Abstract: My training in the field of languages - musical, visual, and verbal - was always marked by attention to the materiality of languages themselves and to the means how they are transmitted to allow their communicative functions. Since the phonatory system, installed in the body itself, these means constitute technologies that have evolved over the centuries, bringing with them new forms of languages, such as the different forms of writing, the Gutenberg galaxy and, from the 19th century onwards, the industrial, electronic, and digital revolutions, each introducing technologies of their own. When language issues are placed in the focus of attention, what matters, since the industrial revolution, is the advent of cognitive technologies, such as photography, cinema, followed by electronic technologies - radio and television -, and, finally, the explosion of the digital revolution with all its new language forms and consequently of cognition, which today are distributed across the most different applications and platforms. The study of this evolution led me to postulate, based on the inspiration gathered from some authors, that human cognition is, since the first forms of writing, growing outside the human skull. Therefore, this is a proposal that concerns the exosomatization of human intelligence and cognition with all the contradictions that this brings. This article is dedicated to explaining this proposal with attention to the way it was developed in my work along the years. Abstract musical visual functions system itself centuries writing th onwards revolutions own matters photography cinema , finally platforms postulate authors skull Therefore brings years

Resumo: A formação da autora deste trabalho, no campo das linguagens - musicais, visuais e verbais - foi sempre marcada pela atenção à materialidade das próprias linguagens e aos meios pelos quais elas são transmitidas, para permitir suas funções comunicativas. Desde o aparelho fonador, instalado no próprio corpo, esses meios se constituem como tecnologias que foram evoluindo, através dos séculos, trazendo consigo novas formas de linguagem, tais como as distintas formas de escrita, a galáxia de Gutenberg e, do século 19 para cá, as revoluções industrial, eletrônica e digital, cada qual introduzindo tecnologias que lhes são próprias. Quando as questões de linguagem são colocadas no foco da atenção, o que importa, desde a revolução industrial, é o advento de tecnologias cognitivas, como são a fotografia, o cinema, seguidas das tecnologias eletrônicas - rádio e televisão - e, por fim, a explosão da revolução digital com todas as suas novas formas de linguagens e consequentemente de cognição, que hoje se distribuem pelos mais distintos aplicativos e plataformas. O estudo dessa evolução levou a autora a postular, a partir da inspiração colhida em alguns autores, que a cognição humana está, desde as primeiras formas de escrita, crescendo fora da caixa craniana. Portanto, uma proposta que diz respeito à exossomatização da inteligência e da cognição humana com todas as contradições que isso traz. Este artigo está dedicado à explicitação dessa proposta, com atenção ao modo como ela foi se desenvolvendo, no seu pensamento. Resumo trabalho musicais transmitidas comunicativas fonador corpo evoluindo séculos escrita 1 cá industrial importa cognitivas fotografia cinema fim plataformas postular autores craniana Portanto traz desenvolvendo pensamento

Resumen Se da una breve descripción de lo que creemos saber hasta el día de hoy sobre la nucleosíntesis de elementos en el universo. Por medio de una reseña cronológica se indican los periodos y mecanismos de su formación. Se formula una prospectiva crítica sobre investigaciones futuras que permitirán validar, modificar o rechazar hipótesis hechas, las cuales involucrarán observaciones conjuntas que abarcan mediciones más finas de radiación cósmica de fondo, cúmulos de galaxias y de ondas gravitacionales producidas por choques de estrellas de neutrones. La información obtenida se combinará con restricciones dadas por modelos teóricos. Tal vez, muchas dudas actuales serán aclaradas, pero nuevas preguntas surgirán.

Abstract We present what we know on nucleosynthesis in the universe and hypotheses that have been made in this regard. A brief description of the universe’s evolution during its different stages is offered, indicating which are the periods and mechanisms of element formation. A critical prospective on future research is formulated to validate, modify, or reject the hypotheses formulated. These will involve joint observations that encompass finer measurements of cosmic background radiation, galaxy clusters, and gravitational waves produced by neutron star collisions. The information thus obtained will be combined with restrictions given by theoretical models. Perhaps many current doubts will be clarified, but new questions will arise.

