No X-rays above background were picked up from either Cloud during the September 20, 1966, Nike-Tomahawk rocket flight nor that of two days later.
The second took off from Johnston Atoll at 17:13 UTC and reached an apogee of 160 km (99 mi), with spin-stabilization at 5.6 rps.
The LMC was not detected in the X-ray range 8–80 keV.
Another was launched from same atoll at 11:32 UTC on October 29, 1968, to scan the LMC for X-rays.
The first discrete X-ray source in Dorado was at RA  05ʰ 20ᵐ Dec −69°, and it was the Large Magellanic Cloud.
This X-ray source extended over about 12° and is consistent with the Cloud.
Its emission rate between 1.5–10.5 keV for a distance of 50 kpc is 4 x 10³⁸ ergs/s.
An X-ray astronomy instrument was carried aboard a Thor missile launched from the same atoll on September 24, 1970, at 12:54 UTC and altitudes above 300 km (186 mi), to search for the Small Magellanic Cloud and to extend observation of the LMC.
The source in the LMC appeared extended and contained star ε Dor.
The X-ray luminosity (Lₓ) over the range 1.5–12 keV was 6 × 10³¹ W (6 × 10³⁸ erg/s).

The Large Magellanic Cloud (LMC) appears in the constellations Mensa and Dorado.
LMC X-1 (the first X-ray source in the LMC) is at RA  05ʰ 40ᵐ 05ˢ Dec −69° 45′ 51″, and is a high-mass X-ray binary (star system) source (HMXB).
Of the first five luminous LMC X-ray binaries: LMC X-1, X-2, X-3, X-4 and A 0538–66 (detected by Ariel 5 at A 0538–66), LMC X-2 is the one that is a bright low-mass X-ray binary system (LMXB) in the LMC.

DEM L316 in the Cloud consists of two supernova remnants.
Chandra X-ray spectra show that the hot gas shell on the upper left has an abundance of iron.
This implies that the upper-left SNR is the product of a Type Ia supernova; much lower such abundance in the lower remnant belies a Type II supernova.

A 16 ms X-ray pulsar is associated with SNR 0538-69.1.
SNR 0540-697 was resolved using ROSAT.
No X-rays above background were picked up from either Cloud during the September 20, 1966, Nike-Tomahawk rocket flight nor that of two days later. The second took off from Johnston Atoll at 17:13 UTC and reached an apogee of 160 km (99 mi), with spin-stabilization at 5.6 rps. The LMC was not detected in the X-ray range 8–80 keV.
Another was launched from same atoll at 11:32 UTC on October 29, 1968, to scan the LMC for X-rays. The first discrete X-ray source in Dorado was at RA  05ʰ 20ᵐ Dec −69°, and it was the Large Magellanic Cloud. This X-ray source extended over about 12° and is consistent with the Cloud. Its emission rate between 1.5–10.5 keV for a distance of 50 kpc is 4 x 10³⁸ ergs/s. An X-ray astronomy instrument was carried aboard a Thor missile launched from the same atoll on September 24, 1970, at 12:54 UTC and altitudes above 300 km (186 mi), to search for the Small Magellanic Cloud and to extend observation of the LMC. The source in the LMC appeared extended and contained star ε Dor. The X-ray luminosity (Lₓ) over the range 1.5–12 keV was 6 × 10³¹ W (6 × 10³⁸ erg/s).
The Large Magellanic Cloud (LMC) appears in the constellations Mensa and Dorado. LMC X-1 (the first X-ray source in the LMC) is at RA  05ʰ 40ᵐ 05ˢ Dec −69° 45′ 51″, and is a high-mass X-ray binary (star system) source (HMXB). Of the first five luminous LMC X-ray binaries: LMC X-1, X-2, X-3, X-4 and A 0538–66 (detected by Ariel 5 at A 0538–66), LMC X-2 is the one that is a bright low-mass X-ray binary system (LMXB) in the LMC.
DEM L316 in the Cloud consists of two supernova remnants. Chandra X-ray spectra show that the hot gas shell on the upper left has an abundance of iron. This implies that the upper-left SNR is the product of a Type Ia supernova; much lower such abundance in the lower remnant belies a Type II supernova.
A 16 ms X-ray pulsar is associated with SNR 0538-69.1. SNR 0540-697 was resolved using ROSAT.
Large Magellanic Cloud