Artigos de revistas sobre o tema "Galaxies primitives"

AbstractWe report on a study of 9 nearby primitive galaxies observed by Hubble’s COS far-UV spectrograph that can serve as templates of high-z galaxies to be observed by JWST. By “primitive galaxies,” we mean galaxies having a low stellar mass, and low gas metallicity, , whether they are local or at high redshift. We find that far-UV spectra of these galaxies show evidence of hard radiation, including X-rays. Following Thuan et al. (2004), we identify these galaxies as massive X-ray binaries containing a massive accreting stellar black hole. We further find that the lower the metallicity, the higher the probability of extremely strong X-radiation. Following Heger et al. (2003), we suggest that the accreting black hold is produced by direct collapse of stars having initial masses greater than 50 . The X-radiation produced by black hole disk directly affects the surrounding interstellar medium, and many of these effects are observable in far-UV spectra.

Context. Galaxy evolution and the effect of the environment are most often studied using scaling relations or regression analyses around a given property. However, these approaches do not take into account the complexity of the physics of the galaxies and their diversity. Aims. We here investigate the effect of the cluster environment on the evolution of galaxies through multivariate, unsupervised classification and phylogenetic analyses applied to two relatively large samples from the Wide-field Nearby Galaxy-cluster Survey (WINGS), one of cluster members and one of field galaxies (2624 and 1476 objects, respectively). Methods. These samples are the largest ones ever analysed with a phylogenetic approach in astrophysics. To be able to use the maximum parsimony (cladistics) method, we first performed a pre-clustering in 300 clusters with a hierarchical clustering technique, before applying it to these pre-clusters. All these computations used seven parameters: B − V, log(Re), nV, ⟨μ⟩e, Hβ, D4000, and log(M*). Results. We have obtained a tree for the combined samples and do not find different evolutionary paths for cluster and field galaxies. However, the cluster galaxies seem to have accelerated evolution in the sense that they are statistically more diversified from a primitive common ancestor. The separate analyses show a hint of a slightly more regular evolution of the variables for the cluster galaxies, which may indicate they are more homogeneous compared to field galaxies in the sense that the groups of the latter appear to have more specific properties. On the tree for the cluster galaxies, there is a separate branch that gathers rejuvenated or stripped-off groups of galaxies. This branch is clearly visible on the colour-magnitude diagram, going back from the red sequence towards the blue one. On this diagram, the distribution and the evolutionary paths of galaxies are strikingly different for the two samples. Globally, we do not find any dominant variable able to explain either the groups or the tree structures. Rather, co-evolution appears everywhere, and could depend itself on environment or mass. Conclusions. This study is another demonstration that unsupervised machine learning is able to go beyond simple scaling relations by taking into account several properties together. The phylogenetic approach is invaluable in tracing the evolutionary scenarios and projecting them onto any bivariate diagram without any a priori modelling. Our WINGS galaxies are all at low redshift, and we now need to go to higher redshfits to find more primitive galaxies and complete the map of the evolutionary paths of present day galaxies.

Abstract Massive Population III stars can die as energetic supernovae that enrich the early Universe with metals and determine the properties of the first galaxies. With masses of about 109 M ⊙ at z ≳ 10, these galaxies are believed to be the ancestors of the Milky Way. This paper investigates the impact of Population III supernova remnants (SNRs) from both Salpeter-like and top-heavy initial mass functions (IMFs) on the formation of first galaxies with high-resolution radiation-hydrodynamical simulations with the ENZO code. Our findings indicate that SNRs from a top-heavy Population III IMF produce more metals, leading to more efficient gas cooling and earlier Population II star formation in the first galaxies. From a few hundred to a few thousand Population II stars can form in the central regions of these galaxies. These stars have metallicities of 10−3–10−2, Z ⊙, greater than those of extremely metal-poor (EMP) stars. Their mass function follows a power-law distribution with dN ( M * ) / dM * ∝ M * α , where M * is stellar mass, and α = 2.66–5.83 and is steeper for a top-heavy IMF. We thus find that EMP stars were not typical of most primitive galaxies.

