R. Margutti Harvard University LOS ALAMOS 2011. Where do we stand Log(Time) Log(Flux) Gamma-ray Prompt X-ray Flares Swift Steep Decay Shallow Decay Normal.

Slides:

Advertisements

Similar presentations

Masanori Ohno (ISAS/JAXA). HXD: keV WAM: 50keV-5MeV XIS: keV X-ray Afterglow (XIS + HXD withToO) Wide energy band ( keV) Ultra-low.

Advertisements

PHASES OF SWIFT X-RAY AFTERGLOWS ( properties and theoretical interpretation ) A. Panaitescu Los Alamos National Laboratory.

Klein-Nishina effect on high-energy gamma-ray emission of GRBs Xiang-Yu Wang ( 王祥玉） Nanjing University, China （南京大學） Co-authors: Hao-Ning He (NJU), Zhuo.

Solar flare hard X-ray spikes observed by RHESSI: a statistical study Jianxia Cheng Jiong Qiu, Mingde Ding, and Haimin Wang.

Bruce Gendre Osservatorio di Roma / ASI Science Data Center Recent activities from the TAROT/Zadko network.

Swift observations of black hole candidate XTE J with P. Casella. T.J. Maccarone & P.A. Evans Peter A. Curran Laboratoire AIM, Irfu /Service d'Astrophysique.

satelliteexperimentdetector type energy band, MeV min time resolution CGRO OSSE NaI(Tl)-CsI(Na) phoswich 0.05–10 4ms COMPTELNaI0.7–300.1s EGRET TASCSNaI(Tl)1-2001s.

Yun-Wei YU 俞云伟 June 22, 2010, Hong Kong. Outline  Background  Implications from the shallow decay afterglows of GRBs  A qualitative discussion on magnetar.

Raffaella Margutti Harvard – Institute for Theory and Computation On behalf of the Harvard SN forensic team Kyoto2013 What happens when jets barely break.

Optical Emission Components of Gamma-Ray Burst Phenomenon Enwei Liang GXU-NAOC Center for Astrophys. & Space Sci. Co-authors: Liang Li (GXU), Shuangxi.

GRB Spectral-Energy correlations: perspectives and issues

Swift/BAT Hard X-ray Survey Preliminary results in Markwardt et al ' energy coded color.

Correlated radio/gamma-ray variability  The hypothesis of correlated variability in radio and gamma-ray is popular  It would indicate a common spatial.

Reverse Shocks and Prompt Emission Mark Bandstra Astro

Global Properties of X-ray Afterglows Observed with XRT ENWEI LIANG （梁恩维） University of Guangxi, Nanning astro.gxu.edu.cn Nanjing

Spectral Energy Correlations in BATSE long GRB Guido Barbiellini and Francesco Longo University and INFN, Trieste In collaboration with A.Celotti and Z.Bosnjak.

XRF associated with SN 2006aj Nature, Val 442 Aug.31 issues Campana et al. p.1008 Pian et al. P Soderberg et al. p.1014 Paolo et al. p.1018.

The questions: How can gamma-ray blazar statistics be parameterized? What parameters fit EGRET data best? –Blazar redshift distribution [ N vs z ] –Blazar.

1 Understanding GRBs at LAT Energies Robert D. Preece Dept. of Physics UAH Robert D. Preece Dept. of Physics UAH.

A burst of new ideas Nature Vol /28 December 2006 徐佩君 HEAR group meeting 12/

The Canonical Swift/UVOT Lightcurve Sam Oates (UCL-MSSL) On behalf of the Swift/UVOT team UCL DEPARTMENT OF SPACE AND CLIMATE PHYSICS MULLARD SPACE SCIENCE.

SLAC, 7 October Multifrequency Strategies for the Identification of Gamma-Ray Sources Marcus Ziegler Santa Cruz Institute for Particle Physics Gamma-ray.

Gamma-Ray Burst Early Afterglows Bing Zhang Physics Department University of Nevada, Las Vegas Dec. 11, 2005, Chicago, IL.

UV/Optical Properties of GRBs with Swift UVOT P. Roming (Penn State University)

Gamma Ray Bursts and LIGO Emelie Harstad University of Oregon HEP Group Meeting Aug 6, 2007.

P. Price (U. of Hawaii) and many others Discovery and identification of the very high redshift afterglow of GRB J. B. Haislip, et al. astro-ph ,

Swift Nanjing GRB Conference Prompt Emission Properties of X-ray Flashes and Gamma-ray Bursts T. Sakamoto (CRESST/UMBC/GSFC)

SONG and mini-SONG Observations of GRB Pulsed Emission Jon Hakkila Presented at the 4th SONG Workshop September 17, 2011 Presented at the 4th SONG Workshop.

