- ID:
- ivo://CDS.VizieR/J/A+AS/133/317
- Title:
- Stellar kinematics in spiral galaxies
- Short Name:
- J/A+AS/133/317
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of absorption spectroscopy on the inner region of 34 Sa-Sc galaxies. We have determined the central velocity dispersion and, for 32 of these objects, stellar rotation curves and velocity-dispersion profiles. Some of these profiles are limited to the bulge, some others do reach a region dominated by the luminosity of the disk. These data are intended to provide basic material for the study of the mass distribution and dynamical status in the central regions of spiral galaxies. Although no elaborate bulge-and-disk photometric decomposition is performed, we estimate the effects of limited resolution and contamination by disk light on the central velocity dispersion of the bulge.
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- ID:
- ivo://CDS.VizieR/J/A+AS/136/509
- Title:
- Stellar kinematics in spiral galaxies. II.
- Short Name:
- J/A+AS/136/509
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a second dataset of absorption spectroscopy on the inner region of spiral galaxies. We have determined the central velocity dispersion for 42 Sa-Sc objects and, for 32 of them, stellar rotation curves and velocity-dispersion profiles. Some of these profiles are limited to the bulge, some others do reach a region dominated by the luminosity of the disk. These data are intended to provide basic material for the study of the mass distribution and dynamical status in the central regions of spiral galaxies. Although no elaborate bulge-and-disk photometric decomposition is performed, we estimate the effects of limited resolution and contamination by disk light on the central velocity dispersion of the bulge. All the material presented in this paper, in particular the spectra, is available on-line.
- ID:
- ivo://CDS.VizieR/J/ApJ/633/844
- Title:
- Stellar mass in disk-dominated galaxies
- Short Name:
- J/ApJ/633/844
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate the correlations among stellar mass (M*), disk scale length (R_d_), and rotation velocity at 2.2 disk scale lengths (V_2.2_) for a sample of 81 disk-dominated galaxies (disk/total>=0.9) selected from the SDSS. We measure V_2.2_ from long-slit H{alpha} rotation curves and infer M* from galaxy i-band luminosities (L_i_) and g-r colors.
- ID:
- ivo://CDS.VizieR/J/MNRAS/449/4048
- Title:
- The H{alpha} rotation curve of M33
- Short Name:
- J/MNRAS/449/4048
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- As part of a long-term project to revisit the kinematics and dynamics of the large disc galaxies of the Local Group, we present the first deep, wide-field (~42arcmin x 56arcmin) 3D-spectroscopic survey of the ionized gas disc of Messier 33. Fabry-Perot interferometry has been used to map its H{alpha} distribution and kinematics at unprecedented angular resolution (~<3 arcsec) and resolving power (~12600), with the 1.6 m telescope at the Observatoire du Mont Megantic. The ionized gas distribution follows a complex, large-scale spiral structure, unsurprisingly coincident with the already-known spiral structures of the neutral and molecular gas discs. The kinematical analysis of the velocity field shows that the rotation centre of the H{alpha} disc is distant from the photometric centre by ~168 pc (sky-projected distance) and that the kinematical major-axis position angle and disc inclination are in excellent agreement with photometric values. The H{alpha} rotation curve agrees very well with the HI rotation curves for 0<R<6.5 kpc, but the H{alpha} velocities are 10^-20^ km/s higher for R>6.5 kpc. The reason for this discrepancy is not well understood. The velocity dispersion profile is relatively flat around 16 km/s, which is at the low end of velocity dispersions of nearby star-forming galactic discs. A strong relation is also found between the H{alpha} velocity dispersion and the H{alpha} intensity. Mass models were obtained using the H{alpha} rotation curve but, as expected, the dark matter halo's parameters are not very well constrained since the optical rotation curve only extends out to 8 kpc.
