VO Fresh

OCA Data Center TAP service

2026-03-13T14:31:21Z

Description

The OCA Data Center's TAP end point. The Table Access
Protocol (TAP) lets you execute queries against our database tables,
inspect various metadata, and upload your own data. It is thus the
VO's premier way to access public data holdings.

Tables exposed through this endpoint include: epn_core from the meteospace schema, columns, groups, key_columns, keys, schemas, tables from the tap_schema schema.

Author(s)

Observatoire de la CÃ´te d'Azur

IVOA id

ivo://purx/solar-dachs/tap

HWO Target Stars and Systems 2025 list (TSS25)

2026-03-11T15:18:22Z

Description: The HWO Target Stars and Systems 2025 (TSS25) list is a community-developed catalog of potential stellar targets for the Habitable Worlds Observatory (HWO) in its survey to directly image Earth-sized planets in the habitable zone. The TSS25 list categorizes potential HWO targets into priority tiers based on their likelihood to be surveyed and the necessity of obtaining observations of their stellar properties prior to the launch of the mission. This target list builds upon previous efforts to identify direct imaging targets and incorporates the results of multiple yield calculations assessing the science return of current design concepts for HWO. The TSS25 list identifies a sample of target stars that are likely to be observed by HWO (Tiers 1 and 2), independent of assumptions about the mission's final architecture. These stars should be the focus of community precursor science efforts in order to mitigate risks and maximize the science output of HWO. This target list is publicly available and is a living catalog that will be continually updated leading up to the mission.
Author(s): Tuchow N.W.; Harada C.K.; Mamajek E.E.; Tanner A.; Hinkel N.R.; Belikov R.,Sirbu D.; Ciardi D.R.; Stark C.C.; Morgan R.M.; Savransky D.; Turmon M.
IVOA id: ivo://cds.vizier/j/pasp/137/j4402

Pavol Jozef Šafárik University Archive TAP service

2026-03-11T09:16:58Z

Description

The Pavol Jozef Šafárik University Archive's TAP end point. The Table Access
Protocol (TAP) lets you execute queries against our database tables,
inspect various metadata, and upload your own data. It is thus the
VO's premier way to access public data holdings.

Tables exposed through this endpoint include: gaia_source_lite_eb, lightcurves, ts_ssa, vari_eclipsing_binary_lite from the gaiadr3_eb schema, obscore from the ivoa schema, acepheids, blap, cepheids, cv, dsct, eclipsing, heartbeat, lightcurves, m54, miras, objects_all, raw_data, rotating, rrlyr, t2cep, transits, ts_ssa from the ogle schema, columns, groups, key_columns, keys, schemas, tables from the tap_schema schema, main from the upjs_img schema, lightcurves, objects, raw_data, ts_ssa from the upjs_ts schema.

Author(s)

UPJŠ Archive

IVOA id

ivo://astro.upjs/tap

OGLE OCVS SSA Lightcurve Datasets

2026-03-11T08:16:58Z

Description

This service exposes OGLE photometric light curves. The light curves
are published per-band and are also discoverable through ObsCore.

Author(s)

Soszyński, I.; Udalski, A.; Szymański, M.K.; Pietrukowicz, P.; Skowron, D.M.; Skowron, J.; Poleski, R.; Mróz, P.; Kozłowski, S.; Ulaczyk, K.; Iwanek, P.; Gromadzki, M.; Rybicki, K.; Wrona, M.; Ratajczak, M.; Mróz, M.; Borowicz, J.; Głowacki, M.; Urbanowicz, M.

IVOA id

ivo://astro.upjs/ogle/q/ssa

SRG/eROSITA sources in Hyades

2026-03-11T07:46:45Z

Description: Using data from the all-sky X-ray survey with the eROSITA telescope onboard the SRG orbital observatory and the optical catalog of Hyades cluster members constructed from Gaia data (2023A&A...678A..75Z), we have investigated the X-ray emission from cluster stars. Of the 395 cluster members located in the eastern Galactic part of the sky, eROSITA detects X-ray emission from 290 stars, 171 of which have been found for the first time in X-rays. At the Hyades distance (~47pc) the median eROSITA sensitivity in this sky region corresponds to a 0.3-2.3keV luminosity L_X_~2.6x10^27^erg/s, allowing 100% of the stars with spectral types from F0 to K5 to be detected within the Hyades tidal radius. We have also investigated objects in the Hyades tidal tail (2019A&A...621L...3M, 2019A&A...621L...2R), where X-ray emission was recorded from 114 of the 281 known tidal tail members, 59 of which have been found in X-rays for the first time.
Author(s): Khamitov I.M.; Bikmaev I.F.; Gilfanov M.R.; Sunyaev R.A.; Medvedev P.S.,Gorbachev M.A.; Sklyanov A.S.; Efremova P.D.; Panarin S.S.
IVOA id: ivo://cds.vizier/j/other/astl/51.412

Abundances for 60 Classical Cepheids (DCEPs)

2026-03-11T07:11:50Z

Description: Classical Cepheids (DCEPs) are among the most important distance calibrators thanks to the correlation between their period and luminosity (PL relation), and play a crucial role in the calibration as the first rung of the extragalactic distance ladder. Given their typical age, they also constitute an optimal tracer of the young population in the Galactic disc. We aim to increase the number of available DCEPs with high-resolution spectroscopic metallicities, study the galactocentric radial gradients of several chemical elements, and analyse the spatial distribution of the Galactic young population of stars in the Milky Way disc. We performed a complete spectroscopical analysis of 136 spectra obtained from three different high- resolution spectrographs, for a total of 60 DCEPs. More than half have pulsational periods longer than 15 days, up to 70 days, doubling the number of stars in our sample with P>15d. We derived radial velocities, atmospheric parameters, and chemical abundances for up to 33 different species. We present an updated list of trusted spectroscopic lines for the detection and estimation of chemical abundances. We used this new set to revisit the abundances already published in the context of the C-MetaLL (Cepheids- Metallicity in the Leavitt Law) survey and increase the number of available chemical species. For the first time (to our knowledge), we present the estimation of abundances for Cepheids for dysprosium (Dy, Z=66), as well as a systematic estimation of erbium (Er, Z=68), lutetium (Lu, Z=71), and thorium (Th, Z=90) abundances. We calculated a galactic radial gradient for [Fe/H] with a slope of -0.064+/-0.002dex/kpc, in good agreement with recent literature estimation. The other elements also exhibit a clear negative radial trend, with this effect diminishing and eventually disappearing for heavier neutron-capture elements. Depending on the proposed spiral arms model present in several literature sources, our most external stars agree on tracing either the Perseus, the Norma-Outer, or both the Outer and the association Outer-Scutum-Centaurus (OSC) arms.
Author(s): Trentin E.; Catanzaro G.; Ripepi V.; Luongo E.; Marconi M.; Musella I.,Cusano F.; Storm J.; Bhardwaj A.; De Somma G.; Leccia S.; Sicignano T.,Molinaro R.; Testa V.
IVOA id: ivo://cds.vizier/j/a+a/707/a142

