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We present first results from the KMOS Ultra-deep Rotation Velocity Survey (KURVS), aimed at studying the outer rotation curves shape and dark matter content of 22 star-forming galaxies at z ∼ 1.5. These galaxies represent 'typical' star-forming discs at z ∼ 1.5, being located within the star-forming main sequence and stellar mass-size relation with stellar masses 9.5 ≤ log(M ⋆/M⊙) ≤ 11.5. We use the spatially resolved H α emission to extract individual rotation curves out to 4 times the effective radius, on average, or ∼10–15 kpc. Most rotation curves are flat or rising between three and six disc scale radii. Only three objects with dispersion-dominated dynamics (v rot/σ0 ∼ 0.2) have declining outer rotation curves at more than 5σ significance. After accounting for seeing and pressure support, the nine rotation-dominated discs with v rot/σ0 ≥ 1.5 have average dark matter fractions of |$50 \pm 20{{\ \rm per\ cent}}$| at the effective radius, similar to local discs. Together with previous observations of star-forming galaxies at cosmic noon, our measurements suggest a trend of declining dark matter fraction with increasing stellar mass and stellar mass surface density at the effective radius. Measurements of simulated EAGLE galaxies are in quantitative agreement with observations up to log |$(M_{\star } R_{\rm eff}^{-2} /\mathrm{M_{\odot } kpc^{-2}}) \sim 9.2$|⁠ , and overpredict the dark matter fraction of galaxies with higher mass surface densities by a factor of ∼3. We conclude that the dynamics of typical rotationally-supported discs at z ∼ 1.5 is dominated by dark matter from effective radius scales, in broad agreement with cosmological models. The tension with observations at high stellar mass surface density suggests that the prescriptions for baryonic processes occurring in the most massive galaxies (such as bulge growth and quenching) need to be reassessed. [ABSTRACT FROM AUTHOR]

We present SAMI-H  i , a survey of the atomic hydrogen content of 296 galaxies with integral field spectroscopy available from the SAMI Galaxy Survey. The sample spans nearly 4 dex in stellar mass (⁠|$M_\star = 10^{7.4}-10^{11.1}~ \rm M_\odot$|⁠), redshift z < 0.06, and includes new Arecibo observations of 153 galaxies, for which we release catalogues and H  i spectra. We use these data to compare the rotational velocities obtained from optical and radio observations and to show how systematic differences affect the slope and scatter of the stellar-mass and baryonic Tully–Fisher relations. Specifically, we show that |$\rm H\alpha$| rotational velocities measured in the inner parts of galaxies (1.3 effective radii in this work) systematically underestimate H  i global measurements, with H  i / |$\rm H\alpha$| velocity ratios that increase at low stellar masses, where rotation curves are typically still rising and |$\rm H\alpha$| measurements do not reach their plateau. As a result, the |$\rm H\alpha$| stellar mass Tully–Fisher relation is steeper (when M ⋆ is the independent variable) and has larger scatter than its H  i counterpart. Interestingly, we confirm the presence of a small fraction of low-mass outliers of the |$\rm H\alpha$| relation that are not present when H  i velocity widths are used and are not explained by 'aperture effects'. These appear to be highly disturbed systems for which |$\rm H\alpha$| widths do not provide a reliable estimate of the rotational velocity. Our analysis reaffirms the importance of taking into account differences in velocity definitions as well as tracers used when interpreting offsets from the Tully–Fisher relation, at both low and high redshifts and when comparing with simulations. [ABSTRACT FROM AUTHOR]

We present detailed stellar specific angular momentum (j *) measurements of 10 star-forming galaxies at z ∼ 1.5−2, using both high and low spatial resolution integral field spectroscopic data. We developed a code that simultaneously models the adaptive optics (AO) assisted observations from OSIRIS/SINFONI along with their natural seeing (NS) counterparts from KMOS at spatial resolutions of [0.1−0.4] arcsec and [0.6−1.0] arcsec, respectively. The AO data reveal 2/10 systems to be mergers and for the remaining eight the mean uncertainties |$\bar{\Delta }j_*$| decrease from 49 per cent (NS), and 26.5 per cent (AO), to 16 per cent in the combined analysis. These j * measurements agree within 20 per cent with simple estimates (⁠|$\tilde{j_*}$|⁠) calculated from Hubble Space Telescope photometry and NS kinematics; however, higher resolution kinematics are required to first identify these discs. We find that the choice of surface mass density model and the measurement of effective radius from photometry are the key sources of systematic effects in the measurement of j * between different analyses. Fitting the j * versus M * relations (Fall 1983) with a fixed power-law slope of β = 2/3, we find a zero-point consistent with prior NS results at z ≥ 1 within ∼0.3 dex. Finally, we find a ∼0.38 dex scatter about that relation that remains high despite the AO data so we conclude it is intrinsic to galaxies at z > 1. This compares to a scatter of ≤0.2 dex for discs at z ≃ 0 pointing to a settling of the Fall relation with cosmic time. [ABSTRACT FROM AUTHOR]

