VO Fresh

V432 Dra UBVRI(RI)c light curves

2026-08-21T12:58:49Z

Description: A little-studied eclipsing star with an elliptical orbit, V432 Dra (V=12.23mag, P=11.63 days, e=0.37, F8 V + F8 V) turned out to be a relatively young system with accelerated apsidal rotation. The following absolute parameters of the component stars were obtained for the first time: T1=6240+/-40K, M1=1.13+/-0.05M_{sun}_, R1=1.10+/-0.02R_{sun}_, T2 = 6215+/-40K, M2=1.12+/-0.05M_{sun}_, R2=1.09+/-0.02R_{sun}_. The relativistic contribution to the apsidal rotation is six times greater than the classical effect, but the observed apsidal period Paps = 13060+/-190 yrs is more than three times shorter than the theoretical value. The photometric parallax of pi=0.00197" (d=507pc) is based on the Gaia value. In evolutionary diagrams, the system is near the Zero Age Main Sequence at an age of 700 mln yrs and shows a metal deficiency of [Fe/H]=-0.17.
Author(s): Volkova A.S.; Volkov I.M.; Naroenkov S.A.
IVOA id: ivo://cds.vizier/j/other/arep/70.461

Euclid. Convective-transition gap of 47 Tuc

2026-08-21T07:46:41Z

Description: We report the first detection of the `convective-transition gap' (also known as the `M-dwarf gap') in the globular cluster 47 Tuc (NGC 104). This feature, linked to a change in the physical properties of late-type dwarfs, has remained elusive, with only two detections so far. Leveraging the large number of stars, high resolution, and photometric precision enabled by Euclid, we detected a statistically significant, sharp discontinuity in the main-sequence luminosity function of 47 Tuc at I_E_~22.9, which we identify as the convective-transition gap. A comparison of the observed properties of the gap in 47 Tuc with theoretical models shows how the gap can be a powerful diagnostic for probing the internal chemical structure of globular clusters and their multiple stellar populations. Following its initial discovery in the metal-poor cluster NGC 6397, the identification of a convective gap in the metal-rich 47 Tuc suggests that this feature is more general than previously thought. These results demonstrate that Euclid can be transformative well beyond cosmology, with impacts across multiple areas of astrophysics, including resolved stellar populations.
Author(s): Libralato M.; Griggio M.; Gerasimov R.; Bedin L.R.; McDonald I.; Altieri B.,Anderson J.; Annibali F.; Balbinot E.; Battaglia G.; Bellini A.,Casenove P.; Cuillandre J.-C.; Dalessandro E.; Ferguson A.M.N.,Jones H.R.A.; Kuijken K.; Majidi F.Z.; Massari D.; Mohandasan A.,Niederhofer F.; Polenta G.; Sakowska J.D.; Soldano F.; Zerbinati C.,Andreon S.; Auricchio N.; Aussel H.; Baccigalupi C.; Baldi M.; Balestra A.,Battaglia P.; Biviano A.; Branchini E.; Brescia M.; Camera S.,Capobianco V.; Carbone C.; Carretero J.; Castellano M.; Castignani G.,Cavuoti S.; Chambers K.C.; Cimatti A.; Colodro-Conde C.; Congedo G.,Conselice C.J.; Conversi L.; Copin Y.; Courbin F.; Courtois H.M.,Cropper M.; Degaudenzi H.; De Lucia G.; Dole H.; Dubath F.; Dupac X.,Farina M.; Farinelli R.; Faustini F.; Ferriol S.; Frailis M.; Franceschi E.,Galeotta S.; George K.; Gillis B.; Giocoli C.; Gracia-Carpio J.; Grazian A.,Grupp F.; Haugan S.V.H.; Hoekstra H.; Holmes W.; Hook I.M.; Hormuth F.,Hornstrup A.; Jahnke K.; Jhabvala M.; Kermiche S.; Kiessling A.; Kubik B.,Kummel M.; Kunz M.; Kurki-Suonio H.; Le Brun A.M.C.; Ligori S.; Lilje P.B.,Lindholm V.; Lloro I.; Mansutti O.; Marggraf O.; Martinelli M.; Martinet N.,Marulli F.; Massey R.J.; Medinaceli E.; Mei S.; Meneghetti M.; Merlin E.,Meylan G.; Mora A.; Moscardini L.; Nakajima R.; Nichol R.C.; Niemi S.-M.,Padilla C.; Paltani S.; Pasian F.; Percival W.J.; Pettorino V.; Poncet M.,Popa L.A.; Raison F.; Renzi A.; Rhodes J.; Riccio G.; Rizzo F.; Romelli E.,Roncarelli M.; Saglia R.; Sakr Z.; Sapone D.; Schirmer M.; Schneider P.,Schrabback T.; Secroun A.; Sihvola E.; Simon P.; Sirignano C.; Sirri G.,Stanco L.; Tallada-Cresp'i P.; Taylor A.N.; Tereno I.; Toft S.,Toledo-Moreo R.; Torradeflot F.; Tutusaus I.; Valiviita J.; Vassallo T.,Wang Y.; Weller J.; Scott D.
IVOA id: ivo://cds.vizier/j/a+a/712/a174

