VO Fresh

Morphological classification of eclipsing binaries from the Gaia

2026-10-25T20:12:12Z

Description

The table contains the results of morphological classification of eclipsing binaries and selected parameters 
from Gaia DR3 (:bibcode: `2023A&A...674A...1G`), including orbital periods, GSP-Phot effective temperatures, and sky coordinates.

Because the morphological classification is based on single-passband Gaia G photometry alone, EW and ellipsoidal 
systems cannot be reliably distinguished. Therefore, systems with orbital periods P > 3 d initially classified as EW 
are explicitly reassigned as "ellipsoidal", since such long-period EW systems are physically unlikely 
for main-sequence stars.

Author(s)

Parimucha, Š., Gabdeev, M., Vaňko, M., Markus, Y., Vozyakova, O.; GAIA Collaboration

IVOA id

ivo://astro.upjs/upjs_gaia_eb/q/classification

Gaia EB classification Cone Search

2026-10-25T20:12:12Z

Description

This resource provides the results of a morphological classification
of 2,184,283 eclipsing binary candidates from the Gaia DR3 catalogue.
The systems are classified into EA/EB and EW types, followed by the
identification of starspot signatures within both morphological
classes.

The classification was performed using a hierarchical computer-vision
pipeline based on a fine-tuned ResNet-18 convolutional neural network
trained on synthetic light curves generated with the ELISa code. The
phase-folded Gaia G-band light curves are represented as 3-channel
128×128 pixel images encoding the flux distribution, its polar
transformation, and the flux gradient.

A tailored augmentation scheme calibrated to the Gaia cadence
distribution was applied to reduce the synthetic-to-real domain gap
(in prep).

Because the morphological classification is based on single-passband
Gaia G photometry alone, EW and ellipsoidal systems cannot be reliably
distinguished. Therefore, systems with orbital periods P > 3 d
initially classified as EW are explicitly reassigned as "ellipsoidal",
since such long-period EW-type systems are physically unlikely for
main-sequence stars.

Author(s)

Parimucha, Š., Gabdeev, M., Vaňko, M., Markus, Y., Vozyakova, O.; GAIA Collaboration

IVOA id

ivo://astro.upjs/upjs_gaia_eb/q/upjs_eb_cone

FAI Assy-Turgen Unmerged Echelle Spectra

2026-10-23T06:41:51Z

Description

Extracted, wavelength-calibrated, unmerged stellar echelle spectra
from the eShel spectrograph on the Zeiss-1000 telescope at Assy-Turgen
Observatory. Each archive record delivers one original IRAF multispec
FITS containing all extracted orders. Wavelength solutions are
recorded separately for each order in the WAT2 header cards, in
Angstroms. Orders are neither flattened nor merged. Downloaded files
retain their original bytes. Wavelength bounds enclose all orders;
they do not imply continuous coverage. Exposure duration is taken from
EXPTIME. Flux calibration and resolving power are not established by
these headers and are not assumed. Generic single-array spectrum
viewers may not support IRAF multispec.

Author(s)

