Perfiles de ansiedad escolar: Diferencias en clima social y violencia entre iguales

Introducción. La ansiedad escolar es definida como un conjunto de síntomas agrupados en respuestas cognitivas, psicofisiológicas y motoras emitidas por un individuo ante situaciones escolares que son percibidas como amenazantes y/o peligrosas. Entre variables escolares relevantes, la ansiedad escolar puede estar influida por la percepción del clima social y la violencia cotidiana observada en el centro por parte del alumnado. El objetivo de este estudio fue identificar si existen combinaciones entre las distintas situaciones que provocan ansiedad escolar dando lugar a diferentes perfiles ansiosos. Además, se persigue comprobar si existen diferencias entre estos perfiles en las variables percepción de clima social y violencia entre iguales. Método. La muestra estuvo compuesta por 365 alumnos de educación secundaria. La ansiedad escolar fue medida con el Inventario de Ansiedad Escolar, el clima social se midió con el Cuestionario de Clima Social del Centro Escolar y la violencia entre iguales mediante el Cuestionario de Violencia Escolar Cotidiana. Resultados. Los análisis de conglomerados identificaron tres perfiles de ansiedad escolar. Los resultados indicaron diferencias estadísticamente significativas entre los tres perfiles en las variables clima referente al profesorado entre los grupos con baja y alta ansiedad escolar y en experiencia personal de sufrir violencia entre el grupo con baja y media ansiedad escolar y entre el grupo con baja y alta ansiedad escolar. La magnitud de las diferencias halladas fue de baja a moderada. Discusión y Conclusiones. Los hallazgos de este estudio resultan relevantes ya que aportan un análisis más exhaustivo de la ansiedad escolar y de las diferencias observadas en otras variables relevantes en el ámbito educativo, como son el clima social del centro escolar y la violencia entre iguales.Introduction. School anxiety is often defined as a set of symptoms grouped into cognitive, psychophysiological and motor responses emitted by an individual in school situations that can be perceived as threatening and/or dangerous. School anxiety may be influenced - among other relevant school variables - by the perception of social climate and the daily violence witnessed by students at school. The aim of this study is to identify whether there are different combinations of school anxiety-provoking situations which give rise to different anxious profiles. Furthermore, it claims to verify whether there are differences between these profiles in terms of the variables: perception of social climate and peer violence. Method. The sample consists of 365 high school students. School anxiety was measured using the School Anxiety Inventory; the social climate was measured with the School Social Climate Questionnaire and peer violence with the Daily School Violence Questionnaire. Results. Cluster analyses have identified three profiles of school anxiety. The results showed statistically significant differences among the three anxiety profiles in the following variables: (1) teacher climate (low and high anxiety) and (2) personal experience of suffering violence (low and medium anxiety; low and high anxiety). The differences were of low-to-moderate intensity. Discussion and Conclusion. The findings of this study are relevant because they provide a more comprehensive analysis of school anxiety and differences in other relevant variables in an educational context, such as the school social climate and peer violence

The cosmic dawn and the epoch of reionization

In this chapter we briefly describe the physics behind the HI 21 cm line in terms of the interplay of the HI gas with the ionized plasma and the Cosmic Microwave Background, and the different phases the system undergoes as the ambient density and UV background evolve with cosmological time. We also address the problematics associated to the metal enrichment of the IGM and the implications for the models of galaxy formation and evolution. We briefly discuss possible synergies with other reionization probes like E-ELT, JWST and ALMA, and conclude by listing a number of cosmological scenarios describing some type of energetic injection in the Universe, scenarios to whose understanding SKA should be able to (at least partially) contribute.The authors acknowledge partial support from the Spanish Ministerio de Economía y Competitividad (MICINN) through projects AYA2013-48623-C2-2, AYA2007-68058-C03-01, AYA2010-21766-C03-02, AYA2012-30789, and the Consolider-Ingenio project CSD2010-00064 (EPI: Exploring the Physics of Inflation). We also acknowledge the support of the Ramón y Cajal fellowship (RyC 2011 148062) awarded by the Spanish MICINN and the Marie Curie Career Integration Grant (CIG 294183).Peer reviewe

Tipos sociométricos, categorías conductuales y aptitudes intelectuales en adolescentes

