- ID:
- ivo://CDS.VizieR/V/36B
- Title:
- Supplement to the Bright Star Catalogue
- Short Name:
- V/36B
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The catalog is an extension of the BSC4 (Hoffleit 1982; see catalog <V/50>) and contains compiled data on stars for which photoelectric determinations are given as 7.10V or brighter and that are not already included in the latter catalog. The data included in the supplement are basically the same as those in the BSC4 itself, and the format of the machine version is very similar. Notable differences are that the NAME column has been omitted, since very few supplement stars have Bayer or Flamsteed designations, and has been replaced with the SAO number. Also, the parallax field includes only data determined from trigonometric methods; all dynamical parallax data have been relegated to the REMARKS. Position-angle data are given in the main table for double stars, whereas they were contained, if reported, only in the REMARKS file of the BSC4. Remarks for supplement stars are given in a separate file of the machine version and are present for 49% of the stars. The introductory file "intro.doc" contains the text given in the introduction to the published catalog except that the figures are, of course, not included. Data included in the catalog "bsc4s.dat" are HD number; DM number; SAO number; double-star code or identification; variable-star identification; right ascension (B1900) declination, right ascension (B2000) declination; galactic coordinates; V magnitude; B-V, U-B, R-I colors; spectral type; annual proper motions; parallax; radial velocity (km/s): and projected rotational velocity v sin i (km/s). Data included for multiple stars are magnitude difference, separation (arcsec), position angle (PA) of components, component identifications (A, B, ...), and number of components (N). A remarks flag is included as a pointer to a remarks file. The third file "remarks.dat" contains the actual remarks for stars flagged in the data file.
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Search Results
- ID:
- ivo://CDS.VizieR/II/135
- Title:
- Suppl. to Diffuse Interstellar Band Measurements
- Short Name:
- II/135
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This bibliographic search has been undertaken in order to gather all data concerning four diffuse interstellar bands (DIB) published since the Snow, York, and Welty (1977) catalogue, and up to 1987.0. These four DIB are : 4430, 5780, 5797, and 6284 Angstrom. In the present set of data, no statistical reduction to a unique system has been made because most of the lists contain only few data.
- ID:
- ivo://CDS.VizieR/J/ApJS/214/19
- Title:
- Suprime-Cam wide-field photometry of Leo A
- Short Name:
- J/ApJS/214/19
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have surveyed a complete extent of Leo A --an apparently isolated gas-rich low-mass dwarf irregular galaxy in the Local Group. The B, V, and I passband CCD images (typical seeing ~0.8") were obtained with the Subaru Telescope equipped with the Suprime-Cam mosaic camera. The wide-field (20'x24') photometry catalog of 38856 objects (V~16-26mag) is presented. This survey is also intended to serve as "a finding chart" for future imaging and spectroscopic observation programs of Leo A.
- ID:
- ivo://CDS.VizieR/J/AJ/132/447
- Title:
- Surface Brightness of 38 Gal. Globular Clusters
- Short Name:
- J/AJ/132/447
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Hubble Space Telescope (HST) allows us to study the central surface brightness profiles of globular clusters at unprecedented detail. We have mined the HST archives to obtain 38 WFPC2 images of Galactic globular clusters with adequate exposure times and filters, which we use to measure their central structure.
- ID:
- ivo://CDS.VizieR/J/ApJ/771/59
- Title:
- Surface brightness of S^4^G face-on galaxies
- Short Name:
- J/ApJ/771/59
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have analyzed the radial distribution of old stars in a sample of 218 nearby face-on disks, using deep 3.6{mu}m images from the Spitzer Survey of Stellar Structure in Galaxies. In particular, we have studied the structural properties of those disks with a broken or down-bending profile. We find that, on average, disks with a genuine single-exponential profile have a scale length and a central surface brightness which are intermediate to those of the inner and outer components of a down-bending disk with the same total stellar mass. In the particular case of barred galaxies, the ratio between the break and the bar radii (R_br_/R_bar_) depends strongly on the total stellar mass of the galaxy. For galaxies more massive than 10^10^M_{sun}_, the distribution is bimodal, peaking at R_br_/R_bar_~2 and ~3.5. The first peak, which is the most populated one, is linked to the outer Lindblad resonance of the bar, whereas the second one is consistent with a dynamical coupling between the bar and the spiral pattern. For galaxies below 10^10^M_{sun}_, breaks are found up to ~10R_bar_, but we show that they could still be caused by resonances given the rising nature of rotation curves in these low-mass disks. While not ruling out star formation thresholds, our results imply that radial stellar migration induced by non-axisymmetric features can be responsible not only for those breaks at ~2R_bar_, but also for many of those found at larger radii.
- ID:
- ivo://CDS.VizieR/J/AJ/143/132
- Title:
- Surface brightness profiles of 10 globulars of M31
- Short Name:
- J/AJ/143/132
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, we present internal surface brightness profiles, using images in the F606W and F814W filter bands observed with the Advanced Camera for Surveys on the Hubble Space Telescope, for 10 globular clusters (GCs) in the outer halo of M31. Standard King models are fitted to the profiles to derive their structural and dynamical parameters. The results show that, in general, the properties of clusters in M31 and the Milky Way fall in the same regions of parameter spaces. The outer halo GCs of M31 have larger ellipticities than most of the GCs in M31 and the Milky Way. Their large ellipticities may be due to galaxy tides coming from satellite dwarf galaxies of M31 or may be related to the apparently more vigorous accretion or merger history that M31 has experienced. The tight correlation of cluster binding energy E_b_ with mass M_mod_indicates that the "fundamental plane" does exist for clusters, regardless of their host environments, which is consistent with previous studies.
