joint gravitational wave - gamma-ray burst detection...
TRANSCRIPT
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Image provided by the Max Planck Institute for Gravitational Physics/Zuse Institute Berlin Eric Howell
Joint gravitational wave - gamma-ray burst detection rates
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Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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EM observations of GRB170817A sGRB detection rates
sGRB/GW detection rates
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GW170817/GRB170817A
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GRB 170817A Luminosity
Swift data
• Distance: 42.5 Mpc (2nd closest GRB – GRB980425)
• Peak Flux: 3.6 +/- 1.1 ph s-1cm-2 [median 7.3 ph s-1cm-2 ]
• Luminosity: 1.4x1047 erg/s [average 1052 erg s-1]
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Structured jet
Top hat: constant emission and lorentz factor across jet
Structured jet: luminosity per solid angle decreases smoothly outside a narrow ultra-relativistic core
A structured jet is a by product of a successful jet penetrating a cocoon (Lazzati et al 2017, Gottlieb 2017, Alexander 2018)
2 popular profiles - Power law or Gaussian
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Structured jet profiles from EM observations
Take parameters from late time EM observations and convert to prompt phase
Fermi prompt observed Eiso
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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VLBI observations (HAS, VLBA, VLA, GBT)
Mooley et al, Nature 2018 constrained the evolution in size, shape, position of GW170817 and identified superluminal motion with milli-arcsec resolution
Observations (> 150 days) supported successful jet breakout
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EM observations of GRB170817A sGRB detection rates
sGRB/GW detection rates
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Infer structured jet profile Assume a Gaussian jet profile with observationally motivated priors
θCORE – Uniform prior
LCORE – Can take a Lognormal distribution around the average sGRB Luminosity as a prior
θVIEW – Gaussian prior based on Mooley et al (15-25 deg) Likelihood function - a lognormal distribution based on the observed luminosity of GRB170817
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θCORE – 4.7 deg LCORE – 1 X 1052 erg s-1 θVIEW – 21 deg
Fold this angular dependence into the Fermi detection efficiency
Inferred GRB170817A structured jet profile
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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The GRB efficiency function assuming a structured jet
Solid line – structured jet Dashed line – top-hat model
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
Viewing angle – distance relation for a GRB170817A-like structured jet profile
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The Fermi detection rate
Fold GRB efficiency function with BNS rate evolution Predicts around 40/yr detections in line with Fermi observations
BNS intrinsic rate Fermi sGRB detection rate
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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EM observations of GRB170817 sGRB detection rates
sGRB/GW detection rates
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BNS rate evolution model
GW BNS detection rate - fold a GW detection efficiency model into a BNS source rate evolution model
Detection efficiency model based on the projection parameter of Finn & Chernoff 1993
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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Future BNS detection rates
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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O3a BNS candidates
0
5
10
15
20
25
BNS NSBH BBH
2 Probability >90%
CANDIDATE PROBABILITY DISTANCE/NETWORK
SKYMAP
190910h BNS (61%), Terrestrial (39%)
230 ± 80 L1
190901ap BNS (86%), Terrestrial (14%)
241 ± 79 L1, V1
190718y Terrestrial (98%), BNS (2%)
227 ± 165 H1,L1,V1
S190510g Terrestrial (58%), BNS (42%)
227 ± 92 H1,L1,V1
S190426c BNS (49%), MassGap (24%), Terrestrial (14%), NSBH (13%)
377 ± 100 H1,L1,V1
190424z BNS (>99%) 157 ± 41 L1, V1
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Future joint sGRB-BNS rates
O3 Observation run 2019-20 Detection range = 120 Mpc Rate = 0.2-1.8(0.6) yr-1
A+ Observation run 2023-26 Detection range = 325Mpc (z=0.07) Rate = 0.7-9.1 (3.2) yr-1
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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Projected joint GW/sGRB event rates
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
Bottom row – percentage of BNS with a sGRB counterpart
As GW range increases – events viewed at wider opening angles more difficult to detect – GRB detector sensitivity critical
A higher percentage BNS with sGRB counterparts will be face-on as GW sensitivity increases
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Conclusions
Inferred a structured jet profile for GRB170817A
Calculated sGRB efficiency curve for Fermi that agrees with observations
Provided Fermi and Joint GW/sGRB detection rates for O3 and beyond
