A low-pass filter with automatic frequency tuning for a bluetooth receiver

A third-order Gm-C Chebyshev low-pass filter with high linearity and automatic frequency programmability has been designed. The filter is intended to be used as a channel-select filter for a zero-IF Bluetooth receiver. The frequency tuning scheme is simpler and has more relaxed specifications than conventional ones. The filter bandwidth is 0.5 MHz and the overall scheme dissipates 1.1 mA from a 1.8-V supply. The third-order intermodulation (IM3) distortion of the filter for a 1Vpp two-tone signal centered at 350 kHz is -67dB.Ministerio de Ciencia y Tecnología TEC2007-67460-C03-02

Abundance analysis of planet-hosting and debris-disk stars

Abstract: We present an analysis of element abundances in planet-hosting and debrisdisk stars based on high-resolution spectra obtained with the FEROS echelle spectrograph and the 2.2-m ESO telescope at La Silla. Atmospheric parameters and abundance patterns for the stars are determined. A comparison of the abundances is made between planethosting stars, debris-disk stars, and field starshttp://astars2013.inasan.ru/proceedings/publishedVersionFil: Carolina Andrea Chavero. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina.Astronomía (incluye Astrofísica y Ciencias del Espacio

Abundance Pattern Analysis of Planet-hosting and Debris-disk Stars

Abstract: About 16 % of the main-sequence solar-like stars are surrounded by dusty debris disks (DD). These disks are the detritus of small bodies collisions and their presence is a very strong signpost of planet formation. One of the most interesting characteristics of stars hosting a giant planet is a direct relationship between metallicity and probability of planet formation, which was found to increase with stellar metallicity Gonzalez (1997). Instead, the small planets would form around host stars (HS) with a wide range of metallicities (Buchhave et al. 2012). On the other hand the presence of debris disks is uncorrelated with metallicity (Chavero et al. 2006, Greaves et al. 2006, Maldonado et al. 2012).http://www.aspbooks.org/a/volumes/article_details/?paper_id=36464Fil: Chavero, Carolina Andrea. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina.Fil: Chavero, Carolina Andrea. Conicet. Argentina.Astronomía (incluye Astrofísica y Ciencias del Espacio

Modelo estadístico para la clasificación de la alimentación de cerdos ibéricos a partir de Cromatografía de gases (CG-FID) y Espectrometría de masas de relaciones isotópicas (GC-C-IRMS)

In the present work we have analyzed a total of 734 subcutaneous fat samples from Iberian pigs with different feeding systems for fattening (“Bellota”, “Recebo”, “Campo” and “Cebo”) over three consecutive years, 2009-2011. Lipids were extracted from the subcutaneous fat on the rump, and after esterification, they were analyzed by Gas Chromatography (GC-FID) and Gas Chromatography- Combustion-Isotope Ratio Mass Spectrometry (GC-C-IRMS). Mean fatty acids and isotope ratios show that there are differences according to the year and feeding systems, two factors that should be taken into account when classifying the animals. The application of different prediction models based on Discriminant analysis has allowed us to establish a method for the classification of animals according to the feeding system type, with a correct percentage of 85% using three or four classification categories (Bellota, Recebo, Campo and/or Cebo) and 91% using only two categories, Cebo and Bellota. This model could provide the basis for appropriate classification of Iberian pigs according to their feeding regime.En el presente trabajo se han analizado un total de 734 muestras de tejido subcutáneo de cerdos ibéricos con distintos tipos de alimentación de engorde (Bellota, Recebo, Cebo y Campo) a lo largo de tres años consecutivos, 2009-2011. Se han extraído los lípidos de la grasa subcutánea de rabadilla, y después de su esterificación, se han analizado por Cromatografía de gases (GC-FID) y por Espectrometría de masas de relaciones isotópicas (GC-C-IRMS). Las medias de los ácidos grasos y de las relaciones isotópicas muestran que existen diferencias según el año y tipo de alimentación, factores que deberían tenerse en cuenta a la hora de clasificar los animales. La aplicación de distintos modelos de predicción basados en análisis discriminante permite establecer un método para la clasificación de los animales según el tipo de alimentación, con un porcentaje de aciertos del 85% utilizando tres o cuatro categorías de clasificación (Bellota, Recebo, Campo y/o Cebo) y del 91% utilizando sólo dos categorías, Cebo y Bellota. Este modelo podría sentar las bases para una clasificación adecuada del cerdo ibérico en función de su alimentación

Statistical model for classifying the feeding systems of Iberian pigs through Gas Chromatography (GC-FID) and Isotope Ratio Mass Spectrometry (GC-C-IRMS)

