Spatially Resolved X-Ray Spectroscopy of Kepler’s Supernova Remnant: Distinct Properties of the Circumstellar Medium and the Ejecta

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.

Download Full-text

Detailed X-Ray Mapping of the Shocked Ejecta and Circumstellar Medium in the Galactic Core-collapse Supernova Remnant G292.0+1.8

The Astrophysical Journal ◽

10.3847/1538-4357/aafafd ◽

2019 ◽

Vol 872 (1) ◽

pp. 31 ◽

Cited By ~ 2

Author(s):

Jayant Bhalerao ◽

Sangwook Park ◽

Andrew Schenck ◽

Seth Post ◽

John P. Hughes

Keyword(s):

Supernova Remnant ◽

Core Collapse ◽

X Ray ◽

Core Collapse Supernova ◽

Circumstellar Medium

Download Full-text

Probing the effects of hadronic acceleration at the SN 1006 shock front

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313009642 ◽

2013 ◽

Vol 9 (S296) ◽

pp. 315-319

Author(s):

Marco Miceli ◽

F. Bocchino ◽

A. Decourchelle ◽

G. Maurin ◽

J. Vink ◽

...

Keyword(s):

Particle Acceleration ◽

Spectral Analysis ◽

Supernova Remnants ◽

Supernova Remnant ◽

Ambient Medium ◽

Cosmic Ray ◽

X Ray ◽

Spatially Resolved ◽

Large Program ◽

Post Shock

AbstractSupernova remnant shocks are strong candidates for being the source of energetic cosmic rays and hadron acceleration is expected to increase the shock compression ratio, providing higher post-shock densities. We exploited the deep observations of the XMM-Newton Large Program on SN 1006 to verify this prediction. Spatially resolved spectral analysis led us to detect X-ray emission from the shocked ambient medium in SN 1006 and to find that its density significantly increases in regions where particle acceleration is efficient. Our results provide evidence for the effects of acceleration of cosmic ray hadrons on the post-shock plasma in supernova remnants.

Download Full-text

XMM-Newton observations of the non-thermal supernova remnant HESS J1731−347 (G353.6-0.7)

Astronomy and Astrophysics ◽

10.1051/0004-6361/201730983 ◽

2017 ◽

Vol 608 ◽

pp. A23 ◽

Cited By ~ 9

Author(s):

V. Doroshenko ◽

G. Pühlhofer ◽

A. Bamba ◽

F. Acero ◽

W. W. Tian ◽

...

Keyword(s):

Supernova Remnant ◽

Galactic Plane ◽

Thermal Power ◽

X Rays ◽

Absorption Column ◽

X Ray ◽

Spatially Resolved ◽

Absorbing Material ◽

First Time ◽

X Ray Absorption

We report on the analysis of XMM-Newton observations of the non-thermal shell-type supernova remnant HESS J1731−347 (G353.6-0.7). For the first time the complete remnant shell has been covered in X-rays, which allowed direct comparison with radio and TeV observations. We carried out a spatially resolved spectral analysis of XMM-Newton data and confirmed the previously reported non-thermal power-law X-ray spectrum of the source with negligible variations of spectral index across the shell. On the other hand, the X-ray absorption column is strongly variable and correlates with the CO emission thus confirming that the absorbing material must be in the foreground and reinforcing the previously suggested lower limit on distance. Finally, we find that the X-ray emission of the remnant is suppressed towards the Galactic plane, which points to lower shock velocities in this region, likely due to the interaction of the shock with the nearby molecular cloud.

Download Full-text

Discovery of a jet-like structure with overionized plasma in the SNR IC 443

Astronomy and Astrophysics ◽

10.1051/0004-6361/201832733 ◽

2018 ◽

Vol 615 ◽

pp. A157 ◽

Cited By ~ 6

Author(s):

Emanuele Greco ◽

Marco Miceli ◽

Salvatore Orlando ◽

Giovanni Peres ◽

Eleonora Troja ◽

...

Keyword(s):

Supernova Remnant ◽

Supernova Explosion ◽

Original Position ◽

Core Collapse ◽

Complex Environment ◽

Energy Bands ◽

X Ray ◽

Spatially Resolved ◽

Pulsar Wind ◽

The Relationship

Context. IC 443 is a supernova remnant (SNR) located in a quite complex environment since it interacts with nearby clouds. Indications for the presence of overionized plasma have been found though the possible physical causes of overionization are still debated. Moreover, because of its peculiar position and proper motion, it is not clear if the pulsar wind nebula (PWN) within the remnant is the relic of the IC 443 progenitor star or just a rambling one seen in projection on the remnant. Aims. Here we address the study of IC 443 plasma in order to clarify the relationship PWN-remnant, the presence of overionization and the origin of the latter. Methods. We analyzed two XMM-Newton observations producing background-subtracted, vignetting-corrected and mosaicked images in two different energy bands and we performed a spatially resolved spectral analysis of the X-ray emission. Results. We identified an elongated (jet-like) structure with Mg-rich plasma in overionization. The head of the jet is interacting with a molecular cloud and the jet is aligned with the position of the PWN at the instant of the supernova explosion. Interestingly, the direction of the jet of ejecta is somehow consistent with the direction of the PWN jet. Conclusions. Our discovery of a jet of ejecta in IC 443 enlarge the sample of core-collapse SNRs with collimated ejecta structures. IC 443’s jet is the first one which shows overionized plasma, possibly associated with the adiabatic expansion of ejecta. The match between the jet’s direction and the original position of the PWN strongly supports the association between the neutron star and IC 443.

