scholarly journals An Atomic and Molecular Study of the Interstellar Medium Around the Supernova Remnant RCW 103

2006 ◽  
Vol 23 (2) ◽  
pp. 69-75 ◽  
Author(s):  
Sergio A. Paron ◽  
Estela M. Reynoso ◽  
Cormac Purcell ◽  
Gloria M. Dubner ◽  
Anne Green
Keyword(s):  
Interstellar Medium ◽  
Shock Front ◽  
Supernova Remnant ◽  
Molecular Study ◽  
Rotational Transition ◽  
Molecular Feature ◽  
Infrared Observations ◽  
Southern Border ◽  
Co Emission ◽  
Compact Array

AbstractWe report on the detection of HCO+ and 12CO emission in the rotational transition J = 1–0 in the vicinity of the shock front at the southern border of the supernova remnant RCW 103, where previous infrared observations suggest an interaction with a molecular cloud. The observations were carried out with the Australian Millimeter Radiotelescope at Mopra. We observed a depletion of HCO+ behind the supernova shock front. In addition, we studied the interstellar medium over an extended region towards RCW 103 based on archival λ 21 cm Hı line observations from the Australia Telescope Compact Array (ATCA) and the Parkes Telescope. No atomic gas was observed in emission in coincidence with the molecular feature. This absence was interpreted in terms of self-absorption processes.

G54.4–0.3: Interaction of a Supernova Remnant with the Interstellar Medium

1991 ◽  
Vol 9 (2) ◽  
pp. 312-312
Author(s):  
Norbert Junkes
Keyword(s):  
Interstellar Medium ◽  
Radial Velocity ◽  
Stellar Wind ◽  
Supernova Remnant ◽  
Radio Continuum ◽  
Model Calculations ◽  
Physical Connection ◽  
Distance Model ◽  
Co Emission

AbstractIn our study of the extended supernova remnant G54.4–0.3, we find a CO emission shell at about 40km s−1 radial velocity, in striking alignment with the radio continuum shell. The correspondence in position and size argues strongly for a physical connection, and allows derivation of the kinematic distance as well as the mass and density of the CO shell. The correlation with an OB association supports the value derived for the kinematic distance. Model calculations suggest that the formation of the CO shell results from a stellar wind and that the supernova remnant has expanded into the wind bubble located inside the shell.

scholarly journals Molecular environments of the supernova remnant G359.1−0.5

2020 ◽  
Vol 493 (3) ◽  
pp. 3947-3955 ◽  
Author(s):  
L K Eppens ◽  
E M Reynoso ◽  
J Lazendic-Galloway ◽  
J A Combi ◽  
J F Albacete-Colombo
Keyword(s):  
Molecular Structure ◽  
Supernova Remnant ◽  
Molecular Study ◽  
Molecular Gas ◽  
Molecular Line ◽  
Γ Rays ◽  
Γ Ray ◽  
Co Emission ◽  
Co Observations ◽  
Morphological Correlation

ABSTRACT We report new CO observations and a detailed molecular-line study of the mixed morphology supernova remnant G359.1−0.5, which contains six OH (1720 MHz) masers along the radio shell, indicative of shock-cloud interaction. Observations of 12CO and 13CO J:1–0 lines were performed in a ∼38 × 38 arcmin area with the on-the-fly technique using the Kit Peak 12 Meter telescope. The molecular study has revealed the existence of a few clumps with densities ∼103 cm−3 compatible in velocity and position with the OH (1720 MHz) masers. These clumps, in turn, appear to be part of a larger, elongated molecular structure ∼34 arcmin long extending between −12.48 and +1.83 km s−1, adjacent to the western edge of the radio shell. According to the densities and relative position with respect to the masers, we conclude that the CO clouds depict unshocked gas, as observed in other remnants with OH (1720 MHz) masers. In addition, we investigated the distribution of the molecular gas towards the adjacent γ-ray source HESS J1745-303 (Aharonian et al. 2006) but could not find any morphological correlation between the γ-rays and the CO emission at any velocity in this region.

scholarly journals A Galactic dust devil: far-infrared observations of the Tornado supernova remnant candidate

2020 ◽  
Vol 499 (4) ◽  
pp. 5665-5678
Author(s):  
H Chawner ◽  
A D P Howard ◽  
H L Gomez ◽  
M Matsuura ◽  
F Priestley ◽  
...  
Keyword(s):  
Radio Emission ◽  
Supernova Remnant ◽  
Far Infrared ◽  
Large Mass ◽  
Dust Devils ◽  
Infrared Observations ◽  
X Ray ◽  
Ss 433 ◽  
Multiple Regions ◽  
Tail Structure