Fesenkov Astrophysical Institute

IVOA id

ivo://fai.kz/fai_echelle_spectra/q/ssa

AMS-02 All Particle Rates Catalog

2026-10-23T00:00:00Z

Description: The AMS02RATES database table records the incident rates for all particle species obtained with the Alpha Magnetic Spectrometer (AMS-02) experiment on the International Space Station (ISS), a cosmic ray particle detector installed in May 2011. The experiment consists of several components, which collectively measure particle species, energy, geomagnetic rigidity, or veto off-axis particles and high-energy photons. The experiment covers the energy range of ~0.1 GeV - ~2 TeV. AMS-02 is the result of a collaboration between MIT, the University of Hawaii, CERN, NASA, the U.S. Department of Energy, and ESA. It was launched on the Space Shuttle Endeavor (STS-134) on May 16, 2011 and was installed three days later at which time science operations commenced. Operations were interrupted by in-flight servicing of the cooling pumps for the silicon tracker: servicing took place between November 2019 and January 2020, after which science operations were restored. It is anticipated to continue operations for as long as the ISS itself remains functional. The rate at which all particle species are observed within a one-second time integration period is recorded for each interval, corrected for the livetime fraction. Each integration period contains the livetime value, observed rate, and the position of the AMS-02 instrument in latitude, longitude, and radius from the Earth's center in the Earth Centered Earth Fixed (ECEF) frame of reference. This database table was first ingested by the HEASARC in July 2026. The AMS-02 team in collaboration with the HEASARC developed the FITS file structure for these data which were created by the HEASARC from daily particle rate data provided by the AMS collaboration. The data and the database table are updated periodically to reflect additional data as they become available. This is a service provided by NASA HEASARC .
Author(s): HEASARC
IVOA id: ivo://nasa.heasarc/ams02rates

AMS-02 Spectral Results Catalog

2026-10-23T00:00:00Z

Description: The AMS02SPEC database table records the spectral results obtained with the Alpha Magnetic Spectrometer (AMS-02) experiment on the International Space Station (ISS), a cosmic ray particle detector installed in May 2011. The experiment consists of several components, which collectively measure particle species, energy, geomagnetic rigidity, or veto off-axis particles and high-energy photons. The experiment covers the energy range of ~0.1 GeV - ~2 TeV. AMS-02 is the result of a collaboration between MIT, the University of Hawaii, CERN, NASA, the U.S. Department of Energy, and ESA. It was launched on the Space Shuttle Endeavor (STS-134) on May 16, 2011 and was installed three days later at which time science operations commenced. Operations were interrupted by in-flight servicing of the cooling pumps for the silicon tracker: servicing took place between November 2019 and January 2020, after which science operations were restored. It is anticipated to continue operations for as long as the ISS itself remains functional. This database table was first ingested by the HEASARC in June 2026. The AMS-02 team in collaboration with the HEASARC developed the FITS file structure for these data. The data have been published in a series of papers (see bibliographic references) and archived in FITS format at the HEASARC. The data and the database table are updated periodically to reflect additional data as they becomes available. This is a service provided by NASA HEASARC .
Author(s): HEASARC
IVOA id: ivo://nasa.heasarc/ams02spec

Chandra Source Catalog Stacked Observation Detections, v2.1.1

2026-10-23T00:00:00Z

Description: The Chandra Source Catalog's Stacked Observation Detections Table (CSCSTACK) includes 493,236 detections (855,402 total entries consisting of detections plus photometric upper limits) based on 10,034 stacks of X-ray observations. Exploiting the unique resolution and very low background of Chandra data, the limiting sensitivity of the catalog is enhanced significantly by stacking (co-adding) multiple observations of the same field prior to source detection. To minimize the impact of the variation in the Chandra point spread function (PSF) with off-axis angles, source detection is constrained to run on stacks of observations that have telescope pointings that are co-located within 60 arcseconds and that were obtained using the same instrument (ACIS or HRC-I). Formally, the observations are matched using a tree clustering algorithm with complete linkage. This means that the pointing direction of every observation in the stack is co-aligned with the pointing direction of every other observation in the stack within 60 arcseconds. The stacked-observation level allows composite properties to be reported from the co-added observations for detections that would otherwise not be visible or have poor S/N in individual observations, while for higher S/N detections the per-observation properties facilitate analysis of variable sources. CSCSTACK is related to the <a href="/W3Browse/chandra/csc.html">Chandra Source Catalog (CSC)</a> catalog, which is the definitive catalog of X-ray sources detected by the Chandra X-ray Observatory. The CSC contains 407,806 unique compact and extended X-ray sources. By combining Chandra's sub-arcsecond on-axis spatial resolution and low instrumental background with consistent data processing, the CSC delivers a wide variety of uniformly calibrated properties and science ready data products for detected sources over four decades of flux. Each identified distinct X-ray source on the sky is represented in the catalog by one or more "stack detection" entries -- one for each stack in which the source has been detected -- and a single "master source" entry. The individual stack entries record all of the properties about a detection extracted from a single stack, as well as associated file-based data products, which are stack-specific. If a source is detected in one or more stacked-observations, photometric upper limits that are useful for temporal variability analyses are calculated for any overlapping stacked- and individual-observations in which the source is not detected. This database table was ingested by the HEASARC in October 2026 and is based on a download of the online version of the "Stacked Observation Detections" table, version 2.2, at the CXC using the CLI. Refer to <a href="https://cxc.harvard.edu/csc/cli/">https://cxc.harvard.edu/csc/cli/</a> for details. This is a service provided by NASA HEASARC .
Author(s): Evans, Civano
IVOA id: ivo://nasa.heasarc/cscstack

