text:
\section{INTRODUCTION}
High polarization quasars (HPQs), along with BL Lac objects, form a
subset of
active galactic nuclei (AGN) known as blazars. HPQs are among the most
energetic AGN.
They are characterized by strong and variable radio, infrared and
optical continuum emission with a high degree of polarization. Blazars
are also strong and variable soft X-ray emitters (Brunner et al. 1994),
and recently have also been found to emit $\geq$100 MeV $\gamma$-rays
(Thompson \etal 1993).  The X-ray spectral measurements of blazars have
shown that the HPQs tend to have flatter spectral indices than the
BL Lac objects (Sambruna \etal 1994).  The uncertainties in these
measurements of spectral indices are, however, generally large due
to the small bandwidth, poor sensitivity, and low-energy absorption
in the interstellar medium.
There is also a general dearth of broad-band spectral
measurements of HPQs extending to hard X-rays, the few exceptions being
3C~279 and 3C~345 (Makino 1989), \pks~(Singh, Rao, \& Vahia 1990),
PKS~0537-441 (Sambruna et al. 1994), 3C~390.3 (Eraclous, Halpern, \&
Livio 1996), and a serendipitous detection of PKS~1502+106
(George \etal 1994).
We chose to carry out X-ray spectral measurements of PKS~1510-089
with the $ASCA$ observatory as previous measurements with the $EXOSAT$
Observatory, reported by Singh \etal (1990) and Sambruna \etal (1994),
indicated an unusually flat X-ray spectrum.

 Radio source PKS~1510-089 was first identified optically as a quasar
with an ultraviolet excess, a visual magnitude of 16.5 (Bolton \& Ekers
1966), and a redshift of $z=0.361$ measured from its emission line
spectrum
(Burbidge \& Kinman 1966).
Optical polarimetric observations by Appenzeller \& Hiltner (1967)
detected
strong (10.9\% $\pm$ 3.8\%) polarization at a position
angle of 177$^{\circ}\pm$9$^{\circ}$.  The strong variability of its
optical
brightness was first reported by Lu (1972) who monitored it for
5 years.  Subsequently it was found that its B magnitude had varied
by $\sim$ 6 magnitudes since 1899.6 (Liller \& Liller 1975).
{\it The range of brightness spanned is larger
than that known for any other quasar.} Its radio emission exhibits very
rapid, large amplitude variations in both total and polarized flux
(Aller,
Aller \& Hodge 1981; Aller, Aller \& Hughes 1996). It is a core
dominated radio source with a {\it
one-sided} jet which subtends about 8\farcs0~in the 20-cm waveband
(O'Dea, Barvainis \& Challis 1988).
Strong infrared (see Landau \etal 1986), millimeter (see Steppe \etal
1988),
and UV emission (Malkan \& Moore 1986) have also been detected from
PKS~1510-089.  $\gamma$-ray emission from PKS~1510-089 has also been
detected  by the $EGRET$ instrument on {\it CGRO} (Thompson et al 1993,
Sreekumar \etal 1996) with a flux of (2.3$\pm$0.57)$\times$10$^{-7}$
photons cm$^{-2}$ s$^{-1}$ for $\gamma$-rays with energies $\geq$100
MeV,
and a photon spectral index of 2.51$\pm$0.36.

The broad-band X-ray observations in 1984 and 1985 with
$EXOSAT$ described by Singh \etal (1990), showed that its X-ray spectrum
is
best fitted by a power-law with photon index $\Gamma$=1.40$\pm$0.35 and
low energy absorption consistent with the Galactic value of N$_{\rm H}$
in its direction (8.1$\times$10$^{20}$cm$^{-2}$) as given by Stark \etal
(1992).
The 2--10~keV flux from $EXOSAT$ observations, was found to be
8.9$\times$10$^{-12}$ ergs cm$^{-2}$ s$^{-1}$ in the observer's frame.
The source is highly luminous with its X-ray luminosity alone being
$\simeq$7$\times$10$^{45}$ ergs s$^{-1}$, assuming isotropic emission,
redshift of 0.361, H$_o$ = 50 km s$^{-1}$ Mpc$^{-1}$, and q$_o$ = 0 in
the Friedmann cosmology.

In this letter, we present new $ASCA$ observations of \pks, along
with an analysis of archival $ROSAT$ data.
Details of the observations and data reduction are given in \S2,
and the results from the spectral analysis in \S3.
We discuss our findings in \S4.

\section {OBSERVATIONS AND DATA REDUCTION}
\subsection {$ASCA$}
   PKS~1510-089 was observed with $ASCA$ on 1996 August 20
as part of the guest observer program (see Table 1 for the log of
observations).
The {\it ASCA} observatory (Tanaka \etal 1994),
contains four imaging thin--foil grazing incidence X-ray telescopes,
two of which are equipped with Solid State Imaging Spectrometers
(SIS) and the other two with Gas Imaging Spectrometers (GIS).
SIS detectors have been described in detail by Burke et al. (1991),
and GIS by Ohashi et al. (1996) and Makishima et al. (1996).
Their properties have been summarized, e.g., in Singh et al. (1996).
Due to radiation damage since the launch of ASCA, at the
time of the observations reported here the spectral
resolution of the SIS detectors had been degraded to
$\sim$10\% at 1~keV.  This spectral resolution is taken into
account by the response matrix generated as part of the analysis of
this spectrum.

The data were selected as described in Singh et al. (1996) using the
FTOOLS/XSELECT software package.
\pks~is the only source detected in the field of view.
The counts and pulse height spectra were accumulated from a source
region
of 4 arcmin radius in the SIS and 6 arcmin radius in the GIS, while
the background was taken from the off-axis source-free regions in the
SIS
and GIS where counts from the outer wings of the point spread function
of
the source were minimized.  The source spectra were grouped
to have a minimum of 20 counts per energy channel prior to spectral
analysis (see \S 3).
We have compared our results to those obtained assuming
background spectra accumulated from deep observations of
blank sky, and obtain consistent results (within statistical
uncertainties).

