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

2020 ◽  
Vol 498 (4) ◽  
pp. 5194-5206 ◽  
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.

scholarly journals Detection of extensive optical emission from the extremely radio faint Galactic supernova remnant G182.4+4.3

2019 ◽  
Vol 486 (4) ◽  
pp. 4701-4709 ◽  
Author(s):  
Robert A Fesen ◽  
Jack M M Neustadt ◽  
Thomas G How ◽  
Christine S Black
Keyword(s):  
Supernova Remnant ◽  
Optical Emission ◽  
Galactic Centre ◽  
Wide Field ◽  
Density Region ◽  
Single Filament ◽  
X Ray ◽  
South West ◽  
Low Dispersion ◽  
Western Limb

Abstract Wide-field H α images of the radio faint Galactic supernova remnant G182.4+4.2 reveal a surprisingly extensive and complex emission structure, with an unusual series of broad and diffuse filaments along the remnant’s south-western limb. Deep [O iii] 5007 Å images reveal no appreciable remnant emission with the exception of a single filament coincident with the westernmost of the broad south-west filaments. The near total absence of [O  iii] emission suggests the majority of the remnant’s optical emission arises from relatively slow shocks (≤70 km s−1), consistent with little or no associated X-ray emission. Low-dispersion optical spectra of several regions in the remnant’s main emission structure confirm a lack of appreciable [O iii] emission and indicate [S  ii]/Hα line ratios of 0.73–1.03, consistent with a shock-heated origin. We find G182.4+4.2 to be a relatively large (d ∼ 50 pc at 4 kpc) and much older (age ∼ 40 kyr) supernova remnant than previously estimated, whose weak radio and X-ray emissions are related to its age, low shock velocity, and location in a low-density region some 12 kpc out from the Galactic Centre.

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

2017 ◽  
Vol 608 ◽  
pp. A23 ◽  
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.

scholarly journals Detailed X-ray Observations of the Cygnus Loop

1983 ◽  
Vol 101 ◽  
pp. 253-260
Author(s):  
W. H.-M. Ku ◽  
K. Long ◽  
R. Pisarski ◽  
M. Vartanian
Keyword(s):  
High Resolution ◽  
Proportional Counter ◽  
Supernova Remnant ◽  
Sounding Rocket ◽  
Loop Structure ◽  
High Quality ◽  
Radio Structure ◽  
X Ray ◽  
Cygnus Loop ◽  
Spatially Resolved

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.

scholarly journals The Role of Wide Field X-ray Surveys in Astronomy

2012 ◽  
Vol 10 (H16) ◽  
pp. 669-670
Author(s):  
Richard D. Saxton
Keyword(s):  
High Variability ◽  
Wide Field ◽  
Clusters Of Galaxies ◽  
Tidal Disruption ◽  
X Ray ◽  
Sky Survey ◽  
History Of ◽  
X Ray Background ◽  
Rare Classes

AbstractWe review the history of X-ray sky surveys from the early experiments to the catalogues of 105 sources produced by ROSAT, Chandra and XMM-Newton. At bright fluxes the X-ray sky is shared between stars, accreting binaries and extragalactic sources while deeper surveys are dominated by AGN and clusters of galaxies. The X-ray background, found by the earliest missions, has been largely resolved into discrete sources at soft (0.3-2 keV) energies but at higher energies an important fraction still escapes detection. The possible identification of the missing flux with Compton-thick AGN has been probed in recent years by Swift and Integral.Variability seen in objects observed at different epochs has proved to be an excellent discriminator for rare classes of objects. The comparison of ROSAT All Sky Survey (RASS) and ROSAT pointed observations identified several Novae and high variability AGN as well as initiating the observational study of Tidal Disruption events. More recently the XMM-Newton slew survey, in conjunction with archival RASS data, has detected further examples of flaring objects which have been followed-up in near-real time at other wavelengths.

scholarly journals Image Digitisation of Outflows and the AAO/UKST Hα Survey

1998 ◽  
Vol 15 (1) ◽  
pp. 165-166
Author(s):  
W. J. Zealey ◽  
S. L. Mader
Keyword(s):  
High Resolution ◽  
Emission Line ◽  
Galactic Plane ◽  
Star Forming ◽  
Star Forming Regions ◽  
Sky Survey ◽  
High Resolution Images ◽  
Line Survey

AbstractThe Hα emission-line survey of the Southern Sky to be carried out by the AAO/UKST will provide deep, high resolution images of Galactic Plane sources allowing the detection of new and existing filamentary sources such as Herbig–Haro objects. Used in conjunction with the existing ESO/SERC Southern Sky Survey Plates, the Hα plates will provide us with the opportunity to study the morphology and environment of new and existing star forming regions.

The Wide Field X-ray Telescope Mission—A Digital Sky Survey in X-rays

2010 ◽  
Author(s):  
S. Murray ◽  
R. Giacconi ◽  
A. Ptak ◽  
P. Rosati ◽  
M. Weisskopf ◽  
...  
Keyword(s):  
Wide Field ◽  
X Rays ◽  
X Ray ◽  
Sky Survey

scholarly journals X-ray line emission from the TYCHO supernova remnant

1980 ◽  
Vol 235 ◽  
pp. L9 ◽  
Author(s):  
S. H. Pravdo ◽  
B. W. Smith ◽  
P. A. Charles ◽  
I. R. Tuohy
Keyword(s):  
Supernova Remnant ◽  
Line Emission ◽  
X Ray

scholarly journals A Search for the Signature of the Diffuse Soft X-ray Background in the ROSAT Wide-Field Camera All-Sky Survey

1996 ◽  
Vol 152 ◽  
pp. 289-293
Author(s):  
R.G. West ◽  
R. Willingale ◽  
J.P. Pye ◽  
T.J. Sumner
Keyword(s):  
Charged Particles ◽  
Field Of View ◽  
Wide Field ◽  
Galactic Latitude ◽  
The Sun ◽  
X Ray ◽  
Cosmic Background ◽  
Sky Survey ◽  
Cosmic Abundance ◽  
X Ray Background

We present the results of an attempt to locate the signature of the diffuse soft X-ray background in the ROSAT Wide-Field Camera (WFC) all-sky survey. After removal of non-cosmic background sources (eg. energetic charged particles), the field-of-view integrated count rate in the WFC S1a filter (90–185 eV) shows no consistent variation with Galactic latitude or longitude. We place limits on the signal from the soft X-ray background (SXRB) in the WFC, and show that these limits conflict with the observations of the Wisconsin Sky Survey if the SXRB in this energy range is assumed to be produced by a thermal plasma of cosmic abundance and a temperature T ~ 106 K within d ~ 100 pc of the Sun.

scholarly journals ASCA Sky Survey Observations and the Cosmic X-Ray Background in 2-10 KeV

1998 ◽  
Vol 188 ◽  
pp. 197-200
Author(s):  
H. Inoue ◽  
T. Takahashi ◽  
Y. Ueda ◽  
A. Yamashita ◽  
Y. Ishisaki ◽  
...  
Keyword(s):  
Energy Range ◽  
Galactic Plane ◽  
Galactic Latitude ◽  
High Galactic Latitude ◽  
X Ray ◽  
Sky Survey ◽  
X Ray Background ◽  
Excess Component ◽  
Highly Uniform

The X-ray background in the energy range above 2 keV is highly uniform except for an excess component along the Galactic plane. The excess along the plane is considered to be associated with our Galaxy, whereas the rest of the emission is believed to be of extragalactic origin. In this paper, the X-ray background at high Galactic latitude is discussed and is designated as the CXB (cosmic X-ray background) to distinguish it from the Galactic origin.

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