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Home All issues Volume 588 (April 2016) A&A, 588 (2016) A111 Full HTML
Volume 588, April 2016
https://doi.org/10.1051/0004-6361/201527752
2. Observations and ...
3. Spectral fitting procedure
4. Results and discussions
Oxygen, neon, and iron X-ray absorption in the local interstellar medium
Efraín Gatuzz1,2,3, Javier A. García4, Timothy R. Kallman5 and Claudio Mendoza3
1 Max-Planck-Institut für Astrophysik, 85741 Garching bei München, Germany
e-mail: egatuzz@mpa-garching.mpg.de
2 Escuela de Física, Facultad de Ciencias, Universidad Central de Venezuela, PO Box 20632, 1020A Caracas, Venezuela
3 Centro de Física, Instituto Venezolano de Investigaciones Científicas (IVIC), PO Box 20632, 1020A Caracas, Venezuela
4 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, 02138, USA
5 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
Aims. We present a detailed study of X-ray absorption in the local interstellar medium by analyzing the X-ray spectra of 24 galactic sources obtained with the Chandra High Energy Transmission Grating Spectrometer and the XMM-Newton Reflection Grating Spectrometer.
Methods. By modeling the continuum with a simple broken power-law and by implementing the new ISMabs X-ray absorption model, we have estimated the total H, O, Ne, and Fe column densities towards the observed sources.
Results. We have determined the absorbing material distribution as a function of source distance and galactic latitude–longitude.
Conclusions. Direct estimates of the fractions of neutrally, singly, and doubly ionized species of O, Ne, and Fe reveal the dominance of the cold component, thus indicating an overall low degree of ionization. Our results are expected to be sensitive to the model used to describe the continuum in all sources.
Key words: ISM: general / ISM: atoms / ISM: abundances / ISM: structure / X-rays: ISM
The interstellar medium (ISM) is one of the most important galactic components. Regarding its chemical composition, it can be enriched with heavy elements by gas accretion from other galaxies, supernova explosions, and stellar winds (Pinto et al. 2013). The analysis of such a dynamic environment is crucial to understand stellar formation and evolutionary processes, which may be performed by means of high-resolution X-ray spectroscopy. Due to their high penetrating power, X-ray photons interact not only with the ISM atomic ions exciting inner-shell levels but also with molecules and solid compounds, thus providing the opportunity to study physical properties such as column densities, ionization fractions, and abundances of astrophysically relevant elements in both the gas and grains (Gatuzz et al. 2015).
Multiple ISM analyses using low-mass X-ray binaries (LMXB) have been carried out in the last decade reporting the presence of a multi-phase ISM structure, which includes a cold gas with low-ionization degree and a hot ionized gas (e.g. Schulz et al. 2002; Takei et al. 2002; Juett et al. 2004; Yao et al. 2009; Liao et al. 2013; Pinto et al. 2013); however, the identification of the highly ionized species is less straightforward than the lowly ionized ones. For example, Gatuzz et al. (2014) performed a study of eight LMXB using high-resolution Chandra spectra, detecting only a Kα absorption feature (22.024 ± 0.003 Å) from highly ionized O vi toward XTE J1817-330. This line was previously identified by Gatuzz et al. (2013a,b) as being intrinsic to the source rather than originating in the local ISM, who concluded that the cold phase is dominant without any further identification of an associated hot gas component. In support of this view, Luo & Fang (2014) have found that most of the absorption lines from highly ionized metals detected in the spectra toward 12 LMXB arise in the hot gas intrinsic to the sources, the ISM only making a small contribution. In a recent study Nicastro (2014) conclude that the absorption line at ~22.275 Å is ubiquitously detected in the spectra of both galactic and extra-galactic sources. It leads to the identification of O ii Kβ from the local ISM thus contradicting its previous identification as an O vi Kα absorption feature of the warm-hot intergalactic medium (WHIM) along the lines of sight toward H 2356–309 (Buote et al. 2009; Fang et al. 2010) and Mkn 501 (Ren et al. 2014).
Location map of the X-ray binaries of the present sample. The left panel shows the sources plotted on a full-sky map in galactic coordinates relative to the galactic center. Red points: Chandra sources. Blue points: XMM-Newton sources. The right panel shows a location map of the X-ray binaries in our sample projected in the galactic plane.
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Gatuzz et al. (2013a,b) performed a detailed evaluation of the oxygen absorption region using Chandra high-resolution spectra from the bright binary XTE J1817–330, observing a complex structure around the K edge that included the presence of Kα, Kβ, and Kγ absorption lines from O i and O ii and Kα from O iii, O vi, and O vii. Gatuzz et al. (2014) fitted the O K edge in the Chandra spectra of eight LMXB with the warmabs photoionization model to determine the ISM ionization degree. In this same work, the O photoabsorption cross-section computed by García et al. (2005) was compared with the most recent calculation by Gorczyca et al. (2013), finding no substantial differences in the modeling of the K-shell region; it is worth emphasising the remarkable accuracy of the oxygen atomic data that was thereby established. It was therefore concluded in this work the dominance of a neutral gas in all the observed lines of sight, with ionic fractions O ii/O i and O iii/O i lower than 0.1.
In addition to oxygen, a benchmark of the neon atomic data was also pursued by Gatuzz et al. (2015). Using the high signal-to-noise spectra of Cygnus X–2 and XTE J1817–330, the positions of the Kβ absorption line in Ne i and Kα, Kβ, and Kγ in Ne ii and Ne iii were determined. The Ne i cross-section computed by Gorczyca & McLaughlin (2000) and those for Ne ii and Ne iii by Juett et al. (2006) were adjusted by shifting the wavelength scale in order to fit the astronomical spectra. With the improved cross sections a new X-ray absorption model, referred to as ISMabs, was developed and made publicly available (Gatuzz et al. 2015). Its advantage lies in the compilation of a database of photoabsorption cross sections for neutrally, singly, and doubly ionized species for all the cosmic abundant elements, namely H, He, C, N, O, Ne, Mg, Si, S, Ar, Ca, and Fe. Although the neutral component is dominant in the ISM, it is found that the inclusion of singly and doubly ionized species leads to more realistic models of the O and Ne K edges; furthermore, the use of a physical model prevents misidentification of absorption features which often occurs in the traditional fitting methods with Gaussian profiles.
ISM X-ray absorption affects all the X-ray observations and is particularly evident in high-resolution grating spectra. Even though a careful modeling of the ISM has been previously attempted, its chemical composition and spatial distribution are still under debate (e.g. identification of a galactic highly ionized gas and the existence of a homogeneous distribution at large scales). Moreover, an imprecise ISM modeling can lead to erroneous conclusions when analyzing other environments such as the galactic halo or the WHIM. In this respect, a comprehensive analysis of the ISM through multiple lines of sight and using a realistic absorption model such as ISMabs would be invaluable to address these issues; consequently, we present an extensive analysis of the ISM using XMM-Newton and Chandra high-resolution X-ray spectra.
The outline of this report is as follows. In Sect. 2 the data reduction process is summarised and in Sect. 3 the data fitting procedure is described. A thorough discussion of the results is given in Sect. 4, and finally, we draw in Sect. 5 the conclusions of this work.
2. Observations and data reduction
In order to carry out the present ISM study we have gathered a sample of X-ray binary spectra from the XMM-Newton Science Archive (XSA1) and the Chandra Source Catalog (CSC2). A total of 24 bright sources have been analyzed, 15 from the XSA and 17 from the CSC, some of which have been observed with both telescopes; details of the observations are reviewed in Appendix A. As shown in Fig. 1, the source locations allow an analysis of the ISM along different lines of sight, and it also depicts the source position projected in the galactic plane. The XMM-Newton spectra were reduced with the standard Scientific Analysis System (SAS) threads3 and the Chandra spectra with the standard CIAO threads4. We have estimated the zero-order position for Chandra spectra with the findzo algorithm5. All spectra were rebinned to 25 counts per channel in order to use χ2 statistics. The spectral fitting was performed with the isis data analysis package (Houck & Denicola 2000, version 1.6.2–306).
ISMabs column densities for Chandra observations as a function of the number of counts. Black points correspond to Chandra TE-mode spectra and blue points to Chandra CC-mode spectra.
ISMabs column density values.
In order to estimate the O, Ne, and Fe column densities we have carried out a broadband fit (11–24 Å) for each source listed in Appendix A using a simple ISMabs*Bknpower model. The Bknpower component corresponds to a broken power-law that in general provides a better fit to the continuum than a single unbroken power-law. In the case of Sco X–1, we analysed the spectra in the 15–24 Å region due to the absence of data below this wavelength range. The ISMabs model (Gatuzz et al. 2015) includes photoabsorption cross sections for neutrally, singly, and doubly ionized species, and the Fe photoabsorption cross-section is taken from metallic iron laboratory measurements (Kortright & Kim 2000). For each source all observations were fitted simultaneously (i.e. using the same absorption parameters and varying the normalisation for each observation); in the case of Chandra, we considered observations with timed exposure (TE) readout mode and continuous clocking (CC) readout mode separately. The free parameters for the ISMabs fits were the H, O, Ne, and Fe column densities, including the O ii, O iii, Ne ii, and Ne iii ions.
Data statistics (e.g. number of counts in the wavelength region of interest) clearly have a significant impact on the absorption modeling. Figure 2 shows the ISMabs column densities obtained from the Chandra observations as function of the number of counts in the O (21–24 Å), Ne (13–15 Å), and Fe (16–18 Å) absorption regions, which brings out a disparity in the O columns when the number of counts is low. This is probably due to the fact that in the CC read mode the details of the spatial distribution are lost, and therefore, there is no way to spatially separate the background from the source. This affects the spectra at long wavelengths where the effective area is smaller and where the background may become comparable to the source signal.
Specifically, CC-mode observations with less than approximately 2000 counts in the O K-edge region give rise to the outliers in the left panel of Fig. 2. Therefore, in the following procedures we excluded observations with a limited number of counts in the O K-edge region (21–24 Å) and Ne K-edge region (13–15 Å). Additional information on the influence of Chandra readout modes in high-resolution spectroscopy are given in Appendix B. Finally, for those sources with observations from both Chandra and XMM-Newton, we have found that the derived columns are in good agreement and, therefore, we take the average of the fit values.
Fit results to all the observations in our sample are listed in Table 1. Upper limits for the column densities (i.e. the highest values obtained for each ion considering their upper errors) in units of 1017 cm-2 are: N(O I) < 32.46; N(O II) < 2.55; N(O III) < 3.37; N(Ne I) < 10.95; N(Ne II) < 2.11; N(Ne III) < 0.20; and N(Fe) < 2.31. Figure 3 shows the column density distribution for each source. The hydrogen and neon column densities are mostly consistent and are homogeneously distributed along their average value; this is expected in neon since it does not form molecules. Oxygen and iron column densities, on the other hand, tend to be more dispersed along the different lines of sight. This is further discussed in Sect. 4.3.
ISMabs column densities values for each source. Gray boxes correspond to a 2σ region around the average value.
Hydrogen column density comparison.
Comparison of hydrogen column densities from different 21 cm surveys with the present ISMabs results. Black data points corresponds to the ISMabs/21 cm ratio using the Dickey & Lockman (1990) measurements. The solid color lines are linear fits to the ISMabs/21 cm values relative to the various determinations from the 21 cm surveys: Dickey & Lockman (1990, red line), Kalberla et al. (2005, green line) and Willingale et al. (2013, blue line).
4.1. Hydrogen column densities
A comparison of the ISMabs hydrogen column densities with the data sets from the 21 cm surveys (Dickey & Lockman 1990; Kalberla et al. 2005; Willingale et al. 2013) is provided in Table 2. The 21 cm hydrogen column densities correspond to the average value of all absorbers within 1° of the source position. It is important to note that Dickey & Lockman (1990) and Kalberla et al. (2005) only consider the atomic H i column density while Willingale et al. (2013) includes both atomic and molecular hydrogen. Figure 4 shows a comparison of the 21 cm measurements with those derived from our ISMabs fits. Black data points corresponds to the ISMabs/21 cm ratio using the Dickey & Lockman (1990) measurements. The solid color lines are linear fits to the ISMabs/21 cm values relative to the various determinations from the 21 cm surveys (Dickey & Lockman 1990; Kalberla et al. 2005; Willingale et al. 2013). For low column densities the ISMabs values tend to be systematically larger than the 21 cm values while for high column densities the ISMabs values tend to be lower than the 21 cm values. We found overall that the best agreement of our results is with those from Willingale et al. (2013).
Comparison of the oxygen, neon, and iron total column densities obtained from the ISMabs model as function of distance (left panels), latitude absolute value (middle panels), and longitude (right panels) for all the analysed sources. Longitude has been rescaled to 0°−180°.
These discrepancies may arise from either a real difference in the intrinsic absorption or the continuum model; also, changes in the region around the X-ray source due to changes in the intrinsic column (e.g. the presence of winds) can increase absorption, and they are thus not resolved by the 21 cm surveys. These effects are more likely to be important in sources with strong stellar winds such as Cyg X–1 and Sco X–1 (Gatuzz et al. 2014). On the other hand, the hydrogen column densities obtained from broadband fits are subject to the uncertainty of the assumed underlying continuum. In some cases, the description of the spectra with different models such as Powerlaw, Bknpower, and Blackbody leads to differences in the column densities despite similar statistics. Therefore, since we are not able to favor a continuum model based on fit statistics, we have adopted for consistency and simplicity the Bknpower model for all observations. We emphasise that the continuum model must be treated carefully in any attempt to perform an ISM analysis with X-ray high-resolution spectroscopy. In this respect our results are expected to be sensitive to the particular model used to describe the continuum in all sources.
4.2. ISM structure
Figure 5 shows a comparison of the oxygen, neon, and iron total column densities from the ISMabs model as a function of distance (left panels), latitude absolute value (central panels), and longitude (right panels) for all the analysed sources. We have found that the column densities tend to increase with distance, the slope being steeper in the case of oxygen, and the general trend is to decrease with galactic latitude. This behavior is expected because the ISM material density decreases along the vertical direction away from the galactic plane. In the case of galactic longitude, it is difficult to establish a clear relationship with the column density but an increase at high longitude (i.e. away from the galactic center) is hinted.
We have derived the column-density unweighted average considering all individual sources, namely (in units of 1017 cm-2) N(O) = 18.43 ± 2.53, N(Ne) = 4.91 ± 1.19, and N(Fe) = 0.90 ± 0.18. Using the total column densities for each element, we have estimated elemental abundances with the relation Nx = AxNh, where Nh is the hydrogen column density, Ax is the abundance, and Nx is the total column density of element x; the resulting values are listed in Table 3. The abundance behavior, in the other hand, tend to be constant with distance and latitude; regarding longitude, sources with high hydrogen column densities tend to have increased abundances at low longitude values. Using the abundance values computed for all individual sources, we have derived unweighted average values relative to solar (Grevesse & Sauval 1998) of AO = 0.70 ± 0.26, ANe = 0.87 ± 0.35, and AFe = 0.67 ± 0.28.
