Galactic conformity measured in semi-analytic models

We study the correlation between the specific star formation rate of central galaxies and neighbour galaxies, also known as 'galactic conformity', out to 20 Mpc/h using three semi-analytic models (SAMs, one from L-GALAXIES and other two from GALFORM). The aim is to establish whether SAMs are able to show galactic conformity using different models and selection criteria. In all the models, when the selection of primary galaxies is based on an isolation criterion in real space, the mean fraction of quenched galaxies around quenched primary galaxies is higher than that around star-forming primary galaxies of the same stellar mass. The overall signal of conformity decreases when we remove satellites selected as primary galaxies, but the effect is much stronger in GALFORM models compared with the L-GALAXIES model. We find this difference is partially explained by the fact that in GALFORM once a galaxy becomes a satellite remains as such, whereas satellites can become centrals at a later time in L-GALAXIES. The signal of conformity decreases down to 60% in the L-GALAXIES model after removing central galaxies that were ejected from their host halo in the past. Galactic conformity is also influenced by primary galaxies at fixed stellar mass that reside in dark matter haloes of different masses. Finally, we explore a proxy of conformity between distinct haloes. In this case the conformity is weak beyond ~ 3 Mpc/h (<3% in L-GALAXIES, <1-2% in GALFORM models). Therefore, it seems difficult that conformity is directly related with a long-range effect.Comment: 15 pages, 7 figures. Accepted for publication in MNRA

Not Hydro: Using Neural Networks to estimate galaxy properties on a Dark-Matter-Only simulation

Using data from TNG300-2, we train a neural network (NN) to recreate the stellar mass ($M^*$) and star formation rate (SFR) of central galaxies in a dark-matter-only simulation. We consider 12 input properties from the halo and sub-halo hosting the galaxy and the near environment. $M^*$ predictions are robust, but the machine does not fully reproduce its scatter. The same happens for SFR, but the predictions are not as good as for $M^*$. We chained neural networks, improving the predictions on SFR to some extent. For SFR, we time-averaged this value between $z=0$ and $z=0.1$, which improved results for $z=0$. Predictions of both variables have trouble reproducing values at lower and higher ends. We also study the impact of each input variable in the performance of the predictions using a leave-one-covariate-out approach, which led to insights about the physical and statistical relation between input variables. In terms of metrics, our machine outperforms similar studies, but the main discoveries in this work are not linked with the quality of the predictions themselves, but to how the predictions relate to the input variables. We find that previously studied relations between physical variables are meaningful to the machine. We also find that some merger tree properties strongly impact the performance of the machine. %We highlight the value of machine learning (ML) methods in helping understand the information contained in different variables, since with its help we were able to obtain useful insights resulting from studying the impact of input variables on the resulting behaviour of galaxy properties. We conclude that ML models are useful tools to understand the significance of physical different properties and their impact on target characteristics, as well as strong candidates for potential simulation methods.Comment: 17 pages, 16 figures, to be published in MNRA

Automated detection of filaments in the large scale structure of the universe

We present a new method to identify large scale filaments and apply it to a cosmological simulation. Using positions of haloes above a given mass as node tracers, we look for filaments between them using the positions and masses of all the remaining dark-matter haloes. In order to detect a filament, the first step consists in the construction of a backbone linking two nodes, which is given by a skeleton-like path connecting the highest local dark matter (DM) density traced by non-node haloes. The filament quality is defined by a density and gap parameters characterising its skeleton, and filament members are selected by their binding energy in the plane perpendicular to the filament. This membership condition is associated to characteristic orbital times; however if one assumes a fixed orbital timescale for all the filaments, the resulting filament properties show only marginal changes, indicating that the use of dynamical information is not critical for the method. We test the method in the simulation using massive haloes($M>10^{14}$h$^{-1}M_{\odot}$) as filament nodes. The main properties of the resulting high-quality filaments (which corresponds to $\simeq33$ of the detected filaments) are, i) their lengths cover a wide range of values of up to $150$h$^{-1}$Mpc, but are mostly concentrated below 50h$^{-1}$Mpc; ii) their distribution of thickness peaks at $d=3.0$h$^{-1}$Mpc and increases slightly with the filament length; iii) their nodes are connected on average to $1.87\pm0.18$ filaments for $\simeq 10^{14.1}M_{\odot}$ nodes; this number increases with the node mass to $\simeq 2.49\pm0.28$ filaments for $\simeq 10^{14.9}M_{\odot}$ nodes.Comment: 17 pages, 13 figures, MNRAS Accepte

