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• W3102976624 abstract "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: it being interpreted as either a gas cloud or a dust-enshrouded star. A recent analysis of polarimetry data in K s -band (2.2 μ m) 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 compared 3D radiative transfer models of the DSO with the near-infrared (NIR) continuum data including polarimetry. In the analysis, we used basic dust continuum radiative transfer theory implemented in the 3D Monte Carlo code Hyperion. Moreover, we implemented 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." @default.
• W3102976624 created "2020-11-23" @default.
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• W3102976624 date "2017-04-12" @default.
• W3102976624 modified "2023-10-16" @default.
• W3102976624 title "Nature of the Galactic centre NIR-excess sources. I. What can we learn from the continuum observations of the DSO/G2 source?" @default.
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• W3102976624 cites W1643132601 @default.
• W3102976624 cites W1648002701 @default.
• W3102976624 cites W1672766972 @default.
• W3102976624 cites W1879383897 @default.
• W3102976624 cites W1966374563 @default.
• W3102976624 cites W1968655978 @default.
• W3102976624 cites W1972518244 @default.
• W3102976624 cites W1973820399 @default.
• W3102976624 cites W1974689993 @default.
• W3102976624 cites W1975864094 @default.
• W3102976624 cites W1985130111 @default.
• W3102976624 cites W2001464283 @default.
• W3102976624 cites W2016573758 @default.
• W3102976624 cites W2016598507 @default.
• W3102976624 cites W2022854803 @default.
• W3102976624 cites W2053680061 @default.
• W3102976624 cites W2061041487 @default.
• W3102976624 cites W2061511714 @default.
• W3102976624 cites W2061820060 @default.
• W3102976624 cites W2070531397 @default.
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• W3102976624 cites W2099746650 @default.
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• W3102976624 cites W2109112103 @default.
• W3102976624 cites W2110284565 @default.
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• W3102976624 cites W2123042076 @default.
• W3102976624 cites W2123710893 @default.
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• W3102976624 cites W2133983488 @default.
• W3102976624 cites W2143916380 @default.
• W3102976624 cites W2152812952 @default.
• W3102976624 cites W2154255185 @default.
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• W3102976624 cites W2203396098 @default.
• W3102976624 cites W2219329309 @default.
• W3102976624 cites W2242848969 @default.
• W3102976624 cites W2255893236 @default.
• W3102976624 cites W2262046936 @default.
• W3102976624 cites W2269513315 @default.
• W3102976624 cites W2294479944 @default.
• W3102976624 cites W2301065891 @default.
• W3102976624 cites W2318791194 @default.
• W3102976624 cites W2602417451 @default.
• W3102976624 cites W2950586646 @default.
• W3102976624 cites W2962780378 @default.
• W3102976624 cites W2964088722 @default.
• W3102976624 cites W3020956034 @default.
• W3102976624 cites W3082207194 @default.
• W3102976624 cites W3099128292 @default.
• W3102976624 cites W3099549883 @default.
• W3102976624 cites W3100035323 @default.
• W3102976624 cites W3100614081 @default.
• W3102976624 cites W3100866521 @default.
• W3102976624 cites W3101686352 @default.
• W3102976624 cites W3101713755 @default.
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• W3102976624 cites W3104526586 @default.
• W3102976624 cites W3105023707 @default.
• W3102976624 cites W3105047227 @default.
• W3102976624 cites W3105633837 @default.
• W3102976624 cites W3121515717 @default.
• W3102976624 cites W3123458820 @default.
• W3102976624 cites W2144619025 @default.
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