Hurley GRB LAT05

SWIFT, GLAST, THE INTERPLANETARY NETWORK, AND GRB FOLLOW-UP STUDIES: 

SWIFT, GLAST, THE INTERPLANETARY NETWORK, AND GRB FOLLOW-UP STUDIES Kevin Hurley UC Berkeley Space Sciences Laboratory Berkeley, CA khurley@ssl.berkeley.edu

DAY IN THE LIFE OF A “TYPICAL” SWIFT BURST: 

DAY IN THE LIFE OF A “TYPICAL” SWIFT BURST GRB is observed by the Burst Alert Telescope (15-350 keV) 3’ location is computed onboard and transmitted immediately to ground >700 astronomers receive automatic notification; first optical observations by automated ground-based telescopes begin immediately Satellite slews so that its X-ray and UV/Optical telescopes can observe Fading X-ray, optical afterglows are found within minutes and 1-10” positions are transmitted to ground Within hours, circulars are sent out by Swift team to describe the burst in detail Non-automated ground-based telescopes begin to observe Astronomers send out circulars to describe their results Radio observations begin ~days later Redshift is measured within ~days

THE SWIFT FOLLOW-UP TEAM: 

THE SWIFT FOLLOW-UP TEAM Consists of 45 astronomers, mostly interested in GRBs (some are interested in X-ray binaries, soft gamma repeaters, survey sources, etc.) They are not Swift co-investigators Carefully selected for Good geographical coverage Good mix of large telescopes and smaller robotic ones; ground- and space-based Good wavelength coverage One gravitational radiation astronomer Minimum duplication of effort and competition for a given facility within team Commitment to spend time working on Swift GRBs

PRINCIPLES OF OPERATION (SHORT SUMMARY): 

PRINCIPLES OF OPERATION (SHORT SUMMARY) Follow-up astronomers must spend a significant amount of their time, usually >20%, or of their allocated observatory time, observing Swift GRBs, SGRs, or survey sources Are responsible for obtaining their own observing time via proposals, or guaranteed time Agree to keep Swift project (Burst Advocate) informed of their plans and results, to help run the mission more efficiently Agree to collaborate with Swift co-I’s in data analysis and publication, as appropriate Do not receive funding directly from the Swift project, but are free to apply for funding via the Swift GI program

THE SWIFT BURST ADVOCATE (BA): 

THE SWIFT BURST ADVOCATE (BA) One BA is assigned to every Swift burst The BA must be a Swift team member, but is not necessarily a follow-up team member BA is responsible for issuing the first Gamma-Ray Burst Coordinates Circulars describing the burst, usually within < 1 hour of the detection (on duty 24/7) BA remains involved in Swift observations of the burst until it is decided to stop observing it BA may, in some cases, become involved in writing papers about the Swift data and other observations of the burst

SWIFT PROJECT’S OBLIGATIONS TO FOLLOW-UP TEAM MEMBERS: 

SWIFT PROJECT’S OBLIGATIONS TO FOLLOW-UP TEAM MEMBERS Perform supplementary analyses of Swift data as required to enhance follow-up observations (examples might be rapid data analysis while observations are in progress, or later assistance for publications) Consult with follow-up team members in planning Swift follow-up observations of a GRB, in order to maximize scientific output, minimize redundant observations, and observe as many GRBs as possible Minimize competition between follow-up team members for time at any particular observatory, by carefully selecting and limiting team members

Slide7: 

SWIFT FOLLOW-UP TEAM MEMBERS NAME INSTITUTE INSTRUMENT/OBSERVATORY 1. Carl Akerlof U. Michigan ROTSE III 2. Charles Alcock SAO TAOS 3. Angelo Antonelli Rome Observatory ESO, REM, FAME 4. Edo Berger Carnegie Observatories Magellan 5. Michael Bode John Moores U. RoboNet 6. Michel Boer CESR TAROT 7. David Buckley SAAO 9 m SALT telescope 8. Ron Canterna WIRO Red Buttes Obs. 0.6 m IR telescope 9.Andrea Cimatti Arcetri LBT 10. Malcolm Coe Southampton Tenerife IRTF, SAAO 11. Thierry Courvoisier ISDC INTEGRAL 12. Stefano Covino Brera ESO, REM 13. Massimo Della Valle Arcetri VLT, LBT, Galileo 14. Tristano Di Girolamo INFN Naples ARGO 15. Brenda Dingus LANL Milagro 16. Alex Filippenko UC Berkeley KAIT, Keck 17. Sam Finn PSU LIGO 18. Fabrizio Fiore Rome Observatory VLT 19. Derek Fox CalTech 60” Palomar 20. Andy Fruchter STScI HST 21. Tim Giblin College of Charleston U.S. Virgin Islands telescope 22. Roberto Gilmozzi VLT VLT 23. Dieter Hartmann Clemson SARA

