text:
\section{Introduction}

The unstable isotope $^{26\!}$Al\  has a mean lifetime of 1.04 Myr. $^{26\!}$Al\
first decays into an excited state of $^{26}$Mg, which de-excites
into the $^{26}$Mg ground state by emitting gamma-ray photons with
the characteristic energy of 1809 keV . The 1809 keV gamma-ray
line from radioactive $^{26\!}$Al\  serves as a tracer of the recent
nucleosynthesis activity in the Galaxy.

The 1809 keV $\gamma$-ray line emission from the Galaxy was first
detected with the Ge spectrometer on the HEAO-C space experiment
(Mahoney et al. 1982). The Compton Observatory sky survey
1991-2000 then with COMPTEL imaging of the $^{26\!}$Al\  line across the sky
showed that $^{26\!}$Al\  emission extends along the Galactic plane, thus
clearly establishing $^{26\!}$Al\  nucleosynthesis as a widely-distributed
Galactic phenomenon (Diehl et al. 1995, Pl\"uschke et al. 2001).
The structure of this emission, alignments of emission maxima with
spiral-arm tangent, and comparisons with tracers of candidate $^{26\!}$Al\
sources, all point to a predominant origin of $^{26\!}$Al\  in massive stars
(Prantzos and Diehl 1996, Chen et al. 1995, Diehl et al. 1995,
Kn\"odlseder 1999).

The detailed study of $^{26\!}$Al\  line emission from the Galaxy is one of
the main science goals of the INTEGRAL mission. SPI aboard
INTEGRAL is a high-resolution spectrometer with energy resolution
of 3 keV (FWHM) at 1809 keV, which therefore adds high-resolution
spectroscopic information to $^{26\!}$Al\  astronomy. The Compton
Observatory in its early design phase included a fifth instrument
`GRSE', a high-resolution spectrometer later abandoned for cost
and complexity reasons. COMPTEL as a scintillation-detector based
instrument had modest spectral resolution of about 10\% (FWHM).
The detailed measurement of $^{26\!}$Al\  line position and shape is
expected to reveal more information beyond the COMPTEL imaging
survey about the $^{26\!}$Al\  sources and their location through the
Doppler effect, induced from Galactic rotation and dynamics of the
ejected $^{26\!}$Al\  as it propagates in the interstellar medium around its
stellar sources.

Earlier INTEGRAL analysis had used 1.5 years of SPI data to first
explore the large-scale spectral characteristics of $^{26\!}$Al\  emission
in the inner Galaxy (Diehl et al. 2006a, 2006b). A detection of
the $^{26\!}$Al\  line from the inner Galaxy with a significance of $\sim
16\sigma$ confirmed the narrowness of the $^{26\!}$Al\  line (FWHM $<2.8$
keV, $2\sigma$), which had already been seen by RHESSI (Smith et
al. 2003) and HEAO-C (Mahoney et al. 1984) earlier. We use
INTEGRAL/SPI data accumulated from five years to extend this study
towards spatially-resolved details of $^{26\!}$Al\  line spectroscopy across
the inner regions of the Galaxy. In this paper, we concentrate on
the spectral and intensity variations of $^{26\!}$Al\  emission along the
Galactic plane. The main goal is to explore if there are
variations from the large-scale properties of $^{26\!}$Al\  emission, such
as bulk motion or enhanced turbulence in specific regions. Our
study will be limited by the brightness of the signal per region,
and hence proceed from broad to more constrained regions along the
plane, as the current exposure and $^{26\!}$Al\  brightness allows; with
more exposure, in particular towards outer regions of the Galaxy
at higher longitudes, the extended INTEGRAL mission is expected to
eventually allow such studies up to the spatial resolution of
about 2.8$^{\circ}$ (FWHM) of the SPI instrument. We also derive
spectra for separate regions of Galactic latitudes, to probe the
symmetry and the scale height of Galactic $^{26\!}$Al\  emission.

In this paper, we first describe the SPI observations and
methods of data analysis. Then we proceed with an update of the
large-scale characteristics of Galactic $^{26\!}$Al\  emission, before
refining the spatial resolution of our study. We discuss the
implications of our findings with respect to the large-scale
distribution of $^{26\!}$Al\  sources, the interstellar medium in their
vicinity, and possible regional deviations.
Studies of specific regions and their $^{26\!}$Al\  emission are underway
and will be reported in separate papers
 (Cygnus -- Martin et al., in preparation; Orion -- Lang et al.,
 in preparation; Sco-Cen -- Diehl et al., in preparation).

\begin{figure}
\centering
\includegraphics[angle=0,width=8.5cm]{f1_exposure.eps}
\caption{Exposure of the sky in Galactic coordinates (the number
at the color bar in units of ksec) for the data selected from
5-year SPI observations for our $^{26\!}$Al\  study (INTEGRAL orbits 43 --
650). The database covers the whole sky, with 29736 individual
pointings, equivalent to a total (deadtime-corrected) exposure
time of 61 Ms. Observations emphasize the Galactic plane,
specially in the inner Galaxy region, but also specific regions of
interest such as Cas A, Cygnus, Carina-Vela, Orion, Virgo, and the
Crab pulsar and nebula.}
\end{figure}

\section{Observations and Data Analysis}

\subsection{SPI observations}

The INTEGRAL spacecraft was launched on October 17, 2002, into a
high-inclination, high-eccentricity orbit intended to avoid the
increased background from the Earth's trapped radiation belts.
INTEGRAL's orbital period is $\sim$ 3 days. The spectrometer SPI
consists of 19 Ge detectors actively shielded by a BGO
anti-coincidence shield. It has a tungsten coded mask in its
aperture which allows imaging at $\sim 2.8^{\circ}$ resolution
within a $16^{\circ} \times 16^{\circ}$ full coded field of view
(imaging on INTEGRAL is mainly performed at lower energies by the
IBIS telescope, with which SPI is co-aligned). The Ge detectors
are sensitive to gamma-rays between 15 keV and 8 MeV, with a total
effective area $\sim 70$ cm$^{2}$ at 1 MeV, and achieve an energy
resolution of $\sim 2.5$ keV at 1 MeV (Roques et al. 2003,
Atti\'{e} et al. 2003). However, cosmic-ray (CR) impacts degrade
this resolution over time, and the instrument SPI is periodically
switched off for 14 days twice a year while annealing (by heating
from cryogenic temperatures $\sim$ 80 K to 100$^{\circ}$C) is
applied to the detectors to restore the energy resolution back to
its pre-launch value by thermal curing heating of the CR-induced
defects (Roques et al. 2003, Leleux et al. 2003).

In space operations, INTEGRAL with its IBIS and SPI telescopes is
pointed with a fixed attitude for intervals of typically $\sim
2000$ s (referred to as {\em pointings\/}), which are successively
arranged as a standard pattern of neighbouring pointings $\simeq
2^\circ$ apart ({\em dithering\/}), and covering target region of
interest for improved imaging (Jensen et al. 2003; Courvoisier et
al. 2003).

We obtain a database from the 5-year SPI observations, i.e. from
the INTEGRAL orbits 43 -- 650, which encompasses 29736 pointings
of the spacecraft and its instruments across the sky, equivalent
to a total deadtime-corrected exposure time of 61 Ms (see the
exposure map in Figure 1).

The instrument operation has been interrupted from a few short
anomalies and the occurrences of solar flares, and most
significantly for the typically two-week annealing episodes
described above, and by the regular perigee passages with
switch-offs due to the high background intensity from the
radiation belts. The sensitivity of our observations were further
reduced by the failure of two of the 19 detectors (December 2003
and July 2004).

\begin{figure}
\centering
\includegraphics[width=9.0cm]{f2_gesat_bkg_color.eps}
\caption{The unfiltered total GEDSAT rates and background rates
for detector 0 around 1809 keV in model fittings versus time (the
INTEGRAL Julian Date, starts at 1 Jan 2000). The total GEDSAT
rates per detector generally vary in a range from 150 -- 300
counts/s, but some erratic cases like zero values and solar flare
spikes are excluded from science analysis with our primary
selections (also see the text). }
\end{figure}

\begin{figure*}
\centering
\includegraphics[width=8.5cm]{f3_c26al_me_map.eps}
\includegraphics[width=8.5cm]{f3_hmdisk_map.eps}
\caption{The COMPTEL maximum entropy $^{26\!}$Al\  map (left, Pl\"uschke et
al. 2001, hereafter COMPTEL MaxEnt) and a homogenous disk model
(right, hereafter Homo Disk, constant brightness along longitudes,
exponential-like in latitudes with scale height 200 pc) for the
inner Galaxy as the input sky models in the model fitting.  }
\end{figure*}

\begin{figure*}
\centering
\includegraphics[width=8cm]{f4_residues_pnt.eps}
\includegraphics[width=8cm]{f4_residues_eng.eps}
\caption{Residuals versus time (pointings, per 30 min, left) and
energies (right) after model fitting of the inner Galaxy region
for the SE database. Residuals around zero confirm that our
background models are adequate, with $\chi^2/d.o.f. = 0.958$ in
model fittings.}
\end{figure*}

\subsection{Data Analysis}

Our data analysis steps include: (1) selection and assembly of
data which are free of contaminations by anomalies and, e.g.,
solar-flare events; (2) modelling the instrumental background; (3)
deriving spectra by fitting the measured data in narrow energy
bins with our background model and a model of the spatial
distribution of celestial gamma-ray emission, folded through the
instrumental response into the data space of the measurement.
These steps have been described in several papers, e.g. Strong et
al. (2005), Diehl et al. (2003), and as applied to gamma-ray lines
specifically in Wang et al. (2007) and Diehl et al. (2006b). Here
we give a concise summary and add comments as relevant for the
studies of this paper.

We first apply a selection filter to reject corrupted or invalid
data. This is done for data sections called `science window',
typically a time interval of $\sim 30$ minutes corresponding to
one pointing. We apply selection windows to `science housekeeping'
parameters such as the count rates in several background tracers,
proper instrument status codes, and orbit phase. For tracing
background, we employ the SPI plastic scintillator anticoincidence
counter (PSAC), and the rate of saturating events in SPI's Ge
detectors (i.e., events depositing $>$ 8 MeV in a single Ge
detector; hereafter referred to as GEDSAT rates, see Figure 2).
This leads to exclusions of solar-flare periods and other periods
of clearly increased / abnormal backgrounds. Additionally, regular
background increases during and after passages through the Earth's
radiation belts are eliminated through a 0.05--0.916 window on
orbital phase.

From the selected events, spectra are accumulated per each
detector and pointing in energy bins of 0.5~keV in the spectral
range of 1785 -- 1826 keV, and together with dead time and
pointing information assembled into the analysis database. From
identically-selected data, we also establish a database for the
background modelling from the adjacent continuum, combining
broader spectral ranges on both sides of the $^{26\!}$Al\  line into single
bins.