The comparison of the oxygen and iron total column densities as a function of the neon column density is shown in Fig. 6, including for each element contributions from the neutrally, singly, and doubly ionized species. The best fitted Nx/NNe abundance ratio for all sources is plotted with the solid red line; ratios from Grevesse & Sauval (1998), Asplund et al. (2009), Lodders et al. (2009) and Juett et al. (2004) are also shown. Neon, being a noble gas, is a suitable baseline since it is only found in atomic form. We find an average ratio of N(O) /N(Ne) = 4.16 ± 0.22 larger than the estimate by Juett et al. (2006) of 3.7 ± 0.3 and lower than the solar values of 4.79 (Lodders et al. 2009), 5.36 (Grevesse & Sauval 1998) and 5.75 (Asplund et al. 2009). We also obtain an average ratio of N(Fe) /N(Ne) = 0.18 ± 0.01 in relatively close agreement with Juett et al. (2006) (0.15 ± 0.01) and lower than the solar ratios by Grevesse & Sauval (1998), Lodders et al. (2009) and Asplund et al. (2009) of 0.26, 0.25 and 0.37, respectively.
Abundance values.
Comparison of the abundance ratios NO/NNe (top panel) and NFe/NNe (bottom panel) obtained from the broadband fit with ISMabs for all the analysed sources. The best fitted Nx/NNe ratio for all sources is plotted with a solid red line. Ratios obtained from Grevesse & Sauval (1998), Asplund et al. (2009), Lodders et al. (2009) and Juett et al. (2004) are respectively shown with green, blue, orange and magenta dashed lines.
The presence of ionized species in the ISM is not negligible and must be considered in order to perform a reliable chemical analysis of its environment. Figure 7 shows a comparison of the O ii/O i, O iii/O i, Ne ii/Ne i, and Ne iii/Ne i ionization fractions as function of distance, latitude absolute value, and longitude. Unlike the column densities, the ionization fractions tend to be approximately constant with the geometric parameters. This result agrees with previous findings regarding the dominance of the ISM cold phase characterized by a low ionization degree (Gatuzz et al. 2013a,b, 2014, 2015). We obtained the following average values: O ii/O i= 0.03 ± 0.01; O iii/O i= 0.03 ± 0.02; Ne ii/Ne i= 0.21 ± 0.05; and Ne iii/Ne i= 0.03 ± 0.02.
Comparison of the ionization fractions O ii/O i, O iii/O i, Ne ii/Ne i, and Ne iii/Ne i obtained with the ISMabs model as function of distance (left panels), the latitude absolute value (middle panels), and longitude (right panels) for all the analysed sources. Longitude has been rescaled to 0°−180°.
4.3. Molecular absorption features
The search for molecular and dust spectral signatures is a topic of current interest in ISM astrophysics. Lee et al. (2009) argued that Chandra and XMM-Newton high-resolution spectra provide a resource to constrain dust properties (e.g. distribution, composition, and abundances). Absorption features due to molecules and dust have been studied previously using LMXB (de Vries & Costantini 2009; Kaastra et al. 2009; Pinto et al. 2010; Costantini et al. 2012; Pinto et al. 2013); in particular, de Vries & Costantini (2009) estimated an oxygen depletion rate to the solid state of 30−50% from an XMM-Newton RGS spectrum of Sco X–1. However, García et al. (2011) showed that, by taking into account an improved photoabsorption cross section for atomic oxygen which takes into account Auger damping, the same observation could be adequately modelled without invoking molecular or dust contributions. The best X-ray absorption model should include both atomic and molecular cross sections. However, since the spectral features from solid compounds are expected to be weak, an accurate modeling of the atomic components is a prerequisite.
In this respect, Pinto et al. (2010) previously analysed XMM-Newton spectra of the binary GS 1826–238, and after modeling the atomic component, they included molecular and dust contributions to diminish the high residuals near the oxygen edge. They derived column densities for andradite (Ca3Fe2Si3O12), amorphous ice (H2O), carbon monoxide (CO), and hercynite (FeAl2O4); however, their model included the same undamped atomic cross sections used in previous studies. Figure 8 shows XMM-Newton spectra of GS 1826–238 in the 21–24 Å region modeled by ISMabs, which takes into account a more recent and Auger-damped atomic cross section. Although ISMabs includes neither molecular nor solid photoabsorption cross-sections, it leads to a good fit of the O K-edge absorption features with well-distributed small residuals; that is, the apparent lack of absorption previously perceived by Pinto et al. (2010) was due, in our opinion, to a poor atomic model. Our results imply an upper limit to the amount of oxygen which can be in molecular or solid form. A quantitative estimate for this limit requires simultaneous fits using both our accurate atomic oxygen K shell cross sections and the best available models for absorption by molecules and dust. This will be the subject of future investigations.
GS 1826–238 XMM-Newton spectra in the oxygen K-edge region. Observations were combined for illustrative purposes.
It is important to note that, since the valence electronic levels of molecules or dust are more fully occupied than those of atoms, the Kα resonance lines from molecules and dust will in general be weaker than atoms, or absent. Thus, the addition of molecules or dust to an atomic model when fitting to observed ISM X-ray spectra will lead to a larger ratio of edge to line. Our fits do not show a systematic discrepancy or statistically significant errors in this ratio, thus reinforcing the conclusion that molecules and grains are a minor contributor to the absorption in the spectral region near the oxygen K edge.
We have performed a thorough analysis of the ISM along 24 lines of sight by means of high-resolution X-ray spectroscopy with spectra obtained from both the Chandra and XMM-Newton space observatories. This is the most complete study to date of this type and considering O and Ne charge states. We have found that data statistics (i.e. number of counts for a given wavelength region) has a sizeable impact on the analysis, which is particularly important in the case of Chandra observations taken in CC-mode as they require a higher number of counts than those in TE-mode in order to avoid background contamination. For sources observed with both telescopes, the derived column densities are in good agreement and thus average values are listed.
Using the ISMabs X-ray absorption model, we have obtained upper limits for the column densities of H i, O i, O ii, O iii, Ne i, Ne ii, Ne iii, and metallic Fe. In the case of hydrogen, we found differences between our fits and the 21 cm surveys. These discrepancies may arise from intrinsic absorption variabilities in each source as well as the particular choice of continuum representation. Our measurements indicate an increase of the column densities with source distance and a decrease with galactic latitude. We find that the ionization fractions, on the contrary, tend to be constant with distance and latitude reinforcing previous conclusions regarding the dominance of the neutral ISM component.
We have also derived the N(O) /N(Ne) and N(Fe) /N(Ne) abundance ratios finding lower values than solar (Grevesse & Sauval 1998). Using the total column densities, we estimate the O, Ne, and Fe abundances to be, respectively, ~70%, ~87%, and ~67% relative to the solar standards of Grevesse & Sauval (1998) and ~97%, ~122%, and Fe ~67% relative to the revised values of Asplund et al. (2009). In general, the abundances show a trend different to that observed in the column densities: they tend to be constant with distance and latitude.
It is important to note that this study only considers a small fraction of the local ISM environment due to the lack of a larger database of bright LMXB to perform a more extensive analysis. Observations with new-generation instrumentation such as Astro-H will allow a finer examination of the ISM large structures. The present work will be followed by a search and study of molecular and dust absorption features.
Note added in proof. While this paper was in review an X-ray analysis of the Galactic ISM was published (Nicastro et al. 2016). We agree with their findings on the presence of both a cold neutral component, dominated by O I, and a warm midly ionized component, which contains O I and O II.
http://xmm.esac.esa.int/xsa/
http://cxc.harvard.edu/csc/
http://xmm.esac.esa.int/sas/current/documentation/threads/
http://cxc.harvard.edu/ciao/threads/gspec.html
http://space.mit.edu/cxc/analysis/findzo/
http://space.mit.edu/asc/isis/
Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481 [NASA ADS] [CrossRef] [Google Scholar]
Buote, D. A., Zappacosta, L., Fang, T., et al. 2009, ApJ, 695, 1351 [NASA ADS] [CrossRef] [Google Scholar]
Costantini, E., Pinto, C., Kaastra, J. S., et al. 2012, A&A, 539, A32 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
de Vries, C. P., & Costantini, E. 2009, A&A, 497, 393 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Dickey, J. M., & Lockman, F. J. 1990, ARA&A, 28, 215 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
Fang, T., Buote, D. A., Humphrey, P. J., et al. 2010, ApJ, 714, 1715 [NASA ADS] [CrossRef] [Google Scholar]
Galloway, D. K., Muno, M. P., Hartman, J. M., Psaltis, D., & Chakrabarty, D. 2008, ApJS, 179, 360 [NASA ADS] [CrossRef] [Google Scholar]
García, J., Mendoza, C., Bautista, M. A., et al. 2005, ApJS, 158, 68 [NASA ADS] [CrossRef] [Google Scholar]
García, J., Ramírez, J. M., Kallman, T. R., et al. 2011, ApJ, 731, L15 [NASA ADS] [CrossRef] [Google Scholar]
Gatuzz, E., García, J., Mendoza, C., et al. 2013a, ApJ, 778, 83 [NASA ADS] [CrossRef] [Google Scholar]
Gatuzz, E., García, J., Mendoza, C., et al. 2013b, ApJ, 768, 60 [NASA ADS] [CrossRef] [Google Scholar]
Gatuzz, E., García, J., Mendoza, C., et al. 2014, ApJ, 790, 131 [NASA ADS] [CrossRef] [Google Scholar]
Gatuzz, E., García, J., Kallman, T. R., Mendoza, C., & Gorczyca, T. W. 2015, ApJ, 800, 29 [NASA ADS] [CrossRef] [Google Scholar]
Gorczyca, T. W., & McLaughlin, B. M. 2000, J. Phys. B: At. Mol. Opt. Phys., 33, L859 [NASA ADS] [CrossRef] [Google Scholar]
Gorczyca, T. W., Bautista, M. A., Hasoglu, M. F., et al. 2013, ApJ, 779, 78 [NASA ADS] [CrossRef] [Google Scholar]
Grevesse, N., & Sauval, A. J. 1998, Space Sci. Rev., 85, 161 [NASA ADS] [CrossRef] [Google Scholar]
Grimm, H.-J., Gilfanov, M., & Sunyaev, R. 2002, A&A, 391, 923 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Houck, J. C., & Denicola, L. A. 2000, in Astronomical Data Analysis Software and Systems IX, eds. N. Manset, C. Veillet, & D. Crabtree, ASP Conf. Ser., 216, 591 [Google Scholar]
Hynes, R. I., Steeghs, D., Casares, J., Charles, P. A., & O'Brien, K. 2004, ApJ, 609, 317 [NASA ADS] [CrossRef] [Google Scholar]
in't Zand, J. J. M., Kuulkers, E., Verbunt, F., Heise, J., & Cornelisse, R. 2003, A&A, 411, L487 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Jonker, P. G., & Nelemans, G. 2004, MNRAS, 354, 355 [NASA ADS] [CrossRef] [Google Scholar]
Juett, A. M., Schulz, N. S., & Chakrabarty, D. 2004, ApJ, 612, 308 [NASA ADS] [CrossRef] [Google Scholar]
Juett, A. M., Schulz, N. S., Chakrabarty, D., & Gorczyca, T. W. 2006, ApJ, 648, 1066 [NASA ADS] [CrossRef] [Google Scholar]
Kaastra, J. S., de Vries, C. P., Costantini, E., & den Herder, J. W. A. 2009, A&A, 497, 291 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Kalberla, P. M. W., Burton, W. B., Hartmann, D., et al. 2005, A&A, 440, 775 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Kortright, J. B., & Kim, S.-K. 2000, Phys. Rev. B, 62, 12216 [NASA ADS] [CrossRef] [Google Scholar]
Kuulkers, E., den Hartog, P. R., in't Zand, J. J. M., et al. 2003, A&A, 399, 663 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Lee, J. C., Xiang, J., Ravel, B., Kortright, J., & Flanagan, K. 2009, ApJ, 702, 970 [NASA ADS] [CrossRef] [Google Scholar]
Liao, J.-Y., Zhang, S.-N., & Yao, Y. 2013, ApJ, 774, 116 [NASA ADS] [CrossRef] [Google Scholar]
Lodders, K., Palme, H., & Gail, H.-P. 2009, in Landolt Börnstein, Vol. VI/4B, 560 [Google Scholar]
Luo, Y., & Fang, T. 2014, ApJ, 780, 170 [NASA ADS] [CrossRef] [Google Scholar]
Nicastro, F. 2014, in The X-ray Universe 2014, ed. J.-U. Ness, 11 [Google Scholar]
Nicastro, F., Senatore, F., Gupta, A., et al. 2016, MNRAS, 457, 676 [NASA ADS] [CrossRef] [Google Scholar]
Paerels, F., Brinkman, A. C., van der Meer, R. L. J., et al. 2001, ApJ, 546, 338 [NASA ADS] [CrossRef] [Google Scholar]
Pinto, C., Kaastra, J. S., Costantini, E., & Verbunt, F. 2010, A&A, 521, A79 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Pinto, C., Kaastra, J. S., Costantini, E., & de Vries, C. 2013, A&A, 551, A25 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Ren, B., Fang, T., & Buote, D. A. 2014, ApJ, 782, L6 [NASA ADS] [CrossRef] [Google Scholar]
Sala, G., & Greiner, J. 2006, ATel, 791, 1 [NASA ADS] [Google Scholar]
Schulz, N. S., Cui, W., Canizares, C. R., et al. 2002, ApJ, 565, 1141 [NASA ADS] [CrossRef] [Google Scholar]
Takei, Y., Fujimoto, R., Mitsuda, K., & Onaka, T. 2002, ApJ, 581, 307 [NASA ADS] [CrossRef] [Google Scholar]
Willingale, R., Starling, R. L. C., Beardmore, A. P., Tanvir, N. R., & O'Brien, P. T. 2013, MNRAS, 431, 394 [NASA ADS] [CrossRef] [Google Scholar]
Yao, Y., Schulz, N. S., Gu, M. F., Nowak, M. A., & Canizares, C. R. 2009, ApJ, 696, 1418 [NASA ADS] [CrossRef] [Google Scholar]
Ziółkowski, J. 2005, MNRAS, 358, 851 [NASA ADS] [CrossRef] [Google Scholar]
Appendix A: Data sample
Table A.1
Chandra observation list.
For this analysis we use a sample of 84 observations; the details of the Chandra and XMM-Newton observations are listed in Tables A.1, A.2. The number of counts for each observation in the broadband fit region (11–24 Å), O K-edge region (21–24 Å), Ne K-edge region (13–15 Å), and Fe L-edge region (16–18 Å) are also included. In the case of Chandra, 20 and 29 observations were taken in TE-mode and CC-mode, respectively.
XMM-Newton observation list.
Figures A.1, A.2 show the best broadband fit for each source in flux units. In cases where more than one observation is present, the observations are fitted simultaneously varying the continuum parameters and have been onlycombined for illustrative purposes. The best-fit model is indicated by a solid red line. In the case of Sco X–1, the broadband fit was performed in the 15–24 Å wavelength range due to the absence of data below 15 Å (see Fig. A.3). The dominant observed absorption features correspond to the O K edge (~23 Å), Ne K edge (~14 Å), Fe L edge (~17 Å), and the O i Kα transition (~23.5 Å). In general, a smooth residual distribution (bottom panels) around these edges is observed, indicating modeling accuracy that relies on the most up-to-date atomic data. It must be emphasised that the absence of molecular photoabsorption cross-sections in the ISMabs model (except for metallic Fe) does not represent a spectral fitting limitation. This issue has been discussed in Sect. 4.3. All data have been rebinned to 25 counts per channel and combined for illustrative purposes
Fig. A.1
ISMabs best broadband fits for the analysed sources where observations are combined for illustrative purposes. In the case of Chandra the read mode (CC-mode or TE-mode) is indicated.
ISMabs best broadband fits for Sco X-1. Observations were combined for illustrative purposes.
Appendix B: Chandra CC-mode notes
The Chandra CC-mode provides a fast readout mode to decrease the pileup effect in bright sources; i.e. the detection of two
photons as a single event with the sum of their energies. While in TE-mode the events are collected for a specific time frame and then read out collectively, in CC-mode they are read out continuously by collapsing them to one row. In the case of a low-count regime, CC-mode data must be analysed carefully because they can be affected by the background that cannot be separated from the source spectrum.
As an example of this effect we show in Fig. B.1 a comparison of the 4U 1636–53 spectra in the 11–24 Å region as obtained by the Chandra TE-mode, CC-mode, and XMM-Newton. All data have been rebinned to 25 counts per channel and combined for illustrative purposes. The total number of counts in the oxygen absorption region (21–24 Å) without rebinning is 1591 (CC-mode), 1035 (TE-mode), and 28240 (RGS). The O i and O ii Kα absorption lines at ~23.5 Å and ~23.35 Å, respectively, are clearly observed in the TE-mode and the RGS data, but they cannot be detected in CC-mode due to background contamination that becomes dominant at ~18−20 Å. For this reason and based on previous tests, we have discarded from our analyses the oxygen column densities derived from observations in CC-mode with less than 2000 counts in the oxygen K-shell region.
Fig. B.1
A comparison of the 4U 1636–53 spectra obtained with XMM-Newton, Chandra TE-mode, and Chandra CC-mode in the broadband region. Observations are combined for illustrative purposes.
In the text
ePUB (1.952 MB)
Low-energy absorption towards the ultra-compact X-ray binary 4U 1850-087 located in the globular cluster NGC 6712
XMM-Newton observations of the low-mass X-ray binary XB 1832–330 in the galactic globular cluster NGC 6652
Interstellar oxygen along the line of sight of Cygnus X-2
VLT spectroscopy and non-LTE modeling of the C/O-dominated accretion disks in two ultracompact X-ray binaries
Interstellar medium composition through X-ray spectroscopy of low-mass X-ray binaries


