7,831 research outputs found
Corruption Prevention in State Colleges and Universities
Corruption is everywhere and even government-run institutions of higher learning are not spared from such dilemma. Corruption inside State Universities and Colleges might be thought to be the small time or less impact problem in governance compared to other government entities amassing hard-earned people’s taxes, butthe fact that schools are the second home of knowledge and values of an individual, therefore, graft and corruption values (inherited, observed or adapted) must first be cut within its grooming point. The study shall focus on how some government-run institutions of higher learning addressed the long standing deep rooted ill of society – corruption in their doorsteps. A review of policies and current practices in their fight of corruption of at least three to four government-run institutions of higher learning shall be showcased in this study. The results of the study shall be awareness and formalization of this infant field in Philippine Governance System and Public Administration encompassing different tools like internal auditing, systems studies, monitoring of government resources utilization, corruption prevention promotion and education drive, integrity systems check, corruption vulnerability assessments, red tape assessment, and the like. A conclusion formulated that corruption prevention should be embraced in all government entities especially in State Universities and Colleges, shifting from the old thought that we react after perpetrators of graft and corruption had amassed national wealth — preventing them doing such, by formulating ways to put in place integrity systems and promoting the culture of good governance for all time.
Keywords: Anti-Corruption, Corruption Prevention, Integrity System, Good Governance, Public Administratio
XMM-Newton and Chandra observations of G272.2-3.2. Evidence of stellar ejecta in the central region
We aim to study the spatial distribution of the physical and chemical
properties of the X-ray emitting plasma of the supernova remnant G272.2-3.2, in
order to get important constraints on its ionization stage, on the progenitor
supernova explosion, and the age of the remnant. We report combined XMM-Newton
and Chandra images, median photon energy map, silicon and sulfur equivalent
width maps, and a spatially resolved spectral analysis for a set of regions of
the remnant. Complementary radio and H{\alpha} observations, available in the
literature, are also used to study the multi-wavelength connection of all
detected emissions. The X-ray morphology of the remnant displays an overall
structure with an almost circular appearance, a centrally brightened hard
region, with a peculiar elongated hard structure oriented along the
northwest-southeast direction of the central part. The X-ray spectral study of
the regions shows distinct K{\alpha} emission-line features of metal elements,
confirming the thermal origin of the emission. The X-ray spectra are well
represented by an absorbed VNEI thermal plasma model, which produces elevated
abundances of Si, S, and Fe in the circular central region, typical of ejecta
material. The values of abundances found in the central region of the SNR favor
a Type Ia progenitor for this remnant. The outer region shows abundances below
the solar value, as expected if the emission arises from the shocked ISM. The
relatively low ionization timescales suggests non-equilibrium ionization. We
identify the location of the contact discontinuity. Its distance to the outer
shock is higher than expected for expansion in a uniform media, what suggests
that the remnant spent most of its time in a more dense medium.Comment: 9 pages, 7 figures. Accepted for publication in A&
AE Aurigae: first detection of non-thermal X-ray emission from a bow shock produced by a runaway star
Runaway stars produce shocks when passing through interstellar medium at
supersonic velocities. Bow shocks have been detected in the mid-infrared for
several high-mass runaway stars and in radio waves for one star. Theoretical
models predict the production of high-energy photons by non-thermal radiative
processes in a number sufficiently large to be detected in X-rays. To date, no
stellar bow shock has been detected at such energies. We present the first
detection of X-ray emission from a bow shock produced by a runaway star. The
star is AE Aur, which was likely expelled from its birthplace by the encounter
of two massive binary systems and now is passing through the dense nebula IC
405. The X-ray emission from the bow shock is detected at 30" to the northeast
of the star, coinciding with an enhancement in the density of the nebula. From
the analysis of the observed X-ray spectrum of the source and our theoretical
emission model, we confirm that the X-ray emission is produced mainly by
inverse Compton upscattering of infrared photons from dust in the shock front.Comment: Accepted for publication in the Astrophysical Journal with number
ApJ, 757, L6. Four figure
On the origin of the jet-like radio/X-ray morphology of G290.1-0.8
The origin and evolution of supernova remnants of the mixed-morphology class
is not well understood. Several remnants present distorted radio or X-ray
shells with jet-like structures. G290.1-0.8 (MSH 11-61A) belongs to this class.
