activity
19972010
most citedStar formation and UV colors of the brightest Cluster Galaxies in the representative XMM-Newton Cluster Structure Survey

70 citations · 260 across the 9 of their papers we have counts for

collaborators

9 papers

astro-ph.CO2010★ 70 cited

Star formation and UV colors of the brightest Cluster Galaxies in the representative XMM-Newton Cluster Structure Survey

Megan Donahue, Seth Bruch, Emily Wang +8

We present UV broadband photometry and optical emission-line measurements for a sample of 32 Brightest Cluster Galaxies (BCGs) in clusters of the Representative XMM-Newton Cluster…

astro-ph.CO2009★ 50 cited

Brightest Cluster Galaxies and Core Gas Density in REXCESS Clusters

D. B. Haarsma, L. Leisman, M. Donahue +7

We investigate the relationship between brightest cluster galaxies (BCGs) and their host clusters using a sample of nearby galaxy clusters from the Representative XMM Cluster Struc…

astro-ph2008★ 1 cited

The Central Component of Gravitational Lens Q0957+561

Deborah B. Haarsma, Joshua N. Winn, Irwin Shapiro +1

In 1981, a faint radio source (G') was detected near the center of the lensing galaxy of the famous "twin quasar" Q0957+561. It is still unknown whether this central radio source i…

astro-ph2005★ 11 cited

The FIRST-Optical-VLA Survey for Lensed Radio Lobes

D. B. Haarsma, J. N. Winn, E. E. Falco +7

We present results from a survey for gravitationally lensed radio lobes. Lensed lobes are a potentially richer source of information about galaxy mass distributions than lensed poi…

astro-ph2000★ 48 cited

Further Investigation of the Time Delay, Magnification Ratios, and Variability in the Gravitational Lens 0218+357

A. S. Cohen, J. N. Hewitt, C. B. Moore +1

High precision VLA flux density measurements for the lensed images of 0218+357 yield a time delay of 10.1(+1.5-1.6)days (95% confidence). This is consistent with independent measur…

astro-ph2000

New VLBI Constraints for 0957+561 Lens Models

Deborah Haarsma, Joseph Leh'ar, Rennan Barkana

Time-delay measurements of 0957+561 based on radio monitoring now agree with optical monitoring. Recent models incorporate many recent observations, but the systematic uncertaintie…