Gas Mass Fractions and Star Formation in Blue-Sequence E/S0 Galaxies

Recent work has identified a population of low-redshift E/S0 galaxies that lie on the blue sequence in color vs. stellar mass parameter space, where spiral galaxies typically reside. While high-mass blue-sequence E/S0s often resemble young merger or interaction remnants likely to fade to the red sequence, we focus on blue-sequence E/S0s with lower stellar masses (< a few 10^10 M_sun), which are characterized by fairly regular morphologies and low-density field environments where fresh gas infall is possible. This population may provide an evolutionary link between early-type galaxies and spirals through disk regrowth. Focusing on atomic gas reservoirs, we present new GBT HI data for 27 E/S0s on both sequences as well as a complete tabulation of archival HI data for other galaxies in the Nearby Field Galaxy Survey. Normalized to stellar mass, the atomic gas masses for 12 of the 14 blue-sequence E/S0s range from 0.1 to >1.0. These gas-to-stellar mass ratios are comparable to those of spiral and irregular galaxies and have a similar dependence on stellar mass. Assuming that the HI is accessible for star formation, we find that many of our blue-sequence E/S0s can increase in stellar mass by 10-60% in 3 Gyr in both of two limiting scenarios, exponentially declining star formation and constant star formation. In a constant star formation scenario, about half of the blue-sequence E/S0s require fresh gas infall on a timescale of <3 Gyr to avoid exhausting their atomic gas reservoirs and evolving to the red sequence. We present evidence that star formation in these galaxies is bursty and likely involves externally triggered gas inflows. Our analysis suggests that most blue-sequence E/S0s are indeed capable of substantial stellar disk growth on relatively short timescales. (abridged)Comment: ApJ, accepted, 26 pages with 12 figures (5 color), 5 table

Ni[((EPPr2)-Pr-i)(2)N](2) complexes : stereolsomers (E = se) and square-planar coordination (E = te)

The reaction of ((Pr2PE)-Pr-i)(2)NM center dot TMEDA (M = Li, E = Se; M = Na, E = Te) with NiBr2 center dot DME in THF affords Ni[((SePPr2)-Pr-i)(2)N](2) as either square-planar (green) or tetrahedral (red) stereoisomers, depending on the recrystallization solvent; the Te analogue is obtained as the square-planar complex Ni[(TeP(i)pr(2))(2)N](2)

MUSTANG 2: a large focal plane array for the 100 m Green Bank Telescope

This paper describes MUSTANG 2, a 338 element focal plane array that is being built for the Green Bank Telescope. Each element consists of a profiled feedhorn coupled to two transition edge sensor bolometers, one for each polarization. Initial deployment will be with 32 detectors, but once fully populated, MUSTANG 2 will be capable of mapping a 8′ × 8′ area to 23 μ Jy in 1 h with good image fidelity on angular scales from 9" to 6′. As well as an instrument overview, the choice of bandpass and the design of the feeds, detectors and readout are given

MUSTANG2: a large focal plan array for the 100 meter Green Bank Telescope

MUSTANG 2 is a 223 element focal plane that operates between 75 and 105 GHz on the 100 meter Green Bank Telescope. It shares many of the science goals of its predecessor, MUSTANG, but will have fifteen times the sensitivity and five times the field-of-view. Angular scales from 900 to 60 will be recovered with high fidelity providing a unique overlap between high resolution instruments such as ALMA and lower resolution single dish telescopes such as ACT or SPT. Individual TES bolometers are placed behind feedhorns spaced by 1.9λ f and are read out using a microwave SQUID multiplexing system

Development of a microwave SQUID-multiplexed TES array for MUSTANG-2

MUSTANG-2 is a 90 GHz feedhorn-coupled, microwave SQUID-multiplexed TES bolometer array in the final stages of development for operation on the 100-m Robert C. Byrd Green Bank Telescope. We present the camera design and report the performance during the first season of observation, in which 64 of the available 215 pixels in the focal plane were populated. We highlight the microwave multiplexing readout technology, which is envisioned as a path to read out the next generation of large pixel-count cryogenic focal planes. In this regard, MUSTANG2 is a pathfinder for this multiplexing technology. We present noise spectra which show no detector noise degradation when read out with microwave SQUID multiplexing, and we present first light images of Jupiter and M87, which demonstrate the end-to-end system performance

Pathways of H(2) toward the Active Site of [NiFe]-Hydrogenase

Hydrogenases catalyze the reversible oxidation of molecular hydrogen (H(2)), but little is known about the diffusion of H(2) toward the active site. Here we analyze pathways for H(2) permeation using molecular dynamics (MD) simulations in explicit solvent. Various MD simulation replicates were done, to improve the sampling of the system states. H(2) easily permeates hydrogenase in every simulation and it moves preferentially in channels. All H(2) molecules that reach the active site made their approach from the side of the Ni ion. H(2) is able to reach distances of <4 Å from the active site, although after 6 Å permeation is difficult. In this region we mutated Val-67 into alanine and perform new MD simulations. These simulations show an increase of H(2) inside the protein and at lower distances from the active site. This valine can be a control point in the H(2) access to the active center