Target SHORT-GRB-KILONOVA: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.0Assigned ID: 65
----- Attempting Submission 1 (Mon Apr 03 13:53:59 GMT 2017) -----Warning (Visit Planner): Target SHORT-GRB-KILONOVA: There is no need or capability to test the scheduling of observations of generic targets in Phase I. This warning will go away the next time the proposal is loaded.
Occurrence: #1 SHORT-GRB-KILONOVAResubmission of visit 7 and new visits 8 and 9.606533967----- Attempting Submission 1 (Thu Jul 13 20:40:37 GMT 2017) -----
----- Attempting Submission 2 (Wed Aug 23 22:06:50 GMT 2017) -----
----- Attempting Submission 3 (Wed Oct 18 18:19:05 GMT 2017) -----
HST Phase II Proposal 15329 (GW170817_apt) successfully submitted.
Receipt: # 15329-3
----- Attempting Submission 4 (Thu Oct 19 19:56:47 GMT 2017) -----
----- Attempting Submission 5 (Thu Dec 14 19:47:00 GMT 2017) -----Visits 1,4,5,6 are already complete. This re-submission is for visit 7 and new visits 8 and 9. The visit planner has been run.Fine-Tuned Search for Kilonova Emission in a Short Gamma-Ray Burst: Implications for the Progenitors, Advanced LIGO, and r-Process NucleosynthesisShort-duration gamma-ray bursts have long been suspected to result from the catastrophic mergers of binaries composed of two neutron stars (NS-NS) and/or a neutron star and a black hole (NS-BH). An important direct signature of NS-NS/NS-BH progenitors is near-infrared emission powered by radioactive r-process material synthesized by the ejection of neutron-rich matter during the merger, a so-called "kilonova". HST observations of the short GRB130603B provided the first tantalizing evidence for such an emission component, but unfortunately lacked detailed spectral and temporal information. Here, we propose fine-tuned TOO observations of a future short GRB that will definitively establish the presence of a kilonova and will also allow us to distinguish an NS-NS from an NS-BH merger, based on the ejecta mass (~0.01 vs. ~0.1 Msun, respectively). The results will not only serve as a smoking gun for compact object merger progenitors, but they will also establish whether compact object mergers are the primary site for cosmic r-process nucleosynthesis. To support and interpret the proposed HST observations, and to rule out alternative explanations for any detected emission, we will obtain a wide range of observations spanning radio to X-rays using active programs at Gemini, Magellan, MMT, VLA, Chandra, and XMM.To determine the expected apparent brightness of the kilonova for the expected range of ejecta masses (0.01 - 0.1 Msun), and to inform our choice of filters, we convolve the models of Barnes & Kasen (2013) as a function of redshift with the ACS/F814W, WFC3/F110W, and WFC3/F160W filter response functions. We calculate the resulting apparent brightness in two rest-frame times of 4 days (peak) and 10 days (post-maximum). The actual observer-frame times for the two HST epochs will therefore be 4x(1+z) days and 10x(1+z) days, where the redshift will be known prior to triggering the HST observations. The choice of filters is designed to straddle the break at 1 micron in the rest-frame, in order to capture the unusually red color of a kilonova relative to the afterglow.
We base our HST trigger criteria and time request on the model with 0.01 Msun so that we can probe the wide range of ejecta masses predicted by numerical simulations (rather than just the bright upper bound of 0.1 Msun; this will allow any non-detections to place meaningful constraints on the nature of the binary (NS-NS vs. NS-BH) and on future searches for optical/near-IR counterparts of Advanced LIGO sources.
Epoch 1 [4x(1+z) days]: We find that at z < 0.2 it is advantageous to use the ACS/F814W and WFC3/F110W filters which give the best combination of sensitivity (5-sigma =27.7 and 27.5 AB mag in 2 orbits each, respectively, using the ACS and WFC3 ETCs) and color contrast (F814W - F110W ~ 1.6 - 2 AB mag). By comparison, the afterglow color in these filters is much bluer, with F814W - F110W ~ 0.3 AB mag. At z = 0.2 - 0.4 we will instead use the WFC3/F110W and F160W filters to capture the spectral peak (5-sigma = 26.3 AB mag for F160W in 2 orbits). The resulting color is F110W - F160W ~ 0.6 - 1.2 AB mag, compared to a bluer color for the afterglow, F110W - F160W ~ 0.3 AB mag. The kilonova emission for 0.1 Msun can be detected to z ~ 0.7, but we truncate our trigger criteria at z =0.4 to be able to detect the emission in the case of 0.01 Msun, typical of NS-NS mergers.
Epoch 2 [10x(1+z) days]: We will only obtain observations in a single filter redward of the 1 micron break since we are only concerned with demonstrating a rapid decline that will help to firm up the kilonova nature and to better constrain the ejecta mass (i.e., the unusually red color will already be established with the first epoch near peak). This will require 2 orbits in F110W (z < 0.2 ) or F160W (z = 0.2 - 0.4). In this case, if the ejecta mass is ~0.01 Msun we will obtain a deep upper limit that will establish the expected rapid fading, while in the case of ~0.1 Msun we will have a second detection.
Templates [>1 month]: We will require template images after the kilonova emission has faded away that match the exposure time and filters of the early observations. This will therefore require a total of 4 orbits (2 orbits in each filter). We note, however, that in the case of ~0.01 Msun a non-detection in the second epoch could be used as a template in one of the two filters (F110W or F160W depending on the redshift), meaning that the final observation will require only 2 orbits. Since we do not know the ejecta mass in advance we request 4 orbits for the final epoch, but may use only 2 orbits.Stellar Physics6falsefalsefalsefalsefalsefalseSUPPORTEDEXT-STARGAMMA RAY BURSTERNOJ2000d<200MpcWFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF160WWFC3/IRImagingNoNoF110WWFC3/IRImagingNoNoF160WPOS-TARGDITHER0.262LINE0.192falsefalse68.14418.39ACS-WFC-DITHER-BOX1falsePOS-TARGDITHER0.572LINE0.365falsefalse74.653418.528WFC3-IR-DITHER-BOX-MIN2falsePOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX3falsePOS-TARGDITHER3.034LINEfalsefalse285.29ACS-WFC-DITHER-LINE4falsePOS-TARGDITHER3.034LINEfalsefalse385.29ACS-WFC-DITHER-LINE5falseThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.1503815875000124.6893274872773(Tic-Visit
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