The effect of maternal weight on pregnancy outcome

Neðst á síðunni er hægt að nálgast greinina í heild sinni með því að smella á hlekkinn Skoða/Opna(view/open)OBJECTIVE: To examine the frequency of adverse outcome during pregnancy and delivery and neonatal complications among normal weight, overweight and obese women at the beginning of pregnancy. MATERIAL AND METHODS: The study is a retrospective cohort study of 600 women, divided in 3 groups on the basis of maternal body mass index (BMI) at the beginning of pregnancy; 300 normal weight women (BMI 19.0-24.9), 150 overweight women (BMI 25.0-29.9) and 150 obese women (BMI ≥ 30). Maternal and neonatal complications were compared between groups. RESULTS: Obese women have a significantly increased risk of; essential hypertension prior to pregnancy (p<0.001), developing gestational hypertension (p=0.03), pre-eclampsia (p=0.007), gestational diabetes (p<0.001), musculoskeletal symptoms (p=0.04), requiring induction of labour (pp=0.006) and being delivered by cesarean section (p<0.001), both emergent (pp=0.012) and elective (pp=0.008) compared to mothers of normal weight and overweight. Neonates of obese mothers have significantly higher birth weight (pp=0.004), larger head circumference (p<0.001) and are more likely to require admission to neonatal ward compared with neonates of normal weight and overweight mothers (pp=0.004). CONCLUSIONS: Obesity carries a significant risk to maternal and neonatal health. During pregnancy maternal complications are increased causing adverse effects for both mother and infant. Women of reproductive age need counselling regarding the adverse effects of obesity on pregnancy outcome.Tilgangur: Að kanna tíðni fylgikvilla á meðgöngu, í fæðingu og hjá nýburum kvenna í kjörþyngd, of þungra og of feitra við upphaf meðgöngu. Þátttakendur og aðferðir: Rannsóknin er afturskyggn og tilfellaviðmiðuð. Upplýsingum um þyngd við upphaf meðgöngu var safnað hjá 600 konum; þar af voru 300 í kjörþyngd (þyngdarstuðull (ÞS) 19,0-24,9), 150 of þungar (ÞS 25,0-29,9) og 150 of feitar (ÞS ³30). Tíðni fylgikvilla var borin saman milli hópanna. Niðurstöður: Of feitar konur eru líklegri til að hafa langvinnan háþrýsting (p<0,001) fyrir þungun, fá meðgönguháþrýsting (p=0,03), meðgöngueitrun (p=0,007), meðgöngusykursýki (p<0,001), einkenni frá stoðkerfi (p=0,04), að framkalla þurfi fæðingu (p=0,006) og að fæða með keisaraskurði (p<0,001), bæði bráða- (p=0,012) og valkeisaraskurði (p=0,008), samanborið við mæður í kjörþyngd og ofþyngd. Nýburar of feitra kvenna eru þyngri (p=0,004), með stærra höfuðummál (p<0,001) og eru oftar lagðir inn á nýburagjörgæslu (p=0,004) en börn mæðra í kjörþyngd og ofþyngd. Ályktun:Offita hefur óæskileg áhrif á heilsufar verðandi mæðra og barna þeirra. Áhrifin koma fram á meðgöngu, í fæðingu og hjá börnum þeirra. Mikilvægt er að konur á barneignaraldri fái upplýsingar um hvaða áhrif offita hefur á meðgöngu, fæðingu og nýbura

Multiple sclerosis - symptoms, diagnosis and treatment

Neðst á síðunni er hægt að nálgast greinina í heild sinni með því að smella á hlekkinn View/OpenMultiple sclerosis is an inflammatory disease of the central nervous system and a common cause of disability among young people. MS is thought to be an autoimmune disease involving both inheritance and environmental factors. The disease is characterized by relapses and the symptoms and course are highly variable. The diagnosis is primarily clinical and supported by results of diagnostic studies. The importance of timely diagnosis has increased with the availability of effective treatment. The purpose of this article is to review symptoms, signs, diagnosis and treatment of multiple sclerosis.Multiple sclerosis (MS) er bólgusjúkdómur í miðtaugakerfinu og algeng orsök fötlunar hjá ungu fólki. MS er talinn vera sjálfsofnæmissjúkdómur sem tengist samspili erfða og umhverfis. Sjúkdómurinn kemur í köstum og geta einkenni og gangur hans verið margbreytilegur. Greining byggir á sjúkdómseinkennum og styðst við niðurstöður rannsókna. Mikilvægi skjótrar greiningar hefur aukist með tilkomu áhrifaríkrar meðferðar. Tilgangur þessarar greinar er að rekja algengustu einkenni, greiningu og meðferð við MS sjúkdómi

