182 research outputs found
Los alcances del Desarrollo Inclusivo en el pensamiento de Carlos Llano
Aún cuando es poco probable que Carlos Llano (1932-2010) haya conocido el concepto de “Desarrollo Inclusivo”, en el conjunto de su obra se encuentran varias aportaciones que encajan con el fondo de esta idea, y que representan enfoques enriquecedores para el contenido en uso de esta noción. Se recoge, en primer lugar, su concepción del desarrollo de la persona humana y la relación de éste con el crecimiento económico. Otra idea fecunda es la revisión del papel que tiene la colaboración, por encima de la competencia, en la productividad de las empresas. Finalmente se propone una ampliación de lo que se entiende por inclusión, de modo que ésta no se restrinja sólo a ser una cualidad del desarrollo, sino un factor constitutivo de éste.Although it is unlikely that Carlos Llano (1932-2010) knew the concept of “Inclusive Growth”, in the whole body of his work there are several contributions that fit the background of this idea, and represent an enriching approach to the content in use of this notion. Firstly, his conception of the development of the human person and the relation of this with the economic growth is collected. Another fruitful idea is the revision of the role of collaboration, above competition, in the productivity of companies. Finally, an expansion of what is meant by inclusion is proposed, so that it is not restricted only to being a quality of development, but a constitutive factor of it
El concepto de deliberación en el comentario de Santo Tomás de Aquino al libro VI de la ética a Nicómaco
Saber escoger lo mejor en cada momento se presenta como una tarea no siempre fácil. Más todavía en la actualidad donde las posibilidades de elección han aumentado desmesuradamente. Paradójicamente, este aumento,lejos de haber favorecido la satisfacción de nuestras necesidades, se ha convertido más bien en fuente de ansiedad y preocupación. El supuesto aumento de libertad que debería haber traído consigo el crecimiento de posibilidades de elección, no se ha traducido en el aumento proporcional de felicidad esperado1
Photometry and spectroscopy of faint candidate spectrophotometric standard DA white dwarfs
We present precise photometry and spectroscopy for 23 candidate
spectrophotometric standard white dwarfs. The selected stars are distributed in
the Northern hemisphere and around the celestial equators and are all fainter
than r ~ 16.5 mag. This network of stars, when established as standards,
together with the three Hubble Space Telescope primary CALSPEC white dwarfs,
will provide a set of spectrophotometric standards to directly calibrate data
products to better than 1%. These new faint standard white dwarfs will have
enough signal-to-noise ratio in future deep photometric surveys and facilities
to be measured accurately while still avoiding saturation in such surveys. They
will also fall within the dynamic range of large telescopes and their
instruments for the foreseeable future. This paper discusses the provenance of
the observational data for our candidate standard stars. The comparison with
models, reconciliation with reddening, and the consequent derivation of the
full spectral energy density distributions for each of them is reserved for a
subsequent paper.Comment: 31 pages, 17 figures, 10 tables, ApJ in press (accepted on December
23rd, 2018
Generalized Second Law and phantom Cosmology: accreting black holes
The accretion of phantom fields by black holes within a thermodynamic context
is addressed. For a fluid violating the dominant energy condition, case of a
phantom fluid, the Euler and Gibbs relations permit two different possibilities
for the entropy and temperature: a situation in which the entropy is negative
and the temperature is positive or vice-versa. In the former case, if the
generalized second law (GSL) is valid, then the accretion process is not
allowed whereas in the latter, there is a critical black hole mass below which
the accretion process occurs. In a universe dominated by a phantom field, the
critical mass drops quite rapidly with the cosmic expansion and black holes are
only slightly affected by accretion. All black holes disappear near the big
rip, as suggested by previous investigations, if the GSL is violated.Comment: 8 pp., no figure
How to Tell a Jet from a Balloon: A Proposed Test for Beaming in Gamma Ray Bursts
If gamma ray bursts are highly collimated, the energy requirements of each
event may be reduced by several (~ 4-6) orders of magnitude, and the event rate
increased correspondingly. Extreme conditions in gamma ray bursters lead to
highly relativistic motions (bulk Lorentz factors Gamma > 100). This results in
strong forward beaming of the emitted radiation in the observer's rest frame.
Thus, all information on gamma ray bursts comes from those ejecta emitted in a
narrow cone (opening angle 1/Gamma) pointing towards the observer. We are at
present ignorant of whether there are ejecta outside that cone or not.