SWIFT FOLLOW-UP TEAM, CONTINUED: 

SWIFT FOLLOW-UP TEAM, CONTINUED NAME INSTITUTE INSTRUMENT/OBSERVATORY 24. Huhai He Inst. H.E. Physics ARGO 25. Nobu Kawai RIKEN Okayama Obs. 50 cm robotic & 91 cm IR telescopes 26. Shri Kulkarni Caltech Keck, Palomar 27. Matt Lehner U. Pennsylvania TAOS 28. Bruce Margon STScI ARC, Apache Point 29. Felix Mirabel ESO VLT, Spitzer 30. Carol Mundell John Moores U. La Palma 2 m robotic telescope 31. Paul O’Brien Leicester U. Faulkes, Liverpool telescopes 32. Hye-Sook Park LLNL LOTIS, Super-LOTIS 33. Holger Pedersen Copenhagen U. Obs. NOT La Palma, ESO 34. Alex Pozanenko IKI FAVOR robotic telescope 35. James Rhoads STScI KPNO, CTIO, NASA IRTF 36. Brad Schaefer UT Austin McDonald, HET 37. Don Schneider PSU HET 38. Mark Skinner Air Force AEOS 39. Ian Smith Rice University AEOS, Misc. IR, sub-mm 40. Chris Stubbs U. Washington ARC, Apache Point 41. Nial Tanvir U. Herfordshire UKIRT, WHT 42. Fred Vrba USNO 1 m, 1.3 m telescopes 43. Nic Walton Cambridge Isaac Newton Telescopes 44. Peter Wheatley Leicester WASP, Faulkes 45. Filippo Zerbi Brera REM

ACRONYMS, WEBSITES: 

ACRONYMS, WEBSITES AEOS: Advanced Electro-Optical System, www.fas.org/spp/military/program/track/aeos.htm ARC: Astrophysics Research Consortium, astro.uchicago.edu/uc-apo/ ARGO: Astrophysical Radiation Ground-based Observatory at YangBaJing, argo.na.infn.it CTIO: Cerro Tololo Inter-American Observatory, www.ctio.noao.edu/ ESO: European Southern Observatory, www.eso.org/ FAME: Fast Alert Machine, grb.mporzio.astro.it Faulkes: The Faulkes Telescope Project in Hawaii & Australia, www.faulkes-telescope.com/ FAVOR: Fast Variability Optical Registrator, rokos.sao.ru/favor/ Galileo: Telescopio Nazionale Galileo, www.tng.iac.es HET: Hobby-Eberly Telescope, www.as.utexas.edu/mcdonald/het/het.html HST: Hubble Space Telescope, www.stsci.edu/hst/ INTEGRAL: International Gamma-Ray Astrophysics Laboratory, integral.esac.esa.int/ IRTF: Infrared Telescope Facility, www.iac.es/telescopes/ten.html Isaac Newton Telescopes: www.ing.iac.es/Astronomy/astronomy.html KAIT: Katzman Automated Imaging Telescope, astron.berkeley.edu/~bait/kait_lwd.html Keck: www2.keck.hawaii.edu/ KPNO: Kitt Peak National Observatory, www.noao.edu/kpno/ LBT: Large Binocular Telescope, medusa.as.arizona.edu/lbto/ LIGO: Laser Interferometer Gravitational Wave Observatory, www.ligo.caltech.edu

Slide10: 

/ Liverpool: The Liverpool Telescope at La Palma, telescope.livjm.ac.uk/ Magellan: www.ociw.edu/lco/magellan/ McDonald Observatory: www.as.utexas.edu/mcdonald/mcdonald.html Milagro: http://www.lanl.gov/milagro/index.shtml NASA IRTF: Infrared Telescope Facility, irtfweb.ifa.hawaii.edu NOT: Nordic Optical Telescope, www.not.iac.es OAR: Astronomical Observatory of Rome, grb.mporzio.astro.it Okayama Astrophysical Observatory: http://www.cc.nao.ac.jp/oao/e/ Palomar 60”: http://www.astro.caltech.edu/palomarnew/60inch.html REM: Rapid Eye Mount, golem.merate.mi.astro.it/projects/rem/ RoboNet: Global Network of Robotic Telescopes: www.astro.livjm.ac.uk/RoboNet/ ROTSE: Robotic Optical Transient Search Experiment, www.rotse.net SAAO: South African Astronomical Observatory, www.saao.ac.za SARA: Southeastern Association for Research in Astronomy, www.astro.clemson.edu/sara.html SALT: South African Large Telescope, www.salt.ac.za/default.htm Super-LOTIS: Livermore Optical Transient Imaging System, slotis.kpno.noao.edu/~ggwilli/LOTIS/index.shtml Spitzer: http://ssc.spitzer.caltech.edu/

