Gravitational Waves and Gamma-Ray Bursts in Multimessenger - - PowerPoint PPT Presentation

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Gravitational Waves and Gamma-Ray Bursts in Multimessenger - - PowerPoint PPT Presentation

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Many thanks to the experimenters building the detectors! Gravitational Waves and Gamma-Ray Bursts in Multimessenger Astrophysics LIGO-G0900996 Szabolcs Mrka Columbia University in the City of New York 2009 Fermi Symposium, Washington DC,

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Szabolcs Márka

Columbia University in the City of New York

Gravitational Waves and Gamma-Ray Bursts in Multimessenger Astrophysics

2009 Fermi Symposium, Washington DC, November, 2009

Many thanks to the experimenters building the detectors!

LIGO-G0900996

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Indirect evidence of gravitational radiation

Hulse Taylor

Matching the theoretical prediction

(Nobel Prize in Physics, 1993)

Video Credit: NASA

arXiv:astro-ph/ 0407149v1

~ diameter of a hydrogen atom !

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Gravitational Wave Sources Transients Repeaters Continuous

Searches for Sources

PRL

Modeled UnModeled Triggered All-Sky/Time

short GRB pulsar SGR supernovae circular inspiral eccentric encounter stochastic bkg. BH-BH merger e.g.

e.g., S5 publications:

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The Global Network

  • f Gravitational Wave Detectors

GEO600 Germany VIRGO Italy LIGO Livingston LIGO Hanford TAMA Japan

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» 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.

Multimessenger Astrophysics with GWs

LHO LLO

Swift/ HETE-2/ IPN/ INTEGRAL RXTE/RHESSI

Graphics courtesy of Zsuzsa Marka

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Basic Glossary: Multimessenger Approaches “Multi-messenger astrophysics”: connecting different kinds of

  • bservations of the same astrophysical event or system

GW Telescopes, Satellites

  • r other external entities

“Looc-Up” strategy:

Flow of trigger information

Image courtesy ROTSE collaboration

GW Telescopes, Satellites

  • r other external entities

“ExtTrig” strategy:

Flow of trigger information

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Pulsars Spinning Down (5th Science Run)

  • The Crab Pulsar [ see Abbott et al., ApJL 683, L45 for details ]

» Null search result implies that < ~2% of the spin-down energy is going into GW emission ( beat spin-down amplitude limit by a factor of ~7 )

  • Other known pulsars [ see e.g., Abbott et al., PRD 76, 042001 for pulsar list]

» PSR J1603–7202 : h0 < 2.3 10–26 » PSR J2124-3358 : ε < 7 10–8

  • Theoretical context

» Normal crystalline crust can have ε to be up to ~4 10–6

[ see e.g., Horowitz & Kadau, PRL 102, 191102 ]

» Exotic forms of crystalline quark matter could sustain ε up to ~10–4 [ see e.g., Owen 2005; Lin 2007; Haskell et al 2007; Knippel &

Sedrakian 2009 ]

Chandra image

Slide inspired by P.Shawhan’s, M.Pitkin’s Amaldi8 talk

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S5y1 Individual SGR Burst Search

  • PRL 101, 211102 (2008)
  • First search sensitive to NS f-

modes

  • LIGO S5 + Astrowatch
  • 191 SGR events including:
  • largest giant flare (SGR 1806-20)
  • SGR 1900+14 storm
  • Ioka MNRAS 327, 639 (2001)
  • Most quantitative, detailed model
  • EGW=~1048 erg not unreasonable

2.9x1045 erg 2.4x1048 erg Isotropic GW emission upper limits at 10kpc Circles: Giant Flare Diamonds: GRB 060806

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Eiso ~ 1045 ergs if at M31 distance

(more similar to SGR than GRB energy)

GRB 070201 – Sky Location

R.A. = 11.089 deg, Dec = 42.308 deg

DM31≈770 kpc

Possible progenitors for short GRBs:

  • NS/NS or NS/BH mergers

Emits strong gravitational waves

  • SGR

May emit GW but weaker

IPN 3-sigma error region [Mazets et al., ApJ 680, 545]

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Example: Model Based Compact Binary Inspiral Search 070201 Exercise matched filtering techniques for inspiral waveform search No plausible gravitational waves identified Exclude compact binary progenitor with masses 1 M⊙ < m1< 3 M⊙ and 1 M⊙ < m2 < 40 M⊙ with D < 3.5 Mpc at 90% CL Exclude any compact binary progenitor in our simulation space at the distance of M31 at > 99% confidence level

DM31

25% 50% 75% 90%

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These do happen from time to time…

GRB 051103

Sky position error box overlaps with M81 group

~3.6 Mpc

(Frederiks et al 2006)

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Some GW+HEN source candidates

