Mounting evidence for the role of distal fallopian tubes in the pathogenesis of epithelial ovarian cancer has led to opportunistic salpingectomy being increasingly performed at the time of benign ...gynecologic surgery. Opportunistic salpingectomy has now been recommended as best practice in the United States to reduce future risk of ovarian cancer even in low-risk women. Preliminary analyses have suggested that performance of opportunistic salpingectomy is increasing.
To examine trends in opportunistic salpingectomy in women undergoing benign hysterectomy and to determine how the publication of the tubal hypothesis in 2010 may have contributed to these trends.
This is a population-based, retrospective, observational study examining the National Inpatient Sample between January 2001 and September 2015. Women younger than 50 years who underwent inpatient hysterectomy for benign gynecologic disease were grouped as hysterectomy alone vs hysterectomy with opportunistic salpingectomy. All women had ovarian conservation, and those with adnexal pathology were excluded. Linear segmented regression with log transformation was used to assess temporal trends. An interrupted time-series analysis was then used to assess the impact of the 2010 publication of the tubal hypothesis on opportunistic salpingectomy trends. A regression-tree model was constructed to examine patterns in the use of opportunistic salpingectomy. A binary logistic regression model was then fitted to identify independent characteristics associated with opportunistic salpingectomy. Sensitivity analysis was performed in women aged 50–65 years to further assess surgical trends in a wider age group.
There were 98,061 (9.0%) women who underwent hysterectomy with opportunistic salpingectomy and 997,237 (91.0%) women who underwent hysterectomy alone without opportunistic salpingectomy. The rate at which opportunistic salpingectomy was being performed gradually increased from 2.4% to 5.7% between 2001 and 2010 (2.4-fold increase; P<.001), predicting a 7.0% rate of opportunistic salpingectomy in 2015. However, in 2010, the rate of opportunistic salpingectomy began to increase substantially and reached 58.4% by 2015 (10.2-fold increase; P<.001). In multivariable analysis, the largest change in the performance of opportunistic salpingectomy occurred after 2010 (adjusted odds ratio, 5.42; 95% confidence interval, 5.34–5.51; P<.001). In a regression-tree model, women who had a hysterectomy at urban teaching hospitals in the Midwest after 2013 had the highest chance of undergoing opportunistic salpingectomy during benign hysterectomy (76.4%). In the sensitivity analysis of women aged 50–65 years, a similar exponential increase in opportunistic salpingectomy was observed from 5.8% in 2010 to 55.8% in 2015 (9.8-fold increase; P<.001).
Our study suggests that clinicians in the United States rapidly adopted opportunistic salpingectomy at the time of benign hysterectomy following the publication of data implicating the distal fallopian tubes in ovarian cancer pathogenesis in 2010. By 2015, nearly 60% of women had undergone opportunistic salpingectomy at benign hysterectomy.
A recent trial demonstrated decreased survival in women with early-stage cervical cancer who underwent radical hysterectomy via minimally invasive surgery compared with laparotomy; however, outcomes ...following trachelectomy have yet to be studied.
To examine trends, characteristics, and survival of reproductive-aged women with early-stage cervical cancer who underwent minimally invasive trachelectomy.
This is a retrospective study examining the National Cancer Database between 2010 and 2015. Women aged <50 years who underwent trachelectomy for stage IA2-IB cervical cancer were grouped by mode of surgery. Clinicopathologic characteristics and outcomes were compared between minimally invasive surgery and laparotomy groups.
A total of 246 women were included, 144 (58.5%, 95% confidence interval, 52.4%–64.7%) of whom had trachelectomy with a minimally invasive surgery approach. Median age was similar between the minimally invasive surgery and laparotomy groups (median, 31 vs 29 years, P = .20). There was a significant increase in the use of minimally invasive surgery from 29.3% in 2010 to 75.0% in 2015 (P < .001). Specifically, minimally invasive surgery became the dominant approach for trachelectomy by year 2011 (54.8%). Hospitals registered in the West (75.0% vs 25.0%) were more likely, whereas those registered in the Midwest (46.9% vs 53.1%) were less likely, to perform minimally invasive surgery (P = .02). Median follow-up was 37 months (interquartile range, 23–51) for the minimally invasive surgery group and 40 months (interquartile range, 26–67) for the laparotomy group. During follow-up, there were 11 (5.3%) deaths, 4 (3.5%) in the minimally invasive surgery group and 7 (7.6%) in the laparotomy group (P = .25).
