Tidal dwarf galaxies (TDGs) are gravitationally bound condensations of gas and stars that formed during galaxy interactions. Here we present multi-configuration ALMA observations of J1023+1952, a TDG in the interacting system Arp 94, where we resolved CO(2–1) emission down to giant molecular clouds (GMCs) at 0.6400 ∼ 45 pc resolution. We find a remarkably high fraction of extended molecular emission (∼80−90%), which is filtered out by the interferometer and likely traces diffuse gas. We detect 111 GMCs that give a similar mass spectrum as those in the Milky Way and other nearby galaxies (a truncated power law with a slope of −1.76±0.13). We also study Larson's laws over the available dynamic range of GMC properties (∼2 dex in mass and ∼1 dex in size): GMCs follow the sizemass relation of the Milky Way, but their velocity dispersion is higher such that the size-linewidth and virial relations appear superlinear, deviating from the canonical values. The global molecular-to-atomic gas ratio is very high (∼1) while the CO(2–1)/CO(1–0) ratio is quite low (∼0.5), and both quantities vary from north to south. Star formation predominantly takes place in the south of the TDG, where we observe projected offsets between GMCs and young stellar clusters ranging from ∼50 pc to ∼200 pc; the largest offsets correspond to the oldest knots, as seen in other galaxies. In the quiescent north, we find more molecular clouds and a higher molecular-to-atomic gas ratio (∼1.5); atomic and diffuse molecular gas also have a higher velocity dispersion there. Overall, the organisation of the molecular interstellar medium in this TDG is quite different from other types of galaxies on large scales, but the properties of GMCs seem fairly similar, pointing to near universality of the star-formation process on small scales. ; Instituto de Salud Carlos III Spanish Government PID2019-106027GA-C44 ; Spanish Ministerio de Economia y Competitividad AYA2017-84897-P ; European Commission ; Junta de Andalucia European Commission FQM108 ; European Research Council (ERC) 726384/EMPIRE 714907 ; MCIU/AEI/FEDER,UE PGC2018-094671-B-I00 AYA2016-76682-C3-2-P ; German Research Foundation (DFG) KR4801/1-1 ; German Research Foundation (DFG) KR4801/2-1
Sánchez-Portal, Miguel et. al. ; The cores of clusters at 0 ≲ z ≲ 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type galaxies. Clusters grow through the accretion of galaxies and groups from the surrounding field, which implies that galaxy properties, notably the star formation ability, are altered as they fall into overdense regions. The critical issues for understanding this evolution are how the truncation of star formation is connected to the morphological transformation and what physical mechanism is responsible for these changes. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a thorough study of the variations in galaxy properties (star formation, AGN activity, and morphology) as a function of environment in a representative and well-studied sample of clusters. To address these questions, the GLACE survey is making a deep panoramic survey of emission line galaxies (ELG), mapping a set of optical lines ([O ii], [O iii], Hβ andHα/[N ii] when possible) in several galaxy clusters at z ~ 0.40, 0.63, and 0.86. Using the tunable filters (TF) of the OSIRIS instrument at the 10.4 m GTC telescope, the GLACE survey applies the technique of TF tomography: for each line, a set of images are taken through the OSIRIS TF, each image tuned at a different wavelength (equally spaced), to cover a rest frame velocity range of several thousand km s-1 centred on the mean cluster redshift, and scanned for the full TF field of view of an 8 arcmin diameter. Here we present the first results of the GLACE project, targeting the Hα/[N ii] lines in the intermediate-redshift cluster ZwCl 0024.0+1652 at z = 0.395. Two pointings have been performed that cover ~2 × rvir. We discuss the specific techniques devised to process the TF tomography observations in order to generate the catalogue of cluster Hα emitters, which contains more than 200 sources down to a star formation rate (SFR) ≲1 M⊙/yr. An ancillary broadband catalogue is constructed, allowing us to discriminate line interlopers