1. Many thanks to the experimenters building the detectors!
Results and Challenges in Astrophysically Triggered Gravitational Wave Searches
TAMA
LIGO-G
VIRGO
LIGO Livingston
Swift/
HETE-2/
IPN/
INTEGRAL
RXTE/RHESSI
LIGO-LHO
LIGO-LLO
LIGO Hanford
*Title:* Results and Challenges in Astrophysically Triggered Gravitational Wave Searches
*Speaker:* Szabolcs Márka, Columbia University in the City of New York *Abstract:* Multimessenger astronomy, including gravitational waves, shall continue to be a fruitful path towards deciphering otherwise hidden aspects of the high-energy transient universe. Gamma-ray, X-ray, optical, radio and neutrino observations of cataclysmic cosmic events are often associated with plausible gravitational wave emission. Beyond strengthening our ability to discover gravitational waves, multimessenger observations can enhance the value of our results. They can enable us to draw conclusions that we would not be able with gravitational waves alone. I will review results of electromagnetically triggered searches, interpret their astrophysical consequences, and present an outlook on the future of triggered multimessenger astrophysics.
…………………………………………………………….
Image Credits:
#1:
LSC DCC: LIGO Z
------
#2:
Zsuzsa Marka
#3:
Image Credit:
M31 The Andromeda Galaxy
by Matthew T. Russell
Date Taken: 10/22/ /2/2005 Location: Black Forest, CO Equipment: RCOS 16" Ritchey-Chretien Bisque Paramoune ME AstroDon Series I Filters SBIG STL-11000M #4
NS-NS merger simulation
Credit: Daniel Price and Stephan Rosswog
@ New Scientist
GEO600,
Hannover, Germany
EM followup:
See talk by E. Katsavounidis!
Szabolcs Márka
Columbia University in the City of New York
LIGO Scientific Collaboration and the Virgo Collaboration
GWDAW 14, Roma, Italy, January 26-29, 2010

2. 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
Confident detection of GWs.
Better background rejection  Higher sensitivity to GW signals.
More information about the source/engine.
Measurements made possible through coincident detection.
GRBs: See talk by L.Piro/N. Gehrels!
See talk by E. Chassande-Mottin!
Swift/
HETE-2/
IPN/
INTEGRAL
RXTE/RHESSI
See talk by J. Camp!
LHO
See poster by K. Hayama!
LLO
Short GRBs: See talk by S. Kobayashi!
Image credit: Zsuzsa Marka – GWDAW12
IceCube: See talk by F. Halzen!
ANTARES: See talk by T. Pradier!

3. Soft Gamma Repeaters (SGRs)
See poster by Z. Marka!
[1] Ioka MNRAS 327, 639 (2001)
[2] Corsi & Owen, LIGO-T
VIR-NOT-ROM-028A-09
[3] Kalmus & Ott, LIGO-G
2.9x1045 erg
2.4x1048 erg
PRL 101, (2008)
Red diamondgiant flare; green starsstorms
Magnetar bursts 2004 thru 2009.
Bursts from 6 magnetars
SGR (discovered 2009)
likely 800 pc from Earth
EGW limits expected 10x lower than before
Numerical simulation work started [3]
Significant advance on the theoretical front
addressable predictions [1,2]

4. Detected by Konus-Wind, INTEGRAL, Swift, MESSENGER
EM Observations - GRB
Described as an
“intense short hard GRB” (GCN 6088)
Duration ~0.15 seconds,
followed by a weaker, softer pulse
with duration ~0.08 seconds
Detected by Konus-Wind, INTEGRAL, Swift, MESSENGER
1200
1000
800
600
400
200
R.A. = deg,
Dec = deg
[Cnt/2ms ]
Courtesy of Konus-Wind
Perley & Bloom 2007
IPN3 annulus intersects
spiral arms of the M31
Hurley et al. 2007, Pal’Shin 2007
refined error box, ≈ 1.1
from the center of M31 still overlaps with the spiral arms
Mazets et al. 2007
Final error box still overlaps M31
Time –To [ms]
Home Brew:
The error box:
Refs:
GCN:
Alex: /Inspiral:
“…The error box area is sq. deg. The center of the box is
1.1 degrees from the center of M31, and includes its spiral
arms. This lends support to the idea that this exceptionally
intense burst may have originated in that galaxy (Perley and
Bloom, GCN 6091)…” from GCN6013
----
M31 The Andromeda Galaxy
by Matthew T. Russell
Date Taken: 10/22/ /2/2005 Location: Black Forest, CO Equipment: RCOS 16" Ritchey-Chretien Bisque Paramoune ME AstroDon Series I Filters SBIG STL-11000M
Antenna responses of LIGO Hanford:

5. DM31≈770 kpc GRB 070201 – Sky Location Eiso ~ 1045 ergs
R.A. = deg, Dec = 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
Home Brew:
The error box:
Refs:
GCN:
Alex: /Inspiral:
“…The error box area is sq. deg. The center of the box is
1.1 degrees from the center of M31, and includes its spiral
arms. This lends support to the idea that this exceptionally
intense burst may have originated in that galaxy (Perley and
Bloom, GCN 6091)…” from GCN6013
----
M31 The Andromeda Galaxy
by Matthew T. Russell
Date Taken: 10/22/ /2/2005 Location: Black Forest, CO Equipment: RCOS 16" Ritchey-Chretien Bisque Paramoune ME AstroDon Series I Filters SBIG STL-11000M
Eiso ~ 1045 ergs
if at M31 distance
(more similar to SGR than GRB energy)
IPN 3-sigma error region [Mazets et al., ApJ 680, 545]

6. Model Based Compact Binary Inspiral Search 070201
Exercise matched filtering techniques for inspiral waveform search
No plausible gravitational waves identified
25%
50%
75%
90%
DM31
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
Paper states: “As a reference
point, a compact binary progenitor with masses 1 M⊙ <
m1 < 3 M⊙ and 1 M⊙ < m2 < 4 M⊙ with D < 3.5 Mpc is excluded
at 90%confidence”
and
“exclude any compact binary
progenitor in our simulation space at the distance of M31 at
the > 99% level.”
Abbott, B. et al. (2008), Astrophysical Journal, pp

7. GRB 051103 ~3.6 Mpc These do happen from time to time…
Sky position error box overlaps with
M81 group
~3.6 Mpc
(Frederiks et al 2006)

8. Search for Gamma-Ray Bursts during S5/VSR1
On-source time searched for GW
Inspirals: See talk by A. Dietz ! arXiv:
Data:
Off-source time used to estimate background
Histogram of lower limits on source distances ( EGW L 0.01 MA )
137 GRBs in the X-Pipeline analysis
derived from the observed GW energy limits
Simulated GW signals
Strong Noise Glitches
E Incoherent
Region eliminated by cut (below dashed line)
Noise Glitches
arXiv:
E Null

9. Far-Future Detectors – Rule of Thumb?
Data is courtesy of VIRGO and the LIGO Scientific Collaboration.
~  ~100 Hz

10. Far-Future Detectors – Rule of Thumb?
y5Gpc

11. Unmodelled GW burst (rough) examplesGC
Astrophys. J. 681 (2008) 1419 and arXiv:
EGWiso ~1046 erg
SGR giant flares and core collapse SN
Based on Gareth Jones’ ILIAS slide.

12. 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.
ET Reach for SGRs GF
10-7!
GRG paper excerpt: LIGO has placed upper limits [2,3,5] onGWemission by SGRs in the range 1046¡1050
erg, depending on frequency, and assuming a nominal source distance of 10 kpc. Typical
LIGO limits in the 1-3 kHz range, expected for f modes, are 10^49 -10^50 erg.
Figure 2 shows the sensitivity of ET to an SGR source at a distance of 10 kpc (a typical
galactic distance) and 0.8 kpc (the estimated distance to SGR [21,47,81]). At
f-mode frequencies ET will be sensitive to GW emissions as low as 10^43 erg, or about 0.01-
1% of the energy content in the EM emission in a giant flare. In the region of Hz,
ET will be able to probe emissions as low as 10^40 erg, i.e. as little as 10^-7 of the total energy
budget.

13. Supernovae and ET?
The upper plot displays the minimum GW energy that a supernova core collapse is required to radiate
in order to be detectable by the Einstein telescope. We give two estimates obtained from Eq. (1) assuming
a GW signature with a low frequency content f = 100 Hz and high frequency content f = 1 kHz. This
quantity is given as a function of the source distance. We also indicate the expected range of radiated GW
energy for several processes [104]. The lower plot shows an estimate of the cumulative event rate (with error
bars) obtained from the star formation rate computed over a catalog of nearby galaxies [14].

14. Low-Energy Neutrinos from Supernovae
The core collapse of a massive star produces an O(~10 s) long pulse of low-energy neutrinos and antineutrinos, amounting to a total energy release of up to ~1053 ergs.
~5 Mt proposed Deep-TITAND neutrino detector:
N ~1 reach is about ~8 Mpc.
Supernova rate estimate can be as large as 1 / yr
Reasonable to expect
~one such event during the lifetime of ET.
Significant uncertainties exist though

15. Unmodelled GW burst (rough) examples
z=1
EGWiso~O(9x1052) erg
Merger phase of compact body coalescence
Ott (2008) arXiv:
Based on Gareth Jones’ ILIAS slide.

16. Great and Energetic Exploratory Science !
There is a bold effort underway to get a new view of the universe
Results published
SGR
GRB070201
S5/VSR1 GRBs
and others …
Advanced Virgo and LIGO are around the corner…
ET is being defined…
… the excitement is high!
Please don’t miss the other multimessenger talks/posters on GWDAW14!