In Galaxy And Mass Assembly Data Release 4 (GAMA DR4), we make available our full spectroscopic redshift sample. This includes 248 682 galaxy spectra, and, in combination with earlier surveys, results in 330 542 redshifts across five sky regions covering ∼250 deg2. The redshift density, is the highest available over such a sustained area, has exceptionally high completeness (95 per cent to rKiDS = 19.65 mag), and is well suited for the study of galaxy mergers, galaxy groups, and the low redshift (z < 0.25) galaxy population. DR4 includes 32 value-added tables or Data Management Units (DMUs) that provide a number of measured and derived data products including GALEX, ESO KiDS, ESO VIKING, WISE and Herschel Space Observatory imaging. Within this release, we provide visual morphologies for 15 330 galaxies to z < 0.08, photometric redshift estimates for all 18 million objects to rKiDS ∼ 25 mag, and stellar velocity dispersions for 111 830 galaxies. We conclude by deriving the total galaxy stellar mass function (GSMF) and its sub-division by morphological class (elliptical, compact-bulge and disc, diffuse-bulge and disc, and disc only). This extends our previous measurement of the total GSMF down to 106.75 M$_{\odot } \, h_{70}^{-2}$ and we find a total stellar mass density of ρ* = (2.97 ± 0.04) × 108 M⊙ h70 Mpc−3 or $\Omega _*=(2.17 \pm 0.03) \times 10^{-3} \, h_{70}^{-1}$. We conclude that at z < 0.1, the Universe has converted 4.9 ± 0.1 per cent of the baryonic mass implied by big bang Nucleosynthesis into stars that are gravitationally bound within the galaxy population.

Our current understanding of galaxy evolution still has many uncertainties associated with the details of accretion, processing, and removal of gas across cosmic time. The next generation of radio telescopes will image the neutral hydrogen (HI) in galaxies over large volumes at high redshifts, which will provide key insights into these processes. We are conducting the COSMOS H I Large Extragalactic Survey (CHILES) with the Karl G. Jansky Very Large Array, which is the first survey to simultaneously observe H I from z = 0 to z ∼ 0.5. Here, we report the highest redshift H I 21-cm detection in emission to date of the luminous infrared galaxy (LIRG) COSMOS J100054.83+023126.2 at z=0.376 with the first 178 hours of CHILES data. The total H I mass is (2.9 ± 1.0) × 10 10 M , and the spatial distribution is asymmetric and extends beyond the galaxy. While optically the galaxy looks undisturbed, the H I distribution suggests an interaction with candidate a candidate companion. In addition, we present follow-up Large Millimeter Telescope CO observations that show it is rich in molecular hydrogen, with a range of possible masses of (1.8 − 9.9) × 10 10 M . This is the first study of the H I and CO in emission for a single galaxy beyond z ∼ 0.2.

Meyer’s (2012) qualitative research on motivation of German karateka initiated the coordinated research project Why Martial Arts? (WMA) to analyse motives in various martial arts styles, like jūdō, taiji, krav maga and wing chun. In 2017, the Japanese Society for the Promotion of Science (JSPS) supported the transposition of the research question to Japanese karatedō and jūdō practitioners. For the German sub-study, 32 interviews were conducted about entry/participation motives, fascination categories, and reasons for choosing karatedō. The design of the Japanese sub-study was based on the aforementioned German study, but due to the higher number of participants (n = 106), a mixed method questionnaire was used and distributed via paper and online versions. The results demonstrate that many motivation categories of Japanese and German karatedō practitioners share similarities in importance and content, although the characteristics of motives can be very different—partly due to cultural specifics.

We present a new technique for the statistical evaluation of the Tully-Fisher relation (TFR) using spectral line stacking. This technique has the potential to extend TFR observations to lower masses and higher redshifts than possible through a galaxy-bygalaxy analysis. It further avoids the need for individual galaxy inclination measurements.To quantify the properties of stacked H i emission lines, we consider a simplistic model of galactic disks with analytically expressible line profiles. Using this model, we compare the widths of stacked profiles with those of individual galaxies. We then follow the same procedure using more realistic mock galaxies drawn from the S 3 -SAX model (a derivative of the Millennium simulation). Remarkably, when stacking the apparent H i lines of galaxies with similar absolute magnitude and random inclinations, the width of the stack is very similar to the width of the deprojected (= corrected for inclination) and dedispersed (= after removal of velocity dispersion) input lines. Therefore, the ratio between the widths of the stack and the deprojected/dedispersed input lines is approximately constant -about 0.93 -with very little dependence on the gas dispersion, galaxy mass, galaxy morphology, and shape of the rotation curve.Finally, we apply our technique to construct a stacked TFR using HIPASS data which already has a well defined TFR based on individual detections. We obtain a Bband TFR with a slope of −8.5 ± 0.4 and a K-band relation with a slope of −11.7 ± 0.6 for the HIPASS data set which is consistent with the existing results.