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The interspecific variation in susceptibility to insecticides by lepidopteran species of soybean [Glycine max L. (Merr.)], cotton (Gossypium hirsutum L.), and maize (Zea mays L.) crops from Brazil were evaluated. Populations of Anticarsia gemmatalis (Hübner) (Lepidoptera: Erebidae), Chrysodeixis includens (Walker), Helicoverpa armigera (Hübner), Spodoptera frugiperda (Smith), Spodoptera eridania (Stoll), Spodoptera cosmioides (Walker), and Spodoptera albula (Walker) (Lepidoptera: Noctuidae) were collected from 2019 to 2021. Early L3 larvae (F2 generation) were exposed to the formulated insecticides methoxyfenozide, indoxacarb, spinetoram, flubendiamide, and chlorfenapyr in diet-overlay bioassays. The median lethal concentrations (LC50) were used to calculate tolerance ratios (TR) of each species in relation to the most susceptible species to each insecticide. The lowest LC50 values were verified for A. gemmatalis to all insecticides tested. Chrysodeixis includens and most of the Spodoptera species were moderately tolerant to methoxyfenozide (TR < 8.0-fold) and indoxacarb (TR < 39.4-fold), whereas H. armigera was the most tolerant species to methoxyfenozide (TR = 21.5-fold), and indoxacarb (TR = 106.4-fold). Spodoptera cosmioides, S. eridania, and S. albula showed highest tolerance to spinetoram (TR > 1270-fold), S. eridania, S. frugiperda, and S. albula to flubendiamide (TR from 38- to 547-fold), and S. albula to indoxacarb (TR = 138.6-fold). A small variation in susceptibility to chlorfenapyr (TR < 4.4-fold) was found among the lepidopteran evaluated. Our findings indicate a large variation in susceptibility to indoxacarb, spinetoram, and flubendiamide and a relatively low variation in susceptibility to methoxyfenozide and chlorfenapyr by lepidopteran species of soybean, cotton, and maize from Brazil.

Not all the light in galaxy groups and clusters comes from stars that are bound to galaxies. A significant fraction of it constitutes the so-called intracluster or diffuse light (ICL), a low surface brightness component of groups/clusters generally found in the surroundings of the brightest cluster galaxies and intermediate/massive satellites. In this review, I will describe the mechanisms responsible for its formation and evolution, considering the large contribution given to the topic in the last decades by both the theoretical and observational sides. Starting from the methods that are commonly used to isolate the ICL, I will address the remarkable problem given by its own definition, which still makes the comparisons among different studies not trivial, to conclude by giving an overview of the most recent works that take advantage of the ICL as a luminous tracer of the dark matter distribution in galaxy groups and clusters., 26 pages, 11 figures, published version uploaded

We improve the model presented in Contini & Gu 2020 that describes the radial mass distribution of brightest cluster galaxies (BCGs) and the diffuse component also known as intra-cluster light (ICL), by assuming that the global BCG+ICL radial mass distribution follows the sum of three profiles: a Jaffe and an exponential profiles for the bulge and disk of the BCG, respectively, and a modified version of an NFW profile for the ICL. We take advantage of a wide sample of BCG+ICL systems simulated with our state-of-art semi-analytic model to: (a) investigate the reliability of our BCG+ICL distribution by looking at several scaling relations between the BCG+ICL stellar mass within different apertures and the total BCG+ICL/halo mass, at different redshift; (b) make a prediction of the distance where the radial distribution transitions from BCG to ICL dominated. We find that our model nicely reproduces all the observed scaling relations investigated at the present time with a compelling degree of precision, but slightly biased-low with respect to observations at higher redshifts ($z\gtrsim 0.5$). The transition radius predicted by our model is in good agreement with recent observational results, and spans a range between $\sim 15$ kpc and $\sim 100$ kpc. It mostly depends on the morphology of the BCG, whether it is bulge or disk dominated, on the amount of ICL with respect to the bulge and/or disk, and on the dynamical state of the group/cluster., 14 pages, 8 figures. Minor corrections after proof, accepted on ApJ

To investigate star-forming activities in early-type galaxies, we select a sample of 52 star-forming S0 galaxies (SFS0s) from the SDSS-IV MaNGA survey. We find that SFS0s have smaller stellar mass compared to normal S0s in MaNGA. After matching the stellar mass to select the control sample, we find that the mean S\'{e}rsic index of SFS0s' bulges (1.76$\pm$0.21) is significantly smaller than that of the control sample (2.57$\pm$0.20), suggesting the existence of a pseudo bulge in SFS0s. After introducing the environmental information, SFS0s show smaller spin parameters in the field than in groups, while the control sample has no obvious difference in different environments, which may suggest different dynamical processes in SFS0s. Furthermore, with derived N/O and O/H abundance ratios, SFS0s in the field show nitrogen enrichment, providing evidence for the accretion of metal-poor gas in the field environment. To study the star formation relation, we show that the slope of the spatially resolved star formation main sequence is nearly 1.0 with MaNGA IFU data, confirming the self-regulation of star formation activities at the kpc scales., Comment: 9 pages, 9 figures, MNRAS accepted

