comprehensive multisensory multimodal integration in astrophysics … · 2018. 12. 14. · ando et...

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 MarkaColumbia Experimental Gravity Group

Columbia University

Image credit: LSC/Sonoma State University/Aurore Simonnet Miami 2018, Ft.Lauderdale, December 2018Based on LIGO-G1801251-x0

The discovery of gravitational waves and their multimessengerfingerprint has opened tremendous opportunities for astrophysics.Extraordinary instrumental breakthroughs in gravitational-wavedetectors, electromagnetic and neutrino observatories shall lead toan information explosion during the coming years and decades,rapidly expanding humanity’s cosmic and scientific horizon.Multisensory observations of gravitational-wave sources promisesopportunities that are complementary to insights gained throughtraditional means. After decades of focused efforts, the observationof an electromagnetic counterpart to the gravitational-wave eventGW170817 by a multitude of instruments highlighted the value ofmultimessenger astrophysics and indicated that short gamma-raybursts (GRB) could arise from mergers of pairs of neutron stars,and, more generally, that binary mergers are capable of acceleratingparticles and producing high-energy emission. ComprehensiveMultisensory Multimodal Integration in Astrophysics is happeningat an accelerated scale promising a bright future.opportunities forLISA.

https://writescience.wordpress.com/tag/gravitational-waves/

http://www.ligo.org/multimedia/gallery/lho.php

1916:

Thanks to D.Shoemaker, S.Larson, and LSC

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 Pustovoit1963 Sov. Phys.–JETP 16 433)

1971:

Thanks to D.Shoemaker, and LSC

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…

Thanks to D.Shoemaker, S.Larson, and LSC

5

https://dspace.mit.edu/bitstream/handle/1721.1/56271/RLE_QPR_105_V.pdf

Massachusetts Institute of Technology, Research Laboratory of Electronics, Quarterly Progress Report, April 15, 1972

Thanks to D.Shoemaker and LSC

1989 Proposal to the US NSF

1990:

Courtesy of LIGO and LSCImages : LIGO Lab

Cred

it: C

alte

ch

How Gravitational-wave Observations Can Shape the Gamma-ray Burst Paradigm?Bartos, Brady, Marka – Topical Review – Editor’s Highlght - CQG

The Birth and Death of Black Holes ++

Courtesy of LSC and Zsuzsa Marka

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

Courtesy of Brian Metzger

Courtesy: Brian Metzger, Columbia University, PCTS18

GW170817

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

2001 http://gravity.physics.uwa.edu.au/amaldi/papers/NDAS.pdf

Basic Glossary: Multimessenger Approaches“Multi-messenger astrophysics”: connecting different kinds of observations of the same astrophysical event or system

GWData

Telescopes, Satellites or other external entities

“Follow-Up” strategy:Flow of trigger

information

Image courtesy R

OTS

E collaboration

GWSearch

Telescopes, Satellites or other external entities

“ExtTrig” strategy:Flow of trigger

information

» 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 …

Confident detection of GWs. Better background rejection ⇒ Higher sensitivity to GW signals.More information about the source/engine.Measurements made possible through coincident detection.

Transient Multimessenger Astrophysics with GWs

LHO

LLO

Swift/HETE-2/

IPN/INTEGRAL

RXTE/RHESSI

Image credit: Zsuzsa Marka – GWDAW12

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 Gamma-ray Burst Paradigm”; Class. Quantum Grav. 30, 123001, 2013 (CQG Highlights)

• GRB triggered searches method development until 2003• First GRB multimessenger search: GRB030329B. Abbott et al. [LIGO Scientific Collaboration], “A search for gravitational waves associated with the gamma ray burst GRB030329 using the LIGO detectors”, Phys. Rev. D 72, 042002, 2005

• S4, S5, S6 GRB triggered searches upper limits

• First astrophysically significant result from LIGO:Non detection of GWs from direction of GRB070201 (Andromeda galaxy) contributed to the detection of the first extragalactic SGR hyperflareB. Abbott et al. [LIGO Collaboration], “Implications for the Origin of GRB 070201 from LIGO Observations”,ApJ., 681, 1419, 2008

