Educando para la vida: Programa de Educación Emocional dirigido a profesores y alumnos de 1º y 2º de ESO

Postgrau en Educació Emocional i Benestar [Presencial]. Institut de Ciències d'Educació i el Grup de Recerca en Orienració Psicopedagògica (GROP). Universitat de Barcelona, Curs: 2018-2019, Tutora: Irene Pellicer RoyoEste proyecto nace con el deseo de sembrar la semilla de la Educación Emocional por vez primera en el centro concertado “Escuelas Santísimo Sacramento” sito en Madrid, ciudad en la que resido. Esta institución, promueve la educación integral de los alumnos con una concepción cristiana de la vida, a través de principios que contemplan la participación de los educadores en los intereses de los alumnos ofreciéndoles elementos de maduración personal y fomentando el desarrollo de competencias que les permitan afrontar y superar situaciones difíciles y/o de riesgo, la creación de un ambiente educativo que sitúe a los estudiantes como protagonistas de su propio proceso de enseñanza-aprendizaje, estimulando su creatividad y cultivando valores como el esfuerzo y el espíritu de trabajo y, todo ello, en un clima de alegría y sentido de fiesta que invita al descubrimiento y celebración de los aspectos positivos de la vida y que está encaminado, por lo tanto, a la búsqueda del bienestar personal (Escuelas Santísimo Sacramento, 2017). Tras varias entrevistas con la orientadora como parte del análisis y valoración del contexto en el que se llevará a cabo la intervención, se han identificado como principales destinatarios del programa de Educación Emocional que aquí se presenta los siguientes grupos: el profesorado de los distintos niveles educativos de este colegio, y los alumnos de 1º y 2º de Educación Secundaria Obligatoria (en adelante, ESO). Las características y necesidades específicas de ambos serán abordadas en el siguiente apartado de este documento..

Diagnostics and modeling of cold laboratory plasmas with high hydrogen content; applications to molecular astrophysics.

First General Meeting in Prague, May 25 - 29, 2015; http://prague2015astrohistory.vscht.cz/Cold plasmas of molecular precursors produced in low pressure glow discharges involve intricate mechanisms of great interest in many scientific and technological fields, such as thin film growth, surface conditioning and so on. In particular, hydrogen containing cold plasmas are currently used in microelectronic devices production, can simulate the border conditions of plasmas generated in fusion reactors, and are efficient sources of very reactive radicals and ions, whose study contributes to clarify the appearance of complex compounds in different regions of interstellar molecular clouds or in Jovian planet ionospheres. In this work, low pressure glow discharges of mixtures of hydrogen with simple molecules and atoms and different isotopic compositions are experimentally diagnosed, and the main mechanisms controlling their behavior are elucidated by kinetic modeling. According to theoretical predictions supported by experimental data, the formation of new molecular species takes place mainly at the reactor surfaces and competes with the fast wall recycling of the precursors, which are previously dissociated by electron impact. On the other hand, the ion distributions result mainly from the balance between electron impact ionizations, which depend markedly on electron energies, and ion-molecule reactions in gas phase, for which the proton affinity of the different neutral species plays a key role. The first detection of the deuterated ammonium ion (NH3D+) in the interstellar medium [1,2], and the refined infrared spectroscopic characterization of the isotopomers 36ArH+ and 36ArH+ [3], the first noble gas molecules found in space [4,5], exemplify the successful interaction between plasma spectroscopy and astronomical observations.The authors acknowledge the financial support from the Spanish MINECO through grants SD2009-00038, FIS2012- 38175 and FIS2013-48087-C2-1-P. Additional funding from ERC-2013-Syg 610256-NANOCOSMOS is also aknowledged.Peer Reviewe

Cold plasmas in laboratory astrochemistry: Ions and carbonaceous dust analogues

Colloquium SFB 956, Physikalische Institute Köln, 18.05.2015Peer Reviewe

Accurate wavenumber measurements of vibration-rotation transitions of 36ArH+ and 38ArH+

