https://www-astro.lbl.gov/~bruce/docuwikis/grb/ 2026-06-03T19:07:52+00:00 https://www-astro.lbl.gov/~bruce/docuwikis/grb/ https://www-astro.lbl.gov/~bruce/docuwikis/grb/lib/tpl/dokuwiki/images/favicon.ico text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:astro-h&rev=1610412637&do=diff This description from the astro-H webpage (<http://astro-h.isas.jaxa.jp/si/01_e.html>) pretty much says it all: “ The HXI consists of four-layers of 0.5 mm thick Double-sided Silicon Strip Detectors (DSSD) and one layer of 0.5—1 mm thick CdTe imaging detector. In this configuration, soft X-ray photons will be absorbed in the Si part (DSSD), while hard X-ray photons go through the Si part and are detected by the newly developed CdTe double strip detector. Fast timing response of silicon strip … text/html 2023-09-12T12:04:02+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:bggrbinfo&rev=1694520242&do=diff The Great Bruce GRB Info Library Welcome to the famous Bruce GRB Info Library. Please comment and fix. Special GRB List GRBComment080319b Prototype? Naked Eye Burst, probably optically brightest, best optical light curve, proposed two-component jet (Racusin+08 text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:bruce_eor_page&rev=1610412637&do=diff Epoch of Re-ionization and or end of cosmic dark ages. Emission Lines from z=6.5 QSO - Role of AGN feedback in quenching star formation- important to EOR modeling - Maiolino+12 Using [CII] 158 um they got > 10 sigma detection of emission line at IRAM for z=6.5 QSO after 18.5 hours. The observation of weak winds implies star formation, while the observation her eof powerful winds indicates AGN-driven powerful winds which quenches star formation. text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:bruce_grb_blast_page&rev=1610412637&do=diff Theory Framework of GRB Blasts The theoretical basis of the GRB blast wave can be simply described (first para section 2 Nava+12 <http://arxiv.org/pdf/1211.2806.pdf>) by these phases (Somehow Nava starts the numbering sequence after acceleration, but I wanted to add it, so I put in a phase 0): text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:emission&rev=1610412637&do=diff GRB Emission Mechanism Theory I am not the best person to reference on this. I am still trying to clarify my understanding ---------- Pure Synchrotron Emission Shen & Zhang 09 paper 2009, MNRAS 398, 1936 shows that (1) Synchrotron can have the same appearance at gamma, X, but very different manifestations at optical, in four cases. This is the most recent treatment, those below are listed for hisotrical interest. (2) the same paper shows that incredible information, lorentz factor, radius… text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:grbratepredict&rev=1610412637&do=diff Smoot Group Technical Report 2012-11-01.a_BG Title: Prediction of UBAT Detection Rates and Estimation of UBAT Duty Cycle Author: Bruce Grossan Version Number: 1.0 Original Date: 2012-10-31 This Version Date: 2012-11-01 (SSL Technical Report number to follow) text/html 2022-04-15T23:53:26+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:gw170817&rev=1650066806&do=diff GW170817 ---------- The Triggers / Detections Trigger detected by Fermi, Integral (though only ~ 3 sigma Integral (GCN 21507) I doubt this was a GCN socket trigger). Ligo Virgo Collaboration reported Aug 17 12:41:06 GMT 2017 (GCN at 13:21). The Search for the EM Counterpart text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:review_of_blf_measurements&rev=1610412637&do=diff Here is my List of Bulk Lorentz Factor (BLF) measurements: I. HE/ME Delay (Limit) Method (and model-dependence): Done by comparing the time delay between the MeV photons and GeV photons to get a BLF lower limit. Basically, if you follow the literature, you get high BLF limit if you have a one-zone model but can get lower BLF if you have multi-zones (e.g. Chang+12 ApJ 759,129 text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:svom_eclairs&rev=1610412637&do=diff ECLAIRS Sensitivity Curve: <http://arxiv.org/pdf/0807.0738.pdf> Here is a detector efficiency Curve for ECLAIRS: from: <http://proceedings.spiedigitallibrary.org/proceeding.aspx?articleid=1361038> text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:swift_instrument&rev=1610412637&do=diff There is a really great page on Swift Instrument efficiencies areas, capabilities, etc. at : <http://heasarc.nasa.gov/docs/swift/proposals/swift_responses.html> The paper on the uvot calibration is here <http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:0708.2259>. The BAT Response Curve (Efficiency or Effective Area vs. Energy) looks like this: The FWHM Spectral resolution of BAT is given here: text/html 2021-01-12T00:50:37+00:00 Anonymous (anonymous@undisclosed.example.com) https://www-astro.lbl.gov/~bruce/docuwikis/grb/doku.php?id=public:x-ray_observations&rev=1610412637&do=diff 'Observing GRB in X-rays:' <ul> <li>GRB and Background Basics</li> 'Spectral Slopes' 'GRBs' You should look at GRB General Observing>Slopes explanation of GRB spectral slopes; I use here BAT-like instrument results. Sakamoto+11 says BAT sees low-E PL w/Photon index -1.6 for LGRB. For SGRB, sakamoto says low-E Photon index -1.2 for SGRB, very different results from Nava