Minimally invasive surgery has become the dominant modality for trachelectomy in reproductive-aged women with stage IA2-IB cervical cancer after year 2011. Survival of women with stage IA2-IB cervical cancer who underwent trachelectomy is generally good regardless of surgical modality. Although our study showed no difference in survival between the minimally invasive surgery and laparotomy approaches, effects of MIS on survival remain unknown and further study is warranted.
Although general relativity underlies modern cosmology, its applicability on cosmological length scales has yet to be stringently tested. Such a test has recently been proposed, using a quantity, EG, ...that combines measures of large-scale gravitational lensing, galaxy clustering and structure growth rate. The combination is insensitive to ‘galaxy bias’ (the difference between the clustering of visible galaxies and invisible dark matter) and is thus robust to the uncertainty in this parameter. Modified theories of gravity generally predict values of EG different from the general relativistic prediction because, in these theories, the ‘gravitational slip’ (the difference between the two potentials that describe perturbations in the gravitational metric) is non-zero, which leads to changes in the growth of structure and the strength of the gravitational lensing effect. Here we report that EG = 0.39 ± 0.06 on length scales of tens of megaparsecs, in agreement with the general relativistic prediction of EG 0.4. The measured value excludes a model within the tensor–vector–scalar gravity theory, which modifies both Newtonian and Einstein gravity. However, the relatively large uncertainty still permits models within f() theory, which is an extension of general relativity. A fivefold decrease in uncertainty is needed to rule out these models.
Celotno besedilo
Dostopno za:
DOBA, IJS, IZUM, KILJ, NUK, PILJ, PNG, SAZU, SIK, UILJ, UKNU, UL, UM, UPUK
The intrinsic alignment of galaxies with the large-scale density field is an important astrophysical contaminant in upcoming weak lensing surveys. We present detailed measurements of the galaxy ...intrinsic alignments and associated ellipticity–direction (ED) and projected shape (w
g+) correlation functions for galaxies in the cosmological hydrodynamic MassiveBlack-II simulation. We carefully assess the effects on galaxy shapes, misalignment of the stellar component with the dark matter shape and two-point statistics of iterative weighted (by mass and luminosity) definitions of the (reduced and unreduced) inertia tensor. We find that iterative procedures must be adopted for a reliable measurement of the reduced tensor but that luminosity versus mass weighting has only negligible effects. Both ED and w
g+ correlations increase in amplitude with subhalo mass (in the range of 1010–6.0 × 1014 h
−1 M⊙), with a weak redshift dependence (from z = 1 to 0.06) at fixed mass. At z ∼ 0.3, we predict a w
g+ that is in reasonable agreement with Sloan Digital Sky Survey luminous red galaxy measurements and that decreases in amplitude by a factor of ∼5–18 for galaxies in the Large Synoptic Survey Telescope survey. We also compared the intrinsic alignments of centrals and satellites, with clear detection of satellite radial alignments within their host haloes. Finally, we show that w
g+ (using subhaloes as tracers of density) and w
δ+ (using dark matter density) predictions from the simulations agree with that of non-linear alignment (NLA) models at scales where the two-halo term dominates in the correlations (and tabulate associated NLA fitting parameters). The one-halo term induces a scale-dependent bias at small scales which is not modelled in the NLA model.
