Searching for Electromagnetic Counterparts of Gravitational-Wave Transients
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Transcript of Searching for Electromagnetic Counterparts of Gravitational-Wave Transients
Searching for Electromagnetic Counterparts of Gravitational-Wave Transients
Marica Branchesi (Università di Urbino/INFN)on behalf of
LIGO Scientific Collaboration and Virgo Collaboration&
Alain Klotz (TAROT telescope) Myrtille Laas-Bourez (Zadko telescope)
DCC: G1100079
A goal of LIGO and Virgo interferometers is the first direct detection of gravitational waves from ENERGETIC ASTROPHYSICAL events:
Mergers of NeutronStars and/or BlackHoles SHORT GRB Kilonovas
Core Collapse of Massive Stars Supernovae LONG GRB
Cosmic String Cusps EM burst
Main motivations for joint GW/EM observations:
Increase the GW detection confidence;
Get a precise (arcsecond) localization, identify host galaxy;
Provide insight into the progenitor physics;
In the long term start a joint GW/EM cosmology.1
Low-latency GW data analysis pipelines allow the use of GW triggers in real time to obtain prompt EM observations
and to search for EM counterparts
The first program of EM follow-up to GW candidates has been performed during two LIGO/Virgo observing periods:
Dec 17 2009 to Jan 8 2010 – Winter RunSep 4 to Oct 20 2010 – Summer Run
The EM-follow-up program in S6-VSR2/3 is a milestone towards advanced detectors era where the chances of GW detections are very enhanced
Presentation Highlights:
Methods followed to obtain low-latency Target of Opportunity EM follow-up observations;
Development of image analysis procedures able to identify the EM counterparts.
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GW Online AnalysisH1 L1 V1
Omega & cWB MBTA for Unmodeled Bursts for signals from Compact Binary Coalescence
GRACE DBARCHIVE
LUMIN GEMfor Optical Telescopes for Swift
Event Validation
• Search algorithms to identify triggers
Send alert to telescope
• Select Statistically Significant Triggers• Determine Pointing Locations10 min.
30 min.
• LIGO (H1 and L1) and Virgo (V1) interferometers
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Requirements to select a trigger as a candidate for the EM follow-up:• Triple coincidence among the three detectors;
• Power above a threshold estimated from the distribution of background events: Target False Alarm Rate Winter Run < 1.00 event per Day
Summer Run < 0.25 event per Day for most of optical facilities < 0.10 event per Day for PTF and Swift
GW Source Sky Localization: signals near threshold localized to regions of tens of square degrees possibly in several disconnected patches
Necessity of wide field of view telescopes
LIGO/Virgo horizon: a stellarmass BH/ NS binary inspiral detected out to 50 Mpc distance that includes thousands of galaxies GW observable sources are likely to be extragalactic Limit regions to observe to Globular Clusters and Galaxies within 50 Mpc
(GWGC catalog White et al. 2011)
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Nearby galaxies and globular clusters (< 50 Mpc) are weighted to select the most probable host of a GW trigger:
• Black crosses nearby galaxies locations
• Rectangles pointing telescope fields chosen to maximize chance to detect the EM counterpart
Mass * LikelihoodP = Distance
Probability Skymap for a simulated GW event
• Likelihood based on GW data• Mass and Distance of the galaxy or the globular cluster
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Observed on-axis LONG and SHORT GRB afterglows peak few minutes after the EM/GW prompt emission
Kilonova model afterglow peaks about a day after the GW event
To discriminate the possible EM counterpart from contaminating transients
The expected EM counterpart afterglows guide observation schedule time
Metzger et al.(2010), MNRAS, 406..265
Kann et al. 2010, ApJ, 720.1513Kann et arXiv:0804.1959
KILONOVASRadioactively Powered EM-transient
LONG/SOFT GRBMassive star Progenitors
SHORT/HARD GRB Compact Object mergers
EM observations as soon as possible after the GW trigger validation
EM observations a day after the GW trigger validation
repeated observations over several nights to study the light curve
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R m
agni
tude
ass
umin
g z=
1
R m
agni
tude
ass
umin
g z=
1
Time (days after burst in the observer frame)Time (days after burst in the observer frame)Time (Days)
Lum
inos
ity (e
rgs
s-1)
Metzger et al.(2010), MNRAS, 406..265
Ground-based and space EM facilities observing the sky at Optical, X-ray and Radio wavelengths involved in the follow-up program
TAROT SOUTH/NORTH1.86° X 1.86° FOV Zadko 25 X 25 arcmin FOV ROTSE1.85 ° X 1.85° FOV QUEST 9.4 square degree FOV
SkyMapper5.6 square degree FOVPi of the Sky20° X 20° FOVPalomar Transient Factory7.8 square degree FOVLiverpool telescope4.6 X 4.6 arcmin FOV
Optical Telescopes
Swift Satellite 0.4° X 0.4° FOV
X-ray and UV/Optical Telescope
Radio Interferometer
LOFAR10 – 250 MHz
Winter/Summer Run
Only Summer Run
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Observations Performed with Optical Telescopes:
Winter run 8 candidate GW triggers, 4 observed by telescopes
Summer run 6 candidate GW triggers, 4 observed by telescopes
Analysis Procedure for Wide Field Optical Images
Limited Sky localization of GW interferometers
Wide field of view optical images
Requires to develop specific methods to detect
the Optical Transient Counterpart of the GW trigger
