tokens: strong negative gas-phase metallicities from the center toward the stripped tails, consistent with an inside-out formation in isolation, followed by a outside-in removal of gas upon infall into the cluster (e.g., Bellhouse et al. 2019 ; Franchetto et al. 2020 ). Our galaxies show offset H α -flux peaks, extended tails of nebular emission, and bow-like and asymmetric velocity maps reminiscent of those seen in jellyfish galaxies. However, the tantalizing alignment of these features with the merger axis is broadly incompatible with galaxies infalling into the cluster radially and, unlike jellyfish galaxies, we actually find consistent evidence against radial metallicity gradients. We can draw comparisons between detailed studies of infalling galaxies in local clusters. For example, Chemin et al. ( 2006 ) conducted a detailed kinematic analysis of 30 typical spiral galaxies in the 1.2 × 10 15 M ⊙ Virgo cluster, located at a distance of just ∼16.5 Mpc. The bulk of their sample is located outside the core of the cluster, specifically at relative velocities and radii larger than our sample (see the phase–space diagram in Figure 5 ). Chemin et al. ( 2006 ) found evidence for disturbed H α kinematics, but the offsets between the peak of the stellar light and the H α are of the order of 0.2–0.4 kpc, which is smaller than what we observe in our galaxies (0.6–1.9 kpc). Outside of its core, the Coma cluster (7 × 10 14 M ⊙ , located at ∼100 Mpc) is dominated by disturbed galaxies with tails of H α emission (Gavazzi et al. 2018 ). Three Coma galaxies are located to the cluster center as close as our galaxies Sausage 6–9 (Figure 5 ). However, these three galaxies are undergoing extreme ram pressure. With only one galaxy powered by SF and two by AGN, there is little to no H α within the stellar disk and the bulk of H α is found outside the galaxies, streaming out in long tails (Yagi et al. 2010 ). Observations of both Coma and Virgo indicate that infalling galaxies can present tails of H α emission and perturbed kinematics, but the H α gas is removed from the outside in, while the peak of the emission, close to the nucleus of the galaxies does not get displaced. Figure 5. Phase–space diagram for the cores of the Sausage, Virgo, and Coma clusters, highlighting kinematically disturbed H α galaxies. We show our five galaxies with respect to the properties of the closest subcluster (as derived from weak lensing and dynamics in Jee et al. 2015 ), together with data from Chemin et al. ( 2006 ) on the Virgo cluster and Gavazzi et al. ( 2018 ) for the Coma cluster. Our galaxies are embedded deep within the ICM. Unlike galaxies at similar cluster-centric radii and relative velocities in Coma and Virgo, which are almost completely devoid of H α within the disk, the Sausage galaxies show H α throughout the stellar disk, with large offsets between the peak of H α and the stellar light. Considering that our galaxies are deeply embedded in the hottest parts of the ICM (see
ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O B-Citation I-Citation I-Citation I-Citation O O B-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O B-CelestialObject O B-CelestialObject O O O O O O O O B-Wavelength I-Wavelength O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject B-CelestialObject O B-CelestialObject I-CelestialObject O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O B-CelestialObject I-CelestialObject O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O B-CelestialObject O B-CelestialObject O O O O O O B-Wavelength I-Wavelength O O O O B-CelestialObject O O B-Wavelength I-Wavelength O O O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O O O O