The dependence of the galaxy stellar-to-halo mass relation on galaxy morphology

We investigate the dependence of the local galaxy stellar-to-halo mass relation (SHMR) on galaxy morphology. We use data from the Sloan Digital Sky Survey DR7 with morphological classifications from Galaxy Zoo, and compare with the EAGLE cosmological simulation. At fixed halo mass in the mass range $10^{11.7}-10^{12.9}M_{\odot}$, the median stellar masses of SDSS disc galaxies are up to a factor of 1.4 higher than the median masses of their elliptical counterparts. However, when we switch from the stellar masses from Kauffmann et al. to those calculated by Chang et al. or Brinchmann et al., the median SHMR from discs and ellipticals coincide in this mass range. For halo masses larger than $10^{13}M_{\odot}$, discs are less massive than ellipticals in same-mass haloes, regardless of whose stellar mass estimates we use. However, we find that for these high halo masses the results for discs may be affected by central/satellite misclassifications. The EAGLE simulation predicts that discs are up to a factor of 1.5 more massive than elliptical galaxies residing in same-mass haloes less massive than $10^{13}M_{\odot}$, in agreement with the Kauffmann et al. data. Haloes with masses between $10^{11.5}$ and $10^{12}M_{\odot}$, that host disc galaxies, were assembled earlier than those hosting ellipticals. This suggests that the discs are more massive because they had more time for gas accretion and star formation. In $10^{12}-10^{12.5}M_{\odot}$ haloes, the central black holes in elliptical galaxies grew faster and became more massive than their counterparts in disc galaxies. This suggests that in this halo mass range the ellipticals are less massive because AGN feedback ejected more of the halo's gas reservoir, reducing star formation, and suppressing the (re)growth of stellar discs.Comment: Accepted for publication in MNRAS, 18 pages, 16 figures. Comments welcome

An analysis of a regular black hole interior model

We analyze the thermodynamical properties of the regular static and spherically symmetric black hole interior model presented by Mboyne and Kazanas. Equations for the thermodynamical quantities valid for an arbitrary density profile are deduced, and from them we show that the model is thermodynamically unstable. Evidence is also presented pointing to its dynamical instability. The gravitational entropy of this solution based on the Weyl curvature conjecture is calculated, following the recipe given by Rudjord, Gr$\varnothing$n and Sigbj$\varnothing$rn, and it is shown to have the expected behavior.Comment: 22 pages, 17 figures, accepted for publication in International Journal of Theoretical Physic

Influence of local structure on relic neutrino abundances and anisotropies

Gravitational potentials of the Milky Way and extragalactic structures can influence the propagation of the cosmic neutrino background (CNB). Of particular interest to future CNB observatories, such as PTOLEMY, is the CNB number density on Earth. In this study, we have developed a simulation framework that maps the trajectories of relic neutrinos as they move through the local gravitational environment. The potentials are based on the dark matter halos found in state-of-the-art cosmological N-body simulations, resulting in a more nuanced and realistic input than the previously employed analytical models. We find that the complex dark matter distributions, along with their dynamic evolution, influence the abundance and anisotropies of the CNB in ways unaccounted for by earlier analytical methods. Importantly, these cosmological simulations contain multiple instances of Milky Way-like halos that we employ to model a variety of gravitational landscapes. Consequently, we notice a variation in the CNB number densities that can be primarily attributed to the differences in the masses of these individual halos. For neutrino masses between $0.01$ and $0.3$ eV, we note clustering factors within the range of $1+\mathcal{O}(10^{-3})$ to $1+\mathcal{O}(1)$. Furthermore, the asymmetric nature of the underlying dark matter distributions within the halos results in not only overdense, but intriguingly, underdense regions within the full-sky anisotropy maps. Gravitational clustering appears to have a significant impact on the angular power spectra of these maps, leading to orders of magnitude more power on smaller scales beyond multipoles of $\ell = 3$ when juxtaposed against predictions by primordial fluctuations. We discuss how our results reshape our understanding of relic neutrino clustering and how this might affect observability of future CNB observatories such as PTOLEMY.Comment: 25 pages, 10 figures, comments are welcom

Warm Dark Matter Constraints Using Milky-Way Satellite Observations and Subhalo Evolution Modeling

