Detection of Stellar Variability in the Central Parsec of the Galaxy

1996 ◽  
Vol 467 ◽  
pp. 645 ◽  
Author(s):  
M. Tamura ◽  
M. W. Werner ◽  
E. E. Becklin ◽  
E. S. Phinney
Keyword(s):  
The Galaxy ◽  
Central Parsec

scholarly journals NuSTAR and Chandra Observations of New X-Ray Transients in the Central Parsec of the Galaxy

2019 ◽  
Vol 885 (2) ◽  
pp. 142 ◽  
Author(s):  
Kaya Mori ◽  
Charles J. Hailey ◽  
Shifra Mandel ◽  
Yve E. Schutt ◽  
Matteo Bachetti ◽  
...  
Keyword(s):  
X Ray ◽  
The Galaxy ◽  
Central Parsec

scholarly journals Stellar and wind properties of massive stars in the central parsec of the Galaxy

2006 ◽  
Vol 2 (14) ◽  
pp. 207-207
Author(s):  
Fabrice Martins ◽  
Reinhard Genzel ◽  
Frank Eisenhauer ◽  
Thibaut Paumard ◽  
Thomas Ott ◽  
...  
Keyword(s):  
Quantitative Analysis ◽  
Massive Stars ◽  
The Galaxy ◽  
Central Parsec

AbstractThe stellar and wind properties of the new population of massive stars in the central parsec of the Galaxy are derived through quantitative analysis with atmosphere models.

scholarly journals Diffraction Limited Near Infrared Imaging of the Central Parsec of the Galaxy

1994 ◽  
Vol 158 ◽  
pp. 379-381
Author(s):  
A. Eckart ◽  
R. Genzel ◽  
R. Hofmann ◽  
B.J. Sams ◽  
L.E. Tacconi-Garman
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Core Radius ◽  
The Galaxy ◽  
K 13 ◽  
Sgr A ◽  
Central Parsec ◽  
Stellar Sources ◽  
Stellar Density ◽  
Source Number

We present deep 1.6 and 2.2 μm images of the central parsec of the Galaxy at a resolution of 0.15″. Most of the flux in earlier seeing limited images comes from about 340 unresolved stellar sources with K≤14. The IRS 16 and 13 complexes are resolved into about two dozen and half a dozen sources, a number of which are probably luminous hot stars. We confirm the presence of a blue near infrared object (K≈13) at the position of the compact radio source Sgr A∗. The spatial centroid of the source number distribution is consistent with the position of Sgr A∗ but not with a position in the IRS 16 complex. The stellar surface density in the central 10″ is very well fitted by an isothermal cluster model with a well defined core radius. The derived core radius of all 340 sources is 0.15±0.05 pc. The central stellar density is a few times 107 M⊙ pc−3. Buildup of massive stars by merging of lower mass stars and collisional disruption of giant atmospheres are very probable processes in the central 0.2 pc.

scholarly journals THE HIGH-DENSITY IONIZED GAS IN THE CENTRAL PARSEC OF THE GALAXY

2010 ◽  
Vol 723 (2) ◽  
pp. 1097-1109 ◽  
Author(s):  
Jun-Hui Zhao ◽  
Ray Blundell ◽  
James M. Moran ◽  
Dennis Downes ◽  
Karl F. Schuster ◽  
...  
Keyword(s):  
High Density ◽  
Ionized Gas ◽  
The Galaxy ◽  
Central Parsec

scholarly journals The magnetic field in the central parsec of the Galaxy

2018 ◽  
Vol 476 (1) ◽  
pp. 235-245 ◽  
Author(s):  
P F Roche ◽  
E Lopez-Rodriguez ◽  
C M Telesco ◽  
R Schödel ◽  
C Packham
Keyword(s):  
Magnetic Field ◽  
The Galaxy ◽  
Central Parsec ◽  
The Magnetic Field

scholarly journals Can supernova shells feed supermassive black holes in galactic nuclei?

