Cannot find file /Users/jlarsson/Desktop/cycle24_87a_final.pdf0Assigned ID: 598
----- Attempting Submission 1 (Fri Apr 08 17:05:36 GMT 2016) -----For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting.
INEFFICIENT ORDERING OF FP-POS POSITIONS
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.
COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details.on Jan 09, 2017 pete challis changed the target for exposure 2 visit 10
from the acqusition star to the supernova SN-1987A-COS-1864007001----- Attempting Submission 1 (Thu Jul 21 16:01:36 GMT 2016) -----
----- Attempting Submission 2 (Mon Jan 09 19:22:10 GMT 2017) -----Supernova 1987A at 30 yearsThis programme will provide a 30 year legacy point for SN 1987A, the brightest supernova since 1604. HST is the essential tool for resolving and analysing SN 1987A's several physical components. The inner, asymmetric ejecta are being heated by X-rays from the circumstellar ring and allow us to directly observe the geometry of the explosion. At the same time the fastest-moving ejecta are interacting with the ring, giving rise to bright emission from shocks. Our latest observations show that the ring is fading and that new spots are appearing outside, signalling that the blast wave has passed the ring and is now interacting with previously unseen material. It is also the beginning of the end for the ring. Here we propose to use COS and STIS to obtain a complete UV/optical spectrum of the ejecta and ring. The spectrum will enable a detailed modelling of the nucleosynthesis, which is a powerful diagnostic of the explosion, and provide a unique opportunity to study a supernova spectrum in the transition phase between a radioactively powered supernova and a shock heated remnant. It will also allow us to distinguish between different excitation mechanisms for the molecular hydrogen, recently discovered in the NIR. We also propose a set of broad and narrow band images to monitor the evolution of the flux and morphology of ejecta, ring and new spots outside the ring. The latter will tell us about the mass-loss history of the progenitor. The proposed observations will provide a crucial complement to recent Herschel and ALMA observations of dust, CO and SiO in the ejecta.Ultraviolet Spectroscopy with COS and STIS
We will take advantage of the complementary capabilities of COS and STIS to provide the definitive UV spectral observations of SN 1987A at late times. With the low background and high effective area of COS, we are ~50 times more sensitive to faint spectral features from the debris, reverse shock, and circumstellar ring (see France et al. 2011a). However, the limited spatial resolution of COS (about 1" in a 2.5" aperture) leaves some spatial-spectral ambiguity in the deep spectral data. We propose to complement the deep COS observations with high angular resolution (0.1"), lower spectral resolution observations with STIS.
The COS observations will probe the line profiles of a whole inventory of high-velocity atomic features and possibly molecular emission in the system. One of the main features in the COS/FUV data is the broad, red-shifted emission component of N V 1240A at a flux of (1-2x10^15 ergs/cm2/s/angstrom) ). Using the COS ETC with this flux, an exposure time of 2.5 orbits with COS G130M will be required to achieve a S/N ratio of 15. To search for the molecular emission lines, we request S/N ~10 in the narrower CIV ring emission in G160M as a baseline for H2 "1600 angstrom bump" studies, based on FUV spectra of protoplanetary disks (France et al. 2011b; France et al. 2014). This can be achieved in ~4.5 orbits with G160M. At this depth, we expect to observe blue-shifted Lyman Alpha (S/N ~20), CIV (S/N ~10), and HeII (S/N ~15). 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 and maximize lifetime of the COS MCP detector. We will perform COS target acquisition following the established offset from an isolated 18th mag star used during previous STIS observations. The acqusition with COS will use NUV/MIRRORA/PSA. In our 2011 COS observations, we successfully demonstrated that by judicious choice of spacecraft roll orientation, we could minimize the impact of stellar light from outside the COS PSA. The flux from "Star 3", 1.7" away from the center of the remnant, does not significantly contaminate the spectrum (<=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 -62 degrees (+/-10 degrees).
We base our STIS observations on our last UV imaging spectroscopy reported in France et al. (2010). STIS gratings G140L, G230L, G430L, and G750L using the 52"x0.2" slit, aligned along the N-S axis of the remnant will provide high angular resolution constraints on the emission over the UV to optical range. To cover the ejecta we will use 3 parallell slits (Fig 2) for the range not covered by COS (the G230L, G430L, and G750L gratings), and a central slit for G140L. This imaging spectroscopy will be used to constrain the relative position of the bright emission features and explore the spatial variation of the lines. For a S/N = 20 at the peak of the northern high-velocity Lyman Alpha emission and the northern Mg II emission feature to ensure high-quality data that will complement the COS spectra. Taking the 2009 SAINTS observations, assuming a 25% ejecta brightening, and running these values through the STIS on-line ETC, we find that we require 3 orbits for G140L and one orbit each for each slit position of G230L, G430L and G 750L. In total, we require 7 + 3 + 3x3x1 = 19 orbits for the spectral observations of SN 1987A.
Imaging with WFPC3: The WFC3/UVIS observations using filters F435W, F625W, F657N and F502N will connect with our earlier observations at similar S/N ratio through drizzled observations. These new images will allow us to follow the light curve, the morphol- ogy of the ejecta, ring and to follow new spots and diffuse gas outside the ring. Based on our 2015 observations we request 3 orbits in total.Stellar Physics6falsetruefalsefalsefalsefalseSUPPORTEDEXT-STARB3-B5 III-Iposition 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 arcsecondJ2000EXT-MEDIUMEJECTAEMISSION LINE NEBULASNROFFSET measured on recent WFC3/UVIS imageEXT-MEDIUMEJECTAEMISSION LINE NEBULASNROFFSET measured on recent WFC3/UVIS imageEXT-MEDIUMEJECTAEMISSION LINE NEBULASNROFFSET measured on recent WFC3/UVIS imageEXT-STARA0-A3 III-IB3-B5 III-INOV=16.071, B-V=-0.156,U-B=-0.886,V-R=-0.057,V-I=-0.109
B=15.915
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COS.A351911, ACQ= MIRROR B + PSA
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on Jan 09, 2017 pete challis changed the target for exposure 2
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