2,570 research outputs found
Carbon and oxygen abundances from recombination lines in low-metallicity star-forming galaxies. Implications for chemical evolution
We present deep echelle spectrophotometry of the brightest emission-line
knots of the star-forming galaxies He 2-10, Mkn 1271, NGC 3125, NGC 5408, POX
4, SDSS J1253-0312, Tol 1457-262, Tol 1924-416 and the HII region Hubble V in
the Local Group dwarf irregular galaxy NGC 6822. The data have been taken with
the Very Large Telescope Ultraviolet-Visual Echelle Spectrograph in the
3100-10420 {\AA} range. We determine electron densities and temperatures of the
ionized gas from several emission-line intensity ratios for all the objects. We
derive the ionic abundances of C and/or O from faint pure
recombination lines (RLs) in several of the objects, permitting to derive their
C/H and C/O ratios. We have explored the chemical evolution at low
metallicities analysing the C/O vs. O/H, C/O vs. N/O and C/N vs. O/H relations
for Galactic and extragalactic HII regions and comparing with results for halo
stars and DLAs. We find that HII regions in star-forming dwarf galaxies occupy
a different locus in the C/O vs. O/H diagram than those belonging to the inner
discs of spiral galaxies, indicating their different chemical evolution
histories, and that the bulk of C in the most metal-poor extragalactic HII
regions should have the same origin than in halo stars. The comparison between
the C/O ratios in HII regions and in stars of the Galactic thick and thin discs
seems to give arguments to support the merging scenario for the origin of the
Galactic thick disc. Finally, we find an apparent coupling between C and N
enrichment at the usual metallicities determined for HII regions and that this
coupling breaks in very low-metallicity objects.Comment: 27 pages, 12 figures, Accepted for publication in Monthly Notices of
the Royal Astronomical Societ
Development and evaluation of a multiplex test for the detection of atypical bacterial DNA in community-acquired pneumonia during childhood
AbstractAn incorrect or late diagnosis can lead to an increase in the morbidity and mortality caused by pneumonia, and the availability of a rapid and accurate microbiological test to verify the aetiology is imperative. This study evaluated a molecular test for the identification of the bacterial cause of atypical community-acquired pneumonia (ACAP). Fifty-four children with pneumonia were studied using bacteriological cultures, Mycoplasma pneumoniae, Coxiella burnetii, Chlamydophila pneumoniae and Legionella spp. serology, and Streptococcus pneumoniae and Legionella antigens. Simultaneously, the presence of bacterial and fungal DNA was tested for in respiratory secretion samples using the Vircell SL kit, including multiplex PCR and amplicon detection by means of line blots. There were 14 cases of ACAP caused by M. pneumoniae, with positive kit results for 13 of them, and two cases of Q-fever, with negative kit results for Coxiella burnetii. The test was negative in the remaining 38 cases (one staphylococcal pneumonia, 20 Streptococcus pneumoniae pneumonias, and 17 probable viral pneumonias). The sensitivity of the test for the detection of M. pneumoniae was 92.8% and the specificity was 100%. The Vircell SL kit allows detection of M. pneumoniae DNA in respiratory secretion samples from children with ACAP
Carbon and oxygen in HII regions of the Magellanic Clouds: abundance discrepancy and chemical evolution
We present C and O abundances in the Magellanic Clouds derived from deep
spectra of HII regions. The data have been taken with the Ultraviolet-Visual
Echelle Spectrograph at the 8.2-m VLT. The sample comprises 5 HII regions in
the Large Magellanic Cloud (LMC) and 4 in the Small Magellanic Cloud (SMC). We
measure pure recombination lines (RLs) of CII and OII in all the objects,
permitting to derive the abundance discrepancy factors (ADFs) for O^2+, as well
as their O/H, C/H and C/O ratios. We compare the ADFs with those of other HII
regions in different galaxies. The results suggest a possible metallicity
dependence of the ADF for the low-metallicity objects, but more uncertain for
high-metallicity objects. We compare nebular and B-type stellar abundances and
we find that the stellar abundances agree better with the nebular ones derived
from collisionally excited lines (CELs). Comparing these results with other
galaxies we observe that stellar abundances seem to agree better with the
nebular ones derived from CELs in low-metallicity environments and from RLs in
high-metallicity environments. The C/H, O/H and C/O ratios show almost flat
radial gradients, in contrast with the spiral galaxies where such gradients are
negative. We explore the chemical evolution analysing C/O vs. O/H and comparing
with the results of HII regions in other galaxies. The LMC seems to show a
similar chemical evolution to the external zones of small spiral galaxies and
the SMC behaves as a typical star-forming dwarf galaxy.Comment: Accepted for publication in MNRAS, 17 pages, 11 figures, 8 table
Computational thinking and robotics in education
After the computational thinking sessions in the previous 2016-2018 editions of TEEM Conference, the fourth edition of this track has been organized in the current 2019 edition. Computational thinking is still a very significant topic, especially, but not only, in pre-university education. In this edition, the robotic has a special role in the track, with a strength relationship with the STEM and
STEAM education of children at the pre-university levels, seeding the future of our society
Effect of Uncertainty on the Reaction Response in Fencing
Biomecanica del rendimiento en esgrim
Neutron-Capture elements in planetary nebulae: first detections of near-Infrared [Te III] and [Br V] emission lines
We have identified two new near-infrared emission lines in the spectra of
planetary nebulae (PNe) arising from heavy elements produced by neutron capture
reactions: [Te III] 2.1019 m and [Br V] 1.6429 m. [Te III] was
detected in both NGC 7027 and IC 418, while [Br V] was seen in NGC 7027. The
observations were obtained with the medium-resolution spectrograph EMIR on the
10.4m Gran Telescopio Canarias at La Palma, and with the high-resolution
spectrograph IGRINS on the 2.7m Harlan J. Smith telescope at McDonald
Observatory. New calculations of atomic data for these ions, specifically
A-values and collision strengths, are presented and used to derive ionic
abundances of Te and Br. We also derive ionic abundances of other
neutron-capture elements detected in the near-infrared spectra, and estimate
total elemental abundances of Se, Br, Kr, Rb, and Te after correcting for
unobserved ions. Comparison of our derived enrichments to theoretical
predictions from AGB evolutionary models shows reasonable agreement for solar
metallicity progenitor stars of 2 - 4 M. The
spectrally-isolated [Br V] 1.6429 m line has advantages for determining
nebular Br abundances over optical [Br III] emission lines that can be blended
with other features. Finally, measurements of Te are of special interest
because this element lies beyond the first peak of the s-process, and thus
provides new leverage on the abundance pattern of trans-iron species produced
by AGB stars.Comment: 9 pages, 1 figure, 4 tables. Accepted for publication in ApJ Letter
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