VO Fresh

GSC 2143-1307 UBVRI(RI)c light curves

2026-10-07T11:14:45Z

Description: Newly discovered by us a new eclipsing short-period star with an elliptical orbit, GSC 2143-1307 (V=14.24m, P=1.85 days, e=0.12, B3 V + B5 V), turned out to be a young massive system with rapid apsidal rotation. The following absolute parameters - temperatures, masses, radii - were obtained for the first time: T1=18500+/-500K, M1=5.1+/-0.5M_{sun}_, R1=2.55+/-0.08R_{sun}_, T2=16200+/-500K, M2=4.2+/-0.4M_{sun}_, R2=2.23+/-0.08R_{sun}_. The apsidal period Paps=90.4+/-0.05 years is equal, within the error bars, to the theoretical value under synchronic conditions between orbital and axial rotations. The distance to the system is d=2.08kpc.
Author(s): Volkova A.S.; Volkov I.M.
IVOA id: ivo://cds.vizier/j/other/astbu/81.454

COMPASS II. Approach to data reduction

2026-10-07T09:11:24Z

Description: Studying the chemical composition of the warm gas surrounding embedded solar-type protostars is one of the areas for which the Atacama Large Millimeter/submillimeter Array (ALMA) is particularly well suited. Recently, the ALMA Large Program Complex Organic Molecules in Protostars with ALMA Spectral Surveys (COMPASS) carried out an observing campaign of a sample of 11 protostellar regions to investigate the chemical impact of their environments and evolutionary stages. The aim of this paper is to provide the observational and procedural information necessary for the community to understand the analysis presented in forthcoming scientific papers by the COMPASS collaboration, and to enable archival research using the data products provided by our team and the ALMA Science Archive. This paper describes the technical setup of the observations, and it outlines the data-processing pipeline and primary data products from this initiative. The Common Astronomy Software Applications (CASA) was used for initial calibration following the standard ALMA Pipeline, and then IMAGER was used for self-calibration and imaging. We describe post-processing done with Python to achieve favorable continuum subtraction, correct for the primary beam response, and extract spectra. We discuss our strategy for mitigating data challenges, including those related to data volume and continuum subtraction for spectral line analysis. The incorporation of IMAGER in our workflow was advantageous in terms of the computing efficiency which allowed us to benchmark several imaging parameters and techniques; we also demonstrate that the imaging outcomes using IMAGER or CASA are scientifically comparable. Numerous data products are generated for the program, including image cubes for the 36 spectral windows targeting each source, extracted spectra, and continuum images.
Author(s): Plunkett A.L.; Maret S.; Harsono D.; Jorgensen J.K.; Coutens A.,Drozdovskaya M.N.; Lee J.-E.; Belloche A.; Cruz-Saenz de Miera F.,van 't Hoff M.L.R.; Jeong J.-H.; Kim C.-H.; Kospal A.; Luetzen M.,McGuire B.A.; Nazari P.; Spezzano S.; Telkamp Z.; Yang Y.-L.; Yun H.-S.,Andreu A.; Bergner J.; Ferrer Asensio J.; Ligterink N.F.W.; Lin Y.,Liu S.-Y.; Marchand P.; Rao M.; Zeng S.
IVOA id: ivo://cds.vizier/j/a+a/714/a50

Ram-pressure stripping with crowd science

2026-10-06T11:30:58Z

Description: We present the first results of Fishing for Jellyfish Galaxies, a pilot citizen-science project using Zooniverse to identify galaxies undergoing ram-pressure stripping (RPS). Volunteers visually inspected colour images of late-type galaxies from the Dark Energy Camera Legacy Survey. The sample consisted of 49703 galaxies selected within 4xR_500_ of clusters and groups, restricted to those brighter than 19th magnitude in the g and r bands, and with a minimum half-light radius of 2 arc seconds, to aid classification. We detail our data processing, including debiasing classifications and optimising vote-fraction thresholds to maximise completeness and purity, calibrated against a ground-truth set of pre-labelled galaxies. Our final catalogue contains 6739 jellyfish candidates (6621 new), 5430 merger candidates, and 29729 undisturbed galaxies, with 3910 jellyfish exhibiting prominent tail-like morphologies. We find that the fraction of RPS candidates rises from ~10% in galaxy groups to ~20-30% in massive clusters, confirming the findings of previous studies carried out on smaller samples. For the subset of our RPS candidate sample with spectroscopic data, we measure a median cluster-centric velocity 53% higher than the general cluster population, consistent with galaxies in early stages of accretion into the cluster. They are also typically late-type blue galaxies with elevated star-formation rates, in agreement with expectations. These results demonstrate that citizen scientists can reliably identify galaxies that undergo environmental processes. We provide the initial release of 37 599 visually classified galaxies as a resource for future studies of galaxy transformation in clusters.
Author(s): Bellhouse C.; Jaffe Y.L.; Crossett J.P.; McGee S.L.; Quiroz I.; Dulcien C.,Smith R.; Poggianti B.M.; Vulcani B.; Sampaio V.; Werle A.; Tomicic N.,Mueller A.; Akerman N.; Ignesti A.; Khoram A.
IVOA id: ivo://cds.vizier/j/a+a/714/a141

