VO Fresh

Gaia EB classification Cone Search

2026-06-03T16:20:45Z

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

Morphological classification of eclipsing binaries from the Gaia

2026-06-03T16:20:45Z

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

MAST GALEX GR6/7 Color Composition HiPS Survey

2026-06-02T15:05:44Z

Description

This is MAST's HiPS survey service for GALEX GR6/7 - Color composition.
HiPS is a hierarchical scheme for the description, storage, and access of sky survey data.

The Galaxy Evolution Explorer (GALEX) satellite is a NASA mission led by the California Institute of Technology to investigate how star formation in galaxies evolved from the early Universe up to the present. GALEX uses microchannel plate detectors to obtain direct images in the near-UV (NUV) and far-UV (FUV) and a grism to disperse light for low resolution spectroscopy. From its launch into low-Earth orbit on April 28, 2003 the GALEX NUV camera operated almost continuously. The Project suspended operations of the FUV camera following an electrical overcurrent in May 2009. GALEX data products include a series of all sky surveys and deep sky surveys in the imaging mode, and partial surveys in the near and far UV spectroscopic modes. The principal imaging studies are the Nearby Galaxy Survey (NGS), Deep (DIS), Medium (MIS), and All Sky Imaging Surveys (AIS). During the course of the mission, the GALEX team have released data to the public through MAST at discrete times. The last complete release was the GR6 (late 2010 through mid 2011 for imaging supplements and the grism survey). A final release of GALEX data arrived in late 2012 at MAST. These included a number of redelivered GR6 data (additional visits and associated coadds from 2003 onwards), along with new tiles within GR7, which span approximately from Jan. 2010 through Feb. 2012

Author(s)

Space Telescope Science Institute Catalogs and Surveys Branch

IVOA id

ivo://archive.stsci.edu/hips/galex

MAST HiPS Server

2026-06-02T15:03:39Z

Description

This is MAST's HiPS survey list
HiPS is a hierarchical scheme for the description, storage, and access of sky survey data.

Author(s)

Space Telescope Science Institute Catalogs and Surveys Branch

IVOA id

ivo://archive.stsci.edu/hips

H.E.S.S. DL3 DR1 - Public Test Data Release 1

2026-06-02T11:51:22Z

Description

IVOA ObsCore HE extension description of event lists for observations
in the H.E.S.S. DL3 DR1.

Author(s)

H.E.S.S. collaboration

IVOA id

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

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

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

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

The Factory and the Beehive. V.

2026-05-29T15:58:44Z

Description: Low-mass (<~1.2M_{sun}_) main-sequence stars lose angular momentum over time, leading to a decrease in their magnetic activity. The details of this rotation-activity relation remain poorly understood, however. Using observations of members of the ~700Myr old Praesepe and Hyades open clusters, we aim to characterize the rotation-activity relation for different tracers of activity at this age. To complement published data, we obtained new optical spectra for 250 Praesepe stars, new X-ray detections for 10, and new rotation periods for 28. These numbers for Hyads are 131, 23, and 137, respectively. The latter increases the number of Hyads with periods by 50%. We used these data to measure the fractional H{alpha} and X-ray luminosities, LH{alpha}/Lbol and LX/Lbol, and to calculate Rossby numbers Ro. We found that at ~700Myr almost all M dwarfs exhibit H{alpha} emission, with binaries having the same overall color-H{alpha} equivalent width distribution as single stars. In the Ro-LH{alpha}/Lbol plane, unsaturated single stars follow a power law with index {beta}=-5.9{\pm}0.8 for Ro>0.3. In the Ro-LX/Lbol plane, we see evidence for supersaturation for single stars with Ro<~0.01, following a power law with index {beta}_sup_=0.5_-0.1_^+0.2^, supporting the hypothesis that the coronae of these stars are being centrifugally stripped. We found that the critical Ro value at which activity saturates is smaller for LX/Lbol than for LH{alpha}/Lbol. Finally, we observed an almost 1:1 relation between LH{alpha}/Lbol and LX/Lbol, suggesting that both the corona and the chromosphere experience similar magnetic heating.
Author(s): Nunez A.; Agueros M.A.; Curtis J.L.; Covey K.R.; Douglas S.T.; Chu S.R.,DeLaurentiis S.; Wang M.(.; Drake J.J.
IVOA id: ivo://cds.vizier/j/apj/962/12