by means of colour diagnostics. The final catalogue contains 174 unique cluster sources. The AGN population is distinguished using different diagnostics and found to be ~37% of the ELG population. The median SFR of the star-forming population is 1.4 M⊙/yr. We studied the spatial distribution of ELG and confirm the existence of two components in the redshift space. Finally, we exploited the outstanding spectral resolution of the TF, attempting to estimate the cluster mass from ELG dynamics, finding M200 = (4.1 ± 0.2) × 1014 M⊙ h-1, in agreement with previous weak-lensing estimates. ; We acknowledge financial support from Spanish MINECO under grant AYA2014-29517-C03-01, AYA2011-29517-C03-02 and AYA2014-58861-C03. E.J.A. acknowledges support from MINECO under grant AYA2013-40611-P. J.M.R.E. acknowledges support from MINECO under grant AYA2012-39168-C03-01. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). I.R.S. acknowledges support from STFC GT/I001573/1, a European Research Council Advanced Programme Dustygal (321334) and a Royal Society/Wolfson Research Merit Award. J.S.S. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 267251 "Astronomy Fellowships in Italy" (AstroFIt). ; Peer Reviewed
Context. M 33 is a gas rich spiral galaxy of the Local Group. Its vicinity allows us to study its interstellar medium (ISM) on linear scales corresponding to the sizes of individual giant molecular clouds. Aims. We investigate the relationship between the two major gas cooling lines and the total infrared (TIR) dust continuum. Methods. We mapped the emission of gas and dust in M 33 using the far-infrared lines of [C ii] and [O i](63 µm) and the total infrared continuum. The line maps were observed with the PACS spectrometer on board the Herschel Space Observatory. These maps have 50 pc resolution and form a ∼370 pc wide stripe along its major axis covering the sites of bright H ii regions, but also more quiescent arm and inter-arm regions from the southern arm at 2 kpc galacto-centric distance to the south out to 5.7 kpc distance to the north. Full-galaxy maps of the continuum emission at 24 µm from Spitzer/MIPS, and at 70 µm, 100 µm, and 160 µm from Herschel/PACS were combined to obtain a map of the TIR. Results. TIR and [C ii] intensities are correlated over more than two orders of magnitude. The range of TIR translates to a range of far ultraviolet (FUV) emission of G0,obs ∼ 2 to 200 in units of the average Galactic radiation field. The binned [C ii]/TIR ratio drops with rising TIR, with large, but decreasing scatter. The contribution of the cold neutral medium to the [C ii] emission, as estimated from VLA H i data, is on average only 10%. Fits of modified black bodies to the continuum emission were used to estimate dust mass surface densities and total gas column densities. A correction for possible foreground absorption by cold gas was applied to the [O i] data before comparing it with models of photon dominated regions. Most of the ratios of [C ii]/[O i] and ([C ii]+[O i])/TIR are consistent with two model solutions. The median ratios are consistent with one solution at n ∼ 2 × 102 cm−3 , G0 ∼ 60, and a second low-FUV solution at n ∼ 104 cm−3 , G0 ∼ 1.5. Conclusions. The bulk of the gas along the lines-of-sight is represented by a low-density, high-FUV phase with low beam filling factors ∼1. A fraction of the gas may, however, be represented by the second solution. ; Spanish Ministerio de Economia y Competitividad AYA2014-53506-P AYA2017-84897-P ; Junta de Andalucia FQM108 ; Junta de Andalucia ; European Union (EU) SOMM17/6105/UGR ; Spanish Ministry of Economy and Competitiveness (MINECO) AYA2016-76219-P ; European Union (EU)
