and GRBs Luigi Piro IAPS/INAF, Rome
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1 Luigi Piro IAPS/INAF, Rome
2 The Science Theme motivating the Athena+ mission
3 and GRBs Key questions for observational astrophysics in How does ordinary matter assemble into the large scale structures we see today? Extended X-ray sources Oppenheimer et al Athena+ WFI Deep Field Pointecouteau, Reiprich et al., 2013 arxiv
4 The Warm-Hot intergalactic medium (WHIM) Where are the missing baryons in the local Universe? What is the underlying mechanism determining the distribution of the hot phase of the cosmic web? Kaastra, Finoguenov et al., 2013 arxiv How does ordinary matter assemble into the large-scale structures that we see today?
5 The first stars, the first BH, the first metals z=1089 Pop III collapsars? Pop II GRBs z=12 z=5 z=0 Dark Ages Reioniza(on! A dominant propor,on of high- z star forma,on takes place in galaxies beyond the reach of JWST at z > 8 ; their nature will hardly be known, but they will be GRB hosts. GRB Quasar Galaxy! There will likely be no direct detec,ons of popula,on III sources; pop III collapsars predicted to produce GRB- like events.
6 Z<Zcr 10 4 formation of clouds M>100 Msun the final mass popiii: gas accretion vs radiation feedback, typical ~40-50 Msun but [ Msun] possible and GRBs Population III Schneider 2005
7 popiii-popii transition Chemical enrichment is highly inhomengenous: popiii and popii coexhists for a long period z=5 Tornatore et al 2007
8 popiii GRBs T 90 =10 4 s Eiso=10 55 erg L=10 52 erg/s Suwa&Ioka 2011
9 Ultralong GRB: a popiii analogue? Flux@z= erg/cm 2 /s Piro+ 2014
10 X-rays probe the close ionized environment Opt- IR Schady et al 2010 X- Ray
11 The first stars and black holes When did the first generation of stars explode to form the first seed black holes and disseminate the first metals in the Universe? Gamma Ray Burst at z=7 by ATHENA-XIFU Jonker, O'Brien et al., 2013 arxiv How do black holes grow and shape the Universe?
12 The Athena Observatory Willingale et al, 2013 arxiv L2 orbit Ariane V <5100 kg power 2500 w 5 year mission Silicon Pore Optics: 2 m 2 at 1 kev 5 arcsec HEW Focal length: 12m Sensitivity: erg cm -2 s -1 X-ray Integral Field Unit: ΔE: 2.5 ev Field of View: 5 arcmin Operating temp: 50 mk Barret et al., 2013 arxiv: Wide Field Imager: ΔE: 125 ev Field of View: 40 arcmin High countrate capability Rau et al arxiv
13 The first Deep Universe X-ray Observatory Athena+ has vastly improved capabilities compared to current or planned facilities, and will impact on virtually all areas of astrophysics Line Sensitivity 100 x ASTRO- H 1000 Survey x Speed XMM- Newton X-ray spectroscopy at the peak of the activity of the Universe Deep survey capability into the dark ages and epoch of reionization
14 GRB fluence distribution and counts in Athena counts in XIFU (at 2hrs for 100 ksec) P.Evans
15 GRB requirements for trigger " XIFU FOV is 5 => localization at ~ arcmin level " For the WHIM only the brightest: " GRB monitor: FOV main driver, area can be relatively small, use prompt as pre-selection " For high z GRB: about (depending on models) GRB at z>7 per year in the Universe. " GRB monitor: Need to secure most of => FOV and sensitivity " If popiii as GRB possibly ultra long and dim and soft (Lobster) " Need photo-z to pre-select in IR
16 Conclusions " GRB are in the core science of Athena as beacons to " Find the missing baryons in the WHIM: " About 10 GRB afterglows per year selected for brightness (prompt emission as proxy) " Find primordial stars sites in the High-z Universe: " About 5 GRB afterglows pre year selected for redshift (photo-z with IR telescopes, other indicators ) " Physics of GRB in Observatory science (late time follow up) " Mission requirement: TOO in 4hrs (2 hrs goal) for 50% of sky
17 Athena science in context Athena is a crucial part of the suite of large observatories needed to reach the science objectives of astronomy in the coming decades
