Characteristics of Swift’s intermediate population bursts

Slides:



Advertisements
Similar presentations
Vanessa Mangano - Venice 2006 Rest frame light curves of Swift GRBs Vanessa Mangano, Giancarlo Cusumano, Valentina La Parola, Eleonora Troja, Teresa Mineo.
Advertisements

GRB : a canonical fake short burst L. Caito, M.G. Bernardini, C.L. Bianco, M.G. Dainotti, R. Guida, R. Ruffini. 3 rd Stueckelberg Workshop July 8–18,
GRBs as cosmological probes Thomas Krühler (DARK) Thanks to J. Fynbo, D. Malesani, J. Hjorth, J. Greiner, D. A. Kann, D. Perley, N. Tanvir, S. Klose and.
Testing the blast wave model with Swift GRBs Peter A. Curran Mullard Space Science Laboratory, UCL with RLC Starling, AJ van der Horst, A Kamble, RAMJ.
GRB Spectral-Energy correlations: perspectives and issues
The Robotic Palomar 60-inch Optical Afterglow Catalog: 2007 János Kelemen, Konkoly Observatory S. Bradley Cenko, CalTech. SRL Derek Fox, Penn State Univ.
Wen-fai Fong Harvard University Advisor: Edo Berger LIGO Open Data Workshop, Livingston, LA GRB ACS/F606W.
Gamma-ray Bursts in Starburst Galaxies Introduction: At least some long duration GRBs are caused by exploding stars, which could be reflected by colours.
DETERMINING THE DUST EXTINCTION OF GAMMA-RAY BURST HOST GALAXIES: A DIRECT METHOD BASED ON OPTICAL AND X-RAY PHOTOMETRY Li Yuan 黎原 Purple Mountain Observatory.
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.
Fundamental Properties of GRB-Selected Galaxies: A Swift/VLT Legacy Survey Palli Jakobsson Centre for Astrophysics Research (University of Hertfordshire)
The line-of-sight towards GRB at z = 2.66: Probing matter at stellar, galactic and intergalactic scales Palli Jakobsson Astronomical Observatory.
Swift Identification of Dark GRBs Palli Jakobsson Jens Hjorth Darach Watson Kristian Pedersen Johan P. U. Fynbo Gulli Björnsson Javier Gorosabel ApJ Letters,
A burst of new ideas Nature Vol /28 December 2006 徐佩君 HEAR group meeting 12/
GRB at z = 5.3 and a Mean Redshift of 2.8 for Swift GRBs A&A, in press (astro-ph/ ) Páll Jakobsson Robert Priddey Darach Watson Priya Natarajan.
Swift Nanjing GRB Conference Prompt Emission Properties of X-ray Flashes and Gamma-ray Bursts T. Sakamoto (CRESST/UMBC/GSFC)
R. Margutti Harvard University LOS ALAMOS Where do we stand Log(Time) Log(Flux) Gamma-ray Prompt X-ray Flares Swift Steep Decay Shallow Decay Normal.
Gamma-ray Bursts in the E-ELT era Rhaana Starling University of Leicester.
The monitoring of GRB afterglows and the study of their host galaxies with the SAO RAS 6-m telescope from 1997 V. Sokolov et al. The review of main results.
Environmental Properties of a Sample of Starburst Galaxies Selected from the 2dFGRS Matt Owers (UNSW) Warrick Couch (UNSW) Chris Blake (UBC) Michael Pracy.
Two birds with one stone: Simultaneous optical polarization monitoring of SN2007uy and XRF080109/SN2008D. Javier Gorosabel Consejo Superior de Investigaciones.
Recent Observations of GRB-Supernovae Bethany Elisa Cobb The George Washington University IAU Symposium 279 March 13, 2012.
01/02/2009Moriond th Rencontres de Moriond Very High Energy Phenomena in the Universe Why the Swift GRB redshift distribution is changing in time.
The First Constraint on the Reionization from GRBs: the Case of GRB Tomonori Totani (Kyoto) Nobuyuki Kawai, George Kosugi, Kentaro Aoki, Toru Yamada,
Angular distribution of GRBs Lajos G. Balázs Konkoly Observatory. Budapest Collaborators: Zs. Bagoly (ELTE). I. Horváth (ZMNE). A. Mészáros (Ch. Univ.
Is the Amati relation due to selection effects? Lara Nava In collaboration with G. Ghirlanda, G.Ghisellini, C. Firmani Egypt, March 30-April 4, 2009 NeutronStars.
The observations of GRB optical afterglow with 6-meter telescope: recent results and future plans T.A. Fatkhullin and SAO RAS follow-up team Nizhnij Arkhyz,
The Long and the Short of Gamma-Ray Bursts Kevin Hurley UC Berkeley Space Sciences Laboratory.
The Optically Unbiased GRB Host (TOUGH) sample Palli Jakobsson Centre for Astrophysics & Cosmology University of Iceland TOUGH 1: Survey Design and Catalogues.
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.
Dark Gamma-Ray Bursts and their Host Galaxies Volnova Alina (IKI RAS), Pozanenko Alexei (IKI RAS)
Radio faint GRB afterglows Sydney Institute for Astronomy (SIfA)/ CAASTRO – The University of Sydney Dr. Paul Hancock with Bryan Gaensler, Tara Murphy,
Host Galaxy of Dark Gamma-Ray Burst GRB Host Galaxy of Dark Gamma-Ray Burst GRB A. Volnova (SAI MSU), A. Pozanenko (ISR RAS), V. Rumyantsev.
Is Angular Distribution of GRBs random? Lajos G. Balázs Konkoly Observatory, Budapest Collaborators: Zs. Bagoly (ELTE), I. Horváth (ZMNE), A. Mészáros.
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,
Galactic Astronomy - Paper Luminosity Functions of GRB Afterglows Dong-hyun Lee 2007/09/18.
The GRB Luminosity Function in the light of Swift 2-year data by Ruben Salvaterra Università di Milano-Bicocca.
Elisabetta Maiorano IASF/INAF, Sezione di Bologna & Dip. Astronomia, Università di Bologna GRB : the burst before the Burst.
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.
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)
Dust-Obscured Gamma-Ray Bursts and the Cosmic Star-Formation Rate Daniel A. Perley (Caltech) A significant minority of GRBs are heavily obscured 4, 5,
Gamma Ray Burst Spectroscopy!. Collaborators: Caltech/Carnegie/Gemini GRB group including Edo Berger, Derek Fox, Antonino Cucchiari, Shri Kulkarni, Alicia.
A complete sample of long bright Swift GRBs: correlation studies Paolo D’Avanzo INAF-Osservatorio Astronomico di Brera S. Campana (OAB) S. Covino (OAB)
1 Gravitational waves from short Gamma-Ray Bursts Dafne Guetta (Rome Obs.) In collaboration with Luigi Stella.
Classification of Gamma-Ray Bursts: an observational review Paolo D’Avanzo INAF – Osservatorio Astronomico di Brera.
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.
Sesto Workshop Daniel Perley Keck Observations of GRB Host Galaxies Keck Observations of 150 GRB Host Galaxies Daniel Perley +Joshua Bloom,
The Host Galaxies of Dust-Obscured Gamma-Ray Bursts
A connection between the 2175 Å dust feature and CI?
Dark Energy Equation-of-State parameter for high redshifts
Gamma-ray Bursts (GRBs)
Dust-Obscured Gamma-Ray Bursts and the Cosmic Star-Formation Rate
GRB host galaxies: A legacy approach Daniele Malesani Collaborators:
Extinction Curves from Gamma-ray Burst Afterglows
Is Angular Distribution of GRBs random?
“Dark” GRB in a Dusty Massive Galaxy at z ~ 2
P. Filliatre Astroparticule et Cosmologie CEA/Service d’Astrophysique
Discovery of the near-IR Afterglow of GRB
Dark Gamma-Ray Bursts and their Host Galaxies
Speaker: Longbiao Li Collaborators: Yongfeng Huang, Zhibin Zhang,
Centre for Astrophysics & Cosmology
GRB and GRB Two long high-energy GRBs detected by Fermi
Center for Computational Physics
Swift observations of X-Ray naked GRBs
Tight Liso-Ep-Γ0 Relation of Long Gamma-Ray Bursts
Paolo D’Avanzo (INAF-Osservatorio Astronomico di Brera);
Presentation transcript:

Characteristics of Swift’s intermediate population bursts A. de Ugarte Postigo, I. Horvath , P. Veres , Z. Bagoly , L. G. Balazs , D. A. Kann , C. C. Thöne , P. D’Avanzo, M.A. Aloy , S. Campana , S. Foley , J. Mao , S. Covino, A. J. Castro-Tirado, J. P. U. Fynbo , J. Gorosabel , P. Jakobsson , L. Amati , and M. Nardini

Sample and classification Classification by Horváth et al. (2010). Clustering analysis. First 4 years of Swift. Burst with redshift (136): 12 short 28 intermediate 82 long Contamination is significant!

Redshift distribution Median redshift: 0.46 for short 1.33 for intermediate 2.05 for long K-S test: Short-long: 0.0004% Short-interm.: 0.6% Interm.-long: 7%

Afterglow luminosity: X-ray K-S test at 100 sec: Short-Interm.: 2.2% Short-Long: 0.02% Interm.-Long: 0.003% K-S test at 104 sec: Short-Interm.: 0.13% Short-Long: 0.003% Interm.-Long: 0.002%

Afterglow luminosity: Optical K-S test at 100 sec: Interm.-Long: 11% K-S test at 104 sec: Interm.-Long: 3.3%

Dark bursts Intermediate: 5 out of 32 are dark (16%). Long: 27 out of 90 are dark (30%). K-S test with only detections give 4.6% of coming from the same population.

Hydrogen column density X-ray: Intermediate bursts similar to long: K-S test gives 5.1% Optical: Small amount of data to do statistics. There is no clear trend.

Optical extinction Same distribution as for long bursts. K-S test gives 61% probability of coming from the same population.

Epeak vs. Eiso correlation Valid for long GRBs but not for short Mostly valid for intermediate bursts. Slight trend to find them above the fit

Spectral lags Short have negligible lags, while intermediate and long tend to positive lags. K-S test: Short-Long: 0.017% Short-Interm.: 0.009% Interm.-Long: 77%

Conclusions Intermediate GRBs are similar to long GRBs in: Spectral lags Epeak vs. Eiso correlation Similar intrinsic extinction But they differ in other aspects: Afterglow luminosity (specially in X-rays) Slightly lower redshifts More long dark bursts Differences with short bursts are more significant Same progenitor as long bursts but with slightly different conditions

Thanks!!!