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Background/Objectives: The pathogenesis of enteritis after abdominal radiotherapy (RT) is unknown, although changes in fecal microbiota may be involved. Prebiotics stimulate the proliferation of Lactobacillus spp and Bifidobacterium spp, and this may have positive effects on the intestinal mucosa during abdominal RT. Subjects/Methods: We performed a randomized, double-blind, placebo-controlled trial involving patients with gynecological cancer who received abdominal RT after surgery. Patients were randomized to receive prebiotics or placebo. The prebiotic group received a mixture of fiber (50 inulin and 50% fructo-oligosaccharide), and the placebo group received 6 g of maltodextrin twice daily from 1 week before to 3 weeks after RT. The number of bowel movements and stool consistency was recorded daily. Diarrhea was evaluated according to the Common Toxicity Criteria of the National Cancer Institute. Stool consistency was assessed using the 7-point Bristol scale. Patients’ quality-of-life was evaluated at baseline and at completion of RT using the EORTC-QLQ-C30 (European Organization for Research and Treatment of Cancer quality-of-life Questionnaire C30) test. Results: Thirty-eight women with a mean age of 60.3±11.8 years participated in the study. Both groups (prebiotic ( n =20) and placebo (n =18)) were comparable in their baseline characteristics. The number of bowel movements per month increased in both groups during RT. The number of bowel movements per day increased in both groups. The number of days with watery stool (Bristol score 7) was lower in the prebiotic group (3.3±4.4 to 2.2±1.6) than in the placebo group ( P =0.08). With respect to quality-of-life, the symptoms with the highest score in the placebo group were insomnia at baseline and diarrhea toward the end of the treatment. In the prebiotic group, insomnia was the symptom with the highest score at both assessments, although the differences were not statistically significant. Conclusions: Prebiotics can improve the consistency of stools in gynecologic cancer patients on RT. This finding could have important implications in the quality-of-life of these patients during treatment.

Catheter-related infection is the most common complication in patients receiving home parenteral nutrition (HPN). The centers with the greatest experience report rates ranging from 0.5 to 2 infections per 1000 days. According to the latest data from the Spanish Home and Ambulatory Artificial Nutrition Group (NADYA), the rate of infection was 1.2 per 1000 days. Among the most common origins of catheter-related infection is extraluminal spread of microorganisms from the skin to the catheter tip, especially in short-term catheters, and intraluminal spread of microorganisms to contamination of the catheter hub, which is the most frequent cause in tunneled catheters. The microorganisms mostly commonly involved are coagulase-negative Staphylococcus, Staphylococcus aureus, Staphylococcus spp. Given the fact that the patients that receive HPN will frequently require long-term treatment, it is important to attempt to maintain the catheter in place during the infectious episodes. This conservative treatment requires not only the treatment of the sepsis, but sterilization of the catheter to prevent recurrence of the infection. We recommend that patients in whom catheter sepsis is suspected be admitted to the hospital to enable the performance of microbiological diagnosis and initiate antibiotic therapy. In many cases, if the response is good, the antibiotic therapy can be completed in the patient's home. [PUBLICATION ABSTRACT]

The past few years have seen the raise of unmanned aerial vehicles (UAV) in geosciences for generating highly accurate digital elevation models (DEM) at low costs, which promises to be an interesting alternative to satellite data for small river basins. The reliability of UAV-derived topography as input to hydraulic modelling is still under investigation: here, we analyse potentialities and highlight challenges of employing UAV-derived topography in hydraulic modelling in a tropical environment, where weather conditions and remoteness of the study area might affect the quality of the retrieved data. We focused on a stretch of the Limpopo River in Mozambique, where detailed ground survey and airborne data were available. First, we tested and compared topographic data derived by UAV (25 cm), RTK-GPS (50 cm DEM), LiDAR (1 m DEM) and SRTM (30 m DEM); then, we used each DEM as input data to a hydraulic model and compared the performance of each DEM-based model against the LiDAR based model, currently used as benchmark by practitioners in the area. Despite the challenges experienced during the field campaign—and described here—, the degree of accuracy in terrain modelling produced errors in water depth calculations within the tolerances adopted in this typology of studies and comparable in magnitude to the ones obtained from high-precision topography models. This suggests that UAV is a promising source of geometric data even in natural environments with extreme weather conditions.