The summer always seems to fly by (too quickly in my opinion) and this year I want to make an effort to do some things that I've been planning to do. It's already almost July so I better get on it! I'm a list maker - it keeps me organized at my job and in life. I can be kind of scattered in my thoughts so lists help me focus on my priorities and things that I want to do. I'm not sure if I'll have time to do all the things I really want to do this summer, but I tried to narrow it down to the top ideas. It will be fun to check back in at the end of the summer and cross off what I did.
Visit Coney Island. I've heard mixed reviews about Coney Island, but I've lived here over three years now and still haven't been. This is a top item on my list - I need to go and formulate my own opinion.
Make a pie from scratch. Pie crust has always been intimidating to me. How does the crust get so buttery and crispy? I think I've done enough research by now, and I made a Triple Berry Galette over the weekend which gave me some practice!
Try Stumptown's Nitro Cold Brew Coffee. Apparently this nitro infused cold brew is the new coffee trend. It's fizzy and has a creamy finish. I'm intrigued. Well I'm at it I also want to try the Stumptown Cold Brew Tonic that uses cherry. More creative iced coffee drinks here.
Eat crab at the beach. Ever since I saw pictures on Instagram of Brooklyn Crab in Redhook I have been dying to do this. I've been looking for places on the Connecticut shore, Rhode Island and Cape Cod but can't find any. If anyone has a recommendation please let me know!
Try boxing! After watching a video of Gigi Hadid boxing, I've been wanting to try this, even though I know I would be hilariously terrible. It just seems like a new and fun way to exercise. My friend boxes during the week on the Hudson River Park so I'm hoping to go with her one week.
Eat pie at Four and Twenty Blackbirds. Drooling. Do I need to have a reason to want to go here? I'm on a pie-high.


