421 research outputs found
Elizabeth Houston and John McIntosh Madison in account with Beverly Robinson, July 24, 1826
An account of money owed and paid by Elizabeth Houston and John McIntosh Madison to Beverly Robinson. It appears the account was prepared by John H.W. McIntosh and sent to Peter Kean, who had power of attorney.
People Included: Maria C. Madison
Places Included: Georgiahttps://digitalcommons.kean.edu/lhc_1820s/1081/thumbnail.jp
Preliminary report of a gas conditioner to improve operational reliability of cryotherapy in developing countries
BACKGROUND: Cryotherapy is a safe, affordable, and effective method of treatment for cervical intraepithelial neoplasia. In some low-resource settings, environmental conditions or qualities of the refrigerant gas can lead to blockage of cryotherapy equipment, terminating treatment. A prototype of a gas conditioner to prevent operational failure was designed, built, and field tested. METHODS: The prototype conditioner device consists of an expansion chamber that filters and dries the refrigerant gas. Users in Peru and Kenya reported on their experience with the prototype conditioner. In Ghana, simulated cryotherapy procedures were used to test the effects of the prototype conditioner, as well as the commonly used "cough technique." RESULTS: Anecdotal reports from field use of the device were favorable. During simulated cryotherapy, the prevalence of blockage during freezing were 0% (0/25) with the device alone, 23.3% (7/30) with the cough technique alone, 5.9% (1/17) with both, and 55.2% (16/29) with neither (Pearson's Chi square = 26.6, df = 3, p < 0.001 (comparison amongst all groups)). CONCLUSION: This prototype design of a cryotherapy gas conditioner is a potential solution for low-resource settings that are experiencing cryotherapy device malfunction
GEMS Survey Data and Catalog
We describe the data reduction and object cataloging for the GEMS survey, a large-area (800 arcmin(2)) two-band (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the Hubble Space Telescope, centered on the Chandra Deep Field-South.STScI HST-GO-9500.01NASA GO-9500, NAS5-26555, NAG5-13063, NAG5-13102European Communityâs Human Potential Programunder contractHPRN-CT-2002-00316, HPRN-CT-2002-00305McDonald Observator
GEMS: Galaxy fitting catalogues and testing parametric galaxy fitting codes
In the context of measuring structure and morphology of intermediate redshift
galaxies with recent HST/ACS surveys, we tune, test, and compare two widely
used fitting codes (GALFIT and GIM2D) for fitting single-component Sersic
models to the light profiles of both simulated and real galaxy data. We find
that fitting accuracy depends sensitively on galaxy profile shape. Exponential
disks are well fit with Sersic models and have small measurement errors,
whereas fits to de Vaucouleurs profiles show larger uncertainties owing to the
large amount of light at large radii. We find that both codes provide reliable
fits and little systematic error, when the effective surface brightness is
above that of the sky. Moreover, both codes return errors that significantly
underestimate the true fitting uncertainties, which are best estimated with
simulations. We find that GIM2D suffers significant systematic errors for
spheroids with close companions owing to the difficulty of effectively masking
out neighboring galaxy light; there appears to be no work around to this
important systematic in GIM2D's current implementation. While this crowding
error affects only a small fraction of galaxies in GEMS, it must be accounted
for in the analysis of deeper cosmological images or of more crowded fields
with GIM2D. In contrast, GALFIT results are robust to the presence of neighbors
because it can simultaneously fit the profiles of multiple companions thereby
deblending their effect on the fit to the galaxy of interest. We find GALFIT's
robustness to nearby companions and factor of >~20 faster runtime speed are
important advantages over GIM2D for analyzing large HST/ACS datasets. Finally
we include our final catalog of fit results for all 41,495 objects detected in
GEMS.Comment: Accepted for publication in ApJS October 2007, v172n2; 25 pages, 16
Figures, 9 Tables; for hi-resolution version, see
http://www.mpia.de/homes/bhaeussl/galaxy_fitting.pdf. For results, catalogues
and files for code-testing, see http://www.mpia.de/GEMS/fitting_paper.htm
GEMS: The Size Evolution of Disk Galaxies
We combine HST imaging from the GEMS survey with photometric redshifts from
COMBO-17 to explore the evolution of disk-dominated galaxies since z<1.1. The
sample is comprised of all GEMS galaxies with Sersic indices n<2.5, derived
from fits to the galaxy images. We account fully for selection effects through
careful analysis of image simulations; we are limited by the depth of the
redshift and HST data to the study of galaxies with absolute magnitudes
M(V)10. We find strong evolution in