We take advantage of a state-of-art semi analytic model of galaxy formation, and the model presented in \citet{contini21a}, to investigate the mass distribution of Brightest Cluster Galaxies (BCGs) and Intra-Cluster Light (ICL) by addressing two points: (1) the region of transition between a BCG dominated distribution and an ICL dominated one, and; (2) the relation between the total BCG+ICL mass and the ICL one alone. We find the transition radius to be independent of both BCG+ICL and halo masses, with an average of 60$\pm$40 kpc, in good agreement with previous observational measurements, but given the large scatter, it can be considered as a sort of physical separation between the two components only on cluster scale. From the analysis of $M_{ICL}-M_{BCG+ICL}$ relation, we build a method able to extract the ICL mass directly from the knowledge of the BCG+ICL one. Given the large scatter on low mass systems, such method under/overpredicts the true value of the ICL in a significant way, up to a factor of three in the worst cases. On the other hand, for $\log M_{BCG+ICL}>12$ or $\log M_{Halo}>14$, the difference between the true value and the one extracted from the $M_{ICL}-M_{BCG+ICL}$ relation ranges between $\pm$30\%. We therefore suggest this relation as a reliable test for observational works aiming to isolate the ICL from the BCG, for systems hosted by haloes on cluster scale., 12 pages, 2 tables and 5 figures. Accepted for publications in ApJ. Small corrections after proof

We take advantage of an analytic model of galaxy formation coupled to the merger tree of an N-body simulation to study the roles of environment and stellar mass in the quenching of galaxies. The model has been originally set in order to provide the observed evolution of the stellar mass function as well as reasonable predictions of the star formation rate-stellar mass relation, from high redshift to the present time. We analyse the stellar mass and environmental quenching efficiencies and their dependence on stellar mass, halo mass (taken as a proxy for the environment) and redshift. Our analysis shows that the two quenching efficiencies are redshift, stellar and halo mass dependent, and that the halo mass is also a good proxy for the environment. The environmental quenching increases with decreasing redshift and is inefficient below $\log M_* \sim 9.5$, reaches the maximum value at $\log M_* \sim 10.5$, and decreases again, becoming poorly efficient at very high stellar mass ($\log M_* \gtrsim 11.5$). Central and satellites galaxies are mass quenched differently: for the former, the quenching efficiency depends very weakly on redshift, but strongly on stellar mass; for the latter, it strongly depends on both stellar mass and redshift in the range $10\lesssim \log M_* \lesssim 11$. According to the most recent observational results, we find that the two quenching efficiencies are not separable: intermediate mass galaxies are environmental quenched faster, as well as intermediate/massive galaxies in more massive haloes. At stellar masses lower than $\log M_* \lesssim 9.5$ both quenching mechanisms become inefficient, independently of the redshift., 13 pages, 8 figures, accepted for publication in ApJ, minor revision after Proof correction

We take advantage of a semi-analytic model with a state-of-art implementation of the formation of the intra-cluster light (ICL) to study the mass distribution of the ICL in galaxy groups and clusters, at different redshifts. We assume the ICL to follow a NFW profile with a different concentration, linked to that of the dark matter by the relation $c_{ICL}=\gamma c_{DM}$, where the parameter $\gamma$ is set to reproduce the observed relation between the stellar mass in the brightest cluster galaxy (BCG) and ICL in the innermost 100 kpc and the halo mass ($M^*_{100}-M_{500}$), at $z=0$. The model is then tested against several theoretical and observational results, from the present time to $z\sim1.5$. Our analysis shows that the fraction of stellar mass in the BCG and ICL within the innermost 100 kpc is an increasing function of redshift, parameter $\gamma$, and a decreasing function of the halo mass. The value of $\gamma$ required to match the observed $M^*_{100}-M_{500}$ is $\gamma=3$ at $z=0$, but there are hints that it might be a function of redshift and halo mass. This result indicates that the distribution of the ICL is more concentrated than the dark matter one, but less concentrated than previously found by other studies. We suggest that a modified version of the NFW is a good description of the distribution of the diffuse light in groups and clusters, which makes the ICL a reliable tracer of the dark matter, in good agreement with recent observational findings., Comment: 12 pages, 6 figures and 1 table. Accepted for publication in ApJ after some revision

We study the roles of stellar mass and environment in quenching the star formation activity of a large set of simulated galaxies by taking advantage of an analytic model coupled to the merger tree extracted from an N-body simulation. The analytic model has been set to match the evolution of the global stellar mass function since redshift $z\sim 2.3$ and give reasonable predictions of the star formation history of galaxies at the same time. We find that stellar mass and environment play different roles: the star formation rate/specific star formation rate-$M_*$ relations are independent of the environment (defined as the halo mass) at any redshift probed, $01$ as generally claimed, while the environment has a minimal role. All the physical processes linked to the environment must act on very short timescales, such that they do not influence the star formation of active galaxies, but increase the probability of a given galaxy to become quiescent., Comment: 13 pages, 8 figures, accepted for publication in ApJ