Fecal microbiota transplantation

Fecal microbiota transplantation (FMT) represents the most promising free-antibiotic therapy in the management of patients with infection by Clostridium difficile, recurrent or refractory to treatment with antibiotics. FMT’s superiority over conventional treatment has been proven in multiple series of cases and recently in experimental prospective randomized clinical trials with a resolution of the infection in over 90% of patient

Clustering and descendants of MUSYC galaxies at z<1.5

We measure the evolution of galaxy clustering out to a redshift of z~1.5 using data from two MUSYC fields, the Extended Hubble Deep Field South (EHDF-S) and the Extended Chandra Deep Field South (ECDF-S). We use photometric redshift information to calculate the projected-angular correlation function, omega(sigma), from which we infer the projected correlation function Xi(sigma). We demonstrate that this technique delivers accurate measurements of clustering even when large redshift measurement errors affect the data. To this aim we use two mock MUSYC fields extracted from a LambdaCDM simulation populated with GALFORM semi-analytic galaxies which allow us to assess the degree of accuracy of our estimates of Xi(sigma) and to identify and correct for systematic effects in our measurements. We study the evolution of clustering for volume limited subsamples of galaxies selected using their photometric redshifts and rest-frame r-band absolute magnitudes. We find that the real-space correlation length r_0 of bright galaxies, M_r<-21 (rest-frame) can be accurately recovered out to z~1.5, particularly for ECDF-S given its near-infrared photometric coverage. There is mild evidence for a luminosity dependent clustering in both fields at the low redshift samples (up to =0.57), where the correlation length is higher for brighter galaxies by up to 1Mpc/h between median rest-frame r-band absolute magnitudes of -18 to -21.5. As a result of the photometric redshift measurement, each galaxy is assigned a best-fit template; we restrict to E and E+20%Sbc types to construct subsamples of early type galaxies (ETGs). Our ETG samples show a strong increase in r_0 as the redshift increases, making it unlikely (95% level) that ETGs at median redshift z_med=1.15 are the direct progenitors of ETGs at z_med=0.37 with equivalent passively evolved luminosities. (ABRIDGED)Comment: 16 pages, 12 figures, 2 tables, accepted for publication in MNRA

The ALMA Frontier Fields Survey - IV. Lensing-corrected 1.1 mm number counts in Abell 2744, MACSJ0416.1-2403 and MACSJ1149.5+2223

[abridged] Characterizing the number counts of faint, dusty star-forming galaxies is currently a challenge even for deep, high-resolution observations in the FIR-to-mm regime. They are predicted to account for approximately half of the total extragalactic background light at those wavelengths. Searching for dusty star-forming galaxies behind massive galaxy clusters benefits from strong lensing, enhancing their measured emission while increasing spatial resolution. Derived number counts depend, however, on mass reconstruction models that properly constrain these clusters. We estimate the 1.1 mm number counts along the line of sight of three galaxy clusters, i.e. Abell 2744, MACSJ0416.1-2403 and MACSJ1149.5+2223, which are part of the ALMA Frontier Fields Survey. We perform detailed simulations to correct these counts for lensing effects. We use several publicly available lensing models for the galaxy clusters to derive the intrinsic flux densities of our sources. We perform Monte Carlo simulations of the number counts for a detailed treatment of the uncertainties in the magnifications and adopted source redshifts. We find an overall agreement among the number counts derived for the different lens models, despite their systematic variations regarding source magnifications and effective areas. Our number counts span ~2.5 dex in demagnified flux density, from several mJy down to tens of uJy. Our number counts are consistent with recent estimates from deep ALMA observations at a 3$\sigma$ level. Below $\approx$ 0.1 mJy, however, our cumulative counts are lower by $\approx$ 1 dex, suggesting a flattening in the number counts. In our deepest ALMA mosaic, we estimate number counts for intrinsic flux densities $\approx$ 4 times fainter than the rms level. This highlights the potential of probing the sub-10 uJy population in larger samples of galaxy cluster fields with deeper ALMA observations.Comment: 19 pages, 14 figures, 3 tables. Accepted for publication in A&