27 pages, 18 figures, 1 table, 1 appendix.-- Pre-print archive. ; We present numerical simulations of the spectral evolution and emission of radio components in relativistic jets. We have developed an algorithm (SPEV) for the transport of a population of non-thermal electrons including radiative losses. For large values of the ratio of gas pressure to magnetic field energy density, \ab \sim 6\times 10^4, quiescent jet models show substantial spectral evolution, with observational consequences only above radio frequencies. Larger values of the magnetic field (\ab \sim 6\times 10^2), such that synchrotron losses are moderately important at radio frequencies, present a larger ratio of shocked-to-unshocked regions brightness than the models without radiative losses, despite the fact that they correspond to the same underlying hydrodynamic structure. We also show that jets with a positive photon spectral index result if the lower limit \gamma_min of the non-thermal particle energy distribution is large enough. A temporary increase of the Lorentz factor at the jet inlet produces a traveling perturbation that appears in the synthetic maps as a superluminal component. We show that trailing components can be originated not only in pressure matched jets, but also in over-pressured ones, where the existence of recollimation shocks does not allow for a direct identification of such features as Kelvin-Helmholtz modes, and its observational imprint depends on the observing frequency. If the magnetic field is large (\ab \sim 6\times 10^2), the spectral index in the rarefaction trailing the traveling perturbation does not change much with respect to the same model without any hydrodynamic perturbation. If the synchrotron losses are considered the spectral index displays a smaller value than in the corresponding region of the quiescent jet model. ; P. M. has performed this work with a European Union Marie Curie Incoming International Fellowship (MEIFCT- 2005-021603) and with the partial support obtained through the grant CSD-2007-00050. M. A. A. is a Ramón y Cajal Fellow of the Spanish Ministry of Education and Science. We acknowledge the support by the Spanish Ministerio de Educación y Ciencia and the European Fund for Regional Development through grants AYA2007-67626-C03-01, AYA2007-67626-C03-02 and AYA2007-67627-C03-03. I. A. has been supported an I3P contract with the Spanish Consejo Superior de Investigaciones Científicas. ; Peer reviewed
The cores of clusters at 0 ? z ? 1 are dominated by quiescent early-type galaxies, whereas the field is dominated by star-forming late-type galaxies. Clusters grow through the accretion of galaxies and groups from the surrounding field, which implies that galaxy properties, notably the star formation ability, are altered as they fall into overdense regions. The critical issues for understanding this evolution are how the truncation of star formation is connected to the morphological transformation and what physical mechanism is responsible for these changes. The GaLAxy Cluster Evolution Survey (GLACE) is conducting a thorough study of the variations in galaxy properties (star formation, AGN activity, and morphology) as a function of environment in a representative and well-studied sample of clusters. To address these questions, the GLACE survey is making a deep panoramic survey of emission line galaxies (ELG), mapping a set of optical lines ([O?ii], [O?iii], Hß andHa/[N?ii] when possible) in several galaxy clusters at z ~ 0.40, 0.63, and 0.86. Using the tunable filters (TF) of the OSIRIS instrument at the 10.4 m GTC telescope, the GLACE survey applies the technique of TF tomography: for each line, a set of images are taken through the OSIRIS TF, each image tuned at a different wavelength (equally spaced), to cover a rest frame velocity range of several thousand km?s-1 centred on the mean cluster redshift, and scanned for the full TF field of view of an 8?arcmin diameter. Here we present the first results of the GLACE project, targeting the Ha/[N?ii] lines in the intermediate-redshift cluster ZwCl?0024.0+1652 at z = 0.395. Two pointings have been performed that cover ~2?×?rvir. We discuss the specific techniques devised to process the TF tomography observations in order to generate the catalogue of cluster Ha emitters, which contains more than 200 sources down to a star formation rate (SFR)??1?M?/yr. An ancillary broadband catalogue is constructed, allowing us to discriminate line interlopers by means of colour diagnostics. The final catalogue contains 174 unique cluster sources. The AGN population is distinguished using different diagnostics and found to be ~37% of the ELG population. The median SFR of the star-forming population is 1.4?M?