ABSTRACT We present complicated dust structures within multiple regions of the candidate supernova remnant (SNR) the ‘Tornado’ (G357.7–0.1) using observations with Spitzer and Herschel. We use point process mapping, ppmap, to investigate the distribution of dust in the Tornado at a resolution of 8 arcsec, compared to the native telescope beams of 5–36 arcsec. We find complex dust structures at multiple temperatures within both the head and the tail of the Tornado, ranging from 15 to 60 K. Cool dust in the head forms a shell, with some overlap with the radio emission, which envelopes warm dust at the X-ray peak. Akin to the terrestrial sandy whirlwinds known as ‘dust devils’, we find a large mass of dust contained within the Tornado. We derive a total dust mass for the Tornado head of 16.7 $\rm M_{\odot }$, assuming a dust absorption coefficient of κ300 = 0.56 $\rm m^2\, kg^{-1}$, which can be explained by interstellar material swept up by a SNR expanding in a dense region. The X-ray, infrared, and radio emission from the Tornado head indicate that this is a SNR. The origin of the tail is more unclear, although we propose that there is an X-ray binary embedded in the SNR, the outflow from which drives into the SNR shell. This interaction forms the helical tail structure in a similar manner to that of the SNR W50 and microquasar SS 433.

scholarly journals The W75 — Cygnus - X IRAS loop:- OB - ‘Bubble’ or SNR?

1991 ◽  
Vol 147 ◽  
pp. 511-512
Author(s):  
D. Ward-Thompson ◽  
E. I. Robson
Keyword(s):  
Spherical Shell ◽  
Shock Front ◽  
Stellar Wind ◽  
Supernova Remnant ◽  
Dust Emission ◽  
Ob Stars ◽  
Wind Action

IRAS Calibrated Raw Detector Data (CRDD) are presented of a part of the Cygnus-X region, incorporating W75, DR21 and W75N, and a previously unknown loop of dust emission is observed. This loop is interpreted as a spherical shell-like shock front, and two alternative explanations for its origin are explored — a wind-blown bubble around an OB association, and an old supernova remnant. The arguments for each are outlined, and it is deduced that there are insufficient OB stars old enough to have formed the loop by combined stellar wind action, although a SNR appears consistent with the data.

scholarly journals Heating of the Interstellar Medium by Supernova Remnants

1983 ◽  
Vol 101 ◽  
pp. 385-392
Author(s):  
Donald P. Cox
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Supernova Remnant ◽  
Low Density ◽  
The Sun ◽  
X Ray ◽  
Interstellar Material ◽  
X Ray Background

We observe the heating of interstellar material in young supernova remnants (SNR). In addition, when analyzing the soft X-ray background we find evidence for large isolated regions of apparently hot, low density material. These, we infer, may have been heated by supernovae. One such region seems to surround the Sun. This has been modeled as a supernova remnant viewed from within. The most reasonable parameters are ambient density no ~ 0.004 cm−3, radius of about 100 pc, age just over 105 years (Cox and Anderson 1982).

scholarly journals The carbon monoxide distribution in the inner Galaxy

1985 ◽  
Vol 106 ◽  
pp. 207-208
Author(s):  
T. M. Bania
Keyword(s):  
Carbon Monoxide ◽  
Kinetic Energy ◽  
Large Deviations ◽  
Galactic Center ◽  
Rotational Transition ◽  
Circular Motion ◽  
Latitude Distribution ◽  
Co Emission

The latitude distribution of the emission from the 12CO J=1→0 rotational transition has been surveyed for the region 350° ≤ 1 ≤ 25° at b = 0′, ±10′ and ±20′. Most of the 12CO emission in the inner Galaxy, the region extending from the galactic center to 4 kpc radius, is produced by three large and massive objects: the nuclear disk/bar, the 3-kpc arm and the “+135 km s-1 feature”. These structures all have observed HI counterparts and each shows extremely large deviations (50–180 km s-1) from circular motion. Observations of 13CO in selected directions show that the two structures outside the nuclear disk each span at least 2 kpc in length and that together they imply ≥ 1055 ergs in kinetic energy of expansion away from the galactic nucleus.

