547 research outputs found

    Obamacare: The Birds Still Sing as Freedom Erodes

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    The article discusses the impact of the U.S. health care bill signed into law by U.S. President Barack Obama in 2010. When provisions begin to take effect in 2014, government spending will reportedly increase such that it would expand the deficit and Americans\u27 freedom will be reduced. The new system turns health insurance companies into government agents with the government determining the premiums, benefits and types of policies to be issued

    Increased leukotriene C 4 and vasogenic edema surrounding brain tumors in humans

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    Leukotrines are pharmacologically active compounds that promote vascular permeability. In this study we sought to determine whether tissue leukotrieneā€“like immunoreactivity was increased in intracranial tumors associated with peritumoral edema. In 20 patients undergoing craniotomy tissue specimens were immediately frozen after removal and tissue leukotriene C 4 levels were determined by radioimmunoassay. An index of peritumoral edema was estimated from preoperative contrast-enhanced computed tomographic scans. There was a significant correlation between brain edema and tissue leukotriene levels ( p < 0.003). Metastatic tumors (n = 8) had the highest leukotriene C 4 level at 13.8 Ā± 8.5 pg/mg tissue (mean Ā± SE) and the highest index of edema 5.7 Ā± 1.8. The mean leukotriene C 4 level in the gliomas (n + 5) ws 6.2 Ā± 2.3 pg/mg tissue and the edema index was 2.1 Ā± 0.6. There was no edema and no neoplasma in he temporal lobes removed for seizure (n + 2), and their level of leukotriene C 4 was 0.4 Ā± 0.1 pg/mg tissue. The formation of leukotriene C 4 is stimulated by intracranial tumors. Leukotrienes increase bloodā€“brain barrier permeability and may be important in the formation of vasogenic edema surrounding tumors.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/50315/1/410190613_ftp.pd

    A multi-parametric flow cytometric assay to analyze DNAā€“protein interactions

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    Interactions between DNA and transcription factors (TFs) guide cellular function and development, yet the complexities of gene regulation are still far from being understood. Such understanding is limited by a paucity of techniques with which to probe DNAā€“protein interactions. We have devised magnetic protein immobilization on enhancer DNA (MagPIE), a simple, rapid, multi-parametric assay using flow cytometric immunofluorescence to reveal interactions among TFs, chromatin structure and DNA. In MagPIE, synthesized DNA is bound to magnetic beads, which are then incubated with nuclear lysate, permitting sequence-specific binding by TFs, histones and methylation by native lysate factors that can be optionally inhibited with small molecules. Lysate proteinā€“DNA binding is monitored by flow cytometric immunofluorescence, which allows for accurate comparative measurement of TF-DNA affinity. Combinatorial fluorescent staining allows simultaneous analysis of sequence-specific TF-DNA interaction and chromatin modification. MagPIE provides a simple and robust method to analyze complex epigenetic interactions in vitro

    The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars IV. Unveiling the Embedded Intermediate-Mass Protostar and Disk within OMC2-FIR3/HOPS-370

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    We present ALMA (0.87~mm and 1.3~mm) and VLA (9~mm) observations toward the candidate intermediate-mass protostar OMC2-FIR3 (HOPS-370; Lbol_{bol}~314~LāŠ™_{\odot}) at āˆ¼\sim0.1" (40~au) resolution for the continuum emission and ~0.25" (100 au) resolution of nine molecular lines. The dust continuum observed with ALMA at 0.87~mm and 1.3~mm resolve a near edge-on disk toward HOPS-370 with an apparent radius of ~100 au. The VLA observations detect both the disk in dust continuum and free-free emission extended along the jet direction. The ALMA observations of molecular lines (H2_2CO, SO, CH3_3OH, 13^{13}CO, C18^{18}O, NS, and H13^{13}CN) reveal rotation of the apparent disk surrounding HOPS-370 orthogonal to the jet/outflow direction. We fit radiative transfer models to both the dust continuum structure of the disk and molecular line kinematics of the inner envelope and disk for the H2_2CO, CH3_3OH, NS, and SO lines. The central protostar mass is determined to be āˆ¼\sim2.5 M_sun with a disk radius of āˆ¼\sim94~au, when fit using combinations of the H2_2CO, CH3_3OH, NS, and SO lines, consistent with an intermediate-mass protostar. Modeling of the dust continuum and spectral energy distribution (SED) yields a disk mass of 0.035~MāŠ™_{\odot} (inferred dust+gas) and a dust disk radius of 62~au, thus the dust disk may have a smaller radius than the gas disk, similar to Class II disks. In order to explain the observed luminosity with the measured protostar mass, HOPS-370 must be accreting at a rate between 1.7 and 3.2Ɨ\times10āˆ’5^{-5}~MāŠ™_{\odot}~yrāˆ’1^{-1}.Comment: Accepted to ApJ; 51 pages, 12 Figures, 7 Table
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