Gut microbiome specific changes in different behavioral profiles in a mouse social defeat stress model.

Comunicación de tipo PósterThe gut microbiome has arisen as one important modulator of general health, including brain function. In fact, disturbances in brain health are commonly mirrored in the microbiome, which could be contributing to pathology. One of the most common brain disorders is depression, which is tightly linked to environmental factors such as stress and drives alterations in regular behavior. However, not much is known about the role of the gut microbiome in response to stress and its relationship to behavior. In this study, the social defeat stress (SDS) paradigm was used as a depressive-like symptoms inducer in 8 w.o. male C57BL/6J mice for 10 days. Mice were segregated in stress resilient and sensitive according to behavior using K-means clustering and behavioral data was interpreted using principal component analysis. Then, the mice microbiome was extracted from fecal pellets after the stress protocol. DNA was extracted and purified followed by 16S (V3-V4) region amplification for sequencing. These data were analyzed to obtain diversity indexes and identify bacterial taxa within samples and groups. Data revealed that mice responded differently to the same stressor. Half the mice were found to have mild depressive-like symptoms whereas the other half showed profound alterations. Behavioral data was found to be explained in three factors: anhedonia, exploration, and motility. Stressed mice showed overall differences in their microbiome, being less diverse and populations associated with higher inflammation. Moreover, the healthy gut associated Verrucomicrobiae class was only identified in stress resilient mice, suggesting a possible relationship with their behavioral phenotype. Altogether, these results show a different behavioral response to stress in animals that reflects in their microbiome, which could be a key factor in determining stress resilience.This study was supported by Ministerio de Ciencia e Innovación - Plan Nacional I+D+I from Spain (PID2020-117464RB-I00) to CP and MP-M; FEDER/Junta de Andalucía - Proyectos I+D+I en el marco del Programa Operativo FEDER Andalucía 2014-2020 (UMA20-FEDERJA-112) to CP and MP-M; Consejería de Conocimiento, Investigación y Universidades, Junta de Andalucía (P20_00460) to CP. PC-P has been funded by the research project PID2020-117464RB-I00. Ministerio de Educación, Cultura y Deporte from Spain (FPU19/03629 to Infantes-López MI). Universidad de Málaga. Campus de Excelencia Internacional Andalucía Tech

La restauración de la villa romana de La Ontavia (Terrinches, Ciudad Real)

En el mes de julio de 2010 se iniciaron las labores de conservación y restauración en el yacimiento romano de La Ontavia (Terrinches, Ciudad Real). Durante cuatro meses se han simultaneado estos trabajos con la excavación arqueológica, en la que han colaborado once alumnos de la Escuela Superior de Conservación y Restauración de Bienes Culturales de la Comunidad de Madrid, bajo la dirección del equipo técnico, realizando prácticas para completar su formación. La intervención llevada a cabo ha estado enfocada a minimizar el efecto de los agentes de deterioro a los que se halla expuesto el yacimiento, que se encuentra al aire libre. El presente artículo tiene como finalidad la difusión de los trabajos de conservación y restauración realizados durante esta campaña, prestando especial atención a la metodología y a los materiales utilizadosIn July 2010 conservation and restoration work began at the Roman site of La Ontavia (Terrinches, Ciudad Real). For four months, the work was carried out alongside the archaeological excavation, involving eleven students from the Madrid School of Cultural Asset Conservation and Restoration, doing work experience under the guidance of a technical team to complete their training. The intervention focused on minimising the effect of the deterioration factors that this open-air site has been exposed to. This article aims to provide a report of the conservation and restoration work carried out in this campaign, paying special attention to the methodology and materials use

Morfología de semillas de siete especies del género Opuntia (Cactaceae) del sureste de Coahuila (México)

