- ID:
- ivo://CDS.VizieR/J/ApJ/857/144
- Title:
- Tidal features from RESOLVE survey & DECaLS images
- Short Name:
- J/ApJ/857/144
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study tidal features around galaxies in the REsolved Spectroscopy Of a Local VolumE (RESOLVE) survey. Our sample consists of 1048 RESOLVE galaxies that overlap with the DECam Legacy Survey, which reaches an r-band 3{sigma} depth of ~27.9mag/arcsec^2^ for a 100arcsec^2^ feature. Images were masked, smoothed, and inspected for tidal features such as streams, shells, or tails/arms. We find tidal features in 17+/-2% of our galaxies, setting a lower limit on the true frequency. The frequency of tidal features in the gas-poor (gas-to-stellar mass ratio <0.1) subsample is lower than in the gas-rich subsample (13+/-3% versus 19+/-2%). Within the gas-poor subsample, galaxies with tidal features have higher stellar and halo masses, ~3x closer distances to nearest neighbors (in the same group), and possibly fewer group members at fixed halo mass than galaxies without tidal features, but similar specific star formation rates. These results suggest tidal features in gas-poor galaxies are typically streams/shells from dry mergers or satellite disruption. In contrast, the presence of tidal features around gas-rich galaxies does not correlate with stellar or halo mass, suggesting these tidal features are often tails/arms from resonant interactions. Similar to tidal features in gas-poor galaxies, tidal features in gas-rich galaxies imply 1.7x closer nearest neighbors in the same group; however, they are associated with diskier morphologies, higher star formation rates, and higher gas content. In addition to interactions with known neighbors, we suggest that tidal features in gas-rich galaxies may arise from accretion of cosmic gas and/or gas-rich satellites below the survey limit.
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- ID:
- ivo://CDS.VizieR/J/AJ/130/2647
- Title:
- Tidal features of 126 nearby red galaxies
- Short Name:
- J/AJ/130/2647
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a study of tidal debris associated with 126 nearby red galaxies, selected from the 1.2{deg}^2^ Multiwavelength Survey by Yale-Chile (MUSYC, Cat. <J/ApJS/162/1>) and the 9.3{deg}^2^ NOAO Deep Wide-Field Survey (Jannuzi & Dey, 1999ASPC..191..111J). In the full sample, 67 galaxies (53%) show morphological signatures of tidal interactions consisting of broad fans of stars, tails, and other asymmetries at very faint surface brightness levels. When restricting the sample to the 86 bulge-dominated early-type galaxies, the fraction of tidally disturbed galaxies rises to 71%, which implies that for every "normal" undisturbed elliptical there are two that show clear signs of interactions. The tidal features are red and smooth and often extend over >50kpc.
- ID:
- ivo://CDS.VizieR/J/MNRAS/417/2347
- Title:
- Tully-Fisher relation for SDSS galaxies
- Short Name:
- J/MNRAS/417/2347
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z<0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).
- 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/AJ/113/22
- Title:
- Tully-Fisher Relation. I.
- Short Name:
- J/AJ/113/22
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Observational parameters which can be used for redshift-independent distance determination using the Tully-Fisher (TF) technique are given for 782 spiral galaxies in the fields of 24 clusters or groups. I band photometry for the full sample was either obtained by us or compiled from published literature. Rotational velocities are derived either from 21 cm spectra or optical emission line long-slit spectra, and converted to a homogeneous scale. In addition to presenting the data, a discussion of the various sources of error on TF parameters is introduced, and the criteria for the assignment of membership to each cluster are given.
- ID:
- ivo://CDS.VizieR/J/A+A/535/A80
- Title:
- Type-2 QSOs in XMM-COSMOS
- Short Name:
- J/A+A/535/A80
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We explore the connection between black hole growth at the center of obscured quasars selected from the XMM-COSMOS survey and the physical properties of their host galaxies. We study a bolometric regime (<Lbol>=8x10^45^erg/s) where several theoretical models invoke major galaxy mergers as the main fueling channel for black hole accretion. To derive robust estimates of the host galaxy properties, we use an SED fitting technique to distinguish the AGN and host galaxy emission. We evaluate the effect on galaxy properties estimates of being unable to remove the nuclear emission from the SED. The superb multi-wavelength coverage of the COSMOS field allows us to obtain reliable estimates of the total stellar masses and star formation rates (SFRs) of the hosts. We supplement this information with a morphological analysis of the ACS/HST images, optical spectroscopy, and an X-ray spectral analysis.