Theoretical investigation of transition data in SI

2026-03-11T07:06:02Z

Description: Accurate and comprehensive atomic data are essential for the modelling of stellar spectra. Uncertainties in the oscillator strengths of specific lines used for abundance analyses directly translate into uncertainties in the derived elemental abundances; and incomplete or biased atomic data sets can impart significant errors in non-local thermodynamic equilibrium modelling. Theoretical calculations of atomic data are therefore crucial to supplement the limited experimental results. In this work, we present extensive atomic data, including oscillator strengths, transition rates and lifetimes, for 1,730 electric dipole (E1) transitions among 107 levels in neutral sulphur (SI) by using the multiconfiguration Dirac-Hartree-Fock (MCDHF) and relativistic configuration interaction (RCI) methods. These levels belong to the configurations 3p^3np (n=3-7),3p^3nf (n=4,5), 3s3p^5, 3p^3ns (n=4-7), and 3p^3nd~(n=3-6). The accuracy of the computed transition rates is assessed by combining the comparison of the differences in transition rates between the Babushkin and Coulomb gauges with a cancellation factor analysis. Approximately 16% of the ab initio results achieved an accuracy classification of A-B, corresponding to uncertainties within 10%, as defined by the Atomic Spectra Database of the National Institute of Standards and Technology (NIST ASD). Applying a fine-tuning technique was found to significantly improve the accuracy of the results in the Coulomb gauge, thereby improving the consistency between the Babushkin and Coulomb gauges; about 24% of the fine-tuned transition data are assigned to the accuracy classes A-B.
Author(s): Li W.; Amarsi A. M.; Jonsson P.
IVOA id: ivo://cds.vizier/j/a+a/707/a141

Astro-COLIBRI Simple Cone Search

2026-03-10T14:20:44.911000Z

Description: IVOA-compliant Simple Cone Search service for Astro-COLIBRI.
IVOA id: ivo://astrocolibri/conesearch

Gaia DR3 eclipsing binaries light curves SSA

2026-03-10T14:10:25Z

Description

This service exposes photometric light curves of eclipsing binaries
from Gaia DR3 epoch photometry via the VO SSA protocol. The light
curves are published per-band and are also discoverable through
ObsCore.

Author(s)

GAIA Collaboration

IVOA id

ivo://astro.upjs/gaiadr3_eb/q/ssa

Omega Cen JWST+HST phot. and proper motions

2026-03-10T11:21:34Z

Description: We combine F115W and F277W images collected with the Near Infrared Camera of the James Webb Space Telescope with multiband, multi-epoch Hubble Space Telescope observations of omega Centauri to investigate its multiple stellar populations and internal kinematics. Our study focuses on a region spanning about 0.9 to 2.3 half-light radii from the cluster center, which is largely unexplored by these telescopes. Using chromosome maps, we identified the principal populations along the upper main sequence and among M dwarfs, distinguishing lower-stream stars chemically akin to first-generation globular cluster stars with similar metallicities from upper-stream stars enriched in helium and nitrogen but oxygen poor. Both streams also host subpopulations with varying metallicities. We found radially anisotropic motions, with upper-stream stars exhibiting significantly stronger anisotropy than lower-stream stars. Subdividing the upper stream into extreme and intermediate light-element populations revealed a gradient in anisotropy, with intermediate stars lying between the lower-stream stars and extreme upper-stream populations. However, metal-rich and metal-poor stars within each stream show moderate kinematic differences. The lower-stream stars show a higher angular momentum dispersion compared to upper-stream stars, and they also exhibit stronger systemic rotation and proper motion skewness, further highlighting their kinematic divergence. Finally, leveraging a mass range of about 0.15 to 0.7 solar masses, we detected a low degree of energy equipartition for all cluster stars, which decreases with radial distance from the cluster center.
Author(s): Ziliotto T.; Milone A.P.; Cordoni G.; Marino A.F.; Legnardi M.V.,Dondoglio E.; Bortolan E.; Muratore F.
IVOA id: ivo://cds.vizier/j/a+a/707/a86

