Comprehensive Multisensory Multimodal Integration in Astrophysics

Transcription

1 Image credit: LSC/Sonoma State University/Aurore Simonnet Based on LIGO-G x0 Miami 2018, Ft.Lauderdale, December 2018 The discovery of gravitational waves and their multimessenger fingerprint has opened tremendous opportunities for astrophysics. Extraordinary instrumental breakthroughs in gravitational-wave detectors, electromagnetic and neutrino observatories shall lead to an information explosion during the coming years and decades, rapidly expanding humanity s cosmic and scientific horizon. Multisensory observations of gravitational-wave sources promises opportunities that are complementary to insights gained through traditional means. After decades of focused efforts, the observation of an electromagnetic counterpart to the gravitational-wave event GW by a multitude of instruments highlighted the value of multimessenger astrophysics and indicated that short gamma-ray bursts (GRB) could arise from mergers of pairs of neutron stars, and, more generally, that binary mergers are capable of accelerating particles and producing high-energy emission. Comprehensive Multisensory Multimodal Integration in Astrophysics is happening at an accelerated scale promising a bright future.opportunities for LISA. Where are we coming from and where are we going: Comprehensive Multisensory Multimodal Integration in Astrophysics (a personal view on Past, Current and Future in MMA) Szabolcs Marka Columbia Experimental Gravity Group Columbia University

2 1916: Thanks to D.Shoemaker, S.Larson, and LSC

3 1956 : Gedanken experiment using interferometry to detect GWs: F.A.E. Pirani, Acta Phys. Polon. 15, 389 (1956) (predates invention of laser by 4 years!) 1963: Laser interferometry for gravitational-wave detection mentioned as theoretical possibility (Gerstenstein and Pustovoit 1963 Sov. Phys. JETP ) 1971: Thanks to D.Shoemaker, and LSC

4 Massachusetts Institute of Technology, Research Laboratory of Electronics, Quarterly Progress Report, April 15, 1972 Late 1960s-1972: Rai Weiss of MIT was teaching a course on GR in the late 60s Wanted a good homework problem for the students Why not ask them to work out how to use laser interferometry to detect gravitational waves?...weiss wrote the instruction book LIGO have been following ever since 5 Thanks to D.Shoemaker, S.Larson, and LSC

5 1989 Proposal to the US NSF Thanks to D.Shoemaker and LSC

6 1990: Courtesy of LIGO and LSC

7 Credit: Caltech

8 The Birth and Death of Black Holes ++ How Gravitational-wave Observations Can Shape the Gamma-ray Burst Paradigm? Bartos, Brady, Marka Topical Review Editor s Highlght - CQG

9 Courtesy of LSC and Zsuzsa Marka

10 LIGO/Virgo and the EM-Follow-up partners, ApJL Oct 16, 2017

11 Courtesy of Brian Metzger

12 Courtesy of Brian Metzger

13 GW Courtesy: Brian Metzger, Columbia University, PCTS18

14 Multimessenger searches for GWs with LIGO take off in ~2000 LIGO joins SNEWS, GCN, and IPN ~2000 NDAS gets data from worldwide network Courtesy: Nasa Courtesy: SuperK Courtesy: NSF

15 Basic Glossary: Multimessenger Approaches Multi-messenger astrophysics : connecting different kinds of observations of the same astrophysical event or system GW Data Follow-Up strategy: Flow of trigger information Telescopes, Satellites or other external entities Image courtesy ROTSE collaboration ExtTrig strategy: Telescopes, Satellites or other external entities Flow of trigger information GW Search

16 Transient Multimessenger Astrophysics with GWs» Gamma-ray transients (GRBs, SGRs)» Optical transients» Neutrino events» Radio transients» X-ray transients» Correlation in time Correlation in direction Information on the source properties, host galaxy, distance RXTE/RHESSI LHO LLO Swift/ HETE-2/ IPN/ INTEGRAL Image credit: Zsuzsa Marka GWDAW12 Confident detection of GWs. Better background rejection Higher sensitivity to GW signals. More information about the source/engine. Measurements made possible through coincident detection.

