Evolution of galaxy scaling relations in clusters at 0.5 &lt;<i>z</i>&lt; 1.5

Pérez-Martínez, J. M.; Ziegler, B.; Dannerbauer, H.; Böhm, A.; Verdugo, M.; Díaz, Ángeles I.; Hoyos, C.

doi:10.1051/0004-6361/201936456

Cited by 7 publications

(7 citation statements)

References 145 publications

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“…Inclusion of such galaxies in a TFR analysis is expected to lead to a larger scatter and possibly zero point offsets in the TFR (see Section 8.1.1 on sample selection). At higher redshifts, several environment-specific TFR studies reported no significant differences in the TFRs in cluster and field populations (Ziegler et al 2003 ;Nakamura et al 2006 ;Jaff é et al 2011a ;P érez-Mart ínez et al 2021 ), while other studies such as Bamford et al ( 2005), Milvang-Jensen et al ( 2003, and P érez-Mart ínez et al ( 2021 , for z ∼ 1.5) found an o v erall brightening of cluster galaxies at a fixed rotational velocity. Other morphologyspecific studies such as Bedregal et al ( 2006 ) and Jaff é et al ( 2014 ) reported fainter magnitudes at a given rotational velocity for lenticular and early-type galaxies compared to spiral galaxies.…”

Section: The Tfrs From An Environmental Perspecti V Ementioning

confidence: 89%

BUDH iES V: the baryonic Tully–Fisher relation at z = 0.2 based on direct H i detections

Gogate

Verheijen

Hulst

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present H i-based B- and R-band Tully-Fisher relations (TFRs) and the Baryonic TFR (BTFR) at z=0.2 using direct H i detections from the Blind Ultra-Deep H i Environmental Survey (BUDH iES). Deep photometry from the Isaac Newton Telescope was used for 36 out of 166 H i sources, matching the quality criteria required for a robust TFR analysis. Two velocity definitions at 20% and 50% of the peak flux were measured from the global H i profiles and adopted as proxies for the circular velocities. We compare our results with an identically constructed z=0 TFR from the Ursa Major (UMa) association of galaxies. To ensure an unbiased comparison of the TFR, all the samples were treated identically regarding sample selection and applied corrections. We provide catalogues and an atlas showcasing the properties of the galaxies. Our analysis is focused on the zero points of the TFR and BTFR with their slopes fixed to the z=0 relation. Our main results are: (1) The BUDH iES galaxies show more asymmetric H i profiles with shallower wings compared to the UMa galaxies, which is likely due to the environment in which they reside, (2) The luminosity-based z=0.2 TFRs are brighter and bluer than the z=0 TFRs, even when cluster galaxies are excluded from the BUDH iES sample, (3) The BTFR shows no evolution in its zero point over the past 2.5 billion years and does not significantly change on the inclusion of cluster galaxies, and (4) proper sample selection and consistent corrections are crucial for an unbiased analysis of the evolution of the TFR.

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Section: The Tfrs From An Environmental Perspecti V Ementioning

confidence: 89%

BUDH iES V: the baryonic Tully–Fisher relation at z = 0.2 based on direct H i detections

Gogate

Verheijen

Hulst

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Because physical mechanisms can affect the angular momentum of the baryons in different ways (i.e., increase or decrease it), an interpretation given in Pelliccia et al (2019) is that this reduction of angular momentum at a fixed stellar mass could be due to galaxy mergers, which is in line with their prevalence in dense environments (e.g., Tomczak et al 2019) and with recent simulations (e.g., Lagos et al 2018). However, the results from Pelliccia et al (2019) and Pérez-Martínez et al (2021) to compare galaxies from different surveys and observed with various instruments (e.g., Pérez-Martínez et al 2021) to reach these conclusions. As in Abril-Melgarejo et al (2021) and Mercier et al (2022), we argue that there might be systematic effects when doing so, mainly driven by different selection functions between different datasets.…”

Section: Introductionmentioning

confidence: 93%

“…Finally, a few studies have tried to probe the impact of the environment on the galaxies' angular momentum (e.g., Pelliccia et al 2019;Pérez-Martínez et al 2021). The current picture that emerges from these studies is that galaxies found in galaxy groups and galaxy clusters at z ∼ 1 seem to have a deficit of angular momentum with respect to field galaxies located at the same redshift.…”