- ID:
- ivo://CDS.VizieR/J/A+A/398/49
- Title:
- UBgRIJKs photometry in the FORS Deep Field
- Short Name:
- J/A+A/398/49
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The FORS Deep Field project is a multi-colour, multi-object spectroscopic investigation of a 7' times 7' region near the south galactic pole based mostly on observations carried out with the FORS instruments attached to the VLT telescopes. It includes the QSO Q0103-260 (z=3.36). The goal of this study is to improve our understanding of the formation and evolution of galaxies in the young Universe. In this paper the field selection, the photometric observations, and the data reduction are described. The source detection and photometry of objects in the FORS Deep Field is discussed in detail. A combined B and I selected UBgRIJKs photometric catalog of 8753 objects in the FDF is presented and its properties are briefly discussed. The formal 50% completeness limits for point sources, derived from the coadded images, are 25.64, 27.69, 26.86, 26.68, 26.37, 23.60 and 21.57 in U, B, g, R, I, J and Ks (Vega-system), respectively. A comparison of the number counts in the FORS Deep Field to those derived in other deep field surveys shows very good agreement.
- ID:
- ivo://CDS.VizieR/J/ApJS/162/49
- Title:
- UBV imaging of irregular galaxies
- Short Name:
- J/ApJS/162/49
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of UBV imaging of a large sample of irregular galaxies: 94 Im systems, 24 blue compact dwarfs (BCDs), and 18 Sm galaxies. We also include JHK imaging of 42 of these galaxies. The sample spans a large range in galactic parameters. Ellipse fit axial ratios, inclinations, and position angles are derived, integrated photometry and azimuthally averaged surface photometry profiles are determined, and exponential fits give the central surface brightnesses, scale lengths, and isophotal and half-power radii.
- ID:
- ivo://CDS.VizieR/J/A+A/415/63
- Title:
- UBVRI surface brightness of 26 bright galaxies
- Short Name:
- J/A+A/415/63
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The UBVRI images of 26 bright spiral galaxies were decomposed in disks and bulges. Correlations of the resulting structural parameters are investigated, giving clues to the formation history of the bulges. We confirm that the large and bright bulges of early-type spirals are similar to elliptical galaxies. They were probably formed prior to the disks in a monolithic collapse or via early mergers. Late-type spirals have tiny and faint bulges with disk-like profiles. These bulges were probably formed after the disk in secular evolution processes, e.g. from a disk instability. The comparison of the color indices of corresponding spirals and bulges with population synthesis computations support above formation scenarios.
- ID:
- ivo://CDS.VizieR/J/A+A/625/A50
- Title:
- Ultra compact dwarf galaxies catalog
- Short Name:
- J/A+A/625/A50
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Photometric surveys of galaxy clusters have revealed a large number of ultra compact dwarfs (UCDs) around predominantly massive elliptical galaxies. Their origin is still debated as some UCDs are considered to be the remnant nuclei of stripped dwarf galaxies while others seem to mark the high-mass end of the star cluster population. We aim to characterize the properties of a UCD found at very close projected distance (r_wproj_=1.1kpc) from the centre of the low-mass (M~10^10^M_{sun}_) early-type galaxy FCC 47. This is a serendipitous discovery from MUSE adaptive optics science verification data. We explore the potential origin of this UCD as either a massive cluster or the remnant nucleus of a dissolved galaxy. We used archival Hubble Space Telescope data to study the photometric and structural properties of FCC 47-UCD1. In the MUSE data, the UCD is unresolved, but we used its spectrum to determine the radial velocity and metallicity. The surface brightness of FCC 47-UCD1 is best described by a single King profile with low concentration C=Rt/Rc~10 and large effective radius (r_eff_=24pc). Its integrated magnitude and blue colour (Mg=-10.55mag, (g-z)=1.46mag) combined with a metallicity of [M/H]=-1.12+/-0.10dex and an age >8Gyr obtained from the full fitting of the MUSE spectrum suggests a stellar population mass of M*=4.87x10^6^M_{sun}_. The low S/N of the MUSE spectrum prevents detailed stellar population analysis. Due to the limited spectral resolution of MUSE, we can only give an upper limit on the velocity dispersion ({sigma}<17km/s), and consequently on its dynamical mass (M_dyn_<1.3x10^7^M_{sun}_). The origin of the UCD cannot be constrained with certainty. The low metallicity, old age, and magnitude are consistent with a star cluster origin, whereas the extended size is consistent with an origin as the stripped nucleus of a dwarf galaxy with a initial stellar mass of a few 10^8^M_{sun}_.
