2,953 research outputs found
Maternal Health Outcomes and Male Partner Involvement Among HIV Infected Women in Rural South Africa
Introduction This study aimed to investigate the association between Male Partner Involvement (MPI) and maternal health outcomes among women attending Prevention of Mother-to-Child Transmission of HIV (PMTCT) services in rural South Africa. The association between Male Partner Participation in the main study (MPP) and maternal health outcomes among these women was also investigated. Methods The study utilized data collected from 535 HIV infected women in a randomized controlled trial between 2015 and 2016. Maternal health outcome data (delivery mode, pregnancy systolic and diastolic blood pressure, pregnancy body mass index, pregnancy CD4 count, and pregnancy viral load) were collected from the women's antenatal record forms accessed from the primary healthcare facilities. Bivariate and multivariable logistic regression models were used to estimate the association between socio-demographic characteristics of the women, MPI, and MPP with maternal health outcomes. Results The mean age of the women was 29.03 years (SD = 5.89). No significant associations were found between MPI and any of the maternal health outcomes contrary to what was hypothesized. Both the bivariate and multivariate analysis indicated a significant association between MPP and higher pregnancy viral load, contrary to the study hypothesis. Insignificant associations were found between MPP and both pregnancy CD4 count and pregnancy blood pressure. The only significant association between maternal health outcomes and socio-demographic characteristics, was between educational attainment and higher pregnancy CD4 count in both the bivariate and multivariate analysis. Conclusion for Practice The study showed no significant support for MPI in improving maternal health outcomes of women in PMTCT in rural South Africa. Future studies should include additional maternal health outcomes for investigation
Monitoring the Large Proper Motions of Radio Sources in the Orion BN/KL Region
We present absolute astrometry of four radio sources in the
Becklin-Neugebauer/Kleinman-Low (BN/KL) region, derived from archival data
(taken in 1991, 1995, and 2000) as well as from new observations (taken in
2006). All data consist of 3.6 cm continuum emission and were taken with the
Very Large Array in its highest angular resolution A configuration. We confirm
the large proper motions of the BN object, the radio source I (GMR I) and the
radio counterpart of the infrared source n (Orion-n), with values from 15 to 26
km/s. The three sources are receding from a point between them from where they
seem to have been ejected about 500 years ago, probably via the disintegration
of a multiple stellar system. We present simulations of very compact stellar
groups that provide a plausible dynamical scenario for the observations. The
radio source Orion-n appeared as a double in the first three epochs, but as
single in 2006. We discuss this morphological change. The fourth source in the
region, GMR D, shows no statistically significant proper motions. We also
present new, accurate relative astrometry between BN and radio source I that
restrict possible dynamical scenarios for the region. During the 2006
observations, the radio source GMR A, located about 1' to the NW of the BN/KL
region, exhibited an increase in its flux density of a factor of ~3.5 over a
timescale of one hour. This rapid variability at cm wavelengths is similar to
that previously found during a flare at millimeter wavelengths that took place
in 2003.Comment: Accepted for publication in Ap
Proper Motions of the Radio Source Orion MR, Formerly Known as Orion n, and New Sources with Large Proper Motions in Orion BN/KL
The infrared source known as Orion n was detected in 1980 with observations
made with the 3.8-m United Kingdom Infrared Telescope. About two decades later,
sensitive observations made with the Very Large Array revealed the presence of
a mJy double radio source apparently coincident in position with the infrared
source n. The radio source was assumed to be the counterpart of the infrared
source. However, over the years it has been concluded that the radio source
shows large proper motions to the south while the infrared source n is
stationary. Here we reanalyze the proper motions of the radio source adding
both older and newer VLA observations than previously used. We confirm the
proper motions of the radio source that at present no longer coincides
positionally with the infrared source. The solution to this problem is, most
probably, that the infrared source n and the radio source are not the same
object: the infrared source is a stationary object in the region while the
radio counterpart is moving as a result of the explosion that took place in
this region some 500 years ago and that expelled large amounts of molecular gas
as well as several compact sources. Considering the paper where it was first
reported, we refer to this double radio source as Orion MR.
In addition, we use these new observations to fully confirm the large proper
motions of the sources IRc23 and Zapata 11. Together with sources BN, I, Orion
MR, and x, there are at least six compact sources that recede from a point in
common in Orion BN/KL. However, IRc23 is peculiar in that its ejection age
appears to be only 300 years. The relatively large number of sources
rules out as a possible mechanism the classic three-body scenario since then
only two escaping bodies are expected: a tight binary plus the third star
involved in the encounter.Comment: 14 pages, 7 figures, to appear in The Astrophysical Journa
Forming an Early O-type Star Through Gas Accretion?