The percentage of BNS with sGRBs counterparts decrease with GW detector sensitivity
Sensitivity of future GRB satellites will be critical
See Future Survey Missions on Tuesday [15:35-17:35]
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BNS rate evolution model
Star formation rate – Madau & Dickinson (2014)
Delay time distribution – P(td) ∝ 1/td ;20 Myr min
Flat Λ cosmology: Ω𝑀=0.31, ΩΛ =0.69, H0=67.8 km s-1Mpc-1 (Planck Collab et al. 2015)
BNS rates – Abbott et al, 2017
1680 Gpc-3 yr -1
Assume that all BNSs can produce a sGRB
+3050 -1310
Howell, Ackley et al 2018 in prep
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Projected joint event rates – events close to jet axis
Howell, Ackley, Rowlinson et al 2018 in prep
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Future BNS detection ranges
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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The GRB efficiency function
Selection function for a top hat jet
Selection function for a structured jet
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θCORE – 4.7 deg LCORE – 1 X 1052 erg s-1 θVIEW – 21 deg
Fold this angular dependence into the Fermi detection efficiency
Inferred GRB170817A structured jet profile
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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ETD – Theseus Joint GW/sGRB rate
THESEUS mission (2026 – 2029) selected with 2 other missions for "phase A" and is under evaluation by ESA. Unique combinations of instruments: Soft X-ray imager SXI – 0.3 – 6 keV 1sr FoV and 1-2 arcsec localisation IR Telescope IRT – 0.7m class 10x10 arcmin FoV (imaging + spectroscopic capabilities) X/Gamma Ray XGIS– instruments covering range 2 – 20 MeV, FoV 2pi sr > 150 keV
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Projected joint event rates
At increased GW detection ranges, GRB emissions from wider opening angles will be more difficult to detect
Howell, Ackley, Rowlinson & Coward, 2019, MNRAS, 485, 1435
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EXTRA SLIDES
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Future BNS detection rates
O3 Observation run 2019-20 Detection range = 120 Mpc Rate = 1-16 (6) yr-1
A+ Observation run 2023-26 Detection range = 325 (z=0.07) Rate = 31-394 (140) yr-1
Howell et al, 2018 astro-ph: 1811.09168
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GW detections looking ahead
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ETD – Theseus Joint GW/sGRB rate
Theseus sGRB rate : 146.15 ^{+265.33}_{-113.96} Theseus + ETD rate : 47.15 ^{+85.60}_{-36.77} Theseus + CE rate : 67.78 ^{+123.05}_{-52.85}
THESEUS mission (2026 – 2029) selected with 2 other missions for "phase A" and is under evaluation by ESA.
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Swift early Follow-up Swift FoV was occulted by earth at time of Fermi-GBM trigger After 1h XRT imaged 90% of GW skymap – no bright sources 12h Swope reported NGC 4993 – no XRT detection
Delayed onset of X-ray (9 days) and Radio (15 days) strongly we were viewing from a wide angle (not an on-axis jet)
VLA ruled out a slightly off-axis jet
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𝝋(𝑳) 𝝋(𝑳)
𝑳 𝑳 𝑳min 𝑳min
The GRB efficiency function Given a flux limit FL there is a limiting accessible luminosity as a function of redshift Lmin(FL, z) Integrate over the luminosity function to determine the detectable fraction of sources – the efficiency (selection) function
Increasing redshift, z
This model works for a top hat jet
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𝝋(𝑳) 𝝋(𝑳)
𝑳 𝑳 𝑳min 𝑳min
The GRB efficiency function
Increasing redshift, z
For a structured jet profile there is also an angular dependence with redshift Lmin(FL, z, 𝜽)
low z : emissions from wider angles are more likely higher z: only see emissions from nearer the core
We need L(𝜽) angular dependence on luminosity
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GRB X-ray Plateaus and GWs
X-ray plateaus (60% SGRBs)
Rowlinson 2010, 2013
Long lived GW emission? Corsi & Meszaros 2009
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Projected joint event rates Epoch Detection range/
Horizon BNS Detection rate (yr-1)
BNS+sGRB/ yr On-axes / yr
O3 (2019-20)
117 Mpc 270 Mpc
1-16 (6) 0.2-1.8(0.6) 0.05-0.6 (0.2)
Design (2021-)
173 Mpc 413 Mpc; z~0.1
4-55 (20) 0.3-3.7 (1.3) 0.1-1.3 (0.5)
A+ (2023-2026)
325 Mpc 843 Mpc; z~0.17
31-394 (140) 0.7-9.1 (3.2) 0.3-3.6 (1.3)
Voyager (2.5G) 2027-2030
736 Mpc; z~0.15 2.4Gpc; z~0.4
438-5598(1988) 1.7-22.0(7.8) 0.8-10.5 (3.7)
Structured jet profiles increase number over top hat The BNS/GW detection fraction limited by Fermi as GW
ranges increase Kilonova and late EM searches for most BNS Fermi will be running sub-threshold pipelines
<- Top hat
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Gamma-ray bursts (GRBs))
10keV-GeV photons
1051-1054 ergs in few seconds
γ-rays - ultra-relativistic energy flow converted to radiation
lon
g-so
ft L
GR
B
sh
ort
-har
d S
GR
B
>2s
< 2
s
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1. Off-axes cocoon model
Matter ejected into circum-merger medium (UVOIR evidence)
Jet drills through ejector it converts fraction of its energy to matter enveloping the jet.
