Short Gamma-ray Bursts: Lessons Learned, Open Questions, and Constraints for the GW Era
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1 Wen-fai Fong Einstein Fellow University of Arizona Short Gamma-ray Bursts: Lessons Learned, Open Questions, and Constraints for the GW Era (observational complement to Enrico s talk) Northwestern University (Aug 2017) Fifty-One Erg 2017 Oregon State University Corvallis, OR
2 Outline Background Environments Collimation Central engine Constraints on GW counterparts
3 merger short gamma-ray burst compact object binary (NS-NS/NS-BH) Illustrated by: Dr. Jessie Berta-Thompson
4 The Basic Picture of Gamma-ray Bursts Progenitor Gamma-rays X-ray Optical Near-IR Radio Central engine Prompt emission Afterglow Figure adapted from Gehrels et al. 2007
5 The Basic Picture of Gamma-ray Bursts Progenitor Gamma-rays X-ray Optical Near-IR Radio Central engine SHORT Prompt emission Afterglow Kouveliotou et al. 1993; Nakar 2007 Figure adapted from Gehrels et al. 2007
6 The Basic Picture of Gamma-ray Bursts Progenitor Gamma-rays X-ray Optical Near-IR Radio Central engine SHORT Prompt emission Afterglow Kouveliotou et al. 1993; Nakar 2007 Figure adapted from Gehrels et al. 2007
7 The importance of afterglows long: 1997, short: 2005 GRB ACS/F814W
8 The importance of afterglows long: 1997, short: 2005 First X-ray afterglow z=0.225? GRB ACS/F814W Gehrels et al. 2005, Bloom et al ~few arcsec
9 The importance of afterglows long: 1997, short: 2005 First X-ray afterglow z=0.225? First optical afterglow z=0.161 GRB ACS/F814W First radio afterglow z=0.257 Gehrels et al. 2005, Bloom et al Fox et al. 2005; Hjorth et al Berger et al. 2005; Panaitescu 2006 ~few arcsec <1 arcsec <1 arcsec
10 The importance of afterglows long: 1997, short: 2005 First X-ray afterglow z=0.225? First optical afterglow z=0.161 GRB ACS/F814W First radio afterglow z=0.257 Gehrels et al. 2005, Bloom et al Fox et al. 2005; Hjorth et al Berger et al. 2005; Panaitescu 2006 ~few arcsec <1 arcsec <1 arcsec Key to localization and placement within a host
11 Outline Background Environments Collimation Central engine Constraints on GW counterparts
12 Host galaxies: Long GRBs Wainwright et al. 2007; Fruchter et al Long GRBs exclusively associated with star-forming galaxies
13 Hosts: Short GRBs Berger 2009; Leibler & Berger 2010; Fong et al. 2013; Berger 2014
14 Hosts: Short GRBs Berger 2009; Leibler & Berger 2010; Fong et al. 2013; Berger 2014 Berger 2014
15 Hosts: Short GRBs Berger 2009; Leibler & Berger 2010; Fong et al. 2013; Berger 2014 Commensurate with older stellar progenitor Delay time distribution P(τ)~ τ -1 Zheng & Ramirez-Ruiz 2007 Berger 2014
16 Short GRB locations Hubble Space Telescope NS/BH kicks + merger times Fong et al. 2010, Fong & Berger 2013
17 Short GRB locations Hubble Space Telescope NS/BH kicks + merger times offset Fong et al. 2010, Fong & Berger 2013 Fryer & Kalogera 1997; Fryer et al. 1999; Bloom et al. 1999; Perna & Belczynski 2002; Belczynski et al. 2006; Zemp et al. 2009
18 Short GRB locations Cumulative Fraction Short GRBs Fong et al. 2010; Fong & Berger 2013 Long GRBs Blanchard et al NS NS mergers Fryer et al. 1999; Bloom et al. 1999; Belczynski et al Projected Physical Offset R (kpc) Fong et al. 2010; Fong & Berger 2013 Short ~ 5 kpc Long ~ 1 kpc v kick ~ 100 km s -1 (see also Behroozi et al. 2014) host-normalized: ~20% are >5r e ~20% are <1r e Long GRBs: Blanchard et al NS-NS models: Fryer et al. 1999; Bloom et al. 1999; Belczynski et al. 2006
19 Cumulative Fraction Short GRBs Fong et al. 2010; Fong & Berger 2013 Long GRBs Blanchard et al NS NS mergers Fryer et al. 1999; Bloom et al. 1999; Belczynski et al Short GRB locations Projected Physical Offset R (kpc) Fong et al. 2010; Fong & Berger 2013 Long GRBs: Blanchard et al NS-NS models: Fryer et al. 1999; Bloom et al. 1999; Belczynski et al Short ~ 5 kpc Long ~ 1 kpc v kick ~ 100 km s -1 (see also Behroozi et al. 2014) host-normalized: ~20% are >5r e ~20% are <1r e Weakly correlated with regions of stellar mass or star formation
