A4 Refereed article in a conference publication
Planetary nebulae populations in the haloes of nearby massive early-type galaxies
Authors: Hartke, J.; Arnaboldi, M.; Gerhard, O.; Ennis, A.; Pulsoni, C.; Coccato, L.; Cortesi, A.; Freeman, K.; Kuijken, K.; Merrifield, M.; Napolitano, N.
Editors: De Marco, Orsola; Zijlstra, Albert; Szczerba, Ryszard
Conference name: Symposium of the International Astronomical Union
Publication year: 2025
Journal: Proceedings of the International Astronomical Union
Book title : Planetary Nebulae: A Universal Toolbox in the Era of Precision Astrophysics
Series title: IAU Symposium
Volume: 19
Issue: 384
First page : 109
Last page: 121
ISSN: 1743-9213
eISSN: 1743-9221
DOI: https://doi.org/10.1017/S174392132300577X
Publication's open availability at the time of reporting: Open Access
Publication channel's open availability : Partially Open Access publication channel
Web address : https://doi.org/10.1017/S174392132300577X
Self-archived copy’s web address: https://research.utu.fi/converis/portal/detail/Publication/505703876
Planetary nebulae (PNe) are excellent tracers of the metal-poor haloes of nearby early-type galaxies. They are commonly used to trace spatial distribution and kinematics of the halo and intracluster light at distances of up to 100 Mpcs. The results on the early-type galaxy M105 in the Leo I group represent a benchmark for the quantitative analysis of halo and intragroup light. Since the Leo I group lies at just a 10 Mpc distance, it is at the ideal location to compare results from resolved stellar populations with the homogeneous constraints over a much larger field of view from the PN populations. In M105, we have – for the first time – established a direct link between the presence of a metal-poor halo as traced by resolved red-giant branch stars and a PN population with a high specific frequency (α-parameter). This confirms our inferences that the high α-parameter PN population in the outer halo of M49 in the Virgo Cluster traces the metal-poor halo and intra-group light.
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Funding information in the publication:
J.H. and A.I.E. acknowledge the financial support from the visitor and mobility program of the Finnish Centre for Astronomy with ESO (FINCA), funded by the Academy of Finland grant nr 306531.