Presentación Power Point de 13 diapositivas. 69th International Symposium on Molecular Spectroscopy, Champaign-Urbana, Illinois (USA), June 16-20 2014 http://210.107.182.111/board/596/The protonated Ar ion 36ArH+ has recently been identified in space in the Crab Nebula, from Herschel spectra. Its R(0) and R(1) transitions lie at 617.5 and 1234.6 GHz, respectively, where atmospheric transmission is rather poor, even for a site as good as that of ALMA. As an alternative, especially after the end of the Herschel mission, rovibrational transitions of ArH+ could be observed in absorption against bright background sources such as the galactic center, or other objects. We report on accurate laboratory wavenumber measurements of 19 lines of the v = 1-0 band of 36ArH+ and 38ArH+, using a hollow cathode discharge cell, a difference frequency laser spectrometer and Ar with natural isotopic composition. Of those lines, only eight had been reported before and with much less accuracy. The data have also been used in a Dunham-type global fit of all published laboratory data (IR and sub-mm) of all isotopologues.N

Continuous waves stimulated raman spectrocopy inside a holow core photonic crystal fiber.

Peer Reviewe

Sensitivity enhancement in high resolution stimulated Raman spectroscopy of gases with hollow-core photonic crystal fibers

4 pags. ; 3 figs.We show the first experimental evidence of the sensitivity enhancement that can be achieved in high resolution stimulated Raman spectroscopy of gases using hollow-core photonic crystal fibers (HCPCFs). Using low power cw lasers and a HCPCF containing the gas, we have observed more than four orders of magnitude enhancement of sensitivity when compared with the cw single focus regime, and a similar sensitivity to that achieved in the more sensitive quasi-cw setups with multipass cells. © 2013 Optical Society of America.This work has been funded by the Spanish MINECO through grants CSD2009-00038, FIS2009-08069, and FIS2012-38175. M.C. acknowledges financial support from EU-FEDER funds through a CSIC JAE-Tec contract.Peer reviewe

High resolution vibration-rotation spectroscopy with two lasers: Infrared and Raman Experiments

Peer Reviewe

CONTINUOUS WAVE STIMULATED RAMAN SPECTROSCOPY INSIDE A HOLLOW CORE PHOTONIC CRYSTAL FIBER

Author Institution: Instituto de Estructura de la Materia (IEM-CSIC), Serrano 123, E-28006 Madrid, Spain. (email to J.L.D.: [email protected])Hollow-core photonic crystal fibers nderline{\textbf{299}}, 358, 2003.} (HCPCF) have raised new opportunities to study light-matter interaction. Dielectric or metallic capillaries are intrinsically lossy, making poor light guides. In contrast, HCPCFs can guide light quite efficiently, due to the band-gap effect produced by an array of smaller channels which surrounds a central hollow core with a few $\mu$m diameter. The tight confinement of light inside the core, that can be filled with gases, as well as a long interaction length, enhance multiple nonlinear phenomena, making it possible to devise new ways to do low signal level spectroscopy, as is the case of high resolution stimulated Raman spectroscopy (SRS). A. Owyoung nderline{\textbf{59}}, 156, 1978} demonstrated high resolution continuous wave SRS in 1978. Shortly afterwards, seeking higher sensitivity, he developed the \textit{quasi-continuous} SRS technique (a high peak power pump laser, interacting with a low power cw probe laser). That variant remains today the best compromise between resolution and sensitivity for gas-phase Raman spectroscopy. In this work, we show the possibility of fully cw stimulated Raman spectroscopy, using a gas cell built around a HCPCF to overcome the limitations posed by the weakness of the stimulated Raman effect when not using pulsed sources. The interaction length (1.2 m), longer than that of a multiple pass refocusing cell, and the narrow diameter of the core (4.8 $\mu$m), can compensate for the much lower laser powers used in the cw set-up. The experimental complexity is considerably reduced and the instrumental resolution is at the 10's of MHz level, limited, with our fiber, by transit time effects. At present, we have demonstrated the feasibility of the experiment, a sensitivity enhancement of $\sim$ 6000 over the single focus regime, and a spectral resolution better than 0.005 \wn in the unresolved Q-branch of the $\nu_1$ component of the Fermi dyad of CO$_2$ at 1388 \wn. Other examples of rotationally resolved spectra will be shown: the Q branch of O$_2$ at 1555 \wn, and the 2$\nu_2$ component of the Fermi dyad of CO$_2$ at 1285 \wn

