- ID:
- ivo://CDS.VizieR/J/A+A/533/A122
- Title:
- Diffuse neutral hydrogen in HIPASS
- Short Name:
- J/A+A/533/A122
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Observations of neutral hydrogen can provide a wealth of information about the distribution and kinematics of galaxies. To learn more about large scale structures and accretion processes, the extended environment of galaxies must also be observed. Numerical simulations predict a cosmic web of extended structures and gaseous filaments. To detect HI beyond the ionisation edge of galaxy disks, column density sensitivities have to be achieved that probe the regime of Lyman limit systems. Typically HI observations are limited to a brightness sensitivity of N_HI_~10^19^cm^-2^ but this has to be improved by at least an order of magnitude.
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/596/A25
- Title:
- Disc breaks across masses and wavelengths
- Short Name:
- J/A+A/596/A25
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Breaks in the surface brightness profiles in the outer regions of galactic discs are thought to have formed by various internal (e.g. bar resonances) and external (e.g. galaxy merging) processes. By studying the disc breaks we aim to better understand what processes are responsible for the evolution of the outer discs of galaxies, and galaxies in general. We use a large well-defined sample to study how common the disc breaks are, and whether their properties depend on galaxy mass. By using both optical and infrared data we study whether the observed wavelength affects the break features as a function of galaxy mass and Hubble type. We studied the properties of galaxy discs using radial surface brightness profiles of 753 galaxies, obtained from the 3.6um images of the Spitzer Survey of Stellar Structure in Galaxies (S4G), and the Ks-band data from the Near InfraRed S0-Sa galaxy Survey (NIRS0S), covering a wide range of galaxy morphologies (-2<=T<=9) and stellar masses (8.5<~log10 (M*/M_{sun}_)<~11). In addition, optical Sloan Digital Sky Survey (SDSS) or Liverpool telescope data was used for 480 of these galaxies. We find that in low-mass galaxies the single exponential profiles (Type I) are most common, and that their fraction decreases with increasing galaxy stellar mass. The fraction of down-bending (Type II) profiles increases with stellar mass, possibly due to more common occurrence of bar resonance structures. The up-bending (Type III) profiles are also more common in massive galaxies. The observed wavelength affects the scalelength of the disc of every profile type. Especially the scalelength of the inner disc (h_i_) of Type II profiles increases from infrared to u-band on average by a factor of ~2.2. Consistent with the previous studies, but with a higher statistical significance, we find that Type II outer disc scalelengths (h_o_) in late-type and low mass galaxies (T>4, log10(M*/M_{sun}_)<~10.5) are shorter in bluer wavelengths, possibly due to stellar radial migration populating the outer discs with older stars. In Type III profiles h_o are larger in the u band, hinting to the presence of young stellar population in the outer disc. While the observed wavelength affects the disc parameters, it does not significantly affect the profile type classification in our sample. Our results indicate that the observed wavelength is a significant factor when determining the profile types in very low mass dwarf galaxies, for which more Type II profiles have been previously found using optical data.
- ID:
- ivo://CDS.VizieR/J/MNRAS/487/2061
- Title:
- Distances for 2062 nearby spiral galaxies
- Short Name:
- J/MNRAS/487/2061
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the final distance measurements for the 2MASS Tully-Fisher (2MTF) survey. The final 2MTF catalogue contains 2062 nearby spiral galaxies in the CMB frame velocity range of 600<cz<10000km/s with a mean velocity of 4805km/s. The main update in this release is the replacement of some archival HI data with newer ALFALFA data. Using the 2MTF template relation, we calculate the distances and peculiar velocities of all 2MTF galaxies. The mean uncertainties of the linear distance measurements are around 22 per cent in all three infrared bands. 2MTF measurements agree well with the distances from the Cosmicflows-3 compilation, which contains 1117 common galaxies, including 28 with SNIa distance measurements. Using distances estimated from the '3-bands combined' 2MTF sample and a {chi}^2^ minimization method, we find best-fitting bulk flow amplitudes of 308+/-26km/s, 318+/-29km/s, and 286+/-25km/s at depths of R_I_=20, 30 and 40h^-1^Mpc, respectively, which is consistent with the {LAMNDA}CDM model and with previous 2MTF results with different estimation techniques and a preliminary catalogue.
- ID:
- ivo://CDS.VizieR/J/other/A+ARV/15.289
- Title:
- Distances of local galaxies
- Short Name:
- J/other/A+ARV/15
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Any calibration of the present value of the Hubble constant (H_0_) requires recession velocities and distances of galaxies. While the conversion of observed velocities into true recession velocities has only a small effect on the result, the derivation of unbiased distances which rest on a solid zero point and cover a useful range of about 4-30Mpc is crucial. A list of 279 such galaxy distances within v<2000km/s is given which are derived from the tip of the red-giant branch (TRGB), from Cepheids, and/or from supernovae of type Ia (SNe Ia).
