scholarly journals 10.7. Absorption columns with bright X-ray sources near the galactic center: — mass estimation in the Galactic center region

1998 ◽  
Vol 184 ◽  
pp. 443-444 ◽  
Author(s):  
Masaaki Sakano ◽  
Mamiko Nishiuchi ◽  
Yoshitomo Maeda ◽  
Katsuji Koyama ◽  
Jun Yokogawa
Keyword(s):  
Simple Form ◽  
Total Mass ◽  
Column Density ◽  
Galactic Center ◽  
Galactic Plane ◽  
Angular Distance ◽  
Mass Determination ◽  
Mass Estimation ◽  
X Ray ◽  
Center Region

We report the column density distribution to the Galactic Center region using the X-ray binary observations with the X-ray satellite ASCA, and demonstrate a new method of the total mass determination near the Galactic Center. The column densities are given by a simple form as a function of the angular distance from the Galactic Plane. Assuming a disklike mass distribution of 500 pc radius, we estimate the total mass to be ~ 6 × 107M⊙.

Mass estimation of cold matters in the Galactic Center region using bright hard X-ray sources

1999 ◽  
Vol 23 (5-6) ◽  
pp. 969-972 ◽  
Author(s):  
M Sakano ◽  
K Koyama ◽  
M Nishiuchi ◽  
J Yokogawa ◽  
Y Maeda
Keyword(s):  
Galactic Center ◽  
Mass Estimation ◽  
X Ray ◽  
Center Region

First results from the NuSTAR “mini-survey” of the Galactic center region

2013 ◽  
Vol 9 (S303) ◽  
pp. 439-443
Author(s):  
Charles J. Hailey ◽  
Keyword(s):  
Galactic Center ◽  
Galactic Plane ◽  
Pulsar Wind Nebulae ◽  
Telescope Array ◽  
X Ray ◽  
Center Region ◽  
First Results ◽  
Pulsar Wind ◽  
Sgr A

AbstractOne of the major science objectives of the Nuclear Spectroscopic Telescope Array (NuSTAR) observatory is to perform the first sub-arcminute, hard X-ray survey of several square degrees of the Galactic plane, centered on a region near the Galactic center. As a prelude to the full survey, which began in July 2013, NuSTAR conducted a ∼500 ks, 0.3 × 0.4° “mini-survey” focused on Sgr A* and its environs. We present analysis of several candidate pulsar wind nebulae and filaments, which are revealed to be intense sources of X-ray emission at >10 keV.

X-ray bursts from the source A1742-294 in the Galactic-center region

2001 ◽  
Vol 27 (8) ◽  
pp. 501-506 ◽  
Author(s):  
A. A. Lutovinov ◽  
S. A. Grebenev ◽  
M. N. Pavlinsky ◽  
R. A. Sunyaev
Keyword(s):  
Galactic Center ◽  
X Ray ◽  
Center Region

scholarly journals Unusual Diffuse X‐Ray Source in the Galactic Center Region

2002 ◽  
Vol 565 (2) ◽  
pp. 1017-1021 ◽  
Author(s):  
Atsushi Senda ◽  
Hiroshi Murakami ◽  
Katsuji Koyama
Keyword(s):  
Galactic Center ◽  
X Ray ◽  
Center Region

High-energy X-ray observations of the Galactic center region

1985 ◽  
Vol 290 ◽  
pp. 557 ◽  
Author(s):  
F. K. Knight ◽  
W. N., III Johnson ◽  
J. D. Kurfess ◽  
M. S. Strickman
Keyword(s):  
Galactic Center ◽  
High Energy ◽  
X Ray ◽  
Center Region

scholarly journals The geometry of the magnetic field in the central molecular zone measured by PILOT

2019 ◽  
Vol 630 ◽  
pp. A74 ◽  
Author(s):  
A. Mangilli ◽  
J. Aumont ◽  
J.-Ph. Bernard ◽  
A. Buzzelli ◽  
G. de Gasperis ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Molecular Clouds ◽  
Angular Resolution ◽  
Galactic Center ◽  
Galactic Plane ◽  
Mean Field ◽  
Field Orientation ◽  
Center Region ◽  
The Mean ◽  
The Magnetic Field