The flash-ionised SN Ibn 2025kzr

2026-10-06T11:28:23Z

Description: Type Ibn supernovae (SNe) are a class of interacting SNe characterised by narrow helium lines in their spectra. We present an extensive observational dataset of the Type Ibn SN 2025kzr at 51 Mpc, including the discovery of a precursor outburst with a peak brightness of Mr~-13.6mag beginning ~55 days before explosion. Our photometry indicates the SN was discovered within the first day of explosion, and showing fast-rising, ultraviolet-bright emission peaking at Mr=-19.26+/-0.09mag and a peak blackbody temperature of T~29000K, consistent with shock breakout within a region of dense and confined circumstellar material (CSM). Our high-cadence spectroscopic dataset spanning 1.9-58.5 days post-explosion shows flash-ionised emission features during the first 10 days. In our SALT spectrum at 3.8 days we observe a pronounced blueshift of the HeII lines by 460 km/s compared to the HeI lines at zero velocity, while a Pickering-decrement analysis reveals a CSM that is fully hydrogen-free. The timing of the disappearance of the flash features combined with the CSM velocity of 1500 km/s imply a mass-loss event ~66 days before explosion, in close agreement with the timing of the precursor observed 55 days before explosion and strongly suggestive of a physical link. We derive a CSM mass of 0.03-1.7M_{sun}_ and a corresponding high mass-loss rate >~10^-1^M_{sun}_/yr. The precursor timescale and energetics suggest an extreme mass-loss event that might be explained by wave-driven mass loss during the late stages of nuclear burning, in particular the oxygen-burning phase. Overall, we favour a single massive Wolf-Rayet progenitor with M_ZAMS~30-40M_{sun}_ to explain SN 2025kzr, although a binary origin cannot be excluded.
Author(s): de Wet S.; Leloudas G.; Buckley D.A.H.; Erasmus N.; Groot P.J.,Zimmerman E.A.; Chen P.; Tampo Y.; Pursiainen M.; Killestein T.,Stoppa F.; Jaisawal G.K.; Gal-Yam A.; Maeda K.; Anderson J.; Chen T.-W.,Gromadzki M.; Gutierrez C.P.; Kankare E.; Muller-Bravo T.E.; Pessi T.,Smartt S.; Sollerman J.; Tartaglia L.; Young D.R.; Alarcon M.R.; Smith K.W.,Stevance H.F.; de Boer T.; Chambers K.; Lin C.-C.; Lowe T.B.; Minguez P.,Nicholl M.; Paek G.S.H.; Wainscoat R.J.
IVOA id: ivo://cds.vizier/j/a+a/714/a86

The PAU Survey: AGNs in galaxy pairs

2026-10-06T11:25:52Z

Description: Leveraging the high-precision photometric redshifts of the Physics of the Accelerating Universe Survey (PAUS), we investigate the connection between active galactic nuclei galaxies (AGNs) and galaxy pairs up to redshift ~1.0. We identify 16824 galaxy pairs with projected separations rp<100kpc and radial velocity differences DV<3500km/s. AGNs are selected by cross-matching PAUS galaxies with multi-wavelength AGNs catalogues, yielding 270 AGNs in pairs out of a parent sample of 8,880 AGNs in PAUS. We construct control samples of isolated AGNs, non-AGNs in pairs, and isolated non-AGNs matched in redshift, absolute magnitude and environment. Active galactic nuclei in pairs show progressively redder rest-frame colours with increasing redshift, particularly at redshifts z>=0.5, whereas isolated AGNs and non-AGNs in pairs show no significant colour evolution and stay at Mg-Mr~0.65. Pairs hosting AGNs are also preferentially morphologically disturbed interacting systems found at smaller projected separations and velocity offsets, consistent with more dynamically advanced interactions. These results provide evidence for a redshift-dependent link between galaxy interactions and AGNs activity, suggesting that interactions play an increasingly important role in triggering nuclear activity at intermediate redshifts. This study highlights the unique capability of PAUS to probe AGNs-galaxy interaction connections beyond the local Universe with unprecedented statistical power.
Author(s): Duplancic F.; Siudek M.; Navarro-Girones D.; Gonzalez E.J.; Rodriguez F.,Alonso S.; Daza-Perilla I.V.; Lambas D.G.; Gaztanaga E.; O'Mill A.L.,Eriksen M.; Carretero J.; Casas R.; Castander F.J.; Garcia-Bellido J.,Hildebrandt H.; Mezcua M.; Miquel R.; Padilla C.; Renard P.; Sanchez E.,Serrano S.; Sevilla-Noarbe I.; Tallada-Crespi P.
IVOA id: ivo://cds.vizier/j/a+a/714/a74

Galactic open clusters abundances

2026-10-06T11:23:09Z

Description: Open clusters are powerful tools for studying the Milky Way. While large spectroscopic surveys now provide spectra for many cluster members, automated pipelines and heterogeneous membership selections can introduce sys- tematics and inflate apparent cluster scatter. Therefore, a homogeneous re-analysis with careful membership control and an explicit treatment of departures from Local Thermodynamic Equilibrium is valuable for establishing robust abundance gradients. The aim is to derive precise Galactic radial abundance gradients for multiple elements using open cluster giants, and to investigate how these gradients depend on cluster age. We re-analysed high-resolution infrared APOGEE Milky Way Mapper spectra from DR19 of the Sloan Digital Sky Survey for 655 open cluster members selected from Gaia data that satisfied strict quality cuts on signal-to-noise ratio. Stellar parameters and 18 elemental abundances were obtained using spectrum fitting with the Python version of Spectroscopy Made Easy, applying Non-Local Thermodynamic Equilibrium corrections for several key atomic species. Further quality control of the results was made by visual inspection of all fitted synthetic spectra. The metallicity of the clusters decreases with Galactocentric radius, following a global slope close to -0.06 dex/kpc. Beyond 10-11 kpc, there is modest flattening. In addition to the elements analysed in the Otto et al. (2026AJ....171...91O) study, we derive open-cluster gradients for V, Cu, Zn and Yb using APOGEE spectra. All elements exhibit negative [X/H] radial gradients of comparable magnitude, while [X/Fe] gradients are close to zero for the alpha and iron-peak groups. Several odd-Z and neutron capture species exhibit mild outward increases in [X/Fe], consistent with nucleosynthetic yields dependent on metallicity and/or delayed production channels for these elements. Old clusters have shallower gradients than young ones. However, the observed age dependence is influenced by the link between cluster age and galactocentric radius in the sample. Compared with Otto et al. (2026AJ....171...91O), the present reanalysis yields generally smaller reported per-cluster abundance uncertainties and suggests distinct, element-dependent revisions to the inferred Galactic trends. While the global gradients align closely with the optical Gaia-ESO results by Magrini et al. (2023A&A...669A.119M, cat. J/A+A/669/A119), we do not observe a straightforward flattening of the gradients with age. Our revised abundance scale reveals a shallower, broken radial metallicity gradient, providing a more robust observational benchmark for Galactic chemical-evolution models.
Author(s): Bijavara Seshashayana S.; Jonsson H.; D'Orazi V.; Cunha K.; Frinchaboy P.,Otto J.M.
IVOA id: ivo://cds.vizier/j/a+a/714/a67