(This article is part of a project by Trans/Form/Ação: Unesp Philosophy Journal. It is the Authorial Philosophy Dossier, to be published in 2022.) My training in the field of languages -- musical, visual, and verbal was always marked by attention to the materiality of languages themselves and to the means how they are transmitted to allow their communicative functions. Since the phonatory system, installed in the body itself, these means constitute technologies that have evolved over the centuries, bringing with them new forms of languages, such as the different forms of writing, the Gutenberg galaxy and, from the 19th century onwards, the industrial, electronic, and digital revolutions, each introducing technologies of their own. When language issues are placed in the focus of attention, what matters, since the industrial revolution, is the advent of cognitive technologies, such as photography, cinema, followed by electronic technologies, radio and television, and, finally, the explosion of the digital revolution with all its new language forms and consequently of cognition, which today are distributed across the most different applications and platforms. The study of this evolution led me to postulate, based on the inspiration gathered from some authors, that human cognition is, since the first forms of writing, growing outside the human skull. Therefore, this is a proposal that concerns the exosomatization of human intelligence and cognition with all the contradictions that this brings. This article is dedicated to explaining this proposal with attention to the way it was developed in my work along the years.

(Este artigo faz parte de um projeto da Trans/Form/Ação: revista de filosofia da Unesp. Trata-se do Dossiê Filosofia Autoral, a ser publicado em 2022.) Minha formação no campo das linguagens, musicais, visuais e verbais foi sempre marcada pela atenção à materialidade das próprias linguagens e aos meios pelos quais elas são transmitidas para permitir suas funções comunicativas. Desde o aparelho fonador, instalado no próprio corpo, esses meios constituem-se como tecnologias que foram evoluindo através dos séculos, trazendo consigo novas formas de linguagem, tais como as distintas formas de escrita, a galáxia de Gutenberg e, do século 19 para cá, as revoluções industrial, eletrônica e digital, cada qual introduzindo tecnologias que lhes são próprias. Quando as questões de linguagem são colocadas no foco da atenção, o que importa, desde a revolução industrial, é o advento de tecnologias cognitivas, como são a fotografia, o cinema, seguidas das tecnologias eletrônicas, rádio e televisão, e, por fim, a explosão da revolução digital com todas as suas novas formas de linguagens e consequentemente de cognição que hoje se distribuem pelos mais distintos aplicativos e plataformas. O estudo dessa evolução levou-me a postular, a partir da inspiração colhida em alguns autores, que a cognição humana está, desde as primeiras formas de escrita, crescendo fora da caixa craniana. Portanto, uma proposta que diz respeito à exossomatização da inteligência e da cognição humana com todas as contradições que isso traz. Este artigo está dedicado à explicitação dessa proposta com atenção ao modo como ela foi se desenvolvendo no meu pensamento.

Abstract This work is a Brazilian-Indian collaboration. It aims at investigating the structural properties of Lenticular galaxies in the Stripe 82 using a combination of S-PLUS (Southern Photometric Local Universe Survey) and SDSS data. S-PLUS is a novel optical multi-wavelength survey which will cover nearly 8000 square degrees of the Southern hemisphere in the next years and the first data release covers the Stripe 82 area. The morphological classification and study of the galaxies’ stellar population will be performed combining the Bayesian Spectral type (from BPZ) and Morfometryka (MFMTK) parameters. BPZ and MFMTK are two complementary techniques, since the first one determines the most likely stellar population of a galaxy, in order to obtain its photometric redshift (phot-z), and the second one recovers non-parametric morphological quantities, such as asymmetries and concentration. The combination of the two methods allows us to explore the correlation between galaxies shapes (smooth, with spiral arms, etc.) and their stellar contents (old or young population). The preliminary results, presented in this work, show how this novel data set opens a new window on our understanding of the nearby universe.

ABSTRACT Our understanding of the structure, composition and evolution of galaxies has strongly improved in the last decades, mostly due to new results based on large spectroscopic and imaging surveys. In particular, the nature of ionized gas, its ionization mechanisms, its relation with the stellar properties and chemical composition, the existence of scaling relations that describe the cycle between stars and gas, and the corresponding evolution patterns have been widely explored and described. More recently, the introduction of additional techniques, in particular integral field spectroscopy, and their use in large galaxy surveys, have forced us to re-interpret most of those recent results from a spatially resolved perspective. This review is aimed to complement recent efforts to compile and summarize this change of paradigm in the interpretation of galaxy evolution. To this end we replicate published results, and present novel ones, based on the largest compilation of IFS data of galaxies in the nearby universe to date.

