Self-reported symptoms and managment by midwestern breast cancer survivors

Lymphedema (LE) is a life-long potential consequence of breast cancer treatment that may affect quality of life of breast cancer survivors in long-term survivorship. Previous studies reported that about 2 million women living with breast cancer are at a lifetime risk for LE development. Information from self-reported lymphedema symptoms and its management will provide potential early detection and intervention to manage LE. The purposes of this study were: To report the frequency of occurrence of commonly self- reported LE symptoms following breast cancer diagnosis and treatment. To find the most commonly reported self-management actions taken for the five LE symptoms.Research supported by NIH/NINR NR05342/NR010293, University of Missouri PRIME funds, and Ellis Fischel Cancer Center research funds

A second planet transiting LTT 1445A and a determination of the masses of both worlds

K.H. acknowledges support from STFC grant ST/R000824/1.LTT 1445 is a hierarchical triple M-dwarf star system located at a distance of 6.86 pc. The primary star LTT 1445A (0.257 M⊙) is known to host the transiting planet LTT 1445Ab with an orbital period of 5.36 days, making it the second-closest known transiting exoplanet system, and the closest one for which the host is an M dwarf. Using Transiting Exoplanet Survey Satellite data, we present the discovery of a second planet in the LTT 1445 system, with an orbital period of 3.12 days. We combine radial-velocity measurements obtained from the five spectrographs, Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations, High Accuracy Radial Velocity Planet Searcher, High-Resolution Echelle Spectrometer, MAROON-X, and Planet Finder Spectrograph to establish that the new world also orbits LTT 1445A. We determine the mass and radius of LTT 1445Ab to be 2.87 ± 0.25 M⊕ and 1.304-0.060+0.067 R⊕, consistent with an Earth-like composition. For the newly discovered LTT 1445Ac, we measure a mass of 1.54-0.19+0.20 M⊕ and a minimum radius of 1.15 R⊕, but we cannot determine the radius directly as the signal-to-noise ratio of our light curve permits both grazing and nongrazing configurations. Using MEarth photometry and ground-based spectroscopy, we establish that star C (0.161 M⊙) is likely the source of the 1.4 day rotation period, and star B (0.215 M⊙) has a likely rotation period of 6.7 days. We estimate a probable rotation period of 85 days for LTT 1445A. Thus, this triple M-dwarf system appears to be in a special evolutionary stage where the most massive M dwarf has spun down, the intermediate mass M dwarf is in the process of spinning down, while the least massive stellar component has not yet begun to spin down.Publisher PDFPeer reviewe

Finishing the euchromatic sequence of the human genome

The sequence of the human genome encodes the genetic instructions for human physiology, as well as rich information about human evolution. In 2001, the International Human Genome Sequencing Consortium reported a draft sequence of the euchromatic portion of the human genome. Since then, the international collaboration has worked to convert this draft into a genome sequence with high accuracy and nearly complete coverage. Here, we report the result of this finishing process. The current genome sequence (Build 35) contains 2.85 billion nucleotides interrupted by only 341 gaps. It covers ∼99% of the euchromatic genome and is accurate to an error rate of ∼1 event per 100,000 bases. Many of the remaining euchromatic gaps are associated with segmental duplications and will require focused work with new methods. The near-complete sequence, the first for a vertebrate, greatly improves the precision of biological analyses of the human genome including studies of gene number, birth and death. Notably, the human enome seems to encode only 20,000-25,000 protein-coding genes. The genome sequence reported here should serve as a firm foundation for biomedical research in the decades ahead

Valency conversion in the type 1 fimbrial adhesin of Escherichia coli

FimH protein is a lectin-like adhesive subunit of type 1, or mannose-sensitive, fimbriae that are found on the surface of most Escherichia coli strains. All naturally occurring FimH variants demonstrate a conserved mannotriose-specific (i.e. multivalent) binding. Here, we demonstrate that replacement of residues 185-279 within the FimH pilin domain with a corresponding segment of the type 1C fimbrial adhesin FocH leads to a loss of the multivalent mannotriose-specific binding property accompanied by the acquisition of a distinct monomannose-specific (i.e. monovalent) binding capability. Bacteria expressing the monovalent hybrid adhesins were capable of binding strongly to uroepithelial tissue culture cells and guinea pig erythrocytes. They could not, however, agglutinate yeast or bind human buccal cells functions readily accomplished by the E. coli-expressing mannotriose-specific FimH variants. Based on the relative potency of inhibiting compounds of different structures, the receptor binding site within monovalent FimH-FocH adhesin has an extended structure with an overall configuration similar to that within the multivalent FimH of natural origin. The monomannose-only specific phenotype could also be invoked by a single point mutation, E89K, located within the lectin domain of FimH, but distant from the receptor binding site. The structural alterations influence the receptor-binding valency of the FimH adhesin via distal effects on the combining pocket, obviously by affecting the FimH quaternary structure

Curiosity meets the Gediz Vallis Ridge: a remnant of a late-stage debris-flow dominated fan

International audienceRecent studies using HiRISE and CTX imagery show that fan-shaped deposits are widespread across Mars and likely formed during the Hesperian and Amazonian periods. Remote imagery and topographic analysis suggest that they may have been produced by both fluvial and debris flow processes and are generally distinct from deltaic deposits such as those in Jezero. Curiosity-based observations of the deeply eroded deposits of the Gediz Vallis Ridge (GVR), lying at the base of Mt. Sharp, now provide our first cross-sectional observation of a Martian fan, revealing episodic deposition by debris flows and reworking by fluvial processes. The fan was deposited on the Stimson formation, a pediment-mantling lithified aeolian deposit. Above the Stimson is a discontinuous fine-grained (≤ gravel size) basal unit with decimeter-scale bedding that is parallel to top of the Stimson. The unit reaches a maximum observable thickness of 15m and is unconformably onlapped by stratified gravel and boulder deposits. Discontinuous layering within these deposits ranges in thickness from 0.25 to 3 m and exhibits a mean slope of 7% oriented parallel to the ridge axis, much gentler than the slope of the basal contact. At progressively higher elevations, five depositional packages are exposed. Each package is composed two facies whose frequency and lateral extent differ: 1) a light toned typically matrix-supported coarse facies with scattered erosionally resistant dark toned gravel and boulders, and 2) a dark-toned typically clast-supported gravel and boulder facies. Grainsize analysis of Chemcam data indicates similar median grainsizes (170-190 mm) in light- and dark toned facies with isolated 1-3m boulders scattered throughout. The light-toned strata appear to be debris flow deposits. The dark toned strata are interpreted to be fluvial, probably derived from surface runoff that concentrated dark stones from the light toned unit into channels and sheetflood deposits while destroying the weaker light toned sediment during transport. The GVR is an erosional remnant of a fan that may have built 10 km downslope, likely in the late Hesperian or early Amazonian. Stratigraphic differences in the five packages suggest significant changes in the magnitude and frequency of surface runoff, but with a supply of meter scale boulders throughout fan evolution