Steady X-ray emission from PKS~1510-089 was detected with a count rates
of
$\sim$0.18 and $\sim$0.14 counts s$^{-1}$ above background in SIS0 and
SIS1 detectors and in energy bands of 0.5 -- 8.2 keV and 0.65 -- 8.0 keV
respectively.  Similarly, the count rates observed with GIS2 and
GIS3 were $\sim$0.12 and $\sim$0.14 counts s$^{-1}$
in the energy bands of 0.75 -- 9.7 keV and 0.70 -- 10.0 keV
respectively.
No significant variability was seen on time scales of minutes to
hours in any of the detectors.
The average X-ray flux in the 0.4 -- 10 keV energy band in the
observer's
frame was $\sim$1.1$\times$10$^{-11}$ ergs cm$^{-2}$ s$^{-1}$ which
implies an X-ray luminosity of $\sim$10$^{46}$ ergs s$^{-1}$
(z=0.361; H$_o$ = 50 km s$^{-1}$ Mpc$^{-1}$; q$_o$ = 0 in the Friedmann
cosmology).
Similarly, the 2--10~keV flux in the observer's frame, was
8.6$\times$10$^{-12}$ ergs cm$^{-2}$ s$^{-1}$ which is within 4\% of the
value observed with EXOSAT, consistent
with the uncertainties in the cross-calibration of the
absolute fluxes of the two satellites.
The flux estimates are based on the best fit spectral models described
in
\S3.

\subsection {$ROSAT$}
PKS~1510-089 was detected in the $ROSAT$ all sky survey (RASS) as well
as during the pointed observations (Siebert et al. 1995). We have
retrieved the publicly-available $ROSAT$ data from the pointed
observations from the archives maintained at NASA High-Energy
Astrophysics
Science Archive Research Center (HEASARC).
The pointed observations were carried out on 1992 August 17 as part of
the $ROSAT$ Guest Observer Program, utilizing a position sensitive
proportional counter (PSPC) as the focal plane detector (Tr\"{u}emper
1983;
Pfeffermann \etal  1987).  The PSPC has a field of view of
2\degrees, an energy resolution (FWHM) of 0.42\% at 1 keV and a nominal
(gain-sensitive) bandwidth for $>$10\% efficiency of 0.1--2.0~keV.
No other X-ray source was detected in the neighborhood of \pks.
The details of the observations are given in Table 1.
The on-source counts were selected from a
circular region having a radius of about 3.25~arcmin and
centered on the source. An X-ray spectrum from the region was
accumulated
for the entire observation. The background was accumulated from
several neighboring regions at approximately the same offset as the
source.
The spectral data from the source were binned from the original
256 channels by grouping the first 176 channels by 8 and the rest by 16
to
improve the signal--to--noise ratio in each energy bin.
These observations resulted in a reasonably good quality spectra
with typical signal--to--noise ratio per bin of 5$\sigma$.

Steady soft X-ray emission from PKS~1510-089 was detected with a count
rate
of $\sim$0.18 counts s$^{-1}$ above background in the energy range
of 0.13 -- 2.0 keV in the observer's frame.
According to Siebert \etal (1995), the source flux changed by a factor
of $\sim$3.5 between the RASS and the pointed mode observation
about 2 years later.  The average X-ray flux in the 1992 pointed
mode observation in the 0.1 -- 2 keV energy band was
2.1$\times$10$^{-12}$ ergs cm$^{-2}$ s$^{-1}$ in the observer's frame.
The flux estimate is based on the best fit spectral models in \S3.

\section {SPECTRAL ANALYSIS AND RESULTS}
\subsection {$ASCA$}
We have analyzed the X-ray spectra obtained from SIS data for E$\geq$0.5
keV
and the GIS data for energies $\geq$0.7 keV.
The spectra were analyzed using \verb+XSPEC+ v9.0 (Arnaud 1996).
We first analyzed the data from each detector separately using a simple
absorbed power-law model with absorption cross-sections and abundances
from Morrison \& McCammon (1983).
The spectra SIS0, SIS1, GIS2 and GIS3
all gave consistent results.  The analysis was then performed jointly on
the
2 SIS detectors, and on the 2 GIS detectors; and finally on all the four
detectors jointly. We fit the spectra from all four instruments
simultaneously, but allowing the normalization of the model to be free
for
each detector to account for differences in the absolute flux
calibrations
of the instruments.  The results based on the joint analyses of all 4
detectors  are given in Table 2.  The results are consistent with the
analysis of spectra from individual detectors, analyzed separately.
The observed spectra from the 4 detectors along with the best fit model
of an
absorbed power-law are shown separately for SIS detectors in Figure 1,
and
for GIS detectors in Figure 2. The fit is very good, having a reduced
chi-square statistic, \chinu~= 1.03.
The resulting spectrum is hard with a photon
index $\Gamma$=1.30$^{+0.06}_{-0.06}$
(where the errors are at 90\% confidence for one parameter of interest),
and an equivalent hydrogen column density estimated from low-energy
absorption of $N_{H}=16\pm4\times$\mbox{$ 10^{20}~{\rm cm}^{-2}$}
which is about twice that due to absorption in our galaxy (see \S1).
The same result is obtained if assume an  absorber at z=0.361, along
with a
fixed absorption from 21-cm measurements in our galaxy.
In Figure 3 we show the 68\%, 90\%, and 99\% confidence contours for the
values of the spectral index and the \NH~allowed by the data.
Motivated by an earlier report about the presence of a Gaussian feature
near
5 keV in the spectrum (Singh et al. 1990),
we also tried adding a similar feature to the $ASCA$
spectra and got a marginal improvement in the quality of the fit.
The best fit line position was at 5.1$\pm$0.4 keV with an equivalent
width of about 87 eV.
Considering the signal to noise in this portion of the spectrum and the
fact
that the overall fit improved only marginally, we regard this equivalent
width as an upper limit. The equivalent width of the emission line
suggested by an $EXOSAT$ observation (Singh et al 1990) was several
times
higher, suggesting that either the line varied or it was spurious.
Alternate models e.g., (i) a broken power-law with a low-energy index
$\Gamma_l$, a break at energy E$_c$ $\sim$0.9 keV, and a high-energy
index
$\Gamma_h$, or (ii) the addition of a blackbody to a simple power-law,
or (iii) a partially covered power-law,  provided
equally good fits to the spectra (see Table 2).
The improvement in the fit was insignificant, however.  Therefore,
the data are not able to distinguish between the absence or the presence of
a low-energy excess in the spectrum.

\subsection {$ROSAT$}
Results from our spectral analysis of the {\it ROSAT} PSPC data are
presented in Table 3.
A simple absorbed power-law model provided a good fit to the PSPC
spectrum.
The data and our best fit power-law model are shown in Figure 4.
The confidence contours for the spectral index and the hydrogen
column density \NH~allowed by the PSPC data are shown in Fig. 3.
The best fit spectral index, $\Gamma$=1.88$\pm$0.28 is
significantly higher than that measured during the $ASCA$
observations.  The corresponding column density \NH, is
(7.6$^{+2.0}_{-1.5}$)$\times$\mbox{$ 10^{20}~{\rm cm}^{-2}$}, which is consistent with
the 21-cm value.  The unabsorbed flux at 1 keV is $\sim$10\% lower
than in the $ASCA$ observations.
The apparent discrepancy between the $ROSAT$ and $ASCA$
observations imply that either variations in both the
spectral index and the absorbing column occurred between the
two epochs, or that the PSPC band is dominated by a
separate, steep spectral component.
The PSPC spectra could be fit equally well by a broken power-law
($\Gamma_l$=
1.9$\pm$0.2, with the hard component fixed at $\Gamma_h$=1.30) with
absorption, however the break energy cannot be constrained (see Table
3.).
A model consisting of a low-energy blackbody and
hard power-law also provides a statistically acceptable
description of the data. However, such a model requires
a value of \NH~less than the Galactic value and hence we consider
it unrealistic.  The PSPC data show no preference for any of the three
models.