Canis Major region with Gaia-DR3

2026-03-10T11:19:45Z

Description: The Canis Major (CMa) star-forming region, a remote molecular cloud complex within the recently discovered Radcliffe Wave, remains underexplored in literature. We revisit the stellar census in the CMa region, characterizing its stellar population, kinematics, and age using recent astrometric and photometric data from the third data release of the Gaia space mission (Gaia-DR3). We conducted a membership analysis of Gaia-DR3 sources across a 16deg^2^ field encompassing the youngest subgroups in CMa. This new stellar census, combined with spectroscopic observations, allowed us to investigate the structure, kinematics, and age of this region. Results: We identified 1531 objects as members of the CMa region, confirming 401 previously known members and introducing 1130 new candidate members. These objects have magnitudes ranging from 10 to 18mag in G band from Gaia DR3. We identified two subgroups of CMa stars in our sample labeled as Cluster A and Cluster B. They are located at roughly the same distance (d_A_=1150^+79^_-88_pc and d_B_=1183^+103^_-108_pc) and exhibit similar space motions that can be derived thanks to the precise radial velocities obtained in this study. The subgroups have a mean isochronal age of about 2-3Myr. However, based on infrared photometry we show that Cluster A has a higher fraction of disc-bearing stars suggesting that it could be somewhat younger than Cluster B. Our analysis provides new insights into the stellar population of the Canis Major region, by identifying new members, characterizing their kinematics, and assessing their evolutionary stages. Future studies incorporating additional data from upcoming Gaia data releases, multi-wavelength and high-resolution spectroscopic observations will be essential for further advancing our understanding of the history of star formation in this region.
Author(s): Nogueira-Silva S.; Galli P.A.B.; Olivares J.; Bouy H.; Popowicz B.P.,Merino P.M.; Santos-Silva T.; Gregorio-Hetem J.; Miret-Roig N.; Alves J.
IVOA id: ivo://cds.vizier/j/a+a/707/a85

TOI-5789.01 planet candidate HARPS-N RVs

2026-03-10T09:34:39Z

Description: Sub-Neptunes with planetary radii of R_p_=~2-4 R_{Earth}_ are the most common planets around solar-type stars in short-period (P<100d) orbits. It is still unclear, however, what their most likely composition is, that is whether they are predominantly gas dwarfs or water worlds. The sub-Neptunes orbiting bright host stars are very valuable because they are suitable for atmospheric characterization, which can break the well-known degeneracy in planet composition from the planet bulk density, when combined with a precise and accurate mass measurement. Here we report on the characterization of the sub-Neptune TOI-5789 c, which transits in front of the bright (V=7.3mag and K_s_=5.35mag) and magnetically inactive K1V dwarf HIP 99452 every 12.93 days, thanks to TESS photometry and 141 high-precision radial velocities obtained with the HARPS-N spectrograph. We find that its radius, mass, and bulk density are R_c_=2.86^+0.18^_-0.15_R_{Earth}_, M_c_=5.00+/-0.50M_{Earth}_, and {rho}_c_=1.16+/-0.23gcm^-3^, and we show that TOI-5789c is a promising target for atmospheric characterization with both JWST and, in the future, Ariel. By analyzing the HARPS-N radial velocities with different tools, we also detect three additional non-transiting planets, namely TOI-5789b, d, and e, with orbital periods and minimum masses of P_b_=2.76 d, M_b_sini=2.12+/-0.28, P_d_=29.6d, M_d_sini=4.29+/-0.68M_{Earth}_, and P_e_=63.0d, M_e_sini=11.61+/-0.97M_{Earth}_. TOI-5789 is a mutually inclined system as the difference between the orbital inclinations of planets b and c must be higher than ~4deg. Nevertheless, from sensitivity studies based on both the HARPS-N and archival HIRES radial-velocity measurements, we can exclude that these relatively high mutual inclinations are due to the perturbation by an outer gaseous giant planet.
Author(s): Bonomo A.S.; Naponiello L.; Sozzetti A.; Benatti S.; Carleo I.; Biazzo K.,Cubillos P.E.; Damasso M.; Di Maio C.; Dorn C.; Hara N.; Polychroni D.,Steinmeyer M.-L.; Collins K.A.; Desidera S.; Dumusque X.; Lanza A.F.,Safonov B.S.; Stockdale C.; Turrini D.; Ziegler C.; Affer L.; D'Arpa M.,Fardella V.; Harutyunyan A.; Lorenzi V.; Malavolta L.; Mancini L.,Mantovan G.; Micela G.; Murgas F.; Nardiello D.; Pagano I.; Palle E.,Pedani M.; Pinamonti M.; Rainer M.; Scandariato G.; Spinelli R.,Zingales T.
IVOA id: ivo://cds.vizier/j/a+a/707/a197

UVIT Observtaion of HCG 77

2026-03-10T09:29:35Z

Description: Interactions and mergers possibly enhance the star formation in dwarf galaxies in a group environment. We aim to study star-forming regions and the spectral energy distribution of two possibly interacting galaxies, PGC 56121 and PGC 56125, in the Hickson Compact Group 77. We utilized the far-ultraviolet (FUV) channel of the Ultra Violet Imaging Telescope (UVIT) on board AstroSat to observe and produce FUV images of the galaxies. Our FUV images are at a much higher resolution in comparison to those obtained from previous galaxy surveys by GALEX in the near-UV and those from PS-1, DSS. We have identified several star-forming regions in the two possibly interacting galaxies, PGC 56121 and PGC 56125. These two galaxies form a pair widely separated in redshift and are seen in projection. We also report the presence of a candidate tidal dwarf galaxy at the end of one of the tidal tails located to the east of the pair, and we identified three major star-forming regions in the tidal dwarf. The spectral energy distribution of three galaxies in the system is presented and analyzed to investigate the key physical properties, such as stellar mass, dust mass, total luminosity, and star formation history, of the three galaxies. Based on these observations and on a comparison with observations in radio, these three galaxies are probably part of a small group of interacting galaxies.
Author(s): Srivastava A.; Jassal H.K.; Gulati M.; Singh K.P.
IVOA id: ivo://cds.vizier/j/a+a/707/a248

eJWST AGN observation catalogue

2026-03-10T09:28:09Z

Description: The European Archive of the James Webb Space Telescope (eJWST) provides access to all data collected by The James Webb Space Telescope (JWST). JWST's capabilities span from studying early universe galaxy formation to probing exoplanet atmospheres. Specifically, for Active Galactic Nuclei (AGN), JWST offers unparalleled opportunities, enabling investigation into AGN phenomena with unprecedented detail through high-resolution imaging, spectroscopy, and photometric data. This study aims to compile and release a catalogue of all AGN observations conducted with JWST. Using eJWST, we systematically filter and organize these observations to facilitate access and retrieval of all of JWST's data products related to AGNs. Our goal is to provide the community with a valuable resource for their research. We compiled the AGN observations in eJWST using specific keywords set by the principal investigators in their proposals, manually reviewing the approved programs of JWST, as well as cross-matching all available observations with available AGN catalogues such as the Million Quasar catalogue, the SDSS MaNGA AGN catalogue, the CDFS catalogue, and others. The resulting catalogue contains a total of 3242 individual AGNs included in JWST observations. This is one of the first extensive collections of AGN observations from the JWST. It includes detailed information about the targets (name, coordinates, redshift), specifics of the JWST observations (instrument, aperture, filter, etc.), and provides links for data downloads.
Author(s): Lenk V.; Labiano A.; Circosta C.; Alonso-Herrero A.; Wylezalek D.
IVOA id: ivo://cds.vizier/j/a+a/707/a110

