405 research outputs found
Fabry-Perot Absorption Line Spectroscopy of the Galactic Bar. II. Stellar Metallicities
We measure the Ca II 8542 line strength in 3360 stars along three
lines-of-sight in the Galactic bar: (l,b) ~ (+/-5.0,-3.5) and Baade's Window,
using Fabry-Perot (FP) absorption line spectroscopy. This is the first attempt
to show that reliable absorption line strengths can be measured using FP
spectroscopy. The Ca II 8542 line is a good indicator of metallicity and its
calibration to [Fe/H] is determined for globular cluster red giants in previous
investigations. We derive such a calibration for the bulge giants and use it to
infer metallicities for our full red clump sample (2488 stars) at all three
lines-of-sight. We present the stellar metallicity distributions along the
major axis of the bar. We find the mean [Fe/H] = -0.09 +/- 0.04 dex in Baade's
Window, and find the distribution in this field to agree well with previous
works. We find gradients in the mean metallicity and its dispersion w.r.t
Baade's WIndow of -0.45 and -0.20 dex respectively at l = +5.5, and of -0.10
dex and -0.20 dex at l = -5.0. We detect a signature of a possible tidal stream
at l = +5.5, in both our velocity and metallicity distributions. Its radial
velocity indicates that it is not associated with the Sagittarius stream. We
also measure the metallicity of a bulge globular cluster NGC 6522 in our
Baade's Window field to be -0.90 +/- 0.10 dex, in agreement with recent
measurements of Zoccali et al. (2008). This agreement demonstrates the
reliability of our metallicity measurements.Comment: accepted for publication in the Astrophysical Journal, 15 pages, 12
figure
Alpha clustering and weak coupling in the A=90 region
From the viewpoint of a unified description of cluster structure and
scattering in the
A=90 region, scattering from Y is investigated.
clustering and weak coupling in Nb is discussed.Comment: 8 pages, 4 figure
Sodium abundances in nearby disk stars
We present sodium abundances for a sample of nearby stars. All results have
been derived from NLTE statistical equilibrium calculations. The influence of
collisional interactions with electrons and hydrogen atoms is evaluated by
comparison of the solar spectrum with very precise fits to the Na I line cores.
The NLTE effects are more pronounced in metal-poor stars since the statistical
equilibrium is dominated by collisions of which at least the electronic
component is substantially reduced. The resulting influence on the
determination of sodium abundances is in a direction opposite to that found
previously for Mg and Al. The NLTE corrections are about -0.1 in thick-disk
stars with [Fe/H] about -0.6. Our [Na/Fe] abundance ratios are about solar for
thick- and thin-disk stars. The increase in [Na/Fe] as a function of [Fe/H] for
metal-rich stars found by Edvardsson et al. (1993) is confirmed. Our results
suggest that sodium yields increase with the metallicity, and quite large
amounts of sodium may be produced by AGB stars. We find that [Na/Fe]ratios,
together with either [Mg/Fe] ratio, kinematic data or stellar evolutionary
ages, make possible the individual discrimination between thin- and thick-disk
membership.Comment: 11pages, 11 figures. A&A accepte
The first chemical abundance analysis of K giants in the inner Galactic disc
The elemental abundance structure of the Galactic disc has been extensively
studied in the solar neighbourhood using long-lived stars such as F and G
dwarfs or K and M giants. These are stars whose atmospheres preserve the
chemical composition of their natal gas clouds, and are hence excellent tracers
of the chemical evolution of the Galaxy. As far as we are aware, there are no
such studies of the inner Galactic disc, which hampers our ability to constrain
and trace the origin and evolution of the Milky Way. Therefore, we aim in this
study to establish the elemental abundance trend(s) of the disc(s) in the inner
regions of the Galaxy. Based on equivalent width measurements in
high-resolution spectra obtained with the MIKE spectrograph on the Magellan II
telescope on Las Campanas in Chile, we determine elemental abundances for 44
K-type red giant stars in the inner Galactic disc, located at Galactocentric
distances of 4-7\,kpc. The analysis method is identical to the one recently
used on red giant stars in the Galactic bulge and in the nearby thin and thick
discs, enabling us to perform a truly differential comparison of the different
stellar populations. We present the first detailed elemental abundance study of
a significant number of red giant stars in the inner Galactic disc. We find
that these inner disc stars show the same type of chemical and kinematical
dichotomy as the thin and thick discs show in the solar neighbourhood. The
abundance trends of the inner disc agree very well with those of the nearby
thick disc, and also to those of the Bulge. The chemical similarities between
the Bulge and the Galactic thick disc stellar populations indicate that they
have similar chemical histories, and any model trying to understand the
formation and evolution of either of the two should preferably incorporate both
of them.Comment: A&A Letters, accepte
Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars. Detailed abundance analysis of OGLE-2008-BLG-209S
AIMS. Our aims are twofold. First we aim to evaluate the robustness and
accuracy of stellar parameters and detailed elemental abundances that can be
derived from high-resolution spectroscopic observations of microlensed dwarf
and subgiant stars. We then aim to use microlensed dwarf and subgiant stars to
investigate the abundance structure and chemical evolution of the Milky Way
Bulge. [ABRIDGED] METHODS. We present a detailed elemental abundance analysis
of OGLE-2008-BLG-209S, the source star of a new microlensing event towards the
Bulge, for which we obtained a high-resolution spectrum with the MIKE
spectrograph on the Magellan Clay telescope. We have performed four different
analyses of OGLE-2008-BLG-209S. [ABRIDGED] We have also re-analysed three
previous microlensed dwarf stars OGLE-2006-BLG-265S, MOA-2006-BLG-099S, and
OGLE-2007-BLG-349S with the same method. This homogeneous data set, although
small, enables a direct comparison between the different stellar populations.
