SINFONI in the Galactic Center: young stars and IR flares in the central light month

By F.Eisenhauer, R.Genzel, T.Alexander, R.Abuter, T.Paumard, T.Ott, A.Gilbert, S.Gillessen, M.Horrobin, S.Trippe and 10 more. 2005

208 citations recorded by the source corpus.

We report 75 milli-arcsec resolution, near-IR imaging spectroscopy within the central 30 light days of the Galactic Center, taken with the new adaptive optics assisted, integral field spectrometer SINFONI on the ESO-VLT. To a limiting magnitude of K~16, 9 of 10 1 based on observations obtained at the Very Large Telescope (VLT) of the European Southern Observatory, Chile

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/40db6aa7c59e4ff55082ce8761acda7614bd68c0

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Citations in the corpus

Our Peculiar Motion Away from the Local Void (2007, background): “Feast & Whitelock (1997) claim the angular velocity at the Solar position is 27.19 ± 0.87 km s−1 kpc−1 and review the details of the local motion of the Sun, while Eisenhauer et al. (2005) report a distance to the Galactic center of R0 = 7.62± 0.32 kpc.”
Stellar and wind properties of massive stars in the central parsec of the Galaxy (2006, background): “…Ghez et al. (2003) and Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20066688 Eisenhauer et al. (2005) had shown that the group of stars located in the central arcsecond of the Galaxy and orbiting very close to the black hole…”
Gravitational waves from scattering of stellar-mass black holes in galactic nuclei (2008, background): “For the remainder of Section 2, we focus our results on MilkyWay-like nuclei, and assume that MSMBH = 3.5 × 106 M (Eisenhauer et al. 2005; Ghez et al. 2005) and that the velocity dispersion of the stars and stellar BHs is σ ∗ = 75 km s−1 (HA06).”
A Log-Quadratic Relation for Predicting Supermassive Black Hole Masses from the Host Bulge Sérsic Index (2006, background): “Distances for 24 of our 27 galaxies were obtained from surface brightness fluctuation measurements and are thus independent of the Hubble constant, as of course is the Milky Way center.”
Detection of the Schwarzschild precession in the orbit of the star S2 near the Galactic centre massive black hole (2020, background): “They determined increasingly precise motions for more than 104 stars, and orbits for ≈ 50 (Schödel et al. 2002; Ghez et al. 2003, 2008; Eisenhauer et al. 2005; Gillessen et al. 2009b; Schödel et al. 2009; Meyer et al. 2012; Boehle et al. 2016; Fritz et al. 2016; Gillessen et al. 2017).”
XHIP: An extended hipparcos compilation (2011, methodology): “…of 225 km s-1, the proper motion of Sgr A* determined by Reid and Brunthaller (2004) implies a distance to the Galactic centre of R0 = 7.4 ± 0.04 kpc, consistent with recent determinations (Reid, 1993; Nishiyama et al., 2006; Bica et al., 2006; Eisenhauer et al., 2005; Layden et al., 1996).”
Observing the shadow of Einstein-Maxwell-Dilaton-Axion black hole (2013, background): “In general, the mass of a black hole can be estimated with the Newtonian orbital motion of the stars surrounding the black hole [1].”
STELLAR POPULATIONS IN THE CENTRAL 0.5 pc OF THE GALAXY. II. THE INITIAL MASS FUNCTION (2013, background): “…our own Milky Way Galaxy, located only 8 kpc away and surrounding a supermassive black hole (SMBH) of mass M∼ 4 × 106 M⊙ (Eckart & Genzel 1997; Ghez et al. 1998, 2000, 2003, 2005, 2008; Genzel et al. 2000; Schödel et al. 2002; Schödel et al. 2003; Eisenhauer et al. 2005; Gillessen et al. 2009a).”
REDDENING AND EXTINCTION TOWARD THE GALACTIC BULGE FROM OGLE-III: THE INNER MILKY WAY'S RV ∼ 2.5 EXTINCTION CURVE (2012, background): “…distance to the Galactic center of ∼9 kpc (Rattenbury et al. 2007a; Vanhollebeke et al. 2009), a large value relative to the geometrically determined distances to the Galactic center of 7.62± 0.32 kpc (Eisenhauer et al. 2005), 8.27 ± 0.29 kpc (Schönrich 2012), and 8.4 ± 0.4 kpc (Ghez et al. 2008).”
IMPLEMENTING FEW-BODY ALGORITHMIC REGULARIZATION WITH POST-NEWTONIAN TERMS (2007, unknown): “The particle masses were m1 = 3.5 × 106M⊙ and m2 = 10M⊙ = 2.85 × 10 −6m1, and the Keplerian orbit had initial semi-major axis a = 0.01 pc, similar to that of the “S” stars (Ghez et al. 2005; Eisenhauer et al. 2005).”
A geometric distance measurement to the Galactic center black hole with 0.3% uncertainty (2019, unknown): “The first measurement was in Eisenhauer et al. (2003), who reported R0 = 7940 ± 420 pc. Eisenhauer et al. (2005) updated this value to R0 = 7620 ± 320 pc. Ghez et al. (2008) reported R0 = 8400 ± 400 pc, and Gillessen et al. (2009) differed slightly with R0 = 8330 ± 350 pc.”
STRONG MASS SEGREGATION AROUND A MASSIVE BLACK HOLE (2008, background): “Similarly, the rates of detectable GW bursts from fly-bys near the Galactic MBH strongly depend on the number of SBHs near it (Hopman et al. 2007).”
Flaring Activity of Sagittarius A* at 43 and 22 GHz: Evidence for Expanding Hot Plasma (2006, background): “The spectral properties of this cluster of stars show massive stars but are generally consistent with normal main sequence O8V/B0V to B9V stars (Eisenhauer et al. 2005; Baganoff et al. 2003; Nayashkin & Sunyaev 2005).”
KINEMATICS OF THE STELLAR HALO AND THE MASS DISTRIBUTION OF THE MILKY WAY USING BLUE HORIZONTAL BRANCH STARS (2012, background): “…things which have insignificant or unexplored effects on our mass estimation e.g. we do not take into account the mass of the super-massive black hole, which is ∼ 4× 106 M⊙ (Schödel et al. 2002; Eisenhauer et al. 2005; Gillessen et al. 2009), and is approximately 1/1000 of the mass of the bulge.”
Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole (2018, background): “…at the Keck telescopes) have delivered more than 104 stellar motions and orbit determinations for ≈ 45 individual stars (Schödel et al. 2002; Ghez et al. 2003, 2008; Eisenhauer et al. 2005; Gillessen et al. 2009b, 2017; Schödel et al. 2009; Meyer et al. 2012; Boehle et al. 2016; Fritz et al. 2016).”
First light for GRAVITY: Phase referencing optical interferometry for the Very Large Telescope Interferometer (2017, background): “On top of this quasi-steady component there is variable emission in the X-ray and infrared bands, which appears as ﬂares, typically a few times per day and lasting for about 1 − 2 h (Bagano ﬀ et al. 2001; Genzel et al. 2003; Eckart et al. 2004; Eisenhauer et al. 2005).”
The Effect of Mass Segregation on Gravitational Wave Sources near Massive Black Holes (2006, methodology): “Our Galactic Center contains a MBH of mass comparable to the MBH mass considered here (Ghez et al. 2005; Eisenhauer et al. 2005).”
The most massive stars in the Arches cluster (2007, methodology): “Data were reduced with the SPRED software (Abuter et al. 2006) as in Eisenhauer et al. (2005) and Paumard et al. (2006).”