18 Athena The first Deep Universe X-ray Observatory High redshift galaxy group 1000 z= vfv Normalised Counts/s/keV 1 z= Energy (kev) Black hole feedback at peak of activity in Universe v=0.2c 0.01 z=2 Athena+ Deep Field Nandra, Barret, Barcons, Fabian, den Herder, Piro, Watson et al arxiv Normalised Counts/s/keV Normalised Counts/s/keV Primordial stellar populations via GRB afterglow follow up Energy (kev) Obscured black hole in the early Universe z= Fe Kα Energy (kev) Energy (kev) 0.70
19 Athena+: a powerful observatory Planets (interaction of solar wind with planet environment and comets) Exoplanets Stellar physics Supernovae (explosion mechanism, heavy element production) Stellar endpoints (physics of outflows and winds in X-ray binaries) Sgr A* Interstellar dust and medium Outflow in X-ray binary, 10ks Jupiter Branduardi-Raymont, Sciortino, et al., 2013 arxiv ; Sciortino, Rauw et al., 2013 arxiv ; Motch, Wilms, et al., 2013 arxiv ; Decourchelle, Costantini et al., 2013 arxiv
20 Acknowledgements The Athena+ Co-ordination Group: Xavier Barcons (ES), Didier Barret (FR), Andy Fabian (UK), Jan-Willem den Herder (NL), Kirpal Nandra (DE), Luigi Piro (IT), Mike Watson (UK) The Athena+ Working Groups: Christophe Adami (FR), James Aird (UK), Jose Manuel Afonso (PT), Dave Alexander (UK), Costanza Argiroffi (IT), Monique Arnaud (FR), Jean-Luc Atteia (F), Marc Audard (CH), Carles Badenes (US), Jean Ballet (FR), Lucia Ballo (IT), Aya Bamba (JP), Anil Bhardwaj (IN), Elia Stefano Battistelli (IT), Werner Becker (DE), Michaël De Becker (BE), Ehud Behar (IL), Stefano Bianchi (IT), Veronica Biffi (IT), Laura Bîrzan (NL), Fabrizio Bocchino (IT), Slavko Bogdanov (US), Laurence Boirin (FR), Thomas Boller (DE), Stefano Borgani (IT), Katharina Borm (DE), Hervé Bourdin (IT), Richard Bower (UK), Valentina Braito (IT), Enzo Branchini (IT), Graziella Branduardi-Raymont (UK), Joel Bregman (USA), Laura Brenneman (USA), Murray Brightman (DE), Marcus Brüggen (DE), Johannes Buchner (DE), Esra Bulbul (USA), Marcella Brusa (IT), Michal Bursa (CZ), Alessandro Caccianiga (IT), Ed Cackett (USA), Sergio Campana (IT), Nico Cappelluti (IT), Massimo Cappi (IT), Francisco Carrera (ES), Maite Ceballos (ES), Finn Christensen (DK), You-Hua Chu (US), Eugene Churazov (DE), Nicolas Clerc (DE), Stephane Corbel (F), Amalia Corral (GR), Andrea Comastri (IT), Elisa Costantini (NL), Judith Croston (UK), Mauro Dadina (IT), Antonino D Ai (IT), Anne Decourchelle (FR), Roberto Della Ceca (IT), Konrad Dennerl (DE), Klaus Dolag (DE), Chris Done (UK), Michal Dovciak (CZ), Jeremy Drake (US), Dominique Eckert (S), Alastair Edge (UK), Stefano Ettori (IT), Yuichiro Ezoe (JP), Eric Feigelson (US), Rob Fender (UK), Chiara Feruglio (FR), Alexis Finoguenov (FI), Fabrizio Fiore (IT), Massimiliano Galeazzi (IT), Sarah Gallagher (CA), Poshak Gandi (UK), Massimo Gaspari (IT), Fabio Gastaldello (IT), Antonis Georgakakis (DE), Ioannis Georgantopoulos (GR), Marat Gilfanov (DE), Myriam Gitti (IT), Randy Gladstone (USA), Rene Goosmann (FR), Eric Gosset (BE), Nicolas Grosso (FR), Manul Guedel (AT), Martin Guerrero (ES), Frank Haberl (DE), Martin Hardcastle (UK), Sebastian Heinz (US), Almudena Alonso Herrero (ES), Anthony Hervé (FR), Mats Holmstrom (SE), Kazushi Iwasawa (ES), Peter Jonker (NL), Jelle Kaastra (NL), Erin Kara (UK), Vladimir Karas (CZ), Joel Kastner (US), Andrew King (UK), Daria Kosenko (FR), Dimita Koutroumpa (FR), Ralph Kraft (US), Ingo Kreykenbohm (D), Rosine Lallement (FR), J. Lee (US), Marianne Lemoine-Goumard (FR), Andrew Lobban (UK), Giuseppe Lodato (IT), Lorenzo Lovisari (DE), Ian McCarthy (UK), Brian McNamara (CA), Antonio Maggio (IT), Roberto Maiolino (UK), Barbara De Marco (DE), Silvia Mateos (ES), Giorgio Matt (IT), Ben Maughan (UK), Pasquale Mazzotta (IT), Mariano Mendez (NL), Andrea Merloni (DE), Giuseppina Micela (IT), Marco Miceli (IT), Robert Mignani (IT), Jon Miller (US), Giovanni Miniutti (ES), Silvano Molendi (IT), Rodolfo Montez (ES), Alberto Moretti (IT), Christian Motch (F)R, Yaël Nazé (BE), Jukka Nevalainen (FI), Fabrizio Nicastro (IT), Paul Nulsen (US), Takaya Ohashi (JP), Paul O Brien (UK), Julian Osborne (UK), Lida