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

Scylla+METAL combined photometry master catalog

2026-05-29T13:11:40Z

Description: By analyzing the spectral energy distributions (SEDs) of resolved stars in nearby galaxies, we can constrain their stellar properties and line-of-sight dust extinction. From the Scylla survey, we obtain ultraviolet to near-infrared photometry from Wide Field Camera 3 on board the Hubble Space Telescope for more than 1.5 million stars in the SMC and LMC. We use the Bayesian Extinction and Stellar Tool (BEAST) to analyze the multiband SEDs of these sources and characterize their initial masses, ages, metallicities, distances, and line-of-sight extinction properties (e.g., AV, RV). We apply quality cuts and perform validation simulations to construct a catalog of over 550000 stars with high-reliability SED fits, which we use to analyze the stellar content and extinction properties of the SMC and LMC. We detect stars with masses as low as 0.6M_{sun}_. BEAST stellar age distributions show a jump in observed stars around 6Gyr ago, which agrees with star formation histories. Extinctions (AV) in both galaxies follow a log-normal distribution. We compare AV with ancillary gas and dust tracers like HI, Halpha, and far-infrared (FIR) dust emission and find positive correlations on a field-by-field basis. We convert observed AV to predicted dust surface densities using the Draine et al. model and find AV-based dust surface densities are a factor of ~2.5 lower than observed FIR-based dust surface densities, a correction factor similar to other studies.
Author(s): Lindberg C.W.; Murray C.E.; Yanchulova Merica-Jones P.; Bot C.,Burhenne C.; Choi Y.; Clark C.J.R.; Cohen R.E.; Gilbert K.M.; Goldman S.R.,Gordon K.D.; Hirschauer A.S.; McQuinn K.B.W.; Roman-Duval J.C.,Sandstrom K.M.; Tarantino E.; Williams B.F.
IVOA id: ivo://cds.vizier/j/apj/982/33

CNN catalog of solar flares

2026-05-29T12:37:14Z

Description: A convolutional neural network (CNN) is used to construct a new catalog for solar flares based on high-resolution (1 s cadence) Geostationary Operational Environmental Satellites (GOES) soft X-ray data. The CNN is trained to identify flare rise episodes. From 2018 January 1 to 2025 August 22, the algorithm detects 111,580 flare candidates, compared with 14,612 events in the corresponding GOES catalog. For each candidate, the probability of being a true positive is quantified by Bayesian inference based on the peak flux, rise time, and temporal coincidence with cataloged events where available. The flare size and waiting-time distributions are studied and compared with the GOES catalog. The CNN catalog shows a steeper power-law index for raw peak fluxes (-2.59+/-0.02) than GOES (-2.25+/-0.04), indicating the CNN's higher sensitivity to small events. After background correction, the indices are -1.97+/-0.02 (CNN) and -2.05+/-0.04 (GOES). The CNN catalog extends the power-law distribution of flare peak fluxes by 1 order of magnitude at the small-flux end compared with the GOES background-subtracted catalog. A Bayesian block analysis of the waiting-time distributions from the GOES and CNN catalogs indicates broad consistency with a piecewise Poisson process. We find that previously reported correlations between flare sizes and waiting times are significantly influenced by obscuration, that is, undercounting weaker or overlapping flares during periods of elevated flux. The new CNN catalog provides a foundation for complete and consistent studies of solar flare statistics.
Author(s): Farhang N.; Wheatland M.S.; Melatos A.
IVOA id: ivo://cds.vizier/j/apjs/284/9

MeerKAT Massive Distant Clusters Survey

2026-05-29T08:09:21Z

Description: We present MeerKAT L-band (central frequency 1.284GHz) observations of a sample of 30 of the most massive Sunyaev-Zel'dovich selected galaxy clusters at z>1 from the ACT DR5 catalogue, providing the first statistical constraints on cluster-scale diffuse radio emission beyond this redshift. Diffuse radio halos are detected in eight clusters (27%), while 21 systems (70%) show no central diffuse emission down to some of the deepest upper limits yet obtained at these redshifts; one additional target is excluded because of poor data quality. The detected halos lie along the established P_1.4GHz_-M_500_ scaling relation measured at low redshift, whereas non-detections populate the lower envelope of the radio power-mass plane, broadly consistent with the known bimodality in this relation. No cluster-scale radio relics or mini-halos are identified in the sample. Mock halo injection simulations are used to derive 3{sigma} upper limits for 18 clusters, showing that a substantial fraction of the high-redshift population remains below current MeerKAT sensitivity at L-band.
Author(s): Phuravhathu D.G.; Hilton M.; Sikhosana S.P.; Klutse D.Y.; Knowles K.,van Marrewijk J.; Mroczkowski T.; Oozeer N.; Partridge B.; Perrott Y.C.,Sifon C.; Sureshkumar U.
IVOA id: ivo://cds.vizier/j/mnras/549/g879

