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MAGNUS. I. A MUSE-DEEP Sample of Early-type Galaxies at Intermediate Redshift

The Astrophysical Journal American Astronomical Society 1009:2 (2026) 149-149

Authors:

Pritom Mozumdar, Michele Cappellari, Christopher D Fassnacht, Tommaso Treu

Abstract:

Abstract We present a sample of 213 early-type galaxies (ETGs) at redshifts 0.25 <  z  < 0.75. We combine deep integral-field spectroscopy from the MUSE-DEEP survey with high-resolution Hubble Space Telescope (HST) imaging to study the structure, kinematics, and stellar populations of these galaxies. We measure spatially resolved stellar kinematics and use the specific angular momentum proxy, λ R , to classify galaxies into fast and slow rotators. The kinematic and photometric axes of fast rotators are generally well aligned, similar to their local counterparts. We find that global stellar population properties, such as age, metallicity, and mass-to-light ratio ( M * / L ), correlate strongly with the central velocity dispersion ( σ e ), following trends established for local ETGs. Slow rotators are typically more massive, have higher σ e , and are more metal rich than fast rotators. We also find a slow rotator fraction consistent with local Universe samples. Our findings indicate that the fundamental structural, kinematic, and stellar population scaling relations of massive ETGs were already in place by z  ∼ 0.75, suggesting their evolutionary pathways have remained stable over the last ∼7 Gyr.
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MAGNUS. II. Rotational Support of Massive Early Type Galaxies Decreased Over the Past 7 Gyr

The Astrophysical Journal American Astronomical Society 1009:1 (2026) 87-87

Authors:

Pritom Mozumdar, Michele Cappellari, Christopher D Fassnacht, Tommaso Treu

Abstract:

Abstract Understanding how the internal kinematics of massive galaxies evolve is key to constraining the physical processes that drive their assembly. We investigate the evolution of rotational support in massive ( log M * / M ⊙ ≥ 10.6 ) early-type galaxies (ETGs) over the past ∼7 Gyr. We use MUSE integral-field spectroscopic (IFS) data for 212 ETGs at intermediate redshift (0.25 <  z  < 0.75) from the MAGNUS sample. We compare their kinematics to a carefully matched local sample of 787 ETGs ( z ≤ 0.05) from the MaNGA survey. Using the specific stellar angular momentum proxy, λ R , we quantify the balance between ordered rotation and random motions. We derive intrinsic λ R values by applying a uniform correction for seeing and point-spread function (PSF) effects to both samples. We find a significant evolutionary trend: The intermediate-redshift ETGs are systematically more rotationally supported than their local counterparts. The median PSF-corrected λ R for the MAGNUS sample is 0.48 ± 0.05, substantially higher than the median of 0.34 ± 0.03 for the matched MaNGA sample. This corresponds to a positive slope in the λ R − z relation of d λ R / d z  = 0.25 ± 0.04 for the combined sample. The decline in rotational support is most pronounced for the most massive ( log M * / M ⊙ > 11.3 ) and highest-velocity-dispersion ( σ e  ≳ 200 km s −1 ) galaxies. Our results provide robust evidence that massive ETGs have undergone significant kinematic evolution, losing angular momentum as they evolve towards the present day, consistent with theoretical models where processes such as dry mergers play a crucial role in shaping the dynamical state of galaxies.
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Stochastic black hole growth tracks stellar mass in ultramassive galaxies

ArXiv 2609.21981 (2026)

Authors:

Michele Cappellari, Dieu D Nguyen, Susan A Kassin
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The JWST Ultramassive Galaxy Sample -- I. Overview, Photometry, and Stellar Kinematics: Selecting Optimal Template Subsets via Non-Negative Matrix Factorization

ArXiv 2609.21979 (2026)

Authors:

Michele Cappellari, Dieu D Nguyen, Susan A Kassin
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The JWST Ultramassive Galaxy Sample -- II. Supermassive Black Hole Masses for 8 Extreme Early-Type Galaxies via Jeans Anisotropic Modelling of High-Resolution Integral-Field NIRSpec Stellar Kinematics

ArXiv 2609.2198 (2026)

Authors:

Michele Cappellari, Dieu D Nguyen, Susan A Kassin
Details from ArXiV