VO Fresh

Euclid Q1 MER Catalog

2026-05-30T00:00:00Z

Description: Euclid Quick Release 1 (Q1) consists of approximately 30 TB of imaging, spectroscopy, and catalogs covering four non-contiguous fields: Euclid Deep Field North (22.9 sq deg), Euclid Deep Field Fornax (12.1 sq deg), Euclid Deep Field South (28.1 sq deg), and LDN1641. Q1 data products include Level 1 raw VIS and NISP frames; Level 2 Calibrated VIS and NISP imaging data; Level 2 calibrated 2-D and 1-D spectra; Level 2 multiwavelength space- and ground-based mosaics; Level 2 catalogs of photometry, photometric redshifts, and spectroscopic measurements; and Level 3 visibility masks.
Author(s): Euclid Consortium
IVOA id: ivo://irsa.ipac/euclid/catalogs/mercat

OpenUniverse 2024 Simulated Rubin Images

2026-05-30T00:00:00Z

Description: OpenUniverse2024 is a project to simulate spatially overlapping imaging surveys to be carried out by the Nancy Grace Roman Telescope and the Vera C. Rubin Observatory. The simulations were carried out on Argonne's Theta cluster and consist of: The LSST ELAIS-S1 Deep Drilling Field (DDF); The Roman Time-Domain Survey (TDS) shifted to overlap the ELAIS region and LSST DDF; Overlapping LSST Wide-Fast-Deep (WFD) survey (with rolling cadence); Overlapping Roman Wide-Area Survey (WAS) in the same region; A deep-field calibration region of the Roman WAS in the same region.
Author(s): OpenUniverse
IVOA id: ivo://irsa.ipac/simulated/images/rubin_openuniverse2024

Roman DC2 Simulated Images

2026-05-30T00:00:00Z

Description: Troxel et al. (2023) simulated 20 square degrees of overlapping synthetic imaging surveys representing the full depth of the Nancy Grace Roman Space Telescope High-Latitude Imaging Survey (HLIS) observing the Dark Energy Science Collaboration (DESC) Data Challenge 2 (DC2) universe. They simulate for the first time fully chromatic images along with the detailed physics of the Sensor Chip Assemblies derived from lab measurements using the flight detectors. The simulated imaging and resulting pixel-level measurements of photometric properties of objects span a wavelength range of ~0.3 to 2.0 microns.
Author(s): M. Troxel
IVOA id: ivo://irsa.ipac/simulated/images/romandc2

OpenUniverse 2024 Simulated Roman Images

2026-05-30T00:00:00Z

Description: OpenUniverse2024 is a project to simulate spatially overlapping imaging surveys to be carried out by the Nancy Grace Roman Telescope and the Vera C. Rubin Observatory. The simulations were carried out on Argonne's Theta cluster and consist of: The LSST ELAIS-S1 Deep Drilling Field (DDF); The Roman Time-Domain Survey (TDS) shifted to overlap the ELAIS region and LSST DDF; Overlapping LSST Wide-Fast-Deep (WFD) survey (with rolling cadence); Overlapping Roman Wide-Area Survey (WAS) in the same region; A deep-field calibration region of the Roman WAS in the same region.
Author(s): OpenUniverse
IVOA id: ivo://irsa.ipac/simulated/images/roman_openuniverse2024

LSST Dark Energy Science Collaboration DC2 Simulated Sky Survey

2026-05-30T00:00:00Z

Description: In preparation for cosmological analyses of the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST), the LSST Dark Energy Science Collaboration (LSST DESC) has created a 300 square degree simulated survey as part of an effort called Data Challenge 2 (DC2). The DC2 simulated sky survey, in six optical bands with observations following a reference LSST observing cadence, was processed with the LSST Science Pipelines (19.0.0).
Author(s): LSST DESC
IVOA id: ivo://irsa.ipac/simulated/images/lsstdesc2021

Cone Search on Observations from Personal Collections

2026-05-29T14:20:38Z

Description: The table with basic parameters of the observed objects
Author(s): Shugarov, S.,Yu.; Vozyakova O.
IVOA id: ivo://astro.upjs/personal/t/personal-objects

Morphological classification of eclipsing binaries from the Gaia

2026-05-29T11:27:04Z

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, overcontact and ellipsoidal 
systems cannot be reliably distinguished. Therefore, systems with orbital periods P > 3 d initially classified as overcontact 
are explicitly reassigned as "ellipsoidal", since such long-period overcontact configurations 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

2026-05-29T11:27:04Z

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 detached and overcontact
configurations, 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, overcontact and ellipsoidal systems cannot be
reliably distinguished. Therefore, systems with orbital periods P > 3
d initially classified as overcontact are explicitly reassigned as
"ellipsoidal", since such long-period overcontact configurations 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

ZTF DR23 Light Curves HATS Catalog

2026-05-29T00:00:00Z

Description

The IRSA HATS Catalog contains multiple collections in the Hierarchical Adaptive Tiling Scheme.
            This includes: ZTF DR23 Light Curves - HATS Collection

            # ZTF DR23 Light Curves - HATS Collection
            creator_did            = ivo://irsa.ipac/ZTF/lc/HATS/ZTF_DR23_Lightcurves
            hats_status            = public main cloneable
            obs_collection         = ZTF_DR23_Lightcurves
            hats_primary_table_url = ztf_dr23_lc-hats
            all_margins            = ztf_dr23_lc-hats_margin_10arcsec
            default_margin         = ztf_dr23_lc-hats_margin_10arcsec
            all_indexes            = objectid ztf_dr23_lc-hats_index_objectid
            default_index          = objectid
            hats_uri               = s3://ipac-irsa-ztf/contributed/dr23/lc/hats
            hats_url               = https://ipac-irsa-ztf.s3.us-east-1.amazonaws.com/contributed/dr23/lc/hats
            obs_regime             = Optical

Author(s)

IRSA

IVOA id

ivo://irsa.ipac/ztf/lc/hats/ztf_dr23_lightcurves

ZTF DR23 Objects Table HATS Catalog

2026-05-29T00:00:00Z

Description

The IRSA HATS Catalog contains multiple collections in the Hierarchical Adaptive Tiling Scheme.
            This includes: ZTF DR23 Objects Table - HATS Collection

