How much dark matter is there inside early-type galaxies?

We study the luminous mass as a function of the dynamical mass inside the effective radius (r_e) of early-type galaxies (ETGs) to search for differences between these masses. We assume Newtonian dynamics and that any difference between these masses is due to the presence of dark matter. We use several samples of ETGs -ranging from 19 000 to 98 000 objects- from the ninth data release of the Sloan Digital Sky Survey. We perform Monte Carlo (MC) simulations of galaxy samples and compare them with real samples. The main results are: i) MC simulations show that the distribution of the dynamical vs. luminous mass depends on the mass range where the ETGs are distributed (geometric effect). This dependence is caused by selection effects and intrinsic properties of the ETGs. ii) The amount of dark matter inside r_e is approximately 7% +- 22%. iii) This amount of dark matter is lower than the minimum estimate (10%) found in the literature and four times lower than the average (30%) of literature estimates. However, if we consider the associated error, our estimate is of the order of the literature average.Comment: 24 pages, 12 figures. MNRAS accepte

High-fidelity reproduction of central galaxy joint distributions with Neural Networks

The relationship between galaxies and haloes is central to the description of galaxy formation, and a fundamental step towards extracting precise cosmological information from galaxy maps. However, this connection involves several complex processes that are interconnected. Machine Learning methods are flexible tools that can learn complex correlations between a large number of features, but are traditionally designed as deterministic estimators. In this work, we use the IllustrisTNG300-1 simulation and apply neural networks in a binning classification scheme to predict probability distributions of central galaxy properties, namely stellar mass, colour, specific star formation rate, and radius, using as input features the halo mass, concentration, spin, age, and the overdensity on a scale of 3 $h^{-1}$ Mpc. The model captures the intrinsic scatter in the relation between halo and galaxy properties, and can thus be used to quantify the uncertainties related to the stochasticity of the galaxy properties with respect to the halo properties. In particular, with our proposed method, one can define and accurately reproduce the properties of the different galaxy populations in great detail. We demonstrate the power of this tool by directly comparing traditional single-point estimators and the predicted joint probability distributions, and also by computing the power spectrum of a large number of tracers defined on the basis of the predicted colour-stellar mass diagram. We show that the neural networks reproduce clustering statistics of the individual galaxy populations with excellent precision and accuracy.Comment: 12 pages, 7 figure

Acinar cell carcinoma of the pancreas with thyroid-like follicular features: first description of a new diagnostic challenging subtype.

Acinar cell carcinomas (ACCs) of the pancreas are a heterogeneous group of neoplasms showing a wide spectrum of morphological features including acinar, solid, glandular, and trabecular architecture. In addition, uncommon cytological aspects have recently been described and include oncocytic, spindle, clear, and pleomorphic cell types. This wide histological spectrum represents a challenge in the diagnostic task for pathologists. Molecular mechanisms involved in the onset and progression of ACCs are not completely known, but, in general, they differ from those observed in ductal adenocarcinomas or neuroendocrine neoplasms of the pancreas and frequently include alterations in the APC/β-catenin pathway. In the present paper, we describe a new variant of ACC showing thyroid-like follicular features and CTNNB1 mutation. This phenotype needs to be included in the spectrum of morphological presentation of ACC

