- ID:
- ivo://CDS.VizieR/J/A+A/356/529
- Title:
- Catalogue of wide binaries
- Short Name:
- J/A+A/356/529
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The list contains a total of 131 binaries (115 systems) belonging to the halo or high-velocity disk. Of these, 122 correspond to wide binaries, that is, binaries with expected major semiaxes larger than 25 AU. The catalogue was constructed by identifying common proper-motion companions to the high-velocity and metal-poor stars studied by Schuster and collaborators (SN: Schuster and Nissen 1988A&AS...73..225S, SPC: Schuster, Parrao and Contreras, 1993, Cat. <J/A+AS/97/951>). Based on Stromgren photometry, Schuster et al. obtained distances, metallicities and ages for their stars. For each star of the SN and SPC catalogues a machine search for common proper-motion companions was made among the NLTT (Cat. <I/98>) stars within 12 minutes of arc. This initial list was checked to avoid errors due to misidentifications, duplicate entries, etc., and was supplemented with some companions listed in the LDS (Luyten, 1987, Cat. <I/130>) and not present in the NLTT (mostly from the southern hemisphere), as well as with additional common-proper- motion companions found in the CCDM (Dommanget and Nys, 1994, Cat. <I/211>). Additional close companions found in the CCDM were retained only if an orbit was given, or if their separations were of less than 1". Wider companions were usually eliminated, unless convincing evidence of their sharing the proper motion of the primary was found. Distances to the primaries were updated using the Hipparcos (Cat. <I/239>) catalogue. The data in the list are as follows (for details see the main paper): The first column contains the Hipparcos number, when available. Column 2 contains other identifications of the star. In the third column its multiplicity is indicated. Column 4 contains the adopted distance to the star. Columns 5 and 6 contain the absolute visual magnitudes of the primary and secondary, respectively. The angular separation between the components is given in Column 7, and the expected value of the major semiaxes in Column 8. Columns 9 and 10 contain the metallicity of the primary and its age, as determined by Schuster and collaborators. The individual ages listed were kindly provided by W. J. Schuster. The peculiar velocity of the binary is given in Column 11. Columns 12 to 15 contain the main galactic orbital parameters; we list the apocentric distance, Rmax, as well as the maximum distance away from the galactic plane reached by the star |zmax|, and the three-dimensional eccentricity e of its galactic orbit. The last column contains various notes.
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- ID:
- ivo://CDS.VizieR/J/AJ/129/2138
- Title:
- Centers of early-type galaxies with HST
- Short Name:
- J/AJ/129/2138
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present observations of 77 early-type galaxies imaged with the PC1 CCD of the Hubble Space Telescope (HST) WFPC2. "Nuker-law" parametric fits to the surface brightness profiles are used to classify the central structure into "core" or "power-law" forms.
- ID:
- ivo://CDS.VizieR/J/MNRAS/398/1129
- Title:
- Central galaxies in groups and clusters
- Short Name:
- J/MNRAS/398/1129
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.
- ID:
- ivo://CDS.VizieR/II/253A
- Title:
- Chandra Deep Field South: multi-colour data
- Short Name:
- II/253A
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table 3 contains the object catalogue of the COMBO-17 CDFS field. The observations were carried out with the Wide Field Imager (WFI) at the MPG/ESO 2.2-m telescope on La Silla, Chile, between October 1999 and January 2001 in four independent observing runs. The field measures 31.5'x30', is centered on RA=03:32:25, DE=-27:48:50 and contains the Chandra Deep Field South. The table contains 63501 objects found on the deep R-band image cdfs_r.fit by SExtractor with S/N>3. The 5-{sigma} magnitude limit for point sources is Rmag=26.0. Morphological information from the SExtractor measurement is included. Multiple observations in different observing runs of six different filters allow the identification of variable objects. The table contains positions, flags and flux measurements in UBVRI and 12 optical medium-band filters. In addition, we include multi-colour classification, photometric redshifts, luminosity distances and a number of absolute restframe magnitudes in different filters (Johnson, Sloan, Bessell). cdfs_u.fit, cdfs_b.fit, cdfs_v.fit, cdfs_r.fit and cdfs_i.fit are coadded sumframes in UBVRI of the CDFS field. These sumframes are stacked from flat-fielded and cosmic-corrected individual images by applying only full pixel shifts. Therefore, the coordinate frames differ slightly between the images. The coordinates in Table 3 refer to image cdfs_r.fit. The images in BVRI are obtained from observations carried out in observing run D (Oct 1999, see also Note (11) in the byte-by-byte description of table3.dat) while the U-band image is obtained from observing run G (Jan 2001). The exposure times are 14400s (U), 5000s (B), 8400s (V), 15000s (R) and 7550s (I). The intensity levels are given in units of photons hitting the detector (already corrected for the gain of the CCD). The data included here supersede the table2.dat of the COMBO-17 published in 2001 (J/A+A/377/442)
- ID:
- ivo://CDS.VizieR/J/A+A/377/442
- Title:
- Chandra Deep Field South: R-band photometry
- Short Name:
- J/A+A/377/442
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table2 is based on an object list that was created by applying SExtractor software to an R-band image coadded from 36 frames with 15070s total exposure time taken in October 1999 using the Wide Field Imager at the MPG/ESO 2.2-m telescope on La Silla, Chile. The field measures 31.5'x30', is centered on 03:32:25-27:48:50 and contains the Chandra Deep Field South. The average PSF is on the order of 0.75". The catalog contains 63501 objects found by SExtractor with S/N>3. It has not been cleaned for spurious detection of false objects arising from scattered light or diffraction spikes of extremely bright stars. Using this object list aperture magnitudes 'Bmag', 'Vmag' and 'Rmag' were measured on B-, V- and R-band images taken in October 1999. These are listed with its errors. Additionally an aperture magnitude 'R2mag' with its error is included that is taken from R-band imaging from February 2000 with an exposure time of 8440s taken in 21 frames, yielding a total exposure time in the R-band of 23510s=6.5h. The 10-sigma magnitude limits for point sources are Bmag=24.9, Vmag=24.6, Rmag=25.1 and R2mag=24.8. The aperture magnitudes were calculated by counting the flux in an aperture with a Gaussian weighting function of 1.3" width. The flux is scaled to the total flux expected for stars.