            # ZTF DR23 Objects Table - HATS Collection
            creator_did            = ivo://irsa.ipac/ZTF/objects/HATS/ZTF_DR23_Objects
            hats_status            = public main cloneable
            obs_collection         = ZTF_DR23_Objects
            hats_primary_table_url = ztf_dr23_objects-hats
            all_margins            = ztf_dr23_objects-hats_margin_10arcsec
            default_margin         = ztf_dr23_objects-hats_margin_10arcsec
            all_indexes            = oid ztf_dr23_objects-hats_index_oid
            default_index          = oid
            hats_uri               = s3://ipac-irsa-ztf/contributed/dr23/objects/hats
            hats_url               = https://ipac-irsa-ztf.s3.us-east-1.amazonaws.com/contributed/dr23/objects/hats
            obs_regime             = Optical

Author(s)

IRSA

IVOA id

ivo://irsa.ipac/ztf/lc/hats/ztf_dr23_objects

The Infrared Telescope in Space Data Atlas

2026-05-28T01:00:00Z

Description

The Infrared Telescope in Space (IRTS) is a cryogenically cooled, small infrared telescope that flew from March - April in 1995. It surveyed approximately 10% of the sky with a relatively wide beam during its 20 day mission.

Four focal-plane instruments , the Near-Infrared Spectrometer (NIRS), the Mid-Infrared Spectrometer (MIRS), the Far-Infrared Line Mapper (FILM), and the Far-Infrared Photometer (FIRP) made simultaneous observations of the sky at wavelengths ranging from 1 to 1000 um.

Author(s)

Hiroshi Murakami, Masahiro Tanaka, Issei Yamamura

IVOA id

ivo://irsa.ipac/irts/spectra

PTF Objects List

2026-05-28T01:00:00Z

Description: Palomar Transient Factory (PTF) is a fully-automated, wide-field survey aimed at a systematic exploration of the optical transient sky. The PTF Objects catalog is a list of the targets that label each individual lightcurve with "collapsed-lightcurve" metrics. For objects with transient_flag = 0, the object is tied to a reference-image (coadd) detection. If so, metadata characterizing the extracted reference-image source is also given. Such objects may be associated with time-variable sources that "survived" the co-addition process. For objects with transient_flag = 1, the object is transient at one or more epochs and would have been flagged as an outlier (hence omitted) during co-addition. If so, no associated reference-image metadata exists, although collapsed-lightcurve metrics are still given.
Author(s): PTF Team
IVOA id: ivo://irsa.ipac/ptf/catalog/ptf_objects

Near-infrared spectra of nearby M dwarfs

2026-05-28T01:00:00Z

Description: The MEarth Survey is a transiting planet survey searching for super Earths around mid-to-late M dwarfs within 33 pc. IRTF SpeX spectra for 498 stars are presented here.
Author(s): Newton et al. (2014)
IVOA id: ivo://irsa.ipac/irtf/mearth

PTF Lightcurve Table

2026-05-28T01:00:00Z

Description: Palomar Transient Factory (PTF) is a fully-automated, wide-field survey aimed at a systematic exploration of the optical transient sky. The PTF Lightcurve table contains the individual lightcurves, i.e., that associates each object (target) in the Objects Table to all epochal apparitions (detections) of that object in the Sources Catalog. It combines all columns and metadata from both the Objects and Sources Catalog tables.
Author(s): PTF Team
IVOA id: ivo://irsa.ipac/ptf/catalog/ptf_lightcurves

PTF Photometric Calibrator Catalog

2026-05-28T01:00:00Z

Description: The Palomar Transient Factory Photometric Calibrator Catalog v1.0 is a photometrically calibrated catalog of non-variable sources from the Palomar Transient Factory (PTF) observations. The catalog contains calibrated R_PTF-filter magnitudes for about 21 million sources brighter than magnitude 19, over an area of about 11233 deg^2. The magnitudes are provided in the PTF photometric system, and the color of a source is required in order to convert these magnitudes into other magnitude systems. The magnitudes in this catalog have typical accuracy of about 0.02 mag with respect to magnitudes from the Sloan Digital Sky Survey. The median repeatability of the catalog's magnitudes for stars between 15 and 16 mag, is about 0.01 mag, and it is better than 0.03 mag for 95% of the sources in this magnitude range. The main goal of this catalog is to provide reference magnitudes for photometric calibration of visible light observations.
Author(s): PTF Team
IVOA id: ivo://irsa.ipac/ptf/catalog/ptf_photcal

PTF Sources Catalog

2026-05-28T01:00:00Z

Description: Palomar Transient Factory (PTF) is a fully-automated, wide-field survey aimed at a systematic exploration of the optical transient sky. The PTF Sources catalog is a table containing all the epoch-based source photometry and metadata extracted from the epochal images (SExtractor-based), specifically to support lightcurve construction for DR3.
Author(s): PTF Team
IVOA id: ivo://irsa.ipac/ptf/catalog/ptf_sources

ISO Spectra from the Short Wavelength Spectrometer

2026-05-28T01:00:00Z

Description: The Infrared Space Observatory (ISO) Spectra from the Short Wavelength Spectrometer (SWS) is a uniform catalog of SWS spectral data. It is served by Atlas and derived from valid, full-scan, 2.4-45.4 micron spectra available in the ISO archive.
Author(s): Sloan et al. (2003)
IVOA id: ivo://irsa.ipac/iso/iso_sws

Three-mm Ultimate Mopra Milky Way Survey (ThrUMMS) DR6

2026-05-28T01:00:00Z

Description: Data Release 6 of ThrUMMS consists of complete data cubes and various moments of line emission (12CO, 13CO, C18O) from molecular clouds, across 60d x 2d of the Fourth Quadrant of the Milky Way at a resolution of 72" in (l,b) and 0.09 km/s in VLSR.
Author(s): Barnes, P.; Barnes, D.; Muller, E.
IVOA id: ivo://irsa.ipac/thrumms

Bulge Radial Velocity Assay

2026-05-28T01:00:00Z

Description: The Bulge Radial Velocity Assay (BRAVA) is a survey that consists of spectra for approximately 8,500 red giants in the Galactic bulge. As part of its goal to understand the formation of the Milky Way and its bulge, BRAVA samples radial velocities of the stars at a large scale along with photometry and titanium oxide (TiO) band strengths.
Author(s): BRAVA Team
IVOA id: ivo://irsa.ipac/brava