SMASTES. I. KVN obs. SiO & H2O masers from AGB stars

2026-05-29T07:34:46Z

Description: Simultaneous observations of 19 H_2_O and SiO maser and thermal lines were performed toward 155 M-type oxygen-rich (O-rich) AGB stars. We used the upgraded four-band (22/43/86/129GHz) wide receiving system of the Korean VLBI Network (KVN). The 155 O-rich stars composed of 50 semiregulars (SRs), 55 Miras, and 50 OH/IR stars were selected based on previous KVN H2O/SiO detected sources. Both H_2_O and SiO masers were detected in 23 stars among 50 SRs, 50 stars among 55 Miras, and 24 stars among 50 OH/IRs, respectively. Out of 50 SRs, H_2_O-only masers, without corresponding SiO maser detection, were observed in four stars. In contrast, no H_2_O-only masers were detected in any of the 55 Mira or 50 OH/IR stars, which differs from the pattern seen with SiO-only masers. Interestingly, in the 50 SRs, the SiO v=1, J=2-1 maser was detected more than the SiO v=1, J=1-0 maser despite requiring a higher excitation energy. The 28 SiO v=0, J=1-0, 2-1, 3-2 lines were detected more frequently at higher rotational transitions, especially in the SRs and Miras. The HCN and SiS were detected from 11 and 3 stars, respectively. For our observational results, we performed statistical analysis on the intensity ratio variations among H_2_O and various SiO masers, chemical environments, and wind kinematics. The characteristics of these property variations were investigated in the IRAS two-color diagram in relation to their evolutionary stages.
Author(s): Baek H.; Cho S.-H.; Kim J.; Son S.-M.; Yoon D.-H.; Suh K.-W.
IVOA id: ivo://cds.vizier/j/aj/170/84

Photometric observations of SN 2024iss

2026-05-29T06:59:59Z

Description: We present optical, ultraviolet, and X-ray observations of supernova (SN) 2024iss, a Type IIb SN that shows a prominent double-peaked light curve. We modeled the first peak with a semianalytical shock-cooling model and the X-ray emission with a free-free model. We also compare the envelope radius and mass-loss rate with those of other Type IIb SNe to explore the relationships between the progenitor envelope and the circumstellar material (CSM). The shock-cooling peak in the V-band light curve reached MV=-17.33+/-0.26mag, while the ^56^Ni-powered second peak attained MV=-17.43+/-0.26mag. Early spectra show an photospheric velocity of ~19400km/s at 3.82 days from the H{alpha} P Cygni profile. The Balmer lines persist at least +87 days after the explosion, characterizing hydrogen-rich ejecta. Modeling the first light-curve peak with the shock-cooling model suggests an extended hydrogen envelope with a mass of 0.11+/-0.04M_{sun}_ and a radius of 244+/-43R_{sun}_. Fitting the second light-curve peak with an Arnett-like model indicates a typical 56 Ni mass of 0.117+/-0.013M_{sun}_ and a relatively low ejecta mass of 1.272+/-0.343M_{sun}_. X-ray observations reveal bright thermal bremsstrahlung emission and indicate a mass-loss rate of 1.6x10^-5^M_{sun}_/yr, which is similar to that of SN 1993J. SN 2024iss occupies a transitional position between the two subclasses of extended (eIIb) and compact (cIIb) Type IIb SNe. Its envelope radius and pre-explosion mass-loss rate appear to be correlated, in agreement with theoretical predictions. The observational properties of SN 2024iss are compatible with a binary interaction scenario being the dominant mechanism for envelope stripping. Furthermore, the low column density of neutral hydrogen suggests a compact CSM with an outer radius of <~1.3x10^14^cm, indicating that the progenitor star experienced eruptive mass loss within ~4yr of its terminal explosion.
Author(s): Chen L.; Wang X.; Wu Q.; Andrews M.; Farah J.; Ochner P.; Reguitti A.,Filippenko A.V.; Brink T.G.; Zhang J.; Song C.; Liu J.; Sand D.J.,Albanese I.; Alexander K.D.; Andrews J.; Bostroem K.A.; Cai Y.-Z.,Christy C.; Esamdin A.; Farina A.; Franz N.; Howell D.A.; Hsu B.; Hu M.,Iskandar A.; Li L.; Li G.; Li D.; Li W.; Liu J.; Mao Y.; McCully C.; Mo J.,Newsome M.; Qi Ni Y.; Pastorello A.; Padilla Gonzalez E.; Pearson J.,Peng H.; Ransome C.; Shrestha M.; Smith N.; Subrayan B.; Terreran G.,Valerin G.; Vinko J.; Vasylyev S.S.; Wang L.; Wang Z.; Wang H.,Wheeler J.C.; Wynn K.; Xiang D.; Yan S.; Yuan W.; Zhang J.; Zheng W.,Zhang Y.
IVOA id: ivo://cds.vizier/j/a+a/710/a33

