1,437 research outputs found
s/alpha/Fe Abundance Ratios in Halo Field Stars: Is there a Globular Cluster Connection?
We try to understand the s- and r-process elements vs Ti/Fe plots derived by
Jehin et al. (1999) for mildly metal-poor stars within the framework of the
analytical semi-empirical models for these elements by Pagel & Tautvaisiene
(1995, 1997). Jehin et al. distinguished two Pop II subgroups: IIa with
alpha/Fe and s-elements/Fe increasing together, which they attribute to pure
SNII activity, and IIb with constant alpha/Fe and a range in s/Fe which they
attribute to a prolonged accretion phase in parent globular clusters. However,
their sample consists mainly of thick-disk stars with only 4 clear halo
members, of which two are `anomalous' in the sense defined by Nissen & Schuster
(1997). Only the remaining two halo stars (and one in Nissen & Schuster's
sample) depart significantly from Y/Ti (or s/alpha) ratios predicted by our
model.Comment: 6 pages, 5 figures To appear in: Roma-Trieste Workshop 1999: `The
Chemical Evolution of the Milky Way: Stars vs Clusters', Vulcano Sept. 1999.
F. Giovanelli & F. Matteucci (eds), Kluwer, Dordrech
A Training Program to Improve IFSP/IEP Goals and Objectives Through the Routines-Based Interview
WOS:000329323800001 (NÂș de Acesso Web of Science)The authors describe a training program designed to improve the knowledge and skills of early childhood interventionists. Within the context of using the Routines-Based Early Intervention approach, this training focused on improving the quality of goals and objectives on individualized plans, through the Routines-Based Interview. We structured the training around five face-to-face sessions and a follow-up 3 months later. Here, we describe the development of the program, its content and methods, and the results on improvement of the goals and objectives with 80 professionals. These participants had completed the training, provided pretraining data, and provided posttraining data. Results showed that the training described here had the desired very large effect: Quality ratings of goals and objectives increased by over three standard deviations
Hydrogen bonding in substituted nitroanilines : isolated nets in 1,3-diamino-4-nitrobenzene and continuously interwoven nets in 3,5-dinitroaniline
Peer reviewedPublisher PD
Measuring professionalsâ perceptions about collaborative consultation in early childhood intervention
We investigated the reliability and construct validity of the Professionalsâ Perceptions about Collaborative Consultation in Early Childhood Intervention Scale (ProPerCECIS), a rating scale developed to measure collaborative consultation in early childhood intervention (ECI). ProPerCECIS was completed by 427 professionals
from 78 ECI teams. The full sample was randomised into sample A, 170 participants, for conducting an exploratory factor analysis (EFA) â and sample B, 257 participants, for performing confirmatory factor analysis (CFA). Multiple-group analysis, with the overall sample, was conducted. The EFA final solution comprised three correlated factors, with acceptable to very good internal consistency: Intervention, Context, and Planning. The CFA supported the three-factor structure. Results supported configural invariance and partial metric invariance, but partial scalar invariance did not hold. Results supported the conceptual framework of collaborative consultation in ECI and suggest that ProPerCECIS can be a useful measure of professionalsâ perceptions about collaborative consultation practices in ECI. ProPerCECIS seems to be particularly suited to assess collaborative practices within services
providing routines-based family-centred interventions. Importantly, because the factor structure for ProPerCECIS holds up for different professional groups, it might be used by transdisciplinary ECI teams.info:eu-repo/semantics/acceptedVersio
Effects of an in-service training program using the routines-based interview
The focus of this study is an in-service training program rooted in routines-based early intervention and designed to improve the quality of goals and objectives on individualized plans. Participants were local intervention team members and other professionals who worked closely with each team. This training program involved a small number of trainees per group, providing multiple learning experiences across time and various opportunities for self-assessment and monitoring. We investigated (a) the perceptions of the participants about the strengths and weaknesses of the training program, (b) medium-term outcomes of the training with a comparison group, (c) and variables associated with the quality of goals and objectives. This study involved training more than 200 professionals, and results support the effectiveness of the program in improving the quality of goals and objectives, showing the importance of the routines-based interview in producing that improvement.info:eu-repo/semantics/acceptedVersio
The Evolution of Carbon and Oxygen in the Bulge and Disk of the Milky Way
The evolution of C and O abundances in the Milky Way can impose strong
constraints on stellar nucleosynthesis and help understanding the formation and
evolution of our Galaxy. The aim is to review the measured C and O abundances
in the disk and bulge of the Galaxy and compare them with model predictions. We
adopt two successful chemical evolution models for the bulge and the disk,
which assume the same nucleosynthesis prescriptions but different histories of
star formation. The data show a clear distinction between the trend of [C/O] in
the thick and thin Galactic disks, while the thick disk and bulge trends are
indistinguishable with a large (>0.5 dex) increase in the C/O ratio in the
range from -0.1 to +0.4 dex for [O/H]. In our models we consider yields from
massive stars with and without the inclusion of metallicity-dependent stellar
winds. The observed increase in the [C/O] ratio with metallicity in the bulge
and thick disk lies between the predictions utilizing the mass-loss rates of
Maeder (1992) and those of Meynet & Maeder (2002). A model without
metallicity-dependent yields completely fails to match the observations. Thus,
the relative increase in carbon abundance at high metallicity appears to be due
to metallicity-dependent stellar winds in massive stars. These results also
explain the steep decline of the [O/Fe] ratio with [Fe/H] in the Galactic
bulge, while the [Mg/Fe] ratio is enhanced at all [Fe/H]. (abridged)Comment: 18 pages, 6 figures, submitted to Astronomy & Astrophysic
The Frequency of Carbon Stars Among Extremely Metal-Poor Stars
We demonstrate that there are systematic scale errors in the [Fe/H] values
determined by the Hamburg/ESO Survey (and by inference by the HK Survey in the
past) for certain extremely metal poor highly C-enhanced giants. The
consequences of these scale errors are that a) the fraction of carbon stars at
extremely low metallicities has been overestimated in several papers in the
recent literature b) the number of extremely metal poor stars known is somewhat
lower than has been quoted in the recent literature c) the yield for extremely
metal poor stars by the HES Survey is somewhat lower than is stated in the
recent literature. A preliminary estimate for the frequency of Carbon stars
among the giants in the HES sample with -4 < [Fe/H] < -2.0 dex is 7.4 +-2.9%;
adding an estimate for the C-enhanced giants with [C/Fe] > 1.0 dex without
detectable C2 bands raises the fraction to 14 +-4$%.
