1. 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/mcsnr/test.php

2. 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 S f = 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 > 0.4

3.  = -0.48 DEM L81  = 0.0

4. X-RAY SPECTRUM OF N103 SNR (usually incorrectly called N103B) LEWIS, K. ET AL. 2003 ApJ, 582, 770 THIS SHOWS THE THERMAL NATURE OF THE EMISSION

5. SNR MCELS J0521-6542 [S II] H  [S II]/H  RATIO3 COLOR

6. 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

7. 0540-693 - A PROTOTYPE COMPOSITE SNR 50-MSEC PULSAR, PWN, O-RICH SHELL, ORGANIZED POLARIZATION IN THE PWN 6-CM RADIO IMAGE

8. N157B ANOTHER COMPOSITE X-ray - contours are 5,10,20,30,40,100,300,6 00 counts from 0.1-10 keV 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. Radio - contours are 2,3,4,6,7 nJy/beam The shell can be seen faintly on the southern part of the radio image.

9. SPECTRUM OF N157B IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS SPECTRUM FOR THIS OBJECT

10. X-RAY SPECTRUM OF N103 SNR NOTE THE MANY LINES OF HIGHLY IONIZED INTERMEDIATE-MASS ELEMENTS LEWIS, K. ET AL. 2003 ApJ, 582, 770

11. 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

12. N19 AREA IN THE SMC RED: X-RAY CONTOURS GREYSCALE: 13-CM RADIO JY/BEAM

13. N19 AREA IN THREE WAVELENGTHS H  22  cm Radio 1.5 - 8 keV X-ray

14. 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.

15. RADIO LUMINOSITY vs DIAMETER FOR LMC SNRs CONCLUSION: THERE IS NO CORRELATION OF LUMINOSITY WITH DIAMETER (IN AGREEMENT WITH PREVIOUS STUDIES) 1987A DEM L71 slope -1.13 corr coef 0.08

16. X-RAY - RADIO LUMINOSITIES OF LMC SNRs CONCLUSION: BRIGHTER X-RAY EMISSION MAY, IN GENERAL, CORRESPOND TO BRIGHTER RADIO BUT THERE IS NO CLEAR CORRELATION DEM L71 slope 0.77 corr. coeff 0.41 DEM L71

17. 1.1 keV 2keV 5 keV CHANDRA IMAGE OF CAS A

18. X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH SNR N132D, THE BRIGHTEST LMC RADIO SOURCE

19. 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. SNR 1E0102-72.3 in the Small Magellanic Cloud

20. 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

21. Preliminary SNR tables at: http://hoth.ccssc.org/mcsnr/test.php Please send us references, new data, etc. We will eventually get proper pages for each SNR. http://hoth.ccssc.org/mcsnr/test.php