/yr. We studied the spatial distribution of ELG and confirm the existence of two components in the redshift space. Finally, we exploited the outstanding spectral resolution of the TF, attempting to estimate the cluster mass from ELG dynamics, finding M200?=?(4.1?±?0.2)?×?1014?M? h-1, in agreement with previous weak-lensing estimates. ; Acknowledgements. We acknowledge the support provided by M. Balogh during the preparation of the GLACE proposal to ESO, as well as his useful suggestions for improving the quality of this paper. We also acknowledge the anonymous referee. We acknowledge financial support from Spanish MINECO under grant AYA2014-29517-C03-01, AYA2011-29517-C03-02 and AYA2014-58861-C03. E.J.A. acknowledges support from MINECO under grant AYA2013-40611-P. J.M.R.E. acknowledges support from MINECO under grant AYA2012-39168-C03-01. We acknowledge support from the Faculty of the European Space Astronomy Centre (ESAC). I.R.S. acknowledges support from STFCGT/I001573/1, a European Research Council Advanced Programme Dustygal (321334) and a Royal Society/Wolfson Research Merit Award. J.S.S. acknowledges funding from the European Union Seventh Framework Programme (FP7/2007−2013) under grant agreement No. 267251 "Astronomy Fellowshipsin Italy" (AstroFIt). Based on observations made with the Gran Telescopio Canarias (GTC), installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofsica de Canarias, on the island of La Palma. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, by the National Aeronautics and Space Administration and the National Science Foundation
Following the recent discovery of X-ray quasi-periodic eruptions (QPEs) coming from the nucleus of the galaxy GSN 069, here we report on the detection of QPEs in the active galaxy named RX J1301.9+2747. QPEs are rapid and recurrent increases of the X-ray count-rate by more than one order of magnitude with respect to a stable quiescent level. During a XMM-Newton observation lasting 48 ks that was performed on 30 and 31 May 2019, three strong QPEs lasting about half an hour each were detected in the light curves of RX J1301.9+2747. The first two QPEs are separated by a longer recurrence time (about 20 ks) compared to the second and third (about 13 ks). This pattern is consistent with the alternating long-short recurrence times of the GSN 069 QPEs, although the difference between the consecutive recurrence times is significantly smaller in GSN 069. Longer X-ray observations will better clarify the temporal pattern of the QPEs in RX J1301.9+2747 and will allow a detailed comparison with GSN 069 to be performed. The X-ray spectral properties of QPEs in the two sources are remarkably similar, with QPEs representing fast transitions from a relatively cold and likely disk-dominated state to a state that is characterized by a warmer emission similar to the so-called soft X-ray excess, a component that is almost ubiquitously seen in the X-ray spectra of unobscured, radiatively efficient active galaxies. Previous X-ray observations of RX J1301.9+2747 in 2000 and 2009 strongly suggest that QPEs have been present for at least the past 18.5 years. The detection of QPEs from a second galactic nucleus after GSN 069 rules out contamination by a Galactic source in both cases, such that QPEs ought to be considered a novel extragalactic phenomenon associated with accreting supermassive black holes. ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)
[EN] Gamma-ray bursts (GRBs) are the most violent explosions in the Universe. Although they were first discovered over half a century ago, yet many problems remain unsolved. Since the successful launch of GRB dedicated missions such as Swift and Fermi, multi-wavelength ground-based observations have provided a new approach to better characterize these events, their host galaxies and understand the underlying physics around the newly born compact objects following the GRB itself. GRB 140629A was a long burst that triggered the Swift satellite and many facilities at different wavelengths followed up this event, including the optical (Swift/UVOT and various facilities worldwide), infrared (Spitzer) and X-rays (Swift/XRT). These data were taken between 40 seconds and 3 yr after the burst trigger, which made this burst