AbstractAn important factor controlling galaxy evolution is feedback from massive stars. It is believed that the nature and intensity of stellar feedback changes as a function of galaxy mass and metallicity. At low mass and metallicity, feedback from massive stars is mainly in the form of photoionizing radiation. At higher mass and metallicity, it is in stellar winds. I Zw 18 is a local blue, compact dwarf galaxy that meets the requirements for a primitive galaxy: low halo mass <109M⊙, strong photoionizing radiation, no galactic outflow, and very low metallicity, log(O/H)+12=7.2. We will describe the properties of massive stars and their role in the evolution of I Zw 18, based on analysis of ultraviolet images and spectra obtained with HST.

This article "The lunar problem is the barrier of the future time of the Earth" is a logical and rational analysis of the formation of the nuclear universe with galaxies, stars, the Sun star, the system of planets and the moons, and arrives at new original and inedited conclusions. The Big Bang of the primitive universe is a sequence programmed by the nature of thermonuclear super explosions in sidereal space. These thermonuclear super explosions swept nuclear sidereal space generating the large mass islands of galaxies like the Milky Way. The Milky Way was the first generation of the hyper-bubbles of the mixture of nuclear masses, which are: geological nuclear mass of attraction of gravity; geological nuclear mass of orbital attraction; geological nuclear mass of orbital repulsion. Because of nuclear hyper tremors, the nucleus of the Milky Way generated the second generation of the super bubbles that were repulsed from the galaxy's nucleus by the action of the geological nuclear mass of orbital repulsion, and then the super bubbles became in the many billions of celestial stars that make up the galactic disc. Because of the hyper tremors, the nucleus of these billions of stars, including the Sun, generated the third generation of super bubbles and large bubbles that were repulsed from the nuclei of the stars by the action of the geological nuclear mass of orbital repulsion, and then the super bubbles and large bubbles have become the sequence of planets, which makes up the orbital disk of the solar system. Due to a small number of nuclear super tremors, the nucleus of the sequence of planets tremble, shook and generated the fourth generation of the small bubbles that were repulsed from the nucleus of the planetary sequence by the action of the geological nuclear mass of orbital repulsion, and then, the small bubbles have become the sequence of moons, which makes up the orbital disk of the planets. And so, began the count the new time, after the sequence of Big Bang explosions.

AbstractGiant molecular clouds (GMCs) are the major reservoirs of molecular gas in galaxies, and the starting point for star formation. As such, their properties play a key role in setting the initial conditions for the formation of stars. We present a comprehensive combined inteferometric/single-dish study of the resolved GMC properties in a number of extragalactic systems, including both normal and dwarf galaxies. We find that the extragalactic GMC properties measured across a wide range of environments, characterized by the Larson relations, are to first order remarkably compatible with those in the Milky Way. Using these data to investigate trends due to galaxy metallicity, we find that: 1) these measurements are not in accord with simple expectations from photoionization-regulated star formation theory; 2) there is no trend in the virial CO-to-H2conversion factor on the spatial scales studied; and 3) there are measurable departures from the Galactic Larson relations in the Small Magellanic Cloud — the object with the lowest metallicity in the sample — where GMCs have velocity dispersions that are too small for their sizes. We will discuss the stability of these clouds in the light of our recent far-infrared analysis of this galaxy, and will contrast the results of the virial and far-infrared studies on the issue of the CO-to-H2conversion factor and what they tell us about the structure of molecular clouds in primitive galaxies.