We present the KMOS Galaxy Evolution Survey (KGES), a K -band Multi-Object Spectrograph (KMOS) study of the H α and [N  ii ] emission from 288 K -band-selected galaxies at 1.2 ≲ z ≲ 1.8, with stellar masses in the range |$\log _{10}(M_{*}/\rm {M}_{\odot })\approx 9$|  – 11.5. In this paper, we describe the survey design, present the sample, and discuss the key properties of the KGES galaxies. We combine KGES with appropriately matched samples at lower redshifts from the KMOS Redshift One Spectroscopic Survey (KROSS) and the SAMI Galaxy Survey. Accounting for the effects of sample selection, data quality, and analysis techniques between surveys, we examine the kinematic characteristics and angular momentum content of star-forming galaxies at z ≈ 1.5, ≈1, and ≈0. We find that stellar mass, rather than redshift, most strongly correlates with the disc fraction amongst star-forming galaxies at z ≲ 1.5, observing only a modest increase in the prevalence of discs between z ≈ 1.5 and z ≈ 0.04 at fixed stellar mass. Furthermore, typical star-forming galaxies follow the same median relation between specific angular momentum and stellar mass, regardless of their redshift, with the normalization of the relation depending more strongly on how disc-like a galaxy's kinematics are. This suggests that massive star-forming discs form in a very similar manner across the ≈10 Gyr encompassed by our study and that the inferred link between the angular momentum of galaxies and their haloes does not change significantly across the stellar mass and redshift ranges probed in this work. [ABSTRACT FROM AUTHOR]

Galaxy clusters have long been theorized to quench the star formation of their members. This study uses integral-field unit observations from the K -band MultiObject Spectrograph (KMOS) – Cluster Lensing And Supernova survey with Hubble (CLASH) survey (K-CLASH) to search for evidence of quenching in massive galaxy clusters at redshifts 0.3 < z < 0.6. We first construct mass-matched samples of exclusively star-forming cluster and field galaxies, then investigate the spatial extent of their H α emission and study their interstellar medium conditions using emission line ratios. The average ratio of H α half-light radius to optical half-light radius (⁠|$r_{\mathrm{e}, {\rm {H}\,\alpha }}/r_{\mathrm{e}, R_{\mathrm{c} } }$|⁠) for all galaxies is 1.14 ± 0.06, showing that star formation is taking place throughout stellar discs at these redshifts. However, on average, cluster galaxies have a smaller |$r_{\mathrm{e}, {\rm {H}\alpha }}/r_{\mathrm{e}, R_{\mathrm{c} } }$| ratio than field galaxies: 〈 |$r_{\mathrm{e}, {\rm {H}\alpha }}/r_{\mathrm{e}, R_{\mathrm{c} } }$| 〉 = 0.96 ± 0.09 compared to 1.22 ± 0.08 (smaller at a 98 per cent credibility level). These values are uncorrected for the wavelength difference between H α emission and R c-band stellar light but implementing such a correction only reinforces our results. We also show that whilst the cluster and field samples follow indistinguishable mass–metallicity (MZ) relations, the residuals around the MZ relation of cluster members correlate with cluster-centric distance; galaxies residing closer to the cluster centre tend to have enhanced metallicities (significant at the 2.6σ level). Finally, in contrast to previous studies, we find no significant differences in electron number density between the cluster and field galaxies. We use simple chemical evolution models to conclude that the effects of disc strangulation and ram-pressure stripping can quantitatively explain our observations. [ABSTRACT FROM AUTHOR]

We present the KMOS-CLASH (K-CLASH) survey, a K -band Multi-Object Spectrograph (KMOS) survey, of the spatially resolved gas properties and kinematics of 191 (pre-dominantly blue) H α-detected galaxies at 0.2 ≲ z ≲ 0.6 in field and cluster environments. K-CLASH targets galaxies in four Cluster Lensing And Supernova survey with Hubble (CLASH) fields in the KMOS IZ -band, over 7 arcmin radius (≈2–3 Mpc) fields of view. K-CLASH aims to study the transition of star-forming galaxies from turbulent, highly star-forming disc-like and peculiar systems at z ≈ 1–3, to the comparatively quiescent, ordered late-type galaxies at z ≈ 0, and to examine the role of clusters in the build-up of the red sequence since z ≈ 1. In this paper, we describe the K-CLASH survey, present the sample, and provide an overview of the K-CLASH galaxy properties. We demonstrate that our sample comprises star-forming galaxies typical of their stellar masses and epochs, residing both in field and cluster environments. We conclude K-CLASH provides an ideal sample to bridge the gap between existing large integral-field spectroscopy surveys at higher and lower redshifts. We find that star-forming K-CLASH cluster galaxies at intermediate redshifts have systematically lower stellar masses than their star-forming counterparts in the field, hinting at possible 'downsizing' scenarios of galaxy growth in clusters at these epochs. We measure no difference between the star formation rates of H α-detected, star-forming galaxies in either environment after accounting for stellar mass, suggesting that cluster quenching occurs very rapidly during the epochs probed by K-CLASH, or that star-forming K-CLASH galaxies in clusters have only recently arrived there, with insufficient time elapsed for quenching to have occurred. [ABSTRACT FROM AUTHOR]

