XI.— Notes on and descriptions of Delias

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Grußwort

In der Reichspogromnacht vom 9. No­vember 1938 wurden 1.400 Synagogen und Beträume, Tausende Wohnun­gen und Geschäfte von Jüdinnen und Juden zerstört und geplündert; mehr mehr als 30.000 Männer in Konzentrationslager verschleppt, un­gefähr hundert wurden ermordet. Dieser vielfach als "Reichskristallnacht" bezeichnete Pogrom, die "Kata­strophe vor der Katastrophe" (Dan Diner), war der Startschuss für die Verdrängung der Juden aus der Wirtschaft und die Arisierung jüdi­schen Eigentums. Er stellte eine Brutalisierung im Umgang mit der jüdischen Bevölkerung dar und war zugleich ein Schritt in Richtung Schoah. Die 75-jährige Wiederkehr der Reichspogromnacht vom 9. auf den 10. No­vember 1938 war für das Landesarchiv Schleswig-Holstein Anlass, dieses Er­eignis im Kontext der jüdischen und der Landes- sowie der nationalsozialis­tischen Gewaltgeschichte erstmals in einer eigenen Ausstellung mit dem Schwerpunkt auf dem Norden Deutschlands zu präsentieren. Die Ausstellung entstand in enger Zusammenarbeit mit der Universität Flensburg und der Landeszentrale für politische Bildung Schleswig-Hol­stein. In Schleswig wurde sie von einer Vortragsreihe begleitet, deren Bei­träge, ergänzt durch weitere Aufsätze, in diesem Band dokumentiert sind. Abbildungen aus der Ausstellung illustrieren die Texte.During the Reichspogromnacht between November 9th and 10th, 1938, in Germany and Austria 1400 synagogues and other Jewish institutions as well as thousands of Jewish homes and shops were destroyed. More than 30.000 men were deported, and at least 100 killed. This pogrom, frequently referred to as „Reichskristallnacht“, marked the beginning of political and economic persecution of Jews in Nazi Germany, and an increasingly brutal treatment of the Jewish minority, thus paving the way for the Holocaust. With regards to the 75th annual recurrence of the Reichspogromnacht, the Landesarchiv Schleswig-Holstein in 2013 presented an exhibition centered around the events of that night in Northern Germany. This exhibition was prepared in close cooperation with the University of Flensburg and the Landeszentrale für politische Bildung Schleswig-Holstein. It was accompanied by a series of lectures that are included in this book as well as some of the illustrations displayed

It Is Not Armed Robbery When Government Takes People's Stuff, It Is Civil Asset Forfeiture

Abstract. Civil asset forfeiture allows the police to profit from crime instead of the criminal by seizing a person’s belongings that were used in illegal activity. The police profit from crime by keeping a percentage of the proceeds they seize. This ends up creating some perverse incentives, such as having more police resources go to seize people’s assets instead of fighting crime. Shifting police efforts away from combating hard crime into fighting so-called “victimless crimes” causes an increase in hard crimes as criminals substitute from soft crimes, such as selling drugs, into hard crimes where the chances of being caught are now lower.Keywords. Theft, Government, Competition.JEL. H0, H10

INTEGRAL observations of V0332+53 in outburst

We present the analysis of a 100ksec Integral(3-100kev) observation of the transient X-ray pulsar V0332+53 inoutburst. The source is pulsating at P=4.3751+/-0.0002s with a clear double pulse from 6 kev to 60 kev. The average flux was ~550mCrab between 20 kev and 60 kev. We modeled the broad band continuum from 5 kev to 100 kev with a power-law modified by an exponential cut off. We observe three cyclotron lines: the fundamental line at 24.9+/-0.1 kev, the first harmonic at 50.5+/-0.1 kev as well as the second harmonic at71.7+/-0.8 kev, thus confirming the discovery of the harmonic lines by Coburn et al. (2005) in RXTE data.Comment: 4 pages, 3 figures. Accepted for publication in A&A Letter

The Orbit of the Eclipsing X-ray Pulsar EXO 1722-363

With recent and archival Rossi X-Ray Timing Explorer (RXTE) X-ray measurements of the heavily obscured X-ray pulsar EXO 1722-363 (IGR J17252-3616), we carried out a pulse timing analysis to determine the orbital solution for the first time. The binary system is characterized by a_x sin(i) = 101 +/- 3 lt-s and P_orb = 9.7403 +/- 0.0004 days (90% confidence), with the precision of the orbital period being obtained by connecting datasets separated by more than 7 years (272 orbital cycles). The orbit is consistent with circular, and e < 0.19 at the 90% confidence level. The mass function is 11.7 +/- 1.2 M_sun and confirms that this source is a High Mass X-ray Binary (HMXB) system. The orbital period, along with the previously known ~414 s pulse period, places this system in the part of the Corbet diagram populated by supergiant wind accretors. Using previous eclipse time measurements by Corbet et al. and our orbital solution, combined with the assumption that the primary underfills its Roche lobe, we find i > 61 degrees at the 99% confidence level, the radius of the primary is between 21 R_sun and 37 R_sun, and its mass is less than about 22 M_sun. The acceptable range of radius and mass shows that the primary is probably a supergiant of spectral type B0I-B5I. Photometric measurements of its likely counterpart are consistent with the spectral type and luminosity if the distance to the system is between 5.3 kpc and 8.7 kpc. Spectral analysis of the pulsar as a function of orbital phase reveals an evolution of the hydrogen column density suggestive of dense filaments of gas in the downstream wake of the pulsar, with higher levels of absorption seen at orbital phases 0.5-1.0, as well as a variable Fe K_alpha line.Comment: Submitted to ApJ, 11 pages, 11 figure

XMM-Newton observation of the long-period polar V1309 Ori: The case for pure blobby accretion

Using XMM-Newton we have obtained the first X-ray observation covering a complete orbit of the longest period polar, V1309 Ori. The X-ray light curve is dominated by a short, bright phase interval with EPIC pn count rates reaching up to 15 cts/sec per 30 sec resolution bin. The bright phase emission is well described by a single blackbody component with kT_bb = (45 +- 3) eV. The absence of a bremsstrahlung component at photon energies above 1 keV yields a flux ratio F_bb/F_br > 6700. This represents the most extreme case of a soft X-ray excess yet observed in an AM Herculis star. The bright, soft X-ray emission is subdivided into a series of individual flare events supporting the hypothesis that the soft X-ray excess in V1309 is caused by accretion of dense blobs. In addition to the bright phase emission, a faint, hard X-ray component is visible throughout the binary orbit with an almost constant count rate of 0.01 cts/sec. Spectral modelling indicates that this emission originates from a complex multi-temperature plasma. At least three components of an optically thin plasma with temperatures kT= 0.065, 0.7, and 2.9 keV are required to fit the observed flux distribution. The faint phase emission is occulted during the optical eclipse. Eclipse ingress lasts about 15--20 min and is substantially prolonged beyond nominal ingress of the white dwarf. This and the comparatively low plasma temperature provide strong evidence that the faint-phase emission is not thermal bremsstrahlung from a post-shock accretion column above the white dwarf. A large fraction of the softer faint-phase emission could be explained by scattering of photons from the blackbody component in the infalling material above the accretion region. The remaining hard X-ray flux could be produced in the coupling region, so far unseen in other polars.Comment: 10 pages, 5 figures, A&A publishe