We select events which trigger one and only one of our 19 Ge
detectors ('single events', SE). We exclude the $\simeq$50\%
fraction of 'multiple' events, because for events interacting in
more than one detector different combinations of single-detector
energies with their correspondingly-different resolutions would be
superimposed for identical values of total energy, thus leading to
an ill-determined spectral energy response. This reduces the total
signal obtained, but guarantees that the spectral response of the
instrument is well-defined for our dataset.

Instrumental background is dominated by a rather smooth spectral
continuum, with instrumental lines superimposed - for our case, a
broad instrumental-line feature centered at 1810~keV comprises
~30\% of the count rate (see Fig. 2 in Diehl et al. 2006b). For
our model of the continuum background, we make use of the
simultaneously-measured events in energy bands adjacent to the $^{26\!}$Al\
line region, at 1785~--~1802~keV plus 1815~--~1826~keV, and use
each detector's count rates in this adjacent range to normalize
the GEDSAT time series with their superior statistical precision
at regular intervals of several days. In Figure 2 we show both the
original GEDSAT count rate history and the background model for
one of our detectors, as it varies over the dataset. It is seen
that anomalous spikes of our background are excluded from our
data, and that there still is significant temporal structure in
our fitted background model. This `adjacent-energies' background
variation model per detector thus is based on high-statistics
GEDSAT rates over short time scales of $\sim$ 100 pointings, as
these have been found to trace the prompt CR activation rather
well. Adjusting these 'templates' to the actual counts per
detector in the 0.5 keV bins used for spectral analysis of the sky
signal then ensures that over longer time scales (typically 3
days, where counts in those narrow bins are statistically
sufficient) any second-order deviations from GEDSAT tracing actual
backgrounds are accounted for. Through this procedure we ensure
that pointing-to-pointing variations are given by our background
tracer, independent of the coded-mask orientation on the sky. The
broad instrumental line feature centered at 1810 keV is actually
found to also be rather well modelled by these 0.5~keV bin
adjustments, indicating that the line and continuum backgrounds
have similar temporal behaviour.

The cosmic-signal spectra are obtained from our measured database
of detector spectra when we combine above background models with a
spatial model for sky emission (Figure 3), allowing for
adjustments of intensity parameters for background and sky
intensities per energy bin:

\begin{equation} D_{e,d,p}=\sum_{m,n}\sum_{j=1}^{k_1}
A_{e,d,p}^{j,m,n}\beta_s^j I_j^{m,n} + \sum_t
\sum_{i=1}^{k_2}\beta^i_{b,t} B^i_{e,d,p} + \delta_{e,d,p}, \end{equation}
where {\it e,d,p} are indices for data space dimensions: energy,
detector, pointing; {\it m,n} indices for the sky dimensions
(galactic longitude, latitude); $A$ is the instrument response
matrix, $I$ is the intensity per pixel on the sky,
$k_1$ is the number of independent sky intensity distribution
maps; $k_2$ is the number of background components, $\delta$ is
the count residue after the fitting. The coefficients $\beta_s$
for the sky map intensity are constant in time, while
$\beta_{b,t}$ is allowed time dependent, to cater for different
background normalizations for each camera configuration of
19/18/17 functional detector elements. The sky brightness
amplitudes $\beta_s$ comprise the resultant spectra of the signal
from the sky. We generally use a maximum-likelihood fitting method
(implemented in a SPI standard tool called {\em spimodfit},
properly accounting for Poisson statistics in our spectra; for
more details, see Strong et al. 2005).

We thus obtain per energy bin the fitted intensity parameter
values with their uncertainties, their covariance matrices, and
the fit residuals. Analysis of residuals, uncertainties, and
covariance matrices are made to determine the validity of the fit
of such a combined model to our measured set of spectra. Residuals
after the model fitting are shown in Figure 4 (residuals with the
time and energies). Reduced $\chi^2$ values around 1.0 confirm
that both our background model and the sky distribution model(s)
are adequate.

We use the sky intensity distribution of $^{26}$Al as derived from
9 years of COMPTEL observations (maximum entropy map, Pl\"uschke
et al. 2001) as the standard reference sky model. We compare this
to different $^{26\!}$Al\  emission tracer models or maps, to assess the
impact of different sky distribution models on the $^{26\!}$Al\  line shape
and intensity (see \S 3). For simultaneous fits of sets of
partial-sky distribution models (in order to derive
spatially-resolved spectra), we use analytical forms of sky
distribution models with prescribed symmetry to avoid biases to
such analysis (see below).

After we obtain fitted-amplitude coefficient spectra for the sky
components, we characterize these spectra and in particular the
$^{26\!}$Al\  line details therein through two different approaches. When
the sky signal is weak, we fit the spectra with Gaussians plus a
linear residual background, and use the Gaussian intensities,
centroid energies, and FWHM widths for relative comparisons, such
as trends along the plane of the Galaxy. When the signal is
sufficiently strong so that we are sensitive to line width
details, we describe the line component not by a single Gaussian
any more, but rather by the convolution of a Gaussian with the
asymmetric instrumental line response as it develops from
degradation of our detectors' resolution and their periodic
restorations through annealings. This allows us to infer immediate
information about the celestial $^{26\!}$Al\  dynamics, which we identify
with this Gaussian, and in particular its width, which arises from
Doppler shifting of the line energies with motion of decaying $^{26\!}$Al\
nuclei relative to the observer. In both cases, we fit these
spectral models to the amplitude values and their uncertainties as
determined from the model fit to the large set of spectra,
performing a maximum-likelihood fit with the Levenberg-Marquardt
algorithm. In the latter case, we derive the entire probability
distribution of the fitted parameter values through a Monte Carlo
Markov Chain (MCMC) method, which allows us in particular to
determine probability constraints for the celestial $^{26\!}$Al\  line
broadening from kinematics. This parameter challenges the spectral
resolution of our instrument (about 3~keV at the $^{26\!}$Al\  line energy),
hence so far is bounded from above only. Such asymmetric parameter
probability distributions may be far from Gaussian, hence require
such more sophisticated treatment (Kretschmer et al. 2009, in
preparation).

\section{$^{26\!}$Al\  in the Inner Galaxy -- An Update}

The spectral characteristics of $^{26\!}$Al\  emission in the inner Galaxy
serve to study the current nucleosynthesis activity and the
properties of the interstellar medium near the $^{26\!}$Al\  sources on a
large-scale averaged scale. We define the ``inner Galaxy'' as the
region $-30^\circ < l < 30^\circ, \ -10^\circ < b <10^\circ$), and
may use this as a representative region for this purpose, since it
coincides with the bright ridge of observed 1809~keV emission as
observed along the plane of the Galaxy. We specifically exclude
regions at higher longitudes such as Cygnus: This region in
particular has been recognized as special, in its supernova to
Wolf-Rayet ratio, for example (Kn\"odlseder et al. 2004); other
emission at large longitudes also may be deviant from the Galactic
average and over-emphasized because nearby. We therefore believe
that using the $-30^\circ < l < 30^\circ$ region will give us a
more representative picture of $^{26\!}$Al\  source environments in the
Galaxy.

\begin{figure*}
\centering
\includegraphics[angle=0,width=8.5cm]{f5_l_spec_c26me_gauss.eps}
\includegraphics[width=8.5cm]{f5_r_spec_c26me_resp.eps}
\caption{Spectrum derived from sky model fitting using the COMPTEL
$^{26\!}$Al\  Maximum Entropy image. The left figure shows the $^{26\!}$Al\  line
fitted with a Gaussian, the width of $\sim$ 3.16 keV (FWHM) being
consistent with instrumental line widths around 1.8 MeV. The right
figure shows the line fitted with a composite line-shape model
using the time-averaged instrumental response as it results from
cosmic-ray degradation and annealings during the time of our
measurement, convolved with a Gaussian representing the cosmic
(intrinsic) $^{26\!}$Al\  line width. The latter is found to be ($< 1.3$
keV, 2$\sigma$). Both fits find that the line is intrinsically
narrow. Systematic variations of derived line fluxes using two
spatial models are less than the statistical uncertainty in the
measurement (fluxes are quoted in units of $10^{-4}\ \mathrm{ph\
cm^{-2}\ s^{-1}\ rad^{-1}}$)}.
\end{figure*}

Fitting our set of observations to the sky intensity distribution
of the $^{26\!}$Al\  maximum entropy image (MaxEnt) from COMPTEL (Figure 3,
left), we obtain the updated inner-Galaxy $^{26\!}$Al\  emission spectrum
shown in Figure 5. MaxEnt is one possible sky intensity
distribution compatible with the COMPTEL data. The $^{26\!}$Al\  line is
detected at $\sim 28\sigma$ significance.

The {\bf $^{26\!}$Al\  gamma-ray flux} from the inner
Galaxy turns out as $(2.93\pm 0.15)\times 10^{-4}$ ph\ cm$^{-2}$\ s$^{-1}$\
rad$^{-1}$. This is consistent with our earlier values $(3.3\pm 0.4)\times 10^{-4}\
\mathrm{ph\ cm^{-2}\ s^{-1}\ rad^{-1}}$ (Diehl et al. 2006a,
2006b), and also with the COMPTEL imaging-analysis
value of $(2.8\pm 0.4)\times 10^{-4}$ ph\ cm$^{-2}$\ s$^{-1}$\
rad$^{-1}$ (Pl\"uschke et al. 2001).
The above value is derived using an asymmetric line shape as best matching
our expectations from SPI's spectral response and eventual additional celestial
line broadening the total $^{26\!}$Al\  gamma-ray flux of
the Gaussian fit as determined for the inner Galaxy region is
$(2.73\pm 0.17)\times 10^{-4}\ \mathrm{ph\ cm^{-2}\ s^{-1}\
rad^{-1}}$.

In our model-fitting approach to derive $^{26\!}$Al\  spectra from
SPI spectra per pointing (Eq. 1),  the adopted sky distribution models may
affect the $^{26\!}$Al\  flux and line shape results.
We estimate the variations and potential systematic uncertainties
introduced by the spatial distribution model of the $^{26\!}$Al\  emission
through variation of this sky distribution model within a plausible range.

Our ``standard'' is the measurement of $^{26\!}$Al\  gamma-ray emission
directly, from COMPTEL. Uncertainties from COMPTEL imaging
analysis have however been shown to allow for a range of images
which are consistent with the COMPTEL measurements (Kn\"odlseder
et al. 1999). We consider the MaxEnt image the compromise between
making use of COMPTEL's imaging resolution of about 3.8$^\circ$
(FWHM) and the attempts to suppress artifacts from statistical
noise. A more conservative COMPTEL image is obtained from the
Multi-resolution Expectation Maximization method (MREM), which
carefully eliminates noise contributions at each iteration and
builds up the image starting from large spatial scales,
terminating once the image obtained does not need further
refinement in this statistical sense (Kn\"odlseder et al. 1999;
Kn\"odlseder 1999). The smooth MREM image from COMPTEL also shows
the inner Galactic ridge as well as Cygnus being bright in $^{26\!}$Al\
emission, yet does not show the few-degree scale features of the
MaxEnt map; we consider these two maps as adequate tests for
systematics from the range of direct $^{26\!}$Al\  measurements.