H.E.S.S. DL3 DR1 Cone Search Service

2026-03-09T23:12:27Z

Description

The release consists of event lists and instrument response functions
for observations of various well-known gamma-ray sources (the Crab
nebula, PKS 2155-304, MSH 15-52, RX J1713.7-3946) as well as
observations of empty fields for background modeling.

Author(s)

H.E.S.S. collaboration

IVOA id

ivo://padc.obspm.he/hess_dr/q/cone

Kolonica timeseries Cone Search

2026-03-09T18:04:37Z

Description: The table with basic parameters of the observed objects
Author(s): UPJŠ
IVOA id: ivo://astro.upjs/upjs_ts/t/kolonica-objects

Kolonica light curves

2026-03-09T18:04:30Z

Description

This service exposes photometric light curves obtained with small
telescopes at the Kolonica Observatory. The first published dataset
covers observations from 2019–2021. The light curves are published
per-band and are also discoverable through ObsCore.

Author(s)

UPJŠ

IVOA id

ivo://astro.upjs/upjs_ts/q/ssa

Hamburg/ESO service SSAP

2026-03-09T14:45:08Z

Description

The Hamburg/ESO survey (HES) is a digital objective prism survey covering
the total southern extragalactic sky. It is based on Kodak IIIa-J plates
which have been taken with the 1m ESO Schmidt telescope and its 4° prism.
The spectral coverage is 3200-5300 Å, at an resolution of 15 Å at H gamma.
The magnitude range covered is roughly between 18.5 and 11 mag in B_J.

This is a collection of uniformly reduced spectra prepared by Norbert
Christlieb.  It is also intended as a sort-of resolver for HES names
(“identifiers“) like ”HE 2301-7732”; unfortunately, these identifiers are
not unique. You will need to apply domain knowledge in order to find the
object actually being referred to when resolving an identifier of this
sort.

Author(s)

Reimers, D.; Wisotzki, L; Christlieb, N.

IVOA id

ivo://org.gavo.dc/hamburg_eso/q/ssa

Lyalpha emission in JADES, GLASS and CEERS gal.

2026-03-09T12:23:46Z

Description: We present the statistical properties of Ly{alpha} emission in 586 galaxies at z=4.5-14.2, observed by multiple JWST/NIRSpec spectroscopy projects, including the JADES, GLASS, CEERS, and GO/DDT programs. We obtain Ly{alpha} equivalent width (EW), Ly{alpha} escape fraction, and ionizing photon production efficiency measurements or upper limits for these galaxies, and confirm that the Lya-emitting galaxy fraction decreases toward higher redshifts. We derive Ly{alpha} luminosity functions from z~5 to z~10-14 with the observed Ly{alpha} EW distributions and galaxy UV luminosity functions, and find an ~3dex decrease in number density at L_Ly{alpha}_=10^42^-10^43^erg/s over the redshift range. Notably, this study presents the first constraints on the Ly{alpha} luminosity function at z~8-14. We obtain the neutral hydrogen fractions of x_HI_=0.17_-0.16_^+0.23^, 0.63_-0.28_^+0.18^, 0.79_-0.21_^+0.13^, and 0.88_-0.13_^+0.11^ at z~6, 7, 8-9, and 10-14, respectively, via comparisons of the reionization models developed by seminumerical simulations with 21cmFAST explaining the observations of Ly{alpha}, UV continuum, and Planck electron optical depth. The high x_HI_ values over z~7-14 suggest a late and sharp reionization, with the primary reionization process occurring at z~6-7. Such a late and sharp reionization is not easily explained by either a clumpy intergalactic medium or sources of reionization in a classical faint-galaxy or a bright-galaxy/active galactic nucleus (AGN) scenario, unless a very high escape fraction or AGN duty cycle is assumed at z~6-7.
Author(s): Kageura Y.; Ouchi M.; Nakane M.; Umeda H.; Harikane Y.; Yoshiura S.,Nakajima K.; Yajima H.; Thai T.T.
IVOA id: ivo://cds.vizier/j/apjs/278/33

Barium abundances from LAMOST MRS DR9 spectra

2026-03-09T12:08:36Z

Description: Based on a template-matching method, we estimate the barium (Ba) abundances for stellar spectra from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Medium-Resolution Spectroscopic Survey (MRS). The Ba abundances of 198,011 stars have been determined from MRS spectra with signal-to-noise ratios (S/N)>40 combined with the stellar atmospheric parameters from the LAMOST Low-Resolution Spectroscopic Survey DR9 by the LAMOST Stellar Parameter Pipeline. The uncertainties in the Ba abundances from the LAMOST MRS spectra are less than 0.3 dex when S/N exceeds 40, which align closely with the results based on the high-resolution UVES spectra from the Gaia-ESO survey obtained by spectral synthesis. Further analysis of Ba abundances from repeated observations of the same stars reveals that random errors related to spectral quality remain below 0.3 dex at the same S/N, with a systematic overestimation for the low-S/N spectra. This extensive sample of stellar Ba abundances will enhance studies of the s-, i-, and r-processes, and deepen our understanding of the chemical-evolution history of the Milky Way.
Author(s): Chen T.-Y.; Shi J.-R.; Yan H.-L.; Beers T.C.; Li C.-Q.; Ding M.-Y.,Xie X.-J.; Shuai L.; Zhou Z.; Tang Y.-J.
IVOA id: ivo://cds.vizier/j/apjs/278/23