Swift-XRT Living Point Source Catalog (LSXPS)

2026-10-23T00:00:00Z

Description: This is the Live Swift X-ray Point Source (LSXPS) catalog of detections by the Swift X-ray Telescope (XRT) used in Photon Counting (PC) mode in the 0.3-10 keV energy range. Swift is a NASA mission with international participation dedicated to studying gamma-ray bursts. It carries three instruments. The BAT is the large field-of-view instrument and operates in the 10-300 keV energy band; and two narrow field instruments, XRT and UVOT, that operate in the X-ray and UV/optical regime, respectively. This catalog is similar to the <a href="swift2sxps.html">2SXPS</a> catalog (Evans, P. A., et al. 2020, ApJS, 247, 54) and uses an almost identical source detection process. The primary change is that this is a living catalog: it is updated in near-real time and transient searches are carried out on each dataset as it is received. The improved statistics (below) compared to 2SXPS for source detections, unique and variables sources, uncatalogued sources, and temporal and total sky area coverage are a function of its ongoing live nature, compared to the static 2SXPS which was current up to 2018-08-01. On average, LSXPS grows by 49 new sources and the unique sky coverage increases 0.94 square degrees per day. This table was added to the HEASARC database in June 2026 and is based on the contents of its dedicated website at <a href="https://www.swift.ac.uk/LSXPS">https://www.swift.ac.uk/LSXPS</a>. The version available from the HEASARC corresponds to the catalog designated as "Sources" on the Leicester website and will typically be updated at the HEASARC within a day or so of a new version appearing on the Leicester website. This is a service provided by NASA HEASARC .
Author(s): Evans et al.
IVOA id: ivo://nasa.heasarc/swiftlsxps

TCO Optical Echelle Spectral Archive

2026-10-22T13:44:51Z

Description

One-dimensional reduced optical stellar spectra obtained at the Three College
Observatory (TCO) with the eShel spectrograph on the 0.81-m telescope.
This collection includes the full supplied archive, including the stars in the
separately published hot-supergiant subset and additional stellar targets.

Wavelengths are computed from the original linear IRAF WCS in Angstroms and
served in meters. Fluxes are relative; continuum normalization is recorded only
where supplied in the metadata. Resolving power R=12000 is adopted from the
existing collection documentation, not measured separately for each spectrum.

Author(s)

Danford, S.; Miroshnichenko, A.

