Diagnostics of Quasar Broad Absorption Line Geometry: X-Ray Observations and Two-dimensional Optical Spectroscopy

A new generation of sensitive X-ray measurements are indicating that the existence of X-ray attenuation column densities, NH > 1024 cm-2, is quite common among broad absorption line quasars (BALQSOs). This is significant to the geometry of the broad absorption line (BAL) outflow. In particular, such an X-ray shield also shields equatorial accretion disk winds from the UV, thereby preventing high-velocity equatorial outflows from being launched. By contrast, bipolar winds initiated by continuum radiation pressure from the funnel of a slim accretion disk flare outward (like a trumpet) and offer vastly different absorbing columns to the X-ray and UV emission that are emitted from distinct regions of the disk, ~6M and ~10M-40M, respectively (where M is the radius of the black hole). Recent numerical work indicates that it is also possible to launch bipolar outflows from the inner regions of a thin disk. The recent discovery with VLBI that the Galactic analog of a BALQSO, the X-ray binary Circinus X-1 (with high-velocity P Cygni X-ray absorption lines), is viewed virtually along the radio jet axis (and therefore along the spin axis of the black hole and the normal to the accretion disk) has rekindled interest in the bipolar models of BALQSOs. We explore this possibility by studying the nearest BALQSO, Mrk 231. High-resolution two-dimensional optical spectroscopy and VLBI mappings of the radio jet axis indicate that the BAL outflow is parallel to the parsec-scale radio jet

Separating C-stars from Dust in the Central Region of the Seyfert 2 Galaxy NGC 1241

The Sy 2 galaxy NGC 1241 presents a 1.5 kpc large circumnuclear ring of star formation (CNR) embracing a small bar plus leading arms. Those structures are P alpha emitters, but barely seen in H alpha. It presents also stellar trailing arms inside the CNR. GEMINI and HST imagery allow the construction of high resolution (V-H) and (J-K_s) color maps as well as a (J-K_s) vs. K color-magnitude diagram (CMD) of this complex region. The CNR is heavily obscured in V, but a fairly transparent window appears in the direction of the nucleus. Nonetheless, the nucleus presents a (J-K_s) color that is redder than the CNR. The CNR is composed of extremely young HII regions still enshrouded in their dust cocoons. However, the nuclear (J-K_s) color can not be explained in this manner. Therefore, we propose the contribution of C-Stars as the most feasible mechanism for explaining the colors. If the nuclear stellar population is comparable to that of the LMC bar, 500 C-stars and 25000 AGB O-rich stars inside 50 pc may reproduce the observed colors. C-Stars release enriched material to the nuclear environment, probably fueling the central engine of this Sy 2 galaxy during the lifetime of stars with masses between 2 M_sun < M_C-star < 6 M_sun (C-star phase). The ejected material that remains trapped in the central potential might also explain the systematically observed increased strength of the optical CN-bands in Sy 2 galaxies and is consistent with the significant contribution of intermediate age stars to the optical continuum of low luminosity AGNs.Comment: The Astrophysical Journal Letters, accepted. 5 figure

From FMTV to WATERS: Lessons Learned from the First Verification Challenge at ECRTS (Artifact)

We propose here solutions to the FMTV 2015 challenge of a distributed video processing system using four different formalisms, as well as the description of the challenge itself. This artifact contains several solutions to various subchallenges, and instructions and scripts to reproduce these results smoothly

From FMTV to WATERS: Lessons Learned from the First Verification Challenge at ECRTS

We present here the main features and lessons learned from the first edition of what has now become the ECRTS industrial challenge, together with the final description of the challenge and a comparative overview of the proposed solutions. This verification challenge, proposed by Thales, was first discussed in 2014 as part of a dedicated workshop (FMTV, a satellite event of the FM 2014 conference), and solutions were discussed for the first time at the WATERS 2015 workshop. The use case for the verification challenge is an aerial video tracking system. A specificity of this system lies in the fact that periods are constant but known with a limited precision only. The first part of the challenge focuses on the video frame processing system. It consists in computing maximum values of the end-to-end latency of the frames sent by the camera to the display, for two different buffer sizes, and then the minimum duration between two consecutive frame losses. The second challenge is about computing end-to-end latencies on the tracking and camera control for two different values of jitter. Solutions based on five different tools - Fiacre/Tina, CPAL (simulation and analysis), IMITATOR, UPPAAL and MAST - were submitted for discussion at WATERS 2015. While none of these solutions provided a full answer to the challenge, a combination of several of them did allow to draw some conclusions

Evolución de Galaxias y QSOs. Modelo evolutivo-explosivo-compuesto: fase final de galaxias y origen explosivo de galaxias enanas

