the vela and geminga pulsars in the mid-infrared · introduction the crab pulsar the axps vela and...

The Vela and Geminga pulsars in the mid-infrared

A. A. Danilenko1, D. A. Zyuzin1, Yu. A. Shibanov1,2

& S. V. Zharikov3

1Ioffe Institute, St. Petersburg, Russia

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

3Observatorio Astronomico Nacional SPM, UNAM, Mexico

Outline

IntroductionThe Crab pulsarThe AXPsVela and Geminga

ResultsIdentification of the pulsars in mid-IRPhotometry

DiscussionThe dust discAn unresolved PWN structure

Conclusions

The Crab pulsar and the nearby knot

Near-IR images and Optical/IR SED of the Crab (Sandberg & Sollerman

(2009)). The pulsar and the knot are marked by the blue and red ticks

consecuently. The Crab mid-IR fluxes are compatible with the spectral

extrapolation from the optical range if we account for contribution from

the knot which is not spatialy resolved from the pulsar in the mid-IR.

Outline




Conclusions

The AXPs

4U 0142+61

Wang, Chakrabarty & Kaplan(2006)

1E 2259+586

Kaplan et al. (2009)

Outline




Conclusions

Vela and Geminga

Vela,

PSR B0833−45;age ∼ 104 yr;distance to, 287+19

−17 pc;associated with SNR G263.9−3.3;Crab-like PWN detected in X-raysonly and some PWN features inγ-rays;

Geminga,

PSR J0633+1746;age ∼ 105 yr;distance to, 250+120

−60 pc;not associated with any SNR;bow shock PWN detected inX-rays and γ-rays;

Outline




Conclusions

Identification of the Vela pulsar

21.5 21.0 20.5 8:35:20.0 19.5RA

psr

5.8 microns

26.0

28.0

30.0

32.0

34.0

36.0

38.0

-45:10:40.0

42.0

44.0

46.0

Dec

psr

J

21.5 21.0 20.5 8:35:20.0 19.5

24.0

26.0

28.0

-45:10:30.0

32.0

34.0

36.0

38.0

40.0

42.0

44.0

RA

Dec

psr

3.6 microns

psr

counter-jet?

o1

H

Figure: The near-IR images (Shibanov et al. (2003)) compared with theSpitzer data. The pulsar counterpart is marked by a tick line and thearrow shows the direction of its proper motion.

Identification of the Geminga pulsar

54.8 54.4 6:33:54.0 53.6

22.0

18.0

14.0

17:46:10.0

06.0

RA

psr

4.5 microns

54.8 54.4 6:33:54.0 53.6

25.0

20.0

15.0

10.0

05.0

17:46:00.0

RA

Dec

psr

3.6 microns

54.8 54.4 6:33:54.0 53.6

22.0

18.0

14.0

17:46:10.0

06.0D

ec

psr

I

54.8 54.4 6:33:54.0 53.6

25.0

17:46:20.0

15.0

10.0

05.0

F160W

psr

Figure: The Spitzer images vs the Subaru and HST ones (Shibanov et al.(2006)). The cross marks the pulsar position at the epoch the I-bandimage was obtained in. A tick line and the arrow marks the pulsarposition and the direction of its proper motion.

Outline




Conclusions

Crab, Vela and Geminga

0

1

2

Log

Fν

[ µJy

]

Js

U

BF67

5WF81

4W

G140

13 13.5 14 14.5 15Log ν [ Hz ]

-1

0

1

2 Geminga

24 µm

3.6 µm

4.5 µm

5.8 µm

8 µm

Spitzer/MIPS

F160W

F110W

I R

F555W

F430WF34

2W

F195F25

S

3

3.5

4

Vela

Crab

Spitzer/IRAC

K H J

Unabsorbed spectra of the Crab,

Vela and Geminga pulsars from the

mid-IR to the optical-UV. Crab:

optical and near-IR (Sandberg &

Sollerman (2009)); mid-IR (Temim

et al. (2009)); Vela: UV, optical,

near-IR (Romani et al. (2005),

Mignani et al. (2007), Shibanov et

al. (2003)); Geminga: UV,

optical/near-IR (Kargaltsev et al.

(2005), Shibanov et al. (2006));

optical spectrum (Martin et al.

(1998))

Multiwavelength spectrum: Vela

9 12 15 18 21 24 27Log ν [ Hz ]

-9

-6

-3

0

3

6L

og F

ν [

µJy

]

Chandraatm+PL

RXTE

OSSECOMPTEL

EGRET

VLT+HST+NTT

Spitzer (IRAC + MIPS)

Fermi LAT

-9 -6 -3 0 3 6 9Log E [ keV ]

Vela

Figure: The mid-IR fluxes are marked by a red circles.