A new way to enhance sensitivity in stimulated Raman spectroscopy: Hollow-core photonic crystal fibers.

Stimulated Raman Scattering gain/loss (SRS) processes have a very low efficiency, so, for spectroscopic applications some combination of pulsed laser sources is normally used. Although continuous wave SRS spectroscopy was demonstrated in 1978 by Owyoung et al.1 getting the highest resolution up to now, shortly after that, he developed the quasi-continuous SRS technique which uses a high peak power pulsed pump laser, which is the best compromise achieved between resolution and sensitivity for these gas-phase spectroscopies. A new way to enhance sensitivity without sacrificing resolution, apart from using multipass refocusing cells and cavity enhanced techniques, is to use hollow-core photonic crystal fibers2 (HCPCF), which are very suitable due to the tight confinement of light and gas inside the core and the long interaction length. In our set-up for cw-SRS loss spectroscopy, a cw-single mode Ar+ probe laser and a cw-single mode tunable dye pump laser (both lasers are stabilized in frequency) interact with a gas sample. Whenever their frequency difference matches that of a Raman-allowed transition of the sample, the probe laser undergoes a loss of power. In our experiment, the gas is placed in a cell formed by a 1.2m length and 4.8µm core diameter HCPCF. We have demonstrated that this new technique enhances the sensitivity of SRS experiments around 6000 times over that of single focus cw-SRS. We will show several examples such as the Q-branch of the ¿1 and 2¿2 components of the Fermi dyad CO2 at 1388 and 1286 cm-1 respectively, or the Q-branch of O2 at 1555 cm-1.Peer Reviewe

High resolution infrared absorption spectroscopy of ions of astrophysical interest: 36ArH+ and 38ArH+

XXII Europhysics Conference on Atomic and Molecular Physics of Ionized Gases, Greifswald, Germany, July 15-19, 2014• 36ArH+ and 38ArH+ have been recently identified by their rotational emissions in the Crab Nebula [1] and the interstellar media [2] from sub-mm spectra obtained with the Herschel Space Observatory. ArH+ is the first noble gas compound observed hitherto in space. Given the atmospheric opacity at these submm frequencies and the current lack of appropriate space telescopes after the recent end of the Herschel mission on Spring 2013, future studies of these ions will rely on ground-based IR observations. Incidentally, the Ar isotopic composition in the interstellar media is 40Ar/ 38Ar/ 36Ar = 0.0 / 15.0 / 85.0 %, but in the Earth’s atmosphere it is: 40Ar/ 38Ar/ 36Ar = 99.6 / 0.06 / 0.34 %; where 40Ar is mainly produced by 40K decay (½ = 1.25 × 109 years). • In laboratories, ArH+ can be efficiently produced in H2 + Ar low pressure plasmas [3,4], but its density depends strongly on the discharge conditions. • In this work, the high resolution IR absorption spectra of 36ArH+ and 38ArH+ generated in a low pressure hollow cathode discharge have been measured with a difference frequency laser spectrometer. Accurate wavenumbers of 19 ro-vibrational lines of the v = 1–0 band in the range 4.1–3.7 μm (2450–2715 cm−1) have been obtained. Of those, only eight had been reported before, and with much larger uncertainty. The results will be useful for further astrophysical searches of these ions.The authors acknowledge the financial support from the Spanish MINECO through the grants SD2009‐00038 (ConsoliderAstromol ), FIS2012‐38175, FIS2010‐16455, AYA2009‐07304 and AYA2012‐32032.N