X-Ray Flashes D. Q. Lamb (U. Chicago) “Astrophysical Sources of High-Energy Particles and Radiation” Torun, Poland, 21 June 2005 HETE-2Swift.

Jet Models of X-Ray Flashes D. Q. Lamb (U. Chicago) Triggering Relativistic Jets Cozumel, Mexico 27 March –1 April 2005.

Testing a two-jet model of short Gamma-ray bursts A. Pozanenko 1 M. Barkov 2,1 P. Minaev 1 1 Space Research Institute (IKI) 2 Max-Planck Institut für Kernphysik.

Swift Annapolis GRB Conference Prompt Emission Properties of Swift GRBs T. Sakamoto (CRESST/UMBC/GSFC) On behalf of Swift/BAT team.

Swift Kyoto GRB Conference BAT2 GRB Catalog Prompt Emission Properties of Swift GRBs T. Sakamoto (CRESST/UMBC/GSFC) on behalf of Swift/BAT.

GRB s CENTRAL -ENGINE & FLARes WARSAW Guido Chincarini & Raffaella margutti 1WARSAW 2009.

Table 2. Latest Results Comparing Prompt Emission from X-ray Flashes and Gamma-Ray Bursts Latest Results Comparing Prompt Emission from X-ray Flashes and.

Rise and Fall of the X-ray flash : an off-axis jet? C.Guidorzi 1,2,3 on behalf of a large collaboration of the Swift, Liverpool and Faulkes Telescopes,

Tests of Curvature Effects in the Temporal and Spectral Properties of GRB Pulses Ashwin Shenoy 1 In collaboration with Eda Sonbas 2, Charles Dermer 3,

Tight correlations in ‘canonical’ lightcurves of Gamma Ray Bursts M.G. Dainotti 1, R. Willingale 2, V.F. Cardone 3, S. Capozziello 4, M. Ostrowski 1 Dainotti.

Gamma-Ray Bursts observed by XMM-Newton Paul O’Brien X-ray and Observational Astronomy Group, University of Leicester Collaborators:- James Reeves, Darach.

June 5, 2006Swift and GRBs1 Soft Gamma-ray observations of GRB prompt emission with Suzaku Wideband All-sky Monitor Masanori Ohno, Yasushi Fukazawa, Kazutaka.

Fermi Observations of Gamma-ray Bursts Masanori Ohno(ISAS/JAXA) on behalf of Fermi LAT/GBM collaborations April 19, Deciphering the Ancient Universe.

Dark Gamma-Ray Bursts and their Host Galaxies Volnova Alina (IKI RAS), Pozanenko Alexei (IKI RAS)

SONG Targets of Opportunity: Searching for Pulses in Gamma-Ray Burst Afterglows Jon Hakkila.

Gamma-Ray Bursts: Open Questions and Looking Forward Ehud Nakar Tel-Aviv University 2009 Fermi Symposium Nov. 3, 2009.

Stochastic Wake Field particle acceleration in GRB G. Barbiellini (1), F. Longo (1), N.Omodei (2), P.Tommasini (3), D.Giulietti (3), A.Celotti (4), M.Tavani.

G O D D A R D S P A C E F L I G H T C E N T E R 1 Recent GRB Results from Swift John Cannizzo/UMBC/Goddard LSC Meeting, Hanford, WA August 16, 2005 LIGO-G Z.

Moriond – 1 st -8 th Feb 2009 – La Thuile, Italy. Page 1 GRB results from the Swift mission Phil Evans, Paul O'Brien and the Swift team.

Dave Tierney S. McBreen, R. Preece, G. Fitzpatrick and the GBM Team Low-Energy Spectral Deviations in a Sample of GBM GRBs DT acknowledges support from.

The Lag-Luminosity Relation in the GRB Source Frame T. N. Ukwatta 1,2, K. S. Dhuga 1, M. Stamatikos 3, W. C. Parke 1, T. Sakamoto 2, S. D. Barthelmy 2,

Gamma-Ray Burst Ring-shaped Jets And Their Afterglows Ming Xu Department of Astronomy, Nanjing University Gamma-ray Sky from Fermi: Neutron.

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…

The Radio Evolution of the Galactic Center Magnetar Joseph Gelfand (NYUAD / CCPP) Scott Ransom (NRAO), Chryssa Kouveliotou (GWU), Mallory S.E. Roberts.

25s detection of the Sy1 galaxy NGC3516 The Palermo BAT survey project Application to a sample of SDSS LINERs V. La Parola, A.Segreto, G. Cusumano, V.