17 Multimessenger searches for GWs with LIGO: GRBs for review of topic see: Bartos I., Brady P., Marka S.; How Gravitational-wave Observations Can Shape the Gammaray Burst Paradigm ; Class. Quantum Grav. 30, , 2013 (CQG Highlights) GRB triggered searches method development until 2003 First GRB multimessenger search: GRB Implications for the Origin of GRB from LIGO Observations, ApJ., 681, 1419, 2008 B. Abbott et al. [LIGO Scientific Collaboration], A search for gravitational waves associated with the gamma ray burst GRB using the LIGO detectors, Phys. Rev. D 72, , 2005 S4, S5, S6 GRB triggered searches upper limits First astrophysically significant result from LIGO: Non detection of GWs from direction of GRB (Andromeda galaxy) contributed to the detection of the first extragalactic SGR hyperflare B. Abbott et al. [LIGO Collaboration], Implications for the Origin of GRB from LIGO Observations, ApJ., 681, 1419, 2008 First coincident observation! Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW and GRB A, Abbott et al., The Astrophysical Journal, 848, L13, 2017

18 Multimessenger searches for GWs with LIGO: SGRs SGR related searches since 2004 (hyperflares, stacked searches) Targeting both initial transient and quasiperiodic oscillations in pulsating tail Abbott B. et al., [LIGO Collaboration], Search for gravitational wave radiation associated with the pulsating tail of the SGR hyperflare of 27 December 2004 using LIGO, Phys. Rev. D. 76:062003, 2007 P. Kalmus, R. Khan, L. Matone, S. Marka, Search method for unmodeled transient gravitational waves associated with SGR flares, Class. Quantum Grav. 24, 659, 2007 B. Abbott et al. [LIGO Collaboration], Search for Gravitational Wave Bursts from Soft Gamma Repeaters, Physical Review Letters 101, , 2008 P. Kalmus, K.C. Cannon, S. Marka, B. Owen, "Stacking Gravitational Wave Signals from Soft Gamma Repeater Bursts", Physical Review D, 80, , ArXiv e-prints, , 2009 Abbott et al., Stacked Search for Gravitational Waves from the 2006 SGR Storm, Astrophysical Journal, 701, L68, arxiv: , 2009 Abadie et al., "Search for Gravitational Wave Bursts from Six Magnetars", The Astrophysical Journal, 734, L35, 2011 Murphy D., Tse M., Raffai P., Bartos I., Khan R., Marka Z., Matone L., Redwine K., Marka S.; Detecting Long-Duration Narrow- Band Gravitational Wave Transients Associated with Soft Gamma Repeater Quasi-Periodic Oscillations ; Phys. Rev. D 87, , 2013

19 Slide Courtesy of Imre Bartos

20 Multimessenger searches for GWs with LIGO: HENs High-energy neutrino GW multimessenger studies since 2006 Original idea presented in 2006 GWDAW meeting, Search method for coincident events from LIGO and IceCube detectors Class. Quantum Gravity, 25, , 2008 Team building: GWHEN <= LIGO, Virgo, Icecube, ANTARES Y. Aso, Z. Marka, C. Finley, J. Dwyer, K. Kotake, S. Marka, Search method for coincident events from LIGO and IceCube detectors Class. Quantum Gravity, 25, , 2008 Baret et al., "Bounding the time delay between high-energy neutrinos and gravitational-wave transients from gamma-ray bursts", Astroparticle Physics, 35, Ando et al., "Colloquium: Multimessenger astronomy with gravitational waves and high-energy neutrinos", Rev. Mod. Phys. 85, , 2013 Bartos et al., "Observational Constraints on Multimessenger Sources of Gravitational Waves and High-Energy Neutrinos", Physical Review Letters, 107, , 2011 Baret et al., "Multimessenger Science Reach and Analysis Method for Common Sources of Gravitational Waves and High-energy Neutrinos", Physical Review D, 85, , 2012 Aartsen et al., Multimessenger search for sources of gravitational waves and high-energy neutrinos: Initial results for LIGO-Virgo and IceCube, Physical Review D, 90, , 2014 (Initial LIGO/Virgo era search) Result from O1/O2 High-energy Neutrino follow-up search of Gravitational Wave Event GW with ANTARES and IceCube, Antares Collaboration, IceCube Collaboration, LIGO Scientific Collaboration, Virgo Collaboration, arxiv: , 2016 Search for high-energy neutrinos from gravitational wave event GW and candidate LVT with ANTARES and IceCube, Albert et al., Physical Review D, 96, , 2017 Search for High-energy Neutrinos from Binary Neutron Star Merger GW with ANTARES, IceCube, and the Pierre Auger Observatory, Albert et al., The Astrophysical Journal, 850, L35, 2017

