- ID:
- ivo://CDS.VizieR/J/A+AS/144/475
- Title:
- Accurate positions for 17124 galaxies
- Short Name:
- J/A+AS/144/475
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper gives accurate coordinates and diameters for 3301 galaxies, companions of UGC galaxies. (about 2764 companions were not yet available in electronic form). In addition previously poor equatorial coordinates are re-measured for 13823 galaxies. These coordinates which have an accuracy of 5'' or better will be used for facilitating the cross-identification with forthcoming catalogues of millions of galaxies.
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Search Results
- ID:
- ivo://CDS.VizieR/J/PASP/110/779
- Title:
- Accurate Positions for MCG Galaxies
- Short Name:
- J/PASP/110/779
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have measured accurate celestial coordinates for over 4000 extragalactic objects primarily drawn from a list of MCG galaxies with no recently published accurate positions. We used IPAC's Skyview program to display FITS images clipped from the Digitized Sky Survey, and to measure the coordinates. The standard deviations in the new positions depend slightly on the measurement command used, but are on the order of 1.0 arcsec to 1.2 arcsec (internal errors). The table of data includes all the duplicate measurements we made, as well as corrections and additions made after the PASP paper was submitted, so has 5120 entries.
- ID:
- ivo://CDS.VizieR/J/A+AS/147/169
- Title:
- Accurate positions of 2978 SBS objects
- Short Name:
- J/A+AS/147/169
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Optical positions of 2978 objects listed in the Second Byurakan Survey (SBS) were obtained using the Digitized Sky Survey (DSS), and are given with an rms un certainty ~1 arcsec in each coordinate.
- ID:
- ivo://CDS.VizieR/J/A+AS/64/247
- Title:
- Accurate positions of Zwicky galaxies
- Short Name:
- J/A+AS/64/247
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Accurate optical positions are given for 1007 galaxies in the Zwicky Catalogue fields 502-505, 519-523, 536-539.
- ID:
- ivo://CDS.VizieR/J/MNRAS/496/1355
- Title:
- Accurate SB2 radial velocities
- Short Name:
- J/MNRAS/496/1355
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Double-lined spectroscopic binaries (SB2s) are one of the main sources of stellar masses, as additional observations are only needed to give the inclinations of the orbital planes in order to obtain the individual masses of the components. For this reason, we are observing a selection of SB2s using the SOPHIE spectrograph at the Haute-Provence observatory in order to precisely determine their orbital elements. Our objective is to finally obtain masses with an accuracy of the order of one percent by combining our radial velocity (RV) measurements and the astrometric measurements that will come from the Gaia satellite. We present here the RVs and the re-determined orbits of 10 SB2s. In order to verify the masses we will derive from Gaia, we obtained interferometric measurements of the ESO VLTI for one of these SB2s. Adding the interferometric or speckle measurements already published by us or by others for 4 other stars, we finally obtain the masses of the components of 5 binary stars, with masses ranging from 0.51 to 2.2 solar masses, including main-sequence dwarfs and some more evolved stars whose location in the HR diagram has been estimated.
- ID:
- ivo://CDS.VizieR/J/MNRAS/474/731
- Title:
- Accurate SB2 radial velocities
- Short Name:
- J/MNRAS/474/731
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The orbital motion of non-contact double-lined spectroscopic binaries (SB2s), with periods of a few tens of days to several years, holds unique, accurate information on individual stellar masses, which only long-term monitoring can unlock. The combination of radial velocity measurements from high-resolution spectrographs and astrometric measurements from high-precision interferometers allows the derivation of SB2 component masses down to the percent precision. Since 2010, we have observed a large sample of SB2s with the SOPHIE spectrograph at the Observatoire de Haute-Provence, aiming at the derivation of orbital elements with sufficient accuracy to obtain masses of components with relative errors as low as 1 per cent when the astrometric measurements of the Gaia satellite are taken into account. In this paper, we present the results from 6 yr of observations of 14 SB2 systems with periods ranging from 33 to 4185 days. Using the TODMOR algorithm, we computed radial velocities from the spectra and then derived the orbital elements of these binary systems. The minimum masses of the 28 stellar components are then obtained with an average sample accuracy of 1.0+/-0.2 per cent. Combining the radial velocities with existing interferometric measurements, we derived the masses of the primary and secondary components of HIP 61100, HIP 95995 and HIP 101382 with relative errors for components (A,B) of, respectively, (2.0, 1.7) per cent, (3.7, 3.7) per cent and (0.2, 0.1) per cent. Using the CESAM2K stellar evolution code, we constrained the initial He abundance, age and metallicity for HIP 61100 and HIP 95995.