In the present work we have analyzed a total of 734 subcutaneous fat samples from Iberian pigs with different feeding systems for fattening (“Bellota”, “Recebo”, “Campo” and “Cebo”) over three consecutive years, 2009-2011. Lipids were extracted from the subcutaneous fat on the rump, and after esterification, they were analyzed by Gas Chromatography (GC-FID) and Gas Chromatography- Combustion-Isotope Ratio Mass Spectrometry (GC-C-IRMS). Mean fatty acids and isotope ratios show that there are differences according to the year and feeding systems, two factors that should be taken into account when classifying the animals. The application of different prediction models based on Discriminant analysis has allowed us to establish a method for the classification of animals according to the feeding system type, with a correct percentage of 85% using three or four classification categories (Bellota, Recebo, Campo and/or Cebo) and 91% using only two categories, Cebo and Bellota. This model could provide the basis for appropriate classification of Iberian pigs according to their feeding regime.<br><br>En el presente trabajo se han analizado un total de 734 muestras de tejido subcutáneo de cerdos ibéricos con distintos tipos de alimentación de engorde (Bellota, Recebo, Cebo y Campo) a lo largo de tres años consecutivos, 2009-2011. Se han extraído los lípidos de la grasa subcutánea de rabadilla, y después de su esterificación, se han analizado por Cromatografía de gases (GC-FID) y por Espectrometría de masas de relaciones isotópicas (GC-C-IRMS). Las medias de los ácidos grasos y de las relaciones isotópicas muestran que existen diferencias según el año y tipo de alimentación, factores que deberían tenerse en cuenta a la hora de clasificar los animales. La aplicación de distintos modelos de predicción basados en análisis discriminante permite establecer un método para la clasificación de los animales según el tipo de alimentación, con un porcentaje de aciertos del 85% utilizando tres o cuatro categorías de clasificación (Bellota, Recebo, Campo y/o Cebo) y del 91% utilizando sólo dos categorías, Cebo y Bellota. Este modelo podría sentar las bases para una clasificación adecuada del cerdo ibérico en función de su alimentación

Evolved stars hint to an external origin of enhanced metallicity in planet-hosting stars

Exo-planets are preferentially found around high metallicity main sequence stars. We aim at investigating whether evolved stars share this property, and what this tells about planet formation. Statistical tools and the basic concepts of stellar evolution theory are applied to published results as well as our own radial velocity and chemical analyses of evolved stars. We show that the metal distributions of planet-hosting (P-H) dwarfs and giants are different, and that the latter do not favor metal-rich systems. Rather, these stars follow the same age-metallicity relation as the giants without planets in our sample. The straightforward explanation is to attribute the difference between dwarfs and giants to the much larger masses of giants' convective envelopes. If the metal excess on the main sequence is due to pollution, the effects of dilution naturally explains why it is not observed among evolved stars. Although we cannot exclude other explanations, the lack of any preference for metal-rich systems among P-H giants could be a strong indication of the accretion of metal-rich material. We discuss further tests, as well as some predictions and consequences of this hypothesis.Comment: A&A, in pres

Sinergini y chalcidoidea (Hymenoptera) asociados a una agalla inducida por Atrusca sp. (Hymenoptera: Cynipidae: Cynipini) de la región noroeste de Sierra de Guadalupe, Estado de México.

Los Cynipidae son insectos inductores de agallas en Quercus. Las agallas son consideradas un microecosistema constituidas por el cinípido inductor (Cynipini), por el c inípido inquilino (Synergini) y por un grupo de avispas (Chalcidoidea) cuya función no está estudiada. En México s e han descrito 180 especies de ci n í pidos, sin embargo, s e conoce poco acerca de la fauna asociada a las agallas y de las interacciones que se presentan, en este trabajo se da a conocer la fauna asociada a un morfotipo de agallas inducida por Atrusca sp. S obre Quercus mexicana . Se encontraro n 290 insect os pertenecientes a tres grupos: 257 Atrusca ( Cynipini) , 8 S ynergus (Synergini) y Chalcidoidea de cuatro géneros, 8 Baryscapus (Eulophidae), 1 Brasema (Eupelmidae), 2 Ormyrus (Ormy r idae), 3 Eurytoma y 2 Sycophila (Eurytomidae ). Los insectos asociados son nuevos registros para Atrusca , este trabajo proporciona bases para futuros estudios relacionados con la ecología de las interacciones en las agallas

Himenópteros asociados a las agallas de Andricus quercuslanigera (Hymenoptera: Cynipidae, Chalcidoidea) de Sierra de Guadalupe, estado de México.