21 High-energy Neutrino follow-up search of Gravitational Wave Event GW with ANTARES and IceCube Antares Collaboration, IceCube Collaboration, LIGO Scientific Collaboration, Virgo Collaboration PRD 93, (2016) High Energy Neutrino + GW Joint Search earch for High-energy Neutrinos from Binary Neutron Star Merger W with ANTARES, IceCube, and the Pierre Auger Observatory NTARES, IceCube, Pierre Auger, LIGO Scientific and Virgo Collaborations pj Lett. 850:L35 (2017) [http]

22 Optical emission from a kilonova following a gravitational-wave-detected neutron-star merger Iair Arcavi, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Dovi Poznanski, Daniel Kasen, Jennifer Barnes, Michael Zaltzman, Sergiy Vasylyev, Dan Maoz & Stefano Valenti Nature volume 551, pages (02 November 2017)

23 Multimessenger searches for GWs with LIGO: EM follow-up program Since pioneering study used SWOPE(!) and MDM telescope, real-time pipeline topology, and galaxy targeting SWOPE J. Kanner, T. L. Huard, S. Márka, D. C. Murphy, J. Piscionere, M. Reed, P. Shawhan, LOOC UP: locating and observing optical counterparts to gravitational wave bursts, Classical and Quantum Gravity 25, , 2008 Near-real time searches development, search program with ~10 MOU during the last weeks of initial LIGO era Large scale program with >70 partners by start of advanced LIGO, facilitated by preparations during and since initial LIGO as well as advancement in theory (Metzger) Result from O1 NGC4993 GW GRB170817A Image: carnegiescience.edu

24 Pioneering fields of science often have more questions than answers

25 Marka, 2010, Open Questions for Multimessenger Observations with Gravitational Wave Detectors? Oh YES! 1. What is the speed of gravitational waves, subluminal or superluminal? 2. Does Einstein's theory of general relativity remain valid in the strong field regime? 3. Does gravity violate parity? 4. Is there a new length scale beyond which general relativity is modified? 5. Which alternative gravity theories can be excluded experimentally? 6. How often can an unidentified electromagnetic transient be explained by a gravitational wave emitter? 7. Is there a high redshift population of intermediate mass black holes? 8. Can gravitational waves help in explaining the origin of Ultra- Luminous X-ray binaries? 9. Can we search for new physics in the ultra-weak field regime? 10. Can a massive graviton serve as a cold-dark-matter candidate? 11. What fraction of the cosmic source's energy is emitted in the form of gravitational waves?

26 Marka, 2010, Open Questions for Multimessenger Observations with Gravitational Wave Detectors? Oh YES! 12.Can gravitational wave detectors provide an early warning to electromagnetic observers to allow the detection of early light curves? 13. Do gravitational measurements of distance agree with the concordance cosmology? 14. What is the mass spectrum and spin distribution of black holes? 15. Are there extra gravitational wave polarizations? 16.Is there a significant non-axisymmetric crust or core dynamics associated with SGRs?