Considering the limitations of gamma-ray telescopes, it has been
plausible to alternatively use maps obtained in
astronomically-more developed wavelength bands, once it it clear
that those trace $^{26\!}$Al\  sources in the Galaxy. Detailed studies have
shown (Kn\"odlseder et al. 1999; Diehl et al. 1996) that among the
best tracers of $^{26\!}$Al\  sources are (1) the infrared emission of warm
dust grains, mapped with the COBE/DIRBE and arising from radiative
heating of dust around clusters of massive stars (Bennett et al.
1996), and (2) radiation of free electrons (free-free emission,
Bremsstrahlung) observed at radio frequencies with the WMAP
satellite, arising from the ionizing massive-star radiation around
massive star clusters. From astrophysical arguments, also maps of
interstellar gas in different forms should trace the locations and
space density of $^{26\!}$Al\  sources. (3) Molecular gas is observed
through CO line emission at radio frequencies, and has been mapped
in rather fine resolution (Dame et al., 1987 and 2001), (4) atomic
hydrogen (HI) sky surveys have been accumulated (e.g. Dickey and
Lockman 1990), and (5) cosmic-ray interactions with interstellar
gas produces penetrating continuum gamma-ray emission which has
been mapped in the EGRET sky survey (Hunter et al. 1997).

Finally, analytical models for the distribution of $^{26\!}$Al\  sources
have been constructed, based on above knowledge of Galactic
structure in its different components (Robin et al. 2003),
properly weighted from astrophysical arguments. (6)
Double-exponential functions (in galactocentric radius, and scale
height above the Galactic plane) have been constructed, as well as
more sophisticated models including (7) spiral structure
components and building on the distribution of free electrons in
the Galaxy as derived from pulsar dispersion measurements (Taylor
\& Cordes 1993, and Cordes \& Lazio 2002). The scale height of $^{26\!}$Al\
sources has been found to lie between the molecular disk (about
50~pc) and the thick disk (about 0.3-1~kpc), with plausible values
around 200~pc.

We compare $^{26\!}$Al\  line spectra determined from these different models
and tracers of $^{26\!}$Al\  sources in the Galaxy. Fifteen different sky
distribution maps have been analyzed, and variations on $^{26\!}$Al\
brightness, $^{26\!}$Al\  line centroid and width parameters are shown in
Figure 6. Systematic variations are within statistical
uncertainties, when we vary the spatial models for $^{26\!}$Al\  emission.
We use their scatter to estimate a ``systematic'' uncertainty,
which turns out as $(2.9\pm 0.2)\times 10^{-4}{\rm ph\ cm^{-2}\
s^{-1}\ rad^{-1}}$, $1809.0\pm 0.09$ keV, $0.5 \pm 0.45$ keV for
the flux, centroid, and width parameters (with 1$\sigma$ error
bars), separately.

As before (Diehl et al., 2006a), we convert our measured $^{26\!}$Al\
intensity into an estimate of the {\bf total current $^{26\!}$Al\  mass} in
the Galaxy, using an assumed geometrical source-distribution model
to extrapolate across the entire Galaxy from our inner-Galaxy
normalization of such a model, as discussed above. This is
required because the flux to mass conversion relies on $^{26\!}$Al\  source
distances, not measured directly in projected sky brightness distribution
maps. Several three-dimensional distribution models are applied and
compared here, e.g.,  an exponential disk model, a ``young-disk''
model, a geometrical representation based on dust emission, and
a multi-component model including spiral-arm structures and based
on abundances of free electrons in interstellar space.
We vary scale height parameters of the appropriate components
to also study the latitude extent of the $^{26\!}$Al\  emission. In all models,
we have taken the distance of the Sun to the Galactic center as
$R_0=$ 8.5~kpc ($^{26\!}$Al\  mass sensitively depends on $R_0$, smaller
$R_0$ will globally reduce the size of the Galaxy, and result in
the smaller amount of $^{26\!}$Al\ ).

The average measured $^{26\!}$Al\  flux of $(2.9\pm 0.2) \times 10^{-4}\
\mathrm{ph\ cm^{-2}\ s^{-1}\ rad^{-1}}$ for the inner Galaxy thus
translates into a Galactic $^{26\!}$Al\  mass of $(2.7\pm 0.7)$ $M_\odot$\  using a
plausible scale height of 180 pc. If we ignored the ejection of
$^{26\!}$Al\  into surrounding cavities and corresponding champagne flows
(see our own scale height determination below), and used the lower
scale heights of O stars or of the molecular disk, we would obtain
lower total amounts around or even below 2 $M_\odot$\ . This emphasizes
the need for spatially-resolved $^{26\!}$Al\  studies (see Sect 5 and Fig.
12 below). The quoted uncertainty here includes both the
statistical uncertainty as propagated from the fitting method, and
the systematical uncertainty derived from variations among
plausible representations of the sky distribution of the emission
plus alternative 3-dimensional $^{26\!}$Al\  source distribution models (see
also Figure A4.1 in Supplemental materials of Diehl et al. 2006a).

The {\bf line width} of $^{26\!}$Al\  conveys global information about the
spread in projected velocities of $^{26\!}$Al\  nuclei when they decay and
emit characteristic 1809~keV gamma-rays. Astrophysical origins of
$^{26\!}$Al\  line width may come from two effects: random motions in the
interstellar medium (Chen et al. 1997) and Galactic differential
rotation (Kretschmer et al. 2003). A line broadening of $\sim$ 1
keV from our line-shape constraints corresponds to thermal Doppler
velocities of $\sim$ 120 km s$^{-1}$.

The Gaussian used to represent the $^{26\!}$Al\  line (Fig.~5 left) shows a
width of $3.16\pm 0.15$ keV (FWHM), consistent with the
instrumental width determined as $\sim 3.1$ keV near 1809~keV from
nearby instrumental lines at 1764 and 1779~keV. This indicates
that the cumulative $^{26\!}$Al\  line emission in the inner Galaxy is
intrinsically rather narrow in energy around the laboratory value,
with little kinematic Doppler broadening, well below SPI's energy
resolution.

\begin{figure*}
\centering
\includegraphics[width=5.5cm]{f6_centroid.eps}
\includegraphics[width=5.5cm]{f6_flux.eps}
\includegraphics[width=5.5cm]{f6_width.eps}
\caption{Comparison of the three line parameters (centroid energy,
flux, width, with 1 $\sigma$ error bars) derived in model fittings
for different distribution models: 1. COMPTEL maximum entropy $^{26\!}$Al\
emission map (Pl\"uschke et al. 2001); 2. COMPTEL MREM $^{26\!}$Al\
emission map (Pl\"uschke et al. 2001); 3. an exponential disk
model (scale radius 4 kpc, scale height 180 pc); 4. a homogenous
disk model (Fig. 3); 5. HI (Dickey \& Lockman 1990); 6. CO (Dame
et al. 1987); 7. radio 408 MHz (Haslam et al. 1995); 8. DIRBE/COBE
240$\mu$m (Bennett et al. 1996); 9. IRAS 12$\mu$m (Wheelock et al.
1991); 10. EGRET ($>100 $ MeV, Hunter et al. 1997); 11. a young
disk model (Robin et al. 2003); 12. the free electron density
distribution model (TC93, scale height 150 pc, Taylor \& Cordes
1993) 13. TC93, scale height 300 pc; 14. the free electron density
distribution model (NE2001, scale height 140 pc, Cordes \& Lazio
2002); 15. NE2001, scale height 330 pc. }
\end{figure*}

For such a strong signal, we can be more ambitious, however, and
attempt to quantitatively constrain the intrinsic (celestial) line
broadening in a statistical probability analysis as described
above (see also Diehl et al. 2006b and Kretschmer et al. 2004). We
know the instrumental line response of our instrument at each
epoch of the mission from detailed studies of a large number of
instrumental lines. The response gradually degrades and develops
an increasing tail component on the low-energy side of the
photopeak energy, due to incomplete charge collection as the
detector's Ge lattice experiences damaging from cosmic-ray
impacts. Annealings restore better charge collection and a
symmetric instrumental-line response whose width is determined and
dominated by statistics of the charge collection. We assemble the
effective instrumental-line response for our study through
appropriate weightings of these time-dependent responses. Then we
fit the convolution of a parameterized Gaussian with this response
shape function, and thus derive values for the celestial $^{26\!}$Al\  line
centroid energy and broadening. MCMC sampling of the probability
distributions of these parameters then allows us to translate the
parameter value uncertainties into probability constraints by
integrating over these distributions. In particular, the
probability distribution of the intrinsic width may not peak at
zero, indicating a small but by itself non-detectable broadening
of the line. In this case, our approach yields a reliable estimate
of the upper bound on line broadening, which is the
astrophysically-relevant quantity to constrain kinematics of
decaying $^{26\!}$Al\  nuclei in the interstellar medium. The fitted
parameters are the line centroid, the intrinsic width of celestial
$^{26\!}$Al\ , the intensity of the line, and two parameters for the
underlying continuum (see Figure 5 right). The intrinsic line
width is now constrained to $<1.3$ keV (2 $\sigma$, which is
consistent and yet significantly smaller than the earlier
constraints based on fewer SPI data (Diehl et al. 2003, 2006b).

\begin{figure*}
\centering
\includegraphics[width=8.5cm]{f7_l_HomoDisk_l0.eps}
\includegraphics[width=8.5cm]{f7_r_HomoDisk_l-60.eps}
\caption{$^{26\!}$Al\  spectra for two Galactic quadrants ({\bf left}
$0^\circ < l < 60^\circ$, and {\bf right} $-60^\circ < l <
0^\circ$). Line centroids relative to the centroid energy of $^{26\!}$Al\
line in the laboratory (1808.65 keV) show a significant blueshift
in the 4th quadrant. Both the spectra have width values near the
value of the instrumental line width, implying that $^{26\!}$Al\  emissions
from two quadrants are the narrow lines. In addition, the $^{26\!}$Al\  flux
of the 4th quadrant is higher than that of the 1st quadrant, and
the flux ratio is $\sim 1.3$. }
\end{figure*}

In the inner Galaxy,  Galactic differential rotation alone can
lead to significant Doppler shifts towards specific longitudes
where the projected-velocity differences with respect to the solar
orbit reach maxima; line broadening results if we integrate over a
larger longitude range with different bulk velocity differences.
Kretschmer et al. (2003) have simulated the $^{26\!}$Al\  line shape
diagnostics in the inner Galaxy due to Galactic rotation and $^{26\!}$Al\
ejection from sources, and find that line broadening of up to 1
keV is expected if the signal is integrated over the inner region
of the Galaxy. Our present large-scale line-shape constraints are
consistent with these expectations.

