Difference between revisions of "EGAL02"
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=== Observational settings/limits === | === Observational settings/limits === | ||
| − | - | + | - 3C454.3 |
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| + | The observations should be organized through the ToO form when the integral photon flux (>100 MeV) reaches 1×10−5 cm−2 s−1. | ||
| + | In this state, LST-1 is expected to detect low-energy gamma-ray signals with ∼30 hours of observations. | ||
| + | If we detect a significant flare and the integral photon flux is still above the mentioned threshold after the flare, we also request another 30 hours of observations after the flare | ||
| + | |||
| + | - Ton 599 | ||
we request 50 hours of observations unless the average integral photon flux (>100 MeV) goes down below 0.5×10−6 cm−2 s−1 | we request 50 hours of observations unless the average integral photon flux (>100 MeV) goes down below 0.5×10−6 cm−2 s−1 | ||
| − | '''It seems the gamma-ray spectrum of Ton 599 is sometimes hard (<2.0) (especially since April) and variable. So even when integral photon flux above 100 MeV is below the original limit (0.5x10-6 cm-2 s-1), there is a possibility to detect this source. When the spectrum is hard enough (e.g. April 23, 2023), it is detectable for a short observation. Thus, we want to request to schedule short exposure observations (1- | + | '''It seems the gamma-ray spectrum of Ton 599 is sometimes hard (<2.0) (especially since April) and variable. So even when integral photon flux above 100 MeV is below the original limit (0.5x10-6 cm-2 s-1), there is a possibility to detect this source. When the spectrum is hard enough (e.g. April 23, 2023), it is detectable for a short observation. Thus, we want to request to schedule short exposure observations (1-2 hours) for monitoring purposes, rather than longer exposure for less nights, when this source can be scheduled (=no collision with other higher priority tasks/sources). If we detect some signs of active state (e.g. high energy photons), we will contact schedulers.''' |
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== Analysis == | == Analysis == | ||
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- wiki page | - wiki page | ||
| − | https://www.lst1.iac.es/wiki/index.php/TON599 | + | -- https://www.lst1.iac.es/wiki/index.php/TON599 |
| + | -- https://www.lst1.iac.es/wiki/index.php/3C454.3 | ||
Latest revision as of 11:23, 17 January 2024
Proposal[edit]
Proposal: EGAL02:Observations of distant bright FSRQs in active states
PI: Seiya Nozaki (nozaki@mpp.mpg.de)
Source: 3C454.3
RA (J2000) 343.49061685 deg
DEC (J2000) 16.14821153 deg
Source: Ton599
RA (J2000) 179.88264131 deg
DEC (J2000) 29.24550745 deg
Observational settings/limits[edit]
- 3C454.3
The observations should be organized through the ToO form when the integral photon flux (>100 MeV) reaches 1×10−5 cm−2 s−1. In this state, LST-1 is expected to detect low-energy gamma-ray signals with ∼30 hours of observations. If we detect a significant flare and the integral photon flux is still above the mentioned threshold after the flare, we also request another 30 hours of observations after the flare
- Ton 599
we request 50 hours of observations unless the average integral photon flux (>100 MeV) goes down below 0.5×10−6 cm−2 s−1
It seems the gamma-ray spectrum of Ton 599 is sometimes hard (<2.0) (especially since April) and variable. So even when integral photon flux above 100 MeV is below the original limit (0.5x10-6 cm-2 s-1), there is a possibility to detect this source. When the spectrum is hard enough (e.g. April 23, 2023), it is detectable for a short observation. Thus, we want to request to schedule short exposure observations (1-2 hours) for monitoring purposes, rather than longer exposure for less nights, when this source can be scheduled (=no collision with other higher priority tasks/sources). If we detect some signs of active state (e.g. high energy photons), we will contact schedulers.
Analysis[edit]
- Summary (Ton599) https://docs.google.com/presentation/d/1gaDXn9cRdHN7RWg4m9iZqNLSwOAlH4m0W2f5V8CqSI8/edit?usp=sharing
- wiki page -- https://www.lst1.iac.es/wiki/index.php/TON599 -- https://www.lst1.iac.es/wiki/index.php/3C454.3