27 Marka, 2010, Open Questions for Multimessenger Observations with Gravitational Wave Detectors? Oh YES! 17. What is the precise origin of SGR flares? (e.g., What is the mechanism for GW and EM emission and how are they correlated?) 18. Is there a fundamental difference between giant and common SGRs? 19. Do quark stars exist? 20. Can we exclude or confirm some of the SGR models? 21. What is the origin of pulsar glitches? 22. What is the composition and structure of neutron stars and their cores? 23. What is the tallest mountain that can be supported by neutron stars? 24. Can we use GW-EM observations to guide or EM+null GW results to distinguish the local extragalactic SGR contributions from the short GRB population?

28 Marka, 2010, Open Questions for Multimessenger Observations with Gravitational Wave Detectors? Oh YES! 25. What is the nature of gravitational collapse? 26. What is the relationship between the supernova progenitor and remnant (e.g., final mass and spin)? 27. If the supernova remnant is not a black hole, how does it behave? (e.g., a transient hypermassive remnant with unstable modes or collapse to a BH?) 28. What happens in a core collapse supernova before the light and neutrinos escape? 29. What is the delay in between neutrinos and gravitational waves in a core collapse supernovae? 30. What is the role of anisotropic neutrino emission in supernovae? 31. What is the mass of a neutrino? 32. Can we see core collapse supernovae in gravitational waves that are not visible in neutrinos? 33. Is there an electromagnetically hidden population of core collapse events? 34. How many dynamical scenarios are associated with core collapse supernovae? Can we distinguish between them? 35. Can pulsar birth kicks result in detectable gravitational waves?

29 Marka, 2010, Open Questions for Multimessenger Observations with Gravitational Wave Detectors? Oh YES! 25.What is the time delay between the electromagnetic brightening and the core collapse of a supernova? 26. What are the properties of the core collapse supernova progenitor? 36. What is the role of the rotation and magnetic fields in stellar core collapse? 37. What is the origin of long and short GRBs? What is the precise dynamics of each GRB engine? 38. Is there any longer-lasting central engine left over from the GRB explosion, and what's its nature? 39. Are there electromagnetically hidden populations of GRBs? 40. Does the hypothesized low luminosity GRB population exist? 41. Can we have direct inferences on the GRB jet parameters from gravitational waves? 42. Can we estimate properties of the nuclear equation state using short GRBs? 43. Can we relate the luminosity distribution of GRBs to beaming and the central engine mechanism?

30 Marka, 2010, Open Questions for Multimessenger Observations with Gravitational Wave Detectors? Oh YES! 25.What is the relationship between the parameters of a compact binary system and it's electromagnetic and neutrino emission? 26. What GRB progenitor models can we confirm or reject? 27. Are there other (sub)classes of GRBs? Do choked GRBs exist? What is the origin of choked GRBs? Cosmic population of choked GRBs? 44. What are the engines producing high energy neutrino and gravitational wave emission together? 45. What is the dynamics/energetics of joint high energy neutrino and gravitational wave emitters? 46. What is the electromagnetic emission of binary neutron star coalescence? 47. What is the electromagnetic emission of a neutron star-black hole coalescence? 48. Is there any electromagnetic emission from binary black hole coalescence? 49. What is the nature of XRFs and their relationship to long GRBs? 50. Is it possible to construct a competitive Hubble diagram based on gravitational wave standard sirens? 51. and dozens of other exciting questions are waiting to be answered by the community!

