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 $\sim$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 ($\sim$ 3$''$) and sensitive 1.3 mm continuum, cyanogen (CN) and vinyl cyanide (C$_2$H$_3$CN) 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 $\times$ 10$^{-2}$ M$_\odot$ yr$^{-1}$. The C$_2$H$_3$CN traces an east-west rotating molecular envelope that surrounds either a single obscured (proto)star with a kinematic mass of 40 M$_{\odot}$ or a small central cluster of B-type stars and that is associated with a compact high velocity bipolar outflow traced by H$_2$O 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 ($\sim$ 10$^{-2}$ -- 10$^{-4}$), 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 12326−-6245 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 12326$-$6245 using Band 6 sensitive and high angular resolution ($\sim$0.2$"$) 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 $\sim$700 yrs, and 10$^{48}$ erg, respectively. Taking into account the recently reported explosive outflows together with IRAS 12326$-$6245, 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 z$\sim$2, an epoch 3 Gyr after the Big Bang. Their age and formation processes have now been explained by an improved generation of galaxy formation models where they form rapidly at z$\sim$3-4, consistent with the typical masses and ages derived from their observations. Deeper surveys have now reported evidence for populations of massive, quiescent galaxies at even higher redshifts and earlier times, however the evidence for their existence, and redshift, has relied entirely on coarsely sampled photometry. These early massive, quiescent galaxies are not predicted by the latest generation of theoretical models. Here, we report the spectroscopic confirmation of one of these galaxies at redshift z=3.717 with a stellar mass of 1.7$\times$10$^{11}$ M$_\odot$ 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