To understand the galaxy population in clusters today, we should also consider the impact of previous environments prior to cluster infall, namely preprocessing. We use YZiCS, a hydrodynamic high-resolution zoom-in simulation of 15 clusters, and focus on the tidal stripping suffered by the dark matter halos of cluster members due to preprocessing. We find ~48% of today's cluster members were once satellites of other hosts. This is slightly higher than previous estimates, in part, because we consider not just group-mass hosts, but hosts of all masses also. Thus, we find the preprocessed fraction is poorly correlated with cluster mass and is instead related to each cluster's recent mass growth rate. Hosts less massive than groups are significant contributors, providing more than one-third of the total preprocessed fraction. We find that halo mass loss is a clear function of the time spent in hosts. However, two factors can increase the mass loss rate considerably; the mass ratio of a satellite to its host, and the cosmological epoch when the satellite was hosted. The latter means we may have previously underestimated the role of high redshift groups. From a sample of heavily tidally stripped members in clusters today, nearly three quarters were previously in a host. Thus, visibly disturbed cluster members are more likely to have experienced preprocessing. Being hosted before cluster infall enables cluster members to experience tidal stripping for extended durations compared to direct cluster infall and at earlier epochs when hosts were more destructive., 13 pages, 12 figures, Accepted for publication in ApJ

We study the growth pathways of Brightest Central Galaxies (BCGs) and Intra-Cluster Light (ICL) by means of a semi-analytic model. We assume that the ICL forms by stellar stripping of satellite galaxies and violent processes during mergers, and implement two independent models: (1) one considers both mergers and stellar stripping (named {\small STANDARD} model), and one considers only mergers (named {\small MERGERS} model). We find that BCGs and ICL form, grow and overall evolve at different times and with different timescales, but they show a clear co-evolution after redshift $z \sim 0.7-0.8$. Around 90\% of the ICL from stellar stripping is built-up in the innermost 150 Kpc from the halo centre and the dominant contribution comes from disk-like galaxies (B/T$, Comment: 14 pages, 9 figures. Accepted for publication in MNRAS

We investigate the galaxy population in simulated proto-cluster regions using a semi-analytic model of galaxy formation, coupled to merger trees extracted from N-body simulations. We select the most massive clusters at redshift $z=0$ from our set of simulations, and follow their main progenitors back in time. The analysis shows that proto-cluster regions are dominated by central galaxies and their number decreases with time as many become satellites, clustering around the central object. In agreement with observations, we find an increasing velocity dispersion with cosmic time, the increase being faster for satellites. The analysis shows that proto-clusters are very extended regions, $\gtrsim 20 \, Mpc$ at $z \gtrsim 1$. The fraction of galaxies in proto-cluster regions that are not progenitor of cluster galaxies varies with redshift, stellar mass and area considered. It is about 20-30 per cent for galaxies with stellar mass $\sim 10^9\,{\rm M}_{\sun}$, while negligible for the most massive galaxies considered. Nevertheless, these objects have properties similar to those of progenitors. We investigate the building-up of the passive-sequence in clusters, and find that their progenitors are on average always active at any redshift of interest of proto-clusters. The main mechanism which quenches their star formation is the removal of the hot gas reservoir at the time of accretion. The later galaxies are accreted (become satellite), and the more the cold gas available, the longer the time spent as active. Central galaxies are active over all redshift range considered, although a non-negligible fraction of them become passive at redshift $z, 14 pages, 11 figures, accepted for publication in MNRAS

a b s t r a c t Introduction: Infectious diseases are a significant cause of morbidity and mortality in patients with con- nective tissue diseases. Corticosteroids and immunosuppressive drugs, such as cyclophosphamide (CYC), increase the risk of infections. The objective of this study was to estimate the incidence rates of severe infections in patients who received treatment with CYC. Patients and methods: The records of 60 patients with systemic autoimmune diseases who received treat- ment with CYC were retrospectively reviewed. We evaluated the rate of severe infections that occurred during CYC therapy and the 3 subsequent months. Results: Systemic lupus erythematosus was the most common disease, and diffuse proliferative glomeru- lonephritis the most frequent indication. Severe infection occurred in 9 patients (15%). Community acquired pneumonia was the most frequent infection with 3 cases (33%) followed by Herpes Zoster with 2 reports (22%). The cumulative dose of corticosteroid was the only significant risk factor for infection, 32.8 ± 16.7 vs 20.1 ± 15.3, P=0.007. Conclusion: The use of lower doses of corticosteroids and an aggressive management of infectious com- plications allow for an acceptable safety profile in patients treated with CYC.