the magnitude-size scaling relation for galaxies with M(V)<-20, corresponding
to a brightening of 1 mag per sqarcsec in rest-frame V-band by z=1. Yet, disks
at a given absolute magnitude are bluer and have lower stellar mass-to-light
ratios at z=1 than at the present day. As a result, our findings indicate weak
or no evolution in the relation between stellar mass and effective disk size
for galaxies with log(M)>10 over the same time interval. This is strongly
inconsistent with the most naive theoretical expectation, in which disk size
scales in proportion to the halo virial radius, which would predict that disks
are a factor of two denser at fixed mass at z=1. The lack of evolution in the
stellar mass-size relation is consistent with an ``inside-out'' growth of
galaxy disks on average (galaxies increasing in size as they grow more
massive), although we cannot rule out more complex evolutionary scenarios.Comment: 22 pages, 16 figures, submitted to Ap
An Explanation for the Observed Weak Size Evolution of Disk Galaxies
Surveys of distant galaxies with the Hubble Space Telescope and from the
ground have shown that there is only mild evolution in the relationship between
radial size and stellar mass for galactic disks from z~1 to the present day.
Using a sample of nearby disk-dominated galaxies from the Sloan Digital Sky
Survey (SDSS), and high redshift data from the GEMS (Galaxy Evolution from
Morphology and SEDs) survey, we investigate whether this result is consistent
with theoretical expectations within the hierarchical paradigm of structure
formation. The relationship between virial radius and mass for dark matter
halos in the LCDM model evolves by about a factor of two over this interval.
However, N-body simulations have shown that halos of a given mass have less
centrally concentrated mass profiles at high redshift. When we compute the
expected disk size-stellar mass distribution, accounting for this evolution in
the internal structure of dark matter halos and the adiabatic contraction of
the dark matter by the self-gravity of the collapsing baryons, we find that the
predicted evolution in the mean size at fixed stellar mass since z~1 is about
15-20 percent, in good agreement with the observational constraints from GEMS.
At redshift z~2, the model predicts that disks at fixed stellar mass were on
average only 60% as large as they are today. Similarly, we predict that the
rotation velocity at a given stellar mass (essentially the zero-point of the
Tully-Fisher relation) is only about 10 percent larger at z~1 (20 percent at
z~2) than at the present day.Comment: 13 pages, 6 figures, accepted for publication in ApJ. Revised in
response to referee's comments to improve clariry. Results are unchange
GEMS: Galaxy Evolution from Morphologies and SEDs
GEMS, Galaxy Evolution from Morphologies and SEDs, is a large-area (800
arcmin2) two-color (F606W and F850LP) imaging survey with the Advanced Camera
for Surveys on HST. Centered on the Chandra Deep Field South, it covers an area
of ~28'x28', or about 120 Hubble Deep Field areas, to a depth of
m_AB(F606W)=28.3 (5sigma and m_AB(F850LP)=27.1 (5sigma) for compact sources. In
its central ~1/4, GEMS incorporates ACS imaging from the GOODS project.
Focusing on the redshift range 0.2<=z<=1.1, GEMS provides morphologies and
structural parameters for nearly 10,000 galaxies where redshift estimates,
luminosities and SEDs exist from COMBO-17. At the same time, GEMS contains
detectable host galaxy images for several hundred faint AGN. This paper
provides an overview of the science goals, the experiment design, the data
reduction and the science analysis plan for GEMS.Comment: 24 pages, TeX with 6 eps Figures; to appear in ApJ Supplement. Low
resolution figures only. Full resolution at
http://zwicky.as.arizona.edu/~rix/Misc/GEMS.ps.g
A weak lensing estimate from GEMS of the virial to stellar mass ratio in massive galaxies to z~0.8
We present constraints on the evolution of the virial to stellar mass ratio
of galaxies with high stellar masses in the redshift range 0.2<z<0.8, by
comparing weak lensing measurements of virial mass M_vir to estimates of
stellar mass M_star from COMBO-17. For a complete sample of galaxies with
log(M_star/ M_\odot) > 10.5, where the majority show an early-type morphology,
we find that the virial mass to stellar mass ratio is given by M_vir/M_star =
53^{+13}_{-16}. Assuming a baryon fraction from the concordance cosmology, this
corresponds to a stellar fraction of baryons in massive galaxies of
Omega_b^*/\Omega_b = 0.10 +/- 0.03. Analysing the galaxy sample in different
redshift slices, we find little or no evolution in the virial to stellar mass
ratio, and place an upper limit of ~2.5 on the growth of massive galaxies
through the conversion of gas into stars from z=0.8 to the present day.Comment: 5 pages, 2 figures, to appear in MNRAS Letters. Version includes
referee comment
GEMS Imaging of Red Sequence Galaxies at z~0.7: Dusty or Old?