Abstract
We present and characterize the catalog of galaxy shape measurements that will be used for cosmological weak lensing measurements in the Wide layer of the first year of the Hyper Suprime-Cam ...(HSC) survey. The catalog covers an area of 136.9 deg2 split into six fields, with a mean i-band seeing of 0${^{\prime\prime}_{.}}$58 and 5σ point-source depth of i ∼ 26. Given conservative galaxy selection criteria for first-year science, the depth and excellent image quality results in unweighted and weighted source number densities of 24.6 and 21.8 arcmin−2, respectively. We define the requirements for cosmological weak lensing science with this catalog, then focus on characterizing potential systematics in the catalog using a series of internal null tests for problems with point-spread function (PSF) modeling, shear estimation, and other aspects of the image processing. We find that the PSF models narrowly meet requirements for weak lensing science with this catalog, with fractional PSF model size residuals of approximately 0.003 (requirement: 0.004) and the PSF model shape correlation function ρ1 < 3 × 10−7 (requirement: 4 × 10−7) at 0${^{\circ}_{.}}$5 scales. A variety of galaxy shape-related null tests are statistically consistent with zero, but star–galaxy shape correlations reveal additive systematics on >1° scales that are sufficiently large as to require mitigation in cosmic shear measurements. Finally, we discuss the dominant systematics and the planned algorithmic changes to reduce them in future data reductions.
The robust estimation of the tiny distortions (shears) of galaxy shapes caused by weak gravitational lensing in the presence of much larger shape distortions due to the point spread function (PSF) ...has been widely investigated. One major problem is that most galaxy shape measurement methods are subject to bias due to pixel noise in the images (‘noise bias’). Noise bias is usually characterized using uncorrelated noise fields; however, real images typically have low-level noise correlations due to galaxies below the detection threshold, and some types of image processing can induce further noise correlations. We investigate the effective detection significance and its impact on noise bias in the presence of correlated noise for one method of galaxy shape estimation. For a fixed noise variance, the biases in galaxy shape estimates can differ substantially for uncorrelated versus correlated noise. However, use of an estimate of detection significance that accounts for the noise correlations can almost entirely remove these differences, leading to consistent values of noise bias as a function of detection significance for correlated and uncorrelated noise. We confirm the robustness of this finding to properties of the galaxy, the PSF, and the noise field, and quantify the impact of anisotropy in the noise correlations. Our results highlight the importance of understanding the pixel noise model and its impact on detection significances when correcting for noise bias on weak lensing.
ABSTRACT We perform a joint analysis of the abundance, the clustering, and the galaxy-galaxy lensing signal of galaxies measured from Data Release 11 of the Sloan Digital Sky Survey III Baryon ...Oscillation Spectroscopic Survey in our companion paper, Miyatake et al. The lensing signal was obtained by using the shape catalog of background galaxies from the Canada France Hawaii Telescope Legacy Survey, which was made publicly available by the CFHTLenS collaboration, with an area overlap of about 105 deg2. We analyze the data in the framework of the halo model in order to fit halo occupation parameters and cosmological parameters ( and ) to these observables simultaneously, and thus break the degeneracy between galaxy bias and cosmology. Adopting a flat ΛCDM cosmology with priors on , , and h from the analysis of WMAP 9 yr data, we obtain constraints on the stellar mass-halo mass relation of galaxies in our sample. Marginalizing over the halo occupation distribution parameters and a number of other nuisance parameters in our model, we obtain and (68% confidence). We demonstrate the robustness of our results with respect to sample selection and a variety of systematics such as the halo off-centering effect and possible incompleteness in our sample. Our constraints are consistent, complementary, and competitive with those obtained using other independent probes of these cosmological parameters. The cosmological analysis is the first of its kind to be performed at a redshift as high as 0.53.
We present a new method for measuring the scale dependence of the intrinsic alignment (IA) contamination to the galaxy-galaxy lensing signal, which takes advantage of multiple shear estimation ...methods applied to the same source galaxy sample. By exploiting the resulting correlation of both shape noise and cosmic variance, our method can provide an increase in the signal-to-noise of the measured IA signal as compared to methods which rely on the difference of the lensing signal from multiple photometric redshift bins. For a galaxy-galaxy lensing measurement which uses LSST sources and DESI lenses, the signal-to-noise on the IA signal from our method is predicted to improve by a factor of ~2 relative to the method of Blazek et al. 2012, for pairs of shear estimates which yield substantially different measured IA amplitudes and highly correlated shape noise terms. We show that statistical error necessarily dominates the measurement of intrinsic alignments using our method. We also consider a physically motivated extension of the Blazek et al. 2012 method which assumes that all nearby galaxy pairs, rather than only excess pairs, are subject to IA. In this case, the signal-to-noise of the method of Blazek et al. 2012 is improved.
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