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14071. Spectroscopic and photometric properties of Tombaugh 1
ID:
ivo://CDS.VizieR/J/AJ/151/6
Title:
Spectroscopic and photometric properties of Tombaugh 1
Short Name:
J/AJ/151/6
Date:
21 Oct 2021
Publisher:
CDS
Description:
Open clusters can be the key to deepening our knowledge on various issues involving the structure and evolution of the Galactic disk and details of stellar evolution because a cluster's properties are applicable to all its members. However, the number of open clusters with detailed analysis from high-resolution spectroscopy or precision photometry imposes severe limitations on studies of these objects. To expand the number of open clusters with well-defined chemical abundances and fundamental parameters, we investigate the poorly studied, anticenter open cluster Tombaugh 1. Using precision uvbyCaH{beta} photometry and high-resolution spectroscopy, we derive the cluster's reddening, obtain photometric metallicity estimates, and, for the first time, present a detailed abundance analysis of 10 potential cluster stars (nine clump stars and one Cepheid). Using the radial position from the cluster center and multiple color indices, we have isolated a sample of unevolved, probable single-star members of Tombaugh 1. From 51 stars, the cluster reddening is found to be E(b-y)=0.221+/-0.006 or E(B-V)=0.303+/-0.008, where the errors refer to the internal standard errors of the mean. The weighted photometric metallicity from m_1_ and hk is [Fe/H]=-0.10+/-0.02, while a match to the Victoria-Regina Stromgren isochrones leads to an age of 0.95+/-0.10 Gyr and an apparent modulus of (m-M)=13.10+/-0.10. Radial velocities identify six giants as probable cluster members, and the elemental abundances of Fe, Na, Mg, Al, Si, Ca, Ti, Cr, Ni, Y, Ba, Ce, and Nd have been derived for both the cluster and the field stars. Tombaugh 1 appears to be a typical inner thin disk, intermediate-age open cluster of slightly subsolar metallicity, located just beyond the solar circle, with solar elemental abundance ratios except for the heavy s-process elements, which are a factor of two above solar. Its metallicity is consistent with a steep metallicity gradient in the galactocentric region between 9.5 and 12 kpc. Our study also shows that Cepheid XZ CMa is not a member of Tombaugh 1 and reveals that this Cepheid presents signs of barium enrichment, making it a probable binary star.
14072. Spectroscopic and photometric redshifts
ID:
ivo://CDS.VizieR/J/ApJS/135/41
Title:
Spectroscopic and photometric redshifts
Short Name:
J/ApJS/135/41
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a comparison between the catalog of spectroscopic redshifts in the Hubble Deep Field (HDF) recently published by Cohen and collaborators (2000, cat. <J/ApJ/538/29>) and the redshifts that our group (Fernandez-Soto et al., 1999, Cat. <J/ApJ/513/34>) has measured for the same objects using photometric techniques. This comparison is performed in order to fully characterize the errors associated with the photometric redshift technique. The compilation of spectroscopic redshifts incorporates previously published results, corrections to previously published wrong values, and new data, and it includes over 140 objects in the HDF proper. It represents the deepest, cleanest, most complete spectroscopic catalog ever compiled.
14073. Spectroscopic binary orbits in NGC 188
ID:
ivo://CDS.VizieR/J/AJ/137/3743
Title:
Spectroscopic binary orbits in NGC 188
Short Name:
J/AJ/137/3743
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present 98 spectroscopic binary orbits resulting from our ongoing radial velocity survey of the old (7Gyr) open cluster NGC 188.