RESUMEN Nuestro entendimiento de la estructura, composición y evolución de las galaxias se ha visto ampliamente modificado en las últimas décadas principalmente debido a la explosión de resultados basados en grandes muestreos en imagen y espectroscopía. En particular, la naturaleza de la ionización observada, su relación con las propiedades estelares y la composición química, la existencia de relaciones evolutivas o de escala que regulan el ciclo entre el gas y las estrellas, y los patrones evolutivos se han explorado y descrito en detalle. Más recientemente, la introducción de técnicas adicionales, en particular la espectroscopía de campo integral, ha forzado a una reinterpretación de estos resultados recientes desde una perspetiva espacialmente resuelta. Este artículo de revisión tiene como objetivo complementar esfuerzos recientes enfocados en la compilación y resumen de este cambio de paradigma en la interpretación de la evolución de las galaxias.

Resumen Se presenta un estudio de la evolución de diferentes posibles progenitores sin materia oscura de la galaxia enana esferoidal Carina, una de las galaxias satélites de la Vía Láctea, mediante simulaciones numéricas Newtonianas de N-Cuerpos. No fue posible reproducir completamente las propiedades observacionales de Carina, y por consiguiente no se pudo determinar un posible progenitor sin materia oscura para la misma; sin embargo, progenitores con masa inicial 1 χ 107 Μʘ y radios de Plummer 0.5 y 0.6 kpc, reprodujeron los valores observacionales de Carina para tres de las cinco variables estudiadas (radio de brillo medio, dispersión de velocidades sobre la visual y distancia galactocéntrica). Por lo tanto estos progenitores podrían ser la base para posteriores trabajos sobre el origen de la galaxia enana Carina.

Abstract We present a study of the evolution of several different dark matter free possible progenitors of the Carina dSph galaxy, one of the satellites of the Milky Way, using Newtonian numerical N-body simulations. It was not possible to reproduce all the observed properties of Carina, therefore a possible dark matter free progenitor of it was not found; nevertheless, progenitors with initial mass 1 χ 107Μʘ and Plummer radii 0.5 and 0.6 kpc reproduced the observational values of Carina for three of the five studied variables (half light radius, line-of-sight velocity dispersion and galactocentric distance). Thus, those satellites could be the starting point for further work about the origin of the Carina dwarf galaxy.

Resumen Se realizan simulaciones de N-cuerpos de la interacción entre la galaxia enana Sagitario y la Vía Láctea para estudiar si es posible reproducir tanto las bifurcaciones en las corrientes de marea como las propiedades físicas de Sagitario. Ambas galaxias son simuladas como conjuntos de partículas (potencial vivo). Las estructuras iniciales son conformadas en GALIC y la interacción gravitacional entre estas galaxias es simulada con GADGET-2. Sagitario inicialmente es una galaxia de tipo disco rotante con dos componentes: Halo de materia oscura y disco estelar y la Vía Láctea como es usual, es una galaxia de disco con tres componentes: halo de materia oscura, disco estelar y esferoide. Se realizan varias simulaciones de la interacción del progenitor de esta galaxia enana con la Vía Láctea, donde el ángulo entre el momento angular orbital y el momento angular del disco es 180° ≤ θ ≤ 0° mostrando que aunque no se reproducen en su totalidad la posición y propiedades físicas del remanente de Sagitario, las bifurcaciones aparecen de modo evidente cuando 180° ≤θ ≤ 90°.

Abstract N-body simulations of the interaction between the Sagittarius dwarf galaxy and the Milky Way are performed to study whether it is possible to reproduce both the bifurcations in the tidal streams and the physical properties of Sagittarius. Both galaxies are simulated as sets of particles (live potentials). The initial structures are formed using GALIC and the gravitational interaction between these galaxies is simulated with GADGET-2. Sagittarius initially is simulated as a rotating disk-type galaxy with two components: dark matter halo and stellar disk and the Milky Way is a disk galaxy with three components: dark matter halo, stellar disk and central spheroid. Several numerical simulations of the interaction of this galaxy with the Milky Way with angles between the orbital angular momentum and the disc angular momentum in the range 180° ≤θ ≤ 0° were performed, showing that, although the position and physical properties of Sagittarius are not reproduced entirely by the remnant, the bifurcations appear clearly when 180° ≤θ < 90°.

