visits 40,50 buffer times updated to
buffertime = exptime - 110 seconds----- Attempting Submission 3 (Mon Dec 13 19:43:04 GMT 2010) -----SAINTS - The SN 1987A Intensive StudySAINTS is a program to observe SN 1987A, the brightest supernova since 1604,
as it matures into the youngest supernova remnant at age 23. HST is the essential
tool for observing SN 1987A's many physical components. A violent encounter is
underway between the fastest-moving debris and the circumstellar ring: shocks
excite "hotspots." Radio, optical, infrared and X-ray fluxes have been rising rapidly:
we have organized VLT, Spitzer, and Chandra observations to understand the
several emission mechanisms at work. The inner debris, excited by radioactive
isotopes from the explosion, is now resolved and seen to be aspherical, providing
direct evidence on the shape of the explosion itself and on dust that formed in
the debris. Questions about SN 1987A remain unanswered. For example, where
is the compact object whose formation sent neutrinos our way in February 1987 ?
A rich and unbroken data set from SAINTS will help answer these central questions
and will build an archive for the future to help answer questions we have not yet
thought to ask. For Cycle 18, these data will include novel observations with the
IR channel of WFC3 and UV observations with COS.Our proposed Cycle 18 imaging program of SN~1987A will provide
continuing information on the luminosity and expansion of the debris,
eruption and evolution of hotspots, all at the highest available
spatial resolution.
Observations using WFC3/UVIS with filters
F435W, F625W, and F675N will connect with our earlier
observations at similar signal-to-noise ratio ($S/N$).
One orbit is requested to obtain these drizzled exposures.
Our proposed WFC3/IR imaging will use
filters F110W, F160W, F164N, F167N requiring 2 orbits to accommodate the
4 filters, 4 pointings and sufficient NSAMP readouts to yield a $S/N
\approx 25-100$ in the hotspots and debris.
The IR images may provide the best limits on emission from a compact
remnant in the debris if there is lower extinction due to dust.
The advantage of HST over AO from the ground is the clean and constant
HST PSF.
The AO PSF halo adds large and variable contamination from the
underlying structures,
which makes both spectroscopy and photometry from the ground
complicated and uncertain. Our experience is that, used together, HST
and ground-based AO is
a very powerful combination. The F167N filter
will also image the high velocity [FeII] 1.64 emission.
The proposed STIS observations will observe the complete SN~1987A ring
using the 52X2 slit with the G750M grating.
The observations will be planned to match orientations of
previous observations (GTO 7123, GO 9428, 10263, 11653).
In this way, subtle changes in the hotspot fluxes can be measured by
using
image subtraction techinques (see Figure 3).
We will obtain spectra through the 52X2 slit in two pointings and
multiple exposures to deliver the observations at the full spatial and
spectral resolution. These high spatial resolution spectra
isolate each spot to complement observations from the ground with high
spectral (but low
spatial) resolution.
The COS observations will probe the collisionless shock at sufficient
depth to constrain models of SN~1987A. We require $S/N$ $\approx$ 15
in the broad, red-shifted component of N~V 1240A visible in our recent STIS
G140L observations. We use
STIS-based flux estimates ($1-2 \times 10^{15}$ ergs/cm$^2$/s/A) to
calculate the COS
exposure times using ETC. We need 2.5 orbits with COS G130M to
achieve $S/N$ $\approx$ 15 (ETC COS.A268514).
To search for the weak coronal lines
we require S/N $\approx$ 10 in the narrower CIV ring emission in G160M.
This can
be achieved in $\approx$ 4.5 orbits (COS.A268618). At this depth, we
expect to observe blue-shifted Ly$\alpha$ (S/N
20), SiIV (S/N $\approx$ 10), and HeII (S/N $\approx$ 15). We will
require S/N $\approx$ 40
pointing verification images ($\approx$ 600s)
with the COS NUV imaging mode to facilitate post-processing
and analysis. Combining these, we require 7 orbits for the
COS observations.
We will observe SN~1987A using four central wavelength settings of
each the G130M (1291, 1300, 1309, 1318) and
G160M (1589, 1600, 1611, 1623) gratings. This ensures
continuous wavelength coverage at
relatively constant S/N, and effectively performs a focal plane split
to minimize fixed pattern noise on the
COS MCP detector. We will perform COS target acquisition following
the established offset from an isolated 18mag star used by the SAINTS team
during previous STIS observations. The acqusition with COS will use NUV/MIRRORA/PSA and
16 seconds per ACQ/SEARCH position. (COS.A269045),
The aperture attenuation for objects outside the COS Primary Science
Aperture (PSA) and the COS cross-dispersion imaging capability ensure
that star 3, 1.7 arcsec to the southeast
(with a 1300A flux of $\approx 10^{-14}$ erg/cm$^2$/s/A, will
not significantly contaminate the spectrum of the remnant ($\lesssim 10\%$), provided we
orient the spacecraft so that the cross-dispersion axis of COS
is parallel to the star-PSA line at an angle of -61.7. (See Figures 6 and 7).
