| Proposal |
Target |
ToO Prob |
Response |
Trigger |
2-8keV Counts |
MDP99 |
Filter |
PI |
Exclusive Use |
IXPE Time [ks] |
NICER Time [ks] |
NuSTAR Time[ks] |
Swift Time [ks] |
|
| 2006 |
1ES 1959+650 |
0.11 |
HIGH |
VHE flux of 0.5 Crab Unit |
7.275 |
1.69 |
OPEN |
LAURA DI GESU |
3 |
200 |
0 |
0 |
0 |
| 2006 |
MRK 501 |
0.09 |
HIGH |
VHE flux of 3 Crab Unit |
4.196 |
2.23 |
OPEN |
LAURA DI GESU |
3 |
0 |
0 |
0 |
0 |
| 2006 |
1ES 0033+595 |
0.08 |
HIGH |
VHE flux of 0.5 Crab Unit |
3.079 |
2.64 |
OPEN |
LAURA DI GESU |
3 |
0 |
0 |
0 |
0 |
| 2006 |
1ES 1011+496 |
0.05 |
HIGH |
VHE flux of 0.5 Crab Unit |
0.67 |
5.57 |
OPEN |
LAURA DI GESU |
3 |
0 |
0 |
0 |
0 |
| 2006 |
MRK 421 |
0.05 |
HIGH |
VHE flux of 3 Crab Unit |
30.54 |
1 |
OPEN |
LAURA DI GESU |
3 |
0 |
0 |
0 |
0 |
| 2006 |
1ES 1218+304 |
0.02 |
HIGH |
VHE flux of 0.5 Crab Unit |
1.055 |
4.44 |
OPEN |
LAURA DI GESU |
3 |
0 |
0 |
0 |
0 |
|
| 2017 |
GRS 1915+105 |
0.15 |
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 |
OPEN |
KARRI KOLJONEN |
|
100 |
0 |
0 |
0 |
|
| 2036 |
LSP/ISP BLAZAR |
0.5 |
MEDIUM |
The ToO will be triggered if the flux of an LSP or an ISP blazar exceeds 4x10^{-11}erg s^{-1}cm{^-2} at 2-8 keV. We will use Fermi, VHE, and Swift Atels and our optical monitoring to identify a flaring LSP or ISP blazar. A Swift ToO will be triggered to measure the X-ray flux of the source if its gamma-ray flux exceeds 1x10^{-6}ph/s/cm^2 and R band brightness increases at least by 1 mag. |
0.5 |
2.5 |
OPEN |
SVETLANA JORSTAD |
|
900 |
0 |
20 |
14 |
|
| 2041 |
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 |
OPEN |
SERGEY TSYGANKOV |
6 |
400 |
0 |
0 |
0 |
|
| 2098 |
4U 1630-47 |
0.33 |
MEDIUM |
The IXPE and NICER observations will be triggered by a rapid increase in the MAXI 2-4~keV count rate from day-to-day, with rate differential exceeding 0.15 photons/s/cm^2/day. |
33.67 |
0.6 |
OPEN |
JAMES STEINER |
2 |
300 |
7 |
0 |
0 |
|
| 2102 |
SWIFT J0243.6+6124 |
0.03 |
MEDIUM |
The three observations will be triggered based on the MAXI and Swift-BAT monitoring programs. The observations should be triggered when the MAXI-GSC (2 20 keV) count rate is higher than 20 ct s^- 1 cm^-2 (or 1.2 ct s^-1 cm^-2 for Swift-BAT). We require one observation per 7 days. |
900 |
0.17 |
GRAY |
HONGHUI LIU |
|
300 |
0 |
0 |
0 |
|
| 2138 |
ACCRETING MSP |
0.5 |
MEDIUM |
A flux 3E-10 erg/cm2/s (0.5-10 keV, = 10 mCrab), as detected by All Sky X-ray monitors. Monitoring with optical robotic telescopes will also be used to detect the onset of an outburst a few days before the source brightens in X-rays. |
3.87 |
0.8 |
OPEN |
ALESSANDRO PAPITTO |
6 |
900 |
0 |
0 |
0 |
|
| 2151 |
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, or NICER). |
7.6 |
1.1 |
OPEN |
JAMES STEINER |
2 |
200 |
5 |
20 |
0 |
| 2151 |
H1743-322 |
0.4 |
LOW |
(1) H1743-322 has exceeded 250 mCrab intensity during the outburst (e.g., seen by MAXI). (2) H1743-322 shows transition to thermal state, defined as MAXI color [4-10/2-4] < 0.25, or if NICER is monitoring, NICER color [4-12/2-4] < 0.2. (3) Thermal state persists for a duration >= 1 week (hardness criterion holds). |
30 |
0.8 |
OPEN |
JAMES STEINER |
2 |
120 |
5 |
20 |
0 |
|
| 2153 |
T CRB |
0.5 |
HIGH |
After the onset of the nova event that will be known from optical observations. |
4.2 |
3 |
OPEN |
MANEL ERRANDO |
6 |
500 |
0 |
0 |
0 |
|
| 2156 |
AQL X-1 |
0.31 |
MEDIUM |
We will use the trigger from the XB-NEWS monitoring campaign with observed the source daily to detect start of the optical outburst. The optical outburst for this source is expected to start roughly 11 days before X-ray rise, which places proposed response time as a medium priority trigger. This trigger will observe the source in hard state. |