Eco Scraps, Inc. manufactures organic, chemical, and manure-free lawn and garden products from food waste. The company processes and recycles food waste into nutrient-rich products that help plants grow healthier. It offers organic soils, organic plant food, and natural liquid fertilizers. The company provides its products through retail stores in the United States, as well as online. Eco Scraps, Inc. was founded in 2010 and is based in South Jordan, Utah with manufacturing locations in Utah, Arizona, Texas, and California. As of December 31, 2014, Eco Scraps, Inc. operates as a subsidiary of The Hawthorne Gardening Company.


Is this all God intends me to be? All body, creating and bearing, loving and serving? Wiping tears and dirty bottoms, serving meal after meal. Teaching and re-teaching the basic lessons of life: be kind, love your enemies, honor your parents, and worship the Creator. Work so important and so encompassing that I feel overwhelmed by its high demands and yet trapped in claustrophobic tightness by my little audience and limited subject matter.
I dream of directing government policy projects with huge objectives that improve the life of millions, of being somebody and using my mind more than my body. I am light years away from that vision. Yet stopping to reflect, I realize that I do lead according to Biblical principles. My audience of children may be limited, but my influence over them is far greater than I could ever have with any constituents.
The work done here at home really matters – yielding tremendous consequences for all eternity. For what happens here day in and day out – these routines and behaviors that we practice, the books that we read, the conversations that we hold – form who we are and inform what we do when we go into the world. It is in this present, each messy moment of it, that we shape characters, form imaginations, decide to follow Christ, and encourage our children to do the same.
Though the work may seem small, it is not so, for we are entrusted with the care of eternal souls. Whether you find yourself here unexpectedly or on purpose, and whether you really like the work or you really don't, I encourage you to live in this present moment that touches eternity. May we be faithful in these not-so-little things.


Abstract. We discuss circle map sequences and subshifts generated by them. We give a characterization of those sequences among them which are linearly recurrent. As an application we deduce zero-measure spectrum for a class of discrete one-dimensional Schr\"odinger operators with potentials generated by circle maps.


text:
Amanda Stanton, Lauren Bushnell reveal they are starting a business together
15 Times Lauren Bushnell Shut Down Critics of Her Weight ... - wetpaint.com
These two alumni of 'The Bachelor' became good friends and are now working together
by Mandy Robinson
May 23, 2017 at 9:40 PM May 23, 2017 at 9:40 PM
Don't miss on the latest updates
Click on the topic that interests you to follow it. We will keep you updated with the news you shouldn't miss.
Lauren Bushnell and Amanda Stanton became really Good Friends while on "The Bachelor." It turns out that these two are actually going to start a business together. ET was able to get all of the details about their big plans and what the business will be. Amanda came by to talk to them on Facebook Live about the details.
What are these two girls planning?
Amanda Stanton revealed that they actually want to start an online boutique together. She shared details saying, "We've been talking about it for so long and I feel like we've just been putting it off because we've been so busy and just dealing with a lot, but hopefully we'll get started on it pretty soon." They will have clothes, shoes and other accessories.
It sounds like this online boutique will have amazing stuff. If you have ever paid attention to how Lauren and Amanda dress, then you know they have great taste in clothes. They already have a ton of social network followers, so this is going to make launching a new business even easier for them.
How are they both doing now?
Amanda Stanton and Josh Murray fell in love on "Bachelor in Paradise" and got engaged. They moved in with each other after the show and then later split. Amanda seems to still be single and Josh was recently on an episode of "Steve Harvey" saying that he is ready to find love again. If Josh Murray has found his perfect girl, then he isn't sharing just yet. Steve did set him up on a couple of dates.
Josh did share today that he doesn't plan on doing "Bachelor in Paradise" this year, though.
Lauren Bushnell just recently revealed that she has split from Ben Higgins. They were engaged and even did a show together called "Lauren and Ben: Happily Ever After?" During the show, Ben called off their wedding, but then it looked like they were going to be fine.
Now, the two have called it quits. Lauren moved back to California and Amanda shared that she is driving up to see her and she is helping her through this hard time. Lauren admitted that she is planning to do some modeling while she is in California, but that is also where her family is from, which explains why she chose there to move.
Are you shocked to hear that Amanda and Lauren are going to start a business together? Do you feel like this will be successful? Sound off in the comments section below on your thoughts, and don't miss watching Rachel Lindsay on "The Bachelorette" on Monday nights on ABC. Her season just started airing, but fans are hoping to watch Rachel find a love that will last.
Mandy Robinson
Mandy Robinson has been a freelance writer for eight years. She will never shy away from a good story and loves to write on the best reality TV spoilers, celeb news and more.
Follow mandy on Facebook Follow mandy on Twitter
Read more on the same topic from Mandy Robinson:
Jill Dillard shares her boys making their own kind of chalk plus a mess '90 Day Fiance' star Zied admits he is jealous type Todd Chrisley denies new accusations against him and wife Julie by daughter Lindsie
Blasting News recommends Mike Tyson wants Tom Brady to return to the Bucs next season Rob Gronkowski weighs in on Brady's future: TB12 will pick Bucs over Raiders Daddy duty for Tom Brady as he spends quality time with daughter Vivian Details about Rachel Lindsay's dress on the premiere of 'The Bachelorette' James Bond star dies at age 69 in Switzerland

redpajama_set_name: RedPajamaCommonCrawl


text:
Best Cities to Live in Every State
Samuel Stebbins
Last Updated: August 13, 2020 6:29 pm
Source: TriggerPhoto / iStock via Getty Images
Kansas: Leawood
> Population: 34,570
> 5 yr. population change: +7.1%
> Median household income: $149,736
> 5 yr. avg. unemployment: 2.4%
Leawood, Kansas, is a city of just under 35,000 residents located about 10 miles south of Kansas City, Missouri. Within commuting distance to one of the largest cities in the Midwest, Leawood's five-year average unemployment rate of 2.4% is less than half the comparable 5.9% national rate. The city is one of the safest in the state, with a violent crime rate of just 77 per 100,000 people, about one-fifth the comparable national rate.
The city's safe streets and a strong job market are likely pulling many new residents and families to Leawood. Over the last five years, the city's population has grown by 7.1%.
Source: Nyttend / Wikimedia Commons
Kentucky: Fort Mitchell
> Population: 8,237
Bolstered by employment opportunities in nearby Cincinnati, Fort Mitchell, Kentucky, boasts one of the strongest job markets in the country. Over the last five years, unemployment in the northern Kentucky city has averaged just 0.4%. The area's widespread employment has reduced the likelihood of financial hardship, and just 8.3% of Fort Mitchell's population lives below the poverty line, one of the lower poverty rates in Kentucky.
Quality of life in Fort Mitchell is bolstered by several parks, containing baseball fields, tennis, basketball, and volleyball courts, pavilions, playgrounds, and picnic areas. The city is also one of the safest in the state, with a violent crime rate of just 48 per 100,000 people, about one-eighth of the comparable national rate.
ALSO READ: Best Public High School in Every State
Source: Infrogmation / Wikimedia Commons
Louisiana: Harahan
Residents of Harahan, Louisiana, a suburb of New Orleans, benefit from a strong job market. The average unemployment rate in the city was just 2.9% over the last five years, lower than in the vast majority of the state. Widespread job opportunities can help reduce the likelihood of financial instability. In Harahan, most households earn more than $63,000 a year, more than in most parts of Louisiana.
Harahan is also a relatively safe city, with only 127 violent crimes reported for every 100,000 people in 2018 — about one-third the national violent crime rate.
Source: P199 / Wikimedia Commons
Maine: Brewer
> 5 yr. population change: -3.2%
Residents of Brewer, Maine, benefit from a low cost of living. Goods and services in the small city located just outside of Bangor are about 10% less expensive than they are nationwide on average. Brewer is also a safe city with a violent crime rate of just 134 for every 100,000 people — well below the national rate of 381 violent crimes per 100,000 Americans. Brewer champions itself as a business-friendly community, and industry does appear to be thriving in the area. Over the last five years, the local unemployment rate has averaged just 2.6%, less than half the comparable national rate.
Maine is struggling with weak population growth, and despite ranking as the best city in the state, Brewer's population is contracting. Over the last five years, the number of people living there has fallen by 3.2%.
Mount Airy Mansion (CC BY-SA 2.0) by Preservation Maryland
Maryland: Mount Airy
Mount Airy, Maryland, is a town of less than 10,000 about 40 miles north of Washington D.C. Of all cities and towns tracked by the FBI, Mount Airy is the safest in Maryland, with only 42 violent crimes for every 100,000 people.
As is often the case in safe communities on this list, Mount Airy has a strong job market and a relatively affluent population. The town's average unemployment rate over the last five years was just 3.1%. Additionally, most households in the area earn over $117,000 a year.
Read more: Special Report, Housing


text:
/*
 * Author: 陈志杭 Caspar
 * Contact: 279397942@qq.com qq:279397942
 * Description: 数据接口契约文件
 * 文件由模板生成,请不要直接修改文件,如需修改请创建一个对应的partial文件
 */
using System;
using System.Collections;
using Zh.DAL.Define.Entities;
using Zh.DAL.Define;
using Zh.DAL.Base.Define;
using Zh.DAL.Define.Contracts;
namespace Zh.DAL.Imp.NH.Contracts
{
    /// <summary>
    /// Activity_ChampionGuessRecord(冠军竞猜记录)表访问类
    /// </summary>
    public partial class ActivityChampionGuessRecordDao : BaseDao<Activity_ChampionGuessRecord>,IActivityChampionGuessRecordDao
    {

    }
}

redpajama_set_name: RedPajamaGithub


Stearns and Foster including box spring. Real good shape.
Welcome Back Snow Birds ! Now is the time to do that all important Golf Cart Maintance!!
A classic this year. No rust, needs paint,rear window, idler pulley. Runs and drives good.v6,auto,cold ac. Stepside.
Three Home Depot garage cabinets, 48×72, 30×72 and 24×72. All assembled and in excellent condition.
Mid-century Modern side or entry table. Cute colors but easily repainted. Original drawer pulls. Please call 507-429-8667.
All wood work bench, excellent like new condition, originally purchased from Harbor Tools for $159.99.