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

Contact binaries period-luminosity-metallicity

2026-05-28T14:29:54Z

Description: Binary stars ubiquitous throughout the Universe are important. Contact binaries (CBs) possessing period-luminosity (PL) relations could be adopted as distance tracers. The PL relations of CBs are influenced by metallicity abundance and color index, which are connected to both the radius and luminosity of stars. Here we propose fine relations of the period-luminosity-metallicity-color (PLZC) from the ultraviolet to infrared bands based on current surveys. The accuracy of the distance estimation is 6% and 8%, respectively, depending on the PLZC relations of the CBs in the infrared and optical bands of the collected data. PLZC models are still more accurate than PLC models in determining intrinsic luminosity, notwithstanding their limited improvement. Meanwhile, these relations based on synthetic photometry are also calibrated. On the basis of the synthetic photometry, a 6% accuracy of distance is estimated. The measured or synthetic data of PLZC or PLC relations in infrared bands comes first in the list of suggestions for distance estimations and is followed by the measured data of optical bands.
Author(s): Song L.-Y.; Tian Z.-J.
IVOA id: ivo://cds.vizier/j/apj/961/248

PDRs4ALL XX. Spectral stitching of MIRI cubes

2026-05-28T10:57:58Z

Description: The Mid-Infrared Instrument (MIRI) is the imager and spectrograph covering wavelengths from 4.9 to 27.9um onboard the James Webb Space Telescope (JWST). The MIRI Medium-Resolution Spectrometer (MRS) consists of four integral field units (IFU) and two wheels with three rotation settings producing four spectral channels and three spectral sub-channels. The twelve resulting spectral data cubes have different fields of view, spatial, and spectral resolutions. The wavelength range of each cube partially overlaps with the neighboring bands, and the overlap regions typically show flux mismatches which have to be corrected by spectral stitching methods. Stitching methods aim to produce a single data cube incorporating the data of the individual sub-channels, which requires matching the spatial resolution and the flux discrepancies. We present Haute Couture, a novel stitching algorithm which uses non-negative matrix factorization (NMF) to perform a matrix completion, where the available MRS data cubes are treated as twelve sub-matrices of a larger incomplete matrix. Prior to matrix completion, we also introduce a novel pre-processing to homogenize the global intensities of the twelve cubes. Our pre-processing consists in jointly optimizing a set of global scale parameters that maximize the fit between the cubes where spectral overlap occurs. We apply our novel stitching method to JWST data obtained as part of the PDRs4All observing program of the Orion Bar, and produce a uniform cube reconstructed with the best spatial resolution over the full range of wavelengths.
Author(s): Canin A.; Fevotte C.; Dobigeon N.; Van De Putte D.; Onaka T.; Berne O.
IVOA id: ivo://cds.vizier/j/a+a/710/a6

SED analysis of X-ray selected AGN in Stripe 82

2026-05-28T09:42:55Z

Description: We perform a systematic, multiwavelength spectral energy distribution (SED) analysis of X-ray detected active galactic nuclei (AGNs) at z=0.2-0.8 with Sloan Digital Sky Survey (SDSS) counterparts in the Stripe 82 region, consisting of 60 type 1 and 137 type 2 AGNs covering a 2-10keV luminosity range of 41.6<logLx<4.7. The latest CIGALE code, where dusty polar components are included, is employed. To obtain reliable host and AGN parameters in type 1 AGNs, we utilize the image-decomposed optical SEDs of host galaxies by Li et al. based on the Subaru Hyper-Suprime Cam images. The mean ratio of black hole masses (MBH) and stellar masses (Mstellar) of our X-ray detected type 1 AGN sample, log(M_BH_/M_stellar_)=-2.7\pm0.5, is close to the local relation between BH and stellar masses as reported by Li et al. for SDSS quasars. This ratio is slightly lower than that found for more luminous (logL_bol_>45) type 1 AGNs at z~1.5. This can be explained by the AGN luminosity dependence of log(M_BH_/M_stellar_), which little evolves with redshift. We confirm the trend that the UV-to-X-ray slope ({alpha}_OX_) or X-ray-to-bolometric correction factor ({kappa}_2-10_) increases with AGN luminosity or Eddington ratio. We find that type 1 and type 2 AGNs with the same luminosity ranges share similar host stellar mass distributions, whereas type 2s tend to show smaller AGN luminosities than type 1s. This supports the luminosity-dependent (or Eddington-ratio-dependent) unified scheme.
Author(s): Setoguchi K.; Ueda Y.; Toba Y.; Li J.; Silverman J.; Uematsu R.
IVOA id: ivo://cds.vizier/j/apj/961/246