Multiwavelength spectrum: Geminga

9 12 15 18 21 24 27Log ν [ Hz ]

-9

-6

-3

0

3

66L

og F

ν [

µJy

]

-9 -6 -3 0 3 6 9Log E [ keV ]

Geminga

radio, upper limits

radio, M&M

Tata group

Whipple

EGRET, α = −0.5

OSSECOMPTEL

OSSE

RXTE

hard BB

soft BB

PL

NIR+optical+FUV


Chandra

Fermi-LAT

PL+sBB+hBB

Figure: The mid-IR fluxes are marked by a red circles.

Outline




Conclusions

Possible contribution from the dust disc

13 13.5 14 14.5 15Log ν [ Hz ]

-1

0

1

2

Log

Fν [

µJy

]

Vela

irradia

ted d

isk

power-law,α = 0.01

Rin = 0.28 +/- 0.05 R

sun

Tin = 834 +/- 63 K

irradiated disk:

Rex = 1.4 +/- 0.4 R

sun

Figure: The spectral fit of the Vela pulsar optical/IR SED by irradiatedpassive dust disc model (Vrtilek et al. (1990)). The solid line is thebest-fitting result and the hatched region shows 1σ uncertainty of the fit.Here we assume that the mid-IR pulsar fluxes are described by power-lawextrapolated from the optical-UV range.

Multiwavelength spectrum of Vela + disc

9 12 15 18 21 24 27Log ν [ Hz ]

-9

-6

-3

0

3

6L

og F

ν [

µJy

]

Chandraatm+PL

RXTE

OSSECOMPTEL

EGRET

VLT+HST+NTT


Fermi LAT

-9 -6 -3 0 3 6 9Log E [ keV ]

Vela

Figure: The same spectral fit as seen on the multiwavelength spectrum.

Outline




Conclusions

The Vela PWN at near-IR

Figure: The near-IR image of the Vela PWN (Shibanov et al. (2003)).The pulsar and the PWN features, o1 and counter-jet, are marked by theblue and red arrows consequently.

Whether the PWN structures can contribute significantly?

13 13.5 14 14.5 15Log ν [ Hz ]

-1

0

1

2

Log

Fν [

µJy

]

o1, a PWN knot?

Vela

SE-feature, a PWN counter jet?

The fluxes of the PWN features, named o1 and conter-jet, are shown. If

we extrapolate two point near-IR spectra of the features to mid-IR band,

so we find that in mid-IR the fluxes of the features must be of same order

as the pulsar fluxes. Bear in mind possible variability of the counter-jet

we may conclude that this features can, at least partially, explain the

observed excess.

Conclusions

◮ The detections of the Vela and Geminga pulsars as well asrecent detections of several Crab-like PWNe (B0540, B1124,3C 58 and G21.5) reveal strong emission excess in the mid-IRband, that was rather difficult to expect in advance.

◮ The question arise: What is the nature of the exesess? Is itthe sign of the hypothetical fall-back discs?

◮ Further studies of these and other pulsars in the mid-IR andespecially submillimetre bands are necessery to get the answer.

Thank you!

The Vela PWN

The mid-IR image incomparison with theChandra one (Helfand etal. (2001)). There is nocounterpart of the X-raytorus-like structure in themid-IR.

The Vela Plerion

40.0 30.0 20.0 10.0 8:35:00.0 50.0 40.0 34:30.0

06:00.0

08:00.0

-45:10:00.0

12:00.0

14:00.0

16:00.0

18:00.0

20:00.0

RA

HRC-I 0.3-10 keV

50.0 40.0 30.0 20.0 10.0 8:35:00.0 50.0 40.0 34:30.0

06:00.0

08:00.0

-45:10:00.0

12:00.0

14:00.0

16:00.0

18:00.0

20:00.0

RA

Dec

IRAC 8 micron

Figure: The large scale structure of the Vela PWN at 8 µm and softX-rays. East boundary of the X-ray plerion correlate with the westboundary of the a brigth extended emission visible in mid-IR.

The Geminga PWN

Figure: Comparison of the mid-IR and HST/NICMOS near-IR (Shibanovet al. (2006)) images with the Chandra ones (Pavlov et al. (2010)).

The Geminga PWN

SPITZER / IRAC 3.6 micron

3" 0.5"

HST / NICMOS 1.6 micron

0.3-10 keVChandra / ACIS-I

5"

0.8 micronSUBARU / I-band

1"

Figure: The transformation of the compact PWN from X-rays, throughoptical/near-IR, to the mid-IR.

Large-scale PWN structure

55.0 54.5 54.0 53.5 6:33:53.0 52.5 52.0 51.5

30.0

25.0

20.0

15.0

10.0

05.0

17:46:00.0

55.0

50.0

45.0

RA

Dec

5.8 micron

C

BY

s2

s1

54.5 54.0 53.5 6:33:53.0 52.5 52.0 51.5

25.0

20.0

15.0

10.0

05.0

17:46:00.0

55.0

45:50.0

RA

ACIS-I

C

BY

s2

s1

Figure: The extended tail at 5.8 µm and X-rays.

the vela and geminga pulsars in the mid-infrared · introduction the crab pulsar the axps vela and...

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