Background and aims: Opuntia’s natural distribution encompasses from Canada to Argentina and it is part of the landscape in some regions of the world. There are between 191 and 215 Opuntia species. The ex situ conservation of this phytogenetic resource has gained relevance, but the species identification using the seeds is a limitation when there is a lack of reliable morphological traits. The purpose of this research work was to characterize the seed morphology of seven Opuntia species and identify their own morphological traits, in order to establish the species’ identification criteria when seeds are the only source of preserved plant material. M&M: We used the attrition and image analysis technique to measure: seed coat thickness (GT), ventral funicular coat thickness (GCFV), embryo’s length, embryo’s surface area, major axis length and minor axis length. The most outstanding traits were detected through exploratory ANDEVA and main components methods. The species classification and forecasting were based on a supervised multivariate analysis. Results: Differences in all the variables among species were significant. Opuntia ficus-indica had the largest seeds. GCFV and GT were the most helpful variables in terms of discrimination. The main component analysis explained 92% of the total variation. K- Nearest Neighbor method was able to forecast correctly 83% of the species classification cases. Conclusions: The assessed seed traits, mainly GCFV and GT, can help in the morphological description of prickly pear species and in the Opuntia species identification, when there are only seeds.Introducción y Objetivos: Opuntia se distribuye naturalmente desde Canadá hasta Argentina, actualmente forma parte del paisaje en algunas regiones del mundo, comprende entre 191 y 215 especies; la conservación ex situ de este recurso fitogenético ha adquirido relevancia, pero la identificación de especies por semilla es una limitante cuando no se tienen caracteres morfológicos confiables. El objetivo del estudio fue caracterizar la morfología de semillas de siete especies de Opuntia e identificar caracteres morfológicos propios, para tener un criterio en la identificación de especies cuando el material vegetal conservado es semilla. M&M: Mediante la técnica de desgaste y análisis de imágenes se evaluó: grosor de testa (GT), grosor de la cubierta funicular ventral (GCFV), longitud del embrión (LE), área del embrión (AE), longitud del eje mayor (LEMA) y del eje menor (LEME). Por medio de ANDEVA exploratorios y componentes principales (CP) se detectaron los caracteres más sobresalientes. Para la clasificación y predicción de especies se realizó un análisis supervisado con los métodos K-NN y LDA. Resultados: Las diferencias en todas las variables entre especies fueron significativas. Opuntia ficus-indica presentó semillas de mayor tamaño. Las variables que más ayudan a discriminar son GCFV y GT. El análisis de componentes principales explicó el 92% de la variación total. El método de predicción K-NN, fue capaz de predecir correctamente el 83% de los casos en la clasificación de las especies. Conclusiones: Los caracteres de semillas evaluados, principalmente el GCFV y GT, pueden coadyuvar en la descripción morfológica de las especies de nopal o o en identificación de especies de Opuntia cuando sólo se tiene semilla

Galaxy clusters and groups in the ALHAMBRA Survey

We present a catalogue of 348 galaxy clusters and groups with $0.2<z<1.2$ selected in the 2.78 $deg^2$ ALHAMBRA Survey. The high precision of our photometric redshifts, close to $1\%$, and the wide spread of the seven ALHAMBRA pointings ensure that this catalogue has better mass sensitivity and is less affected by cosmic variance than comparable samples. The detection has been carried out with the Bayesian Cluster Finder (BCF), whose performance has been checked in ALHAMBRA-like light-cone mock catalogues. Great care has been taken to ensure that the observable properties of the mocks photometry accurately correspond to those of real catalogues. From our simulations, we expect to detect galaxy clusters and groups with both $70\%$ completeness and purity down to dark matter halo masses of $M_h\sim3\times10^{13}\rm M_{\odot}$ for $z<0.85$. Cluster redshifts are expected to be recovered with $\sim0.6\%$ precision for $z<1$. We also expect to measure cluster masses with $\sigma_{M_h|M^*_{CL}}\sim0.25-0.35\, dex$ precision down to $\sim3\times10^{13}\rm M_{\odot}$, masses which are $50\%$ smaller than those reached by similar work. We have compared these detections with previous optical, spectroscopic and X-rays work, finding an excellent agreement with the rates reported from the simulations. We have also explored the overall properties of these detections such as the presence of a colour-magnitude relation, the evolution of the photometric blue fraction and the clustering of these sources in the different ALHAMBRA fields. Despite the small numbers, we observe tentative evidence that, for a fixed stellar mass, the environment is playing a crucial role at lower redshifts (z$<$0.5).Comment: Accepted for publication in MNRAS. Catalogues and figures available online and under the following link: http://bascaso.net46.net/ALHAMBRA_clusters.htm

