| Proposal |
Target |
ToO Prob |
Response |
Trigger |
2-8keV countrate |
MDP99 |
Dither |
Filter |
PI |
Exclusive Use |
IXPE Time [ ks ] |
XRISM Time[ ks ] |
NuSTAR Time [ ks ] |
Swift Time [ ks ] |
|
| 3001 |
V 0332+53 |
0.1 |
MEDIUM |
The criterion for the requested ToO observation triggering is based on the ongoing monitoring of the source with Swift (BAT) and MAXI. The observation will be triggered if the source luminosity will exceed the critical value of 5x10^37 erg/s. |
200 |
1 |
MEDIUM |
OPEN |
SERGEY TSYGANKOV |
6 |
600 |
0 |
0 |
0 |
| 3001 |
4U 0115+63 |
0.1 |
MEDIUM |
The criterion for the requested ToO observation triggering is based on the ongoing monitoring of the source with Swift (BAT) and MAXI. The observation will be triggered if the source luminosity will exceed the critical value of 5x10^37 erg/s. |
200 |
1 |
MEDIUM |
OPEN |
SERGEY TSYGANKOV |
6 |
600 |
0 |
0 |
0 |
| 3001 |
GRO J1744-28 |
0.1 |
MEDIUM |
The criterion for the requested ToO observation triggering is based on the ongoing monitoring of the source with Swift (BAT) and MAXI. The observation will be triggered if the source luminosity will exceed the critical value of 5x10^37 erg/s. |
200 |
1 |
MEDIUM |
OPEN |
SERGEY TSYGANKOV |
6 |
600 |
0 |
0 |
0 |
| 3001 |
GRO J1008-57 |
0.1 |
MEDIUM |
The criterion for the requested ToO observation triggering is based on the ongoing monitoring of the source with Swift (BAT) and MAXI. The observation will be triggered if the source luminosity will exceed the critical value of 5x10^37 erg/s. |
200 |
1 |
MEDIUM |
OPEN |
SERGEY TSYGANKOV |
6 |
600 |
0 |
0 |
0 |
| 3001 |
1A 0535+262 |
0.1 |
MEDIUM |
The criterion for the requested ToO observation triggering is based on the ongoing monitoring of the source with Swift (BAT) and MAXI. The observation will be triggered if the source luminosity will exceed the critical value of 5x10^37 erg/s. |
200 |
1 |
MEDIUM |
OPEN |
SERGEY TSYGANKOV |
6 |
600 |
0 |
0 |
0 |
| 3001 |
KS 1947+300 |
0.1 |
MEDIUM |
The criterion for the requested ToO observation triggering is based on the ongoing monitoring of the source with Swift (BAT) and MAXI. The observation will be triggered if the source luminosity will exceed the critical value of 5x10^37 erg/s. |
200 |
1 |
MEDIUM |
OPEN |
SERGEY TSYGANKOV |
6 |
600 |
0 |
0 |
0 |
|
| 3031 |
H1743-322 |
0.3 |
MEDIUM |
H1743-322 is detected in a rising outburst and exceeds 50 mCrab intensity from any monitoring mission (e.g., MAXI, Swift BAT, etc). |
7.6 |
1.1 |
MEDIUM |
OPEN |
JAMES STEINER |
2 |
200 |
0 |
40 |
20 |
| 3031 |
H1743-322 |
0.4 |
LOW |
(1) H1743-322 has exceeded 250 mCrab intensity during the outburst (e.g., as seen by MAXI). (2) H1743-322 shows transition to thermal state, e.g., defined as MAXI color [4-10/2-4] < 0.25. (3) Thermal state persists for a duration >= 1 week (hardness criterion holds). |
30 |
0.8 |
MEDIUM |
OPEN |
JAMES STEINER |
2 |
100 |
0 |
40 |
20 |
|
| 3036 |
MRK 421 |
0.5 |
MEDIUM |
MAXI: > 0.27 photons cm-2 s-1 in the 2.0 20.0 keV band or Swift-XRT >85 cts/s in the 0.3 10 KeV band or VERITAS >5e-10 ph m-2 s-1 above 200 GeV |
3.1 |
7 |
MEDIUM |
OPEN |
OLIVIER HERVET |
|
150 |
0 |
0 |
40 |
|
| 3091 |
NGC 4151 |
0.1 |
HIGH |
33 Swift pointings (1 ks each) spaced every 4 days, starting 8 days before each window and ending 10 days before the windows end. If the observed flux is F(2-8 keV)<=5e-11 erg/s/cm^2 for two consecutive pointings, then IXPE and simultaneous NuSTAR observations are triggered. |
0.409 |
4.8 |
MEDIUM |
OPEN |