PGIR survey long period variables catalog

2026-10-05T09:23:31Z

Description: Long Period Variables (LPVs) are stars with periods of several hundred days, representing the late, dust-enshrouded phase of stellar evolution in low to intermediate mass stars. In this paper, we present a catalog of 154755 LPVs using near-IR lightcurves from the Palomar Gattini-IR (PGIR) survey. PGIR has been surveying the entire accessible northern sky (DE>-28{deg}) in the J-band at a cadence of 2-3 days since 2018 September, and has produced J-band lightcurves for more than 60 million sources. We used a gradient-boosted decision tree classifier trained on a comprehensive feature set extracted from PGIR lightcurves to search for LPVs in this data set. We developed a parallelized and optimized code to extract features at a rate of ~0.1s per lightcurve. Our model can successfully distinguish LPVs from other stars with a true positive rate of 95%. Cross-matching with known LPVs, we find 70369 (~46%) new LPVs in our catalog.
Author(s): Suresh A.; Karambelkar V.; Kasliwal M.M.; Ashley M.C.B.; De K.,Hankins M.J.; Moore A.M.; Soon J.; Soria R.; Travouillon T.
IVOA id: ivo://cds.vizier/j/pasp/136/h4203

Stellar parameters for TESS FGK stars

2026-10-05T09:05:13Z

Description: Precise homogeneous stellar characterisation is crucial for our understanding of the physical properties of exoplanets, their demographics and the environment from which they are formed. We present a homogeneous catalogue of 717807 TESS FGK dwarfs and early subgiants, making use of isochrones along with Gaia DR3 inputs of photometry, parallax and spectroscopic temperature and metallicity, thus providing one of the largest homogeneous catalogues of stellar ages for TESS stars to date. We determine values for distance, logg, M/H, Teff, radius, mass and age. For our best fit values, we calculate median fractional errors of 4.29%, 4.49%, 1.74% and 50.00% on radius, mass, temperature and age respectively. We compare and validate our catalogue values to various literature sources which employ other isochrone grids and asteroseismology. In addition, we identify 278 TESS exoplanet hosts and 915 candidates and recalculate the planet radii for such systems. These homogeneous parameters provide a state-of-the art sample to probe the effect of physical stellar parameters on exoplanet characteristics and architectures.
Author(s): Waines F.M.; Weeks A.; Van Eylen V.
IVOA id: ivo://cds.vizier/j/mnras/551/g1593

Characterizing bright delta Scuti pulsators

2026-10-05T09:00:15Z

Description: Pulsations in delta Scuti stars exhibit a wide range of excited frequencies and amplitudes, but the underlying principles governing their amplitude distribution remain unclear. We revisit this problem using a global, energy-based perspective. For a complete sample of 3200 bright delta Scuti stars observed by TESS, integrated power spectral density (PSD) of the Fourier spectrum allows us to measure the overall pulsation signal. From this, we derive a proxy for the total pulsation energy. We uncover a bimodality among higher-frequency delta Scuti stars in their integrated PSD, possibly suggesting the presence of two distinct pulsation regimes. In addition, we identify an apparent upper limit to the total pulsation energy, indicating a constrained energy budget for these pulsations. This feature is not evident when stars are characterized solely by their dominant mode amplitude.
Author(s): Mani P.; Bedding T.R.; Murphy S.J.; Hey D.; Love T.
IVOA id: ivo://cds.vizier/j/mnras/552/g1780

Membership Study of Open Cluster NGC 6134

2026-10-05T08:52:20Z

Description: We present the results of our study on the membership of open star clusters in the southern hemisphere, NGC 6134. The position of NGC 6134 is located near the galaxy's plane, so the apparent position in the sky is in an area with high stellar density. This poses a challenge in distinguishing between cluster member stars and field stars. For this purpose, we use the Hierarchical Density-Based Spatial Clustering of Applications with Noise (HDBSCAN) algorithm on astrometric data from Gaia Data Release 3 (DR3). We take stars as samples up to a distance of 90 parsecs from the cluster's center as membership determination samples. The spatial scope of this sample is intentionally larger than previous studies on this star cluster, as some recent membership studies have concluded that the size of star clusters turns out to be larger than what has been reported. The results of our study produced a consistent number of members with the results of other studies with the same sample size. The clustering algorithm was then performed multiple times using different values of the radius sample. We determined that NGC 6134 has 888 members (membership probability >= 0.5), with a radius of 30 parsecs from the cluster's center.
Author(s): Yusuf M.; Ramadhan D.G.; Jatmiko A.T.P.; Perhati T.; Ramadhan S.,Arwinata H.I.; Yap F.; Satya L.; Mandey D.; Arifyanto M.I.; Premadi P.W.
IVOA id: ivo://cds.vizier/j/other/jphcs/2773.4

