Internal kinematics of spiral galaxies in distant clusters

Kutdemir, Elif; Ziegler, B.; Peletier, Reynier F.; Rocha, C. Da; Boehm, A.; Verdugo, M.

doi:10.1051/0004-6361/200913262

Cited by 12 publications

(16 citation statements)

References 124 publications

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“…This suggests that while the field population of galaxies at 0.3<z<0.6 already contains a significant fraction of galaxies showing some degree of distortion, cluster-specific interactions contribute to enhance their asymmetry index, increasing the fraction of irregular galaxies according to our gas kinematics asymmetry criterion. These results are in line with previous studies that reported significant fractions of field galaxies with perturbed kinematics at intermediate redshifts (Yang et al 2008, Kutdemir et al 2010.…”

Section: Kinematic State and Environmentsupporting

confidence: 93%

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Pérez-Martínez

Ziegler

Böhm

et al. 2020

A&A

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Aims. In order to understand the role of the different processes that drive galaxy evolution in clusters, we need comprehensive studies that simultaneously examine several of the most important physical properties of galaxies. In this work we study the interplay between the kinematic state and star formation activity of galaxies in the RXJ1347-1145 cluster complex at z∼0.45. Methods. We used VLT/VIMOS to obtain slit spectra for 95 galaxies across the 40 x40 area where the RXJ1347-1145 cluster complex resides. We determined the cluster membership of our targets by identifying one or more of the available emission lines within the wavelength range. Our spectroscopy is complemented with archival SUBARU/Suprime-Cam deep photometric observations in five optical bands (B, V, Rc, Ic, z'). We examined the kinematic properties of our sample attending to the degree of distortion of the extracted rotation curves. Regular rotating galaxies were included in our Tully-Fisher analysis while the distorted ones were used to study the role of cluster-specific interactions with respect to star formation and AGN activity. Results. Our analysis confirmed the cluster membership for approximately half of our targets. We report a higher fraction of galaxies with irregular gas kinematics in the cluster environment than in the field. Cluster galaxies with regular rotation display a moderate brightening in the B-band Tully-Fisher relation compatible with the gradual evolution of the stellar populations with lookback time, and no significant evolution in the stellar-mass Tully-Fisher relation, in line with previous studies at similar redshift. Average specific star formation rate (sSFR) values are slightly lower in our cluster sample (-0.15 dex) with respect to the main sequence of starforming galaxies, confirming the role of the environment in the early quenching of star formation in clusters. Finally, we carried out an exploratory observational study on the stellar-to-halo mass relation finding that cluster galaxies tend to have slightly lower stellar mass values for a fixed halo mass compared to their field counterparts.

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Section: Kinematic State and Environmentsupporting

confidence: 93%

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Pérez-Martínez

Ziegler

Böhm

et al. 2020

A&A

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“…We find however that ∼50% of the cluster galaxies display irregular kinematics in contrast to what is found in the field at similar redshifts (∼30%, Böhm et al 2004) and in agreement with other studies in clusters (e.g. Bösch et al 2013, Kutdemir et al 2010 which points out to additional processes operating in clusters that distort the galaxy kinematics. Figure 1.…”

