Infrared emission from X-ray and optically emitting regions in the Cygnus Loop supernova remnant

High quality X-ray spectral and imaging observations of the Cygnus Loop have been obtained with three different instruments. The High Resolution Imager (HRI) on the Einstein Observatory was used to obtain arcsecond resolution images of select bright regions in the Cygnus Loop which permit detailed comparisons between the X-ray, optical, and radio structure of the Loop. The Imaging Proportional Counter (IPC) on the Einstein Observatory was used to obtain an arcminute resolution map of essentially the full Loop structure. Finally, an Imaging Gas Scintillation Proportional Counter (IGSPC), carried aloft by a sounding rocket last fall, obtained modest resolution, spatially resolved spectrophotometry of the Cygnus Loop. An X-ray map of the Loop in the energy of the 0 VIII line was obtained. These data combine to yield a very powerful probe of the abundance, temperature, and density distribution of material in the supernova remnant, and in the interstellar medium.

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Soft X‐Ray Spectroscopy of the Cygnus Loop Supernova Remnant

The Astrophysical Journal ◽

10.1086/587936 ◽

2008 ◽

Vol 680 (1) ◽

pp. 328-335 ◽

Cited By ~ 9

Author(s):

R. L. McEntaffer ◽

W. Cash

Keyword(s):

Supernova Remnant ◽

X Ray ◽

Cygnus Loop

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SOFT X-RAY SPECTROSCOPY OF THE CYGNUS LOOP SUPERNOVA REMNANT

The Astrophysical Journal ◽

10.1088/0004-637x/766/1/51 ◽

2013 ◽

Vol 766 (1) ◽

pp. 51 ◽

Cited By ~ 4

Author(s):

Phil Oakley ◽

Randall McEntaffer ◽

Webster Cash

Keyword(s):

Supernova Remnant ◽

X Ray ◽

Cygnus Loop

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Studies of the X-ray emission from supernova remnants

Proceedings of the Royal Society of London Series A - Mathematical and Physical Sciences ◽

10.1098/rspa.1974.0162 ◽

1974 ◽

Vol 340 (1623) ◽

pp. 423-437

Keyword(s):

Supernova Remnants ◽

Column Density ◽

Supernova Remnant ◽

Crab Nebula ◽

Lower Intensity ◽

X Ray ◽

Cassiopeia A ◽

Cygnus Loop ◽

A Value ◽

The Crab Nebula

Supernova remnants are now recognized as a class of soft X-ray emitting-objects. The evolution of a remnant’s X-ray emission is discussed and a number of possible X-ray emission mechanisms are described. The spectrum of the Crab Nebula has been studied with Copernicus. The data have been used to derive a value of the gas column density of the interstellar medium. The X-ray structure and spectrum of the remnant Cassiopeia. A have been investigated and the results are presented. A high resolution X-ray map of the Puppis A supernova remnant has been obtained and the interpretation of the X-ray structure is discussed. X-ray emission has been detected from the pulsar PSR 08 33-45. This observation is compared with data obtained from the Uhuru satellite in order to derive the gas column density to the source. Weak soft X-ray emission has been detected from the Cygnus Loop in the regions expected but a t a lower intensity – a search for regions of higher intensity is continuing. A programme to identify known radio remnants as X-ray emitters is in progress and the results obtained so far are reported.

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An X-ray and optical study of the interaction of the Cygnus Loop supernova remnant with an interstellar cloud

The Astrophysical Journal ◽

10.1086/175651 ◽

1995 ◽

Vol 444 ◽

pp. 787 ◽

Cited By ~ 34

Author(s):

James R. Graham ◽

N. A. Levenson ◽

J. J. Hester ◽

J. C. Raymond ◽

R. Petre

Keyword(s):

Supernova Remnant ◽

Interstellar Cloud ◽

Optical Study ◽

X Ray ◽

Cygnus Loop

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ASCA Observation of the Cygnus Loop Supernova Remnant

Symposium - International Astronomical Union ◽

10.1017/s0074180900115001 ◽

1998 ◽

Vol 188 ◽

pp. 254-255

Author(s):

E. Miyata ◽

H. Tsunemi

Keyword(s):

Surface Brightness ◽

Supernova Remnant ◽

High Surface ◽

Apparent Size ◽

High Surface Brightness ◽

X Ray ◽

Cygnus Loop ◽

Spatially Resolved ◽

Absorption Features

The Cygnus Loop is the prototype shell-like supernova remnant (SNR) and one of the brighest SNRs in X-ray wavelength. We have observed the entire Cygnus Loop with the X-ray satellite, ASCA. Its large apparent size, high surface brightness, and low absorption features have made the Cygnus Loop to be an ideal target for the study of the spatially-resolved spectroscopic structure in detail. Part of this work was summarized in Miyata (1996). Here, we present the first X-ray image of the Cygnus Loop obtained with ASCA.