Water ice absorption map in the Milky Way

2026-10-05T08:37:02Z

Description: Interstellar ice plays a key role in the thermal evolution of the interstellar medium and in astrochemical pathways, yet its large-scale distribution remains poorly constrained. We use the Wide-field Infrared Survey Explorer (WISE) and the Two Micron All Sky Survey (2MASS) photometry to estimate water ice absorption in the W1/WISE band by correcting the observed colors for reddening and intrinsic stellar colors. This allows us to construct a first Milky Way water ice map. By varying input parameters, we test the stability of the method and identify the extinction law as the dominant source of uncertainty. Using synthetic photometry, we also quantify how different physical and observational parameters influence W1 band water ice absorption. The strong correlation between the measurement from photometric method and spectroscopic water ice abundance confirms that the W1 band signature originates from the 3um ice feature. We present the relationship between ice absorption in W1 band and water ice optical depth from theory and observations. Finally, we provide a preliminary Milky Way-scale map of water ice distribution.
Author(s): Cao Z.; Jiang B.; Meingast S.
IVOA id: ivo://cds.vizier/j/a+a/714/a99

Type Ia SNe NaI D line strength

2026-10-05T08:32:33Z

Description: Type Ia supernovae (SNe Ia) are thermonuclear runaways of some white dwarfs in binary systems. They have been extensively studied, yet their progenitor and explosion mechanisms remain poorly understood. We study a large sample of SNe Ia comparing the narrow interstellar absorption features in their spectra with various photometric and spectroscopic supernova properties, as well as environmental characteristics. The sodium absorption is significantly stronger in younger, more star-forming and more centrally located SNe Ia, as expected. However, we also show that there is a relation with intrinsic properties that is independent of the environment. In fact, there is substantial evidence for two environmental SN Ia populations, an old and a young one, with the young population showing significantly different distributions of sodium strength when divided according to the SiII ejecta velocity, nebular velocity, extinction, E(B-V), and reddening curve, RV. Performing a clustering of the SNe Ia, we recover an old population of SNe with low extinction and normal ejecta velocity, while the young population can indeed be subdivided into a group of highly-extincted, high-velocity SNe Ia with much stronger blueshifted sodium absorption, and another of low-extincted, normal-velocity objects with little sodium absorption. We interpret this relation of intervening material with intrinsic properties as evidence for the young SN Ia population, occurring in young and star-forming environments, to have asymmetric radiation that interacts with nearby material, and whose observables depend on the viewing angle. Finally, we show that the cosmological mass-step is consistent with these populations.
Author(s): Gonzalez-Gaitan S.; Gutierrez C.P.; Duarte J.; Santos R.; Martins G.,Anderson J.P.; Galbany L.
IVOA id: ivo://cds.vizier/j/a+a/714/a96

Cassini Scalar Helium MAG Calibrated Housekeeping Data Collection

2026-10-02T17:04:38Z

Description

This collection contains Cassini scalar helium (SHM) magnetometer
housekeeping data collected between 1999-08-18 and 2005-06-08.

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_shm_hkrate_asc/ppi/epn_core

Cassini MAG Calibrated Full Res. Data in RTN Coords. Collection

2026-10-02T17:04:30Z

Description

Cassini magnetic-field data in the highest time resolution available,
from the Fluxgate Magnetometer (FGM) instrument in RTN coordinates

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_full_rtn/ppi/epn_core

Cassini MAG Calibrated 1 Sec. Avg. Data in KSO Coords. Collection

2026-10-02T17:04:07Z

Description

This collection contains Cassini magnetic-field 1 second averages in
KSO coordinates, from the Fluxgate Magnetometer (FGM) instrument.

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_1sec_kso/ppi/epn_core

Cassini MAG Calibrated 1 Sec. Avg. Data in GSE Coords. Collection

2026-10-02T17:03:46Z

Description

This collection contains Cassini magnetic-field 1 second averages, in
GSE coordinates, from the Fluxgate Magnetometer (FGM) instrument.

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_1sec_gse/ppi/epn_core

RR Lyrae variables in M3

2026-10-02T11:13:16Z

Description: We present a comprehensive photometric study of RR Lyrae stars in the M3 globular cluster, utilizing a vast data set of 3140 optical (UBVRI) CCD images spanning 35yr from astronomical data archives. We have successfully identified previously known 238 RR Lyrae stars from the photometric data, comprising 178 RRab, 49 RRc, and 11 RRd stars. Multiband periodogram was used to significantly improve the long-term periods of 65 percent of RR Lyrae stars in our sample, thanks to the unprecedentedly long temporal coverage of the observations. The light curve templates were used to obtain accurate and precise mean magnitudes and amplitudes of all RR Lyrae variables. We combined optical (UBVRI) and near-infrared (NIR, JHKs) photometry of RR Lyrae variables to investigate their location in the colour-magnitude diagrams as well as the pulsation properties such as period distributions, Bailey diagrams and amplitude ratios. The period-luminosity relations in R and I bands and Period-Wesenheit relations were derived after excluding outliers identified in CMDs. The Period-Wesenheit relations calibrated via the theoretically predicted relations were used to determine a distance modulus of {mu}=15.04+/-0.04(stats)+/-0.19(syst.)mag (using metal-independent WBV Wesenheit) and {mu}=15.03+/-0.04(stats)+/-0.17(syst.)mag (using metal-dependent WVI Wesenheit) {mu}=15.03+/-0.04(stats)+/-0.17(syst.). Our distance measurements are in excellent agreement with published distances to M3 in the literature. We also employed an artificial neural network based comparison of theoretical and observed light curves to determine physical parameters (mass, luminosity, and effective temperature) for 79 non-Blazhko RRab stars that agree with limited literature measurements.
Author(s): Kumar N.; Bhardwaj A.; Singh H.P.; Rejkuba M.; Marconi M.; Prugniel P.
IVOA id: ivo://cds.vizier/j/mnras/531/2976