Euclid Q1 strong gravitational lens

2026-08-21T07:27:07Z

Description: We present an end-to-end, iterative pipeline for efficient identification of strong galaxy-galaxy lensing systems, applied to the Euclid Q1 imaging data. Starting from VIS catalogues, we reject point sources, apply a magnitude cut (IE<=24) on deflectors, and run a pixel-level artefact/noise filter to build 96x96 pix cutouts; VIS+NISP colour composites are constructed with a VIS-anchored luminance scheme that preserves VIS morphology and NISP colour contrast. A VIS-only seed classifier supplies clear positives and typical impostors, from which we curate a morphology-balanced negative set and augment scarce positives. Among the six compact CNNs studied initially, a modified VGG16 (GlobalAveragePooling + 256/128 dense layers with the last nine layers trainable) performs best; the training set grows from 27 seed lenses (augmented 67x to 1809) plus 2000 negatives to a colour dataset of 30686 images. After three rounds of iterative fine-tuning, human grading of the top 4000 candidates ranked by the final model yields 441 Grade A/B candidate lensing systems, including 311 overlapping with the existing Q1 strong-lens catalogue, and 130 additional A/B candidates (9 As and 121 Bs) not previously reported. Independently, the model recovers 740 out of 905 (81.8%) candidate Q1 lenses within its top 20000 predictions, considering off-centred samples. Candidates span IE~17-24 AB mag (median 21.3 AB mag) and are redder in YE-HE than the parent population, consistent with massive early-type deflectors. Each training iteration required about a week for a small team, and the approach easily scales to future wide-area Euclid releases; future work will calibrate the selection function via lens injection, extend recall through uncertainty-aware active learning, and explore multi-scale or attention-based neural networks with fast post-hoc vetters that incorporate lens models into the classification.
Author(s): Euclid Coll.; Xu X.; Chen R.; Li T.; Cooray A.R.; Schuldt S.,Acevedo Barroso J.A.; Stern D.; Scott D.; Meneghetti M.; Despali G.,Chopra J.; Cao Y.; Cheng M.; Buda J.; Zhang J.; Furumizo J.; Valencia R.,Jiang Z.; Tortora C.; Lines N.E.P.; Collett T.E.; Fotopoulou S.; Galan A.,Manjon-Garcia A.; Gavazzi R.; Iwamoto L.; Kruk S.; Millon M.; Nugent P.,Saulder C.; Sluse D.; Wilde J.; Walmsley M.; Courbin F.; Metcalf R.B.,Altieri B.; Amara A.; Andreon S.; Auricchio N.; Baccigalupi C.; Baldi M.,Balestra A.; Bardelli S.; Battaglia P.; Bender R.; Biviano A.; Branchini E.,Brescia M.; Camera S.; Capobianco V.; Carbone C.; Cardone V.F.,Carretero J.; Casas S.; Castellano M.; Castignani G.; Cavuoti S.,Cimatti A.; Colodro-Conde C.; Congedo G.; Conselice C.J.; Conversi L.,Copin Y.; Courtois H.M.; Cropper M.; Da Silva A.; Degaudenzi H.,De Lucia G.; Dolding C.; Dole H.; Dubath F.; Dupac X.; Dusini S.,Escoffier S.; Farina