Using the TCEV distribution function with systematic and non-systematic data in a regional flood frequency analysis

Due to the social and economic implications, flood frequency analysis must be done with the highest precision. For this reason, the most suitable statistical model must be selected, and the maximum amount of information must be used. Floods in Mediterranean rivers can be produced by two different mechanisms, which forces the use of a non-traditional distribution like the TCEV. The information can be increased by using additional non-systematic data, or with a regional analysis, or both. Through the statistical gain concept, it has been shown that in most cases the use of additional non-systematic information can decrease the quantile estimation error in about 50%. In a regional analysis, the␣benefit of additional information in one station, is propagated to the rest of␣the␣stations with only a small decrease with respect to the at-site equivalent analysis.     

The Evolution of Star-Forming Galaxies: The SFR Density of the Universe

The evolution of the Star Formation Rate (SFR) density of the Universe as a function of look-back time is a fundamental parameter in order to understand the formation and evolution of galaxies. The current picture, only outlined in the last years, is that the global SFR density has dropped by about an order of magnitude from a redshift of z∼1.5 to the current value at z=0. Because these SFR density studies are now extended to the whole range in redshift, it becomes mandatory to combine data from different SFR tracers. At low redshifts, optical emission lines are the most widely used. Using Hα as current-SFR tracer, the Universidad Complutense de Madrid (UCM) Survey provided the first estimation of the global SFR density in the Local Universe. The Hα flux in emission is directly related to the number of ionizing photons and, modulo IMF, to the total mass of stars formed. Metallic lines like [OII]λ3727 and [OIII]λ5007 are affected by metallicity and excitation. Beyond redshifts z∼0.4, Hα is not observable in the optical and [OII]λ3727 or UV luminosities have to be used. The UCM galaxy sample has been used to obtain a calibration between [OII]λ3727 luminosity and SFR specially suitable for the different types of star-forming galaxies found by deep spectroscopic surveys in redshifts up to z∼1.5. These calibrations, when applied to recent deep redshift surveys confirm the drop of the SFR density of the Universe since z∼1 previously infered in the UV. However, the fundamental parameter that determines galactic evolution is mass, not luminosity. The mass function for local star-forming galaxies is critical for any future comparison with other galaxy populations of different evolutionary status. Hα velocity-widths for UCM galaxies indicate that besides a small fraction of 10¹⁰-10¹¹ M_⊙ starburst nuclei spirals, the majority have dynamical masses in the ∼10⁹ M_⊙ range. A comparison with published data for faint blue galaxies suggests that star-forming galaxies at z∼1 would have SFR per unit mass and burst strengths similar to those at z=0, but being intrinsically more massive. This revised version was published online in July 2006 with corrections to the Cover Date.     

Hubble Space Telescope-WFPC2/Hα Observations of the Ejected Nebula M1-67

We present HST-WFPC2/Hα deep images of the ejected nebula M1-67. Our data suggest that M1-67 is the imprint of a previous, slow LBV wind ejected from the central star WR124, now a WN8 star. We find evidence that the LBV wind is highly variableand anisotropic. Some dense, persisting clumps have possibly been ejected directly from the stellar surface. This revised version was published online in July 2006 with corrections to the Cover Date.     

The depositional environment of Mauddud limestone,Greater Burgan oil field,Kuwait

Six microfacies are defined on quantitative petrographic data in a carbonate/clastic sequence from the subsurface, oil producing Mauddud Formation of early Middle Cretaceous age. These are, in descending order of importance and abundance: (1) biomicritic wackestone-packstone, (2) argillaceous mudstone, (3) micritic mudstone, (4) glauconitic sandstone, (5)Orhitolina pelsparitic grainstone, and (6) argillaceous dolomite.Sedimentation took place during a marine transgression onto a very shallow, intertidal, restricted marine shelf lagoons. Facies variations appear to be related to depth and energy changes and proximity to areas of clastic deposition. These changes may have been controlled by slight tectonic events in the hinterland and changes in the rate of basin subsidence.

---

Zusammenfassung Auf der Grundlage quantitativer petrographischer Daten werden sechs Mikrofazies in einer karbonat/klastischen Folge aus der unter der ErdoberflÄche liegenden, ölliefernden Mauddud-Formation der frühen Mittelkreide definiert. In absteigender Reihenfolge der Bedeutung und HÄufigkeit sind dieses: (1) biomikritischer wackestone-packstone, (2) toniger Schlickstein, (3) unkritischer Schlickstein, (4) glaukonitischer Sandstein, (5) Orbitolina-führender pelsparitischer Grainstone und (6) toniger Dolomit.Die Sedimentation erfolgte wÄhrend einer marinen Transgression auf sehr flache, intertidale Lagunen eines begrenzten marinen Schelfs. Die Fazies-Variationen scheinen mit den Wechseln in Wassertiefe und Energie sowie der mit NÄhe von Gebieten mit klastischer Sedimentation zusammenzuhÄngen.Diese Wechsel könnten durch kleinere tektonische Ereignisse im Hinterland und durch VerÄnderungen der Absenkungsrate des Beckens ausgelöst worden sein.

