VO Fresh

PN G054.2-03.4 light and velocity curves

2026-03-03T08:41:38Z

Description: The Necklace nebula is a bipolar, post-common-envelope planetary nebula, the central star of which has been shown to have a dwarf carbon star companion. We aim to understand the origins of the Necklace and its dwarf carbon central star. We study the carbon abundance of the nebula through far ultraviolet spectroscopy obtained with the Hubble Space Telescope. Furthermore, through simultaneous modelling of multiband light and velocity curves, we attempt to constrain the parameters of the central star system. Puzzlingly, we find that the region of the inner nebula observed with the Hubble Space Telescope is seemingly not carbon- rich, at odds with the dwarf carbon star nature of the companion of the central star. The initial mass of the nebular progenitor was likely very close to the limit to become carbon-rich, perhaps experiencing a very late thermal pulse. The dwarf carbon star companion is found to be significantly inflated with respect to that expected for an isolated main sequence star of the same mass. The properties of the central binary are consistent with the progenitor having become carbon-rich and its companion having accreted a significant amount of that carbon-enriched material. However, it is unclear how this evolutionary hypothesis can be reconciled with the inner nebula potentially being carbon poor.
Author(s): Jones D.; Corradi R.L.M.; Garcia Perez G.A.; Morisset C.; Garcia-Rojas J.,Sabin L.; Balick B.; Wise J.; Mampaso A.; Munday J.; Rodriguez-Gil P.,del Mar Rubio-Diez M.; Santander-Garcia M.; Sowicka P.; Csukai A.,Hillwig T.C.; Henderson de la Fuente A.; Terwel J.H.
IVOA id: ivo://cds.vizier/j/a+a/707/a169

SN 2024acyl light curves

2026-03-03T08:35:25Z

Description: We present a photometric and spectroscopic analysis of the Type Ibn supernova (SN) 2024acyl. It rises to an absolute magnitude peak of M_o=-17.58+/-0.15mag in 10.6 days, and displays a rapid linear post-peak light-curve decline in all bands (e.g., gamma_0-60(V)_=0.097+/-0.002mag/d), similar to most SNe Ibn. The optical pseudobolometric light curve peaks at (3.5+/-0.8)x10^42^erg/s, with a total radiated energy of (5.0+/-0.4)x10^48^erg. The spectra are dominated by a blue continuum at early stages, with narrow P-Cygni HeI lines and flash-ionisation emission lines of CIII, NIII, and HeII. The P-Cygni HeI features gradually evolve and become emission-dominated in late-time spectra. The H-alpha line is detected throughout the entire spectral evolution, which indicates that the circumstellar material (CSM) is helium-rich with some residual amount of hydrogen. Our multiband light-curve modelling yields estimates of the ejecta mass of M_ej_=0.49^+0.11^_-0.09_M_{sun}_, with a kinetic energy of E_k_=0.06^+0.01^_-0.01_x10^51^erg, and a ^56^Ni mass of M_Ni_=0.018M_{sun}_. The inferred CSM properties are characterised by a mass of M_CSM_= 0.51 (+0.05/-0.04) M_sun, an inner radius of R_0_=17.8^+3.6^_-3.0_AU, and a density rho_CSM_=(8.3^+2.7^_-1.2_)x10^-12^g/cm^3^. The multi-epoch spectra are well reproduced by the CMFGEN/he4p0 model, corresponding to a He-ZAMS mass of 4M_{sun}_ (H-ZAMS mass 18.11M_{sun}_, pre-SN mass 3.16M_{sun}_). These findings are consistent with a scenario of an SN powered by ejecta-CSM interaction, originating from a low-mass helium star that evolved within an interacting binary system where the CSM with some residual hydrogen may originate from the mass-transfer process. We also discuss an extreme scenario involving the possible merger of a helium white dwarf. In addition, a channel of core-collapse (CC) explosion of a late-type Wolf-Rayet (WR) star with hydrogen (WNH), or a transitional star between an Of and a WR type (e.g., an Ofpe/WN9 star) with fallback accretion, cannot be entirely ruled out.
Author(s): Cai Y.-Z.; Pastorello A.; Maeda K.; Zhao J.-W.; Wang Z.-Y.; Peng Z.-H.,Reguitti A.; Tartaglia L.; Filippenko A.V.; Pan Y.; Valerin G.; Kumar B.,Wang Z.; Fraser M.; Anderson J.P.; Benetti S.; Bose S.; Brink T.G.,Cappellaro E.; Chen T.-W.; Chen X.-L.; Elias-Rosa N.; Esamdin A.,Gal-Yam A.; Gonzalez-Banuelos M.; Gromadzki M.; Gutierrez C.P.,Inserra C.; Iskandar A.; Kangas T.; Kankare E.; Kravtsov T.,Kuncarayakti H.; Li L.-P.; Liu C.-X.; Liu X.-K.; Lundqvist P.,Matilainen K.; Mattila S.; Moran S.; Mueller-Bravo T.E.; Nagao T.,Petrushevska T.; Pignata G.; Salmaso I.; Smartt S.J.; Sollerman J.,Srivastav S.; Stritzinger M.D.; Wang L.-T.; Yan S.-Y.; Yang Y.,Yang Y.-P.; Zheng W.; Zou X.-Z.; Chen L.-Y.; Du X.-L.; Fang Q.-L.,Fiore A.; Ragosta F.; Zha S.; Zhang J.-J.; Liu X.-W.; Bai J.-M.; Wang B.,Wang X.-F.
IVOA id: ivo://cds.vizier/j/a+a/707/a157

Bar morphologies of HSC-SSP disc galaxies

2026-03-03T08:25:55Z

Description: We investigate the role of galactic bars in fuelling and triggering Active Galactic Nucleus (AGN) in disc galaxies up to z~0.8. We utilise a Deep Learning model, fine-tuned on Galaxy Zoo volunteer classifications, to identify (strongly and weakly) barred and unbarred disc galaxies in Hyper Suprime-Cam Subaru Strategic Program i-band images. We select AGN using three independent diagnostics: mid-infrared colours, X-ray detections, and spectral energy distribution (SED) fitting. The SED analysis, performed using CIGALE, quantifies the relative AGN contribution to the total galaxy luminosity (f_AGN_) and the AGN luminosity (L_disc_). We assess the impact of bars by comparing AGN incidence and properties in barred galaxies against carefully constructed redshift-, stellar mass-, and colour-matched unbarred control samples. Our binary AGN classification experiment demonstrates that barred disc galaxies host a higher fraction of AGN compared to their unbarred counterparts, though the significance depends on the AGN selection method, with a more modest excess for SED AGN, and control sample size. This suggests a contributing role for bars in the global AGN budget. The contribution of bars to AGN fuelling appears confined to systems where the AGN has a lower relative contribution to the host galaxy's emission (f_AGN_<0.75). Crucially, we find a significant dearth of barred disc galaxies hosting AGN with f_AGN_>0.75, independent of bar strength. Consistent with this, the fraction of barred galaxies among AGN hosts decreases with increasing L_disc_. Combined with previous results, we suggest that bars may contribute to fuelling the population of low-to-moderate luminosity AGN, but major mergers are the principal mechanism for triggering the most powerful and dominant accretion events.
Author(s): La Marca A.; Nardone M.T.; Wang L.; Margalef-Bentabol B.; Kruk S.,Trager S.C.
IVOA id: ivo://cds.vizier/j/a+a/707/a152