Las agallas en Quercus se consideran un microecosistema, debido a que en ellas se asocian diferentes grupos de avispas: los Cynipini (Cynipidae) como inductores, los Synergini y Ceroptresini (Cynipidae) como inquilinos y los Chalcidoidea como parasitoides o hiperparasitoides. En México se han descrito 184 especies de cinípidos, sin embargo, se conoce poco acerca de la fauna asociada (inquilinos y calcidoídea) y de su ecología. En este estudio se da a conocer la fauna asociada a agallas inducidas por Andricus quercuslanigera (= A. linaria) en Quercus rugosa. Se recolectaron 1.096 agallas emergieron 367 especímenes: 108 A. quercuslanigera (Cynipini), 130 Synergus (Synergini), 6 Eupelmus (Eupelmidae), 10 Eurytoma (Eurytomidae), 96 Acaenacis (Pteromalidae), 13 Ormyrus (Ormyridae) y 4 Torymus (Torymidae). El género Acaenacis se cita por primera vez para la fauna mexicana

The VISTA Variables in the Vía Láctea eXtended (VVVX) ESO public survey: Completion of the observations and legacy

© 2024 ESO. This is the accepted manuscript version of an article which has been published in final form at https://doi.org/10.1051/0004-6361/202450584The ESO public survey VISTA Variables in the V\'ia L\'actea (VVV) surveyed the inner Galactic bulge and the adjacent southern Galactic disk from $2009-2015$. Upon its conclusion, the complementary VVV eXtended (VVVX) survey has expanded both the temporal as well as spatial coverage of the original VVV area, widening it from $562$ to $1700$ sq. deg., as well as providing additional epochs in $JHK_{\rm s}$ filters from $2016-2023$. With the completion of VVVX observations during the first semester of 2023, we present here the observing strategy, a description of data quality and access, and the legacy of VVVX. VVVX took $\sim 2000$ hours, covering about 4% of the sky in the bulge and southern disk. VVVX covered most of the gaps left between the VVV and the VISTA Hemisphere Survey (VHS) areas and extended the VVV time baseline in the obscured regions affected by high extinction and hence hidden from optical observations. VVVX provides a deep $JHK_{\rm s}$ catalogue of $\gtrsim 1.5\times10^9$ point sources, as well as a $K_{\rm s}$ band catalogue of $\sim 10^7$ variable sources. Within the existing VVV area, we produced a $5D$ map of the surveyed region by combining positions, distances, and proper motions of well-understood distance indicators such as red clump stars, RR Lyrae, and Cepheid variables. In March 2023 we successfully finished the VVVX survey observations that started in 2016, an accomplishment for ESO Paranal Observatory upon 4200 hours of observations for VVV+VVVX. The VVV+VVVX catalogues complement those from the Gaia mission at low Galactic latitudes and provide spectroscopic targets for the forthcoming ESO high-multiplex spectrographs MOONS and 4MOST.Peer reviewe

The Galaxy platform for accessible, reproducible, and collaborative data analyses: 2024 update

YesGalaxy (https://galaxyproject.org) is deployed globally, predominantly through free-to-use services, supporting user-driven research that broadens in scope each year. Users are attracted to public Galaxy services by platform stability, tool and reference dataset diversity, training, support and integration, which enables complex, reproducible, shareable data analysis. Applying the principles of user experience design (UXD), has driven improvements in accessibility, tool discoverability through Galaxy Labs/subdomains, and a redesigned Galaxy ToolShed. Galaxy tool capabilities are progressing in two strategic directions: integrating general purpose graphical processing units (GPGPU) access for cutting-edge methods, and licensed tool support. Engagement with global research consortia is being increased by developing more workflows in Galaxy and by resourcing the public Galaxy services to run them. The Galaxy Training Network (GTN) portfolio has grown in both size, and accessibility, through learning paths and direct integration with Galaxy tools that feature in training courses. Code development continues in line with the Galaxy Project roadmap, with improvements to job scheduling and the user interface. Environmental impact assessment is also helping engage users and developers, reminding them of their role in sustainability, by displaying estimated CO2 emissions generated by each Galaxy job.NIH [U41 HG006620, U24 HG010263, U24 CA231877, U01 CA253481]; US National Science Foundation [1661497, 1758800, 2216612]; computational resources are provided by the Advanced Cyberinfrastructure Coordination Ecosystem (ACCESS-CI), Texas Advanced Computing Center, and the JetStream2 scientific cloud. Funding for open access charge: NIH. ELIXIR IS and Travel grants; EU Horizon Europe [HORIZON-INFRA-2021-EOSC-01-04, 101057388]; EU Horizon Europe under the Biodiversity, Circular Economy and Environment program (REA.B.3, BGE 101059492); German Federal Ministry of Education and Research, BMBF [031 A538A de.NBI-RBC]; Ministry of Science, Research and the Arts Baden-Württemberg (MWK) within the framework of LIBIS/de.NBI Freiburg. Galaxy Australia is supported by the Australian BioCommons which is funded through Australian Government NCRIS investments from Bioplatforms Australia and the Australian Research Data Commons, as well as investment from the Queensland Government RICF program.Please note, contributors are listed in alphabetical order