M.; Farinelli R.; Farrens S.; Ferriol S.; Finelli F.,Fosalba P.; Frailis M.; Franceschi E.; Fumana M.; Galeotta S.; George K.,Gillard W.; Gillis B.; Giocoli C.; Gomez-Alvarez P.; Gracia-Carpio J.,Grazian A.; Grupp F.; Haugan S.V.H.; Holmes W.; Hormuth F.; Hornstrup A.,Jahnke K.; Jhabvala M.; Joachimi B.; Kermiche S.; Kiessling A.; Kubik B.,Kuemmel M.; Kunz M.; Kurki-Suonio H.; Le Brun A.M.C.; Ligori S.,Lilje P.B.; Lindholm V.; Lloro I.; Mainetti G.; Maiorano E.; Mansutti O.,Marcin S.; Marggraf O.; Martinelli M.; Martinet N.; Marulli F.; Massey R.J.,Medinaceli E.; Mei S.; Melchior M.; Merlin E.; Meylan G.; Mora A.,Moresco M.; Moscardini L.; Nakajima R.; Neissner C.; Nichol R.C.,Niemi S.-M.; Nightingale J.W.; Padilla C.; Paltani S.; Pasian F.,Pedersen K.; Percival W.J.; Pettorino V.; 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.; Schirmer M.; Schneider P.; Schrabback T.,Secroun A.; Seidel G.; Sihvola E.; Simon P.; Sirignano C.; Sirri G.,Stanco L.; Tallada-Crespi P.; Taylor A.N.; Tereno I.; Tessore N.; Toft S.,Toledo-Moreo R.; Torradeflot F.; Tutusaus I.; Valenziano L.; Valiviita J.,Vassallo T.; Verdoes Kleijn G.; Veropalumbo A.; Wang Y.; Weller J.,Zacchei A.; Zamorani G.; Zerbi F.M.; Zucca E.; Ballardini M.; Bolzonella M.,Burigana C.; Cabanac R.; Calabrese M.; Cappi A.; Castro T.,Escartin Vigo J.A.; Gabarra L.; Hemmati S.; Macias-Perez J.; Maoli R.,Martin-Fleitas J.; Mauri N.; Monaco P.; Nucita A.A.; Pezzotta A.,Poentinen M.; Risso I.; Scottez V.; Sereno M.; Tenti M.; Tucci M.; Viel M.,Wiesmann M.; Akrami Y.; Andika I.T.; Angora G.; Anselmi S.; Archidiacono M.,Atrio-Barandela F.; Bazzanini L.; Bergamini P.; Bertacca D.; Bethermin M.,Beutler F.; Blot L.; Borgani S.; Brown M.L.; Bruton S.; Calabro A.,Camacho Quevedo B.; Caro F.; Carvalho C.S.; Cogato F.; Conseil S.,Cucciati O.; Davini S.; Desprez G.; Diaz-Sanchez A.; Di Domizio S.,Diego J.M.; Duc P.-A.; Duret V.; Elkhashab M.Y.; Enia A.; Fang Y.,Finoguenov A.; Franco A.; Ganga K.; Gasparetto T.; Gaztanaga E.,Giacomini F.; Gianotti F.; Gozaliasl G.; Guidi M.; Gutierrez C.M.; Hall A.,Hernandez-Monteagudo C.; Hildebrandt H.; Hjorth J.; Kajava J.J.E.; Kang Y.,Kansal V.; Karagiannis D.; Kiiveri K.; Kim J.; Kirkpatrick C.C.; Lepori F.,Leroy G.; Lesci G.F.; Lesgourgues J.; Liaudat T.I.; Liu S.J.,Magliocchetti M.; Magnier E.A.; Mannucci F.; Martins C.J.A.P.; Maurin L.,Miluzio M.; Moretti C.; Morgante G.; Naidoo K.; Navarro-Alsina A.,Nesseris S.; Paoletti D.; Passalacqua F.; Paterson K.; Patrizii L.,Pisani A.; Potter D.; Pratt G.W.; Quai S.; Radovich M.; Rojas K.; Roster W.,Sacquegna S.; Sahlen M.; Sanders D.B.; Sarpa E.; Scarlata C.; Schneider A.,Schultheis M.; Sciotti D.; Sellentin E.; Smith L.C.; Tanidis K.; Tao C.,Tarsitano F.; Testera G.; Teyssier R.; Tosi S.; Troja A.; Venhola A.,Vergani D.; Vernardos G.; Verza G.; Vinciguerra S.; Walton N.A.,Wright A.H.; Yeung H.W.
IVOA id: ivo://cds.vizier/j/a+a/712/a207