Warm dark matter (WDM) can potentially explain small-scale observations that currently challenge the cold dark matter (CDM) model, as warm particles suppress structure formation due to free-streaming effects. Observing small-scale matter distribution provides a valuable way to distinguish between CDM and WDM. In this work, we use observations from the Dark Energy Survey and PanSTARRS1, which observe 270 Milky-Way satellites after completeness corrections. We test WDM models by comparing the number of satellites in the Milky Way with predictions derived from the Semi-Analytical SubHalo Inference ModelIng (SASHIMI) code, which we develop based on the extended Press-Schechter formalism and subhalos' tidal evolution prescription. We robustly rule out WDM with masses lighter than 4.4 keV at 95% confidence level for the Milky-Way halo mass of $10^{12} M_\odot$. The limits are a weak function of the (yet uncertain) Milky-Way halo mass, and vary as $m_{\rm WDM}>3.6$-$5.1$ keV for $(0.6$-$2.0) \times 10^{12} M_\odot$. For the sterile neutrinos that form a subclass of WDM, we obtain the constraints of $m_{\nu_s}>11.6$ keV for the Milky-Way halo mass of $10^{12} M_{\odot}$. These results based on SASHIMI do not rely on any assumptions of galaxy formation physics or are not limited by numerical resolution. The models, therefore, offer a robust and fast way to constrain the WDM models. By applying a satellite forming condition, however, we can rule out the WDM mass lighter than 9.0 keV for the Milky-Way halo mass of $10^{12} M_\odot$.Comment: 14 pages, 8 figures; Comments welcome. v2: Accepted for publication in PR

Expresión diferencial de genes en Pyropia columbina (Bangiales, Rhodophyta) bajo hidratación y desecación natural

Indexación: Web of Science; Scielo.RESUMEN. En Zonas Costeras rocosas, la desecación es gatillada porción Cambios Diarios en los Niveles de marea, y la Evidencia indica experimental de Me Distribución de las algas en la zona intermareal no está Relacionada estafa do palabra capacidad, párr tolerar la desecación. En Este Contexto, la Presencia de Pyropia columbina en la zona alta del intermareal sí Explica Por Su excepcional tolerancia fisiológica a la desecación. Este Estudio explora las Vías Metabólicas involucradas en la tolerancia a la desecación en P. columbina, un Través de la Caracterización de do transcriptoma Bajo Condiciones de hidratación contrastantes. Se obtuvó 1410 TER provenientes de dos Librerías de substracción de ADNc de frondas Naturalmente hidratadas y desecadas. Los transcriptomas de emba Librerías contienen transcritos de Diversas Rutas Metabólicas Relacionadas a la tolerancia. Entre el los transcritos expresados ​​15% estan involucrados en la Síntesis de Proteínas, do Procesamiento y degradacion, 14,4% Asociados un Fotosíntesis y cloroplasto, el 13,1% una mitocondrial Respiración and function, 10,6% al metabolism de la Pared Celular y 7,5% a la Actividad ANTIOXIDANTE, Proteínas chaperonas y factors de Defensa (catalasa, tiorredoxina, Proteínas de choque térmico, P450 citocromo). In Ambás Librerías sí DESTACA La Presencia De genes / Proteínas no descritos en algas. Proporciona Información This El Primer Trabajo molecular Que Estudia la tolerancia a desecación en P. columbina y Sus Resultados Ayudan a explicar los patrones clásicos de Distribución descritos párr algas en la zona intermareal. Palabras clave: Pyropia, desecación porción Estrés, EST, macroalgas, transcriptómica, Proteínas.ABSTRACT. In rocky shores, desiccation is triggered by daily tide changes, and experimental evidence suggests that local distribution of algal species across the intertidal rocky zone is related to their capacity to tolerate desiccation. In this context, the permanence of Pyropia columbina in the high intertidal rocky zone is explained by its exceptional physiological tolerance to desiccation. This study explored the metabolic pathways involved in tolerance to desiccation in the Chilean P. columbina, by characterizing its transcriptome under contrasting conditions of hydration. We obtained 1,410 ESTs from two subtracted cDNA libraries in naturally hydrated and desiccated fronds. Results indicate that transcriptome from both libraries contain transcripts from diverse metabolic pathways related to tolerance. Among the transcripts differentially expressed, 15% appears involved in protein synthesis, processing and degradation, 14.4% are related to photosynthesis and chloroplast, 13.1% to respiration and mitochondrial function (NADH dehydrogenase and cytochrome c oxidase proteins), 10.6% to cell wall metabolism, and 7.5% are involved in antioxidant activity, chaperone and defense factors (catalase, thioredoxin, heat shock proteins, cytochrome P450). Both libraries highlight the presence of genes/proteins never described before in algae. This information provides the first molecular work regarding desiccation tolerance in P. columbina, and helps, to some extent, explaining the classical patterns of ecological distribution described for algae across the intertidal zone.http://ref.scielo.org/jm5rc

The effect of gas accretion on the radial gas metallicity profile of simulated galaxies