Section: Introductionmentioning

confidence: 99%

Stellar angular momentum of disk galaxies at z ≈ 0.7 in the MAGIC survey

Mercier,

Epinat,

Contini

et al. 2023

A&A

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Aims. At intermediate redshift, galaxy groups and clusters are thought to impact galaxy properties such as their angular momentum. We investigate whether the environment has an impact on the galaxies’ stellar angular momentum and identify underlying driving physical mechanisms. Methods. We derived robust estimates of the stellar angular momentum using Hubble Space Telescope (HST) images combined with spatially resolved ionised gas kinematics from the Multi-Unit Spectroscopic Explorer (MUSE) for a sample of ∼200 galaxies in groups and in the field at z ∼ 0.7 drawn from the MAGIC survey. Using various environmental tracers, we study the position of the galaxies in the angular momentum–stellar mass (Fall) relation as a function of environment. Results. We measured a 0.12 dex (2σ significant) depletion of stellar angular momentum for low-mass galaxies (M⋆ < 1010 M⊙) located in groups with respect to the field. Massive galaxies located in dense environments have less angular momentum than expected from the low-mass Fall relation but, without a comparable field sample, we cannot infer whether this effect is mass or environmentally driven. Furthermore, these massive galaxies are found in the central parts of the structures and have low systemic velocities. The observed depletion of angular momentum at low stellar mass does not appear linked with the strength of the over-density around the galaxies but it is strongly correlated with (i) the systemic velocity of the galaxies normalised by the dispersion of their host group and (ii) their ionised gas velocity dispersion. Conclusions. Galaxies in groups appear depleted in angular momentum, especially at low stellar mass. Our results suggest that this depletion might be induced by physical mechanisms that scale with the systemic velocity of the galaxies (e.g., stripping or merging) and that such a mechanism might be responsible for enhancing the velocity dispersion of the gas as galaxies lose angular momentum.

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“…Hydrodynamical cluster-specific interactions between the interstellar medium (ISM) of galaxies and the intracluster medium (ICM) include ram pressure stripping (RPS, Gunn & Gott 1972), the removal of the hot halo gas (Larson et al 1980), as well as viscous stripping, and thermal evaporation (Cowie & Songaila 1977). These cluster-specific processes require different ambient conditions such as high ICM gas densities or low relative velocities between galaxies, imprinting specific features in the stellar and gas component of the cluster members, which can be observed, for example, in their light distribution (Hernández-Fernández et al 2012), structural parameters (Kuchner et al 2017), velocity fields (Pérez-Martínez et al 2017, Pérez-Martínez et al 2021, and oxygen abundances (Ciocan et al 2020, Maier et al 2022. Studies of intermediate redshift cluster galaxies also find evidence that environmental quenching not only depends on the ICM density, but also on the stellar mass of the galaxy, with less massive systems being more strongly affected by environmental mechanisms (e.g.…”

Section: Introductionmentioning

confidence: 99%

Morpho-kinematics of MACS J0416.1-2403 low-mass galaxies

Ciocan

Ziegler

Böhm

et al. 2022

A&A

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We use optical integral field spectroscopy from VLT/MUSE, as well as photometric observations from Hubble Space Telescope and VLT/HAWK-I, to study the morpho-kinematics of 17 low mass (log(M/M ) < 9.5) MACS J0416.1-2403 cluster galaxies at R 200 and 5 field galaxies with a redshift of z ∼0.4. By measuring fluxes of strong emission lines from the MUSE data, we have recovered the star formation rates, gas-phase metallicities, spatially resolved gas kinematics and also investigated the ionising mechanisms. We have analysed the structure and morphology of the galaxies from the optical and infrared photometric data, performing a multi-component decomposition into a bulge and a disk. The spatially resolved gas velocity fields of the cluster members and field galaxies were modelled using a 3D approach, which allowed us to retrieve their intrinsic gas kinematics, including the maximum rotation velocity and velocity dispersion. This enabled us to study scaling relations such as the Tully-Fisher and the stellar mass -S 0.5 relation for low mass galaxies in different environments and to search for signatures of cluster-specific processes using disturbed gas velocity fields as tracers. Most galaxies from our sample fall in the star forming and composite region in the BPT diagnostic diagram, which allows the ionising sources in a galaxy to be disentangled. The cluster and field population can be classified as star forming main-sequence galaxies, with only a sub-sample of four quenched systems. We observe significant scatter for the cluster galaxies in the mass-metallicity plane, and the lowest mass systems deviate from the predictions of the fundamental metallicity relation, showing higher metallicities, whereas the higher mass ones are in accordance with the model predictions. This might hint at the cut-off of pristine gas inflow and/or the removal of the hot halo gas as the mechanisms driving these offsets. Our morpho-kinematic analysis reveals a sub-sample of dwarfs with maximum velocities v max <50 km/s and v max, gas /σ gas < 1, which depart from the Tully-Fisher relation. This might indicate that their interstellar medium is affected by external environmental processes, such as RPS. However, ∼ 30% of the cluster galaxies have rotation-dominated gas disks and follow the Tully-Fisher relation within 1σ. Using the S 0.5 parameter, which links the dynamical support of ordered motions with that of random motions, we can separate between galaxies affected by gravitational processes and hydrodynamical ones. In the stellar mass -S 0.5 plane, both cluster and field galaxies follow a tight sequence, with only a sub-population of 5 galaxies strongly departing (> 4σ) from this relation, showing high σ gas values. Both the morphology and kinematics of the outlier galaxies hint at a combination of pre-processing and cluster-specific interactions affecting their stellar and gas disks. Thus, in our sample of low-mass galaxies in a rich cluster at z ∼ 0.4, 65% exhibit disordered motions in their velocity fields, in contrast to previous ...

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Evolution of galaxy scaling relations in clusters at 0.5 <z< 1.5

Cited by 7 publications

References 145 publications

BUDH iES V: the baryonic Tully–Fisher relation at z = 0.2 based on direct H i detections

BUDH iES V: the baryonic Tully–Fisher relation at z = 0.2 based on direct H i detections

Stellar angular momentum of disk galaxies at z ≈ 0.7 in the MAGIC survey

Morpho-kinematics of MACS J0416.1-2403 low-mass galaxies

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