Local LIRGs clumps physical properties

2026-03-03T08:23:56Z

Description: We investigated the properties of the interstellar medium (ISM) at giant molecular cloud (GMC) scales (~100 pc) in a sample of 27 nearby luminous infrared galaxies (LIRGs) spanning all interacting stages along the merger sequence, i.e. from isolated systems to late-stage mergers. In particular, we study the relations between star-formation (SF) and molecular gas surface density as a function of the interaction stage by (1) defining beam-sized (unresolved, line-of-sight) regions and (2) identifying actual gas clumps and physical structures within the galaxies. In total, we identify more than 4000 beam-sized CO-emitting regions defined on scales of ~100pc and more than 1000 molecular gas clumps in the sample. To map the distribution of molecular gas we used the Atacama Large Millimeter/submillimeter Array (ALMA) to observe the J=2-1 CO transition, and to map the distribution of star formation we used the Hubble Space Telescope (HST) observations of the Pa{alpha} or Pa{beta} hydrogen recombination lines. We derived spatially resolved Kennicutt-Schmidt (KS) relations for each LIRG in the sample. When using beam-sized regions, we find that 67% of galaxies follow a single relation between {SIGMA}SFR and {SIGMA}H2. However, in the remaining galaxies, the relation splits into two branches - one characterised by higher {SIGMA}SFR and {SIGMA}H2, the other by lower value - indicating the presence of a duality in this relation. In contrast, when using physical gas clumps, the duality disappears and all galaxies show a single trend. These results provide two complementary perspectives when studying the star formation process. The first maximises the number statistics (beam-sized regions), and the second focuses on actual structures associated with gas clumps in which the measured sizes have a physical meaning. We also studied other ISM and clump properties as a function of the merger stage of the LIRG systems. We find that isolated galaxies and systems in early stages of interaction exhibit smaller amounts of gas and lower star formation rates (SFRs). As the merger progresses, however, the amount of gas in the central kiloparsecs of the galaxy undergoing the merger increases, along with the SFR, and the slope of the KS relation becomes steeper, indicating an increase in the SF efficiency of the molecular gas clumps. Clumps in late-stage mergers are predominantly located at small distances from the nucleus, confirming that most of the activity is concentrated in the central regions. Interestingly, the relation between the star formation efficiency and the boundedness parameter (which measures the effects of gravity against velocity dispersion) evolves from being roughly flat in the early stages of the merger to becoming positive in the final phases, indicating that clump self-gravity only starts to regulate the star formation process between the early and mid merger stages.
Author(s): Sanchez-Garcia M.; Diaz-Santos T.; Barcos-Munoz L.; Evans A.S.; Song Y.,Pereira-Santaella M.; Garcia-Burillo S.; Linden S.T.; Ricci C.; Lenkic L.,Zanella A.; Armus L.; Eibensteiner C.; Teng Y.-H.; Saravia A.; Buiten V.A.,Privon G.C.; Torres-Alba N.; Saito T.; Larson K.L.; Bianchin M.,Medling A.M.; Lai T.; Donnelly G.P.; Charmandaris V.; Bohn T.; Lofaro C.M.,Meza G.
IVOA id: ivo://cds.vizier/j/a+a/707/a144

MaNGA and ATLAS3D ETGs kinematic data

2026-03-03T08:22:37Z

Description: This study aims to make a comparative analysis of galaxy kinematics using IllustrisTNG simulations and integral-field spectroscopy (IFS) observations. We identify 2342 early-type galaxies (ETGs) from the TNG100 simulation and 236 ETGs from the TNG50 simulation to compare with those from MaNGA and ATLAS^3D^ surveys. For these systems, we measure key kinematic parameters widely employed in both observational and simulation-based studies, including the intrinsic spin parameter {lambda}_R,intr_ (it indicates that the {lambda}_R_ parameter is measured when the galaxy is viewed edge-on), the cylindrical rotational energy fraction {kappa}_rot_, and structural mass ratios such as the spheroid mass fraction f_spheroid_ and the stellar halo mass fraction f_halo_. This study performs a comparative kinematic analysis of early-type galaxies using IllustrisTNG simulations and IFS data from MaNGA and ATLAS^3D^ . We demonstrate that standard classifiers --- the {lambda}_R_(Re)=0.31 SQRT(epsilon) relation and k_5_{bar} coefficient (the higher-order term of the Fourier decomposition of velocity fields) --- fail to align with kinematic bimodality. Revised thresholds are proposed: the spin {lambda}_R,intr_~0.4, the ratio of rotation energy {kappa}_rot_~0.5, and the mass fraction of a spheroid component f_spheroid_~0.6. It provides a universal threshold that classifies all kinds of galaxies into rotation-dominated (fast rotators) and random motion-dominated (slow rotators) cases. Scaling relations derived from TNG enable estimation of {kappa}_rot_ and f_spheroid_ from observations. TNG simulations exhibit a bimodality deficit, characterized by a lack of fast rotators and suppressed {lambda}_R,intr_, attributable to excess galaxies with intermediate rotation and high spheroid/stellar halo mass. A novel method for estimating stellar halo mass fractions from IFS kinematics is introduced, though significant uncertainties persist.
Author(s): Zhong W.; Du M.; Lu S.; Jin Y.; Zhu K.
IVOA id: ivo://cds.vizier/j/a+a/707/a137

Catalog of gamma-ray source candidates

2026-03-03T08:20:28Z

Description: Sixteen years of continuous observations with the Fermi Large Area Telescope (LAT) provide an unprecedented opportunity to search for faint or previously unrecognized gamma-ray emitters, particularly at high energies where the angular resolution improves and the diffuse background is reduced. We present a new catalog of gamma-ray source candidates identified using a data-driven, clustering-based analysis of Pass 8 LAT data above 3GeV at Galactic latitudes |b|>10{deg}. The pipeline integrates the SIeving MEthod for FInding Core, version 3 (SIMEFIC III) for photon denoising with the density-based spatial clustering of applications with noise (DBSCAN) algorithm. We detect 3112 gamma-ray cluster candidates, of which 2932 are associated with known gamma-ray sources. Cross-matching yields 37 counterparts in 1CGH, 23 in CRATES, 21 in Roma-BZCAT, 17 in MST-12yr. The remaining 370 clusters have no known gamma-ray counterpart and are proposed as new source candidates.
Author(s): Akhondi F.; Soor M.; Hedayati K.
IVOA id: ivo://cds.vizier/j/a+a/707/a61

Properties of 145 SNe Ia

2026-03-02T20:04:24Z

Description: Photospheric and high-velocity features (PVFs and HVFs) of SiII {lambda}6355 and CaII IR3 lines in supernova Ia (SN Ia) spectra provide insights into ejecta structure, energetics, and circumstellar interaction, yet their interplay remains poorly understood. We analyse a representative sample of 145 nearby SNe Ia observed within +/-5d of B-band maximum light, including normal, 91T-, and 91bg-like events with measured light-curve decline rates ({Delta}m_15_) and SiII and CaII line properties from the literature. We model PVF and HVF velocity distributions using Gaussian Mixture Models, compare SiII and CaII PVF velocity distributions, assess CaII HVF properties, and test correlations between SiII PVF velocities and {Delta}m_15_, with emphasis on HVF effects. For the first time, we show that the CaII PVF velocity distribution, measured for the same events at the same phases as SiII, is predominantly unimodal, in contrast to the well-known bimodal SiII PVF distribution that supports the high-velocity/normal-velocity division. This contrast likely reflects a subclass-dependent formation depth of the CaII line, as supported by a positive correlation (>3.3{sigma}) between {Delta}m_15_ and the velocity offset between CaII and SiII PVFs, particularly in faster-declining SNe Ia. Importantly, HVFs do not significantly bias PVF velocity distributions. A significant negative correlation (>3.3{sigma}) between SiII PVF velocity and {Delta}m_15_ is found only for HVF-weak SNe Ia, consistent with more energetic explosions yielding faster ejecta, while this trend vanishes in HVF-strong events, likely due to circumstellar interaction. These results underscore the critical role of HVFs and SN Ia subclass in interpreting ejecta kinematics in both models and observations.
Author(s): Hakobyan A.A.; Gevorgyan M.H.; Karapetyan A.G.; Mamon G.A.; Kunth D.,Adibekyan V.; Barkhudaryan L.V.
IVOA id: ivo://cds.vizier/j/mnras/546/f2281

