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 X-ray Structure of the Supernova Remnant G78.2+2.1

1983 ◽  
Vol 101 ◽  
pp. 281-286
Author(s):  
L. A. Higgs ◽  
T. L. Landecker ◽  
F. D. Seward
Keyword(s):  
Supernova Remnant ◽  
The South ◽  
X Ray ◽  
South Eastern ◽  
Einstein Observatory

The south-eastern portion of the supernova remnant G78.2+2.1, in Cygnus, has been detected as a weak X-ray source by the Einstein Observatory. The X-ray structure is similar to that of the radio filaments in this region, and confirms that X-ray emission in this portion of the “Cygnus super-bubble” does originate in a known supernova remnant. Marginally significant variations in X-ray hardness across the mapped area have been detected and can be related to known radio and optical features of the remnant. In its X-ray properties, G78.2+2.1 resembles IC443.

scholarly journals Heating of the Interstellar Medium by Supernova Remnants

1983 ◽  
Vol 101 ◽  
pp. 385-392
Author(s):  
Donald P. Cox
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Low Density ◽  
The Sun ◽  
X Ray ◽  
Interstellar Material ◽  
X Ray Background

We observe the heating of interstellar material in young supernova remnants (SNR). In addition, when analyzing the soft X-ray background we find evidence for large isolated regions of apparently hot, low density material. These, we infer, may have been heated by supernovae. One such region seems to surround the Sun. This has been modeled as a supernova remnant viewed from within. The most reasonable parameters are ambient density no ~ 0.004 cm−3, radius of about 100 pc, age just over 105 years (Cox and Anderson 1982).

scholarly journals Deciphering the nature of the pulsar wind nebula CTB 87 with XMM–Newton

2019 ◽  
Vol 491 (2) ◽  
pp. 3013-3021 ◽  
Author(s):  
B Guest ◽  
S Safi-Harb ◽  
A MacMaster ◽  
R Kothes ◽  
B Olmi ◽  
...  
Keyword(s):  
Supernova Remnant ◽  
Thermal Emission ◽  
Plasma Temperature ◽  
Evolutionary Stage ◽  
Reverse Shock ◽  
X Ray ◽  
Upper Limit ◽  
Supernova Shell ◽  
Pulsar Wind ◽  
Hydrodynamical Simulations

ABSTRACT CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded by a compact and a more extended X-ray nebula. Here, we use a deep XMM–Newton observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05 cm−3 for a plasma temperature kT ∼ 0.8 keV. The morphology and spectral properties are consistent with a ∼20-kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations.

scholarly journals XMM-Newton Observation of SNR RX J1713.7–3946

2004 ◽  
Vol 218 ◽  
pp. 73-76 ◽  
Author(s):  
G. Cassam-Chenaï ◽  
A. Decourchelle ◽  
J. Ballet ◽  
J.-L. Sauvageot ◽  
G. Dubner
Keyword(s):  
Column Density ◽  
Supernova Remnant ◽  
Synchrotron Emission ◽  
Spectral Parameters ◽  
X Ray ◽  
First Results ◽  
Photon Index

We present the first results of the observations of the supernova remnant RX J1713.7–3946 (also known as G347.3–0.5) obtained with the EPIC instrument on board the XMM-Newton satellite. We show a 5-pointings mosaiced image of the X-ray synchrotron emission. We characterize this emission by mapping its spectral parameters (absorbing column density NH and photon index γ). The synchrotron spectrum is flat at the shock and steep in the interior of the remnant. NH is well correlated with the X-ray brightness. A strong NH is found in the southwest rim of RX J1713.7–3946. We suggest that the SNR is interacting with a HI region there.

scholarly journals Non-Equilibrium Ionization in Puppis A

1983 ◽  
Vol 101 ◽  
pp. 245-252
Author(s):  
P. F. Winkler ◽  
C. R. Canizares ◽  
B. C. Bromley
Keyword(s):  
High Resolution ◽  
Spectroscopic Data ◽  
Supernova Remnant ◽  
Optical Data ◽  
Equilibrium Conditions ◽  
X Ray ◽  
Flux Measurements ◽  
Far From Equilibrium ◽  
Einstein Observatory ◽  
Non Equilibrium

High resolution X-ray spectroscopy of the brightest knot of emission in the Puppis A supernova remnant shows that it is made up of ionizing plasma, far from equilibrium. Flux measurements in several X-ray lines enable us to determine the non-equilibrium conditions: electron temperature, ion populations, and time since the knot was heated by the supernova shock. Imaging and spectroscopic data from the Einstein Observatory together suggest that this knot is a cloud of density about 10 cm−3 which has recently been shocked to a temperature 7 × 106 K. Radio and optical data on the region appear consistent with this picture.

scholarly journals X-ray studies of Seyfert galaxies and quasars

1986 ◽  
Vol 119 ◽  
pp. 253-259
Author(s):  
Claude R. Canizares ◽  
Gerard A. Kriss ◽  
John Kruper ◽  
C. Megan Urry
Keyword(s):  
Distribution Function ◽  
Statistical Analysis ◽  
Column Density ◽  
High Redshift ◽  
Seyfert Galaxies ◽  
Spectral Indices ◽  
X Ray ◽  
Survey Sample ◽  
Einstein Observatory

