73 research outputs found
A Lone Male
Perhaps you have wondered what goes through a man\u27s mind as he opens the door of MacKay Hall. Is he out of his realm? Is he uncomfortable in a woman \u27s world ? Let\u27s ask him how he feels. (And you can get further information from the male who\u27s seated next to you in one of your home economics classes.
Phi Upsilon Omicron
Yellow and white are the colors of Phi Upsilon Omicron, and the girls wearing ribbons of these hues this month are new pledges of the fraternity
Graduate Recital: Kirby Reese, Trumpet; Joy Knapp, Piano; April 17, 1977
Hayden AuditoriumSunday AfternoonApril 17, 19774:00 p.m
A Sunyaev-Zel'dovich Effect Survey for High Redshift Clusters
Interferometric observations of the Sunyaev-Zel'dovich Effect (SZE) toward
clusters of galaxies provide sensitive cosmological probes. We present results
from 1 cm observations (at BIMA and OVRO) of a large, intermediate redshift
cluster sample. In addition, we describe a proposed, higher sensitivity array
which will enable us to survey large portions of the sky. Simulated
observations indicate that we will be able to survey one square degree of sky
per month to sufficient depth that we will detect all galaxy clusters more
massive than 2x10^{14} h^{-1}_{50}M_\odot, regardless of their redshift. We
describe the cluster yield and resulting cosmological constraints from such a
survey.Comment: 7 pages, 6 figures, latex, contribution to VLT Opening Symposiu
Imaging the Sunyaev-Zel'dovich Effect
We report on results of interferometric imaging of the Sunyaev-Zel'dovich
Effect (SZE) with the OVRO and BIMA mm-arrays. Using low-noise cm-wave
receivers on the arrays, we have obtained high quality images for 27 distant
galaxy clusters. We review the use of the SZE as a cosmological tool. Gas mass
fractions derived from the SZE data are given for 18 of the clusters, as well
as the implied constraint on the matter density of the universe, . We
find . A best guess for the matter
density obtained by assuming a reasonable value for the Hubble constant and
also by attempting to account for the baryons contained in the galaxies as well
as those lost during the cluster formation process gives .
We also give preliminary results for the Hubble constant. Lastly, the power for
investigating the high redshift universe with a non-targeted high sensitivity
SZE survey is discussed and an interferometric survey is proposed.Comment: 14 pages, 7 figures, latex, contribution to Nobel Symposium "Particle
Physics and the Universe" to appear in Physica Scripta and World Scientific,
eds L. Bergstrom, P. Carlson and C. Fransso
Markov Chain Monte Carlo joint analysis of Chandra X-ray imaging spectroscopy and Sunyaev-Zeldovich Effect data
X-ray and Sunyaev-Zeldovich Effect data can be combined to determine the
distance to galaxy clusters. High-resolution X-ray data are now available from
the Chandra Observatory, which provides both spatial and spectral information,
and Sunyaev-Zeldovich Effect data were obtained from the BIMA and OVRO arrays.
We introduce a Markov chain Monte Carlo procedure for the joint analysis of
X-ray and Sunyaev-Zeldovich Effect data. The advantages of this method are the
high computational efficiency and the ability to measure simultaneously the
probability distribution of all parameters of interest, such as the spatial and
spectral properties of the cluster gas and also for derivative quantities such
as the distance to the cluster. We demonstrate this technique by applying it to
the Chandra X-ray data and the OVRO radio data for the galaxy cluster Abell
611. Comparisons with traditional likelihood-ratio methods reveal the
robustness of the method. This method will be used in follow-up papers to
determine the distances to a large sample of galaxy clusters.Comment: ApJ accepted, scheduled for ApJ 10 October 2004, v614 issue. Title
changed, added more convergence diagnostic tests, Figure 7 converted to lower
resolution for easier download, other minor change
A Preliminary Detection of Arcminute Scale Cosmic Microwave Background Anisotropy with the BIMA Array
We have used the Berkeley-Illinois-Maryland-Association (BIMA) array
outfitted with sensitive cm-wave receivers to expand our search for arcminute
scale anisotropy of the Cosmic Microwave Background (CMB). The interferometer
was placed in a compact configuration toobtain high brightness sensitivity on
arcminute scales over its 6.6' FWHM field of view. The sensitivity of this
experiment to flat band power peaks at a multipole of l=5530 which corresponds
to an angular scale of ~2'. We present the analysis of a total of 470 hours of
on-source integration time on eleven independent fields which were selected
based on their low IR contrast and lack of bright radio sources. Applying a
Bayesian analysis to the visibility data, we find CMB anisotropy flat band
power Q_flat = 6.1(+2.8/-4.8) microKelvin at 68% confidence. The confidence of
a non- zero signal is 76% and we find an upper limit of Q_flat < 12.4
microKelvin at 95% confidence. We have supplemented our BIMA observations with
concurrent observations at 4.8 GHz with the VLA to search for and remove point
sources. We find the point sources make an insignificant contribution to the
observed anisotropy.Comment: 8 pages, 2 figures, submitted to Astrophysical Journa
The Iowa Homemaker vol.41, no.7
Foolproof Bachelor Budget, Gaylin Morgan, page 4
A “Lone Male”, Joy Reese, page 5
It All Started With ADAM, Sherry Stoddard, page 6
Going Forth, Dan Taylor, page 9
Bottled Beauty Since 1600 B.C., Diane Sharbo, page 10
What’s the Matter?, Bob MacDonough, page 11
The Awful Beginning, Don Wishart, page 12
Found: Scientific Formula for Women, page 15
When Men Entertain, Sylvia Noid, page 16
The Man Behind “the lady from Hancock”, LaVeda Jansonius, page 16
“We Want Steak!”, Barb Pierson, page 1
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