NGC 7006's RR Lyrae physical properties

2026-03-02T20:04:21Z

Description: A 5-yr CCD photometric VI time series of NGC 7006 is employed to perform a detailed analysis of the known population of variable stars. In the process, we have corrected inconsistent classifications, sky coordinates and found 10 new cluster member variables. An independent reddening estimate with a value E(B-V) = 0.08 +/- 0.05 is made. Using Fourier decompositions of RR Lyrae light curves and well-established calibrations, the cluster mean metallicity and distance [Fe/H]ZW = -1.53 +/- 0.15 and 41.2 +/- 1.4 kpc are estimated based on an extended sample of cluster member RRab stars. Using the Gaia DR3 data, we performed an extensive membership analysis that leads to a clean colour-magnitude diagram, and hence to the identification of variables that are likely field stars, and to considerations on the variable distribution in the horizontal branch (HB). A double-mode RR Lyrae and three CW stars are discussed. The origin of CW stars from precursors in the blue tail of the HB with very thin (~0.06 +/- 0.01 M_{Sun}_) envelopes is argued. Our models indicate that the main-sequence predecessor of RR Lyrae stars had a mass of 0.82-0.85 M_{Sun}_ and lost about 25-35 per cent of its mass during the red giant branch events before settling in the HB some 12-13.5 Gyr later.
Author(s): Arellano Ferro A.; Rojas Galindo F.C.; Bustos Fierro I.H.; Muneer S.,Yepez M.A.; Giridhar S.
IVOA id: ivo://cds.vizier/j/mnras/519/2451

Binary stars from LRS LAMOST DR10 & Gaia DR3

2026-03-02T20:03:40Z

Description: Binary stars are prevalent yet challenging to detect. We present a novel approach using convolutional neural networks (CNNs) to identify binary stars from low-resolution spectra obtained by the LAMOST survey. The CNN is trained on a data set that distinguishes binaries from single main-sequence stars based on their positions on the Hertzsprung-Russell diagram. Specifically, the training data labels stars with mass ratios between approximately 0.71 and 0.93 as intermediate-mass-ratio binaries, while excluding those beyond this range. The network achieves high accuracy with an area under the receiver operating characteristic curve of 0.949 on the test set. Its performance is further validated against known eclipsing binaries (97% detection rate) and binary stars identified by radial velocity variations (92% detection rate). Applying the trained CNN to a sample of one million main-sequence stars from LAMOST DR10 and Gaia DR3 yields a catalog of 468,634 binary stars, which are mainly intermediate-mass-ratio binaries given the training data. This catalog includes 115 binary stars located beyond 10 kpc from the Sun and 128 crossmatched with known exoplanet hosts from the NASA Exoplanet Archive. This new catalog provides a valuable resource for future research on the properties, formation, and evolution of binary systems, particularly for statistically characterizing large populations.
Author(s): Jing Y.; Mao T.-X.; Wang J.; Liu C.; Chen X.
IVOA id: ivo://cds.vizier/j/apjs/277/15

APOKASC-3: evolved KIC stars with APOGEE

2026-03-02T20:03:38Z

Description: In the third APOKASC catalog, we present data for the complete sample of 15,808 evolved stars with APOGEE spectroscopic parameters and Kepler asteroseismology. We used 10 independent asteroseismic analysis techniques and anchor our system on fundamental radii derived from Gaia L and spectroscopic Teff. We provide evolutionary state, asteroseismic surface gravity, mass, radius, age, and the data used to derive them for 12,418 stars. This includes 10,036 exceptionally precise measurements, with median fractional uncertainties in {nu}_max_, {Delta}{nu}, mass, radius, and age of 0.6%, 0.6%, 3.8%, 1.8%, and 11.1%, respectively. We provide more limited data for 1624 additional stars that either have lower-quality data or are outside of our primary calibration domain. Using lower red giant branch (RGB) stars, we find a median age for the chemical thick disk of 9.14+/-0.05(ran) +/-0.9(sys) Gyr with an age dispersion of 1.1Gyr, consistent with our error model. We calibrate our red clump (RC) mass loss to derive an age consistent with the lower RGB and provide asymptotic GB and RGB ages for luminous stars. We also find a sharp upper-age boundary in the chemical thin disk. We find that scaling relations are precise and accurate on the lower RGB and RC, but they become more model dependent for more luminous giants and break down at the tip of the RGB. We recommend the use of multiple methods, calibration to a fundamental scale, and the use of stellar models to interpret frequency spacings.
Author(s): Pinsonneault M.H.; Zinn J.C.; Tayar J.; Serenelli A.; Garcia R.A.,Mathur S.; Vrard M.; Elsworth Y.P.; Mosser B.; Stello D.; Bell K.J.,Bugnet L.; Corsaro E.; Gaulme P.; Hekker S.; Hon M.; Huber D.,Kallinger T.; Cao K.; Johnson J.A.; Liagre B.; Patton R.A.; Santos A.R.G.,Basu S.; Beck P.G.; Beers T.C.; Chaplin W.J.; Cunha K.; Frinchaboy P.M.,Girardi L.; Godoy-Rivera D.; Holtzman J.A.; Jonsson H.; Meszaros S.,Reyes C.; Rix H.-W.; Shetrone M.; Smith V.V.; Spoo T.; Stassun K.G.,Wang Ji
IVOA id: ivo://cds.vizier/j/apjs/276/69

PS1-MDS supernovae classifications

2026-03-02T20:03:36Z

Description: With the advent of the Vera C. Rubin Observatory, the discovery rate of supernovae (SNe) will surpass the rate of SNe with real time spectroscopic follow-up by 3 orders of magnitude. Accurate photometric classifiers are essential to both select interesting events for follow-up in real time and for archival population-level studies. In this work, we investigate the impact of observable host-galaxy information on the classification of SNe, both with and without additional light-curve and redshift information. We find that host-galaxy information alone can successfully isolate relatively pure (>90%) samples of Type Ia SNe with or without redshift information. With redshift information, we can additionally produce somewhat pure (>70%) samples of Type II SNe and superluminous SNe. Additionally with redshift information, host- galaxy properties do not significantly improve the accuracy of SN classification when paired with complete light curves. In the absence of redshift information, however, galaxy properties significantly increase the accuracy of photometric classification. As a part of this analysis, we present the first formal application of a new objective function, the weighted hierarchical cross entropy, to the problem of SN classification. This objective function more naturally accounts for the hierarchical nature of SN classes and, more broadly, transients. Finally, we present a new set of SN classifications for the Pan-STARRS Medium Deep Survey of SNe that lack spectroscopic redshift, increasing the full photometric sample to >4400 events.
Author(s): Villar V.A.; Gomez S.; Berger E.; Gagliano A.
IVOA id: ivo://cds.vizier/j/apjs/276/3

The EMP star SPLUS J142445.34-254247.1 with GHOST

2026-03-02T20:03:10Z

Description: We report on a chemo-dynamical analysis of SPLUS J142445.34-254247.1 (SPLUS J1424-2542), an extremely metal-poor halo star enhanced in elements formed by the rapid neutron-capture process (r-process). This star was first selected as a metal-poor candidate from its narrowband S-PLUS photometry and followed up spectroscopically in medium resolution with Gemini-South/GMOS, which confirmed its low-metallicity status. High-resolution spectroscopy was gathered with GHOST at Gemini-South, allowing for the determination of the chemical abundances for 36 elements, from carbon to thorium. At [Fe/H]=-3.39, SPLUS J1424-2542 is one of the lowest-metallicity stars with measured Th and has the highest log{epsilon}(Th/Eu) observed to date, making it part of the "actinide-boost" category of r-process-enhanced stars. The analysis presented here suggests that the gas cloud from which SPLUS_J1424-2542 formed must have been enriched by at least two progenitor populations. The light-element (Z<=30) abundance pattern is consistent with the yields from a supernova explosion of metal-free stars with 11.3-13.4M_{sun}_, and the heavy-element (Z>=38) abundance pattern can be reproduced by the yields from a neutron star merger (1.66M_{sun}_ and 1.27M_{sun}_) event. A kinematical analysis also reveals that SPLUS J1424-2542 is a low-mass, old halo star with a likely in situ origin, not associated with any known early merger events in the Milky Way.
Author(s): Placco V.M.; Almeida-Fernandes F.; Holmbeck E.M.; Roederer I.U.,Mardini M.K.; Hayes C.R.; Venn K.; Chiboucas K.; Deibert E.; Gamen R.,Heo J.-E.; Jeong M.; Kalari V.; Martioli E.; Xu S.; Diaz R.,Gomez-Jimenez M.; Henderson D.; Prado P.; Quiroz C.; Ruiz-Carmona R.,Simpson C.; Urrutia C.; McConnachie A.W.; Pazder J.; Burley G.,Ireland M.; Waller F.; Berg T.A.M.; Robertson J.G.; Hartman Z.,Jones D.O.; Labrie K.; Perez G.; Ridgway S.; Thomas-Osip J.
IVOA id: ivo://cds.vizier/j/apj/959/60

