A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

Zharikov, S. V.; Shibanov, Yu. A.; Zyuzin, D. A.; Mennickent, R. E.; Komarova, V. N.

doi:10.1051/0004-6361:200810429

Cited by 14 publications

(34 citation statements)

References 29 publications

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“…The η H ∝ η B empirical relationship derived from the plot (thick solid line) allows one to predict IR magnitudes for all pulsars that have been detected in the optical, but not yet in the near-IR, and vice versa. Based on the observed PSR J1124-5916 flux upper limits in the near-IR obtained here and in the optical provided by Zharikov et al (2008), we can constrain the pulsar position region on the efficiency plain (shaded region in Fig. 6) and conclude that its efficiencies are at least lower than those of younger pulsars.…”

Section: Pulsar Flux Upper Limits and Efficienciesmentioning

confidence: 57%

“…1). It is elongated in the same SE-NW direction as the torus-like part of the PWN in other spectral domains (e.g., Zharikov et al 2008). We are therefore confident that it is the real near-IR counterpart of the pulsar+PWN system.…”

Section: Pulsar+pwn Near-ir Counterpartmentioning

confidence: 64%

“…To verify our optical fluxes of the pulsar+PWN system obtained with the VLT (Zharikov et al 2008) we inspected the HST …”

Section: Hst Archival Datamentioning

confidence: 99%

“…It may be overestimated because of a possible contribution of unresolved stars located near the PWN boundary, but can be taken as a confident upper limit on the system flux in this band. The measured and available observed counterpart magnitudes, fluxes in physical units, and de-reddened fluxes for a most plausible interstellar extinction range of 1. m 86 < ∼ A V < ∼ 2. m 10 (Zharikov et al 2008) are collected in Table 2.…”

Section: Pulsar+pwn Near-ir Counterpartmentioning

confidence: 99%

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The PSR J1124-5916 wind nebula in the near-infrared

Zharikov

Zyuzin²,

Shibanov

et al. 2013

A&A

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Context. The young radio pulsar J1124-5916 is associated with the Cas A like supernova remnant G292.0+1.8. It powers a compact torus-like pulsar wind nebula with a jet first detected in X-rays and then identified in the optical and mid-infrared. Aims. We carried out deep near-infrared observations of the pulsar field to identify the pulsar and its nebula in this range. Methods. The direct-imaging mode of the NACO adaptive optics instrument at the ESO VLT in the H and K s bands was used.Results. We detected a faint, H = 21.30(10) and K s = 20.45(10), extended elliptical object in both bands, whose center position is consistent with the X-ray position of the pulsar. The morphology of the object and the orientation of its major axis agree well with those observed for the pulsar torus-like nebula in the mid-infrared, optical, and X-rays. This suggests that it is the near-infrared counterpart of the nebula. The measured fluxes compiled with the data in other ranges show a complicated unabsorbed power-law spectrum of the torus-like nebula with several steep breaks between the near-infrared and mid-infrared, the optical and X-rays, and possibly in the mid-infrared. This implies a multiple relativistic particle population responsible for the synchrotron emission of the nebula in different spectral ranges. We have not resolved the pulsar counterpart from its nebula and place only upper limits on its brightness, H ≥ 23.9 and K s ≥ 22.7. Based on that, its contribution to the total near-infrared flux of the pulsar+nebula system is ≤10%, which is comparable with the expected contribution in the optical.

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Section: Pulsar Flux Upper Limits and Efficienciesmentioning

confidence: 57%

Section: Pulsar+pwn Near-ir Counterpartmentioning

confidence: 64%

“…To verify our optical fluxes of the pulsar+PWN system obtained with the VLT (Zharikov et al 2008) we inspected the HST …”

Section: Hst Archival Datamentioning

confidence: 99%

Section: Pulsar+pwn Near-ir Counterpartmentioning

confidence: 99%

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The PSR J1124-5916 wind nebula in the near-infrared

Zharikov

Zyuzin²,

Shibanov

et al. 2013

A&A

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“…A common origin of the optical and X-ray nonthermal components independently on pulsar age and the presence of spectral breaks was proposed by Zharikov et al (2004Zharikov et al ( , 2005 based on a strong correlation of the optical and X-ray nonthermal luminosities for a set of ordinary pulsars detected in the optical and X-ray domains (see also Zavlin & Pavlov 2004b). Analysis of the phase aligned optical and X-ray pulse profiles would be useful to verify this hypothesis for Geminga, as it has been partly done for PSR B0656+14 .…”