IVOA id

ivo://fai.kz/tco_echelle_spectra/q/ssa

Bolometric magnitudes & corrections for 128 stars

2026-10-21T13:17:06Z

Description: A method of obtaining bolometric corrections (BC_V_) from observed high- resolution, high signal-to-noise spectra is described. The method is applied to the spectra of 128 stars collected from the literature with well-determined effective temperatures (Teff) with the S_{lambda}_(V) transparency profiles of Bessell and Landolt. The computed BC_V_ values are found to be accurate within several millimagnitudes, and the effect of different S_{lambda}_(V) values is found to be no more than 0.015mag. The measured visual-to-bolometric ratio (L_V_/L) from the sample spectra and classically determined BC_V_ from bolometric (M_Bol_) and visual (M_V_) absolute magnitudes helped us to determine the zero-point constant (C_2_) of the BC_V_ scale. The determined C_2_ for each star for each S_{lambda}_(V) profile revealed C_2_=2.3653+/-0.0067mag if the S_{lambda}_(V) profile of Bessell is used and C_2_=2.3826+/-0.0076mag if the S_{lambda}_(V) profile of Landolt is used. Expanding C_Bol_=71.197425...mag and c_Bol_=-18.997351...mag announced by IAU2015GARB2, and using the definition of C_2_=C_Bol_-C_V_=c_Bol_-c_V_, where capital C is the absolute magnitude and lowercase c is the apparent magnitude and subscripts indicate bolometric and visual, the zero-point constants-C_V_=68.8321+/-0.0067mag and c_V_=-21.3627+/-0.0067mag, if L_V_ and are in SI units-were determined corresponding to S_{lambda}_(V) of Bessell. The zero-point constants corresponding to S_{lambda}_(V) of Landolt are smaller, but the difference is not more than 0.02mag. Typical and limiting accuracies for predicting a stellar luminosity from an apparent magnitude and a distance are analyzed.
Author(s): Yucel G.; Bilir S.; Bakis V.; Eker Z.
IVOA id: ivo://cds.vizier/j/aj/171/49

IAC80 telescope images

2026-10-21T11:40:31.568000Z

Description: General optical CCD observations of the north sky with the IAC80 telescope at the Teide Observatory (Tenerife)
IVOA id: ivo://iacvo/iac80images

The IAC Morphological Catalog of Northern Galactic Planetary Nebulae

2026-10-21T11:19:39.072000Z

Description: The IAC Morphological Catalog of Northern Galactic Planetary Nebulae (PNs)
IVOA id: ivo://iacvo/planetarynebula

Warm Jupiter migration pathways. I. Radial veloc.

2026-10-21T08:51:41Z

Description: Giant planets are expected to predominantly form beyond the water-ice line and occasionally undergo inward migration. Unlike hot Jupiters, which can result from high-eccentricity tidal migration, warm Jupiters between 0.1 and 1au (~10-365days) are in many ways more challenging to explain because they reside outside the tidal influence of their host stars. Warm Jupiters should therefore preserve traces of their origins as their eccentricities are directly related to their past interactions. We analyze the eccentricities of 200 warm Jupiters orbiting 194 Sunlike host stars (with FGKM spectral types) using 18,587 radial velocity (RV) measurements across 40 high-resolution spectrographs. RVs are compiled from the literature and are supplemented with 540 new observations from MINERVA-Australis at Mount Kent Observatory and the Habitable-zone Planet Finder spectrograph at McDonald Observatory's Hobby-Eberly Telescope, which are timed to improve eccentricity constraints by sampling orbits near periastron passage. The overarching goal of this program is to establish the relative importance of giant planet migration channels through the largest homogeneous analysis of warm Jupiter orbital properties to date. In particular, we evaluate and compare the impact of different system architectures and host star characteristics on the population-level eccentricity distributions of warm Jupiters. Here, we present the target sample, observations, orbit-fitting procedure, and parameter summary statistics of our survey. All orbit fit solutions, parameter posterior chains, and merged RV tables for each system are made publicly available.
Author(s): Morgan M.; Bowler B.P.; Tran Q.H.; Wittenmyer R.A.; Wright D.J.; Zhou G.,Fairnington T.R.
IVOA id: ivo://cds.vizier/j/apjs/280/76