Warm Spitzer monitoring of RZ Psc

2026-03-02T20:03:08Z

Description: RZ Piscium (RZ Psc) is well known in the variable star field because of its numerous irregular optical dips in the past 5 decades, but the nature of the system is heavily debated in the literature. We present multiyear infrared monitoring data from Spitzer and WISE to track the activities of the inner debris production, revealing stochastic infrared variability as short as weekly timescales that is consistent with destroying a 90km sized asteroid every year. ALMA 1.3mm data combined with spectral energy distribution modeling show that the disk is compact (~0.1-13au radially) and lacks cold gas. The disk is found to be highly inclined and has a significant vertical scale height. These observations confirm that RZ Psc hosts a close to edge-on, highly perturbed debris disk possibly due to migration of recently formed giant planets that might be triggered by the low-mass companion RZ Psc B if the planets formed well beyond the snowlines.
Author(s): Su K.Y.L.; Kennedy G.M.; Rieke G.H.; Hughes A.M.; Lin Y.-C.; Kittling J.,Jackson A.P.; Anche R.M.; Liu H.B.
IVOA id: ivo://cds.vizier/j/apj/959/43

Kast and LRIS spectra of SNIa SN 2020hvf

2026-03-02T20:03:05Z

Description: We present nebular spectroscopy of SN 2020hvf, a Type Ia supernova (SNIa) with an early bump in its light curve. SN 2020hvf shares many spectroscopic and photometric similarities to the carbon-rich high-luminosity "03fg-like" SNe Ia. At >240 days after peak brightness, we detect unambiguous emission from [CaII] {lambda}{lambda}7291,7324, which is rarely observed in normal SNe Ia and only seen in peculiar subclasses. SN 2020hvf displays "sawtooth" emission profiles near 7300{AA} that cannot be explained with single symmetric velocity components of [FeII], [NiII], and [CaII], indicating an asymmetric explosion. The broad [CaII] emission is best modeled by two velocity components offset by 1220km/s, which could be caused by ejecta associated with each star in the progenitor system, separated by their orbital velocity. For the first time in an SN Ia, we identify narrow (FWHM=180{\pm}40km/s) [CaII] emission, which we associate with a wind from a surviving, puffed-up companion star. Few published spectra have sufficient resolution and the signal-to-noise ratio necessary to detect similar narrow [CaII] emission; however, we have detected similar line profiles in other 03fg-like SNe Ia. The extremely narrow velocity width of [CaII] has only otherwise been observed in SNe Iax at late times. Since this event likely had a double-degenerate "super-Chandrasekhar" mass progenitor system, we suggest that a single white dwarf (WD) was fully disrupted and a wind from a surviving companion WD is producing the observed narrow emission. It is unclear whether this unique progenitor and explosion scenario can explain the diversity of 03fg-like SNe Ia, potentially indicating that multiple progenitor channels contribute to this subclass.
Author(s): Siebert M.R.; Foley R.J.; Zenati Y.; Dimitriadis G.; Schmidt E.; Yang G.,Davis K.W.; Taggart K.; Rojas-Bravo C.
IVOA id: ivo://cds.vizier/j/apj/958/173

Spectroscopy study of nearby LOFAR M dwarfs

2026-03-02T20:01:25Z

Description: Recent observations with the LOw Frequency ARray (LOFAR) have revealed 19 nearby M dwarfs showing bright circularly polarised radio emission. One of the possible sources of such emission is through magnetic star-planet interactions (MSPI) with unseen close-in planets. We present initial results from a spectroscopic survey with the Habitable-zone Planet Finder (HPF) and NEID spectrographs designed to characterize this sample and further investigate the origin of the radio emission. We provide four new insights into the sample. I) We uniformly characterize the stellar properties, constraining their effective temperatures (Teff), surface gravities (logg), metallicities ([Fe/H]), projected rotational velocities (vsini*), rotation periods (Prot), stellar radii (R*), and stellar inclinations (i*) where possible. Further, from a homogenous analysis of the HPF spectra, we infer their chromospheric activity and spectroscopic multiplicity states. From this, we identify GJ 625, GJ 1151, and LHS 2395 as single, quiescent stars amenable to precise RV follow-up, making them strong MSPI candidates. II) We show that the distribution of stellar inclinations are compatible with an isotropic distribution, providing no evidence for a preference to pole-on configurations. III) We refine the radial velocity solution for GJ 625 b, the only currently known close-in planet in the sample, reducing the uncertainty in its orbital period by a factor of three, to facilitate future phase-dependent radio analysis. IV) Finally, we identify GJ 3861 as a spectroscopic binary with an orbital period of P=14.841181_-0.00010_^+0.00011^d and with a mass ratio of q=0.7663_-0.0018_^+0.0020^, making it the only confirmed binary with a relatively short orbit in the sample, where we surmise the radio emission is likely related to magnetospheric interactions between the two stars. These results advance our understanding of radio-emitting M dwarfs and establish an observational foundation for identifying MSPI.
Author(s): Koo E.; Stefansson G.; Kavanagh R.D.; Delamer M.; Mahadevan S.,Callingham J.R.; Vedantham H.; Robertson P.; Bruijne D.; Bender C.F.,Canas C.I.; Diddams S.; Espinoza-Retamal J.I.; Fernandes R.B.,Halverson S.; Kanodia S.; Krolikowski D.; Lin A.S.J.; Pope B.J.S.,Roy A.; Schwab C.; Terrien R.; Wright J.T.
IVOA id: ivo://cds.vizier/j/a+a/706/a98

AT2019aalc as a TDE in an AGN

2026-03-02T20:01:20Z

Description: To date, three nuclear transients have been associated with high-energy neutrino events. These transients are generally thought to be powered by tidal disruptions of stars (TDEs) by massive black holes. However, AT2019aalc, hosted in a Seyfert-1 galaxy, was not yet classified due to a lack of multiwavelength observations. Interestingly, the source has re-brightened 4 years after its discovery.To date, three nuclear transients have been associated with high-energy neutrino events. These transients are generally thought to be powered by tidal disruptions of stars (TDEs) by massive black holes. However, AT2019aalc, hosted in a Seyfert-1 galaxy, was not yet classified due to a lack of multiwavelength observations. Interestingly, the source has re-brightened 4 years after its discovery. Our aim is to constrain the physical mechanism responsible for the second optical flare, which may also provide clues to the origin of the initial event. We conducted a multi-wavelength monitoring program (from radio to X-rays) of AT2019aalc during its re-brightening in 2023/2024. The observations revealed multiple X-ray flares during the second optical flaring episode of the transient and a uniquely bright UV counterpart. The second flare, similarly to the first one, is also accompanied by IR dust echo emission. A long-term radio flare is found with an inverted spectrum. Optical spectroscopic observations reveal the presence of Bowen Fluorescence lines and strong high-ionization coronal lines indicating an extreme level of ionization in the system. The results suggest that the transient can be classified as a Bowen Fluorescence Flare (BFF), a relatively new sub-class of flaring active galactic nuclei (AGN). AT2019aalc can be also classified as an extreme coronal line emitter (ECLE). We found that, in addition to AT2019aalc, another BFF AT2021loi is spatially coincident with a high-energy neutrino event. We propose a repeating TDE scenario within an AGN framework to explain the multi-wavelength properties of AT2019aalc and suggest a possible connection among ECLEs, BFFs, and TDEs occurring in AGNs.
Author(s): Veres P.M.; Franckowiak A.; van Velzen S.; Adebahr B.; Taziaux S.,Necker J.; Stein R.; Kier A.; Mueller A.; Bomans D.J.; Jordana-Mitjans N.,Kowalski M.; Hammerstein E.; Marci-Boehncke E.; Reusch S.; Garrappa S.,Rose S.; Kashyap Das K.
IVOA id: ivo://cds.vizier/j/a+a/706/a324

