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Mamon, Mark Anthony C.,Ramos, Gliceria B. Korean Society of Animal Sciences and Technology 2017 한국축산학회지 Vol.59 No.4
Background: Selenium is one of the trace minerals whose deficiency is known to lead to complications of female reproduction. The identified gaps in researches regarding selenium and pregnancy include optimizing the dosage of selenium supplementation, timing of supplementation, finding the best form and type of selenium, and selenium administration combined with other antioxidants. Hence, this study was conceptualized to address one of the identified gaps, that is, to find out the best timing of selenium administration around the time of pregnancy. Specifically, this study aimed to assess the effects of maternal Selenium-supplementation, administered at various stages of periconception period, on murine blastocyst morphology, percent occurrence of good quality blastocysts, and implantation status. Methods: ICR female mice were randomly assigned into the unsupplemented group (Group I) receiving basal diet without selenium, and treatment groups given with $3.0{\mu}g$ selenium-supplement per day during pregestation only (Group II), pregestation-throughout-gestation (Group III) and gestation only (Group IV). Both blastocyst morphology and implantation status were assessed. Results: The morphometric measurements of blastocysts appeared to be unaffected by selenium-supplementation at different stages of periconception. Selenium-supplementation at pregestation only (Group II) and gestation only (Group IV) produced higher percent occurrence of good quality blastocysts and lower percent pre-implantation loss than Group III. Among all the treatment groups, Group III (Selenium-supplementation during pregestation-to-gestation) yielded the lowest quality blastocysts and highest percent pre-implantation loss. Conclusion: Maternal selenium-supplementation during pregestation and gestation stages of the periconception period yielded a high percent occurrence of good quality blastocysts and pre-implantation success.
Revisiting the Bulge-Halo Conspiracy. I. Dependence on Galaxy Properties and Halo Mass
Shankar, Francesco,Sonnenfeld, Alessandro,Mamon, Gary A.,Chae, Kyu-Hyun,Gavazzi, Raphael,Treu, Tommaso,Diemer, Benedikt,Nipoti, Carlo,Buchan, Stewart,Bernardi, Mariangela,Sheth, Ravi,Huertas-Company, American Astronomical Society 2017 The Astrophysical Journal Vol.840 No.1
<P>We carry out a systematic investigation of the total mass density profile of massive (log M-star / M-circle dot greater than or similar to 11.3) early-type galaxies and its dependence on galactic properties and host halo mass with the aid of a variety of lensing/dynamical data and large mock galaxy catalogs. The latter are produced via semi-empirical models that, by design, are based on just a few basic input assumptions. Galaxies. with measured stellar masses, effective radii, and Sersic indices, are assigned, via abundance matching relations, host dark matter halos characterized by a typical Lambda CDM profile. Our main results are as follows. (1) In line with observational evidence, our semi-empirical models naturally predict that the total, mass-weighted density slope at the effective radius gamma' is not universal, steepening for more compact and/or massive galaxies, but flattening with increasing host halo mass. (2) Models characterized by a Salpeter or variable initial mass function (IMF) and uncontracted dark matter profiles are in good agreement with the data, while a Chabrier IMF and/or adiabatic contractions/expansions of the dark matter halos are highly disfavored. (3) Currently available data on the mass density profiles of very massive galaxies (log M-star / M-circle dot greater than or similar to 12), with M-halo greater than or similar to 3 x 10(14) M-circle dot, favor instead models with a stellar profile flatter than a Sersic one in the very inner regions (r less than or similar to 3-5 kpc), and a cored NFW or Einasto dark matter profile with median halo concentration a factor of similar to 2 or less than or similar to 1.3, respectively, higher than those typically predicted by N-body numerical simulations.</P>