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The existence of a period-luminosity relation for RR Lyrae variables as
measured at IRAC mid-infrared wavelengths allows Spitzer to estimate
distances to individual stars with 2% errors. The SMASH program will
exploit this unprecedented opportunity to precisely map structures
throughout the halo of our Galaxy. SMASH will construct the first 3-D
map of one of the larger satellites of the Milky Way
... [Show full abstract] (Sagittarius), it
will determine precise distances to four more satellites (Ursa Minor,
Carina, Sculptor & Bootes) and make the only measurements of stars
in tidal streams accurate enough to determine their individual positions
within the debris. This proposal describes some of the ground-breaking
science enabled by this program, from increased accuracy in determining
the orbits of satellite galaxies, to revolutionary constraints on the
mass, shape and orientation of our Milky Way's dark matter halo. The
foundational importance of these data sets cannot be overstated. These
Milky Way structures lie far beyond the reach of any current or proposed
future direct parallax measurements. Moreover, the combination of the
SMASH results with proper motions from ESA's upcoming astrometric
mission, Gaia, can effectively stretch Gaia's horizon for full 6D
phase-space maps of our Galaxy by nearly four orders of magnitude in
volume! These data and the resulting distance measurements will become
Spitzer's legacy to the Galactic Astronomy community for years to come. Read more January 2014 · EAS Publications Series Read more July 2016
Athena is one of L-class missions selected in the ESA Cosmic Vision 2015-2025 program for the science theme of the Hot and Energetic Universe. The Athena model payload includes the X-ray Integral Field Unit (X-IFU), an advanced actively shielded X-ray microcalorimeter spectrometer for high spectral resolution imaging, utilizing cooled Transition Edge Sensors. This paper describes the preliminary
... [Show full abstract] architecture of Instrument Control Unit (ICU), which is aimed at operating all XIFU’s subsystems, as well as at implementing the main functional interfaces of the instrument with the S/C control unit. The ICU functions include the TC/TM management with S/C, science data formatting and transmission to S/C Mass Memory, housekeeping data handling, time distribution for synchronous operations and the management of the X-IFU components (i.e. CryoCoolers, Filter Wheel, Detector Readout Electronics Event Processor, Power Distribution Unit). ICU functions baseline implementation for the phase-A study foresees the usage of standard and Space-qualified components from the heritage of past and current space missions (e.g. Gaia, Euclid), which currently encompasses Leon2/Leon3 based CPU board and standard Space-qualified interfaces for the exchange commands and data between ICU and X-IFU subsystems. Alternative architecture, arranged around a powerful PowerPC-based CPU, is also briefly presented, with the aim of endowing the system with enhanced hardware resources and processing power capability, for the handling of control and science data processing tasks not defined yet at this stage of the mission study. Read more January 2011
Gaia will provide unprecedented information on the distribution,
dynamics and binarity of stars within 1-2 kpc of the Sun. I discuss how
this information could be used to test theories of star formation.
Read more Article Full-text available October 2012 · GAIA - Ecological Perspectives on Science and Society
Reaktion auf I. Seidl und A. Zahrnt. 2012. Abhängigkeit vom Wirtschaftswachstum als Hindernis für eine Politik innerhalb der limits to growth. GAIA 21/2: 108 – 115
View full-text April 2017 · Proceedings of the International Astronomical Union
We derive and compare kinematic parameters of the Galaxy using the PMA and Gaia TGAS data. Two methods are used in calculations: evaluation of the Ogorodnikov-Milne model (OMM) parameters by the least square method (LSM) and a decomposition on a set of vector spherical harmonics (VSH). We trace dependencies on the distance of the derived parameters including the Oort constants A and B and the
... [Show full abstract] rotational velocity of the Galaxy Vrot at the Solar distance for the common sample of stars of mixed spectral composition of the PMA and TGAS catalogues. The distances were obtained from the TGAS parallaxes or from reduced proper motions for fainter stars.
The A, B and Vrot parameters derived from proper motions of both catalogues used show identical behaviour but the values are systematically shifted by about 0.5 mas/yr.
The Oort B parameter derived from the PMA sample of red giants shows gradual decrease with increasing the distance while the Oort A has a minimum at about 2 kpc and then gradually increases.
As for models chosen for calculations, first, we confirm conclusions of other authors about the existence of extra-model harmonics in the stellar velocity field. Secondly, not all parameters of the OMM are statistically significant, and the set of parameters depends on the stellar sample used. Read more Article Full-text available June 2011 · Astronomy and Astrophysics
Surface brightness asymmetries are a very common feature of stars. Among
other effects they cause a difference between the projected barycentre and
photocentre. The evolution of those surface features makes this difference
time-dependent. In some cases, e. g. for supergiant stars, the displacement can
be a non-negligible fraction of the star radius R, and if R>1 AU, of the
... [Show full abstract] investigate the impact of surface brightness asymmetries on both
the Gaia astrometric solution and the data processing flow with a theoretical
approach. We show that when the amplitude of the displacement is comparable to
the epoch astrometric precision, the resulting astrometric solution of a
genuine single star may be, in some cases, of low quality (with some parameters
up to 10 sigma off). In this case, we provide an analytical prediction of the
impact of the photocentre motion on both chi squared and the uncertainty in the
astrometric parameters. Non-single star solutions are found, if allowed for the
closest stars. A closer look at the parameters of the orbital solutions reveals
however that they are spurious (since the semi-major axis is smaller than
either its error or the stellar radius). It is thus possible to filter out
those spurious orbital solutions. Interestingly, for the stocastic solutions,
the stochastic noise appears to be a good estimate of the photocentric noise. View full-text September 2000 · Autonomous Agents and Multi-Agent Systems
This article presents Gaia: a methodology for agent-oriented analysis and design. The Gaia methodology is both general, in that it is applicable to a wide range of multi-agent systems, and comprehensive, in that it deals with both the macro-level (societal) and the micro-level (agent) aspects of systems. Gaia is founded on the view of a multi-agent system as a computational organisation
... [Show full abstract] consisting of various interacting roles. We illustrate Gaia through a case study (an agent-based business process management system). Read more December 2011
The determination of stellar ages is fundamental to understand the
formation and evolution of the Galaxy. We determine the age of stars by
combining their position in the HR diagram with stellar evolutionary
tracks or isochrones. The goal of this study is to prepare the tools
that will be used to age-date stars after the Gaia mission.
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