LCs of KMT-2022-BLG-0086 with 2L2s & 3L1S models

2026-05-28T08:28:15Z

Description: We present the analysis of a microlensing event KMT-2022-BLG-0086 of which the overall light curve is not described by a binary-lens single-source (2L1S) model, which suggests the existence of an extra lens or an extra source. We found that the event is best explained by the binary-lens binary-source (2L2S) model, but the 2L2S model is only favored over the triple-lens single-source (3L1S) model by {Delta}{chi}^2^~9. Although the event has noticeable anomalies around the peak of the light curve, they are not enough covered to constrain the angular Einstein radius {theta}_E_, thus we only measure the minimum angular Einstein radius {theta}_E,min_. From the Bayesian analysis, it is found that that the binary lens system is a binary star with masses of (m_1_,m_2_)=(0.46^+0.35^_-0.25_M_{sun}_,0.75^+0.67^_-0.55_M_{sun}_) at a distance of D_L_=5.87^+1.21^_-1.79_kpc, while the triple lens system is a brown dwarf or a massive giant planet in a low-mass binary-star system with masses of (m_1_,m_2_,m_3_)= (0.43^+0.41^_-0.35_M_{sun}_,0.056^+0.055^_-0.047_M_{sun}_, 20.84^+20.20^_-17.04_M_{sun}_), at a distance of D_L_=4.06^+1.39^_-3.28_kpc, indicating a disk lens system. The 2L2S model yields the relative lens-source proper motion of {mu}_rel_>=4.6mas/yr that is consistent with the Bayesian result, whereas the 3L1S model yields {mu}_rel_>=18.9mas/yr, which is more than three times larger than that of a typical disk object of ~6mas/yr and thus is not consistent with the Bayesian result. This suggests that the event is likely caused by the binary-lens binary-source model.
Author(s): Chung S.-J.; Hwang K.-H.; Yee J.C.; Gould A.; Bond I.A.; Yang H.,(the Leading Authors); Albrow M.D.; Jung Y.K.; Han C.; Ryu Y.-H.,Shin I.-G.; Shvartzvald Y.; Zang W.; Cha S.-M.; Kim D.-J.; Kim S.-L.,Lee C.-U.; Lee D.-J.; Lee Y.; Park B.-G.; Pogge R.W.,(the Kmtnet Collaboration); Abe F.; Bennett D.P.; Bhattacharya A.,Fukui A.; Hamada R.; Hirao Y.; Ishitani Silva S.; Koshimoto N.,Miyazaki S.; Muraki Y.; Nagai T.; Nunota K.; Olmschenk G.; Ranc C.,Rattenbury N.J.; Satoh Y.; Sumi T.; Suzuki D.; Terry S.K.; Tristram P.J.,Vandorou A.; Yama H.; (the Moa Collaboration)
IVOA id: ivo://cds.vizier/j/aj/170/75

Red giant branch stars in M30 and M92

2026-05-28T08:16:51Z

Description: We perform a comparative study of the ex situ second-parameter pair globular clusters (GCs) M30 and M92, having similar metallicities but different horizontal branch morphologies. We obtain similar mean primordial carbon abundances for both clusters. However, M92 shows a large dispersion in carbon due to a more extended C-N anticorrelation, while M30 exhibits a higher primordial nitrogen abundance, suggesting that they have different chemical enrichment histories. Our new results confirm our previous result that M92 is a metal-complex GC showing a bimodal metallicity distribution. We also find that the metal-rich group of stars in M92 shows a helium enhancement as large as {Delta}Y~0.05 from the red giant branch bump V magnitudes, which can also be supported by (i) a lack of bright red giant branch stars, (ii) synthetic evolutionary horizontal branch population models and (iii) the more extended spatial distribution due to different degree of the diffusion process from their lower masses. We reinterpret the [Eu/Fe] measurements by others, finding that the two metallicity groups of stars in M92 have significantly different [Eu/Fe] abundances with small scatters. This strongly suggests that they formed independently out of well-mixed interstellar media in different environments. We suggest that M92 is a more complex system than a normal GC, most likely a merger remnant of two GCs or an even more complex system. In the Appendix, we address the problems with the recently developed color-temperature relations and the usage of broadband photometry in the populational taggings.
Author(s): Lee J.-W.
IVOA id: ivo://cds.vizier/j/apj/961/227

