Trigonometric parallax and proper motion of Sagittarius A* measured by VERA using the new broad-band back-end system OCTAVE-DAS

We successfully measured the trigonometric parallax of Sagittarius A* (Sgr A*) to be $117\pm 17$ micro-arcseconds ($\mu$as) using the VLBI Exploration of Radio Astrometry (VERA) with the newly developed broad-band signal-processing system named OCTAVE-DAS. The measured parallax corresponds to a Galactocentric distance at the Sun of $R_0=8.5_{-1.1}^{+1.5}$ kpc. By combining the astrometric results with VERA and the Very Long Baseline Array (VLBA) over a monitoring period of 25 years, the proper motion of Sgr A* is obtained to be $({\mu }_{\alpha },{\mu }_{\delta })=(-3.133\pm 0.003,-5.575\pm 0.005)$ mas yr${}^{-1}$ in equatorial coordinates, corresponding to $({\mu }_l,{\mu }_b)=(-6.391\pm 0.005,-0.230\pm 0.004)$ mas yr${}^{-1}$ in Galactic coordinates. This gives an angular orbital velocity of the Sun of ${\mathrm{\Omega }}_{\odot }=30.30\pm 0.02$ km s${}^{-1}$ kpc${}^{-1}$. We find upper limits to the core wander, $\mathrm{\Delta }\theta <0.20$ mas (1.6 AU), peculiar motion, $\mathrm{\Delta }\mu <0.10$ mas yr${}^{-1}$ (3.7 km s${}^{-1}$), and acceleration, $a<2.6$ $\mu$as yr${}^{-2}$ (0.10 km s${}^{-1}$ yr${}^{-1}$) for Sgr A*. Thus, we obtained upper mass limits of $\approx$ 3 $\times$ 10${}^4$$M_{\odot }$ and $\approx$ 3 $\times$ 10${}^3$$M_{\odot }$ for the supposed intermediate-mass black holes at 0.1 and 0.01 pc from the Galactic center, respectively.