1. S3/S4 BNS/PBH RESULTS and UPPER LIMITS
Chad Hanna, LSU
presented for the LSC on behalf of the inspiral group

2. OUTLINE Overview – what do we need for an upper limit on rate?
Details common to all 4 searches
Details about searches – S3 BNS, S4 BNS, S3 PBH, S4 PBH
How to compute upper limit
Upper limit results
Common Details – times analyzed, waveforms, coincidence, chisq, rsq, distance
cut, vetoes
Details about searches – efficiency, bgVsFg, loudest
event
Upper limit – if i have done my job people will
have all the quantities necessary for upperlimit
except population

3. + = Overview For the upper limit we need... 1. Times analyzed
H1H2L1
136 hrs
1. Times analyzed
2. Detector efficiency as a
function of distance
3. Loudest event and
probability of background
foreground
4. Astrophysical population
of sources +
H1H2 515 hrs. =
Upper limit on rate per galaxy

4. Common Details H1H2L1 H1H2 515 hrs. 365 hrs. H1L1 46 hrs. H1H2L1 H2L1
SOMEWHERE TALK ABOUT THE DISTINCTION OF VETOES AND DEADTIME AND HOW WE USE LOSS OF EFFICIENCY INSTEAD.
ALSO EXPLAIN WHY WE LOOKED AT DIFFERENT TIMES FOR S4 THAN S3.

5. S3 BNS - Efficiency Mass Range: 1.0-3.0 Msun Chirp distance =
H1H2L1
Mass Range:
Msun
Chirp distance =
effective distance
scaled by;
(Mchirp 1.4/Mchirp)5/6
Mention at june lsc 'chirp distance defined'

6. S3 BNS LOUDEST EVENT H1L1 trigger with ~85 combined effective
SNR squared

7. S3 PBH - Efficiency Mass Range: 0.35-1.0 Msun Chirp distance =
H1H2L1
Mass Range:
Msun
Chirp distance =
effective distance
scaled by;
(Mchirp 1.4/Mchirp)5/6
Mention at june lsc 'chirp distance defined'

8. S3 PBH Loudest Event H1L1 trigger with ~92 combined effective
SNR squared

9. S4 BNS Efficiency Mass Range: 1.0-3.0 Msun Chirp distance =
H1H2L1
Mass Range:
Msun
Chirp distance =
effective distance
scaled by;
(Mchirp 1.4/Mchirp)5/6

10. S4 BNS Efficiency

11. S4 BNS Loudest Event H1L1 trigger with ~86 combined effective
SNR squared

12. S4 PBH - Efficiency Mass Range: 0.35-1.0 Msun Chirp distance =
H1H2
Mass Range:
Msun
Chirp distance =
effective distance
scaled by;
(Mchirp 1.4/Mchirp)5/6
Mention at june lsc 'chirp distance defined'

13. S4 PBH Loudest Event H1L1 trigger with ~96 combined effective
SNR squared

14. S4 PBH Loudest Event

15. Population Model

16. Probability of Background
Probability that
an event is
background is
calculated from
time slides

17. Probability of foreground
Need
number of
galaxies
and derivative

18. Model Independent Errors

19. Model Dependent Errors
Barred Spiral Milky Way Illustration Credit: R. Hurt (SSC), JPL-Caltech, NASA
From
~2700 Galaxies
to 25 Mpc

20. Upper limit Ti = time analyzed in years
Ni = Number of galaxies (MW, 1010Lsun,...whatever you would like)
nfi = foreground probability
nbi = background probability

21. Upper limit S4 PBH Rate given vs mass S4 BNS rate Gaussian dist.
= XX

22. Conclusion

23. Chirp Distance

24. S4 BNS horizon distance H1

25. Effective SNR