Detection limits in the SHINE F150 survey

2026-03-02T20:01:18Z

Description: In high-contrast imaging, a novel detection algorithm for angular differential imaging (ADI) sequences has recently been introduced: the Regime Switching Model (RSM). This advanced statistical tool enhances the distinction between planetary signals and bright speckles by simultaneously combining multiple ADI-based post-processing techniques. In this study, we apply the RSM algorithm to analyze the F150 sample from the SHINE high-contrast imaging survey carried out with VLT/SPHERE, aiming to enhance detection limits and identify new exoplanet candidates. Additionally, we investigate how environmental conditions influence post-processed noise distributions and detection thresholds. We generate detection maps and contrast curves for 213 observations in the F150 SHINE sample using the RSM algorithm. A clustering approach based on environmental parameters is used to group observations with similar noise characteristics. We propose two methods for defining radial detection thresholds in the RSM maps: fitting a log-normal distribution to the post-processed noise and maximizing the F1 score. We also assess the performance of various combinations of post-processing techniques within the RSM framework to identify optimal configurations. This study demonstrates the utility of clustering based on observational parameters, effectively distinguishing features like wind-driven halos and low-wind effects. Detection thresholds vary significantly across clusters, differing by up to a factor of 10, highlighting the importance of considering observational environments. Log-normal thresholds provide conservative, noise-aware limits, while F1 score-based thresholds offer observation-specific results, both showing compatibility overall. RSM improves detection limits by an average factor of two at arcsec and five at inner working angles compared to standard PCA processing. This study reports more than 30 newly detected signals, including one promising candidate awaiting second-epoch confirmation.
Author(s): Sabalbal M.; Absil O.; Dahlqvist C.-H.; Delorme P.
IVOA id: ivo://cds.vizier/j/a+a/706/a275

Sample of Hertzsprung gap sources

2026-03-02T20:01:16Z

Description: Mass transfer between stars in binary systems profoundly impacts their evolution, yet many aspects of this process (especially the stability, mass loss, and eventual fate of such systems) remain poorly understood. One promising avenue to constrain these processes is through the identification and characterisation of systems undergoing active mass transfer. Inspired by the slow brightening preceding stellar merger transients, we worked on a method to identify Galactic mass-transferring binaries in which the donor is a Hertzsprung gap star. We constructed an initial sample of Hertzsprung gap stars using the Gaia EDR3 contribution Starhorse catalogue, and we identified candidate mass-transferring systems by selecting sources that exhibit Balmer emission features (as seen in the low-resolution Gaia XP spectra), mid-infrared excess (from WISE photometry), and photometric variability (inferred from the error in the Gaia G-band magnitude). This multi-criteria selection yielded a sample of 67 candidates, which we further analysed using complementary photometric and spectroscopic data, as well as information from cross-matched archival catalogues. Among our candidates, we identified at least nine eclipsing binaries and some sources that are potential binaries as well. Three sources in our sample are strong candidates for mass-transferring binaries with a yellow component, and three more are binaries with a Be star. Notably, three sources in our sample are strong candidates for hosting a compact companion, based on their ultraviolet or X-ray signatures. The main sources of contamination in our search are hot but highly reddened stars (primarily Oe and Be stars) as well as regular pulsating stars such as delta Scuti and Cepheid variables. As an additional outcome of this work, we present a refined new catalogue of 308 Hertzsprung gap stars, selected using improved extinction corrections and stricter emission-line criteria. This enhanced sample is expected to contain a significantly higher fraction of scientifically valuable mass-transferring binaries.
Author(s): Garcia-Moreno G.; Blagorodnova N.; Anders F.; Weiler M.; Wichern H.,Britavskiy N.; de Wet S.
IVOA id: ivo://cds.vizier/j/a+a/706/a249

HARPS-N 10yrs precise solar radial velocities

2026-03-02T20:01:15Z

Description: The HARPS-N solar telescope has been observing the Sun every possible day since the summer of 2015. We recently released 10 years of these data, which are available online.The goal of this manuscript is to present the different optimisations made to the ESPRESSO data reduction software used to extract the published HARPS-N solar spectra, to describe data curation, and to perform some analyses that demonstrate the extreme RV precision of those data. By analysing all the HARPS-N wavelength solutions over 13 years, we bring to light instrumental systematics at the 1ms level. We mitigate those systematics by curating the thorium line list used to derive the wavelength solution, and by applying a correction to the drift of thorium lines induced by the aging of thorium-argon hollow cathode lamps. After optimisation, we demonstrate a peak-to-peak precision on the HARPS-N wavelength solution better than 0.75ms over 13 years. We then carefully curate the decade of HARPS-N re-reduced solar observations by rejecting 30% of the data affected either by clouds, bad atmospheric conditions} or well-understood instrumental systematics. Finally, we correct the curated data for spurious sub-\ms RV effects caused by erroneous instrumental drift measurements and by changes in the spectral blaze function over time. After curation and correction, a total of 109466 HARPS-N solar spectra and respective RVs over a decade are available. The median photon-noise precision of the RV data is 0.28ms and, on daily timescales, the median RV rms is 0.49ms, similar to the level imposed by stellar granulation signals. On 10-year timescales, the large RV rms of 2.95\ms results from the RV signature of the Sun's magnetic cycle. When modeling this long-term effect using the Bremen Composite Magnesium II activity index, we demonstrate a long-term RV precision of 0.41ms. We also analysed contemporaneous HARPS-N and NEID solar RVs and found the data from both instruments to be of similar quality and precision. However, an analysis of the RV difference between these two RV datasets over the three available years gives a surprisingly large RV rms of 1.3ms. This variation is dominated by an unexplained trend that could be caused by a different sensitivity to stellar activity of the two datasets. Once this trend is modeled, the overall RV rms for three years reaches 0.79ms, and the RV rms during the low activity phase decreases to 0.6ms, compatible with what is expected from supergranulation. This decade of high-cadence HARPS-N solar observations with short- and long-term precision below 1ms represents a crucial dataset for further understanding stellar activity signals in solar-type stars and to advance other science cases requiring such extreme precision.
Author(s): Dumusque X.; Al Moulla K.; Cretignier M.; Buchschacher N.; Segransan D.,Phillips D.F.; Affer L.; Aigrain S.; John A.A.; Bonomo A.S.; Bourrier V.,Buchhave L.A.; Collier Cameron A.; Cegla H.M.; Cortes-Zuleta P.,Cosentino R.; Costes J.; Damasso M.; de Beurs Z.L; Ehrenreich D.,Ghedina A.; Gonzales M.; Haywood R.D.; Klein B.; Lakeland B.S.,Langellier N.; Latham D.W.; Leleu A.; Lodi M.; Lopez-Morales M.; Lovis C.,Malavolta L.; Maldonado J.; Mantovan G.; Matinez Fiorenzano A.F.,Micela G.; Milbourne T.; Molinari E.; Mortier A.; Naponiello L.,Nicholson B.A.; O'Sullivan N.K.; Pepe F.; Pinamonti M.; Piotto G.,Rescigno F.; Rice K.; Dimitar S.; Silva A.M.; Sozzetti A.; Stalport M.,Tavella S.; Udry S.; Vanderburg A.; Vissapragada S.; Watson C.A.
IVOA id: ivo://cds.vizier/j/a+a/706/a231

Pristine survey. XXVIII.

