Short GRBs: Progenitors, r-process Nucleosynthesis, and Gravitational Waves. Edo Berger Harvard University
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1 Short GRBs: Progenitors, r-process Nucleosynthesis, and Gravitational Waves Edo Berger Harvard University GWPAW 2015 Osaka, Japan June 2015
2 Objectives Berger 2014 Annual Reviews of Astronomy & Astrophysics, 52, 43
3 Objectives Determine the explosion and environmental properties of short GRBs Test the association of short GRBs with compact object binary mergers (NS-NS / NS-BH) If established, use the properties of short GRBs to study the electromagnetic counterparts of gravitational wave sources. Berger 2014 Annual Reviews of Astronomy & Astrophysics, 52, 43
4 The Harvard GRB Program
5 The Harvard GRB Program
6 The Harvard GRB Program
7 The Harvard GRB Program Graduate Students: Kate Alexander Peter Blanchard Philip Cowperthwaite Ian Czekala Maria Drout Margaret McLean George Miller Ashley Villar Wen-fai Fong (Einstein Fellow at Univ of Arizon) Tanmoy Laskar (Jansky Fellow at UC Berkeley) Ragnhild Lunnan (Postdoc at Caltech/Stockholm) Philip Cowperthwaite GW/EM counterparts Wen-fai Fong Short GRBs Postdoctoral Fellows: Raffaella Margutti Matthew Nicholl Peter Williams Ashley Zauderer (at Templeton) Ryan Chornock (Asst. Prof. at Ohio Univ) Ryan Foley (Asst. Prof. Univ of Illinois) Undergraduate Students: Melissa McIntosh Benjamin Cook (CfA) Natania Wolansky Caroline Huang (JHU) Tova Holmes (UCB) Camille Leibler (UCSC) Isaac Shivvers (UCB) Meredith MacGregor (CfA) Ethan Kruse (UW) Jordan Bock
8 Compact Object Merger Predictions
9 Compact Object Merger Predictions
10 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts
11 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types
12 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities
13 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis
14 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
15 Lack of Supernova Associations Hjorth et al. 2005
16 Lack of Supernova Associations EB Hjorth et al. 2005
17 Lack of Supernova Associations EB Hjorth et al Nearly all in star forming galaxies
18 Elliptical Host Galaxies
19 Elliptical Host Galaxies B EB et al z = z = Castro-Tirado et al. 2005; Gehrels et al. 2005; Hjorth et al. 2005; Bloom et al. 2006; Prochaska et al z = Fong et al A
20 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
21 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
22 Host Galaxy Demographics Progenitors that only track stellar mass (older than ~Gyr) should be 1:1 in star-forming and elliptical galaxies
23 Host Galaxy Demographics Progenitors that only track stellar mass (older than ~Gyr) should be 1:1 in star-forming and elliptical galaxies Both stellar mass and star formation influence the short GRB rate: P(τ) τ 1 Fong et al. 2013
24 Host Galaxy Demographics Progenitors that only track stellar mass (older than ~Gyr) should be 1:1 in star-forming and elliptical galaxies Leibler & EB 2010 Both stellar mass and star formation influence the short GRB rate: P(τ) τ 1 Fong et al Elliptical hosts track stellar mass, but star-forming hosts have lower than expected masses RSF ~ 3 REll per unit mass
25 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
26 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
27 Locations Within/Around Host Galaxies
28 Host-Less Short GRBs HST/ACS/F606W 2 EB 2010 ~25% of short GRBs with optical afterglows have no obvious coincident hosts to >27 th mag in optical/nir.