Virtual Blocks: a serious game for spatial ability improvement on mobile devices

This paper presents a novel spatial instruction system for improving spatial abilities of engineering students. A 3D mobile game application called Virtual Blocks has been designed to provide a 3D virtual environment to build models with cubes that help students to perform visualization tasks to promote the development of their spatial ability during a short remedial course. A validation study with 26 freshman engineering students at La Laguna University (Spain) has concluded that the training had a measurable and positive impact on students spatial ability. In addition, the results obtained using a satisfaction questionnaire show that Virtual Blocks is considered an easy to use and stimulating application.This work has been partially supported by the (Spanish) National Program for Studies and Analysis project "Evaluation and development of competencies associated to the spatial ability in the new engineering undergraduate courses" (Ref. EA2009-0025) and the (Spanish) National Science Project "Enhancing Spatial REasoning and VIsual Cognition with advanced technological tools (ESREVIC)" (Ref TIN2010-21296-C02-02)Martín Dorta, NN.; Sanchez Berriel, I.; Bravo, M.; Hernández, J.; Saorin, JL.; Contero, M. (2014). Virtual Blocks: a serious game for spatial ability improvement on mobile devices. Multimedia Tools and Applications. 73(3):1575-1595. https://doi.org/10.1007/s11042-013-1652-0S15751595733Baartmans BG, Sorby SA (1996) Introduction to 3-D spatial visualization. Prentice Hall, Englewood CliffsClements D, Battista M (1992) Geometry and spatial reasoning. In: Grouws DA (ed) Handbook of research on mathematics teaching and learning. New York, pp 420–464Cohen J (1988) Statistical power analysis for the behavioral sciences, 2nd edn. Erlbaum, HillsdaleDe Lisi R, Cammarano DM (1996) Computer experience and gender differences in undergraduate mental rotation performance. Comput Hum Behav 12:351–361Deno JA (1995) The relationship of previous experiences to spatial visualization ability. Eng Des Graph J 59(3):5–17Feng J, Spence I, Pratt J (2007) Playing an action video game reduces gender differences in spatial cognition. Psychol Sci 18(10):850–855French JW (1951) The description of aptitude and achievement tests in terms of rotated factors. Psychometric monograph 5Guilford JP, Lacy JI (1947) Printed classification tests, A.A.F. Aviation Psychological Progress Research Report, 5. US. Government Printing Office, Washington DCHalpern DF (2000) Sex differences and cognitive abilities. Erlbaum, MahwahHöfele C (2007) Mobile 3D graphics: learning 3D graphics with the Java Micro Edition. Editorial ThomsonKajiya JT, Kay TL (1989) Rendering fur with three dimensional textures. In Proceedings of the 16th Annual Conference on Computer Graphics and interactive Techniques SIGGRAPH ’89. ACM Press, New York pp 271–280Linn MC, Petersen AC (1985) Emergence and characterization of gender differences in spatial abilities: a meta-analysis. Child Dev 56:1479–1498Martin-Dorta N, Sanchez-Berriel I, Bravo M, Hernandez J, Saorin JL, Contero M (2010) A 3D educational mobile game to enhance student’s spatial skills, ICALT, pp.6–10, 2010 10th IEEE International Conference on Advanced Learning TechnologiesMartin-Dorta N, Saorin J, Contero M (2008) Development of a fast remedial course to improve the spatial abilities of engineering students. J Eng Educ 27(4):505–514Martin-Dorta N, Saorin JL, Contero M (2011) Web-based spatial training using handheld touch screen devices. Educ Technol Soc 14(3):163–177McGee MG (1979) Human spatial abilities: psychometric studies and environmental, genetic, hormonal, and neurological influences. Psychol Bull 86:889–918Noguera JM, Segura RJ, Ogayar CJ, Joan-Arinyo R (2011) Navigating large terrains using commodity mobile devices. Comput Geosci 37:1218–1233Okagaki L, Frensch PA (1994) Effects of video game playing on measures of spatial performance: gender effects in late adolescence. J Appl Dev Psychol 15(1):33–58Pulli K, Aarnio T, Miettinen V, Roimela K, Vaarala J (2007) Mobile 3D graphics with OpenGL ES and M3G. Editorial Morgan KaufmannQuaiser-Pohl C, Geiser C, Lehmann W (2005) The relationship between computer-game preference, gender, and mental-rotation ability. Personal Individ Differ 40(3):609–619Smith IM (1964) Spatial ability- its educational and social significance. The University of London Press, LondonSorby S (2007) Developing 3D spatial skills for engineering students. Australas Assoc Eng Educ 13(1):1–11Terlecki MS, Newcombe NS (2005) How important is the digital divide? The relation of computer and videogame usage to gender differences in mental rotation ability. Sex Roles 53(5/6):433–441Terlecki MS, Newcombe NS, Little M (2008) Durable and generalized effects of spatial experience on mental rotation: gender differences in growth patterns. Appl Cogn Psychol 22:996–1013Thurstone LL (1950) Some primary abilities in visual thinking (Tech. Rep. No. 59). IL University of Chicago Psychometric Laboratory, ChicagoThurstone LL, Thurstone TG (1941) Factorial studies of intelligence. Psychometric monographs. Chicago Press, ChicagoVanderberg S, Kuse A (1978) Mental Rotation, a group test of three dimensional spatial visualization. Percept Mot Skills 47:599–604Zimmerman WS (1954) Hypotheses concerning the nature of the spatial factors. Educ Psychol Meas 14:396–40

The ALHAMBRA survey : B−B-band luminosity function of quiescent and star-forming galaxies at 0.2≤z<10.2 \leq z < 1 by PDF analysis

