A 3D view of the SN 1987A Ejecta
SN 1987A represents the most important source of information about the explosion physics of any SN. For this the morphology of the ejecta is together with the radioactive isotopes the best diagnostics. From HST imaging in H-alpha and NIR AO imaging in Si/Fe at 1.64 mu one finds completely different morphologies, with the 1.64 mu image dominated by the processed core and H-alpha by the surrounding H envelope. Besides Cas A (Type IIb), this is the only core collapse SN where we have this information. We propose to use STIS to map the debris in SN 1987A in 3D with the best possible angular resolution. There has been no such STIS map since 2004, while the physics of the emission has undergone some profound changes. From being powered by radioactivity the energy input is now dominated by X-rays from the collision with the circumstellar ring. Compared to 2004 the 3D structure can be determined with a factor of ~ 3 better spatial resolution and also better spectral resolution. The 3D structure in H-alpha can also give independent clues to where the large mass of dust detected by Herschel is located as well as its properties. It also gives a complementary view of the ejecta to the future ALMA imaging in CO which will have similar spatial resolution. Besides the debris we will be able to probe the ~ 10,000 km/s reverse shock close to the ring in H-alpha. By observing this also in Ly-alpha one may test different emission processes which have been proposed, as well as probing the region producing the synchrotron emission observed by ALMA. The opportunity to observe the SN in this stage will never come back!
We are proposing for 17 orbits with STIS. The spectroscopic observations will provide 3-D
maps of the complete debris and of the N and S sides of the reverse shock and equatorial
ring. We propose to use 5 adjacent 0.1 slit positions for 3 orbits each to map SN 1987A (as
shown in figure 1) for a total of 15 orbits. The G750L grating provides adequate spectral
resolution to separate the emission from the reverse shock, collision hotspots, and debris.
Figure 5 shows a previous STIS/G750L observation from 2010 using the 0.2 slit with an
exposure of 3 orbits. The proposed STIS observations will be dithered in the spatial direction
with 6-12 exposures to remove the Cosmic Rays, and the many hot and dead STIS pixels.
Based on the large increase in flux from the ejecta, We expect the proposed observations to
yield a S/N ratio of about 10/pixel in the debris emission, 100 for the collision emission, and
20/pixel in the brightest parts of the reverse shock. We can detect the reverse shock out to
10,000 km/sec (S/N 3/pixel).
ISM AND CIRCUMSTELLAR MATTER
12
false
false
false
false
false
SUPPORTED
EXT-STAR
B3-B5 III-I
position is measured from both STIS and UVIS images
Also on PLATE A298 position is 5:35:30.484 -69:16:18.36
so all these positions agree to about 0.1 arcsecond
J2000
EXT-MEDIUM
EJECTA
EMISSION LINE NEBULA
SNR
OFFSET measured on recent WFC3/UVIS image
EXT-MEDIUM
EJECTA
EMISSION LINE NEBULA
SNR
OFFSET measured on recent WFC3/UVIS image
EXT-MEDIUM
EJECTA
EMISSION LINE NEBULA
SNR
OFFSET measured on recent WFC3/UVIS image
EXT-MEDIUM
EJECTA
EMISSION LINE NEBULA
SNR
OFFSET measured on recent WFC3/UVIS image
EXT-MEDIUM
EJECTA
EMISSION LINE NEBULA
SNR
OFFSET measured on recent WFC3/UVIS image
STIS/CCD
Spectroscopic
No
No
G750L
7751
STIS/FUV-MAMA
Spectroscopic
No
No
G140L
1425
STIS/CCD
Imaging
No
No
F28X50LP
WFC3/UVIS
Imaging
No
No
F475W
WFC3/UVIS
Imaging
No
No
F606W
WFC3/UVIS
Imaging
No
No
F814W
WFC3/UVIS
Imaging
No
No
F657N
ACS/WFC
Imaging
No
No
F475W
ACS/WFC
Imaging
No
No
F606W
ACS/WFC
Imaging
No
No
F814W
ACS/WFC
Imaging
No
No
F658N
Timing link suitability includes constraints ([Sequence (01 02 03 04 05 06) within 30.0 days])
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just in ncase the SLEW to position sn1987a-stis3 is wrong, and the slit
lands on star 2.... the exposures are safe
STIS.sp.518462
nearby star2 is V=15.0 E(B-V) =0.15 BIII star
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