Near-infrared observations of PSR J1357−6429

Zyuzin, D.; Zharikov, S. V.; Shibanov, Yu. A.; Danilenko, A.; Mennickent, R. E.; Kirichenko, A.

doi:10.1093/mnras/stv2401

Cited by 10 publications

(9 citation statements)

References 20 publications

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“…The power-law slope inferred for the DSO, see Eq. (1), is qualitatively consistent with the observations of neutron stars in near-infrared bands (Mignani et al 2012;Zharikov et al 2013;Zyuzin et al 2016), however, it appears to be steeper than for observed pulsars (Mignani et al 2012), which have the mean spectral index α ≈ 0.7.…”

Section: Possible Non-thermal Origin Of the Sed: Nir-"excess"supporting

confidence: 88%

“…The qualitative behaviour of the continuum radiation of the DSO is similar to the SED of few young pulsars detected in NIR domains (Mignani et al 2012;Zharikov et al 2013;Zyuzin et al 2016) that are dominated by magnetospheric synchrotron radiation. Moreover, they exhibit a significant linear polarized emission with the polarization degree of a few 10% (Zajczyk et al 2012).…”

Section: Summary Of Observational Constraintssupporting

confidence: 70%

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Nature of the Galactic centre NIR-excess sources

Britzen

Eckart

Shahzamanian

et al. 2017

A&A

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Context. The Dusty S-cluster Object (DSO/G2) orbiting the supermassive black hole (Sgr A*) in the Galactic centre has been monitored in both near-infrared continuum and line emission. There has been a dispute about the character and the compactness of the object: interpreting it as either a gas cloud or a dust-enshrouded star. A recent analysis of polarimetry data in K s -band (2.2 µm) allows us to put further constraints on the geometry of the DSO. Aims. The purpose of this paper is to constrain the nature and the geometry of the DSO. Methods. We compare 3D radiative transfer models of the DSO with the NIR continuum data including polarimetry. In the analysis, we use basic dust continuum radiative transfer theory implemented in the 3D Monte Carlo code Hyperion. Moreover, we implement analytical results of the two-body problem mechanics and the theory of non-thermal processes.Results. We present a composite model of the DSO -a dust-enshrouded star that consists of a stellar source, dusty, optically thick envelope, bipolar cavities, and a bow shock. This scheme can match the NIR total as well as polarized properties of the observed spectral energy distribution (SED). The SED may be also explained in theory by a young pulsar wind nebula that typically exhibits a large linear polarization degree due to magnetospheric synchrotron emission. Conclusions. The analysis of NIR polarimetry data combined with the radiative transfer modelling shows that the DSO is a peculiar source of compact nature in the S cluster (r 0.04 pc). It is most probably a young stellar object embedded in a non-spherical dusty envelope, whose components include optically thick dusty envelope, bipolar cavities, and a bow shock. Alternatively, the continuum emission could be of a non-thermal origin due to the presence of a young neutron star and its wind nebula. Although there has been so far no detection of X-ray and radio counterparts of the DSO, the analysis of the neutron star model shows that young, energetic neutron stars similar to the Crab pulsar could in principle be detected in the S cluster with current NIR facilities and they appear as apparent reddened, near-infrared-excess sources. The searches for pulsars in the NIR bands can thus complement standard radio searches, which can put further constraints on the unexplored pulsar population in the Galactic centre. Both thermal and non-thermal models are in accordance with the observed compactness, total as well polarized continuum emission of the DSO.

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Section: Possible Non-thermal Origin Of the Sed: Nir-"excess"supporting

confidence: 88%

Section: Summary Of Observational Constraintssupporting

confidence: 70%

Nature of the Galactic centre NIR-excess sources

Britzen

Eckart

Shahzamanian

et al. 2017

A&A

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“…Furthermore, candidate counterparts have been found for PSR J0205+6449 (Moran et al 2013) and PSR J1357−6429 (Zyuzin et al 2016). Here, we found a candidate counterpart to another γ-ray pulsar, PSR J1741−2054.…”

Section: Discussionsupporting

confidence: 57%

“…PSR J1741−2054 would then be the third γ-ray pulsar discovered by Fermi for which a candidate optical/ infrared counterpart has been found, after PSR J0205+6449 (Moran et al 2013) and PSR J1357−6429 (Zyuzin et al 2016). Multi-epoch optical observations will allow us to measure the proper motion of the PSR J1741−2054 candidate counterpart and confirm the optical identification, whereas multi-band photometry will be needed to determine the pulsar spectrum in the optical.…”

Section: Discussionmentioning

confidence: 99%

A CANDIDATE OPTICAL COUNTERPART TO THE MIDDLE AGED Γ-Ray PULSAR PSR J1741–2054*

Mignani

Testa

Marelli

et al. 2016

ApJ

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We carried out deep optical observations of the middle aged γ-ray pulsar PSR J1741−2054 with the Very Large Telescope (VLT). We identified two objects, of magnitudes m v = 23.10 ± 0.05 and m v = 25.32 ± 0.08, at positions consistent with the very accurate Chandra coordinates of the pulsar, the faintest of which is more likely to be its counterpart. From the VLT images we also detected the known bow-shock nebula around PSR J1741 −2054. The nebula is displaced by ∼0 9 (at the 3σ confidence level) with respect to its position measured in archival data, showing that the shock propagates in the interstellar medium consistently with the pulsar proper motion. Finally, we could not find evidence of large-scale extended optical emission associated with the pulsar wind nebula detected by Chandra, down to a surface brightness limit of ∼28.1 mag arcsec −2 . Future observations are needed to confirm the optical identification of PSR J1741−2054 and characterize the spectrum of its counterpart.

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“…Another handful of γ-ray pulsars have been observed after their discovery by Fermi, but not detected yet, with 10mclass telescopes: PSR J1357−6429 (Mignani et al 2011), PSR J1028−5819 (Mignani et al 2012), PSR J1048−5832 (Razzano et al 2013;Danilenko et al 2013), PSR J0007+7303 , PSR J0357+3205 (De Luca et al 2011;Kirichenko et al 2014), and PSR J2021+3651 (Kirichenko et al 2015). Recently, PSR J1357−6429 might have been identified in the near infrared (Zyuzin et al 2016).…”

Section: Introductionmentioning

confidence: 99%