We study the effect of the gas accretion rate (M˙ accr) on the radial gas metallicity profile (RMP) of galaxies using the EAGLE cosmological hydrodynamic simulations, focusing on central galaxies of stellar mass M 109 M at z ≤ 1. We find clear relations between M˙ accr and the slope of the RMP (measured within an effective radius), where higher M˙ accr are associated with more negative slopes. The slope of the RMPs depends more strongly on M˙ accr than on stellar mass, star formation rate (SFR), or gas fraction, suggesting M˙ accr to be a more fundamental driver of the RMP slope of galaxies. We find that eliminating the dependence on stellar mass is essential for pinning down the properties that shape the slope of the RMP. Although M˙ accr is the main property modulating the slope of the RMP, we find that it causes other correlations that are more easily testable observationally: At fixed stellar mass, galaxies with more negative RMP slopes tend to have higher gas fractions and SFRs, while galaxies with lower gas fractions and SFRs tend to have flatter metallicity profiles within an effective radius.Fil: Collacchioni, Florencia. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Lagos, Claudia D.P.. University of Western Australia; Australia. Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions; Australia. Universidad de Copenhagen; DinamarcaFil: Mitchell, Peter D.. Leiden University; Países Bajos. Université Claude Bernard Lyon 1; FranciaFil: Schaye, Joop. Leiden University; Países BajosFil: Wisnioski, Emily. Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions; Australia. Australian National University. Research School of Astronomy and Astrophysics; AustraliaFil: Cora, Sofia Alejandra. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Correa, Camila A.. Leiden University; Países Bajo

Effects of oxidative stress during human and animal reproductions: A review

Given its high ability to damage important cellular components (lipids, proteins and deoxyribonucleic acid), oxidative stress is now recognized as one of the most common mechanisms associated with development of a variety of diseases and natural events such as pregnancy. During reproduction period, there is a change in the pro-oxidant and antioxidant balance due to the body and circulation modifications that are inherent to the pregnancy process. The present paper discusses the role of oxidative stress on the reproduction process. More effective defense strategies are needed to decrease the deleterious effects of oxidative-stress-induced gestation. This approach could be achieved by antioxidant status alteration. Further clinical and experimental studies are needed for better understanding of oxidative stress mechanism and the impact of antioxidant supplementation on reproduction

ESTILOS DE VIDA DE ESTUDIANTES UNIVERSITARIOS DE CIENCIAS DE LA SALUD

Objetivos: El objetivo de este artículo es realizar una revisión de las publicaciones que revelen el impacto de los estilos de vida en la salud integral de estudiantes universitarios del área ciencias de la salud. Métodos : La revisión fue efectuada mediante búsqueda electrónica de artículos relacionados con estilos de vida en estudiantes universitarios pertenecientes a las escuelas de ciencias de la salud. Las fuentes de búsqueda fueron ISI, SCIELO, MEDLINE, BVS y PUBMED. Los términos de búsqueda fueron: estilo de vida, estudiantes universitarios y ciencias de la salud. Para esta revisión se seleccionaron los artículos publicados que tuvieron experiencias investigativas desde el 2010 a la actualidad y los que incluyeron aspectos teórico-conceptuales se consideró los publicados desde el año 2000. Resultados: De los 83 artículos revisados, se descartaron 38 por no cumplir con el criterio de haber realizado la investigación en el área de ciencias de la salud, y 12 fueron retirados por ser publicados antes del 2010, quedando solo 33 artículos para esta revisión bibliográfica. De los 33 artículos seleccionados, 18 estudios cumplieron con los criterios de investigación, 15 fueron considerados para incluir aspectos teórico – conceptuales. Respecto a la actividad física, un estudio evidenció que el 40% de los jóvenes universitarios no realiza ningún ejercicio físico; otra investigación demostró que solo el 44% de los estudiantes de ciencias de la salud practicaban los recomendados 30 minutos de ejercicio 5 días por semana. Además los patrones alimentarios de los estudiantes fueron inadecuados, haciéndose necesario un cambio en el 90% de la población, siendo la “comida chatarra” la que más consumieron los participantes. Por otro lado, los datos de un estudio revelaron que 1 de cada 5 de los estudiantes universitarios presentan alteraciones en su salud mental y el consumo de tabaco y/o drogas, aparece como factor de riesgo. Conclusión: La mayoría de los estudiantes universitarios de ciencias de la salud no aplican sus conocimientos en sus propios estilos de vida (alimentación, actividad física y demás prácticas). Esto revela la urgencia de crear programas universitarios que modifiquen y promuevan estilos de vida saludable. DOI:https://doi.org/10.25176/RFMH.v16.n2.67