supporting

confidence: 91%

Linking star formation and galaxy kinematics in the massive cluster Abell 2163

Menacho¹,

Verdugo²

2014

Proc. IAU

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The origin of the morphology-density relation is still an open question in galaxy evolution. It is most likely driven by the combination of the efficient star formation in the highest peaks of the mass distribution at high-z and the transformation by environmental processes at later times as galaxies fall into more massive halos. To gain additional insights about these processes we study the kinematics, star formation and structural properties of galaxies in Abell 2163 a very massive (∼4×10 15 M , Holz & Perlmutter 2012) merging cluster at z=0.2.We use high resolution spectroscopy with VLT/VIMOS to derive rotation curves and dynamical masses for galaxies that show regular kinematics. Galaxies that show irregular rotation are also analysed to study the origin of their distortion. This information is combined with stellar masses and structural parameters obtained from high quality CFHT imaging. From narrow band photometry (2.2m/WFI), centered on the redshifted Hα line, we obtain star formation rates.Although our sample is still small, field and cluster galaxies lie in a similar Tully-Fisher relation as local galaxies. Controlling by additional parameters like SFRs or bulge-to-disk ratio do not affect this result. We find however that ∼50% of the cluster galaxies display irregular kinematics in contrast to what is found in the field at similar redshifts (∼30%, Böhm et al. 2004) and in agreement with other studies in clusters (e.g. Bösch et al. 2013, Kutdemir et al. 2010 which points out to additional processes operating in clusters that distort the galaxy kinematics. Figure 1. Star forming galaxies in A2163 selected by their Hα emission (small dots). We show in this diagram the cluster galaxies for which we studied their kinematics. Diamonds mark galaxies with regular rotation wheras stars those with irregular kinematics. Dashed lines show constant SFRs whereas the gray area mark the expected sSFR-M relation for this redshift. The most massive galaxy in our sample is a large edge-on spiral clearly expericing ram-pressure stripping as evidenced by its kinematics and trailing star forming regions.

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“…Our analysis and those of Bamford et al and Miller et al hence show an increased intrinsic TFR scatter at intermediate redshifts. This increase might be due to a larger contribution of non-circular motions, for example, that is, to kinematically heated disks (e.g., Förster-Schreiber et al 2009) or more frequent mismatches between photometric and kinematic position angle (e.g., Kutdemir et al 2010) than locally. In principle, it would also be possible that the stellar populations have an effect on the intrinsic TFR scatter, for example due to a broader distribution in stellar M/L ratios toward higher redshifts.…”

Section: Discussionmentioning

confidence: 99%

Disk galaxy scaling relations at intermediate redshifts

Boehm¹,

Ziegler²

2016

A&A

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Aims. Galaxy scaling relations such as the Tully-Fisher relation (between the maximum rotation velocity V max and luminosity) and the velocity-size relation (between V max and the disk scale length) are powerful tools to quantify the evolution of disk galaxies with cosmic time. Methods. We took spatially resolved slit spectra of 261 field disk galaxies at redshifts up to z ≈ 1 using the FORS instruments of the ESO Very Large Telescope. The targets were selected from the FORS Deep Field and William Herschel Deep Field. Our spectroscopy was complemented with HST/ACS imaging in the F814W filter. We analyzed the ionized gas kinematics by extracting rotation curves from the two-dimensional spectra. Taking into account all geometrical, observational, and instrumental effects, these rotation curves were used to derive the intrinsic V max .Results. Neglecting galaxies with disturbed kinematics or insufficient spatial rotation curve extent, V max was reliably determined for 124 galaxies covering redshifts 0.05 < z < 0.97. This is one of the largest kinematic samples of distant disk galaxies to date. We compared this data set to the local B-band Tully-Fisher relation and the local velocity-size relation. The scatter in both scaling relations is a factor of ∼2 larger at z ≈ 0.5 than at z ≈ 0. The deviations of individual distant galaxies from the local Tully-Fisher relation are systematic in the sense that the galaxies are increasingly overluminous toward higher redshifts, corresponding to an overluminosity ∆M B = −(1.2 ± 0.5) mag at z = 1. This luminosity evolution at given V max is probably driven by younger stellar populations of distant galaxies with respect to their local counterparts, potentially combined with modest changes in dark matter mass fractions. The analysis of the velocity-size relation reveals that disk galaxies of a given V max have grown in size by a factor of ∼1.5 over the past ∼8 Gyr, most likely through accretion of cold gas and/or small satellites. From scrutinizing the combined evolution in luminosity and size, we find that the galaxies that show the strongest evolution toward smaller sizes at z ≈ 1 are not those that feature the strongest evolution in luminosity, and vice versa.

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Internal kinematics of spiral galaxies in distant clusters

Cited by 12 publications

References 124 publications

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Galaxy kinematics across different environments in the RXJ1347−1145 cluster complex

Linking star formation and galaxy kinematics in the massive cluster Abell 2163

Disk galaxy scaling relations at intermediate redshifts

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