The Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey I: X-ray Properties of Clusters Detected as Extended X-ray Sources

In the construction of an X-ray selected sample of galaxy clusters for cosmological studies, we have assembled a sample of 495 X-ray sources found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey. The sample covers the celestial region with declination $\delta \ge 0\deg$ and galactic latitude $|b_{II}| \ge 20\deg$ and comprises sources with a count rate $\ge 0.06$ counts s$^{-1}$ and a source extent likelihood of 7. In an optical follow-up identification program we find 378 (76%) of these sources to be clusters of galaxies. ...Comment: 61 pages; ApJS in press; fixed bug in table file; also available at (better image quality) http://www.xray.mpe.mpg.de/theorie/NORAS

Weak-Lensing Mass Measurements of Five Galaxy Clusters in the South Pole Telescope Survey Using Magellan/Megacam

We use weak gravitational lensing to measure the masses of five galaxy clusters selected from the South Pole Telescope (SPT) survey, with the primary goal of comparing these with the SPT Sunyaev--Zel'dovich (SZ) and X-ray based mass estimates. The clusters span redshifts 0.28 < z < 0.43 and have masses M_500 > 2 x 10^14 h^-1 M_sun, and three of the five clusters were discovered by the SPT survey. We observed the clusters in the g'r'i' passbands with the Megacam imager on the Magellan Clay 6.5m telescope. We measure a mean ratio of weak lensing (WL) aperture masses to inferred aperture masses from the SZ data, both within an aperture of R_500,SZ derived from the SZ mass, of 1.04 +/- 0.18. We measure a mean ratio of spherical WL masses evaluated at R_500,SZ to spherical SZ masses of 1.07 +/- 0.18, and a mean ratio of spherical WL masses evaluated at R_500,WL to spherical SZ masses of 1.10 +/- 0.24. We explore potential sources of systematic error in the mass comparisons and conclude that all are subdominant to the statistical uncertainty, with dominant terms being cluster concentration uncertainty and N-body simulation calibration bias. Expanding the sample of SPT clusters with WL observations has the potential to significantly improve the SPT cluster mass calibration and the resulting cosmological constraints from the SPT cluster survey. These are the first WL detections using Megacam on the Magellan Clay telescope.Comment: Main body: 18 pages, 7 figures, 6 tables. Appendix: 6 pages, 10 figures. Accepted by ApJ. New version incorporates changes from accepted articl

Redshifts, Sample Purity, and BCG Positions for the Galaxy Cluster Catalog from the First 720 Square Degrees of the South Pole Telescope Survey

We present the results of the ground- and space-based optical and near-infrared (NIR) follow-up of 224 galaxy cluster candidates detected with the Sunyaev-Zel'dovich (SZ) effect in the 720 deg^2 of the South Pole Telescope (SPT) survey completed in the 2008 and 2009 observing seasons. We use the optical/NIR data to establish whether each candidate is associated with an overdensity of galaxies and to estimate the cluster redshift. Most photometric redshifts are derived through a combination of three different cluster redshift estimators using red-sequence galaxies, resulting in an accuracy of Δz/(1 + z) = 0.017, determined through comparison with a subsample of 57 clusters for which we have spectroscopic redshifts. We successfully measure redshifts for 158 systems and present redshift lower limits for the remaining candidates. The redshift distribution of the confirmed clusters extends to z = 1.35 with a median of z_(med) = 0.57. Approximately 18% of the sample with measured redshifts lies at z > 0.8. We estimate a lower limit to the purity of this SPT SZ-selected sample by assuming that all unconfirmed clusters are noise fluctuations in the SPT data. We show that the cumulative purity at detection significance ξ > 5(ξ > 4.5) is ≥95% (≥70%). We present the red brightest cluster galaxy (rBCG) positions for the sample and examine the offsets between the SPT candidate position and the rBCG. The radial distribution of offsets is similar to that seen in X-ray-selected cluster samples, providing no evidence that SZ-selected cluster samples include a different fraction of recent mergers from X-ray-selected cluster samples

Giant phyllodes tumor of the breast: a clinical observation

The paper describes a case of giant phyllodes tumor of the breast. Phyllodes tumor is a rare type of fibroepithelial tumor composed of epithelial and connective tissue with the predominant development of a connective tissue component. Surgery is the only radical treatment

Volcanic pulses in the siberian traps as inferred from permo-triassic geomagnetic secular variations

© Cambridge University Press 2015. There is little reason to believe that eruption of the Siberian Traps occurred gradually. On the contrary, trap emplacement likely occurred in the form of brief but voluminous volcanic pulses, as for example demonstrated for theDeccan Traps (Chenet et al., 2008, 2009) in India and for the Karoo Traps (Moulin et al., 2011, 2012) in South Africa. To search for evidence of such pulses during formation of the Siberian Traps, and to obtain time constraints on eruptive activity we have undertaken a paleomagnetic study of several important trap volcanic sections from the Norilsk and Maymecha-Kotuy areas (Figure 5.1). To complement our work, we include paleomagnetic directions published by Heunemann et al. (2004) from the Norilsk area. A brief description of the sampling areas and the paleomagnetic results are presented below. Sampling Detailed paleomagnetic sampling was carried out on the Medvejia and Truba sections in the Maymecha-Kotuy region (Figure 5.1a, b) during field seasons in 2008 and 2009, and on the Sunduk and Ergalakh sections in the Norilsk region in 2010 (Figure 5.1c). Between 8 and 20 oriented hand samples were collected from individual lava flows or tuff units. In total, about 1400 samples, representing 133 lava flows, were collected and studied

La Patrie : journal quotidien, politique, commercial et littéraire

25 octobre 18531853/10/25 (A13,N299)