Strong Gravitational Lensing by the Super-massive cD Galaxy in Abell 3827

We have discovered strong gravitational lensing features in the core of the nearby cluster Abell 3827 by analyzing Gemini South GMOS images. The most prominent strong lensing feature is a highly-magnified, ring-shaped configuration of four images around the central cD galaxy. GMOS spectroscopic analysis puts this source at z~0.2. Located ~20" away from the central galaxy is a secondary tangential arc feature which has been identified as a background galaxy with z~0.4. We have modeled the gravitational potential of the cluster core, taking into account the mass from the cluster, the BCG and other galaxies. We derive a total mass of (2.7 +- 0.4) x 10^13 Msun within 37 h^-1 kpc. This mass is an order of magnitude larger than that derived from X-ray observations. The total mass derived from lensing data suggests that the BCG in this cluster is perhaps the most massive galaxy in the nearby Universe.Comment: Minor typo corrections introduced. Journal reference and DOI added. 5 pages, 3 figures (2 in colors), 2 table

Measurement of a Metallicity Gradient in a z=2 Galaxy: Implications for Inside-Out Assembly Histories

We present near-infrared imaging spectroscopy of the strongly-lensed z=2.00 galaxy SDSS J120601.69+514227.8 (`the Clone arc'). Using OSIRIS on the Keck 2 telescope with laser guide star adaptive optics, we achieve resolved spectroscopy with 0.20 arcsecond FWHM resolution in the diagnostic emission lines [O III], Halpha, and [N II]. The lensing magnification allows us to map the velocity and star formation from Halpha emission at a physical resolution of ~300 pc in the galaxy source plane. With an integrated star formation rate of ~50 Msun/yr, the galaxy is typical of sources similarly studied at this epoch. It is dispersion-dominated with a velocity gradient of +/- 80 km/s and average dispersion sigma = 85 km/s; the dynamical mass is 2.4 \times 10^{10} Msun within a half-light radius of 2.9 kpc. Robust detection of [N II] emission across the entire OSIRIS field of view enables us to trace the gas-phase metallicity distribution with 500 pc resolution. We find a strong radial gradient in both the [N II]/Halpha and [O III]/Halpha ratios indicating a metallicity gradient of -0.27 +/- 0.05 dex/kpc with central metallicity close to solar. We demonstrate that the gradient is seen independently in two multiple images. While the physical gradient is considerably steeper than that observed in local galaxies, in terms of the effective radius at that epoch, the gradient is similar. This suggests that subsequent growth occurs in an inside-out manner with the inner metallicity gradient diminished over time due to radial mixing and enrichment from star formation.Comment: 6 pages, 4 figures, accepted by ApJ Letter

The Dark Matter Distribution in Abell 383: Evidence for a Shallow Density Cusp from Improved Lensing, Stellar Kinematic and X-ray Data

We extend our analyses of the dark matter (DM) distribution in relaxed clusters to the case of Abell 383, a luminous X-ray cluster at z=0.189 with a dominant central galaxy and numerous strongly-lensed features. Following our earlier papers, we combine strong and weak lensing constraints secured with Hubble Space Telescope and Subaru imaging with the radial profile of the stellar velocity dispersion of the central galaxy, essential for separating the baryonic mass distribution in the cluster core. Hydrostatic mass estimates from Chandra X-ray observations further constrain the solution. These combined datasets provide nearly continuous constraints extending from 2 kpc to 1.5 Mpc in radius, allowing stringent tests of results from recent numerical simulations. Two key improvements in our data and its analysis make this the most robust case yet for a shallow slope \beta of the DM density profile \rho_DM ~ r^-\beta on small scales. First, following deep Keck spectroscopy, we have secured the stellar velocity dispersion profile to a radius of 26 kpc for the first time in a lensing cluster. Secondly, we improve our previous analysis by adopting a triaxial DM distribution and axisymmetric dynamical models. We demonstate that in this remarkably well-constrained system, the logarithmic slope of the DM density at small radii is \beta < 1.0 (95% confidence). An improved treatment of baryonic physics is necessary, but possibly insufficient, to reconcile our observations with the recent results of high-resolution simulations.Comment: Accepted to ApJ Letter