14074. Spectroscopic Binary Orbits Ninth Catalog (Dynamic Version)
ID:
ivo://nasa.heasarc/sborbitcat
Title:
Spectroscopic Binary Orbits Ninth Catalog (Dynamic Version)
Short Name:
SpecBinOrbits
Date:
09 May 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Ninth Catalog of Spectroscopic Binary Orbits (SB9) continues the series of compilations of spectroscopic orbits carried out over the past 35 years by Batten and collaborators, e.g., the 8th SBO Catalog (SB8, &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/V/64"&gt;CDS Catalog V/64&lt;/a&gt;) of Batten, Fletcher and MacCarthy 1989, Publ. DAO, 17, 1. This catalog is regularly updated. This version of SB9 contains orbits for over three thousand binary systems; notice that the numbers of orbits and binary systems included in this version differ from those in the reference publication, as the latter reflected the 2004 May 1 status of the catalog, when it had 2694 orbits for 2386 binary systems. There is an online version of this catalog, maintained by the authors, which is continuously updated, at &lt;a href="http://sb9.astro.ulb.ac.be/"&gt;http://sb9.astro.ulb.ac.be/&lt;/a&gt;. This table was created by the HEASARC based on the &lt;a href="https://cdsarc.cds.unistra.fr/ftp/cats/B/sb9"&gt;CDS Catalog B/sb9&lt;/a&gt;, using the files main.dat, alias.dat, orbits.dat and notes.txt. The CDS updates it regularly, and this HEASARC version is accordingly updated within a week of such updates. This is a service provided by NASA HEASARC .
14075. Spectroscopic binary population of ONC and NGC2264
ID:
ivo://CDS.VizieR/J/ApJ/821/8
Title:
Spectroscopic binary population of ONC and NGC2264
Short Name:
J/ApJ/821/8
Date:
21 Oct 2021
Publisher:
CDS
Description:
We examine the spectroscopic binary population for two massive nearby regions of clustered star formation, the Orion Nebula Cluster (ONC) and NGC 2264, supplementing the data presented by Tobin et al. (2009, J/ApJ/697/1103) with more recent observations and more extensive analysis. The inferred multiplicity fraction up to 10 au based on these observations is 5.3+/-1.2% for NGC 2264 and 5.8+/-1.1% for the ONC; these values are consistent with the distribution of binaries in the field in the relevant parameter range. Eight of the multiple systems in the sample have enough epochs to perform an initial fit for the orbital parameters. Two of these sources are double-lined spectroscopic binaries; for them, we determine the mass ratio. Our reanalysis of the distribution of stellar radial velocities toward these clusters presents a significantly better agreement between stellar and gas kinematics than was previously thought.
14076. Spectroscopic catalog in 24 clusters
ID:
ivo://CDS.VizieR/J/ApJS/188/280
Title:
Spectroscopic catalog in 24 clusters
Short Name:
J/ApJS/188/280
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a spectroscopic catalog of (mostly) red galaxies in 24 galaxy clusters in the redshift range 0.17<z<0.92 obtained with the LRIS instrument on the Keck I telescope. Here we describe the observations and the galaxy spectra, including the discovery of three cD galaxies with LINER emission spectra, and the spectroscopic discovery of four new galaxy-galaxy lenses in cluster environments. All but two of the galaxy clusters observed as part of this experiment were previously known.
14077. Spectroscopic catalog of 10 rich galaxy clusters
ID:
ivo://CDS.VizieR/J/ApJS/122/51
Title:
Spectroscopic catalog of 10 rich galaxy clusters
Short Name:
J/ApJS/122/51
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).
14078. Spectroscopic distances of 322 NLTT stars
ID:
ivo://CDS.VizieR/J/A+A/442/211
Title:
Spectroscopic distances of 322 NLTT stars
Short Name:
J/A+A/442/211
Date:
21 Oct 2021
Publisher:
CDS
Description:
Distance estimates based on low-resolution spectroscopy and Two Micron All Sky Survey (2MASS, Cat. <II/246>) J magnitudes are presented for 322 nearby candidates from Luyten's NLTT catalogue (<I/98>). Mainly relatively bright (typically 7<Ks<11) and red high proper motion stars have been selected according to their 2MASS magnitudes and optical-to-infrared colours (+1<R-Ks<+7). Some LHS stars previously lacking spectroscopy have also been included. We have classified the majority of the objects as early-M dwarfs (M2-M5). More than 70% of our targets turned out to lie within the 25pc horizon of the catalogue of nearby stars, with 50 objects placed within 15pc and 8 objects being closer than 10pc. Three objects in the 10pc sample have no previously published spectral type: LP 876-10 (M4), LP 870-65 (M4.5), and LP 869-26 (M5). A large fraction of the objects in our sample (57%) ave independent distance estimates, mainly by the recent efforts of Reid and collaborators. Our distance determinations are generally in good agreement with theirs. 11 rather distant (d>100pc) objects have also been identified, including a probable halo, but relatively hot (Teff=13000K) white dwarf (LHS 1200) and 10 red dwarfs with extremely large tangential velocities (250<v_t_<1150km/s). Altogether, there are 11 red dwarfs (including one within 70pc) with tangential velocities larger than about 250km/s. All these objects are suspected to be in fact subdwarfs, if so, their distances would be only about half of our original estimates. The three most extreme objects in that respect are the K and early M dwarfs LP 323-168, LHS 5343 and LP 552-21 with corrected distances between 180pc and 400pc and resulting tangential velocities still larger than about 400km/s.