If we interpret line broadening of the $^{26\!}$Al\  line from the inner
Galaxy in terms of interstellar-medium characteristics, the
intrinsic-width constraint of $<1.3$ keV corresponds to 160
km~s$^{-1}$ as a corresponding 2$\sigma $ limit on ISM velocities.
This is well within the plausible and acceptable range for the
environment of normal interstellar-medium turbulence (Chen et al.
1997), leading us to conclude that, within uncertainties, the
average velocities of decaying $^{26\!}$Al\  in the Galaxy are not
abnormally-high (compare discussion after Naya et al. 1996 in Chen
et al. 1997).

In summary, the measured line width of $^{26\!}$Al\  from the inner Galaxy
is consistent with Galactic rotation and modest
interstellar-medium turbulence around the sources of $^{26\!}$Al\ . This
confirms earlier results on the $^{26\!}$Al\  line width from HEAO-C
(Mahoney et al. 1984), RHESSI (Smith 2003), and SPI on INTEGRAL
(Diehl et al. 2006b). The GRIS balloon experiment had reported a
very broad line with a width $\sim 5.4$ keV (Naya 1996), which is
inconsistent with these measurements and clearly ruled out. This
is reassuring: within uncertainties, the average velocities of
decaying $^{26\!}$Al\  in the Galaxy are not abnormally-high (see discussion
in Chen et al. 1997).

\begin{figure*}
\centering
\includegraphics[angle=0,width=7.5cm]{f8_tl_HomoDisk_l0.eps}
\includegraphics[angle=0,width=7.5cm]{f8_tr_HomoDisk_l30.eps}
\includegraphics[angle=0,width=7.5cm]{f8_bl_HomoDisk_l-30.eps}
\includegraphics[angle=0,width=7.5cm]{f8_br_HomoDisk_l-60.eps}
\caption{$^{26\!}$Al\  spectra of four segments along the Galactic plane (
$-60^\circ < l < 60^\circ$).  }
\end{figure*}

The relative position of {\bf the $^{26\!}$Al\  gamma-ray line centroid}
with respect to the laboratory-determined $^{26\!}$Al\  decay energy value
of 1808.65 $\pm 0.07$~keV (Firestone \& Ekstr\"om 2004) yields
information on potential bulk motion of $^{26\!}$Al\  in the Galaxy. The $^{26\!}$Al\
line centroid energy from the whole inner Galaxy is determined at
$1808.92\pm 0.06$ keV from the Gaussian fit and $1809.03\pm 0.08$
keV from the instrumental-response-convolved fit, even after
considering uncertainties, the measured centroid energy is  higher
than the laboratory value. The effect of this blueshift for the
whole inner Galaxy will be discussed below.

In our determination of $^{26\!}$Al\  line properties, we represent the
spectra derived from detailed model fitting by a line component
for $^{26\!}$Al\  plus a linear component which could capture any underlying
systematics in our background or sky modellings. We expect that
our adjacent-energy background model component will eliminate
Galactic continuum emission, at least to first order, if the
spectral shape is rather flat across our 40~keV energy range
(1785--1826~keV). The diffuse gamma-ray continuum in the inner
Galaxy is $\sim 2\times 10^{-6}\ \mathrm{ph\ cm^{-2}\ s^{-1}
rad^{-1}\ keV^{-1}}$ in the energy band of 1 -- 2 MeV (Strong et
al. 1999). Indeed, we find that offsets above zero in our spectra
are rather small and negligible, supporting this property of our
background model.

\section{$^{26\!}$Al\  emission along Galactic longitudes}

The 9-year COMPTEL imaging of $^{26\!}$Al\  line emission had already
suggested some asymmetry in the inner Galaxy: the fourth Galactic
quadrant appears somewhat brighter than the first quadrant
(Pl\"uschke (2000) finds a significance of 2.5$\sigma$ for a
brightness difference). COMPTEL could provide the image details of
$^{26\!}$Al\  in the Galaxy, but no significant spectral information due to
its spectral resolution of about 150~keV near the $^{26\!}$Al\  line. SPI
with its Ge detectors features sufficiently-high spectral
resolution to allow astrophysical constraints from $^{26\!}$Al\  line
shapes, averaged over the Galaxy as discussed above, but also for
different regions along the Galactic plane due to its imaging
properties as a coded-mask telescope.

\begin{figure}
\centering
\includegraphics[width=8.5cm]{f9_HomoDisk_l-5.eps}
\caption{$^{26\!}$Al\  spectrum from the  Galactic center ($-5^\circ<l<
5^\circ,\ -10^\circ<b< 10^\circ$). The determined line centroid
energy ($1808.58\pm 0.27$ keV) is consistent with the laboratory
value.}
\end{figure}

In this section, we will proceed towards increasing spatial
resolution along the Galactic plane, starting out from testing
Galactic asymmetries between the first and fourth quadrant. $^{26\!}$Al\
line parameters toward the different directions of the Galactic
plane are determined using separate sky maps covering each sky
region, simultaneously fitting these together with our background
model to the entire sky survey database. $^{26\!}$Al\  line fluxes, centroid
energies, and line widths then are derived by a simple Gaussian
fit to the $^{26\!}$Al\  line in the resulting spectra, as we are interested
in relative changes between different portions of the sky. This
will allow us to identify line shifts from bulk motion such as
expected from large-scale Galactic rotation, and hints for
additional line broadenings in particular regions, which would
reflect increased $^{26\!}$Al\  velocities in such regions. A homogenous
disk model (see Figure 2 right, $-60^\circ < l < 60^\circ, \
-10^\circ < b < 10^\circ$, scale height 200 pc ) is used here to
avoid a bias of sky distribution models along the Galactic plane,
for such relative comparison.

$^{26\!}$Al\  spectra for the 1st ($0^\circ < l < 60^\circ$) and 4th
quadrant ($-60^\circ < l < 0^\circ$ ) are presented in Figure 7.
In the 4th quadrant we note a blueshift of $0.49\pm 0.07$ keV
relative to the centroid energy of $^{26\!}$Al\  line in the laboratory, but
no significant redshift in the 1st quadrant is apparent ($\sim
0.04\pm 0.10$ keV). Both spectra have width values compatible with
no significant  $^{26\!}$Al\  line broadenings. The indicated $^{26\!}$Al\  asymmetry
between the two inner Galactic quadrants appears again, with a
flux ratio of $\sim 1.3\pm 0.2$.

We proceed further towards more confined Galactic regions using
four sub-maps with 30 degree width along Galactic longitude, to
obtain $^{26\!}$Al\  spectra for these regions shown in Figure 8: (1)
$0^\circ < l < 30^\circ$, (2) $30^\circ < l < 60^\circ$, (3)
$-30^\circ < l < 0^\circ$, and (4) $-60^\circ < l < -30^\circ$.
Centroid energy shifts of the $^{26\!}$Al\  line are found, $+0.15\pm 0.12$
keV and $-0.61\pm 0.09$ keV in regions (1) and (3) respectively,
as expected from large-scale Galactic rotation. The inner region
($-30^\circ < l < 30^\circ$) is seen to be much brighter than the
two outer regions of the Galaxy, consistent with the COMPTEL $^{26\!}$Al\
map (note that here we use a homogeneous sky distribution model as
the model-fitting prior). The indicated $^{26\!}$Al\  emission asymmetry for
the 1st and 4th quadrants also shows up again between regions (3)
and (1), with a flux ratio of $\sim 1.15\pm 0.18$. Even further
out, region (4) may also be brighter than (2) by $\sim 1.6\pm
0.6$. Since smaller regions include less $^{26\!}$Al\  signal, these
differences are, however, not significant.

Challenging the imaging capability of SPI for diffuse and extended
emission, we refine spatial structure even more towards smaller
longitude intervals. In Figure 9, we show a spectrum representing
the Galactic center region ($-5^\circ<l< 5^\circ, -10^\circ
<b<10^\circ$), where the $^{26\!}$Al\  line is still significant ($>
4\sigma$). The line centroid energy is determined at $1808.58\pm
0.27$ keV, and is consistent with the laboratory value -- no line
shift from bulk motion is indicated.

\begin{figure*}
\centering
\includegraphics[angle=0,width=5.5cm]{f10_tl_HomoDisk_l0.eps}
\includegraphics[angle=0,width=5.5cm]{f10_ml_HomoDisk_l20.eps}
\includegraphics[angle=0,width=5.5cm]{f10_bl_HomoDisk_l40.eps}
\includegraphics[angle=0,width=5.5cm]{f10_tr_HomoDisk_l-20.eps}
\includegraphics[angle=0,width=5.5cm]{f10_mr_HomoDisk_l-40.eps}
\includegraphics[angle=0,width=5.5cm]{f10_br_HomoDisk_l-60.eps}
\caption{$^{26\!}$Al\  spectra of six segments along the Galactic plane (
$-60^\circ < l < 60^\circ$). Small longitude degree bin
($20^\circ$) makes the detections of $^{26\!}$Al\  not significant in the
regions of $40^\circ < |l| < 60^\circ$.}
\end{figure*}

Then we also derive spectra for six smaller longitude intervals of
20 degree width along the Galactic plane ($-60^\circ < l <
60^\circ$, see Figure 10). The $^{26\!}$Al\  line is still detected for the
inner Galaxy ($-40^\circ < l < 40^\circ$, $> 6\sigma$ for each
$20^\circ$ bin region), but only marginal for the two outer
regions ($40^\circ < l < 60^\circ$ and $-60^\circ < l <
-40^\circ$, $< 4\sigma$). This may be attributed to both less $^{26\!}$Al\
brightness and to less exposure in these regions, compared to the
inner Galaxy.

For the four inner regions, $^{26\!}$Al\  line centroid shifts are observed.
When we use the $^{26\!}$Al\  line centroid energy of 1808.65 keV from the
laboratory as a reference (rather than our own determination, Fig.
9), we obtain $^{26\!}$Al\  line centroid energy shifts along Galactic
longitudes as shown in Figure 11. Evidently, towards positive
longitudes of $\sim 0^\circ - 40^\circ$, the redshift in energy is
minor, $\sim 0.1$ keV, while for negative longitudes, the
blueshift is substantial, $\sim 0.4$ keV for $-20^\circ <l<
0^\circ$ and up to 0.8 keV for $-40^\circ <l< -20^\circ$. This
asymmetry of $^{26\!}$Al\  line energy shifts along the Galactic plane is
inconsistent with simple azimuthally-symmetric Galactic rotation;
it is clear evidence for pronounced spiral-arm structure in the
inner Galaxy, and possibly peculiar bulk motion along the Galaxy's
bar (e.g. Englmaier \& Gerhard 1999, Hammersley et al. 2007 and
references therein).