Great Observatories All-sky LIRG Survey

2026-05-28T01:00:00Z

Description: The GOALS sample consists of a total of 179 LIRGs (log (L_IR/L_sun) = 11.0-11.99) and 22 ultra-luminous infrared galaxies (ULIRGs: log (L_IR/L_sun) > 12.0) selected from the IRAS Revised Bright Galaxy Sample; these 201 objects comprise a statistically complete flux-limited sample of infrared-luminous galaxies in the local universe. The GOALS objects have been the subject of an intense multi-wavelength observing campaign, including space-based imaging and spectroscopy from Spitzer and Herschel.
Author(s): GOALS team
IVOA id: ivo://irsa.ipac/goals/spectra

The California Legacy Survey. I. Planet catalog

2026-05-27T10:12:24Z

Description: We present a high-precision radial velocity (RV) survey of 719 FGKM stars, which host 164 known exoplanets and 14 newly discovered or revised exoplanets and substellar companions. This catalog updated the orbital parameters of known exoplanets and long-period candidates, some of which have decades-longer observational baselines than they did upon initial detection. The newly discovered exoplanets range from warm sub-Neptunes and super-Earths to cold gas giants. We present the catalog sample selection criteria, as well as over 100,000 RV measurements, which come from the Keck-HIRES, APF-Levy, and Lick- Hamilton spectrographs. We introduce the new RV search pipeline RVSearch (http://california-planet-search.github.io/rvsearch/) that we used to generate our planet catalog, and we make it available to the public as an open-source Python package. This paper is the first study in a planned series that will measure exoplanet occurrence rates and compare exoplanet populations, including studies of giant planet occurrence beyond the water ice line, and eccentricity distributions to explore giant planet formation pathways. We have made public all radial velocities and associated data that we use in this catalog.
Author(s): Rosenthal L.J.; Fulton B.J.; Hirsch L.A.; Isaacson H.T.; Howard A.W.,Dedrick C.M.; Sherstyuk I.A.; Blunt S.C.; Petigura E.A.; Knutson H.A.,Behmard A.; Chontos A.; Crepp J.R.; Crossfield I.J.M.; Dalba P.A.,Fischer D.A.; Henry G.W.; Kane S.R.; Kosiarek M.; Marcy G.W.,Rubenzahl R.A.; Weiss L.M.; Wright J.T.
IVOA id: ivo://cds.vizier/j/apjs/255/8

ALMA observations counterparts of SDSS dr14Q

2026-05-27T09:02:55Z

Description: The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that lie in the aggregate ALMA footprint observed since ALMA Cycle 0. The ALMA fluxes are extracted in an automatic fashion, using the ALMA Data Mining Toolkit. All extractions above a signal-to-noise cut of 3.5 are considered, they have been visually inspected and the reliable detections are presented in a catalogue of 376 entries, corresponding to 275 unique quasars. Interesting targets found in the process, i.e. lensed or jetted quasars as well as quasars with nearby submm counterparts are highlighted, to facilitate further studies or potential follow up observations.
Author(s): Wong A.; Hatziminaoglou E.; Borkar A.; Popping G.; Perez-Fournon I.,Poidevin F.; Stoehr F.; Messias H.
IVOA id: ivo://cds.vizier/j/mnras/523/23

New star clusters towards Galactic anticentre

2026-05-27T06:34:34Z

Description: We report the discovery of 31 new open clusters (OCs) identified in Gaia DR3 data through a systematic search over 220 adjacent 1{deg}*1{deg} fields towards the Galactic anticentre, in the direction of the Perseus arm gap. Eight of them display low-density structures, possibly indicating open cluster remnants properties. The objects were identified and characterized through a combined analysis of photometric, kinematic, and spatial distributions, a methodology successfully applied in our previous works. Their structural properties, mean proper motions, ages, distances and reddening were derived and their centres cross-matched with the available catalogues. The clusters are low-concentrated systems and are mostly located within $34$ kpc. They do not belong to the Perseus arm, but may be associated with the Outer Norma arm. The Gulf of Camelopardalis region appears as an interruption in the Perseus arm, possibly reflecting low star-formation activity, dust obscuration, or that the Milky Way is a flocculent, rather than a grand-design spiral galaxy.
Author(s): Ferreira F.A.; Angelo M.S.; Santos J.F.C. Jr; Corradi W.J.B.; Maia F.F.S.
IVOA id: ivo://cds.vizier/j/mnras/548/g621

The CatSouth and CatGlobe QSO candidate catalogs

2026-05-26T12:43:33Z

Description: The Gaia DR3 has provided a large sample of more than 6.6 million quasar candidates with high completeness but low purity. Previous work on the CatNorth quasar candidate catalog has shown that including external multiband data and applying machine learning methods can efficiently purify the original Gaia DR3 quasar candidate catalog and improve the redshift estimates. In this paper, we extend the Gaia DR3 quasar candidate selection to the Southern Hemisphere using data from SkyMapper, CatWISE, and Visible and Infrared Survey Telescope for Astronomy surveys. We train an XGBoost classifier on a unified set of high-confidence stars and spectroscopically confirmed quasars and galaxies. For sources with available Gaia BP/RP spectra, spectroscopic redshifts are derived using a pretrained convolutional neural network (RegNet). We also train an ensemble photometric redshift estimation model based on XGBoost, TabNet, and FT-Transformer, achieving a root mean square error of 0.2256 and a normalized median absolute deviation of 0.0187 on the validation set. By merging CatSouth with the previously published CatNorth catalog, we construct the unified all-sky CatGlobe catalog with nearly 1.9 million sources at G<21, providing a comprehensive and high-purity quasar candidate sample for future spectroscopic and cosmological investigations.
Author(s): Fu Y.; Wu X.-B.; Bouwens R.J.; Caputi K.I.; Pang Y.; Zhu R.; Yang D.-M.,Qin J.; Wang H.; Wolf C.; Li Y.; Joshi R.; Zhang Y.; Huo Z.-Y.; Ai Y.L.
IVOA id: ivo://cds.vizier/j/apjs/279/54