Partial sequences of the DNA polymerase delta (pold) gene from Taenia saginata-like adult worms were sequenced. Phylogenetic analysis revealed that pold gene sequences were clearly divided into two clades, differing from each other in five to seven nucleotides. There is little doubt that T. saginata and Taenia asiatica were once separated into two distinct taxa as has been concluded in previous studies. On the other hand, most of the adult worms, which were identified as T. asiatica using mitochondrial DNA, were homozygous for an allele that originated from the allele of T. saginata via single nucleotide substitution. These results indicate that most of the adult worms, which had been called T. asiatica, are not actually ‘pure T. asiatica’ but instead originated from the hybridization of ‘pure T. saginata’ and ‘pure T. asiatica’.

The homeodomain (encoded by the homeobox) is the DNA‐binding domain of a large variety of transcriptional regulators involved in controlling cell fate decisions and development. Mutations of homeobox‐containing genes cause several diseases in humans. A variety of missense mutations giving rise to human diseases have been described. These mutations are an excellent model to better understand homeodomain molecular functions. To this end, homeobox missense mutations giving rise to human diseases are reviewed. Seventy‐four independent homeobox mutations have been observed in 17 different genes. In the same genes, 30 missense mutations outside the homeobox have been observed, indicating that the homeodomain is more easily affected by single amino acids changes than the rest of the protein. Most missense mutations have dominant effects. Several data indicate that dominance is mostly due to haploinsufficiency. Among proteins having the homeodomain as the only DNA‐binding domain, three “hot spot” regions can be delineated: 1) at codon encoding for Arg5; 2) at codon encoding for Arg31; and 3) at codons encoding for amino acids of recognition helix. In the latter, mutations at codons encoding for Arg residues at positions 52 and 53 are prevalent. In the recognition helix, Arg residues at positions 52 and 53 establish contacts with phosphates in the DNA backbone. Missense mutations of amino acids that contribute to sequence discrimination (such as those at positions 50 and 54) are present only in a minority of cases. Similar data have been obtained when missense mutations of proteins possessing an additional DNA‐binding domain have been analyzed. The only exception is observed in the POU1F1 (PIT1) homeodomain, in which Arg58 is a “hot spot” for mutations, but is not involved in DNA recognition. Hum Mutat 18:361–374, 2001. © 2001 Wiley‐Liss, Inc.

It is known that massive stars form as result of the fragmentation of molecular clumps. However, what is not clear is whether this fragmentation gives rise to cores massive enough to form directly high-mass stars, or leads to cores of low and intermediate mass that generate massive stars acquiring material from their environment. Detailed studies towards clumps at early stages of star formation are needed to collect observational evidence that shed light on this issue. The infrared-quiet massive clump AGAL G035.1330-00.7450, located at a distance of 2.1 kpc, is a promising object to study both the fragmentation and the star formation activity at early stages. Using millimeter observations of continuum and molecular lines obtained from the Atacama Large Millimeter Array database at Bands 6 and 7, we study the substructure of this source. The angular resolution of the data at Band 7 is about 0\\farcs7, which allow us to resolve structures of about 0.007 pc (\\(\\sim\\)1500 au). We found that the clump harbours four dust cores (C1-C4) with masses below 3 M\\(_{\\odot}\\). Cores C3 and C4 exhibit well collimated, young, and low-mass molecular outflows. C1 and C2 present CH\\(_3\\)CN J=13--12 emission, from which we derive rotational temperatures of about 180 and 100 K, and masses of about 1.4 and 0.9 M\\(_{\\odot}\\), respectively. The moment 1 map of the CH\\(_3\\)CN emission suggests the presence of a rotating disk towards C1, which is confirmed by the CH\\(_3\\)OH and CH\\(_3\\)OCHO (20-19) emissions. On the other hand, CN N=2-1 emission shows a clumpy and filamentary structure that seems to connect all the cores. These filaments might be tracing the remnant gas of the fragmentation processes taking place within the clump, or gas that is being transported towards the cores, which would imply a competitive accretion scenario.