text:
The German Navy 1919-1935 (Vorläufige Reichsmarine)
On November 11th, 1918, Germany signed the armistice ending the First World War. On April 16th, 1919, before the Treaty of Versailles was enacted, Germany established a new navy – the Vorläufige Reichsmarine or Interim Imperial German Navy. Two years later on March 31st, 1921, the name was changed when Vorläufige was dropped and the navy became simply the Reichsmarine. It was at this time that the Reichsmarine – which had been founded in 1919 – became the full-fledged German navy. The Reichsmarine flag was first flown on April 11th, 1921, and the Kaiser's flag was hoisted for the last time on December 31st, 1921. The navy that existed between 1919 and 1935 was in every way transitory, even when the term Vorläufige was removed from the title. The German navy was in every way "Interim" before 1935. The Reichsmarine would exist until May 21st, 1935, when the Kriegsmarine was officially formed.
The first commander of the Vorläufige Reichsmarine was Vice-Admiral Adolf von Trotha. One of Trotha's first and assuredly most important orders was for the scuttling of the German fleet of nearly 50 ships interned at Scapa Flow on June 21st, 1919, to prevent them from being handed over to the British. The signing of the Treaty of Versailles took place on June 28th, 1919, and the restrictions placed upon the new Vorläufige Reichsmarine was very harsh – more so as a result of the order to scuttle the German fleet a few days earlier.
Although heavily regulated after June of 1919 by the restrictions of the Treaty of Versailles, the Reichsmarine existed none-the-less. The Vorläufige Reichsmarine attempted to carry on the grand traditions of the Kaiserlichemarine of WWI, but it was virtually impotent as a result of a total lack of modern vessels and the lingering scars of the attempted naval mutinies during the last days of WWI. The weak and almost exclusively defensive Reichsmarine existed under the following guidelines, drawn up by the navy itself; To enforce the laws of the state in German coastal areas, to control German territorial waters, to prevent piracy in German waters, to defend German coastal regions from annexation by other coastal states, to control coastal seaplanes, to perform courtesy visits, to secure against naval blockades, and to perform the various hydrographic survey, fishery protection, and oceanographic work. Naval planners wouldn't have to wait long for the beginnings of a stronger navy though, as preparations for an increasingly powerful navy began to take place almost as soon as the Treaty restricting such things was signed. The Kriegsmarine – formed in 1935 – had its roots founded firmly in the advances of the Reichsmarine. In fact, most of the vintage WWI Reichsmarine ships would go on to become an actual part of the new Kriegsmarine, and many of the major ships of the Kriegsmarine were launched during the Reichsmarine period.
Listed below are those ships that are known to have served in the Reichsmarine. The first listing is of the ships that survived WWI and served in the initial Vorläufige Reichsmarine, the second listing is of those ships launched during the period of the Reichsmarine between 1919-1935. In both cases, those ships that are known to have gone on to serve in the Kriegsmarine are marked as such.
Ships that Survived WWI and Served in the Vorläufige Reichsmarine:
Elass
Lothringen
Schlesien*
Schleswig-Holstein*
Niobe*
Nymphe*
Thetis*
G7 (later T108)
G10 (later T110)
Torpedo Boats:
T108* (ex-G7)
T110* (ex-G10)
Minesweepers
38 Vessels
Gunnery Tenders
plus 5 others
Auxiliary Vessels
18 Picket vessels
8 fishery protection vessels
2 accommodation ships
4 survey vessels
1 sailing ship
various minor craft
Ships Built for the Vorläufige Reichsmarine Between 1919 – 1935:
Armored Ships:
Deutschland* (initially ersatz Preussen)
Admiral Scheer* (initially ersatz Lothringen)
Admiral Graf Spee* (initially ersatz Braunschweig)
Emden*
Königsberg*
Karlsruhe*
Köln*
Leipzig*
Möwe*
Seeadler*
Greif*
Albatros*
Kondor*
Falke*
Wolf*
Iltis*
Luchs*
Tiger*
Jaguar*
Leopard*
Submarines:
U1*
U25*
Fast Attack Craft:
Narwal UZ(S)18
K-boat UZ(S)12
UZ(S)16 (later W.1, W = Guard Boat)
S2*
Other Vessels:
Elbe* (fishery protection vessel)
Weser* (fishery protection vessel)
Bremse* (gunnery training ship)
R1* (motor minesweeper)
R2* (")
R10* (")
ReichswehrThe German Imperial Army 1918 – 1935
anchour
ReichsmarineThe German Navy 1919-1935
HeerThe Nazi German Army 1935-1945
LuftwaffeThe Nazi German Air Force 1935-1945
KriegsmarineThe Nazi German Navy 1935-1945
Waffen-SSThe Nazi German Armed Waffen-SS 1933-1945
WehrmachtsgefolgeAuxiliary Organizations
FreiwilligeForeign Volunteers
AlliierteAxis Powers
KollaborationAxis Collaboration
Research German Military Records
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If you want to have fun and burn calories, then this 30 minutes Cardio Kickboxing session is for you. This full workout aims to burn an average of 250 -- 300Cals. We'll be doing lots of punches and kicks and they are great moves to burn fat and to tone up on your hips, thighs, waist and arms. So get ready to throw me some punches and kicks!
45 seconds workout with 15 seconds rest for each exercise. Once you have completed Round 1, rest for 1 minute and repeat all the exercises again for Round 2. Stretch for 5 minutes at the end of the workout.


text:
West Park, NY
Best Events Near You in West Park, New York
Exhibition - Hot/Cold: Expressions in Wax
Tuesday, Jan 21, 2020 from 9:30am to 5:30pm
Arts Mid-Hudson
Wednesday, Jan 22, 2020 from 9:30am to 5:30pm
Thursday, Jan 23, 2020 from 9:30am to 5:30pm
West Park Top Searches
Friday, Jan 24, 2020 from 9:30am to 5:30pm
Back In Black and Never Say Die
The Chance Theater
Back In Black (AC/DC TRIBUTE), Never Say Die- The Ultimate Black Sabbath Experience , SixXV
The Chance
Ulster Performing Arts Center
Levitated, Empty Vessel, Fateless, Diamonds to Dust , Parkbench Messiah , Charred Graves
John Valby
Shuli Egar
Laugh It Up Comedy Club
Ross the Boss, Power Theory, Divine Incarnation
Monday, Jan 27, 2020 from 9:30am to 5:30pm
Circus With Miller Middle School
Four Horsemen (metallica trib), Something Wicked this way comes , Mainline, White Noize
The Four Horsemen – The Ultimate Tribute to Metallica
2nd Nature Skate Park
1 Highland Industrial Park
Rules: - No bikes - No graffiti - No glass containers - No fighting or shoving - Please dispose of your trash properly&nbs...
Angelo Canna Town Park
Joseph D Spencer Lane
Cairo, NY
Arm of the Sea Theater
Malden on Hudson, NY
Our mission is to create theater that inspires wonder, provokes thought, gives joy and enriches the public imagination. We believe that such theate...
Featured Homes For Sale in West Park!
Palisades Parkway or Route 9W North
Bear Mountain, NY
Bear Mountain State Park is situated in rugged mountains rising from the west bank of the Hudson River. The park features a large play field, shade...
Belleayre Mountain Ski Center
181 Galli Curci Rd
Highmount, NY
From the beginning, Belleayre was an immediate hit. Local residents still remember how skiers pitched tents outside the lodge to be first...
1601 Route 9D
Garrison, NY
Boscobel is situated on the east bank of the Hudson River opposite the United States Military Academy at West Point. The mansion and surrounding gr...
Bowl O Fun Skate Park
Monroe, NY
Caramoor Center for Music and the Arts
149 Girdle Ridge Road
Caramoor is the legacy of Walter and Lucie Rosen who built the luxurious Mediterranean-style villa and filled it with their treasures. Walter Rosen...
Cary Institute of Ecosystem Studies
2801 Sharon Turnpike (Route 44)
Millbrook, NY
The Cary Institute is one of the largest ecological programs in the world. More important than its size, however, is the quality of its output. Boo...
Center For Performing Arts At Rhinebeck
About Us The CENTER for Performing Arts at Rhinebeck (known familiarly as The CENTER, and legally as Rhinebeck Performing Arts, Inc. or RPA) is a n...
Chatham Skate Park
Chatham, NY
The first phase of the concrete skate park will be approximately 5100 square feet and will include a street plaza design and a bowl/pool to appease...
Clearwater's Great Hudson River Revival
1 Croton Point Ave.
Mission of the FestivalClearwater's Great Hudson River Revival is produced by the nonprofit, member-supported, environmental organization Hud...
D and H Canal Historical Society and Museum
23 Mohonk Road
High Falls, NY
Mission Statement: Now celebrating our 40th year, the purpose of the D & H Canal Historical Society is to preserve, protect and perpetua...
Delaware and Ulster Railroad
Arkville, NY
History Tracing the Proud History of the Ulster & Delaware Railroad When a scenic train ride was established in Arkville, NY in 1986, the excur...
Drop In Skate Park
107 Pleasant Avenue
Hillburn, NY
Dutchess County Fairgrounds
6550 Spring Brook Avenue
Vision StatementOur vision is a society actively engaged in the pursuit and promotion of our rural and agricultural heritage, from neighborhood bac...
Eisenhower Hall Theatre
655 Pitcher Road
Highland Falls, NY
The Eisenhower Hall Theatre at West Point is dedicated to bringing great performances to the United States Corps of Cadets and to its friends and n...
Empire State Railway Museum
70 Lower High St
Phoenicia, NY
History From the late 1800's through the 1940's the rugged steam locomotives of the Ulster & Delaware, Catskill Mountain Railroad, New York C...
Falcon Ridge Folk Festival
44 County Road 7D
Hillsdale, NY
Directions The Falcon Ridge Folk Festival is located at Dodds Farm, just off Route 22 north of Hillsdale, New York. Hillsdale is in the Tri-State ...


Porcelain veneers, also known as porcelain laminates, can make teeth look straighter, lighter in color and appear longer. They could be compared to false fingernails, since they're placed over the front of the teeth extending over the edges. Unlike crowns which cover the whole tooth, veneers cover very little of the back of the tooth. Veneers are natural and lifelike since they contain no metal. This allows them to be translucent like natural teeth, unlike porcelain-to-metal crowns.
Prior to the veneer process it is best to have a "Smile Analysis" to design and computer image the desired result. The veneering process involves just two steps. The teeth are prepared for veneers at the first visit. This involves the removal of about only one-half of a millimeter of tooth structure from the front of the teeth and only one millimeter from the edge. An impression of the teeth is then made, a color or shade for the veneers is selected and photographs taken. At the second visit the teeth are conditioned and the veneers are bonded to the teeth with porcelain-to-tooth bond, the strongest bond used in dentistry.
Patients should be made aware of the different types of veneers . At Delmarva Dental Services we use "fire-stacked porcelain" veneers from DaVinci Dental Laboratory in California. This requires less tooth structure removal and creates a more natural smile. Some dental offices use a "pressed ceramic" veneer involving a considerable amount of tooth structure removal. This veneer has a more artificial look. Crowning or capping teeth is even more drastic with the removal of about four times the amount of tooth structure.
Veneers last a very long time. They do not stain or wear down. Porcelain veneers have been in existence since the mid 1980's. We, at Delmarva Dental Services, P.A., have been providing our patients with this service since 1987.