Inflates forming a hot mildly relativistic (Γ ~2-3 ) expanding cocoon
Narrow jet (~10o)- drills out leaving a fraction of energy in the cocoon Wide jet (~30o)- - choked and deposits all energy in cocoon Both scenarios predict weak gamma ray emission over wide opening angles.
[Gottlieb et al. 2017a,b, Nakar et al. 2017, Lazzati et al, 2017a,b, Bromberg et al. 2017]
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Comparison to other models of GRB170817A structured jet
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Comparison to other models of GRB170817A structured jet
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Comparison to other models of GRB170817A structured jet
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Talk outline
Key EM prompt and follow-up observations
Infer a structured jet profile for GRB170817A
Produce a model for BNS source rate evolution and
Detection rate for future GW IFO upgrades
Calculate sGRB efficiency curve for Fermi and calculate
Fermi sGRB detection rate (cross check)
Fermi and Joint GW/sGRB detection rates – the percentage of BNS with sGRBs counterparts decrease as GW detectors become more sensitive
Look at 3G era
• See also complementary study led by • Nihar Gupte, Imre Bartos on DCC
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Joint GW/sGRB detection rate
Assume Fermi GBM
All BNS can have associated sGRBs
BNS source rate evolution O2 BNS rate and standard assumptions
BNS detections - fold in GW BNS efficiency curves
Fermi and Joint GW/sGRB detection rates - fold in a Fermi detection efficiency curve (based on wide angled emissions suggested by EM observations of GRB170817)
• See also complementary study led by • Nihar Gupte, Imre Bartos on DCC
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VLBI observations (HAS, VLBA, VLA, GBT)
Mooley et al, Nature 2018 constrained the evolution in size, shape, position of GW170817 and identified superluminal motion with milli-arcsec resolution
Observations (> 150 days) suggest successful jet breakout from a cocoon (consistent with structured jet model)
Choked jet cocoon scenario produces a shallower decay
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The angular dependence on maximum detection distance
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BNS rate to Fermi sGRB rate (assuming top hat)
Joint on-axis GW-BNS detection rate - fold a GRB detection efficiency model, FoV, DC etc
Howell, Ackley, Rowlinson et al 2018 in prep
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Projected joint event rates 3G
Assuming 2G DRB detector (Fermi) – some instrument like Theseus (G. Stratta et al 2018) would be better
ETD - 19.62 ^{+35.62}_-15.30} /yr
CE - 22.39 ^{+40.64}_{-17.46} /yr
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Late time radio observations of off-axes emissions
Lazzati et al, 2018
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Cocoon (choked jet)/structured jet scenarios can be discriminated by late observations
indistinguishable until the peak time (~ 200-300 days) post-peak slopes are expected to differ – i.e. cocoon will have a shallower decay than jet models
Troja et al. 2018 (astro-ph:1801.06516 )
3 GHz
5keV
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Fermi detection distance to SJ model
Less extreme Lazzati 2017 cocoon-jet breakout model (dashed) consistent with low θv edge up to around θv =20
Howell, Ackley et al 2018 in prep
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On-axes low-luminosity burst
A dimmer LF lower limit requires a rate increase of 100 For consistency with the O2 BNS rate upper limit
requires an average on-axis beaming angle of > 24 deg sGRB Sample with observed jet breaks [3 – 8]deg
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This scenario is disfavoured by the geometry Steep drop-off suggests low-probability Similar scenario exists when considering Epeak
GRB observed slightly off-axis
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GBM: keV-30 MeV; 70% sky
LAT: 0.02-300 GeV ; 20% sky; 240 GRBs/yr (40s sGRBs) >10GeV photons detected
BAT: 15-150 KeV; 10% sky
XRT: arc min localisation >1000 GRBs (13% sGRBs) > 200 redshifts
Satellites for GW/GRB coincidence detection
Fermi
(2008-)
Swift
(late 2004-)
INTEGRAL
(2002-)
IBIS (Imager) ; 15keV-10MeV SPI (Spectrometer) SPI-ACS (AntiCoincidence Shield) surrounds SPI
75–2000 keV; all sky > 75 keV; 20 sGRBs/yr
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Multimessenger pathways and end products
Chu, Howell, Rowlinson et al., MNRAS, 2015
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Multimessenger Pathways associated with NS mergers
Chu, Howell, Rowlinson et al., MNRAS, 2015
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GRB170817 with Theseus
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SNR scaling
Scale SNR for untriggered against triggered using sky region and observation duration (P B. Patricelli et al 2016)
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EM observations of GRB170817 BNS detection Rates sGRB detection rates
sGRB/GW detection rates
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EM observations of GRB170817 BNS detection Rates sGRB detection rates
sGRB/GW detection rates