El objetivo de este estudio fue analizar la relación entre tipos sociométricos, categorías conductuales y aptitudes intelectuales en una muestra de 1349 (51.7% varones) adolescentes españoles de 12 a 16 años. La identificación sociométrica de los estudiantes se realizó mediante el Programa Socio y para el análisis de las aptitudes intelectuales se administró el Test de Aptitudes Mentales Primarias (PMA; Thurstone, 1938; TEA, 1996). Las hipótesis del estudio plantean, en primer lugar, que los estudiantes nominados positivamente por sus iguales presentarán puntuaciones significativamente superiores en las diferentes escalas del PMA que los estudiantes nominados negativamente por sus compañeros y, en segundo lugar, que las aptitudes intelectuales serán una variable predictora estadísticamente significativa de los tipos sociométricos y categorías conductuales. Los resultados muestran que los estudiantes nominados positivamente obtuvieron puntuaciones significativamente más altas en las diferentes aptitudes intelectuales que los nominados negativamente. Las aptitudes intelectuales resultaron un predictor significativo de los tipos sociométricos, ya que a medida que aumenta la puntuación en las diferentes aptitudes intelectuales los estudiantes presentaron mayor probabilidad de ser nominados positivamente por sus compañeros

Auto-atribuciones Académicas: Diferencias de Género y Curso en Estudiantes de Educación Secundaria

El análisis de las autoatribuciones académicas constituyeun aspecto esencial del componente afectivo y emocionalde la motivación escolar en estudiantes de educaciónsecundaria obligatoria (ESO). El objetivo de este estudiofue analizar, mediante un diseño transversal, las diferenciasde género y curso y el papel predictivo de estas variables enlas atribuciones causales académicas de los alumnos medidasa través de las escalas generales de la Sydney AttributionScale (SAS). El cuestionario fue administrado a 2.022estudiantes (51.08% chicos) de 1º a 4º de ESO. El rangode edad fue de 12 a 16 años (M = 13.81; DT = 1.35).Los resultados derivados de los análisis de varianza y de los tamaños del efecto (índice d) revelaron que los chicosatribuyeron sus éxitos significativamente más a su capacidad,mientras las chicas los atribuyeron significativamente másal esfuerzo. Respecto a las atribuciones de fracaso escolar,los resultados indicaron que los chicos los atribuyeronsignificativamente más a la falta de esfuerzo que las chicas.Asimismo, se hallaron diferencias de curso académico en lamayoría de las atribuciones causales analizadas. Los análisisde regresión logística indicaron que el género y el cursofueron predictores significativos de las atribuciones causalesacadémicas, aunque los resultados variaron para cada unade las escalas de la SAS. Los resultados son discutidos enrelación a la necesidad de diseñar programas de intervenciónque tengan en cuenta las variables sexo y curso académico

Planck 2015 results. XXV. Diffuse low-frequency Galactic foregrounds

Interstellar and circumstellar matter.-- et al.We discuss the Galactic foreground emission between 20 and 100 GHz based on observations by Planck and WMAP. The total intensity in this part of the spectrum is dominated by free-free and spinning dust emission, whereas the polarized intensity is dominated by synchrotron emission. The Commander component-separation tool has been used to separate the various astrophysical processes in total intensity. Comparison with radio recombination line templates verifies the recovery of the free-free emission along the Galactic plane. Comparison of the high-latitude Hα emission with our free-free map shows residuals that correlate with dust optical depth, consistent with a fraction (≈30%) of Hα having been scattered by high-latitude dust. We highlight a number of diffuse spinning dust morphological features at high latitude. There is substantial spatial variation in the spinning dust spectrum, with the emission peak (in Iν) ranging from below 20 GHz to more than 50 GHz. There is a strong tendency for the spinning dust component near many prominent H ii regions to have a higher peak frequency, suggesting that this increase in peak frequency is associated with dust in the photo-dissociation regions around the nebulae. The emissivity of spinning dust in these diffuse regions is of the same order as previous detections in the literature. Over the entire sky, the Commander solution finds more anomalous microwave emission (AME) than the WMAP component maps, at the expense of synchrotron and free-free emission. This can be explained by the difficulty in separating multiple broadband components with a limited number of frequency maps. Future surveys, particularly at 5–20 GHz, will greatly improve the separation by constraining the synchrotron spectrum. We combine Planck and WMAP data to make the highest signal-to-noise ratio maps yet of the intensity of the all-sky polarized synchrotron emission at frequencies above a few GHz. Most of the high-latitude polarized emission is associated with distinct large-scale loops and spurs, and we re-discuss their structure. We argue that nearly all the emission at 40deg > l > −90deg is part of the Loop I structure, and show that the emission extends much further in to the southern Galactic hemisphere than previously recognised, giving Loop I an ovoid rather than circular outline. However, it does not continue as far as the “Fermi bubble/microwave haze”, making it less probable that these are part of the same structure. We identify a number of new faint features in the polarized sky, including a dearth of polarized synchrotron emission directly correlated with a narrow, roughly 20deg long filament seen in Hα at high Galactic latitude. Finally, we look for evidence of polarized AME, however many AME regions are significantly contaminated by polarized synchrotron emission, and we find a 2σ upper limit of 1.6% in the Perseus region.The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). This research was supported by an ERC Starting (Consolidator) Grant (no. 307209) and STFC Consolidated Grant (no. ST/L000768/1).Peer Reviewe

