THE 2008 MULTIWAVELENGTH CAMPAIGN OF THE TeV RADIO-GALAXY M 87

2009 ◽  
Vol 18 (10) ◽  
pp. 1493-1498
Author(s):  
◽  
PIERRE COLIN ◽  
MATTHIAS BEILICKE ◽  
FREDERICK DAVIES ◽  
D. E. HARRIS ◽  
...  
Keyword(s):  
High Resolution ◽  
Radio Galaxy ◽  
Time Correlation ◽  
Line Of Sight ◽  
Emission Process ◽  
X Ray ◽  
Cherenkov Telescopes ◽  
Extragalactic Object ◽  
Spatially Resolved ◽  
Radio Band

M 87 is the first and brightest radio galaxy detected in the TeV regime. It is the closest extragalactic object showing variability and the only one that does not have its jet pointing toward the line of sight. The structure of the M 87 jet is spatially resolved in X-ray, optical and radio observations. Time correlation between the TeV flux and emission at other wavelengths provides a unique opportunity to localize the VHE emission process occurring in active galaxy nuclei. For 10 years, M87 has been monitored in the TeV band by imaging air Cherenkov telescopes (IACT) as well as in X-ray, optical and radio bands. In 2008, the three main IACTs, H.E.S.S./MAGIC/VERITAS, coordinated their observations in a joint campaign. In February, high TeV activities with rapid flares have been detected. Contemporaneously, M 87 was observed with high resolution instruments in the X-ray (Chandra) and Radio band (VLBA).

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 Characterization of spatially resolved high resolution x-ray spectrometers for high energy density physics and light source experiments

2014 ◽  
Vol 85 (11) ◽  
pp. 11D612 ◽  
Author(s):  
K. W. Hill ◽  
M. Bitter ◽  
L. Delgado-Aparacio ◽  
P. Efthimion ◽  
N. A. Pablant ◽  
...  
Keyword(s):  
High Resolution ◽  
Energy Density ◽  
Light Source ◽  
High Energy ◽  
High Energy Density ◽  
X Ray ◽  
High Energy Density Physics ◽  
Spatially Resolved

Spatially resolved high resolution x-ray spectroscopy for magnetically confined fusion plasmas (invited)

2008 ◽  
Vol 79 (10) ◽  
pp. 10E302 ◽  
Author(s):  
A. Ince-Cushman ◽  
J. E. Rice ◽  
M. Bitter ◽  
M. L. Reinke ◽  
K. W. Hill ◽  
...  
Keyword(s):  
High Resolution ◽  
Fusion Plasmas ◽  
X Ray ◽  
Spatially Resolved ◽  
Magnetically Confined

scholarly journals The Cycles of Alpha Centauri

2009 ◽  
Vol 5 (S264) ◽  
pp. 146-149
Author(s):  
Thomas R. Ayres
Keyword(s):  
High Resolution ◽  
Triple System ◽  
The Sun ◽  
X Ray ◽  
Spatially Resolved ◽  
Common Basis ◽  
Cosmic Object

AbstractThe main AB pair of the nearby Alpha Centauri triple system has one of the most extensive X-ray records of any cosmic object, stretching over three decades. The primary, α Cen A (G2V), is a near twin of the Sun, with a similarly soft (1–2 MK) corona. The secondary, α Cen B (K1V), is more active than the Sun, with a generally harder coronal spectrum. Here, spatially resolved measurements of the pair by Chandra's High Resolution Camera are compared, on a common basis, with previous pointings from ROSAT and XMM-Newton.

Spatially resolved high-resolution x-ray spectroscopy of high-current plasma-focus discharges

2010 ◽  
Vol 81 (10) ◽  
pp. 10E312 ◽  
Author(s):  
S. Zając ◽  
J. Rzadkiewicz ◽  
O. Rosmej ◽  
M. Scholz ◽  
Zhao Yongtao ◽  
...  
Keyword(s):  
High Resolution ◽  
Plasma Focus ◽  
High Current ◽  
X Ray ◽  
Spatially Resolved

scholarly journals Determining Chemically and Spatially Resolved Atomic Profile of Low Contrast Interface Structure with High Resolution