RV & light curves of 8 gas giant systems

2026-05-26T12:12:22Z

Description: Essential information about the formation and evolution of planetary systems can be found in their architectures-in particular, in stellar obliquity ({psi})-as they serve as a signature of their dynamical evolution. Here we present ESPRESSO observations of the Rossiter-McLaughlin (RM) effect of eight warm gas giants, revealing that, independently of the eccentricities, all of them have relatively aligned orbits. Our five warm Jupiters (WASP-106 b, WASP-130 b, TOI-558 b, TOI-4515 b, and TOI-5027 b) have sky-projected obliquities |{lambda}|~0-10{deg}, while the two less massive warm Saturns (K2-139 b and K2-329 A b) are slightly misaligned, having |{lambda}|~15-25{deg}. Furthermore, for K2-139 b, K2-329 A b, and TOI-4515 b, we also measure true 3D obliquities {psi}~15-30{deg}. We also report a nondetection of the RM effect produced by TOI-2179 b. Through hierarchical Bayesian modeling of the true 3D obliquities of hot and warm Jupiters, we find that around single stars warm Jupiters are statistically more aligned than hot Jupiters. Independent of eccentricities, 95% of the warm Jupiters have {psi}<=25{deg} with no misaligned planets, while hot Jupiters show an almost isotropic distribution of misaligned systems. This implies that around single stars warm Jupiters form in primordially aligned protoplanetary disks and subsequently evolve in a more quiescent way than hot Jupiters. Finally, we find that Saturns may have slightly more misaligned orbits than warm Jupiters, but more obliquity measurements are necessary to be conclusive.
Author(s): Espinoza-Retamal J.I.; Jordan A.; Brahm R.; Petrovich C.; Sedaghati E.,Stefansson G.; Hobson M.J.; Tala Pinto M.; Munoz D.J.; Boyle G.; Leiva R.,Suc V.
IVOA id: ivo://cds.vizier/j/aj/170/70

LAMOST VMP MSTO and red giant star metallicities

2026-05-26T09:26:10Z

Description: We present a catalog of 8440 candidate very metal-poor (VMP; [Fe/H]<=-2.0) main-sequence turn-off (MSTO) and red giant stars in the Milky Way, identified from low-resolution spectra in LAMOST DR10. More than 7000 of these candidates are brighter than G~16, making them excellent targets for high-resolution spectroscopic follow-up with 4-10m class telescopes. Unlike most previous studies, we employed an empirical calibration to estimate metallicities from the equivalent widths of the calcium triplet lines, taking advantage of the high signal-to-noise ratio in the red arm of LAMOST spectra. We further refined this calibration to improve its reliability for more distant stars. This method enables robust identification of VMP candidates with metallicities as low as [Fe/H]=-4.0 among both MSTO and red giant stars. Comparisons with metal-poor samples from other spectroscopic surveys and high-resolution follow-up observations confirm the accuracy of our estimates, showing a typical median offset of ~0.1dex and a standard deviation of ~0.2dex.
Author(s): Li X.; Chen H.; Huang Y.; Zhang H.; Beers T.C.; Zhu L.; Liu J.
IVOA id: ivo://cds.vizier/j/apjs/279/53

Planet masses, radii, and orbits from K2 mission

2026-05-26T09:00:57Z

Description: We report the masses, sizes, and orbital properties of 86 planets orbiting 55 stars observed by NASA's K2 Mission with follow-up Doppler measurements by the HIRES spectrometer at the W. M. Keck Observatory and the Automated Planet Finder at Lick Observatory. Eighty-one of the planets were discovered from their transits in the K2 photometry, while five were found based on subsequent Doppler measurements of transiting planet-host stars. The sizes of the transiting planets range from Earth-size to larger than Jupiter (1-3R_{Earth}_ is typical), while the orbital periods range from less than a day to a few months. For 32 of the planets, the Doppler signal was detected with significance greater than 5{sigma} (51 were detected with >3{sigma} significance). An important characteristic of this catalog is the use of uniform analysis procedures to determine stellar and planetary properties. This includes the transit search and fitting procedures applied to the K2 photometry, the Doppler fitting techniques applied to the radial velocities (RVs), and the spectral modeling to determine bulk stellar parameters. Such a uniform treatment will make the catalog useful for statistical studies of the masses, densities, and system architectures of exoplanetary systems. This work also serves as a data release for all previously unpublished RVs and associated stellar activity indicators obtained by our team for these systems, along with derived stellar and planet parameters.
Author(s): Howard A.W.; Sinukoff E.; Blunt S.; Petigura E.A.; Crossfield I.J.M.,Isaacson H.; Kosiarek M.; Rubenzahl R.A.; Brewer J.M.; Fulton B.J.,Dressing C.D.; Hirsch L.A.; Knutson H.; Livingston J.H.; Mills S.M.,Roy A.; Weiss L.M.; Benneke B.; Ciardi D.R.; Christiansen J.L.,Cochran W.D.; Crepp J.R.; Gonzales E.; Hansen B.M.S.; Hardegree-Ullman K.,Howell S.B.; Lepine S.; Martinez A.O.; Rogers L.A.; Schlieder J.E.,Werner M.; Polanski A.S.; Angelo I.; Beard C.; Behmard A.; Bouma L.G.,Brinkman C.L.; Chontos A.; Dai F.; Dalba P.A.; Giacalone S.,Grunblatt S.K.; Hill M.L.; Kane S.R.; Lubin J.; Mayo A.W.; Mocnik T.,Murphy J.M.A.; Rice M.; Rosenthal L.J.; Tyler D.; Van Zandt J.; Yee S.W.
IVOA id: ivo://cds.vizier/j/apjs/278/52

