Surface brightness profile of the Milky Way’s nuclear star cluster

By R. Schödel, A. Feldmeier, D. Kunneriath, S. Stolovy, N. Neumayer, P. Amaro-Seoane, Shogo Nishiyama. 2014

154 citations recorded by the source corpus.

Context. Although the Milky Way nuclear star cluster (MWNSC) was discovered more than four decades ago, several of its key properties have not been determined unambiguously up to now because of the strong and spatially highly variable interstellar extinction toward the Galactic centre. Aims. In this paper we aim at determining the shape, size, and luminosity/mass of the MWNSC. Methods. To investigate the properties of the MWNSC, we used Spitzer/IRAC images at 3:6 and 4:5 m, where interstellar extinction is at a minimum but the overall emission is still dominated by stars. We corrected the 4:5 m image for PAH emission with the help of the IRAC 8:0 m map and for extinction with the help of a [3:6 4:5] colour map. Finally, we investigated the symmetry of the

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/41b75b8c769dbd92d5f2200691e11f5838c0b8c4

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Citations in the corpus

Formation and Evolution of Compact-object Binaries in AGN Disks (2019, background): “Because the BH distribution extends to larger radii (e.g., Freitag et al. 2006; Antonini 2014; Feldmeier et al. 2014; Schödel et al. 2014; Generozov et al. 2018), preexisting binaries may not have the outer cutoff at ∼1 pc as in the LMXB observations.”
Masses and scaling relations for nuclear star clusters, and their co-existence with central black holes (2016, unknown): “For the MW NSC, we use mass and size estimates from Schödel et al. (2014),MNSC = (2.5± 0.4)× 107M , reff,NSC = 4.2 ± 0.4 pc.”
Greatly Enhanced Merger Rates of Compact-object Binaries in Non-spherical Nuclear Star Clusters (2017, background): “…regions of the Milky Way show that this region is dominated by a dense NC consisting of a population of old stars with a total mass of ∼ 3 × 107M⊙ (Schödel et al. 2014, 2017; Feldmeier-Krause et al. 2017) with most young stars residing inside ∼ 0.5 pc (Schödel et al. 2014, 2017;…”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, methodology): “Adapted from Schödel et al. (2014a) with permission c© ESO.”
Nuclear star clusters (2009, methodology): “The rotation of NSCs was investigated by Tsatsi et al. (2017), who found that their models could match the observed flattening (Schödel et al. 2014a), and rotation signature (Feldmeier et al. 2014) of the Milky Way NSC (Figs.”