• First coincident observation!Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A, Abbott et al., The Astrophysical Journal, 848, L13, 2017

“Implications for the Origin of GRB 070201 from LIGO Observations”, ApJ., 681, 1419, 2008

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 1806 - 20 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, 211102, 2008

P. Kalmus, K.C. Cannon, S. Marka, B. Owen, "Stacking Gravitational Wave Signals from Soft Gamma Repeater Bursts", Physical Review D, 80, 042001, ArXiv e-prints, 0904.4906, 2009

Abbott et al., “Stacked Search for Gravitational Waves from the 2006 SGR 1900+14 Storm”, Astrophysical Journal, 701, L68, arXiv:0905.0005, 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, 103008, 2013

Slide Courtesy of Imre Bartos

Multimessenger searches for GWs with LIGO: HENs

High-energy neutrino – GW multimessenger studies since 2006

Original idea presented in 2006 GWDAW meeting,

Team building: GWHEN

High Energy Neutrino + GW Joint Search

High-energy Neutrino follow-up search of Gravitational Wave Event GW150914 with ANTARES and IceCube Antares Collaboration, IceCube Collaboration, LIGO Scientific Collaboration, Virgo Collaboration PRD 93, 122010 (2016)

Search for High-energy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger ObservatoryANTARES, IceCube, Pierre Auger, LIGO Scientific and Virgo CollaborationsApJ Lett. 850:L35 (2017) [http]

Optical emission from a kilonova following a gravitational-wave-detected neutron-star mergerIair Arcavi, Griffin Hosseinzadeh, D. Andrew Howell, Curtis McCully, Dovi Poznanski, Daniel Kasen, Jennifer Barnes, Michael Zaltzman, SergiyVasylyev, Dan Maoz & Stefano ValentiNature volume 551, pages 64–66 (02 November 2017)

Multimessenger searches for GWs with LIGO: EM follow-up program• Since 2007 - pioneering study used SWOPE(!) and MDM

telescope, real-time pipeline topology, and galaxy targeting

• 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 –

GW170817 – GRB170817A

SWOPE

Image: carnegiescience.edu

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, 184034, 2008

Pioneering fields of science often have more questions than answers…

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?

Marka, 2010, http://iopscience.iop.org/1742-6596/243/1/012001/pdf/1742-6596_243_1_012001.pdf


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?



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?



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?



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?



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!


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

Benefits• Target for small FoV telescopes• Decrease false positive rate

Can we make a catalog in the right timeframe, distance range and sky area?

1 week 200-500 Mpc 100 deg2

• 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)

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

Path Forward: Build Galaxy Catalogs (a possible approach)

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 MNRAS477, 639–647 (2018) [http]

Cherenkov Telescope Array is Well Suited to Follow Up Gravitational Wave Transients MNRAS 443, 738-749 (2014)

Bartos, Huard, Marka, APJ 2016

JAMES WEBB SPACE TELESCOPE CAN DETECT KILONOVAE IN GRAVITATIONAL WAVE FOLLOW-UP SEARCH

Bartos, Huard, Marka, APJ 2016

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

Can BBH mergers produce a counterpart?

Possible processes in dense environments

Other possibilities: Stellar core collapse: collapsing core clumps (Loeb 2016), Gas remains from stellar progenitor (Perna+ 2016, Mink+ 2017)

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.

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).

from Open Questions to Instruments that can answer them…

Questions and Prioritization Developed in Consultation with: Marica Branchesi, David Reitze, Alessandra Corsi, Wen-faiFong, David Shoemaker, Peter Shawhan, Kohta Murase, Zsuzsa Marka, Chad Hanna, Peter Meszaros, Derek Fox, Miguel Alejandro Mostafá, Leo Singer, Edo Berger, Nils Andersson, Samaya Nissanke, Raffaella Margutti

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).

from Open Questions to Instruments that can answer them…

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?

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?



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)?

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. 32 065001 doi:10.1088/0264-9381/32/6/065001

Questions?

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