Our goal is to study the evolution of the $B-$band luminosity function (LF) since $z=1$ using ALHAMBRA data. We used the photometric redshift and the $I-$band selection magnitude probability distribution functions (PDFs) of those ALHAMBRA galaxies with $I\leq24$ mag to compute the posterior LF. We statistically studied quiescent and star-forming galaxies using the template information encoded in the PDFs. The LF covariance matrix in redshift-magnitude-galaxy type space was computed, including the cosmic variance. That was estimated from the intrinsic dispersion of the LF measurements in the 48 ALHAMBRA sub-fields. The uncertainty due to the photometric redshift prior is also included in our analysis. We modelled the LF with a redshift-dependent Schechter function affected by the same selection effects than the data. The measured ALHAMBRA LF at $0.2\leq z<1$ and the evolving Schechter parameters both for quiescent and star-forming galaxies agree with previous results in the literature. The estimated redshift evolution of $M_B^* \propto Qz$ is $Q_{\rm SF}=-1.03\pm0.08$ and $Q_{\rm Q}=-0.80\pm0.08$, and of $\log \phi^* \propto Pz$ is $P_{\rm SF}=-0.01\pm0.03$ and $P_{\rm Q}=-0.41\pm0.05$. The measured faint-end slopes are $\alpha_{\rm SF}=-1.29\pm0.02$ and $\alpha_{\rm Q}=-0.53\pm0.04$. We find a significant population of faint quiescent galaxies, modelled by a second Schechter function with slope $\beta=-1.31\pm0.11$. We find a factor $2.55\pm0.14$ decrease in the luminosity density $j_B$ of star-forming galaxies, and a factor $1.25\pm0.16$ increase in the $j_B$ of quiescent ones since $z=1$, confirming the continuous build-up of the quiescent population with cosmic time. The contribution of the faint quiescent population to $j_B$ increases from 3% at $z=1$ to 6% at $z=0$. The developed methodology will be applied to future multi-filter surveys such as J-PAS.Comment: Accepted for publication in Astronomy and Astrophysics. 25 pages, 20 figures, 7 table

Reviewing, indicating, and counting books for modern research evaluation systems

In this chapter, we focus on the specialists who have helped to improve the conditions for book assessments in research evaluation exercises, with empirically based data and insights supporting their greater integration. Our review highlights the research carried out by four types of expert communities, referred to as the monitors, the subject classifiers, the indexers and the indicator constructionists. Many challenges lie ahead for scholars affiliated with these communities, particularly the latter three. By acknowledging their unique, yet interrelated roles, we show where the greatest potential is for both quantitative and qualitative indicator advancements in book-inclusive evaluation systems.Comment: Forthcoming in Glanzel, W., Moed, H.F., Schmoch U., Thelwall, M. (2018). Springer Handbook of Science and Technology Indicators. Springer Some corrections made in subsection 'Publisher prestige or quality

The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large-scale two-point correlation function

We obtain constraints on cosmological parameters from the spherically averaged redshift-space correlation function of the CMASS Data Release 9 (DR9) sample of the Baryonic Oscillation Spectroscopic Survey (BOSS). We combine this information with additional data from recent CMB, SN and BAO measurements. Our results show no significant evidence of deviations from the standard flat-Lambda CDM model, whose basic parameters can be specified by Omega_m = 0.285 +- 0.009, 100 Omega_b = 4.59 +- 0.09, n_s = 0.96 +- 0.009, H_0 = 69.4 +- 0.8 km/s/Mpc and sigma_8 = 0.80 +- 0.02. The CMB+CMASS combination sets tight constraints on the curvature of the Universe, with Omega_k = -0.0043 +- 0.0049, and the tensor-to-scalar amplitude ratio, for which we find r < 0.16 at the 95 per cent confidence level (CL). These data show a clear signature of a deviation from scale-invariance also in the presence of tensor modes, with n_s <1 at the 99.7 per cent CL. We derive constraints on the fraction of massive neutrinos of f_nu < 0.049 (95 per cent CL), implying a limit of sum m_nu < 0.51 eV. We find no signature of a deviation from a cosmological constant from the combination of all datasets, with a constraint of w_DE = -1.033 +- 0.073 when this parameter is assumed time-independent, and no evidence of a departure from this value when it is allowed to evolve as w_DE(a) = w_0 + w_a (1 - a). The achieved accuracy on our cosmological constraints is a clear demonstration of the constraining power of current cosmological observations.Comment: 26 pages, 15 figures. Minor changes to match version accepted by MNRA