EAVN Astrometry toward the Extreme Outer Galaxy: Kinematic distance with the proper motion of G034.84-00.95

Abstract

We aim to reveal the structure and kinematics of the Outer-Scutum-Centaurus (OSC) arm located on the far side of the Milky Way through very long baseline interferometry (VLBI) astrometry using KaVA, which is composed of KVN (Korean VLBI Network) and VERA (VLBI Exploration of Radio Astrometry). We report the proper motion of a 22 GHz H${}_2$O maser source, which is associated with the star-forming region G034.84$-$00.95, to be (${\mu }_{\alpha }\cos \delta$, ${\mu }_{\delta }$) = ($-$1.61$\pm$0.18, $-$4.29$\pm$0.16) mas yr${}^{-1}$ in equatorial coordinates (J2000). We estimate the 2D kinematic distance to the source to be 18.6$\pm$1.0 kpc, which is derived from the variance-weighted average of kinematic distances with LSR velocity and the Galactic-longitude component of the measured proper motion. Our result places the source in the OSC arm and implies that G034.84$-$00.95 is moving away from the Galactic plane with a vertical velocity of $-$38$\pm$16 km s${}^{-1}$. Since the H I supershell GS033+06$-$49 is located at a kinematic distance roughly equal to that of G034.84$-$00.95, it is expected that gas circulation occurs between the outer Galactic disk around G034.84$-$00.95 with a Galactocentric distance of 12.8${}_{-0.9}^{+1.0}$ kpc and halo. We evaluate possible origins of the fast vertical motion of G034.84$-$00.95, which are (1) supernova explosions and (2) cloud collisions with the Galactic disk. However, neither of the possibilities are matched with the results of VLBI astrometry as well as spatial distributions of H II regions and H I gas.

arXiv commentAccepted for publication in PASJ. 14 figures; 8 tables

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Cited by in corpus (3)

• Overview of the Observing System and Initial Scientific Accomplishments of the East Asian VLBI Network (EAVN)
• A large misalignment between continuous jet and discrete ejecta in microquasar GRS 1915+105 during its obscured phase
• First Trigonometric Parallax Measurements with the KVN and VERA Array (KaVA)