Detection of chromatic microlensing in Q 2237+0305 A

We present narrowband images of the gravitational lens system Q~2237+0305 made with the Nordic Optical Telescope in eight different filters covering the wavelength interval 3510-8130 \AA. Using point-spread function photometry fitting we have derived the difference in magnitude versus wavelength between the four images of Q~2237+0305. At $\lambda=4110$ \AA, the wavelength range covered by the Str\"omgren-v filter coincides with the position and width of the CIV emission line. This allows us to determine the existence of microlensing in the continuum and not in the emission lines for two images of the quasar. Moreover, the brightness of image A shows a significant variation with wavelength which can only be explained as consequence of chromatic microlensing. To perform a complete analysis of this chromatic event our observations were used together with Optical Gravitational Lensing Experiment light curves. Both data sets cannot be reproduced by the simple phenomenology described under the caustic crossing approximation; using more realistic representations of microlensing at high optical depth, we found solutions consistent with simple thin disk models ($r_{s}\varpropto \lambda^{4/3}$); however, other accretion disk size-wavelength relationships also lead to good solutions. New chromatic events from the ongoing narrow band photometric monitoring of Q~2237+0305 are needed to accurately constrain the physical properties of the accretion disk for this system.Comment: 9 pages, 9 figures, 2 tables. Matches ApJ published version. Some references adde

Near-Infrared K and L' Flux Ratios in Six Lensed Quasars

We examine the wavelength dependence of flux ratios for six gravitationally lensed quasars using K and L' images obtained at the Gemini North 8m telescope. We select lenses with source redshifts z_s < 2.8 so that K-band images probe rest-frame optical emission from accretion disks, while L'-band images probe rest-frame near-infrared flux emitted (in part) from the more extended surrounding torus. Since the observations correspond to different source sizes, the K and L' flux ratios are sensitive to structure on different scales and may be useful for studying small-structure in the lens galaxies. Four of the six lenses show differences between K and L' flux ratios. In HE 0435$-1223, SDSS 0246-0825, and HE 2149-2745 the differences may be attributable to known microlensing and/or intrinsic variability. In SDSS 0806+2006 the wavelength dependence is not easily attributed to known variations, and may indicate the presence of substructure. By contrast, in Q0142-100 and SBS 0909+523 the K and L' flux ratios are consistent within the uncertainties. We discuss the utility of the current data for studying chromatic effects related to microlensing, dust extinction, and dark matter substructure.Comment: 19 pages, 4 Figures, 4 Tables, AJ accepte

Towards Detecting The 2175-{\AA} Dust Feature Associated With Strong High Redshift Mg {\ss}II Absorption Lines