- ID:
- ivo://CDS.VizieR/J/ApJ/859/5
- Title:
- Surface brightness profiles of NGC2784 group vs Virgo
- Short Name:
- J/ApJ/859/5
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We investigate surface brightness profiles (SBPs) of dwarf galaxies in field, group, and cluster environments. With deep BVI images from the Korea Microlensing Telescope Network Supernova Program, SBPs of 38 dwarfs in the NGC 2784 group are fitted by a single-exponential or double-exponential model. We find that 53% of the dwarfs are fitted with single-exponential profiles ("Type I"), while 47% of the dwarfs show double-exponential profiles; 37% of all dwarfs have smaller sizes for the outer part than the inner part ("Type II"), while 10% have a larger outer than inner part ("Type III"). We compare these results with those in the field and in the Virgo cluster, where the SBP types of 102 field dwarfs are compiled from a previous study and the SBP types of 375 cluster dwarfs are measured using SDSS r-band images. As a result, the distributions of SBP types are different in the three environments. Common SBP types for the field, the NGC 2784 group, and the Virgo cluster are Type II, Type I and II, and Type I and III profiles, respectively. After comparing the sizes of dwarfs in different environments, we suggest that since the sizes of some dwarfs are changed due to environmental effects, SBP types are capable of being transformed and the distributions of SBP types in the three environments are different. We discuss possible environmental mechanisms for the transformation of SBP types.
- ID:
- ivo://CDS.VizieR/J/ApJ/749/121
- Title:
- Surface brightness profiles of z=2 galaxies
- Short Name:
- J/ApJ/749/121
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We use deep Hubble Space Telescope Wide Field Camera 3 near-infrared imaging obtained of the GOODS-South field as part of the CANDELS survey to investigate a stellar mass-limited sample of quiescent galaxies at 1.5<z<2.5. We measure surface brightness profiles for these galaxies using a method that properly measures low surface brightness flux at large radii. We find that quiescent galaxies at z~2 very closely follow Sersic profiles, with n_median_=3.7, and have no excess flux at large radii. Their effective radii are a factor of ~4 smaller than those of low-redshift quiescent galaxies of similar mass. However, there is a significant spread in sizes ({sigma}_log_10_r_e__=0.24), with the largest z~2 galaxies lying close to the z=0 mass-size relation. We compare the stellar mass surface density profiles with those of massive elliptical galaxies in the Virgo Cluster and confirm that most of the mass growth which occurs between z~2 and z=0 must be due to accretion of material onto the outer regions of the galaxies. Additionally, we investigate the evolution in the size distribution of massive quiescent galaxies. We find that the minimum size growth required for z~2 quiescent galaxies to fall within the z=0 size distribution is a factor of ~2 smaller than the total median size growth between z~2 and z=0.
- ID:
- ivo://CDS.VizieR/J/MNRAS/445/3512
- Title:
- Surface density of dark matter haloes
- Short Name:
- J/MNRAS/445/3512
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this article, we test the conclusion of the universality of the dark matter (DM) halo surface density {mu}_0D_={rho}_0_*r_0. According to our study, the dispersion of values of {mu}_0D_ is twice as high as that found previously by other authors. We conclude that the DM surface density and its Newtonian acceleration are not constant but correlate with the luminosity, morphological type, (B-V)_0_ colour index and content of neutral hydrogen. These DM parameters are higher for more luminous systems of early types with red colour and low gas content. We also found that the correlation of DM parameters with colour index appears to be the manifestation of a stronger relation between DM halo mass and the colour of a galaxy. This finding is in agreement with cosmological simulations. These results leave little room for the recently claimed universality of DM column density. We also found that isolated galaxies in our sample (contained in the Analysis of the interstellar Medium of Isolated GAlaxies (AMIGA) catalogue) do not differ significantly in their value of {mu}_0D_ from the entire sample. Thus, since the AMIGA catalogue gives a sample of galaxies that have not interacted with a significant mass neighbour in the past 3Gyr, the difference between systems with low and high values of {mu}_0D_ is not related to merging events during this period of time.
- ID:
- ivo://CDS.VizieR/J/ApJ/763/73
- Title:
- Surface density profiles of GOODS-South galaxies
- Short Name:
- J/ApJ/763/73
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present stellar mass surface density profiles of a mass-selected sample of 177 galaxies at 0.5<z<2.5, obtained using very deep Hubble Space Telescope optical and near-infrared data over the GOODS-South field, including recent CANDELS data. Accurate stellar mass surface density profiles have been measured for the first time for a complete sample of high-redshift galaxies more massive than 10^10.7^M_{sun}_. The key advantage of this study compared to previous work is that the surface brightness profiles are deconvolved for point-spread function smoothing, allowing accurate measurements of the structure of the galaxies. The surface brightness profiles account for contributions from complex galaxy structures such as rings and faint outer disks. Mass profiles are derived using radial rest-frame ug color profiles and a well-established empirical relation between these colors and the stellar mass-to-light ratio. We derive stellar half-mass radii from the mass profiles, and find that these are on average ~25% smaller than rest-frame g-band half-light radii. This average size difference of 25% is the same at all redshifts, and does not correlate with stellar mass, specific star formation rate, effective surface density, S\'ersic index, or galaxy size. Although on average the difference between half-mass size and half-light size is modest, for approximately 10% of massive galaxies this difference is more than a factor of two. These extreme galaxies are mostly extended, disk-like systems with large central bulges. These results are robust, but could be impacted if the central dust extinction becomes high. ALMA observations can be used to explore this possibility. These results provide added support for galaxy growth scenarios wherein massive galaxies at these epochs grow by accretion onto their outer regions.