Resumen Introduccion Las infecciones son una de las principales causas de morbimortalidad en los pacientes con enfermedades autoinmunes sistemicas. Los corticoides y los inmunosupresores como la ciclofosfamida (CF) son algunos de los factores que se asocian a esta complicacion. El objetivo de este estudio fue determinar el porcentaje de pacientes que presentaron infecciones graves durante el tratamiento con CF y en los 3 meses posteriores. Pacientes y metodos Se realizo un analisis retrospectivo de 60 pacientes con diferentes enfermedades autoinmunes que recibieron tratamiento con CF. Se valoro el porcentaje de infecciones graves. Resultados La patologia mnas comun fue el lupus eritematoso sistemico y la indicacion mas comun fue la glomerulonefritis proliferativa difusa. El 15% de los pacientes presento un episodio infeccioso. Las infecciones mas frecuentes fueron neumonia adquirida en la comunidad en 3 casos y herpes zoster en 2 casos. La dosis acumulada de corticoides fue el unico parametro que se asocio a infecciones 32,8 ± 16,7 vs. 20,1 ± 15,3 p = 0,007. Conclusion Un seguimiento estricto, la utilizacion de corticoides en la menor dosis posible y el tratamiento energico de los procesos infecciosos permiten un perfil de seguridad aceptable en aquellos pacientes tratados con CF.

Many studies confirmed the efficacy and safety of continuous infusion of intrajejunal levodopa/carbidopa gel (CIILG) for advanced Parkinson's disease (PD). Although this treatment is widely used, definite inclusion/exclusion criteria do not exist. In this prospective open-label study, we evaluated the long-term outcome in 28 consecutive patients and sought to detect any predictive factor to identify the best candidates for CIILG therapy. The assessment was carried out routinely at baseline, after 6 months and every year with UPDRS III-IV, FOG Questionnaire, non-motor symptoms scale, PD questionnaire (PDQ-8), cognitive and psychiatric status evaluation (MMSE, FAB, NPI) and caregiver's quality of life. 17/28 patients reached the 24-month follow-up. A statistically significant beneficial effect was shown on motor complications in short- and long-term follow-up, also on axial symptoms like gait disturbances. A concomitant improvement in PDQ8 score was observed, with a parallel mild amelioration, but not significant, on Caregivers QoL. When classified according to their outcome on QoL, the only predictive positive factor was less severe at Neuropsychiatric Inventory (NPI) score at baseline. Considering the improvement in motor scores (duration of "off" period), the more advanced age was associated with a poorer outcome. Our results confirmed a sustained efficacy and safety in long-term follow-up and suggest that younger age at operation and absence or mild presence of psychiatric/behavioural symptoms could be considered valid predicting factors in selecting the best candidates for this efficacious therapy.

We study the formation of the Intra-Cluster Light (ICL) using a semi-analytic model of galaxy formation, coupled to merger trees extracted from N-body simulations of groups and clusters. We assume that the ICL forms by (1) stellar stripping of satellite galaxies and (2) relaxation processes that take place during galaxy mergers. The fraction of ICL in groups and clusters predicted by our models ranges between 10 and 40 per cent, with a large halo-to-halo scatter and no halo mass dependence. We note, however, that our predicted ICL fractions depend on the resolution: for a set of simulations with particle mass one order of magnitude larger than that adopted in the high resolution runs used in our study, we find that the predicted ICL fractions are ~30-40 per cent larger than those found in the high resolution runs. On cluster scale, large part of the scatter is due to a range of dynamical histories, while on smaller scale it is driven by individual accretion events and stripping of very massive satellites, $M_{*} \gtrsim 10^{10.5} M_{\odot}$, that we find to be the major contributors to the ICL. The ICL in our models forms very late (below $z\sim 1$), and a fraction varying between 5 and 25 per cent of it has been accreted during the hierarchical growth of haloes. In agreement with recent observational measurements, we find the ICL to be made of stars covering a relatively large range of metallicity, with the bulk of them being sub-solar., Comment: Accepted for Publication in MNRAS, 19 pages, 13 figures, 1 table

We study the connection between the observed star formation rate-stellar mass (SFR-$M_*$) relation and the evolution of the stellar mass function (SMF) by means of a subhalo abundance matching technique coupled to merger trees extracted from a N-body simulation. Our approach consist of forcing the model to match the observed SMF at redshift $z \sim 2.3$, and let it evolve down to $z \sim 0.3$ according to a $\tau$ model, an exponentially declining functional form which describes the star formation rate decay of both satellite and central galaxies. In this study, we use three different sets of SMFs: ZFOURGE data from Tomczak et al.; UltraVISTA data from Ilbert et al. and COSMOS data from Davidzon et al. We also build a mock survey combining UltraVISTA with ZFOURGE. Our modelling of quenching timescales is consistent with the evolution of the SMF down to $z \sim 0.3$, with different accuracy depending on the particular survey used for calibration. We tested our model against the observed SMFs at low redshift and it predicts residuals (observation versus model) within $1\sigma$ observed scatter along most of the stellar mass range investigated, and with mean residuals below 0.1 dex in the range $\sim [10^{8.7}-10^{11.7}] M_{\odot}$. We then compare the SFR-$M_*$ relation predicted by the model with the observed one at different redshifts. The predicted SFR-$M_*$ relation underpredicts the median SFR at fixed stellar mass relative to observations at all redshifts. Nevertheless, the shapes are consistent with the observed relations up to intermediate-mass galaxies, followed by a rapid decline for massive galaxies., Comment: 16 pages, accepted for publication in ApJ, minor changes after proof