Planck 2015 results. XXII. A map of the thermal Sunyaev-Zeldovich effect

Cosmology (including clusters of galaxies).-- et al.We have constructed all-sky Compton parameters maps, y-maps, of the thermal Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored component separation algorithms to the 30 to 857 GHz frequency channel maps from the Planck satellite. These reconstructed y-maps are delivered as part of the Planck 2015 release. The y-maps are characterized in terms of noise properties and residual foreground contamination, mainly thermal dust emission at large angular scales, and cosmic infrared background and extragalactic point sources at small angular scales. Specific masks are defined to minimize foreground residuals and systematics. Using these masks, we compute the y-map angular power spectrum and higher order statistics. From these we conclude that the y-map is dominated by tSZ signal in the multipole range, 20 <ℓ< 600. We compare the measured tSZ power spectrum and higher order statistics to various physically motivated models and discuss the implications of our results in terms of cluster physics and cosmology.The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).Peer Reviewe

Planck intermediate results. XXXVI. Optical identification and redshifts of Planck SZ sources with telescopes at the Canary Islands observatories

Catalogs and data.-- et al.We present the results of approximately three years of observations of Planck Sunyaev-Zeldovich (SZ) sources with telescopes at the Canary Islands observatories as part of the general optical follow-up programme undertaken by the Planck Collaboration. In total, 78 SZ sources are discussed. Deep-imaging observations were obtained for most of these sources; spectroscopic observations in either in long-slit or multi-object modes were obtained for many. We effectively used 37.5 clear nights. We found optical counterparts for 73 of the 78 candidates. This sample includes 53 spectroscopic redshift determinations, 20 of them obtained with a multi-object spectroscopic mode. The sample contains new redshifts for 27 Planck clusters that were not included in the first Planck SZ source catalogue (PSZ1).The Planck Collaboration acknowledges the support of: ESA; CNES, and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU). A.S., R.B., H.L., and J.A.R.M. acknowledge financial support from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2011 Severo Ochoa Program MINECO SEV-2011-0187, and the Consolider-Ingenio project CSD2010-00064 (EPI: Exploring the Physics of Inflation).Peer Reviewe

Planck 2015 results. XXVII. The second Planck catalogue of Sunyaev-Zeldovich sources

Catalogs and data.-- et al.We present the all-sky Planck catalogue of Sunyaev-Zeldovich (SZ) sources detected from the 29 month full-mission data. The catalogue (PSZ2) is the largest SZ-selected sample of galaxy clusters yet produced and the deepest systematic all-sky surveyof galaxy clusters. It contains 1653 detections, of which 1203 are confirmed clusters with identified counterparts in external data sets, and is the first SZ-selected cluster survey containing >103 confirmed clusters. We present a detailed analysis of the survey selection function in terms of its completeness and statistical reliability, placing a lower limit of 83% on the purity. Using simulations, we find that the estimates of the SZ strength parameter Y5R500are robust to pressure-profile variation and beam systematics, but accurate conversion to Y500 requires the use of prior information on the cluster extent. We describe the multi-wavelength search for counterparts in ancillary data, which makes use of radio, microwave, infra-red, optical, and X-ray data sets, and which places emphasis on the robustness of the counterpart match. We discuss the physical properties of the new sample and identify a population of low-redshift X-ray under-luminous clusters revealed by SZ selection. These objects appear in optical and SZ surveys with consistent properties for their mass, but are almost absent from ROSAT X-ray selected samples.The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).Peer Reviewe

Planck intermediate results: XXVIII. Interstellar gas and dust in the Chamaeleon clouds as seen by Fermi LAT and Planck