Study of dipolar magnetic field for 2673 stars

2026-05-28T08:10:32Z

Description: During the last two decades, thousands of stellar magnetic fields have been measured using the Zeeman-Doppler imaging method. No unified database gathers all measurements in an homogeneous way. The magnetic field of a star is a key ingredient of its plasma interactions with companions, either other stars or exoplanets, and of its radio and X-ray emissions. The dipolar component of a star's magnetic field, in particular, allows one to estimate the magnetic (Poynting) flux carried away by the stellar wind, that sweeps across exoplanets or their magnetospheres and is believed to drive electron acceleration and radio emissions. Here we aim at building a database of known stellar magnetic fields, inferring the dipolar component of the field, and we present the methods that we have developed to estimate a star's magnetic field when no measurement is available. We have compiled published Zeeman-Doppler measurements of stellar magnetic fields into a database, showing how to extract the dipolar component from various measurements. We have included several other stellar parameters in the database (mass, radius, rotation period, effective temperature, age, V-band magnitude). Then we have built and compared two extrapolation methods to infer stellar magnetic fields from the other stellar parameters: a K-Nearest Neighbors method and a neural network trained on the database. We present a database of over 2600 stars with an estimate of their dipolar magnetic field, and methods to predict such a parameter for other stars where it is not measured, to much better than an order of magnitude.
Author(s): Duchene N.; Girard J.N.; Zarka P.
IVOA id: ivo://cds.vizier/j/a+a/710/a16

Multiple images of Abell 2744 from JWST

2026-05-28T07:57:17Z

Description: We present a new high-resolution free-form mass model of A2744 that combines both weak-lensing (WL) and strong-lensing (SL) data sets from JWST. The SL data set comprises 286 multiple images, presenting the most extensive SL constraint to date for a single cluster. The WL data set, employing photo-z selection, yields a source density of ~350arcmin^-2^, marking the densest WL constraint ever. The combined mass reconstruction enables the highest-resolution mass map of A2744 within the ~1.8Mpcx1.8Mpc reconstruction region to date, revealing an isosceles triangular structure with two legs of ~1Mpc and a base of ~0.6Mpc. Although our algorithm, which is called MAximum-entropy ReconStruction (MARS), is entirely blind to the cluster galaxy distribution, the resulting mass reconstruction traces the brightest cluster galaxies remarkably well. The five strongest mass peaks coincide with the five most luminous cluster galaxies within <~2". We do not detect any unusual mass peaks that are not traced by the cluster galaxies, unlike the findings in previous studies. Our mass model shows the smallest scatter of SL multiple images in both source (~0.05") and image (~0.1") planes, which is lower than in previous studies by a factor of ~4. Although MARS represents the mass field with an extremely large number of free parameters (~300000), it converges to a solution within a few hours because we use a deep-learning technique. We make our mass and magnification maps publicly available.
Author(s): Cha S.; HyeongHan K.; Scofield Z.P.; Joo H.; Jee M.J.
IVOA id: ivo://cds.vizier/j/apj/961/186

Missing pairs in open cluster catalogs

2026-05-28T07:56:04Z

Description: Open clusters (OCs) in our Galaxy can be found in pairs, possibly forming physical binaries, or in groups. These objects offer unique insights into the process of star formation and testify to the dynamical interactions at local and galactic scales. Therefore, building as complete a census as possible is a valuable endeavor. This work is aimed at identifying and characterizing new OC pair candidates that had been overlooked in previous studies. Two recent comprehensive catalogs were cross-matched to identify OCs in the first catalog that had been missing from the second one. From this list, counterparts in the second catalog were searched within a 3D distance of 50 pc. Candidate pairs were then selected by applying constraints on the tangential velocity (TV) difference. An orbital integration was performed to assess gravitational binding. The similarity in terms of the radial velocity (RV) and age was evaluated. We identified seven isolated binary cluster candidates, comprising two likely bound systems with stable orbits over 100 Myr; two pairs with a possible common origin but lacking RV confirmation; and three pairs with significant velocity discrepancies, suggesting they are unbound or in transitional states. We also identified six cluster group candidates, while refining the membership of known complexes such as UBC_672 and NGC_1977, and discovering a new group around FSR_0198. Notably, the UBC_392 group exhibits coherent proper motions but inconsistent RVs and large age spreads, indicating that it is not gravitationally bound. Additionally, we reconciled 15 clusters with discrepant nomenclature between the two catalogs. Multi-catalog integration combined with kinematic and dynamical validation is essential for establishing a complete census of Galactic cluster pairs. Our findings have effectively expanded the known binary cluster sample and provided refined targets for future studies.
Author(s): Hu Q.; Cai Y.; Soubiran C.; Dai Y.; Li Y.; Luo Y.; Qin M.
IVOA id: ivo://cds.vizier/j/a+a/710/a4

