SUPERNOVA REMNANTS IN THE

MAGELLANIC CLOUDS

JOHN R. DICKELJOHN R. DICKELUNIVERSITY OF NEW MEXICOUNIVERSITY OF NEW MEXICO

ANDAND

ROSA MURPHY WILLIAMSROSA MURPHY WILLIAMSCOLUMBUS STATE UNIVERSITYCOLUMBUS STATE UNIVERSITY

Preliminary SNR tables at:http://hoth.ccssc.org/mcsnr/test.php

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 > 0.4

= -0.48

DEM L81= 0.0

X-RAY SPECTRUM OF N103 SNR

(usually incorrectly called N103B)

LEWIS, K. ET AL. 2003 ApJ, 582, 770THIS SHOWS THE THERMAL NATURE OF THE

EMISSION

SNR MCELS J0521-6542

[S II] H

[S II]/H

RATIO3 COLOR

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

0540-693 - A PROTOTYPE COMPOSITE SNR 50-MSEC PULSAR, PWN, O-RICH SHELL,ORGANIZED POLARIZATION IN THE PWN

6-CM RADIO IMAGE

N157B ANOTHER COMPOSITE

X-ray - contours are 5,10,20,30,40,100,300,600 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 are2,3,4,6,7 nJy/beam

The shell can be seen faintly on the southern part of the radio image.

SPECTRUM OF N157B

IT WILL BE VERY DIFFICULT TO MAKE ONE CONTINUOUS SPECTRUM FOR THIS OBJECT

X-RAY SPECTRUM OF N103 SNRNOTE THE MANY LINES OF HIGHLY

IONIZED INTERMEDIATE-MASS ELEMENTS

LEWIS, K. ET AL. 2003 ApJ, 582, 770

H LINE PROFILE TOWARD THE TYPE Ia BALMER-DOMINATED SNR 0519-

675

UNEQUILIBRATED VELOCITY 1180 KM/SEQUILIBRATED 1580 KM/S

SMITH, R. C. ET AL. 1991, ApJ, 375, 652

N19 AREA IN THE SMC

RED: X-RAY CONTOURS GREYSCALE: 13-CM RADIO

JY/B

EAM

N19 AREA IN THREE WAVELENGTHS

H22cm Radio 1.5 - 8 keV X-ray

SOME STATISTICS

LMC SMCTOTAL 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.

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 -1.13corr coef 0.08

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 0.77corr. coeff 0.41

DEM L71

1.1 keV 2keV 5 keV

CHANDRA IMAGE OF CAS A

X-RAY IMAGE AND RADIO CONTOURS OF THE OXYGEN RICH SNR N132D,

THE BRIGHTEST LMC RADIO SOURCE

radio X-ray optical in the light of [O III] characteristic of oxygen rich SNRsNote 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

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

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.