0
Assigned ID: 889
----- Attempting Submission 1 (Fri Mar 06 22:53:36 GMT 2020) -----
Please find attached our updated submission for GO 16275 to study kilonovae, with visits now defined for target GRB 210704A.
Please let us know if there are any questions or changes needed.
(Updated strategy for visit M3)
Best Wishes,
Nial Tanvir, Andrew Levan
1266359787
----- Attempting Submission 1 (Tue Jun 30 17:22:40 GMT 2020) -----
----- Attempting Submission 2 (Mon Sep 27 19:06:35 GMT 2021) -----
HST Phase II Proposal 16275 successfully submitted.
Receipt: # 16275-2
----- Attempting Submission 3 (Fri Oct 01 13:39:45 GMT 2021) -----
Compact binary mergers: R-process kilonovae and ultra-relativistic jets
The discovery of a gamma-ray flash and kilonova (KN; aka. macronova), AT2017gfo, associated with the first binary neutron star (BNS) merger detected by aLIGO/AdV, GW170817, heralded the era of GW+EM multi-messenger astronomy. This landmark event confirmed both the association of short GRBs with binary mergers, and that neutron star material can be ejected in sufficient quantities to power a detectable radioactive transient. It opened a new window on several long-standing problems in astrophysics, cosmology and fundamental physics, including the possibility that BNS and NSBH compact binary mergers represent the dominant source of heavy r-process elements in the universe. However, the lack of success in identifying similar events in the O3 run of the gravitational wave detector network so far has highlighted that their rate is low in the nearby universe (e.g. d<200 Mpc), thus opportunities for intensive study of kilonovae, crucial to understanding their heavy element yields, for example, will be infrequent. Here we propose a ToO campaign targeting a kilonova discovered during cycle 28. This is between the GW network science runs, but KNe may still be found in blind surveys, accompanying short-GRBs, or during GW engineering runs. HST has already made unique contributions to the follow-up of AT2017gfo and its off-axis relativistic jet, and also provided the primary evidence for the most compelling cases of KNe following SGRBs. Our program is flexible to adapt for different possible scenarios, and will be crucial for understanding the diversity of EM signatures from neutron star compact binary mergers, and providing the data to test increasingly sophisticated KN models.
We intend to conduct comprehensive UV to IR observations of a kilonova. This will include early UV imaging and IR spectroscopic observations with both G102 and G141. As the source becomes too faint for ground based optical observations we will include optical (F475W/F606W/F814W) observations which will map the late time behaviour of the associated kilonova and the emergence of any afterglow component.
Given the uncertainty in the field due to the limited number of detections we specifiy a range of possible observations which are described below. However, it may be necessary to update the phaseII at the time of the submission. To avoid a very crowded phaseII we do not include copies of our individual observations, may be request multiple repeats of the same one (which we will copy to a new phaseII at the time of submisison).
The observations specified are:
U1 -1 orbit F336W
U2 - 1 orbit F438W
U3 - 1 orbit F475W
U4 - 1 orbit F555W
U5 - 1 orbit F606W
U6 - 1 orbit F625W
U7 - 1 orbit F775W
U8 - 1 orbit F814W
M1 - 1 orbit F475W/F606W/F814W
M2 - 1 orbit F606W/F140W
M3 - 1 orbit F105W/F160W
G1- 1orbit F110W/G102
R1 - 1 orbit F160W/G141
I1 - 1 orbit F105W
I2 - 1 orbit F110W
I3 - 1 orbit F125W
I4 - 1 orbit F140W
I5 - 1 orbit F160W
G2 - 3 orbit F110W/G102
R2 - 3 orbit F160W/G141
Our team has a great deal of expertise in observations of gamma-ray burst, supernovae and gravitational wave counterparts. We led the first HST observations of the counterpart of GW170817 as published in numerous paper (e.g. Tanvir et al. 2017 ApJ 848 17, Levan et al. 2017 ApJ 848 18, Hjorth et al. 2017 ApJ 848 28, Cantiello et al. 2018).
This proposal is from a large international collaboration that contains members of the major wide-field search teams for kilonova including ATLAS, BlackGEM, GOTO, PanSTARRS and ZTF. Hence we are in a strong position to identify likely sources. We have access to major follow-up facilities from 2-8m on the ground and with ALMA, VLA, ATCA and GMRT in the radio.
Our collaboration also includes significant expertise in theoretical interpretation. It contains a mixture of faculity, postdoctoral and student members and training is an important element of the programme. This ensures we have both the expertise and the resources to undertake these observations.
Stellar Physics and Stellar Types
6
false
false
false
false
false
false
false
30
true
SUPPORTED
EXT-STAR
GAMMA RAY BURSTER
NEUTRON STAR
J2000
KN discovered from GW or otherwise
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Imaging
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Imaging
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F555W
WFC3/UVIS
Imaging
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No
F775W
WFC3/UVIS
Imaging
No
No
F625W
WFC3/IR
Spectroscopic
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No
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WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F110W
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Imaging
No
No
F160W
WFC3/UVIS
Imaging
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No
F606W
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F475W
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Imaging
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F438W
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No
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F105W
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No
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/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vI1.xml
(Tic-Visit
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true
1
0
Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vI2.xml
(Tic-Visit
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true
1
0
Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vI3.xml
(Tic-Visit
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1
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Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vI4.xml
(Tic-Visit
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1
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Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vI5.xml
(Tic-Visit
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true
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Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vG2.xml
(Tic-Visit
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(Tic-Orbit
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(Tic-Orbit
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true
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Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vR2.xml
(Tic-Visit
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(Tic-Orbit
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true
3
0
Awaiting KN trigger
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vM2.xml
(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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true
1
0
Awaiting KN discovery
The scheduling data was generated by CASM 29.2.
CASM was run in Phase II mode.
/Users/nrt3/Desktop/Proposals/HSTc28/Phase2/OP-cache/16275_trigger_v3-vM3.xml
(Tic-Visit
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:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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(Tic-Orbit
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true
1
0