millisecond pulsar population · pulsar recycling binary sn low mass x-ray binary state bill...

11th Bonn Neutron Star Workshop on Formation and Evolution Of Neutron Stars

11/12/2017

Amruta Jaodand

Amruta Jaodand11th Bonn Neutron Star Workshop

COMPANY NAME

MILLISECOND PULSAR

POPULATION

Amruta Jaodand11th Bonn Neutron Star Workshop

1. Millisecond Pulsars

2.Current Population

3.Applications

4.Future Prospects

4.1.Potential Science Questions

Outline

Amruta Jaodand11th Bonn Neutron Star Workshop

Millisecond Pulsars

1

Introduction

Amruta Jaodand11th Bonn Neutron Star Workshop

DISCOVERY1982, D. Backer, Millisecond Pulsar, PSR J1937+21

P < 10ms in this talk.

Amruta Jaodand11th Bonn Neutron Star Workshop

DISCOVERY1982, D. Backer, Millisecond Pulsar, PSR J1937+21

RL=P*c/2π

Radhakrishnan and Cooke, 1969

P < 10ms in this talk.

Amruta Jaodand11th Bonn Neutron Star Workshop

PULSAR RECYCLING

Binary SN Low Mass X-ray

Binary State

Bill Saxton; NRAO/AUI/NSF

Radio Millisecond

Pulsar State

Backer, Kulkarni et al. 1982 - Short period, small period derivative

Alpar, Cheng, Ruderman & Shaham, A new class of radio pulsars, Nature, 300, 728, 1982Radhakrishnan & Srinivasan 1982

Amruta Jaodand11th Bonn Neutron Star Workshop

Current PopulationDiverse Manifestations

2

Amruta Jaodand11th Bonn Neutron Star Workshop

CURRENT STATUS

105 yr

106 yr

107 yr

108 yr

109 yr

10 10G

10 11G

10 12G

10 13G

10 14G

10�3 10�2 10�1 100 101

Period (s)

10�22

10�20

10�18

10�16

10�14

10�12

10�10

Perio

dD

eriv

ativ

e

SGR/AXPBinaryRadio-IR Emission”Radio-Quiet”RRATPulsed Thermal X-raySNR

1 Young Pulsars

Double NS

Magnetars

2 Normal pulsars

4 Millisecond Pulsars

2976 pulsars in total

Made using M

att Pitkin's psrqpy package

Amruta Jaodand11th Bonn Neutron Star Workshop

CURRENT STATUS

105 yr

106 yr

107 yr

108 yr

109 yr

10 10G

10 11G

10 12G

10 13G

10 14G

10�3 10�2 10�1 100 101

Period (s)

10�22

10�20

10�18

10�16

10�14

10�12

10�10

Perio

dD

eriv

ativ

e

SGR/AXPBinaryRadio-IR Emission”Radio-Quiet”RRATPulsed Thermal X-raySNR

1 Young Pulsars

Double NS

Magnetars

2 Normal pulsars

4 Millisecond Pulsars

2976 pulsars in total

Made using M

att Pitkin's psrqpy package

Amruta Jaodand11th Bonn Neutron Star Workshop

CURRENT STATUS

105 yr

106 yr

107 yr

108 yr

109 yr

10 10G

10 11G

10 12G

10 13G

10 14G

10�3 10�2 10�1 100 101

Period (s)

10�22

10�20

10�18

10�16

10�14

10�12

10�10

Perio

dD

eriv

ativ

e

SGR/AXPBinaryRadio-IR Emission”Radio-Quiet”RRATPulsed Thermal X-raySNR

1 Young Pulsars

Double NS

Magnetars

2 Normal pulsars

4 Millisecond Pulsars

107 yr

108 yr

109 yr

10 10G

10 11G

10�3 10�2 10�1 100 101

Period (s)

10�22

10�21

10�20

10�19

10�18

10�17

Perio

dD

eriv

ativ

e

BinaryRadio-IR Emission

2976 pulsars in total

Made using M

att Pitkin's psrqpy package

Amruta Jaodand11th Bonn Neutron Star Workshop

CURRENT STATUS

105 yr

106 yr

107 yr

108 yr

109 yr

10 10G

10 11G

10 12G

10 13G

10 14G

10�3 10�2 10�1 100 101

Period (s)

