MILLISECOND PULSAR POPULATION
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1 MILLISECOND PULSAR POPULATION on Formation and Evolution Of Neutron Stars 11/12/2017 COMPANY NAME
2 Outline 1. Millisecond Pulsars 2.Current Population 3.Applications 4.Future Prospects 4.1.Potential Science Questions
3 1 Millisecond Pulsars Introduction
4 DISCOVERY 1982, D. Backer, Millisecond Pulsar, PSR J P < 10ms in this talk.
5 1982, D. Backer, Millisecond Pulsar, PSR J DISCOVERY Radhakrishnan and Cooke, 1969 RL=P*c/2π P < 10ms in this talk.
6 PULSAR RECYCLING Backer, Kulkarni et al Short period, small period derivative Alpar, Cheng, Ruderman & Shaham, A new class of radio pulsars, Nature, 300, 728, 1982 Radhakrishnan & Srinivasan 1982 Bill Saxton; NRAO/AUI/NSF Binary SN Low Mass X-ray Binary State Radio Millisecond Pulsar State
7 2 Current Population Diverse Manifestations
8 CURRENT STATUS Period Derivative yr 10 6 yr SGR/AXP Binary 10 7 yr 10 8 yr 10 9 yr 1 Young Pulsars Radio-IR Emission Radio-Quiet RRAT Pulsed Thermal X-ray SNR Double NS Magnetars G G G 2 Normal pulsars G G Made using Matt Pitkin's psrqpy package 4 Millisecond Pulsars Period (s) 2976 pulsars in total
9 CURRENT STATUS Period Derivative yr 10 6 yr SGR/AXP Binary 10 7 yr 10 8 yr 10 9 yr 1 Young Pulsars Radio-IR Emission Radio-Quiet RRAT Pulsed Thermal X-ray SNR Double NS Magnetars G G G 2 Normal pulsars G G Made using Matt Pitkin's psrqpy package 4 Millisecond Pulsars Period (s) 2976 pulsars in total
10 CURRENT STATUS Period Derivative yr 10 8 yr 10 5 yr 10 9 yr 10 6 yr SGR/AXP Binary Binary Radio-IR Emission Radio-IR Emission Radio-Quiet RRAT Pulsed Thermal X-ray SNR 10 7 yr 10 8 yr 10 9 yr 1 Young Pulsars Double NS Magnetars G G G G G 2 Normal pulsars G G Made using Matt Pitkin's psrqpy package 4 Millisecond Pulsars Period (s) 2976 pulsars in total
11 CURRENT STATUS Period Derivative yr 10 8 yr 10 5 yr 10 9 yr 10 6 yr SGR/AXP Binary Binary Radio-IR Emission Radio-IR Emission Radio-Quiet RRAT Pulsed Thermal X-ray SNR 10 7 yr 10 8 yr 10 9 yr 1 Young Pulsars Double NS Magnetars G G G G G 2 Normal pulsars G G Made using Matt Pitkin's psrqpy package 4 Millisecond Pulsars Period (s) 2976 pulsars in total 308 millisecond pulsars (F0>100Hz) 18 millisecond pulsars (F0>500Hz) 2 millisecond pulsars (F0>700Hz)
12 300 PSR BOOM No. of recycled MSPs More than double the MSPs! Time (YY-MM-DD) Sky surveys: Parkes Multi-Beam led the way! GBT-drift scan and North Celestial Cap surveys; Arecibo MHz drift-scan and ALFA survey; HTRU- Northern and Southern sky surveys Fermi Treasure Map New telescopes, new backends, new algorithms - acceleration searches
13 Diversity in MSPs (P< 10ms) MSP MANIFESTATIONS MIRUM LECTORUM Isolated 113 Triple 1 Binary are in Globular Clusters, 116 Radio sources, 73 Gamma-ray sources, 51 X-ray sources
14 MSP BINARIES Black Widows Black Widow pulsar, 30% B , Fruchter et al.(1988) MIRUM LECTORUM Companion Mass, < M_sun Orbital Period, short <3.5 hrs Orbital evolution, peculiar, spin-orbit coupling Known Black Widows, 40
15 MSP BINARIES Redbacks Redback pulsars, 30% Companion Mass, M_sun Orbital periods, 4-15 hr MIRUM LECTORUM Non-deterministic orbital variations Almost Roche Lobe Filling, Breton et al.(2010) Known Redbacks, 22
16 MSP BINARIES Transitional Millisecond Pulsars Bill Saxton; NRAO/AUI/NSF Binary SN Low Mass X-ray Binary State Radio Millisecond Pulsar State PSR J , (1.69 ms) Archibald et al. (2009) XSS J , (1.69 ms) Bassa et al. (2014) PSR J I (3.9 ms) Papitto et al. (2013) 3FGL J (?? ms) Bogdanov & Halpern (2015)
17 MSP BINARIES Triple MSP System Ransom et al Fig. : Jason Hessels PSR J : HZ See talk by Anne Archibald