Star clusters in M31 from PAndAS and deep learning

2026-03-09T11:56:43Z

Description: The identification of star clusters holds significant importance in studying galaxy formation and evolution history. However, the task of swiftly and accurately identifying star clusters from vast amounts of photometric images presents an immense challenge. To address these difficulties, we employ deep learning models for image classification to identify young disk star clusters in M31 from the Pan-Andromeda Archaeological Survey (PAndAS) images. For training, validation, and testing, we utilize the Panchromatic Hubble Andromeda Treasury survey catalogs. We evaluate the performance of various deep learning models, using different classification thresholds and limiting magnitudes. Our findings indicate that the ResNet-50 model exhibits the highest overall accuracy. Moreover, using brighter limiting magnitudes and increasing the classification thresholds can effectively enhance the accuracy and precision of cluster identification. Through our experiments, we found that the model achieves optimal performance when the limiting magnitude is set to brighter than 21 mag. Based on this, we constructed a training data set with magnitudes less than 21 mag and trained a second ResNet-50 model. This model achieved a purity of 89.30%, a recall of 73.55%, and an F1 score of 80.66% when the classification threshold was set to 0.669. Applying the second model to all sources in the PAndAS fields within a projected radius of 30 kpc from the center of M31, we identified 2228 new unique star cluster candidates. We conducted visual inspections to validate the results produced by our automated methods, and we ultimately obtained 1057 star cluster candidates, of which 745 are newly identified.
Author(s): Zhang B.; Chen B.; Yuan H.; Chen P.; Wang S.; Zhang L.; Ren Yi; Guo H.
IVOA id: ivo://cds.vizier/j/apjs/278/16

OGLE OCVS lightcurve points

2026-03-09T10:10:10Z

Description

This form allows the selection of Lightcurve points for the entire
OGLE Varibale Star Collection.

Author(s)

IVOA id

ivo://astro.upjs/ogle/lc/lc-web

OGLE objects Cone Search

2026-03-09T09:49:14Z

Description

This table is a unified catalogue of objects from the OGLE Collection of Variable Stars (OCVS) (https://www.astrouw.edu.pl/ogle/ogle4/OCVS).
It was constructed by merging variable-type–specific ident.dat tables with selected columns from tables containing parameters: cep.dat, cepF.dat, cep1O.dat, cepF1O.dat, cep1O2O.dat, cep1O2O3O.dat, cep2O3O.dat, Miras.dat, and others.

The corresponding light curves can be discovered via TAP through the ts_ssa or obscore tables, or through the SSA service. Light curves can be extracted using the associated DataLink services.

Author(s)

IVOA id

ivo://astro.upjs/ogle/o/ogle-objects

12CO gas structures of protoplanetary disks

2026-03-09T09:25:40Z

Description: We present measurements of key protoplanetary disk properties inferred from parametric models of ALMA ^12^CO spectral line visibilities. We derived gas-disk radii, integrated fluxes, optically thick emission layers, and brightness temperature profiles for the disk population of the old (4-14Myr) Upper Scorpius star-forming region. We measured CO emission sizes for 37 disks with bright CO J=3-2 emission (S/N>10 on the integrated flux; out of the 83 disks with CO detections), finding that the median radius containing 90% of the flux is ~82au, with radii spanning from 22 up to 247au. We report a correlation between the ^12^CO brightness temperatures and stellar luminosities, with a Pearson coefficient of 0.6, which we used to prove that the ^12^CO optically thick emission layer primarily emanates from a region below the superheated dust, which is optically thin to the stellar irradiation. Moreover, we derive 33 CO emission-surface height profiles, finding a median aspect ratio of <z/r>~0.16 in a range from ~0.01 up to ~0.45 over the sample. Finally, we comment on the multiple systems in our sample, of which only some were already known. These results confirm that it is possible to derive bulk disk properties by modeling moderate-angular-resolution ALMA visibilities.
Author(s): Zallio L.; Rosotti G.P.; Vioque M.; Miotello A.; Andrews S.M.; Manara C.F.,Carpenter J.M.; Empey A.; Kurtovic N.T.; Law C.J.; Longarini C.,Paneque-carreno T.; Teague R.; Villenave M.; Yen H.-W.; Zagaria F.
IVOA id: ivo://cds.vizier/j/a+a/705/a49

Massive stars in the Milky Way

2026-03-09T09:19:51Z

Description: Massive stars play a significant role in different branches of astronomy, from shaping the processes of star and planet formation to influencing the evolution and chemical enrichment of the distant universe. Despite their high astrophysical significance, these objects are rare and difficult to detect. With Gaia's advent, we now possess extensive kinematic and photometric data for a significant portion of the Galaxy that can unveil, among others, new populations of massive star candidates. In order to produce bonafide bright (G magnitude <12) massive-star candidate lists (threshold set to spectral type B2 or earlier but with slight changes in this threshold also explored) in the Milky Way subject to be followed up by future massive spectroscopic surveys, we developed a Gaia DR3 plus literature data based methodology. We trained a balanced random forest (BRF) with the spectral types from the Skiff compilation as labels. Our approach yields a completeness of ~80% and a purity ranging from 0.51+/-0.02 for probabilities between 0.6 and 0.7, up to 0.85+/-0.05 for the 0.9-1.0 range. To externally validate our methodology, we searched for and analyzed archival spectra of moderate- to high-probability (p>0.6) candidates that are not contained in our catalog of labels. Our independent spectral validation confirms the expected performance of the BRF, spectroscopically classifying 300 stars as B3 or earlier (due to observational constraints imposed on the B0-3 range), including 107 new stars. Based on the most conservative yields of our methodology, our candidate list could increase the number of bright massive stars by ~50%. As a byproduct, we developed an automatic methodology for spectral typing optimized for LAMOST spectra, based on line detection and characterization that guides a decision path.
Author(s): Monsalves N.; Bayo A.; Jaque Arancibia M.; Bodensteiner J.,Guerrero Caneppa A.; Sanchez-Saez P.; Angeloni R.
IVOA id: ivo://cds.vizier/j/a+a/704/a155

Kolonica images

2026-03-09T08:49:09Z

Description

The images in this collection were acquired to monitor selected sky
fields around eclipsing binary stars at the Kolonica Observatory,
Slovakia.

