footwear retailer Aldo, the collection features 23 styles with prices from £80-£480, and includes a range of styles from brogues to heels and boots.
The collection will be exclusive to Selfridges until September 1. ASOS, Nordstrom and Macy's will carry the line this fall.
Do you see yourself rocking a Madonna 'Truth or Dare' shoe?
Click here to see the full collection and let me know how many familiar styles you spot.


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<!-- From: file:/C:/Users/lizhuo/Documents/GitHub/LogisticsPlatform/Client/LogisticsPlatform_stable/app/src/main/res/layout/activity_good_result_detail.xml -->

redpajama_set_name: RedPajamaGithub


text:
Patch est un court métrage d'animation germano-suisse réalisé par Gerd Gockell, sorti en 2014. Il remporte le prix spécial du jury pour un court métrage au festival international du film d'animation d'Annecy 2014.

Synopsis
À travers une série d'œuvres abstraites, le film dépeint les tensions entre l'abstrait et le figuratif.

Fiche technique
 Titre : Patch
 Réalisation : Gerd Gockell
 Scénario : Ute Heuer
 Musique : Phil McCammon
 Montage : Gerd Gockell
 Animateur : Gerd Gockell et Ute Heueur
 Producteur : Gerd Gockell
 Production : Anigraf
 Pays :  et
 Durée : 3 minutes et 20 secondes
 Date de sortie :
  :
  :

Récompenses et distinctions
En 2014, le film reçoit le prix spécial du jury pour un court métrage au Festival international du film d'animation d'Annecy.

Notes et références

Liens externes

Film suisse sorti en 2014
Film allemand sorti en 2014
Court métrage d'animation suisse
Court métrage d'animation allemand
Film récompensé au Festival du film d'animation d'Annecy

redpajama_set_name: RedPajamaWikipedia


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