The impact from survey depth and resolution on the morphological classification of galaxies

We consistently analyse for the first time the impact of survey depth and spatial resolution on the most used morphological parameters for classifying galaxies through non-parametric methods: Abraham and Conselice-Bershady concentration indices, Gini, M20moment of light, asymmetry, and smoothness. Three different non-local data sets are used, Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) and Subaru/XMMNewton Deep Survey (SXDS, examples of deep ground-based surveys), and Cosmos Evolution Survey (COSMOS, deep space-based survey). We used a sample of 3000 local, visually classified galaxies, measuring their morphological parameters at their real redshifts (z ~ 0). Then we simulated them to match the redshift and magnitude distributions of galaxies in the non-local surveys. The comparisons of the two sets allow us to put constraints on the use of each parameter for morphological classification and evaluate the effectiveness of the commonly used morphological diagnostic diagrams. All analysed parameters suffer from biases related to spatial resolution and depth, the impact of the former being much stronger. When including asymmetry and smoothness in classification diagrams, the noise effects must be taken into account carefully, especially for ground-based surveys. M20 is significantly affected, changing both the shape and range of its distribution at all brightness levels. We suggest that diagnostic diagrams based on 2-3 parameters should be avoided when classifying galaxies in ground-based surveys, independently of their brightness; for COSMOS they should be avoided for galaxies fainter than F814 = 23.0. These results can be applied directly to surveys similar to ALHAMBRA, SXDS and COSMOS, and also can serve as an upper/lower limit for shallower/deeper ones.Ministerio de Economía y Competitividad AYA2010-15169, AYA2013-42227-P, AYA2013-4318

The impact from survey depth and resolution on the morphological classification of galaxies

We consistently analyse for the first time the impact of survey depth and spatial resolution on the most used morphological parameters for classifying galaxies through non-parametric methods: Abraham and Conselice-Bershady concentration indices, Gini, M20moment of light, asymmetry, and smoothness. Three different non-local data sets are used, Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) and Subaru/XMMNewton Deep Survey (SXDS, examples of deep ground-based surveys), and Cosmos Evolution Survey (COSMOS, deep space-based survey). We used a sample of 3000 local, visually classified galaxies, measuring their morphological parameters at their real redshifts (z ~ 0). Then we simulated them to match the redshift and magnitude distributions of galaxies in the non-local surveys. The comparisons of the two sets allow us to put constraints on the use of each parameter for morphological classification and evaluate the effectiveness of the commonly used morphological diagnostic diagrams. All analysed parameters suffer from biases related to spatial resolution and depth, the impact of the former being much stronger. When including asymmetry and smoothness in classification diagrams, the noise effects must be taken into account carefully, especially for ground-based surveys. M20 is significantly affected, changing both the shape and range of its distribution at all brightness levels. We suggest that diagnostic diagrams based on 2-3 parameters should be avoided when classifying galaxies in ground-based surveys, independently of their brightness; for COSMOS they should be avoided for galaxies fainter than F814 = 23.0. These results can be applied directly to surveys similar to ALHAMBRA, SXDS and COSMOS, and also can serve as an upper/lower limit for shallower/deeper ones.MP acknowledge financial support from JAE-Doc programme of the Spanish National Research Council (CSIC), co-funded by the European Social Fund. This research was supported by the Junta de Andalucia through project TIC114, and the Spanish Ministry of Economy and Competitiveness (MINECO) through projects AYA2010-15169, AYA2013-42227-P, and AYA2013-43188-P.Peer Reviewe