Section: Multiwavelength Spectramentioning

confidence: 98%

Subaru optical observations of the two middle-aged pulsars PSR B0656+14 and Geminga

Shibanov¹,

Zharikov²,

Komarova

et al. 2006

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Aims. We carried out a deep subarcsecond BRI imaging of the two middle-aged pulsars to establish their properties in the optical range. Methods. Astrometry and photometry methods are applied to identify the pulsars and to measure their fluxes. We also reanalyze archival ESO/NTT and HST broadband data and find that some published fluxes for Geminga were estimated inaccurately. The resulting dereddened broadband spectra in the near-IR-UV range are analyzed and compared with available data from the radio through gamma-rays. Results. Both pulsars are detected at > ∼ 10σ level. Geminga is for the first time reliably detected in the I band with a magnitude of 25. m 10 ± 0.14. The dereddened spectra of both pulsars are remarkably similar to each other and show significant flux increases towards the far-UV and near-IR, and a wide flux excess in V − I bands. This suggests a multicomponent structure of the optical emission. The nonthermal power law component of the pulsar magnetospheric origin dominates in the most part of the optical range. For PSR B0656+14 it is compatible with a low energy extension of the power law tail seen in hard X-rays. For Geminga the respective extension overshoots by a factor of 100 the nonthermal optical flux, which has a less steep spectral slope than in X-rays. This implies a spectral break at a photon energy ∼1 keV. The flux increases towards the far-UV are compatible with contributions of the Rayleigh-Jeans parts of the blackbody components from whole surfaces of the neutron stars dominating in soft X-rays. The V − I excess, which is most significant for PSR B0656+14, suggests a third spectral component of still unidentified origin. Faint, a few arcseconds in size nebulae extended perpendicular to the proper motion directions of the pulsars, are seen around both objects in our deepest I band images. They can be optical counterparts of the bow-shock head of Geminga and of the tentative pulsar wind nebula of PSR B0656+14 observed in X-rays.

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The G292.0+1.8 pulsar wind nebula in the mid-infrared

Zyuzin

Danilenko²,

Zharikov³

et al. 2009

A&A

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Context. G292.0+1.8 is a Cas A-like supernova remnant that contains the young pulsar PSR J1124-5916 powering a compact toruslike pulsar wind nebula visible in X-rays. A likely counterpart to the nebula has been detected in the optical VRI bands. Aims. To confirm the counterpart candidate nature, we examined archival mid-infrared data obtained with the Spitzer Space Telescope. Methods. Broad-band images taken at 4.5, 8, 24, and 70 μm were analyzed and compared with available optical and X-ray data. Results. The extended counterpart candidate is firmly detected in the 4.5 and 8 μm bands. It is brighter and more extended in the bands than in the optical, and its position and morphology agree well with the coordinates and morphology of the torus-like pulsar wind nebula in X-rays. The source is not visible in 24 and 70 μm images, which are dominated by bright emission from the remnant shell and filaments. We compiled the infrared fluxes of the nebula, which probably contains a contribution from an unresolved pulsar in its center, with the optical and X-ray data. The resulting unabsorbed multiwavelength spectrum is described by power laws of significantly steeper slope in the infrared-optical than in X-rays, implying a double-knee spectral break between the optical and X-rays. The 24 and 70 μm flux upper limits suggest a second break and a flatter spectrum at the long wavelength limit. These features are common to two other pulsar wind nebulae associated with the remnants B0540-69.3 and 3C 58 and observed in all three ranges. Conclusions. The position, morphology, and spectral properties of the detected source allow us to confirm that it is the infrared-optical counterpart to both the pulsar and its wind nebula system in the G292.0+1.8 supernova remnant.

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A likely optical counterpart of the G292.0+1.8 pulsar wind nebula

Cited by 14 publications

References 29 publications

The PSR J1124-5916 wind nebula in the near-infrared

The PSR J1124-5916 wind nebula in the near-infrared

Subaru optical observations of the two middle-aged pulsars PSR B0656+14 and Geminga

The G292.0+1.8 pulsar wind nebula in the mid-infrared

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