311 research outputs found
A photometric study of the Orion OB 1 association. 2: Photometric analysis
The procedures adopted for analysis of photometric data in terms of color excesses, intrinsic color indexes, absolute visual magnitudes, and rotational-velocity effects are discussed in detail for Orion association B-, intermediate (I)-, and AF-type stars. The effects of the nebular environment and a comparison of various calibrations of Balmer-line and four-color indexes are considered for the determination of individual absolute magnitudes for B-type stars. When absolute magnitudes of stars in the region of the Orion Nebula are determined from the beta index, emission mechanisms appear to spuriously brighten them. A detailed comparison of absolute magnitudes derived from Balmer-line indexes and MK spectral-type calibrations is presented. The data are also examined with regard to the effects of polarization and infrared excesses. The results suggest a complex combination of intracluster and circumstellar origins for these processes
A photometric study of the Orion OB 1 association. 1: Observational data
An extensive catalog of observational data is presented for stars in the region of the young stellar association Orion OB 1. In addition to new photoelectric observations obtained on the uvbyB and UBV systems, photoelectric and spectroscopic data were compiled for the stars observed and for several bright members of the association having available photometric indices. Mean weighted values were computed for the uvbyB and UBV data and are tabulated in summary tables which include all references for individual values. These tables are expected to be reasonably complete for association members earlier than spectral type A0. From an analysis of currently available proper motion, radial velocity, and photometric data, membership criteria were derived and qualitative membership probabilities for 526 stars were summarized. A set of charts is included for assistance in identification of the program stars in all regions of the association
Light Element Abundance Inhomogeneities in Globular Clusters: Probing Star Formation and Evolution in the Early Milky Way
Abundance patterns of the elements C, N, and O are sensitive probes of
stellar nucleosynthesis processes and, in addition, O abundances are an
important input for stellar age determinations. Understanding the nature of the
observed distribution of these elements is key to constraining protogalactic
star formation history. Patterns deduced from low-resolution spectroscopy of
the CN, CH, NH, and CO molecules for low-mass stars in their core-hydrogen or
first shell-hydrogen burning phases in the oldest ensembles known, the Galactic
globular star clusters, are reviewed. New results for faint stars in NGC 104
(47 Tuc, C0021-723) reveal that the bimodal, anticorrelated pattern of CN and
CH strengths found among luminous evolved stars is also present in stars
nearing the end of their main-sequence lifetimes. In the absence of known
mechanisms to mix newly synthesized elements from the interior to the
observable surface layers of such unevolved stars, those particular
inhomogeneities imply that the original material from which the stars formed
some 15 billion years ago was chemically inhomogeneous in the C and N elements.
However, in other clusters, observations of abundance ratios and C isotope
ratios suggest that alterations to surface chemical compositions are produced
as stars evolve from the main sequence through the red giant branch. Thus, the
current observed distributions of C, N, and O among the brightest stars (those
also observed most often) may not reflect the true distribution from which the
protocluster cloud formed. The picture which is emerging of the C, N and O
abundance patterns within globular clusters may be one whichComment: 12 pages in uuencoded compressed postscript (including figures), to
appear in the Canadian Journal of Physics (Special Issue in Honor of G.