RESULTS. We find that OGLE-2008-BLG-209S is a subgiant star that has a
metallicity of [Fe/H] ~-0.33. It possesses [alpha/Fe] enhancements similar to
what is found for Bulge giant stars at the same metallicity, and what also is
found for nearby thick disc stars at the same metallicity. In contrast, the
previous three microlensing dwarf stars have very high metallicities,
[Fe/H]>+0.4, and more solar-like abundance ratios, i.e. [alpha/Fe]~0. The
decrease in the [alpha/Fe] ratio with [Fe/H] is the typical signature of
enrichment from low and intermediate mass stars. We furthermore find that the
results for the four Bulge stars, in combination with results from studies of
giant stars in the Bulge, seem to favour a secular formation scenario for the
Bulge.Comment: Accepted for publication in A&A, 17 pages, online table will be
available in published version, or by contacting the first autho
AntiâVascular Endothelial Growth Factor Drugs Compared With Panretinal Photocoagulation for the Treatment of Proliferative Diabetic Retinopathy: A Cost-Effectiveness Analysis
\ua9 2024Objectives: This study aimed to evaluate the cost-effectiveness of antiâvascular endothelial growth factor drugs (anti-VEGFs) compared with panretinal photocoagulation (PRP) for treating proliferative diabetic retinopathy (PDR) in the United Kingdom. Methods: A discrete event simulation model was developed, informed by individual participant data meta-analysis. The model captures treatment effects on best corrected visual acuity in both eyes, and the occurrence of diabetic macular edema and vitreous hemorrhage. The model also estimates the value of undertaking further research to resolve decision uncertainty. Results: Anti-VEGFs are unlikely to generate clinically meaningful benefits over PRP. The model predicted anti-VEGFs be more costly and similarly effective as PRP, generating 0.029 fewer quality-adjusted life-years at an additional cost of \ua33688, with a net health benefit of â0.214 at a \ua320 000 willingness-to-pay threshold. Scenario analysis results suggest that only under very select conditions may anti-VEGFs offer potential for cost-effective treatment of PDR. The consequences of loss to follow-up were an important driver of model outcomes. Conclusions: Anti-VEGFs are unlikely to be a cost-effective treatment for early PDR compared with PRP. Anti-VEGFs are generally associated with higher costs and similar health outcomes across various scenarios. Although anti-VEGFs were associated with lower diabetic macular edema rates, the number of cases avoided is insufficient to offset the additional treatment costs. Key uncertainties relate to the long-term comparative effectiveness of anti-VEGFs, particularly considering the real-world rates and consequences of treatment nonadherence. Further research on long-term visual acuity and rates of vision-threatening complications may be beneficial in resolving uncertainties
Chemical evolution of the Galactic bulge as traced by microlensed dwarf and subgiant stars. II. Ages, metallicities, detailed elemental abundances, and connections to the Galactic thick disc
The Bulge is the least understood major stellar population of the Milky Way.
Most of what we know about the formation and evolution of the Bulge comes from
bright giant stars. The underlying assumption that giants represent all the
stars, and accurately trace the chemical evolution of a stellar population, is
under debate. In particular, recent observations of a few microlensed dwarf
stars give a very different picture of the evolution of the Bulge from that
given by the giant stars. [ABRIDGED] We perform a detailed elemental abundance
analysis of dwarf stars in the Galactic bulge, based on high-resolution spectra
that were obtained while the stars were optically magnified during
gravitational microlensing events. [ABRIDGED] We present detailed elemental
abundances and stellar ages for six new dwarf stars in the Galactic bulge.