We report detections of 39 2175-{\AA} dust extinction bump candidates associated with strong Mg II absorption lines at z$\sim$ 1--1.8 on quasar spectra in Sloan Digital Sky Survey (SDSS) DR3. These strong Mg II absorption line systems are detected among 2,951 strong Mg II absorbers with the rest equivalent width $W_r\lambda2796 >$ 1.0{\AA} at $1.0 < z < 1.86$, which is part of a full sample of 7,421 strong Mg II absorbers compiled by Prochter et al. (2006). The redshift range of the absorbers is chosen to allow the 2175-{\AA} extinction features to be completely covered within the SDSS spectrograph operation wavelength range. An upper limit of the background quasar emission redshift at z$=$2.1 is set to prevent the Ly$\alpha$ forest lines from contaminating the sensitive spectral region for the 2175-{\AA} bump measurements. The FM90 (Fitzpatrick & Massa 1990) parameterization is applied to model the Optical/UV extinction curve in the rest frame of Mg II absorbers of the 2175-{\AA} bump candidates. The simulation technique developed by Jiang et al. (2010a, b) is used to derive the statistical significance of the candidate 2175-{\AA} bumps. A total of 12 absorbers are detected with 2175-{\AA} bumps at a 5$\sigma$ level of statistical significance, 10 are detected at a 4$\sigma$ level and 17 are detected at a 3$\sigma$ level. Most of the candidate bumps in this work are similar to the relatively weak 2175-{\AA} bumps observed in the Large Magellanic Clouds (LMC) LMC2 supershell rather than the strong ones observed in the Milky Way (MW). This sample has greatly increased the total number of 2175-{\AA} extinction bumps measured on SDSS quasar spectra. Follow-up observations may rule out some of possible false detections and reveal the physical and chemical natures of 2175-{\AA} quasar absorbers.Comment: 71 pages, 6 tables, 49 figures, accepted by ApJ, Table 1 is available entirely at http://home.ustc.edu.cn/~jpaty/dataset/qso_dr7.dat ;Table 2 is available entirely at http://home.ustc.edu.cn/~jpaty/dataset/rejected.lis

Analyzing the Flux Anomalies of the Large-Separation Lensed Quasar SDSS J1029+2623

Using a high resolution radio image, we successfully resolve the two fold image components B and C of the quasar lens system SDSS J1029+2623. The flux anomalies associated with these two components in the optical regime persist, albeit less strongly, in our radio observations, suggesting that the cluster must be modeled by something more than a single central potential. We argue that placing substructure close to one of the components can account for a flux anomaly with negligible changes in the component positions. Our best fit model has a substructure mass of ~10^8 solar masses up to the mass-sheet degeneracy, located roughly 0.1 arcsecs West and 0.1 arcsecs North of component B. We demonstrate that a positional offset between the centers of the source components can explain the differences between the optical and radio flux ratios.Comment: 5 pages, 3 figures, 2 tables, accepted to ApJ Letter

The Highest Resolution Mass Map of Galaxy Cluster Substructure To Date Without Assuming Light Traces Mass: LensPerfect Analysis of Abell 1689

We present a strong lensing mass model of Abell 1689 which resolves substructures ~25 kpc across (including about ten individual galaxy subhalos) within the central ~400 kpc diameter. We achieve this resolution by perfectly reproducing the observed (strongly lensed) input positions of 168 multiple images of 55 knots residing within 135 images of 42 galaxies. Our model makes no assumptions about light tracing mass, yet we reproduce the brightest visible structures with some slight deviations. A1689 remains one of the strongest known lenses on the sky, with an Einstein radius of RE = 47.0" +/- 1.2" (143 +3/-4 kpc) for a lensed source at zs = 2. We find a single NFW or Sersic prole yields a good fit simultaneously (with only slight tension) to both our strong lensing (SL) mass model and published weak lensing (WL) measurements at larger radius (out to the virial radius). According to this NFW fit, A1689 has a mass of Mvir = 2.0 +0.5/-0.3 x 10^15 Msun / h70 (M200 = 1.8 +0.4/-0.3 x 10^15 Msun / h70) within the virial radius rvir = 3.0 +/- 0.2 Mpc / h70 (r200 = 2.4 +0.1/-0.2 Mpc / h70), and a central concentration cvir = 11.5 +1.5/-1.4 (c200 = 9.2 +/- 1.2). Our SL model prefers slightly higher concentrations than previous SL models, bringing our SL+WL constraints in line with other recent derivations. Our results support those of previous studies which find A1689 has either an anomalously large concentration or significant extra mass along the line of sight (perhaps in part due to triaxiality). If clusters are generally found to have higher concentrations than realized in simulations, this could indicate they formed earlier, perhaps as a result of early dark energy.Comment: 27 pages, 17 figures, submitted to ApJ. See http://www.its.caltech.edu/~coe/LPA1689/ for complete set of color multiple images (observed and delensed) and more. Comments welcome at http://scirate.com/who.php?id=1005.xxxx&what=comments (insert arXiv number at xxxx; free & easy registration