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Morphology and Physics of Supernova Remnants

Highlights of Astronomy ◽

10.1017/s1539299600008960 ◽

1992 ◽

Vol 9 ◽

pp. 223-228 ◽

Cited By ~ 1

Author(s):

B. Aschenbach

Keyword(s):

Survey Data ◽

Supernova Remnants ◽

Supernova Remnant ◽

Thermal Pressure ◽

X Ray ◽

Cygnus Loop ◽

Sky Survey ◽

Pressure Equilibrium ◽

Spectrally Resolved

AbstractSpectrally resolved X-ray images of the Cygnus Loop and the Vela supernova remnant have been obtained during the ROSAT all sky survey. The remnants show highly filamentary brightness distributions. Temperatures between 1·106 K and 10·106 K have been measured. Both remnants show significant deviation from thermal pressure equilibrium. The highest pressure excursions of up to a factor of 50 are associated with the X-ray brightest filaments. Pressure variations are expected for very recently shocked clouds, on a smaller scale though. In a limited search of the all sky survey data 14 extended objects have been found, which have tentatively been identified as previously unknown supernova remnants. A total number of ~ 60 new remnants are expected from the analysis of the full sky.

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Some recent observations of supernova remnants emitting X-rays

Proceedings of the Royal Society of London Series A - Mathematical and Physical Sciences ◽

10.1098/rspa.1979.0054 ◽

1979 ◽

Vol 366 (1726) ◽

pp. 311-327

Keyword(s):

Supernova Remnants ◽

Supernova Remnant ◽

X Rays ◽

Coronal Line ◽

Crystal Spectrometer ◽

X Ray ◽

Cygnus Loop ◽

The Galaxy ◽

Two Distinct Temperatures ◽

Line Observation

There are currently believed to be 13 X-ray sources which can be fairly confidently identified with galactic supernova remnants. All of these sources are thought to be at reasonably small distances, thus supporting the view that absorption in the interstellar medium prevents us from seeing the more distant galactic remnants with the level of sensitivity currently available from soft X-ray instrumentation. Of the older remnants, the Cygnus Loop and Puppis-A are discussed in the light of recent observations. Several mapping experiments show that the Cygnus Loop exhibits a shell-like structure in X-rays, though with considerable fine structure. From these experiments, it is still not clear how uniform is the temperature over the X-ray emitting region. In addition, results from a crystal spectrometer are described which imply that the temperature may be higher than had been previously determined from proportional counter observations. Results from observations of Puppis-A are presented. These imply that two distinct temperatures exist in this source. It is argued that this may represent the interaction of the expanding shock front with a relatively dense interstellar cloud. The sources W44 and γ -Cygni supernova remnant are discussed and it is suggested that these may now be regarded as members of the class of confirmed X-ray emitting supernova remnants. Finally, an optical coronal line observation of the remnant N49 in the L. M. C. is considered, and it is suggested that this source is a likely candidate to be detected as the first X-ray emitting supernova remnant outside the galaxy.

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Discovery of recombining plasma inside the extended gamma-ray supernova remnant HB9

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2461 ◽

2019 ◽

Vol 489 (3) ◽

pp. 4300-4310 ◽

Cited By ~ 5

Author(s):

A Sezer ◽

T Ergin ◽

R Yamazaki ◽

H Sano ◽

Y Fukui

Keyword(s):

Supernova Remnant ◽

Gamma Ray ◽

Radio Continuum ◽

Continuum Emission ◽

Large Area ◽

Imaging Spectrometer ◽

X Ray ◽

East Region ◽

X Ray Imaging ◽

Collisional Ionization

ABSTRACT We present the results from the Suzaku X-ray Imaging Spectrometer observation of the mixed-morphology supernova remnant (SNR) HB9 (G160.9+2.6). We discovered recombining plasma (RP) in the western Suzaku observation region and the spectra here are well described by a model having collisional ionization equilibrium (CIE) and RP components. On the other hand, the X-ray spectra from the eastern Suzaku observation region are best reproduced by the CIE and non-equilibrium ionization model. We discuss possible scenarios to explain the origin of the RP emission based on the observational properties and concluded that the rarefaction scenario is a possible explanation for the existence of RP. In addition, the gamma-ray emission morphology and spectrum within the energy range of 0.2–300 GeV are investigated using 10 yr of data from the Fermi Large Area Telescope (LAT). The gamma-ray morphology of HB9 is best described by the spatial template of radio continuum emission. The spectrum is well fit to a log-parabola function and its detection significance was found to be 25σ. Moreover, a new gamma-ray point source located just outside the south-east region of the SNR’s shell was detected with a significance of 6σ. We also investigated the archival H i and CO data and detected an expanding shell structure in the velocity range of $-10.5$ and $+1.8$ km s−1 that is coinciding with a region of gamma-ray enhancement at the southern rim of the HB9 shell.

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