Figure 11 shows the intensity distribution of $^{26\!}$Al\  emission (from
the same 20$^{\circ}$ regions, Figure 10) along the Galactic
plane, adding the (longitude-range normalized) Galactic-Center
region $^{26\!}$Al\  intensity  ($|l|< 5^\circ$, Figure 9) for comparison.
The variability of $^{26\!}$Al\  intensity along the Galactic plane again is
evident.

We note that the $^{26\!}$Al\  line in the region of $20^\circ < l <
40^\circ$ appears somewhat broadened, with a Gaussian width of
FWHM$\sim 4.15\pm 0.75$ keV (also see Figure 11). This may hint
towards a peculiar $^{26\!}$Al\  source region towards this direction, which
could be associated with the Aquila region (Rice et al. 2006).
Broadening could result from higher turbulence if the $^{26\!}$Al\  source
region is younger than average and dominated by the $^{26\!}$Al\  ejection
from more massive stars (see Kn\"odlseder et al. 2004). Further
studies would be interesting, and have the potential to identify
star formation otherwise occulted by foreground molecular clouds.

\section{Latitudinal variations of $^{26\!}$Al\  emission}

The interpretation of $^{26\!}$Al\  imaging and spectral results relies on
(uncertain) distances of $^{26\!}$Al\  sources. Along the line-of-sight, the
detected $^{26\!}$Al\  signal could originate from local star-formation
complexes ($\sim 100$ pc), or from the nearest part of the
Sagittarius-Carina arm ($1-2$ kpc), or from the Galactic center
region ($\sim 8$ kpc), or even from the distant side of the Galaxy
($> 10$ kpc).

\begin{figure}
\centering
\includegraphics[angle=0,width=7.5cm]{f11_l_eng.eps}
\includegraphics[angle=0,width=7.5cm]{f11_flux_cBin_c1deg.eps}
\includegraphics[angle=0,width=7.5cm]{f11_fwhm.eps}
\caption{{\bf Top:} $^{26\!}$Al\  line energy shifts along the Galactic
plane ( $-60^\circ <l<60^\circ$, with longitude bin widths of
$20^\circ$, $^{26\!}$Al\  spectra from Figure 10) relative to the line
centroid of the $^{26\!}$Al\  line (fitted energy 1808.65 keV). {\bf
Center:} $^{26\!}$Al\  intensity distribution along the Galactic plane (from
Figures 9, 10). For comparison, the COMPTEL-derived $^{26\!}$Al\  intensity
profile is shown (solid line, and dashed lines when integrated
over the same longitude bins).  {\bf Bottom:} $^{26\!}$Al\  FWHM (Gaussian
fitting) variation along the Galactic longitudes, a broad $^{26\!}$Al\  line
feature is detected toward the longitudes $20^\circ < l <
40^\circ$. }
\end{figure}

In this section, we explore a possibility to resolve the $^{26\!}$Al\
signals for local complexes from the large scales of the Galaxy
through different latitudinal signatures. For such analysis, we
split a homogenous-disk model (Figure 3 right) into sub-maps along
Galactic latitudes, and derive separate $^{26\!}$Al\  spectra for the
different latitude ranges simultaneously through model fitting to
our observations. We study the $^{26\!}$Al\  emission for three intervals
along latitudes, $-5^\circ<b<5^\circ $ (low latitudes),
$5^\circ<b<20^\circ$ and $-20^\circ<b<-5^\circ$ (intermediate
latitudes). $^{26\!}$Al\  emission for low latitudes ($|b|<5^\circ$) should
be dominated by a large-scale origin in the Galactic disk, while
$^{26\!}$Al\  emission at higher latitudes ($|b|>5^\circ$) could originate
from more local star-formation systems such as OB associations in
the Gould Belt. This definition is similar to the one used in
pulsar population studies (Wang et al. 2005). The Gould Belt is an
ellipsoidal shaped ring-like structure delineated by the groups of
nearby stellar groups within $\simeq$~1~kpc, with semi-major and
minor axes of $\sim 500$ pc and 340 pc, respectively (Perrot \&
Grenier 2003). The center of this structure is located towards
$l=130^\circ$ , displaced from the Sun's location by about 200 pc
(Guillout et al. 1998). The Vela region is located near the outer
boundary of the Gould Belt towards $l\sim -90^\circ$ . The nearby
Sco-Cen region at about 140~pc distance towards $l\sim -10^\circ,
\ b\sim 10^\circ$ probably also belongs to the Gould Belt. The
origin of this structure is debated, between triggered sequential
star formation propagating outwards from its center, and an
external triggering event such as a high-velocity cloud falling
through the Galaxy's plane (see Perrot \& Grenier 2003 and
P\"oppel 1997).

Figure 12 displays the $^{26\!}$Al\  intensity distribution along Galactic
latitudes for $|l|<60^\circ$. No $^{26\!}$Al\  signal is detected at
negative latitudes ($-20^\circ<b<-5^\circ$), while weak $^{26\!}$Al\
emission is detected at positive latitudes ($\sim 2\sigma,\
5^\circ<b<20^\circ$). We also derive latitudinally-separated $^{26\!}$Al\
emission for the 1st and 4th quadrants separately again through
model fitting, also shown in Figure 11. No $^{26\!}$Al\  signal is detected
for off-plane regions of the 1st quadrant, while in the 4th
quadrant, $^{26\!}$Al\  emission is still clearly detected (3$\sigma$) in
the latitude region $5^\circ<b<20^\circ$. This $^{26\!}$Al\  emission
towards $b>5^\circ,\ l<0^\circ$ could be attributed to the nearby
Sco-Cen star-formation complex at $\simeq$~140~pc distance.

We also determine the scale height of the Galactic plane in $^{26\!}$Al\
emission by comparing the fit quality for sets of two different
plausible geometrical models for the $^{26\!}$Al\  source density
distribution in the Galaxy, varying their scale height parameter
(Fig. 12 right). We use a Galactocentric double-exponential disk
model (ExpDisk) described by
\begin{equation}
\rho(R,z)\propto\mathrm{e}^{-\left( \frac{R}{R_0} +
\frac{|z|}{z_0} \right)},
\end{equation}
where $R$ is the Galactocentric distance within the plane, and $z$
is the height above the plane, with $R_0=3.5$~kpc and $z_0$ as the
scale radius and height parameter. Alternatively, we use a model
which includes the spiral-arm structure of the Galaxy as derived
by Taylor \& Cordes (1993); we use only their components for the
inner Galaxy and the spiral arms, with identical scale height
parameter (in this model, the density perpendicular to the disk is
described as sech$\left(z/z_0\right)$). In order to avoid a bias
from bright special regions such as Cygnus/Vela/Carina, we
restrict this analysis to data within $|l|<60\degr$ and
$|b|<30\degr$. Fig. 12 (right) shows the variation of
log-likelihood values with different scale heights for both model
types. Here, the values for the exponential-disk models have been
shifted by $+16$, as the spiral-arm model systematically provides
a better description of our data. With $-2\log$L being
asymptotically $\chi^2$ distributed, we derive a scale height of
$130^{+120}_{-70}$~pc $(1\sigma)$ for the $^{26\!}$Al\  emission in the
inner Galactic disk, from the spiral arm model constraints. This
confirms previous such studies based on COMPTEL data (Diehl et al.
1998).

\begin{figure*}
\centering
\includegraphics[width=8.5cm]{f12_LatDistrib.eps}
\includegraphics[width=8.5cm]{f12_Scaleheight.eps}
\caption{\textbf{Left:} $^{26\!}$Al\  intensities versus Galactic latitudes
(solid lines, $|l|<60^\circ$). $^{26\!}$Al\  emission from low latitudes
(the Galactic disk) dominates ($|b|<5^\circ$). For comparison, $^{26\!}$Al\
intensities for each Galactic quadrant are also shown. Significant
$^{26\!}$Al\  emission is detected towards $b>5^\circ,\ l<0^\circ$.
\textbf{Right:} Determination of the Galactic-disk scale height.
Shown is the logarithmic likelihood-ratio for the exponential-disk
(dashed line) and spiral-arm structure models (solid line) for
different scale height values. Log-likelihood values for the
exponential-disk model have been offset by $+16$. }
\end{figure*}

\section{Summary and Conclusions}

The study of the $^{26\!}$Al\  line and its details in different regions of
the Galaxy is one of the main goals of the SPI spectrometer on
INTEGRAL. Using five years of SPI data, we find the $^{26\!}$Al\  signal
from the inner Galaxy ($|l|<30^\circ,\ |b|<10^\circ $) with a high
significance of $\sim 28\sigma$. The $^{26\!}$Al\  flux integrated over the
inner Galaxy of $(2.9\pm 0.2)\times 10^{-4}\ \mathrm{ph\ cm^{-2}\
s^{-1}\ rad^{-1}}$ is consistent with our own and other earlier
measurements, though significantly lower than the ones from
measurements with instruments which have even more modest spatial
resolution on the sky (see Figure 2 of Diehl et al. 2004). Taking
the distance of the Sun to the Galactic center as $R_0=$ 8.5 kpc,
we convert the measured $^{26\!}$Al\  flux to a Galactic $^{26\!}$Al\  mass of
$(2.7\pm 0.7)$ $M_\odot$\ . We compared different plausible models for the
sky distribution of $^{26\!}$Al\  emission and how it may affect the global
$^{26\!}$Al\  flux measurement. We find that different sky distribution
models do not substantially affect $^{26\!}$Al\  intensity and line shapes
for the integrated inner Galaxy, and we have used the observed
variations of $^{26\!}$Al\  mass values to estimate a systematic
uncertainty, added to the statistical uncertainty from the model
fitting, to yield the $\pm 0.7$ $M_\odot$\  uncertainty quoted.

The $^{26\!}$Al\  line centroid energy appears blue-shifted relative to the
laboratory value of $1808.65\pm 0.07$ keV if integrated over the
inner Galaxy ($1809.0\pm 0.1$ keV). With refined spatial
resolution this turns out to be mostly due to asymmetric bulk
motion which we find along the plane of the Galaxy, and attribute
to asymmetries in inner spiral arms and to the Galaxy's bar. In
particular, for the central longitude bin towards the Galactic
Center, the signal is strong enough to allow for a rather small
longitude range integration, and we find a $^{26\!}$Al\  line centroid
consistent with the laboratory value and thus with the absence of
bulk motion relative to the Sun. Also, here the $^{26\!}$Al\  line appears
as most-narrow with an upper limit of 1.3 keV (2$\sigma$). The
measured line width of $^{26\!}$Al\  from the large-scale integrated inner
Galaxy with an upper limit of 1.3 keV (2$\sigma$) is consistent
with expectations from both Galactic rotation and modest
interstellar-medium turbulence around the sources of $^{26\!}$Al\
(turbulent velocities constrained below 160 km s$^{-1}$ even when
disregarding the effects of galactic rotation).  Our line width
results are consistent with previous reports by HEAO-C (Mahoney et
al. 1984), RHESSI (Smith 2003), but the very broad line with a
width $\sim 5.4$ keV reported by GRIS (Naya et al. 1996) is
clearly ruled out by our SPI measurements ( $4\sigma$ significance
level ).