Ring galaxies from DESI Legacy Imaging Surveys DR9

2026-05-26T08:39:11Z

Description: The formation and evolution of ring structures in galaxies are crucial for understanding the nature and distribution of dark matter, galactic interactions, and the internal secular evolution of galaxies. However, the limited number of existing ring galaxy catalogs has constrained deeper exploration in this field. To address this gap, we introduce a two-stage binary classification model based on the Swin Transformer architecture to identify ring galaxies from the DESI Legacy Imaging Surveys. This model first selects potential candidates and then refines them in a second stage to improve classification accuracy. During model training, we investigated the impact of imbalanced data sets on the performance of the two-stage model. We experimented with various model combinations applied to the data sets of the DESI Legacy Imaging Surveys DR9, processing a total of 573,668 images with redshifts ranging from z_spec=0.01-0.20 and mag_r_<17.5. After applying the two-stage filtering and conducting visual inspections, the overall precision of the models exceeded 64.87%, successfully identifying a total of 8052 newly discovered ring galaxies. With our catalog, the forthcoming spectroscopic data from DESI will facilitate a more comprehensive investigation into the formation and evolution of ring galaxies.
Author(s): Zhang A.; Kong X.; Liu B.; Li N.; Bu Y.; Yi Z.; Liu M.
IVOA id: ivo://cds.vizier/j/apjs/279/52

TESS Ten Thousand Catalog: Eclipsing Binaries

2026-05-26T07:17:38Z

Description: The Transiting Exoplanet Survey Satellite (TESS) has surveyed nearly the entire sky in full-frame image mode with a time resolution of 200s to 30 minutes and a temporal baseline of at least 27 days. In addition to the primary goal of discovering new exoplanets, TESS is exceptionally capable at detecting variable stars, and in particular short-period eclipsing binaries, which are relatively common, making up a few percent of all stars, and represent powerful astrophysical laboratories for deep investigations of stellar formation and evolution. We combed Sectors 1-82 of the TESS full-frame image data searching for eclipsing binary stars using a neural network that identified ~1.2 million stars with eclipse-like features. Of these, we have performed an in-depth analysis on ~60,000 targets using automated methods and manual inspection by citizen scientists. Here we present a catalog of 10,001 uniformly vetted and validated eclipsing binary stars that passed all our ephemeris and photocenter tests, as well as complementary visual inspection. Of these, 7936 are new eclipsing binaries while the remaining 2065 are known systems for which we update the published ephemerides. We outline the detection and analysis of the targets, discuss the properties of the sample, and highlight potentially interesting systems. Finally, we also provide a list of ~900,000 unvetted and unvalidated targets for which the neural network found eclipse-like features with a score higher than 0.9, and for which there are no known eclipsing binaries within a sky-projected separation of a TESS pixel (~21").
Author(s): Kostov V.B.; Powell B.P.; Fornear A.U.; Di Fraia M.Z.; Gagliano R.,Jacobs T.L.; de Lambilly J.S.; Durantini Luca H.A.; Majewski S.R.,Omohundro M.; Orosz J.; Rappaport S.A.; Salik R.; Short D.; Welsh W.,Alexandrov S.; da Silva C.M.; Dunning E.; Guhne G.; Huten M.; Hyogo M.,Iannone D.; Lee S.; Magliano C.; Sharma M.; Tarr A.; Yablonsky J.,Acharya S.; Adams F.; Barclay T.; Montet B.T.; Mullally S.; Olmschenk G.,Prsa A.; Quintana E.; Wilson R.; Balcioglu H.; Kruse E.,The Eclipsing Binary Patrol Collaboration
IVOA id: ivo://cds.vizier/j/apjs/279/50

Large Interstellar Polarisation Survey. III

2026-05-26T00:00:00Z

Description: Our understanding of dust in the diffuse interstellar medium remains incomplete with regard to the structure, composition, size distribution, and alignment properties of its grains. Joint observations of reddening, starlight polarisation spectra, and polarised dust emission for individual sightlines provide essential constraints on such properties. We study a far-UV selected sample of 96 reddening curves, for which optical linear polarisation spectra were obtained with FORS at the VLT as part of the Large Interstellar Polarisation Survey (LIPS). Starlight polarisation spectra for 60 stars are presented in this work. These data are combined with Gaia distance estimates and Planck thermal dust emission. A three-component dust model is made publicly available. It consists of nanoparticles, amorphous grains, and micrometre-sized dust agglomerates, varying axial ratios, porosities, sizes, element abundances, and alignment efficiencies to match the observations. The diversity of reddening and polarisation spectra is well reproduced by prolate grains with typical axial ratios of two, a porosity of 10%, and high alignment efficiencies. Such efficiencies can be achieved with radiative torque alignment theory (RAT), but not with imperfect Davis-Greenstein (IDG) alignment, except when adjusting the magnetic-field orientation to maximise the polarisation. Micrometre-sized dust contributes wavelength-independent grey extinction in the optical, accounts for about one-third of the visual extinction, and carries one-third of the dust mass. A follow-up submillimetre survey with high-resolution polarimetry will further constrain grain shapes and alignment physics.
Author(s): Siebenmorgen R.; Bagnulo S.; Fanciullo L.; Vannieuwenhuyse T.; Guillet V.
IVOA id: ivo://cds.vizier/j/a+a/709/a277

MEGARA/GTC IFU cubes of IRAS 17020+4544

2026-05-25T11:32:24Z

Description: The narrow-line Seyfert 1 (NLSy1) galaxy, IRAS 17020+4544, is one of the few known sources exhibiting a multi-phase outflow in the highly ionized and molecular phases consistent with AGN feedback operating in the "energy-conserving" regime. We aim to characterize the properties of the ionized warm ionized gas in IRAS 17020+4544 using new optical integral-field spectroscopic (IFS) data, and to assess the presence of outflowing ionized gas and its connection with the other gas phases and its role in the AGN feedback. We analyze new optical seeing-limited IFS observations obtained with MEGARA at the Gran Telescopio Canarias (GTC) in both low- (R~6000; LR) and medium-resolution (R~12000; MR) modes. We model the H{alpha} and [OIII]{lambda}5007 emission lines using multi-Gaussian fitting to characterize in detail the ionized gas kinematics, particularly that of the ionized outflow, to derive its energetics and compare it with those of the X-ray and molecular phases. Diagnostic diagrams (WHAN, WHaD, and BPT) are used to investigate the dominant ionization mechanism. We identify a fast ionized outflow traced by both H{alpha} and [OIII] emission lines, with similar extensions (Rout~1kpc and ~0.5kpc, respectively) and velocities (vout~1460 and 1240km/s, respectively). A slower ionized outflow (vout~450km/s) is also detected in the secondary component of the [OIII] line. The fast outflow follows an "energy-conserving" regime in both H{alpha} and the [OIII] lines (from the LR setup), while the slower outflow follows a "momentum-driven" regime. The ionized outflows are enclosed within the molecular outflow detected with NOEMA (R_CO_=2.8+/-0.3kpc), and the large momentum boosts derived in both phases suggest efficient AGN feedback, likely dominated by radiatively driven winds (quasar-mode) rather than kinetic (jet-driven) processes. Ionization diagnostics indicate that the outflow is primarily AGN-driven, although a contribution from star formation- driven excitation cannot be ruled out, and some contribution from shocks cannot be excluded on smaller scales. Our results support a scenario where the multi-phase outflow in IRAS17020+4544 is AGN-driven and "energy-conserving" in the different (i.e., highly ionized, warm ionized and molecular) phases, efficiently coupling the AGN energy to the host galaxy's interstellar medium. The molecular outflow appears to be the dominant phase, while the ionized phase contributes less to the mass budget and feedback efficiency.
Author(s): Bellocchi E.; Longinotti A.L.; Salome Q.; Gil de Paz A.,Torres-Papaqui J.P.; Mayya D.; Krongold Y.; Castillo-Morales A.,Robleto-Orus A.; Catalan-Torrecilla C.; Vega O.; Rosa-Gonzalez D.
IVOA id: ivo://cds.vizier/j/a+a/709/a260

