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main:grb_observing [2014/11/06 01:36]
bruce 		main:grb_observing [2021/01/12 00:50] (current)
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 ====== Observing GRBs ====== ====== Observing GRBs ======
 +----
  
  
 +====== Space Backgrounds & Environment======
 +----
  
-====== X-ray Observations ====== 
  
 +===== Particle & CR Environment and Issues =====
  
  
 +^Document Name+Link^Date^Type^Author^Comment^Keywords^
 +|"World Maps of Constant B, L, and Flux Contours", E. G. Stassinopoulos, NASA SP-3054, Goddard Space Flight Center, 1970 {{:main:stassinopoulos_earth_mag_field_particles.pdf|stassinopoulos.pdf}} |1970|NASA Report|Stassinopoulos|Reference on Space Particle Environment|Particle background, latitude, SAA, electron population, particle contours, high background region, map of radiation belts, van allen belts, cutoff of rigidity,COR|
  
  
-Observing GRB in X-rays: +===== Diffuse X-ray Background ===== 
-GRB and Background Basics+ 
 +===== Diffuse UV background ===== 
 + 
 + 
 + is given in [[Media:1987AJ_____94__876O.pdf]] 
 + 
 +===== Diffuse Optical-IR background ===== 
 + 
 +My favorite plot of space (zodiacal) background opt-NIR is the one by Michael Lampton (though I think aldering's analysis below is better:  
 + 
 +{{ :main:lampton_space_bgnd.png?direct&300 |lampton_space_bgnd.png}} 
 + 
 +I believe you can take as definitive Greg Aldering's analysis of space background for SNAP {{:main:aldering01_space_zodi.pdf|aldering01_space_zodi.pdf}} DO NOT USE without attribution!!! (called the "white paper" elsewhere, probably a section of, or a study for the white paper; the original file was just called zodi.ps).   
 + 
 +It is important to understand that the zodi varies depending on angle between sun and pointing.  I *think* in the optical it doesn't vary so much, but don't quote me on that.  
 +</ul> 
 +</ul> 
 + 
 + 
 + 
 +====== X-ray Observations ====== 
 +---- 
  
 ===== Spectral Slopes ===== ===== Spectral Slopes =====
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-====== X-ray Energy Band Selection ======+===== X-ray Energy Band Selection =====
  
  
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 File:grb_vs_dxrb_spectra.png File:grb_vs_dxrb_spectra.png
-{{ :main:observing_xbands:grb_vs_dxrb_spectra.png?direct&300 |}}+{{ :main:observing_xbands:grb_vs_dxrb_spectra.png?direct&600 |}}
  
 So, the DXRB is almost as hard as SGRB up to ~ 25 keV, then it is very steep. So, the DXRB is almost as hard as SGRB up to ~ 25 keV, then it is very steep.
 Now let's see that in Counts space, which helps visualize results below. Now let's see that in Counts space, which helps visualize results below.
 File:grbvdxrb_counts.png File:grbvdxrb_counts.png
-{{ :main:observing_xbands:grbvdxrb_counts.png?direct&300 |}}+{{ :main:observing_xbands:grbvdxrb_counts.png?direct&600 |}}
  
 How far should I integrate up or down?  How far should I integrate up or down? 
  
  
-======= How Far to Integrate Down in Energy ======++==== How Far to Integrate Down in Energy ====
  
  
-======= How far to integrate up in energy  =======+ 
 +==== How far to integrate up in energy  ====
  
  
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 If you integrate spectra in count rate space, you see that LGRB rise briskly to ~ 25 keV, then gradually flatten. File:intgd_spectra.png If you integrate spectra in count rate space, you see that LGRB rise briskly to ~ 25 keV, then gradually flatten. File:intgd_spectra.png
-{{ :main:observing_xbands:intgd_spectra.png?direct&300 |}}+{{ :main:observing_xbands:intgd_spectra.png?direct&600 |}}
  
 However, if you make a VERY SIMPLE assumption that the background is dominated by the DXRB (it isn't!! There are particles!!!!) you could make a simple argument that you should integrate to high energies because S/N keeps improving:  File:simplified_snr_vs_Emax.png However, if you make a VERY SIMPLE assumption that the background is dominated by the DXRB (it isn't!! There are particles!!!!) you could make a simple argument that you should integrate to high energies because S/N keeps improving:  File:simplified_snr_vs_Emax.png
-{{ :main:observing_xbands:simplified_snr_vs_emax.png?direct&300 |}}+{{ :main:observing_xbands:simplified_snr_vs_emax.png?direct&600 |}}
  
 So, I suspect the particle background spectrum is very hard, and truth is not so optimistic (without active veto). Still, it seems that it should be OK to go all the way up to 100 keV (but recall Chris' caution about being saturated by particle and other events just over your maximum energy threshold; take care with finite resolution and dynamic range). So, I suspect the particle background spectrum is very hard, and truth is not so optimistic (without active veto). Still, it seems that it should be OK to go all the way up to 100 keV (but recall Chris' caution about being saturated by particle and other events just over your maximum energy threshold; take care with finite resolution and dynamic range).
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 Note that the SGRB are still rising at the highest energy while the LGRB is flattening. Note that the SGRB are still rising at the highest energy while the LGRB is flattening.
  
 +
 +----
 +
 +===== What about integrating down? =====
 +  
 +
 +How far down should one go in energy before this is not favorable increase in S/N? 
 +
 +{{ :main:observing_xbands:grb_intgd_down.png?direct&600 |}}  this from singu!~/projects/xethreshhi2lo.pro
 +
 +{{ :main:observing_xbands:grb_snr_intgd_down.png?direct&600 |}}
 +
 +So, its quite clear that you still get photons for BOTH spectra in this idealized picture.  I think even HETE got like one SGRB (don't quote me). 
  
  
  
 ====== Optical Observations ====== ====== Optical Observations ======
 +----
 +
 +
 +===== Lya Forest Spectroscopy =====
 + 
 +
 +Of interest because high-z grb may provide very bright light sources for very high-z Lyman Alpha Forests.
 +
 +
  
 +Some papers to check out some day: 
  
 +http://arxiv.org/abs/1309.1477v1      Observational Requirements for Lyman-alpha Forest Tomographic Mapping of Large-Scale Structure at z ~ 2
  
  
main/grb_observing.1415237819.txt.gz · Last modified: 2021/01/12 00:50 (external edit)

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