20 A population of host-less short GRBs? Berger 2010; Fong & Berger 2013; Tunnicliffe et al. 2014
21 A population of host-less short GRBs? high-z z>2.5 low-l L<0.1L* kicked Berger 2010; Fong & Berger 2013; Tunnicliffe et al ( kpc)
22 Comparison to galaxy luminosity function Host H band Magnitude L<<0.1L * HST NIR limit 0.1L* L* Coincident hosts "Host less" high-z? z>2.5 low-l? <<0.1L * kicked z> Redshift Fong & Berger 2013 (see also: Behroozi et al. 2014)
23 A population of host-less short GRBs? high-z z>2.5 low-l L<<0.1L * kicked Berger 2010; Fong & Berger 2013; Tunnicliffe et al ( kpc)
24 A population of host-less short GRBs? high-z z>2.5 low-l L<<0.1L * kicked Berger 2010; Fong & Berger 2013; Tunnicliffe et al origin in globular clusters? Lee et al. 2010; Stratta et al ( kpc)
25 A population of host-less short GRBs? Cumulative Fraction Short GRBs w/ W/ Cycle UNPUBLISHED Long GRBs NS NS merger models PRELIMINARY Projected Physical Offset R (kpc) high-z z>2.5 low-l L<<0.1L * kicked origin in globular clusters? Lee et al. 2010; Stratta et al ( kpc)
26 Short GRB locations in the context of other transients Extreme Ca-rich Gap Transients PTF Ia SNe Short GRBs Cumulative Fraction Cumulative Fraction Host-Normalized Projected Offset (R/R eff ) Lunnan et al but not the Drout et al most extreme
27 Outline Background Environments Collimation Central engine Constraints on GW counterparts
28 highly collimated spherical Implications: Energy scale, Event Rate
29 Rate (Gpc -3 yr -1 ) 10 4 Volumetric Rates observed short GRB Nakar 2007 Kalogera et al. 2004; Kim et al. 2006; Dominik et al. 2012; Kim et al. 2015; Belczynski et al. 2016
30 Rate (Gpc -3 yr -1 ) 10 4 Volumetric Rates failed short GRBs? Galactic double Population neutron synthesis stars observed short GRB Nakar 2007 Kalogera et al. 2004; Kim et al. 2006; Dominik et al. 2012; Kim et al. 2015; Belczynski et al. 2016
31 Rate (Gpc -3 yr -1 ) 10 4 Volumetric Rates failed short GRBs? collimated? Galactic double Population neutron synthesis stars observed short GRB actual SGRB? Nakar 2007 Kalogera et al. 2004; Kim et al. 2006; Dominik et al. 2012; Kim et al. 2015; Belczynski et al. 2016
32 An introduction to jet breaks F t jet time θ jet α t jet 3/8 Rhoads 1999; Sari, Piran & Halpern 1999
33 An introduction to jet breaks F t jet time θ jet α t jet 3/8 Rhoads 1999; Sari, Piran & Halpern 1999 Later break corresponds to wider opening angle (assumes on-axis orientation) van Eerten & MacFadyen 2013
34 A Decade of Observations Five known jet breaks in short GRBs Flux (mjy) 7 deg 6 deg 5 deg GRB A Burrows et al. 2006; Soderberg et al Fong et al Troja et al X-ray optical + radio X-ray + optical + radio
35 Jet Opening Angles REMAKE Long Short Number Opening Angle (degrees) j Short GRBs from: Berger et al. 2005; Burrows et al. 2006; Soderberg et al. 2006; Nicuesa-Guelbenzu et al. 2009; Coward et al. 2012; Fong et al. 2012; Berger et al. 2013; Fong et al. 2014; Troja et al Long GRBs from: Frail 2001, Berger 2003, Bloom 2003, Ghirlanda 2004,Friedman & Bloom 2005, Racusin 2009, Filgas 2011, Cenko 2010/2011, Goldstein 2011
36 Jet Opening Angles REMAKE Number Long Short Opening Angle (degrees) j Inferred energy: Eiso ~ erg Etrue ~ erg Inferred rates: Gpc -3 yr yr -1 (<200 Mpc) Fong et al Short GRBs from: Berger et al. 2005; Burrows et al. 2006; Soderberg et al. 2006; Nicuesa-Guelbenzu et al. 2009; Coward et al. 2012; Fong et al. 2012; Berger et al. 2013; Fong et al. 2014; Troja et al Long GRBs from: Frail 2001, Berger 2003, Bloom 2003, Ghirlanda 2004,Friedman & Bloom 2005, Racusin 2009, Filgas 2011, Cenko 2010/2011, Goldstein 2011
37 Rate (Gpc -3 yr -1 ) 10 4 Volumetric Rates Galactic Population actual double synthesis short GRB neutron stars observed short GRB Kalogera et al. 2004; Kim et al. 2006; Dominik et al. 2012; Kim et al. 2015; Belczynski et al. 2016; Nakar 2007
