Where do we stand
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Where do we stand. ?. Log(Flux ). Swift. End of the prompt. A few hours. Log(Time ). Kyoto 2010. Log(Flux ). X-Ray Flares. Log(Time ). Kyoto 2010. GRB X- ray Flares. R. Margutti G. Chincarini , G. Bernardini , J. Mao, C. Guidorzi. Early-time flare catalog .

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Where do we stand

Where do we stand

?

Log(Flux)

Swift

End of the prompt

A few hours

Log(Time)

Kyoto 2010


Where do we stand

Log(Flux)

X-Ray Flares

Log(Time)

Kyoto 2010


Where do we stand

GRB X-ray Flares

R. Margutti

G. Chincarini, G. Bernardini, J. Mao, C. Guidorzi

Early-time flare catalog

Late-time flare catalog

Bright flare analysis

t< 103s

t> 103s

9 flares

X-ray + gamma-ray

Very good statistics

113 flares

4 different energy bands

Asymmetric profile

36 flares

Asymmetric profile

Evolution with time

(up to t≈106 s)

051117A

Spectral evolution

Evolution with energy band

Poster: #

Evolution with time

Evolution with energy band

Margutti et al., MNRAS accepted, Astro-ph: 1004.1568

Astro-ph: 1004.0901

As-complete-as-possible observational picture of the X-ray flare phenomenology

AIM:

Kyoto 2010


Where do we stand

?

GRB X-ray Flares

OBSERVATIONALLY: What distinguishes a flare from a prompt pulse

Do flares follow the entire set of temporal and spectral relations found from the analysis of prompt emission pulses?

Width(T)

Luminosity(T)

Ep(t)

Ep(t)-Liso(t)

Ep-Liso

Width(E)

Lag-Lum

Kyoto 2010


Where do we stand

The Method:

Trise

Tdecay

Width

Tpeak

Amplitude

If with redshift:

Peak Luminosity

Energy

Evolution with ENERGY BAND

Evolution with Tpeak

GRB060904B

Among different flares

In the same flare

Kyoto 2010


Where do we stand

Width (t)

Width=trise+tdecay

Width=trise + tdecay

Log(width)

Log(tpeak)

TIME

Kyoto 2010


Where do we stand

Luminosity (t)

Flares get fainter and fainter

Early time sample

TIME

Kyoto 2010


Where do we stand

Spectral Evolution (t)

060904B Flare:

Prompt:

BATSE pulse

Peak Energy

Time

(Peng 2009)

Within single flare and pulses

TIME

Kyoto 2010


Where do we stand

Ep(t)-Liso(t)

Ep,i (keV)

Ep,i (keV)

060904B Flare

060418 Flare

Liso (erg/s)

Liso (erg/s)

Prompt

Ep,i (keV)

Ghirlanda 2010

Liso (erg/s)

Kyoto 2010


Where do we stand

Ep-EisoEp-Liso

Prompt data from Nava 2009

Flares

Flares

Kyoto 2010


Where do we stand

Width(E)

FLARES

PROMPT

High energy profiles peak before

Flare peak Lag

Kyoto 2010


Where do we stand

Lag-Luminosity

PROMPT

CCF lag, time integ.

50-100 vs 100-200 keV

1-10000 keVLpeak

(Ukwatta 2010)

Norris 2000 relation

Peak lag, flares

0.3-1vs 3-10 keV

0.3-10 keVLpeak

(Margutti 2010)

FLARES

Kyoto 2010


Where do we stand

Summary: Flares paradigm

High energy flareprofiles rise faster, decay faster and peak before the low energy emission.

FLARES EVOLVE WITH TIME

As time proceeds flares become wider, with larger peak lag, lower luminosities and softer emission.

Kyoto 2010


Where do we stand

Summary:

FLARES EVOLVE WITHTIME

Margutti 2010

FLARES

PROMPT

Width(T)

Luminosity(T)

Ep(t)

Ep(t)-Liso(t)

Ep-Liso

Width(E)

Lag-Lum

≈const

≈const

≈similar

?

Kyoto 2010

Astro-ph: 1004.1568

Astro-ph: 1004.0901


Where do we stand

THANK YOU!!

Kyoto 2010


Where do we stand

Back-up slides


Where do we stand

Lag - HR


Where do we stand

HRrise-HRdecay


Where do we stand

Energy dependence of the parameter


Where do we stand

Lpeak-Width


Where do we stand

Trise-tdecay


Where do we stand

Ioka plot


Where do we stand

Flare and prompt energy


Where do we stand

SED


Where do we stand

BAT-XRT spectral index

BAT

XRT


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