We study the amount and distribution of dark matter substructures within dark matter haloes, using a large set of high-resolution simulations ranging from group size to cluster size haloes, and carried our within a cosmological model consistent with WMAP 7-year data. In particular, we study how the measured properties of subhaloes vary as a function of the parent halo mass, the physical properties of the parent halo, and redshift. The fraction of halo mass in substructures increases with increasing mass. There is, however, a very large halo-to-halo scatter that can be explained only in part by a range of halo physical properties, e.g. concentration. At given halo mass, less concentrated haloes contain significantly larger fractions of mass in substructures because of the reduced strength of tidal disruption. Most of the substructure mass is located at the outskirts of the parent haloes, in relatively few massive subhaloes. This mass segregation appears to become stronger at increasing redshift, and should reflect into a more significant mass segregation of the galaxy population at different cosmic epochs. When haloes are accreted onto larger structures, their mass is significantly reduced by tidal stripping. Haloes that are more massive at the time of accretion (these should host more luminous galaxies) are brought closer to the centre on shorter time-scales by dynamical friction, and therefore suffer of a more significant stripping. The halo merger rate depends strongly on the environment with substructure in more massive haloes suffering more important mergers than their counterparts residing in less massive systems. This should translate into a different morphological mix for haloes of different mass.

We study colors and metallicities of the Brightest Cluster Galaxies (BCGs) and Intra-Cluster Light (ICL) in galaxy groups and clusters, as predicted by a semi-analytic model of galaxy formation, coupled with a set of high-resolution N-body simulations. The model assumes stellar stripping and violent relaxation processes during galaxy mergers to be the main channels for the formation of the ICL. We find that BCGs are more metal-rich and redder than the ICL, at all redshifts since the ICL starts to form ($z\sim 1$). In good agreement with several observed data, our model predicts negative radial metallicity and color gradients in the BCG+ICL system. By comparing the typical colors of the ICL with those of satellite galaxies, we find that mass and metals in the ICL come from galaxies of different mass, depending on the redshift. Stripping of low mass galaxies, $9, Comment: 12 pages, 6 figures, accepted for publication in ApJ after minor revision

The intra-cluster light (ICL) in observations is usually identified through the surface brightness limit method. In this paper, for the first time we produce the mock images of galaxy groups and clusters using a cosmological hydro- dynamical simulation, to investigate the ICL fraction and focus on its dependence on observational parameters, e.g., the surface brightness limit (SBL), the effects of cosmological redshift dimming, point spread function and CCD pixel size. Detailed analyses suggest that the width of point spread function has a significant effect on the measured ICL fraction, while the relatively small pixel size shows almost no influence. It is found that the measured ICL fraction depends strongly on the SBL. At a fixed SBL and redshift, the measured ICL fraction decreases with increasing halo mass, while with a much faint SBL, it does not depend on halo mass at low redshifts. In our work, the measured ICL fraction shows clear dependence on the cosmological redshift dimming effect. It is found that there are more mass locked in ICL component than light, suggesting that the use of a constant mass-to-light ratio at high surface brightness levels will lead to an underestimate of ICL mass. Furthermore, it is found that the radial profile of ICL shows a characteristic radius which is almost independent of halo mass. The current measurement of ICL from observations has a large dispersion due to different methods, and we emphasize the importance of using the same definition when observational results are compared with the theoretical predictions., Comment: 17 pages, 8 figures, 1 table; accepted for publication in ApJ

The ammonium salt of 6-amino-2-hydroxy-3,5-dinitropyrazine has been synthesised from 2,6-dimethoxy-3,5-dinitropyrazine and its properties (DSC, crystal structure, impact sensitiveness and thermochemical properties) are compared with the analogous benzene derivative, ammonium 3,5-diaminopicrate. 2009 Wiley-VCH Verlag GmbH Co. KGaA, Weinheim.

Whilst measuring the energy of combustion of a series of novel energetic polyphosphazenes which contained both phosphorus and fluorine in varying ratios, the non-ideal aqueous combustion species monofluoro-, difluoro- and hexafluoro-phosphoric acids were observed, in addition to the expected H3PO4 and HF. The same aqueous products were also observed to arise from combustion of physical mixtures of P- and F-containing compounds. A quantitative analytical method based on 19F NMR spectroscopy and Ion Chromatography of the bomb solutions was developed. However, since monofluoro- and difluoro-phosphoric acids are hydrolytically unstable, it was necessary to replace the water normally added to the bomb at the outset of the calorimetric experiments with an aqueous buffer solution to inhibit hydrolysis and hence obtain meaningful analytical data. Despite the relatively low precision ΔcU data obtained with the available adiabatic, static bomb calorimeter, the magnitude of the corrections to standard states account...