Abstract Photoionized nebulae, comprising HII regions and planetary nebulae, are excellent laboratories to investigate the nucleosynthesis and chemical evolution of several elements in the Galaxy and other galaxies of the Local Group. Our purpose in this investigation is threefold: (i) compare the abundances of HII regions and planetary nebulae in each system in order to investigate the differences derived from the age and origin of these objects, (ii) compare the chemical evolution in different systems, such as the Milky Way, the Magellanic Clouds, and other galaxies of the Local Group, and (iii) investigate to what extent the nucleosynthesis contributions from the progenitor stars affect the observed abundances in planetary nebulae, which constrains the nucleosynthesis of intermediate mass stars. We show that all objects in the samples present similar trends concerning distance-independent correlations, and some constraints can be defined on the production of He and N by the PN progenitor stars.

Resumen Las nebulosas fotoionizadas, incluyendo regiones HII y nebulosas planetarias, son excelentes laboratorios para investigar la nucleosíntesis y la evolución química de varios elementos, en nuestra galaxia y en galaxias del Grupo Local. En este trabajo: (i) comparamos las abundancias en regiones HII y nebulosas planetarias para investigar las diferencias que se derivan de las edades y el origen de estos objetos; (ii) comparamos la evolución química en distintos sistemas, como la Vía Láctea, las Nubes de Magallanes y otras galaxias del Grupo Local; (iii) investigamos qué tanto la contribución de las estrellas progenitoras a la nucleosíntesis afecta las abundancias observadas en las nebulosas planetarias, lo cual constriñe la nucleosíntesis de estrellas de masa intermedia. Mostramos que todos los objetos estudiados presentan tendencias similares en cuanto a las correlaciones independientes de las distancias, y encontramos que pueden definirse límites a la producción de He y N en las estrellas progenitoras de las nebulosas planetarias.

ABSTRACT The survival time of initially compact associations of galaxy-size dark matter halos, obtained at the present epoch from a series of ΛCDM cosmological simulations, is studied by means of dynamical N-body simulations. The time evolution of such systems from the present epoch up to 5 Gyr into the future is followed. We find that out of 14 initial compact associations only 1 (≈ 10%) suffers a full merger, and the others still have at least two discernible members in such a time span, although they have suffered multiple mergers. Our results support the hypothesis that the majority of current compact galaxy groups will not suffer a complete merger within the next few gigayears, and that some of them (≈ 10%) may even evolve without a single merger. We conclude that no overmerging problem exists in compact groups.

RESUMEN Se estudia el tiempo de supervivencia de asociaciones compactas de halos galácticos de materia oscura, obtenidas de simulaciones cosmológicas en un escenario ΛCDM, mediante simulaciones dinámicas de N-cuerpos. La evolución de tales sistemas se sigue por 5 Gyr a partir de la época actual. Encontramos que de las 14 configuraciones compactas iniciales solamente 1 (≈ 10%) sufre una fusión total de sus 4 miembros, y el resto aún conservan al menos 2 miembros, aunque hayan sufrido fusiones múltiples. Nuestros resultados apoyan la hipótesis de que la mayoría de los grupos compactos actuales no sufrirán una fusión completa en los próximos giga-años, y que varios (≈ 10%) incluso podrían vivir sin sufrir una fusión en 5 Gyr. Concluímos que no existe un problema de sobrefusión en grupos compactos en la cosmología ΛCDM.