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.

scholarly journals Mm CO observation of the old nova NQ Vul

1990 ◽  
Vol 122 ◽  
pp. 199-199
Author(s):  
J. S. Albinson ◽  
A. Evans
Keyword(s):  
Interstellar Medium ◽  
Rotational Transition ◽  
Millimetre Wave ◽  
University Of Texas ◽  
Evolutionary Phase ◽  
Mass Estimate ◽  
The University ◽  
Nova Outbursts ◽  
Broad Feature

AbstractWe have observed the old nova NQ Vul in the J = 2 → 1 rotational transition of 12CO at 230.5 GHz at the University of Texas Millimetre Wave Observatory. The spectrum shows narrow features which clearly arise in the local interstellar medium. However these local features are superimposed on a broad feature which peaks at ~ 63 mK. This feature is centred on velocity VLSR ≃ 26 ± 9 km s−1–consistent with that expected for NQ Vul–and has FWHM 80 ± 20 km s−1. The peak antenna temperature corresponds to an integrated flux of 3.2 × 10−15 erg s−1 cm−2.Assuming LTE and a distance of 1.2 kpc the mass of CO is ~ 10−6M⊙ if the line is optically thin. The CO mass is comparable with the total mass ejected in 1976 (4) so the CO we detect at millimetre wavelengths has nothing to do with the 1976 outburst. If the CO/H ratio in the emitting material is similar to that in the interstellar medium (2), the total mass is ~ 0.6 M⊙.The CO mass rules out an origin both in the 1976 outburst and in the post-outburst phase: the CO must have originated in material ejected by the NQ Vul system prior to the 1976 outburst. There are two possibilities. First, the CO may have formed in material accumulated following a large number of nova outbursts. Second, the CO may have been present, or formed, in material ejected by the NQ Vul system during a previous evolutionary phase. The deduced mass is comparable to the mass of CO seen around planetary nebulae (3); the outflow velocity (~ 40 km s−1) would also be in line with this interpretation.In either case, the above mass estimate of 0.6 M⊙ (based on the interstellar CO/H ratio) is likely to be an upper limit as we would expect an enhancement of heavy elements in any ejected material. A determination of 12C/13C and other isotopic ratios would be valuable to pin down the origin of the CO.

scholarly journals G18.95-1.1, A Composite Supernova Remnant Interacting with the Ambient Interstellar Medium

1988 ◽  
Vol 101 ◽  
pp. 253-256
Author(s):  
E. Fürst ◽  
W. Reich ◽  
E. Hummel ◽  
Y. Sofue
Keyword(s):  
Spectral Line ◽  
Interstellar Medium ◽  
Radio Source ◽  
Supernova Remnant ◽  
Radio Continuum ◽  
New Radio ◽  
Galactic Radio

AbstractNew radio continuum and spectral line observations of the Galactic radio source G18.95-1.1 are reported. The distance to G18.95-1.1 is 2 kpc as derived from HI-21 cm spectral line observations. These data also indicate an interaction with the interstellar medium. The radio continuum observations classify G18.95-1.1 as a composite supernova remnant.

scholarly journals Chandra Study of the Central Object Associated with the Supernova Remnant MSH 11–62

2004 ◽  
Vol 218 ◽  
pp. 203-206
Author(s):  
Ilana Harrus ◽  
Joseph P. Bernstein ◽  
Patrick O. Slane ◽  
Bryan Gaensler ◽  
John P. Hughes ◽  
...  
Keyword(s):  
Neutron Star ◽  
Radio Emission ◽  
Supernova Remnant ◽  
Loss Rate ◽  
Thermal Emission ◽  
Compact Object ◽  
Small Region ◽  
Compact Source ◽  
Synchrotron Nebula ◽  
Compact Array

We present results from our analysis of Chandra data on the supernova remnant MSH 11–62 (also known as G291.0−0.1). Our previous ASCA analysis showed that MSH 11–62 is most likely a composite remnant whose strong non-thermal emission is powered by a compact object, most probably a pulsar. The present analysis confirms in a spectacular fashion the earlier detection of a compact source. The Chandra data reveal a small region with a hard non-thermal spectrum located at the tip of the central radio emission seen in data taken at the Australia Telescope Compact Array (ATCA). This source is likely the young rapidly rotating neutron star powering the synchrotron nebula in MSH 11–62. Compared to other young rotation-powered pulsars the Chandra specrum of MSH 11–62 implies an energy loss rate of Ė ∼ 5 × 1036 ergs s−1.

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