We have used the 30'x30' Hubble Space Telescope image mosaic from the Galaxy
Evolution from Morphology and SEDs (GEMS) project in conjunction with the
COMBO-17 deep photometric redshift survey to define a sample of nearly 1500
galaxies with 0.65 < z < 0.75. With this sample, we can study the distribution
of rest-frame V-band morphologies more than 6 Gyr ago, without differential
bandpass shifting and surface brightness dimming across this narrow redshift
slice. Focusing on red-sequence galaxies at z ~ 0.7, we find that 85% of their
combined rest-frame V-band luminosity density comes from visually-classified
E/S0/Sa galaxies (at V-band magnitudes brighter than -19.5). Similar results
are obtained if automated classifiers are used. This fraction is identical to
that found at the present day, and is biased by less than 10% by large scale
structure and the morphology-density relation. Under the assumption that
peculiar and edge-on disk galaxies are red by virtue of their dust content, we
find that less than 13% of the total rest-frame V-band luminosity of the z ~
0.7 red galaxy population is from dusty galaxies.Comment: ApJL, in press. For a version of this paper with a full-resolution
figure visit http://www.mpia-hd.mpg.de/homes/bell/res.html The GEMS
collaboration website is http://www.mpia-hd.mpg.de/GEMS/gems.htm Added
discussion of the implications of our results for hierarchical and monolithic
formation scenarios for early-type galaxie
History of Galaxy Interactions and their Impact on Star Formation over the Last 7 Gyr from GEMS
We perform a comprehensive estimate of the frequency of galaxy mergers and
their impact on star formation over z~0.24--0.80 (lookback time T_b~3--7 Gyr)
using 3698 (M*>=1e9 Msun) galaxies with GEMS HST, COMBO-17, and Spitzer data.
Our results are: (1) Among 790 high mass (M*>=2.5e10 Msun) galaxies, the
visually-based merger fraction over z~0.24--0.80, ranges from 9%+-5% to 8%+-2%.
Lower limits on the major and minor merger fractions over this interval range
from 1.1% to 3.5%, and 3.6% to 7.5%, respectively. This is the first
approximate empirical estimate of the frequency of minor mergers at z<1. For a
visibility timescale of ~0.5 Gyr, it follows that over T_b~3--7 Gyr, ~68% of
high mass systems have undergone a merger of mass ratio >1/10, with ~16%, 45%,
and 7% of these corresponding respectively to major, minor, and ambiguous
`major or minor' mergers. The mean merger rate is a few x 1e-4 Gyr-1 Mpc-3. (2)
We compare the empirical merger fraction and rate for high mass galaxies to a
suite of Lambda CDM-based models: halo occupation distribution models,
semi-analytic models, and hydrodynamic SPH simulations. We find qualitative
agreement between observations and models such that the (major+minor) merger
fraction or rate from different models bracket the observations, and show a
factor of five dispersion. Near-future improvements can now start to rule out
certain merger scenarios. (3) Among ~3698 M*>=1e9 Msun galaxies, we find that
the mean SFR of visibly merging systems is only modestly enhanced compared to
non-interacting galaxies over z~0.24--0.80. Visibly merging systems only
account for less than 30% of the cosmic SFR density over T_b~3--7 Gyr. This
suggests that the behavior of the cosmic SFR density over the last 7 Gyr is
predominantly shaped by non-interacting galaxies.Comment: Accepted for Publication in the Astrophysical Journal. 17 pages of
text, 21 figures, 3 tables. Uses emulateapj5.st
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