Thermal properties of three Fermi pulsars

Andrey Danilenko1, Anna Karpova1,2, Aida Kirichenko1,2,Yury Shibanov1,2, Peter Shternin1,2, Sergey Zharikov3

& Dmitry Zyuzin1

1Ioffe Institute, St. Petersburg, Russia

2St. Petersburg State Polytechnical Univ., St. Petersburg, Russia

3Observatorio Astronomico Nacional SPM, UNAM, Mexico

Outline

Motivation

Results

Summary

Outline

Motivation

Results

Summary

Thermal radiation from INS. Why important

◮ from ∼ 102 till ∼ 105 years (middle-aged) NSs cool down vianeutrino emission

◮ neutrino emissivity depends on state and composition ofsupranuclear matter inside NSs

◮ also superfluidity

◮ observations in soft X-rays and UV give us Teff

◮ comparison of Teff with predictions of the cooling theory givesus neutrino emissivity

Nearby middle-aged pulsars, such as Vela and “Three Musketeers”(Geminga, B0656 and B1055), are of particular importance.

Fermi gives us

several promising targets (see Abdo et al. 2013)PSRs J0357+3205, J1741−2054 and J0633+0632

◮ their ages are ∼ 104–105 years and they are not farther than 1 kpc(Abdo et al. 2013)

◮ J0357+3205 and J0633+0632. X-ray data were analyzed previously(De Luca et al. 2011, Marelli et al. 2013, Ray et al. 2011)

◮ J1741−2054 X-ray PWN and Hα bow-shock were detected(Romani et al. 2010)

◮ Large number of J1741−2054 photons were collected during 300 ksChandra observations, PI Roger Romani, “A Legacy study of therelativistic Shocks of PWN”

◮ J1741−2054. phase-resolved spectroscopy of the non-thermalcomponent of the X-ray emission based on XMM data (Marelli etal. 2014)

We analyzed X-ray data available in Chandra and XMM-Newton

archives. We also observed J0357+3205 in the optical with GTC. For

details see papers by Kirichenko et al. 2014 and Karpova et al. 2014

Fermi gives us

several promising targets (see Abdo et al. 2013)PSRs J0357+3205, J1741−2054 and J0633+0632

◮ their ages are ∼ 104–105 years and they are not farther than 1 kpc(Abdo et al. 2013)

◮ J0357+3205 and J0633+0632. X-ray data were analyzed previously(De Luca et al. 2011, Marelli et al. 2013, Ray et al. 2011)

◮ J1741−2054 X-ray PWN and Hα bow-shock were detected(Romani et al. 2010)

◮ Large number of J1741−2054 photons were collected during 300 ksChandra observations, PI Roger Romani, “A Legacy study of therelativistic Shocks of PWN”

◮ J1741−2054. phase-resolved spectroscopy of the non-thermalcomponent of the X-ray emission based on XMM data (Marelli etal. 2014)

We analyzed X-ray data available in Chandra and XMM-Newton

archives. We also observed J0357+3205 in the optical with GTC. For

details see papers by Kirichenko et al. 2014 and Karpova et al. 2014

Fermi gives us

several promising targets (see Abdo et al. 2013)PSRs J0357+3205, J1741−2054 and J0633+0632

◮ their ages are ∼ 104–105 years and they are not farther than 1 kpc(Abdo et al. 2013)

◮ J0357+3205 and J0633+0632. X-ray data were analyzed previously(De Luca et al. 2011, Marelli et al. 2013, Ray et al. 2011)

◮ J1741−2054 X-ray PWN and Hα bow-shock were detected(Romani et al. 2010)

◮ Large number of J1741−2054 photons were collected during 300 ksChandra observations, PI Roger Romani, “A Legacy study of therelativistic Shocks of PWN”

◮ J1741−2054. phase-resolved spectroscopy of the non-thermalcomponent of the X-ray emission based on XMM data (Marelli etal. 2014)

We analyzed X-ray data available in Chandra and XMM-Newton

archives. We also observed J0357+3205 in the optical with GTC. For

details see papers by Kirichenko et al. 2014 and Karpova et al. 2014

Fermi gives us

several promising targets (see Abdo et al. 2013)PSRs J0357+3205, J1741−2054 and J0633+0632

◮ their ages are ∼ 104–105 years and they are not farther than 1 kpc(Abdo et al. 2013)

◮ J0357+3205 and J0633+0632. X-ray data were analyzed previously(De Luca et al. 2011, Marelli et al. 2013, Ray et al. 2011)

◮ J1741−2054 X-ray PWN and Hα bow-shock were detected(Romani et al. 2010)

◮ Large number of J1741−2054 photons were collected during 300 ksChandra observations, PI Roger Romani, “A Legacy study of therelativistic Shocks of PWN”

◮ J1741−2054. phase-resolved spectroscopy of the non-thermalcomponent of the X-ray emission based on XMM data (Marelli etal. 2014)

We analyzed X-ray data available in Chandra and XMM-Newton

archives. We also observed J0357+3205 in the optical with GTC. For

details see papers by Kirichenko et al. 2014 and Karpova et al. 2014

Outline

Motivation

Results

Summary

Standard cooling theory predictions

NSs cool down via MURCA, no enhanced neutrino emission, no superfluidity

102 104 1060.1

1

3 2 1

T [MK]

t [yr]

1 PSR J1741-20542 PSR J0357+32053 PSR J0633+0632

(see Yakovlev & Pethick 2004 and Yakovlev et al. 2011)

J1741−2054 and “Three Musketeers”

blackbody + power-law, Teff = 60 ± 2 eV, R = 17 ± 3 Dkpc km

102 104 1060.1

1

PSR J1741-2054

3 2

1

T [MK]

t [yr]

Musketeers1 PSR 0656+142 Geminga3 PSR B1055-52

Karpova et al. 2014

Multiwavelength spectrum of B1055−52

UV observations show that the surface may be cooler.