\subsection{$ROSAT$ and $ASCA$ Combined Spectral Analysis}
If we accept the simple absorbed power-law then there
is a significant difference between the spectral index and \NH~observed
by $ROSAT$ in 1992 compared to that observed by $ASCA$ 4 years later.
Since there were no measurements above 2 keV in 1992, the hard X-ray
flux seen with $ASCA$ might have varied even though the 1-keV flux
hardly changed.  In that case, joint fitting of $ROSAT$ and $ASCA$
data would not be meaningful.  In the likely case that a more complex
spectrum is present with a change around 1-keV, the joint
fitting can constrain the additional parameters involved in
multi-component
models.  We, therefore, carried out multi-component, multi-instrument
model
fitting, the results of which are given in Table 4.
We fit the spectra from all five instruments simultaneously,
but allowing the normalization of the model to be free for each
detector to account for differences in the absolute flux calibrations
of the instruments and changes in source intensity between the two
epochs.
As expected, a simple power-law model gives
an acceptable fit only if the \NH~is allowed to be significantly lower
than the Galactic value in the direction of \pks.
Both the broken power-law and blackbody plus power-law models
give acceptable fits to the data with the \NH~value almost
consistent with the Galactic value (see Table 4).
A partially covered power-law model with Galactic absorption and a very
high absorption intrinsic to the source at z=0.361, gives a somewhat
poorer fit.  Thus we conclude that the most likely explanation of the
$ROSAT$ \& $ASCA$ observations is that a powerlaw of photon index
$\Gamma \simeq$ 1.3 dominates the spectrum above $\gtrsim$ 1~keV with
a 2--10~keV flux $\simeq$8.6$\times$10$^{-12}$ ergs cm$^{-2}$ s$^{-1}$
at both epochs in the observer's frame.
A separate, steeper spectral component dominates at lower energies,
the specific form of which cannot be unambiguously determined.

\section {DISCUSSION}
$ASCA$ observations show that the 0.5 -- 10 keV X-ray spectrum of
\pks~is hard ($\Gamma \simeq$ 1.3).   Although earlier observations with
the $EXOSAT$ (Singh \etal 1990; Sambruna \etal 1994) had indicated
that the X-ray spectrum of \pks~might be this hard,
those measurements were not conclusive due to a relatively
poor signal-to-noise ratio.
The observed spectral index is significantly flatter than that
of the typical radio-loud quasars ($< \Gamma >$=1.66$\pm$0.07,
Lawson \etal 1992; Cappi \etal 1997),
radio-quiet quasars($< \Gamma >$=1.90 $\pm$0.11, Lawson \etal 1992;
Williams \etal 1992),
and BL Lac objects ($< \Gamma >$ = 2.20$^{+0.17}_{-0.15}$,
Sambruna \etal 1994).
The observed spectrum is, however, similar to that of other HPQs
observed in both the hard
(e.g. 3C~345 with $\Gamma$=1.4$\pm$0.09, Makino 1989;
PKS~0537-441 with $\Gamma$=1.26$^{+0.24}_{-0.31}$ Sambruna et al. 1994)
and the soft
(e.g. 0212+735 with $\Gamma$=0.44$^{+0.39}_{-0.41}$
and 0836+710 with $\Gamma$=1.4$\pm$0.05, Brunner \etal 1994)
X-ray bands.
Thus, based on an admittedly small number of examples,
HPQs do appear to show X-ray spectra that are flatter than those of
other core-dominated radio-loud quasars.

PKS 1510-089 was observed in the near ultraviolet band with the
International
Ultraviolet Explorer (IUE) low-dispersion spectrographs during the early
1980s. There are three SWP exposures and two LWR exposures in the
archive.
The SWPs include one nondetection and two spectra obtained over a
nominal
1-year baseline whose continuum levels are equivalent to the
1$\sigma$ level. One LWR exposure was underexposed and resulted in
a nondetection. There is, however, no evidence of variability in the
available UV data, although it cannot be ruled out either.
Though weakly detected on one occasion with the short- and long-
wavelength instruments, redshifted emission lines of Ly-$\alpha$ and
O~VI/Lyman-$\beta$ are clearly detected, with several other normally
prominent
emission lines possibly present. The UV continuum is well approximated
by a
power law with index -1.2 ($\nu$ vs $f_{\nu}$).

We constructed a multifrequency spectrum using measurements
from the published literature.  The spectrum is shown in Figure 5.
We note that these data do not result from simultaneous or even
contemporaneous observations. The ``radio'' points at 1.5 and 4.9 GHz
are
from O'Dea et al. (1985); we note however that Aller et al. (1996), who
present a 20-year radio light curve for PKS 1510-089, show that
it varies by at least factors of 5, mainly in series of
flare-like events occurring on ~yearly time scales (and sometimes
persisting for ~months). The near IR measurement at 1.5$\mu$m
is from Landau et al. (1986) and we used the visual magnitude of
V=16.5 of Bolton \& Elkers (1966) to derive  a
flux point corresponding to 5500 \AA. We used the UV measurements
obtained from the IUE archives as described previously.
The optical and UV fluxes have been corrected for galactic extinction
using the extinction law of Seaton (1979) and a color excess estimated
from the galactic \NH~values derived from the 21-cm measurements.
The $\gamma$-ray flux at energies $\geq$100 MeV has been
taken from $EGRET$ measurements (Thompson et al 1993).

The multiwaveband spectrum of
PKS~1510-089 resembles that of many other blazars detected by $EGRET$,
with the bulk of the luminosity being emitted as $\gamma$-rays
(e.g. see Fig.5 of von Montigny et al (1995) -- indeed, we note the
multiwaveband spectrum of PKS~1510-089 is globally very similar to the
BL Lac Mrk~421).
In the popular relativistic jet models, the hard X- and $\gamma$-ray
emission is proposed to arise as a result of inverse-Compton scattering
of
low energy photons by relativistic electrons within the jet
(e.g., see von Montigny et al (1995), and references therein).
We suggest that the double powerlaw form found above might indicate
that the {\it ROSAT} data are dominated by the steep tail of this low
energy
emission (often assumed to be synchrotron radiation) while the
flatter inverse-Compton scattered component dominates
the {\it ASCA} data $>1$~keV.
We suggest that even though superluminal motion has not (yet) been
detected
in this source, the emission is likely to be relativistically beamed.

