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A Three-Dimensional Analytical Model of the Interstellar Extinction within the Nearest Kiloparsec

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Abstract

We present a new version of our analytical model of the spatial interstellar extinction variations within the nearest kiloparsec from the Sun. This model treats the three-dimensional (3D) dust distribution as a superposition of three overlapping layers: (1) the layer along the Galactic midplane, (2) the layer in the Gould Belt, and (3) the layer passing through the Cepheus and Chamaeleon dust cloud complexes. In each layer the dust density decreases exponentially with increasing distance from the midplane of the layer. In addition, there are sinusoidal longitudinal extinction variations along the midplane of each layer. We have found the most probable values of 29 parameters of our model using four data sets: the 3D stellar reddening maps by Gontcharov and Mosenkov (2017), Lallement et al. (2019), and Green et al. (2019) and the extinctions inferred by Anders et al. (2022) for 993 291 giants from the Gaia Early Data Release 3. All of the data give similar estimates of the model parameters. The extinction for a star or a point in space is predicted by our model with an accuracy from \(\sigma(A_{\textrm{V}})=0.07\) to 0.37 for high and low Galactic latitudes, respectively. The natural fluctuations of the dust medium dominate in these values. When ignoring the fluctuations of the medium, the average extinction for an extended object (a galaxy, a star cluster, a dust cloud) or a small region of space is predicted by our model with an accuracy from \(\sigma(A_{\textrm{V}})=0.04\) to 0.15 for high and low Galactic latitudes, respectively. Green et al. (2019) and Anders et al. (2022) give in unison an estimate of \(A_{\textrm{V}}=0.12^{m}\) for the extinction at high latitudes across the whole Galactic dust half-layer above or below the Sun with the natural fluctuations of the medium \(\sigma(A_{\textrm{V}})=0.06^{m}\). If such a high estimate is subsequently confirmed, then it will require to explain how a substantial amount of dust ended up far from the Galactic midplane. Our model is a step in this explanation.

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Notes

  1. https://data.aip.de/projects/starhorse2021.html or https://cdsarc.cds.unistra.fr/viz-bin/cat/I/354

  2. http://argonaut.skymaps.info/

  3. https://cdsarc.cds.unistra.fr/viz-bin/cat/J/PAZh/43/521

  4. https://astro.acri-st.fr/gaia_dev/

  5. The Galactic rectangular coordinate system with the origin in the Sun and the \(X\), \(Y\), and \(Z\) axes directed toward the Galactic center, in the direction of Galactic rotation, and toward the Galactic north pole, respectively, is considered.

  6. Only 12 921 of the 993 291 AKQ22 giants (1.3\(\%\)) exhibit such a high extinction that is not predicted by our model.

  7. Figures 3 and 6 have different scale heights along the vertical axis.

  8. Nulling the extinctions within 40 pc of the Sun does not change the standard deviations of the \(A_{\textrm{V}}\) residuals and the correlation coefficients at all, since the extinctions here anyway are very close to zero.

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Authors and Affiliations

  1. Pulkovo Astronomical Observatory, Russian Academy of Sciences, 196140, St. Petersburg, Russia

    G. A. Gontcharov, A. V. Mosenkov, S. S. Savchenko, V. B. Il’in, A. A. Marchuk, A. A. Smirnov, P. A. Usachev & D. M. Polyakov

  2. Department of Physics and Astronomy, Brigham Young University, N283 ESC, Provo, UT 84602, USA

    A. V. Mosenkov & N. Hebdon

  3. St. Petersburg State University, 199034, St. Petersburg, Russia

    S. S. Savchenko, V. B. Il’in, A. A. Marchuk, A. A. Smirnov, P. A. Usachev & D. M. Polyakov

  4. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Karachai-Cherkessian Republic, Russia

    S. S. Savchenko & P. A. Usachev

  5. St. Petersburg State University of Aerospace Instrumentation, 190000, St. Petersburg, Russia

    V. B. Il’in

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  1. G. A. Gontcharov
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Gontcharov, G.A., Mosenkov, A.V., Savchenko, S.S. et al. A Three-Dimensional Analytical Model of the Interstellar Extinction within the Nearest Kiloparsec. Astron. Lett. 48, 578–600 (2022). https://doi.org/10.1134/S1063773722100024

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