38 Rate (Gpc -3 yr -1 ) 10 4 Volumetric Rates ALIGO O1 (NS-NS) Abbott et al (ApJ: 832, 21) Galactic Population actual double synthesis short GRB neutron stars observed short GRB Kalogera et al. 2004; Kim et al. 2006; Dominik et al. 2012; Kim et al. 2015; Belczynski et al. 2016; Nakar 2007
39 Rate (Gpc -3 yr -1 ) 10 4 Volumetric Rates ALIGO O1 (NS-NS) Abbott et al (ApJ: 832, 21) (NS-BH) Galactic Population actual double synthesis short GRB neutron stars observed short GRB Kalogera et al. 2004; Kim et al. 2006; Dominik et al. 2012; Kim et al. 2015; Belczynski et al. 2016; Nakar 2007
40 Outline Background Environments Collimation Central engine Constraints on GW counterparts
41 hypermassive neutron star ( magnetar )
42 Atypical behavior: Extended emission Perley et al. 2009
43 Atypical behavior: Extended emission Perley et al. 2009
44 Atypical behavior: X-ray plateaus and flares plateau Rowlinson et al. 2013
45 Atypical behavior: X-ray plateaus and flares plateau Grupe et al Rowlinson et al Signatures of magnetars? Metzger et al 2011; Gompertz et al. 2014; Lü et al. 2015; Siegel et al. 2016
46 Radio signatures of magnetars Luminosity Time Models calculated from Nakar & Piran 2011; Metzger & Bower 2014
47 Radio signatures of magnetars energy density Luminosity mass Time Models calculated from Nakar & Piran 2011; Metzger & Bower 2014
48 Radio signatures of magnetars energy density Luminosity mass Predicted to peak at MHz to GHz frequencies Time Models calculated from Nakar & Piran 2011; Metzger & Bower 2014
49 Constraints on signatures from magnetars
50 Constraints on signatures from magnetars Rotational Energy (erg) Magnetar E max Fong, Metzger, Berger & Özel 2016 See also: Metzger & Bower 2014 Horesh et al Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 )
51 Constraints on signatures from magnetars Rotational Energy (erg) A M ej =0.03 M sol Magnetar E max Fong, Metzger, Berger & Özel 2016 See also: Metzger & Bower 2014 Horesh et al Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 )
52 Constraints on signatures from magnetars Rotational Energy (erg) RULED OUT M ej =0.03 M sol Magnetar E max A PERMITTED Fong, Metzger, Berger & Özel 2016 See also: Metzger & Bower 2014 Horesh et al Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 )
53 Constraints on signatures from magnetars Rotational Energy (erg) A Afterglow Berger et al Fong et al PERMITTED M ej =0.03 M sol Magnetar E max Fong, Metzger, Berger & Özel 2016 See also: Metzger & Bower 2014 Horesh et al Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 )
54 Constraints on signatures from magnetars Rotational Energy (erg) A PERMITTED M ej =0.03 M sol Magnetar E max Fong, Metzger, Berger & Özel 2016 See also: Metzger & Bower 2014 Horesh et al E<few x erg Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 )
55 Constraints on signatures from magnetars M ej =0.03 M sol Fong, Metzger, Berger & Özel 2016 Rotational Energy (erg) A A A A A A B Previous Magnetar E max Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 )
56 Constraints on signatures from magnetars M ej =0.03 M sol Fong, Metzger, Berger & Özel 2016 Rotational Energy (erg) A A A A A A B Previous Magnetar E max Circumburst 10 Density 10 (cm 3 10 ) 10 2 Circumburst Density (cm 3 ) E< erg model with many tunable parameters
57 Outline Background Environments Collimation Central engine Constraints on GW counterparts
58 Isotropic counterparts are more promising black hole ) ϴobs Currently, GRBs are discovered on-axis > Most GW events will be off-axis >
59 r-process kilonova Li & Paczynski 1998 Metzger et al Barnes & Kasen 2013 Tanaka & Hotokezaka 2013 Metzger & Fernández 2014 Tanaka et al Fontes et al Kasen et al Foucart et al Montes et al Fernández et al Siegel et al Wollaeger et al. 2017
