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GRB physics and cosmology with spectrum-energy correlation

GRB physics and cosmology with spectrum-energy correlation. Lorenzo Amati INAF – IASF Bologna (Italy). Outline GRB: standard scenarios and open issues Spectrum-energy correlation and its implications GRB cosmology with spectrum-energy correlation Future perspectives.

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GRB physics and cosmology with spectrum-energy correlation

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  1. GRB physics and cosmology with spectrum-energy correlation Lorenzo Amati INAF – IASF Bologna (Italy)

  2. Outline • GRB: standard scenarios and open issues • Spectrum-energy correlation and its implications • GRB cosmology with spectrum-energy correlation • Future perspectives

  3. Standard scenarios for GRB origin LONG SHORT • energy budget up to >1054 erg • long duration GRBs • metal rich (Fe, Ni, Co) circum-burst environment • GRBs occur in star forming regions • GRBs are associated with SNe • likelycollimated emission • energy budget up to 1051 - 1052 erg • short duration (< 5 s) • clean circum-burst environment • old stellar population

  4. Standard scenarios for GRB phisics • ms time variability + huge energy + detection of GeV photons -> plasma occurring ultra-relativistic (G > 100) expansion (fireball or firejet) • non thermal spectra -> shocks synchrotron emission (SSM) • fireball internal shocks -> prompt emission • fireball external shock with ISM -> afterglow emission

  5. Open issues (several, despite obs. progress) • GRB prompt emission physics • most time averaged spectra of GRBs are well fit by synchrotron shock models • at early times, some spectra inconsistent with optically thin synchrotron: possible contribution of IC component and/or thermal emission from the fireball photosphere

  6. Afterglow emission physics • consistency with synchrotron predictions found e.g. for GRB 970508 • deviations in the X-ray band from synchrotron: found for GRB000926 (Harrison et al. 2001) and GRB010222 (in ‘t Zand et al. 2001). • they are consistent with relevant Inverse Compton on the low energy photons

  7. Early afterglow • new features seen by Swift in X-ray early afterglow light curves (initial very steep decay, early breaks, flares) mostly unpredicted and unexplained • initial steep decay: continuation of prompt emission, mini break due to patchy shell, IC up-scatter of the reverse shock sinchrotron emission ? • flat decay: probably “refreshed shocks” (due either to long duration ejection or short ejection but with wide range of G) ? • flares: could be due to: refreshed shocks, IC from reverse shock, external density bumps, continued central engine activity, late internal shocks… ~ -3 ( 1 min ≤ t ≤ hours ) ~ -0.7 10^5 – 10^6 s ~ - 1.3 ~ -2 10^2 – 10^3 s 10^4 – 10^5 s

  8. GeV emission • CGRO/EGRET detected VHE (from 30 MeV up to 18 GeV) photons for a few GRBs • VHE emission can last up to thousends of s after GRB onset • average spectrum of 4 events well described by a simple power-law with index ~2 , consistent with extension of low energy spectra • GRB 941017,measured by EGRET-TASC shows a high energy component inconsistent with synchrotron shock model • Recent AGILE detection of 2-3 >500 MeV photons

  9. Prompt optical emission • GRB990123: first detection (by ROTSE) of prompt optical emission • optical light curve does not follow high energy light curve: evidence for a different origin (reverse shock ?) • GRB041219 (RAPTOR) contrary to GRB990123, the optical light curve follows the high energy light curve: evidence for same origin (internal shocks ?)r

  10. the challenging “naked eye” GRB080319B: complexity and energetics Bloom et al. 2008

  11. Circum-burst environment • evidence of overdense and metal enriched circum-burst environment from absorption and emission features • emission lines in afterglow spectrum detected by BeppoSAX but not by Swift • Swift detects intrinsic NH for many GRB afterglows • optical (Lya) NH often inconsistent with X-ray NH prompt afterglow Amati et al.,Science, 2000 Antonelli et al., ApJ, 2001

  12. Collimated or isotropic ? • lack of jet breaks in several Swift X-ray afterglow light curves, in some cases, evidence of achromatic break • challenging evidences for Jet interpretation of break in afterglow light curves or due to present inadequate sampling of optical light curves w/r to X-ray ones and to lack of satisfactory modeling of jets ?

  13. GRB/SN connection • are all long GRB produced by a type Ibc SN progenitor ? • which fraction of type Ibc SN produces a GRB, and what are their peculiarities ? • are the properties (e.g., energetics) of the GRB linked to those of the SN ?