We have computed the Galactic Habitable Zones (GHZs) of the Andromeda galaxy (M31) based on the probability of terrestrial planet formation, which depends on the metallicity (Z) of the interstellar medium, and the number of stars formed per unit surface area. The GHZ was obtained from a chemical evolution model built to reproduce a metallicity gradient in the galactic disk, [O/H](r)=-0.015 dex kpc-1x r(kpc) + 0.44 dex. If we assume that Earth-like planets form with a probability law that follows the Z distribution shown by stars with detected planets, the most probable GHZ per pc² is located between 3 and 7 kpc for planets with ages between 6 and 7 Gyr. However, the highest number of stars with habitable planets is located in a ring between 12 and 14 kpc with a mean age of 7 Gyr. 11% and 6.5% of the all formed stars in M31 may have planets capable of hosting basic and complex life, respectively.

Calculamos la Zona de Habitabilidad Galáctica (ZHG) de M31 basándonos en la probabilidad de formación de planetas terrestres dependiente de la metalicidad (Z) del medio interestelar. La ZHG fue determinada a partir de un modelo de evolución química construido para reproducir un gradiente de metalicidad en el disco galáctico: [O/H](r)=-0.015 dex kpc-1 x r(kpc) + 0.44 dex. Suponiendo que los planetas tipo Tierra se forman bajo una ley de probabilidad que sigue la distribución de Z mostrada por las estrellas con planetas, la ZHG más probable se localiza entre 3 y 7 kpc para planetas con edades entre 6 y 7 Ga, aunque el mayor número de estrellas con planetas habitables se encuentra en un anillo localizado entre 12 y 14 kpc y edad promedio de 7 Ga. El 11% y 6.5% de todas las estrellas formadas en M31 tendrían planetas capaces de albergar vida básica y compleja, respectivamente.

Using the abundance matching technique, we infer the local stellar and baryonic mass-halo mass ( Ms- Mh and Mb - Mh) relations separately for central blue and red galaxies (BGs and RGs). The observational inputs are the SDSS central BG and RG stellar mass functions and the measured gas mass-Ms relations. For halos associated to central BGs, the distinct ACDM halo mass function is used and set up to exclude: (i) the observed group/cluster mass function and (ii) halos with a central major merger at resdshifts z ≤ 0.8. For central RGs, the complement of this 5 mass function to the total one is used. At Mh > 10(11.5) ΜΘ, the Ms of RGs tend to be higher than those of BGs for a given Mh, the difference not being larger than 1.7. At Mh < 10(11.5) ΜΘ, this trend is inverted. For BGs (RGs): (a) the maximum value of f s = Ms / Mh is 0.021+0.016 -0.009(0.034 +0.026 -0.015)and it is attained at log(Mh/ΜΘ) = 12.0 (= 11.9); (b) f s ∞ Mh ( f s ∞ Mh³) at the low-mass end while at the high-mass end, f s ∞ Mh-0.4 (f s ∞ Mh-06). The baryon mass fractions, f b = Mb / Mh, of BGs and RGs reach maximum values of f b = 0.028 +0.018 -0.011 y f b = 0.034 +0.025 -0.014., respectively. At Mh < 10(11.3) ΜΘ, the dependence of f b on Mh is much steeper for RGs than for BGs. We discuss the differences found in the f s - Mh and f b - Mh relations between BGs and RGs in the light of semi-empirical galaxy evolution inferences.

Con la tecnica del empate de abundancias, las relaciones locales masa estelar y bariónica-masa de halo (Ms- Mh y Mb- Mh) para galaxias centrales azules y rojas (GAs y GRs) se infieren por separado. Se hace uso de las funciones de masa estelar galáctica observadas de GAs y GRs y las respectivas relaciones masa de gas-Ms. Las funciones de masa de halos asociados a las GAs y GRs centrales se toman de una descomposición adecuadamente obtenida de la función de halos distinguibles ACDM. Para Mh >~10(11.5) ΜΘ, la Ms de GRs tiende a ser mayor que la de GAs a una dada Mh, pero no más que un factor ~1.7. Para Mh >~10(11.5)ΜΘ, esta tendencia se invierte. Para GAs (GRs): (a) el máximo de f s= Ms /Mh es 0.021+0.016 -0.009(0.034 +0.026 -0.015) y se alcanza a log (Mh / ΜΘ) = 12.0 (= 11.9); (b) f s ∞Mh(f s ∞Mh³) hacia el lado de bajas masas, mientras que en el otro extremo f s ∞ Mh-0'4 (f s ∞ Mh-0.6). Las f b= Mb / Mh de GAs y GRs son cercanas para Mh >~10(11.7) ΜΘ, y alcanzan valores maximos de f b = 0.028 +0.018 -0.011 y f b = 0.034 +0.025 -0.014. Hacia masas menores la dependencia de f b sobre Mh es mucho más empinada para GRs que para GAs. Discutimos las diferencias encontradas para las relaciones f s-Mh y f b- Mh entre GAs y GRs a la luz de inferencias semi-empíricas de evolución galáctica.

