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B L A C K H O L E S O N F I R E ASTRID LAMBERTS SHEA - PowerPoint PPT Presentation

Jan 09, 2023 •121 likes •528 views

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

  1. 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

  2. A NEW ERA IN ASTRONOMY LIGO-Virgo Science Collaboration, 2016

  3. A NEW ERA IN ASTRONOMY LIGO-Virgo Science Collaboration, 2016 Bright Loud future : Virgo, eLISA, EM counterparts

  5. Previously known BH

  6. Previously known BH LIGO detections

  7. 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

  8. 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?

  9. B I N A RY E V O L U T I O N

  10. B I N A RY E V O L U T I O N

  11. B I N A RY E V O L U T I O N

  12. B I N A RY E V O L U T I O N

  13. B I N A RY E V O L U T I O N

  14. B I N A RY E V O L U T I O N

  15. B I N A RY E V O L U T I O N

  16. B I N A RY E V O L U T I O N

  17. B I N A RY E V O L U T I O N

  18. B I N A RY E V O L U T I O N

  19. B I N A RY E V O L U T I O N

  20. B I N A RY E V O L U T I O N

  21. B I N A RY E V O L U T I O N Billions of years

  22. D E L AY T I M E D I S T R I B U T I O N 10 � 5 dN m dt ∝ t � 1 � ) BH mergers ( M � 1 10 � 6 10 � 7 0.01 Z � 10 � 8 0.1 Z � 0.3 Z � 10 � 9 10 7 10 8 10 9 10 10 (Lamberts+16) t delay (yr)

  23. D E L AY T I M E D I S T R I B U T I O N 10 � 5 dN m dt ∝ t � 1 � ) • Low metallicity: BH mergers ( M � 1 10 � 6 most massive remnants 10 � 7 0.01 Z � 10 � 8 0.1 Z � 0.3 Z � 10 � 9 10 7 10 8 10 9 10 10 (Lamberts+16) t delay (yr)

  24. D E L AY T I M E D I S T R I B U T I O N 10 � 5 dN m dt ∝ t � 1 � ) • Low metallicity: BH mergers ( M � 1 10 � 6 most massive remnants 10 � 7 • higher metallicity : long delay 0.01 Z � 10 � 8 0.1 Z � 0.3 Z � 10 � 9 10 7 10 8 10 9 10 10 (Lamberts+16) t delay (yr)

  25. L O W Z S TA R S : B I M O D A L F O R M AT I O N Semi-analytic model (Lamberts+16) Lookback time formation

  26. L O W Z S TA R S : B I M O D A L F O R M AT I O N Semi-analytic model (Lamberts+16) Lookback time formation Milky Way

  27. L O W Z S TA R S : B I M O D A L F O R M AT I O N Semi-analytic model (Lamberts+16) Lookback time formation Dwarf galaxy Milky Way

  28. 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 1 (Lamberts+16) Lookback time formation Metallicity/Sun (Confirmed in Elbert+17, Mapelli+17)

  29. 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 Milky Way 1 (Lamberts+16) Lookback time formation Metallicity/Sun (Confirmed in Elbert+17, Mapelli+17)

  30. 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 Dwarf galaxy Milky Way 1 (Lamberts+16) Lookback time formation Metallicity/Sun (Confirmed in Elbert+17, Mapelli+17)

  31. 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=.5 z=2 z=1 constant ~7 billion years Full sample Dwarf galaxies “invisible” 
 GW150914-like with EM observations (Lamberts+16)

  32. P L AY I N G W I T H F I R E ( P R E L I M I N A RY ) 10 3 1 1 stars formed mergers current horizon 10 4 m12i 0 10 2 m12i 0 10 3 Z/ Z � � 1 Z/ Z � � 1 10 1 10 2 � 2 � 2 10 0 10 1 � 3 � 3 10 0 10 � 1 0 2 4 6 8 10 12 0 2 4 6 8 10 12 formation time (Gyr) formation time (Gyr) (Wetzel+16)

  33. P L AY I N G W I T H F I R E ( P R E L I M I N A RY ) 10 3 1 mergers current horizon 10 2 m12i 0 Z/ Z � � 1 10 1 � 2 10 0 � 3 10 � 1 0 2 4 6 8 10 12 formation time (Gyr)

  34. P L AY I N G W I T H F I R E ( P R E L I M I N A RY ) 10 3 10 0 1 1 stars formed mergers current horizon m10y 0 m10y 0 10 2 10 � 1 Z/ Z � � 1 Z/ Z � � 1 10 1 10 � 2 � 2 � 2 � 3 � 3 10 0 10 � 3 0 2 4 6 8 10 12 0 2 4 6 8 10 12 formation time (Gyr) formation time (Gyr)

  35. P L AY I N G W I T H F I R E ( P R E L I M I N A RY ) 10 0 1 1 stars formed mergers current horizon m10v 0 m10v 0 10 � 1 10 1 Z/ Z � � 1 Z/ Z � � 1 10 � 2 � 2 � 2 � 3 � 3 10 0 10 � 3 0 2 4 6 8 10 12 0 2 4 6 8 10 12 formation time (Gyr) formation time (Gyr) Consistent with Lamberts+16 MW-like galaxies have little scatter, less clear for dwarfs

  36. M E R G E R S V S M E TA L L I C I T Y 10 4 m12i 10 3 log(N merger ) 10 2 All Metallicities Z:0-0.013 Z:0.013-0.02 10 1 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 10 0 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 × 10 10 Time (Gyr)

  37. M E R G E R S V S M E TA L L I C I T Y 10 4 Detection horizon m12i 10 3 log(N merger ) 10 2 All Metallicities Z:0-0.013 Z:0.013-0.02 10 1 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 10 0 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 × 10 10 Time (Gyr)

  38. M E R G E R S V S M E TA L L I C I T Y All Metallicities All Metallicities 10 1 10 1 Z:0-0.013 Z:0-0.013 Z:0.013-0.02 Z:0.013-0.02 Z:0.02-0.032 Z:0.02-0.032 Z:0.032-0.054 Z:0.032-0.054 10 0 10 0 Z:0.054-0.082 Z:0.054-0.082 Z:0.082-0.13 Z:0.082-0.13 Z:0.13-0.16 Z:0.13-0.16 log(N merger ) log(N merger ) 10 − 1 10 − 1 10 − 2 10 − 2 m10v m10q 10 − 3 10 − 3 10 − 4 10 − 4 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 0.0 0.2 0.4 0.6 0.8 1.0 1.2 1.4 × 10 10 × 10 10 Time (Gyr) Time (Gyr) Consistent with Lamberts+16 MW-like galaxies have little scatter, less clear for dwarfs

  39. C O M I N G ( S O O N ? ) 100 detections in 5 years EM follow-up -> host galaxies 3 detectors -> some triangulation eLISA: mapping compact binaries in the MW

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