We study the connection between the observed star formation rate-stellar mass (SFR-$M_*$) relation and the evolution of the stellar mass function (SMF) by means of a Subhalo Abundance Matching technique coupled to merger trees extracted from a N-body simulation. Our approach, which considers both galaxy mergers and stellar stripping, is to force the model to match the observed SMF at redshift $z>2$, and let it evolve down to the present time according to the observed (SFR-$M_*$) relation. In this study, we use two different sets of SMFs and two SFR-$M_*$ relations: a simple power law and a relation with a mass-dependent slope. Our analysis shows that the evolution of the SMF is more consistent with a SFR-$M_*$ relation with a mass-dependent slope, in agreement with predictions from other models of galaxy evolution and recent observations. In order to fully and realistically describe the evolution of the SMF, both mergers and stellar stripping must be considered, and we find that both have almost equal effects on the evolution of SMF at the massive end. Taking into account the systematic uncertainties in the observed data, the high-mass end of the SMF obtained by considering stellar stripping results in good agreement with recent observational data from the Sloan Digital Sky Survey (SDSS). At $\log M_* < 11.2$, our prediction at z=0.1 is close to \citet{li-white09} data, but the high-mass end ($\log M_* > 11.2$) is in better agreement with \citet{dsouza15} data which account for more massive galaxies., 16 pages, 9 figures. Accepted by ApJ

By means of our own cosmological-hydrodynamical simulation and semi-analytical model we studied galaxy population properties in clusters and groups, spanning over 10 different bands from UV to NIR, and their evolution since redshift z=2. We compare our results in terms of galaxy red/blue fractions and luminous-to-faint ratio (LFR) on the Red Sequence (RS) with recent observational data reaching beyond z=1.5. Different selection criteria were tested in order to retrieve galaxies belonging to the RS: either by their quiescence degree measured from their specific SFR ("Dead Sequence"), or by their position in a colour-colour plane which is also a function of sSFR. In both cases, the colour cut and the limiting magnitude threshold were let evolving with redshift, in order to follow the natural shift of the characteristic luminosity in the LF. We find that the Butcher-Oemler effect is wavelength-dependent, with the fraction of blue galaxies increasing steeper in optical colours than in NIR. Besides, only when applying a lower limit in terms of fixed absolute magnitude, a steep BO effect can be reproduced, while the blue fraction results less evolving when selecting samples by stellar mass or an evolving magnitude limit. We then find that also the RS-LFR behaviour, highly debated in the literature, is strongly dependent on the galaxy selection function: in particular its very mild evolution recovered when measured in terms of stellar mass, is in agreement with values reported for some of the highest redshift confirmed (proto)clusters. As to differences through environments, we find that normal groups and (to a lesser extent) cluster outskirts present the highest values of both star forming fraction and LFR at low z, while fossil groups and cluster cores the lowest: this separation among groups begins after z~0.5, while earlier all group star forming properties are undistinguishable., revised version, A&A accepted (11 pages, 6 figures)

Taking advantage of a high-resolution simulation coupled with a state-of-art semi-analytic model of galaxy formation, we probe the mass segregation of galaxies in groups and clusters, focusing on which physical mechanisms are driving it. We find evidence of mass segregation in groups and clusters up to the virial radius, both looking at the galaxy stellar mass and subhalo mass. The physical mechanism responsible for that is consistent with dynamical friction, a drag-force that brings more massive galaxies faster towards the innermost regions of the halo. At odds with observational results, we do not find the inclusion of low-mass galaxies in the samples, down to stellar mass $M_* = 10^9 \, M_{\odot}$, to change the overall trend shown by intermediate and massive galaxies. Moreover, stellar stripping as well as the growth of galaxies after their accretion, do not contribute either in shaping mass segregation or mixing the radial mass distribution. Beyond the virial radius we find an "anti-mass segregation" in groups that progressively weakens in clusters. The continuous accretion of new objects and recent merger events play a different role depending on the halo mass onto which accreting material is falling., 6 pages, 3 figures, 2 tables. Accepted for publication in MNRAS letters

A well calibrated method to describe the environment of galaxies at all redshifts is essential for the study of structure formation. Such a calibration should include well understood correlations with halo mass, and the possibility to identify galaxies which dominate their potential well (centrals), and their satellites. Focusing on z = 1 and 2 we propose a method of environmental calibration which can be applied to the next generation of low to medium resolution spectroscopic surveys. Using an up-to-date semi-analytic model of galaxy formation, we measure the local density of galaxies in fixed apertures on different scales. There is a clear correlation of density with halo mass for satellite galaxies, while a significant population of low mass centrals is found at high densities in the neighbourhood of massive haloes. In this case the density simply traces the mass of the most massive halo within the aperture. To identify central and satellite galaxies, we apply an observationally motivated stellar mass rank method which is both highly pure and complete, especially in the more massive haloes where such a division is most meaningful. Finally we examine a test case for the recovery of environmental trends: the passive fraction of galaxies and its dependence on stellar and halo mass for centrals and satellites. With careful calibration, observationally defined quantities do a good job of recovering known trends in the model. This result stands even with reduced redshift accuracy, provided the sample is deep enough to preserve a wide dynamic range of density., Comment: 19 pages, 12 figures, accepted for publication in MNRAS

Infectious diseases are a significant cause of morbidity and mortality in patients with connective tissue diseases. Corticosteroids and immunosuppressive drugs, such as cyclophosphamide (CYC), increases the risk of infections. The objective of this study was to estimate the incidence rates of severe infections in patients who received treatment with CYC.The records of 60 patients with systemic autoimmune diseases who received treatment with CYC were retrospectively reviewed. We evaluated the rate of severe infections that occurred during CYC therapy and the 3 subsequent months.Systemic lupus erythematosus was the most common disease, and diffuse proliferative glomerulonephritis the most frequent indication. Severe infection occurred in 9 patients (15%). Community acquired pneumonia was the most frequent infection with 3 cases (33%) followed by Herpes Zoster with 2 reports (22%). The cumulative dose of corticosteroid was the only significant risk factor for infection 32.8±16.7 vs. 20.1±15.3 P=.007.The use of lower doses of corticosteroids and an aggressive management of infectious complications, allows for an acceptable safety profile in patients treated with CYC.