Musicoterapia en una Unidad de Cuidados Intensivos Neonatales: experiencia benéfica para el binomio

ResumenIntroducciónDesde hace varios años se está utilizando la música como herramienta terapéutica y preventiva en la neonatología, se han documentado en un gran número de artículos de investigación, sin embargo, en México esta técnica es poco utilizada.ObjetivoMejorar las condiciones de los neonatos atendidos en una Unidad de Cuidados Intensivos (UCIN) y sus familiares, mediante el uso de musicoterapia, para minimizar el estrés y los daños colaterales.Materiales y métodosUn grupo de 2 neonatólogos, 3 residentes de pediatría, 10 enfermeras y un concertista profesional de violín, llevaron a cabo 6 sesiones musicales semanales en la Unidad de Cuidados Intensivos Neonatales Externos del Hospital Civil de Guadalajara. Durante el concierto se valoró individualmente a cada neonato, registrando los signos vitales por monitorización electrónica, además se registró el estado anímico de los familiares.ResultadosDurante las sesiones de música los neonatales no presentaron cambios significativos en sus constantes vitales, en el personal de la UCIN y en los padres de recién nacidos hospitalizados se vieron efectos benéficos, refiriendo disminución del estrés y altos índices de satisfacción.ConclusionesLa música puede tener un efecto positivo como terapia coadyuvante en neonatos de alto riesgo, principalmente en prematuros. Se recomienda difundir y aplicar esta metodología en las UCIN del país.AbstractIntroductionSince several years ago, music has been used as a therapeutic and preventive tool in neonatology. A great number of research papers have been written on the subject; however, this technique is rarely used in Mexico.ObjectiveTo improve the condition of neonates at Neonatal Intensive Care Units (NICU) and their relatives, in order to minimize any stress and collateral damage.Material and methods: A group of two neonatologists, 3 residents, 10 nurses and a professional concert violinist, conducted six weekly music sessions in the Outpatient Neonatal Intensive Care Unit (ONICU) of our institution. During the concert, we individually assessed each newborn, recording vital signs through electronic monitoring; additionally, we recorded the mood of any other family members present.ResultsDuring the music sessions, the neonatal patients showed no significant changes in vital signs; yet, ONICU staff and the parents/relatives of hospitalized newborns showed beneficial effects, reporting decreased stress and high levels of satisfaction.ConclusionsMusic can have a positive effect as adjunctive therapy in high-risk newborns, especially in premature babies. We therefore recommend applying this methodology in the ONICU

Planeación y gestión estratégica de la empresa Baldwin en el simulador de negocios Capstone

En este documento se presentan los resultados obtenidos por la empresa Baldwin en el simulador de negocios CAPSTONE a través de la implementación de la estrategia planteada por los autores. El primer capítulo muestra el marco teórico sobre estrategia, en el cual se describen algunos casos y el análisis de sus problemáticas para así, con herramientas planteadas en múltiples teorías presentar posibles escenarios de soluciones contextualizadas. En el segundo capítulo se expone la industria de sensores, en la cual se desenvuelve la competencia, las estrategias genéricas, los elementos que tendrán influencia en la toma de decisiones, la compañía Baldwin, su equipo directivo y su planeación estratégica. Del capítulo tres al seis se muestra la información obtenida en el Courier, detallando los resultados obtenidos por Baldwin en la competencia a partir del año 2020 y hasta el año 2027. Se analizan los indicadores del BSC, las áreas de investigación y desarrollo, finanzas, producción, mercadotecnia, recursos humanos, calidad y el comportamiento de la industria, con el objetivo de observar el desarrollo de la estrategia planteada y los ajustes para posicionar a la compañía como líder. En el séptimo capítulo se presentan las conclusiones generales a las que llegó el equipo directivo de Baldwin al haber operado a la compañía durante ocho años. También se explican los resultados obtenidos, las complicaciones con las que se enfrentaron, las soluciones propuestas, los aprendizajes obtenidos, e individualmente se exponen los conocimientos adquirido en los cursos de IDI2, IDI 3 e IDI 4, junto con su experiencia y vivencias adquiridas durante la maestría en administración

Desarrollo de estrategias para mejorar la comercialización de obras de arte elaboradas por Karla Betancourt en Tlaquepaque, Jalisco en el periodo Agosto a Diciembre 2022

ITESO, A.C