Author(s)

UPJŠ

IVOA id

ivo://astro.upjs/upjs_img/i/i

4LAC FSRQs & BL Lac objects energy distributions

2026-03-09T08:36:29Z

Description: A sample of 312 low-frequency-peaked BL Lacertae objects (LBLs) and 694 flat-spectrum radio quasars (FSRQs) with the parameters of both redshift and gamma-ray photon spectral index ({Gamma}_{gamma}_) is compiled from the Fourth Catalog of Active Galactic Nuclei Data Release 2 from the Fermi Large Area Telescope (LAT). The multiwavelength data of the sample sources are downloaded from the Space Science Data Center, and then matched to the corresponding gamma-ray data from the Fermi-LAT Fourth Source Catalog DR2. The synchrotron radiation peak frequency and Compton dominance (CD) parameters of the sources are obtained by using a log-parabolic model to fit the average-state multiwavelength spectral energy distribution. A support vector machine in the logL_{gamma}_-{Gamma}_{gamma}_ frame is utilized to delineate the optimal boundary between FSRQs and LBL sources. The 1{sigma} position of the Gaussian fitting on the histograms of the {Gamma}_{gamma}_, log{nu}_peak_^syn^, and CD parameter distributions are also introduced. With this criterion, 25 FSRQ candidates are selected from LBL sample sources. The optical spectral identification result confirms that 8 out of 13 candidate sources available with the optical spectral data exhibit the relationship of EW>5{AA}.
Author(s): Liang S.; Yang W.G.; Zheng Y.G.; Kang S.J.
IVOA id: ivo://cds.vizier/j/apjs/278/11

Discovery of bright z~=7 LBGs in Euclid COSMOS

2026-03-09T08:32:59Z

Description: We present a search for z ~= 7 Lyman-break galaxies using the 1.72 deg^2^ near-infrared UltraVISTA survey in the COSMOS field, reaching 5 {sigma} depths in Y of 26.2. We incorporate deep Euclid optical and Euclid + Spitzer NIR imaging for a full spectral energy distribution (SED) fitting analysis. We find 289 candidate galaxies at 6.5 <= z <= 7.5 covering -22.6 <= MUV <= -20.2, faint enough to overlap with Hubble Space Telescope studies. We conduct a separate selection by including complementary Euclid performance verification imaging (reaching 5 {sigma} depths of 26.3), yielding 140 galaxies in 0.65 deg^2^, with 38 sources unique to this sample. We compute the rest-frame UV luminosity function (UV LF) from our samples, extending below the knee (M*=-21.14). We find that the shape of the UV LF is consistent with both a Schechter function and double-power law (DPL) at the magnitudes probed by this sample, with a DPL preferred at MUV < -22.5 when bright-end results are included. The UltraVISTA+Euclid sample provides a clean measurement of the LF due to the overlapping near-infrared filters identifying molecular absorption features in the SEDs of ultra-cool dwarf interlopers, and a dditional faint galaxies are recovered. A comparison with JWST LFs at z > 7 suggests a gentle evolution in the bright-end slope, although this is limited by a lack of robust bright-end measurements at z > 9. We forecast that in the Euclid Deep Fields, the removal of contaminant ultra-cool dwarfs as point sources will be possible at JE < 24.5. Finally, we present a high-equivalent-width Lyman-{alpha} emitter candidate identified by combining HSC, VISTA, and Euclid broadband photometry, highlighting the synergistic power t hese instruments will have in the Euclid Auxiliary Fields for identifying extreme sources in the Epoch of Reionisation.
Author(s): Varadaraj R.G.; Bowler R.A.A.; Jarvis M.J.; Weaver J.R.; Banados E.,Holloway P.; Caputi K.I.; Wilkins S.M.; Yang D.; Milvang-Jensen B.,Gabarra L.; Oesch P.A.; Amara A.; Andreon S.; Auricchio N.; Baccigalupi C.,Baldi M.; Bardelli S.; Biviano A.; Branchini E.; Brescia M.; Camera S.,Canas-Herrera G.; Capobianco V.; Carbone C.; Carretero J.; Castellano M.,Castignani G.; Cavuoti S.; Chambers K.C.; Cimatti A.; Colodro-Conde C.,Congedo G.; Conselice C.J.; Conversi L.; Copin Y.; Courbin F.,Courtois H.M.; Cropper M.; Da Silva A.; Degaudenzi H.; De Lucia G.; Dole H.,Dubath F.; Duncan C.A.J.; Dupac X.; Dusini S.; Escoffier S.; Farina M.,Farinelli R.; Faustini F.; Ferriol S.; Finelli F.; Fosalba P.,Fourmanoit N.; Frailis M.; Franceschi E.; Fumana M.; Galeotta S.; George K.,Gillis B.; Giocoli C.; Gracia-Carpio J.; Grazian A.; Grupp F.; Guzzo L.,Haugan S.V.H.; Hoar J.; Hoekstra H.; Holmes W.; Hook I.M.; Hormuth F.,Hornstrup A.; Jahnke K.; Jhabvala M.; Joachimi B.; Keihanen E.; Kermiche S.,Kiessling A.; Kilbinger M.; Kubik B.; Kummel M.; Kunz M.; Kurki-Suonio H.,Le Brun A.M.C.; Ligori S.; Lilje P.B.; Lindholm V.; Lloro I.; Mainetti G.,Maino D.; Maiorano E.; Mansutti O.; Marggraf O.; Martinelli M.; Martinet N.,Marulli F.; Massey R.J.; Medinaceli E.; Mei S.; Melchior M.; Mellier Y.,Meneghetti M.; Merlin E.; Meylan G.; Mora A.; Moresco M.; Moscardini L.,Nakajima R.; Neissner C.; Niemi S.-M.; Padilla C.; Paltani S.; Pasian F.,Pedersen K.; Percival W.J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.,Popa L.A.; Pozzetti L.; Raison F.; Renzi A.; Rhodes J.; Riccio G.,Romelli E.; Roncarelli M.; Rossetti E.; Saglia R.; Sakr Z.; Sapone D.,Sartoris B.; Schirmer M.; Schneider P.; Schrabback T.; Secroun A.,Seidel G.; Serrano S.; Simon P.; Sirignano C.; Sirri G.; Stanco L.,Starck J.-L.; Steinwagner J.; Tallada-Crespi P.; Taylor A.N.; Teplitz H.I.,Tereno I.; Tessore N.; Toft S.; Toledo-Moreo R.; Torradeflot F.,Tutusaus I.; Valenziano L.; Valiviita J.; Vassallo T.; Veropalumbo A.,Wang Y.; Weller J.; Zamorani G.; Zerbi F.M.; Zucca E.; Martin-Fleitas J.,Scottez V.; Viel M.
IVOA id: ivo://cds.vizier/j/a+a/707/a239