Enhanced magnetic activity after period gap

2026-10-02T10:36:26Z

Description: For low-mass stars (M<1.4M_{sun}_), the connection between stellar rotation and magnetic activity governs stellar spin-down, shapes the environments of their exoplanets, and provides an age-diagnostic via magneto-gyro-chronology. Recently, unexpected phenomena known as the intermediate rotation period gap and the rotational stalling have been discovered. These are likely due to internal angular momentum redistribution, and mark departures from a smooth spin-down evolution. These rotational features have been shown to cause enhanced magnetic activity on the photosphere, as measured by the photometric index from light curves (Sph), in both cluster and field stars. However, their influence on other magnetic activity proxies, and particularly in field stars, remains poorly understood. In this work, we study the impact of the intermediate-period gap on chromospheric magnetic activity as traced by the CaII infrared triplet (IRT) index. We target the stars observed by the Kepler mission, as this is the largest and most reliable sample of field stars with measured rotation periods sensitive to the gap. We calculate the CaII IRT index for the Kepler stars using the spectroscopic information from the Gaia mission data release three (DR3). We study the rotation-activity relation as a function of location on the Hertzsprung-Russell (HR) diagram and spectral type, finding that K dwarfs are more active than G dwarfs, which in turn are more active than F dwarfs. For main-sequence stars, we find that chromospheric magnetic activity is also enhanced after the intermediate- period gap, mirroring its effect on the photospheric Sph index. Our work reveals that the intermediate-period gap marks a genuine transition in stellar magnetic behavior, not only at the photosphere but also at the chromosphere. This highlights the need to account for its signatures across activity proxies, as well as its impact on exoplanet habitability and the age-rotation-activity relation.
Author(s): Godoy-Rivera D.; Mathur S.; Richey-Yowell T.; Santos A.R.G.; Garcia R.A.,Grossmann D.H.; Claytor Z.R.; Beck P.G.
IVOA id: ivo://cds.vizier/j/a+a/714/a124

V557 Mon photometry and spectra

2026-10-02T10:22:01Z

Description: The unstable mass accretion process in young stellar objects (YSOs) often triggers observable outbursts. These episodic accretion events play a critical role in stellar mass assembly during the pre-main-sequence phase. In this paper, we present observations of an eruptive young star in the Rosette Nebula, identified by the Gaia Science Alerts system using Gaia time-series data. We aim to investigate the evolution of the brightness and mass accretion rate of V557 Mon throughout its outburst and subsequent decline. In addition, we trace the evolution of the inner accretion disk during the outburst by monitoring molecular emission features. We compiled multi-band photometric time series from Gaia, ZTF, and several 1m-class ground-based telescopes and obtained optical and near-infrared spectra at multiple epochs covering the outburst and fading phases. Stellar parameters were derived from quiescent colour/spectra and spectral energy distribution (SED) fitting. We also measured the mass accretion rate and fit models to molecular emission bands. Since late 2024, V557 Mon has undergone a year-long outburst consistent with EXor variability. Based on quiescent photometry, V557 Mon has a spectral type of M1 with an extinction of AV=1.8+/-0.3mag, consistent with a 0.4-0.5M_{sun}_ star at an age of 2Myr. Our multi-epoch spectra and u-band photometry indicate a peak accretion rate of 6.3x10^^-7^M_{sun}_/yr during the outburst, roughly 70 times higher than in quiescence. We report the detection of hot water vapour emission bands, together with TiO, VO, and CO emission features. Using ExoMol models, we measured the inner-disk temperature changed from 3000K to 2000K during the fading phase of the outburst. We report a recent EXor outburst in a low-mass Class II YSO. Our observations reveal the transient formation of a hot molecular inner disk, traced by variable water vapour emission during the EXor event. A positive correlation is found between the molecular excitation temperature and the overall stellar brightness.
Author(s): Guo Z.; Osses J.; Fermiano V.; Zhou Y.; Fang M.; Herczeg G.; Carvalho A.,Elbakyan V.; Hillenbrand L.; Wang M.; Liu H.; Liu Y.; Briceno C.; Singh K.,Ivanov V.D.; Ninan J.; Giannini T.; Aliaga A.; Morris C.; Montesinos M.,Zhao H.; Contreras Pena C.; Jose J.; Chand T.; Chen W.-P.; Wang W.-H.,Huang Y.; Lopez C.; Fernandez-Schlosser P.; Correa-Herrera D.; Kurtev R.,Rodriguez V.; Lizana-Vidal C.; Borissova J.; Kuhn M.; Saito R.K.; Yadav R.K.
IVOA id: ivo://cds.vizier/j/a+a/714/a98