2020 ◽  
Vol 644 ◽  
pp. A72
Author(s):  
J. Palouš ◽  
S. Ehlerová ◽  
R. Wünsch ◽  
M. R. Morris
Keyword(s):  
Accretion Disk ◽  
Galactic Center ◽  
Galactic Nuclei ◽  
Rotational Axis ◽  
Average Mass ◽  
The Galaxy ◽  
Gravitational Pull ◽  
Thin Layer Approximation ◽  
Hydrodynamical Simulations ◽  
Central Parsec

Aims. We simulate shells created by supernovae expanding into the interstellar medium of the nuclear region of a galaxy, and analyze how the shell evolution is influenced by the supernova position relative to the galactic center, by the interstellar matter density, and by the combined gravitational pull of the nuclear star cluster and supermassive black hole (SMBH). Methods. We adopted simplified hydrodynamical simulations using the infinitesimally thin layer approximation in 3D (code RING) and determined whether and where the shell expansion may bring new gas into the inner parsec around the SMBH. Results. The simulations show that supernovae occurring within a conical region around the rotational axis of the galaxy can feed the central accretion disk surrounding the SMBH. For ambient densities between 103 and 105 cm−3, the average mass deposited into the central parsec by individual supernovae varies between 10 and 1000 solar masses depending on the ambient density and the spatial distribution of supernova events. Supernovae occurring in the aftermath of a starburst event near a galactic center can supply two to three orders of magnitude more mass into the central parsec, depending on the magnitude of the starburst. The deposited mass typically encounters and joins an accretion disk. The fate of that mass is then divided between the growth of the SMBH and an energetically driven outflow from the disk.

scholarly journals SiO and H2O Masers in the Central Parsec of the Galaxy

1998 ◽  
Vol 164 ◽  
pp. 229-230 ◽  
Author(s):  
Karl M. Menten ◽  
Mark J. Reid
Keyword(s):  
Galactic Center ◽  
Radio Continuum ◽  
Continuum Emission ◽  
Proper Motions ◽  
Infrared Images ◽  
Evolved Stars ◽  
The Galaxy ◽  
Sgr A ◽  
Central Parsec ◽  
Infrared Sources

AbstractWe have discovered maser emission from SiO and H2O molecules toward a number of evolved stars within the central parsec of our Galaxy. The maser positions can be registered with milliarcsecond precision relative to the radio continuum emission of the nonthermal Galactic center source Sgr A*. Since the masing stars are prominent infrared sources, our data can be used to locate the position of Sgr A* on infrared images of the Galactic center region. Using VLBA observations it will be possible to measure proper motions of the maser stars, which can be used to put constraints on the mass distribution in the central parsec.

The Mechanism and Timescale of Nodal Precession: Two Nuclear Stellar Disks in the Galactic Center

2015 ◽  
Vol 24 (1) ◽  
Author(s):  
B. P. Kondratyev
Keyword(s):  
Time Scales ◽  
Galactic Center ◽  
Weighted Average ◽  
Dynamical Model ◽  
The Galaxy ◽  
Circular Rings ◽  
Orbital Precession ◽  
Central Parsec

AbstractA dynamical model of interacting nuclear stellar rings in the central parsec of our Galaxy is constructed. We discuss the physical sources of nodal precession and of the associated time scales. For approximate study of the mutual orbital precession, we replace broad nuclear rings by weighted average narrow circular rings. The model with narrow circular rings is shown to adequately describe the nodal precession. The period of relativistic apsidal precession in the center of the Galaxy,

scholarly journals Study of the molecular gas in the central parsec of the Galaxy through regularized 3D spectroscopy

2013 ◽  
Vol 9 (S303) ◽  
pp. 83-85
Author(s):  
A. Ciurlo ◽  
T. Paumard ◽  
D. Rouan ◽  
Y. Clénet
Keyword(s):  
Molecular Gas ◽  
Imaging Data ◽  
Ionized Gas ◽  
Central Cavity ◽  
Neutral Gas ◽  
The Galaxy ◽  
Circumnuclear Disk ◽  
Cool Gas ◽  
Central Parsec ◽  
Spectro Imaging

AbstractThe cool gas in the central parsec of the Galaxy is organized in the surrounding circumnuclear disk, made of neutral gas, and the internal minispiral, composed of dust and ionized gas. In order to study the transition between them we have investigated the presence of H2 neutral gas in this area, through NIR spectro-imaging data observed with SPIFFI. To preserve the spatial resolution we implemented a new method consisting of a regularized 3D fit. We concentrated on the supposedly fully ionized central cavity and the very inner edge of the CND. H2 is detected everywhere: at the boundary of the CND and in the central cavity, where it seems to split in two components, one in the background of the minispiral and one inside the Northern arm.

Diffraction Limited Near Infrared Imaging of the Central Parsec of the Galaxy

1994 ◽  
pp. 379-381
Author(s):  
A. Eckart ◽  
R. Genzel ◽  
R. Hofmann ◽  
B. J. Sams ◽  
L. E. Tacconi-Garman
Keyword(s):  
Near Infrared ◽  
Infrared Imaging ◽  
Near Infrared Imaging ◽  
The Galaxy ◽  
Central Parsec
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