a good case to investigate the properties of the dominant jet and its host galaxy. The absorption features displayed in the optical spectrum, taken with the 6.0m BTA telescope, confirmed the redshift of this GRB (z = 2.276 0.001). We found no strong spectral evolution when fitting the spectral energy distribution of the afterglow from the X-rays to optical wavelengths. The hydrogen column density NH was constrained to be 7.2×1021cm−2 along the line of sight. The afterglow in this burst could be explained by a blast wave jet with a long-lasting central engine expanding into a uniform medium in the slow cooling regime. At the end of energy injection, a normal decay phase was observed in both the optical and X-ray bands. An achromatic jet break was also found in the afterglow light curves 0.4 d after the trigger. We fitted the multi-wavelength data simultaneously with a model (based on numerical simulations) and found that the observations could be explained by a narrow uniform jet in a dense environment with a half-opening angle of 6:7 viewed 3:8 off-axis, implying a total released energy of 1:4 1054 erg. Using the redshift and opening angle, we found that GRB 140629A followed both the Ghirlanda and Amati relations. The peak time of the light curve was identified as the onset of the forward shock (181 s after trigger) and we could constrain the initial Lorentz factor (Γ0) in the range 82-118. After fitting the host galaxy spectral energy distribution, we found the host to be a low mass, star-forming galaxy with a star formation rate (SFR) of log(SFR) = 1.1+0.9−0.4 M yr−1. We also obtained a value for the neutral hydrogen density NHI by fitting the optical spectrum, from which we derived logNHI = 21:0 0:3, classifying this host as a damped Lyman-alpha system. High ionisation lines (N V,Si IV) were also detected in the optical spectrum. Furthermore, polarisation observations by the MASTER network indicated that this burst was weakly polarised. GRB 190829A was detected by both Fermi and Swift but what made a unique event out of it was the detection of very high energy (VHE) gamma-rays by the High-Energy Stereoscopic System telescopes (HESS). The prompt gamma-ray emission displayed two emission episodes separated by a quiescent gap of 40 s. We followed it up with the 10.4 m Gran Telescopio CANARIAS (GTC) and gathered observations of the afterglow of GRB 190829A and its underlying supernova during the following days. We determined the redshift of this event (z = 0.0785 0.005) and compared GRB 190829A to GRB 180728A, another GRB with similar prompt behaviour at VHE energies, and discussed the implications regarding the underlying physical mechanisms producing these two GRBs. Together with the prompt emission data, the 10.4 m GTC data was used to better understand the emission mechanisms and possible progenitors. In the detailed analysis of the multi-band observations of the afterglow, we found the observational properties of the multi-wavelength afterglow could be explained by the cooling frequency passing between the optical and X-ray bands at the early epoch. A few days after, we saw the transition from the afterglow spectrum to the underlying supernova (dubbed SN 2019oyw) spectrum, which dominated the light curve at later times. Although the prompt emission temporal properties of GRB 190829A and GRB 180728A were similar, the two gamma-ray pulses were different in the spectral domain. We also found that the SN 2019oyw associated with GRB 190829A is powered by Ni decay and could be classified as a Type Ic-BL (broad line) supernova. The spectroscopic and photometric properties of this supernova were consistent with those observed for SN 1998bw (also related to another burst, GRB 980425) but SN 2019oyw evolved much faster than SN 1998 bw. Besides these above mentioned two long-duration GRBs, we also investigated the prompt emission and the afterglow properties of a sample of shortduration gamma-ray bursts (sGRBs) including GRB 130603B and another eight sGRB events during 2012-2015. They were observed by several multi-wavelength facilities, including the 10.4m GTC telescope. Prompt emission high energy data of those events were obtained by INTEGRAL-SPI-ACS, Swift-BAT and