- ID:
- ivo://CDS.VizieR/J/AJ/147/134
- Title:
- Tully-Fisher relation for S^4^G galaxies
- Short Name:
- J/AJ/147/134
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We combine data from the Spitzer Survey for Stellar Structure in Galaxies, a recently calibrated empirical stellar mass estimator from Eskew et al., and an extensive database of HI spectral line profiles to examine the baryonic Tully-Fisher (BTF) relation. We find (1) that the BTF has lower scatter than the classic Tully-Fisher (TF) relation and is better described as a linear relationship, confirming similar previous results, (2) that the inclusion of a radial scale in the BTF decreases the scatter but only modestly, as seen previously for the TF relation, and (3) that the slope of the BTF, which we find to be 3.5+/-0.2({Delta}logM_baryon_/{Delta}logv_c_), implies that on average a nearly constant fraction (~0.4) of all baryons expected to be in a halo are "condensed" onto the central region of rotationally supported galaxies. The condensed baryon fraction, M_baryon_/M_total_, is, to our measurement precision, nearly independent of galaxy circular velocity (our sample spans circular velocities, v _c_, between 60 and 250km/s, but is extended to v_c_~10km/s using data from the literature). The observed galaxy-to-galaxy scatter in this fraction is generally {<=} a factor of 2 despite fairly liberal selection criteria. These results imply that cooling and heating processes, such as cold versus hot accretion, mass loss due to stellar winds, and active galactic nucleus driven feedback, to the degree that they affect the global galactic properties involved in the BTF, are independent of halo mass for galaxies with 10<v_c_<250km/s and typically introduce no more than a factor of two range in the resulting M_baryon_/M_total_. Recent simulations by Aumer et al. of a small sample of disk galaxies are in excellent agreement with our data, suggesting that current simulations are capable of reproducing the global properties of individual disk galaxies. More detailed comparison to models using the BTF holds great promise, but awaits improved determinations of the stellar masses.
- ID:
- ivo://CDS.VizieR/J/ApJ/816/L14
- Title:
- Tully-Fisher relation in disk galaxies from SPARC
- Short Name:
- J/ApJ/816/L14
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In a {Lambda} cold dark matter ({Lambda}CDM) cosmology, the baryonic Tully-Fisher relation (BTFR) is expected to show significant intrinsic scatter resulting from the mass-concentration relation of dark matter halos and the baryonic-to-halo mass ratio. We study the BTFR using a sample of 118 disk galaxies (spirals and irregulars) with data of the highest quality: extended HI rotation curves (tracing the outer velocity) and Spitzer photometry at 3.6{mu}m (tracing the stellar mass). Assuming that the stellar mass-to-light ratio ({Upsilon}_*_) is nearly constant at 3.6{mu}m, we find that the scatter, slope, and normalization of the BTFR systematically vary with the adopted {Upsilon}_*_. The observed scatter is minimized for {Upsilon}_*_>~0.5M_{Sun}_/L_{Sun}_, corresponding to nearly maximal disks in high-surface-brightness galaxies and BTFR slopes close to ~4. For any reasonable value of {Upsilon}_*_, the intrinsic scatter is ~0.1dex, below general {Lambda}CDM expectations. The residuals show no correlations with galaxy structural parameters (radius or surface brightness), contrary to the predictions from some semi-analytic models of galaxy formation. These are fundamental issues for {Lambda}CDM cosmology.