From our study of $^{26\!}$Al\  emission in spatially-restricted regions along the
plane of the Galaxy, we find:
\begin{itemize}
\item{}
$^{26\!}$Al\  brightness appears asymmetric for the two inner quadrants,
with a flux ratio of the 4th quadrant to the 1st of $\sim 1.3 \pm
0.2$ (Figure 7).
\item{}
The $^{26\!}$Al\  line energy varies clearly along the Galactic plane
(Figure 11): a minor redshift ($\sim 0.1$ keV) for positive
longitudes, but significant blueshift ($\sim 0.4-0.8$ keV) for
negative longitudes.
\item{}
The $^{26\!}$Al\  line towards the direction of $20^\circ < l < 40^\circ$
shows a hint for additional line broadening.
\item{}
The scale height of Galactic-plane $^{26\!}$Al\  emission is
$130^{+120}_{-70}$~pc $(1\sigma)$, determined towards
the inner Galaxy ($|l|<60\degr$).
\item{}
There is a strong hint for $^{26\!}$Al\  emission in the fourth Galactic
quadrant at intermediate latitudes $l<0^\circ,\ b>5^\circ$ (Fig.11).
\end{itemize}

This leads us to several astrophysical implications and the
``bar'' structures:
\begin{itemize}
\item{}
The disk of our Galaxy apparently is not azimuthally-symmetric.
The $^{26\!}$Al\  brightnesses for the two inner quadrants appear different,
both from our INTEGRAL and from earlier COMPTEL results, favoring
the fourth quadrant. $^{26\!}$Al\  line shifts towards the blue in such
brighter regions are more pronounced than the redshifts on the
fainter side of the disk, unexpected from a simple and symmetric
Galaxy model and its large-scale rotation properties. These
phenomena may reflect variations in the space distribution of
young stars, possibly related to the inner parts of the spiral
arms and their interfaces to the ``molecular ring'' and the
``bar'' structures. Large non-circular motions have been seen in
HI and CO observations (Mulder \& Liem 1986; Gerhard \& Vietri
1986), and also from the NIR light distribution (Binney et al.
1997), in addition to source count asymmetries (Nikolaev \&
Weinberg 1997) and non-symmetric gas dynamics (Englmaier \&
Gerhard 1999). The bar is most clearly traced in infrared emission
from dust (Marshall et al. 2008), which suggests a position angle
of $\sim 25^\circ$ of the bar with the near end pointing towards
us in the first quadrant, and a total length of about 4~kpc. The
transition regions between spiral arms and bar are likely to incur
star formation (Verley et al. 2007), and affect the dynamics of
gas and stars. Simply superimposing a homogeneous star-forming bar
to the rotating spiral would, however, not agree with our results
- the inner Galaxy structure may be more complex.  Localized
star-forming regions could lead to peculiar motion of hot gas
ejected from winds and supernovae, which might dominate over
large-scale Galactic rotation. Such activity could be the cause of
the observed asymmetry of the $^{26\!}$Al\  line intensities and line energy
shifts in the inner Galaxy. On the other hand, other more nearby
$^{26\!}$Al\  source regions could be responsible for these irregularities,
such as the nearest part of the Sagittarius-Carina arm in the
fourth quadrant, or regions/complexes attributed to the Gould Belt
such as the Scorpius-Centaurus-Lupus groups. Refined $^{26\!}$Al\  studies
and their combination with astrometry from other tracers of
Galactic structure could help to understand the role of our
Galaxy's bar.
\item{}
The $^{26\!}$Al\  emission asymmetry ($1.3\pm 0.2$) between fourth and first
quadrant of the Galaxy is lower than the intensity contrast of
$1.8^{+0.5}_{-0.3}$ reported for positron annihilation emission
from the disk of the Galaxy (Weidenspointner et al. 2008). $^{26\!}$Al\  by
itself releases a positron in 82\% of its decays; it is uncertain,
however, how this translates into annihilation photons, from the
variety of slowing down and annihilation processes which determine
the fate of positrons in interstellar space. Both spatial and
temporal variations and non-linearities scaling with gas density
may occur.
\item{}
The scale height of Galactic-plane $^{26\!}$Al\  emission is significantly
larger than the molecular-gas
disk scale height of $\simeq$~50~pc, yet significantly smaller than
the ``thick disk'' part of the Galaxy. It is consistent with
$^{26\!}$Al\  being ejected from star-forming regions, and partly extending
more towards the Galactic halo where gas pressure is lower than
within the plane of the Galaxy (``champagne flows'').
\item{}
Localized regions may deviate in interesting detail from the
large-scale averaged properties of $^{26\!}$Al\  source regions. The
direction of $20^\circ < l < 40^\circ$ corresponds to the Aquila
region, and our hint for additional line broadening may be due to
increased interstellar turbulence from stellar-wind and supernova
activity at the characteristic age of stellar groups of that
region, which may have created a supershell of substantial size
(320 $\times$ 550~pc, see Maciejewski et al. 1996). Similar
arguments are being explored for the Cygnus region, based on
earlier hints of peculiar $^{26\!}$Al\  emission (Martin et al. in
preparation). The hint for $^{26\!}$Al\  emission at $l<0^\circ,\ b>5^\circ$
(Fig. 12) may be attributed to the relatively nearby star forming
complexes of the Sco-Cen association (de Geus 1992). Sco-Cen and
several nearby stellar groups are attributed to the larger
structure of the ``Gould Belt'', which is suggested to have been
more actively forming stars during the last 30 Myr (Grenier 2000,
Perrot \& Grenier 2003). These examples indicate that
spatially-resolved $^{26\!}$Al\  emission properties may enable new
diagnostics of the interactions of massive stars with their
surroundings, when combined with other astronomical constraints on
cold gas and stars of such regions.
\end{itemize}

INTEGRAL/SPI will continue to accumulate more data for several
years, to cover more sky regions in the outer Galaxy and at
intermediate latitudes. This will allow us to deepen the studies
reported in this paper, and to refine spatial information on the
$^{26\!}$Al\  line and/or increase the significance of the results reported
above, as signal statistics increases and instrumental-background models
are tightened.   These studies will help us to better understand the
properties of ISM near groups of massive stars, and the bulk
motion of gas in the inner Galaxy from Galactic rotation and other
peculiar kinematics. Nearby $^{26\!}$Al\  sources may be also discriminated
with better exposure towards candidate regions, improving our
determination of the $^{26\!}$Al\  mass in the Galaxy and towards regions where the
stellar census is known to a better degree.
Studies of $^{26\!}$Al\  from nearby star-formation
regions (e.g., Cygnus, Vela, Sco-Cen, Orion) are a promising diagnostic
for the massive star origin of Galactic $^{26\!}$Al\  and kinematics of $^{26\!}$Al\
ejecta in ISM. From this, important constraints on massive-star
and supernova nucleosynthesis are obtained, refining our models of
their complex interiors (see e.g. Woosley and Heger 2007, or
Chieffi and Limongi 2006).

\section*{Acknowledgments}
We are grateful to the anonymous referee for the comments to
improve the draft. The INTEGRAL project is supported by government
grants in the member states of the hardware teams. The SPI project
has been completed under responsibility and leadership of CNES. We
are grateful to ASI, CEA, CNES, DLR, ESA, INTA, NASA, and OSTC for
support. W. Wang is also supported by the National Natural Science
Foundation of China under grant 10803009.

redpajama_set_name: RedPajamaArXiv


text:
Poyet: We deserved more
Written By Tom Coleman
Getty Images https://images.daznservices.com/di/library/omnisport/a8/77/guspoyet-cropped_1sibhu4wahxs612aektvjs2458.jpg?t=-209910174&w=500&quality=80
Sunderland boss Gus Poyet felt his side were unlucky to come away with nothing from their 2-1 Premier League defeat at Tottenham.
The hosts took the lead after just three minutes through Jan Vertonghen at White Hart Lane on Saturday, before Sebastian Larsson curled home a 30-yard free-kick just after half-an-hour.
A tenacious performance from the visitors - who handed a debut to new signing Jermain Defoe as part of a 5-3-2 formation - looked to have sealed a point before Christian Eriksen lashed home from just outside the area with two minutes left.
"When the winning goal is so late, it hurts," said Poyet. "But it's part of football. You need to be good all the time, not 88 minutes or 89 minutes.
Tottenham 2 Sunderland 1: Defoe fails to shine as Eriksen wins it
"That's disappointing, but I think that for a new formation and a new way of playing away at White Hart Lane we were doing quite alright, so it's a shame that we didn't get something from the game."
Despite that optimism, Poyet could not hide his concern at a lack of goals this season.
Sunderland are the Premier League's second-lowest scorers, with Steven Fletcher and Danny Graham both spurning good opportunities on Saturday.
Poyet added: "The chance for Fletcher...if you did it 10 times he would have scored nine. Unfortunately that was the 10th time.
"I think the two chances from Graham were good enough to put one of them in the back of the net. I think if you keep creating those chances you've got to make sure you score, because the rest is going to get better and better."
Defoe's performance against his old club, after arriving from Toronto FC on Friday, could not lift Sunderland, and he struggled to make an impact before being replaced by Graham with 15 minutes left.
"I played him for a little bit longer than expected but he is going to get better and better and I'm sure when he gets that first chance he's going to put the ball into the back of the net," said Poyet. "I think it was a good start and a great place for him to start playing for us."

redpajama_set_name: RedPajamaCommonCrawl


China views the United States as a declining power, but at the same time believes that Washington is trying to fight back to undermine, and even disrupt, the economic and military growth that point to China's becoming the world's most powerful country, according to the analyst, Wang Jisi, the co-author of "Addressing U.S.-China Strategic Distrust," a monograph published this week by the Brookings Institution in Washington and the Center for International and Strategic Studies at Peking University.
Mr. Wang, who has an insider's view of Chinese foreign policy from his positions on advisory boards of the Chinese Communist Party and the Ministry of Foreign Affairs, contributed an assessment of Chinese policy toward the United States. Kenneth Lieberthal, the director of the John L. Thornton China Center at Brookings, and a former member of the National Security Council under President Bill Clinton, wrote the appraisal of Washington's attitude toward China.
In a joint conclusion, the authors say the level of strategic distrust between the two countries has become so corrosive that if not corrected the two countries risk becoming open antagonists.
The United States is no longer seen as "that awesome, nor is it trustworthy, and its example to the world and admonitions to China should therefore be much discounted," Mr. Wang writes of the general view of China's leadership.