We present results of studies carried out with the imaging instruments on the Einstein Observatory. We summarize a statistical analysis of the X-ray properties of optically selected, radio quiet quasars including nine new high redshift quasars detected in two deep X-ray surveys. We find that the X-ray to optical luminosity ratio of optically selected quasars decreases with increasing optical luminosity. It depends only weakly, if at all, on redshift. However, the distribution function does not properly account for the properties of the X-ray selected Medium Sensitivity Survey sample (MSS). We note that part of the discrepancy could be due to the presence of red, low luminosity quasars in the MSS but not in the optically selected samples. We also summarize some results from a detailed study of the X-ray properties of 64 Seyfert galaxies. None of the spectral fits performed for the brightest 20 required unusually steep spectra, although in many cases the spectral indices were not well constrained. Of the ten objects with good measurements of the absorbing column density, three showed excesses above the galactic value while the remaining seven gave excess columns generally less than 2 × 1020 cm−2 and consistent with zero. Variability studies of the full Seyfert sample showed three objects to be variable on timescales of a few hours. One of these is the Seyfert II Mkn 78.

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⊙.

scholarly journals Differential Imaging of [Fe X] in IC 443

1988 ◽  
Vol 101 ◽  
pp. 407-410
Author(s):  
Larry Brown ◽  
Bruce E. Woodgate ◽  
Robert Petre
Keyword(s):  
Emission Line ◽  
Electron Density ◽  
Temperature Region ◽  
Supernova Remnant ◽  
Coronal Line ◽  
X Ray ◽  
Imaging Camera ◽  
Differential Imaging ◽  
Einstein Observatory ◽  
Gas Pressures

AbstractThis paper presents images of two areas of the supernova remnant IC443 showing emission from the [Fe X] 6374Å red coronal line taken with an emission line differential imaging camera. The areas are in the vicinity of strong soft X-ray emission as observed with the Einstein Observatory. The [Fe X] emission is patchy on the scale of seconds of arc. For the highest emission regions we find an electron density of approximately 100 cm−3 and gas pressures of 108cm−3K. No correlation is found between the X-ray and [Fe X] knots, and the results support a clumpy, multi-temperature region where the [Fe X] knots are balanced between collapse and evaporation.

scholarly journals X-Ray Observations of M87’s Halo

1980 ◽  
Vol 5 ◽  
pp. 689-693
Author(s):  
D. Fabricant ◽  
M. Lecar ◽  
P. Gorenstein
Keyword(s):  
Proportional Counter ◽  
Total Mass ◽  
Precise Determination ◽  
Virgo Cluster ◽  
Field Of View ◽  
Two Dimensional ◽  
X Ray ◽  
Einstein Observatory ◽  
Extended Emission

We briefly describe the soft X-ray image of M87 obtained using the imaging proportional counter aboard the Einstein Observatory. These data provide further strong evidence for the existence of a massive halo of dark matter surrounding M87 and allow a much more precise determination of its mass. Two pointing positions of the satellite were analyzed; one centered on M87, the other 63’ south and 25’ east of M87. The field of view of the imaging proportional counter is 60’ × 60’, and it attains a two dimensional spatial resolution of ˜ 1.5’ in a spectral range spanning 0.1 to 4.5 keV.As previous reports had suggested (Gorenstein et al. 1977; Fabricant et al. 1978), the present observations show M87 to be a strong, very extended, thermal X-ray source with a temperature near 2 keV, surrounded by weaker and still more extended emission from hotter gas associated with the Virgo cluster as a whole (Davison, 1978; Lawrence, 1978). We find M87 to have a total 0.5-4.5 keV X-ray luminosity of about 2 × 1043 ergs/sec, and an extrapolated 2-6 keV luminosity of approximately 1 × 1043 ergs/sec. The total mass of gas inferred from the X-ray measurement exceeds 1012 solar masses.

scholarly journals N49: The Site of a Gamma-ray Burst. Preliminary Results from X-ray Observations

1983 ◽  
Vol 101 ◽  
pp. 573-577
Author(s):  
G. Pizzichini ◽  
T. L. Cline ◽  
U. D. Desai ◽  
B. J. Teegarden ◽  
W. D. Evans ◽  
...  
Keyword(s):  
High Resolution ◽  
Supernova Remnant ◽  
Gamma Ray ◽  
Large Magellanic Cloud ◽  
X Rays ◽  
Radio Image ◽  
Gamma Ray Burst ◽  
X Ray ◽  
Preliminary Results ◽  
Einstein Observatory

The error box of the unusual Gamma-Ray Burst of March 5, 1979 falls completely inside the optical and radio image of the Supernova Remnant N49 in the Large Magellanic Cloud. This region was observed twice in x-rays with the High Resolution Imager of the Einstein Observatory, six weeks and nearly two years after the Gamma-Ray Burst. We show the comparison between the two observations.

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