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The Future of Z > 7 Astronomy with Gamma-Ray Bursts

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The Future of Z > 7 Astronomy with Gamma-Ray Bursts The Future of z > 7 Astronomy with Gamma-Ray Bursts Sandra Savaglio Max-Planck Institute for Extraterrestrial Physics GRB 011121 redshift z = 0.362 3.98 Gyr ago Long-duration Gamma-Ray Burst: Short-duration Gamma-Ray Burst: Core Collapse SN Merger of Neutron Stars/Black Holes 172: number of GRBs with measured redshift today 6.7: highest redshift known 1051 ergs: typical energy emitted in photons, in a couple of minutes 10 billion years: the time required by the sun to emit the same energy 1054 ergs: energy emitted in gravitational waves and neutrinos Rate: 1/105 yr−1 / galaxy (a few / day detectable on Earth ) What can we investigate? A partial view.... 1. Star formation under extreme conditions 2. Massive stars (supernovae, WR) 3. Black Holes 4. Reionization of the universe 5. Cosmic chemical evolution 6. SFR history of the universe 7. Small galaxies at high redshift 8. First stars at z>7 9. Cosmology GRBs as cosmological probes GRB 080913 GRB 011121 most distant galaxy Big Bang most distant quasar GRB redshift record holder: GRB 080913 (z = 6.7) log N = 0.0, x =1.0 z=6.710 HI HI log NHI = 21.0, xHI=0.0 z=6.692 at z=6.74 " Ly 0 (arbitrary units) ! F 7500 8000 8500 9000 9500 Wavelength (Å) J. Greiner, T. Kruehler, J.P.U. Fynbo, A. Rossi, R. Schwarz, S. Klose, S. Savaglio, N.R. Tanvir, S. McBreen, T. Totani, B.B. Zhang, X.F. Wu, D. Watson, S.D. Barthelmy, A.P. Beardmore, P. Ferrero, N. Gehrels, D.A. Kann, N. Kawai, A. Kuepcue Yoldas, P. Meszaros, B. Milvang-Jensen, S.R. Oates, D. Pierini, P. Schady, K. Toma, P.M. Vreeswijk, A. Yoldas, B. Zhang, P. Afonso, K. Aoki, D.N. Burrows, C. Clemens, R. Filgas, Z. Haiman, D.H. Hartmann, G. Hasinger, J. Hjorth, E. Jehin, A.J. Levan, E.W. Liang, D. Malesani, T.-S. Pyo, S. Schulze, G. Szokoly, H. Terada, K. Wiersema (2009) GRB 080319B: the brightest source recorded by humanity -40 GRB 080319B z = 0.937 GRB 050904 (7.5 Gyr ago) Visual GRB 990123 magnitude -35 m=5.6 Most Luminous QSO Known -30 [AB] r M -25 distribution SDSS QSO -20 SN 2006gy 6.7 hours after m=19.1 10-4 10-2 100 102 Time Since Explosion [day] Bloom et al. (2008 March 24, ApJ Submitted, 42 pages) 2008: the Year of Gamma-Ray Bursts -40 GRB 080319B -35 Most Luminous QSO Known GRB 080319B -30 [AB] Brightest source recorded by humanity r M -25 distribution SDSS QSO -20 10-4 10-2 100 102 Time Since Explosion [day] log N = 0.0, x =1.0 z=6.710 HI HI log NHI = 21.0, xHI=0.0 z=6.692 at z=6.74 " Ly GRB 080913 Second most distant object known 0 (arbitrary units) ! F 7500 8000 8500 9000 9500 Wavelength (Å) GRB redshift distribution GRB redshift Near IR Berger et al. (2007) Berger etal. GRB host GRB 050904z=6.3 confirmed galaxyatz>5 Smallest spectroscopically Z/Z M ✶ ☉ ~ 10 ~1/6 9.5 M ☉ Only seenwithGRBs Only –18 –1 –2 –1 flux (10 erg s cm Å ) (2006) etal. Totani 1.5 0.0 0.5 1.0 7000 GRB afterglow Savaglio. Glazebrook &LeBorgne(2009) Glazebrook Savaglio. 7500 Ly-! 