Can running cause BACK PAIN?
Back pain when running? To answer your worries, watch this week's video and know why. A lot of people nowadays love to run to stay fit. Sometimes, runners can experience back pain unexpectedly. This may be because their body positioning is incorrect. In this video, we ask you to imagine the tissues in our back as a big broadsheet. Once we hunch forward, the sheet on our back is forced to stretch, creating tension. So the first thing to do in order to avoid this is to start looking at our posture.
← Why good posture hurts my SHOULDERS?


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I use a sliding scale for our winery tours , which includes pickup and drop-off within a 10 mile radius of Temecula, picnic lunch and tastings at three wineries. The fee for two people is $225, for four people it's $390 and for six it's $490. Single riders are $125 each. Inquire about rates for odd numbers. I can carry seven passengers. I provide chilled, bottled water at no extra charge. Gratuities are at your discretion and are greatly appreciated. Customary gratuities are 15 – 20% of the full, non-discounted fare.
Each tour is custom tailored to the group I am taking out. I look forward to showing you the beautiful Temecula Valley, Southern California Wine Country. Feel free to call me (951) 907-9701 or email me attom@wineormous.com with any questions. Cheers!
We are a member of the Temecula Wine Country Responsible Partner Program.


text:
Opposition's Behavior 'Undemocratic', Proves Nothing Wrong In New Farm Laws: Tomar
The minister said instead of protesting in Parliament against the farm laws, the opposition should have listened if they cared for farmers.
Narendra Singh Tomar says nothing wrong with new farm laws. (File photo) | PTI
2021-08-10T20:20:52+05:30 Opposition's Behavior 'Undemocratic', Proves Nothing Wrong In New Farm Laws: Tomar
Published: 10 Aug 2021, Updated: 10 Aug 2021 8:23 pm
Calling Opposition's protest in Parliament on farm laws as 'undemocratic', Union Agriculture Minister Narendra Singh Tomar said 'it proves there is nothing wrong in the new farm laws'.
He however said the "problem lies in perception".
In the Upper House, the Opposition protested vehemently when its request for a calling attention motion on agriculture issues was converted into a short-duration discussion.
While the discussion was underway amid the din, the protesting members trooped into the well with sloganeering. In fact a protesting member climbed atop the table of the secretary general.
Stating that this "irresponsible behavior" of the Opposition has hurt the democracy, Tomar said, "I reproach the undemocratic behavior of Congress, TMC and AAP in the House when the discussion began on agriculture."
He said if the Opposition members were concerned about farmers and agriculture, they would have participated in the discussion and kept their view points instead of protesting.
"We were ready to listen to their criticism as well as their suggestions. If the policies were to be amended based on those suggestions, the government was open to that also," he said.
Tomar further said the Upper House discussed the Covid-19 issue and the government wanted discussion should take place on agriculture as it is connected with everyone's life.
However, the irresponsible behaviour of the Opposition in the House during discussion on agriculture has hurt the Indian democracy.
"Today, this step of Opposition proves that there is nothing wrong in the farm laws, it is in their perception. (Aaj vipaksh ke is kadam se, ek baar ... siddh hogaya hai krishi sudaar kaanoonon mein kala kuchh bhee nahin hai.Vipaksh ke kapade mein kaalaapan dikahi deta hai)," he said.
The Opposition wants to mislead the country by telling lies. Its motive is to do vote-bank politics and family-based politics with selfish intension, he added.
The minister highlighted that the government under the leadership of Prime Minister Narendra Modi has taken several measures to improve the farm sector and many schemes are being implemented which all have lead to growth in the sector and prosperity in the lives of farmers.
"But the Congress members are unable to digest this," he said, adding that the farmers across the country are standing with the new farm laws and agriculture schemes.
Condemning the ruckus created in the Upper House, Parliamentary Affairs Minister Prahlad Joshi told reporters that the Opposition had demanded that agriculture matters should be discussed and the Chair accepted it.
"Later the opposition created a ruckus sitting on the reporter's table and threw book over chair and members....They were sitting on the table even after the House was adjourned. Some staff have been hurt. ....we have never seen such behaviour," he said, and asked what the Congress and its allies want.
The government is ready for discussion on the agrarian crisis, he said, adding that the OBC bill being passed in the Lok Sabha is not being tolerated by them.
Eight months on, thousands of farmers mainly from Punjab, Haryana and western Uttar Pradesh have been camping at Delhi's borders in protest against the three laws.
The government and unions have held 11 rounds of talks, the last being on January 22, to break the deadlock and end the farmers' protest. Talks have not resumed following widespread violence during a tractor rally by protesting farmers on January 26. (With PTI inputs)
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Outlook Web Desk Narendra Singh Tomar New Delhi National


In many organizations, personnel costs are one of the largest budget items. Leaders in any business, regardless of size, need people aligned and working together for high levels of performance.
To achieve this high level performance, a "Best Practice" is to utilize employee assessments. They help reveal more consistent, in-depth and objective information about employees than most managers can uncover on their own.
Candidates have a tendency to embellish their qualifications. According to the Society of Human Resource Management (SHRM), 53% of resumes they reviewed contained false information. This number may increase as jobs become harder to find, or candidates become more desperate for work.
There is a tendency to "filter-scrub" employee information. In today's litigious society, former employers share little, especially anything negative. Even internal candidates may not be who they appear in their performance reviews. Sometimes well-meaning supervisors are less than objective.
People are difficult to read. Looking at a candidate is often like looking at an iceberg. 90% of the "total person" is below the surface, not easily observed or understood.
Valid assessments uncover truthful information in a very cost and time effective manner. This solid information enables better management of your workforce, with greater productivity and profits.
Screening: Good pre-hire assessments will quickly screen out applicants who lack the fundamental skills, qualifications and/or behaviors you are seeking.
Selecting: Selection assessments often support other related activities such as resume reviews and interviews. For example, knowing what and how to probe during the interview can ultimately help make a better hiring decision.
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One of the most valuable assets of your organization are your people. Invest a lot in them, and you get a lot back. We encourage you to contact us today to let us show you firsthand the valuable information assessments reveal and how you can apply our talent management solutions to help maximize your workforce productivity.


And nestl'd in His little Head.
And Captive Him, who Captives All.
The silken Bond, and held Him fast.
Incumber'd in the silken String.
He never There must hope to dwell.
Who ne'er intended Harm to Thee.
For Harm was meant, and Harm to Me.
Vain Fears that vex thy Virgin Heart!
And freely let Me fly again.
And freely Thou again shalt fly.
The Captive thus gave up his Quiver.
A little, flutt'ring, idle Guest.
Gives Grief, or Pleasure; spares, or kills.


text:
Bodies in peril
A tonally strange collection that misses the mark
by Caitlin McGregor •
Everybody: A book about freedom by Olivia Laing
Picador, $44.99 hb, 349 pp
Olivia Laing (photograph by Sophie Davidson)
Olivia Laing describes her latest book, Everybody: A book about freedom, as one about 'bodies in peril and bodies as a force for change'. I would describe Everybody as a biographical project, about people whose work engaged with the ideas of bodies and freedom in the twentieth century. This might seem like a subtle difference, but it's an important one: had Laing conceptualised and framed the book in the latter way, I think Everybody would be a less frustrating read. As it stands, Laing's biographical writing, while insightful and rigorously researched, ends up feeling like an (admittedly deft) avoidance tactic; Everybody sets out to be a book that takes a hard and uncomfortable look at the topic of bodies and their roles in the pursuit and denial of freedom, but it doesn't quite dare to do so directly. It ends up being a book about people who have.
Olivia Laing
Caitlin McGregor
Caitlin McGregor is an essayist based in regional Victoria. Her work has appeared in a range of magazines and literary journals, including Going Down Swinging, Overland, The Big Issue, Kill Your Darlings and Voiceworks. In 2018 she was a judge for the John Marsden & Hachette Australia Prize for Young Writers, and has worked as an editor, submission reader and creative writing tutor. In 2019, she received the inaugural Kat Muscat Highly Commended Award, and was a writer-in-residence at the Melbourne Recital Centre. Caitlin is currently working on an essay collection that explores and interrogates ideas about 'care'.
Everybody: A book about freedom
by Olivia Laing
Letter collection
Dear Prime Minister: Letters to Robert Menzies, 1949–1966 by Martyn Lyons
by Brenda Niall
Frances Burke: Designer of modern textiles by Nanette Carter and Robyn Oswald-Jacobs
by Christopher Menz
Silverview by John le Carré
by Morag Fraser
January–February 2022, no. 439
These Precious Days by Ann Patchett
by Nicole Abadee
April 2000, no. 219
The Twelfth of Never: A memoir by Louis Nowra
by David McCooey
July 1991, no. 132
Being Alone with Oneself by Charmian Clift
by Jan Smark Nilsson
December 2019, no. 417
The Best Australian Science Writing 2019 by Bianca Nogrady
by Robyn Arianrhod


Cushions are component of every area including room. They serve numerous functions. You rest your directly it and also sleep. It is so easy to include spring color and also convenience to your residence with pillows. You can stitch them on your own or acquire the pillow kinds from craft, hobby or chain store and afterwards decorate them on your own. From little bitty cushions that can be used to embellish doorknobs to large pillows that can be utilized as extra seating, cushions can transform the appearance of the space in a split second! If you are seeking the right 27 Stylish How to Make Your Own Pillow Inserts for your demands, we recommend that you review this post.
There are numerous of cushion that you can pick from. Several of the forms that you can pick from are reinforce pillows, needlepoint pillows, and so forth. You can always discover methods how to accent your bed room with these attractive pillows. The same idea is also applied if you utilize these attractive pillows for your living area or other room. You have to keep in mind that also if you only use it to relax your head on, these pillows have to be very positive as well as comfortable. This has not been taken much focus by a lot of people. The final worry about getting cushions is picking what kind of pillows to acquire. The acquisition will certainly depend upon where the pillows will certainly be placed. See also other unique 27 Stylish How to Make Your Own Pillow Inserts listed below here!