We present the first far infrared (FIR) dust emission polarization map covering the full extent of Milky Way’s central molecular zone (CMZ). The data, obtained with the PILOT balloon-borne experiment, covers the Galactic center region − 2° < ℓ < 2°, − 4° < b < 3° at a wavelength of 240 μm and an angular resolution of 2.2′. From our measured dust polarization angles, we infer a magnetic field orientation projected onto the plane of the sky (POS) that is remarkably ordered over the full extent of the CMZ, with an average tilt angle of ≃22° clockwise with respect to the Galactic plane. Our results confirm previous claims that the field traced by dust polarized emission is oriented nearly orthogonally to the field traced by GHz radio synchrotron emission in the Galactic center region. The observed field structure is globally compatible with the latest Planck polarization data at 353 and 217 GHz. Upon subtraction of the extended emission in our data, the mean field orientation that we obtain shows good agreement with the mean field orientation measured at higher angular resolution by the JCMT within the 20 and 50 km s−1 molecular clouds. We find no evidence that the magnetic field orientation is related to the 100 pc twisted ring structure within the CMZ. The low polarization fraction in the Galactic center region measured with Planck at 353 GHz combined with a highly ordered projected field orientation is unusual. This feature actually extends to the whole inner Galactic plane. We propose that it could be caused by the increased number of turbulent cells for the long lines of sight towards the inner Galactic plane or to dust properties specific to the inner regions of the Galaxy. Assuming equipartition between magnetic pressure and ram pressure, we obtain magnetic field strength estimates of the order of 1 mG for several CMZ molecular clouds.

scholarly journals The Mass and Structure of the Remnant of Tycho's Supernova

1983 ◽  
Vol 101 ◽  
pp. 1-15 ◽  
Author(s):  
Paul Gorenstein ◽  
Frederick Seward ◽  
Wallace Tucker
Keyword(s):  
Total Mass ◽  
Column Density ◽  
Supernova Remnant ◽  
Average Density ◽  
Equilibrium Calculation ◽  
Free Expansion ◽  
X Ray ◽  
Upper Limit ◽  
Interstellar Material ◽  
Einstein Observatory

A high resolution X-ray image of Tycho's supernova remnant obtained from the Einstein Observatory reveals three components of X-ray emission that we identify with shocked interstellar material, diffuse ejecta, and clumpy ejecta. This picture is applied to derive the mass of X-ray emitting material. Assuming a distance of 3 kpc, an absorbing column density of 3 × 1021 atoms/cm2, and using an ion-electron non-equilibrium calculation for the emissivity, we find the average density of the ISM is 0.4 atoms/cm3, and the energy contained in the remnant is 1.4 × 1051 ergs. The total mass of X-ray emitting material in the remnant is ≈4 M⊙, ≈2 M⊙ ejecta and ≈2 M⊙ swept up, putting the remnant at an intermediate state between a free expansion and the Sedov phase. There is no evidence for neutron star. The upper limit on the surface temperature is in the range 1.1 to 1.8 × 106K.

scholarly journals THE BOLOCAM GALACTIC PLANE SURVEY: λ = 1.1 AND 0.35 mm DUST CONTINUUM EMISSION IN THE GALACTIC CENTER REGION

2010 ◽  
Vol 721 (1) ◽  
pp. 137-163 ◽  
Author(s):  
John Bally ◽  
James Aguirre ◽  
Cara Battersby ◽  
Eric Todd Bradley ◽  
Claudia Cyganowski ◽  
...  
Keyword(s):  
Galactic Center ◽  
Galactic Plane ◽  
Continuum Emission ◽  
Center Region

scholarly journals Tracing the Milky Way’s Vestigial Nuclear Jet

2021 ◽  
Vol 922 (2) ◽  
pp. 254
Author(s):  
Gerald Cecil ◽  
Alexander Y. Wagner ◽  
Joss Bland-Hawthorn ◽  
Geoffrey V. Bicknell ◽  
Dipanjan Mukherjee
Keyword(s):  
Galactic Center ◽  
Galactic Plane ◽  
Hubble Space Telescope ◽  
Seyfert Galaxy ◽  
Radio Continuum ◽  
X Ray ◽  
Multiple Paths ◽  
Ngc 1068 ◽  
Sgr A ◽  
Hydrodynamical Simulations

Abstract MeerKAT radio continuum and XMM-Newton X-ray images have recently revealed a spectacular bipolar channel at the Galactic Center that spans several degrees (∼0.5 kpc). An intermittent jet likely formed this channel and is consistent with earlier evidence of a sustained, Seyfert-level outburst fueled by black hole accretion onto Sgr A* several Myr ago. Therefore, to trace a now weak jet that perhaps penetrated, deflected, and percolated along multiple paths through the interstellar medium, relevant interactions are identified and quantified in archival X-ray images, Hubble Space Telescope Paschen α images and Atacama Large Millimeter/submillimeter Array millimeter-wave spectra, and new SOAR telescope IR spectra. Hydrodynamical simulations are used to show how a nuclear jet can explain these structures and inflate the ROSAT/eROSITA X-ray and Fermi γ-ray bubbles that extend ± 75° from the Galactic plane. Thus, our Galactic outflow has features in common with energetic, jet-driven structures in the prototypical Seyfert galaxy NGC 1068.

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