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LIGO/Virgo collaborations are actually testing and developing several Image Analysis Techniques
based on:
• Image Subtraction Methods (for Palomar Transient Factory, ROTSE and SkyMapper)
• Catalog Cross-Check Methods (for TAROT, Zadko, QUEST and Pi of the Sky)
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The rest of the talk focuses on a Catalog-based Detection Pipeline
under development for TAROT and Zadko:methodology and preliminary results obtained using
images with simulated transients
Catalog-based Detection Pipeline for images taken by TAROT and Zadko telescopes
TAROT South/North• 0.25 meter telescope• FOV 1.86° X 1.86° • Single Field Observation of 180 s exposure• Red limiting magnitude of 17.5
Zadko• 1 meter telescope• FOV 25 X 25 arcmin • Five Fields Observation of 120 s exposure• Red limiting magnitude of 20.5
Afterglow Light Curves (source distance d=50 Mpc)
Time (days)
App
aren
t Red
mag
nitu
de
LONG GRB
SHORT GRB
KILONOVA
TAROT limiting magnitudeZadko limiting magnitude
“Afterglow light curves” for LONG/SHORT and
Kilonova transients at a distance of 50 Mpc
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detect sources in each image
select“unknown objects”
(not in USNO2A)
Catalog-based Detection Pipeline to identify the Optical Counterparts in TAROT and Zadko images
SExtractor to build catalog of all the objects visible in each image
Match Algorithm (Valdes et al 1995; Droege et al 2006) to identify “known stars” in USNO2A (catalog of 5 billion stars down to R ≈ 19 mag)
select centralpart of
the imageFOV restricted to region with radius = 0.8 deg for TAROT and 0.19 deg for Zadko
avoid problemsat image edges
Magnitude consistency
to recover possible transients that
overlap with known galaxies/stars
Recover from the list of “known objects”: |USNO_mag – TAROT_mag| > 4σ
Octave Code
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search for objects in common to
several images
Spatial cross-positional check with match-radius of 10 arcsec for TAROT and 2 arcsec for Zadkochosen on the basis of position uncertainties
reject cosmic rays, noise, asteroids...
select objects in “on-source”
“On-source region” = regions occupied by Globular Clusters and Galaxies up to 50 Mpc (GWGC catalog, White et al 2011)
reject backgroundevents
“Light curve” analysis
reject “contaminatingobjects” (galaxy, variable stars, false transients..)
Possible Optical counterparts
…..Catalog-based Detection Pipeline
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“Light curve” analysis - cut based on the expected luminosity dimming of the EM counterparts
recall magnitude α [-2.5 log10 (Luminosity)]
expect Luminosity α [time- β] magnitude α [2.5 β log10(time)] slope index = measurement of (2.5 β) to discriminate expected light curve from “contaminating events”The expected slope index for SHORT/LONG GRB is around 2.7 and kilonova is around 3
Optical counterparts the ones with slope index > 0.5
Coloured points = Optical LGRB TransientsBlack squares = contaminating objects
Contaminating objects that could pass the cut are only variable AGN or Cepheid stars
Saturation effects
Red magnitudeA
DU
cou
nts
not saturatedsaturatedDis
tanc
e in
Mpc
Initial Red magnitude
Slop
e In
dex
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Image characterization - limiting magnitude
used a set of 10 test TAROT images (180 sec exposure)
limiting magnitude of 15.5 for all images
Image Limiting Magnitude: point where Differential/Integral Source Counts distribution (vs magnitude) bends and moves away from the power law of the reference USNOA
Differential Source Counts Integral Source Counts
R magnitudeR magnitude
Cou
nts(
0.5
mag
bin
)/sq
degr
ee
Cou
nts(
<mag
)/sq
degr
ee
+x x
+Limiting magnitudeLimiting magnitudeUSNOA countsUSNOA counts
TAROT image counts TAROT image counts
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Monte Carlo simulations at the Computing Center in Lyon:
Injections of fake transients modelled using on-axis GRB and Kilonova afterglow light curves
Time origin (time of GW trigger) set 1 day before the first imageSHORT/HARD GRB Kilonova Objects LONG/SOFT GRB
SGRB, LGRB intrinsic luminosity range parametrized by a magnitude offset 0 ÷ 8SGRB, LGRB: random offset 0 ÷ 8SGRB0, LGRB0: offset set to 0 SGRB8,LGRB8: offset set to 8
Preliminary results on Distance_50% horizon (Mpc):
SGRB SGRB0 SGRB8 LGRB LGRB0 LGRB8 Kilonova 15 100 ------ 400 2500 80 10
Simulations using different sets of images and different time schedule wrt the GW trigger give similar results
Preliminary tests on sensitivity : obtained by running the Detection Pipeline over images with injections of Fake Transients
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Effic
ienc
y
Effic
ienc
y
Distance (Mpc)Distance (Mpc)Distance (Mpc)
Effic
ienc
y
kilonovaSGRBSGRB0SGRB8
LGRBLGRB0LGRB8
Conclusions:
The first EM follow-ups to GW candidates have been performed by the LIGO/Virgo community in association with
several Partner EM Observatories
“EM counterpart Detection pipelines” based on different analysis techniques are under test and development
Preliminary results suggest that “Catalog-based Detection Pipeline” is able to detect on-axis GRB and Kilonova afterglows
for TAROT and Zadko images Efforts are in progress to improve the efficiency and to
extend the use to other telescope images
The analysis of the images observed during the Winter/Summer LIGO/Virgo run is on-going