1. 1 John Nousek (Penn State University) Neil Gehrels (Goddard Space Flight Center) Five Years of Science: GRBs and More! International Workshop on Astronomical X-ray Optics - Prague, Czech Rep. – 6-9 Dec. 2009

2. 2 Swift launch: 20 Nov 2004 !!

3. 3 5 th Anniversary of Swift Conference Celebration of Swift held at Penn State, 18-20 Nov. 2009 Attracted more than 150 participants – 1/3 Penn State, 1/3 US & 1/3 from ten other countries Discussed impact of Swift on areas of astrophysics, and planned for future developments and science direction of the Swift Observatory

4. 4  Swift has redefined the field of GRB science.  GRB backgroud  Swift comparisons  Duration  Host galaxies  Distance distributions  Energetics  Beaming Swift GRB Science ARAA Annual Reviews 2009 Gehrels, Ramirez-Ruiz and Fox

5. 5 GRB Properties Two types: Short GRBs (t < 2s) Long GRBs (t > 2s) Redshift range: 0.2 - ~2 SGRBs 0.009 - 8.2 LGRBs Energy release in  -rays: 10 49 -10 50 ergs SGRBs 10 50 -10 51 ergs LGRBs Jet opening angle: ~15 deg SGRBs ~5 deg LGRBs Both types have delayed & extended high-E emission ARAA article GRB 990123 HST image Fruchter et al.

6. 6 GRB Spectra prompt afterglow with synchrotron fit GRB 051111 Butler et al. 2006

7. 7 VELA GRB discovery 1973 Compton / BATSE isotropy & inhomogeneity 2 duration classes 1991 Compton / EGRET GeV extended emission 1994 short long

8. 8 BeppoSAX afterglow & distance 1997 Fireball Model 1997 Mészáros & Rees 1997 HETE-II GRB030329 / SN2003dh XRFs ~ 2003

9. BAT XRT UVOT 3 instruments, each with: - lightcurves - images - spectra Rapid slewing spacecraft Rapid telemetry to ground. Swift Mission BAT Position - 2 arcmin T<10 sec XRT Position - 5 arcsec T<90 sec UVOT Position - < 1 arcsec T<2 min XRT BAT

10. Short GRB Swift Statistics 475 GRB as of 1 Nov 2009 85% with X-ray detections ~60% with optical detection 155 with redshift (41 prior to Swift) 46 short GRBs localized (0 prior to Swift) Fast Rise Exponential Decay

11. Swift GRB Data UVOT image BAT lightcurve XRT lightcurve GRB 091029 GRB

12. Swift GRB Data BAT lightcurve XRT lightcurve GRB 091029 flare steep-flat-medium shape UVOT image GRB

13. 13 Short vs Long short long Time (s) Number Gamma Rays Time (s) Numåber Gamma Rays Soft Hard Hardness Ratio Duration (s) short long Kouveliotou et al. 2003

14. 14 GRB Spectroscopy z Time GRB Optical Brightness (10 9 years) 8.3 13.0090423 K = 20 @ 20 min 6.7 12.8080813 K = 19 @ 10 min 6.29 12.8 050904 J = 18 @ 3 hrs 5.6 12.6060927 I = 16 @ 2 min 5.312.6050814 K = 18 @ 23 hrs 5.1112.5060522 R = 21 @ 1.5 hrs Prochaska et al. 2008 Savaglio 2006 GRB 080607

15. Blast from the past! GRB 090423 Lyman break redshifted from UV to IR z = 8.29 look back time = 13.0 billion light years GROND Greiner et al Tanvir et al. 2009; Salvaterra et al. 2009 McMahon & Tanvir

16. 16 Evolution of Swift Operations – GRBs & More! Original prime mission: 2004-2006 – Swift the GRB Explorer Up to Nov. 2004 – Pre-launch: –Swift primarily a GRB detection and afterglow followup mission –Ground-breaking operations design allows immediate response to GRBs –Automated follow-up allows introduction of new GRB without new schedule –Targets of Opportunity limited to new non-Swift GRBs or rare events Expected schedule re-plans only once / month; ToO once / week –Planning using TAKO software / five times a week Prime mission – 2005-2006: –Execution closely follows plans, except: XRT TEC power supply fails, forcing operations to passively maintain XRT below -50 C Automated target process is great success allowing highly flexible and rapid ToO response

17. 17 Swift Operations Currently 1 st mission extension: 2006-2008 – High-z GRBs and the GI Program –Swift reduces time on late afterglow followup and increases effort on finding high redshift GRBs Swift introduces GI targets, followed by pressure for increased ToO and monitoring campaigns –TAKO planning software modified to incorporate XRT temperature control; other ancillary software improves ACS reliability –Improved ToO automation allows multiple ToOs in short period without new schedule (including nights and week-ends) –Targets of Opportunity and Monitoring Campaigns occur every day Typical load of 4-12 ToO or Monitoring observations every day

18. 18 Supernova Studies with Swift XRT and UVOT observations of SNe -66 observed to date of all types (26 Ia, 18 Ibc, 22 II) -UV, optical & X-ray densely-sampled light curves -Largest sample of SN light curves in the UV -Unique UV characterizations of SN Ia's (incl UV spectra) SN 2006bp (Type IIP) Immler et al. 2007 Brown et al. 2008 XRTUVOT optUVOT UV Supernova Lightcurves

19. X-Ray SN Studies Immler et al. - XRT observations probe SNe environments & mass-loss rates - Signature of SN shock traveling through dense shell - Shells are outer H/He-rich layers from Luminous Blue Variable phase SN 2006jc SN 2008bo SN 2006bp

