- ID:
- ivo://CDS.VizieR/J/AN/336/70
- Title:
- Velocities and proper motions of Galactic Cepheids
- Short Name:
- J/AN/336/70
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The kinematics and distribution of classical Cepheids within ~3 kpc from the Sun suggest the existence of the outer ring R1R2' in the Galaxy. The optimum value of the solar position angle with respect to the major axis of the bar, theta_b, providing the best agreement between the distribution of Cepheids and model particles is theta_b_=37+/-13{deg}. The kinematical features obtained for Cepheids with negative Galactocentric radial velocity V_R_ are consistent with the solar location near the descending segment of the outer ring R2. The sharp rise of extinction toward of the Galactic center can be explained by the presence of the outer ring R1 near the Sun.
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- ID:
- ivo://CDS.VizieR/J/AJ/159/242
- Title:
- Velocities and transit times in the Kepler-88 system
- Short Name:
- J/AJ/159/242
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the discovery of Kepler-88d (P_d_=1403{+/-}14days, Msin_i_d__=965{+/-}44M_{Earth}_=3.04{+/-}0.13M_J_, e_d_=0.41{+/-}0.03) based on six years of radial velocity (RV) follow-up from the W.M.Keck Observatory High Resolution Echelle Spectrometer spectrograph. Kepler-88 has two previously identified planets. Kepler-88b (KOI-142.01) transits in the NASA Kepler photometry and has very large transit timing variations (TTVs). Nesvorny+, performed a dynamical analysis of the TTVs to uniquely identify the orbital period and mass of the perturbing planet (Kepler-88c), which was later was confirmed with RVs from the Observatoire de Haute-Provence (OHP). To fully explore the architecture of this system, we performed photodynamical modeling on the Kepler photometry combined with the RVs from Keck and OHP and stellar parameters from spectroscopy and Gaia. Planet d is not detectable in the photometry, and long-baseline RVs are needed to ascertain its presence. A photodynamical model simultaneously optimized to fit the RVs and Kepler photometry yields the most precise planet masses and orbital properties yet for b and c: P_b_=10.91647{+/-}0.00014days, M_b_=9.5{+/-}1.2M_{Earth}_, P_c_=22.2649{+/-}0.0007days, and M_c=214.0{+/-}5.3M_{Earth}_. The photodynamical solution also finds that planets b and c have low eccentricites and low mutual inclination, are apsidally anti-aligned, and have conjunctions on the same hemisphere of the star. Continued RV follow-up of systems with small planets will improve our understanding of the link between inner planetary system architectures and giant planets.
- ID:
- ivo://CDS.VizieR/J/ApJ/649/201
- Title:
- Velocities and Washington photometry in Carina dSph
- Short Name:
- J/ApJ/649/201
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A new large-area Washington M, T2+DDO51 filter survey of more than 10deg^2^ around the Carina dSph galaxy reveals a spectroscopically confirmed power-law radial density break population of Carina giant stars extending several degrees beyond the central King profile. Magellan telescope MIKE spectroscopy establishes the existence of Carina stars to at least 4.5 times its central King limiting radius, rlim, and primarily along Carina's major axis. To keep these stars bound to the dSph would require a global Carina mass-to-light ratio of M/L>=6300(M/L)_{sun}}. The MIKE velocities, supplemented with ~950 additional Carina field velocities from archived VLT+GIRAFFE spectra with r<~rlim, demonstrate a nearly constant Carina velocity dispersion (sigma_v_) to just beyond r=rlim and both a rising and a velocity shear at still larger radii. Together, the observational evidence suggests that the discovered extended Carina population represents tidal debris from the dSph.
- ID:
- ivo://CDS.VizieR/J/MNRAS/426/739
- Title:
- Velocities for seven transiting hot Jupiters
- Short Name:
- J/MNRAS/426/739
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present seven new transiting hot Jupiters from the WASP-South survey. The planets are all typical hot Jupiters orbiting stars from F4 to K0 with magnitudes of V=10.3-12.5. The orbital periods are all in the range of 3.9-4.6d, the planetary masses range from 0.4 to 2.3-M_Jup_ and the radii from 1.1 to 1.4R_Jup_. In line with known hot Jupiters, the planetary densities range from Jupiter-like to inflated ({rho}=0.13-1.07{rho}_Jup_). We use the increasing numbers of known hot Jupiters to investigate the distribution of their orbital periods and the 3-4d 'pile-up'.