We present a comprehensive physical and chemical study of the fragmentation and star formation activity towards the massive clump AGAL G338.9188+0.5494 harbouring the extended green object EGO 338.92+0.55(b). The presence of an EGO embedded in a massive clump, suggests, at clump scale, that high-mass star formation is occurring. The main goal of this work is to find evidence of such high-mass star formation, but at core scale. Using mm observations of continuum and lines obtained from the ALMA database at Bands 6 and 7, we study the substructure of the massive clump. The angular resolution of the data is about 0.5'', which allow us to resolve structures of about 0.01pc (\\(\\sim\\) 2000 au) at the distance of 4.4 kpc. The continuum emission at 340 GHz reveals that the molecular clump is fragmented in five cores, labeled from C1 to C5. The \\(^{12}\\)CO J=3--2 emission shows the presence of molecular outflows related to three of them. The analysis of the CH\\(_3\\)CN and CH\\(_3\\)CCH emissions suggests temperatures of about 340 and 72~K, respectively, for C1, showing that the methyl cyanide would trace a gas layer closer to the protostar than the methyl acetylene. The obtained mass of core C1 ranges from 3 to 10 M\\(_{\\odot}\\). We found that the discovered molecular outflow arising from core C1 should be the main responsible for the 4.5 \\(\\mu\\)m extended emission. The average mass and energy of such a molecular outflow is about 0.5 M\\(_{\\odot}\\)~and \\(10^{46}\\)~erg, respectively, which suggest that 10 M\\(_{\\odot}\\) is the most likely mass value for core C1. Additionally we found that the region is chemically very rich with several complex molecular species. Particularly, from the analysis of the CN emission we found strong evidence that such a radical is indirectly tracing the molecular outflows, more precisely the border of the cavity walls carved out by such outflows.

The fragmentation of a molecular cloud that leads to the formation of high-mass stars occurs on a hierarchy of different spatial scales. The large molecular clouds harbour massive molecular clumps with massive cores embedded in them. The fragmentation of these cores may determine the initial mass function and the masses of the final stars. Therefore, studying the fragmentation processes in the cores is crucial to understand how massive stars form. The hot molecular core G34-MM1, embedded in IRDC G34.34+00.24 located at a distance of 3.6 kpc, is a promising object to study both the fragmentation and outflow processes. Using data at 93 and 334 GHz obtained from the Atacama Large Millimeter Array (ALMA) database we studied G34-MM1 with great detail. The angular resolution of the data at 334 GHz allowed us to resolve structures of about 0.014 pc (\\(\\sim\\)2900 au). We found evidence of fragmentation towards the molecular hot core G34-MM1 at two different spatial scales. The dust condensation MM1-A (about 0.06 pc in size) harbours three molecular subcores candidates (SC1 through SC3) detected in \\(^{12}\\)CO J=3-2 emission, with typical sizes of about 0.02 pc. From the HCO\\(^+\\) J=1-0 emission, we identify, with better angular resolution than previous observations, two perpendicular molecular outflows arising from MM1-A. We suggest that subcores SC1 and SC2, embedded in MM1-A, harbour the sources responsible of the main and the secondary molecular outflow, respectively. Finally, from the radio continuum emission at 334 GHz, we marginally detected another dust condensation, named MM1-E, from which a young, massive, and energetic molecular outflow arises. The fragmentation of the hot molecular core G34-MM1 at two different spatial scales, together with the presence of multiple molecular outflows associated with it, would support a competitive accretion scenario.

This paper presents a review of ideas that interconnect Astrochemistry and Galactic Dynamics. Since these two areas are vast and not recent, each one has already been covered separately by several reviews. After a general historical introduction, and a needed quick review of processes like the stellar nucleosynthesis which gives the base to understand the interstellar formation of simple chemical compounds (H2, CO, NH3 and H2O), we focus on a number of topics which are at the crossing of the two areas, Dynamics and Astrochemistry. Astrochemistry is a flourishing field which intends to study the presence and formation of molecules as well as the influence of them into the structure, evolution and dynamics of astronomical objects. The progress in the knowledge on the existence of new complex molecules and of their process of formation originates from the observational, experimental and theoretical areas which compose the field. The interfacing areas include star formation, protoplanetary disks, the role of the spiral arms and the chemical abundance gradients in the galactic disk. It often happens that the physical conditions in some regions of the ISM are only revealed by means of molecular observations. To organise a classification of chemical evolution processes, we discuss about how astrochemistry can act in three different contexts: i. the chemistry of the early universe, including external galaxies, ii. star forming regions, and iii. AGB stars and circumstellar envelopes. We mention that our research is stimulated by plans for instruments and projects, such as the on-going LLAMA, which consists in the construction of a 12m sub-mm radio telescope in the Andes. Thus, modern and new facilities can play a key role in new discoveries not only in astrochemistry but also in radio astronomy and related areas. Furthermore, the research of the origin of life is also a stimulating perspective.