20. SN 2008D Shock Breakout - XRT monitoring of NGC 2770 (27 Mpc) revealed extremely luminous X-ray outburst - E X ~ 2x10 46 ergs - No BAT, no radio late >> probably no jets - UVOT detection of SN rising 90 min later - SN Ib/c - Shock breakout. May occur for all SN Soderberg et al. 2008 9 Jan 2008 SN 2007uy

21. 21 - 25 novae observed - Rise and fall of few keV emission from shocked ejecta - Super-Soft emission in some from WD surface (kT BB ~ 30 eV) - Extensive observations of RS Oph 2006 (~400 ksec) revealed unexpected luminous SSS state and 35 sec QPO - Earth mass ejected at ~4000 km/s into wind of companion Red Giant RS Oph Nova Studies with Swift Thermonuclear detonation of accumulated accretion on white dwarf 1.6 kpc

22. 22 BAT triggered on a stellar flare from nearby (d=5 pc) EV Lac (dM3e, P rot ~4 days) XRT spectra show Fe K 6.4 keV emission first for an active dMe star UVOT enhancement large but unknown: instrument safed at >200,000 counts/s Brightest stellar flare observed E rad ~ 10 38 erg EV Lac is young magnetically active isolated star. –Previous super-flare was from binary RS CVn system, II Peg Swift Trigger on Large Stellar Flare Osten et al 2007, 2008 EV Lac 25 Apr 2008

23. 23 Newly discovered source (Atel #1456) Known pulsar in outburst (Atel #1426) 536 sources monitored 65 detectable on a daily basis ~60 with > 30 mcrab outbursts ~15 mCrab sensitivity in 1 day http://swift.gsfc.nasa.gov/docs/swift/results/transients/ BAT Sky Monitoring SWIFT J1816.7-1613 4U 0115+634 Krimm et al

24. 24 TOOs for Transients & GRBs - Swift can perform rapid X-ray and optical observations of transients - TOO rapidly uploaded as RA & DEC. Response time is <1 hour to 1 day - Web page for TOO requests http://www.swift.psu.edu/too.html - Duty scientists always on call for urgent TOOs - New "command from home" mode for after-hour TOOs - Expert international teams provide rapid advice * GRB follow-up(48 members) * Supernova(22 members) * CVs & novae(24 members) * Hard X-ray survey(18 members) * AGN (4 members) * GeV and TeV  -rays(4 members) - Daily planning telecon to decide schedules

25. 25 Swift Operations Ahead 2 nd mission extension: 2009-2011 – Swift: the ToO Observatory –Swift executes ~70-75 separate pointings per day Each pointing is planned, although significant labor by human science planner to have each pointing a different target –Under an initiative approved by 2008 Senior Review, MOC has conducted an Automation Initiative to streamline science planning –Elements include: Target management database – MySQL database to automatically ingest target information from ToO requests, target lists from GI approved proposals and GRB information from GCN circulars More highly automated TAKO software – will allow higher automation to XRT temperature control and ACS slew behavior –Goal is to allow faster, easier science planning, with capability to increase GI monitoring campaigns and rapid ToO response to large numbers of targets

26. 26 Conclusions Swift has delivered a remarkably successful science mission to date, powered by an innovative operations concept that has continued to evolve as driven by scientific interest The latest changes will enable an even more responsive observatory, giving more GI monitoring and ToO responsiveness For Senior Review 2010, How do you suggest ways to use Swift, and how is that important for astrophysics?

27. 27 Cosmic Timeline & Early Universe Probes z=12z=5 z=0

28. Hint That These Probes Work z=6.29 GRB 050904 SDSS Quasar z=6.28

29. Swift & SDSS only probed the very near edge of reionization We need a statistically significant sample that probes well into the epoch of reionization –We need to find 30-50 GRBs from 5<z<12 ~10x what Swift found (5<z<7) –We need to find 200-400 quasars from 6<z<10 ~10x all z>6 quasars found (6<z<6.5) We Need Higher Redshift Observations z=12z=5

30. Current capabilities from Swift & SDSS needed to observe high redshift objects are: –Rapid localization and observations of GRBs –Rapid notifications to enable observations by other facilities –A very large field of view for finding GRBs & quasars BREADTH versus Depth for rare objects (Critical) To probe high redshift objects we need: –Greater sensitivity to high redshift bursts Redshifted gamma-ray photons into the X-ray –Prompt, uniform follow-up of afterglows in the IR (Critical) –Rapid redshift determination (in minutes) –Observations above the atmosphere are essential to eliminate terrestrial lines that confuse surveys Current Capabilities & Needs

31. 31 The Solution: JANUS 196019802000 Testing Support BCDD EF GHI JKL RST VWX XYZ TUV Space Network ABC 1960197020201980199020002010 Increasing Capabilities X-Ray Flash Monitor (XRFM): Detects & localizes high-z GRBs 1-20 keV, 4 sr field-of-view Near-IR Telescope (NIRT): High-z GRB & quasar spectroscopy 0.7-1.7 μm, 1″ pos, redshifts, 0.36 degree 2 field-of-view, Spacecraft: Rapid communication w/ ground, rapid slewing (50°/100 sec), stable platform

32. 32 JANUS Mission Concept – Sky Survey Mode ~400 quasars 20,000 square degree Survey

33. 33 JANUS Mission Concept – GRB Mode ~50 GRBs

34. 34 JANUS Objectives Determine star formation history by using ~50 GRBs Explore the coevolution of galaxies & black holes by using ~400 quasars Determine if dominant source of reionization