Combining these with previous events, here re-analysed with the same methods,
we study a homogeneous sample of 15 stars, which constitute the largest sample
to date of microlensed dwarf stars in the Galactic bulge. We find that the
stars span the full range of metallicities from [Fe/H]=-0.72 to +0.54, and an
average metallicity of =-0.08+/-0.47, close to the average metallicity
based on giant stars in the Bulge. Furthermore, the stars follow well-defined
abundance trends, that for [Fe/H]<0 are very similar to those of the local
Galactic thick disc. This suggests that the Bulge and the thick disc have had,
at least partially, comparable chemical histories. At sub-solar metallicities
we find the Bulge dwarf stars to have consistently old ages, while at
super-solar metallicities we find a wide range of ages. Using the new age and
abundance results from the microlensed dwarf stars we investigate possible
formation scenarios for the Bulge.Comment: New version accepted for publication in Astronomy and Astrophysic
Early Galactic Evolution of Carbon, Nitrogen and Oxygen
We present results on carbon, nitrogen, and oxygen abundances for a sample of
unevolved metal-poor stars with metallicities in the range -0.3< [Fe/H]< -3.
Oxygen abundances derived from different indicators are compared showing
consistently that in the range 0.3 >[Fe/H]>-3.0, the [O/Fe] ratio increases
from approximately 0 to 1. We find a good agreement between abundances based on
the forbidden line, the OH and IR triplet lines when gravities based on
Hipparcos} parallaxes are considered for the sample stars. Gravities derived
from LTE ionization balance in metal-poor stars with [Fe/H]< -1 are likely too
low, and could be responsible for an underestimation of the oxygen abundances
derived using the [OI] line. [C/Fe] and [N/Fe] ratios appear to be constant,
independently of metallicity, in the same range. However, they show larger
scatter than oxygen at a given metallicity, which could reflect the larger
variety of stellar production sites for these other elements.Comment: 10 pages, 3 figures, To appear in the proceedings of the conference
"The Chemical Evolution of The Milky Way: Stars versus Clusters", eds. F.
Matteucci and F. Giovannelli, Vulcano, Italy, September 20-24 199
Oxygen Abundances in Two Metal-Poor Subgiants from the Analysis of the 6300 A Forbidden O I Line
Recent LTE analyses (Israelian et al. 1998 and Bosegaard et al. 1999) of the
OH bands in the optical-ultraviolet spectra of nearby metal-poor subdwarfs
indicate that oxygen abundances are generally higher than those previously
determined. The difference increases with decreasing metallicity and reaches
delta([O/Fe]) ~ +0.6 dex as [Fe/H] approaches -3.0.
Employing high resolution (R = 50000), high S/N (~ 250) echelle spectra of
the two stars found by Israelian et al. (1998) to have the highest
[O/Fe]-ratios, viz, BD +23 3130 and BD +37 1458, we conducted abundance
analyses based on about 60 Fe I and 7-9 Fe II lines. We determined from Kurucz
LTE models the values of the stellar parameters, as well as abundances of Na,
Ni, and the traditional alpha-elements, independent of the calibration of color
vs scales. We determined oxygen abundances from spectral synthesis of
the stronger line (6300 A) of the [O I] doublet.
The syntheses of the [O I] line lead to smaller values of [O/Fe], consistent
with those found earlier among halo field and globular cluster giants. We
obtain [O/Fe] = +0.35 +/- 0.2 for BD +23 3130 and +0.50 +/- 0.2 for BD +37
1458. In the former, the [O I] line is very weak (~ 1 mA), so that the quoted
[O/Fe] value may in reality be an upper limit.
Therefore in these two stars a discrepancy exists between the [O/Fe]- ratios
derived from [O I] and the OH feature, and the origin of this difference
remains unclear. Until the matter is clarified, we suggest it is premature to
conclude that the ab initio oxygen abundances of old, metal-poor stars need to
be revised drastically upward.Comment: 38 pages, 5 tables, 14 figures To appear in July 1999 AJ Updated
April 16, 1999. Fixed typo
The RAVE Survey: Constraining the Local Galactic Escape Speed
We report new constraints on the local escape speed of our Galaxy. Our
analysis is based on a sample of high velocity stars from the RAVE survey and
two previously published datasets. We use cosmological simulations of disk
galaxy formation to motivate our assumptions on the shape of the velocity
distribution, allowing for a significantly more precise measurement of the
escape velocity compared to previous studies. We find that the escape velocity
lies within the range 498\kms < \ve < 608 \kms (90 per cent confidence), with
a median likelihood of 544\kms. The fact that \ve^2 is significantly
greater than 2\vc^2 (where \vc=220\kms is the local circular velocity)
implies that there must be a significant amount of mass exterior to the Solar
circle, i.e. this convincingly demonstrates the presence of a dark halo in the
Galaxy. For a simple isothermal halo, one can calculate that the minimum radial
extent is kpc. We use our constraints on \ve to determine the mass
of the Milky Way halo for three halo profiles. For example, an adiabatically
contracted NFW halo model results in a virial mass of
and virial radius of
kpc (90 per cent confidence). For this model the circular
velocity at the virial radius is 142^{+31}_{-21}\kms. Although our halo
masses are model dependent, we find that they are in good agreement with each
other.Comment: 19 pages, 9 figures, MNRAS (accepted). v2 incorporates minor cosmetic
revisions which have no effect on the results or conclusion
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