Primary lymphedema is characterized by altered morphological development of lymphatic vessels causing fluid accumulation in interstitial spaces. In familial forms, it is primarily transmitted as a dominant Mendelian trait with heterozygous mutations in genes involved in lymphangiogenesis. We used PCR and direct sequencing to analyze the region of the fms-related tyrosine kinase 4 (FLT4) gene encoding the "tyrosine-kinase domain" and the single exon of the forkhead box C2 (FOXC2) gene in 46 Italian probands with primary lymphedema, 42 of whom had familial forms. We identified 12 mutations in 12 patients (12/46, 26%), six in the FLT4 gene and six in the FOXC2 gene. Most of the mutations (9/12, 75%) were new, and none were identified in 100 healthy subjects or listed in the NCBI dbSNP. A clear relation emerged between genotype and phenotype because 4/5 (80%) probands with onset at birth showed FLT4 mutations and 4/5 (80%) probands without distichiasis and with FOXC2 mutations had an amino-acid substitution outside the forkhead domain. Besides the allelic heterogeneity shown by unique mutations in each proband, the absence of mutations in almost 75% of familial cases of primary lymphedema also suggests genetic heterogeneity.

The pilot investigation on the use of UV as an alternative disinfectant to NaOCI was started in 1992 at Trani (South Italy) municipal wastewater treatment plant (335 m3/h). The results collected after six months continuous operation enabled us to compare UV and NaOCl disinfection effectiveness on the basis of secondary effluent characteristics, quantify photoreactivation effects, evidence possible DBP formation and assess costs.

The observed relationship between stellar mass and effective radius for early type galaxies, pointed out by many authors, is interpreted in the context of Clausius' virial maximum theory. In this view, it is strongly underlined that the key of the above mentioned correlation is owing to the presence of a deep link between cosmology and the existence of the galaxy Fundamental Plane. Then the ultimate meaning is: understanding visible mass - size correlation and/or Fundamental Plane means understanding how galaxies form. The mass - size relationship involves baryon (mainly stellar) mass and its typical dimension related to the light, but it gets memory of the cosmological mass variance at the equivalence epoch. The reason is that the baryonic component virializes by sharing virial energy in about equal amount between baryons and dark matter, this sharing depending, in turn, on the steepness of the dark matter distribution. The general strategy consists in using the two-component tensor virial theorem for determining the virialized baryonic configurations. A King and a Zhao density profile are assumed for the inner baryonic and the outer dark matter component, respectively, at the end of the relaxation phase. All the considerations are restricted to spherical symmetry for simplicity. The effect of changing the dark-to-baryon mass ratio, m, is investigated inside a LambdaCDM scenario. A theoretical mass - size relation is expressed for the baryonic component, which fits fairly well to the data from a recently studied galaxy sample. Finally, the play of intrinsic dispersion on the mass ratio, m, is discussed in the light of the cusp/core problem and some consequences are speculated about the existence of a limit, m_l, expected by the theory., 36 pages, 8 figures (Accepted for publication in New Astronomy)

In the Clausius’ virial maximum theory (TCV) [Secco and Bindoni, NewA 14, 567 (2009)] to explain the galaxy Fundamental Plane (FP) a natural explanation follows about the observed relationship between stellar mass and effective radius, M ∗ − r e , for early type galaxies (ETGs). The key of this correlation lies in the deep link which has to exist between cosmology and the existence of the FP. The general strategy consists in using the two-component tensor virial theorem to describe the virial configuration of the baryonic component of mass M B ≃ M ∗ embedded in a dark matter (DM) halo of mass M D at the end of relaxation phase. In a ΛCDM flat cosmology, starting from variance at equivalence epoch, we derive some preliminary theoretical relationships, M ∗ − r e , which are functions of mass ratio m = M D ∕ M B . They appear to be in agreement with the trends extracted from the data of galaxy sample used by [Tortora et al., MNRAS 396, 1132 (2009)].

The theory of the Clausius’ virial maximum proposed by Secco (2000, 2001, 2005) is based on the existence of a maximum in the Clausius’ Virial potential energy of a baryonic component when it is completely embedded inside a dark matter (DM) halo. When this maximum is reached the baryonic inner component acquires a scale length in its own gravity field due to the induced effect on it from the dark matter gravitation. The existence of this special configuration among the infinity number of those an inner component may assume inside an outer DM halo is able to explain the typical scale relationships observed for the early type galaxies (ETGs) which derive from their lying on the Fundamental Plane (FP). To prove that we model an ETG in the following way: an inner baryonic component of stellar kind built‐up by a King‐model with a cut‐off and a DM halo with a cored power law density profile. The two components, which are gravitationally interacting, settle on virial equilibrium after violent relaxation. The new improved model allows us to understand more deeply the dynamical reason of the FP existence and in particular why it has a tilt. The main puzzle may be also fully understood that is why the FP is degenerated with respect to the initial density perturbation spectrum in a CDM hierarchical clustering cosmological scenario.