10�22

10�20

10�18

10�16

10�14

10�12

10�10

Perio

dD

eriv

ativ

e

SGR/AXPBinaryRadio-IR Emission”Radio-Quiet”RRATPulsed Thermal X-raySNR

1 Young Pulsars

Double NS

Magnetars

2 Normal pulsars

4 Millisecond Pulsars

107 yr

108 yr

109 yr

10 10G

10 11G

10�3 10�2 10�1 100 101

Period (s)

10�22

10�21

10�20

10�19

10�18

10�17

Perio

dD

eriv

ativ

e

BinaryRadio-IR Emission

308 millisecond pulsars (F0>100Hz) 18 millisecond pulsars (F0>500Hz) 2 millisecond pulsars (F0>700Hz)

2976 pulsars in total

Made using M

att Pitkin's psrqpy package

Amruta Jaodand11th Bonn Neutron Star Workshop

PSR BOOM

New telescopes, new backends, new algorithms - acceleration searches

2004-03-28

2004-07-27

2005-03-11

2005-05-21

2006-01-26

2006-05-09

2007-01-09

2007-11-22

2009-05-05

2010-05-07

2011-07-23

2012-05-17

2013-03-28

2013-07-04

2013-11-04

2014-03-17

2014-11-13

2015-03-13

2015-06-29

2015-11-10

2016-11-14

2017-03-17

Time (YY-MM-DD)

0

50

100

150

200

250

300

No

.o

fre

cyc

led

MSP

s More than double the MSPs!

Sky surveys: Parkes Multi-Beam led the way! GBT-drift scan and North Celestial Cap surveys; Arecibo - 327 MHz drift-scan and ALFA survey;

HTRU- Northern and Southern sky surveys

Fermi Treasure Map

Amruta Jaodand11th Bonn Neutron Star Workshop

MIRUM LECTORUM

Triple 1

Isolated 113

Binary 194

120 are in Globular Clusters, 116 Radio sources, 73 Gamma-ray sources, 51 X-ray sources

MSP MANIFESTATIONS

Diversity in MSPs (P< 10ms)

Amruta Jaodand11th Bonn Neutron Star Workshop

30%

MIRUM LECTORUM

MSP BINARIES

Black Widows

“Black Widow” pulsar,

B1957+20, Fruchter et al.(1988)

Companion Mass, <0.01-0.1 M_sun

Orbital Period, short <3.5 hrs

Orbital evolution, peculiar, spin-orbit

coupling

Known Black Widows, 40

Amruta Jaodand11th Bonn Neutron Star Workshop

30%

MIRUM LECTORUM

MSP BINARIES

Redbacks

“Redback” pulsars,

Companion Mass, 0.15-0.4 M_sun

Orbital periods, 4-15 hr

Non-deterministic orbital

variations

Almost Roche Lobe Filling, Breton et al.(2010) Known Redbacks, 22

Amruta Jaodand11th Bonn Neutron Star Workshop

MSP BINARIES

PSR J1023+0038, (1.69 ms) Archibald et al. (2009) XSS J12270−4859, (1.69 ms) Bassa et al. (2014) PSR J1824–2452I (3.9 ms) Papitto et al. (2013)

3FGL J1544-1125 (?? ms) Bogdanov & Halpern (2015)

Transitional Millisecond Pulsars

Binary SN Low Mass X-ray

Binary State

Bill Saxton; NRAO/AUI/NSF

Radio Millisecond

Pulsar State

Amruta Jaodand11th Bonn Neutron Star Workshop

MSP BINARIES

Triple MSP System

PSR J0337+1715: 365.95 HZ

Fig. : Jason Hessels

See talk by Anne Archibald

Ransom et al. 2014

Amruta Jaodand11th Bonn Neutron Star Workshop

0 100 200 300 400 500 600 700 800

Spin frequency (Hz)