We rely on the results of an extensive set of homogeneous detailed abundance
analyses of stars expected to have [Fe/H] < -3.0 dex selected from the HES to
establish these claims. We have found that the Fe-metallicity of the cooler
(Teff < 5200K) C-stars as derived from spectra taken with HIRES at Keck are a
factor of ~10 higher than those obtained via the algorithm used by the HES
project to analyze the moderate resolution follow-up spectra, which is
identical to that used until very recently by the HK Survey. This error in
Fe-abundance estimate for C-stars arises from a lowering of the emitted flux in
the continuum bandpasses of the KP (3933 A line of CaII) and particularly the
HP2 (Hdelta) indices used to estimate [Fe/H] due to absorption from strong
molecular bands.Comment: Accepted to the ApJL after a very lengthly duel with the 3
simultaneous referee
The GIRAFFE Inner Bulge Survey (GIBS). I. Survey Description and a kinematical map of the Milky Way bulge
The Galactic bulge is a massive, old component of the Milky Way. It is known
to host a bar, and it has recently been demonstrated to have a pronounced
boxy/peanut structure in its outer region. Several independent studies suggest
the presence of more than one stellar populations in the bulge, with different
origins and a relative fraction changing across the bulge area. This is the
first of a series of papers presenting the results of the Giraffe Inner Bulge
Survey, carried out at the ESO-VLT with the multifibre spectrograph FLAMES.
Spectra of ~5000 red clump giants in 24 bulge fields have been obtained at
resolution R=6500, in the infrared Calcium triplet wavelength region at 8500
{\AA}. They are used to derive radial velocities and metallicities, based on
new calibration specifically devised for this project. Radial velocities for
another ~1200 bulge red clump giants, obtained from similar archive data, have
been added to the sample. Higher resolution spectra have been obtained for 450
additional stars at latitude b=-3.5, with the aim of investigating chemical
abundance patterns variations with longitude, across the inner bulge. In total
we present here radial velocities for 6392 RC stars. We derive a radial
velocity, and velocity dispersion map of the Milky Way bulge, useful to be
compared with similar maps of external bulges, and to infer the expected
velocities and dispersion at any line of sight. The K-type giants kinematics is
consistent with the cylindrical rotation pattern of M-giants from the BRAVA
survey. Our sample enables to extend this result to latitude b=-2, closer to
the Galactic plane than probed by previous surveys. Finally, we find strong
evidence for a velocity dispersion peak at (0,-1) and (0,-2), possibly
indicative of a high density peak in the central 250 pc of the bulgeComment: A&A in pres
s- and r-process element abundances in the CMD of 47 Tucanae using the Robert Stobie Spectrograph on SALT
A recent study by Wylie et al 2006 has revealed that s-process element
abundances are enhanced relative to iron in both red giant branch and
asymptotic giant branch stars of 47 Tucanae. A more detailed investigation into
s-process element abundances throughout the colour-magnitude diagram of 47
Tucanae is vital in order to determine whether the observed enhancements are
intrinsic to the cluster. This paper explores this possibility through
observational and theoretical means. The visibility of s- and r-process element
lines in synthetic spectra of giant and dwarf stars throughout the colour
magnitude diagram of 47 Tucanae has been explored. It was determined that a
resolving power of 10 000 was sufficient to observe s-process element abundance
variations in globular cluster giant branch stars. These synthetic results were
compared with the spectra of eleven 47 Tucanae giant branch stars observed
during the performance verification of the Robert Stobie Spectrograph on the
Southern African Large Telescope. Three s-process elements, Zr, Ba, Nd, and one
r-process element, Eu, were investigated. No abundance variations were found
such that [X/Fe] = 0.0 +/- 0.5 dex. It was concluded that this resolving power,
R ~ 5000, was not sufficient to obtain exact abundances but upper limits on the
s-process element abundances could be determined.Comment: 7 pages, 11 figure
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