18,345 research outputs found
60 Years of Rural Reconstruction Movement in the Philippines (PRRM) = 回顧菲律賓鄉村建設運動60年
PRRM did not go to the countryside to disperse buffalos though that’s not necessarily a bad thing. PRRM did disperse buffalos and other farm animals but it went to the countryside for nobler reason---the liberation of the peasant from poverty and oppression. It sought to do this through mass education and mass movement.
By 2012 PRRM will have spanned a period running in parallel to the postwar development history of the Philippines. It was founded in 1952 during the administration of President Magsaysay, called “Man of the Masses”. PRRM peaked in the 1960s, declined in the late 1970s through to the 1980s, and rebounded after the 1986 EDSA revolution
On the distribution of proportions and ratios as indicators of ungulate body condition
In the wildlife literature various studies have shown that the amount of fat around the kidneys is
often a good indicator of body condition and health of ungulate species ([1],[2]). Wildlife biologies often
measure the weights of fat around the kidneys and the kidneys themselves (without fat), comparing
these two quantities and transforming them into a ratio or a proportion as surrogates of body condition
of dead animals. Later, they use these indices as response variables to model the e®ect of covariates
or treatments, such as age group and season of the year, on body condition. The more commonly
used models are ANOVA-type. Most debate has been concentrated on whether or not to use a simple
ANOVA model of ratios or proportions with ¯xed e®ects, or an ANCOVA model using fat weight as
response variable, and the kidneys weight as a covariate ([3]). Results have taken by surprise some
biologists because using one or another model with both response variables could lead to very di®erent
results for what it considered the most important e®ects. In this manuscript we attempt to highlight
the main di®erences and the distributional properties of these response variables, ratio and proportion
Neural-network selection of high-redshift radio quasars, and the luminosity function at z~4
We obtain a sample of 87 radio-loud QSOs in the redshift range 3.6<z<4.4 by
cross-correlating sources in the FIRST radio survey S{1.4GHz} > 1 mJy with
star-like objects having r <20.2 in SDSS Data Release 7. Of these 87 QSOs, 80
are spectroscopically classified in previous work (mainly SDSS), and form the
training set for a search for additional such sources. We apply our selection
to 2,916 FIRST-DR7 pairs and find 15 likely candidates. Seven of these are
confirmed as high-redshift quasars, bringing the total to 87. The candidates
were selected using a neural-network, which yields 97% completeness (fraction
of actual high-z QSOs selected as such) and an efficiency (fraction of
candidates which are high-z QSOs) in the range of 47 to 60%. We use this sample
to estimate the binned optical luminosity function of radio-loud QSOs at , and also the LF of the total QSO population and its comoving density. Our
results suggest that the radio-loud fraction (RLF) at high z is similar to that
at low-z and that other authors may be underestimating the fraction at high-z.
Finally, we determine the slope of the optical luminosity function and obtain
results consistent with previous studies of radio-loud QSOs and of the whole
population of QSOs. The evolution of the luminosity function with redshift was
for many years interpreted as a flattening of the bright end slope, but has
recently been re-interpreted as strong evolution of the break luminosity for
high-z QSOs, and our results, for the radio-loud population, are consistent
with this.Comment: 20 pages. Accepted for publication in MNRAS on 3 March 201
Use of neural networks for the identification of new z>=3.6 QSOs from FIRST-SDSS DR5
We aim to obtain a complete sample of redshift > 3.6 radio QSOs from FIRST
sources having star-like counterparts in the SDSS DR5 photometric survey
(r<=20.2). We found that simple supervised neural networks, trained on sources
with SDSS spectra, and using optical photometry and radio data, are very
effective for identifying high-z QSOs without spectra. The technique yields a
completeness of 96 per cent and an efficiency of 62 per cent. Applying the
trained networks to 4415 sources without DR5 spectra we found 58 z>=3.6 QSO
candidates. We obtained spectra of 27 of them, and 17 are confirmed as high-z
QSOs. Spectra of 13 additional candidates from the literature and from SDSS DR6
revealed 7 more z>=3.6 QSOs, giving and overall efficiency of 60 per cent. None
of the non-candidates with spectra from NED or DR6 is a z>=3.6 QSO,
consistently with a high completeness. The initial sample of z>=3.6 QSOs is
increased from 52 to 76, i.e. by a factor 1.46. From the new identifications
and candidates we estimate an incompleteness of SDSS for the spectroscopic
classification of FIRST 3.6<=z<=4.6 QSOs of 15 percent for r<=20.2.Comment: 16 pages, 9 figures accepted for publication in MNRA
SPH simulations of the chemical evolution of bulges
We have implemented a chemical evolution model on the parallel AP3M+SPH DEVA
code which we use to perform high resolution simulations of spiral galaxy
formation. It includes feedback by SNII and SNIa using the Qij matrix
formalism. We also include a diffusion mechanism that spreads newly introduced
metals. The gas cooling rate depends on its specific composition. We study the
stellar populations of the resulting bulges finding a potential scenario where
they seem to be composed of two populations: an old, metal poor,
-enriched population, formed in a multiclump scenario at the beginning
of the simulation and a younger one, formed by slow accretion of satellites or
gas, possibly from the disk due to instabilities.Comment: 2 pages, 3 figures. Proceedings of IAUS 245 "Formation and Evolution
of Galaxy Bulges
The role of magnetoplasmons in Casimir force calculations
In this paper we review the role of magneto plasmon polaritons in the Casimir
force calculations. By applying an external constant magnetic field a strong
optical anisotropy is induced on two parallel slabs reducing the reflectivity
and thus the Casimir force. As the external magnetic field increases, the
Casimir force decreases. Thus, with an an external magnetic field the Casimir
force can be controlled.The calculations are done in the Voigt configuration
where the magnetic field is parallel to the slabs. In this configuration the
reflection coefficients for TE and TM modes do not show mode conversion.Comment: contribution to QFEXT09, Norman, Oklahoma 200
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