TAP interface of the 5XMM XMM-Newton Catalogue

2026-10-20T13:08:37.560000Z

Description

The 5XMM-DR15 catalogue is significantly different from previous versions of the XMM-Newton
                    serendipitous source catalogue. This version has been produced following a rereduction of 
                    all of the data that was publicly available as of 1st November 2024. Contrary to previous releases,
                    there is only a single version of the 5XMM-DR15 catalogue, which is a stacked catalogue of all 
                    of the XMM-Newton data, containing one line of information corresponding to the stacked source
                    and then subsequent lines with information per observation, providing either a detection
                    or an upper limit. The stacking procedure has been significantly improved with regards to
                    previous versions and many new added-value products are also provided,
                    including for the first time the Optical Monitor (OM) detections when a counterpart to
                    the X-ray source is identified, a measure of the OM long-term variability for each filter
                    and source classification, along with further multi-wavelength information, notably WISE
                    and Gaia counterparts where they exist, and a link to further tables with other multi-wavelength data.
                    Also new in 5XMM-DR15 are X-ray source classification, simple spectral fitting, long-term variability
                    of the X-ray source, and the photometric redshifts for extragalactic sources, along with the spectral
                    redshift, when it is available. 5XMM-DR15 contains source detections drawn from 14616 XMM-Newton
                    EPIC observations, covering an energy interval from 0.2 keV to 12 keV. These observations were made
                    between 2000 January 19 and 2024 October 14 and all datasets were publicly available by 2024 November 1,
                    but not all public observations are included in this catalogue

Author(s)

SSC XMM-Newton

IVOA id

ivo://xcatdb/tap

Eclipse minimum epochs of TIC 322208686 from TESS

2026-10-20T12:46:37Z

Description: TIC 322208686 is known to be a detached binary that exhibits two types of variability: pulsation and eclipse. We present the physical properties of the target star using the short-cadence TESS data from sectors 24, 57, and 58, and our echelle spectra that show the presence of a tertiary companion. The spectral analysis led to the triple-lined radial velocities and the atmospheric parameters of the eclipsing components. Joint modeling of these observations reveals that the eclipsing pair contains two F-type stars with masses 1.564+/-0.012M_{sun}_ and 1.483+/-0.012M_{sun}_, radii 1.588+/-0.011R_{sun}_ and 1.500+/-0.012R_{sun}_, effective temperatures 7028+/-100K and 7020+/-110K, and luminosities 5.51+/-0.32L_{sun}_and 4.90+/-0.32L_{sun}_. The light contributions of the three stars obtained from this modeling match well with those calculated from the observed spectra. The binary star parameters are in satisfactory agreement with evolutionary model predictions for age t=0.4Gyr and metallicity Z=0.03. We extracted 11 significant frequencies from the TESS light residuals with the binary effects removed. Of these, five signals between 0.65day-1 and 1.89day-1 can be considered as {gamma} Dor pulsations originating mainly from the primary component, while the other frequencies are likely instrumental artifacts or combination terms. These results suggest that TIC 322208686 is a hierarchical triple, containing a pulsating eclipsing pair and a tertiary companion.
Author(s): Lee J.W.; Hong K.; Jeong M.-J.; Park J.-H.; Rittipruk P.; Kim H.-Y.
IVOA id: ivo://cds.vizier/j/aj/171/47

K2-19 transit time measurements & predictions

2026-10-20T11:37:16Z

Description: K2-19 is a star, slightly smaller than the Sun, that hosts three transiting planets. Two of these, K2-19 b and c, are between the size of Neptune and Saturn and have orbital periods near a 3:2 commensurability, and exhibit strong transit-timing variations (TTVs). A previous TTV analysis reported moderate eccentricities of ~0.20+/-0.03 for the two planets, but such high values would imply rapid orbital decay for the innermost planet d. Here, we present an updated analysis that includes eight new transit times from TESS, which extends the time baseline from three years to a decade, and employ a gradient-aware TTV modeling code. We confirm that the system resides in resonance with a small libration amplitude, but find a broader constraints on eccentricity that range from a few percent up to 0.2. These revised eccentricities alleviate previous concerns regarding rapid tidal circularization and support the long-term dynamical stability of the system.
Author(s): Entrican P.M.; Petigura E.A.; Petit A.C.; Gilbert G.J.; Masuda K.
IVOA id: ivo://cds.vizier/j/aj/171/46

XMM-Newton EPIC Source Catalogue at ESA

2026-10-20T10:52:06.758000Z

Description: Latest version of the XMM-Newton Serendipitous Source Catalogue at ESAC
IVOA id: ivo://esavo/xsa/cs/5xmm

