High-Frequency Observations and Theoretical Interpretation of Recombination-Line Emission in the Direction of the Supernova Remnant 3c 391

1973 ◽  
Vol 184 ◽  
pp. 83 ◽  
Author(s):  
Diego A. Cesarsky ◽  
Catherine J. Cesarsky
Keyword(s):  
High Frequency ◽  
Supernova Remnant ◽  
Line Emission ◽  
Theoretical Interpretation ◽  
Recombination Line

Observations of high-frequency carbon recombination-line emission in NGC 2024 and IC 1795

1977 ◽  
Vol 218 ◽  
pp. 659 ◽  
Author(s):  
L. J. Rickard ◽  
B. Zuckerman ◽  
P. Palmer ◽  
B. E. Turner
Keyword(s):  
High Frequency ◽  
Line Emission ◽  
Recombination Line

scholarly journals Corrigendum: Classification of Supernova Remnants and HII Regions from their Recombination Line Emission

1973 ◽  
Vol 26 (2) ◽  
pp. 267 ◽  
Author(s):  
JR Dickel ◽  
DK Milne
Keyword(s):  
Supernova Remnants ◽  
Supernova Remnant ◽  
Line Emission ◽  
Hii Regions ◽  
Recombination Line ◽  
Hii Region ◽  
Galactic Source ◽  
Source Number

The galactic source number designations G35'6-0'4 and G35�5-0�0 in Table 1 should be interchanged. Thus G35'6-0'4 is the supernova remnant and G35�5 -0�0 appears to be an HII region. The authors thank Dr. T Velusamy for calling this error to their attention.

OBSERVATION OF 13CO AND METHANOL LINE EMISSION FROM SUPERNOVA REMNANT KES 79

2012 ◽  
Vol 3 (1) ◽  
pp. 19-26 ◽  
Author(s):  
Valery M. Shulga ◽  
S. Y. Zubrin ◽  
V. V. Myshenko
Keyword(s):  
Supernova Remnant ◽  
Line Emission

Radio Recombination Line Emission from Ultracompact HII Regions

1990 ◽  
pp. 83-92 ◽  
Author(s):  
E. Churchwell ◽  
C. M. Walmsley ◽  
D. O. S. Wood ◽  
H. Steppe
Keyword(s):  
Line Emission ◽  
Hii Regions ◽  
Recombination Line ◽  
Radio Recombination Line ◽  
Ultracompact Hii

scholarly journals High-velocity interstellar absorption associated with the supernova remnant W28

2020 ◽  
Vol 495 (3) ◽  
pp. 2909-2920 ◽  
Author(s):  
Adam M Ritchey
Keyword(s):  
High Velocity ◽  
Molecular Cloud ◽  
Supernova Remnant ◽  
Line Emission ◽  
Line Of Sight ◽  
Interstellar Gas ◽  
Lower Velocity ◽  
North East ◽  
The North ◽  
Visible Wavelengths

ABSTRACT We present an analysis of moderately high-resolution optical spectra obtained for the sightline to CD−23 13777, an O9 supergiant that probes high-velocity interstellar gas associated with the supernova remnant W28. Absorption components at both high positive and high negative velocity are seen in the interstellar Na i D and Ca ii H and K lines towards CD−23 13777. The high-velocity components exhibit low Na i/Ca ii ratios, suggesting efficient grain destruction by shock sputtering. High column densities of CH+, and high CH+/CH ratios, for the components seen at lower velocity may be indicative of enhanced turbulence in the clouds interacting with W28. The highest positive and negative velocities of the components seen in Na i and Ca ii absorption towards CD−23 13777 imply that the velocity of the blast wave associated with W28 is at least 150 km s−1, a value that is significantly higher than most previous estimates. The line of sight to CD−23 13777 passes very close to a well-known site of interaction between the supernova remnant and a molecular cloud to the north-east. The north-east molecular cloud exhibits broad molecular line emission, OH maser emission from numerous locations, and bright extended GeV and TeV γ-ray emission. The sightline to CD−23 13777 is thus a unique and valuable probe of the interaction between W28 and dense molecular gas in its environs. Future observations at ultraviolet and visible wavelengths will help to better constrain the abundances, kinematics, and physical conditions in the shocked and quiescent gas along this line of sight.