2015 ◽  
Vol 5 (1) ◽  
Author(s):  
Maheswar Nayak ◽  
P. C. Pradhan ◽  
G. S. Lodha ◽  
A. Sokolov ◽  
F. Schäfers
Keyword(s):  
High Resolution ◽  
Electron Density ◽  
Resonant Scattering ◽  
Interface Structure ◽  
Distribution Profile ◽  
Low Contrast ◽  
X Ray ◽  
Spatially Resolved ◽  
Quantitative Manner ◽  
Non Destructive

Abstract We present precise measurements of atomic distributions of low electron density contrast at a buried interface using soft x-ray resonant scattering. This approach allows one to construct chemically and spatially highly resolved atomic distribution profile upto several tens of nanometer in a non-destructive and quantitative manner. We demonstrate that the method is sensitive enough to resolve compositional differences of few atomic percent in nano-scaled layered structures of elements with poor electron density differences (0.05%). The present study near the edge of potential impurities in soft x-ray range for low-Z system will stimulate the activity in that field.

scholarly journals Modeling of the spatially resolved nonthermal emission from the Vela Jr. supernova remnant

2018 ◽  
Vol 618 ◽  
pp. A155 ◽  
Author(s):  
Iurii Sushch ◽  
Robert Brose ◽  
Martin Pohl
Keyword(s):  
Magnetic Field ◽  
High Resolution ◽  
Supernova Remnants ◽  
High Energy ◽  
Radial Dependence ◽  
Electromagnetic Spectrum ◽  
X Ray ◽  
Spatially Resolved ◽  
Magnetic Field Profile ◽  
Broadband Emission

Vela Jr. (RX J0852.0−4622) is one of just a few known supernova remnants (SNRs) with a resolved shell across the whole electromagnetic spectrum from radio to very-high-energy (>100 GeV; VHE) gamma-rays. Its proximity and large size allow for detailed spatially resolved observations of the source, making Vela Jr. one of the primary sources used for the study of particle acceleration and emission mechanisms in SNRs. High-resolution X-ray observations reveal a steepening of the spectrum toward the interior of the remnant. In this study we aim for a self-consistent radiation model of Vela Jr. which at the same time would explain the broadband emission from the source and its intensity distribution. We solve the full particle transport equation combined with the high-resolution one-dimensional (1D) hydrodynamic simulations (using Pluto code) and subsequently calculate the radiation from the remnant. The equations are solved in the test particle regime. We test two models for the magnetic field profile downstream of the shock: damped magnetic field, which accounts for the damping of strong magnetic turbulence downstream, and transported magnetic field. Neither of these scenarios can fully explain the observed radial dependence of the X-ray spectrum under spherical symmetry. We show, however, that the softening of the spectrum and the X-ray intensity profile can be explained under the assumption that the emission is enhanced within a cone.

scholarly journals Mapping the gas thermodynamic properties of the massive cluster merger MOO J1142+1527 at z = 1.2

2020 ◽  
Vol 228 ◽  
pp. 00026
Author(s):  
F. Ruppin ◽  
R. Adam ◽  
P. Ade ◽  
P. André ◽  
A. Andrianasolo ◽  
...  
Keyword(s):  
Thermodynamic Properties ◽  
Angular Resolution ◽  
Morphological Properties ◽  
Line Of Sight ◽  
High Angular Resolution ◽  
Signal To Noise ◽  
X Ray ◽  
Spatially Resolved ◽  
Multi Wavelength ◽  
Massive Cluster

We present the results of the analysis of the very massive cluster MOO J1142+1527 at a redshift z = 1.2 based on high angular resolution NIKA2 Sunyaev-Zel’dovich (SZ) and Chandra X-ray data. This multi-wavelength analysis enables us to estimate the shape of the temperature profile with unprecedented precision at this redshift and to obtain a map of the gas entropy distribution averaged along the line of sight. The comparison between the cluster morphological properties observed in the NIKA2 and Chandra maps together with the analysis of the entropy map allows us to conclude that MOOJ1142+1527 is an on-going merger hosting a cool-core at the position of the X-ray peak. This work demonstrates how the addition of spatially-resolved SZ observations to low signal-to-noise X-ray data can bring valuable insights on the intracluster medium thermodynamic properties at z > 1.

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