- ID:
- ivo://CDS.VizieR/J/ApJ/562/254
- Title:
- Velocities in A1750, A3395 and A3528
- Short Name:
- J/ApJ/562/254
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We study three prominent bimodal X-ray clusters: A3528, A1750, and A3395. Using observations taken with ROSAT and ASCA, we analyze the temperature and surface brightness distributions. We also analyze the velocity distributions of the three clusters using new measurements supplemented with previously published data. We examine both the overall cluster properties, as well as the two subcluster elements in each. These results are then applied to the determination of the overall cluster masses; they demonstrate excellent consistency between the various methods used. While the characteristic parameters of the subclusters are typical of isolated objects, our temperature results for the regions between the two subclusters clearly confirm the presence of merger activity. These three clusters represent a progression of equal-sized subcluster mergers, starting from initial contact to immediately before first core passage.
22536. Velocities in Abell 3266
- ID:
- ivo://CDS.VizieR/J/AJ/112/36
- Title:
- Velocities in Abell 3266
- Short Name:
- J/AJ/112/36
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.
- ID:
- ivo://CDS.VizieR/J/ApJ/665/1067
- Title:
- Velocities in Cl 0024+16 and MS 0451-03
- Short Name:
- J/ApJ/665/1067
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We examine resolved spectroscopic data obtained with the Keck II telescope for 44 spheroidal galaxies in the fields of two rich clusters, Cl 0024+16 (z=0.40) and MS 0451-03 (z=0.54) and contrast this with similar data for 23 galaxies within the redshift interval 0.3<z<0.65 in the GOODS northern field. For each galaxy we examine the case for systemic rotation, derive central stellar velocity dispersions sigma and photometric ellipticities epsilon. Using morphological classifications obtained via Hubble Space Telescope imaging as the basis, we explore the utility of our kinematic quantities in distinguishing between pressure-supported ellipticals and rotationally supported lenticulars (S0s).
22538. Velocities in Coma cluster
- ID:
- ivo://CDS.VizieR/J/A+AS/111/265
- Title:
- Velocities in Coma cluster
- Short Name:
- J/A+AS/111/265
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- (no description available)
22539. Velocities in NGC 4449
- ID:
- ivo://CDS.VizieR/J/AJ/124/3157
- Title:
- Velocities in NGC 4449
- Short Name:
- J/AJ/124/3157
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A detailed kinematic analysis of ionized gas in the nearby irregular galaxy NGC 4449 is presented. Observations were conducted in the spectral lines of H{alpha} and [S II]. Our scanning Fabry-Perot interferometric observations are presented from both a global and a local perspective. We have analyzed the global velocity field, the spatially extended diffuse gaseous component, and the H II region populations and, furthermore, have determined the rotation curve based on the heliocentric radial velocities of the global H{alpha} spatial distribution.
- ID:
- ivo://CDS.VizieR/J/AJ/105/1251
- Title:
- Velocities in Pisces-Perseus supercluster.
- Short Name:
- J/AJ/105/1251
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Measurements of 544 radial velocities, 229 optical and 315 in the 21cm HI line, are presented for galaxies, mostly in the declination strip +33.5 deg<Dec<+39.5deg in the region of the Pisces-Perseus supercluster. These are combined with other available data to investigate the linear structure identified as the main supercluster ridge. The main ridge of the supercluster extends at least 50h^-1Mpc before it disappears into the zone of avoidance east of Perseus. Confinement both on the plane of the sky and in the velocity dimension imply an axial ratio of greater than ten to one and an inclination with respect to the plane of the sky of less than about 12 degrees. The smoothed volume density contrast over the whole ridge averages more than a factor of 6 relative to the average density derived for the whole sample. The relative proximity, low inclination to the plane of the sky, and high contrast relative to the foreground and background, help to make the Pisces-Perseus filament one of the most prominent features in the extragalactic sky on large scales.
