Introducción. El Placer en la Edad Media: artículos presentados en el 2013 International Medieval Congress, Leeds.

No disponible en català. Vegeu resum en anglèsThe papers in this edition of Mirabilia are derived from presentations at the 2013 Leeds International Medieval Congress (IMC). As a large gathering of scholars, the largest of its kind in Europe, with numerous sessions for short presentations, the IMC has proved an ideal forum for early career scholars. Many a young scholar, from both hemispheres and from every continent, has presented her or his first international paper at Leeds. But it is not only a forum for young scholars. Established academics come every year, presenting new ideas alongside their peers: as can be seen in the following collection

The SAMI Galaxy Survey: the intrinsic shape of kinematically selected galaxies

Using the stellar kinematic maps and ancillary imaging data from the Sydney AAO Multi Integral field (SAMI) Galaxy Survey, the intrinsic shape of kinematically-selected samples of galaxies is inferred. We implement an efficient and optimised algorithm to fit the intrinsic shape of galaxies using an established method to simultaneously invert the distributions of apparent ellipticities and kinematic misalignments. The algorithm output compares favourably with previous studies of the intrinsic shape of galaxies based on imaging alone and our re-analysis of the ATLAS3D data. Our results indicate that most galaxies are oblate axisymmetric. We show empirically that the intrinsic shape of galaxies varies as a function of their rotational support as measured by the "spin" parameter proxy Lambda_Re. In particular, low spin systems have a higher occurrence of triaxiality, while high spin systems are more intrinsically flattened and axisymmetric. The intrinsic shape of galaxies is linked to their formation and merger histories. Galaxies with high spin values have intrinsic shapes consistent with dissipational minor mergers, while the intrinsic shape of low-spin systems is consistent with dissipationless multi-merger assembly histories. This range in assembly histories inferred from intrinsic shapes is broadly consistent with expectations from cosmological simulations.Comment: 15 pages, 11 figures, MNRAS in prin

Classic and modern in the therapy of hepatic hidatid cysts – experience of a general surgery center

Clinica II Chirurgie, Spitalul Județean de Urgențe ”Sf. Spiridon”, Iași UMF ”Gr.T. Popa” Iași, Al XI-lea Congres al Asociației Chirurgilor „Nicolae Anestiadi” din Republica Moldova și cea de-a XXXIII-a Reuniune a Chirurgilor din Moldova „Iacomi-Răzeșu” 27-30 septembrie 2011INTRODUCERE. În ultimii 20 de ani, asistăm la o tendință de afirmare a terapiilor mai puțin invazive pentru pacienții cu chist hidatic hepatic (radiologie intervențională, endoscopie intervențională, puncții eco sau CT-ghidate, tehnici chirurgicale laparoscopice precum şi asocieri ale acestora). SCOP. Ne-am propus o comparație între rezultatele după abordul clasic şi cel minim-invaziv pentru tratamentul echinococozei hepatice. MATERIAL ŞI METODĂ. Au fost analizate retrospectiv 180 cazuri de chist hidatic hepatic operate în Clinica I Chirurgie Iaşi, România în perioada 2004-2010. Au fost selectate pentru analiză următoarele variabile: localizarea chistului, tipul acestuia (conform clasificării propuse de Informal Working Group on Echinococcosis), calea de abord, tehnica chirurgicală, durata evoluției postoperatorii, complicațiile survenite, recidivele şi asocierea chimioterapiei antiparazitare. Pentru analiza statistică s-au folosit testele neparametrice Mann-Whitney U şi Spearman cu pragul de semnificație p<0.05. REZULTATE. Leziunile s-au tratat prin puncție echoghidată (n=6;3.3%); pe cale laparoscopică (n= 48;26.6%) şi abord clasic (n=126;70.1%). Pe cale laparoscopică s-au efectuat: inactivare-aspirație-drenaj şi inactivare-aspirație-perichistectomie parțială. Pe cale clasică s-au practicat: inactivare-aspirație-drenaj, inactivare-aspirație-perichistectomie parțială, perichistectomie ideală, hepatectomie reglată, hepatectomie atipică. Abordul minim-invaziv se corelează semnificativ cu tipul I-II al chisturilor (p=0.016) şi cu localizarea acestora în segmentele II, III şi VI (p=0.001). Durata evoluției postoperatorii a fost semnificativ mai redusă după abordul laparoscopic (p=0.003) comparativ cu cea după intervențiile clasice „minimale” (inactivare-aspirație-drenaj şi inactivare-aspirație-perichistectomie parțială) practicate pentru leziunile tip I-III, dar diferența dintre numărul de zile de îngrijiri după abordul laproscopic vs. chirurgie radicală (perichistectomie ideală, hepatectomie) este nesemnificativă. Nu am întâlnit corelații semnificative între apariția recidivelor/complicațiilor şi tipul de abord. Chimioterapia antiparazitară, instituită în 118 de cazuri (65.5%), se corelează semnificativ cu o rată redusă a recidivelor survenite în 9 cazuri (5%). CONCLUZII. Boala hidatică beneficiază astăzi de o terapie multimodală în care chimioterapia, PAIR-ul, videochirurgia şi chirurgia clasică trebuie să se completeze cât mai fericit şi nu să se excludă. Chiar dacă „pierde din indicații”, chirurgia clasică rămâne „rezerva strategică” în terapia chistului hidatic.INTRODUCTION. In the last 20 years, we noticed an outstanding of less invasive therapy for the patients with hidatid disease (interventional radiology, interventional endoscopy, eco- or CT punctions, laparoscopy and association between these). AIM. We intend to compare the results after classic and laparoscopic approach as treatment for hepatic echinococcosis. METHODS. We analysed 180 cases operated in 1st Surgical Clinic, Iasi, Romania, between 2004-200. We recorded the fallowing parameters: location, type (classification approved by Informal Working Group on Echinococcosis), approaching type, surgical technique, postoperative evolution, complications, recurrences and chemotherapy. We used Mann-Whitney U and Spearman tests (p<0.05).RESULTS. The cases were solved by eco guidance punction (n=6; 3.3%); laparoscopic (n= 48; 26.6%) and classic approach (n=126; 70.1%). Minim invasive approach we did inactivation-suction-drainage and partial perichistectomy. Using open approach we did inactivation-suction-drainage, partial perichistectomy, total perichistectomy and hepatectomy. Laparoscopic treatment has significant correlation with type I-II (p=0.016) located in segments II, III and IV (p=0.001). Postoperative evolution is significant lower for laparoscopic methods (p=0.003) comparing with the „minimal” open techniques used for lesions type I-III. There is no significant differentiation between laparoscopic procedures and open radical surgery (total perichistectomy and hepatectomy). We did not register significant correlations about recurrences and complications. Chemotherapy used in 8 cases is correlated with a low rate of recurrence 9 cases (5%).CONCLUSIONS. Hidatid disease has the benefits of a multimodal therapy. Chemotherapy, PAIR, video surgery and open approach are completing themselves and not excluding each other. Even if classic methods are less frequent used, it remains as a „back up solution” in the therapy of hidatid cyst disease