There are no comments for Tariff Bill, 1921. Click here to post the first comment.
TARIFF BILL, 1921. 'Cures All the Ills of Man or Beast.' Cartoon, 1921, by Rollin Kirby commenting on the resurrection of the Fordney Emergency Tariff Bill, vetoed by President Woodrow Wilson but signed, 1921, by President Warren G. Harding.


text:
Q: How can I tell if my activity was started by a broadcast receiver? I have an alarm clock application I am making. I have one activity where the user sets the time for the alarm. This registers a broadcast receiver class I have made to receive a broadcast at the time of the alarm, using AlarmManager. I then start a new activity in the receivers onReceive(). When this second activity starts, the alarm clock sound is played in onStart(). How can I tell if my activity has been started by a receiver or if the user is just multitasking with the application? I don't want my sound to play when the user silences the alarm, presses the home button, and then renters the app (while still on the sound playing activity).

A: Just send an extra via the intent you use in your onReceive() method:
Intent intent = new Intent(this, NextActivity.class);
intent.putExtras("playSound", true);

in your "sound playing" activity, you have to play the sound in onCreate():
boolean playSound = getIntent().getBooleanExtra("playSound", false);

This will return false if the intent-extra "playSound" does not exist or is set to false, true if it is set to true.

onCreate() is only called once (when the activity starts), while onStart() gets called everytime a user reenters your activity (i.e. through recent apps). You can see this in the lifecycle:

(diagram source)
Where Paused is called when something draws over you activity (e.g. low battery dialog), Stopped is called if you "exit" your app (e.g. through the home-button).

A: Start an activity or a service, etc., based on a received broadcast then you need a standalone broadcast receiver and you put that in your android manifest file. If you want your activity itself to respond to broadcasts then you create an instance of a broadcast receiver in your activity and register it there.
public class BRActivity extends Activity {
private BroadcastReceiver broadcastReceiver = new BroadcastReceiver(){
    @Override
    public void onReceive(Context context, Intent intent) {
        ..................
        ..................
    }
};

public void onResume() {
    super.onResume();

    IntentFilter filter = new IntentFilter();
    filter.addAction(BROADCAST_ACTION);

    this.registerReceiver(this.broadcastReceiver , filter);
}

public void onPause() {
    super.onPause();

    this.unregisterReceiver(this.broadcastReceiver );
}

}
So, this way the receiver is instantiated when the class is created (could also do in onCreate). Then in the onResume/onPause I handle registering and unregistering the receiver. Then in the reciever's onReceive method I do whatever is necessary to make the activity react the way I want to when it receives the broadcast.

A: You can do as below:

*

*For each alarm user sets, you put an boolean flag in sharedpreference to true. E.g. you have three alarms then in sharedpreference you will have 3 flags.

*Now suppose a alarm broadcast is received for alarm1 and activity2 is started.

*Now in activity2 first thing you check is whether the flag for alarm1 which you set in sharedpreference is true or false, if true play sound.

*When user silences the alarm or press home button then you can mark this flag to false, so next time if user starts activity from background, flag in sharedpreference will be false and sound will not be played.

Same thing you can achieve using sqlite db, by setting flags in sqlite db table instead of sharedpreference.

A: For the intent used to launch the sound playing activity use the FLAG_ACTIVITY_EXCLUDE_FROM_RECENTS flag. So if the user moves out of the activity, it cannot be resumed.
Intent intent = new Intent(context, SoundActivity.class);
intent.setFlags(Intent.FLAG_ACTIVITY_EXCLUDE_FROM_RECENTS);

or in manifest
<activity
        android:name="SoundActivity"
        android:excludeFromRecents="true" >
</activity>

A: There are couple of solutions:
(1) one approach is to use a Singleton Class which can be shared across activity.
In this approach set a boolean flag of Singleton class in BroadcastReceiver and then check that flag in the activity (which is fired from your BroadcastReceiver) where you play sound. Please reset the flag if it is set. This solution assumes that the Broadcast receiver is part of your Android App package.
(2)
Alternatively, you can also use Intet.putExtra ("Key", Value) method when you start an activity from BroadcastReceiver. You can check this key in the Activity you started from BroadcastReceiver to know who started this activity.
So this will take care of detecting where you come from.
If you are simply trying to set single (one-shot ) alarm then creating another activity for playing the sound is OK. If you set repeat alarm ( alarm plays at a multiple interval), I am not sure how your application will behave.
I prefer to play the sound in the Broadcast receiver itself (registered as remote receiver in manifest) for a specified duration for a given alarm ( like 30 sec of sound or you can ask user to configure it).
So this way you can use the same BroadcastReceiver for playing sound for single-shot & multi-repeat alarm.
I will use the same PendingIntent for setting both Single-shot and multi-repeat alarm.

A: This is the code to find if app is started via broadcast receiver.
public class AlarmReceiver extends BroadcastReceiver
{
    @Override
    public void onReceive(Context context, Intent intent)
    {

    String AlarmTriggerString = (String)intent.getSerializableExtra("AlarmTrigger");
    Intent i = new Intent();
    i.setClassName("com.prasath.viki.bot","com.prasath.viki.bot.MainActivity");
    intent.setFlags(Intent.FLAG_ACTIVITY_REORDER_TO_FRONT|Intent.FLAG_ACTIVITY_NEW_TASK);
    i.putExtra("FromBroacastReceiver",true);
    i.putExtra("AlarmTrigger",AlarmTriggerString);
    context.startActivity(i);

    }
}

protected void onCreate(Bundle savedInstanceState)
{
    super.onCreate(savedInstanceState);
    setContentView(R.layout.activity_main);
    boolean FromReceiver = (boolean)getIntent().getSerializableExtra("FromBroacastReceiver");
    String AlarmTriggerString = (String) getIntent().getSerializableExtra("AlarmTrigger");
    if(AlarmTriggerString != null && FromReceiver != null && FromReceiver == true)
    {
       // do something
    }
}

A: You can simply set flag or any value in Intent that will determine what's your purpose in that class ..
For Ex: For playing sound set a Boolean value to TRUE in Intent and send same over that class using bundle ..
Else
Set that Boolean value to FALSE if starting alarm class from some other class.

redpajama_set_name: RedPajamaStackExchange


text:
package jsettlers.mapcreator.tools;

import java.util.Set;

import jsettlers.common.position.ShortPoint2D;
import jsettlers.mapcreator.data.MapData;
import jsettlers.mapcreator.tools.shapes.EShapeType;
import jsettlers.mapcreator.tools.shapes.ShapeType;

/**
 * Interface for all tools, displayed in the tree
 *
 * @author Andreas Butti
 *
 */
public interface Tool extends ToolNode {

	/**
	 * Return a Set with all supported shape types
	 *
	 * @return Read only list
	 */
	public Set<EShapeType> getSupportedShapes();

	/**
	 * Editing
	 *
	 * @param map
	 * @param shape
	 * @param start
	 * @param end
	 * @param uidx
	 */
	public void apply(MapData map, ShapeType shape, ShortPoint2D start, ShortPoint2D end, double uidx);

	/**
	 * Start the editing
	 *
	 * @param data
	 * @param shape
	 * @param pos
	 */
	public void start(MapData data, ShapeType shape, ShortPoint2D pos);
}


text:
Q: How to invoke a command using specific proxy server? Some applications support proxy (http proxy or socks proxy), and some are not.
For browsers, I can specify proxy server in the preferences/options dialog, and other applications may be able to configure proxy servers in config files.
For general purpose, can I invoke a command using a specific proxy? Like following:
$ proxy-exec --type sock5 --server 1.2.3.4:8000 -- wget/ftp ...

I'm using Ubuntu Maverick.
P.S.
In win32, it can be implemented by hijacking the socket dlls, maybe, I'm not familiar with Linux programming, but I guess it's possible in Linux. though.

A: Most Linux commands that access the Internet look in the HTTP_PROXY, FTP_PROXY, and SOCKS_SERVER environment variables for proxy information.  So, to do something like your example, just run:
export SOCKS_SERVER=1.2.3.4:8000
wget http://superuser.com/q/262956

The syntax for HTTP_PROXY and FTP_PROXY is slightly different:
export HTTP_PROXY=http://1.2.3.4:3128/
export FTP_PROXY=ftp://1.2.3.4:25/

The default GNOME desktop environment included with Ubuntu's proxy settings has an Apply System-Wide button, which will automatically set those environment variables for you.  Otherwise, you can add the export lines to your ~/.bashrc file to make them take effect at every login.
Unfortunately, wget doesn't support SOCKS at all.  You can use curl, which is included with Ubuntu, to achieve many things that wget does.  Unfortunately, it doesn't check SOCKS_SERVER, while it does check HTTP_PROXY (as does wget).  To use curl to download this page with a SOCKS5 server (performing DNS resolution with that server) and save it as superuser.html, run this:
curl --socks5-hostname 1.2.3.4:8000 http://superuser.com/q/262956 > superuser.html

If you want to make curl always use that SOCKS proxy, you could create a shell alias.  Just add the following line to your ~/.bashrc:
alias curl='curl --socks5-hostname 1.2.3.4:8000'

You will need to restart your terminal or run that line as if it were a command for the changes to take effect.

A: Try proxychains.
It can be installed with apt-get. Then you'll need to create a config file in either of
1) ./proxychains.conf
2) $(HOME)/.proxychains/proxychains.conf
3) /etc/proxychains.conf **

and you'll be able to invoke another commands like proxychains wget google.com - the connections will go through proxy. You can specify multiple proxies used at once or in random order.
For example:
➜  ssh -ND 4000 sockshost &
[1] 3446
➜  wget whoer.net -q -O- | grep remote_addr
89.71.*.*
➜  cat proxychains.conf
[ProxyList]
socks5 127.0.0.1 4000
➜  proxychains wget whoer.net -q -O- | grep remote_addr
|D-chain|-<>-127.0.0.1:4000-<><>-95.211.121.18:80-<><>-OK
78.98.*.*

I stripped some HTML tags and IPs, but as you can see the proxy was used and the IP address did change.

A: wget does not support socks, curl works as Patches said:
curl --socks5-hostname 1.2.3.4:8000 https://superuser.com/q/262956/66003

If you need wget you can install tsocks.
Install sudo aptitude install tsocks and setup:
$ sudo vim /etc/tsocks.conf
server = 1.2.3.4
server_type = 5
server_port = 8000

Usage:
tsocks wget https://superuser.com/q/262956/66003


Today Gabriel 'eibriel' Caraballo arrived in the studio. In the past years he's worked as lead TD for the Kiribati film project in Argentina, responsible for the pipeline, asset/project software, and making sure Blender fits into the overall production well.
Gabriel will be working for two months with Francesco on our own pipeline, especially making sure things work smoothly in the Blender Cloud, so we can collaborate with external artists, better plan and manage the project, and give every Gooseberry supporter a great overview and download access to everything we do.
Awesome! Eibriel it's very clever, and humble firefighting guy! he built from 0 the our puzzle and volatile pipeline in Kiribati's project. He with the blender's talented artists and developers I'm sure it will end building and outstanding solid and smooth pipeline. Really glad for him! a pleasure to work with him.
Hey Eibriel, wow!, suddenly you appear in the Blender Institute! you didn't tell me anything about this! haha, congratulations!!, I hope to see you here again in San Luis.
By the way, bring here some Blender's T-Shirt please!, I'll pay for it ;) .
I'll ask Ton for some T-Shirt!!