0102030405060708090

100110120

No.

ofre

cycl

edM

SPs

OUTLIERS Spin frequency Distribution

Observational bias or formation mechanism? Bassa et al 2017 - 707 Hz first galactic field MSP

Plenius et al. 2017 - 411.89 Hz

Amruta Jaodand11th Bonn Neutron Star Workshop

0 100 200 300 400 500 600 700 800

Spin frequency (Hz)

0102030405060708090

100110120

No.

ofre

cycl

edM

SPs

OUTLIERS Spin frequency Distribution

Observational bias or formation mechanism? Bassa et al 2017 - 707 Hz first galactic field MSP

Plenius et al. 2017 - 411.89 Hz

56500 57000 57500 58000

Time(MJD)

�2

�1

0

1

2

3

⌫�

⌫ 0(1

0�7

Hz)

Obs. 2 Obs. 3 Obs. 4-7 Obs. 8-10 Obs. 11-14

Spin down extrapolatedfrom radio pulsar state

Best-fit constant spin-downin LMXB state: Full Baseline

Best-fit constant spin-downin LMXB state: Short Baseline

Current spin-frequencymeasurements in LMXB state

�10

�5

0

5

10

P�

P0

(10�

10

ms)

Jaodand et al. 2016

Amruta Jaodand11th Bonn Neutron Star Workshop

OUTLIERS

Redbacks

Image from Papitto et al. 2014, arXiv:1310.7803

Black Widows

Chen et al. 2013

PSR J2129−0429

PSR J1301+0833

Extreme Black Widows — Tidarreans: PSR J1301+0833, Companion Mass < 0.01 M_sun

Redback at bifurcation — PSR J2129−0429, Companion Mass = 0.44 M_sun , P_orb=15.2 hr

Romani et al. 2016

Bellm et al.2015

Amruta Jaodand11th Bonn Neutron Star Workshop

OUTLIERS

Antoniadis et al. 2013, Antoniadis et al. 2016

Bimodal mass distribution: With low mass (1.39 M_sun) and high mass (1.8 M_sun)

1) Precise known mass 2) Known total mass 3) Known mass ratio

PSR J0348+0432 : 2.01+/-0.04 ,M_sun

MSPS

DNS

Amruta Jaodand11th Bonn Neutron Star Workshop

Applications

3

Precise Timers & Strongly Self-Gravitating

Amruta Jaodand11th Bonn Neutron Star Workshop

PULSAR TIMING ARRAYS

LIGO-VIRGO: gravitational waves (GWs) from BBHs and BNSs (GW170817)

PTAs probe GWs in the nHz regime from: a) Cosmic strings b) Supermassive black hole merger - stochastic signal and merger

event

Sanidas et al. 2012, Jose J. Blanco-Pillado et al. 2017

Lentati et al. 2015, Verbiest et al. 2016, Mingarelli et al. 2017

Fig. : Christopher Berry

See talk by H. Middleton

Amruta Jaodand11th Bonn Neutron Star Workshop

EQUATION OF STATE

Review: Ozel and Freire 2016

Millisecond pulsar mass measurement: Fantastic timers, low orbital eccentricities

1. Pulsars in GCs - eccentricity due to interaction

2. Shapiro delay measurement

3. Spectroscopic measurement - Balmer lines

4. Stellar triples

Ransom et al. 2005, Freire et al 2008

Jacoby et al. 2005, Demorest et al. 2010

Callanan et al. 1998, Antoniadis et al. 2012

Champion et al 2008, Ransom et al. 2014

Millisecond pulsar radius measurement:

1. Spectroscopic measurement 2. Timing Measurements See talk by N.U.Bastian for more details

Amruta Jaodand11th Bonn Neutron Star Workshop

OTHER APPLICATIONS

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

tMSPs are fantastic probes of low-level accretion onto neutron stars

Accreting millisecond X-ray pulsars Review: Patruno and Watts 2012

Jaodand, Hessels & Archiabld 2017

Accretion Physics

Bogdanov 2017

Amruta Jaodand11th Bonn Neutron Star Workshop

Future Prospects

4

New Means To Find MSPS & Holy Grails

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfinders

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’s large field of view, collecting area, bandwidth

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’s large field of view, collecting area, bandwidth

Millisecond pulsar yield : ~3000 MSPs, 1000 in globular clusters

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’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),

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’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)

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’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

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’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!

