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Los códigos y algoritmos en el estudio de fenómenos físicos han sido de gran utilidad, sin embargo, poco ha sido la aplicabilidad en los últimos 20 años desde su aparición al desconocer las bondades y ventajas, además de la robustez y complejidad que implica la manipulación. El objetivo fue revisar, identificar y reconocer la estructura de Enzo, las formulaciones matemáticas base, condiciones de frontera, refinamiento, validación y verificación con énfasis hidrodinámico. De esto se revisaron las aplicaciones que se le han asignado al código en el estudio de procesos cosmológicos y astrofísicos. La evolución ha sido notable, considerando que prioritariamente el equipo original de trabajo que lo desarrollo ha continuado investigando, generando lazos académicos para la conservación y mejora de Enzo. Conocer y divulgar este tipo de códigos puede permitir en un futuro no solo aplicarlo a procesos astrofísicos, sino a climatología e ingeniería.

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 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 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]