     Based on Figure 5, PKS 1510-089 may be among a subclass
of blazar AGN which exhibit the so called big blue-bump component.
In order to study the blue-bump emission, we subtracted a
power-law  component, connecting the X-ray, IR, and mm radio
points, from the multifrequency spectrum to obtain residuals in
the optical-UV region. A statistically significant, positive
residual is obtained. We emphasize that variability could
account for some or all of this apparent residual.  We then fit a
thermal
accretion disk spectrum to these residual spectra.  The model
involves thermal emission due to viscous dissipation in a
steady-state, accretion disk which has been modified to include
the effects of gravitational red-shift and focusing (e.g. Sun
\& Malkan, 1989); we have employed computational methods similar
to those described in Czerny et al. (1986).  A Schwarzchild
metric was used in the calculations and an inclination of
sin~$i$ = 0.5 was assumed.  We fixed the inner disk radius at 3R$_{g}$
and R$_{out}$/R$_{in}$$\simeq$200. We were unable to obtain a reasonable
fit
to the optical and UV data without reducing R$_{out}$/R$_{in}$ to this
level; values more typically fitted to AGN are of order
R$_{out}$/R$_{in}$$\simeq$10$^3$.  Again, this could possibly be
attributed to variability -- we suspect that the actual visual flux at
the time of the UV measurements may have been significantly higher.

    If the blue-bump residual we depict here is NOT an artifact
of non-simultaneous measurements of a highly variable source,
PKS 1510-089 is among a minority of the extreme blazar AGN which
both emit gamma-rays and exhibit a blue-bump component.
Another blazar with a blue-bump
component is 3C 345 (e.g. Webb et al 1994), but it was
never detected at more than a 3.5$\sigma$ level with $EGRET$.

A detailed discussion of the various physical models proposed for such
objects is beyond the scope of the current paper.
Further simultaneous, broad-band UV, X- \& $\gamma$-ray observations are
required to constrain physical models.

\acknowledgments
We wish to thank the entire $ASCA$ team for making these observations
possible.
This research has made use of $ROSAT$ archival data obtained through the
High Energy Astrophysics Science Archive Research Center, HEASARC,
Online
Service, provided by the NASA-Goddard Space Flight Center.

\clearpage

redpajama_set_name: RedPajamaArXiv


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Mars Rover Curiosity Wraps Up Drilling Work, Prepares for Long Drive
NASA's Curiosity Mars rover used the Mars Hand Lens Imager (MAHLI) instrument on its robotic arm to illuminate and record this nighttime view of the sandstone rock target "Windjana." Image released May 15, 2014.
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NASA's Mars rover Curiosity is about to hit the road again.
The 1-ton Curiosity rover has finished its drilling operations at a sandstone slab dubbed "Windjana," successfully delivering collected samples to its onboard scientific instruments for analysis. The robot will soon resume the long drive toward the base of Mount Sharp, which has long been its ultimate destination, mission officials said.
The rover bored a 2.5-inch-deep (6.4 centimeters) hole into Windjana earlier this month, performing its third full sample-collecting drilling activity since touching down inside Mars' huge Gale Crater in August 2012.
The previous two drilling operations, which investigated fine-grained mudstones at a site called Yellowknife Bay, allowed mission scientists to determine that the Red Planet could have supported microbial life billions of years ago.
Yellowknife Bay is close to Curiosity's landing site. Windjana is about 2.5 miles (4 kilometers) southwest, on the way toward the foothills of Mount Sharp, which rises more than 3 miles (5 km) into the Martian sky from Gale Crater's center.
This view from the Mars Hand Lens Imager (MAHLI) on NASA's Curiosity Mars Rover shows the rock target "Windjana" and its immediate surroundings after inspection of the site by the rover. The drilling of a test hole and a sample collection hole produced the mounds of drill cuttings that are less red than the other visible surfaces. Image released May 15, 2014. (Image credit: NASA/JPL-Caltech/MSSS)
Mission scientists want Curiosity to climb up through these foothills, reading a history of the Red Planet's changing environmental conditions as it goes. The rover's measurements could help shed light on why and when Mars changed from a relatively warm and wet planet to the cold and dry world we know today, NASA officials have said.
Curiosity is exploring the Red Planet with the aid of 10 different scientific instruments. Two of the workhorses are the Chemistry and Mineralogy instrument (CheMin) and the Sample Analysis at Mars instrument (SAM), both of which sit on the rover's main body.
CheMin and SAM will perform a detailed analysis of the Windjana samples, as they did for the powder collected at Yellowknife Bay.
While Windjana powder has already been delivered to both CheMin and SAM, Curiosity carries still more of the material, which may be transferred to the instruments during pauses in the rover's driving if need be, NASA officials said.
Follow Mike Wall on Twitter @michaeldwall and Google+. Follow us @Spacedotcom, Facebook or Google+. Originally published on Space.com.
NASA's James Webb Space Telescope may miss March 2021 launch, GAO report says
NASA is turning off the Spitzer Space Telescope. Its infrared eye changed our view of the universe.
SpaceX launches 60 new Starlink satellites, sticks rocket landing at sea
On This Day in Space: Jan. 29, 1989: Phobos 2 enters orbit around Mars
Jupiter and Saturn may leave marks on the sun's corpse


text:
package org.compass.annotations.test.id;

import org.compass.annotations.test.AbstractAnnotationsTestCase;
import org.compass.annotations.test.Converted;
import org.compass.core.CompassHits;
import org.compass.core.CompassSession;
import org.compass.core.CompassTransaction;
import org.compass.core.config.CompassConfiguration;
import org.compass.core.mapping.CompassMapping;
import org.compass.core.mapping.ResourcePropertyMapping;
import org.compass.core.mapping.osem.ClassIdPropertyMapping;
import org.compass.core.mapping.osem.ClassMapping;
import org.compass.core.spi.InternalCompassSession;

/**
 * @author kimchy
 */
public class IdTests extends AbstractAnnotationsTestCase {

    protected void addExtraConf(CompassConfiguration conf) {
        conf.addClass(A.class).addClass(B.class);
    }

    public void testIdsPaths() throws Exception {

        InternalCompassSession session = (InternalCompassSession) openSession();