Galaxy And Mass Assembly (GAMA): bulge-disc decomposition of KiDS data in the nearby Universe

We derive single Sérsic fits and bulge-disc decompositions for 13 096 galaxies at redshifts z \u3c 0.08 in the GAMA II equatorial survey regions in the Kilo-Degree Survey (KiDS) g, r, and i bands. The surface brightness fitting is performed using the Bayesian two-dimensional profile fitting code PROFIT. We fit three models to each galaxy in each band independently with a fully automated Markov chain Monte Carlo analysis: a single Sérsic model, a Sérsic plus exponential and a point source plus exponential. After fitting the galaxies, we perform model selection and flag galaxies for which none of our models are appropriate (mainly mergers/Irregular galaxies). The fit quality is assessed by visual inspections, comparison to previous works, comparison of independent fits of galaxies in the overlap regions between KiDS tiles and bespoke simulations. The latter two are also used for a detailed investigation of systematic error sources. We find that our fit results are robust across various galaxy types and image qualities with minimal biases. Errors given by the MCMC underestimate the true errors typically by factors 2–3. Automated model selection criteria are accurate to \u3e90 per cent role= presentation style= box-sizing: border-box; margin: 0px; padding: 0px; border: 0px; font-variant: inherit; font-stretch: inherit; line-height: normal; font-family: inherit; vertical-align: baseline; display: inline; word-spacing: normal; overflow-wrap: normal; white-space: nowrap; float: none; direction: ltr; max-width: none; max-height: none; min-width: 0px; min-height: 0px; position: relative; \u3e\u3e90 per cent\u3e90 per cent as calibrated by visual inspection of a subsample of galaxies. We also present g−r component colours and the corresponding colour–magnitude diagram, consistent with previous works despite our increased fit flexibility. Such reliable structural parameters for the components of a diverse sample of galaxies across multiple bands will be integral to various studies of galaxy properties and evolution. All results are integrated into the GAMA database

Jarlmanns saga og Hermanns: A Translation

Agnete Lothʼs edition of the longer version of Jarlmanns saga og Hermanns included an accompanying English paraphrase (by Gillian Fellows Jensen), but there has never been a full translation into English, much less of the shorter version as edited by Hugo Rydberg. We rectify that omission here, providing a normalized text of Rydbergʼs edition with an English translation alongside in the hopes of making this entertaining saga more accessible to a wider audience

