1. Francisco Virgili, LJMU June 22, 2012 GRBs 2012 Liverpool C. Mundell, A. Melandri, C. Guidorzi, R. Margutti, A. Gomboc, S. Kobayashi, V. Pal’shin, etc…

2.  GRB 091024 case study Observations Analysis  Temporal  Spectral (limited)  Energetics Interpretation  Other ultra-long GRBs

3. GBM bg subtracted lc Gruber+ 2011

4. BAT emission up to ~T 0 +483 s XRT starting at ~T 0 +53 min Evans+ 2009

5. x 2

6. FTN LT KAIT Super-LOTIS SRO Gemini FTN LT KAIT Super-LOTIS SRO Gemini

7.  3 optical peaks (451 +/- 18 s; 2222 +214 s 5081 +306 s)  No correlation to gamma-ray peaks (~ 0s, 600s, 950 s)  Steep rise/fall of 1st peak

8.  Calculate fractional signal power density (fpd) for various time slices of the KW and BAT lc.  Find a variety of timescales, specifically 2 short timescales (0.5 and 1 s) and 2 long timescales (7 and 14s) R. Margutti+ 2008 (arxiv:0809.0189)

9.  Same analysis as full signal but on three different regimes of the BAT lightcurve: -200:250 s 250:800 s 800:1200 s  Short var in 1 st and 3 rd emission episode  Longer timescales in period of quiescence

10.  Vary over energy channels  Softest energy range has no short timescale component  Hardest scales show clear peak at low variability timescales

11.  Limited spectral information: 1 st episode: BAT+GBM 2 nd and 3 rd : GBM only Waiting on KW spectra (ideally GBM+KW)  All segments fit with CPL  1 st : α = -0.89, Ep=461 keV -0.89, 522 keV (joint)  2 nd : -1.2, 311 keV  3 rd : -1.58, 388 keV -1.57, 275 keV -1.49, 472 keV Gruber+ 2011

12.  z=1.092  Energetics:  Total Eiso: 6-8e53 erg Most (2e53 erg) in last emission episode Time-resolved: Most in very last peak Amati: Consistent (Amati+ 2008)

13.  No radio data (sadly)…but if we did… Extend analysis from Mundell+ 2007, Melandri+ 2009 1 1 100

14.  Table from V. Pal’shin  Also add GRB 110709B (B.B. Zhang’s talk), GRB 111209 (FTN obs)

15.  Long-lived central engine activity (~500- 600s in RF) Similar variability timescales at early and late times  No correlation of gamma and optical emission Different emission regions  Indicative of RS peak followed by FS emission in optical LC Rise/fall slopes of 1 st peak

16.  Comprehensive/broadband study of prompt and any afterglow emission of ultra-long GRBs KW sample has many bursts with good spectral/temporal coverage