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We present the kinematic results for the supernova remnant (SNR) CTB 1, obtained with the PUMA equipment of the 2.1-m telescope at San Pedro Mártir National Astronomical Observatory, Baja California, Mexico. The observations were made on the H α line using a Fabry–Perot interferometer. The kinematics derived from the Fabry–Perot velocity cubes allowed us to estimate a kinematic distance for this SNR. We estimate that CTB1 is about 3.8 kpc from the sun, corresponding to a linear diameter of 19 pc, with an expansion velocity of |$286 \rm ~ km ~s^{-1}$|⁠. Additionally, we analyse the diffuse X-ray emission from CTB 1 using data from the XMM–Newton observatory. From the best fits to the spectrum of southwest and northeast regions, we obtained a hot plasma temperature |$\sim 0.1-0.3 ~\rm keV$| with an overabundance in O and Ne and a lower abundance in Fe, which could be caused by a SNR with a stellar progenitor between 10 to |$70 \, \rm {\rm M}_{\odot }$|⁠. The initial energy of the supernova explosion is estimated between (0.6–1.0) × 1050 erg for soft X-ray emission. The X-ray emission also presents a non-thermal component of low surface brightness in the hard X-ray band. Images in radio and X-ray emission allow us to classify CTB 1 as mixed-morphology supernova type. The evolution models show that the cloudy ISM model is the only one that reproduces the mixed morphology type observed in the SNR CTB 1. [ABSTRACT FROM AUTHOR]

We study the kinematics of the western optical filament of the radio shell W50 with imaging Fabry–Perot spectroscopy using the [S  ii ] (λ6717 Å and λ6731 Å) line doublet. The high [S  ii ]/H α line ratio of this filament, as well as the complexity of the radial velocity profiles obtained in this work ensure that this filament and diffuse regions are the optical counterpart of W50 hosting the peculiar object SS 433. We derive a kinematical distance of 4.7 ± 0.5 kpc, validating a previously derived distance based on the assumption that H i or CO gas is associated with W50. Our distance estimate is in agreement with the distance to SS 433 derived from proper motions. Shock velocities of up to 120 km s−1 are estimated for the [S  ii ] emitting regions. We derive an age between 1.0 and 1.9 × 105 yr considering that W50 is a remnant of a supernova explosion or a bubble blown by the action of the jets of the central SS 433 source, respectively. Age values are compatible with the age of SS 433. We also estimate the energy deposited by the supernova in the interstellar medium and alternatively, the luminosity of a wind-blown bubble fed by the relativistic jets of SS 433, obtaining reasonable values. We examine the different scenarios for the formation of W50. We conclude that a supernova remnant scenario rejuvenated by the interaction of SS 433 jets, acting as a piston, evolving in a three-phase medium with photo-evaporation, describes better the different observations and theoretical models of this system. [ABSTRACT FROM AUTHOR]

We present observations in X-ray and optical emission of the supernova remnant (SNR) 0520–69.4 in the Large Magellanic Cloud. Using XMM – Newton observatory data, we produced images of the diffuse X-ray emission and spectra to obtain the X-ray parameters, such as luminosity and temperature, of hot plasma in the SNR. Diffuse X-ray emission with filled-centre morphology goes beyond the Hα region, suggesting that the hot gas escapes through the pores of the Hα shell. We fitted a model that has a plasma temperature of 1.1 × 107 K for an X-ray thermal luminosity of 3.3 × 1035 erg s−1. However, from Hα and [O  iii ] Fabry–Perot observations obtained with the Marseille Hα Survey of the Magellanic Clouds and the Milky Way at La Silla, European Southern Observatory, we are able to obtain physical parameters such as the velocity of the shock induced in the cloudlets emitting at optical wavelengths and the electron density of this gas. With the parameters described above, we test the model proposed by White & Long (1991, ApJ, 373, 543) for explaining the mixed-morphology observed. [ABSTRACT FROM AUTHOR]

We present direct images in the Hα and [S II] λλ6717,6731 Å lines of the Galactic supernova remnant (SNR) G109.1-1.0 (CTB 109). We confirm that the filaments detected are the optical counterpart of the X-ray and radio SNR due to their high [S II]/H α line ratios. We study for the first time the kinematics of the optical counterpart of SNR CTB 109 using the Universidad Nacional Aut´onoma de M´exico scanning Fabry–Perot interferometer PUMA. We estimate a systemic velocity of VLSR = -50 ± 6 km s-1 for this remnant and an expansion velocity of Vexp = 230 ± 5 km s-1. From this velocity and taking into account previous studies of the kinematics of objects at that Galactic longitude, we derive a distance to SNR CTB 109 of 3.1 ± 0.2 kpc, locating it in the Perseus arm. Using the [S II] λ6717/[S II] λ6731 line ratio, we find an electronic density value around ne = 580 cm-3. Considering that this remnant is evolving in a low-density medium with higher-density cloudlets responsible for the optical emission, we determine the age and energy deposited in the ISM by the supernova explosion (E0) in both the Sedov–Taylor phase and the radiative phase. For both cases, the age is thousands of years and E0 is rather typical of SNRs containing simple pulsars, so that the energy released to the ISM cannot be used to distinguish between SNRs hosting typical pulsars from those hosting powerful magnetars, like CTB 109. [ABSTRACT FROM AUTHOR]

