Star formation activity in the southern Galactic HII region G351.63-1.25

The southern Galactic high mass star-forming region, G351.6-1.3, is a HII region-molecular cloud complex with a luminosity of 2.0 x 10^5 L_sun, located at a distance of 2.4 kpc. In this paper, we focus on the investigation of the associated HII region, embedded cluster and the interstellar medium in the vicinity of G351.6-1.3. We address the identification of exciting source(s) as well as the census of stellar populations. The ionised gas distribution has been mapped using the Giant Metrewave Radio Telescope (GMRT), India at three continuum frequencies: 1280, 610 and 325 MHz. The HII region shows an elongated morphology and the 1280 MHz map comprises six resolved high density regions encompassed by diffuse emission spanning 1.4 pc x 1.0 pc. The zero age main-sequence (ZAMS) spectral type of the brightest radio core is O7.5. We have carried out near-infrared observations in the JHKs bands using the SIRIUS instrument on the 1.4 m Infrared Survey Facility (IRSF) telescope. The near-infrared images reveal the presence of a cluster embedded in nebulous fan-shaped emission. The log-normal slope of the K-band luminosity function of the embedded cluster is found to be 0.27 +- 0.03 and the fraction of the near-infrared excess stars is estimated to be 43%. These indicate that the age of the cluster is consistent with 1 Myr. The champagne flow model from a flat, thin molecular cloud is used to explain the morphology of radio emission with respect to the millimetre cloud and infrared brightness.Comment: 18 pages, 8 figures, To be published in MNRA

Radio and infrared study of the star forming region IRAS 20286+4105

A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 - B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be {\sim} 175 M{\sun} and 30 M{\sun}. The mass-radius relation and the surface density of the clumps do not qualify them as massive star forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located toward the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.Comment: 20 pages, 16 figures, accepted for publication in MNRA

Prospective study comparing the safety and efficacy of totally tubeless percutaneous nephrolithotomy vs standard percutaneous nephrolithotomy

Background: To evaluate the feasibility and safety of totally tubeless percutaneous nephrolithotomy (PCNL) Vs standard PCNL.Methods: From August 2014 to January 2016, 66 patients underwent PCNL in our institute. Of this group, 35 patients underwent traditional nephrostomy drainage following PCNL. A tubeless procedure was performed in the remaining 31 patients. These  groups were compared with respect to age, stone burden, intraoperative events, postoperative pain, analgesic requirements, soakage, postoperative change in hemoglobin, hospitalization time and complication rates.Results: Two groups were comparable with respect to age, stone burden (2.03 cm Vs. 2.12 cm) and intraoperative events. The mean pain score (day2 - 4.95 vs. 2.95) (day3 - 4.33 vs. 1.44) and analgesic requirement (mg diclofenac) (day2 - 140.22 vs. 65.31) (day3 - 124.44 vs. 43.89) was significantly less for group 2 on day 2 and 3. There was significant problem of soakage from nephrostomy tract in group 1. Patients in group 2 returned faster to normal activities but there was no difference found in drop in hemoglobin, complication rates even in subset of patients with large stone burden. No patient required readmission in the follow-up for pain, obstruction or infection in group 2. One patient developed urinoma which resolved conservativelyConclusions: In selected cases totally tubeless PCNL is feasible and safe

Probing the massive star forming environment - a multiwavelength investigation of the filamentary IRDC G333.73+0.37

We present a multiwavelength study of the filamentary infrared dark cloud (IRDC) G333.73+0.37. The region contains two distinct mid-infrared sources S1 and S2 connected by dark lanes of gas and dust. Cold dust emission from the IRDC is detected at seven wavelength bands and we have identified 10 high density clumps in the region. The physical properties of the clumps such as temperature: 14.3-22.3 K and mass: 87-1530 M_sun are determined by fitting a modified blackbody to the spectral energy distribution of each clump between 160 micron and 1.2 mm. The total mass of the IRDC is estimated to be $~4700 M_sun. The molecular line emission towards S1 reveals signatures of protostellar activity. Low frequency radio emission at 1300 and 610 MHz is detected towards S1 (shell-like) and S2 (compact morphology), confirming the presence of newly formed massive stars in the IRDC. Photometric analysis of near and mid-infrared point sources unveil the young stellar object population associated with the cloud. Fragmentation analysis indicates that the filament is supercritical. We observe a velocity gradient along the filament, that is likely to be associated with accretion flows within the filament rather than rotation. Based on various age estimates obtained for objects in different evolutionary stages, we attempt to set a limit to the current age of this cloud.Comment: 26 pages, 20 figures, accepted by Ap

An audit cycle to improve an emergency surgery ambulatory clinic

Marés Deulovol, Frederic; Florensa Ferrer, Adolf;Vilaseca, JosepPla mig de l'escultura de bonze situada a la part inferior de l'Obelisc a Pi i Margall. Mesura 4,19 x 1,21 x 0,70 metres i és de escultura de bronze, obelisc aplacat de granit gris