Sensory Perception

Different types of sensory systems with their functional modalities will be presented. The biological bases for how these functions are generated and modified will then be described. As vision is the principal means of perception, we will focus in this course most on visual processing. Scientific data will be integrated into the lectures, such that students develop critical skills in analyzing data and proposing hypotheses

A single H/ACA small nucleolar RNA mediates tumor suppression downstream of oncogenic RAS.

Small nucleolar RNAs (snoRNAs) are a diverse group of non-coding RNAs that direct chemical modifications at specific residues on other RNA molecules, primarily on ribosomal RNA (rRNA). SnoRNAs are altered in several cancers; however, their role in cell homeostasis as well as in cellular transformation remains poorly explored. Here, we show that specific subsets of snoRNAs are differentially regulated during the earliest cellular response to oncogenic RASG12V expression. We describe a novel function for one H/ACA snoRNA, SNORA24, which guides two pseudouridine modifications within the small ribosomal subunit, in RAS-induced senescence in vivo. We find that in mouse models, loss of Snora24 cooperates with RASG12V to promote the development of liver cancer that closely resembles human steatohepatitic hepatocellular carcinoma (HCC). From a clinical perspective, we further show that human HCCs with low SNORA24 expression display increased lipid content and are associated with poor patient survival. We next asked whether ribosomes lacking SNORA24-guided pseudouridine modifications on 18S rRNA have alterations in their biophysical properties. Single-molecule Fluorescence Resonance Energy Transfer (FRET) analyses revealed that these ribosomes exhibit perturbations in aminoacyl-transfer RNA (aa-tRNA) selection and altered pre-translocation ribosome complex dynamics. Furthermore, we find that HCC cells lacking SNORA24-guided pseudouridine modifications have increased translational miscoding and stop codon readthrough frequencies. These findings highlight a role for specific snoRNAs in safeguarding against oncogenic insult and demonstrate a functional link between H/ACA snoRNAs regulated by RAS and the biophysical properties of ribosomes in cancer

Magnetic fields in M dwarfs from the CARMENES survey

M dwarfs are known to generate the strongest magnetic fields among main-sequence stars with convective envelopes, but the link between the magnetic fields and underlying dynamo mechanisms, rotation, and activity still lacks a consistent picture. In this work we measure magnetic fields from the high-resolution near-infrared spectra taken with the CARMENES radial-velocity planet survey in a sample of 29 active M dwarfs and compare our results against stellar parameters. We use the state-of-the-art radiative transfer code to measure total magnetic flux densities from the Zeeman broadening of spectral lines and filling factors. We detect strong kG magnetic fields in all our targets. In 16 stars the magnetic fields were measured for the first time. Our measurements are consistent with the magnetic field saturation in stars with rotation periods P<4d. The analysis of the magnetic filling factors reveal two different patterns of either very smooth distribution or a more patchy one, which can be connected to the dynamo state of the stars and/or stellar mass. Our measurements extend the list of M dwarfs with strong surface magnetic fields. They also allow us to better constrain the interplay between the magnetic energy, stellar rotation, and underlying dynamo action. The high spectral resolution and observations at near-infrared wavelengths are the beneficial capabilities of the CARMENES instrument that allow us to address important questions about the stellar magnetism.Comment: 13 pages of main text, 14 pages of online material, 2 table

Dark Matter and Fundamental Physics with the Cherenkov Telescope Array

The Cherenkov Telescope Array (CTA) is a project for a next-generation observatory for very high energy (GeV-TeV) ground-based gamma-ray astronomy, currently in its design phase, and foreseen to be operative a few years from now. Several tens of telescopes of 2-3 different sizes, distributed over a large area, will allow for a sensitivity about a factor 10 better than current instruments such as H.E.S.S, MAGIC and VERITAS, an energy coverage from a few tens of GeV to several tens of TeV, and a field of view of up to 10 deg. In the following study, we investigate the prospects for CTA to study several science questions that influence our current knowledge of fundamental physics. Based on conservative assumptions for the performance of the different CTA telescope configurations, we employ a Monte Carlo based approach to evaluate the prospects for detection. First, we discuss CTA prospects for cold dark matter searches, following different observational strategies: in dwarf satellite galaxies of the Milky Way, in the region close to the Galactic Centre, and in clusters of galaxies. The possible search for spatial signatures, facilitated by the larger field of view of CTA, is also discussed. Next we consider searches for axion-like particles which, besides being possible candidates for dark matter may also explain the unexpectedly low absorption by extragalactic background light of gamma rays from very distant blazars. Simulated light-curves of flaring sources are also used to determine the sensitivity to violations of Lorentz Invariance by detection of the possible delay between the arrival times of photons at different energies. Finally, we mention searches for other exotic physics with CTA.Comment: (31 pages, Accepted for publication in Astroparticle Physics

Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010

Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED). Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail. Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E> 100 GeV) γ-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population. Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2–10 keV band and the VHE γ-ray flux above 200 GeV, consistent with the γ-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE γ-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 × 104<γ< 6 × 105, where γ is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands. Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (δ, B and R), in addition to the parameters related to the particle population.Fil: Aleksic, J.. IFAE; EspañaFil: Ansoldi, S.. Università di Udine; ItaliaFil: Antonelli, L. A.. INAF National Institute for Astrophysics; ItaliaFil: Antoranz, P.. Università di Siena; ItaliaFil: Babic, A.. University of Rijeka; CroaciaFil: Bangale, P.. Max-Planck-Institut für Physik; AlemaniaFil: Barres de Almeida, U.. Max-Planck-Institut für Physik; AlemaniaFil: Barrio, J. A.. Universidad Complutense de Madrid; EspañaFil: Becerra Gonzalez, J.. Inst. de Astrofísica de Canarias; EspañaFil: Bednarek, W.. University of Łódź,; PoloniaFil: Bernardini, E.. Deutsches Elektronen-Synchrotron (DESY); AlemaniaFil: Biasuzzi, B.. Università di Udine; ItaliaFil: Biland, A.. ETH Zurich; SuizaFil: Blanch, O.. IFAE; EspañaFil: Boller, A.. ETH Zurich; SuizaFil: Bonnefoy, S.. Universidad Complutense de Madrid; EspañaFil: Bonnoli, G.. INAF National Institute for Astrophysics ; ItaliaFil: Borracci, F.. Max-Planck-Institut für Physik; AlemaniaFil: Bretz, T.. Universität Würzburg ; AlemaniaFil: Carmona, E.. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas ; EspañaFil: Carosi, A.. INAF National Institute for Astrophysics; ItaliaFil: Colin, P.. Max-Planck-Institut für Physik; AlemaniaFil: Colombo, E.. Inst. de Astrofísica de Canarias; EspañaFil: Contreras, J. L.. Universidad Complutense; EspañaFil: Cortina, J.. IFAE; EspañaFil: Covino, S.. INAF National Institute for Astrophysics; ItaliaFil: Da Vela, P.. Università di Siena; ItaliaFil: Dazzi, F.. Max-Planck-Institut für Physik; AlemaniaFil: Pichel, Ana Carolina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Rovero, Adrian Carlos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: The Veritas Collaboration.Fil: The MAGIC Collaboration

Measurement of the cosmic ray spectrum above 4×10184{\times}10^{18} eV using inclined events detected with the Pierre Auger Observatory

A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\gamma}$ with index $\gamma=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV.Comment: Replaced with published version. Added journal reference and DO

The first record of the genus Plega Navás, 1928 (Neuroptera: Rhachiberothidae: Symphrasinae) as a parasitoid of the sawfly genus Monoctenus Dahlbom, 1835 (Hymenoptera: Symphyta: Diprionidae)

The genus Plega Navás, 1928, belongs to the subfamily Symphrasinae, a group recently transferred from Mantispidae to Rhachiberothidae. This genus is herein reported as parasitoid of the symphytan family Diprionidae for the first time, becoming the first record of association between this neuropteran subfamily and non-aculeate Hymenoptera. This new association was discovered in “Ixcateopan de Cuauhtémoc”, in the Mexican state of Guerrero, where Plega spinosa Ardila et al., 2019 was found associated with immatures of the sawfly Monoctenus cuauhtemoci De Lira, 2021, a pest in forests of Juniperus flaccida Schlechtendal (white cedar). The neuropteran was found to be the most abundant parasitoid of this symphytan, becoming a potential candidate for biological control of phytophagous sawflies in juniper forests, an economically important plant species for the wood industry in the region. Considering the behavior and morphological aspects of the primary larvae and the behavior of the adults of Plega, three possible scenarios in which the primary larvae of P. spinosa board the larvae of Monoctenus to complete its life cycle are outlined. This finding reinforces the hypothesis of a generalist ectoparasitoid lifeway of the larvae of the genus Plega on larvae and pupae of holometabolous insects

Desarrollo de una propuesta de mejora para los procesos de fabricación en el sector de alimentos

El servicio y atención al cliente en los restaurantes prácticamente tiende a ofrecer lo mismo que sus competidores, por esta razón la mayoría de ellos convergen al fracaso. La logística que se debe emplear para garantizar el buen funcionamiento de la propuesta de los negocios en el sector de comidas rápidas se hace cada vez más importante, porque se debe recopilar una serie de información necesaria para lograr los objetivos que desea cumplir todo empresario. Desde la selección de proveedores calificados, los procesos y procedimientos estandarizados para desarrollar los productos, hasta la venta y satisfacción al consumidor final en el momento oportuno. La investigación del mercado es muy relevante para pronosticar y anticiparse a la demanda de los futuros y vigentes clientes. Es indispensable el manejo sistémico y logístico de una entidad empresarial de alimentos, ya que se deben organizar todas las actividades dentro de un proceso de fabricación. Es importante crear valor para los comensales, implementando las buenas prácticas de los procesos de fabricación del producto, satisfaciendo los tiempos de entrega a los comensales, mediante las diferentes herramientas de estudio como la estandarización de procesos y procedimientos, diagramas de flujo y diseño de planta para poder implementar dichas herramientas dentro de las entidades empresariales del sector de comida rápida y de esta forma lograr diagnosticar problemas a tiempo para dar una rápida respuesta y satisfacer las necesidades del mercado

Parámetros de resistencia mecánica de muros de tapial con un % en volumen de adición de tallos de cebada, Yauli - Huancavelica, 2021.

