The Present and Future of GRB Cosmography Andrew S. Friedman (Harvard-CfA) & Joshua S. Bloom...
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Transcript of The Present and Future of GRB Cosmography Andrew S. Friedman (Harvard-CfA) & Joshua S. Bloom...
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The Present and Future The Present and Future of GRB Cosmographyof GRB Cosmography
Andrew S. Friedman (Harvard-CfA) & Andrew S. Friedman (Harvard-CfA) & Joshua S. Bloom (Harvard-CfA / UC Berkeley)Joshua S. Bloom (Harvard-CfA / UC Berkeley)
www.cosmicbooms.netwww.cosmicbooms.net
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OutlineOutlineMotivations: What is GRB Cosmography?
Brief HistoryCurrent WorkFuture Prospects
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MotivationsMotivationsGRBs – brightest explosions in universe Detectable out to high z (>5, ~10-20?)Gamma-rays penetrate dustAny evolution likely to be orthogonal to
that of Type Ia SNeSwift satellite in space! Years before
SNAP (2010?, zmax ~ 1.7)A GRB standard candle could serve as an independent probe of the geometry & expansion history of the universe, complementary to SNe Ia
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But wait, high z is ΩM-dominated – boring!Only low z regime is good for ΩΛ, w, right?
And very few low-z GRBs (now), including peculiar bursts 980425, 031203, (+future)
However, survey in full range 0 < z < 2 is crucial to pin down dark energy systematics (Linder & Huterer 2003)
GRBs already comparable in number to SNe Ia in 1<z<2, (zmax ~ 1.7 now, SNAP)
Ultimately, independent techniques are always a good thing in science
MotivationsMotivations
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Empirical standard candle ultimately derives from microphysics (e.g. SNe Ia, Chandra. Limit)
Scatter about standard candle can help quantify burst diversity (e.g. peculiar Ia’s)
Empirical corrections to scatter (e.g. MLCS, stretch – Ia’s), can yield new physical insight
Large deviations from the standard candle (outliers) may indicate different physical mechanisms for making GRBs – i.e. different progenitor systems (e.g. Type II SNe)
Turning the game around - Pick a cosmology - GRB standard candles can tell you about the progenitors of GRBs
MotivationsMotivations
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GRB Cosmography?GRB Cosmography?
It must be indep. of redshift (z), i.e. roughly constant from burst to burst
It can depend on properties of both the prompt emission and the afterglow, although the latter are more observationally expensive
Let’s review the search in the set of GRBs with known z (now ~40 events)
What function of observables might serve as a useful GRB standard candle? Purely empirical approach.
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HistoryHistoryEiso distribution – spans several orders
of mag. – Eiso is a bad standard candle
Data from Friedman & Bloom 2004 (astro-ph/0408413), ApJ/subm
Fluence in observed bandpass
Cosmological k-correction
Luminosity Distance (theory)
Hubble constant /70 kms-1Mpc-1
Redshift
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But GRBs are beamed. Eγ distribution is much narrower than Eiso (Frail et. al 2001, Piran et. al 2001, Bloom et. al 2003), but not sufficient for cosmology (Bloom et. al 2003)
HistoryHistory
15 GRBs (fb), 17 GRBs (z) Frail et. al 2001
24 GRBs (fb), 28 GRBs (z) Bloom et. al 2003
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Updated comparison of Eiso and Eγ dist.
HistoryHistory
Data from Friedman & Bloom 2004 (astro-ph/0408413), ApJ/subm
33 GRBs (fb), 39 GRBs (z)
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Eγ is getting worse as a standard candle with new data: e.g. 030329, 031203, XRF 020903,…
Bloom et. al 2003
Frail et. al 2001
Ghirlanda et. al 2004
HistoryHistory
Friedman & Bloom 2004
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Beaming inferred from steepening of afterglow light curve
Stanek et. al 1999
HistoryHistory
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This prescription of Egamma is model dependent! Top hat jet.
Eg meaningful, modulo external density (usually unconstrained), gamma-ray efficiency, kcor bandpass, and jet model
HistoryHistory