Oskinova (DE), Florian Pacaud (DE), Frederik Paerels (US), Mat Page (UK), Iossif Papadakis (GR), Giovanni Pareschi (IT), Robert Petre (US), Pierre-Olivier Petrucci (FR), Enrico Piconcelli (IT), Ignazio Pillitteri (IT), C. Pinto (UK), Jelle de Plaa (NL), Etienne Pointecouteau (FR), Trevor Ponman (UK), Gabriele Ponti (DE), Delphine Porquet (FR), Ken Pounds (UK), Gabriel Pratt (FR), Peter Predehl (DE), Daniel Proga (US), Dimitrios Psaltis (US), David Rafferty (NL), Miriam Ramos-Ceja (DE), Piero Ranalli (IT), Elena Rasia (US), Arne Rau (DE), Gregor Rauw (BE), Nanda Rea (IT), Andy Read (UK), James Reeves (UK), Thomas Reiprich (DE), Matthieu Renaud (FR), Chris Reynolds (US), Guido Risaliti (IT), Jerome Rodriguez (FR), Paola Rodriguez Hidalgo (CA), Mauro Roncarelli (IT), David Rosario (DE), Mariachiara Rossetti (IT), Agata Roszanska (PL), Emmanouil Rovilos (UK), Ruben Salvaterra (IT), Mara Salvato (DE), Tiziana Di Salvo (IT), Jeremy Sanders (DE), Jorge Sanz-Forcada (ES), Kevin Schawinski (CH), Joop Schaye (NL), Salvatore Sciortino (IT), Paola Severgnini (I), Francesco Shankar (FR), Stuart Sim (IE), Christian Schmid (DE), Randall Smith (US), Andrew Steiner (US), Beate Stelzer (IT), Gordon Stewart (UK), Tod Strohmayer (US), Lothar Strüder (DE), Ming Sun (US), Yoh Takei (JP), Andreas Tiengo (IT), Francesco Tombesi (US), Ginevra Trinchieri (IT), Asif ud-doula (US), Eugenio Ursino (NL), Lynne Valencic (US), Eros Vanzella (IT), Simon Vaughan (UK), Cristian Vignali (IT), Jacco Vink (NL), Fabio Vito (IT), Marta Volonteri (FR), Daniel Wang (US), Natalie Webb (FR), Richard Willingale (UK), Joern Wilms (DE), Michael Wise (NL), Diana Worrall (UK), Andrew Young (UK), Luca Zampieri (IT), Jean In t Zand (NL), Andreas Zezas (GR), Yuying Zhang (DE), Irina Zhuravleva (US) Bold Face Denotes Working Group Chairs Athena+ Coordination Group: K. Nandra, D. Barret, X. Barcons, J.-W. den Herder, A. Fabian, L. Piro, M. Watson Athena+ Working Groups (~250 people) Athena+ supporters (~ 1200 astronomers) Special thanks to the review team: M. Arnaud, J. Bregman, F. Combes, R. Kennicutt, R. Maiolino, R. Mushotzky, T. Ohashi, K. Pounds, C. Reynolds, H. Röttgering, M. Rowan-Robinson, C. Turon, G. Zamorani More information, white paper, 15 supporting papers at:
21 ADDITIONAL SLIDES
22
23 GRBs: pathways to unvisible protogalaxies
24 Follow-up of high-z GRB with large facilities Op,cal/IR abs. spectroscopy of the host galaxy X-ray spectroscopy of the progenitor environment
25 popiii vs popii popii GRBs are expected to exist at redshifts z~15-20 and popiii are expected to form down to z<2.5 Weak enrichment Strong enrichment Bromm&Loeb 2006
26 Determining Environments with GRBs Aberglow spectroscopy can provide redshib, chemical abundances, dust, & molecular content Vreeswijk et al GRB z=6.3 Kawai et al 2006
27 Ultralong as proxy popiii GRBs Low metallicity Blue SuperGiant (Gendre et al. 13) => low mass rate, external stellar layers able to fuel central engine for Evidence of afterglow with very low density wind and hot thermal cocoon associated to low metallicity BSG (LP et al 2014) Close (z<0.7) and few: low probability of forming low metallicity supergiants
28 Ultimate mission for high-z GRBs Lobster Wide Field X-ray monitor Light-weight scintillator (~7-300 kev) for temporal triggering and spectrum IR telescope for afterglow spectroscopy X-ray telescope for afterglow (high res. spectroscopy)
29 Science requirements for (high-z) GRBs About ~ 50/yr at z>7 (Butler et al 2010) FoV >~ 1 sr (about 15 in 3 yrs) Mixed popii and III, with popiii dominating at z>10 High-z GRB so far popii GRB, To catch popiii collapsar (long and faint) requires a X-ray sensitivity of <1mCrab in > s (enabled by focussing techniques as Lobster-eye optics)
30 High resolution spectroscopy in GRB " Need at least cts to enable high resolution spectroscopy " More than 60% of the afterglows (with Tstart ~2-4 hours and integration 100ksec) with A+ " For weak lines as in the WHIM need 5-10x more " About 15% afterglows
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