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Andrea M. Ghez measures stellar orbits around the supermassive black hole at the center of the Milky Way. Her team's Keck observations combined astrometry with radial velocities for the short-period star S0-2.

An angular orbit alone leaves a mass-distance degeneracy of an angular stellar orbit. Adding Doppler spectroscopy supplies a physical velocity scale, allowing central mass and Euclidean distance to be fitted together. Their 2008 analysis inferred roughly four million solar masses at a Euclidean distance of eight kiloparsecs, and examined how source confusion and assumptions about central motion affected the result.^[ref]

A kiloparsec is $10^3$ parsecs, approximately $3.086\times 10^{19}$ metres or $3262$ light-years. It is a useful unit for distances within and between galaxies: a length quoted as $8\mathrm{kpc}$ is $8000\mathrm{pc}$.

The underlying parsec is defined geometrically as $(648000/\pi )$ astronomical units. Consequently the stellar parallax relation $d(\mathrm{pc})=1/p(\mathrm{arcsec})$ makes a kiloparsec correspond approximately to a parallax of one milliarcsecond. The small angle illustrates why distant stars require precise astrometry.

Messier 82, also called M82, is a nearby starburst galaxy used to study how intense star formation drives a large galactic outflow. Its bright stellar disk, obscuring interstellar dust and extended gas emission trace different components; a bright feature in one wavelength band need not represent most of the outflow's mass or energy.

A concrete measurement is to compare diffuse X-ray emission above the disk with compact sources inside it. ROSAT imaging and spectroscopy detected the wind's X-rays to roughly six kiloparsecs from the plane. The observations separated point sources from diffuse emission and found that the latter was not well described as a freely expanding wind: shocked material interacting with the flow could instead account for the emission.^[ref]

This makes M82 an illuminating stellar feedback laboratory. The inference runs from spatially resolved spectra to gas conditions and then to a physical outflow model; a photograph of gas extending away from the disk does not by itself determine its temperature, energy source or escape rate.