Gaia EDR3 white dwarfs Ca abundances

2026-10-02T10:12:12Z

Description: White dwarf (WD) atmospheric metal pollution provides strong evidence for the presence of remnant planetary material, and it can be used as an indirect tracer of outer planetary systems. We analyze whether the presence of a wide stellar companion affects the occurrence of outer planetary systems by comparing the incidence of calcium pollution in hydrogen-atmosphere WDs in wide binaries and in apparently single stars. We constructed two sample pairs: a large homogeneous SDSS low-resolution spectroscopic set (4844 single WDs; 322 WDs in wide binaries) and a smaller high-resolution sample (83 single WDs; 34 WDs in wide binaries). For each WD, we measured calcium abundances or upper limits and computed detectability-corrected cumulative pollution fractions that account for variations in effective temperature, signal-to-noise ratio, and spectral resolution. In the SDSS-based samples, we find pollution fractions below ~1%, defined as the fraction of white dwarfs with detected Ca relative to the total number of white dwarfs, for both single WDs and WDs in wide binaries. After correcting for detectability, the cumulative abundance distributions of the two populations are statistically consistent. The same conclusion was obtained for the higher-resolution samples, despite their different raw detection fractions. Our results indicate no statistically significant difference in the occurrence rate of remnant outer planetary systems between single stars and stars with wide (~200au) companions, within the current uncertainties. These uncertainties are significant because the samples contain only a small number of polluted WDs. The corrected detectability cumulative fraction approach used here provides a framework for comparing samples with different detection sensitivities and can be extended to larger spectroscopic datasets. Such samples will be required to determine whether wide stellar companions affect the survival and delivery of planetary material and to search for more subtle trends, for example, as a function of companion separation.
Author(s): Lizana-Vidal C.; Aguilera-Gomez C.; Rogers L.K.; Bonsor A.,Munoz-Arriagada M.I.; Dufour P.; Bravo-Parra C.; Salugova E.
IVOA id: ivo://cds.vizier/j/a+a/714/a64

On the rotation period of the O giant xi Per

2026-10-02T10:07:44Z

Description: OB stars exhibit line profile variability, often over timescales associated with rotation, notably in their ultraviolet wind-sensitive lines in which "discrete absorption components" recur cyclically. We searched for periodicity in spectral regions of the O7.5III(n)((f)) star xi Persei that are formed very close to the star and are least likely to be affected by doublet overlap or irregular transient phenomena. We identified the low-velocity wind region probed by the NIV lambda 1718{AA} line as the most uncontaminated spectral region for which a large and homogeneous dataset is available: 307 International Ultraviolet Explorer (IUE) spectra over 12 years, and 11 STIS (onboard the Hubble Space Telescope) spectra taken 21 years later. We also studied 322 time-resolved HeII lambda 4686{AA} spectra. We searched for periodicities in high-precision space photometry (MOST, BRITE, and TESS), covering 13 years. We also reconsidered X-ray studies with Chandra. A CLEAN analysis and subsequent weighted least-squares fit of the flux in this region resulted in a unique period of 2.040514+/-0.000020d, interpreted as due to rotation. The phase of maximum flux in the NIV, SiIV, Halpha, and HeII line profiles, and X-ray variability studies, coincide. We also found this period with low amplitude in the photometric data, albeit with large intrinsic scatter, and with a deviating maximum phase. Given the coherent periodic behaviour of several observables probing the region of the wind nearest the stellar surface, we propose that xi Per has an as-yet undetected weak global surface magnetic field. We excluded a rotation period of ~4d based on stellar parameters. The sinusoidal behaviour suggested that only one magnetic pole is visible, implying an inclination of i~51deg, and therefore, beta<~90-i=39deg for the magnetic obliquity. We present a conceptual framework within which weak wind confinement by a global magnetic field can create a small magnetospheric disc, while allowing the formation of more classic `corotating interaction regions' at higher magnetic latitudes. The periodic variations are then understood to result from the changing projected area of the magnetospheric disc as a function of rotational phase, both along the line of sight and off the stellar limb.
Author(s): Henrichs H.F.; Sudnik N.; David-Uraz A.
IVOA id: ivo://cds.vizier/j/a+a/714/a63

Gaia DR3 [Fe/H] from LAMOST DR10

2026-10-02T10:03:52Z

Description: Gaia DR3 provides astrophysical parameters for hundreds of millions of stars but the [M/H] from its GSP-Phot module suffer from systematic bias. In this paper, we estimate stellar metallicities from Gaia DR3 data, using the homogeneous spectroscopic iron abundances [Fe/H] of LAMOST DR10 as training labels. We have cross-matched LAMOST DR10 [Fe/H] with Gaia DR3 and trained a gradient-boosted decision-tree regressor (XGBoost) on 1.20 million AFGK stars, using only Gaia-derived inputs and proxies. We validated the estimates on held-out LAMOST stars, on GALAH DR4 and APOGEE DR17, and on 46 open clusters, and applied the model to measure the radial metallicity gradient of the disk of the Milky Way. On the held-out test set, the model reaches a mean absolute error of 0.052dex and R^2^=0.94 with negligible bias, against 0.242dex for GSP-Phot on the same stars. The estimates transfer well to external surveys with a mean absolute error of 0.066dex (GALAH) and 0.068dex (APOGEE). For open clusters, the median difference between our estimated [Fe/H] and [Fe/H] from spectroscopy surveys is 0.041dex which is smaller than both GSP-Phot (0.248dex) and previous work on an APOGEE-trained XG-Boost model (0.067dex). When we applied our model to the disk, it recovers a broken thin disk radial gradient (inner +0.119, outer -0.058dex/kpc with a break near 5.9kpc) and an open-cluster gradient of -0.066dex/kpc, both in agreement with previous high-resolution spectroscopy works. Our estimated [Fe/H] values are accurate to 0.05dex to 0.07dex for AFGK stars within the range [Fe/H]>~-2.5; below this limit the predictions should be treated as lower bounds. The catalogue and the trained model are publicly available on Zenodo. These estimates are suitable for chemical studies of the Milky Way.
Author(s): Srivastava D.; Niedzielski A.; Smiljanic R.
IVOA id: ivo://cds.vizier/j/a+a/714/a59

