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--- main:grb_observing [2014/11/06 01:38]
bruce
+++ main:grb_observing [2021/01/12 00:50] (current)
@@ Line 1: / Line 1: @@
 ====== 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 =====
@@ Line 28: / Line 55: @@
-====== X-ray Energy Band Selection ======
+===== X-ray Energy Band Selection =====
@@ Line 44: / Line 71: @@
-======= 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  ====
@@ Line 65: / Line 93: @@
 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 ======
+----
+===== 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

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