1. The Early Time Properties of GRBs : Canonical Afterglow and the Importance of Prolonged Central Engine Activity Andrea Melandri Collaborators : C.G.Mundell, S. Kobayashi, D. Bersier, I. A. Steele, C.Guidorzi, A. Gomboc, R. J. Smith, D. Carter, M. F. Bode Astrophysics Research Institute, Liverpool JMU, UK

2. Outline Canonical X-ray afterglow Early optical light curves: canonical? X-ray/Optical analysis The role of prolonged central engine activity - afterglow detections - dark bursts Beyond the Fireball : GRB 070419A Conclusions

3. Generic X-ray Light curve (Zhang et al. 2006) ~ -3 ~ -0.5 ~ - 1.2 ~ -2 10 2 – 10 3 s10 3 – 10 4 s 10 4 – 10 5 s Prompt Emission High latitude emission Late internal shocks Standard FS emission Jet break Prolonged central engine activity Energy injection into the FS RS with ε B & ε e much larger than for FS Time dependent ε B & ε e Dust scattering Precursor fireball Cannonballs Geometrical models + other …….

4. Typical X-ray Light curve (Nousek et al. 2006, O’Brien et al. 2006)

5. The X-ray “canonical” light curve is not ubiquitous But…. Oddball cases e.g. : Nousek et al. 2006, Evans et al. 2008 Melandri et al. 2008 The same mechanisms should produce the optical radiation. Optical should track X-ray flux, but this is not observed in many GRBs

6. Early Optical Light curve Oates et al. 2009 Melandri et al. 2008 At early times

7. Optical/X-ray analysis Simplest explanation in the Fireball model : A : no break in the Opt or in the X-ray band  C with respect to the Opt and X-ray bands B : no break in the Opt, break in the X-ray band  Passage of C through the X-ray band C : break in the Opt, no break in the X-ray band  Passage of C through the Opt band D : break in the Opt and in the X-ray band  Cessation of energy injection or jet break

8. Optical/X-ray analysis A possible explanation is the additional X-ray emission produced by late-time central engine activity, observed as an enhanced component in late-time afterglow light curves. Sample : 63 GRBs (24 detections + 39 upper limits): We observed achromatic breaks for only 1 GRB. The majority of the afterglows in our sample (14/24) are in good agreement (or consistent) with the standard model. However, for a significant fraction of our sample (10 cases) the observed data can not be explained with this model, even if modifications (i.e. energy injection or variation of the ambient matter) are assumed. Melandri et al. 2008 Detections

9. Optical/X-ray analysis The majority of the bursts are “Dark” independent of the selected time. 10 : were identified at NIR, demonstrating a small population of bursts in high density environments. 29 : we suggest that if late-time central engine activity is responsible for the production of early X-ray afterglow emission then the additional emission will mask the simultaneous (but fainter) FS emission, resulting in a larger observed X-ray flux than expected (while the optical flux is not suppressed). Dark Bursts

10. One case…..070419A (Melandri et al. 2009)  -ray T 90 ~ 110 seconds FRED profile Single shot few hundred seconds long Average  -ray fluence (5 x 10 -7 erg cm -2 ) Peak photon flux (~0.14) at the low end of the distribution for Swift GRBs X-ray Some intrinsic rest-frame absorption Weak evidence for evolution of N H (~4 x 10 21 cm -2 ) and  X (~2.2) Central engine still active up to 10 3 seconds, then FS emission takes over (  X ~1.2)

11. One case…..070419A (Melandri et al. 2009) Optical -1.5 0.6 1.5 0.4 Refreshed shocks could not be ruled out BUT the energy injection rate should be tuned very carefully + we need a sharp cessation of the injection to get a clear break Assumption of a finely tuned long-lived central engine (consistent with the same conditions invoked to explain the plateau phase in many X-ray light curves of GRBs) Clearly too complex to be explained with the FS model Features are too sharp to be explained as density enhancement If RS dominating at early times  t peak ~ 450 s,  ~ 350  t ~ 1500 s = the passage of m,r  m,r ~ 3 x 10 5 Hz; m,f ~  m,r ~ 4 x 10 20 Hz  FS should peak t ~ 4 x 10 6 s !! If the fireball is magnetized (with R B ~ 10 6 ) then m,f could be smaller  the ratio between RS and FS luminosity should be ~ 4 x 10 5 when in reality it is only 2 order of magnitude !!

12. Conclusions 60% of the detected afterglows in our sample are “consistent” with the “standard model” Few GRBs are not easily explained in the context of the simple fireball model even when modification are made (i.e. energy injection, variation of the density matter, magnetized fireball, tail component following the fireball, etc…) The Dark Bursts fraction remains high (~50%) despite deep early-time observations Enhanced X-ray emission from late time central engine activity plays a big role and may explain “non-standard” light curves (like GRB070419A) and Dark Bursts Enhanced X-ray emission from late time central engine activity plays a big role and may explain “non-standard” light curves (like GRB070419A) and Dark Bursts