Context. It is thought that fossil systems are relics of structure formation in the primitive Universe. They are galaxy aggregations that have assembled their mass at high redshift with few or no subsequent accretion. Observationally these systems are selected by large magnitude gaps between their 1st and 2nd ranked galaxies (Δm12). Nevertheless, there is still debate over whether or not this observational criterium selects dynamically evolved ancient systems. Aims. We have studied the properties of the nearby fossil group RX J075243.6+455653 in order to understand the mass assembly of this system. Methods. Deep spectroscopic observations allow us to construct the galaxy luminosity function (LF) of RX J075243.6+455653 down to Mr*+6. The analysis of the faint-end of the LF in groups and clusters provides valuable information about the mass assembly of the system. In addition, we have analyzed the nearby large-scale structure around this group. Results. We identified 26 group members within r200 ~ 0.96 Mpc. These galaxies are located at Vc = 15551 ± 65 km s-1 and have a velocity dispersion of σc = 333 ± 46 km s-1. The X-ray luminosity of the group is LX = 2.2 × 1043 h70-2 erg s-1, resulting in a mass of M = 4.2 × 1013 h70-1 within 0.5r200. The group has Δm12 = 2.1 within 0.5r200, confirming the fossil nature of this system. RX J075243.6+455653 has a central brightest group galaxy (BGG) with Mr = −22.67, one of the faintest BGGs observed in fossil systems. The LF of the group shows a flat faint-end slope (α = −1.08 ± 0.33). This low density of dwarf galaxies is confirmed by the low value of the dwarf-to-giant ratio (DGR = 0.99 ± 0.49) for this system. Both the lack of dwarf galaxies and the low luminosity of the BGG suggests that RX J075243.6+455653 still has to accrete mass from its nearby environment. This mass accretion will be achieved because it is the dominant structure of a rich environment formed by several groups of galaxies (15) within ~ 7 Mpc from the group center and with ± 1000 km s-1. Conclusions. RX J075243.6+455653 is a group of galaxies that has not yet completed the process of its mass assembly. This new mass accretion will change the fossil state of the group. This group is an example of a galaxy aggregation selected by a large magnitude gap but still in the process of the accretion of its mass.

The possibility that life, primitive or advanced, might exist in other places of the Universe has occupied the minds of scientists and lay-people for thousands of years. It is only in the last 25 years, however, that we have finally begun to search for answers to this profound question using experimental techniques. The goal of Astronomy is to understand the origin and evolution of planets, stars, galaxies and of the Universe as a whole. The appearance of life is an integral part of this whole process and our picture of the Universe will never be complete until we will comprehend also the significance of life in the process of Cosmic Evolution.

AbstractMassive Population III stars die as pair-instability supernovae (PI SNe), the most energetic thermonuclear explosions in the universe with energies up to 100 times those of Type Ia or Type II SNe. Their extreme luminosities may allow them to be observed from the earliest epochs, revealing the nature of Pop III stars and the primitive galaxies in which they reside. We present numerical simulations of Pop III PI SNe done with the radiation hydrodynamics code RAGE and calculations of their light curves and spectra performed with the SPECTRUM code. We find that 150 - 250 M⊙ PI SNe will be visible to the James Webb Space Telescope (JWST) out to z ~ 30 and to z ~ 15 - 20 in all-sky NIR surveys by the Wide Field Infrared Survey Telescope (WFIRST).

The James Webb Space Telescope (JWST) has made startling discoveries regarding the early universe. It has revealed galaxies as soon as 300 million years after the Big Bang, challenging current galaxy formation models. Additionally, it has identified massive, bright galaxies in the young universe, contradicting the standard ΛCDM model&apos;s age estimate of 13.8 Gyr. This prompts a re-evaluation of galaxy formation and cosmological models. There is a strong tension between JWST high-redshift galaxy observations and Planck Cosmic Microwave Background (CMB) satellite measurements. Even alternative cosmological models, including those incorporating dark matter–baryon interaction, f(R) gravity, and dynamical dark have failed to resolve this tension. One possible solution is that the Universe&apos;s age exceeds predictions by the ΛCDM model. The study challenges this by introducing a method based on blue straggler stars (BSs) within GCs, comparing ages with other models. The ages obtained are compared with those of other models to certify that they are equally valid. These values are comparable within the error ranges except for the clusters: NGC104, NGC 5634, IC 4499, NGC 6273 and NGC 4833, finding their respective ages to be between 14.7 and 21.6 Gyr, surpassing the commonly accepted age of the Universe. These results inferred an age for the Universe of around 26 Gyr, close to 26.7 Gyr. This value aligns that suggested by the cosmological model named Covarying Coupling Constants + TL (CCC+TL). Such a value is consistent with early universe observations from the James Webb Space Telescope (JWST). The results of the present paper reinforces the advocating for a critical review of models encompassing dark mass, dark energy, and the dynamics of the Universe, particularly in explaining the presence of primitive massive galaxies, very old GCs, and very old and poor metallic stars.

