Edo Berger (Harvard CfA) Eliot Quataert, Siva Darbha, Dan Kasen, & Daniel Perley (UC Berkeley) Almudena Arcones (U Basel) & Gabriel Martinez-Pinedo (GSI, Darmstadt) Brian Metzger EM Counterparts of Neutron Star EM Counterparts of Neutron Star Binary Mergers and their Detection in Binary Mergers and their Detection in the Era of Advanced LIGO the Era of Advanced LIGO In Collaboration In Collaboration with: with: Princeton University NASA Einstein Fellow LIGO Open Data Workshop, Livingston, LA, LIGO Open Data Workshop, Livingston, LA, October 27, 2011 October 27, 2011
21
Embed
Edo Berger (Harvard CfA) Eliot Quataert, Siva Darbha, Dan Kasen, & Daniel Perley (UC Berkeley)
EM Counterparts of Neutron Star Binary Mergers and their Detection in the Era of Advanced LIGO. Brian Metzger. Princeton University NASA Einstein Fellow. In Collaboration with:. Edo Berger (Harvard CfA) Eliot Quataert, Siva Darbha, Dan Kasen, & Daniel Perley (UC Berkeley) - PowerPoint PPT Presentation
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
Edo Berger (Harvard CfA)
Eliot Quataert, Siva Darbha, Dan Kasen, & Daniel Perley (UC Berkeley)
Almudena Arcones (U Basel) & Gabriel Martinez-Pinedo (GSI, Darmstadt)
Brian Metzger
EM Counterparts of Neutron Star Binary EM Counterparts of Neutron Star Binary Mergers and their Detection in the Era of Mergers and their Detection in the Era of
Advanced LIGOAdvanced LIGO
In Collaboration with:In Collaboration with:
Princeton University NASA Einstein Fellow
LIGO Open Data Workshop, Livingston, LA, October 27, LIGO Open Data Workshop, Livingston, LA, October 27, 20112011
Electromagnetic Counterparts of NS-NS/NS-BH Mergers
Importance of EM Detection: Astrophysical Context (e.g. Identify Host Galaxy & Environment)
Peak Brightness MPeak Brightness MVV= -15 @ t ~ 1 day for M= -15 @ t ~ 1 day for Mejej = 10 = 10-2-2 M M
Monte Carlo Radiative Transfer Monte Carlo Radiative Transfer (SEDONA; Kasen et al. 2006)(SEDONA; Kasen et al. 2006)
CAVEAT: Fe composition assumed for opacity CAVEAT: Fe composition assumed for opacity
What What doesdoes a pure r-process photosphere look like? a pure r-process photosphere look like?
““kilo-nova”kilo-nova”
Metzg
er et al. 2010
Far Off Axis (obsobs = 4jj ) - The Kilonova is Isotropic
jjobs
Range of kilonova models w different ejecta mass Mej ~10-3 - 0.1 M and velocity v ~ 0.1-0.3 c
Detection requires depth r ~ 22-24 and cadence <~ 1 day (standard LSST 4-day survey not sufficient)
GRB 080503: Candidate Kilonova
(Perley, BDM et al. 2009)
Best-Fit Kilonova Parameters: v ~ 0.1 c, Mej ~ few 10-2 M , z ~ 0.1
z = 0.561z = 0.561
Where’s the Host Where’s the Host Galaxy?Galaxy?
Optical Rebrightening @ t ~ 1 day
ConclusionsConclusions Direct detection of gravitational waves is expected within the next Direct detection of gravitational waves is expected within the next >~5 years, but maximizing the science return requires identifying >~5 years, but maximizing the science return requires identifying and localizing an EM counterpart. and localizing an EM counterpart.
Short GRBs are detectable & identifiable, but are limited to <~ 1 Short GRBs are detectable & identifiable, but are limited to <~ 1 detection yrdetection yr-1-1 and may not provide localization. These rare and may not provide localization. These rare detections are nevertheless crucial, so an operational detections are nevertheless crucial, so an operational -ray satellite -ray satellite similar to Fermi GBM is important.similar to Fermi GBM is important.
No optical or radio facilities can provide all-sky coverage at a No optical or radio facilities can provide all-sky coverage at a cadence and depth matched to the expected counterpart light cadence and depth matched to the expected counterpart light curves curves targeted follow-up is required. targeted follow-up is required.
Optical afterglow emission is easily detectable for on-axis events Optical afterglow emission is easily detectable for on-axis events with rapid follow-up. However, off-axis optical afterglows are only with rapid follow-up. However, off-axis optical afterglows are only detectable for detectable for obsobs < 2 < 2 j j (even with LSST) (even with LSST) and hence are limited to and hence are limited to <~ 10% of all mergers.<~ 10% of all mergers.
Radio afterglow emission is isotropic, but existing and planned are Radio afterglow emission is isotropic, but existing and planned are not sufficiently sensitive, given the low Enot sufficiently sensitive, given the low Ejetjet/n from existing SGRB /n from existing SGRB afterglows.afterglows.
Isotropic kilonovae are in principle detectable for most events, but Isotropic kilonovae are in principle detectable for most events, but require a follow-up telescope with sensitivity similar to Pan-require a follow-up telescope with sensitivity similar to Pan-STARRs/LSST and a short cadence.STARRs/LSST and a short cadence.
This is going to be hard, so we need to start planning now! This is going to be hard, so we need to start planning now!
Zhang & MacFadyen 2009Zhang & MacFadyen 2009
Gamma-Ray Burst “Afterglows” - Synchrotron Emission Gamma-Ray Burst “Afterglows” - Synchrotron Emission from Shock Interaction with the Circumburst Mediumfrom Shock Interaction with the Circumburst Medium