A relation to estimate the redshift from the X-ray afterglow light curve Bruce Gendre (IASF-Roma/INAF) & Michel Boër (OHP/CNRS)

Masnori Ohno (ISAS/JAXA). Long/Short GRBs are different ? There are two GRB classes, Long/Short GRBs in T90 distribution Different origin ? Hardness ratio;

Daisuke YONETOKU (Kanazawa Univ.) T. Murakami (Kanazawa Univ.), R. Tsutsui, T. Nakamura (Kyoto Univ.), K. Takahashi (Nagoya Univ.) The Spectral Ep–Lp and.

Alessandra Corsi (1,2) Dafne Guetta (3) & Luigi Piro (2) (1)Università di Roma Sapienza (2)INAF/IASF-Roma (3)INAF/OAR-Roma Fermi Symposium 2009, Washington.

Fermi GBM Observations of Gamma-Ray Bursts Michael S. Briggs on behalf of the Fermi GBM Team Max-Planck-Institut für extraterrestrische Physik NASA Marshall.

R. M. Kippen (LANL) – 1 – 23 April, 2002  Short transients detected in WFC (2–25 keV) with little/no signal in GRBM (40–700 keV) and no BATSE (>20 keV)

Stochastic wake field particle acceleration in Gamma-Ray Bursts Barbiellini G., Longo F. (1), Omodei N. (2), Giulietti D., Tommassini P. (3), Celotti A.

A complete sample of long bright Swift GRBs: correlation studies Paolo D’Avanzo INAF-Osservatorio Astronomico di Brera S. Campana (OAB) S. Covino (OAB)

Gamma-ray bursts Tomasz Bulik CAM K, Warsaw. Outline ● Observations: prompt gamma emission, afterglows ● Theoretical modeling ● Current challenges in.

Fermi Gamma-ray Burst Monitor

The Mysterious Burst After the Short Burst Jay Norris Brief History, Overview, Central Questions Spectral lag distributions (long & short GRBs) Pulse width.

1 HETE-II Catalogue HETE-II Catalogue Filip Münz, Elisabetta Maiorano and Graziella Pizzichini and Graziella Pizzichini for HETE team Burst statistics.

Gamma-ray Bursts (GRBs)

GRB spectral evolution: from complex profile to basic structure

GRB and GRB Two long high-energy GRBs detected by Fermi

Swift observations of X-Ray naked GRBs

GRB spectral evolution: from complex profile to basic structure

Presentation transcript:

R. Margutti Harvard University LOS ALAMOS 2011

Where do we stand Log(Time) Log(Flux) Gamma-ray Prompt X-ray Flares Swift Steep Decay Shallow Decay Normal Decay s s~10 4 s t -1 Is there any physical link between a prompt pulse and an X-ray flare?

Log(Time) Log(Flux) Gamma-ray Prompt X-ray Flares Flares are softer and less energetic time-stretched versions of a prompt pulse Margutti et al., 2010,MNRAS, 406, 2149 Temporal Properties 1.Pulse Asymmetry 2.Fast rise- Exponential decay Spectral Properties 1.Band spectral energy distribution 2.Peak energy evolution with time Ep(t) 3. Ep(t)-Liso(t) 4. Lag-Luminosity relation

Lag-Luminosity PROMPT FLARES Lag Margutti et al., 2010,MNRAS, 406, 2149 LONG!!!!

LOS ALAMOS A A A

LOS ALAMOS 2011

Different tools Different definitions (e.g. pulse-peak lag vs. CCF lag) PULSE property vs. Time-averaged measurements Strongly dependent on the definition of the energy bands used Using rest-frame defined energy bands is enough?

LOS ALAMOS 2011 Different tools Different definitions (e.g. pulse-peak lag vs. CCF lag) PULSE property vs. Time-averaged measurements Strongly dependent on the definition of the energy bands used Using rest-frame defined energy bands is enough?

LOS ALAMOS 2011 Homogenous analysis of a statistically significant number of GRBs Step back to the analysis of more basic effects that are known to contribute to the lag measure to understand how each of them is correlated to the final lag measure Time resolved approach to determine a MAP of the obs. properties of GRBs with time.

LOS ALAMOS 2011

Epeak (t) alpha (t) beta (t) Lag (t) Variability (t) Pulses properties(t) Pulses properties (E) ??

LOS ALAMOS 2011 Galaxy NNN Gamma-Ray Burst (GRB050822) 1) Selection of a GRB 2) Production of a MAP of properties 3) Writing of a document ACT as a TEAM Useful for FUNDING (we have something to show..)

LOS ALAMOS 2011 WISH LIST: GRB detected by Swift- Fermi Prompt emission seen by XRT Prompt emission see by UVOT Bright Known z …good for GBM-BAT cross calibration…

LOS ALAMOS 2011 Raffaella: Variability Time scale of BAT; XRT expertise (XRT+BAT spectral fits; pulse properties in the X-ray regime) Mike: Time-resolved lag using the CCF John: Prompt Pulse properties List of people to complete….