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Indirect Detection: Clustering of GW Events
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Classroom Contents
Introduction to Primordial Black Hole Dark Matter - Lecture 2
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- 1 12:00 pm, 09 NOVEMBER 2020
- 2 Outline
- 3 Indirect detection: GWs from PBH Binary Mergers
- 4 Q: Does PBH Dark Matter have testable GW predictions?
- 5 Indirect Detection: The GW Mass Spectrum
- 6 Indirect Detection: Stellar Mass Spectrum
- 7 Indirect Detection: Constraints on PBH fraction
- 8 Indirect Detection: Orbital Eccentricity
- 9 Indirect Detection: Individual and Effective Spin
- 10 Indirect Detection: Stochastic GW Background
- 11 Indirect Detection: Clustering of GW Events
- 12 Indirect Detection: 03a Data Hot Off the Press!
- 13 Indirect Detection: 03a Fit with Astro Channels
- 14 Indirect Detection: 03a Fit with Accrediting PBHs
- 15 PBH Dark Matter: Constraining the Mass Fraction
- 16 Microlensing: Illustration
- 17 PBH Dark Matter: Existing Constraints
- 18 PBH Dark Matter: The "LIGO Window"
- 19 Direct Detection: New Transient Probes
- 20 Fast Radio Bursts!
- 21 Constraining MACHOs: Fast Radio Burst Lensing
- 22 Strong Lensing of FRBs: Unique Signature
- 23 PBH DM LIGO Window: Constraints Tightening!
- 24 Observational Outlook: Timeline
- 25 PBH DM: Other Windows Open?
- 26 From PBH to Primordial Power Spectrum Limits
- 27 PBHs as SMBH Seeds: Future Tight! Constraints
- 28 Takeaway: Lots of Ways to Probe PBH Scenario!
- 29 Thank you!
- 30 PBH DM: Other Windows Open?
