2008
DOI: 10.1086/592738
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Abstract: We report new precision measurements of the properties of our Galaxy's supermassive black hole. Based on astrometric (1995Y2007) and radial velocity (RV; 2000Y2007) measurements from the W. M. Keck 10 m telescopes, a fully unconstrained Keplerian orbit for the short-period star S0-2 provides values for the distance (R 0 ) of 8:0 AE 0:6 kpc, the enclosed mass (M bh ) of 4:1 AE 0:6 ; 10 6 M , and the black hole's RV, which is consistent with zero with 30 km s À1 uncertainty. If the black hole is assumed to be at… Show more

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Cited by 1,464 publications
(1,676 citation statements)
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“…This is similar to that found for galaxies that host powerful radio AGN (e.g Chiaberge & Marconi 2011), and considerably larger than for spiral galaxies such as the Milky Way (MBH ∼ 4 × 10 6 M⊙, Ghez et al 2008). These values are similar to the black hole mass estimates for 0313-192 (Keel et al 2006) and J2345-0449 (Bagchi et al 2014).…”
Section: Black Hole Mass Estimate For J1649+2635supporting
confidence: 88%
“…This is similar to that found for galaxies that host powerful radio AGN (e.g Chiaberge & Marconi 2011), and considerably larger than for spiral galaxies such as the Milky Way (MBH ∼ 4 × 10 6 M⊙, Ghez et al 2008). These values are similar to the black hole mass estimates for 0313-192 (Keel et al 2006) and J2345-0449 (Bagchi et al 2014).…”
Section: Black Hole Mass Estimate For J1649+2635supporting
confidence: 88%
“…Located 8.4 ± 0.6 kpc (Reid et al 2009) away at the Galactic Center, Sagittarius A* (hereafter Sgr A*) is the nearest "supermassive" black hole with a mass of ∼ 4 × 10 6 M (Ghez et al 2008). Despite its relative proximity, the source of emission from Sgr A* is still unknown.…”
Section: Sagittarius A*mentioning
confidence: 99%
“…A 4×10 6  M black hole is coincident with the compact nonthermal radio source SgrA * at the center of the Galaxy (Reid & Brunthaler 2004;Ghez et al 2008;Gillessen et al 2009). The estimated mass accretion rate onto Sgr A * is several orders of magnitude smaller than the rate at which young, windy stars in the innermost 0.5 pc supply mass to the Bondi radius of Sgr A * (Coker & Melia 1997;Cuadra et al 2006Cuadra et al , 2008.…”
Section: Introductionmentioning
confidence: 99%