LTI-GRAVITY observations of Ton 599

2026-05-28T07:52:57Z

Description: Parsec-scale jets of blazars have so far been spatially resolved only in millimeter and submillimeter wavelengths, where very long baseline interferometry can be used to obtain milliarcsecond-scale images of the jets. We have attempted to spatially resolve the near-infrared emission in jet-dominated blazars for the first time. We used the VLTI-GRAVITY instrument to obtain milliarcsecond-scale near-infrared interferometric observations of a flaring blazar Ton 599. Additionally, we observed four non-flaring blazars using the GRAVITY-wide mode, where a nearby bright star is used as a fringe tracker. We modeled the squared visibilities of Ton 599 and found that they are incompatible with a single unresolved point source unless there is a significant amount of additional unknown coherence loss in the instrument. With the present data, we cannot distinguish between a model with an unresolved point source and extended emission or coherence loss and a model with a single Gaussian component. This suggests that we are seeing the unresolved or only partially resolved jet-base in near-infrared wavelengths. The wide-field mode of GRAVITY was challenging for the additional relatively faint targets, resulting in either non-detections or poor-quality data that could not be modeled. Our observations demonstrate that it is possible to detect the compact jet emission in blazars with near-infrared interferometry, suggesting that with the improved GRAVITY+ instrument it will be possible to spatially resolve and image the near-infrared emission of blazar jets.
Author(s): Hovatta T.; Lindfors E.; Korhonen H.; Kharb P.; Wittkowski M.; Labdon A.,Pursimo T.; Wiik K.
IVOA id: ivo://cds.vizier/j/a+a/710/a15

Sgr A* MeerKAT 2.79GHz light curve

2026-05-28T07:50:33Z

Description: The supermassive black hole Sagittarius A* (Sgr A*) exhibits temporal and spectral variability across the electromagnetic spectrum. However, variability at radio frequencies below ~5GHz for timescales shorter than a day remains largely unexplored. We investigate the variability of Sgr A* at 2.79GHz on short timescales (1-min), to probe an under-explored regime of its emission process. Through point-source model fitting in the uv-domain, we analyse the flux density variation of Sgr A* over an 8h observation. We detect flux variation on a few tens of minute timescale with a modulation index of 6.11%, a mean flux density of 827+/-0.1(stat)+/-33(sys)mJy, and a mean spectral slope of 0.08+/-0.03. Furthermore, we measure the slope of the structure function of the observed light curve as 0.81+/-0.05 with a characteristic timescale of about 120-min. Our study at low radio frequencies is a critical step toward constraining the physical mechanisms that drive Sgr A*'s variable emission and its spectral energy distribution. Our study suggests that variability at centimetre and millimetre wavelengths is likely more closely related than previously thought.
Author(s): Kaur K.; Rammala-Zitha I.; Basu A.; Witzel G.; Wielgus M.; Balakrishnan V.,Barr E.D.; Brunthaler A.; Buchner S.; Champion D.J.; Hoeft M.; Khan S.,Kloeckner H.-R.; Koenig C.; Kramer M.; Venkatraman Krishnan V.; Ma Y.K.,Mao S.A.; Padmanabh P.V.; Ranchod S.; Sridhar S.S.; Wagenveld J.D.,Wharton R.S.; Wucknitz O.
IVOA id: ivo://cds.vizier/j/a+a/710/l6

redMaPPer clusters with ident. substructure

2026-05-28T07:43:42Z

Description: Numerical simulations of hierarchical structure formation predict that galaxy clusters retain significant dark matter substructure, a signature of their ongoing assembly. This substructure is traced by both the spatial distribution of member galaxies and perturbations in the hot intracluster medium. Merging events significantly impact the thermodynamic state of clusters, introducing scatter in observable mass scaling relations and thereby affecting their use as precision cosmology probes. We statistically quantified the prevalence and properties of substructure in optical galaxy clusters and directly investigated its impact on X-ray morphology and scaling relations, leveraging new data from the DECaLS Legacy Survey and the SRG/eROSITA all-sky survey. We applied the hierarchical density-based clustering algorithm HDBSCAN to the redMaPPer galaxy cluster catalog to identify and characterize substructure from the probabilistic membership assignments. This provides a refined membership catalog and a classification of each cluster as containing substructure or not. We then cross-matched this sample with the eROSITA X-ray morphology catalog to correlate optical substructure with a comprehensive set of X-ray morphological parameters. Finally, we analyzed the scaling relation between X-ray luminosity and optical richness for clusters with and without substructure. Substructure is a common feature, present in approximately 40% of clusters; a quarter of the full sample exhibits a fractional contribution to richness in excess of 35%. We find a highly significant correlation between optical substructure and disturbed X-ray morphologies, a trend that is strongest for high-mass clusters. The clusters with substructure also drive a stronger redshift evolution in the scatter of the Lx-{lambda} relation. At low redshifts (z<0.2), they display a systematically higher X-ray luminosity at fixed richness compared to relaxed systems. We demonstrate that substructure identification with redMaPPer is viable and essential for enhancing the precision of cluster cosmology. We attribute the enhanced effect of mergers on X-ray properties at low redshifts to the increased density contrast of low-redshift cool cores and longer substructure survival times, which are possibly due to the suppression of disruptive mixing by effects such as magnetic draping. At lower cluster richness, a discordance between X-ray morphology and the merging state indicates a growing relative importance of active galactic nucleus feedback in governing X-ray morphology.
Author(s): Tuomainen R.; Finoguenov A.; Comparat J.; Doubrawa L.
IVOA id: ivo://cds.vizier/j/a+a/710/a57