En este trabajo presentamos nuevos resultados de nuestro modelo evolutivo-explosivo-compuesto de Galaxias, Cuásares y AGNs. En particular: explicamos el concepto de fase final de una galaxia y el hecho de que al menos una fracción de las galaxias enanas pueden ser explicadas con este modelo. También sugerimos que el prototipo de galaxia starburst M82 puede ser una galaxia enana en la fase previa a la final. Además comentamos nuevas observaciones Gemini de BAL+FeII+IR QSOs a medio-alto redshift. Para poder interpretar estos resultados en un contexto más amplio hemos realizado una introducción a nuestro modelo y algunos de los resultados previos más relevantes, entre ellos: (i) Diagrama de Evolución de Galaxias, QSOs, y AGNs; (ii) NuestroModelo Evolutivo-Explosivo-Compuesto explica en un mismo proceso: la interacción de ?Starburst? y los Agujeros Negros supermasivos que generan HiperNovas, el Origen de los Rayos Cósmicos Ultra-Energéticos y la Materia Oscura. (iii) Observación y Teoría de la Formación y de la fase final de Galaxias, via Explosión de HiperNovas en QSOs y AGNs.We present new results of our evolutionary-explosive- composite model of Galaxies, Quasars and AGNs. In particular: we explain the concept of final phase of a galaxy and the fact that at least a fraction of dwarf galaxies can be explained by this model (as a stage prior to the final). In addition, we explain that the prototype of the starburst galaxy M82 could be a dwarf galaxy previous to the final phase. Also, we discuss new Gemini observations BAL + FeII + IR medium-high redshift QSOs. To interpret these results we performed an introduction to our model and some of the most previous relevant results, including: (i) Evolution Diagram of Galaxies, QSOs and AGNs; (ii) Our Evolutionary-Explosive-Compound Model explains in the same process: the interaction of “Starburst” and Supermassive black holes that generate hypernova, the Origin of Ultra Energetic Cosmic Rays and Dark Matter. (iii) Observation and Theory of Formation and Final Phase of Galaxies via hypernova explosions in QSOs and AGNs.Fil: Lipari, Sebastian Luis. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; ArgentinaFil: Terlevich, R.J.. University of Cambridge; Reino UnidoFil: Taniguchi, Y.. Eihme University; JapónFil: Mediavilla, E.. Instituto de Astrofísica de Canarias; EspañaFil: Bergmann, M.. Gemini Observatory; ChileFil: García Lorenzo, B.. Instituto de Astrofísica de Canarias; EspañaFil: Sánchez, S.F.. Instituto Nacional de Astrofísica, Óptica y Electrónica; MéxicoFil: Zheng, W.. John Hopkins University; Estados UnidosFil: Punsly, B.. International Center for Relativistic Astrophysics Network; ItaliaFil: Merlo, David Constantino. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba; Argentin

From FMTV to WATERS: Lessons Learned from the First Verification Challenge at ECRTS

We present here the main features and lessons learned from the first edition of what has now become the ECRTS industrial challenge, together with the final description of the challenge and a comparative overview of the proposed solutions. This verification challenge, proposed by Thales, was first discussed in 2014 as part of a dedicated workshop (FMTV, a satellite event of the FM 2014 conference), and solutions were discussed for the first time at the WATERS 2015 workshop. The use case for the verification challenge is an aerial video tracking system. A specificity of this system lies in the fact that periods are constant but known with a limited precision only. The first part of the challenge focuses on the video frame processing system. It consists in computing maximum values of the end-to-end latency of the frames sent by the camera to the display, for two different buffer sizes, and then the minimum duration between two consecutive frame losses. The second challenge is about computing end-to-end latencies on the tracking and camera control for two different values of jitter. Solutions based on five different tools - Fiacre/Tina, CPAL (simulation and analysis), IMITATOR, UPPAAL and MAST - were submitted for discussion at WATERS 2015. While none of these solutions provided a full answer to the challenge, a combination of several of them did allow to draw some conclusions

Observation of Fine Time Structures in the Cosmic Proton and Helium Fluxes with the Alpha Magnetic Spectrometer on the International Space Station

International audienceWe present the precision measurement from May 2011 to May 2017 (79 Bartels rotations) of the proton fluxes at rigidities from 1 to 60 GV and the helium fluxes from 1.9 to 60 GV based on a total of $1 \times 10^9$ events collected with the Alpha Magnetic Spectrometer aboard the International Space Station. This measurement is in solar cycle 24, which has the solar maximum in April 2014. We observed that, below 40 GV, the proton flux and the helium flux show nearly identical fine structures in both time and relative amplitude. The amplitudes of the flux structures decrease with increasing rigidity and vanish above 40 GV. The amplitudes of the structures are reduced during the time period, which started one year after solar maximum, when the proton and helium fluxes steadily increase. Above $\sim 3$  GV the p/He flux ratio is time independent. We observed that below $\sim 3$  GV the ratio has a long-term decrease coinciding with the period during which the fluxes start to rise

Optical and IR emission of a sample of IRAS galaxies

We report on observations of 12 southem warm IRAS galaxies. Using absolute fluxes of lines in the optical region in connection with diagnostic diagrams, we have classified these galaxies in terms of the principal excitation mechanisms and have found that ali the galaxies are Seyferts. Far-infrared colours also are used to analyse these objects. Good correlations between the luminosity at 25 and 60 μm and the Hα luminosity are found. The far-infrared luminosity of Seyfert galaxies seems to depend more strongly on the number of ionizing photons than on the amount of dust

Cache related pre-emption delays in hierarchical scheduling

International audienceHierarchical scheduling provides a means of composing multiple real-time applications onto a single processor such that the temporal requirements of each application are met. This has become a popular technique in industry as it allows applications from multiple vendors as well as legacy applications to co-exist in isolation on the same platform. However, performance enhancing features such as caches mean that one application can interfere with another by evicting blocks from cache that were in use by another application, violating the requirement of temporal isolation. In this paper, we present analysis that bounds the additional delay due to blocks being evicted from cache by other applications in a system using hierarchical scheduling when using either a local FP or EDF scheduler