---

Résumé Des données pétrographiques quantitatives permettent de définir six microfacies dans une série clasto-carbonatée d'âge crétacé inférieur du sous-sol de la région pé trolifère de Mauddud. Ce sont par ordre décroissant d'importance et d'abondance: (1) des wacstones-pacstone biomicritiques; (2) des argilites; (3) des argilites micritiques; (4) des grès glauconitiques; (5) des grainstone pelsparitiques à orbitolines; (6) des dolomies argileuses.La sédimentation se produisit au cours d'une transgression marine dans des lagunes très plates, intercotidales, d'une plate-forme continentale de faible étendue. Les variations de facies semblent Être dues à des changements de profondeur et d'énergie, ainsi qu'à la proximité de régions à sédimentation clastique.Ces changements pourraient résulter de légers mouvements tectoniques dans l'arrière-pays et de variations dans le degré de subsidence du bassin de sédimentation.

---

- Mauddud, ( ). : 1) ; 2) ; 3) ; 4) ; 5) , 6) . , . , , , . , .

     

Chromian spinel in the Ivrea-Verbano layered igneous complex,western Alps,Italy

Summary Spinel occurs in the pyroxenitic, peridotitic and gabbroic layers of the Ivrea-Verbano layered igneous complex. Its composition varies between picotite and Mg-hercynite. Maximum Cr₂O₃ contents are found in the spinels of the dunitic cumulitic layers occurring at some height above the base of the complex. Chromium deposits are absent. The lack of chromite and of chromium deposits is attributed to the early fractionation of clinopyroxene (which depleted the residual liquid in chromium) instead of olivine, as a consequence of the relatively high pressure prevailing during crystallization (8 kb). The relationships betweenfO₂-composition of spinel-composition of the silicate phases indicate thatfO₂ exerted a major control on the internal stratigraphy of the single layers and on the pattern of fractionation. The variation offO₂ are on their turn related to accidental variations of the pressure acting on the magma.It is finally suggested that chromium deposits are limited to low pressure layered intrusions, where the magma has been emplaced rapidly into a shallow magma chamber. No chromium concentration is to be expected in those complexes that crystallized into deep-seated magma chambers and that fractionated at relatively high pressure, not markedly different from that at which the magma was produced. One of the major controls on the presence of chromium deposits results, therefore, to be the geotectonic environment of intrusion.

---

Chrom-Spinell im geschichteten vulkanischen Komplex von Ivrea-Verbano, Westalpen, Italien

Zusammenfassung Für die Spinelle der Pyroxenit-, Peridotit- und Gabbro-Lagen des Ivrea-Verbano-Intrusivkomplexes wurde eine Zusammensetzung im Bereich Picotit und Mg-Herzynit bestimmt. Die Dunit-Lagen im basalen Anteil des Komplexes führen Spinelie mit Cr₂O₃-Gehalten bis zu 30 Gew-%. Chromerz-Konzentrationen fehlen jedoch, was auf die fraktionierte Kristallisation von Klinopyroxen (und Entstehung Cr-Restschmelzen) an Stelle von Olivin, als Folge der bei relativ hohem Druck (8 kbar) erfolgten Intrusion, zurückzuführen ist. Die Beziehungen zwischen Sauerstoffpartialdruck und Spinell- und Silikat-Zusammensetzung zeigen den bedeutendenfO₂-Einfluß auf den stratigraphischen Aufbau der einzelnen Gesteinslagen und auf die fraktionierenden Kristallisationsvorgänge. Die schwankendenfO₂-Werter stehen in Zusammenhang mit den ebenfalls variierenden auf das Magma wirkenden Drücken.Es ist anzunehmen, daß Chromerzkonzentrationen nur in geschichteten Intrusivkomplexen vorkommen, die sich unter niederem Druck bzw. in einer oberflächennahen Magma-Kammer bildeten, und nicht in jenen, die tiefer intrudierten und bei hohem Druck kristallisierten. Von großer Bedeutung für die Bildung von Chromerzlagerstätten ist also das geotektonische Milieu der Intrusion.

---

---

With 7 Figures