We present stellar specific angular momentum j * measurements of two z  ∼ 1.5 galaxies in the KGES sample and 12 DYNAMO z  ∼ 0.1 analogues of high-redshift galaxies. We combine natural seeing integral field spectroscopic data to trace line emission out to high multiples of effective radius r e, with adaptive optics assisted Keck/OSIRIS observations to trace the rapid rise in rotation curve in the inner regions. Our spaxel-wise integration method gives results that are on average within measurement uncertainty of the traditional rotation curve model method. At z  ∼ 0, combining GMOS and OSIRIS data sets improves the measurement uncertainty in j * from 13 per cent (GMOS only) or 16 per cent (OSIRIS only) to 10 per cent. At z  ∼ 1.5, systematics allow for at best 20 per cent uncertainty on j *. DYNAMO analogues of high- z galaxies have low j * for their stellar mass M *, and low bulge-to-total light ratio β for their j */ M *. The high- z galaxy COSMOS 127977 has j */ M * consistent with normal local disc galaxies, while UDS 78317 is consistent with local analogues. However, our high-resolution OSIRIS data reveal that UDS 78317 may be a merging system. We report a relationship between distance to the β− j */ M * plane and the ratio of velocity dispersion to rotational velocity σ/ v max, where galaxies that deviate more from the plane are more dispersion-dominated due to turbulence. Much of the scatter in M *− j * that is not explained by variations in the bulge-to-total ratio or evolution with redshift may be driven by increased turbulence due to star formation, or by treating mergers as rotating discs. [ABSTRACT FROM AUTHOR]

We analyse maps of the spatially resolved nebular emission of ≈1500 star-forming galaxies at z ≈ 0.6–2.2 from deep K -band Multi-Object Spectrograph and MUSE observations to measure the average shape of their rotation curves. We use these to test claims for declining rotation curves at large radii in galaxies at z ≈ 1–2 that have been interpreted as evidence for an absence of dark matter. We show that the shape of the average rotation curves, and the extent to which they decline beyond their peak velocities, depends upon the normalization prescription used to construct the average curve. Normalizing in size by the galaxy stellar disc-scale length after accounting for seeing effects (⁠|$R_{\rm {d}}^{\prime }$|⁠), we construct stacked position-velocity diagrams that trace the average galaxy rotation curve out to |$6R_{\rm {d}}^{\prime }$| (≈13 kpc, on average). Combining these curves with average H  i rotation curves for local systems, we investigate how the shapes of galaxy rotation curves evolve over ≈10 Gyr. The average rotation curve for galaxies binned in stellar mass, stellar surface mass density and/or redshift is approximately flat, or continues to rise, out to at least |$6R_{\rm {d}}^{\prime }$|⁠. We find a trend between the outer slopes of galaxies' rotation curves and their stellar mass surface densities, with the higher surface density systems exhibiting flatter rotation curves. Drawing comparisons with hydrodynamical simulations, we show that the average shapes of the rotation curves for our sample of massive, star-forming galaxies at z ≈ 0–2.2 are consistent with those expected from lambda cold dark matter theory and imply dark matter fractions within 6 R d of at least ≈60 per cent. [ABSTRACT FROM AUTHOR]

The Tully–Fisher relation (TFR) is an empirical relation between galaxy luminosity and rotation velocity. We present here the first TFR of galaxies beyond the local Universe that uses carbon monoxide (CO) as the kinematic tracer. Our final sample includes 25 isolated, non-interacting star-forming galaxies with double-horned or boxy CO integrated line profiles located at redshifts z ≤ 0.3, drawn from a larger ensemble of 67 detected objects. The best reverse K s-band, stellar mass and baryonic mass CO TFRs are, respectively, $$M_{K_{\text{s}}}=(-8.4\pm 2.9)[\log {(\frac{W_{50}/\rm {km\, s^{-1}}}{\sin {i}})}-2.5] + (-23.5\pm 0.5)$$, $$\log {(M_{\star } / {\rm M}_\odot)}=(5.2\pm 3.0)[\log {(\frac{W_{50}/\rm {km\, s^{-1}}}{\sin {i}})}-2.5]+ (10.1\pm 0.5)$$ and $$\log {(M_{\rm b} / {\rm M}_\odot)}=(4.9\pm 2.8)[\log {(\frac{W_{50}/\rm {km\, s^{-1}}}{\sin {i}})}-2.5] + (10.2\pm 0.5)$$, where $$M_{K_{\text{s}}}$$ is the total absolute K s-band magnitude of the objects, M ⋆ and M b their total stellar and baryonic masses, and W 50 the width of their line profile at 50 per cent of the maximum. Dividing the sample into different redshift bins and comparing to the TFRs of a sample of local (z = 0) star-forming galaxies from the literature, we find no significant evolution in the slopes and zero-points of the TFRs since z ≈ 0.3, this in either luminosity or mass. In agreement with a growing number of CO TFR studies of nearby galaxies, we more generally find that CO is a suitable and attractive alternative to neutral hydrogen (H  i). Our work thus provides an important benchmark for future higher redshift CO TFR studies. [ABSTRACT FROM AUTHOR]