2,119 research outputs found
Fiducial Stellar Population Sequences for the VJKs Photometric System
We have obtained broad-band near-infrared photometry for seven Galactic star
clusters (M92, M15, M13, M5, NGC1851, M71 and NGC6791) using the WIRCam
wide-field imager on the Canada-France-Hawaii Telescope, supplemented by images
of NGC1851 taken with HAWK-I on the VLT. In addition, 2MASS observations of the
[Fe/H] ~ 0.0 open cluster M67 were added to the cluster database. From the
resultant (V-J)-V and (V-Ks)-V colour-magnitude diagrams (CMDs), fiducial
sequences spanning the range in metallicity, -2.4 < [Fe/H] < +0.3, have been
defined which extend (for most clusters) from the tip of the red-giant branch
(RGB) to ~ 2.5 magnitudes below the main-sequence turnoff. These fiducials
provide a valuable set of empirical isochrones for the interpretation of
stellar population data in the 2MASS system. We also compare our newly derived
CMDs to Victoria isochrones that have been transformed to the observed plane
using recent empirical and theoretical colour-Teff relations. The models are
able to reproduce the entire CMDs of clusters more metal rich than [Fe/H] ~
-1.4 quite well, on the assumption of the same reddenings and distance moduli
that yield good fits of the same isochrones to Johnson-Cousins BV(RI)C
photometry. However, the predicted giant branches become systematically redder
than the observed RGBs as the cluster metallicity decreases. Possible
explanations for these discrepancies are discussed.Comment: 18 pages, 20 figures, Accepted for publication in A
Fiducial Stellar Population Sequences for the u'g'r'i'z' System
We describe an extensive observational project that has obtained high-quality
and homogeneous photometry for a number of different Galactic star clusters
(including M 92, M 13, M 3, M 71, and NGC 6791) spanning a wide range in
metallicity (-2.3<[Fe/H]<+0.4), as observed in the u'g'r'i'z' passbands with
the MegaCam wide-field imager on the Canada-France-Hawaii Telescope. By
employing these purest of stellar populations, fiducial sequences have been
defined from color-magnitude diagrams that extend from the tip of the red-giant
branch down to approximately 4 magnitudes below the turnoff: these sequences
have been accurately calibrated to the standard u'g'r'i'z' system via a set of
secondary photometric standards located within these same clusters.
Consequently, they can serve as a valuable set of empirical fiducials for the
interpretation of stellar populations data in the u'g'r'i'z' system.Comment: 16 pages, 7 tables, 13 figures; accepted for publication in A
Color-Magnitude Diagram Constraints on the Metallicities, Ages, and Star Formation History of the Stellar Populations in the Carina Dwarf Spheroidal Galaxy
Victoria-Regina isochrones for [alpha/Fe] and a wide
range in [Fe/H], along with complementary zero-age horizontal branch (ZAHB)
loci, have been applied to the color-magnitude diagram (CMD) of Carina. The
color transformations that we have used have been "calibrated" so that
isochrones provide excellent fits to the -diagrams of M3 and
M92, when well supported estimates of the globular cluster (GC) reddenings and
metallicities are assumed. The adopted distance moduli, for both the GCs and
Carina, are based on our ZAHB models, which are able to reproduce the old HB
component (as well as the luminosity of the HB clump) of the dwarf spheroidal
galaxy quite well --- even if it spans a range in [Fe/H] of ~ 1.5 dex, provided
that [alpha/Fe] varies with [Fe/H] in approximately the way that has been
derived spectroscopically. Ages derived here agree reasonably well with those
found previously for the old and intermediate-age turnoff stars, as well as for
the period of negligible star formation (SF) activity (~ 6-10 Gyr ago). CMD
simulations have been carried out for the faintest turnoff and subgiant stars.
They indicate a clear preference for SF that lasted several Gyr instead of a
short burst, with some indication that ages decrease with increasing [Fe/H]. In
general, stellar models that assume spectroscopic metallicities provide
satisfactory fits to the observations, including the thin giant branch of
Carina, though higher oxygen abundances than those implied by the adopted
values of [alpha/Fe] would have favorable consequences.Comment: 15 pages, including 12 figures; accepted for publication in the
Astrophysical Journa
An Examination of Recent Transformations to the BV(RI)_C Photometric System from the Perspective of Stellar Models for Old Stars
Isochrones for ages > 4 Gyr and metallicities in the range -2.5 < [Fe/H] <
+0.3 that take the diffusion of helium and recent advances in stellar physics
into account are compared with observations in the Johnson-Cousins BV(RI)_C
photometric system for several open and globular star clusters. The adopted
color-Teff relations include those which we have derived from the latest MARCS
model atmospheres and empirical transformations for dwarf and subgiant stars
given by Casagrande et al (2010, A&A, 512, 54; CRMBA). Those reported by
VandenBerg & Clem (2003, AJ, 126, 778) have also been considered, mainly to
resolve some outstanding questions concerning them. Remarkably, when the
subdwarfs in the CRMBA data set that have sigma_pi/pi < 0.15 are superimposed
on a set of 12 Gyr isochrones spanning a wide range in [Fe/H], the inferred
metallicities and effective temperatures agree, in the mean, with those given
by CRMBA to within +/- 0.05 dex and +/- 10 K, respectively. Thus the hot Teff
scale derived by CRMBA is nearly identical with that predicted by stellar
models and consequently, there is excellent consistency between theory and
observations on the H-R diagram and the different color-magnitude diagrams
considered in this investigation. To obtain similar consistency, the colors
obtained from the MARCS and VandenBerg & Clem B-V vs. Teff relations for
metal-poor dwarf stars should be adjusted to the red by 0.02-0.03 mag. In
general, isochrones that employ the CRMBA transformations provide reasonably
good fits to our BV(RI)_C photometry for main-sequence stars in the globular
clusters 47 Tuc, M3, M5, M92 and NGC 1851 - but not the cluster giants (when
adopting the synthetic MARCS colors). We speculate that differences between the
actual heavy-element mixtures and those assumed in the theoretical models may
be the primary cause of this difficulty.Comment: To appear in 2010, AJ, 140, 102
Efficacy of Strobilurin fungicides on yield and milling quality traits in red lentil
Non-Peer Reviewe
Adding nutritional value to lentils (Lens culinaris Medik.)
Non-Peer Reviewe
Variation in pinto seed coat darkening
Non-Peer ReviewedDarkening of the seed coat is a significant economic problem in pinto bean production. Beans that have darkened are considered old, more difficult to cook, and prices are discounted. Some varieties darken much more quickly than others and, as a result, are more often downgraded than those that retain their bright background colour. On a Pulse Canada marketing mission to Mexico in April 2002, all pinto bean buyers consistently identified the sample with the brightest background as their preference. They complained about the quality of pintos coming out of the Midwest USA and the eastern Prairies, primarily due to the darkened seed coats. We grew 10 different pinto varieties in four different environments and subjected the harvested beans to aging to determine the level of variability for seed coat darkening in the varieties. Varieties that maintain their bright background will be used in future breeding efforts to develop non-darkening pinto varieties
Relative bioavailability of iron in Bangladeshi traditional meals prepared with iron-fortified lentil dal
Non-Peer Reviewe
Flat pulses in a flat land – what’s on the horizon?
Non-Peer Reviewe
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