We present chemical evolution models of the Galactic disk with different Z dependent yields. We find that a moderate mass loss rate for massive stars of solar metallicity produces an excellent fit to the observed C/H and C/O gradients of the Galactic disk. The best model also fits: the H, He, C, and O abundances derived from recombination lines of M17, the protosolar abundances, and the C/O-O/H, C/Fe-Fe/H, and O/Fe-Fe/H relations derived from solar vicinity stars. The agreement of the model with the protosolar abundances implies that the Sun originated at a Galactocentric distance similar to the one it has now. Our model for r = 3 kpc implies that a fraction of the stars in the direction of the bulge formed in the inner disc. We obtain a good agreement between our model and the C/O versus O/H relationship derived from extragalactic H II regions in spiral galaxies.

Presentamos modelos de evolución química del disco galáctico con diferentes rendimientos dependientes de Z. Encontramos que una tasa moderada de pérdida de masa en estrellas masivas de metalicidad solar produce un excelente ajuste con los gradientes de C/H y C/O del disco de la Galaxia. El mejor modelo reproduce: las abundancias de H, He, C y O derivadas de líneas de recombinación en M17, las abundancias protosolares y las relaciones C/O-O/H, C/Fe-Fe/H y O/Fe-Fe/H derivadas de estrellas de la vecindad solar. La concordancia del modelo con las abundancias protosolares implica que el Sol se originó a una distancia galactocéntrica similar a la actual. El modelo para r = 3 kpc implica que una fracción de las estrellas en la dirección del bulbo se formó en el disco interno. Nuestro modelo reproduce la relación C/O-O/H derivada de regiones H II extragalácticas en galaxias espirales.

The determination of accurate chemical abundances of planetary nebulae (PN) in different galaxies allows us to obtain important constraints on chemical evolution models for these systems. We have a long-term program to derive abundances in the galaxies of the Local Group, particularly the Large and Small Magellanic Clouds. In this work, we present our new results on these objects and discuss their implications in view of recent abundance determinations in the literature. In particular, we obtain distance-independent correlations involving He, N, O, Ne, S, and Ar, and compare the results with data from our own Galaxy and other galaxies in the Local Group. As a result of our observational program, we have a large database of PN in the Galaxy and the Magellanic Clouds, so that we can obtain reliable constraints on the nucleosynthesis processes in the progenitor stars in galaxies of different metallicities.

La determinación precisa de las abundancias químicas en las nebulosas planetarias (PN) de diferentes galaxias nos permite obtener importantes límites para los modelos de evolución química en estos sistemas. Tenemos un programa a largo plazo para derivar abundancias en las galaxias del Grupo Local, en particular, la Nube Mayor y la Nube Menor de Magallanes. En este trabajo presentamos nuestros resultados para estos objetos,y discutimos sus implicaciones en el contexto de nuevas determinaciones de abundancias reportadas en la literatura. En particular, obtenemos correlaciones independientes de la distancia que involucran al He, N, O, Ne, S y Ar, comparamos los resultados con datos sobre nuestra propia galaxia y otras del Grupo Local. Como resultado de nuestras observaciones, hemos obtenido una gran base de datos, por lo cual podemos obtener límites confiables a los procesos de nucleosíntesis en las estrellas progenitoras en galaxias de diferentes metalicidades.

