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B L A C K H O L E S O N F I R E
ASTRID LAMBERTS
SHEA GARRISON-KIMMEL/PHIL HOPKINS/DREW CLAUSEN/KALI DRANGO
GALFRESCA, Aug 25, 2017
LIGO-Virgo Science Collaboration, 2016
B L A C K H O L E S O N F I R E ASTRID LAMBERTS SHEA - - PowerPoint PPT Presentation
B L A C K H O L E S O N F I R E ASTRID LAMBERTS SHEA - - PowerPoint PPT Presentation
B L A C K H O L E S O N F I R E ASTRID LAMBERTS SHEA GARRISON-KIMMEL/PHIL HOPKINS/DREW CLAUSEN/KALI DRANGO GALFRESCA, Aug 25, 2017 A NEW ERA IN ASTRONOMY LIGO-Virgo Science Collaboration, 2016 A NEW ERA IN ASTRONOMY LIGO-Virgo Science
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LIGO-Virgo Science Collaboration, 2016
Bright Loud future : Virgo, eLISA, EM counterparts
A NEW ERA IN ASTRONOMY
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Previously known BH
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Previously known BH LIGO detections
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L O W M E TA L L I C I T Y P R O G E N I T O R S
(LIGO Coll.)
Binary evolution -> low metallicity progenitor stars
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L O W M E TA L L I C I T Y P R O G E N I T O R S
(LIGO Coll.)
Binary evolution -> low metallicity progenitor stars Conditions of formation?
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
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B I N A RY E V O L U T I O N
Billions of years
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D E L AY T I M E D I S T R I B U T I O N
107 108 109 1010
tdelay (yr)
109 108 107 106 105
BH mergers (M1
)
dNm dt ∝ t1
0.01Z 0.1Z 0.3Z
(Lamberts+16)
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D E L AY T I M E D I S T R I B U T I O N
107 108 109 1010
tdelay (yr)
109 108 107 106 105
BH mergers (M1
)
dNm dt ∝ t1
0.01Z 0.1Z 0.3Z
- Low metallicity:
most massive remnants (Lamberts+16)
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D E L AY T I M E D I S T R I B U T I O N
107 108 109 1010
tdelay (yr)
109 108 107 106 105
BH mergers (M1
)
dNm dt ∝ t1
0.01Z 0.1Z 0.3Z
- Low metallicity:
most massive remnants
- higher metallicity :
long delay (Lamberts+16)
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L O W Z S TA R S : B I M O D A L F O R M AT I O N
(Lamberts+16) Lookback time formation
Semi-analytic model
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L O W Z S TA R S : B I M O D A L F O R M AT I O N
(Lamberts+16) Lookback time formation
Milky Way
Semi-analytic model
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L O W Z S TA R S : B I M O D A L F O R M AT I O N
(Lamberts+16) Lookback time formation
Dwarf galaxy Milky Way
Semi-analytic model
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B I M O D A L F O R M AT I O N O F G W 1 5 0 9 1 4 P R O G E N I T O R S
Metallicity/Sun (Lamberts+16) Lookback time formation 1
(Confirmed in Elbert+17, Mapelli+17)
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B I M O D A L F O R M AT I O N O F G W 1 5 0 9 1 4 P R O G E N I T O R S
Metallicity/Sun (Lamberts+16) Lookback time formation 1
Milky Way
(Confirmed in Elbert+17, Mapelli+17)
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B I M O D A L F O R M AT I O N O F G W 1 5 0 9 1 4 P R O G E N I T O R S
Metallicity/Sun (Lamberts+16) Lookback time formation 1
Dwarf galaxy Milky Way
(Confirmed in Elbert+17, Mapelli+17)
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S TA R F O R M AT I O N I N D WA R F G A L A X I E S
z=2 z=1 z=.5 z=.2 “invisible” with EM observations GW150914-like Full sample Dwarf galaxies (Lamberts+16) constant ~7 billion years
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P L AY I N G W I T H F I R E ( P R E L I M I N A RY )
2 4 6 8 10 12
formation time (Gyr)
3 2 1
1
Z/Z
mergers current horizon m12i 101 100 101 102 103
2 4 6 8 10 12
formation time (Gyr)
3 2 1
1
Z/Z
stars formed m12i 100 101 102 103 104
(Wetzel+16)
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P L AY I N G W I T H F I R E ( P R E L I M I N A RY )
2 4 6 8 10 12
formation time (Gyr)
3 2 1
1
Z/Z
mergers current horizon m12i 101 100 101 102 103
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P L AY I N G W I T H F I R E ( P R E L I M I N A RY )
2 4 6 8 10 12
formation time (Gyr) 3 2 1
1
Z/Z
mergers current horizon m10y 103 102 101 100 2 4 6 8 10 12
formation time (Gyr) 3 2 1
1
Z/Z
stars formed m10y 100 101 102 103
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P L AY I N G W I T H F I R E ( P R E L I M I N A RY )
2 4 6 8 10 12
formation time (Gyr) 3 2 1
1
Z/Z
mergers current horizon m10v 103 102 101 100
Consistent with Lamberts+16 MW-like galaxies have little scatter, less clear for dwarfs
2 4 6 8 10 12
formation time (Gyr) 3 2 1
1
Z/Z
stars formed m10v 100 101
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M E R G E R S V S M E TA L L I C I T Y
0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4
Time (Gyr)
×1010
100 101 102 103 104
log(Nmerger)
m12i
All Metallicities Z:0-0.013 Z:0.013-0.02 Z:0.02-0.032 Z:0.032-0.054 Z:0.054-0.082 Z:0.082-0.13 Z:0.13-0.16
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M E R G E R S V S M E TA L L I C I T Y
0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4
Time (Gyr)
×1010
100 101 102 103 104
log(Nmerger)
m12i
All Metallicities Z:0-0.013 Z:0.013-0.02 Z:0.02-0.032 Z:0.032-0.054 Z:0.054-0.082 Z:0.082-0.13 Z:0.13-0.16
Detection horizon
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M E R G E R S V S M E TA L L I C I T Y
0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4
Time (Gyr)
×1010
10−4 10−3 10−2 10−1 100 101
log(Nmerger)
m10v
All Metallicities Z:0-0.013 Z:0.013-0.02 Z:0.02-0.032 Z:0.032-0.054 Z:0.054-0.082 Z:0.082-0.13 Z:0.13-0.16
0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4
Time (Gyr)
×1010
10−4 10−3 10−2 10−1 100 101
log(Nmerger)
m10q
All Metallicities Z:0-0.013 Z:0.013-0.02 Z:0.02-0.032 Z:0.032-0.054 Z:0.054-0.082 Z:0.082-0.13 Z:0.13-0.16
Consistent with Lamberts+16 MW-like galaxies have little scatter, less clear for dwarfs
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