scholarly journals Atacama Compact Array observations of the pulsar-wind nebula of SNR 0540-69.3

2020 ◽  
Vol 496 (2) ◽  
pp. 1834-1844
Author(s):  
P Lundqvist ◽  
N Lundqvist ◽  
C Vlahakis ◽  
C-I Björnsson ◽  
J R Dickel ◽  
...  
Keyword(s):  
Spectral Index ◽  
Supernova Remnant ◽  
Broad Band ◽  
Line Emission ◽  
Published Data ◽  
Strong Emission ◽  
Band Filter ◽  
Pulsar Wind ◽  
Infrared Data ◽  
Compact Array

ABSTRACT We present observations of the pulsar-wind nebula (PWN) region of SNR 0540-69.3. The observations were made with the Atacama Compact Array (ACA) in Bands 4 and 6. We also add radio observations from the Australia Compact Array at 3 cm. For 1.449–233.50 GHz, we obtain a synchrotron spectrum $F_{\nu } \propto \nu ^{-\alpha _{\nu }}$, with the spectral index αν = 0.17 ± 0.02. To conclude how this joins the synchrotron spectrum at higher frequencies, we include hitherto unpublished AKARI mid-infrared data, and evaluate published data in the ultraviolet (UV), optical, and infrared (IR). In particular, some broad-band filter data in the optical must be discarded from our analysis due to contamination by spectral line emission. For the UV/IR part of the synchrotron spectrum, we arrive at $\alpha _{\nu } = 0.87^{+0.08}_{-0.10}$. There is room for 2.5 × 10−3 M⊙ of dust with a temperature of ∼55 K if there are dual breaks in the synchrotron spectrum, one around ∼9 × 1010 Hz and another at ∼2 × 1013 Hz. The spectral index then changes at ∼9 × 1010 Hz from αν = 0.14 ± 0.07 in the radio to $\alpha _{\nu } = 0.35^{-0.07}_{+0.05}$ in the millimetre-to-far-IR range. The ACA Band 6 data marginally resolve the PWN. In particular, the strong emission $\text{$\sim$} 1\hbox{$.\!\!^{\prime \prime }$}5$ south-west of the pulsar, seen at other wavelengths, and resolved in the 3 cm data with its 0.″8 spatial resolution, is also strong in the millimetre range. The ACA data clearly reveal the supernova remnant shell ∼20–35 arcsec west of the pulsar, and for the shell we derive αν = 0.64 ± 0.05 for the range 8.6–145 GHz.

A Search for Deuterium Recombination-Line Emission from Orion a

1973 ◽  
Vol 184 ◽  
pp. 397 ◽  
Author(s):  
Diego A. Cesarsky
Keyword(s):  
Line Emission ◽  
Recombination Line

Observations of Recombination-Line Emission in the Direction of Two Supernova Remnants

1973 ◽  
Vol 183 ◽  
pp. L143 ◽  
Author(s):  
Diego A. Cesarsky ◽  
Catherine J. Cesarskly
Keyword(s):  
Supernova Remnants ◽  
Line Emission ◽  
Recombination Line

An Attempt to Detect Recombination Line Emission from the Cygnus X-3 Outburst

1972 ◽  
Vol 239 (95) ◽  
pp. 126-126 ◽  
Author(s):  
B. G. LESLIE ◽  
W. A. DENT
Keyword(s):  
Line Emission ◽  
Recombination Line

scholarly journals Broad Balmer line emission and cosmic ray acceleration efficiency in supernova remnant shocks

2013 ◽  
Vol 558 ◽  
pp. A25 ◽  
Author(s):  
G. Morlino ◽  
P. Blasi ◽  
R. Bandiera ◽  
E. Amato
Keyword(s):  
Supernova Remnant ◽  
Line Emission ◽  
Cosmic Ray ◽  
Balmer Line ◽  
Cosmic Ray Acceleration
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