29 EB 2010 Host-Less Short GRBs
30 EB 2010 Host-Less Short GRBs
31 Host-Less Short GRBs EB 2010 host-less
32 Host-Less Short GRBs EB 2010 w/ hosts host-less
33 Host-Less Short GRBs z ~ ~10 = kpc EB 2010 w/ hosts host-less
34 Offset Distribution Cumulative Fraction Short GRBs Long GRBs NS NS merger models C.C. SNe Ia SNe good agreement with NS-NS/NS-BH population synthesis Projected Physical Offset δr (kpc) Fong et al. 2010; EB 2010; Fong & EB 2013
35 Offset Distribution Cumulative Fraction Short GRBs Long GRBs NS NS merger models C.C. SNe Ia SNe Projected Physical Offset δr (kpc) Fong et al. 2010; EB 2010; Fong & EB % at <1 re 20% at >5 re Cumulative fraction good agreement with NS-NS/NS-BH population synthesis Short GRBs Long GRBs C.C. SNe Type Ia SNe Host normalized Offset δr/r e
36 Locations Within/Around Host Galaxies
37 (Lack of) Correlation with Stellar Light Short GRBs (opt) Short GRBs (UV) All Bursts Fong & EB 2013 Cumulative fraction Long GRBs 0.2 C.C. SNe 0.1 Type Ia SNe (opt) Type Ia SNe (UV) Fractional flux
38 (Lack of) Correlation with Stellar Light Short GRBs (opt) Short GRBs (UV) All Bursts Fong & EB 2013 Cumulative fraction Long GRBs 0.2 C.C. SNe 0.1 Type Ia SNe (opt) Type Ia SNe (UV) Fractional flux Strongly correlated
39 (Lack of) Correlation with Stellar Light Weakly correlated Cumulative fraction Short GRBs (opt) Short GRBs (UV) All Bursts 0.3 Long GRBs 0.2 C.C. SNe 0.1 Type Ia SNe (opt) Type Ia SNe (UV) Fractional flux Fong & EB 2013 Strongly correlated
40 (Lack of) Correlation with Stellar Light Weakly correlated Cumulative fraction Short GRBs (opt) Short GRBs (UV) All Bursts 0.3 Long GRBs 0.2 C.C. SNe 0.1 Type Ia SNe (opt) Type Ia SNe (UV) Fractional flux Fong & EB 2013 Strongly correlated Short GRB sites are weakly correlated with stellar light; progenitors migrate from birth to explosion sites.
41 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
42 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
43 Afterglows: Energy & Density log(flux) Sari et al log(freq)
44 Afterglows: Energy & Density log(flux) EK,iso & n EK,iso & n EK,iso Sari et al log(freq)
45 Afterglows: Energy & Density log(flux) radio optical X-ray EK,iso & n EK,iso & n EK,iso Sari et al log(freq)
46 Afterglows: Best-Case Examples EB et al E γ,iso erg / EK,iso erg / θj > 15 / n cm 3
47 Afterglows: Best-Case Examples EB et al Soderberg et al E γ,iso erg / EK,iso erg / θj > 15 / n cm 3 E γ erg / EK erg / θj 7 / n cm 3 E γ erg / EK erg / θj 6 / n cm 3 Fong et al. 2014
48 Afterglows: Statistical Distributions Fong et al. in prep. E K,iso (erg) GRB A c < X, e = B = n (cm )
49 Afterglows: Statistical Distribution Fong et al. in prep. E K,iso (erg) GRB A c < X, e = B = n (cm ) X-ray
50 Afterglows: Statistical Distribution Fong et al. in prep. E K,iso (erg) GRB A c < X, e = B = n (cm ) optical X-ray
51 Afterglows: Statistical Distribution Fong et al. in prep. E K,iso (erg) GRB A c < X, e = B = n (cm 3 ) radio optical X-ray
52 Afterglows: Statistical Distribution Fong et al. in prep. E K,iso (erg) GRB A c < X, e = B = n (cm ) radio optical X-ray
53 Afterglows: Statistical Distribution Fong et al. in prep. E K,iso (erg) GRB A c < X, e = B =0.1 P(n) P(E K,iso ) 0 n (cm 3 ) n (cm 3 ) EK,iso ( ) erg n (2 6) 10 3 cm 3 radio optical X-ray
54 Fong et al. in prep. Afterglows: Statistical Distribution
55 Afterglows: Statistical Distribution Cumulative Probability Fong et al. in prep n (cm 3 ) n ~ 10 2 cm 3 Cumulative Probability E K,iso (erg) EK,iso ~ erg
56 Jets: Energetics & Rates θj ~10 E γ ~ EK ~ few erg Long Short Fong, EB, et al. 2012; Fong, EB, et al Number Opening Angle j (degrees)
57 Jets: Energetics & Rates θj ~10 E γ ~ EK ~ few erg Long Short Fong, EB, et al. 2012; Fong, EB, et al Robs ~ 10 Gpc 3 yr 1 RGW ~ yr 1 (200 Mpc) Number Opening Angle j (degrees)
