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Context. The characterization of white dwarf atmospheres is crucial for accurately deriving stellar parameters such as effective temperature, mass, and age. However, the inclusion of physical processes such as convective mixing and convective dilution in current white dwarf atmospheric models offers a prediction of the spectral evolution of these objects. To constrain these models, accurate observational data and analyses are necessary. Aims. We aim to classify the population of white dwarfs up to 500 pc into hydrogen-rich or hydrogen-deficient atmospheres based on Gaia spectra and to derive an accurate spectral type-temperature distribution, namely, the ratio between the number of non-DAs to the total number of white dwarfs as a function of the effective temperature for the largest observed unbiased sample of these objects. Methods. We took advantage of the recent Gaia low-resolution spectra available for 76 657 white dwarfs up to 500 pc. We calculated the synthetic J-PAS narrow-band photometry and fit the spectral energy distribution of each object with up-to-date models for hydrogen-rich and helium-rich white dwarf atmospheres. We estimated the probability for a white dwarf to have a hydrogen-rich atmosphere and validated the results using the Montreal White Dwarf Database. Finally, precise effective temperature values were derived for each object using La Plata evolutionary models. Results. We successfully classified a total of 65 310 white dwarfs (57 155 newly classified objects) into DAs and non-DAs with an accuracy of 94%. An unbiased subsample of nearly 34 000 objects was built, from which we computed a precise spectral distribution spanning an effective temperature range from 5500 to 40 000 K, while accounting for potential selection effects. Conclusions. Some characteristic features of the spectral evolution, such as the deficit of helium-rich stars at Teff ˜ 35 000 - 40 000 K and in the range of 22 000 ¿ Teff ¿ 25 000 K, as well as a gradual increase from, We acknowledge support from MINECO under the PID2020-117252GB-I00 grant and by the AGAUR/Generalitat de Catalunya grant SGR-386/2021. P.C. acknowledges financial support from the Govern- ment of Comunidad Autónoma de Madrid (Spain) via postdoctoral grant ‘Atrac- ción de Talento Investigador’ 2019-T2/TIC-14760. R.M.O. is funded by INTA through grant PRE-OBSERVATORIO. MC acknowledges grant RYC2021- 032721-I, funded by MCIN/AEI/10.13039/501100011033 and by the Euro- pean Union NextGenerationEU/PRTR. RR acknowledges support from Grant RYC2021-030837-I funded by MCIN/AEI/ 10.13039/501100011033 and by “European Union NextGenerationEU/PRTR”. F.J.E. acknowledges support from ESA through the Faculty of the European Space Astronomy Centre (ESAC) – Funding reference 4000139151/22/ES/CM. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www. cosmos.esa.int/gaia), processed by the Gaia Data Processing and Anal- ysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/ consortium). Funding for the DPAC has been provided by national insti- tutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work has made use of the Python package GaiaXPy, devel- oped and maintained by members of the Gaia Data Processing and Analy- sis Consortium (DPAC) and in particular, Coordination Unit 5 (CU5), and the Data Processing Centre located at the Institute of Astronomy, Cambridge, UK (DPCI). This publication makes use of VOSA, developed under the Spanish Virtual Observatory (https://svo.cab.inta-csic.es) project funded by MCIN/AEI/10.13039/501100011033/ through grant PID2020-112949GB-I00. We extensively made used of Topcat (Taylor 2005). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. We acknowledge use of the ADS bibliographic services., Peer Reviewed, Postprint (published version)

The third data release of Gaia has provided low resolution spectra for 100 000 white dwarfs (WDs) that, together with the excellent photometry and astrometry, represent an unrivalled benchmark for the study of this population. In this work, we first built a highly-complete volume-limited sample consisting in 12 718 WDs within 100 pc from the Sun. The use of VOSA tool allowed us to perform an automated fitting of their spectral energy distributions to different atmospheric models. In particular, the use of spectrally derived J-PAS photometry from Gaia spectra led to the classification of DA and non-DA WDs with an accuracy ¡ 90%, tested in already spectroscopically labelled objects. The excellent performance achieved was extended to practically the whole population of WDs with effective temperatures above 5500 K. Our results show that, while the A branch of the Gaia WD Hertzsprung-Russell diagram is practically populated by DA WDs, the B branch is largely formed by non-DAs (65%). The remaining 35% of DAs within the B branch implies a second peak at 0.8 M in the DA- mass distribution. Additionally, the Q branch and its extension to lower temperatures can be observed for both DA and non-DA objects due to core crystallisation. Finally, we derived a detailed spectral evolution function, which confirms a slow increase of the fraction of non-DAs as the effective temperature decreases down to 10 500 K, where it reaches a maximum of 36% and then decreases for lower temperatures down to 31%, We are greatly indebted to Detlev Koester for providing us with his white dwarf model atmosphere spectra. ST acknowledges fruitful discussion and data provided by Carlos López-Sanjuan. We also thank to the referee Dr Jay Holberg for his valuable comments. FJE acknowledges financial support from the Servicio P ¨ublico de Empleo Estatal, Spain. PC acknowledges financial support from the Government of Comunidad Autónoma de Madrid (Spain) via postdoctoral grant ‘Atracción de Talento Investigador’ 2019-T2/TIC-14760. ST and ARM acknowledge support from MINECO under the PID2020-117252GB-I00 grant. ARM acknowledges support from Grant RYC-2016-20254 funded by MCIN/AEI/10.13039/501100011033 and by ESF Investing in your future. RMO is funded by INTA through grant PRE- OBSERVATORIO. MEC acknowledges support from NASA grants (HGC) 80NSSC17K0008 and (LWS) 80NSSC20K0193 and the University of Colorado Boulder., Peer Reviewed, Postprint (published version)

206 p, Los abusos sexuales contra niñas, niños y adolescentes son una problemática grave y extendida, con una alta incidencia en nuestra sociedad. Se estima que afecta a una de cada cuatro niñas y a uno de cada siete niños, generalmente antes de cumplir los 13 años, siendo la incidencia mayor en los colectivos en exclusión. __ Pese a ello, no existe formación reglada sobre esta materia para las y los profesionales que tienen relación directa en la intervención de casos con víctimas de abuso sexual. Esto es, no se trabajan los abusos sexuales en los grados, másteres y formaciones continuas de las y los profesionales que tienen relación con infancia y adolescencia (medicina, psicología, trabajo social, educación, etc.). __ Mediante este libro se busca comenzar a colmar esta necesidad. En lugar de focalizar en la concienciación o sensibilización sobre la problemática, se apuesta por trabajar los principales criterios y contenidos necesarios, en la intervención de casos de abuso, en los ámbitos profesionales más implicados: educación, servicios sociales, seguridad, justicia y salud. Es objetivo principal de este libro el fomento del trabajo interdisciplinar, en red, entre los diferentes profesionales que participan en las respuestas institucionales ante un caso de abuso sexual contra niñas, niños y adolescentes.