Everything in the universe is movable or being moved, starting from galaxies and planets to the smallest object, such as the atom. But how can we conceptualize the motion of such entities and what are the basic elements of sequential scene? To do that, a theory of the sequential schematic scene-building has developed to treat this issue. This theory deals with the basic dynamic, on-line, or real-time perceptual processes by which we build a scene. The study focuses on the schematic, not conceptual, elements of sequential scenes which deal with the highly abstracted, primitive system. Such system is considered as the skeleton or building blocks of any sequential scene. To make the theory more applicable, the study selects a scene from Dan Brown’s The Da Vinci Code to be analyzed in terms of the theory developed. The study arrived at a conclusion that the moveable scene can include a group of sequential schematic structures, such as the mover, motion, causality, geometrical structures, and containment. All these elements work together sequentially in the sense that they are inherently consolidated.

The article analyzes the phenomena of ethnicity and tradition in the context of the development of society from the traditional type to the globalised one. In the conducted analysis of various approaches to their interpretation, the vulnerable positions of such trends as primordialism, constructivism, and instrumentalism are considered. As an alternative, helping to eliminate controversial points, an attempt is made to use the theories of M.G. Мakljuen and M. Castells. Application of the paradigm of informationalism provides an opportunity to use the optics of communication to analyse the transformation of the semantic and functional content of the cultural/ethnic tradition in the life of society. The influence of the evolution of mass media on the existence of a cultural tradition can be traced within the framework of various social systems: a primitive tribal community and an agrarian society; industrial and post-industrial; globalized and digital society. A comparative analysis of the characteristic features of the social development of each of the types of societies is intended to reveal the factors influencing the transformation of the functional and semantic continuum of traditional/ethnic culture in different eras. Among essential aspects of these changes are the following: changing the role and function of traditional culture in the life of society; transformation of subject-object relations in the communication field that forms ideas about ethnicity and tradition. This, in turn, significantly affects the identification processes at the personal and group levels of the modern society.

Infrared astronomy, particularly in spectroscopy, could benefit in a decisive way from an implementation of telescopes on the Moon since the largest telescopes on Earth are practically limited to 40 m and in space to 10 m. On the Moon, a collector larger than on Earth becomes conceivable, thanks to the low gravity and the absence of wind, in having the advantages of space. Passively cooled in the bottom of a permanently shadowed crater at the northern or the southern pole, it could reach unprecedented spectral sensitivity on a large part of the infrared domain, making possible spectral analysis of the most primitive galaxies and of the terrestrial exoplanet atmospheres. A project aiming at the detection of the weak cosmic microwave background spectral distortions is also presented. Several identical 1.5 m cryo-cooled telescopes at 2.5 K to fit in a launcher, with an imaging Fourier transform spectrometer in each unit, deposited in a cold crater and pointing in the same direction in lunar survey mode, would build for this fundamental goal the equivalent of a large telescope at an extremely low temperature. Last, the feasibility of these projects is discussed. This article is part of a discussion meeting issue ‘Astronomy from the Moon: the next decades'.

AbstractVery metal-poor stars ([Fe/H] &lt; –2.0) inform our understanding of the formation and evolution of the Galaxy, and the physical conditions in the earliest star-forming environments of the Universe. They play an integral part in the paradigms of stellar populations, stellar archaeology, and near-field cosmology. We review the carbon-rich and carbon-normal sub-populations of the most iron-poor stars, providing insight into chemical enrichment at the earliest times in the Universe. We also discuss the role of very metal-poor stars in providing insight into the Galaxy’s halo, thick disk, and bulge, and the promise they hold for the future. A comparison between the abundances obtained for the nine most Fe-poor stars ([Fe/H] &lt; –4.5) (all but one of which is C-rich) with abundances obtained from far-field cosmology suggests that the former are the most chemically primitive objects yet observed and probably older than the DLA- and sub-DLA systems for which data are currently available from far-field studies.