New sample of low mass ratio contact binary systems

2026-05-28T07:40:28Z

Description: This study explores multiple aspects of W Ursae Majoris (W UMa) contact binary systems with low mass ratios. We provide empirical insights into their definition, structure, rotational stability, and parameter relations. We first examined the range of mass ratios that characterize these systems, and based on an analysis of 818 contact binaries, we established an empirical threshold of q~0.27 to identify systems with a low mass ratio. To investigate the rotational stability, we conducted a Monte Carlo analysis of the squared gyration radii (k1^2^ and k2^2^) and assessed the resulting spin-to-orbital angular momentum ratio (Jspin/Jorb). While k1 remains nearly constant, k2 and Jspin/Jorb decrease slightly with increasing mass ratio. This emphasizes the role of the secondary star's internal structure. Moreover, we compiled a dedicated sample of 115 contact binaries with a low mass ratio and estimated their absolute parameters using Gaia DR3 parallaxes. From this dataset, we derived empirical parameter relations for systems with a low mass ratio that provide a useful reference for future observational and theoretical studies. The resulting datasets and statistical summaries offer benchmarks for modeling, stability evaluation, and evolutionary studies of W UMa-type binaries with low mass ratios.
Author(s): Poro A.; Poggiani R.; Foroutanfar A.; Harzandjadidi R.; Kahali Poor N.,Alicavus F.
IVOA id: ivo://cds.vizier/j/a+a/710/a49

Vertical structure of protoplanetary disks

2026-05-28T07:36:25Z

Description: High-resolution imaging in scattered light has revealed complex morphologies in protoplanetary/circumstellar disks. Measuring their vertical height is key to understanding disk structure, evolution, and the properties of embedded dust. This work aims to develop a robust methodology for fitting elliptical shapes to scattered light images of protoplanetary disks in order to extract vertical height profiles of the dust scattering surface (tau=1) across a large and morphologically diverse disk sample. The dataset comprises 92 unique near-infrared polarimetric images of individual systems obtained with VLT/SPHERE. The goal is to identify trends in vertical structure across morphologies and test for correlations with stellar mass, age, and disk dust mass. Using the height profiles, this work also investigates the implications of the constrained height for the masses of potential embedded planets. A structure extraction and ellipse fitting (SEEF) algorithm, is implemented using edge detection and Gaussian fitting to locate the structure within protoplanetary disks. Fitting ellipses to the structure reveals spatial offsets from the centre of the ellipse and the star, interpreted as vertical height assuming circular ring geometry. Disk inclination, position angle (PA), and aspect ratio (h_tau_=1/r) are also derived. The SEEF algorithm obtained successful vertical height measurements for 92 unique disks, revealing variations in height profiles consistent with flared disk geometries. Analysis of the full sample shows that the vertical height profile cannot be confidently described by a single power-law relation. Subdivision of the sample by disk morphology revealed no strong correlations within most categories, with the exception of extended disks (r_outer_>=150au), which exhibited a strong correlation with a single power-law trend. Investigation into underlying disk properties revealed no correlation for its affect to the vertical height structure. This work presents a consistent methodology for measuring the vertical structure of circumstellar disks using ellipse fitting on scattered light images. While trends in height structure remain weakly correlated for the full sample and many disk morphologies, extended disks (r_outer_>=150au) stand out as the only subgroup showing a clear power-law flaring trend. The lack of a strong correlation across other morphologies and with system properties like stellar or dust mass suggests that either differing disk morphologies exhibit different vertical height profiles or that another, unidentified factor is influencing the disk flaring.
Author(s): Byrne J.; Ginski C.; van Capelleveen R.F.; Fitzgerald N.; Garufi A.,Coyne C.; Lawlor C.; McLachlan D.
IVOA id: ivo://cds.vizier/j/a+a/710/a38

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

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

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

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

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 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