  14. short / long classification and physics • Swift GRB 060614: a long GRB with a very high lower limit to the magnitude of an associated SN -> association with a GRB/SN is excluded • high lower limit to SN also for GRB 060505 (and, less stringently, XRF 040701) • In the spectral lag – peak luminosity plane, GRB060614 lies in the short GRBs region -> need for a new GRB classification scheme ? Gehrels et al., Nature, 2006

  15. Alternative scenarios • EMBH / fireshell model (Ruffini et al.) • CannonBall (CB) (Dar et al.) • Precessing jet (Fargion’s talk), stochastic wakefield plasma acceleration (Barbiellini et al.), ns-quark star transition, … • Short GRB as SGR giant outburst at high z

  16. The Ep,i – Eiso correlation • GRB spectra typically described by the empirical Band function with parameters a= low-energy index, b= high-energy index, E0=break energy • Ep = E0 x (2 + a) = observed peak energy of the nFn spectrum

  17. from redshift, fluence and spectrum, it is possible to estimate the cosmologica-rest frame peak energy, Ep,i, and the radiated energy assuming isotropic emission, Eiso • isotropic luminosities and radiated energy are huge; both Ep,i and Eiso and span several orders of magnitude Ep,i = Epx (1 + z) log(Eiso)= 1.0 , s = 0.9 log(Ep,i )= 2.52 , s = 0.43 (Amati, MNRAS, 2006)

  18. Amati et al. (2002) analyzed a sample of 12 BeppoSAX events with known redshift • we found evidence of a strong correlation between Ep,i and Eiso, highly significant (r = 0.949, chance prob. 0.005%) despite the low number of GRBs included in the sample Ep,i= kEiso (0.52+/-0.06) Amati et al. , A&A, 2002

  19. analysis of an updated sample of long GRBs/XRFs with firm estimates of z and Ep,i (41 events) gives a chance probability for the Ep,i-Eiso correlation of ~10-15 and a slope of 0.57+/-0.02 • the scatter of the data around the best fit power-law can be fitted with a Gaussian with s(logEp,i) ~ 0.2 (~0.15 extra-poissonian) • confirmed by the most recent analysis (more than 70 events, Ghirlanda et al. 2008, Amati et al. 2008) • only firm outlier the local peculiar GRB 980425 (GRB 031203 debated) Amati et al. 2008

  20. all long Swift GRBs with known z and published estimates or limits to Ep,i are consistent with the correlation • the parameters (index, normalization,dispersion) obatined with Swift GRBs only are fully consistent with what found before • Swift allows reduction of selection effects in the sample of GRB with known z -> the Ep,i-Eiso correlation is passing the more reliable test: observations ! Amati 2006, Amati et al. 2008

  21. Implications of the Ep,i – Eiso correlation • physics of prompt emission still not settled, various scenarios: SSM internal shocks, IC-dominated internal shocks, external shocks, photospheric emission dominated models, kinetic energy dominated fireball , poynting flux dominated fireball) • e.g., Ep,i  G-2 L1/2 tn-1 for syncrotron emission from a power-law distribution of electrons generated in an internal shock (Zhang & Meszaros 2002, Ryde 2005) • e.g., Ep,i  G Tpk  G2 L-1/4 in scenarios in whch for comptonized thermal emission from the photosphere dominates (e.g. Rees & Meszaros 2005, Thomson et al. 2006)

  22. jet geometry and structure • XRF-GRB unification models • viewing angle effects Uniform/variable jet PL-structured /universal jet Uniform/variable jet PL-structured /universal jet

  23. The Ep,i – Eiso correlation and sub-energetic GRB • GRB980425 not only prototype event of GRB/SN connection but closest GRB (z = 0.0085) and sub-energetic event (Eiso ~ 1048 erg, Ek,aft ~ 1050 erg) • GRB031203: the most similar case to GRB980425/SN1998bw: very close (z = 0.105), SN2003lw, sub-energetic

  24. the most common explanations for the (apparent ?) sub-energetic nature of GRB980425 and GRB031203 and their violation of the Ep,i – Eiso correlation assume that they are NORMAL events seen very off-axis (e.g. Yamazaki et al. 2003, Ramirez-Ruiz et al. 2005) • d=[g(1 - bcos(qv - Dq))]-1 , DEp  d , DEiso  d(1+a) a=1÷2.3 -> DEiso  d(2 ÷3.3) Yamazaki et al., ApJ, 2003 Ramirez-Ruiz et al., ApJ, 2004

  25. GRB 060218, a very close (z = 0.033, second only to GRB9809425), with a prominent association with SN2006aj, and very low Eiso (6 x 1049 erg) and Ek,aft -> very similar to GRB980425 and GRB031203 • but, contrary to GRB980425 and (possibly) GRB031203, GRB060218 is consistent with the Ep,i-Eiso correlation -> evidence that it is a truly sub-energetic GRB -> likely existence of a population of under-luminous GRB detectable in the local universe • also XRF 020903 is very weak and soft (sub-energetic GRB prompt emission) and is consistent with the Ep-Eiso correlation Amati et al., 2007

