SUPERNOVA REMNANTS

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SUPERNOVA REMNANTS IN THE MAGELLANIC CLOUDS
JOHN R. DICKEL UNIVERSITY OF NEW MEXICO AND ROSA
MURPHY WILLIAMS COLUMBUS STATE UNIVERSITY
Preliminary SNR tables at http//hoth.ccssc.org/m
csnr/test.php
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SNR IDENTIFICATION

• EXTENDED GENERALLY SHELL -LIKE OBJECT - 0.2 PC
  FOR 1987A TO 158 PC FOR DEM L203
• (1 PC IS 4 ARCSEC AT THE LMC AND 3.4 ARCSEC
  AT THE SMC)
• NON THERMAL RADIO SPECTRA - TYPICAL SPECTRAL
  INDICES, ? -0.5,
• WHERE Sf const f?
• THERMAL X-RAYS - TYPICAL TEMP 1 keV WITH A
  LARGE SPREAD
• CAVEAT - PULSAR WIND NEBULAE HAVE FLATTER RADIO
  SPECTRA AND NON-THERMAL HIGH ENERGY X-RAY TAILS
• S II/ Ha gt 0.4

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?? -0.48
DEM L81
?? 0.0
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X-RAY SPECTRUM OF N103 SNR(usually incorrectly
called N103B)
THIS SHOWS THE THERMAL NATURE OF THE EMISSION
LEWIS, K. ET AL. 2003 ApJ, 582, 770
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SNR MCELS J0521-6542
RATIO
3 COLOR
S II H???????????????
S II/H?
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TYPE CLASSIFICATION OF MAGELLANIC CLOUD SNRS

• CORE COLLAPSE
• PRESENCE OF A PULSAR OR OTHER COMPACT REMAINS
  
• IN A REGION OF YOUNG STARS
• OXYGEN RICH
• TYPE Ia
• XRAY SPECTRA SHOW LINES OF HIGHLY IONIZED
  INTERMEDIATE MASS ELEMENTS
• BALMER DOMINATED IN OPTICAL

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0540-693 - A PROTOTYPE COMPOSITE SNR 50-MSEC
PULSAR, PWN, O-RICH SHELL, ORGANIZED POLARIZATION
IN THE PWN
6-CM RADIO IMAGE
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N157B ANOTHER COMPOSITE
X-ray - contours are 5,10,20,30,40,100,300,600
counts from 0.1-10 keV
Radio - contours are 2,3,4,6,7 nJy/beam
The shell can be seen faintly on the southern
part of the radio image.
The 16-msec X-Ray pulsar is at the center of the
bright X-Ray contours and at the position of the
cross in the radio image.
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SPECTRUM OF N157B
IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS
SPECTRUM FOR THIS OBJECT
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X-RAY SPECTRUM OF N103 SNRNOTE THE MANY LINES OF
HIGHLY IONIZED INTERMEDIATE-MASS ELEMENTS
LEWIS, K. ET AL. 2003 ApJ, 582, 770
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H? LINE PROFILE TOWARD THE TYPE Ia
BALMER-DOMINATED SNR 0519-675
UNEQUILIBRATED VELOCITY 1180 KM/S EQUILIBRATED
1580 KM/S SMITH, R. C. ET AL. 1991, ApJ, 375, 652
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N19 AREA IN THE SMC
JY/BEAM
RED X-RAY CONTOURS
GREYSCALE 13-CM RADIO
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N19 AREA IN THREE WAVELENGTHS
H????????22?cm Radio 1.5 - 8 keV X-ray
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SOME STATISTICS

LMC SMC TOTAL NUMBER OF SNRS
49 19 CORE COLLAPSE
12 4
TYPE Ia
6 1 UNKNOWN
31 14
STANDARD STATISTICS EXPECTED IN IRREGULAR
GALAXIES PREDICT ABOUT 10 TYPE Ia SNe.
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RADIO LUMINOSITY vs DIAMETER FOR LMC SNRs
slope -1.13 corr coef 0.08
1987A
DEM L71
CONCLUSION THERE IS NO CORRELATION OF
LUMINOSITY WITH DIAMETER (IN AGREEMENT WITH
PREVIOUS STUDIES)
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X-RAY - RADIO LUMINOSITIES OF LMC SNRs
DEM L71
DEM L71
slope 0.77 corr. coeff 0.41
CONCLUSION BRIGHTER X-RAY EMISSION MAY, IN
GENERAL, CORRESPOND TO BRIGHTER RADIO BUT THERE
IS NO CLEAR CORRELATION
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1.1 keV 2keV
5 keV
CHANDRA IMAGE OF CAS A
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X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH
SNR N132D, THE BRIGHTEST LMC RADIO SOURCE
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SNR 1E0102-72.3 in the Small Magellanic Cloud
radio X-ray optical in the light of O
III characteristic of oxygen rich SNRs Note that
the radio shell lies outside the X-ray one an
unusual condition in shell SNRs.
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THE MAGELLANIC CLOUD CANDIDATES ARE ABOUT 20
TIMES FURTHER AWAY THAN CAS A SO THE REQUIRED
SENSITIVITY NEEDS TO BE INCREASED BY A FACTOR OF
400.THE INTERNATIONAL X-RAY OBSERVATORY (IXO)
WILL BE ABOUT 100 TIMES MORE SENSITIVE THAN
CHANDRA THEREFORE WITH MODESTLY LONGER EXPOSURES
THE FIRST TASK FOR IXO SHOULD BE TO FIND THE
COOLING NEUTRON STARS IN N132D AND 1E0102-723.
THE REWARD FOR DOING SO A BOTTLE OF EITHER
DICKEL TENNESSEE WHISKEY OR GRUET NEW MEXICO
CHAMPAGNE
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Preliminary SNR tables athttp//hoth.ccssc.org/
mcsnr/test.phpPlease send us references, new
data, etc.We will eventually get proper pages
for each SNR.