In Search of New MSPs for Pulsar Timing Arrays. Kevin Stovall, NRAO Socorro NANOGrav Collaboration
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1 In Search of New MSPs for Pulsar Timing Arrays Kevin Stovall, NRAO Socorro NANOGrav Collaboration NRAO Postdoc Symposium, March 27, 2017
2 NANOGrav = US/Canada-based collaboration working to detect nhz GW via pulsar timing. Large and still growing collaboration: Currently over 80 members (~45 SP, ~25 PD, ~10 GS) Geographically distributed, ~20 different institutions. Strong commitment to undergrad education and involvement in research. Awarded $14.5M / 5 year NSF Physics Frontier Center grant See for more info
3 Pulsar Timing Arrays NANOGrav monitors a set of very stable millisecond pulsars (MSPs) to look for GW signals. Such signals would be correlated vs. pulsar angular separation. The NANOGrav Collaboration et al. 2015, ApJ, 813, 65 Hellings & Downs Curve Image Credit: David Champion Other PTA Experiments Parkes Pulsar Timing Array (PPTA) European Pulsar Timing Array (EPTA) International Pulsar Timing Array (IPTA) Hellings & Downs 1983, ApJ, 265, 39
4 Pulsar Timing Array
5 Pulsar Timing Array
6 Current Telescopes Arecibo Observatory Green Bank Telescope 305 meter diameter Dec range:-1 deg to 38 deg Sources visible for ~2 hours L-Band SEFD ~ 2 Jy 100 meter diameter Dec range: > -45 deg Sources visible for many hours L-Band SEFD ~ 10 Jy
7 Frequency Coverage GUPPI PUPPI
8 MSPs
9 Why we need more MSPs M = 80, c= 5yr 1, M = 20, c= 20yr 1, M = 20, c= 5yr 1, M = 80, c= 5yr 1, = 100ns = 100ns = 100ns =1µs h i T [yr] Siemens et al. 2013, CQG, 30, 4015
10 Where to Search for MSPs? Nearby MSPs are expected to be essentially isotropic. Searches in 1990s found many MSPs at a wide range of Galactic latitudes. Low frequencies are optimal: Dispersion/Scattering are less of a problem out of Galactic plane, so we can take advantage of steep spectrum Larger beam size -> faster survey speed
11 Large Area Pulsar Surveys Green Bank North Celestial Cap (GBNCC) Arecibo 327 MHz Drift Scan (AO327)
12 Survey Parameter Comparison Survey Center Frequency (MHz) Bandwidth (MHz) Frequency Resolution (khz) Sample Time (us) Integration Time (s) Style AO /69 56/24 125/82 64 Drift GBNCC Pointed AO327 - Deneva et al. 2013, ApJ, 775, 51 GBNCC - Stovall et al. 2014, ApJ, 791, 67 AO327 Collaborators: J. Deneva, M. Bagchi, P. Freire, F. Jenet, J. Martinez, M. McLaughlin GBNCC Collaborators: S. Ransom, M. Decesar, R. Lynch, J. Swiggum, H. Al Ali, P. Chawla, T. Cromartie, J. Hessels, F. Jenet, D. Kaplan, V. Kaspi, V. Kondratiev, J. van Leeuwen, M. McLaughlin, M. Roberts, X. Siemens, R. Spiewak, I. Stairs
13 Survey Sensitivities
14 GBNCC 145 Pulsars 18 MSPs 11 RRATs 1 DNS (2 more?) 2 wide binaries ~75% complete We plan to make data available, ~500 TB, we are converting from 8-bit to 2-bit
15 GBNCC Discoveries 5 MSPs added to NANOGrav so far, 2 more currently being tested for potential inclusion and ~5 others currently being follow-ed up that may be included in the future
16 J Is a 2.87-ms pulsar in a 96-minute orbit with a solar mass (9 MJ) companion. GBNCC Discoveries Assuming inclination angle of 60 degrees: separation between the two stars is about 0.5 solar radii Appears to be a black widow system, but no radio eclipses
17 GBNCC Discoveries J Eclipsing system with an optically detected companion. Spectrum is most similar to a white dwarf, but has high metallicity. Pulsar mass is ~1.84(11) solar masses Counts per Bin Stovall et al. 2014, ApJ, 791, Pulse Phase 1.5 Kaplan et al. 2012, ApJ, 753, 174 2
18 GBNCC Discoveries J ms pulsar with a DM of 22 pc/cm^3 (D~1 kpc). In a 512 day orbit with a ~0.4 solar mass companion Dec (J2000) WIYN B-band s 15 m s RA (J2000) 2 h 14 m s 15 m
19 AO327 Discoveries to date: 72 Pulsars, 8 MSPs,13 RRATs, 2 DNSs, 1 wide binary
20 AO327 Discoveries 3 MSPs added to NANOGrav so far, ~3 others currently being followed up that may be included in the future
21 AO327 Discoveries PSR J ms pulsar with DM of 10.8 pc/cm^3 in a 32 day orbit with a 0.2 solar mass companion, but eccentricity ~0.13. Observed Period(ms) PSR J Time of Observation(MJD) Disrupted Triple System? Unlikely RD-AIC? Maybe Freire & Tauris 2014, MNRAS, 438, L86 Circumbinary disk? Maybe Antoniadis et al. 2016, ApJ, 830, 36 Antoniadis 2014, ApJ, 797, 24
22 PSR J ms pulsar with a DM of 30.3 pc/cm^3 in an eccentric orbit (0.112) with a ~1.2 solar mass companion. Shapiro Delay measurement combined with rate of advance of periastron gives MP=1.559(5) solar masses and MC=1.174(4) solar masses. Largest pulsar mass for DNS system and companion has lowest neutron star mass. AO327 Discoveries
23 5 Year MSPs
24 9 Year MSPs
25 11 Year MSPs
26 Current MSPs
27 Current MSPs
28 NANOGrav MSPs
29 Conclusion NANOGrav is using pulsars as a galactic scale gravitational wave detector. We gain sensitivity by finding additional MSPs and we have reason to believe not all good MSPs have been found. There are multiple large-scale search efforts ongoing to find suitable MSPs and they have added many new MSPs to the array. Eight out of the ~60 MSPs being timed were found in the 2 surveys mentioned here (within the past 5 years) and more are currently being tested for future inclusion.
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