4 HFF clusters members structural parameters

2026-05-25T11:30:28Z

Description: We present a detailed study of the stellar kinematic properties of red member galaxies in the cores of four strong lensing galaxy clusters at intermediate redshifts included in the Hubble Frontier Fields programme: Abell 2744 (z=0.307), Abell S1063 (z=0.346), MACS J0416.1-2403 (z=0.397), and MACS J1149.6+2223 (z=0.542). We focussed on a large sample of 723 red cluster members in the four clusters, selected spectroscopically and photometrically, and we measured their structural parameters using MORPHOFIT for all Hubble Frontier Fields bands. Taking advantage of deep (3.1h to 17h of exposure time) integral-field spectroscopic data from the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope, available for the cores of all four clusters, we tested a pipeline based on the public spectral fitting code pPXF to reliably and systematically measure the line-of-sight stellar velocity dispersion {sigma} of cluster members with a spectral S/N>=10, with a statistical uncertainty consistently below 5%. The resulting catalogue contains 213 measured {sigma} values across the four clusters. Combining stellar kinematics and multi-band galaxy morphology, we calibrated the Fundamental Plane relation in the rest-frame r band for the early-type cluster members, selected from their colour and morphology; we found compatible parameters both across the clusters and in comparison with large samples of early-type field galaxies, and noted hints of zero-point evolution with redshift. Finally, we used the calibrated Fundamental Plane relations to assign a velocity dispersion value to all 723 red cluster members and studied the velocity dispersion function for each cluster, down to log{sigma}[km/s]=1.5. In spite of the intrinsic variability between the four clusters resulting from their assembly history, a Schechter function fit of the velocity functions suggests compatible parameters: a positive {alpha} slope with values in the range 0.55-1.60 and log{sigma}*[km/s] between 2.18 and 2.47. Unlike previous works, we extended the systematic study of the central velocity dispersion of cluster galaxies to lower-{sigma} regimes. We suggest that deeper insights on the evolution of member galaxies may be obtained with a larger cluster sample spanning a wider redshift range.
Author(s): Granata G.; Tortorelli L.; Grillo C.; Rosati P.; D'Addona M.; Mercurio A.,Angora G.; Bergamini P.; Caminha G.B.
IVOA id: ivo://cds.vizier/j/a+a/709/a254

Carbon star candidates from LAMOST and SDSS

2026-05-22T13:51:44Z

Description: Carbon stars are critical for understanding stellar evolution and exploring cosmic chemistry. This paper provides 7809 carbon star candidates identified from the Large-Area Multi-Object Fiber Optic Spectroscopic Telescope (LAMOST) DR11 and Sloan Digital Sky Survey (SDSS) DR18, using a parallel carbon star feature recognition method. This method deploys a parallel multi-interval feature representation model and a k-nearest neighbor classification model, effectively characterizing local and global molecular bands of carbon stars and enhancing feature discrimination, especially for weak features that are highly susceptible to noise interference. The recognition performance F1-score can exceed 96%. Moreover, with parallel strategies for interval representation, the search efficiency has improved. And we construct a new catalog of carbon stars subtypes, including 1616 barium (Ba) stars, 1720 C-H stars, 1621 C-N stars, 1205 C-R stars, and 1647 stars labeled as "Unknown" due to their low signal-to-noise ratios (S/Ns). Compared with the LAMOST DR11 pipeline, carbon stars by Li+ 2024, J/ApJS/271/12 and the SDSS DR18 pipeline, we identify 1403 and 1644 new candidates from LAMOST, and 661 new candidates from SDSS DR18, respectively. In our catalog, the majority of C-N, C-R, and Ba stars from LAMOST are located at low Galactic latitudes with |b|=30{deg}, while most candidates from SDSS are located at high Galactic latitudes. And the vast majority of Ba, C-H, C-R, and Unknown stars show relatively high effective temperatures. Some carbon stars exhibit stellar activity, potentially influenced by dense interstellar materials, internal magnetic fields, and rotation effects. In the g, r, and i bands, C-N and Unknown stars from LAMOST exhibit lower S/Ns, influenced by high interstellar density at low Galactic latitudes, while Unknown stars from SDSS show higher S/Ns. Among the newly discovered carbon stars, Ba from LAMOST, Unknown from SDSS, and C-R stars have higher S/Ns than other subclasses.
Author(s): Zhou L.; Cai J.; Yang H.; Luo A.; Li Y.; Shi C.; Zhang B.; Tian J.,Yuan Y.; Yang Y.
IVOA id: ivo://cds.vizier/j/apjs/279/40