The ALHAMBRA survey: reliable morphological catalogue of 22 051 early- and late-type galaxies

Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) is photometric survey designed to trace the cosmic evolution and cosmic variance. It covers a large area of ~4 deg2 in eight fields, where seven fields overlap with other surveys, allowing us to have complementary data in other wavelengths. All observations were carried out in 20 continuous, medium band (30 nm width) optical and 3 near-infrared (JHK) bands, providing the precise measurements of photometric redshifts. In addition, morphological classification of galaxies is crucial for any kind of galaxy formation and cosmic evolution studies, providing the information about star formation histories, their environment and interactions, internal perturbations, etc. We present a morphological classification of >40 000 galaxies in the ALHAMBRA survey. We associate to every galaxy a probability to be early type using the automated Bayesian code GALSVM. Despite of the spatial resolution of theALHAMBRAimages (~1 arcsec), for 22 051 galaxies, we obtained the contamination by other type of less than 10 per cent. Of those, 1640 and 10 322 galaxies are classified as early-(down to redshifts ~0.5) and late-type (down to redshifts ~1.0), respectively, with magnitudes F613W ≤ 22.0. In addition, for magnitude range 22.0 < F613W ≤ 23.0, we classified other 10 089 late-type galaxies with redshifts ≤1.3.We show that the classified objects populate the expected regions in the colour-mass and colour-magnitude planes. The presented data set is especially attractive given the homogeneous multiwavelength coverage available in the ALHAMBRA fields, and is intended to be used in a variety of scientific applications. The low-contamination catalogue (<10 per cent) is made publicly available with this paper. © 2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.This research was supported by the Junta de Andalucía through projects PO8-TIC-03531 and TIC114, the Spanish Ministry of Economy and Competitiveness (MINECO) through projects AYA2006-14046, AYA2010-15169, AYA2010-22111-C03-02, AYA2011-29517-C03-01, and the Generalitat Valenciana through project GV/Prometeo 2009/064. MP acknowledges financial support from JAE-Doc program of the Spanish National Research Council (CSIC), co-funded by the European Social Fund.Peer Reviewe

The ALHAMBRA survey: Bayesian photometric redshifts with 23 bands for 3 deg2

A. Molino et al.The Advance Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) survey has observed eight different regions of the sky, including sections of the Cosmic Evolution Survey (COSMOS), DEEP2, European Large-Area Infrared Space Observatory Survey (ELAIS), Great Observatories Origins Deep Survey North (GOODS-N), Sloan Digital Sky Survey (SDSS) and Groth fields using a new photometric system with 20 optical, contiguous ~300-Å filters plus the JHKs bands. The filter system is designed to optimize the effective photometric redshift depth of the survey, while having enough wavelength resolution for the identification of faint emission lines. The observations, carried out with the Calar Alto 3.5-m telescope using the wide-field optical camera Large Area Imager for Calar Alto (LAICA) and the near-infrared (NIR) instrument Omega-2000, represent a total of ~700 h of on-target science images. Here we present multicolour point-spread function (PSF) corrected photometry and photometric redshifts for ~438 000 galaxies, detected in synthetic F814W images. The catalogues are complete down to a magnitude I~24.5AB and cover an effective area of 2.79 deg2. Photometric zero-points were calibrated using stellar transformation equations and refined internally, using a new technique based on the highly robust photometric redshifts measured for emission-line galaxies. We calculate Bayesian photometric redshifts with the Bayesian Photometric Redshift (BPZ)2.0 code, obtaining a precision of δz/(1+zs)=1 per cent for I<22.5 and δz/(1+zs)=1.4 per cent for 22.5<I<24.5. The global n(z) distribution shows a mean redshift 〈z〉=0.56 for I<22.5 AB and 〈z〉=0.86 for I<24.5 AB. Given its depth and small cosmic variance, ALHAMBRA is a unique data set for galaxy evolution studies. © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.We acknowledge financial support from the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. Part of this work was supported by Junta de Andalucía, through grant TIC-114 and the Excellence Project P08-TIC-3531, and by the Spanish Ministry for Science and Innovation through grants AYA2006-1456, AYA2010-15169, AYA2010-22111-C03-02, AYA2010-22111-C03-01 and Generalitat Valenciana project Prometeo 2009/064.Peer Reviewe

