• DOI:10.1051/0004-6361/202243117
• Corpus ID: 246210142

The halo of M105 and its group environment as traced by planetary nebula populations. II. Using kinematics of single stars to unveil the presence of intragroup light around the Leo I galaxies NGC 3384 and M105

@article{Hartke2022TheHO,
  title={The halo of M105 and its group environment as traced by planetary nebula populations. II. Using kinematics of single stars to unveil the presence of intragroup light around the Leo I galaxies NGC 3384 and M105},
  author={Johanna Hartke and Magda Arnaboldi and Ortwin Gerhard and Lodovico Coccato and Michael Merrifield and K. Kuijken and Claudia Pulsoni and Adriano Agnello and Souradeep Bhattacharya and Chiara Spiniello and Arianna Cortesi and Kenneth C. Freeman and Nicola R. Napolitano and Aaron J. Romanowsky},
  journal={Astronomy \& Astrophysics},
  year={2022}
}

• J. Hartke, M. Arnaboldi, +11 authors A. Romanowsky
• Published 21 January 2022
• Physics
• Astronomy & Astrophysics

Context. M105 (NGC 3379) is an early-type galaxy in the nearby Leo I group, the closest galaxy group to contain all galaxy types and therefore an excellent environment to explore the low-mass end of intra-group light (IGL) assembly. Aims. We present a new and extended kinematic survey of planetary nebulae (PNe) in M105 and the surrounding 30′ × 30′ in the Leo I group with the Planetary Nebula Spectrograph (PN.S) to investigate kinematically distinct populations of PNe in the halo and the surrounding IGL. Methods. We use PNe as kinematic tracers of the diffuse stellar light in the halo and IGL, and employ photo-kinematic Gaussian mixture models to (i) separate contributions from the companion galaxy NGC 3384, and (ii) associate PNe with structurally defined halo and IGL components around M105. Results. We present a catalogue of 314 PNe in the surveyed area and firmly associate 93 of these with the companion galaxy NGC 3384 and 169 with M105. The PNe in M105 are further associated with its halo (138) and the surrounding exponential envelope (31). We also construct smooth velocity and velocity dispersion fields and calculate projected rotation, velocity dispersion, and λR profiles for the different components. PNe associated with the halo exhibit declining velocity dispersion and rotation profiles as a function of radius, while the velocity dispersion and rotation of the exponential envelope increase notably at large radii. The rotation axes of these different components are strongly misaligned. Conclusions. Based on the kinematic profiles, we identify three regimes with distinct kinematics that are also linked to distinct stellar population properties: (i) the rotating core at the centre of the galaxy (within 1 Reff) formed in situ and is dominated by metal-rich ([M/H]≈ 0) stars that also likely formed in situ, (ii) the halo from 1 to 7.5 Reff consisting of a mixture of intermediate-metallicity and metal-rich stars ([M/H]> −1), either formed in situ or was brought in via major mergers, and (iii) the exponential envelope reaching beyond our farthest data point at 16 Reff , predominately composed of metal-poor ([M/H]< −1) stars. The high velocity dispersion and moderate rotation of the latter are consistent with those measured for the dwarf satellite galaxies in the Leo I group, indicating that this exponential envelope traces the transition to the IGL.