2017
DOI: 10.1093/mnras/stx1154
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Bow shocks in a newly discovered maser source in IRAS 20231+3440

Abstract: From measuring the annual parallax of water masers over one and a half years with VERA, we present the trigonometric parallax and corresponding distance of another newly identified water maser source in the region of IRAS 20231+3440 as π = 0.611 ± 0.022 mas and D = 1.64 ± 0.06 kpc respectively. We measured the absolute proper motions of all the newly detected maser spots (30 spots) and presented two pictures describing the possible spatial distribution of the water maser as the morphology marks out an arc of m… Show more

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Cited by 5 publications
(2 citation statements)
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“…The strongest water masers occur on the western side of the apex at a projected distance of ≈ r 0 from both the apex and the axis of the bow shock. The total width of the bow shock traced by CM2-W1 (∼500 au) is similar to the size scale of maser arcs that are perpendicular to the outflow direction as seen in VLBI observations of more distant massive star formation regions like W49N (Gwinn 1994), and somewhat larger than the maser arcs recently resolved in AFGL 5142 (Burns et al 2016) and IRAS 20231+3440 (Ogbodo et al 2017). Thus, these maser features appear to be a common result of the impact of high-velocity jets from massive protostars.…”
Section: The Water Maser Bow Shocksupporting
confidence: 76%
“…The strongest water masers occur on the western side of the apex at a projected distance of ≈ r 0 from both the apex and the axis of the bow shock. The total width of the bow shock traced by CM2-W1 (∼500 au) is similar to the size scale of maser arcs that are perpendicular to the outflow direction as seen in VLBI observations of more distant massive star formation regions like W49N (Gwinn 1994), and somewhat larger than the maser arcs recently resolved in AFGL 5142 (Burns et al 2016) and IRAS 20231+3440 (Ogbodo et al 2017). Thus, these maser features appear to be a common result of the impact of high-velocity jets from massive protostars.…”
Section: The Water Maser Bow Shocksupporting
confidence: 76%
“…The above physical properties from observations yield a momentum rate Ṗ ∼ 4 × 10 −3 M ⊙ yr −1 km s −1 for the protostellar outflow of M17 MIR. This is comparable to outflows of 10 −3 − 10 0 M ⊙ yr −1 km s −1 driven by MYSOs (Moscadelli et al 2016), and one magnitude higher than the outflow from a low-mass YSO in IRAS 20231+3440 (Ogbodo et al 2017).…”
Section: Outflow Rate and Disk Accretion Rate Of M17 Mirmentioning
confidence: 64%