Fermi Collaborations et al.The nearby Chamaeleon clouds have been observed in γ rays by the Fermi Large Area Telescope (LAT) and in thermal dust emission by Planck and IRAS. Cosmic rays and large dust grains, if smoothly mixed with gas, can jointly serve with the H i and 12CO radio data to (i) map the hydrogen column densities, NH, in the different gas phases, in particular at the dark neutral medium (DNM) transition between the H i-bright and CO-bright media; (ii) constrain the CO-to-H2 conversion factor, XCO; and (iii) probe the dust properties per gas nucleon in each phase and map their spatial variations across the clouds. We have separated clouds at local, intermediate, and Galactic velocities in H i and 12CO line emission to model in parallel the γ-ray intensity recorded between 0.4 and 100 GeV; the dust optical depth at 353 GHz, τ353; the thermal radiance of the large grains; and an estimate of the dust extinction, AVQ, empirically corrected for the starlight intensity. The dust and γ-ray models have been coupled to account for the DNM gas. The consistent γ-ray emissivity spectra recorded in the different phases confirm that the GeV–TeV cosmic rays probed by the LAT uniformly permeate all gas phases up to the 12CO cores. The dust and cosmic rays both reveal large amounts of DNM gas, with comparable spatial distributions and twice as much mass as in the CO-bright clouds. We give constraints on the H i-DNM-CO transitions for five separate clouds. CO-dark H2 dominates the molecular columns up to AV ≃ 0.9 and its mass often exceeds the one-third of the molecular mass expected by theory. The corrected AVQ extinction largely provides the best fit to the total gas traced by the γ rays. Nevertheless, we find evidence for a marked rise in AVQ/NH with increasing NH and molecular fraction, and with decreasing dust temperature. The rise in τ353/NH is even steeper. We observe variations of lesser amplitude and orderliness for the specific power of the grains, except for a coherent decline by half in the CO cores. This combined information suggests grain evolution. We provide average values for the dust properties per gas nucleon in the different phases. The γ rays and dust radiance yield consistent XCO estimates near 0.7 × 1020 cm-2 K-1 km-1 s. The AVQ and τ353 tracers yield biased values because of the large rise in grain opacity in the CO clouds. These results clarify a recurrent disparity in the γ-ray versus dust calibration of XCO, but they confirm the factor of 2 difference found between the XCO estimates in nearby clouds and in the neighbouring spiral arms.The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, J.A., and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).Peer Reviewe

Planck 2015 results. XXI. The integrated Sachs-Wolfe effect

Cosmology (including clusters of galaxies).-- et al.This paper presents a study of the integrated Sachs-Wolfe (ISW) effect from the Planck 2015 temperature and polarization data release. This secondary cosmic microwave background (CMB) anisotropy caused by the large-scale time-evolving gravitational potential is probed from different perspectives. The CMB is cross-correlated with different large-scale structure (LSS) tracers: radio sources from the NVSS catalogue; galaxies from the optical SDSS and the infrared WISE surveys; and the Planck 2015 convergence lensing map. The joint cross-correlation of the CMB with the tracers yields a detection at 4σ where most of the signal-to-noise is due to the Planck lensing and the NVSS radio catalogue. In fact, the ISW effect is detected from the Planck data only at ≈3σ (through the ISW-lensing bispectrum), which is similar to the detection level achieved by combining the cross-correlation signal coming from all the galaxy catalogues mentioned above. We study the ability of the ISW effect to place constraints on the dark-energy parameters; in particular, we show that ΩΛ is detected at more than 3σ. This cross-correlation analysis is performed only with the Planck temperature data, since the polarization scales available in the 2015 release do not permit significant improvement of the CMB-LSS cross-correlation detectability. Nevertheless, the Planck polarization data are used to study the anomalously large ISW signal previously reported through the aperture photometry on stacked CMB features at the locations of known superclusters and supervoids, which is in conflict with ΛCDM expectations. We find that the current Planck polarization data do not exclude that this signal could be caused by the ISW effect. In addition, the stacking of the Planck lensing map on the locations of superstructures exhibits a positive cross-correlation with these large-scale structures. Finally, we have improved our previous reconstruction of the ISW temperature fluctuations by combining the information encoded in all the previously mentioned LSS tracers. In particular, we construct a map of the ISW secondary anisotropies and the corresponding uncertainties map, obtained from simulations. We also explore the reconstruction of the ISW anisotropies caused by the large-scale structure traced by the 2MASS Photometric Redshift Survey (2MPZ) by directly inverting the density field into the gravitational potential field.The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MINECO, JA, and RES (Spain); Tekes, AoF, and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); ERC and PRACE (EU).Peer Reviewe