Fermi- GBM satellites. The prompt emission data by INTEGRAL in the 0.1–10 MeV energy range for sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A, and sGRB 151228A did not show signs of the extended emission or the precursor activity and their spectral and temporal properties were found to be similar to those seen in case of other short-duration bursts. For sGRB 130603B, our new afterglow photometric data constrained the pre-jet-break temporal decay due to denser temporal coverage. Its afterglow light curve, containing both our new data as well as previously published photometric data, was broadly consistent with the interstellar medium (ISM) afterglow model. Modelling the host galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software supported a scenario where the burst environment was undergoing moderate star formation activity. From the inclusion of our late-time data for the additional eight sGRBs, we were able to place tight constraints on the non-detection of the afterglow, host galaxy or any underlying 'kilonova' emission. Finally, our late-time afterglow observations of the short-duration GRB 170817A (related to the gravitational wave GW 170817) are also discussed and compared with the sub-set of short-duration GRBs. ; [ES] Los estallidos de rayos gamma (GRBs) son los fenómenos más energéticos del Universo que, descubiertos hace más de medio siglo, presentan en la actualidad muchos incógnitas que aún están por resolver. Tras el lanzamiento exitoso de Swift y Fermi, la observación de los GRBs en múltiples longitudes de onda está proporcionando un nuevo enfoque para poder comprender mejor este fenómeno. Uno de los GRBs estudiados en este trabajo ha sido GRB 140629A, un estallido de larga duración que detectó el satélite Swift y que se pudo observar en diferentes longitudes de onda, obteniéndose un conjunto de datos abundantes que incluye el óptico (por medio de Swift/UVOT y de otras instalaciones astronómicas en todo el mundo), infrarrojo (Spitzer) y rayos X (Swift/XRT). Los datos analizados se tomaron entre 40 segundos y 3 años después del GRB, haciendo de este un caso propicio para poder investigar las propiedades tanto de la emisión colimada como de la de la galaxia anfitriona. A través de las líneas de absorción características presentes en el espectro óptico se derivó el corrimiento al rojo de este GRB (z = 2.276 0.001). Por otro lado, la evolución de la distribución espectral de energía en el rango del óptico a los rayos X no es significativa. La densidad de columna de hidrógeno NH se midió en 7.2 ×1021cm−2 a lo largo de la línea de visión. La postluminiscencia observada se puede explicar por medio de la existencia de un chorro colimado resultante de la onda expansiva procedente de un motor central de larga duración, produciéndose la expansión en un medio uniforme y en el régimen de enfriamiento lento. También al final de la fase de inyección de energía, se observa una fase de declive tanto en la banda óptica como en la de rayos X. Igualmente se encuentra una desviación (rotura) de la caída del flujo observado de la postluminiscencia, de manera acromática, en las curvas de luz de la posluminiscencia 0.4 d después del GRB. Ajustamos los datos de las múltiples longitudes de onda de manera simultáneamente con un modelo basado en una simulación numérica y encontramos que las observaciones pueden explicarse por un chorro uniforme estrecho en un ambiente denso con un ángulo de abertura de 6:7 visto 3:8 fuera de su eje, lo que implica que se liberó una energía total de 1:4 1054 erg. Usando el valor del corrimiento al rojo y el ángulo de abertura, encontramos que GRB 140629A obedece las relaciones de Ghirlanda y Amati. Desde el momento del máximo de la curva de luz, identificado como el inicio de la onda de choque que se propaga en el tiempo (181 s después del disparo), el factor de Lorentz inicial (Γ0) debe situarse en el rango 82-118. Haciendo un ajuste de los valores fotométricos de la galaxia anfitriona, encontramos se trata de una galaxia de baja masa con formación estelar y una tasa de formación estelar de log(SFR)=1.1+0.9−0.4 M yr−1 . Obtenemos un valor de la densidad del hidrógeno neutro NHI ajustando el espectro óptico, logNHI = 21:0 