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’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

Fig: M. Kramer

Amruta Jaodand11th Bonn Neutron Star Workshop

INTERFEROMETRIC ERA

Higher instantaneous sensitivities for SKA, MeerKAT and pathfindersSKA’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

Fig: M. Kramer

Astron Hackathon

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS • VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr,

34000 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

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS • VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr,

34000 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

• Lofar 2M Sky Survey (LoTSS) - Shimwell et al. 2016

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS • VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr,

34000 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

• Lofar 2M Sky Survey (LoTSS) - Shimwell et al. 2016

• 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

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS • VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr,

34000 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

• Lofar 2M Sky Survey (LoTSS) - Shimwell et al. 2016

• 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

• Low-frequency surveys (<200 MHz)- LOTAAS etc. steep spectrum sources Coenen et al. 2014, Bassa et al. 2017, Plenius et al.2017

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS • VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr,

34000 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

• Lofar 2M Sky Survey (LoTSS) - Shimwell et al. 2016

• 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

• High frequency (>5GHz)- flat spectrum sources

• Low-frequency surveys (<200 MHz)- LOTAAS etc. steep spectrum sources Coenen et al. 2014, Bassa et al. 2017, Plenius et al.2017

Amruta Jaodand11th Bonn Neutron Star Workshop

NEW SKY SURVEYS • VLA Sky Survey (VLASS) - 3 epochs of high cadence observation (4504 hr,

34000 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

• Lofar 2M Sky Survey (LoTSS) - Shimwell et al. 2016

• 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

• High frequency (>5GHz)- flat spectrum sources

• Low-frequency surveys (<200 MHz)- LOTAAS etc. steep spectrum sources Coenen et al. 2014, Bassa et al. 2017, Plenius et al.2017

• NICER Gendreau and Arzoumanian, Nature Astronomy 1, (2017)

Amruta Jaodand11th Bonn Neutron Star Workshop

HOLY GRAILS

Formation Mechanisms? Specific observation strategies.

Fantastic pulsars and how to find them?

Amruta Jaodand11th Bonn Neutron Star Workshop

HOLY GRAILS

Sub-ms pulsars

Formation Mechanisms? Specific observation strategies.

Fantastic pulsars and how to find them?

Amruta Jaodand11th Bonn Neutron Star Workshop

HOLY GRAILS

Ultracompact binaries? P_orb < 1hr

Sub-ms pulsars

Formation Mechanisms? Specific observation strategies.

Fantastic pulsars and how to find them?

Amruta Jaodand11th Bonn Neutron Star Workshop

HOLY GRAILS

Ultracompact binaries? P_orb < 1hr

Sub-ms pulsars

MSP-BH systems

Formation Mechanisms? Specific observation strategies.

Fantastic pulsars and how to find them?

Amruta Jaodand11th Bonn Neutron Star Workshop

HOLY GRAILS

Ultracompact binaries? P_orb < 1hr

Massive neutrons stars : M_NS > 2.5 M_Sun ?

Sub-ms pulsars

MSP-BH systems

Formation Mechanisms? Specific observation strategies.

Fantastic pulsars and how to find them?

Amruta Jaodand11th Bonn Neutron Star Workshop

HOLY GRAILS

Ultracompact binaries? P_orb < 1hr

Massive neutrons stars : M_NS > 2.5 M_Sun ?

Sub-ms pulsars

MSP-BH systems

MSP with planets

Formation Mechanisms? Specific observation strategies.

Fantastic pulsars and how to find them?

Amruta Jaodand11th Bonn Neutron Star Workshop

SUMMARY

•Population of MSPs has nearly doubled since 2010

•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

Amruta Jaodand11th Bonn Neutron Star Workshop

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

Amruta Jaodand: amruta.jaodand@gmail.com Tweet: @amrutajaodand