- ID:
- ivo://CDS.VizieR/J/AJ/123/51
- Title:
- Distribution of Abell and APM clusters
- Short Name:
- J/AJ/123/51
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a comparison of how well the large-scale structure of the universe is traced by clusters from the Abell catalog and from the Automated Plate Measuring Facility (APM). We investigate selection functions for both cluster catalogs, using samples of all clusters (including clusters with estimated redshifts) and samples of clusters with measured redshifts. We present a catalog of superclusters of galaxies, based on APM clusters up to a redshift z_lim_=0.13.
- ID:
- ivo://CDS.VizieR/J/ApJS/178/1
- Title:
- Distribution of HII regions in disk galaxies
- Short Name:
- J/ApJS/178/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- It is known that interstellar gas has a fractal structure in a wide range of spatial scales with a fractal dimension that seems to be a constant around D_f_~2.7. It is expected that stars forming from this fractal medium exhibit similar fractal patterns. Here we address this issue by quantifying the degree to which star-forming events are clumped. We develop, test, and apply a precise and accurate technique to calculate the correlation dimension Dc of the distribution of HII regions in a sample of disk galaxies.
- ID:
- ivo://CDS.VizieR/VII/168
- Title:
- Double Galaxies in SGP region
- Short Name:
- VII/168
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- 630 double systems of galaxies brighter than about 17mag(B) were found by examining 100 glass copies of ESO(B) survey plates, covering the Southern Galactic Cap (GLAT<-50deg, DE<-27deg). The selection criteria are similar to those defined by Zonn (1962). The measuring, reduction and error analysis parameters have been described by Zou et al. (1984).
- ID:
- ivo://CDS.VizieR/J/MNRAS/300/417
- Title:
- Durham/UKST Galaxy Redshift Survey
- Short Name:
- J/MNRAS/300/417
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.
- ID:
- ivo://CDS.VizieR/J/A+A/644/A144
- Title:
- Dusty star-forming galaxies physical properties
- Short Name:
- J/A+A/644/A144
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The dust-to-stellar mass ratio (M_dust_/M*) is a crucial yet poorly constrained quantity to understand the complex physical processes involved in the production of dust, metals and stars in galaxy evolution. In this work we explore trends of M_dust_/M* with different physica parameters using observations of 300 massive, dusty star-forming galaxies detected with ALMA up to z~5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that M_dust_/M* evolves with redshift, stellar mass, specific star formation rate and integrated dust size, differently for main sequence and starburst galaxies. In both galaxy populations M_dust_/M* increases until z~2 followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between M_dust_/M* and M* holds up to z~5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that M_dust_/M* in starbursts reflects the increase in molecular gas fraction with redshift, and attains the highest values for sources with the most compact dusty star-formation. The state-of-the-art cosmological simulations that include self-consistent dust growth, broadly reproduce the evolution of M_dust_/M* in main sequence galaxies, but underestimate it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust growth timescales relative to observations. Phenomenological models based on the main-sequence/starburst dichotomy and analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high M_dust_/M* is due to rapid dust grain growth in metal enriched interstellar medium. This work highlights multifold benefits of using M_dust_/M* as a diagnostic tool for: (1) disentangling main sequence and starburst galaxies up to z~5; (2) probing the evolutionary phase of massive objects; and (3) refining the treatment of the dust life cycle in simulations.
- ID:
- ivo://CDS.VizieR/J/MNRAS/468/2645
- Title:
- Dynamics of A3266. I. An Optical View.
- Short Name:
- J/MNRAS/468/2645
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present spectroscopy of 880 galaxies within a 2-degree field around the massive, merging cluster Abell 3266. This sample, which includes 704 new measurements, was combined with the existing redshifts measurements to generate a sample of over 1300 spectroscopic redshifts; the largest spectroscopic sample in the vicinity of A3266 to date. We define a cluster sub-sample of 790 redshifts which lie within a velocity range of 14000 to 22000km/s and within 1 degree of the cluster centre. A detailed structural analysis finds A3266 to have a complex dynamical structure containing six groups and filaments to the north of the cluster as well as a cluster core which can be decomposed into two components split along a northeast-southwest axis, consistent with previous X-ray observations. The mean redshift of the cluster core is found to be 0.0594+/-0.0005 and the core velocity dispersion is given as 1462+/-99km/s. The overall velocity dispersion and redshift of the entire cluster and related structures are 1337+/-67 km/s and 0.0596+/-0.0002, respectively, though the high velocity dispersion does not represent virialised motions but rather is due to relative motions of the cluster components. We posit A3266 is seen following a merger along the northeast southwest axis, however, the rich substructure in the rest of the cluster suggests that the dynamical history is more complex than just a simple merger with a range of continuous dynamical interactions taking place. It is thus likely that turbulence in A3266 is very high, even for a merging cluster.
