The Vela pulsar in the near-infrared

Shibanov, Yu. A.; Koptsevich, A. B.; Sollerman, J.; Lundqvist, Peter

doi:10.1051/0004-6361:20030652

Cited by 45 publications

(101 citation statements)

References 35 publications

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“…The pulsar's spectrum is characterized by a flat power-law with spectral index α = −0.04 ± 0.04, consistent with the values derived from broad-band photometry (Mignani & Caraveo 2001;Shibanov et al 2003;Kargaltsev & Pavlov 2007). We have compared the newly derived optical spectral index of Vela with those of all rotation-powered INSs for which a power-law component has been identified in the optical/IR spectrum.…”

Section: Discussionsupporting

confidence: 76%

The optical spectrum of the Vela pulsar

Mignani¹,

Zharikov²,

Caraveo³

2007

A&A

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Context. Our knowledge of the optical spectra of Isolated Neutron Stars (INSs) is limited by their intrinsic faintness. Among the fourteen optically identified INSs, medium resolution spectra have been obtained only for a handful of objects. No spectrum has been published yet for the Vela pulsar (PSR B0833-45), the third brightest (V = 23.6) INS with an optical counterpart. Optical multi-band photometry underlines a flat continuum. Aims. In this work we present the first optical spectroscopy observations of the Vela pulsar, performed in the 4000−11 000 Å spectral range. Methods. Our observations have been performed at the ESO Very Large Telescope (VLT) using the FORS2 instrument.Results. The spectrum of the Vela pulsar is characterized by a flat power-law F ν ∝ ν −α with α = −0.04 ± 0.04 (4000−8000 Å), which compares well with the values obtained from broad-band photometry. This confirms, once more, that the optical emission of Vela is entirely of magnetospheric origin. Conclusions. The comparison between the optical spectral indeces of rotation-powered INSs does not show evidence for a spectral evolution, suggesting that, as in the X-rays, the INS aging does not affect the spectral properties of the magnetospheric emission. At the same time, the optical spectral indeces are found to be nearly always flatter then the X-rays ones, clearly suggesting a general spectral turnover at lower energies.

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Section: Discussionsupporting

confidence: 76%

The optical spectrum of the Vela pulsar

Mignani¹,

Zharikov²,

Caraveo³

2007

A&A

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“…K-band flux values in italics have been derived from the extrapolation of the J and H-band fluxes. (1) Sollerman (2003); (2) radio dispersion measure, Cordes & Lazio (2002); (3) Sollerman et al (2000); (4) Kaplan & Moon (2006); (5) Lortet et al (1987); (6) Shibanov et al (2003); (7) radio parallax, Dodson et al (2003); (8) Mignani et al (2003); (9) Koptsevich et al (2001); (10) radio parallax, Brisken et al (2003); (11) Pavlov et al (1997); (12) optical parallax, Caraveo et al (1996); (13) Kargaltsev et al (2005); (14) (2002); (17) Gaensler et al (2005); (18) Israel et al (2003); (19) Israel et al (2004); (20) Rea et al (2004); (21) Hulleman et al (2001); (22) Kothes et al (2002); (23) Woods et al (2004); (24) Israel et al (2005); (25) + revised downward to 2.5 kpc (Gotthelf & Halpern 2005). Table 2 as a function of the NSs rotational energy lossĖ.…”

