Difference between revisions of "EGAL02"

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(Observational settings/limits)
(Proposal)
 
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=== Observational settings/limits ===
 
=== Observational settings/limits ===
  
- original criteria to observe Ton 599
+
- 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
 
  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 (1-1.5 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).'''
+
'''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.'''
 
 
=== Performed observation ===
 
===== Ton 599 =====
 
* 2023-04-19 (no detection)
 
** run 12768, 12769, 12770, 12771, 12772, 12774
 
* 2023-04-23 (3-5 sigma?)
 
** run 12832, 12833, 12834, 12835
 
  
=== Analysis ===
+
== Analysis ==
 
- Summary (Ton599)
 
- Summary (Ton599)
 
https://docs.google.com/presentation/d/1gaDXn9cRdHN7RWg4m9iZqNLSwOAlH4m0W2f5V8CqSI8/edit?usp=sharing
 
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

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