The next gallery at the museum honours the celebrated automobile designer, Gordon Buehrig, who was responsible for some of the most iconic cars in the United States during a career that lasted some 45 years. Immediately following a stint at Stutz, where he was responsible for the three lightweight boattailed Black Hawk Speedsters raced at LeMans in 1929, he joined Duesenberg Inc. as the in-house body designer in June 1929. He was ultimately responsible for the designs for half of the coachwork that was to adorn the Model J. In addition, he was the designer of the Auburn 851 Speedster and the Cord 810/812. A master of the clay model, Buehrig's gallery shows models used for designing the Cord 810/812, along with tools of the craftsmen, and other highlights of his illustrious career.
In the former Accounting Department room is now to be found the Gallery of Technology, which features some of the interesting technical achievements of the company. In addition to a bare chassis Cord L-29, illustrating the impressive front-wheel drive system, the room is dominated by the rather amazing Duesenberg V-16 engine, designed to be the most powerful aircraft engine available until the end of World War I meant the end of this and other Duesenberg aircraft engine development.
In 1909 Indiana ranked only behind Michigan in terms of automobile manufacturing in the United States and can boast of having had some 350 individual car makers. A fascinating gallery in the museum houses a display entitled "Hoosier Made: World Driven" featuring fine cars from Indiana companies, some more famous than others.
Automobile enthusiasts Baron Jr., Miles, and Sam Collier of New York's Collier Advertising dynasty were instrumental in forming the Airmobile Racing Club of America in the 1930s. This 1932 Auburn Speedster was owned by Sam Collier who nicknamed the car Beelzebub. The vehicle was somewhat modified for racing by adding the small Brooklands windshields, the large tachometer and the copper cooling coil. The vehicle was road raced in Europe in 1933 against smaller cars such as MGs, Bugattis, and Model A Fords. In 1936 Sam raced it at the Cotton carnival Road Race in Memphis where he took top honors for the Touring Class. In 1937, Sam's brother Baron Jr., sped to a second place overall victory in the Climb to the Clouds race held at Mt. Washington.
The final gallery in a tour of the museum is housed in the former Purchasing and Accounting Office and is devoted to early Auburn cars, from 1903 to 1924. The display cars are shown on a nice carpeted area, meant to invoke an upmarket car dealership.
It was following the disappointing sales of 1924 that E.L. Cord was brought in to revive Auburn's fortunes and see led it to profitability until the Depression ended his empire. E.L. Cord's office is found along a corridor lined with pictures from the company racing successes.


Just imagine it: you're awfully late for your highly romantic Valentine's Day date, your boyfriend is already there, waiting for you at the fancy restaurant where he's booked a table for two... what do you do? How about.... speed driving your truck, your love truck there? Don't let your attention get caught by all those pretty little red hearts floating in the air or by the waving big, big, spectacular looking red roses in this dreamland and don't get too surprised to find yourself in the situation of having to roll over some... huge puffs of whipped cream: the Valentine- Day special symbols are... everywhere. Stay focused on the bumpy, challenging track and make sure you don't crash or run out of time before you manage to reach that luxurious restaurant and enjoy your... romantic Valentine's Day dinner!


text:
HomeLatest NewsEgypt Latest NewsEgypt, Israel Agree on $500 Million Fine to End Gas Dispute
Egypt, Israel Agree on $500 Million Fine to End Gas Dispute
June 17, 2019 MEO Staff Egypt Latest News, Israel Latest News
Egypt reached a settlement agreement with state-owned Israel Electric Corp. to pay a reduced fine for halting deliveries of natural gas, ending a dispute that started about seven years ago.
The accord signed June 16 cuts the fine to $500 million from $1.7 billion after reaching "an amicable agreement" out of a "keenness to avail an environment attractive to investment," Egypt's oil ministry said Sunday in an emailed statement.
Israel Electric, the state-owned utility, had sued Egyptian state entities after Egypt broke a contract signed in 2005 to supply the fuel. Israeli officials at the time said the termination could damage peace accords between the two nations.
Egypt ultimately canceled gas exports to Israel in 2012 after a section of a pipeline that connects the two countries was repeatedly attacked by militants and, with its own reserves dwindling, it diverted supplies for domestic use.
The fine will be amortized over 8 1/2 years and the National Bank of Egypt will issue a letter of credit.
Egypt's Gas Deal with Israel
On Feb. 19, a consortium of oil companies led by the U.S.'s Noble Oil and Israel's Delek signed a contract to supply the Egyptian energy company Dolphinus with up to 32 billion cubic meters of Israeli gas over ten years.
The deal jolted people in the Middle East and beyond. The Egyptian public wondered why Egypt, the second-largest natural gas producer in Africa, was importing gas. Even more startling was that the deal came against a backdrop of the recent inauguration of Egypt's huge Zohr gas field. While the leaders of both countries applauded the deal, it caused a public outcry in Egypt.
Egypt has repeatedly declared its intention to become a natural gas hub for Europe. The country is located off the southern shores of the continent, which is one of the largest energy markets in the world. Europe's domestic energy production has been in a steady decline. It is already importing a lot of energy, with increased reliance on imports to come. North Africa is one of the viable options for meeting Europe's gas demand. Despite pipeline and liquid natural gas infrastructure that connects North African gas exporters to European buyers, Russia's Gazprom managed to outmaneuver North African gas exporters in 2017 by supplying the largest share of imports in important markets such as Italy.
Egypt's desire to become a natural gas hub for Europe makes sense. It not only has substantial gas reserves of its own, but sits astride a major transit route for oil and gas shipments from the Persian Gulf to Europe. Natural gas discoveries in the Eastern Mediterranean, coupled with legislation liberalizing Egypt's energy market, are bolstering its gas-hub aspirations. One of the new laws allows foreign companies to use Egypt's import and distribution facilities to trade in natural gas. Rising production from domestic fields and the presence of two largely idle natural gas liquefaction plants at Idku and Damietta will enable Egypt to import gas from Israel and Cyprus, then export it to Europe and Asia.
With rising domestic production and the deployment of renewable and nuclear energy to generate electricity, Egypt could develop a gas surplus this year. The deal with Israel will help it attain its goal of becoming a gas hub. In the short run, it will help it meet its gas demand before the Zohr field starts production in 2019.
Noble and Delek have been struggling to find buyers for their gas in the wake of anti-monopoly proceedings the Israeli government instituted against them. So far, they have managed to find buyers for only part of the production capacity in two fields: Israeli energy companies, the Jordanian Power Company and the Palestinian Power Company. The consortium has been planning to start first-stage production from the Leviathan field in 2019. But it had contracted to sell only half of the first-stage capacity of 5.7 billion cubic meters before the Egyptian deal took place. It was crucial that it contract for the remaining volume before beginning second-stage development.
Natural gas is both an economic and geopolitical commodity. This means that any transnational gas deal contains trappings of geopolitics. There are ongoing maritime disputes over natural gas rich territorial waters between Cyprus and Turkey, as well as between Lebanon and Israel. Although the Israel-Egypt gas deal was signed between companies and not governments, it is hard not to mix business and political interests in cross-border infrastructure projects. This is especially true in a region as tumultuous as the Middle East.
Recent energy discoveries in the eastern Mediterranean basin have certainly brought new dimensions to the geopolitical arena, but in the case of the Israeli-Egyptian gas deal, there are more signs that it's a convergence of business interests between sellers and buyers than it is geopolitics.
As Egypt starves, Sisi stirs horror in Libya and Sudan
Germany Approves €800m Arms Export Deal to Egypt
Libya Latest News
UAE 'optimistic' after Libyan ally 'Haftar' meets PM Sarraj
May 4, 2017 MEO Staff Libya Latest News, Uae Latest News
The United Arab Emirates voiced optimism a political settlement could be reached in Libya after it hosted rare talks on Tuesday between its Libyan ally and the internationally recognized premier. The UAE is, with Egypt, the [ More … ]
Mass hunger strike at al-Aqrab prison over denial of family visits and dire conditions
July 31, 2019 MEO Staff Egypt Latest News
The Egyptian authorities must immediately end cruel and inhumane detention conditions and allow regular family visits at al-Aqrab maximum security prison in Tora where approximately 130 detainees have gone on a mass hunger strike for [ More … ]
Israeli forces detain 9 Palestinians, interrogate children in West Bank raids
January 6, 2017 MEO Staff Israel Latest News, Palestine Latest News
Israeli forces detained at least nine Palestinians across the occupied West Bank during overnight raids carried out between Wednesday and Thursday, and interrogated several Palestinian children, according to Palestinian and Israeli sources. In the West [ More … ]


text:
Home » Review » Movie » The Babadook
By Ananda Dillon @anandawrites on November 28, 2014
A modern horror of a single mother preyed upon by a children's book character.
The feel of a horror film is almost more important than the content. And for all the grit and grime the Eli Roth's of this world have pumped out, there is something truly refreshing in Jennifer Kent's simplistic and intelligent new Australian horror film The Babadook. Even more refreshing is a distinct lack of gore, cheap frights or action-crazed plot. In an age where most horror films are phoned-in re-hashings of tales already told, The Babadook plays with a nostalgia all can relate to, the adolescent and irrational fear of an unknown evil determined to torment for the sake of tormenting, in an original and satisfying way.
In her directorial début, Kent, who also wrote the film, presents the touching tale of a single mother, Amelia (Essie Davis) at her wit's end with her high-strung 6-year old Robbie (Daniel Henshall). Scraping by with her job at an elderly care home and being pulled out often to deal with complaints from her son's school regarding his behavior, her situation is made that much more bleak by the fact that her son is a living reminder of her beloved husband's untimely death as he was driving her to the hospital to give birth when he was killed. Robbie grates at his mother's nerves with constant complaining of monsters and a tendency to build homemade weapons.
One night Robbie picks a new book from his bookshelf for his mother to read him before bed. As Amelia reads the darkly drawn story, a macabre and frightening figure presents itself in the pages: "Whether it's in a word, or in a look, you can't get rid of the Babadook." Robbie rightly freaks out, and Amelia has to soothe him to get him to calm down. Amelia wonders at the book's appearance, but when Robbie claims to start seeing the Babadook at home, in the car, and at school she starts to take the book more seriously, shredding it and throwing it into the trash. When it reappears later, she realizes something more sinister is at hand. She goes to the police, thinking perhaps a stalker is threatening her and Robbie, but the dark signs around her imply she and Robbie are on their own.
Kent's story plays with traditional horror devices of mother-as-protective-hero (à la Poltergeist) and mother-as-threat (à la Carrie), teetering back and forth between both. In this way she challenges the notion that a mother is only as good or as bad as each extreme. Instead Amelia is a refreshingly modern mother. Stressed, under-sexed, lacking sleep and patience and generally trying to raise a child on her own in a world of snobby soccer moms and judgmental school system officials. Like all great horror films, the evil presented represents a part of our own psyches, the kind that feeds off our darkest thoughts, and in this case, Amelia's own misplaced blame for her husband's death. When Robbie pushes his cousin out of a treehouse for poking fun of his fatherless-ness or screeches from the backseat of his car for not getting his way, it's hard not to want to strangle him a bit ourselves.
The Babadook itself is hardly seen—though the pages of the children's book are plenty frightening in giving it form, thank you designer/illustrator Alexander Juhasz—but Kent affectively holds tension with excellent sound use and an overall dread that plagues every scene. Even the set design, with all the grey and dark blue walls of their home, plenty of dark corners, provides a cloud of gloom and doom mixed into every scene. One would think this small family could solve a few of their problems with a few coats of brightly colored paint. Instead Amelia begs a doctor for sleeping pills to force her son to sleep and give her the much-needed rest she desires. But in a state of exhaustion Amelia becomes even more vulnerable to the dark thoughts already residing in her, as the Babadook urges her to do what both ultimately want: to kill Robbie.
The Babadook holds more scares than any film all year, but more importantly maintains anxiety throughout its entirety (if you watch at home, we highly recommend lights off and sound way up). Kent taps into the horror genre's ability to provide a platform for women to showcase their psychological versatility. It's not simply woman as victim or monster. And the fear that keeps children from leaving their bed at night suspicious of what lies underneath, or the fear of what lurks in the dark of our closets at night, or the noises that always seem to come from right behind closed doors, these are the fears that power the Babadook, and indeed the dark side of our own imaginations. The film's modern ending doesn't try to neatly soothe our fears, but instead acts as a reminder that darkness never goes away, but can be kept at bay.
The Babadook is available on VOD or in limited theaters today.
The Babadook Movie review
Star Wars: The Force Awakens Debuts Teaser
The teaser trailer for Star Wars: The Force Awakens is finally here.