Slide11: 

TAOS: Taiwanese-American Occultation Survey, www.llnl.gov/urp/igpp/igpp-astro/taos/ TAROT: Rapid Action Telescope for Transient Objects, www.cesr.fr/~boer/tarot/ UKIRT: United Kingdom Infrared Telescope, www.jach.hawaii.edu/JACpublic/UKIRT/home.html UVI: US Virgin Islands Telescope, http://astro.uvi.edu/ USNO: US Naval Observatory, Flagstaff Station, http://www.nofs.navy.mil/ UVI: US Virgin Islands Telescope, http://astro.uvi.edu/ USNO: US Naval Observatory, Flagstaff Station, http://www.nofs.navy.mil/ VLT: Very Large Telescope, www.eso.org WASP: The UK Wide-field Automated Survey Programme, www.star.le.ac.uk/~pjw/wasp/wasp_escience.html WHT: William Herschel Telescope, www.ing.iac.es/Astronomy/telescopes/wht WIRO: Wyoming Infrared Observatory, faraday.uwyo.edu/observatories/wiro/

FOUR TYPES OF FOLLOW-UP FACILITIES: 

FOUR TYPES OF FOLLOW-UP FACILITIES Automated telescopes; slew automatically within seconds to a GRB position whenever possible. FOV’s vary widely, from <degree to tens of degrees. Non-steerable facilities, like Milagro and LIGO; observe a large fraction of the sky more or less continuously Space-based telescopes (INTEGRAL, XMM, HST); in principle, they can respond to Swift GRBs on a ToO basis, but this may take a day or more Large, steerable, ground-based telescopes Facilities like 1 and 2 could observe GLAST bursts directly if location accuracy is in the degree or less range

MAIN INTERACTIONS BETWEEN THE BA AND THE FOLLOW-UP TEAM: 

MAIN INTERACTIONS BETWEEN THE BA AND THE FOLLOW-UP TEAM BA needs to know when to give up control of a burst, to allow a new burst to be observed; in many cases an element in this decision will be the quantity and quality of follow-up observations being planned or conducted Follow-up astronomer may need to request a particular type or duration of observation by Swift to complement his or her observations Some aspects of the Burst Advocate model might be appropriate for GLAST

SWIFT/GLAST SYNERGY: 

SWIFT/GLAST SYNERGY Swift can only observe bursts up to ~350 keV; GLAST can complete Swift energy spectra GLAST will generally observe a different part of the sky from Swift; Swift can perform ToO observations of GLAST GRBs, and obtain small error boxes for them from the X-ray afterglow (GLAST localization must be better than 26’); these GRBs would be observable by large telescopes LAT could follow up Swift bursts up to ~1 hour later to observe delayed high energy photons

SWIFT HAS SPOILED FOLLOW-UP ASTRONOMERS: 

SWIFT HAS SPOILED FOLLOW-UP ASTRONOMERS All the data are public They are used to getting 3’ positions instantly They are used to getting 10” positions within a few hours They are used to getting burst parameters (durations, spectra, fluences) within a few hours They are used to getting a new burst notification every few days (Swift detection rate is 100/year); low false positive rate Result: they no longer chase every burst

GLAST AND THE INTERPLANETARY NETWORK: 

GLAST AND THE INTERPLANETARY NETWORK The interplanetary network (IPN) consists of GRB detectors on 8 missions: Ulysses, Mars Odyssey, MESSENGER, Swift, Wind, HETE, RHESSI, and INTEGRAL It localizes GRBs to ~arcminute accuracy by timing their arrival at these spacecraft It detects ~200 GRBs/year The localization data are useful to people who do not need instantaneous notifications, but do require data on many bursts (e.g., AMANDA)

INTEGRATING THE GAMMA-RAY BURST MONITOR INTO THE IPN: 

INTEGRATING THE GAMMA-RAY BURST MONITOR INTO THE IPN The GBM will detect GRBs whose localizations can’t be improved By integrating the Monitor into the IPN, we can obtain refined positions for many of them The requirements are An onboard clock which is accurate to ~milliseconds A reasonably accurate spacecraft ephemeris GRB lightcurves with time resolution in the 10’s of ms range