Asteroseismology of 687 TESS red giants

2026-05-22T13:15:12Z

Description: The individual modes and asymptotic parameters are important characteristics of stellar oscillation. Using TESS 2 minute cadence data from Sectors 1 to 75, we perform asteroseismic analysis of 687 red giants, and provide their oscillation mode parameters. The mode parameters, including frequencies {nu}_n,l_, amplitudes A_n,l_, and line widths {Gamma}_n,l_, are obtained through Markov Chain Monte Carlo fitting. The median uncertainty for frequency is 0.047{mu}Hz. Using the radial mode frequencies, we calculate the values of {Delta}{nu}, and derive asymptotic parameters ({epsilon}p, {epsilon}c, {delta}{nu}0l, q, and {Delta}{Pi}1) based on l=0,1,2 modes. For red giants with {Delta}{nu}>15.6{mu}Hz, there is a weaker correlation between {delta}{nu}02 and {Delta}{nu}, and a stronger mass dependence, compared to stars with lower {Delta}{nu}. Additionally, the ratio {delta}{nu}02/{Delta}{nu} presents a pronounced increase with {Delta}{nu} decrease, as these stars undergo rapid core contraction and their convective envelopes extend deep into the interior. At this stage, the ratio {delta}{nu}02/{Delta}{nu} may serve as a robust indicator for diagnosing the location of the convective boundary. Furthermore, the {epsilon}c values can be a potential index to distinguish red clump (RC) and secondary RC stars from red giant branch stars in the TESS field.
Author(s): Zhou J.; Bi S.; Li Y.; Yu J.; Li T.; Zhang X.; Ye L.; Li M.; Long L.,Sun T.; Chen Y.
IVOA id: ivo://cds.vizier/j/apjs/279/37

Confirmed AGN type 1 & 2 from sp. in Kepler fields

2026-05-22T12:35:59Z

Description: We utilized the Edelson & Malkan (2012, J/ApJ/751/52) and Stern+ 2012ApJ...753...30S selection techniques and other methods to identify active galactic nuclei (AGN) candidates that were monitored during the Kepler prime and K2 missions. Subsequent to those observations, we obtained 125 long-slit optical spectra with the Lick 3m telescope, 58 spectra with the Palomar 5m telescope, and three spectra with the Keck 10m telescope to test these identifications. Of these 186 AGN candidates, 105 were confirmed as Type 1 AGN and 35 as Type 2 AGN, while the remaining 46 were found to have other identifications (e.g., stars and normal galaxies). This indicated an overall reliability of ~75%, while the two main methods had much higher reliability, 87%-96%. The spectra indicated redshifts out to z=3.4. Then, we examined the AGN sample properties through the Baldwin-Phillips-Terlevich diagram and compared the AGNs' spectral energy distributions with those from the literature. We found that our sample yielded the same AGN population as those identified through other methods, such as optical spectroscopy.
Author(s): Tsan T.; Malkan M.; Edelson R.; Smith K.; Stern D.; Graham M.
IVOA id: ivo://cds.vizier/j/apjs/279/22

The California-Kepler Survey. XI. Activity

2026-05-22T11:44:31Z

Description: Surveys of exoplanet host stars are valuable tools for assessing population level trends in exoplanets, and their outputs can include stellar ages, activity, and rotation periods. We extracted chromospheric activity measurements from the California-Kepler Survey Gaia survey spectra in order to probe connections between stellar activity and fundamental stellar properties. Building on the California Kepler Survey's legacy of 1189 planet host star stellar properties including temperature, surface gravity metallicity, and isochronal age, we add measurements of the CaII H and K lines as a proxy for chromospheric activity for 879 planet hosting stars. We used these chromospheric activity measurements to derive stellar rotation periods. We find a discrepancy between photometrically derived and activity-derived rotation periods for stars on the Rossby Ridge. These results support the theory of weakened magnetic braking. We find no evidence for metallicity-dependent activity relations, within the metallicity range of -0.2 to +0.3 dex. With our single epoch spectra we identify stars that are potentially in Maunder minimum-like state using a combination of log(R_HK_^'^) and position below the main sequence. We do not yet have the multiyear time series needed to verify stars in Maunder minimum-like states. These results can help inform future theoretical studies that explore the relationship between stellar activity, stellar rotation, and magnetic dynamos.
Author(s): Isaacson H.; Kane S.R.; Carter B.; Howard A.W.; Weiss L.; Petigura E.A.,Fulton B.
IVOA id: ivo://cds.vizier/j/apj/961/85

N2H+ & CCS abundances in HII star forming regions

2026-05-22T11:39:10Z

Description: Using the Institut de Radioastronomie Millmetrique 30m telescope, we presented observations of N_2_H^+^J=1-0, CCS J_N_=8_7_-7_6_ and 7_7_-6_6_ lines toward a large sample of ultracompact H II regions (UC H IIs). Among our 88 UC H IIs, 87 and 33 sources were detected in the N_2_H^+^J=1-0 and CCS J_N_=8_7_-7_6_ lines, respectively. For the CCS 7_7_-6_6_ transition, we detected emission in 10 out of 82 targeted sources, all of which also exhibited emission in the CCS J_N_=8_7_-7_6_ line. Physical parameters are derived for our detections, including the optical depth and excitation temperature of N_2_H^+^, the rotational temperature of CCS and the column density. Combining our results and previous observation results in different stages of high-mass star-forming regions (HMSFRs), we found that the column density ratio N(N_2_H^+^)/N(CCS) increases from high-mass starless cores through high-mass protostellar cores to UC H IIs. This implies that N(N_2_H^+^)/N(CCS) can trace the evolution process of HMSFRs. It was supported by our gas-grain chemical model, which shows that N(N_2_H^+^)/N(CCS) increases with the evolution age of HMSFRs. The temperature, density and chemical age were also constrained from our best-fit model at each stage. Thus, we propose N(N_2_H^+^)/N(CCS) as a reliable chemical clock of HMSFRs.
Author(s): Chen J.L.; Zhang J.S.; Ge J.X.; Wang Y.X.; Yu H.Z.; Zou Y.P.; Yan Y.T.,Wang X.Y.; Wei D.Y.
IVOA id: ivo://cds.vizier/j/aj/170/74

TGSSADR Source Catalogue

2026-05-22T11:00:15Z

Description

This service queries the catalogue of radio sources from the images
of the TIFR GMRT Sky Survey (TGSS) Alternative Data Release (up to 1
deg square). This data release contains previously unpublished data
from the TIFR GMRT Sky Survey (TGSS), which has been independently
reprocessed. It includes continuum stokes I images of 99.5 percent of
the radio sky north of -53° DEC (3.6π sr, or 90 percent of the full
sky) at a resolution of 25“ x 25” north of 19° DEC and 25“ x 25” /
cos(DEC-19°) south of 19°, and a median noise of 3.5 mJy/beam. The
extracted radio source catalog contains positions, flux densities,
sizes and more for 0.62 Million sources down to a 7-sigma
peak-to-noise threshold.