14079. Spectroscopic [Fe/H] of Kepler stars
ID:
ivo://CDS.VizieR/J/ApJ/770/43
Title:
Spectroscopic [Fe/H] of Kepler stars
Short Name:
J/ApJ/770/43
Date:
21 Oct 2021
Publisher:
CDS
Description:
It has been shown that F, G, and early K dwarf hosts of Neptune-sized planets are not preferentially metal-rich. However, it is less clear whether the same holds for late K and M dwarf planet hosts. We report metallicities of Kepler targets and candidate transiting planet hosts with effective temperatures below 4500K. We use new metallicity calibrations to determine [Fe/H] from visible and near-infrared spectra. We find that the metallicity distribution of late K and M dwarfs monitored by Kepler is consistent with that of the solar neighborhood. Further, we show that hosts of Earth- to Neptune-sized planets have metallicities consistent with those lacking detected planets and rule out a previously claimed 0.2dex offset between the two distributions at 6{sigma} confidence. We also demonstrate that the metallicities of late K and M dwarfs hosting multiple detected planets are consistent with those lacking detected planets. Our results indicate that multiple terrestrial and Neptune-sized planets can form around late K and M dwarfs with metallicities as low as 0.25 solar. The presence of Neptune-sized planets orbiting such low-metallicity M dwarfs suggests that accreting planets collect most or all of the solids from the disk and that the potential cores of giant planets can readily form around M dwarfs. The paucity of giant planets around M dwarfs compared to solar-type stars must be due to relatively rapid disk evaporation or a slower rate of planet accretion, rather than insufficient solids to form a core.
14080. Spectroscopic follow-up of 100pc WDs in SDSS & Gaia
ID:
ivo://CDS.VizieR/J/ApJ/898/84
Title:
Spectroscopic follow-up of 100pc WDs in SDSS & Gaia
Short Name:
J/ApJ/898/84
Date:
25 Oct 2021 07:21:33
Publisher:
CDS
Description:
We present follow-up spectroscopy of 711 white dwarfs within 100pc, and we present a detailed model atmosphere analysis of the 100pc white dwarf sample in the Sloan Digital Sky Survey footprint. Our spectroscopic follow-up is complete for 83% of the white dwarfs hotter than 6000K, where the atmospheric composition can be constrained reliably. We identify 1508 DA white dwarfs with pure hydrogen atmospheres. The DA mass distribution has an extremely narrow peak at 0.59M_{sun}_ and reveals a shoulder from relatively massive white dwarfs with M=0.7-0.9M_{sun}_. Comparing this distribution with binary population synthesis models, we find that the contribution from single stars that form through mergers cannot explain the overabundance of massive white dwarfs. In addition, the mass distribution of cool DAs shows a near absence of M>1M_{sun}_ white dwarfs. The pile-up of 0.7-0.9M_{sun}_ and the disappearance of M>1M_{sun}_ white dwarfs is consistent with the effects of core crystallization. Even though the evolutionary models predict the location of the pile-up correctly, the delay from the latent heat of crystallization by itself is insufficient to create a significant pile-up, and additional cooling delays from related effects like phase separation are necessary. We also discuss the population of infrared-faint (ultracool) white dwarfs and demonstrate for the first time the existence of a well-defined sequence in color and magnitude. Curiously, this sequence is connected to a region in the color-magnitude diagrams where the number of white dwarfs with a helium- dominated atmosphere is low. This suggests that the infrared-faint white dwarfs likely have mixed H/He atmospheres.

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