0:3, clasificando este sistema como un sistema de Lyman-alfa amortiguado. Las líneas de alta ionización (N V, Si IV) también se detectan en el referido espectro. Y las observaciones de polarización realizadas por el telescopio MASTER indican que este estallido es un evento débilmente polarizado. El segundo evento de los estudiados ha sido GRB 190829A, que fue detectado por Fermi y Swift y también a rayos-gamma de muy alta energía (VHE) por HESS (Sistema estereoscópico de alta energía). La emisión temprana mostró dos episodios de emisión separados por un intervalo sin actividad alguna con una duración de 40 s. Presentamos las observaciones del 10.4 m Gran Telescopio CANARIAS (GTC) en relación a la post-luminiscencia de GRB 190829A y su supernova subyacente. El corrimiento al rojo de este evento se detectó con z=0.0785 0.005. También comparamos GRB 190829A con GRB 180728A, un estallido con un comportamiento similar, y discutimos las implicaciones en los mecanismos físicos subyacentes que producen estos dos GRBs. Los datos fotométricos multi-banda junto con la observación espectroscópica de este evento se tomaron con el telescopio GTC de 10.4m. Junto con los datos de la emisión inicial, los datos del GTC se utilizan para comprender los mecanismos de emisión y el posible progenitor. En el análisis detallado de las observaciones multibanda del resplandor, encontramos que este evento es consistente con el paso de la frecuencia de enfriamiento entre las bandas ópticas y de rayos X en épocas tempranas. Luego estudiamos la supernova subyacente 2019oyw, que domina las fases más tardías. Aunque las propiedades temporales de emisión rápida de GRB 190829A y GRB 180728A son similares, los dos pulsos de rayos-gamma son diferentes en el dominio espectral. Encontramos que SN 2019oyw, asociada con GRB 190829A se puede explicar por la desintegración de Ni y ha sido clasificada como una supernova de Tipo Ic-BL. Las propiedades espectroscópicas y fotométricas de esta supernova son consistentes con las observadas para SN 1998bw (asociada a GRB 980425), pero mostrando una evolución más rápida. Además de los dos GRBs de larga duración reseñados anteriormente, también investigamos la emisión rápida y las propiedades de la postluminiscencia del estallido de rayos gamma de corta duración GRB 130603B así como de otros 8 eventos GRB de corta duración, detectados durante el periodo 2012-2015, y observados por varias instalaciones en diferentes longitudes de onda, incluyendo el telescopio GTC de 10.4 m de diámetro. Los satélites INTEGRAL (SPI-ACS), Swift (BAT) and Fermi (GBM) obtuvieron datos de alta energía de dichos GRBs. Los datos de emisión temprana por INTEGRAL en el rango de energía de 0,1 a 10 MeV para sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A y sGRB 151228A no muestran ningún indicio de la emisión extendida o la actividad precursora y sus propiedades espectrales y temporales son similares a los que se ven en el caso de otros GRBs de corta duración. Para sGRB 130603B, nuestros nuevos datos fotométricos en relación a la posluminiscencia restringen el decaimiento temporal previo al desvío en la curva de luz producida por la expasión del chorro, gracias a haber dispuesto de una cobertura temporal más completa. La curva de luz de la postluminiscencia, que contiene tanto nuestros datos fotométricos nuevos como los publicados anteriormente, es consistente con el modelo de post-luminiscencia atravesando un medio de tipo interestelar (ISM). El modelado de las galaxias anfitrionas de sGRB 130603B y sGRB 141212A, utilizando el software LePHARE, respalda un escenario en el que el entorno de la explosión en la galaxia huésped está experimentando una actividad de formación estelar moderada. A partir de la inclusión de nuestros datos para los otros 8 GRBs de corta duración anteriormente referidos, podemos imponer restricciones estrictas a la no detección de la postluminiscencia, la galaxia anfitriona o cualquier emisión de kilonova subyacente. Nuestras observaciones tardías en el tiempo, de la post-luminiscencia de sGRB 170817A / GW170817 también se discuten y comparan con el subconjunto de GRBs de corta duración. ; With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709. ; Peer reviewed