        CompassMapping mapping = session.getMapping();
        ClassMapping AMApping = (ClassMapping) mapping.getRootMappingByAlias("A");
        ClassIdPropertyMapping[] idMappings = AMApping.getClassIdPropertyMappings();
        assertEquals(1, idMappings.length);
        ResourcePropertyMapping[] resourcePropertyMappings = idMappings[0].getResourceIdMappings();
        assertEquals(1, resourcePropertyMappings.length);
        assertEquals("test", resourcePropertyMappings[0].getPath().getPath());
        assertEquals("test", resourcePropertyMappings[0].getName());

        CompassTransaction tr = session.beginTransaction();

        A a = new A();
        a.setId(1);
        a.setValue("value");
        session.save(a);

        a = session.load(A.class, 1);
        assertEquals("value", a.getValue());

        CompassHits hits = session.find("value");
        assertEquals(1, hits.length());

        tr.commit();
        session.close();
    }

    public void testConvertedId() {
        CompassSession session = openSession();
        CompassTransaction tr = session.beginTransaction();

        B b = new B();
        b.id = new Converted("value1", "value2");

        session.save(b);

        session.load(B.class, b.id);

        tr.commit();
        session.close();
    }

}

redpajama_set_name: RedPajamaGithub


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How much would you expect to pay in order to play for a $100,000 prize pool? $100? $200? At most online poker rooms, this is exactly what you'll pay. And if you're lucky, you might be able to make it to the $100,000 poker tournament through a freeroll or satellite. Of course, at Full Tilt Poker, you can bypass all of the satellites and expensive buy-ins by playing in their Big Little Tournament.
The Big Little Tournament only costs $2 + $0.20 to play in, and you'll be able to compete for the aforementioned $100k prize pool. Of course, if you are really low on cash, there are still satellites for the Big Little Tournament; some of the satellites are as low as $0.35 or 5 Full Tilt Points.
No matter how you choose to enter the Big Little Tournament, keep in mind that the main event happens on the last Sunday of every month at 12:30 ET. Also, the number of players who can compete in this tourney is capped at 100,000 so don't procrastinate on signing up. If you do procrastinate, you'll miss out on the opportunity to play poker for the $9,000 first place prize.
To begin registering for the Big Little Tournament, visit the poker software at Full Tilt and choose Lobby, Choose Lobby View and Standard View. Once you've done this, go to Tournament, Guarantee, Hold'em, No-Limit and Micro; this will bring up the Big Little Tournament.
But before you do any of this, it's a good idea to sign up for Full Tilt's 27% rakeback deals. This ensures that you'll be earning rackback on your Big Little Tournament buy-in as well as any other tournament you play at Full Tilt. Make sure to check out Full Tilt's other online poker deals too since they are one of the best poker sites in terms of rolling out fresh new deals.


text:
Lady Gaga's Applause VS Katy Perry's Roar - Which Is Best?
POP EMERGENCY! After numerous leaks and cries of outrage from the hardcore fans, Lady Gaga and Katy Perry have both rush-released their highly anticipated new singles. Do they live up to the hype? And which is best? Listen to both songs now after the jump.
Co-produced by Lady Gaga and DJ White Shadow, Applause is the lead single from the singers forthcoming ARTPOP album and to be honest, it seems to be a bit of a grower. While Applause may not immediately strike listeners in the same way that Bad Romance did, I personally think that the song has the potential to surpass Born This Way given some repeated listens. I love the sound of her voice on the track but Gaga needs this to be a smash after the lukewarm reception she received for her previous album. Is it inventive enough? Give us another Telephone goddammit!
Katy Perry has a lot to live up to following the ridiculous success of the Teenage Dream album so what do you do? Call Max Martin! New song Roar has a fantastic pop chorus that just hits you instantly and while it may not represent much of an evolution in the singers sound, its already a guaranteed hit in my eyes. But will the rest of her upcoming Prism album be any good? It's definitely got potential if Roar is anything to go by.
So what did you think? Who has the best comeback single? Whose album excites you most? And are these songs good enough to keep both pop princesses on top? Personally, I can't get enough of Applause, even though Roar is probably the better song but let me know what you think by commenting, liking and sharing below. Also, vote now in our poll to let us know which song is best.
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7 Paktika Children Killed By Roadside Bomb: Officials | .:: Elections 2014 ::.
At least seven children were killed and three others were wounded on Monday by a roadside bomb blast in southeastern Paktika province, local officials said.
The children, all 6 to 10 years old, and from the same extended family, were killed while playing near a road in the Khairkot District, said spokesman of the provincial Governor Mukhlis Afghan.
The victims were taken to a nearby hospital for emergency care.
No one has claimed responsibility for the bomb.
Insurgents routinely plant explosives along well-traveled roads, purportedly targeting Afghan and NATO troops. But the bombs are indiscriminate and often kill civilians.
According to the most recent United Nations civilian casualty report, issued in July, 74 percent of civilian casualties in Afghanistan in the first half of 2013 were caused by insurgents. The majority of those were said to have been caused by roadside bombs.


The study details major risks to the productivity of pulpwood plantations established to supply the new mill, including catastrophic fires, peatland subsidence and flooding, social conflict, and pests and diseases. Indonesia's massive fires in 2015 heavily damaged these plantations. An analysis cited in the report found that 293,000 hectares within four APP supplier concessions burned in the 2015 fires.