Section: Resultsmentioning

confidence: 99%

VLT/NACOobservations of the high-magnetic field radio pulsar PSR J1119-6127

Mignani

Perna

Rea

et al. 2007

A&A

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Context. Recent radio observations have unveiled the existence of a number of radio pulsars with spin-down derived magnetic fields in the magnetar range. However, their observational properties appear to be more similar to those of the classical radio pulsars than to the magnetars's ones. Aims. To shed light on this puzzle we first have to determine whether the spin-down derived magnetic field values for these radio pulsars are indeed representative of the actual neutron star magnetic field or if they are polluted, e.g. by the effects of a torque from a fallback disk. Methods. To investigate this possibility, we have performed deep IR (J, H, K s bands) observations of one of these high magnetic field radio pulsars (PSR J1119-6127) with the ESO VLT to search for IR emission which can be associated with a disk. Results. No IR emission is detected from the pulsar position down to J ∼ 24, H ∼ 23 and K s ∼ 22. Conclusions. By comparing our flux upper limits with the predictions of fallback disk models, we have found that we can only exclude the presence of a disk with accretion rateṀ > ∼ 3 × 10 16 g s −1 . This lower limit cannot rule out the presence of a substantial disk torque on the pulsar, which would then lead to overestimate the value of the magnetic field inferred from P andṖ. We have also compared the upper limit on the IR luminosity of PSR J1119-6127 with the IR luminosities of rotation-powered pulsars and magnetars. We found that, while magnetars are intrinsically more efficient IR emitters than rotation-powered pulsars, possibly because of their higher magnetic field, the relatively low IR emission efficiency of PSR J1119-6127 suggests that it is more similar to the latters than to the former.

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“…Our upper limits show that the real optical fluxes of the pulsar cannot significantly exceed the extrapolation of its X-ray spectrum to the optical range. This is typical for non-thermal radiation from pulsars detected in the optical and X-rays, including the Crab (Sandberg & Sollerman 2009), Vela (Shibanov et al 2003), some middle-aged (Shibanov et al 2006), and old pulsars (Zharikov et al 2004;Zavlin & Pavlov 2004).…”

Section: Multi-wavelength Spectrum and Luminositiesmentioning

confidence: 87%

Deep optical imaging of theγ-ray pulsar J1048–5832 with the VLT

Danilenko¹,

Kirichenko

Sollerman

et al. 2013

A&A

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Context. PSR J1048-5832 is a young radio-pulsar that has recently been detected in γ-rays with Fermi, and also in X-rays with Chandra and XMM-Newton. It powers a compact pulsar wind nebula visible in X-rays and is in many ways similar to the Vela pulsar. Aims. We present deep optical observations made with the ESO Very Large Telescope to search for optical counterparts of the pulsar and its nebula and to explore their multi-wavelength emission properties. Methods. The data were obtained in the V and R bands and were compared with archival data in other spectral domains. Results. We do not detect the pulsar in the optical and derive informative upper limits of R 28. m 1 and V 28. m 4 for its brightness. Using a red-clump star method, we estimate an interstellar extinction towards the pulsar of A V ≈ 2 mag, which is consistent with the absorbing column density derived from X-rays. The respective distance agrees with the dispersion measure distance. We reanalysed the Chandra X-ray data and compared the dereddened upper limits with the unabsorbed X-ray spectrum of the pulsar. We find that regarding its optical-X-ray spectral properties this γ-ray pulsar is not distinct from other pulsars detected in both ranges. However, like the Vela pulsar, it is very inefficient in the optical and X-rays. Among a dozen optical sources overlapping with the pulsar X-ray nebula we find one with V ≈ 26. m 9 and R ≈ 26. m 3, whose colour is slightly bluer than that of the field stars and is consistent with the peculiar colours typical for pulsar nebula features. It positionally coincides with a relatively bright feature of the pulsar X-ray nebula, resembling the Crab wisp and is located in ∼2 from the pulsar. We suggest this source as a counterpart candidate to the feature. Conclusions. Based on the substantial interstellar extinction towards the pulsar and its optical inefficiency, additional optical studies should be carried out at longer wavelengths.

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The Vela pulsar in the near-infrared

Cited by 45 publications

References 35 publications

The optical spectrum of the Vela pulsar

The optical spectrum of the Vela pulsar

VLT/NACOobservations of the high-magnetic field radio pulsar PSR J1119-6127

Deep optical imaging of theγ-ray pulsar J1048–5832 with the VLT

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