31 Multimessenger searches for GWs with LIGO: EM follow-up program II Galaxy catalog is a key ingredient Included in original GWHEN and LOOC-UP programs Completeness is still an issue LOOC-UP paper, 2008 Bartos, Crotts,Marka, APJL 2015 GALAXY SURVEY ON THE FLY: PROSPECTS OF RAPID GALAXY CATALOGING TO AID THE ELECTROMAGNETIC FOLLOW-UP OF GRAVITATIONAL WAVE OBSERVATIONS

32 Path Forward: Build Galaxy Catalogs (a possible approach) Bartos, Crotts,Marka, APJL 2015 GALAXY SURVEY ON THE FLY: PROSPECTS OF RAPID GALAXY CATALOGING TO AID THE ELECTROMAGNETIC FOLLOW-UP OF GRAVITATIONAL WAVE OBSERVATIONS Benefits Target for small FoV telescopes Decrease false positive rate Can we make a catalog in the right time frame, distance range and sky area? 1 week Mpc 100 deg 2 Extended H-alpha survey (R-band comparison) Only want galaxies within horizon distance Only need source direction Meter class telescopes work. Don t need very high completeness (Hanna+ 2014)

33 Strategies for the Follow-up of Gravitational Wave Transients with the Cherenkov Telescope Array I. Bartos, T. Di Girolamo, J.R. Gair, M. Hendry, I.S. Heng, T.B. Humensky, S. Marka, Z. Marka, C. Messenger, R. Mukherjee, D. Nieto, P. O'Brien, M. Santander MNRAS 477, (2018) [http] Cherenkov Telescope Array is Well Suited to Follow Up Gravitational Wave Transients MNRAS 443, (2014)

34 Bartos, Huard, Marka, APJ 2016 JAMES WEBB SPACE TELESCOPE CAN DETECT KILONOVAE IN GRAVITATIONAL WAVE FOLLOW-UP SEARCH

35 JWST/NIRCam will be able to regularly survey GW event candidates for kilonova counterparts => statistically significant sample size of kilonova emission parameters rapidly find kilonovae => detailed study of temporal and spectral evolution Bartos, Huard, Marka, APJ 2016

36 Can BBH mergers produce a counterpart? Possible processes in dense environments Black holes AGN disks (Bartos+ 2017&2017, Stone+ 2017) Galactic centers may harbor thousands of stellar mass black holes within the inner parsec (Morris 1993, O Leary+ 2009). A fraction of black holes may be in binaries (30%; Pfuhl 2014). Some galactic centers accrete large amounts of gas (active galactic nuclei). Binaries migrate into the disk and then rapidly inspiral via dynamical friction. Other possibilities: Stellar core collapse: collapsing core clumps (Loeb 2016), Gas remains from stellar progenitor (Perna+ 2016, Mink+ 2017)

37 from Open Questions to Instruments that can answer them 1. What are the main challenges of EM-follow up in the upcoming years? 2. Do BBH mergers produce EM emission? How, when and in what environment were merging binary black hole systems formed? 3. Do NS-NS mergers lead to prompt BH formation, or a (meta)stable heavy NS? How can we use GW+EM observations to answer that? 4. How to deal with the future's detection of distant BNS sources in MMA? 5. Hopes and facts for new multi-wavelength large survey and characterization instruments? In general, what are the key EM counterpart instruments going to be for the next 5-30 years? What instruments are not partners yet that can improve the capabilities of the EM counterpart classification? How will the third generation of GW detectors change EM-follow up procedure and prospects? What unplanned instruments do we need for best MMA science? What questions from EM observers for GW field? How can EM observations evolve to better inform GW searches/strategy, and vice versa? 6. How accurate/reliable does the astrophysics needs to be ultimately? How good can it be feasibly? Questions and Prioritization Developed in Consultation with: 7. How GW+EM observations can delineate between different formation scenarios for NS-NS/NS- BH/BBH mergers? Marica Branchesi, David Reitze, Alessandra Corsi, Wen-fai Fong, David Shoemaker, Peter Shawhan, Kohta Murase, Zsuzsa Marka, Chad Hanna, Peter Meszaros, Derek Fox, 8. What do kilonovae really look like in the statistical sense; are there sub-types? (Light curve, spectrum, brightness). Miguel Alejandro Mostafá, Leo Singer, Edo Berger, Nils Andersson, Samaya Nissanke, Raffaella Margutti