18 OUTLIERS Spin frequency Distribution No. of recycled MSPs Spin frequency (Hz) Observational bias or formation mechanism? Bassa et al Hz first galactic field MSP Plenius et al Hz
19 OUTLIERS Spin frequency Distribution 0 (10 7 Hz) No. of recycled MSPs Obs. 2 Obs. 3 Obs. 4-7 Obs Obs Jaodand et al Spin down extrapolated from radio pulsar state Best-fit constant spin-down in LMXB state: Full Baseline Best-fit constant spin-down in LMXB state: Short Baseline Current spin-frequency measurements in LMXB state Spin Time(MJD) frequency (Hz) P P0 (10 10 ms) Observational bias or formation mechanism? Bassa et al Hz first galactic field MSP Plenius et al Hz
20 Image from Papitto et al. 2014, arxiv: OUTLIERS PSR J PSR J Black Widows Redbacks Chen et al Extreme Black Widows Tidarreans: PSR J , Companion Mass < 0.01 M_sun Romani et al Redback at bifurcation PSR J , Companion Mass = 0.44 M_sun, P_orb=15.2 hr Bellm et al.2015
21 OUTLIERS PSR J : 2.01+/-0.04,M_sun MSPS Bimodal mass distribution: With low mass (1.39 M_sun) and high mass (1.8 M_sun) DNS 1) Precise known mass 2) Known total mass 3) Known mass ratio Antoniadis et al. 2013, Antoniadis et al. 2016
22 3 Applications Precise Timers & Strongly Self-Gravitating
23 PULSAR TIMING ARRAYS Fig. : Christopher Berry LIGO-VIRGO: gravitational waves (GWs) from BBHs and BNSs (GW170817) PTAs probe GWs in the nhz regime from: a) Cosmic strings Sanidas et al. 2012, Jose J. Blanco-Pillado et al b) Supermassive black hole merger - stochastic signal and merger event Lentati et al. 2015, Verbiest et al. 2016, Mingarelli et al See talk by H. Middleton
24 EQUATION OF STATE Millisecond pulsar mass measurement: Fantastic timers, low orbital eccentricities 1. Pulsars in GCs - eccentricity due to interaction Ransom et al. 2005, Freire et al Shapiro delay measurement Jacoby et al. 2005, Demorest et al Spectroscopic measurement - Balmer lines Callanan et al. 1998, Antoniadis et al Stellar triples Champion et al 2008, Ransom et al Millisecond pulsar radius measurement: Review: Ozel and Freire Spectroscopic measurement 2. Timing Measurements See talk by N.U.Bastian for more details
25 OTHER APPLICATIONS Accretion Physics Bogdanov 2017 tmsps are fantastic probes of low-level accretion onto neutron stars Jaodand, Hessels & Archiabld 2017 Accreting millisecond X-ray pulsars Review: Patruno and Watts 2012 Understanding of pulsar emission physics Galactic centre excess? See talks by: Stellar Evolution - John Antoniadis Inter stellar medium - Caterina Tiburzi Strong field tests of gravity - Shao and Archibald
26 4 Future Prospects New Means To Find MSPS & Holy Grails
27 INTERFEROMETRIC ERA Fig: M. Kramer
28 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders
29 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth
30 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters
31 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters Kramer (2004), SKA Science, Smits et al. (2008),
32 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters Kramer (2004), SKA Science, Smits et al. (2008), SKA science tome (2014), Kramer and Stappers (2015)
33 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters Kramer (2004), SKA Science, Smits et al. (2008), SKA science tome (2014), Kramer and Stappers (2015) Computational challenges: First we need to find PSRs
34 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters Kramer (2004), SKA Science, Smits et al. (2008), SKA science tome (2014), Kramer and Stappers (2015) Computational challenges: First we need to find PSRs and then we need to time the PSRs!