Author(s)

Intema, H.; Mooley, K.

IVOA id

ivo://astron.nl/tgssadr/q/cone

Planet-forming disks

2026-05-22T09:12:19Z

Description: The evolution of planet-forming disks and the processes of planet formation influence each other, and both of them are possibly impacted by the local environment. Extensive high-resolution imagery of disks across space and time is the best tool for determining their evolution. We compiled a comprehensive list of disk-bearing young stars with near-IR high-contrast images available. The sample sums up to 268 sources, including 51 targets with no prior publications, which makes this study the largest of its kind and the most extensive release of IR disk images to date. Our census reveals very diverse disk and ambient morphologies. Disks in Lupus are bright, in Chamaeleon are faint, in Corona Australis and Taurus are frequently surrounded by ambient emission. Disks experience an abrupt increase in IR brightness between 2Myr and 5Myr. The earliest IR disk cavities around single stars arise after 2-3Myr explaining why are young disks faint in the near-IR, and determining which disks can live longer. Well-known, high-longevity disks (>8Myr) are always bright. Ambient material is detected in more than 20% of young sources but the fraction drops with time. We find a clear correspondence for the presence of ambient material with the stellar variability, near-IR excess, and mass accretion rate as well as, in turn, with spirals and shadows in disks. Half of the disks with ambient material show spirals while none of them show rings. We therefore propose that the spirals and the disk warps responsible for shadows are generally induced by late infall from the medium, and that this also affects the stellar accretion. The emerging picture proves the fundamental role of the environment for the disk evolution and planet formation.
Author(s): Garufi A.; Ginski C.; Benisty M.; Vioque M.; Winter A.; Huang J.,Manara C.F.; Dominik C.
IVOA id: ivo://cds.vizier/j/a+a/709/a269

RVs and photometry light curves of TOI-5624

2026-05-22T09:10:21Z

Description: Following the 2022 alert of a TESS object of interest transiting TOI-5624 (a G7, Vstar ~100pc away), a CHEOPS campaign in 2023 detected four planetary signals at P_b_~3.4, P_c_~7.9, P_d_~13.7, and P_e_~21.5 days, later confirmed by additional TESS and CHEOPS photometry in 2024-2025. By using TESS and CHEOPS photometry along with HARPS-N and SOPHIE high-resolution spectra, we determined the planet properties and performed a dynamical analysis of the system. After analysing the photometric data, we extracted and modelled the radial velocity (RV) time series using two independent methodologies both within a Markov chain Monte Carlo framework. We further integrated the N-body equations of motion, while simultaneously fitting the transit times and the detrended RVs, to dynamically characterise the system. We present the discovery of four transiting sub-Neptunes with radii of R_b_=2.314+/-0.035R_{Earth}_, R_c_=2.474+/-0.042R_{Earth}_, R_d_=3.584_-0.050_^+0.051^ R_{Earth}_, and R_e_=3.247_-0.043_^+0.042^ R_{Earth}_ and masses of M_b_=9.4+/-1.4M_{Earth}_, M_c_=4.8+/-1.9M_{Earth}, M_d_=4.9+/-2.2M_{Earth}_, and M_e_=8.9_-3.0_^+2.9^M_{Earth}_. Our photometric analysis reveals that the outermost transiting planet TOI-5624e shows significant transit time variations (TTVs). Indeed, we find a robust Keplerian signal in the RV time series close to the 2:1 period commensurability with TOI-5624e, which explains the TTV pattern exhibited by TOI-5624e according to our dynamical analysis. We label this non-transiting planet as TOI-5624f and find its minimum mass to be M_f_*sini_f_=13.0+/-3.7M_{Earth}_. Among the known systems hosting more than four planets, the remarkable precision with which the radii have been measured (<1.7%) and the firm assessment (>3{sigma}) of the mass for at least three planets has been previously reached only for TRAPPIST-1. Additional photometric observations will enable a better sample of the TTV modulation and a more robust dynamical determination of the masses.
Author(s): Bonfanti A.; Gandolfi D.; Leonardi P.; Osborn H.P.; Serrano L.M.,Hebrard G.; Billot N.; Bekkelien A.; Olofsson G.; Broeg C.; Nardiello D.,Sousa S.G.; Wilson T.G.; Correia A.C.M.; Pezzotti C.; Brandeker A.,Fossati L.; Gillon M.; Stalport M.; Akinsanmi B.; Alibert Y.; Alonso R.,Asquier J.; Barczy T.; Barrado D.; Barros S.C.C.; Baumjohann W.; Benz W.,Borsato L.; Castro-Gonzalez A.; Collier Cameron A.; Csizmadia Sz.,Cubillos P.E.; Davies M.B.; Deleuil M.; Delfosse X.; Deline A.,Demangeon O.D.S.; Demory B.-O.; Derekas A.; Destriez F.; Edwards B.,Ehrenreich D.; Erikson A.; Fortier A.; Fridlund M.; Gazeas K.; Gudel M.,Gunther M.N.; Hara N.; Heidari N.; Heitzmann A.; Helling C.; Isaak K.G.,Keller T.; Kiss L.L.; Kitzmann D.; Korth J.; Lacedelli G.; Lam K.W.F.,Laskar J.; Lecavelier des Etangs A.; Leleu A.; Lendl M.; Magrin D.,Maxted P.F.L.; Mecina M.; Merin B.; Mordasini C.; Nascimbeni V.,Ottensamer R.; Pagano I.; Palle E.; Peter G.; Piazza D.; Piotto G.,Pollacco D.; Queloz D.; Ragazzoni R.; Rando N.; Rauer H.; Ribas I.,Santos N.C.; Scandariato G.; Segransan D.; Simon A.E.; Smith A.M.S.,Sulis S.; Szabo Gy.M.; Udry S.; Ulmer-Moll S.; Van Grootel V.,Venturini J.; Verrecchia F.; Villaver E.; Walton N.A.; Wolf S.,Wolter D.; Zingales T.
IVOA id: ivo://cds.vizier/j/a+a/709/a265