1. Stellar populations and merger rates of brightest cluster galaxies a billion years ago: SDSS MaNGA IFU spectroscopy.
- Author
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Edwards, Louise O V, Hamel, Kevin A S J, Shy, Joseph C, Hernandez, Jonathan, Holguin Luna, Priscilla, Higgins, Denvir J, Chawla, Theo, Gavidia, Adriana, and Cole, Samuel
- Subjects
STELLAR mergers ,STELLAR populations ,STAR formation ,GALAXY mergers ,SPECTROMETRY ,GALACTIC evolution ,GALAXY clusters - Abstract
We investigate the spectroscopic properties of 85 brightest cluster galaxies (BCGs) and their companions observed with the SDSS MaNGA integral field unit. Galaxy redshifts are between 0.08 < z < 0.15, allowing for a field-of-view up to 80 × 80 kpc. For the main galaxies: the average age of the BCG cores is 7.66 |$\, \pm \,$| 1.36 Gyr with no significant gradient out to |$2\, R_ {e}$| ; the average metallicity of the BCG cores is |$[Z/H]=0.23\, \pm \, 0.03$| with a negative gradient of Δ[ Z /H]/Δ(R/R
e ) = –0.14 |$\, \pm \, 0.09$| which flattens beyond |$1.2\, R_ {e}$|. Velocity dispersion gradients are mostly flat, but a few positive slopes are seen in the most massive galaxies. Emission lines are present in 12 of the BCGs, most often confined to the central |$\sim 2\,$| kpc with emission line ratios well-described by a LINER or AGN excitation source. There are 78 companion galaxies identified and 9 have nebular emission lines that indicate recent star formation. The companions with flux ratios of 4:1 and 20:1 within 30 kpc of their BCG's core are studied. The companion galaxies have a median age of 7.65 |$\, \pm \,$| 1.55 Gyr and are high-metallicity systems, with a median [ Z / H ] = 0.17 ± 0.07. Close spectroscopic companions with higher merging probabilities have an average merging time of 0.5 ± 0.2 Gyr. The average merger rate is 0.08 |$\, \pm \, 0.12 \,$| Gyr−1 for 4:1 companions and 0.26 |$\, \pm \, 0.22 \,$| Gyr−1 for 20:1 companions, allowing for an increase in mass of 2.3 |$\, \pm \,$| 3.4 per cent Gyr−1 and 3.5 |$\, \pm \,$| 3.2 per cent Gyr−1 , respectively. [ABSTRACT FROM AUTHOR]- Published
- 2024
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