We present the first weak-lensing-based scaling relation between galaxy cluster mass, M WL , and integrated Compton parameter Y sph . Observations of 18 galaxy clusters at z 0.2 were obtained with the Subaru 8.2-m telescope and the Sunyaev-Zel'dovich Array. The M WL −Y sph scaling relations, measured at ∆ = 500, 1000, and 2500 ρ c , are consistent in slope and normalization with previous results derived under the assumption of hydrostatic equilibrium (HSE). We find an intrinsic scatter in M WL at fixed Y sph of 20%, larger than both previous measurements of M HSE − Y sph scatter as well as the scatter in true mass at fixed Y sph found in simulations. Moreover, the scatter in our lensing-based scaling relations is morphology dependent, with 30 -40% larger M WL for undisturbed compared to disturbed clusters at the same Y sph at r 500 . Further examination suggests that the segregation may be explained by the inability of our spherical lens models to faithfully describe the three-dimensional structure of the clusters, in particular, the structure along the line-of-sight. We find that the ellipticity of the brightest cluster galaxy, a proxy for halo orientation, correlates well with the offset in mass from the mean scaling relation, which supports this picture. This provides empirical evidence that line-of-sight projection effects are an important systematic uncertainty in lensing-based scaling relations.

We investigate the utility of a new, self-similar pressure profile for fitting Sunyaev-Zel'dovich (SZ) effect observations of galaxy clusters. Current SZ imaging instruments-such as the Sunyaev-Zel'dovich Array (SZA)-are capable of probing clusters over a large range in a physical scale. A model is therefore required that can accurately describe a cluster's pressure profile over a broad range of radii from the core of the cluster out to a significant fraction of the virial radius. In the analysis presented here, we fit a radial pressure profile derived from simulations and detailed X-ray analysis of relaxed clusters to SZA observations of three clusters with exceptionally high-quality X-ray data: A1835, A1914, and CL J1226.9+3332. From the joint analysis of the SZ and X-ray data, we derive physical properties such as gas mass, total mass, gas fraction and the intrinsic, integrated Compton y-parameter. We find that parameters derived from the joint fit to the SZ and X-ray data agree well with a detailed, independent X-ray-only analysis of the same clusters. In particular, we find that, when combined with X-ray imaging data, this new pressure profile yields an independent electron radial temperature profile that is in good agreement with spectroscopic X-ray measurements.

We present high-resolution CARMA 230 GHz continuum imaging of nine deeply embedded protostars in the Serpens Molecular Cloud, including six of the nine known Class 0 protostars in Serpens. This work is part of a program to characterize disk and envelope properties for a complete sample of Class 0 protostars in nearby low-mass star-forming regions. Here, we present CARMA maps and visibility amplitudes as a function of uv-distance for the Serpens sample. Observations are made in the B, C, D, and E antenna configurations, with B configuration observations utilizing the CARMA Paired Antenna Calibration System. Combining data from multiple configurations provides excellent uv-coverage (4-500 kλ), allowing us to trace spatial scales from 10 2 to 10 4 AU. We find evidence for compact disk components in all of the observed Class 0 protostars, suggesting that disks form at very early times (t < 0.2 Myr) in Serpens. We make a first estimate of disk masses using the flux at 50 kλ, where the contribution from the envelope should be negligible, assuming an unresolved disk. The resulting disk masses range from 0.04 M to 1.7 M , with a mean of approximately 0.2 M. Our high-resolution maps are also sensitive to binary or multiple sources with separations 250 AU, but significant evidence of multiplicity on scales <2000 AU is seen in only one source.

We report measurements of the Sunyaev-Zel'dovich (SZ) effect in three highredshift (0.89 ≤ z ≤ 1.03), X-ray selected galaxy clusters. The observations were obtained at 30 GHz during the commissioning period of a new, eight-element interferometer -the Sunyaev-Zel'dovich Array (SZA) -built for dedicated SZ effect observations. The SZA observations are sensitive to angular scales larger than those subtended by the virial radii of the clusters. Assuming isothermality and hydrostatic equilibrium for the intracluster medium, and gas-mass fractions consistent with those for clusters at moderate redshift, we calculate electron temperatures, gas masses, and total cluster masses from the SZ data. The SZderived masses, integrated approximately to the virial radii, are 1.9 +0.5 −0.4 × 10 14 M ⊙ for Cl J1415.1+3612, 3.4 +0.6 −0.5 × 10 14 M ⊙ for Cl J1429.0+4241 and 7.2 +1.3 −0.9 × 10 14 M ⊙ for Cl J1226.9+3332. The SZ-derived quantities are in good agreement with the cluster properties derived from X-ray measurements.Subject headings: cosmology: observations -galaxies: individual (NGC5529) -clusters: individual (Cl J1415.1+3612, Cl J1429.0+4241, Cl J1226.9+3332) -Sunyaev-Zel'dovich Effect -cosmic microwave background -techniques: interferometric

We present an analysis of the diffuse emission at 5 GHz in the first quadrant of the Galactic plane using two months of preliminary intensity data taken with the C-Band All Sky Survey (C-BASS) northern instrument at the Owens Valley Radio Observatory, California.Combining C-BASS maps with ancillary data to make temperature-temperature plots we find synchrotron spectral indices of β = −2.65 ± 0.05 between 0.408 GHz and 5 GHz and β = −2.72 ± 0.09 between 1.420 GHz and 5 GHz for −10 • < |b| < −4 • , 20 • < l < 40 • . Through the subtraction of a radio recombination line (RRL) free-free template we determine the synchrotron spectral index in the Galactic plane (|b| < 4 • ) to be β = −2.56 ± 0.07 between 0.408 GHz and 5 GHz, with a contribution of 53 ± 8 per cent from free-free emission at 5 GHz. These results are consistent with previous low frequency measurements in the Galactic plane.By including C-BASS data in spectral fits we demonstrate the presence of anomalous microwave emission (AME) associated with the Hii complexes W43, W44 and W47 near 30 GHz, at 4.4 σ, 3.1 σ and 2.5 σ respectively. The CORNISH VLA 5 GHz source catalogue rules out the possibility that the excess emission detected around 30 GHz may be due to ultra-compact Hii regions. Diffuse AME was also identified at a 4σ level within 30 • < l < 40 • , −2 • < b < 2 • between 5 GHz and 22.8 GHz.