Gaia-Kepler-TESS host stellar properties catalog

2026-10-20T08:43:50Z

Description: We present the first homogeneous catalog of Kepler, K2, and TESS host stars and the corresponding catalog of exoplanet properties, which contain 10022 stars and 10189 planets, respectively. We used isochrone fitting and Gaia DR3 photometry, parallaxes, and spectroscopic metallicities to compute precise, homogeneous Teff, log(g), masses, radii, mean stellar densities, luminosities, ages, distances, and V-band extinctions for 3387, 618, 6017 Kepler, K2, and TESS host stars, respectively. We compared our stellar properties to studies using fundamental and precise constraints, such as interferometry and asteroseismology, and find residual scatters of 2.8%, 5.6%, 5.0%, and 31%, with offsets of 0.2%, 1.0%, 1.2%, and 0.7% between our Teff, radii, masses, and ages and those in the literature, respectively. In addition, we compute planet radii, semimajor axes, and incident fluxes for as many as 4285, 678, and 5226 Kepler, K2, and TESS planets, respectively, and find that the exoplanet radius gap is less prominent in the K2, TESS, and combined samples than in the Kepler sample alone. We suspect this difference is due to heterogeneous planet-to-star radius ratios, shorter time baselines of K2 and TESS, smaller sample sizes, and the different gap locations hinted at by the K2 (~1.5R_{Earth}_) and TESS (~1.8R_{Earth}_) planet radius distributions. Finally, we identify a clear radius inflation trend in thousands of hot Jupiters and find 151 hot sub-Neptunian desert planets, in addition to a population of 233 young (<=1Gyr) host stars as potential opportunities for testing theories of planet formation and evolution.
Author(s): Berger T.A.; Schlieder J.E.; Huber D.
IVOA id: ivo://cds.vizier/j/aj/171/23

Light curves of KMT-2022-BLG-1818Lb,c

2026-10-19T15:19:42Z

Description: We present the discovery and analysis of the sixth microlensing two-planet system, KMT-2022-BLG-1818Lb,c, detected by a follow-up program targeting high-magnification events. The second planet was identified from implausible physical parameters for the models with a single planet. Both planets are subject to the well-known "close/wide" degeneracy, although for the first planet, which has a super-Jovian mass ratio of q_2_~5x10^-3^ in both solutions, the close topology, with a normalized separation of s~0.70, is clearly preferred by {Delta}{chi}^2^=26. However, contrary to all previous two-planet microlensing systems, the mass ratio for the second planet, q_3_, is substantially (factor of ~10) different for the Close and Wide topologies of the first planet. While this degeneracy is resolved in the present case due to high-cadence follow-up observations, the appearance of this new degeneracy indicates the need for caution in the analysis of future two-planet systems. A Bayesian analysis suggests that the host is likely a K dwarf star in the Galactic disk. The first planet is probably a super-Jupiter on a Jupiter-like orbit, while the second planet is a Saturn-class planet on either a Mercury-like or Saturn-like orbit.
Author(s): Li H.; Zhang J.; Han C.; Zang W.; Jung Y.K.; Udalski A.; Sumi T.; Yang H.,Kuang R.; Mao S.; (the Leading Authors); Albrow M.D.; Chung S.-J.,Gould A.; Hwang K.-H.; Ryu Y.-H.; Shin I.-G.; Shvartzvald Y.; Yee J.C.,Cha S.-M.; Kim D.-J.; Kim S.-L.; Lee C.-U.; Lee D.-J.; Lee Y.; Park B.-G.,Pogge R.W.; (the Kmtnet Collaboration); Monard B.; Tang Y.; Dong S.,Liu Z.; Christie G.; Mccormick J.; Natusch T.; Qian Q.; Maoz D.; Zhu W.,(the Map and ufun Follow-up Team); Mroz P.; Szymanski M.K.; Skowron J.,Poleski R.; Soszynski I.; Pietrukowicz P.; Kozlowski S.; Rybicki K.A.,Iwanek P.; Ulaczyk K.; Wrona M.; Gromadzki M.; Mroz M.J.,(the Ogle Collaboration); Abe F.; Bando K.; Bennett D.P.; Bhattacharya A.,Bond I.A.; Fukui A.; Hamada R.; Hamada S.; Hamasak N.; Hirao Y.,Ishitani Silva S.; Koshimoto N.; Matsubara Y.; Miyazaki S.; Muraki Y.,Nagai T.; Nunota K.; Olmschenk G.; Ranc C.; Rattenbury N.J.; Satoh Y.,Suzuki D.; Terry S.; Tristram P.J.; Vandorou A.; Yama H.,(the Moa Collaboration)
IVOA id: ivo://cds.vizier/j/aj/171/41