- ID:
- ivo://CDS.VizieR/J/ApJ/669/765
- Title:
- Chandra X-ray sources in LALA Cetus field
- Short Name:
- J/ApJ/669/765
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The 174ks Chandra Advanced CCD Imaging Spectrometer exposure of the Large Area Lyman Alpha Survey (LALA) Cetus field is the second of the two deep Chandra images on LALA fields. In this paper we present the Chandra X-ray sources detected in the Cetus field, along with an analysis of X-ray source counts, stacked X-ray spectrum, and optical identifications. A total of 188 X-ray sources were detected: 174 in the 0.5-7.0keV band, 154 in the 0.5-2.0keV band, and 113 in the 2.0-7.0keV band. The X-ray source counts were derived and compared with LALA field (172ks exposure).
- ID:
- ivo://CDS.VizieR/J/A+A/657/A16
- Title:
- Chromatic variations in microlensing events
- Short Name:
- J/A+A/657/A16
- Date:
- 16 Mar 2022 00:52:23
- Publisher:
- CDS
- Description:
- To a first approximation, the microlensing phenomenon is achromatic and great advancements have been achieved with regard to the interpretation of the achromatic signals, leading to the discovery and characterization of well above 100 new exoplanets. At a higher order accuracy in the observations, microlensing has a chromatic component (a color term) that has thus far been explored to a much lesser extent. Here, we analyze the chromatic microlensing effect of four different physical phenomena, which have the potential to contribute key knowledge of the stellar properties that is not easily achievable with other methods of observation. Our simulation is limited to the case of main-sequence source stars. Microlensing is particularly sensitive to giant and sub-giant stars near the Galactic center. While this population can be studied in short snapshots by the largest telescopes in the world, a general monitoring and characterization of the population can be achieved by use of more accessible medium-sized telescopes with specialized equipment via dual-color monitoring from observatories at sites with excellent seeing. We limit the results of this study to what will be achievable from the Danish 1.54m telescope at La Silla observatory based on the use of the existing dual-color lucky imaging camera. Such potential monitoring programs of the bulge population from medium-sized telescopes include the characterization of starspots, limb-darkening, the frequency of close-in giant planet companions, and gravity darkening for blended source stars. We conclude our simulations with quantifying the likelihood of detecting these different phenomena per object where they are present to be ~60 and ~30% for the above-mentioned phenomena when monitored during both high-magnification and caustic crossings, respectively.
- ID:
- ivo://CDS.VizieR/J/AJ/133/2495
- Title:
- Classification of RASS optical counterparts
- Short Name:
- J/AJ/133/2495
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Previous work (Rutledge et al., 2000ApJS..131..335R) statistically identified 5492 optical counterparts, with >~90% confidence, from among the ~18000 X-ray sources appearing in the ROSAT All-Sky Survey Bright Source Catalog (RASS BSC; Voges et al. 1999, Cat. <IX/10>). Using low-resolution spectra in the wavelength range 3700-7900{AA}, we present spectroscopic classifications for 195 of these counterparts which have not previously been classified. Of these 195, we find 168 individual stars of F, G, K, or M type, 6 individual stars of unknown type, 6 double stars, 6 AGNs or galaxies, and 7 unclassifiable objects; the spectra of the 2 remaining objects were saturated.
- ID:
- ivo://CDS.VizieR/J/MNRAS/259/233
- Title:
- Cluster SC2008-57(A3667)
- Short Name:
- J/MNRAS/259/233
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- (Abstract of the paper) We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.
- ID:
- ivo://CDS.VizieR/J/ApJS/243/12
- Title:
- Colors of the Outer Solar System Origins Survey
- Short Name:
- J/ApJS/243/12
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Colours of the Outer Solar System Origins Survey is acquiring near-simultaneous g, r, and J photometry of unprecedented precision with the Gemini North Telescope, targeting nearly 100 trans-Neptunian objects (TNOs) brighter than m_r_=23.6mag discovered in the Outer Solar System Origins Survey. Combining the optical and near-infrared photometry with the well-characterized detection efficiency of the Colours of the Outer Solar System Origins Survey target sample will provide the first flux-limited compositional dynamical map of the outer solar system. In this paper, we describe our observing strategy and detail the data reduction processes we employ, including techniques to mitigate the impact of rotational variability. We present optical and near-infrared colors for 35 TNOs. We find two taxonomic groups for the dynamically excited TNOs, the neutral and red classes, which divide at g-r~0.75. Based on simple albedo and orbital distribution assumptions, we find that the neutral class outnumbers the red class, with a ratio of 4:1 and potentially as high as 11:1. Including in our analysis constraints from the cold classical objects, which are known to exhibit unique albedos and r-z colors, we find that within our measurement uncertainty our observations are consistent with the primordial solar system protoplanetesimal disk being neutral class dominated, with two major compositional divisions in grJ color space.