- ID:
- ivo://CDS.VizieR/J/A+A/647/A152
- Title:
- Tully-Fisher relation in MAGIC groups
- Short Name:
- J/A+A/647/A152
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Galaxies in dense environments are subject to interactions and mechanisms that directly affect their evolution by lowering their gas fractions and consequently reducing their star-forming capacity earlier than their isolated counterparts. The aim of our project is to get new insights into the role of environment in the stellar and baryonic content of galaxies using a kinematic approach, through the study of the Tully-Fisher relation (TFR). We study a sample of galaxies in eight groups, over-dense by a factor larger than 25 with respect to the average projected density, spanning a redshift range of 0.5<z<0.8 and located in ten pointings of the MAGIC MUSE Guaranteed Time Observations program. We perform a morpho-kinematics analysis of this sample and set up a selection based on galaxy size, [OII]{lambda}{lambda}3727,3729 emission line doublet signal-to-noise ratio, bulge-to-disk ratio, and nuclear activity to construct a robust kinematic sample of 67 star-forming galaxies. We show that this selection considerably reduces the number of outliers in the TFR, which are predominantly dispersion-dominated galaxies. Similar to other studies, we find that including the velocity dispersion in the velocity budget mainly affects galaxies with low rotation velocities, reduces the scatter in the relation, increases its slope, and decreases its zero-point. Including gas masses is more significant for low-mass galaxies due to a larger gas fraction, and thus decreases the slope and increases the zero-point of the relation. Our results suggest a significant offset of the TFR zero-point between galaxies in low- and high-density environments, regardless of the kinematics estimator used. This can be interpreted as a decrease in either stellar mass by ~0.05-0.3dex or an increase in rotation velocity by ~0.02-0.06dex for galaxies in groups, depending on the samples used for comparison. We also studied the stellar and baryon mass fractions within stellar disks and found they both increase with stellar mass, the trend being more pronounced for the stellar component alone. These fractions do not exceed 50%. We show that this evolution of the TFR is consistent either with a decrease in star formation or with a contraction of the mass distribution due to the environment. These two effects probably act together, with their relative contribution depending on the mass regime.
- ID:
- ivo://CDS.VizieR/J/A+A/587/A160
- Title:
- 3.6um S4G Galactic bars characterization
- Short Name:
- J/A+A/587/A160
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Stellar bars play an essential role in the secular evolution of disk galaxies because they are responsible for the redistribution of matter and angular momentum. Dynamical models predict that bars become stronger and longer in time, while their rotation speed slows down. We use the Spitzer Survey of Stellar Structure in Galaxies (S^4^G) 3.6um imaging to study the properties (length and strength) and fraction of bars at z=0 over a wide range of galaxy masses (M*~=10^8^-10^11^M_{sun}_) and Hubble types (-3<=T<=10). We calculated gravitational forces from the 3.6um images for galaxies with a disk inclination lower than 65{deg}. We used the maximum of the tangential-to-radial force ratio in the bar region (Qb) as a measure of the bar-induced perturbation strength for a sample of ~600 barred galaxies. We also used the maximum of the normalized m=2 Fourier density amplitude (A_2_^max^) and the bar isophotal ellipticity ({epsilon}) to characterize the bar. Bar sizes were estimated i) visually, ii) from ellipse fitting, iii) from the radii of the strongest torque, and iv) from the radii of the largest m=2 Fourier amplitude in the bar region. By combining our force calculations with the HI kinematics from the literature, we estimated the ratio of the halo-to-stellar mass (Mh/M*) within the optical disk and by further using the universal rotation curve models, we obtained a first-order model of the rotation curve decomposition of 1128 disk galaxies. We probe possible sources of uncertainty in our Qb measurements: the assumed scale height and its radial variation, the influence of the spiral arms torques, the effect of non-stellar emission in the bar region, and the dilution of the bar forces by the dark matter halo (our models imply that only ~10% of the disks in our sample are maximal). We find that for early- and intermediate-type disks (-3<=T<5), the relatively modest influence of the dark matter halo leads to a systematic reduction of the mean Qb by about 10-15%, which is of the same order as the uncertainty associated with estimating the vertical scale height. The halo correction on