El siguiente estudio investigativo que lleva por título: Parámetros de resistencia mecánica de muros de tapial con un % en volumen de adición de tallos de cebada, Yauli-Huancavelica, 2021. Tuvo como finalidad fundamtenal, la determinación del incremento de los parámetros de resistencia mecánica del muro de tapial con un % en volumen de adición de tallos de cebada, Yauli-Huancavelica, 2021, de la misma manera se determinó la resistencia de tapial a compresión, tracción indirecta y flexión con una muestra patrón de 0% de adición de tallos de cebada y muestras con adición de tallos de cebada en 10%,15% y 20%. De acuerdo a este planteamiento, el presente proyecto investigativo es de tipo aplicado, de nivel explicativo, con método científico y diseño experimental por lo que se manipuló los % en volumen de adición de tallos de cebada para medir el parámetro de resistencia mecánica de los muros de tapial, la técnica que se utilizó fue la observación directa y el instrumento la ficha de observación, la población de esta investigación está constituida por 72 especímenes y la muestra está por 48. Finalmente se concluyó que los parámetros de resistencia mecánica de muros de tapial al adicionar un porcentaje de volumen de tallo de cebada incrementan de manera creciente y favorable, obteniéndose un resultado óptimo con 15% en volumen de adición de tallo de cebada. Sin embargo, para los valores como el 20% de adición de tallos de cebada la resistencia disminuye en relación al tapial con 15% de adición

The 2009 multiwavelength campaign on Mrk 421: Variability and correlation studies

Aims: We perform an extensive characterization of the broadband emission of Mrk 421, as well as its temporal evolution, during the non-flaring (low) state. The high brightness and nearby location (z = 0.031) of Mrk 421 make it an excellent laboratory to study blazar emission. The goal is to learn about the physical processes responsible for the typical emission of Mrk 421, which might also be extended to other blazars that are located farther away and hence are more difficult to study. Methods: We performed a 4.5-month multi-instrument campaign on Mrk 421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. This extensive radio to very-high-energy (VHE; E> 100 GeV) γ-ray dataset provides excellent temporal and energy coverage, which allows detailed studies of the evolution of the broadband spectral energy distribution. Results: Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical/UV and X-rays extending over the duration of the campaign. Conclusions: The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multi-wavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk 421 during non-flaring activity. Such a temporally extended X-ray/VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies.Fil: Aleksic, J.. IFAE; EspañaFil: Ansoldi, S.. Università di Udine; ItaliaFil: Antonelli, L. A.. INAF National Institute for Astrophysics; ItaliaFil: Antoranz, P.. Università di Siena; ItaliaFil: Babic, A.. University of Rijeka; CroaciaFil: Bangale, P.. Max-Planck-Institut für Physik; AlemaniaFil: Barres de Almeida, U.. Max-Planck-Institut für Physik; AlemaniaFil: Barrio, J. A.. Universidad Complutense de Madrid; EspañaFil: Becerra Gonzalez, J.. Inst. de Astrofísica de Canarias; EspañaFil: Bednarek, W.. University of Lodz; PoloniaFil: Berger, K.. Inst. de Astrofísica de Canarias; EspañaFil: Bernardini, E.. Deutsches Elektronen-Synchrotron (DESY); AlemaniaFil: Bijand, A.. ETH Zurich; SuizaFil: Blanch, O.. IFAE; EspañaFil: Bock, R. K.. Max-Planck-Institut für Physik; AlemaniaFil: Bonnefoy, S.. Universidad Complutense; EspañaFil: Bonnoli, G.. INAF National Institute for Astrophysics; ItaliaFil: Borracci, F.. Max-Planck-Institut für Physik; AlemaniaFil: Bretz, T.. Universität Würzburg,; AlemaniaFil: Carmona, E.. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas; EspañaFil: Carosi, A.. INAF National Institute for Astrophysics; EspañaFil: Carreto Fidalgo, D.. Universität Würzburg; AlemaniaFil: Colin, P.. Max-Planck-Institut für Physik; AlemaniaFil: Colombo, E.. Inst. de Astrofísica de Canarias; EspañaFil: Contreras, J. L.. Universidad Complutense; EspañaFil: Cortina, J.. IFAE; EspañaFil: Covino, S.. INAF National Institute for Astrophysics; ItaliaFil: Pichel, Ana Carolina. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: Rovero, Adrian Carlos. Consejo Nacional de Investigaciónes Científicas y Técnicas. Oficina de Coordinación Administrativa Ciudad Universitaria. Instituto de Astronomía y Física del Espacio. - Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales. Instituto de Astronomía y Física del Espacio; ArgentinaFil: The Magic Collaboration.Fil: The Veritas Collaboration