Optical spectra of HD 14134

2026-10-02T09:52:35Z

Description: The post-main sequence (MS) evolution of massive stars encompasses phases in which the stars display high variability. One such class of objects are the blue supergiants which may be in either the pre- or post-red supergiant phase of their evolution. Their variability patterns might provide constraints for a proper classification of the objects. Teh study aims to characterise the observed variability of the B supergiant HD14134 and to investigate the imprint of a time-variable wind on the brightness variation of the star and its impact on the detectability of pulsation signals. Spectroscopic data were collected over a 5-month period and combined with photometry from TESS. Stellar parameters were derived from modelling of the time-averaged spectrum with CMFGEN and the SED and were confirmed with stellar evolution models computed with MESA. The light curves and radial velocity curves of selected lines were analysed to determine pulsation signals. The wind variability and its imprint on the stellar brightness were investigated from an analysis of the Halpha line. Predictions of mode excitations were computed with the GYRE pulsation code and compared to the frequencies determined from the observations. A g-mode with a period of ~19.2d and its harmonics are consistently detected in all data sets. The spectra unveil strong, non-periodic wind variability and 3 frequency signals were identified as due to this wind variability. The stellar parameters and age derived for HD14134 together with the absence of radial pulsations classify the star as a post-MS object evolving towards the red-supergiant stage, questioning its classification as alpha Cyg variable. The results reinforce that simultaneous long-term spectroscopic and photometric monitoring is indispensable for reliable frequency detections and for disentangling of variabilities imprinted by a time-variable wind from those imposed by pulsations.
Author(s): Guha S.; Kraus M.; Sanchez Arias J.P.; Nemeth P.; Kaminski K.
IVOA id: ivo://cds.vizier/j/a+a/714/a46

AMS-02 All Particle Rates Catalog

2026-10-02T00:00:00Z

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

AMS-02 Spectral Results Catalog

2026-10-02T00:00:00Z

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

Chandra Source Catalog Stacked Observation Detections, v2.1.1

2026-10-02T00:00:00Z

Description: The Chandra Source Catalog's Stacked Observation Detections Table (CSCSTACK) includes 493,236 detections (855,402 total entries consisting of detections plus photometric upper limits) based on 10,034 stacks of X-ray observations. Exploiting the unique resolution and very low background of Chandra data, the limiting sensitivity of the catalog is enhanced significantly by stacking (co-adding) multiple observations of the same field prior to source detection. To minimize the impact of the variation in the Chandra point spread function (PSF) with off-axis angles, source detection is constrained to run on stacks of observations that have telescope pointings that are co-located within 60 arcseconds and that were obtained using the same instrument (ACIS or HRC-I). Formally, the observations are matched using a tree clustering algorithm with complete linkage. This means that the pointing direction of every observation in the stack is co-aligned with the pointing direction of every other observation in the stack within 60 arcseconds. The stacked-observation level allows composite properties to be reported from the co-added observations for detections that would otherwise not be visible or have poor S/N in individual observations, while for higher S/N detections the per-observation properties facilitate analysis of variable sources. CSCSTACK is related to the <a href="/W3Browse/chandra/csc.html">Chandra Source Catalog (CSC)</a> catalog, which is the definitive catalog of X-ray sources detected by the Chandra X-ray Observatory. The CSC contains 407,806 unique compact and extended X-ray sources. By combining Chandra's sub-arcsecond on-axis spatial resolution and low instrumental background with consistent data processing, the CSC delivers a wide variety of uniformly calibrated properties and science ready data products for detected sources over four decades of flux. Each identified distinct X-ray source on the sky is represented in the catalog by one or more "stack detection" entries -- one for each stack in which the source has been detected -- and a single "master source" entry. The individual stack entries record all of the properties about a detection extracted from a single stack, as well as associated file-based data products, which are stack-specific. If a source is detected in one or more stacked-observations, photometric upper limits that are useful for temporal variability analyses are calculated for any overlapping stacked- and individual-observations in which the source is not detected. This database table was ingested by the HEASARC in July 2026 and is based on a download of the online version of the "Stacked Observation Detections" Table v. 2.1.1, at the CXC using the CLI. Refer to <a href="https://cxc.harvard.edu/csc/cli/">https://cxc.harvard.edu/csc/cli/</a> for details. This is a service provided by NASA HEASARC .
Author(s): Evans, Civano
IVOA id: ivo://nasa.heasarc/cscstack

Swift-XRT Living Point Source Catalog (LSXPS)

2026-10-02T00:00:00Z

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

ESDC Multi-mission Data Services TAP

2026-10-01T13:29:33.182000Z

Description: The ESDC Multi-mission Data Services (EMDS) TAP service provides unified access to metadata across multiple ESDC Science Archives, supporting interoperability, standardised data discovery, and long-term service sustainability. The service implements the IVOA Table Access Protocol (TAP) standard and enables access to metadata exposed through both mission-specific data models and the IVOA Observation Core Components (ObsCore) data model. The archives currently accessible through the EMDS TAP service include Einstein Probe, EXOSAT, ISO, Cheops, Smile, Ulysses, and Proba-3.
IVOA id: ivo://esavo/emds/tap

J-PAS-E2DR (October, 2026)

2026-10-01T08:30:00Z

Description: J-PAS E2DR Extended Early Data Release (October, 2026) HiPS catalogue. J-PAS is a 57-band photometric optical survey, observing the Northern Hemisphere from the dedicated JST250 telescope and the JPCam instrument at the Observatorio Astrofísico de Javalambre (OAJ, Teruel, Spain). . Please include the following in any published material that makes use of this data: "Based on observations made with the JST250 telescope and JPCam camera of the J-PAS Survey at the Observatorio Astrofísico de Javalambre, in Teruel, owned, managed and operated by the Centro de Estudios de Física del Cosmos de Aragón."
Author(s): Centro de Estudios de Física del Cosmos de Aragón (CEFCA)
IVOA id: ivo://cefca/j-pas/j-pas-e2dr