The recent detection of longer wavelength transients following gamma ray
bursts allows an empirical test of whether gamma ray bursts are collimated jets
or spherical fireballs. The bulk Lorentz factor of the burst ejecta will
decrease with time after the event, as the ejecta sweep up the surrounding
medium. Thus, radiation from the ejecta is beamed into an ever increasing solid
angle as the burst remnant evolves. It follows that if gamma ray bursts are
highly collimated, many more optical and radio transients should be observed
without associated gamma rays than with them. Published supernova searches may
contain enough data to test the most extreme models of gamma ray beaming. We
close with a brief discussion of other possible consequences of beaming,
including its effect on the evolution of burst remnants.Comment: Original replaced with accepted refereed manuscript. 11 pages, uses
AASTeX 4.0 LaTeX macros. To be published in The Astrophysical Journal
Letters, vol. 487, p. L1 (20 September 1997
Late time cosmic acceleration from vacuum Brans-Dicke theory in 5D
We show that the scalar-vacuum Brans-Dicke equations in 5D are equivalent to
Brans-Dicke theory in 4D with a self interacting potential and an effective
matter field. The cosmological implication, in the context of FRW models, is
that the observed accelerated expansion of the universe comes naturally from
the condition that the scalar field is not a ghost, i.e., . We
find an effective matter-dominated 4D universe which shows accelerated
expansion if . We study the question of whether
accelerated expansion can be made compatible with large values of ,
within the framework of a 5D scalar-vacuum Brans-Dicke theory with variable,
instead of constant, parameter . In this framework, and based on a
general class of solutions of the field equations, we demonstrate that
accelerated expansion is incompatible with large values of .Comment: In V2 the summary section is expanded. To be published in Classical
and Quantum Gravity
A Calibration of NICMOS Camera 2 for Low Count-Rates
NICMOS 2 observations are crucial for constraining distances to most of the
existing sample of z > 1 SNe Ia. Unlike the conventional calibration programs,
these observations involve long exposure times and low count rates. Reciprocity
failure is known to exist in HgCdTe devices and a correction for this effect
has already been implemented for high and medium count-rates. However
observations at faint count-rates rely on extrapolations. Here instead, we
provide a new zeropoint calibration directly applicable to faint sources. This
is obtained via inter-calibration of NIC2 F110W/F160W with WFC3 in the low
count-rate regime using z ~ 1 elliptical galaxies as tertiary calibrators.
These objects have relatively simple near-IR SEDs, uniform colors, and their
extended nature gives superior signal-to-noise at the same count rate than
would stars. The use of extended objects also allows greater tolerances on PSF
profiles. We find ST magnitude zeropoints (after the installation of the NICMOS
cooling system, NCS) of 25.296 +- 0.022 for F110W and 25.803 +- 0.023 for
F160W, both in agreement with the calibration extrapolated from count-rates
1,000 times larger (25.262 and 25.799). Before the installation of the NCS, we
find 24.843 +- 0.025 for F110W and 25.498 +- 0.021 for F160W, also in agreement
with the high-count-rate calibration (24.815 and 25.470). We also check the
standard bandpasses of WFC3 and NICMOS 2 using a range of stars and galaxies at
different colors and find mild tension for WFC3, limiting the accuracy of the
zeropoints. To avoid human bias, our cross-calibration was "blinded" in that
the fitted zeropoint differences were hidden until the analysis was finalized.Comment: Accepted for Publication in the Astronomical Journal. New version
contains added referenc
K Corrections For Type Ia Supernovae and a Test for Spatial Variation of the Hubble Constant
Cross-filter K corrections for a sample of "normal" Type Ia supernovae (SNe)
have been calculated for a range of epochs. With appropriate filter choices,
the combined statistical and systematic K correction dispersion of the full
sample lies within 0.05 mag for redshifts z<0.7. This narrow dispersion of the
calculated K correction allows the Type Ia to be used as a cosmological probe.
We use the K corrections with observations of seven SNe at redshifts 0.3 < z
<0.5 to bound the possible difference between the locally measured Hubble
constant (H_L) and the true cosmological Hubble constant (H_0).Comment: 6 pages, 3 Postscript figures, uuencoded uses crckapb.sty and
psfig.sty. To appear in Thermonuclear Supernovae (NATO ASI), eds. R. Canal,
P. Ruiz-LaPuente, and J. Isern. Postscript version is also available at
http://www-supernova.lbl.gov
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