2026-03-02T20:01:13Z

Description: The outer Galactic halo remains relatively unexplored, particularly regarding its metallicity distribution, merger debris, and the population of very and extremely metal-poor ([Fe/H]<-2.5) stars. Using photometric metallicities from the Pristine survey data release 1 (PDR1) and Pristine- synthetic (PGS) catalogue and DR3 astrometry, we constructed well-characterised samples of bright (G<17.6) red giant branch (RGB) stars in the outer halo. With accurate distances, these samples enable studies of the halo's metallicity distribution, accreted debris, and very metal-poor (VMP) substructures beyond 40 kpc. We selected giants by excluding stars with reliable parallaxes in brightness ranges where dwarfs are measurable. Purity and completeness were validated against the Pristine spectroscopic training set. Distances were derived using BaSTI isochrone fitting combined with Pristine metallicity estimates. The photometric distances reach ~100kpc (PDR1) and ~70kpc (PGS), with typical uncertainties of 12% and scatter up to 20-40% compared to parallax- and StarHorse-based distances. The PDR1 sample provides a nearly unbiased metallicity-distance view, while the PGS sample offers an all-sky map, especially at the very metal-poor end. Using PDR1-giants, we traced the halo metallicity distribution function out to 101 kpc, fitting a three-component Gaussian mixture model. The most metal-poor component becomes increasingly dominant with distance, as beyond 50kpc, 40-50% of the stars are very metal-poor ([Fe/H]<-2.0). With added radial velocities, we identified metallicity trends in integrals-of-motion space and investigated accreted debris. The PGS sample reveals substructures, including the Pisces Plume, where 41 VMP stars are linked to the Magellanic stream. We publish two RGB catalogues: PDR1-giants (180314 stars, with 10096 very metal-poor candidates and 2096 beyond 40kpc) and PGS-giants (2420898 stars, with 75679 very metal-poor candidates and 267 beyond 40kpc). These catalogues represent extensive resources for future outer halo studies.
Author(s): Viswanathan A.; Bystroem A.; Starkenburg E.; Foppen A.; Straat J.,Montelius M.; Sestito F.; Venn K.A.; Navarrete C.; Matsuno T.; Martin N.F.,Thomas G.F.; Ardern-Arentsen A.; Battaglia G.; Fouesneau M.; Navarro J.,Vitali S.
IVOA id: ivo://cds.vizier/j/a+a/706/a195

Euclid. ERO. IC 10 and NGC 6822

2026-03-02T20:01:11Z

Description: Star clusters are valuable indicators of galaxy evolution, offering insights into the buildup of stellar populations across cosmic time. Understanding the intrinsic star cluster populations of dwarf galaxies is particularly important given these systems' role in the hierarchical growth of larger systems. We use data from Euclid's Early Release Observation programme to study star clusters in two star-forming dwarf irregular galaxies in the Local Group, NGC 6822 and IC 10 [M*~(1-4)x10^8^M_{sun}_]. With Euclid, star clusters are resolved into individual stars across the main bodies and haloes of both galaxies. Through visual inspection of the IE images, we uncover 30 new star cluster candidates in NGC 6822 and 16 in IC 10, ranging from compact to diffuse extended clusters. We compile and re-evaluate previously identified literature candidates, resulting in final combined catalogues of 52 (NGC 6822) and 71 (IC 10) cluster candidates with confidence-based classifications. We present homogeneous photometry in IE, YE, JE, and HE, and in archival UBVRI data, alongside size measurements and properties derived from the spectral energy distribution fitting code BAGPIPES. Through synthetic cluster injection, we conclude our sample is ~50% complete to M<~10^3^M_{sun}_ for ages <~100Myr, and to M<~2x10^4^M_{sun}_ for ages of ~10Gyr. We find that IC 10 has more young clusters than NGC 6822, and its young clusters extend to higher masses, consistent with its starburst nature. We find several old massive (>~10^5^M_{sun}_) clusters in both dwarfs, including an exceptional cluster in NGC 6822's outskirts with a mass of 1.3x10^6^M_{sun}_, nearly twice as massive as any other old cluster in either galaxy. In NGC 6822, we also identify a previously undetected, old, and extended cluster (R_h_=12.4+/-0.11pc). Using well-defined criteria, we identify 11 candidate GCs in NGC 6822 and nine in IC 10. Both galaxies have high specific frequencies (S_N) for their luminosities but remain consistent with the known GC scaling relationships in the low-luminosity regime.
Author(s): Howell J.M.; Ferguson A.M.N.; Larsen S.; Lancon A.; Annibali F.,Cuillandre J.-C.; Hunt L.K.; Martinez-Delgado D.; Massari D.; Saifollahi T.,Voggel K.; Altieri B.; Andreon S.; Auricchio N.; Baccigalupi C.; Baldi M.,Bardelli S.; Biviano A.; Branchini E.; Brescia M.; Brinchmann J.; Camera S.,Canas-Herrera G.; Candini G.P.; Capobianco V.; Carbone C.; Carretero J.,Castellano M.; Castignani G.; Cavuoti S.; Cimatti A.; Colodro-Conde C.,Congedo G.; Conselice C.J.; Conversi L.; Copin Y.; Courbin F.; Courtois H.M.,Cropper M.; Da Silva A.; Degaudenzi H.; De Lucia G.; Dubath F.,Duncan C.A.J.; Dupac X.; Dusini S.; Escoffier S.; Farina M.; Farinelli R.,Faustini F.; Ferriol S.; Finelli F.; Frailis M.; Franceschi E.; Fumana M.,Galeotta S.; George K.; Gillis B.; Giocoli C.; Gracia-Carpio J.; Grazian A.,Grupp F.; Haugan S.V.H.; Hoekstra H.; Holmes W.; Hormuth F.; Hornstrup A.,Jahnke K.; Jhabvala M.; Keihaenen E.; Kermiche S.; Kubik B.; Kuemmel M.,Kunz M.; Kurki-Suonio H.; Le Brun A.M.C.; Le Mignant D.; Ligori S.,Lilje P.B.; Lindholm V.; Lloro I.; Mainetti G.; Maino D.; Maiorano E.,Mansutti O.; Marggraf O.; Martinelli M.; Martinet N.; Marulli F.,Massey R.J.; Medinaceli E.; Mei S.; Melchior M.; Mellier Y.; Meneghetti M.,Merlin E.; Meylan G.; Mora A.; Moresco M.; Moscardini L.; Nakajima R.,Neissner C.; Niemi S.-M.; Padilla C.; Paltani S.; Pasian F.; Pedersen K.,Percival W.J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.; Popa L.A.,Raison F.; Renzi A.; Rhodes J.; Riccio G.; Romelli E.; Roncarelli M.,Saglia R.; Sakr Z.; Sapone D.; Sartoris B.; Schirmer M.; Schneider P.,Schrabback T.; Secroun A.; Seidel G.; Serrano S.; Simon P.; Sirignano C.,Sirri G.; Skottfelt J.; Stanco L.; Steinwagner J.; Tallada-Crespi P.,Taylor A.N.; Teplitz H.I.; Tereno I.; Toft S.; Toledo-Moreo R.,Torradeflot F.; Tutusaus I.; Valenziano L.; Valiviita J.; Vassallo T.,Wang Y.; Weller J.; Zamorani G.; Zinchenko I.A.; Martin-Fleitas J.,Scottez V.
IVOA id: ivo://cds.vizier/j/a+a/706/a185

SN 2021efd, SN 2019tsf photometry and spectra

2026-03-02T20:01:10Z

Description: Stripped-envelope supernovae (SESNe), including Type IIb, Ib, and Ic supernovae (SNe), originate from the explosions of massive stars whose outer envelopes have been largely removed during their lifetimes. The main stripping mechanism for the hydrogen (H) envelope in the progenitors of SESNe is often considered to be interaction with a binary companion, while that for the helium (He) layer is unclear. We study the process of the He-layer stripping in the progenitors of SESNe, which is closely related to the origin of their diverse observational properties. We conducted photometric and spectroscopic observations of the Type Ib SN 2021efd, which shows signs of interaction with H-free circumstellar material (CSM). At early phases, its photometric and spectroscopic properties resemble those of typical Type Ib SNe. Around 30 days after the r-band light curve (LC) peak, until at least ~770 days, the multi-band LCs display excessive luminosity compared to regular SESNe and at least three distinct peaks. The light curve evolution is similar to that of SN 2019tsf, whose previously unpublished spectrum at 400 days is also presented here. The nebular spectrum of SN 2021efd shows narrow emission lines (~1000km/s) in various species, such as OI, CaII, MgII, HeI, [OI], [CaII], and [SII]. Based on the observations, we studied the properties of the ejecta and CSM of SN 2021efd. Our observations suggest that SN 2021efd is a Type Ib SN interacting with CSM with the following parameters: The estimated ejecta mass, explosion energy, and 56Ni-56 mass are 2.2M_{sun}_, 9.1*10^50 erg, of 0.14M_{sun}_, respectively, while the estimated CSM mass, composition, and distribution are at least a few times 0.1M_{sun}_, H-free, and clumpy, respectively. Based on the estimated ejecta properties, we conclude that this event is a transitional SN whose progenitor was experiencing He-layer stripping at the epoch of the explosion, and was on the way to becoming a carbon-oxygen star (as the progenitors of Type Ic SNe) from a He star (as the progenitors of Type Ib SNe). The estimated CSM properties suggest that the progenitor had some episodic mass ejections with the rate of ~0.005-0.01M_{sun}_/yr for the last decade and slightly smaller before this final phase at least from ~200 years before the explosion, for the assumed CSM velocity of 100km/s. For the case of ~1000km/s, the necessary mass-loss rate would be increased by a factor of ten, and the timescales decreased by a factor of ten.
Author(s): Pyykkinen N.; Nagao T.; Kuncarayakti H.; Stritzinger M.D.; Kangas T.,Maeda K.; Chen P.; Sollerman J.; Burns C.; Bose S.; Folatelli G.,Ferrari L.; Morrell N.; Reguitti A.; Salmaso I.; Mattila S.; Gal-Yam A.,Fremling C.; Anand S.; Kasliwal M.; Gutierrez C.P.; Galbany L.,Hoogendam W.; Schulze S.; Ashall C.; Medler K.; Pfeffer C.M.; Lundqvist P.,Rusholme B.; Adler J.
IVOA id: ivo://cds.vizier/j/a+a/706/a183