58 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
59 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
60 r-process Nucleosynthesis: Kilonova neutron-rich ejecta: Tidal tails Accretion disk outflows HMNS winds Decompressed neutron-rich ejecta r-process (A ~ 100) Li & Paczynski 1998; Metzger et al. 2008; Rosswog et al. 2012; Kasen et al. 2013
61 r-process Nucleosynthesis: Kilonova neutron-rich ejecta: Tidal tails Accretion disk outflows HMNS winds Decompressed neutron-rich ejecta r-process (A ~ 100) vej ~ c Mej ~ M } Lp ~ erg/s tp ~ day-week Li & Paczynski 1998; Metzger et al. 2008; Rosswog et al. 2012; Kasen et al. 2013
62 r-process Nucleosynthesis: Kilonova neutron-rich ejecta: Tidal tails Accretion disk outflows HMNS winds Decompressed neutron-rich ejecta r-process (A ~ 100) vej ~ c Mej ~ M } Lp ~ erg/s tp ~ day-week Li & Paczynski 1998; Metzger et al. 2008; Rosswog et al. 2012; Kasen et al. 2013
63 GRB B: The First Kilonova? EB et al. 2013; Tanvir et al Excess near-ir emission at ~1 week matching kilonova
64 GRB B: The First Kilonova? Mej ~ 0.05 M EB et al. 2013; Tanvir et al Excess near-ir emission at ~1 week matching kilonova
65 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
66 Compact Object Merger Predictions No association with massive stars no SNe, elliptical hosts Broad delay-time distribution mix of host galaxy types Natal Kicks offsets, low circumburst densities r-process nucleosynthesis Gravitational waves
67 Joint GW / EM Detections Distance (energy scale) Astrophysical context (NS/BH binary formation) Behavior of matter (hydrodynamics, jets) Nature of remnant (BH, magnetar) Metzger & EB 2012
68 Joint GW / EM Detections Distance (energy scale) Astrophysical context (NS/BH binary formation) Behavior of matter (hydrodynamics, jets) Nature of remnant (BH, magnetar) Metzger & EB 2012 Typical localization ~ 100 deg 2
69 Joint GW / Short GRB Detections Metzger & EB 2012 The short GRB rate in the GW volume is low; all-sky coverage is more important than accurate positions (temporal coincidence)
70 Joint GW / Optical Afterglow Detections Metzger & EB 2012
71 Joint GW / Optical Afterglow Detections Metzger & EB 2012
72 Joint GW / Radio Afterglow Detections The peak brightness is ~5 50 μjy, not feasible across a GW localization region EB 2014 The timescale for radio emission is ~1 10 years The energies and circumburst densities from short GRBs indicate that blind radio searches will be ineffective
73 Joint GW / Kilonova Detection Cowperthwaite et al. 2015
74 Joint GW / Kilonova Detection r ~ 25.5 mag i ~ 23.5 mag z ~ 22.5 mag Cowperthwaite et al. 2015
75 Joint GW / Kilonova Detection r ~ 25.5 mag i ~ 23.5 mag z ~ 22.5 mag Kilonova detections require rapid, deep, wide-field observations with ~4 8 m telescopes DECam, Pan-STARRS2, Subaru/HSC Cowperthwaite et al. 2015
76 Joint GW / Kilonova Identification Cowperthwaite et al. 2015
77 Joint GW / Kilonova Identification The combination of red color and fast rise time will help to distinguish kilonovae from other contaminating fast optical transients Cowperthwaite et al. 2015
78 Joint GW / Kilonova Identification The combination of red color and fast rise time will help to distinguish kilonovae from other contaminating fast optical transients Cowperthwaite et al. 2015
79 Summary Short GRB observations match our expectations for NS-NS/ NS-BH mergers: - Broad delay-time distribution - Kicks offsets, low density (n ~ 10 2 cm 3 ) - r-process nucleosynthesis Beaming: E ~10 49 erg; RGW ~ 10 yr 1 (R γ ~ 0.3 yr 1 ) We have already seen the on-axis EM counterparts of NS-NS/ NS-BH mergers; this guides follow-up of GW sources Most promising approach is optical follow-up at ~1 μm with 4 8m wide-field telescopes (DECam, HSC); radio follow-up of candidates on timescale of months years
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