WOCS. XCVII. RVs & orbit param. in NGC 188

2026-10-19T12:04:03Z

Description: We present 35 new spectroscopic-binary orbits from our extended radial-velocity (RV) survey of the old (6.4+/-0.2Gyr) open cluster NGC 188. Using data from the WIYN Open Cluster Study (WOCS) and APOGEE-2, this work nearly doubles the temporal baseline of the previous RV study of NGC 188. We obtain orbital solutions within a stellar sample that spans a magnitude range of 10.8<=G<=16.5 (0.9-1.2M_{sun}_). With revised membership determinations using Gaia DR3 proper motions and parallaxes, we reassess the cluster binary frequency and period-eccentricity distribution. The incompleteness-corrected binary frequency is 33.1%+/-3.8% for periods less than 104days, and the tidal-circularization period is 14.4_-0.11_^+0.14^days. We find evidence that giants are deficient in short-period orbits and suggest that the missing giants may have undergone mass transfer and in part formed the population of blue straggler stars (BSSs) and blue lurkers. Among the binaries of note, we highlight WOCS 3953 as a blue lurker candidate, WOCS 5020 and WOCS 4945 as very long-period eccentric BSSs, and WOCS 4230 as a BSS with a very close WD companion.
Author(s): Narayan R.S.; Linck E.; Mathieu R.D.; Geller A.M.
IVOA id: ivo://cds.vizier/j/aj/171/102

WOCS XCV. NGC 7789 phot., Li, & rotation

2026-10-19T08:04:55Z

Description: Precision UBVRI photometry of NGC 7789 is combined with Gaia data to map reddening variations across the cluster face. Hydra spectra, Gaia astrometry, and isochrone fitting constrain the absolute reddening, apparent modulus, and age, respectively, to E(B-V)=0.30+/-0.02, (m-M)=12.51+/-0.06, and 1.46+/-0.02Gyr for [Fe/H] between -0.2 and solar; the spectroscopic [Fe/H]=-0.13+/-0.068 (median absolute deviation) from 156 single-star members. Corrections for variable reddening reduce the scatter in the unevolved main sequence below the turnoff. A(Li) is derived for only single-star members from the G dwarf Li plateau to the tip of the red giant branch. Giants separate into two distinct groups: probable first-ascent giants with detectable Li that decline with evolution toward the red giant tip, and stars within the clump and the asymptotic giant branch, which only exhibit upper limits. The A(Li) structure from the turnoff to the unevolved main sequence, including the Li dip, and the presence of an extended color spread among the upper main-sequence stars, are attributed to the vsini distribution, indicating the wall of the Li dip as the true hot boundary of the Kraft break. Differences in the color-magnitude diagram topology of NGC 7789 and NGC 752 are explored and attributed to differences in the individual cluster vsini distributions. Prior indications that main-sequence stars more massive than the Li dip evolve redward across the Li wall, undergoing rotational spin-down and Li depletion like stars within the Li dip, are confirmed.
Author(s): Anthony-Twarog B.J.; Brunker S.W.; Deliyannis C.P.; Rich E.,Steinhauer A.; Sun Q.; Twarog B.A.
IVOA id: ivo://cds.vizier/j/aj/171/40