1.0 0.0 8700 SED ofGRBhost 8000 observed wavelength (Å) 9500 8500 Ly-" 9000 CIV at z=4.840 S II, Si II Si II* 9500 O I C II 10000 Only seen with GRBs Fine structure lines in ISM out of Milky Way GRB 060418 z=1.490 Vreeswijk, Ledoux, Smette, Ellison, Jaunsen, Andersen, Fruchter, Fynbo, Hjorth, Kaufer, Møller, Petitjean, Savaglio, Wijers (2007) Only seen with GRBs 2175 Å dust bump at high redshift Wavelength [Å] GRB rest frame 1000 2000 3000 4000 5000 6000 7000 18 19 100 2175 Å dust bump 20 GRB 070802 z=2.45 Jy] µ 21 10 AB Magnitude 22 Flux density [ 23 LMC−like: A =1.8 24 V 1 SMC−like: AV=1.0 MW−like: AV=0.9 Data 5000 10000 15000 20000 25000 Wavelength [Å] observers frame Krühler, Küpcü Yoldaş, Greiner, Clemens, McBreen, Primak, Savaglio, Yoldaş, Szokoly, Klose (2008) Only seen with GRBs 2175 Å dust bump at high redshift 2.0 ) 2 1.5 GRB 080607 z=3.036 1.0 AV = 3.2 0.5 Relative Flux (erg/s/Ang/cm 0.0 4000 4500 5000 5500 ) 2 Wavelength (Ang) 6 2175 Å bump 4 2 0 6000 7000 8000 9000 Relative Flux (erg/s/Ang/cm Wavelength (Ang) Prochaska et al. (2009) flux (10–18 erg s–1 cm–2 Å–1) 0.0 0.0 0.5 0.5 1.0 1.0 1.5 1.5 7000 7000 Totani et al. (2006) etal. Totani GRB 050904atz=6.3 GRB 050904atz=6.3 7500 7500 Ly-! Reionization of the universe Reionization oftheuniverse 1.0 1.0 0.0 0.0 8700 8700 8000 8000 observed wavelength(Å) observed wavelength(Å) 9500 9500 8500 8500 Ly-" 9000 9000 CIV at z=4.840 S II, Sii II Sii II* 9500 9500 O I C II 10000 10000 Reionization of the universe IGM largelyIGM was already ionized largely ionized byat z = 6z.3 = 6.3 GRB 050904 at z=6.3 Totani et al. (2006) Star formation rate density of the universe t [Gyr] Chary, Berger, & Cowie (2007) 13 8 42 1 1 ] -0.3 (1+z) -3 0.1 3.4 -3.5 (1+z) (1+z) Mpc -1 -2 yr 10 . GRB: Yüksel et al. (2008) Hopkins & Beacom (2006) [M LBG: Bouwens et al. (2008) * -3 . R 10 Mannucci et al. (2007) Verma et al. (2007) LAE: Ota et al. (2008) -4 10 0 1 234 5 6 7 8 z Yüksel, Kistler, Beacom, & Hopkins (2008) Rasmussen (NBI) Rasmussen Board P.I. : S. D’Odorico (ESO), F. Hammer (GEPI), L. Kaper (Univ. Amsterdam), R. Pallavicini (INAF), P. Kjaergaard Kjaergaard P. (INAF), Pallavicini R. Amsterdam), (Univ. Kaper L. Hammer(GEPI), F. D’Odorico (ESO), S. : Prototype instrument for ELT instrumentfor Prototype flux (10–18 erg s–1 cm–2 Å–1) 1.5 0.0 0.5 1.0 GRB 050904 at z=6.3 (Totani etal.2006) GRB 050904atz=6.3(Totani 7000 7500 Ly-! GRB 050904 at z=11.3 1.0 0.0 8700 8000 observed wavelength(Å) 9500 8500 Ly-" 9000 CIV at z=4.840 S II, Si II Si II* 9500 O I C II 10000 WhatPrototype can we instrument expect with for ELT?ELT (S. D’Odorico, private communication) GRB 080319B at z = 9 with ELT NIR magnitude m = 11.5 -40 -40 GRB 080319B GRB 080319B at z = 9 z = 0.937 (0.5 Gyr after BB) (7.5 Gyr ago) -35 -35 Most Luminous QSO Known Most Luminous QSO Known -30 -30 [AB] [AB] r r M M -25 -25 distribution SDSS QSO distribution SDSS QSO -20 -20 -4 -2 0 2 10 10 10 10 10-3 10-1- 10 1000 Time Since Explosion [day] Observed Time Since Explosion [day] 34.7 hours after m = 25.0 Conclusions ➊ GRBs shining through a universe hard to see in other ways ➋ GRBs very promising probes of z > 7 universe ➌ Ideal targets for ELTs .
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