- ID:
- ivo://CDS.VizieR/J/MNRAS/387/1099
- Title:
- Spectroscopic study of 10 high SB galaxies
- Short Name:
- J/MNRAS/387/1099
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Photometry and long-slit spectroscopy are presented for a sample of six galaxies with a low surface-brightness stellar disc and a bulge. The characterizing parameters of the bulge and disc components were derived by means of a two-dimensional photometric decomposition of the images of the sample galaxies. Their surface-brightness distribution was assumed to be the sum of the contribution of a Sersic bulge and an exponential disc, with each component being described by elliptical and concentric isophotes of constant ellipticity and position angle. The stellar and ionized-gas kinematics were measured along the major and minor axes in half of the sample galaxies, whereas the other half was observed only along two diagonal axes. Spectra along two diagonal axes were obtained also for one of the objects with major and minor axis spectra. The kinematic measurements extend in the disc region out to a surface-brightness level mu_R_~24mag/arcsec^2^, reaching in all cases the flat part of the rotation curve. The stellar kinematics turns out to be more regular and symmetric than the ionized-gas kinematics, which often shows the presence of non-circular, off-plane and non-ordered motions. This raises the question about the reliability of the use of the ionized gas as the tracer of the circular velocity in the modelling of the mass distribution, in particular in the central regions of low surface-brightness galaxies.
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Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/146/45
- Title:
- Spectroscopy of 6 early-type galaxies
- Short Name:
- J/AJ/146/45
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Adaptive optics assisted SINFONI observations of the central regions of 10 early-type galaxies are presented. Based primarily on the SINFONI kinematics, 10 black hole (BH) masses occupying the high-mass regime of the M_BH_-{sigma} relation are derived using three-integral Schwarzschild models. The effect of dark matter (DM) inclusion on the BH mass is explored. The omission of a DM halo in the model results in a higher stellar mass-to-light ratio, especially when extensive kinematic data are used in the model. However, when the diameter of the sphere of influence--computed using the BH mass derived without a dark halo--is at least 10 times the point-spread function FWHM during the observations, it is safe to exclude a DM component in the dynamical modeling, i.e., the change in BH mass is negligible. When the spatial resolution is marginal, restricting the mass-to-light ratio to the right value returns the correct M_BH_ although a dark halo is not present in the model. Compared to the M_BH_-{sigma} and M_BH_-L relations of McConnell et al., the 10 BHs are all more massive than expected from the luminosities and 7 BH masses are higher than expected from the stellar velocity dispersions of the host bulges. Using new fitted relations, which include the 10 galaxies, we find that the space density of the most massive BHs (M_BH_>~10^9^M_{sun}_) estimated from the M_BH_-L relation is higher than the estimate based on the M_BH_-{sigma} relation and the latter is higher than model predictions based on quasar counts, each by about an order of magnitude.
- ID:
- ivo://CDS.VizieR/J/AJ/130/1037
- Title:
- Spiral galaxies rotation curve data
- Short Name:
- J/AJ/130/1037
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present new long-slit H{alpha} spectroscopy for 403 non-interacting spiral galaxies, obtained at the Palomar Observatory 5m Hale telescope, which is used to derive well-sampled optical rotation curves. Because many of the galaxies show optical emission features that are significantly extended along the spectrograph slit, a technique was devised to separate and subtract the night sky lines from the galaxy emission. We exploit a functional fit to the rotation curve to identify its center of symmetry; this method minimizes the asymmetry in the final, folded rotation curve. We derive rotational widths using both velocity histograms and the Polyex model fit. The final rotational width is measured at a radius containing 83% of the total light as derived from I-band images.
- ID:
- ivo://CDS.VizieR/J/ApJS/127/39
- Title:
- Stellar and gas kinematics in early-type galaxies
- Short Name:
- J/ApJS/127/39
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present data on stellar and gaseous kinematics of 14 gas-rich early-type galaxies. File galaxies.dat contains the list of observed galaxies, with coordinates, distance, absolute magnitude, and position angles. File stellar.dat contains stellar rotation curves and velocity dispersion profiles. File gaseous.dat contains the gaseous velocity profiles.
- 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.
- 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/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.