The distance of the Galactic supernova remnant (SNR) IC443 (G189.1+3.0, 3C157) is uncertain. Results based on measurements in the optical range from 0.7 to 1.5 kpc, while the assumption that the SNR is associated with the HII region S249 implies a distance of 1.5-2 kpc. We present the kinematics of the north-eastern region of SNR IC443. The results were obtained using a scanning Fabry-Pérot interferometer at the Hα line. The kinematics derived from the Fabry-Pérot velocity cubes enabled us to obtain the kinematic distance to this nebula. We estimate that IC 443 is located about 1.9 kpc from the Sun. IC 443 shows a complex morphology consisting of three interconnected roughly spherical subshells that have substantially different radii and centroids. The geometry is fully constrained by the structural and kinematic data. Two of these subshells together define the usually assumed boundaries of IC443, while the third includes optical filaments that extend beyond the bright north-eastern rim. These filaments have been shown to have well-correlated non-thermal radio counterparts. We present the kinematic results of Hα Fabry-Pérot observations obtained with the PUMA equipment at the 2.1-m telescope of the Observatorio Astronömico Nacional at San Pedro Mártir, Baja California,México. These results enable us to distinguish between the SNR and the HII region S249, both of which are in the line of sight. We find that the HII region is located 0.6 kpc in front of the SNR. [ABSTRACT FROM AUTHOR]

We report the results of a kinematical Ha survey of the Large Magellanic Cloud (LMC) presented in the form of a kinematical and photometric catalogue of 210 H II regions. The observations have been obtained with a scanning Fabry-Perot interferometer that produced data cubes corresponding to 66 different pointings over this galaxy, each with a field of view of 38 arcmin, covering almost the whole extent of the LMC. We find a bimodal distribution of the Hα luminosity of LMC H II regions. We also derive the local star formation and star formation rate (SFR) per unit area of the nebulae, concluding that star formation in the LMC has proceeded until the present time at an average rate of roughly 0.11 M⊙ yr-1. Also, we do not find any correlation between the SFR or ΣSFR with ΔV (full width at half-maximum for a single Gaussian profile and the difference in velocities for multiple-components velocity profiles), the diameter, the distance to the kinematical centre of the LMC and age of the nebulae. Over most of the LMC ΔV appears to be of the order of 30?km?s-1. However, in a few regions the ΔV of the velocity profiles is as large as 50-100 kms-1, corresponding to identified supernova remnants and superbubbles undergoing expansion motions. [ABSTRACT FROM AUTHOR]

This work describes an extensive and eminently observational study, carried out with an Hα filter, of the kinematics of the ionized gas in the large emission region (220 pc) DEM L208 which is located in the south-east part of the Large Magellanic Cloud (LMC). The intention was to establish the region's general kinematic and morphological characteristics, and to analyse its possible association with a larger structure, aiming above all to contribute to the elaboration of a detailed global kinematics image of the LMC. The nebula's edges are well defined, with fairly regular Gaussian profiles, and can be represented by a systemic radial velocity of approximately 250 km s−1 for the brightest area of DEM L208. The radial velocity fields obtained present a main component with a well-defined profile, as well as other weaker components of larger speed, which may be indicative of expansion motion or of another layer of gas. In some regions we find evidence that the disturbance of the medium is due to stellar winds from the interior of the nebula; in others the profiles observed are found to be consistent with very intense stellar winds from Wolf–Rayet stars. [ABSTRACT FROM PUBLISHER]

This paper is the second of a series of papers in which we are exploring the coevolution of galaxies and groups in the local Universe, by adopting a multiwavelength approach. Here, we present the photometric and kinematic characterization of two groups, USGC U268 and USGC U376 (U268 and U376 hereafter), which are located in different regions of the Leo cloud. We revisit the group membership, using results from recent redshift surveys, and we investigate their substructures. U268, which is composed of 10 catalogued members and 11 new added members, has a small fraction (24 per cent) of early-type galaxies (ETGs). U376 has 16 catalogued members plus eight new added members, with 38 per cent of ETGs. We find that there are significant substructures in both groups, which suggests that they are likely to be accreting galaxies. U268 is located in a more loose environment than U376. For each member galaxy, broad-band integrated and surface photometry have been obtained in farultraviolet (FUV) and near-ultraviolet (NUV) with the Galaxy Evolution Explorer (GALEX), and in the u, g, r, i and z (Sloan Digital Sky Survey) bands. Ha imaging and two-dimensional high-resolution kinematical data have been obtained using the scanning Fabry-P'erot interferometer (PUMA) at the 2.12-m telescope at San Pedro M'artir (Baja California, Mexico). We have improved the galaxy classification and we have detected morphological and kinematical distortions that might be connected either to ongoing and/or past interaction/accretion events or to environmental-induced secular evolution. U268 appears to be more active than U376, with a large fraction of galaxies showing interaction signatures (60 per cent versus 13 per cent). The presence of bars among late-type galaxies is 10 percent in U268 and 29 percent in U376. The cumulative distribution of the FUV-NUV colours of galaxies in U268 is significantly different from that in U376, with galaxies in U268 being bluer than those in U376. In the (FUV-r versus Mr) and (NUV-r versus Mr) planes, no members of U268 are found in the red sequence; even ETGs lie in the blue sequence, or in the 'green valley'. Most (i.e. 80 per cent) of the early-type members in U376 inhabit the red sequence. A large fraction of galaxies, of different morphological types, are located in the green valley, while the blue sequence is underpopulated compared with U268. [ABSTRACT FROM AUTHOR]