  26. GRB060218 was a very long event (~3000 s) and without XRT mesurement (0.3-10 keV) Ep,i would have been over-estimated and found to be inconsistent with the Ep,i-Eiso correlation • Ghisellini et al. (2006) found that a spectral evolution model based on GRB060218 can be applied to GRB980425 and GRB031203, showing that these two events may be also consistent with the Ep,i-Eiso correlation • sub-energetic GRB consistent with the correlation; apparent outliers(s) GRB 980425 (GRB 031203) could be due to viewing angle or instrumental effect

  27. Recent Swift detection of an X-ray transient associated with SN 2008D at z = 0.0064, showing a light curve and duration similar to GRB 060218 • Peak energy limits and energetics consistent with a very-low energy extension of the Ep,i-Eiso correlation • Evidence that this transient may be a very soft and weak GRB (XRF 080109), thus confirming the existence of a population of sub-energetic GRB ? Modjaz et al., ApJ, 2008 Li, MNRAS, 2008

  28. Ep,i – Eiso correlation and short GRBs • only very recently, redshift estimates for short GRBs • all SHORT Swift GRBs with known redshift and lower limits to Ep.i are inconsistent with the Ep,i-Eiso correlation • intriguingly, the soft tail of GRB050724 is consistent with the correlation • GRB 060614: no SN, first pulse inconsistent with correlation, sfto/long tail consistent: evidence that two different emission mechanisms are at work in both short and long GRB, with different relative efficiency in the two classes (thus generating also intermediate) Amati, NCimB, 2006

  29. GRB-SN connection and the Ep,i-Eiso correlation • GRB 060218 and other GRB with firmest evidence of association with a SN are consistent with the Ep,i-Eiso correlation • GRB 060614: the long GRB with a very deep lower limit to the magnitude of an associated SN is consistent with the correlation too • GRB 060505: stringent lower limit to SN magnitude, inconsistent with correlation, but it is likely short • XRF 08019 / SN 2008D: possible very low energy GRB, possibly consistent with with the correlation • Further evidence that GRB properties are independent on those of the SN Amati et al. A&A, 2007

  30. GRB cosmology with Ep,i – Eiso correlation • GRB have huge luminosity, a redshift distribution extending far beyond SN Ia • high energy emission -> no extinction problems • unfortunately, they are not standard candles ! • but need to investigate their properties to find ways to standardize them (if possible)

  31. Standardizing GRB with 3-parameters spectrum-energy correlations • the Ep,i-Eiso correlation becomes tighter when adding a third observable: jet opening angle (qjet -> Eg = [1-cos(qjet)]*Eiso (Ghirlanda et al. 2004) or “high signal time” T0.45 (Firmani et al. 2006) • the logarithmic dispersion of these correlations is very low: can they be used to standardize GRB ? • jet angle inferred from break time in optical afterglow decay, while Ep,i-Eiso-T0.45 correlation based on prompt emission properties only

  32. Methods (e.g., Ghirlanda et al, Firmani et al., Dai et al., Zhang et al.): Ep,i = Ep,obsx (1 + z) Dl = Dl (z, H0, WM, WL, …) • general purpouse: estimate c.l. contours in 2-param surface (e.g. WM-WL) • general method: construct a chi-square statistics for a given correlation as a function of a couple cosmological parameters • method 1 – luminosity distance: fit the correlation and construct an Hubble diagram for each couple of cosmological parameters -> derive c.l. contours based on chi-square

  33. method 2 – minimum correlation scatter: for each couple of cosm.parameters compute Ep,i and Eiso (or Eg), fit the points with a pl and compute the chi-square -> derive c.l. contours based on chi-square surface • method 3: bayesian method assuming that the correlation exists and is unique Ghirlanda et al., 2004 Firmani et al. 2007

  34. What can be obtained with 150 GRB with known z and Ep and complementarity with other probes (SN Ia, CMB) • complementary to SN Ia: extension to much higher z even when considering the future sample of SNAP (z < 1.7), cross check of results with different probes Ghirlanda, Ghisellini et al. 2005, 2006,2007

  35. Drawbacks: lack of solid physical explanation • physics of prompt emission still not settled, various scenarios: SSM internal shocks, IC-dominated internal shocks, external shocks, photospheric emission dominated models, kinetic energy dominated fireball , poynting flux dominated fireball) • e.g., Ep,i  G-2 L1/2 tn-1 for syncrotron emission from a power-law distribution of electrons generated in an internal shock (Zhang & Meszaros 2002, Ryde 2005); for Comptonized thermal emission • geometry of the jet (if assuming collimated • emission) and viewing angle effects also • may play a relevant role

  36. Drawbacks: lack of calibration • differently to SN Ia, there are no low-redshift GRB (only 1 at z < 0.1) -> correlations cannot be calibrated in a “cosmology independent” way • would need calibration with a good number of events at z < 0.01 or within a small range of redshift -> neeed to substantial increase the number of GRB with estimates of redshift and Ep • Bayesian methods have been proposed to “cure” the circularity problem (e.g., Firmani et al., 2006), resulting in slightly reduced contours w/r to simple (and circularity free) scatter method (using Lp,iso-Ep,i-T0.45 corr.)