We would like to use coordinated parallels where feasiable during
the long COS exposures. SAINTS member Nino Panagia and his
students have been industrious in using the parallel images
obtained during our spectroscopic visits which provides information on
the stellar population and star-formation history of this region of the LMC.ISM AND CIRCUMSTELLAR MATTER12false0.00.0falsefalsefalsefalsefalsefalseSUPPORTEDEXT-STARSUPERNOVAThis object was generated by the targetselector and retrieved from the NED database.J200005 35 27.9000-69 16 10.00J2000EXT-STARB3-B5 III-ISUPERNOVAThis object was generated by the targetselector and retrieved from the NED database.B=15.92, U=15.03J200005 35 27.9000-69 16 10.00J2000EXT-MEDIUMEMISSION LINE NEBULASNRThis object was generated by the targetselector and retrieved from the NED database.05 35 27.9000-69 16 10.00J2000EXT-STARA0-A3 III-IB3-B5 III-IV=16.071, B-V=-0.156,U-B=-0.886,V-R=-0.057,V-I=-0.109
B=15.915
U=15.029
COS.A351911, ACQ= MIRROR B + PSA
Brightest pixel 18.753
Count rate entire detector 515.776 ives: Time = 11.8457B=15.915, U=15.029J200005 35 27.9000-69 16 10.00J2000EXT-MEDIUMSNRThis object was generated by the targetselector and retrieved from the NED database.05 35 27.9000-69 16 10.00J2000WFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF164NWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF167NWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF657NSTIS/CCDSpectroscopicNoNoG750M6581COS/FUVSpectroscopicNoNoG130M1309COS/FUVSpectroscopicNoNoG160M1600COS/NUVImagingNoNoMIRRORAACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF475WACS/WFCImagingNoNoF814WACS/WFCImagingNoNoF658NWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF657NPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX1falsePOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN2falseThe scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode.The between is just suggestion. It would useful to get these data during this
time period, but its not critical.(Tic-Visit
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)false30The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode.please use SAA free orbits.Past STIS spectra (GO 7123, 7587, 8243, 8806, 11653) have avoided the use of the following guide stars; we also request their exclusion: 9162.0247 5:35:55.781 -69:09:52.63 8.92 3 1 448.96 05ZW; 9163.0606 5:37:26.026 -69:21:42.41 12.77 3 1 675.31 05ZW; 9163.0775 5:37:44.940 -69:20:05.68 11.91 3 1 738.05 05ZW; 9163.0933 5: 37:36.307 -69:06:44.42 12.84 0 1 913.91 05ZW; 9163.0948 5:37:38.971 -69:10:15.46 11.56 3 1 798.03 05ZW; 9163.0976 5:37:46.306 -69:20:50.42 10.95 3 1 757.05 05ZW; 9163.0979 5:37:47.071 -69:09:11.09 10.30 3 1 869.06 05ZW; 9166.0229 5:35:26.179 -69:28:02.93 11.36 3 1 663.23 05ZW; 9166.0750 5:34:45.540 -69:23:24.68 12.98 3 1 450.65 05ZW; 9166.0800 5:34:28.980 -69:25:40.04 12.78 3 1 611.46 05ZW; 9167.0336 5:37:02.275 -69:22:51.67 12.31 3 1 601.04 05ZW; 9167.0507 5:36:47.107 -69:29:54.56 9.07 3 1 874.09 05ZW; 9167.0510 5:36:40.378 -69:23:17.12 12.54 0 1 529.46 05ZW; 9167.0663 5:36:40.058 -69:22:43.64 12.57 3 1 505.04 05ZW(Tic-Visit
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:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
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)false20Timing link suitability includes constraints ([50 After 40 by 30.0 to 120.0 days])The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode./tmp/OPVisit63592.xml57ideal angle is 75(Tic-Visit
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)true30COS.A351911
Model ID = 98217
+ Kurucz (B3V): Temp = 18700, LogZ = 0.0, Logg = 3.9
. Renormalized to Johnson U = 15.03 in magnitudes relative to Vega
COS.A351916 Kurucz (B5V): Temp = 15400,
I avereage the two.. 12 seconds with B3V, and 16 seconds with B5Vstar 3: V=15.60 B-V 0.46 U-B -0.89
V = 15.60 B=16.06 U=15.17 B3 star
Exposure ID: COS.A331360
If the aperture falls on nearby star 3;COS.A331366
Brightest pixel 16.484
Count rate entire detector 491.586
Exposure time (seconds) = 600.0000
Model ID = 96513
+ Kurucz (B3V): Temp = 18700, LogZ = 0.0, Logg = 3.9
. Renormalized to Johnson U = 15.17 in magnitudes relative to Vega
The distance between star 3 and the edge of the COS aperture is 0.69",
figure 7.1 show the throughput is 0.7Timing link suitability includes constraints ([50 After 40 by 30.0 to 120.0 days])The scheduling data was generated by CASM 18.3.1.CASM was run in Phase II mode./tmp/OPVisit63589.xml55ideal angle is 75 same as visit 30(Tic-Visit
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)true40COS.A351911
Model ID = 98217
+ Kurucz (B3V): Temp = 18700, LogZ = 0.0, Logg = 3.9
. Renormalized to Johnson U = 15.03 in magnitudes relative to Vega
COS.A351916 Kurucz (B5V): Temp = 15400,
I avereage the two.. 12 seconds with B3V, and 16 seconds with B5Vstar 3: V=15.60 B-V 0.46 U-B -0.89
V = 15.60 B=16.06 U=15.17 B3 star
Exposure ID: COS.A331360
If the aperture falls on nearby star 3;COS.A331366
Brightest pixel 16.484
Count rate entire detector 491.586
Exposure time (seconds) = 600.0000
Model ID = 96513
+ Kurucz (B3V): Temp = 18700, LogZ = 0.0, Logg = 3.9
. Renormalized to Johnson U = 15.17 in magnitudes relative to Vega
The distance between star 3 and the edge of the COS aperture is 0.69",
figure 7.1 show the throughput is 0.7