SINFONI in the Galactic Center: Young Stars and Infrared 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 11 more. 2005

504 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fccf0d3f5440d529f326f9a8a20e48b06cf85640

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Citations in the corpus

A Massive Cluster of Red Supergiants at the Base of the Scutum-Crux Arm (2007, methodology): “In determining the distance to Wd 1, these authors used the Galactic center distance DGal ¼ 7:6 0:3 kpc, as determined by Eisenhauer et al. (2005) and the solar rotation velocity of ¼ 214 7 km s 1, averaged from measurements byReid&Brunthaler (2004) and Feast&Whitelock (1997).”
Stellar Remnants in Galactic Nuclei: Mass Segregation (2006, background): “From infrared photometry and spectroscopy, these stars appear to be main-sequence (MS) objects with masses of order 4–16 M and are therefore younger than 100 Myr (Gezari et al. 2002; Ghez et al. 2003; Eisenhauer et al. 2005).”
Starbursts near supermassive black holes: young stars in the Galactic Centre, and gravitational waves in LISA band (2006, background): “…period of the S-star is that of S1, ¶ We acknowledge Scott Tremaine for attracting our attention to the RR as a potentially important relaxation mechanism for the S-star relaxation, in 2004. c© 0000 RAS, MNRAS 000, 000–000 which has Porb = 94yr (Eisenhauer et al., 2005, see also Ghez et al., 2005).”
LINE DERIVED INFRARED EXTINCTION TOWARD THE GALACTIC CENTER (2011, methodology): “In addition, we also compute the effective filter extinctions for a bright Sgr A* like spectrum (Eisenhauer et al. 2005; Gillessen et al. 2006) which follows a power-law with a slope β = 0.5 in νLν (Hornstein et al. 2007; Dodds-Eden et al. 2009) as example of a very red source.”
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.”
Doing Science with eLISA: Astrophysics and Cosmology in the Millihertz Regime (2012, background): “By determining the number of systems in the Galaxy and their period distribution, the rate at which they will merge will be measured.”
An X-Ray, Infrared, and Submillimeter Flare of Sagittarius A* (2007, background): “However, a great deal of uncertainty was generated by the conflicting measurements of the IR spectral index during the flares (Ghez et al. 2005; Eisenhauer et al. 2005; Gillessen et al. 2006; Krabbe et al. 2006).”
A New Sample of Low-Mass Black Holes in Active Galaxies (2007, background): “Within the inactive sample of galaxies with dynamical BH masses, the BH in M32, MBH=(2.5+3.0−2.0) × 10 6 M⊙, has the lowest mass (Tremaine et al. 2002; excluding the Milky Way, whose modern mass is 3.5×106 M⊙; e.g., Ghez et al. 2005; Eisenhauer et al. 2005).”
A DISK OF YOUNG STARS AT THE GALACTIC CENTER AS DETERMINED BY INDIVIDUAL STELLAR ORBITS (2008, methodology): “However, the number of young stars in the disk drops at radii smaller than 0.08 pc; and at radii of .0.04 pc, none of the observed young S-stars are in the disk (Ghez et al. 2005b; Eisenhauer et al. 2005).”
Peering through the veil: near-infrared photometry and extinction for the Galactic nuclear star cluster (2009, background): “For example, the majority of stars within 0.5” of Sgr A* are of early-type (e.g. Eisenhauer et al. 2005).”
Measuring Distance and Properties of the Milky Way’s Central Supermassive Black Hole with Stellar Orbits (2008, methodology): “This is somewhat surprising as this would suggest that similar removal of biased points might lower the Eisenhauer et al. (2005) results.”
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).”
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).”
An Update on Monitoring Stellar Orbits in the Galactic Center (2016, background): “A few years later, orbits for a handful of stars had been determined (Ghez et al. 2005; Eisenhauer et al. 2005), and again a few years later, the number of known orbits exceeded 20 (Gillessen et al. 2009b).”
Polarimetry of near-infrared flares from Sagittarius A* (2006, background): “The distance to this closest MBH is only 7.6 ± 0.3 kpc (Eisenhauer et al. 2005).”
Stellar Proper Motions in the Galactic Bulge from Deep Hubble Space Telescope ACS WFC Photometry (2008, methodology): “With the geometrically determined SunYGalactic center distance RS ¼ 7:62 0:2 kpc (Eisenhauer et al. 2005), this bulge distance is consistent with the distance of intersection of the bulge major axis with the line of sight for bulge orientation angle k 14 .”