MW GCs physical parameters with OrbIT code

2026-03-02T20:01:08Z

Description: In hierarchical structure formation, the content of a galaxy is determined both by its in-situ processes and by material added via accretions. Globular clusters in particular represent a window for the study of the different merger events that a galaxy underwent. Establishing the correct classification of in-situ and accreted tracers, and distinguishing the various different progenitors that contributed to the accreted population are important tools to deepen our understanding of galactic formation and evolution. Our aim is to refine our knowledge of the assembly history of the Milky Way by studying the dynamics of its globular cluster population and establishing an updated classification among in-situ objects and the different merger events identified. We used a custom built orbit integrator to derive precise orbital parameters, integrals of motions and adiabatic invariants for the globular cluster sample studied. By properly accounting for the rotating bar, which transforms the underlying model in a time-varying potential, we proceeded to a complete dynamical characterisation of the globular clusters. We present a new catalogue of clear associations between globular clusters and structures (both in-situ and accreted) in the Milky Way, and a full table of derived parameters. By using all dynamical information available, we were able to attribute previously unassociated or misclassified globular clusters to the different progenitors, including those responsible for the Aleph, Antaeus, Cetus, Elqui, and Typhon merger events. By using a custom built orbit integrator and properly accounting for the time-varying nature of the Milky Way potential, we have shown the depth of information that can be extracted from a purely dynamical analysis of the globular clusters of our Galaxy. By merging our dynamical analysis with complementary chronochemical studies, we will be able to uncover the remaining secrets of the accretion history of the Milky Way.
Author(s): De Leo M.; Zoccali M.; Olivares-Carvajal J.; Acosta-Tripailao B.; Gran F.,Contreras-Ramos R.
IVOA id: ivo://cds.vizier/j/a+a/706/a130

LDN 1495 free-floating planetary mass objects

2026-03-02T20:01:03Z

Description: Substellar objects, including brown dwarfs and free-floating planetary-mass objects, are a significant product of star formation. Their sensitivity to initial conditions and early dynamical evolution makes them especially valuable for studying both planetary and stellar formation processes. We search for brown dwarfs and isolated planetary mass objects in a young star forming region to better constrain their formation mechanisms. We take advantage of Euclid unprecedented sensitivity, spatial resolution and wide-field of view to search for brown dwarfs and free-floating planetary mass objects in the LDN 1495 region of the Taurus molecular clouds. We combine the recent Euclid Early Release Observations with older very deep ground-based images obtained over more than 20 yr to derive proper motions and multi-wavelength photometry, and select members based on their morphology and their position in a proper motion diagram and in 9 color-magnitude diagrams. We identify 15 point sources with proper motions, colors, and luminosity consistent with being members of LDN 1495. Six of these objects were already known M9-L1 members. The remaining nine are newly identified sources that could have spectral types ranging from late-M to early-T with masses potentially as low as 1~2M_Jup_ based on their luminosity and according to evolutionary models. However, follow-up observations are needed to confirm their nature, spectral type and membership. If extrapolated to the entire Taurus star forming region, this result suggests the potential presence of several dozen free-floating planetary mass objects.
Author(s): Bouy H.; Martin E.L.; Cuillandre J.-C.; Barrado D.; Tamura M.; Bertin E.M.,Zerjal; Points S.; Olivares J.; Huelamo N.; Rodrigues T.
IVOA id: ivo://cds.vizier/j/a+a/696/a80

HERMES Data Archive Portal

2026-03-02T11:13:49Z

Description

High resolution spectra from the HERMES spectrograph at the Flemish
Mercator Telescope, operated by KU Leuven at the Roque de Los
Muchachos Observatory on the island of La Palma. HERMES (High
Efficiency and Resolution Mercator Echelle Spectrograph) covers the
377-900 nm wavelength range in one fixed setting.

Author(s)

Prins, S.; Dirickx, M.; Van Winckel, H.; Raskin, G.

IVOA id

ivo://mercator/hermes/q/ssa

PACS Point Source Catalog: Observation Table

2026-03-02T10:00:00Z

Description: To maximise the science return of the PACS data sets, a homogeneous Herschel/PACS Point Source Catalogue (HPPSC) was constructed from all the scan map observations. The catalogue enables a systematic and unbiased comparison of sensitivity across different Herschel fields that single programs will generally not be able to provide.
Author(s): PPSC Team
IVOA id: ivo://irsa.ipac/herschel/catalog/ppsc/ppsc_obstbl

2MASS Full Survey Image Atlas

2026-03-02T10:00:00Z

Description: Photometric calibration for 2MASS was performed using observations of calibration fields made at regular intervals during each night of survey operations. Measurements of standard stars in the fields were used to derive the photometric zero point offsets as a function of time during each night. Atmospheric extinction coefficients were derived from 2MASS observations made over long periods. 2MASS calibration fields, or tiles, are 1° long in declination and approximately 8.5' wide in right ascension. There are 35 regular survey calibration fields distributed at approximately two hour intervals in right ascension near declinations of approximately -30°, 0° and +30°. An additional five calibration fields were defined in and around the Large and Small Magellanic Clouds to support the deep observation (6x) campaign towards the end of survey operations. Calibration scan Atlas Images, and Point and Extended Source Working Databases (Cal-PSWDB and Cal-XSWDB), analogous to those from the main survey, were produced from the calibration scan pipeline data reduction.
Author(s): 2MASS Team
IVOA id: ivo://irsa.ipac/2mass/images/full

2MASS Long Exposure (6x) Image Atlas

2026-03-02T10:00:00Z

Description

During the final months of 2MASS observatory operations, a campaign of targeted "long exposure" observations was carried out during times when no previously unscanned parts of the sky were available for the main survey. These observations used the same freeze-frame scanning technique employed for the survey, but with READ2-READ1 exposures six times longer than was used for normal survey observations (hence they are referred to as "6x" observations). The 2MASS 6x measurements were intended to probe ~1 magnitude deeper than the main survey in unconfused regions.

Approximately 590 deg2 of sky distributed in 30 targeted regions were scanned at least once using the long exposures. Most of this area is concentrated in two large, comprehensive surveys of the Large and Small Magellanic Clouds, 383 deg2 and 127 deg2, respectively. Twenty-eight additional smaller fields were mapped in the 6x mode from both observatories, covering targets that include the Pleiades open cluster, galactic star formation complexes, M31, nearby galaxy clusters and the Lockman Hole.