Qb becomes important for later types, implying a reduction of ~20-25% for T=7-10. Whether the halo correction is included or not, the mean Qb shows an increasing trend with T. However, the mean A_2_^max^ decreases for lower mass late-type systems. These opposing trends are most likely related to the reduced force dilution by bulges when moving towards later type galaxies. Nevertheless, when treated separately, both the early- and late-type disk galaxies show a strong positive correlation between Qb and A_2_^max^. For spirals the mean {epsilon}~0.5 is nearly independent of T, but it drops among S0s (~0.2). The Qb and {epsilon} show a relatively tight dependence, with only a slight difference between early and late disks. For spirals, all our bar strength indicators correlate with the bar length (scaled to isophotal size). Late-type bars are longer than previously found in the literature. The bar fraction shows a double-humped distribution in the Hubble sequence (~75% for Sab galaxies), with a local minimum at T=4 (~40%), and it drops for M*<~10^9.5-10^M_{sun}_. If we use bar identification methods based on Fourier decomposition or ellipse fitting instead of the morphological classification, the bar fraction decreases by ~30-50% for late-type systems with T>=5 and correlates with Mh/M*. Our Mh/M* ratios agree well with studies based on weak lensing analysis, abundance matching, and halo occupation distribution methods, under the assumption that the halo inside the optical disk contributes roughly a constant fraction of the total halo mass (~4%). We find possible evidence for the growth of bars within a Hubble time, as (1) bars in early-type galaxies show larger density amplitudes and disk-relative sizes than their intermediate-type counterparts, and (2) long bars are typically strong. We also observe two clearly distinct types of bars, between early- and intermediate-type galaxies (T<5) on one side, and the late-type systems on the other, based on the differences in the bar properties. Most likely this distinction is connected to the higher halo-to-stellar ratio that we observe in later types, which affects the disk stability properties.
- ID:
- ivo://CDS.VizieR/J/AJ/145/101
- Title:
- Updated nearby galaxy catalog
- Short Name:
- J/AJ/145/101
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present an all-sky catalog of 869 nearby galaxies having individual distance estimates within 11Mpc or corrected radial velocities V_LG_<600km/s. The catalog is a renewed and expanded version of the Catalog of Neighboring Galaxies by Karachentsev et al (2004, cat. J/AJ/127/2031). It collects data on the following galaxy observables: angular diameters, apparent magnitudes in far-UV, B, and K_s_bands, H{alpha} and HI fluxes, morphological types, HI-line widths, radial velocities, and distance estimates. In this Local Volume (LV) sample, 108 dwarf galaxies still remain without measured radial velocities. The catalog yields also calculated global galaxy parameters: linear Holmberg diameter, absolute B magnitude, surface brightness, HI mass, stellar mass estimated via K-band luminosity, HI rotational velocity corrected for galaxy inclination, indicative mass within the Holmberg radius, and three kinds of "tidal index," which quantify the local density environment. The catalog is supplemented with data based on the local galaxies, which presents their optical and available H{alpha} images, as well as other services. We briefly discuss the Hubble flow within the LV and different scaling relations that characterize galaxy structure and global star formation in them. We also trace the behavior of the mean stellar mass density, HI-mass density, and star formation rate density within the volume considered.
- ID:
- ivo://CDS.VizieR/J/MNRAS/326/473
- Title:
- Vel. Distribution of low-luminosity E galaxies
- Short Name:
- J/MNRAS/326/473
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The shape of the line-of-sight velocity distribution (LOSVD) is measured for a sample of 14 elliptical galaxies, predominantly low-luminosity ellipticals. The sample is dominated by galaxies in the Virgo cluster but also contains ellipticals in nearby groups and low density environments. The parameterization of the LOSVD due to Gerhard and van der Marel & Franx is adopted, which measures the asymmetrical and symmetrical deviations of the LOSVD from a Gaussian by the amplitudes h3 and h4 of the Gauss-Hermite series. Rotation, velocity dispersion, h3 and h4 are determined as a function of radius for both major and minor axes using the Fourier Correlation Quotient method of Bender (1990). Galaxy spectra are rebinned in the direction of the spectroscopic slit to a minimum signal-to-noise ratio (S/N) of 60 per angstrom. Rotation and velocity dispersion are determined separately for S/N = 30 per angstrom.