A Lancaster County resident is urging his city council to put a ban on the distribution of plastic bags.
Could plastic bags soon be banned in central Pennsylvania?
That's the goal of one Lancaster County resident who wants retailers to stop giving out plastic bags to customers, according to reports from Lancaster Online.
On Tuesday, the city council will consider a resolution "to promote and utilitze reusable bags" to reduce the use of disposable plastic ones.
Randolph Hernandez, the man who proposed the resolution, provided the council with a list of 10 businesses and five environmental groups who support the measure, according to LNP.
Lancaster isn't the only city pursuing a bag ban. Philadelphia Mayor Jim Kenney passed an executive order last year to move toward a bag ban, as previously reported by PennLive.
Americans use 100 billion plastic bags a year, according to the Center for Biological Diversity. And in the oceans, plastic debris kills an estimated 100,000 marine animals a year, according to the Earth Resource Foundation.
California was the first state in 2014 to enact a ban on single-use plastic bags at large retail stores, and it was approved by voters in 2016. Other cities with plastic bag bans include Chicago, Boston, Seattle, New York, and Washington, D.C.
To learn more about the local resolution, read the Lancaster Online report here.
Also of interest, here's a look at where your recyclables end up.


Breast Health Tip– Get enough Sleep!
As September rolls in, everyone's schedules start to fall back into place. Summer is fun but it's usually filled with a lot of events, activities, and vacations that change your usual schedule.
I love September. It might be the mentality of 'going back to school' but I always feel like it's a new beginning and a great time to start new habits. It is also a time where I get back into my usual sleeping schedule.
Proper sleep is just as important as nutrition and exercise! But many of us are not getting enough of it. Studies show that 40 million Americans suffer from sleep disorders and 60 percent of adults report having sleep problems a few nights a week or more.
Sleep can help with breast cancer prevention! A study published in the National Cancer institute found that nurses that worked the night shift had a 50% increase risk of breast cancer. The reason for this is because of the daily rhythms of the sun and the hormone 'melatonin.' Melatonin is a hormone secreted by the pineal gland in the brain and it helps regulate the body's circadian rhythms.
Melatonin is extremely powerful against and fighting breast cancer if you go to bed early and it's dark.
Stay tuned to learn more about Melatonin and Sleep Cycles!


Send automatic reminders to customers when is time to re-order. Proven to increase sales for goods requiring periodical replacement.
If your product line contains items that need regular replenishment – such as how to sell supplements, replacement parts, pet products, home maintenance, etc – then Time to Reorder is perfect for you!
This additional plugin will allow you to configure reminders that will automatically be sent to your customers notifying them that it's time to reorder their item.
Keep your customers well supplied with their renewable products automatically!
* This App is supported by 3dcart.
Q: Is it possible to set the reminders to automatically send emails and not show the options to the customer to set the reminder or turn off the reminder?
HackerGuardian is a fully configurable vulnerability assessment and reporting service for networks and web servers.
Send extra newsletters from 3dcart!


text:
Average length of stay in hospital in the UK 2010-2017
Published by Conor Stewart, Sep 18, 2019
In the period from 2010 to 2017, the average length of hospital stay for acute care in the United Kingdom (UK) has not changed significantly. In 2010, the average length of stay in hospital was 6.1 days, by 2017 it was 5.9 days after remaining at six days in intervening years.
High amount of admissions to hospital
There were almost 1.4 million admissions to hospital between January and March 2018 in England. This quarterly figure of admissions has remained fairly consistent since 2014. The busiest hospital trust in England by admissions in the year 2017/18 was the Manchester University Hospitals Foundation Trust with almost 305 thousand admissions.
Situation in Accident and Emergency
In the third quarter of 2017/18, A&E in England received over six million attendees. The number of attendances has been creeping upwards since 2012. 6.7 percent of people attending A&E in the last year were diagnosed with a dislocation, fracture, joint injury or amputation, followed by 6.2 percent with a respiratory condition.
Average length of hospital stay for acute care in the United Kingdom (UK) from 2010 to 2017* (in days)
Average length of stay in days
* Excludes cases of childbirth without complications.
Hospitals in the United Kingdom
Leading busiest hospitals in England 2018/19, by number of admissions
Accident and emergency attendances in England 2012/13-2018/19, by gender
Emergency admissions to NHS hospitals in Scotland 2005-2019
Postnatal length of stay in hospitals in England 2018/19
Statistics on "Hospitals and hospital departments in the United Kingdom"
Admissions to NHS hospitals in England, quarterly Q2 2016/17 - Q2 2019/20
Admissions to NHS hospitals in Wales 2004/05-2017/18
Admissions to NHS hospitals in Northern Ireland 2010/11-2018/19
Overall rating of NHS acute hospitals core services in England in 2019, by service
Accident and emergency attendances in England 2018/19, by age
Share of accident and emergency attendances in England 2018/19, by diagnosis
England: emergency calls that received a face to face emergency response 2011-2017
Category A emergency calls resulting in an emergency response in England 2011-2017
Category A emergency calls: ambulance response within 8 minutes in England 2012-2017
Category A emergency calls: ambulance response within 19 minutes in England 2011-2018
Category A emergency calls resulting in an ambulance response in England 2011-2017
Deaths caused by mental disorders in England and Wales 2018, by gender and age
England: detentions after admission to hospital 2009-2019
Detentions under the Mental Health Act 1983 in England 2009-2019
Detentions under the Mental Health Act 1983 in England 2018/19, by age
Psychiatric inpatient admissions in Scotland 2009-2019
Psychiatric inpatient length of stay in Scotland 2018/19
Admissions to mental health hospitals in Northern Ireland 2009-2019
Average length of stay in mental health hospitals in Northern Ireland 2009/10-2018/19
Number of maternal deliveries in NHS hospitals in England 2018/19, by age
Antenatal length of stay in hospitals in England 2018/19
Childbirth: method of delivery in NHS hospitals in England 2018/19
Place of maternity in hospital in England 2018/19
Maternities in National Health Service hospitals in England 2005-2019
Childbirth: person conducting delivery in England 2018/19
Childbirth: method of delivery in NHS hospitals in Scotland 2018/19
England: cancer patients starting treatment within 31 days of decision 2018/19
England: patients starting treatment for cancer within two months of referral 2018/19
Cancer patients: seen by hospital within 3 months of referral in England 2010-2018
Cancer specialist referral as soon as necessary in England 2010-2018
Individuals diagnosed with cancer in Scotland 2013-2017, by treatment type
Patients starting treatment for cancer within two months in Wales 2019
Cancer patients starting treatment within two months in Wales 2016-2019
Hospital care: cancer care as an inpatient in the United Kingdom (UK) 2018
Average length of stay in hospital in Portugal 2010-2017
Average length of stay in hospital in Slovakia 2010-2017
Average length of stay in hospital in Spain 2013-2016
Average length of stay in hospital in Estonia 2010-2017
Average length of stay in hospital in Latvia 2010-2017
Average length of stay in hospital in Hungary 2010-2017
Average length of stay in hospital in Slovenia 2010-2017
Average length of stay in hospital in France 2013-2015
Average length of stay in hospitals in Czechia 2010-2017
Average length of stay in hospitals in Austria 2010-2017
Average length of stay in hospital in Lithuania 2010-2017
Italy: number of hospital admissions 2017, by geographic area
Number of hospital stays in U.S. super-utilizers and other patients by payer 2012
Chronic conditions in hospital stays among U.S. super-utilizers by payer 2012
Mean yearly hospital stays in U.S. super-utilizers and other patients by payer 2012
Leading OR procedures in hospitalizations among U.S. children 2012
Peru: hospitalizations due to genitourinary diseases 2011-2016, by gender
Hospital stays for diagnosis of mood disorders by age and gender
Peru: procedure shares by type 2016
PM10 emissions from plastics products manufacturing in the UK 1990-2017
OECD. (July 2, 2019). Average length of hospital stay for acute care in the United Kingdom (UK) from 2010 to 2017* (in days) [Graph]. In Statista. Retrieved January 17, 2020, from https://www.statista.com/statistics/881260/average-length-of-hospital-stay-in-uk/
OECD. "Average length of hospital stay for acute care in the United Kingdom (UK) from 2010 to 2017* (in days)." Chart. July 2, 2019. Statista. Accessed January 17, 2020. https://www.statista.com/statistics/881260/average-length-of-hospital-stay-in-uk/
OECD. (2019). Average length of hospital stay for acute care in the United Kingdom (UK) from 2010 to 2017* (in days). Statista. Statista Inc.. Accessed: January 17, 2020. https://www.statista.com/statistics/881260/average-length-of-hospital-stay-in-uk/
OECD. "Average Length of Hospital Stay for Acute Care in The United Kingdom (Uk) from 2010 to 2017* (in Days)." Statista, Statista Inc., 2 Jul 2019, https://www.statista.com/statistics/881260/average-length-of-hospital-stay-in-uk/
OECD, Average length of hospital stay for acute care in the United Kingdom (UK) from 2010 to 2017* (in days) Statista, https://www.statista.com/statistics/881260/average-length-of-hospital-stay-in-uk/ (last visited January 17, 2020)


And don't forget to bring a contribution to the festival's food drive, benefiting the Somerville Homeless Coalition!
It's easy-- just bring a can or two of food to the festival.
Suggested donation: $2: You'll get a cool tiger sticker!
Or buy a tiger tee or tote to support the fest!
Rain date: Sunday, August 12 from 6-10pm.
Pikliz International Kitchen, Casa B, Cantina La Mexicana, Union Square Pizza, El Mineirao, Machu Chicken, Tasty Momo, Bao Nation, Siam Ginger, 7ate9 Bakery, In Season, Gracie's Ice Cream, and the Arts Council's Nibble Culinary Entrepreneurs.
Poetry by Tim Hall, magic and more from Jungle Jim, Xuchipili Folkloric Ballet, and performances by Robson Leemos and Violin Viv.
Music by Tarciso Alves Forró Band from 6:30-8:30 PM, a WildEye photobooth, and foodcourt seating.
The Somerville Flea is curating a mini artisan market - check out vintage goods and handmade items!
Intercambio presents Global Warming, magician Bob Filene's "Magic for Smart People," caricatures, face painting, tarot card reading, and much more!
Walk, bike or take public transport if at all possible!
Two travel lanes on Somerville Ave.
between Prospect and Webster, closest to the plaza, will be closed to traffic.
The outside two lanes will accommodate two-way traffic.