text:
Sydney Named as 2018 Invictus Games Host
By Danielle Pope	| November 15, 2016
The Paralympic style Games for injured veterans are coming to Sydney
Sydney has been announced as the next host city for Prince Harry's Invictus Games, an international sporting event for injured veterans.
Featuring Paralympic-style multi sports events, the Games began in London in 2014. Since then, the Games have gone to Florida and will be in Toronto next year.
In making the announcement, Prince Harry mentioned how the world had been moved by the courage of the participants, as they overcame their challenges in order to compete. "The Invictus Games have shown us what can be achieved when wounded, injured and sick servicemen and women rediscover their fighting spirit through sport," said the Prince. "We have all been inspired."
In deciding where the Games should be held, the Invictus Foundation had three criteria. The host city needed to be iconic, with a proud military history, and its people would really get behind the competitors. "It was an easy decision really", said the Prince, "The 2018 Invictus Games are coming to Sydney".
Paralympic gold medallist and former combat engineer Curtis McGrath will be an ambassador for the Sydney Games. McGrath suffered traumatic injuries when he stepped on an improved explosive device in Afghanistan in 2012, but went on to compete in the Games in Florida. "We have been through trauma," he said, "But we can get together and support each other throughout the games. We are using the power of sport to help us get better."
You can find out more about the Invictus Games Foundation here
BREAKING NEWS: Prince Harry announces which iconic city will be hosting the 2018 #InvictusGames! pic.twitter.com/b6VVVcyAcB
— Invictus Games (@WeAreInvictus) November 12, 2016
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Wayne Williams is serving life in prison in connection to two murders but is suspected of a string of child deaths in Atlanta.
Atlanta officials announced they are reopening 22 cases related to the decades old murders of African-American children and young adults.
Atlanta Mayor Keisha Lance Bottoms and Police Chief Erica Shields announced they were taking another look at the cases. At least 28 children, teens and adults were killed in and around Atlanta from 1979 to 1981, igniting fear across the city.
"It would certainly be in order for us to look once again at evidence that the city of Atlanta has in its possession…to once again take a fresh look at these cases and to determine once and for all if there's additional evidence that may be tested that may give some peace - to the extent that peace can be had in a situation like this- to the victims' families," Bottoms said.
Wayne Williams, 60, is serving a life sentence for the murder of two adults and officials believe he's responsible for some of the other deaths. Williams, who maintains his innocence, has never faced charges related to the children's deaths and questions about other possible suspects have lingered since his 1982 conviction.
According to the Atlanta Journal-Constitution, the new investigation will involve the Atlanta Police Department, the Fulton County District Attorney's Office and the Georgia Bureau of Investigation using modern technology to test evidence such as DNA and carpet fibers.
Atlanta Police have also established a hotline, 404-546-2603, for tipsters looking to provide information.
The announcement came just as a new documentary about the case aired on Investigation Discovery.


text:
Ernest Francis Acheson (September 19, 1855 – May 16, 1917) was a newspaper editor and a representative to the United States House of Representatives.

Biography
He was born in Washington, Pennsylvania on September 19, 1855, son of Alexander W. and Jane (Wishart) Acheson. He attended the public schools there, and then went on to Washington and Jefferson College in 1875.

He was an honorary graduate of Washington and Jefferson College in 1875; studied law with M. C. Acheson at Washington, Pennsylvania, was admitted to the bar in 1877 and practiced law there until 1879. He purchased the newspaper Washington Weekly Observer, of which he was editor. In 1889, he established a daily edition of the same paper. He received the honorary degree of A.M., from Washington and Jefferson College in 1889.

On November 22, 1882, he was married to Jannie B., daughter of Galbraith Stewart.

He was elected as a Republican to the United States House of Representatives in 1894, and continued to serve until 1909, having been an unsuccessful candidate for the nomination in 1908. Acheson was served in the 54th, 55th, 56th, 57th and 58th congresses. He became president of the Pennsylvania editorial association in January, 1893, and recording secretary of the National Editorial Association in June, 1893.

In 1909 he returned to editorial work until his retirement in 1912. He died in Washington, Pennsylvania, in 1917.

References

Citations

Sources

External links
The Political Graveyard

1855 births
1917 deaths
Editors of Pennsylvania newspapers
Politicians from Pittsburgh
Washington & Jefferson College alumni
Republican Party members of the United States House of Representatives from Pennsylvania
19th-century American politicians

redpajama_set_name: RedPajamaWikipedia


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I would highly recommend confirming that your battery is not flat or missing and or dead. Have you tried jump starting the vehicle? I would also check battery connections. If not, try that, follow specific procedure per your Saturn owners manual. If you are successful in getting the car started, I would highly recommend you taking it to a qualified service repair facility (Repair Pal Certified Service Center) to have it fully evaluated to see why it happen and prevent further issues.
Are there any warning lights that come on? ABS, Brake or Traction Control? I would highly recommend you take your vehicle to a qualified Certified Service Facility because it does NOT seem to safe to drive in its present condition. All the best.
I would recommend taking it to a qualified service station. So that they could properly analyze various system along with the proper alloted time in order to verify, isolate your vehicle concern. Best of luck.
I hope I'm wrong, but seems like some solid state component may have gotten wet during the car wash. Best of wishes.
for starters,It seems that your Transmission has an electrical malfunction. Take it to your normal service station to have it inspected. Best of wishes.
It could be a number of things. Vacuum Leak, Idle speed circuit, Automatic Transmission Fault? I would highly recommend you take it to a qualified service facility to have it analyzed to determine root cause of failure. Best of luck.
Good evening, Did the A/C System work last season/year after your compressor was replaced? If so it might a new malfunction, It is after all 14 yrs old vehicle. However i would highly recommend you call up that facility to see what might be going on with the A/C system. Most repairs/service comes with a 12 month or 12,000 mile warranty. Best of wishes and keep us posted on what is found after vehicle gets inspected.
With a 15 yr old vehicle it can be just about anything. No spark condition at ignition coil, no fuel pressure at engine, unmeatered air intake leak etc... I would let them do their due dilagence and troubleshoot the issue without any input. I see too many instances today that regular people go to the internet and read a post/suggestion and strongly believe that their vehicle is suffering from the same condition without ever testing a single component. Then when it arrives to a qualified service station. Vehicle has a couple of parts installed, frustrated vehicle owner, yet still full of suggestion/ input. Just beware must automotive technicians have hundreds if not thousands of hours of training/ experience at their skillful craft. My only ews suggestion is if you have another authorized key try it to see if it starts w/ that one. Best of wishes.


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Sao Mai Phu My Resort has 3 stars with 98 rooms in Phu My - Ba Ria - Vung Tau, rated 6.1 /10, "Pleasant".
Thai Phong Hotel has 2 stars with 30 rooms in Phu My - Ba Ria - Vung Tau.
Nha Viet Hotel Vung Tau has 2 stars in Phu My - Ba Ria - Vung Tau.
Lesco Resort has 2 stars with 60 rooms in Phu My - Ba Ria - Vung Tau.
Tan Hoang Mao Hotel has 3 stars with 126 rooms in Ba Ria City - Ba Ria - Vung Tau.
HD Ho Tram Hotel has 2 stars with 26 rooms in Phuoc Thuan - Ba Ria - Vung Tau.
Hoa Cau Motel Ho Tram has 2 stars with 17 rooms in Ho Tram Beach - Ba Ria - Vung Tau.
Sapphire Ho Tram 1 Villa has 2 stars with 12 rooms in Ho Tram Beach - Ba Ria - Vung Tau.
Sapphire Ho Tram 2 Villa has 2 stars with 12 rooms in Ho Tram Beach - Ba Ria - Vung Tau.