Round robin testing initiative for fiber reinforced polymer (FRP) reinforcement

An international Round Robin Testing (RRT) programme on FRP reinforcement was conducted within the framework of the Marie Curie Research Training Network, ENCORE, and with the support of Task Group 9.3 of the International Federation for Structural Concrete (fib). Eleven laboratories and six manufacturers and suppliers participated in this exercise. As part of this extensive experimental endeavour, one or more of the following tests were performed by the participating laboratories: 1) tensile tests on FRP bars and strips; 2) tensile tests on FRP laminates; 3) double bond shear tests on FRP laminates (Externally Bonded Reinforcement, EBR) and FRP bars/strip (Near Surface Mounted reinforcement, NSM). This paper will discusses the results of the RRT initiative, among which the experimental results of bond tests on concrete specimens strengthened with EBR and NSM FRP

The SAMI Galaxy Survey: The role of disc fading and progenitor bias in kinematic transitions

We use comparisons between the Sydney-AAO Multi-object Integral Field Spectrograph (SAMI) Galaxy Survey and equilibrium galaxy models to infer the importance of disc fading in the transition of spirals into lenticular (S0) galaxies. The local S0 population has both higher photometric concentration and lower stellar spin than spiral galaxies of comparable mass and we test whether this separation can be accounted for by passive aging alone. We construct a suite of dynamically self-consistent galaxy models, with a bulge, disc, and halo using the galactics code. The dispersion-dominated bulge is given a uniformly old stellar population, while the disc is given a current star formation rate putting it on the main sequence, followed by sudden instantaneous quenching. We then generate mock observables (r-band images, stellar velocity, and dispersion maps) as a function of time since quenching for a range of bulge/total (B/T) mass ratios. The disc fading leads to a decline in measured spin as the bulge contribution becomes more dominant, and also leads to increased concentration. However, the quantitative changes observed after 5 Gyr of disc fading cannot account for all of the observed difference. We see similar results if we instead subdivide our SAMI Galaxy Survey sample by star formation (relative to the main sequence). We use EAGLE simulations to also take into account progenitor bias, using size evolution to infer quenching time. The EAGLE simulations suggest that the progenitors of current passive galaxies typically have slightly higher spin than present day star-forming disc galaxies of the same mass. As a result, progenitor bias moves the data further from the disc fading model scenario, implying that intrinsic dynamical evolution must be important in the transition from star-forming discs to passive discs

The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies

We use integral-field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence of recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10% of their spectra within the SAMI field of view. These Hd-strong (HDS) galaxies (HDSGs) are rare, making up only similar to 2% (25/1220) of galaxies with stellar mass log(M-*/M-circle dot) &gt; 10. The HDSGs make up a significant fraction of nonpassive cluster galaxies (15%; 17/115) and a smaller fraction (2.0%; 8/387) of the nonpassive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence of star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the HDS signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R(200) of the cluster center and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected phase space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that has entered the central 0.5r(200,3D) cluster region within the last similar to 1 Gyr. In the eight of nine cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram pressure stripping on their first passage through the cluster

Self-consistent bulge/disk/halo galaxy dynamical modeling using integral field kinematics

We introduce a method for modeling disk galaxies designed to take full advantage of data from integral field spectroscopy (IFS). The method fits equilibrium models to simultaneously reproduce the surface brightness, rotation, and velocity dispersion profiles of a galaxy. The models are fully self-consistent 6D distribution functions for a galaxy with a Sérsic profile stellar bulge, exponential disk, and parametric dark-matter halo, generated by an updated version of GalactICS. By creating realistic flux-weighted maps of the kinematic moments (flux, mean velocity, and dispersion), we simultaneously fit photometric and spectroscopic data using both maximum-likelihood and Bayesian (MCMC) techniques. We apply the method to a GAMA spiral galaxy (G79635) with kinematics from the SAMI Galaxy Survey and deep g- and r-band photometry from the VST-KiDS survey, comparing parameter constraints with those from traditional 2D bulge–disk decomposition. Our method returns broadly consistent results for shared parameters while constraining the mass-to-light ratios of stellar components and reproducing the H i-inferred circular velocity well beyond the limits of the SAMI data. Although the method is tailored for fitting integral field kinematic data, it can use other dynamical constraints like central fiber dispersions and H i circular velocities, and is well-suited for modeling galaxies with a combination of deep imaging and H i and/or optical spectra (resolved or otherwise). Our implementation (MagRite) is computationally efficient and can generate well-resolved models and kinematic maps in under a minute on modern processors.Publisher PDFPeer reviewe