0
Assigned ID: 4584
----- Attempting Submission 1 (Wed May 24 20:18:59 GMT 2023) -----
This pattern is not used in this proposal.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
VISIT TO BE ACTIVATED 12, 16 AND 18 (3 orbits total)
to be performed between Aug 25 and Aug 29
1179191686
----- Attempting Submission 1 (Thu Sep 14 18:17:27 GMT 2023) -----
----- Attempting Submission 2 (Fri Aug 22 14:21:55 GMT 2025) -----
Your proposal could not be saved.
Submission aborted.
----- Attempting Submission 3 (Fri Aug 22 23:29:32 GMT 2025) -----
Orbit overrun is only for templates - those visits are not activated.
A holistic view of compact binary mergers: from kilonova to afterglow
The fate of two compact objects is to spiral into each other and eventually collide (or merge) due to angular momentum and energy losses to gravitational radiation. By combining extreme gravity, copious emission of gravitational waves, and luminous electromagnetic radiation, these mergers serve as excellent astrophysical laboratories to explore a wide range of fundamental problems: from the formation of ultrafast outflows to the cosmic production of heavy metals, from the equation of state of cold ultra-dense matter to the expansion rate of the universe. Our understanding of these systems was revolutionized in 2017 by the discovery of GW170817, the first mergers of two neutron stars (NSs) studied through gravitational waves and light. Thanks to its proximity and an unprecedented observing campaign, this one event revealed the rich complexity of the merger phenomenon and opened up new horizons for the study of these systems. Here we propose a comprehensive investigation of compact binary mergers aimed at maximizing the scientific return of future GW events. By using of the unique HST capabilities, we will map the explosion properties and environment of NS mergers with unprecedented detail, thus realizing in full the potential of multi-messenger astrophysics.
We request 6 orbits of disruptive ToO observations split between 3 visits.
We will use the WFC3/UVIS camera with the F225W and F336W filters and grism G280 for bright events.
We request 6 orbits of disruptive ToO observations split between 3 visits.
We will use the WFC3/IR camera with the F105W, F125W, and F160W filters and grisms G102/G141 for bright events.
We request 12 orbits of non-disruptive ToO observations split between 4 visits.
We will use the WFC3/UVIS and IR cameras with the F606W, F814W, F110W, and F160W filters.
Our team has decades-long experience in the field of GRBs and transients. We actively participated to the observing campaign of GW170817, leading the IR spectroscopy and multi-color imaging with HST (PI: Troja/Levan/Tanvir), optical spectroscopy and imaging with Gemini (PI: Troja), the X-ray afterglow observations with Chandra (PI: Troja), as well as long-term radio monitoring with VLA (PI: Troja).
We have approved long-term programs on the VLA (PI: Troja), the 4.3m LDT telescope (PI: Kutyrev), and the newly commissioned PRIME wide-field nIR imager dedicated to the GW follow-up. These facilities will be used to scan the LIGO sky localizations, identify optimal candidates and classify them through rapid multicolor imaging oor spectroscopy. In addition, we were recently awarded a long-term ToO program on JWST to follow-up a nearby kilonova and determine its evolution up to 4 months after the merger.
The proposed HST program would be an excellent complement to these JWST observations, and would allow us to assemble a benchamrk dataset for kilonova studies.
Our team includes key members of the Swift mission, which will be used in synergy with HST to guide the UV follow-up, and experienced observers as well as leading theoreticians in the kilonova (Fryer, Korobkin, Wollaeger) and afterglow (Van Eerten, Ryan) modeling. We are thus uniquely positioned to maximize the scientific return of the proposed observations.
Finally, as part of the activities funded by the AHEAD2020 consortium, the PI (who is the coordinator of the relevant work package) started to build the infrastructure for a public archive of kilonova and afterglow data of GW sources. High-quality data products will be compliants with ESO's Phase3 standards, and provided to the community through a dedicated portal.
Stellar Physics and Stellar Types
Large Scale Structure of the Universe
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false
true
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SUPPORTED
STAR
EJECTA
NEUTRON STAR
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J2000
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GW counterpart
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WFC3/UVIS
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Imaging
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WFC3/UVIS
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WFC3/UVIS
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WFC3/UVIS
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true
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The scheduling data was generated by CASM 33.1.
CASM was run in Phase II mode.
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The scheduling data was generated by CASM 33.1.
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The scheduling data was generated by CASM 33.1.
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The scheduling data was generated by CASM 33.1.
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