The european urology residents education programme hands-on training format: 4 years of hands-on training improvements from the European School of Urology

Background: The European School of Urology (ESU) started the European Urology Residents Education Programme (EUREP) in 2003 for final year urology residents, with hands-on training (HOT) added later in 2007. Objective: To assess the geographical reach of EUREP, trainee demographics, and individual quality feedback in relation to annual methodology improvements in HOT. Design, setting, and participants: From September 2014 to October 2017 (four EUREP courses) several new features have been applied to the HOT format of the EUREP course: 1:1 training sessions (2015), fixed 60-min time slots (2016), and standardised teaching methodology (2017). The resulting EUREP HOT format was verified by collecting and prospectively analysing the following data: total number of participants attending different HOT courses; participants’ age; country of origin; and feedback obtained annually. Results and limitations: A total of 796 participants from 54 countries participated in 1450 HOT sessions over the last 4 yr. This included 294 (20%) ureteroscopy (URS) sessions, 237 (16.5%) transurethral resection (TUR) sessions, 840 (58%) basic laparoscopic sessions, and 79 (5.5%) intermediate laparoscopic sessions. While 712 residents (89%) were from Europe, 84 (11%) were from non-European nations. Of the European residents, most came from Italy (16%), Germany (15%), Spain (15%), and Romania (8%). Feedback for the basic laparoscopic session showed a constant improvement in scores over the last 4 yr, with the highest scores achieved last year. This included feedback on improvements in tutor rating (p = 0.017), organisation (p < 0.001), and personal experience with EUREP (p < 0.001). Limitations lie in the difficulties associated with the use of an advanced training curriculum with wet laboratory or cadaveric courses in this format, although these could be performed in other training centres in conjunction with EUREP. Conclusions: The EUREP trainee demographics show that the purpose of the course is being achieved, with excellent feedback reported. While European trainees dominate the demographics, participation from a number of non-European countries suggests continued ESU collaboration with other national societies and wider dissemination of simulation training worldwide.EUREP is supported by educational grant from Olympus.info:eu-repo/semantics/acceptedVersio

MUSE-ALMA Halos V: Physical properties and environment of z < 1.4 HI quasar absorbers

We present results of the MUSE-ALMA Halos, an ongoing study of the Circum-Galactic Medium (CGM) of low redshift galaxies (z < 1.4), currently comprising 14 strong HI absorbers in five quasar fields. We detect 43 galaxies associated with absorbers down to star formation rate (SFR) limits of 0.01-0.1 solar masses/yr, found within impact parameters (b) of 250 kpc from the quasar sightline. Excluding the targeted absorbers, we report a high detection rate of 89 per cent and find that most absorption systems are associated with pairs or groups of galaxies (three to eleven members). We note that galaxies with the smallest impact parameters are not necessarily the closest to the absorbing gas in velocity space. Using a multi-wavelength dataset (UVES/HIRES, HST, MUSE), we combine metal and HI column densities, allowing for derivation of the lower limits of neutral gas metallicity as well as emission line diagnostics (SFR, metallicities) of the ionised gas in the galaxies. We find that groups of associated galaxies follow the canonical relations of N(HI) -- b and W_r(2796) -- b, defining a region in parameter space below which no absorbers are detected. The metallicity of the ISM of associated galaxies, when measured, is higher than the metallicity limits of the absorber. In summary, our findings suggest that the physical properties of the CGM of complex group environments would benefit from associating the kinematics of individual absorbing components with each galaxy member.Comment: Accepted for publication in MNRAS; 23 pages, 25 figure

Optimum speed control for industrial trucks by using the example of van carriers

Portalstapler, auch als Van Carrier oder Straddle Carrier bekannt, werden in großer Stückzahl auf Containerterminals zum Transportieren und Stapeln von Containern eingesetzt. Aufgrund ihrer hohen Schwerpunktlage können diese Fahrzeuge beim schnellen Durchfahren enger Kurven umkippen. In diesem Beitrag wird das Konzept eines Algorithmus zur optimalen Geschwindigkeitsregelung für diese Fahrzeuge und erste Simulationsergebnisse vorgestellt. Der Algorithmus wirkt vorausschauend und soll dafür sorgen, dass das Fahrzeug selbst beim Einlenken aus maximaler Fahrgeschwindigkeit auf den maximalen Lenkwinkel mit maximaler Lenkgeschwindigkeit durch gezielten Bremseingriff stabil bleibt.Van carriers, also known as straddle carriers, are used in large numbers in container terminals for transporting and stacking containers. Due to their high located center of gravity it is possible that they tip over during fast driving around tight curves. In this paper a concept for an algorithm for optimum speed control and first simulation results will be presented. The algorithm looks ahead to ensure that the vehicle remains stable even when turning from maximum driving speed to the maximum steering angle with maximum steering speed by the use of selective brak

ALMACAL VII: First Interferometric Number Counts at 650 μm

Measurements of the cosmic far-infrared background (CIB) indicate that emission from many extragalactic phenomena, including star formation and black hole accretion, in the Universe can be obscured by dust. Resolving the CIB to study the population of galaxies in which this activity takes place is a major goal of submillimetre astronomy. Here, we present interferometric 650휇m submillimetre number counts. Using the Band 8 data from the ALMACAL survey, we have analysed 81 ALMA calibrator fields together covering a total area of 5.5 arcmin2 . The typical central rms in these fields is ∼ 100휇Jy beam−1 with the deepest maps reaching 휎 = 47휇Jy beam−1 at sub-arcsec resolution. Multi-wavelength coverage from ALMACAL allows us to exclude contamination from jets associated with the calibrators. However, residual contamination by jets and lensing remain a possibility. Using a signal-to-noise threshold of 4.5휎, we find 21 dusty, star-forming galaxies with 650휇m flux densities of ≥ 0.7mJy. At the detection limit we resolve ' 100 per cent of the CIB at 650휇m, a significant improvement compared to low resolution studies at similar wavelength. We have therefore identified all the sources contributing to the EBL at 650 microns and predict that the contribution from objects with flux 0.

ALMACAL IV: a catalogue of ALMA calibrator continuum observations

We present a catalogue of ALMA flux density measurements of 754 calibrators observed between 2012 August and 2017 September, for a total of 16263 observations in different bands and epochs. The flux densities were measured by reprocessing the ALMA images generated in the framework of the ALMACAL project, with a new code developed by the Italian node of the European ALMA Regional Centre. A search in the online data bases yielded redshift measurements for 589 sources (∼78 per cent of the total). Almost all sources are flat spectrum, based on their low-frequency spectral index, and have properties consistent with being blazars of different types. To illustrate the properties of the sample, we show the redshift and flux density distributions as well as the distributions of the number of observations of individual sources and of timespans in the source frame for sources observed in bands 3 (84−116 GHz) and 6 (211−275 GHz). As examples of the scientific investigations allowed by the catalogue, we briefly discuss the variability properties of our sources in ALMA bands 3 and 6 and the frequency spectra between the effective frequencies of these bands. We find that the median variability index steadily increases with the source-frame time lag increasing from 100 to 800  d, and that the frequency spectra of BL Lacs are significantly flatter than those of flat-spectrum radio quasars. We also show the global spectral energy distributions of our sources over 17 orders of magnitude in frequency