38 from Open Questions to Instruments that can answer them 1. What are the main challenges of EM-follow up in the upcoming years? 2. Do BBH mergers produce EM emission? How, when and in what environment were merging binary black hole systems formed? 3. Do NS-NS mergers lead to prompt BH formation, or a (meta)stable heavy NS? How can we use GW+EM observations to answer that? 4. How to deal with the future's detection of distant BNS sources in MMA? 5. Hopes and facts for new multi-wavelength large survey and characterization instruments? In general, what are the key EM counterpart instruments going to be for the next 5-30 years? What instruments are not partners yet that can improve the capabilities of the EM counterpart classification? How will the third generation of GW detectors change EM-follow up procedure and prospects? What unplanned instruments do we need for best MMA science? What questions from EM observers for GW field? How can EM observations evolve to better inform GW searches/strategy, and vice versa? 6. How accurate/reliable does the astrophysics needs to be ultimately? How good can it be feasibly? 7. How GW+EM observations can delineate between different formation scenarios for NS-NS/NS- BH/BBH mergers? 8. What do kilonovae really look like in the statistical sense; are there sub-types? (Light curve, spectrum, brightness).

39 more Open Questions in Astrophysics 9. Can we catch the X-ray afterglows of binary mergers without detecting a GRB? 10. What else do we need from EM counterparts to maximize science return of GW observations? 11. Will wide-field instruments for detecting GRBs (broadly defined) continue to be available throughout the next decades of discovery? 12. How will the third generation of GW detectors change EM-follow up instruments procedure and prospects? 13. GW triggered analysis (GRB, SN, FRB, pulsar glitches, SGR): how to use and maximize all the EM observables, models, theory and phenomenology? 14. What science return is expected with statistical studies GW/EM detection? How to maximize it? 15. How well will we understand the equation of state as observation are made in the future? To what extent is the physics implemented in simulations? 16. What is the best strategy for seeking optical/ir counterparts as observations and observatories evolve? 17. What more is required from the modeling side (numerical/theoretical) for kilonova/grb/radio + GW interpretation? 18. What detections we need to meaningfully probe cocoon and off-axis scenaria?

40 more Open Questions in Astrophysics 19. Future needs from modeling and simulations of astrophysical sources of gravitational waves including emission and population models. 20. Will we detect a GW signal from a core-collapse supernova during the lifetime of aligo/a+? 21. To what extent can EM observations actually evolve to even better inform GW searches/strategy, and vice versa? 22. What are the relative rates among formation scenaria? 23. What are the questions experimentalist have for data analysis, theory and phenomenology; and vice versa? 24. Is there a universal beaming angle for short GRBs, or does it vary? 25. How robust are kilonova model predictions? What are the tests of the future to probe robustness? 26. What more do we need from the GRB observational, theory and phenomenology communities? 27. How can radio counterparts searches be further enhanced? 28. How multiple EM/GW detections can constrain formation and evolution model of compact objects?

41 more Open Questions in Astrophysics 29. At which point do observations of binaries begin to constrain population synthesis models or simulations? 30. What mass distribution of black holes in merging binaries will tell us? 31. How multiple kilonova detections (possibly with low SNR) can further restrict the model? 32. How incomplete are current merger simulations? 33. Consistency and evolution of astrophysical source rate predictions from numerical simulations and MMA/GW observations; 34. Do stellar-mass BBH mergers feed a merger tree that builds much higher-mass BHs? 35. Are NS masses in merging binaries consistent with other measured NS masses? 36. To what extent will MMA observations constrain GW models (eg. within the magnetar model)?

42 Comprehensive Multisensory Multimodal Integration in Astrophysics Figure 14 from Gravitational lensing by spinning black holes in astrophysics, and in the movie Interstellar Oliver James et al 2015 Class. Quantum Grav doi: / /32/6/065001

43 Questions?