Download Full-text

G107.0+9.0: a new large optically bright, radio, and X-Ray faint galactic supernova remnant in Cepheus

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2765 ◽

2020 ◽

Vol 498 (4) ◽

pp. 5194-5206 ◽

Cited By ~ 1

Author(s):

Robert A Fesen ◽

Kathryn E Weil ◽

John C Raymond ◽

Laurent Huet ◽

Martin Rusterholz ◽

...

Keyword(s):

Supernova Remnant ◽

Galactic Plane ◽

Line Emission ◽

Wide Field ◽

X Ray ◽

Spatially Resolved ◽

Sky Survey ◽

Line Survey ◽

Low Dispersion ◽

Western Limb

ABSTRACT Wide-field H α images of the Galactic plane have revealed a new supernova remnant (SNR) nearly 3 deg in diameter centred at l = 107.0, b = +9.0. Deep and higher resolution H α and [O iii] 5007 Å images show dozens of H α filaments along the remnant’s northern, western, and southwestern limbs, but few [O iii] bright filaments. The nebula is well detected in the H α Virginia Tech Spectral-Line Survey images, with many of its brighter filaments even visible on Digital Sky Survey images. Low-dispersion spectra of several filaments show either Balmer dominated, non-radiative filaments, or the more common SNR radiative filaments with [S II]/H α ratios above 0.5, consistent with shock-heated line emission. Emission line ratios suggest shock velocities ranging from ≤70 km s−1 along its western limb to ≃ 100 km s−1 along its northwestern boundary. While no associated X-ray emission is seen in ROSAT images, faint 1420 MHz radio emission appears coincident with its western and northern limbs. Based on an analysis of the remnant’s spatially resolved H α and [O iii] emissions, we estimate the remnant’s distance at ∼1.5−2.0 kpc implying a physically large (dia. = 75−100 pc) and old (90−110 × 103 yr) SNR in its post-Sedov radiative phase of evolution expanding into a low-density interstellar medium (n0 = 0.05−0.2 cm−3) and lying some 250−300 pc above the Galactic plane.

Download Full-text

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.

Download Full-text

An X-ray Pulsar, Metal-rich Ejecta, and Shocked Ambient Medium in the Supernova Remnant G292.0+1.8

Symposium - International Astronomical Union ◽

10.1017/s0074180900180969 ◽

2004 ◽

Vol 218 ◽

pp. 199-202

Author(s):

John P. Hughes ◽

Robert B. Friedman ◽

Patrick Slane ◽

Sangwook Park

Keyword(s):

High Resolution ◽

Supernova Remnant ◽

Ambient Medium ◽

Compact Object ◽

Optical Counterpart ◽

Reverse Shock ◽

X Ray ◽

Pulsar Wind ◽

Circumstellar Medium

We report the discovery of pulsed X-ray emission from the compact object CXOU J112439.1-591620 within the Galactic supernova remnant G292.0+1.8 using the High Resolution Camera on the Chandra X-Ray Observatory. The X-ray period is consistent with the extrapolation of the radio period and spindown rate of PSR J1124−5916. The X-ray pulse is single peaked and broad. There is no optical counterpart to a limit of MV ∼ 26. The pressure in the pulsar wind nebula is considerably less than that in the reverse-shock-heated ejecta and circumstellar medium, indicating that the reverse shock has not yet begun to interact with the nebula.

Download Full-text

The Structure of the Oxygen-rich Supernova Remnant G292.0+1.8 from [ITAL]Chandra[/ITAL] X-Ray Images: Shocked Ejecta and Circumstellar Medium

The Astrophysical Journal ◽

10.1086/338861 ◽

2002 ◽

Vol 564 (1) ◽

pp. L39-L43 ◽

Cited By ~ 56

Author(s):

Sangwook Park ◽

Peter W. A. Roming ◽

John P. Hughes ◽

Patrick O. Slane ◽

David N. Burrows ◽

...

Keyword(s):

Supernova Remnant ◽

X Ray ◽

Circumstellar Medium

Download Full-text

Layered and ion implantation specimens as possible reference materials for the electron-probe microanalysis

Proceedings, annual meeting, Electron Microscopy Society of America ◽

10.1017/s0424820100132893 ◽

1992 ◽

Vol 50 (2) ◽

pp. 1652-1653

Author(s):

G. Remond ◽

R.H. Packwood ◽

C. Gilles ◽

S. Chryssoulis

Keyword(s):

Ion Implantation ◽

Reference Materials ◽

Analytical Techniques ◽

Thin Film Deposition ◽

Film Deposition ◽

X Ray ◽

Spatially Resolved ◽

Analytical Expressions ◽

Original Approach ◽

Depth Concentration

Merits and limitations of layered and ion implanted specimens as possible reference materials to calibrate spatially resolved analytical techniques are discussed and illustrated for the case of gold analysis in minerals by means of x-ray spectrometry with the EPMA. To overcome the random heterogeneities of minerals, thin film deposition and ion implantation may offer an original approach to the manufacture of controlled concentration/ distribution reference materials for quantification of trace elements with the same matrix as the unknown.In order to evaluate the accuracy of data obtained by EPMA we have compared measured and calculated x-ray intensities for homogeneous and heterogeneous specimens. Au Lα and Au Mα x-ray intensities were recorded at various electron beam energies, and hence at various sampling depths, for gold coated and gold implanted specimens. X-ray intensity calculations are based on the use of analytical expressions for both the depth ionization Φ (ρz) and the depth concentration C (ρz) distributions respectively.

Download Full-text