  37. “Crisis” of 3-parameters spectrum-energy correlations • Recent debate on Swift outliers to the Ep-Eg correlation (including both GRB with no break and a few GRB with chromatic break) • Recent evidence that the dispersion of the Lp-Ep-T0.45 correlation is significantly higher than thought before and comparable to the Ep,i-Eiso corr. Campana et al. 2007 Rossi et al. 2008

  38. Using the simple Ep,i-Eiso correlation for cosmology • Based on only2 observables: • a) much higher number of GRB that can be used • b) reduction of systematics • Evidence that a fraction of the extrinsic scatter of the Ep,i-Eiso correlation is due to choice of cosmological parameters used to compute Eiso Simple PL fit 70 GRB Amati et al. 2008

  39. By quantifying the extrinsic scatter with a proper log-likelihood method, WM can be constrained to 0.04-0.40 (68%) for a flat LCDM universe (WM = 1 excluded at 99.9% c.l.) • releasing assumption of flat universe still provides evidence of low WM, with a low sensitivity to WL • significant constraints on both WM and WL (and likely on dark energy EOS) expected from sample enrichment and z extension by present and next GRB experiments (e.g., Swift, Konus_WIND, GLAST, SVOM) • completely independent on other cosmological probes (e.g., CMB, type Ia SN, BAO; clusters…) and free of circularity problems 70 REAL 70 REAL + 150 SIM. Amati et al. 2008

  40. The future: what is needed ? • increase the number of z estimates, reduce selection effects and optimize coverage of the fluence-Ep plane in the sample of GRBs with known redshift • more accurate estimates of Ep,i by means of sensitive spectroscopy of GRB prompt emission from a few keV (or even below) and up to at least ~1 MeV • Swift is doing greatly the first job but cannot provide a high number of firm Ep estimates, due to BAT ‘narrow’ energy band (sensitive spectral analysis only from 15 up to ~200 keV) • Ep estimates for some Swift GRBs from Konus (from 15 keV to several MeV) ant, to minor extent, RHESSI and SUZAKU NARROW BAND BROAD BAND

  41. 2008(-2011 ?): GLAST (AGILE) + Swift: • accurate Ep (GLAST/GBM = 15-5000 keV) and z estimate (plus study of GeV emission) for simultaneously detected events • by assuming that Swift will follow-up ALL GLAST GRB, about 80 GRB with Ep and z in 3 years • AGILE and GLAST: second peak at E > 100 MeV ? (e.g., IC like in Blazars)

  42. In the 2011-2015 time frame a significant step forward expected from SVOM: • spectral study of prompt emission in 1-5000 keV -> accurate estimates of Ep and reduction of systematics (through optimal continuum shape determination and measurement of the spectral evolution down to X-rays) • fast and accurate localization of optical counterpart and prompt dissemination to optical telescopes -> increase in number of z estimates and reduction of selection effects • optimized for detection of XRFs, short GRB, sub-energetic GRB • substantial increase of the number of GRB with known z and Ep -> test of correlations and calibration for their cosmological use

  43. GRB as cosmological beacons: EDGE/XENIA (under study) • GRB can be used as cosmological beacons for study of the IGM up to z > 6 • Because of the association with the death of massive stars GRB allow the study the evolution of massive star formation and the evolution of their host galaxy ISM back to the early epochs of the Universe (z > 6) EDGE Team

  44. End of the talk

  45. Backup slides

  46. Gamma-Ray Bursts • most of the flux detected from 10-20 keV up to 1-2 MeV • measured rate (by an all-sky experiment on a LEO satellite): ~0.8 / day • bimodal duration distribution • fluences (= av.flux * duration) typically of ~10-7 – 10-4 erg/cm2 short long

  47. The GRB phenomenon: VHE • CGRO/EGRET detected VHE (from 30 MeV up to 18 GeV) photons for a few GRBs • VHE emission can last up to thousends of s after GRB onset • average spectrum of 4 events well described by a simple power-law with index ~2 , consistent with extension of low energy spectra

  48. afterglow emission (> 1997): X, optical, radio counterparts

  49. … and host galaxies • host galaxies long GRBs: blue, usually regular and high star forming, GRB located in star forming regions • host galaxies of short GRBs (very recent): elliptical, irregular galaxies, away from star forming region (but still unclear) Long Short GRB 050509b

  50. in 1997 discovery of afterglow emission by BeppoSAX • first X, optical, radio counterparts, redshifts, energetics GRB 970508, Metzger et al., Nature, 1997

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