Author(s)

IRSA

IVOA id

ivo://irsa.ipac/2mass/images/sixxcat

2MASS Calibration Image Atlas

2026-03-02T10:00:00Z

Description: Photometric calibration for 2MASS was performed using observations of calibration fields made at regular intervals during each night of survey operations. Measurements of standard stars in the fields were used to derive the photometric zero point offsets as a function of time during each night. Atmospheric extinction coefficients were derived from 2MASS observations made over long periods. 2MASS calibration fields, or tiles, are 1° long in declination and approximately 8.5' wide in right ascension. There are 35 regular survey calibration fields distributed at approximately two hour intervals in right ascension near declinations of approximately -30°, 0° and +30°. An additional five calibration fields were defined in and around the Large and Small Magellanic Clouds to support the deep observation (6x) campaign towards the end of survey operations. Calibration scan Atlas Images, and Point and Extended Source Working Databases (Cal-PSWDB and Cal-XSWDB), analogous to those from the main survey, were produced from the calibration scan pipeline data reduction.
Author(s): 2MASS Team
IVOA id: ivo://irsa.ipac/2mass/images/cal

AKARI-HSC Band-Merged Catalog in the North Ecliptic Pole Wide Field

2026-03-02T10:00:00Z

Description: The North Ecliptic Pole field is a natural deep-field location for many satellite observations. It has been targeted many times since it was surveyed by the AKARI space telescope with its unique wavelength coverage from the near- to mid-infrared (mid-IR). Many follow-up observations have been carried out, making this field one of the most frequently observed areas with a variety of facilities, accumulating abundant panchromatic data from the X-ray to the radio wavelength range. Recently, a deep optical survey with the Hyper Suprime-Cam (HSC) at the Subaru telescope covered the NEP-Wide (NEPW) field, which enabled Kim et al. (2021) to identify faint sources in the near- and mid-IR bands, and to improve the photometric redshift (photo-z) estimation. The AKARI-HSC Band-Merged Catalog in the NEPW Field contains multiband photometry for 91,861 AKARI sources observed over the NEPW field. It combines various photometric data from the GALEX UV to submillimetre (sub-mm) bands (e.g. Herschel/SPIRE, JCMT/SCUBA-2). About 20 000 AKARI sources are newly matched to the HSC data, most of which seem to be faint galaxies in the near- to mid-infrared AKARI bands.
Author(s): Kim et al.
IVOA id: ivo://irsa.ipac/akari/catalog/akarinepw

z0MGS_Dust Catalog

2026-03-02T10:00:00Z

Description: The z0MGS_Dust project consists of Herschel images from PACS and SPIRE available for 1578 galaxies, dust emission parameters for 819 galaxies, and integrated photometry and dust parameters for 877 galaxies. The final catalog used in this study uses WISE and Herschel data to derive interstellar dust parameters and scaling relations with other galactic information such as stellar mass, star formation rate, and related values.
Author(s): Chastenet et al.
IVOA id: ivo://irsa.ipac/herschel/catalogs/z0mgs_dust

Hi-GAL 360 degree Catalogue of Clump Physical Properties

2026-03-02T10:00:00Z

Description: Hi-GAL compact sources detected between 70 and 500 microns are presented in this catalog, covering the full 360 degrees of Galactic longitude.
Author(s): Hi-GAL team
IVOA id: ivo://irsa.ipac/herschel/catalog/hi-gal/hi-gal360clump

PACS Point Source Catalog: 100 microns

2026-03-02T10:00:00Z

Description: To maximise the science return of the PACS data sets, a homogeneous Herschel/PACS Point Source Catalogue (HPPSC) was constructed from all the scan map observations. The catalogue enables a systematic and unbiased comparison of sensitivity across different Herschel fields that single programs will generally not be able to provide.
Author(s): PPSC Team
IVOA id: ivo://irsa.ipac/herschel/catalog/ppsc/ppsc100

PACS Point Source Catalog: 160 microns

2026-03-02T10:00:00Z

Description: To maximise the science return of the PACS data sets, a homogeneous Herschel/PACS Point Source Catalogue (HPPSC) was constructed from all the scan map observations. The catalogue enables a systematic and unbiased comparison of sensitivity across different Herschel fields that single programs will generally not be able to provide.
Author(s): PPSC Team
IVOA id: ivo://irsa.ipac/herschel/catalog/ppsc/ppsc160

PACS Point Source Catalog: Rejected Source List

2026-03-02T10:00:00Z

Description: To maximise the science return of the PACS data sets, a homogeneous Herschel/PACS Point Source Catalogue (HPPSC) was constructed from all the scan map observations. The catalogue enables a systematic and unbiased comparison of sensitivity across different Herschel fields that single programs will generally not be able to provide.
Author(s): PPSC Team
IVOA id: ivo://irsa.ipac/herschel/catalog/ppsc/ppsc_rejsl

PACS Point Source Catalog: Extended Source List

2026-03-02T10:00:00Z

Description: To maximise the science return of the PACS data sets, a homogeneous Herschel/PACS Point Source Catalogue (HPPSC) was constructed from all the scan map observations. The catalogue enables a systematic and unbiased comparison of sensitivity across different Herschel fields that single programs will generally not be able to provide.
Author(s): PPSC Team
IVOA id: ivo://irsa.ipac/herschel/catalog/ppsc/ppsc_extsl

PACS Point Source Catalog: 70 microns

2026-03-02T10:00:00Z

Description: To maximise the science return of the PACS data sets, a homogeneous Herschel/PACS Point Source Catalogue (HPPSC) was constructed from all the scan map observations. The catalogue enables a systematic and unbiased comparison of sensitivity across different Herschel fields that single programs will generally not be able to provide.
Author(s): PPSC Team
IVOA id: ivo://irsa.ipac/herschel/catalog/ppsc/ppsc70

WISE All-Sky Image Atlas

2026-03-02T10:00:00Z

Description

The Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010, AJ, 140, 1868) is a NASA Medium Class Explorer mission that conducted a digital imaging survey of the entire sky in the 3.4, 4.6, 12 and 22 um mid-infrared bandpasses (hereafter W1, W2, W3 and W4). WISE produced and released to the world astronomical and educational communities and general public a digital Image Atlas covering the sky in the four survey bands, and a reliable Source Catalog containing accurate photometry and astrometry for over 500 million objects. 

The WISE Image Atlas is comprised of 18,240 4095x4095 pix @1.375"/pix FITS format image sets. One image set is produced for each Atlas Tile. Each image set consists of four intensity images, four depth of coverage maps, and four uncertainty maps.

Author(s)

WISE Team

IVOA id

ivo://irsa.ipac/wise/images/allsky

WISE 3-Band Cryo Image Atlas

2026-03-02T10:00:00Z

Description

NASA's Wide-field Infrared Survey Explorer (WISE; Wright et al. 2010) mapped the sky at 3.4, 4.6, 12, and 22 um (W1, W2, W3, W4) in 2010 with an angular resolution of 6.1", 6.4", 6.5", & 12.0" in the four bands. During the full cryogenic survey phase, 7 January 2010 to 6 August 2010, when the detectors and telescope were cooled by solid hydrogen in both inner and outer cryogen tanks, WISE achieved 5 sigma point source sensitivities better than 0.08, 0.11, 1 and 6 mJy in unconfused regions on the ecliptic in the four bands. The sky was covered 1.2 times during this period, and the data acquired were used to construct the products for the March 2012 WISE All-Sky Data Release.

The WISE 3-Band Cryo survey phase began on 6 August 2010 following the exhaustion of frozen hydrogen in the payload's outer cryogen tank. WISE scanned approximately 30% of the sky over the next 54 days while the focal planes were cooled by hydrogen ice in the inner cryogen tank. The telescope warmed from the 12 K maintained during the main mission to 45 K. Imaging data in the 3.4, 4.6 and 12 um bands were acquired, but elevated thermal emission from the telescope prevented useful data from being collected in the 22 um band. As illustrated in Figures 1 and 2, the 3-Band Cryo 3.4 and 4.6 um band measurements are nearly as sensitive as those in the full cryogenic survey, but the increasing temperature and reduced exposure times of the 12 um measurements result in significantly lower sensitivity.

Author(s)

WISE Team

IVOA id

ivo://irsa.ipac/wise/images/3bandcryo

Euclid ERO

2026-03-02T10:00:00Z

Description: The ERO program is an initiative of the Euclid Science Team / ESA to collect 1 day of observations to showcase the Euclid mission and its capabilities before the start of the nominal survey. The ERO data products available at IRSA for the convenience of the US astronomy community are the same data products that are available through ESAC. The FITS files were processed with an ERO-specific pipeline, which is different from the standard Euclid pipeline that will be used for future data releases.
Author(s): Euclid ERO Teams
IVOA id: ivo://irsa.ipac/euclid/images/ero