Short GRBs: HENs can also be emitted during binary mergers (Nakar 2007; Bloom et

  • al. 2007; Lee & Ramirez-Ruiz 2007). The ν flux is expected to be large enough for the

current generation of detectors. Prospects for detection in GW too. Low-Luminosity GRBs: Associated with particularly energetic population of core- collapse supernovae. Might also be strong neutrino emitters (Murase et al. 2006; Gupta & Zhang 2007; Wang et al. 2007). Expected event rate in the local volume is more than an order of magnitude larger than that of conventional long GRBs (Liang et al. 2007; Soderberg et al. 2006). ”Failed” GRBs: Associated with plausible baryon-rich jets. Optically thick, can be hidden from conventional astronomy, neutrinos and GWs might to be able to reveal their properties. Ando & Beacom (2005), Razzaque et al. 2004; Horiuchi & Ando 2008. Long GRBs: In the prompt and afterglow phases, high-energy neutrinos (105-1010 GeV) are expected to be produced by accelerated protons in relativistic shocks (e.g., Waxman & Bahcall 1997; Vietri 1998; Waxman 2000). Good prospects for detection in GW too.

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Likelihood Function for Spatial Overlap: LIGO + Virgo

LIGO+Virgo PSF IceCube 22 string PSF

LIGO + Virgo:

– Triple coincidence – Improved “point” spread function – Reduced coincident noise trigger rate

  • Y. Aso et al. APS'08 and

CQG 25, 114039, 2008 Pradier arXiv:0807.2567v1 and

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Astronomical Reach x10 better amplitude sensitivity ⇒ x1000 rate=(reach)3 ⇒ 1 year of Initial LIGO

< 1 day of Advanced LIGO !

Circular Inspirals: ~20 / year (Kalogera et al. 2006) Eccentric Encounters:~ several / year (O’Leary, Kocsis, Loeb 2008)

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Far-Future Detectors – Rule of Thumb?

Data is courtesy of VIRGO and the LIGO Scientific Collaboration.

~ × 10 @ ~100 Hz

Einstein Telescope Gravitational Wave observatory (planned)

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Far-Future Detectors – Rule of Thumb?

y 5Gpc

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Unmodelled GW burst (rough) examples EGWiso ~1046 erg SGR giant flares M31 GC

  • Astrophys. J. 681 (2008) 1419 and arXiv:0808.2050

Based on Gareth Jones’ ILIAS slide.

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ET Reach for SGRs

Minimum energy in gravitational waves detectable by ET as a function of frequency for an SGR source. This limit assumes isotropic and narrowband GW emission.

GF

10-7!

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Unmodelled GW burst (rough) examples EGWiso~O(9x1052) erg Merger phase of compact body coalescence z=1

Based on Gareth Jones’ ILIAS slide.

Ott (2008) arXiv:0809.0695

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This is great exploratory science !

  • There is a bold effort underway to get a new view of the universe
  • Initial LIGO has reached its design sensitivity

– Several astrophysically interesting results are out from S5

฀ SGR1806-20 ฀ GRB070201 ฀ Crab-spindown ฀ and others to come…

  • Active data sharing collaboration with VIRGO
  • Enhanced LIGO is here
  • Advanced LIGO is around the corner… the excitement is high!
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LIGO Scientific Collaboration

l Australian Consortium for Interferometric Gravitational Astronomy l The Univ. of Adelaide l Andrews University l The Australian National Univ. l The University of Birmingham l California Inst. of Technology l Cardiff University l Carleton College l Charles Sturt Univ. l Columbia University l CSU Fullerton l Embry Riddle Aeronautical Univ. l Eötvös Loránd University l University of Florida l German/British Collaboration for the Detection of Gravitational Waves l University of Glasgow l Goddard Space Flight Center l Leibniz Universität Hannover l Hobart & William Smith Colleges l Inst. of Applied Physics of the Russian Academy of Sciences l Polish Academy of Sciences l India Inter-University Centre for Astronomy and Astrophysics l Louisiana State University l Louisiana Tech University l Loyola University New Orleans l University of Maryland l Max Planck Institute for Gravitational Physics l University of Michigan l University of Minnesota l The University of Mississippi l Massachusetts Inst. of Technology l Monash University l Montana State University l Moscow State University l National Astronomical Observatory

  • f Japan

l Northwestern University l University of Oregon l Pennsylvania State University l Rochester Inst. of Technology l Rutherford Appleton Lab l University of Rochester l San Jose State University l Univ. of Sannio at Benevento, and Univ. of Salerno l University of Sheffield l University of Southampton l Southeastern Louisiana Univ. l Southern Univ. and A&M College l Stanford University l University of Strathclyde l Syracuse University l Univ. of Texas at Austin l Univ. of Texas at Brownsville l Trinity University l Tsinghua University l Universitat de les Illes Balears l Univ. of Massachusetts Amherst l University of Western Australia l Univ. of Wisconsin-Milwaukee l Washington State University l University of Washington