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Q: Selenium - How to open new Chrome Window, using Javascript Executors I have an edit button on a page. I want to open this in a new window.
At the moment, this code will click the edit button and have it open in the default window:
    Actions actions = new Actions(driver);
    JavascriptExecutor jse = (JavascriptExecutor) driver;
    actions.moveToElement(elem1).click();
    jse.executeScript("arguments[0].click()", elem1);

To open it in another window, I tried doing something like
Actions newwin = new Actions(driver);
newwin.keyDown(Keys.SHIFT).click(elem1).keyUp(Keys.SHIFT).build().perform();

However, this returns an error, because it's not actually moving to the element and finding it. If I scroll down to where the edit button is manually while my script is running, the edit page will get opened in a new window, as wanted.
However, I don't want to manually have to scroll down to the edit button every time I run my Selenium script.
I tried doing something like this:
Actions newwin = new Actions(driver);       newwin.moveToElement(elem1).keyDown(Keys.SHIFT).click(elem1).keyUp(Keys.SHIFT).build().perform();
But it still was not able to select the edit element and open it in a new window.
Does anyone have any ideas how I can make this work?

A: you already said its not scrolling down. so that is the source of your problem.
you dont need to create another action for this if you just want a new window.
window.onload = function() {
document.getElementById("actualID").onclick = function(){
    return !window.open(this.href, "actualID", "width=666,height=666");
}

-with your existing code, can you print to console the position of elements to
confirm that the edit button can actually be seen (in the DOM)...debugging.
-use CSS or ID for your locator first then try others.
you can you create an event and wrap it into a promise and make this cleaner.

A: Okay got it guys..
I needed to scroll it into view first, then I could right click and open it in a new window
I was having issues because I really wanted to do it in 1 step, but I broke it down into 2:
        ((JavascriptExecutor) driver).executeScript("arguments[0].scrollIntoView(true);",
elem1);
    Thread.sleep(500);

    Actions newwin = new Actions(driver);
    newwin.keyDown(Keys.SHIFT).click(elem1).keyUp(Keys.SHIFT).build().perform();

redpajama_set_name: RedPajamaStackExchange


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A Fire Burns in the Center of the Mandap Photo by Bia Sampaio In the center of the mandap, or wedding altar, a fire is kindled. Mangalphera With Agni as a witness, the couple performs Mangalphera walking around Agni four times, which solidifies their marriage and makes them husband and wife. The sisters and brothers from each side will generally dance in groups or will perform skits. May this love always be tied and stay strong regardless of any difficulties that they face in life. Saptapadi The bride and groom take seven steps together, symbolizing the beginning of their journey through life as partners.
She hosts an annual Wedding Expo as New England's first and only wedding resource dedicated to South Asian brides. Kumbha Sthapana The Brahmin Priest invites Lord Vishnu to join the ceremony. If the stars of the boy and girl are in perfect harmony, then the marriage talks proceed further. The paste is believed to signify a harmonious mental union. In Punjabis, the Giddha nad Bhangra are the popular dance forms for the Sangeet night ceremony.
It was really sweet I love the family wedding portraits! Some even hire famous musicians and singers to present beautiful melodic performances. Cash or a check is fine. The nuances of a ceremony may also vary greatly due to factors such as region and language. Relatives from out of state and even out of country gather and bring bits and pieces of their newly adopted cultures. Q: My Hindu friends are getting married. Everyone wishes the newly-wed a happy, joyous and prosperous future. It is a symbol of holiness and of perfection and of peace.
The couple is now married. Janwaas Ganesh and his Baraat are offered a comfortable place to rest while they enjoy refreshments and sweets until they are called to the Mandap wedding shrine. The paste is soaked overnight for maximum infusion and then poured inside a plastic cone. Whether you're invited as a guest, attending as a member of the wedding party, or are simply curious, there are a few of the Hindu wedding rituals and traditions you should expect to see. Vidai - Farewell to the Bride The Vidai is one of the most emotional parts of the ceremony.
Marriage is a great social event in our society. It starts with the hunt for the perfect match followed by celebrations, lasting at least for a week, before marriage. It is meant to unite two persons so firmly that, although they retain two separate bodies, they become one in spirit. This first song is the song that played as our grandparents, parents, wedding party, flower girls and ring bearer entered the room. The leaves and branches produce a red-orange dye known as Lawsone that is responsible for imparting the characteristic color when bound with protein molecules of the upper skin layer. Dwaar Puja Prayers are offered to Lord Ganesha, who is the remover of all obstacles and a symbol of peace, friendship, and happiness.
As well as being the union of two souls, it is also regarded as a bond between two families. Red represents happiness and good luck to the married couple. At this time, Jaimini and Varun will also exchange wedding rings. Vidaai - Farewell After lunch is the Vidaai ceremony. Traditionally, Lakshmi, the Hindu goddess of wealth, fortune and prosperity, is invoked in the mangala sutra and the bride is said to receive blessings throughout her marriage. The ceremony takes place in a mandap wedding pavilion built to represent the universe.
The days of singing simple traditional songs about Banna-Banni with dolaks, spoons and harmonium, are over. Today the ceremony will be performed both in Sanskrit and English. I will have to fit a Joanna Newsom song, somewhere in mine. Arrival of the Bride Suchita enters, carrying a coconut decorated with turmeric and vermilion, symbolizing prosperity. Floral and paisley motifs dominate this style and the designs are generally curvy with lots of emphasis on vines. There'll often be up to four stations of chefs preparing food for guests.
Ashirvad Prayer and Blessings Once the wedding rituals have been completed, the couple touches the feet of their parents and the priest, asking for their Aashirwaad, or blessings. The sindhur is indicative of a blood union, and it is the unmistakable mark of a married woman. The Vedic Mantras chanted during the sacred ceremony refer to the bride and bridegroom as Prukruthi and Purusha. Antar Patt The Antar Patt veil is placed in front of the groom, signifying the separate lives of the bride and groom, which will soon end with their union. Saptapadi Groom's name stresses to Bride's name the need for harmony and devotion in life, while the couple walks together seven steps, vowing: With God as our guide let us take: The first step for prosperity The second step for strength The third step for wealth The fourth step for happiness The fifth step for progeny The sixth step for nature's bounty The seventh step for companionship Exchange of wedding vows Vachan Shuaang Groom's name places sindoor red powder , the traditional mark of a suhaagwati stree married woman in the parting of Bride's name's hair.
Raksha Bandhanam Mantras and hymns are chanted by the priest to protect the bride and groom against any evil spirits during the ceremony. Their wedding garment is called a Lehenga, which is a long skirt with a matching top and scarf. We will finish by reciting vows to each other in both Sanskrit and English: some of these are ancient and repeated at many weddings while others we have written ourselves. Furthermore, Mehndi is one of the sixteen adornments of the bride and her beauty is incomplete without it. It is preceded by a band which plays all the latest tunes.