5 AGNs soft excess and X-ray continuum

2026-03-09T08:26:29Z

Description: Changing-state active galactic nuclei (CSAGNs) exhibit rapid variability, with mass accretion rates that can change by several orders of magnitude in a few years. This provides us with a unique opportunity to study the evolution of the inner accretion flow almost in real time. Here, we used over 1000 observations to study the broadband X-ray spectra of a sample of five CSAGNs, spanning three orders of magnitude in Eddington ratio ({lambda}_Edd_), using phenomenological models to trace the evolution of key spectral components. We derive several fundamental parameters, such as the photon index, soft excess strength, reflection strength, and luminosities of the soft excess and primary continuum. We find that the soft excess and primary continuum emissions show a very strong positive correlation (p<<10^-10^), suggesting a common physical origin. The soft excess strength does not show any dependency on the reflection parameter, suggesting that in these objects the soft excess is not dominated by a blurred ionized reflection process. On the other hand, the strength of the soft excess is found to be strongly positively correlated with the Eddington ratio (p<<10^-10^), and we find that the soft excess vanishes below log {lambda}Edd~-2.5. Moreover, we find a clear 'V'-shaped relation for {Gamma}-{lambda}Edd, with a break at log{lambda}Edd=-2.47+/-0.09. Our findings indicate a change in the geometry of the inner accretion flow at low Eddington ratios, and that the soft excess is primarily produced via warm Comptonization.
Author(s): Jana A.; Ricci C.; Tortosa A.; Dimopoulos G.; Trakhtenbrot B.; Bauer F.E.,Temple M.; Koss M.; Gupta K.K.; Chang H.-K.; Diaz Y.; Illic Y.; Kallova K.,Shablovinskaya E.
IVOA id: ivo://cds.vizier/j/a+a/707/a213

TOI-3288 A b and TOI-4666 b light and RV curves

2026-03-09T08:20:34Z

Description: Gas giant planets orbiting low-mass stars (Teff<=4600K) are uncommon outcomes of planet formation. Increasing the sample of well-characterised giants around early M dwarfs will enable population-level studies of their properties, offering valuable insights into their formation and evolutionary histories. We aim to confirm and characterise giant exoplanets transiting M dwarfs identified by the TESS mission. To this end, we have started the Gas giAnts Transiting lOw-mass Stars (GATOS) program within the NIRPS Guaranteed Time Observations (GTO). High-resolution spectroscopic data are obtained in the optical and near-infrared (nIR), combining HARPS and NIRPS. We derive radial velocities (RVs) via the cross-correlation function and implement a novel post-processing procedure to further mitigate telluric contamination in the nIR. The resulting RVs are jointly fit with TESS and ground-based photometry to derive the orbital and physical parameters of the systems. We present the GATOS program and its first results. We confirm two gas giants transiting the low-mass stars TOI-3288 A (K9V, Teff=3933+/-48K) and TOI-4666 (M2.5V, Teff=3512+/-36K). TOI-3288 A hosts a hot Jupiter with a mass of 2.11+/-0.08M_Jup_ and a radius of 1.00+/-0.03R_Jup_, with an orbital period of 1.43 days (Teq=1059+/-20K). TOI-4666 hosts a 0.70+/-0.06M_Jup_ warm Jupiter (Teq=713+/-14K) with a radius of 1.11+/-0.04R_Jup_, with an orbital period of 2.91 days. At a population level, we identify a decrease in planetary mass with spectral type, where late M dwarfs host less massive giant planets than early M dwarfs. More massive gas giants that deviate from this trend are preferentially hosted by more metal-rich stars. Furthermore, we find an increased binarity fraction among low-mass stars hosting gas giants, which may play a role in enhancing giant planet formation around low-mass stars. These mass characterizations contribute to the growing catalogue of well-defined giant exoplanets around low-mass stars. The observed population trends agree with theoretical predictions, where higher metallicity can compensate for lower disk masses, and wide binary systems may influence planet formation and migration through Kozai-Lidov cycles or disk instabilities.
Author(s): Frensch Y.G.C.; Bouchy F.; Lo Curto G.; L'Heureux A.; de Lima Gomes R.,Faria J.; Dumusque X.; Malo L.; Cointepas M.; Srivastava A.; Bonfils X.,Delgado-Mena E.; Nari N.; Artigau E.; Baron F.; Barros S.C.C.; Benneke B.,Bryan M.; Canto Martins B.L.; de Castro Leao I.; Cloutier R.; Cook N.J.,Cowan N.B.; Cristo E.; De Medeiros J.R.; Delfosse X.; Doyon R.,Ehrenreich D.; Gonzalez Hernandez J.I.; Lafreniere D.; Lovis C.; Melo C.,Mignon L.; Mordasini C.; Pepe F.; Rebolo R.; Rowe J.; Santos N.C.,Segransan D.; Suarez Mascareno A.; Udry S.; Valencia D.; Wade G.,Al Moulla K.; Allart R.; Almenara J.M.; Barkaoui K.; Cadieux C.,Castro-Gonzalez A.; Collins K.A.; Fajardo-Acosta S.B.; Forveille T.; Gan T.,Gomes da Silva J.; Grieves N.; Hobson M.J.; Howell S.; Lamontagne P.,Messamah L.; Nielsen L.D.; Osborn A.; Parc L.; Piaulet-Ghorayeb C.,Stassun K.G.; Stefanov A.K.; Striegel S.; Ulmer-Moll S.; Vaulato V.,Watkins C.N.
IVOA id: ivo://cds.vizier/j/a+a/707/a73

