Target GW1: 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.
Please find attached our submission for consideration for Cycle 25 "Rapid observations of the first gravitational wave counterparts"
2140915323
Assigned ID: 557
----- Attempting Submission 1 (Fri Apr 07 15:04:47 GMT 2017) -----
This error seems to relate to running the visit planner on a generic target. I believe this should not be necessary in phase 1 and indeed it says the error should go away.
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
ORBITAL VISIBILITY OVERRUN
This is a follow-up submission which contains additional visits (Y6-8) which place the target at the various corners of the UVIS detectors to provide a better opportunity for guide stars.
583442275
----- Attempting Submission 1 (Thu Jul 20 13:17:37 GMT 2017) -----
----- Attempting Submission 2 (Mon Sep 09 20:35:33 GMT 2019) -----
----- Attempting Submission 3 (Thu Jan 30 21:05:59 GMT 2020) -----
----- Attempting Submission 4 (Sun Mar 15 19:36:25 GMT 2020) -----
These errors refer to visits which are not being activated.
Rapid observations of the first gravitational wave counterparts
We propose a series of disruptive ToO observations of the first electromagnetic counterparts to gravitational wave sources. These observations will track the likely rapidly fading counterparts to levels a factor 10 fainter than possible from the ground. They will determine the spectral and temporal evolution, evaluate their power sources, ascertain their contribution to the production of heavy elements in the Universe, pinpoint them on their host galaxies, characterise their environments and provide information to hone further searches. These observations will provide a unique and powerful view of a newly discovered, but long awaited class of astronomical object.
This is a proposal to obtain HST observations of the first electromagnetic counterparts to gravitational wave sources. It
is a disruptive ToO programme, with the first observations taking place after a few days (3-6 after trigger) and subsequent observations at ~1 week intervals, with some later time follow-up Our programme
envisages different strategies depending on the nature of the counterpart, and we outline these below.
However, as this is a new field, and there is very limited information about the nature of the counterparts it may be necessary to tweak this stragegy at the time of trigger in order to ensure the highest possible scientific return.
Rapid follow-up
1) Optical/IR counterpart discovery
In this case we will likely trigger IR spectroscopy to search for kilonova emission. This will be through visits G1 and G2 which call for G102 and G141 grism spectroscopy as well as short direct images in F125W and F160W. Our later observations will be imaging in F125W and F160W (visits I1 and I2) to track the lightcurve. If the source is very faint, then we may omit the grism spectroscopy and use the X visits in F140W instead.
2) X-ray only counterpart discovery
Here we assume that deep optical observations at the counterpart location have failed to identify a optical counterpart. In this case we will conduct a deep imaging search with HST. This will use visits X1-X4 (1 and 2 orbit visits in F140W) in order to conduct a deep search for any kilonova emission.
Slow follow-up
Once the initial observations are complete we will map the evolution of the counterpart for as long as it is visible to HST. We will use optical or IR filters for this as appropriate. For these later observations we will use single orbit integrations in each filter (vists I3-I7, possibly repeated as necessary).
At very late times we will also characterise the environment of the transient. For this we may use UV observaitons and narrow band observations to search for star formation at the transient location (visits N1-N3 depending on the redshift of the source).
Stellar Physics
6
false
false
false
false
false
false
false
SUPPORTED
UNIDENTIFIED
RADIO EMITTER
J2000
candidate GW counterpart
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Spectroscopic
No
No
G102
WFC3/IR
Spectroscopic
No
No
G141
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F336W
WFC3/UVIS
Imaging
No
No
F390W
WFC3/IR
Imaging
No
No
F125W
WFC3/IR
Imaging
No
No
F160W
WFC3/IR
Imaging
No
No
F140W
WFC3/UVIS
Imaging
No
No
F657N
WFC3/UVIS
Imaging
No
No
F656N
WFC3/UVIS
Imaging
No
No
F658N
POS-TARG
DITHER
0.572
LINE
0.365
false
false
74.653
4
18.528
WFC3-IR-DITHER-BOX-MIN
1
false
POS-TARG
DITHER
DITHER
3
0.474
WFC3-IR-DITHER-LINE-3PT
false
false
0.605
2
0
POS-TARG
LINE
41.788
2
true
POS-TARG
DITHER
0.173
LINE
0.112
false
false
81.785
4
23.884
WFC3-UVIS-DITHER-BOX
3
false
POS-TARG
DITHER
0.145
LINE
false
false
2
46.84
WFC3-UVIS-DITHER-LINE
4
false
POS-TARG
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DITHER
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0.145
WFC3-UVIS-DITHER-BOX
false
81.785
false
0.112
0.173
2
46.84
POS-TARG
LINE
23.884
5
true
The scheduling data was generated by CASM 28.0.
CASM was run in Phase II mode.
F125W/G102 1 orbit
(Tic-Visit
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true
1
1
Awaiting SGRB trigger
The scheduling data was generated by CASM 28.0.
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F140W/G141 1 orbit
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true
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Awaiting SGRB trigger
The scheduling data was generated by CASM 28.0.
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Awaiting SGRB trigger
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true
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Awaiting SGRB trigger
The scheduling data was generated by CASM 28.0.
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true
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Awaiting SGRB trigger
The scheduling data was generated by CASM 28.0.
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(Tic-Visit
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true
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Awaiting SGRB trigger
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true
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Awaiting SGRB trigger
The scheduling data was generated by CASM 28.0.
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(Tic-Visit
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true
2
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The scheduling data was generated by CASM 28.0.
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(Tic-Visit
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true
1
0
Awaiting SGRB trigger
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(Tic-Visit
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true
1
0
Awaiting SGRB trigger
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(Tic-Visit
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true
1
1
Awaiting Dark GRB position from Chandra
The scheduling data was generated by CASM 28.0.
CASM was run in Phase II mode.
(Tic-Visit
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:si-vis-utilization 2860
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true
1
1
Awaiting Dark GRB position from Chandra
The scheduling data was generated by CASM 28.0.
CASM was run in Phase II mode.
(Tic-Visit
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)
true
1
1
Awaiting Dark GRB position from Chandra
The scheduling data was generated by CASM 28.0.
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(Tic-Visit
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:max-dark-utilization 1920
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)
true
1
0
Awaiting Dark GRB position from Chandra
The scheduling data was generated by CASM 28.0.
CASM was run in Phase II mode.
(Tic-Visit
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)
true
1
0
Awaiting Dark GRB position from Chandra
The scheduling data was generated by CASM 28.0.
CASM was run in Phase II mode.
(Tic-Visit
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