We present high angular resolution ( 3) and sensitive 1.3 mm
continuum, cyanogen (CN) and vinyl cyanide (CHCN) line observations
made with the Submillimeter Array (SMA) toward one of most highly obscured
objects of the W51 IRS2 region, W51 North. We find that the CN line exhibits a
pronounced inverse P-Cygni profile indicating that the molecular gas is
infalling inwards this object with a mass accretion rate between 4 and 7
10 M yr. The CHCN traces an east-west
rotating molecular envelope that surrounds either a single obscured (proto)star
with a kinematic mass of 40 M or a small central cluster of B-type
stars and that is associated with a compact high velocity bipolar outflow
traced by HO masers and SiO molecular emission. We thus confirm that the
W51 North region is part of the growing list of young massive star forming
regions that have been associated with infalling motions and with large mass
accretion rates ( 10 -- 10), strengthening the evidence for
massive stars forming with very high accretion rates sufficient to quench the
formation of an UCHII region.Comment: Accepted by Astronomy and Astrophysics Letter
One, Two, Three ... An Explosive Outflow in IRAS 123266245 revealed by ALMA
In the last years there has been a substantial increase in the number of the
reported massive and luminous star-forming regions with related explosive
outflows thanks to the superb sensitivity and angular resolution provided by
the new radio, infrared, and optical facilities. Here, we report one more
explosive outflow related with the massive and bright star-forming region IRAS
123266245 using Band 6 sensitive and high angular resolution (0.2)
Atacama Large Millimeter/Submillimeter Array (ALMA) observations. We find over
10 molecular and collimated well-defined streamers, with Hubble-Lemaitre like
expansion motions, and pointing right to the center of a dusty and molecular
shell (reported for the first time here) localized in the northern part of the
UCHII region known as G301.1A. The estimated kinematic age, and energy for the
explosion are 700 yrs, and 10 erg, respectively. Taking into
account the recently reported explosive outflows together with IRAS
123266245, we estimate an event rate of once every 90 yr in our Galaxy,
similar to the formation rate of massive stars.Comment: Accepted to The Astrophysical Journal Letter
A Qualitative Exploration of the Meaning and Understanding of Male Partner Involvement in Pregnancy-Related Care Among Men in Rural South Africa
Male partner involvement (MPI) during antenatal care has been promoted as an effective intervention to improve maternal and newborn health outcomes. Although MPI is commonly defined as men attending antenatal clinic visits with their female partner, few men attend antenatal clinic visits in rural communities in the province of Mpumalanga, South Africa. The study aimed to qualitatively explore the meaning and understanding of MPI as perceived by men visiting primary health care clinics in rural communities in Mpumalanga. Six focus groups discussions (n = 53) were conducted, digitally recorded, simultaneously transcribed, and translated verbatim into English. Data were analyzed using thematic content analysis. Perceptions of male roles during and after pregnancy differed among men. Male involvement was understood as giving instrumental support to female partners through financial help, helping out with physical tasks, and providing emotional support. Accompanying female partners to the clinic was also viewed as partner support, including behaviors such as holding a spot for her in the clinic queues. Community attitudes, traditional beliefs, and negative experiences in health facilities were barriers for MPI. This study provides support for concerted efforts to work with both men and women within the cultural context to explore the important roles of all members of the family in working together to provide the best possible health outcomes for mother and infant. In particular, future interventions should focus on making antenatal care services more responsive to male partners, and improving male partner accessibility in health care facilities
A massive, quiescent galaxy at redshift of z=3.717
In the early Universe finding massive galaxies that have stopped forming
stars present an observational challenge as their rest-frame ultraviolet
emission is negligible and they can only be reliably identified by extremely
deep near-infrared surveys. These have revealed the presence of massive,
quiescent early-type galaxies appearing in the universe as early as z2,
an epoch 3 Gyr after the Big Bang. Their age and formation processes have now
been explained by an improved generation of galaxy formation models where they
form rapidly at z3-4, consistent with the typical masses and ages derived
from their observations. Deeper surveys have now reported evidence for
populations of massive, quiescent galaxies at even higher redshifts and earlier
times, however the evidence for their existence, and redshift, has relied
entirely on coarsely sampled photometry. These early massive, quiescent
galaxies are not predicted by the latest generation of theoretical models.
Here, we report the spectroscopic confirmation of one of these galaxies at
redshift z=3.717 with a stellar mass of 1.710 M whose
absorption line spectrum shows no current star-formation and which has a
derived age of nearly half the age of the Universe at this redshift. The
observations demonstrates that the galaxy must have quickly formed the majority
of its stars within the first billion years of cosmic history in an extreme and
short starburst. This ancestral event is similar to those starting to be found
by sub-mm wavelength surveys pointing to a possible connection between these
two populations. Early formation of such massive systems is likely to require
significant revisions to our picture of early galaxy assembly.Comment: 6 pages, 7 figures. This is the final preprint corresponding closely
to the published version. Uploaded 6 months after publication in accordance
with Nature polic
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