Looking into the faintEst WIth MUSE (LEWIS): Exploring the nature of ultra-diffuse galaxies in the Hydra I cluster - III. Untangling UDG 32 from the stripped filaments of NGC 3314A with multi-wavelength data

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Volume 695 (March 2025)

A&A, 695 (2025) A91

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Table 1.

Structural and stellar population properties predicted for UDG from formation scenarios involving gravitational interactions, compared with those for UDG 32.

Observables	RPS clumps	Tidally heated dwarfs	TDG-like	UDG 32
References.	(1,2,3)	(4,5)	(6,7,8,9)	this work; (10)
Stellar mass	∼10^3.5 − 10⁸ M_⊙	∼10⁸ − 10⁹ M_⊙	∼10⁷ − 10⁹ M_⊙	$6 . 7_{- 1.8}^{+ 2.0} \times 10^{7} M_{⊙}$ $6.7^{+2.0}_{-1.8}\times 10^{7}\,M_\odot$
g − r colour	Blue	0.4 − 0.5 mag	Blue	0.54 − 0.61 mag ^(a)
Dust content	A_V ≲ 1.5 mag	Dwarf-like	A_V ≲ 1.5 mag	$A_{V} = 0 . 17_{- 0.13}^{+ 0.26}$ $A_V = 0.17^{+0.26}_{-0.13}$ mag
Age	∼0.01 − 0.4 Gyr	Dwarf-like: ∼6 − 14 Gyr	≲4 Gyr	$7 . 7_{- 2.8}^{+ 2.9} Gyr$ $7.7^{+2.9}_{-2.8}\,\mathrm{Gyr}$
Metallicity [M/H]	Moderate	Dwarf-like (following the dwarf MZR: ≲ − 1 dex)	Enhanced (compared to the dwarf MZR)	$0 . 07_{- 0.32}^{+ 0.19}$ $0.07^{+0.19}_{-0.32}$ dex
Gas content	Yes	No	Possible	No
UV emission	Yes	No	Possible	To be constrained
GC content	No	Dwarf-like	No	No
DM content	No	Dwarf-like	No	To be constrained

^(a)

Notes.Integrated colours from OmegaCAM and DECam respectively. Also note the gradient towards redder colours (∼1 mag) in the outskirts of UDG 32 reported in Iodice et al. (2021).

References: (1) Poggianti et al. (2019); (2) Werle et al. (2024); (3) Lora et al. (2024); (4) Bennet et al. (2018); (5) Jones et al. (2021); (6) Kaviraj et al. (2012); (7) Duc et al. (2014); (8) Ploeckinger et al. (2018); (9) Ivleva et al. (2024); (10) Iodice et al. (2021).

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