Purpose To report a rare case of vitreous haemorrhage and retinal vasculitis secondary to cat scratch disease, caused by Bartonella henselae. Methods A 42-year-old apparently healthy farmer presented with a 5-day history of blurred vision in his right eye. Right visual acuity was 20/25. Slit-lamp examination of the right eye revealed mild vitreous haemorrhage and diffuse retinal haemorrhages in the middle-peripheral retina. The left eye was unremarkable. Fluorescein angiography showed signs of retinal vasculitis in the right eye. The patient owned several cats, but had no history of cat bites or scratches. Results A blood sample taken on the day of admission revealed the presence of IgM (titre=1:40) and IgG (titre=1:80) to B. henselae. Accordingly, the diagnosis of cat-scratch disease was made. The retinal vasculitis resolved after 8 days of therapy with oral azithromycin. Conclusion Apart from neuroretinitis, the ocular complication associated with cat-scratch disease may include vitreous haemorrhage and retinal vasculitis.

Purpose Purpose: The reported incidence of G6PD deficiency in Sardina, Italy, ranges from 10% to 15%. Hemizygous males have totally deficient erythrocytes. Evidence indicates that patients with G6PD deficiency are protected against ischemic heart and cerebrovascular disease, retinal vein occlusion, and nonarteritic anterior ischemic optic neuropathy. The purpose of this study was to assess the incidence of G6PD deficiency in Sardinian men with proliferative diabetic retinopathy (PDR) and ascertain whether G6PD deficiency may have a protective effect against this vascular disorder. Methods Methods: G6PD blood levels were measured in 524 men with PDR. 1262 non-diabetic men undergoing cataract surgery served as controls. The Z test was used to assess differences in G6PD deficiency prevalence rates between groups. The odds ratio (OR) was used to evaluate the association between G6PD deficiency and PDR. Results Results: G6PD deficiency was found in 30 (5.7%) out of 524 patients with PDR and in 107 (8.5%) out of 1262 controls. Differences between PDR patients and controls were statistically significant (Z = 1.99, P

Objetivo: El objetivo del presente trabajo fue establecer si había asociación entre el consumo de agua obtenida de fuentes subterráneas, sólo desinfectada con cloro, y la presencia de protozoos intestinales en una población pediátrica. Población. Se estudiaron cuatro grupos de niños, de cuatro meses a doce años de edad, que compartían similares condiciones socioeconómicas y sanitarias. Los grupos A (n = 34), B (n = 36) y C (n = 45), consumían agua de red proveniente de fuentes subterráneas, sólo tratada con cloro antes de ser distribuida. El grupo control, D (n = 34), consumía agua de fuente superficial con tratamiento de potabilización convencional completo. Material y métodos. En cada grupo se analizó el agua, desde el punto de vista fisicoquímico, bacteriológico y parasitológico y se realizaron cultivos coproparasitológicos seriados a los niños seleccionados. Se realizó, además, una encuesta a los padres. Resultados: Se comprobó contaminación bacteriológica y parasitológica en algunas de las perforaciones que abastecían a los grupos de población A, B y C. Se detectaron quistes u ooquistes de protozoos en los tanques B y C. Los porcentajes de estudios copropa-rasitológicos positivos en los niños residentes en cada grupo fueron: A, 47%; B, 41%; C, 67% y D, 12%. Se obtuvieron diferencias significativas entre A y D (p = 0,0039; OR 5,16 [1,43-19,65]), B y D (p = 0,012; OR 4,14 [1,16-15,62]) y entre C y D (p < 10-5; OR 11,60 [3,35-42,88]). Según los resultados de la encuesta, los cuatro grupos compartían condiciones socio-económico-sanitarias similares. Conclusiones: En las muestras estudiadas, las diferencias relativas existentes entre el grupo control y el resto de los grupos estudiados permitirían inferir que existe un alto riesgo de infección con protozoos intestinales cuando se consume agua contaminada de origen subterráneo que sólo fue clorada antes de su distribución.

Gamma-hydroxbutyric acid is a compound found in mammalian brain that is structurally related to the neurotransmitters gamma-aminobutyric acid and glutamic acid. Gamma-hydroxybutyric acid effects dopaminergic systems in the brain and may be a neurotransmitter. Gamma-hydroxybutyric acid was first reported as a drug of abuse in 1990 and continues to be abused by bodybuilders, participants of “rave” dance parties, and polydrug abusers. Physical dependence can develop after prolonged, high-dose use, and overdoses have been widely reported. Its use in sexual assaults as a “date rape” drug and availability on the internet have recently emerged. Gamma-hydroxybutyric acid has established efficacy as an anesthetic agent, and preliminary evidence supports its utility in the treatment of alcohol dependence, opiate dependence, and narcolepsy.