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Walter Mosley's latest Easy Rawlins novel, "Charcoal Joe," comes on the heels of the author winning the Grand Master Award from the Mystery Writers of America in April. No one familiar with the quality and quantity of Mosley's creative output was surprised by this honor. His output encompasses more than four dozen books — including 14 Rawlins novels — science fiction, nonfiction and essays. He's been awarded PEN America's Lifetime Achievement Award.
So it' s no surprise that Mosley, an L.A. native whose father migrated out west from Louisiana, is attuned to the uneasy America that blacks inhabit. The fictional Easy, a child of New Iberia, La., who migrates to Los Angeles, is too. The central twist in "Devil," set in 1948 L.A., turns on the different worlds that whites and blacks inhabit in the same place. "Charcoal Joe," set in the same city exactly two decades later, finds that things are different, if not all that much improved.
Chandler's novels and James Ellroy's "L.A. Quartet" both covered the same city and era — the 1940s and 1950s — but neither offered any real insight into the black side of town. Think of the wrongly charged black suspects in Ellroy's brilliant "L.A. Confidential," for example. The black guys are there as a plot complication. The detectives really don't pay any price for blowing them away. If Easy had investigated? That would have been the story, full stop.
As "Charcoal Joe" opens, we find Easy in a good place. He's flush with cash from a previous case. He's going to propose to his girlfriend. He's down to one smoke per day. Racial progress has been enough that he can enroll his daughter, Feather, in a posh private school in the white side of town. And he's been able to open a three-man firm in a building that seems a metaphor for the city: Once an elegant residence for a rich white guy, it's been cut up into three businesses. The first floor is an antique store of faded quality. The second floor, run by the landlord, is a Japanese family-owned and -operated insurance brokerage. Easy's new three-man detective agency — one Jewish partner and one black — is on the third. Two of the couples working in the building are interracial.
Likewise, the murder that forms the spine of the narrative is racially complicated. "A white man named Peter Boughman and some other guy named Ducky" were shot to death in a house in Malibu, Rawlins's longtime friend Raymond "Mouse" Alexander tells him. Seymour Brathwaite, a well-to-do black postgraduate student at UCLA, lived nearby, heard the shots and went to investigate, Mouse says. Brathwaite was found standing beside the bodies when the police came. He had no gun but was booked for murder.
The hitch is that Brathwaite is the son of a friend of the fearsome Rufus Tyler, a.k.a. Charcoal Joe, an elderly black man, who is good at cards, killing people and Getting Stuff Done. Charcoal, who has done Easy a favor in the past, now wants to call in his tab.
If you've read Mosley before, you know that Easy is probably going to figure things out by the end, though at a cost. But like the crosstown drive from West L.A. to Watts, you don't hop in the car with Easy Rawlins for the destination. You ride shotgun for the trip.
Neely Tucker, a national reporter for The Washington Post, is the author of "Only the Hunted Run: A Sully Carter Novel," which will be published in August.


text:
The World Falls Apart Into Facts
Samson Young, Tokyo, 13 Apr - 5 Jun 2021
The World Falls Apart Into Facts: Samson Young
Ota Fine Arts is delighted to present 'The World Falls Apart Into Facts', a solo exhibition by Hong Kong artist Samson Young. Young's creations utilize sound, performance, and installation. His practice has been highly-acclaimed both domestically and internationally, and he was selected for the Hong Kong pavilion at the 57th Venice Biennale in 2017.
For The World Falls Apart Into Facts (2019), the video installation featured in this exhibition, Young conducted a research project on music from both historical and political perspectives. This research follows the genealogy of the Chinese folk song Molihua (Jasmine Flower), the melody of which can also be heard in the opera Turandot. Molihua was imported into Europe through the British Empire's encounter with the imperial Qing court, and after a period of propagation and rearrangement in Europe, the tune was 're-imported' back into China. Young compares and contrasts the song's transmission history with that of the melody of Japanese Togaku - court music that was imported into Japan from China during the Tang dynasty, which has since become as one of few extant sources of Tang music. In the video, we hear an original composition that is played by, among other instruments, a touristic souvenir-instrument. Through the work, Young examines the interactions that occur when a piece of music crosses cultures, to consider what it means to hear with the ears of another, and questions the notions of cultural purity and authenticity at large.
We hope to invite you to experience the worldview of Samson Young, where the humorous visual on the screen and the contrasting in-depth research co-exists as one.
Special thanks to Edouard Malingue Gallery


text:
Games fair "Play it!": 14.000 visitors play in the iron and steel works
On Sunday, March 31, around 18 p.m., the second edition of the still young Duisburg games fair "Play it!" ended. Around 14.000 enthusiastic visitors flocked to the Kraftzentrale in the North Landscape Park over the three days of the event to try out board and card games in the middle of an old industrial plant. A noticeable increase in the number of visitors suggests that the "Play it!" will be successful again in 2020. the 3rd "Play it!" will then take place from March 27th to 29th.
Duisburg game fair is growing
While 11.300 visitors took part in the opening event last year, around 2019 game fans were already drawn to the Duisburg landscape park in 14.000. This corresponds to an increase of almost 24 percent, a value that also applies to the expansion of this year's exhibition space. Almost 100 exhibitors - mainly well-known industry giants, but also small publishers and game designers - presented their ideas for three days.
The event hall got full, especially on the weekend. Photo: André Volkmann
The supporting program with a panel discussion, workshops, tournaments and a flea market was also well received by the visitors, says Verlag Nostheide. The event also received attention from the city administration of the city of Duisburg: On Saturday, March 30th, André Haack, the city's head of economic affairs, visited the games fair to find out more about the board and card game industry as part of a tour.
The two weekend days were popular with visitors, especially Sunday, when numerous families with children streamed into the event hall. Children aged four and over are particularly attracted to the range of games on offer. "This is 'tip-top' for children from the age of six," reveals a father who attended the "Play it!" with his wife and five children.
Picture gallery: Play it! 2019
Photo: Andre Volkmann
Manfred Lamplmair from rudy-Games would like to see children in particular "use smartphones sensibly". Photo: André Volkmann
Photo: André Volkmnn
Overview instead of crowds: Photo: André Volkmann
The "Play it!" runs until March 31st in the Duisburg Landscape Park. Photo: André Volkmann
For the very little ones, however, the playful possibilities are rather limited. Here one wishes for the future more specifically aligned play stations, for example with building blocks. The extended family noticed the size of the Duisburg games fair positively: "I think the size is great. We were already in Essen with the children last year; However, SPIEL was too big for us," says the mother. The "Play it!" scores with this as a family-friendly event.
The prerequisites for establishing yourself as a permanent fixture in the event landscape of the card and board game industry are in place: The next "Play it!" will take place from March 27th to 29th, 2020.
Previous Game fair "Play it!" begins in Duisburg
Next Cheering mood in the town hall: Ratinger Spieletage celebrate their 10th birthday
Crime role-playing game "A Bavarian Tale": Secrets of a village idyll
New editions for Borderlands 3 announced - Season Pass 2 starts November 10th
Lost Ark: Which class is the best?
Cyberpunk 2077: action role-playing game news in streaming show


text:
IDRIVE DISTRICT MEDIA ROOM BLOG
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Orlando's Most Dynamic Destination!
Covid Related Business Openings
Mature Travel
Official Visitor Services
Rosen College of Hospitality
Spas in Resort Area
Visitor Safety Tips
I-Drive Orlando Updates
Beyond I-Drive Orlando
I-Ride Trolley
I-Drive Hotelier Organizes Immediate Community Opportunity to Raise $1,000,000 for Urgently Needed Haiti Earthquake Relief Effort
Note: For the first time, March 19-21, the public will be able to view the Little Haiti House, a low-cost, eco-friendly, earthquake and hurricane-resistant home developed for use in Haiti by Orlando hotelier Harris Rosen. Attendees may walk through the 36' x 12' model home at the Central Florida Home & Garden Show in Hall North B in the Orange County Convention Center's North/South complex off Universal Blvd. See how renewable energy sources such as wind and solar power, as well as plant-based fuels, make this a smart and affordable solution to Haiti's rebuilding effort. Donations will also be accepted, with 100 percent of contributions going directly to the Rosen Haiti Relief Fund. For the latest information on the Haitian relief effort, visit www.rosengivesback.com/the-harris-rosen-foundation/haiti/.
Guests can also see the house and support the Relief Fund while sampling gourmet cuisine on Saturday, March 20 from 6-9 p.m. during a special after-hours fundraising event, "Rosen Hotels' Homeowners for Haiti." For just $25, which includes free admission to the show, guests can sample a mix of sweet and savory dishes from the award-winning Rosen Hotels' restaurants, including Jack's Place at Rosen Plaza, Everglades at Rosen Centre and A Land Remembered and Cala Bella Italian bistro at Rosen Shingle Creek. Complimentary wine and non-alcoholic beverages are also included. This first-of-its-kind event was created specifically to benefit the victims of the Haiti earthquake through the Rosen Haiti Relief Fund. Tickets for this special event are limited and must be purchased in advance online. To purchase, go to www.FloridaHomeShows.com and enter in the special code, HAITIHOUSE.
For details on the Home & Garden Show, visit www.floridahomeshows.com or call 1-877-871-7469.
Visitors to the International Drive Resort Area, businesses, partners and residents have a chance to join in the Haitian earthquake relief effort by making a financial contribution or by donating supplies.
The Harris Rosen Foundation, Inc., a non-profit 501(c)(3) organization, headed by I-Drive hotelier, Harris Rosen, has joined forces with Sen. Bill Nelson's office and various local Haitian community leaders to provide direct assistance to the victims of the earthquake in Haiti. In the past the Harris Rosen Foundation has collected and personally delivered food, water filters, school supplies and medical supplies to the citizens of Haiti. Now plans are underway to send emergency relief to those in need.
Luann Brooks, Executive Director of the International Drive Master Transit & Improvement District, encourages everyone to support this effort made possible by Rosen.
"The Harris Rosen Foundation offers all of us in the hospitality industry a chance to donate financially or by to provide specific items that are needed so desperately by those in Haiti who have been devastated by this tragedy. Please donate through one of the following two convenient methods by the Friday, Jan. 22 deadline so that we may contribute immediately to this effort."
Rosen plans long-term relief effort after the immediate goal is reached and gave the campaign a kick-start with a $250,000 donation.
Make a financial contribution to the Harris Rosen Foundation:
100% of the contribution will go toward purchasing much needed supplies. All items will be delivered by the Foundation's own task force with the help of Senator Bill Nelson's office. All donations are tax-deductible. Click here to donation.
Donate supplies to help in immediate relief efforts:
Please donate items from the following list:
· Please do not donate clothes, shoes or food at this time.
· Blankets.
· Towels and Washcloths.
· Hygiene Products (soap, toothpaste, shampoo, etc.)
· First Aid Kits.
· Antibiotics.
· Medical Supplies (bandages, gauze, peroxide, etc.)
· Bug Spray.
· Flashlights and Batteries.
The most convenient drop-off location for I-Drive visitors and businesses is the Rosen Centre Hotel, I-Ride Trolley stop 27, 9840 International Drive, Orlando 32819.
Additional locations include:
First Haitian Baptist Church of Orlando
4701 Lennox Blvd., Orlando 32811
Child Development Center of Orlando (7a.m. - 6 p.m.)
11553 Winter Garden Vineland Rd., Orlando 32836
Center for Multicultural Wellness & Prevention
641 N. Rio Grande Ave., Orlando 32805
Jewish Community Center Maitland Campus
851 N. Maitland Ave., Maitland 32751
Jewish Community Center Jack & Lee Rosen Southwest Orlando Campus
11184 S. Apopka-Vineland Road, Orlando 32836
For more information, please visit www.rosengivesback.com/the-harris-rosen-foundation/haiti/.
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