Herzberg
A photometric study of the Orion OB 1 association. 3: Subgroup analyses
The four principal subgroups of the association were examined in detail using individual distances and reddening values determined for their B type members. Subgroup 1a appeared not to show a spread in age nor did it show a systematic distance increase with right ascension when fainter members were considered. An eastwardly increase in distance was found for subgroup 1b but the reddening law for the east Belt appeared normal. Small subclusterings in the vicinity of the Orion Nebula appeared not to differ in the evolutionary state but their ages were considerably greater than those of stars in the nebulae and its associated cluster
Mathematical Analysis of Computer Generated Binary Fourier Transform Holograms
A rigorous mathematical treatment of a general binarization process for computer generated binary Fourier transform hologram is developed. Further a generalized error diffusion coefficient matrix is derived. In the view of these mathematical results we distinguish different binarization methods by the error diffusion process. Some binarization methods, their properties, and computational demands are investigated. Examples are presented
Analysis of linearized inverse problems in ultrasound transmission imaging
The purpose of this paper is to analyze the linearized inverse problem during the iterativesolution process of the ill-posed nonlinear inverse problem of image reconstruction for ultra-sound transmission imaging. We show that the conjugate gradient applied to normal equation(CGNE) method gives more reliable solutions for linearized systems than Tikhonov regular-ization methods. The linearized systems are more sensitive when treated by CGNE than byTikhonov regularization methods. The Tikhonov regularization is less effective at the be-ginning of the outer-loop iteration, where the nonlinearity is dominating while the conjugategradient for the linearized system stops earlier. Only when the linear approximation is goodenough to describe the whole system, Tikhonov regularization can fully play its role and giveslightly better reconstruction results as compared to CGNE in a very noisy case
NGC 2419, M92, and the Age Gradient in the Galactic Halo
The WFPC2 camera on HST has been used to obtain deep main sequence photometry
of the low-metallicity ([Fe/H]=-2.14), outer-halo globular cluster NGC 2419. A
differential fit of the NGC 2419 CMD to that of the similarly metal-poor \
standard cluster M92 shows that they have virtually identical principal
sequences and thus the same age to well within 1 Gyr. Since other
low-metallicity clusters throughout the Milky Way halo have this same age to
within the 1-Gyr precision of the differential age technique, we conclude that
the earliest star (or globular cluster) formation began at essentially the same
time everywhere in the Galactic halo throughout a region now almost 200 kpc in
diameter. Thus for the metal-poorest clusters in the halo there is no
detectable age gradient with Galactocentric distance. To estimate the absolute
age of NGC 2419 and M92, we fit newly computed isochrones transformed through
model-atmosphere calculations to the (M_V,V-I) plane, with assumed distance
scales that represent the range currently debated in the literature.
Unconstrained isochrone fits give M_V(RR) = 0.55 \pm 0.06 and a resulting age
of 14 to 15 Gyr. Incorporating the full effects of helium diffusion would
further reduce this estimate by about 1 Gyr. A distance scale as bright as
M_V(RR) = 0.15 for [Fe/H] = -2, as has recently been reported, would leave
several serious problems which have no obvious solution in the context of
current stellar models.Comment: 32 pages, aastex, 9 postscript figures; accepted for publication in
AJ, September 1997. Also available by e-mail from [email protected]
NGC 5128: The Giant Beneath
I review what we have learned about the old stellar population of NGC 5128,
the only large E galaxy close enough that we can currently observe individual
stars as faint as the horizontal branch. Although its galaxy type is still a
matter of debate for some, the uncertainties over distance are now largely
resolved; comparison of five stellar distance indicators gives d=3.8 +- 0.1
Mpc. The globular cluster system, which was once perplexingly invisible, is now
known to be predominantly old with a substantial metal-rich component. The GCS
total population and luminosity function are normal and the clusters follow the
same fundamental plane relation as those in the Milky Way and M31. Finally, the
halo out to at least ~7r_{eff} is dominated by metal-rich stars which are also
predominantly old, with age and metallicity tantalizingly similar to the
majority of globular clusters.Comment: PASA in pres
OC-0060: Workflow automation for ultrafast kilovoltage-megavoltage conebeam CT for image guided radiotherapy
Exploring the photometric signatures of magnetospheres around Helium-strong stars
The photometric variations due to magnetically confined material around
He-strong stars are investigated within the framework of the Rigidly Rotating
Magnetosphere (RRM) model. For dipole field topologies, the model is used to
explore how the morphology of light curves evolves in response to changes to
the observer inclination, magnetic obliquity, rotation rate and optical depth.
The general result is that double-minimum light curves arise when the
obliquity and/or inclination are close to 90 degrees; no light variations are
seen in the opposite limit; and for intermediate cases, single-minimum light
curves occur. These findings are interpreted with the aid of a simple,
analytical torus model, paving the way for the development of new
photometric-based constraints on the fundamental parameters of He-strong stars.
Illustrative applications to five stars in the class are presented.Comment: 9 pages, 7 figures, to appear in MNRA
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