35 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters Kramer (2004), SKA Science, Smits et al. (2008), SKA science tome (2014), Kramer and Stappers (2015) Computational challenges: First we need to find PSRs and then we need to time the PSRs! MachineLearning: Eatough et al (2010), Lyon et al. 2016
36 INTERFEROMETRIC ERA Fig: M. Kramer Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders SKA s large field of view, collecting area, bandwidth Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters Kramer (2004), SKA Science, Smits et al. (2008), SKA science tome (2014), Kramer and Stappers (2015) Astron Hackathon Computational challenges: First we need to find PSRs and then we need to time the PSRs! MachineLearning: Eatough et al (2010), Lyon et al. 2016
37 NEW SKY SURVEYS
38 NEW SKY SURVEYS VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr, deg2, 6 sources at SNR of 10/deg2) First epoch commenced in this year in Sep. 2-4GHz survey : Flat as well as modest spectrum sources VLASS white papers, Bhakta et al. 2017
39 NEW SKY SURVEYS VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr, deg2, 6 sources at SNR of 10/deg2) First epoch commenced in this year in Sep. 2-4GHz survey : Flat as well as modest spectrum sources VLASS white papers, Bhakta et al Lofar 2M Sky Survey (LoTSS) - Shimwell et al. 2016
40 NEW SKY SURVEYS VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr, deg2, 6 sources at SNR of 10/deg2) First epoch commenced in this year in Sep. 2-4GHz survey : Flat as well as modest spectrum sources VLASS white papers, Bhakta et al Lofar 2M Sky Survey (LoTSS) - Shimwell et al CHIME - Inaugrated this year, 250 deg2, 10 pulsars simultaneously, 700 pulsars a day Cycle through all PTA pulsars in 10 days Ng et al. 2017
41 NEW SKY SURVEYS VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr, deg2, 6 sources at SNR of 10/deg2) First epoch commenced in this year in Sep. 2-4GHz survey : Flat as well as modest spectrum sources VLASS white papers, Bhakta et al Lofar 2M Sky Survey (LoTSS) - Shimwell et al CHIME - Inaugrated this year, 250 deg2, 10 pulsars simultaneously, 700 pulsars a day Cycle through all PTA pulsars in 10 days Ng et al Low-frequency surveys (<200 MHz)- LOTAAS etc. steep spectrum sources Coenen et al. 2014, Bassa et al. 2017, Plenius et al.2017
42 NEW SKY SURVEYS VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr, deg2, 6 sources at SNR of 10/deg2) First epoch commenced in this year in Sep. 2-4GHz survey : Flat as well as modest spectrum sources VLASS white papers, Bhakta et al Lofar 2M Sky Survey (LoTSS) - Shimwell et al CHIME - Inaugrated this year, 250 deg2, 10 pulsars simultaneously, 700 pulsars a day Cycle through all PTA pulsars in 10 days Ng et al Low-frequency surveys (<200 MHz)- LOTAAS etc. steep spectrum sources Coenen et al. 2014, Bassa et al. 2017, Plenius et al.2017 High frequency (>5GHz)- flat spectrum sources
43 NEW SKY SURVEYS VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr, deg2, 6 sources at SNR of 10/deg2) First epoch commenced in this year in Sep. 2-4GHz survey : Flat as well as modest spectrum sources VLASS white papers, Bhakta et al Lofar 2M Sky Survey (LoTSS) - Shimwell et al CHIME - Inaugrated this year, 250 deg2, 10 pulsars simultaneously, 700 pulsars a day Cycle through all PTA pulsars in 10 days Ng et al Low-frequency surveys (<200 MHz)- LOTAAS etc. steep spectrum sources Coenen et al. 2014, Bassa et al. 2017, Plenius et al.2017 High frequency (>5GHz)- flat spectrum sources NICER Gendreau and Arzoumanian, Nature Astronomy 1, (2017)
44 HOLY GRAILS Fantastic pulsars and how to find them? Formation Mechanisms? Specific observation strategies.
45 HOLY GRAILS Fantastic pulsars and how to find them? Sub-ms pulsars Formation Mechanisms? Specific observation strategies.
46 HOLY GRAILS Fantastic pulsars and how to find them? Sub-ms pulsars Ultracompact binaries? P_orb < 1hr Formation Mechanisms? Specific observation strategies.
47 HOLY GRAILS Fantastic pulsars and how to find them? Sub-ms pulsars Ultracompact binaries? P_orb < 1hr MSP-BH systems Formation Mechanisms? Specific observation strategies.
48 HOLY GRAILS Fantastic pulsars and how to find them? Sub-ms pulsars Ultracompact binaries? P_orb < 1hr MSP-BH systems Massive neutrons stars : M_NS > 2.5 M_Sun? Formation Mechanisms? Specific observation strategies.
49 HOLY GRAILS Fantastic pulsars and how to find them? Sub-ms pulsars Ultracompact binaries? P_orb < 1hr MSP-BH systems Massive neutrons stars : M_NS > 2.5 M_Sun? MSP with planets Formation Mechanisms? Specific observation strategies.
50 Population of MSPs has nearly doubled since 2010 SUMMARY We expect a new burst in MSP discoveries with new surveys such as SKA New discoveries lead to diversity and diversity in pulsar population translates to fantastic new probes of physics! Extragalactic pulsars? Creative use of MSPs - scintillometry - Open to new finds during MSP searches such as FRBs and unknowns
51 : Acknowledgments Plots supported by Matt Pitkin's Psrqpy package ATNF pulsar catalogue P. Freire s globular cluster catalogue D. Lorimer s Galactic MSP catalogue A.Patruno's MSP catalogue Jason Hessels for guidance! Wonderful reviews
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