Mignani, Pavlov & Kargaltsev 2010

Standard cooling scenario

Here “3′” marks temperature of B1055−52 measured from UV

102 104 1060.1

1 3

PSR J1741-2054

3' 2 1

T [MK]

t [yr]

Musketeers1 PSR 0656+142 Geminga3 PSR B1055-523' PSR B1055-52, UV data

Karpova et al. 2014

J0633+0632 requires faster cooling processes?

hydrogen atmosphere + power-law, Teff ≈ 40 ± 15 eV

102 104 1060.1

T s [MK]

t [yr]

1PSR J0633+0632

Outline

Motivation

Results

Summary

Summary

◮ J1741−2054 looks similar to PSR B1055−2054, it is hotterthan the standard cooling scenario predicts.

◮ J0633+0632 is likely the coldest NS on the neutrino coolingstage. Requires faster cooling processes?

What to do next

◮ Observations of J1741−2054 in UV (Hubble).

◮ Observations of J0633+0632 with XMM-Newton.

Summary

◮ J1741−2054 looks similar to PSR B1055−2054, it is hotterthan the standard cooling scenario predicts.

◮ J0633+0632 is likely the coldest NS on the neutrino coolingstage. Requires faster cooling processes?

What to do next

◮ Observations of J1741−2054 in UV (Hubble).

◮ Observations of J0633+0632 with XMM-Newton.

The Chandra/ACIS-S spectrum of J0633+0632

10−4

10−3

0.01

0.1

norm

aliz

ed c

ount

s s−

1 ke

V−

1

10.5 2 5

−0.01

0

0.01

norm

aliz

ed c

ount

s s−

1 ke

V−

1

Energy (keV)

II (BB+PL), C=264.6 (dof=658)II

10−4

10−3

0.01

0.1

norm

aliz

ed c

ount

s s−

1 ke

V−

1

10.5 2 5

−0.01

0

0.01

norm

aliz

ed c

ount

s s−

1 ke

V−

1

Energy (keV)

II (BB+PL)GABS, C=248.5 (dof=655)II

Is there a line? Posterior predictive check

0 5 10 15LRT statistic

0.0

0.1

0.2

0.3

0.4

0.5

0.6

p.d.f. LRTdata = 16.1

p < 0.001

Figure: None of 1000 simulations has LRT greater than the observedone, that is, p-value is less than 0.001.

T vs R for NSA+PL

5 10 15 20R∞ [ d500pc km ]

30

35

40

45

50

T∞ [ eV

]

NSA+PL

2.300

4.610

9.210

Figure: ∆χ2 = χ

2− χ

2min

= 2.3, 4.61, and 9.21

Kirichenko et al. 2014

Multiwavelength spectrum of J0357+3205

15 16 17 18Log ν [ Hz ]

-4

-3

-2

-1

0

1L

og F

ν [ µ

Jy ]

-2 -1 0Log E [ keV]

-5

-4

-3

-2

-1

0

1

2

Log

Fν [

µJy

] GTCXMM and Chandra

Fermi

Sloan g’

Kirichenko et al. 2014

J1741−2054

02.0 17:42:00.0 58.0 56.0 41:54.0

53:0

0.0

30.0

-20:

54:0

0.0

30.0

55:0

0.0

Right ascension

Dec

linat

ion

PSR J1741-2054

Chandra/ACIS 0.7-8.0 keV

Karpova et al. 2014

The best-fit BB+PL model

−4

−3

−2

−1

Log

[ co

unts

s−1

keV

−1 ]

0 1 Log E [ keV ]

−0.02

−0.01

0.00

0.01

0.02

0.03

cou

nts

s−1 k

eV−1

Karpova et al. 2014

NH and Teff vs the distance

0.6 0.7 0.8 0.9 1.0 1.1D [ R13km kpc ]

1.0

1.1

1.2

1.3

1.4

1.5

1.6

1.7

NH [ 10

21 cm

−2 ]

0.6 0.7 0.8 0.9 1.0 1.1D [ R13km kpc ]

57

58

59

60

61

62

63

64

T [ eV

]

Figure: ∆χ2 = χ

2− χ

2min

= 2.3, 4.61, and 9.21

Karpova et al. 2014

Field of J0633+0632

52.0 48.0 44.0 6:33:40.0

34:0

0.0

6:33

:00.

032

:00.

031

:00.

0

Right ascension

Dec

linat

ion

Chandra/ACIS 0.3-8.0 keV

PSR J0633+0632pulsar

Galactic plane

1 deg

Monoceros Loop (SNR)

ROSETTE NEBULA (OB)

Summary

What have been done

◮ J1741 looks like forth Musketeer

◮ J0633 is probably cool and has an absorption feature

What to do next

◮ UV observations of J1741 (Hubble)

◮ XMM observations of J0633

Summary

What have been done

◮ J1741 looks like forth Musketeer

◮ J0633 is probably cool and has an absorption feature

What to do next

◮ UV observations of J1741 (Hubble)

◮ XMM observations of J0633