<p>We report results on the radial velocity dispersion profile built out to the outskirts of NGC 4147, a Milky Way globular cluster with detected strong tidal tails. The cluster was chosen to probe, from an observational point of view, recent simulations that suggest that rising velocity dispersion profiles at large distances from the clusters’ centers would be seen in globular clusters without tidal tails. From GEMINI@GMOS spectra, centered in the infrared Ca II triplet region, of selected stars located along the onset of NGC 4147’s tidal tails, we measured their radial velocities and overall metallicities. The derived metallicities were used to ultimately assess the highly-ranked cluster candidates of 9 stars, located between <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10079_Article_IEq1.gif" Format="GIF" Height="6" Rendition="HTML" Resolution="72" Type="Linedraw" Width="17" /> </InlineMediaObject> <EquationSource Format="TEX">$\sim $</EquationSource> <EquationSource Format="MATHML"><math> <mo>∼</mo> </math></EquationSource> </InlineEquation>7 and 33 pc from the cluster’s center, suitable for testing the aforementioned simulation. We complemented the present radial velocities with others available in the literature for the cluster’s members, and built a cluster velocity dispersion profile, which suggests a mostly flat or slightly rising profile at large distances from the cluster’s center. This outcome confirms that kinematically hot outermost cluster stars are seen in NGC 4147, which disproves the recent model predictions. Nevertheless, the mean velocity dispersion of the outermost cluster’s stars agrees with NGC 4147 being formed in a <InlineEquation ID="IEq2"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10079_Article_IEq2.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="23" /> </InlineMediaObject> <EquationSource Format="TEX">$10^8$</EquationSource> <EquationSource Format="MATHML"><math> <msup> <mn>10</mn> <mn>8</mn> </msup> </math></EquationSource> </InlineEquation>–<InlineEquation ID="IEq3"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10079_Article_IEq3.gif" Format="GIF" Height="16" Rendition="HTML" Resolution="72" Type="Linedraw" Width="23" /> </InlineMediaObject> <EquationSource Format="TEX">$10^9$</EquationSource> <EquationSource Format="MATHML"><math> <msup> <mn>10</mn> <mn>9</mn> </msup> </math></EquationSource> </InlineEquation> <InlineEquation ID="IEq4"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="12036_2025_10079_Article_IEq4.gif" Format="GIF" Height="17" Rendition="HTML" Resolution="72" Type="Linedraw" Width="28" /> </InlineMediaObject> <EquationSource Format="TEX">$\hbox {M}_\odot $</EquationSource> <EquationSource Format="MATHML"><math> <msub> <mtext>M</mtext> <mo>⊙</mo> </msub> </math></EquationSource> </InlineEquation> dwarf galaxy with a cored dark matter profile that was later accreted to the Milky Way.</p>

On the dark matter formation scenario of NGC 4147

期刊论文
发表日期：

2025年7月26日

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Andrés E. Piatti

摘要

We report results on the radial velocity dispersion profile built out to the outskirts of NGC 4147, a Milky Way globular cluster with detected strong tidal tails. The cluster was chosen to probe, from an observational point of view, recent simulations that suggest that rising velocity dispersion profiles at large distances from the clusters’ centers would be seen in globular clusters without tidal tails. From GEMINI@GMOS spectra, centered in the infrared Ca II triplet region, of selected stars located along the onset of NGC 4147’s tidal tails, we measured their radial velocities and overall metallicities. The derived metallicities were used to ultimately assess the highly-ranked cluster candidates of 9 stars, located between $\sim $ $\sim$ 7 and 33 pc from the cluster’s center, suitable for testing the aforementioned simulation. We complemented the present radial velocities with others available in the literature for the cluster’s members, and built a cluster velocity dispersion profile, which suggests a mostly flat or slightly rising profile at large distances from the cluster’s center. This outcome confirms that kinematically hot outermost cluster stars are seen in NGC 4147, which disproves the recent model predictions. Nevertheless, the mean velocity dispersion of the outermost cluster’s stars agrees with NGC 4147 being formed in a $10^8$ $10^{8}$ – $10^9$ $10^{9}$ $\hbox {M}_\odot $ $M_{⊙}$ dwarf galaxy with a cored dark matter profile that was later accreted to the Milky Way.