AGN multiwavelength SED in POX 52

2026-03-09T08:10:18Z

Description: The nearby dwarf galaxy POX 52 at z=0.021 hosts an active galactic nucleus (AGN) with a black hole (BH) mass of M_BH_~10^5-6^M_{sun}_ and an Eddington ratio of ~0.1-1. This object provides the rare opportunity to study both AGN and host-galaxy properties in a low-mass highly accreting system. To do so, we collected its multiwavelength data from X-ray to radio. First, we construct a spectral energy distribution, and by fitting it with AGN and host-galaxy components, we constrain AGN-disk and dust-torus components. Then, while considering the AGN-disk emission, we decompose optical Hubble Space Telescope images. As a result, it is found that a classical bulge component is probably present, and its mass (M_bulge_) is consistent with an expected value from a local relation. Lastly, we analyze new quasi-simultaneous X-ray (0.2-30keV) data obtained by the Nuclear Spectroscopic Telescope Array and XMM-Newton. The X-ray spectrum can be reproduced by multicolor blackbody, warm and hot coronae, and disk and torus reflection components. Based on this, the spin is estimated to be a_spin_=0.998-0.814, which could suggest that most of the current BH mass was achieved by prolonged mass accretion. Given the presence of the bulge, POX 52 would have undergone a galaxy merger, while the M_BH_-M_bulge_ relation and the inferred prolonged accretion could suggest that AGN feedback occurred. Regarding the AGN structure, the spectral slope of the hot corona, its relative strength to the bolometric emission, and the torus structure are found to be consistent with Eddington-ratio dependencies found for nearby AGNs.
Author(s): Kawamuro T.; Ricci C.; Yamada S.; Noda H.; Li R.; Temple M.J.; Tortosa A.
IVOA id: ivo://cds.vizier/j/apj/960/15

Colours from low-z LS DR9 galaxies

2026-03-07T00:00:00Z

Description: Radial colour gradients within galaxies arise from gradients of stellar age, metallicity, and dust reddening. Large samples of colour gradients from wide- area imaging surveys can complement smaller integral-field spectroscopy data sets and can be used to constrain galaxy formation models. Here, we measure colour gradients for low-redshift galaxies (z < 0.1) using photometry from the DESI Legacy Imaging Survey DR9. Our sample comprises ~93000 galaxies with spectroscopic redshifts and ~574000 galaxies with photometric redshifts. We focus on gradients across a radial range 0.5R_eff_ to R_eff_, which corresponds to the inner disc of typical late-type systems at low redshift. This region has been the focus of previous statistical studies of colour gradients and has recently been explored by spectroscopic surveys such as MaNGA. We find that the colour gradients of most galaxies in our sample are negative (redder towards the centre), consistent with the literature. We investigate empirical relationships between colour gradient, average g-r and r-z colour, Mr, M*, and sSFR. Trends of gradient strength with M_r_ (M*) show an inflection around Mr~-21(log_10_M*/M_{Sun}_ ~10.5). Below this mass, colour gradients become steeper with increasing M*, whereas colour gradients in more massive galaxies become shallower. We find that positive gradients (bluer stars at smaller radii) are typical for galaxies of M_*_~10^8^M_{Sun}_. We compare our results to age and metallicity gradients in two data sets derived from fits of different stellar population libraries to MaNGA spectra, but find no clear consensus explanation for the trends we observe. Both MaNGA data sets seem to imply a significant contribution from dust reddening, in particular, to explain the flatness of colour gradients along the red sequence.
Author(s): Liao L.-W.; Cooper A.P.
IVOA id: ivo://cds.vizier/j/mnras/518/3999

ALMACAL IX calibrators for DSFGs/SMGs sources

2026-03-07T00:00:00Z

Description: Wide, deep, blind continuum surveys at submillimetre/millimetre (submm/mm) wavelengths are required to provide a full inventory of the dusty, distant Universe. However, conducting such surveys to the necessary depth, with sub-arcsec angular resolution, is prohibitively time-consuming, even for the most advanced submm/mm telescopes. Here, we report the most recent results from the ALMACAL project, which exploits the 'free' calibration data from the Atacama Large Millimetre/submillimetre Array (ALMA) to map the lines of sight towards and beyond the ALMA calibrators. ALMACAL has now covered 1001 calibrators, with a total sky coverage around 0.3 deg^2^, distributed across the sky accessible from the Atacama desert, and has accumulated more than 1000 h of integration. The depth reached by combining multiple visits to each field makes ALMACAL capable of searching for faint, dusty, star-forming galaxies (DSFGs), with detections at multiple frequencies to constrain the emission mechanism. Based on the most up- to-date ALMACAL data base, we report the detection of 186 DSFGs with flux densities down to S_870{mu}m_ ~ 0.2 mJy, comparable with existing ALMA large surveys but less susceptible to cosmic variance. We report the number counts at five wavelengths between 870 {mu}m and 3 mm, in ALMA bands 3, 4, 5, 6, and 7, providing a benchmark for models of galaxy formation and evolution. By integrating the observed number counts and the best-fitting functions, we also present the resolved fraction of the cosmic infrared background (CIB) and the CIB spectral shape. Combining existing surveys, ALMA has currently resolved about half of the CIB in the submm/mm regime.
Author(s): Chen J.; Ivison R.J.; Zwaan M.A.; Smail I.; Klitsch A.; Peroux C.,Popping G.; Biggs A.D.; Szakacs R.; Hamanowicz A.; Lagos C.
IVOA id: ivo://cds.vizier/j/mnras/518/1378