- ID:
- ivo://CDS.VizieR/J/MNRAS/458/3272
- Title:
- Accurate SB2 radial velocities
- Short Name:
- J/MNRAS/458/3272
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In anticipation of the Gaia astrometric mission, a large sample of spectroscopic binaries has been observed since 2010 with the Spectrographe pour l'Observation des PHenomenes des Interieurs Stellaires et des Exoplanetes spectrograph at the Haute-Provence Observatory. Our aim is to derive the orbital elements of double-lined spectroscopic binaries (SB2s) with an accuracy sufficient to finally obtain the masses of the components with relative errors as small as 1 per cent when the astrometric measurements of Gaia are taken into account. In this paper, we present the results from five years of observations of 10 SB2 systems with periods ranging from 37 to 881d. Using the todmor algorithm, we computed radial velocities from the spectra, and then derived the orbital elements of these binary systems. The minimum masses of the components are then obtained with an accuracy better than 1.2 per cent for the 10 binaries. Combining the radial velocities with existing interferometric measurements, we derived the masses of the primary and secondary components of HIP 87895 with an accuracy of 0.98 and 1.2 per cent, respectively.
- ID:
- ivo://CDS.VizieR/J/MNRAS/442/2240
- Title:
- Accurate water maser positions from HOPS
- Short Name:
- J/MNRAS/442/2240
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on high spatial resolution water maser observations, using the Australia Telescope Compact Array, towards water maser sites previously identified in the H2O southern Galactic Plane Survey (HOPS) within the area covering Galactic coordinates from l=290 to l=30 and b=-0.5 to b=+0.5. Of the 540 maser sites identified in the single-dish observations of Walsh et al. (2011MNRAS.416.1764W, Cat. J/MNRAS/416/1764), we detect emission in all but 31 fields. These maser sites together comprise 2790 individual spectral features (maser spots), with brightnesses ranging from 0.06Jy to 576Jy and with velocities ranging from -238.5 to +300.5km/s. Based on a definition of maser site size of 4-arcsec (except for G000.667+0.028, also known as Sgr B2, which we treat as a special case), we identify 631 maser sites. We have compared the positions of these sites to the literature to associate the sites with astrophysical objects. We identify 433 (69%) with star formation, 121 (19%) with evolved stars and 77 (12%) as unknown. Comparing the properties of maser sites of different origins, we find that those associated with evolved stars tend to have more maser spots and have smaller angular sizes than those associated with star formation. We present evidence that maser sites associated with evolved stars show an increased likelihood of having a velocity range between 15 and 35 km/s compared to other maser sites. We suggest this is because many of these maser sites are associated with the circumstellar shells of the evolved stars, which are expanding at these velocities. Of the 31 non-detections, we conclude they were not detected due to intrinsic variability and confirm previous results showing that such variable masers tend to be weaker and have simpler spectra with fewer peaks. Of the small number of maser sites showing linear features, we find evidence for lines that are both perpendicular and parallel to known outflows, suggesting that in star formation, H_2_O maser origins may be as varied and as complex as those of class II methanol masers.
- ID:
- ivo://CDS.VizieR/J/A+AS/131/431
- Title:
- Accurate wavelengths in the Sun spectrum
- Short Name:
- J/A+AS/131/431
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Central line wavelengths in the spectrum of the Sun observed at the centre of the disc, and in the flux spectrum, line identification and solar log(gf).
- ID:
- ivo://CDS.VizieR/J/A+A/638/A9
- Title:
- A census of the near-by Psc-Eri stellar stream
- Short Name:
- J/A+A/638/A9
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Within a sphere of 400pc radius around the Sun, we search for members of the Pisces-Eridanus (Psc-Eri) stellar stream in the Gaia Data Release 2 DR2) data set. We compare basic astrophysical characteristics of the stream with those of the Pleiades. We used a modified convergent-point method to identify stars with 2D - velocities consistent with the space velocity of the Psc-Eri stream and the Pleiades, respectively. We found 1387 members of the Psc-Eri stream in a G-magnitude range from 5.1mag to 19.3mag at distances between 80 and 380pc from the Sun. The stream has a nearly cylindrical shape with a length of at least 700pc and a thickness of 100pc. The accumulated stellar mass of the 1387 members amounts to about 770M_{sun}_, and the stream is gravitationally unbound. For the stream we found an age of about 135Myr. In many astrophysical properties Psc-Eri is comparable to the open cluster M45 (the Pleiades): in its age, its luminosity function (LF), its present-day mass function (PDMF) as well as in its total mass. Nonetheless, the two stellar ensembles are completely unlike in their physical appearance. We cautiously give two possible explanations for this disagreement: (i) the star-formation efficiency in their parental molecular clouds was higher for the Pleiades than for Psc-Eri or/and (ii) the Pleiades had a higher primordial mass segregation immediately after the expulsion of the molecular gas of the parental cloud.