In this paper we apply and discuss a method for the determination of the magnetic field (H) evolution in supernova remnants (SNRs) from radio luminosity at given frequency v to diameter (Lv - D) correlation. We assumed that H evolves as H ∞ D-δ, where D is the diameter of the remnant. A value δ <img border=0 width=20 height=15 src="../../../../../img/revistas/rmaa/v43n1/a2s1.jpg"> 1.2 is obtained under the equipartition assumption from the equations for revised equipartition calculation (REC) and by using the data sample from the nearby starburst galaxy M82. We try to investigate whether or not SNRs in M82 are in the equipartition state. This is done by comparison of our empirically obtained δwith the theoretical value expected for equipartition conditions. The inconsistency between the value obtained for equipartition conditions and adiabatic expansion (δ = 1.5) and the value empirically obtained herein can be explained mainly by the influence of sensitivity selection effects which tend to flatten the slope of the Lv - D relations for extragalactic samples.

En este artículo aplicamos y discutimos un método para la determinación de la evolución del campo magnético en los remanentes de supernova (SNRs) a partir de la relación entre la luminosidad en radio a la frecuencia v y el diámetro (Lv - D). Asumimos que H evoluciona como H ∞ D-δ, donde D es el diámetro del remanente. El valor δ <img border=0 width=20 height=15 src="../../../../../img/revistas/rmaa/v43n1/a2s1.jpg">1.2 se obtiene con la hipótesis de equipartición a partir de las ecuaciones del cálculo revisado de equipartición (REC) y usando la muestra de datos de la galaxia de brote estelar M82. Intentamos investigar si los remanentes de la supernova en M82 están en estado de equipartición o no, comparando la 6 empíricamente obtenida con el valor teórico esperado para equipartición. La diferencia entre el valor obtenido teóricamente para la equipartición con expansión adiabática (δ = 1.5) y el valor empírico obtenido aquí se puede explicar principalmente como debido a efectos de selección en la sensibilidad, que tienden a aplanar la pendiente de la relación Lv - D para las muestras extragalácticas.

We use observational constraints on the galactic ionizing photon production, the surface mass distribution of field M dwarfs, and the mass distribution of brown dwarfs in clusters to produce an effective galactic initial mass function (IMF). We assume that the IMF can be expressed as the product of a smooth function of mass m (in units of MΘ),ψ (m), and a time dependent rate. We express the star formation rate per unit area per unit logarithmic mass interval as <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s1.jpg"><img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s8.jpg"><img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s2.jpg">/[dA dln m] <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s8.jpg"><img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s3.jpg" > or = <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s4.jpg">[l - exp - <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s7.jpg">]; for (m < m u ), with <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s5.jpg" > or = 0.8 (the asymptotic low-mass slope inferred from the mass distribution in young clusters at sub-stellar masses), Γ = 1.35 (the negative of the high-mass slope), m ch = 0.24 (producing a maximum at m max~ m ch), and m u = 120. For a disk age of 11 Gyr, the average value of the star formation rate per unit logarithmic mass interval at 1 MΘ at the solar circle is <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s6.jpg">620 kpc-2 Myr-1, and the ratio of the present to the mean SFR is b (t0 ) = 1.085, where t0 is the age of the disk.

Se propone una función inicial de masa efectiva (FIME) para la Galaxia que satisface las siguientes restricciones observacionales: la producción de fotones ionizantes en la Galaxia, la distribución en masa de la densidad superficial de estrellas M y la distribución en masa de Enanas Marrones en asociaciones estelares jóvenes. Se supone que la FIME puede ser expresada como el producto de una función suave de la masa m (en unidades de MΘ), ψ (m) y una tasa dependiente del tiempo. Esta es: <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s1.jpg"><img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s8.jpg"><img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s2.jpg">/ [dA dln m] <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s8.jpg"><img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s3.jpg" > o = <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s4.jpg">[;l - exp - <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s7.jpg">] para (m < m u ), donde <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s5.jpg" > o = 0.8 (pendiente asintótica a masas bajas inferida de la distribución de masa en la región sub-estelar en asociaciones jóvenes), Γ= 1.35 (pendiente asintótica a masas altas), m ch = 0.24 (que produce un máximo a m max ~ m ch), y m u = 120. Para una edad del disco galáctico de 11 Gyr, el valor promedio de la tasa de formación estelar por unidad logarítmica de masa a 1 MΘ en el círculo solar es <img width=32 height=32 src="../../../../../img/revistas/rmf/v52s3/a1s6.jpg">620 kpc-2 Myr-1 y la razón entre la SFR presente y la SFR media es b (t0 ) = 1.085.