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Home • Blog • The Impact of Holt v. Hobbs on Native American Inmates
The Impact of Holt v. Hobbs on Native American Inmates
By Joel West Williams, Staff Attorney
Native American Rights Fund
Holt v. Hobbs, a recent unanimous decision by the U.S. Supreme Court protecting a Muslim prisoner's right to wear a half-inch beard, has important implications for Native American inmates seeking accommodation of their religious practices. In Holt, the Court held that Arkansas violated the Religious Land Use and Institutionalized Persons Act (RLUIPA) where its grooming policy did not allow beards and it refused to grant a religious exemption to an inmate whose Muslim religion required him to wear a beard.
The Court had granted review in that case, shortly before a group of Native American inmates from Alabama requested the Court's review in Knight v. Thompson, a case where Native Americans were denied the ability to wear long hair consistent with their Native religious beliefs due to a restrictive grooming policy in Alabama's male prisons. The Native American Rights Fund, representing the National Congress of American Indians and Huy filed "friend of the Court" briefs supporting the prisoners in both Holt and Knight (here and here). The Court has held the Knight petition since May 2014 and now, with its decision in Holt, has rescheduled it for a January 23, 2015, conference.
Like Mr. Holt, the Native American prisoners in Knight seek relief under RLUIPA, which requires that a substantial burden on an inmate's religious exercise be the least restrictive means of furthering a compelling government interest. This standard, referred to as "strict scrutiny," is the most stringent legal standard applied to laws and government rules. A lack of consistent application of this rigorous standard by the courts has allowed some prison systems to unduly restrict religious practices of Native American inmates.
Since the Nebraska prison system became the first in the U.S. to accommodate sweat lodge in 1972, many others have gradually accommodated a variety of religious practices unique to Native Americans, including sweat lodge, tobacco use and long hair. Now, 80% of U.S. prison systems allow Native Americans to wear long hair, either through blanket policies or special religious exemptions. By and large, prison officials have found ways to mitigate the minimal risks associated with these practices and have observed numerous benefits to Native inmate behavior and rehabilitation as a result.
However, a handful of prison systems stubbornly refuse to accommodate certain facets of Native religion, such as long hair at issue in Knight. Those prison officials fear certain Native American practices threaten prison safety, security and/or hygiene. Yet, in Knight, Alabama prison officials admittedly did not investigate, or even consider, the successful accommodation measures taken by the 80% of prison systems allowing long for Native American inmates. Moreover, rather than apply RLUIPA's strict scrutiny to Alabama's arguments and ask, "Why not Alabama?" the lower courts in Knight deemed the policies of other jurisdictions simply irrelevant to the operation of Alabama prisons and accorded "due deference" to the admittedly uninformed opinions of Alabama prison officials.
Holt holds that this approach is wrong. Much like Knight, the Arkansas prison officials in Holt feared safety and security issues and ignored the successful measures taken by the vast majority of prison systems to safely accommodate religious beards. The Holt opinion makes clear that these successful, widespread accommodations are indeed relevant and indicate that Arkansas was not utilizing the "least restrictive means." Additionally, the Supreme Court emphasized that courts cannot use "due deference" to prison officials' opinions as a means of practicing "unquestioning acceptance," thereby abdicating judicial responsibility to apply RLUIPA's very rigorous standard. Courts must demand persuasive proof that denial of an exemption to a specific person is the least restrictive means of furthering compelling penological interests. Like the prison officials in Holt, the officials in Knight failed to meet this standard, and the court applied an unquestioning acceptance of their opinions. It is an error that has plagued the cases of several Native American inmates through several decades of litigation, and we believe that Holt should remedy this persistent issue.
The Holt opinion changes a fundamental aspect of how certain prison systems deal with Native Americans and their religious practices. For those Natives who reside in the darkest corners of U.S. penal systems, it is no longer the rule that they cannot engage in their traditional religious practices merely because their jailors say so. Courts will demand more, just as Congress intended when it enacted RLUIPA.
Huy: helping Indigenous prison inmates
Nov 5th, 2021 Read article
Tribal Leaders Tell Gov. Inslee About Problems With Criminal Justice and Health Care Changes
Oct 30th, 2021 Read article
Indigenous prisoner human rights organization awarded $50,000 grant
Indigenous Prisoner Religious Rights Organization Awarded $50,000 Grant
Oct 18th, 2021 Read post
Wash. DOC Pledges to Restore Indigenous Religious Freedoms
Jun 21st, 2021 Read post
Huy Gives $10,500 in COVID Relief to Indigenous Prisoners
Mar 22nd, 2021 Read post
© 2022 Huy
Huy logo design: Louie Gong, Eighth Generation
Where indicated and on the homepage, images copyright: Jack McNeel
Where indicated, images copyright: Richard Ross
Website design and development: Dave Riensche


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In Adelanto, California "civil litigation" refers to the process through which a court determines legal disputes that are not criminal in nature. They can involve private and public entities.
In Adelanto, California, the purpose of civil litigation is not punishment or retribution for the perpetrator, or to deter future wrongdoing.
Adelanto, California civil litigation is rather designed to make sure that individuals who injure someone else due to intentional or negligent conduct are made to compensate their victims for the harm they caused. This compensation almost always takes the form of money. Other relief, such as injunctions, can also be made available under some circumstances, but this is rare.
Many different instances that might lead to civil litigation in Adelanto, California. Remember, a legal wrong can be committed in almost any situation. Of course, there are some situations that give rise to civil litigation in Adelanto, California more often than others.
Employment: The employer / employee relationship is one of the more frequent sources of civil litigation in Adelanto, California. Wage and hour violations, racial discrimination, and on-the-job injuries can all lead to civil litigation.
Personal Injury: When an individual suffers a physical injury caused by the negligent or intentional conduct of another person, the law of Adelanto, California authorizes them to seek compensation from the person who caused the harm. Civil litigation is normally the best way to seek this compensation, if the person who injured you (as is often the case) is unwilling to voluntarily compensate you for the harm they caused. Normally, a court will order the defendant to pay the plaintiff money as compensation. When this is inadequate, other relief, such as injunctions, can be made available.
Family: Family relations in Adelanto, California can be a source of serious friction, as you may already know. The most serious disputes normally come up during and after a divorce, and often involve disagreements over the distribution of marital property, child custody, and child or spousal support.
How Can a Adelanto, California Lawyer Help?
Adelanto, California civil litigation can be pretty complex, and often emotionally charged. Civil litigation issues can also arise when you least expect them.
Thus, it's always a good idea to find a lawyer in Adelanto, California who specializes in civil litigation, if it looks like you're going to be facing a civil litigation issue in the near future.