60 r-process kilonova Red or blue? or very red? (mid-ir) (Fontes et al. 2015; Wollaeger et al. 2017) (for details, see Rodrigo Fernández talk) Li & Paczynski 1998 Metzger et al Barnes & Kasen 2013 Tanaka & Hotokezaka 2013 Metzger & Fernández 2014 Tanaka et al Fontes et al Kasen et al Foucart et al Montes et al Fernández et al Siegel et al Wollaeger et al. 2017
61 A smoking gun? Kilonova of GRB B 9 days 30 days Subtraction v ej = c M ej = M sol OPTICAL Berger, Fong & Chornock 2013 NEAR-IR Tanvir et al First direct evidence for a compact object merger origin
62 A smoking gun? Kilonova of GRB B 9 days 30 days Subtraction v ej = c M ej = M sol OPTICAL NEAR-IR Tanvir et al First direct evidence for a compact object merger origin apparent magnitude [AB mag] Models: γa 1 γb 1 γc 1 γd 1 DZ1 RE-VISITED γa 2 γb 2 γc 2 γd 2 DZ2 F160W at z=0.356 Wollaeger et al time [d] GRB130603B Absolute magnitude
63 Testing the current era of models
64 Testing the current era of models Optical Luminosity λl λ (erg s -1 ) M ej, v ej Near-IR Luminosity λl λ (erg s -1 ) Rest-frame Time after Burst (days) Optical (r, 0.6 um) Rest-frame Time after Burst (days) Near-IR (J, 1.3 um) Fong, Margutti, Chornock et al GRB B: Berger, Fong, and Chornock 2013; Tanvir et al Kilonova models from: Barnes & Kasen 2013, Tanaka et al. 2014, Kasen et al. 2015
65 Testing the current era of models Optical Luminosity λl λ (erg s -1 ) M ej, v ej Near-IR Luminosity λl λ (erg s -1 ) Rest-frame Time after Burst (days) Optical (r, 0.6 um) Rest-frame Time after Burst (days) Near-IR (J, 1.3 um) Fong, Margutti, Chornock et al GRB B: Berger, Fong, and Chornock 2013; Tanvir et al Kilonova models from: Barnes & Kasen 2013, Tanaka et al. 2014, Kasen et al. 2015
66 Testing the current era of models Optical Luminosity λl λ (erg s -1 ) Near-IR Luminosity λl λ (erg s -1 ) Rest-frame Time after Burst (days) Rest-frame Time after Burst (days) Optical (r, 0.6 um) Near-IR (J, 1.3 um) Fong, Margutti, Chornock et al GRB B: Berger, Fong, and Chornock 2013; Tanvir et al Kilonova models from: Barnes & Kasen 2013, Tanaka et al. 2014, Kasen et al. 2015
67 Testing the current era of models Optical Luminosity λl λ (erg s -1 ) GRB B Previous sgrbs Near-IR Luminosity λl λ (erg s -1 ) GRB B Previous sgrbs GRB B Rest-frame Time after Burst (days) Optical (r, 0.6 um) Rest-frame Time after Burst (days) Near-IR (J, 1.3 um) More optimistic (e.g., brighter) models would violate short GRB observations (for update, see Andrew Levan s talk) Fong, Margutti, Chornock et al GRB B: Berger, Fong, and Chornock 2013; Tanvir et al Kilonova models from: Barnes & Kasen 2013, Tanaka et al. 2014, Kasen et al. 2015
68 NS-NS vs. NS-BH? 1) Imprinted on offset distribution? Growing highly-kicked subset 2) Imprinted on kilonova luminosity distribution? Future observations will bring clarity SHORT GRB 3) Clues from the central engine? Ongoing NS-BH? CHOKED/FAILED Murguia-Berthier et al. 2017
69 Summary Environments Hosts & locations indicate compact object mergers Q: NS-NS vs. NS-BH? Globular cluster channel? Collimation Short GRB, ALIGO, and predicted rates are all consistent Q: What fraction of mergers create short GRBs? Central engine Anomalous X-ray behavior observed in ~20% of short GRBs Q: Can this activity be explained by magnetars? Constraints on GW counterparts Need deep searches in the GW era given current kilonova models
70 Summary Environments Hosts & locations indicate compact object mergers Q: Growing highly-kicked population? Collimation Short GRB, ALIGO, and predicted rates are all consistent Q: What fraction of mergers create short GRBs? Central engine Anomalous X-ray behavior observed in ~20% of short GRBs Q: What is causing this activity? Constraints on GW counterparts Limits from short GRBs can constrain most optimistic models STAY TUNED
71 thank you Saguaro National Park West, Tucson, AZ
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