We present high angular resolution (0.86'') observations of the kinematics molecular hydrogen in one zones interaction a cloud with Galactic supernova remnant IC 443. This has been done using scanning Fabry-Pérot interferometer at near-IR line 2.12 μm hydrogen. The derived from velocity cubes thus obtained allows us to have better insight into type motions (and thereby shocks) gas smaller scales this zone interaction, taking account complex morphology and knots, diffuse gas, filaments that...

We present scanning Fabry-Perot observations of the planetary nebula NGC 2346 at near-infrared vibrationally excited line H2 S(1) 1–0 2.122 μm. The kinematics matches a model two ellipsoids with an outflow velocity proportional to distance gas from central star and moving radially outward. stronger emission is located in equatorial torus expanding 16 km s-1. It likely that shock between 6 s-1, depending on assumed red giant envelope (0 10 s-1), excites molecular gas. Depending those limiting...

In this paper we describe the FIT\textit{spec} code, a data mining tool for automatic fitting of synthetic stellar spectra. The program uses database 27\,000 {\sc cmfgen} models atmospheres arranged in six-dimensional (6D) space, where each dimension corresponds to one model parameter. From these library 2\,835\,000 spectra were generated covering ultraviolet, optical, and infrared region electromagnetic spectrum. Using adjust effective temperature surface gravity. 6D array also get...

Context. Local Group (LG) analogs (LGAs) are galaxy associations dominated by a few bright spirals reminiscent of the LG. The NGC 3447/NGC 3447A system is member LGG 225 group, nearby LGA. This considered physical pair composed an intermediate-luminosity late-type spiral, 3447 itself, and irregular companion, 3447A, linked faint, short filament matter. A ring-like structure in outskirts has been emphasised Galaxy Evolution Explorer (GALEX) observations. Aims. work aims to contribute study...

We present a detailed kinematic analysis of two selected nebulae in the Local Group irregular galaxy IC 1613. The are S8, only known supernova remnant this galaxy, and S3, Wolf-Rayet nebula associated with WO star galaxy. For S8 we have obtained analyzed its radial velocity field, where found complex profiles that can be fitted by several components. These also show presence high-velocity, low-density gas. From expansion velocity, estimated preshock density, calculated basic parameters...

Abstract We study the kinematics of emission lines that arise from many physical processes in NGC 6153 based upon deep, spatially resolved, high-resolution spectra acquired with UVES spectrograph at European Southern Observatory Very Large Telescope. Our most basic finding is plasma complex, especially its temperature structure. The defines a classic expansion law, outer part expanding fastest (normal nebular plasma). However, permitted O i , C ii N and Ne present constant velocity second...

Aims. We present a database of 43 340 atmospheric models (∼80 000 at the conclusion project) for stars with stellar masses between 9 and 120 M ⊙ , covering region OB main-sequence Wolf-Rayet in Hertzsprung-Russell diagram. Methods. The were calculated using ABACUS I supercomputer atmosphere code CMFGEN. Results. parameter space has six dimensions: effective temperature T eff luminosity L metallicity Z three wind parameters: exponent β terminal velocity V ∞ volume filling factor F cl . For...

We have surveyed the inner 5' of Orion Nebula by means Hα and [N II] Fabry-Perot imaging spectroscopy to present a kinematical study Herbig-Haro objects in nebula. The studied this work are HH 202, 203, 204, 529, 269, other associated features. For 202 we find new features that, because their high velocities (up 100 km s-1), indicate presence an outflow that probably is flow not cataloged previously. could be only part larger outflow. Large internal motions found fainter regions 203-204, as...

ABSTRACT We present the kinematic results for supernova remnant (SNR) CTB 1, obtained with PUMA equipment of 2.1-m telescope at San Pedro Mártir National Astronomical Observatory, Baja California, Mexico. The observations were made on H α line using a Fabry–Perot interferometer. kinematics derived from velocity cubes allowed us to estimate distance this SNR. that CTB1 is about 3.8 kpc sun, corresponding linear diameter 19 pc, an expansion $286 \rm ~ km ~s^{-1}$. Additionally, we analyse...

We present scanning Fabry-Perot observations of HH 311 covering the red [S II] lines. A study kinematics this region shows a number knots, which appear to be kinematically associated with 111 outflow. also detect diffuse emission, appears light from knots that is scattered on dust in surrounding environment. comparison line widths previously measured proper motions leads us conclude moving into mostly stationary From this, we it likely leading working surface blue lobe outflow and no further...

In this work we report the radial velocity field of molecular hydrogen in five planetary nebulae, obtained from scanning Fabry-Perot interferometer observatins at near-infrared vibrationally excited line H 2 S(1) 1-0 2.122 μm. Direct images nebulae both transitions and 2-1 are used order to discriminate between shocks fluorescence as excitation mechanism . Finally, some physical parameters derived.

ABSTRACT We present observations of the optical and X-ray emission from Galactic supernova remnant W51C. From [S ii] Fabry–Pérot interferometry H α images we detect filaments that are part counterpart remnant. obtain kinematic distance to W51C, showing it is one shortest distances reported in literature. also estimate other physical properties such as velocity shock induced cloudlets emitted at wavelengths electron density those cloudlets. XMM–Newton observatory archival data, diffuse this...

Abstract We present a tool for analysis and fit of stellar spectra using mega database 15,000 atmosphere models OB stars. have developed software tools, which allow us to find the model that best fits an observed spectrum, comparing equivalent widths line ratios in spectrum with all database. use H α , β γ δ lines as criterion gravity He II λ4541/He I λ4471, λ4200/(He I+He λ4026), λ4387, λ4200/He λ4144 T eff .