The Nuclear Cluster of the Milky Way: Star Formation and Velocity Dispersion in the Central 0.5 Parsec

Krabbe, A.; Genzel, R.; Eckart, A.; Najarro, F.; Lutz, D.; Cameron, M.; Kroker, H.; Tacconi-Garman, L. E.; Thatte, Niranjan; Weitzel, L.; Drapatz, S.; Geballe, T. R.; Sternberg, A.; Kudritzki, R. P.

doi:10.1086/309579

Cited by 311 publications

(205 citation statements)

References 37 publications

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“…Most of the stars outside the central 0.4 pc of the GC are (Krabbe et al 1995). To cull out the young population from the older, we use the CO line strengths from the Adaptive Optics Demonstration Science Data Set of the Gemini telescope.…”

Section: (A) Stellar Photometrymentioning

confidence: 99%

“…Faint (compared to the stars discussed right below) blue stars known as the "S-stars" or "S-cluster" are observed in the immediate vicinity (within 0.04 pc) of the SMBH. Krabbe et al (1995) identified them as massive main-sequence stars with a spectral type of B0-B9. Further from the center, between ∼ 0.04 and ∼ 0.4 pc, a few tens of OB supergiants, giants, and main-sequence stars are observed along with a pool of faint red stars.…”

Section: Introductionmentioning

confidence: 99%

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Mass Distribution in the Central Few Parsecs of Our Galaxy

Oh¹,

Kim²,

Figer³

2009

Journal of The Korean Astronomical Society

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We estimate the enclosed mass profile in the central 10 pc of the Milky Way by analyzing the infrared photometry and the velocity observations of dynamically relaxed stellar population in the Galactic center. HST/NICMOS and Gemini Adaptive Optics images in the archive are used to obtain the number density profile, and proper motion and radial velocity data were compiled from the literature to find the velocity dispersion profile assuming a spherical symmetry and velocity isotropy. From these data, we calculate the the enclosed mass and density profiles in the central 10 pc of the Galaxy using the Jeans equation. Our improved estimates can better describe the exact evolution of the molecular clouds and star clusters falling down to the Galactic center, and constrain the star formation history of the inner part of the Galaxy.

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Section: (A) Stellar Photometrymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Mass Distribution in the Central Few Parsecs of Our Galaxy

Oh¹,

Kim²,

Figer³

2009

Journal of The Korean Astronomical Society

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“…From the optical and IR observations, the very high level of extinction to the GC was already appreciated, and one simple explanation seemed to be that our Galaxy could be harboring a Seyfert 2-like nucleus of low but still significant luminosity. Such an interpretation was supported by parallel developments in the IR leading to the discovery of many high mass-loss stars in the inner parsec (4)(5)(6), and estimates on the basis of their stellar winds suggested that sufficient material should be available to fuel Sgr A* at a level typical of other LLAGN, ∼a few × 10 −4 the canonical maximum allowed accretion luminosity, L Edd (see, e.g., refs. 7 and 8).…”

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confidence: 93%

Revelations in our own backyard: Chandra’s unique Galactic Center discoveries

Markoff¹

2010

Proc. Natl. Acad. Sci. U.S.A.

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Before the launch of Chandra, our Galactic Center supermassive black hole, Sgr A*, had never been positively identified outside the radio bands. A great deal has changed in the past decade, starting with the discovery that our own backyard harbors a very weak, yet clearly active, galactic nucleus. I will review how this revelation has been a boon for accretion studies around black holes in general and has helped us place our own Galaxy in context within the active galactic nuclei (AGN) zoology. Chandra’s exquisite resolution has also unveiled entirely new populations of faint sources and transients, as well as regions of extreme gas dynamics and hints of prior, more typical AGN-like activity in our Galactic Center.

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“…Nuclear cluster of massive stars Allen, Hyland & Hillier (1990) and Forrest et al (1987) reported on broad lines toward the IRS 16 complex that were due to Ofpe/WN9 stars and a luminous object 8" SW of the central cluster -the AF star. Krabbe et al (1991Krabbe et al ( , 1995 found a cluster of He I stars concentrated on the IRS 16 complex and the small IRS 13 cluster about 4" to the east of the center. Najarro et al (1994Najarro et al ( , 1997 for the first time performed detailed atmospheric model calculations of the brightest central hot stars.…”

Section: Introductionmentioning

confidence: 99%

“…Eckart et al (1992;see also Eckart & Genzel 1997; and references therein) obtained diffraction limited images and derived for the first time stellar proper motions in the central cluster. Beginning in the late eighties several groups began measuring radial velocities of late type, red giant and supergiants (e.g., Rieke & Rieke 1988;Sellgren et al 1990;Krabbe et al 1995;Haller et al 1996). The combination of radial velocities of the red giant and supergiants as well as the young and massive He I stars and proper motions resulted in a confirmation of the presence of a 3 x 10 6 M 0 dark mass associated with Sgr A*.…”

Section: Introductionmentioning

confidence: 99%

Hot stars in the Galactic Center

Eckart¹,

Ott²,

Genzel³

et al. 1999

Symp. - Int. Astron. Union

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Abstract. The central parsec of our Galaxy is powered by a cluster of young massive hot stars which formed a few million years ago. Within that cluster the seven most luminous (L >10 5 . 75 L 0 ) and moderately hot (T <10 4 . 5 K) blue supergiants contribute half of the ionizing luminosity of that region. These stars probably formed when a dense cloud fell into the center < 10 7 years ago, was highly compressed there, and became gravitationally unstable. Over six years of high spatial resolution, near-infrared imaging and spectroscopy have made it possible to carry out a detailed investigation of the stars in the central cluster and its enclosed mass. As one result of a detailed variability study of the central cluster stars we found that the bright He I star IRS 16SW is a short-period variable with a period of ""9.72 days. It is most likely an eclipsing binary with a lower mass limit of~100 solar masses. Line of sight velocities and proper motions have been measured for these hot stars (as well as ",,200 other stars) down to separations of less than five light days from the compact radio source Sgr A* at the dynamic center of the Milky Way. These confirmed measurements imply the presence of a central dark mass of 2.6 x 10 6 solar masses. The dark mass at the center of the Milky Way is currently the most compelling case for a massive black hole. Simple physical considerations show that this dark mass cannot consist of a stable cluster of stars, stellar remnants, substellar condensations or a degenerate gas of elementary particles but that at least 10 3 to 10 5 solar masses must be in the form of a massive black hole associated with Sgr A* itself.

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The Nuclear Cluster of the Milky Way: Star Formation and Velocity Dispersion in the Central 0.5 Parsec

Cited by 311 publications

References 37 publications

Mass Distribution in the Central Few Parsecs of Our Galaxy

Mass Distribution in the Central Few Parsecs of Our Galaxy

Revelations in our own backyard: Chandra’s unique Galactic Center discoveries

Hot stars in the Galactic Center

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