Estimation of the Hubble Constant and Constraint on Descriptions of Dark Energy

TL;DR

This paper discusses methods for precisely measuring the Hubble Constant using water maser emissions, emphasizing technological requirements and potential future improvements for constraining dark energy and cosmological parameters.

Contribution

It proposes a direct, high-precision method for estimating H0 via water maser observations, detailing observational strategies and instrumental needs for achieving 1% accuracy.

Findings

Identification of optimal redshift range 0.02<z<0.06 for small samples

Requirement of VLBI with high sensitivity and resolution

Potential of space-VLBI and SKA to improve measurements

Abstract

Joint analysis of Cosmic Microwave Background, Baryon Acoustic Oscillation, and supernova data has enabled precision estimation of cosmological parameters. New programs will push to 1% uncertainty in the dark energy equation of state and tightened constraint on curvature, requiring close attention to systematics. Direct 1% measurement of the Hubble constant (H0) would provide a new constraint. It can be obtained without overlapping systematics directly from recessional velocities and geometric distance estimates for galaxies via the mapping of water maser emission that traces the accretion disks of nuclear black holes. We identify redshifts 0.02<z<0.06 as best for small samples, e.g., 10 widely distributed galaxies, each with 3% distance uncertainty. Knowledge of peculiar radial motion is also required. Mapping requires very long baseline interferometry (VLBI) with the finest angular resolution, sensitivity to individual lines of a few mJy-km/s, and baselines that can detect a complex of ~10 mJy lines (peak) in < 1 min. For 2010-2020, large ground apertures (50-100m diameter) augmenting the VLBA are critical, such as EVLA, GBT, Effelsberg, and the Large Millimeter Telescope, for which we propose a 22 GHz receiver and VLBI instrumentation. A space-VLBI aperture may be required, thus motivating US participation in the Japanese VSOP-2 mission (launch c.2013). This will provide 3-4x longer baselines and ~5x improvement in distance uncertainty. There are now 5 good targets at z>0.02, out of ~100 known masers. A single-dish discovery survey of >10,000 nuclei (>2500 hours on the GBT) would build a sample of tens of potential distance anchors. Beyond 2020, a high-frequency SKA could provide larger maser samples, enabling estimation of H0 from individually less accurate distances, and possibly without the need for peculiar motion corrections.