We aim to investigate the nature of this supernova remnant in order to unveil
the origin of its particular morphology. We based our work on the study of the
X-ray emitting plasma properties and the conditions imposed by the cold
interstellar medium where the remnant expanded. We use archival radio, HI line
data and X-ray observations from XMM-Newton and Chandra observatories, to study
G290.1-0.8 and its surrounding medium. Spatially resolved spectral analysis and
mean photon energy maps are used to obtain physical and geometrical parameters
of the source. Radio continuum and HI line maps give crucial information to
understand the radio/X-ray morphology. The X-ray images show that the remnant
presents two opposite symmetric bright spots on a symmetry axis running towards
the NW-SE direction. Spectral analysis and mean photon energy maps confirm that
the physical conditions of the emitting plasma are not homogeneous throughout
the remnant. In fact, both bright spots have higher temperatures than the rest
of the plasma and its constituents have not reached ionization equilibrium yet.
HI line data reveal low density tube-like structures aligned along the same
direction. This evidence supports the idea that the particular X-ray morphology
observed is a direct consequence of the structure of the interstellar medium
where the remnant evolved. However, the possibility that an undetected
point-like object, as a neutron star, exists within the remnant and contributes
to the X-ray emission cannot be discarded. Finally, we suggest that a supernova
explosion due to the collapse of a high-mass star with a strong bipolar wind
can explain the supernova remnant morphology.Comment: 8 pages, 6 figures. Accepted for publication in A&
Seasonal fluctuations of cosmopolitan inversion frequencies in a natural population of Drosophila melanogaster
International audienc
Evidence of non-thermal X-ray emission from HH 80
Protostellar jets appear at all stages of star formation when the accretion
process is still at work. Jets travel at velocities of hundreds of km/s,
creating strong shocks when interacting with interstellar medium. Several cases
of jets have been detected in X-rays, typically showing soft emission. For the
first time, we report evidence of hard X-ray emission possibly related to
non-thermal processes not explained by previous models of the post-shock
emission predicted in the jet/ambient interaction scenario. HH 80 is located at
the south head of the jet associated to the massive protostar IRAS 18162-2048.
It shows soft and hard X-ray emission in regions that are spatially separated,
with the soft X-ray emission region situated behind the region of hard X-ray
emission. We propose a scenario for HH 80 where soft X-ray emission is
associated to thermal processes from the interaction of the jet with denser
ambient matter and the hard X-ray emission is produced by synchrotron radiation
at the front shock.Comment: Accepted for publication in ApJ
High-pressure, low-abundance water in bipolar outflows. Results from a Herschel-WISH survey
(Abridged) We present a survey of the water emission in a sample of more than
20 outflows from low mass young stellar objects with the goal of characterizing
the physical and chemical conditions of the emitting gas. We have used the HIFI
and PACS instruments on board the Herschel Space Observatory to observe the two
fundamental lines of ortho-water at 557 and 1670 GHz. These observations were
part of the "Water In Star-forming regions with Herschel" (WISH) key program,
and have been complemented with CO and H2 data. We find that the emission from
water has a different spatial and velocity distribution from that of the J=1-0
and 2-1 transitions of CO, but it has a similar spatial distribution to H2, and
its intensity follows the H2 intensity derived from IRAC images. This suggests
that water traces the outflow gas at hundreds of kelvins responsible for the H2
emission, and not the component at tens of kelvins typical of low-J CO
emission. A warm origin of the water emission is confirmed by a remarkable
correlation between the intensities of the 557 and 1670 GHz lines, which also
indicates the emitting gas has a narrow range of excitations. A non-LTE
radiative transfer analysis shows that while there is some ambiguity on the
exact combination of density and temperature values, the gas thermal pressure
nT is constrained within less than a factor of 2. The typical nT over the
sample is 4 10^{9} cm^{-3}K, which represents an increase of 10^4 with respect
to the ambient value. The data also constrain within a factor of 2 the water
column density. When this quantity is combined with H2 column densities, the
typical water abundance is only 3 10^{-7}, with an uncertainty of a factor of
3. Our data challenge current C-shock models of water production due to a
combination of wing-line profiles, high gas compressions, and low abundances.Comment: 21 pages, 13 figures. Accepted for publication in A&
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