33 |
1.4 |
OPEN |
YASH BHARGAVA |
|
300 |
8 |
20 |
0 |
| 2156 |
AQL X-1 |
0.31 |
MEDIUM |
To trigger the soft state observation, we will use the MAXI daily lightcurves to monitor the transition of the source. Prior outbursts indicate that the transition in the source takes about 10 days which will be sufficient to trigger the soft state observation. |
116.8 |
0.5 |
OPEN |
YASH BHARGAVA |
|
100 |
2 |
20 |
0 |
|
| 2176 |
CANDIDATE NU BLAZAR |
0.2 |
MEDIUM |
An IceCube real-time neutrino event alert and a nearby low-frequency-peaked blazar with a 2-10 keV flux >10^-11 erg s^-1 cm^-2 and a power-law index <=2 observed by Swift-XRT |
0.074 |
14 |
OPEN |
QI FENG |
|
200 |
0 |
0 |
0 |
|
| 2189 |
RELATIVISTIC_TDE |
0.2 |
MEDIUM |
A relativistic jetted TDE with a 2-8 keV flux of >2e-11 erg/s/cm^2. |
0.14 |
10 |
OPEN |
DHEERAJ PASHAM |
|
150 |
45 |
0 |
0 |
|
| 2190 |
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 NICER > 15e-10 erg cm-2 s-1 or VERITAS >5e-10 ph m-2 s-1 above 200 GeV |
3.1 |
7 |
OPEN |
OLIVIER HERVET |
|
150 |
0 |
0 |
28 |
|
| 2191 |
4U 1630-47 |
0.5 |
MEDIUM |
We will monitor the outburst of the source through MAXI and any other publicly available X-ray datasets. We will trigger the IXPE observation as soon as: 1) the source reaches a MAXI HR at which absorption lines have been previously detected or pure soft states, or 2) clear X-ray absorption lines are reported in the current outburst. |
28.2 |
0.5 |
OPEN |
MAXIME PARRA |
|
165 |
15 |
20 |
0 |
| 2191 |
H 1743-322 |
0.1 |
MEDIUM |
We will monitor the outburst of the source through MAXI and any other publicly available X-ray datasets. We will trigger the IXPE observation as soon as: 1) the source reaches a MAXI HR at which absorption lines have been previously detected or pure soft states, or 2) clear X-ray absorption lines are reported in the current outburst. |
78.2 |
0.4 |
OPEN |
MAXIME PARRA |
|
0 |
0 |
0 |
0 |
| 2191 |
GRO J1655-40 |
0.05 |
MEDIUM |
We will monitor the outburst of the source through MAXI and any other publicly available X-ray datasets. We will trigger the IXPE observation as soon as: 1) the source reaches a MAXI HR at which absorption lines have been previously detected or pure soft states, or 2) clear X-ray absorption lines are reported in the current outburst. |
143.2 |
0.3 |
OPEN |
MAXIME PARRA |
|
0 |
0 |
0 |
0 |
| 2191 |
IGR J17091-3624 |
0.1 |
MEDIUM |
We will monitor the outburst of the source through MAXI and any other publicly available X-ray datasets. We will trigger the IXPE observation as soon as: 1) the source reaches a MAXI HR at which absorption lines have been previously detected or pure soft states, or 2) clear X-ray absorption lines are reported in the current outburst. |
17.3 |
0.7 |
OPEN |
MAXIME PARRA |
|
0 |
0 |
0 |
0 |
| 2191 |
WIND EMITTING BHLMXB |
0.25 |
MEDIUM |
We will monitor the outburst of the source through MAXI and any other publicly available X-ray datasets. We will trigger the IXPE observation as soon as: 1) the source reaches a MAXI HR at which absorption lines have been previously detected or pure soft states, or 2) clear X-ray absorption lines are reported in the current outburst. |
4.7 |
1.4 |
OPEN |
MAXIME PARRA |
|
0 |
0 |
0 |
0 |
|
| 2239 |
GS 1826-24 |
0.1 |
LOW |
We will regularly monitor the spectral state of the source by using the publicly available MAXI/GSC observations and trigger the Target of Opportunity observation when the source has transitioned to the hard state. The trigger probability is based on the time interval between 1) when it fully transitioned to the soft state and now, and 2) the time interval when it was in the hard state before. |
2.6 |
4 |
OPEN |
MASON NG |
|
630 |
0 |
0 |
0 |