VITTORIA GIANOLLI |
|
900 |
0 |
75 |
33 |
|
| 3101 |
GRS 1915+105 |
0.1 |
MEDIUM |
We plan to conduct the proposed IXPE observation during a period when the source exhibits an X-ray flare, surpassing the MAXI/GSC count rate of 0.2 cps. |
6.2 |
1.5 |
MEDIUM |
OPEN |
KARRI KOLJONEN |
|
100 |
0 |
0 |
0 |
|
| 3111 |
BH XRB |
0.5 |
MEDIUM |
Before triggering we will use MAXI monitoring to confirm that the predicted IXPE 2--8 keV count rate of the outbursting source is ≥30 c/s (corresponding to a flux of 3.83e-9 erg cm^-2 s^-1, and we will use 1ks of Swift/XRT monitoring per trigger to confirm the presence of a Type-C QPO. |
30 |
0.49 |
MEDIUM |
OPEN |
MELISSA EWING |
6 |
300 |
0 |
20 |
0 |
|
| 3129 |
ACCRETING MSP |
0.5 |
MEDIUM |
A 0.5-10 keV flux > 3E-10 erg/cm2/s (~10 mCrab) from an already known or newly discovered AMSP, as detected by All Sky X-ray monitors (e.g., Einstein Probes), and/or when optical robotic telescopes (e.g. XB-NEWS at LCO) detect the onset of the outburst, a few days before the source brightens in X-ray. |
3.87 |
0.8 |
MEDIUM |
OPEN |
ALESSANDRO PAPITTO |
6 |
900 |
0 |
80 |
0 |
|
| 3171 |
T CRB |
0.5 |
HIGH |
After the onset of the nova event that will be known from optical observations. |
4.2 |
3 |
MEDIUM |
OPEN |
MANEL ERRANDO |
3 |
500 |
0 |
0 |
0 |
|
| 3207 |
V404 CYG |
0.08 |
MEDIUM |
We would trigger the observations when the source crosses a threshold of 30 mCrab of flux in 2-10 keV band in MAXI. |
2.2 |
1.9 |
MEDIUM |
OPEN |
SUDIP CHAKRABORTY |
6 |
300 |
0 |
40 |
0 |
| 3207 |
V4641 SGR |
0.2 |
MEDIUM |
We would trigger the observations when the source crosses a threshold of 30 mCrab of flux in 2-10 keV band in MAXI. |
2.1 |
1.8 |
MEDIUM |
OPEN |
SUDIP CHAKRABORTY |
6 |
300 |
0 |
40 |
0 |
|
| 3208 |
HER X-1 |
1 |
LOW |
See the phase dependence. The given ephemeris is good to a few days but has to be adjusted about 35 days ahead of the first IXPE observation. |
15 |
1.5 |
MEDIUM |
OPEN |
HERMAN MARSHALL |
6 |
750 |
45 |
0 |
0 |
|
| 3252 |
SOFT-STATE BHXB |
0.3 |
MEDIUM |
Black Hole X-ray binary entering the soft state with disk temperature having exceeded at least 1.0 keV and surpassed a brightness of 300 mCrab. This will be determined through MAXI and Swift monitoring, as well as community ATels. |
91.14 |
0.25 |
MEDIUM |
OPEN |
SWATI RAVI |
6 |
450 |
0 |
40 |
4 |
| 3252 |
SOFT-STATE BHXB |
0.45 |
LOW |
Black Hole X-ray binary entering the soft state with disk temperature having exceeded at least 1.0 keV and surpassed a brightness of 300 mCrab. This will be determined through MAXI and Swift monitoring, as well as community ATels. This second trigger is intended to probe the disk at 0.9 keV |
91.14 |
0.25 |
MEDIUM |
OPEN |
SWATI RAVI |
6 |
950 |
0 |
40 |
4 |
|
| 3258 |
GRS 1915+105 |
0.03 |
MEDIUM |
The source returns to to it's pre-2019 flux state (>~0.2 c/s in MAXI 2-10keV band), and monitoring shows evidence it is in the \chi spectral state |
25.5 |
0.7 |
MEDIUM |
OPEN |
EDWARD NATHAN |
|
250 |
0 |
60 |
0 |
| 3258 |
GRS 1915+105 |
0.3 |
MEDIUM |
The source returns to to it's pre-2019 flux state (>~0.2 c/s in MAXI 2-10keV band), and monitoring shows evidence it is in a disc-dominated spectral state |
90.27 |
0.28 |
MEDIUM |
OPEN |
EDWARD NATHAN |
|
400 |
0 |
60 |
0 |
| 3258 |
GRS 1915+105 |
0.03 |
MEDIUM |
The source returns to to it's pre-2019 flux state (>~0.2 c/s in MAXI 2-10keV band), and monitoring shows evidence it is demonstrating exotic variability |
117.973 |
0.32 |
MEDIUM |
OPEN |
EDWARD NATHAN |
|
300 |
0 |
60 |
0 |