I. MUFFIT: A multi-filter fitting code for stellar population diagnostics

Numerical methods and codes.-- et al.[Aims]: We present MUFFIT, a new generic code optimized to retrieve the main stellar population parameters of galaxies in photometric multi-filter surveys, and check its reliability and feasibility with real galaxy data from the ALHAMBRA survey. [Methods]: Making use of an error-weighted X2-test, we compare the multi-filter fluxes of galaxies with the synthetic photometry of mixtures of two single stellar populations at different redshifts and extinctions, to provide the most likely range of stellar population parameters (mainly ages and metallicities), extinctions, redshifts, and stellar masses. To improve the diagnostic reliability, MUFFIT identifies and removes from the analysis those bands that are significantly affected by emission lines. The final parameters and their uncertainties are derived by a Monte Carlo method, using the individual photometric uncertainties in each band. Finally, we discuss the accuracies, degeneracies, and reliability of MUFFIT using both simulated and real galaxies from ALHAMBRA, comparing with results from the literature. [Results]: MUFFIT is a precise and reliable code to derive stellar population parameters of galaxies in ALHAMBRA. Using the results from photometric-redshift codes as input, MUFFIT improves the photometric-redshift accuracy by ∼10-20%. MUFFIT also detects nebular emissions in galaxies, providing physical information about their strengths. The stellar masses derived from MUFFIT show excellent agreement with the COSMOS and SDSS values. In addition, the retrieved age-metallicity locus for a sample of z ≤ 0.22 early-type galaxies in ALHAMBRA at different stellar mass bins are in very good agreement with the ones from SDSS spectroscopic diagnostics. Moreover, a one-to-one comparison between the redshifts, ages, metallicities, and stellar masses derived spectroscopically for SDSS and by MUFFIT for ALHAMBRA reveals good qualitative agreements in all the parameters, hence reinforcing the strengths of multi-filter galaxy data and optimized analysis techniques, like MUFFIT, to conduct reliable stellar population studies.L.A.D.G. acknowledges support from the "Caja Rural de Teruel" for developing this research. A.J.C. is a Ramon y Cajal Fellow of the Spanish Ministry of Science and Innovation. This work has been supported by the "Programa Nacional de Astronomia y Astrofisica" of the Spanish Ministry of Economy and Competitiveness (MINECO) under grant AYA2012-30789, as well as by FEDER funds and the Government of Aragon, through the Research Group E103. L.A.D.G. also thanks the Mullard Space Science Laboratory (MSSL) and Royal Astronomical Society (RAS) for offering the opportunity to support and develop part of this research in collaboration with I.F. MINECO grants AYA2010-15081, AYA2010-15169, AYA2010-22111-C03-01, AYA2010-22111-C03-02, AYA2011-29517-C03-01, AYA2013-40611-P, AYA2013-42227-P, AYA2013-43188-P, AYA2013-48623-C2-1, AYA2013-48623-C2-2, and AYA2014-58861-C3-1 are also acknowledged, together with Generalitat Valenciana projects Prometeo 2009/064 and PROMETEOII/2014/060, and Junta de Andalucia grants TIC114, JA2828, and P10-FQM-6444. MP acknowledges financial support from the JAE-Doc programme of the Spanish National Research Council (CSIC), co-funded by the European Social Fund.Peer Reviewe