An inspection of the contemporary physics literature reveals that, while matter is treated at all levels of study, from Newtonian mechanics to quantum field theory, antimatter is solely treated at the level of second quantization. For the purpose of initiating the restoration of full equivalence in the treatment of matter and antimatter in due time, and as the classical foundations of an axiomatically consistent inclusion of gravitation in unified gauge theories recently appeared elsewhere, in this paper we present a classical representation of antimatter which begins at the primitive Newtonian level with corresponding formulations at all subsequent levels. By recalling that charge conjugation of particles into antiparticles is antiautomorphic, the proposed theory of antimatter is based on a new map, called isoduality, which is also antiautomorphic (and more generally, antiisomorphic), yet it is applicable beginning at the classical level and then persists at the quantum level where it becomes equivalent to charge conjugation. We therefore present, apparently for the first time, the classical isodual theory of antimatter, we identify the physical foundations of the theory as being the novel isodual Galilean, special and general relativities, and we show the compatibility of the theory with all available classical experimental data on antimatter. We identify the classical foundations of the prediction of antigravity for antimatter in the field of matter (or vice-versa) without any claim on its validity, and defer its resolution to specifically identified experiments. We identify the novel, classical, isodual electromagnetic waves which are predicted to be emitted by antimatter, the so-called space–time machine based on a novel non-Newtonian geometric propulsion, and other implications of the theory. We also introduce, apparently for the first time, the isodual space and time inversions and show that they are nontrivially different than the conventional ones, thus offering a possibility for the future resolution whether far away galaxies and quasars are made up of matter or of antimatter. The paper ends with the indication that the studies are at their first infancy, and indicates some of the open problems. To avoid a prohibitive length, the paper is restricted to the classical treatment, while studies on operator profiles are treated elsewhere.

RESUMENEste artículo propone un recorrido a través de la figura del pensador de la Baja Edad Media a la Ilustración. Publicada en 1621, la Anatomía de la melancolía de Robert Burton dibuja la imagen del filósofo nuevo, opuesto a los desvergonzados filosofastros que daban título a la comedia de 1615. Demócrito Júnior supone la confirmación de la nueva figura intelectual que ha dejado atrás al clerc de la Baja Edad Media: el humanista del Renacimiento que, gracias a la rehabilitación llevadaa cabo por Marsilio Ficino del mal de la bilis negra, confiesa con orgullo su carácter melancólico, propio del genio fuera de lo común. Su sucesor, el philosophe del siglo XVIII ya no necesita acudir a la afección atrabiliaria para postularse como el guía que ha de conducir y domesticar al pueblo.PALABRAS CLAVE: melancolía, filosofastros, época moderna, philosophe, pueblo.ABSTRACTThis article proposes a journey through the figure of the thinker from the late Middle Ages to the Enlightenment. Published in 1621, Robert Burton’s Anatomy of Melancholy depicts the image of the new philosopher as opposed to those shameless philosophasters, to which the title of his 1615 comedy refers. Democritus Junior embodies the confirmation of the new intellectual figure that has abandoned the clerc of the late Middle Ages: that Renaissance humanist who, thanks to Marsilio Ficino’s rehabilitation of the malady of the black bile, proudly confesses his melancholiccharacter, typical of extraordinary geniuses. His successor, the 18th century philosophe, no longer needs to resort to bad-tempered humour in order to present himself as the guide destined to direct and domesticate common people.KEY WORDS: melancholy, philosophasters, early modern period, philosophe, common people.BIBLIOGRAFÍAAgamben, G., Stanze. 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Abstract Recent studies on dwarf galaxies reveal that some of them harbor a massive black hole (BH), which is believed to have a similar mass of the Supermassive BH ‘seeds’ at early times. The origin and growth of the primitive BHs are still open questions, since these BH seeds are hardly observed at high redshifts. Therefore, massive BH of dwarf galaxies can be the perfect candidates to untangle BH ‘seeds’ properties and their influence on their host galaxy evolution, since massive BH may preserve their initial conditions due to its quiet merger and accretion histories. We use optical integral field unit observations, obtained with the Gemini GMOS-IFU, to study the gas emission and kinematics in four dwarf galaxies, candidates to host massive BH, based on the analysis of their [Fe x] luminosities measured from SDSS spectra. The [Fe x] emission line is not detected in our GMOS in any of the galaxies, prompting speculation that its absence in our recent data may stem from a past tidal disruption event coinciding with the observation period of the SDSS data. All galaxies exhibit extended gas emissions, and the spatially resolved emission-line ratio diagnostic diagrams present values that suggest AGN photoionization from the [S ii] – BPT diagram. The gas velocity fields of all galaxies are indicative of disturbed rotation patterns, with no detection of gas outflows in any of the sources. Although the [S ii] – BPT diagrams indicate AGN photoionization, further confirmation through multi-wavelength observations is required to validate this scenario.