Dust in II Zw 096

2026-10-01T08:23:46Z

Description: Galaxy mergers drive intense radiation environments that fundamentally alter interstellar dust properties through photo-destruction and thermal processing. The luminous infrared galaxy II Zw 096 presents several distinctive regions, including starburst clumps and a proposed buried AGN in region D1, making it an ideal laboratory for studying dust evolution under extreme conditions. This work aims to determine the carbonaceous dust properties across II Zw 096 by characterizing the spatial variations in carbonaceous feature ratios and investigate how intense radiation fields process carbonaceous dust grains, using the relationship between dust processing signatures and traditional radiation field diagnostics. Using JWST NIRSpec IFU and MIRI MRS, carbonaceous features were observed and analyzed using the Continuum and Feature Extraction tool (CAFE) with 61 carbonaceous features from the PDRs4all project and new absorption features for ice and crystalline silicates. We analyze spatial variations in carbonaceous feature ratios at multiple resolutions (0.281", 0.787" and 0.961") to trace dust composition and grain size distribution. The 3.4/3.3 um ratio probes aliphatic versus aromatic content, while the 11.3/3.3um ratio diagnoses grain size distribution. The 3.4/3.3um ratio spans between 0.056-0.148, with the lowest values near the proposed AGN (D1) and starburst clumps (C0, D0), indicating preferential destruction of C-H bonds connected to aliphatic structures in highly irradiated environments. The 11.3/3.3 um ratio varies from 0.334 up to ~2.348 in D1. Both PAH ratios show no clear correlation with [NeIII]/[NeII], suggesting ionization diagnostics either break down in extreme merger environments, or as an effect of tracing different ISM phases and radiation-field regimes in this highly obscured merger environment. We detect water ice (3.1um), CO_2_ ice (4.27um), and crystalline silicates (11.1um) with spatial distributions anti-correlating with carbonaceous processing signatures. Spatial resolution critically affects dust diagnostics: the 3.4/3.3um dynamic range doubles when increasing the resolution from 0.961" to 0.281", demonstrating that apparent uniformity at low resolution masks significant variations in compact regions undergoing intense dust processing. Multiple coherent diagnostics point to intense dust processing, such as photodestruction of the smallest nanograins and aromatisation, consistent with a buried AGN in D1, though definitive confirmation remains elusive.
Author(s): Olander G.; Schirmer T.; Aalto S.; del Palacio S.; Diaz-Santos T.; Inami H.,Armus L.; Buiten V.; Knudsen K.K.; Konig S.; Lai T.S.-Y.; Lenkic L.,Linden S.T.; Nyman G.; Riesco C.; van der Werf P.; Vlemmings W.,Sameera W.M.C.; Wethers C.
IVOA id: ivo://cds.vizier/j/a+a/714/a43

Tidal tails from NGC7492 along Sgr stream

2026-10-01T08:22:09Z

Description: The formation, extension, and morphology of extra-tidal stars around globular clusters depend on the internal kinematics of the host cluster and the influence of the Galactic potential. Tracing the kinematics of faint tidal tails sheds light on their formation and contribution to the Milky Way halo assembly. NGC 7492 is an outer halo globular cluster with conflicting evidence regarding the presence of tidal tails. If present, the tails are expected to be faint and embedded in the Sagittarius tidal stream, located at a similar heliocentric distance but having different kinematics. We carried out a GIRAFFE spectroscopic follow-up of ten fields at the expected location of tidal tails associated with NGC 7492 to obtain the radial velocity component. Gaia parallaxes were used to remove foreground contaminants, while only loose constraints on Gaia proper motion were applied to select the targets. From the high-resolution spectra, radial velocities and metallicities were derived for more than 700 stars, from the red giant branch down to the upper main sequence. Cluster and extra-tidal stars were identified based on their proper motions, radial velocities, and metallicities. This population extends over at least ~1.8deg from the cluster center, confirming the tidal tails previously detected only photometrically. The extra-tidal stars are located at positions consistent with spray-particle models for the cluster's disruption. The Sagittarius stream is also clearly identified through its distinct proper motion distribution, radial velocities and more metal-rich population. Despite the low spatial density of extra-tidal stars, the kinematic signature of the cluster is clearly detected, confirming the presence of tidal tails overlapping on the sky with the Sagittarius stream, though the two structures are physically unrelated. The present spectroscopic dataset provides a robust basis for future studies aimed at extending the characterization of the tails, both in extension and limiting magnitude.
Author(s): Navarrete C.; Rojas-Arriagada A.; Piatti A.E.; Carballo-Bello J.A.,Sbordone L.; Kundu R.; Belokurov V.; Koposov S.E.; Vitral E.; Boldrini P.,Palicio P.A.
IVOA id: ivo://cds.vizier/j/a+a/714/a39

LINCC Frameworks - Hugging Face - mmu_cfa_seccsn

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_cfa_seccsn

LINCC Frameworks - Hugging Face - mmu_cfa_snii

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_cfa_snii

LINCC Frameworks - Hugging Face - mmu_chandra_spectra

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_chandra_spectra

LINCC Frameworks - Hugging Face - mmu_csp_csp

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_csp_csp

LINCC Frameworks - Hugging Face - mmu_des_y3_sne_ia

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_des_y3_sne_ia

LINCC Frameworks - Hugging Face - mmu_desi_edr_sv3

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_desi_edr_sv3

LINCC Frameworks - Hugging Face - mmu_desi_provabgs

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_desi_provabgs

LINCC Frameworks - Hugging Face - mmu_euclid_q1

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_euclid_q1

LINCC Frameworks - Hugging Face - mmu_foundation

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_foundation