AMS-02 All Particle Rates Catalog

2026-08-21T00:00:00Z

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

2026-08-21T00:00:00Z

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

2026-08-21T00:00:00Z

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)

2026-08-21T00:00:00Z

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

AGN flares from ZTF DR23

2026-08-20T14:11:23Z

Description: Active galactic nuclei (AGNs) are known to exhibit stochastic variability across a wide range of timescales and wavelengths. AGN flares are extreme outbursts that deviate from this typical behavior and may trace a range of energetic physical processes. Using 6yr of data from Zwicky Transient Facility Data Release 23, we conduct a systematic search for AGN flares among a sample of well-sampled AGNs and AGN candidates. We construct two catalogs: the AGN Flare Coarse Catalog, containing 28,504 flares identified via Bayesian blocks and Gaussian processes, and the AGN Flare Refined Catalog, comprising 1984 high-confidence flares selected using stricter criteria. We analyze their spatial distribution, temporal characteristics, host-AGN type, and potential origins. Some flares can be associated with known supernovae, tidal disruption events, or blazars, and a few may be linked to binary black hole mergers or microlensing events.
Author(s): He L.; Liu Z.-Y.; Niu R.; Zhou M.-S.; Zou P.-R.; Gao B.-Z.; Liang R.-D.,Zhu L.-G.; Wang J.-M.; Jiang N.; Cai Z.-Y.; Jiang J.-A.; Dai Z.-G.,Yuan Y.-F.; Chen Y.-J.; Zhao W.
IVOA id: ivo://cds.vizier/j/apjs/282/13

HI dwarf galaxies in FASHI with DECaLS DR9 phot.

2026-08-20T12:58:04Z

Description: We present a sample of low HI mass (M_HI_<10^8^M_{sun}_) dwarf galaxies detected by The FAST All Sky HI Survey (FASHI) project. Due to the faint and irregular morphology of these galaxies, the default photometry is often inaccurate. Therefore, we utilized The Dark Energy Camera Legacy Survey data to perform careful photometric measurements, and find that the low HI mass galaxies have similar stellar mass densities to dwarf elliptical galaxies. Compared to other dwarf galaxy populations, the HI-selected dwarfs exhibit higher stellar mass densities than ultradiffuse galaxies, and similar densities to HI-selected low-surface-brightness galaxies, albeit with lower stellar masses, suggesting a possible evolutionary connection among these populations. By classifying the galaxies according to their HI spectral-line profiles, we show that the double-peaked sources conform closely to the Tully-Fisher relation, whereas the single-peaked sources follow the Faber-Jackson relation but with large scatter. This indicates that the single-peaked systems are likely dispersion dominated and that the relationship between stellar mass and halo mass in such systems may remain consistent across both low- and high- mass regimes. These findings suggest that HI-selected dwarf galaxies with single-peaked HI profiles may share a similar dynamical state with massive ellipticals, offering new insights into their structural evolution and the diversity of formation pathways for low-mass galaxies.
Author(s): Cheng C.; Huang J.-S.; Du W.; Zhang H.-X.; Zhang C.-P.; Zhu M.,Orellana G.
IVOA id: ivo://cds.vizier/j/apjs/281/66

Optical photometry & sp. of type IIn SN2021qqp

2026-08-20T12:09:50Z

Description: We present optical photometry and spectroscopy of the Type IIn supernova (SN) 2021qqp. Its unusual light curve is marked by a long precursor for ~300d, a rapid increase in brightness for ~60d, and then a sharp increase of ~1.6mag in only a few days to a first peak of Mr~-19.5mag. The light curve then declines rapidly until it rebrightens to a second distinct peak of Mr~-17.3mag centered at ~335d after the first peak. The spectra are dominated by Balmer lines with a complex morphology, including a narrow component with a width of ~1300km/s (first peak) and ~2500km/s (second peak) that we associate with the circumstellar medium (CSM) and a P Cygni component with an absorption velocity of ~8500km/s (first peak) and ~5600km/s (second peak) that we associate with the SN-CSM interaction shell. Using the luminosity and velocity evolution, we construct a flexible analytical model, finding two significant mass-loss episodes with peak mass loss rates of ~10 and ~5M_{sun}_/yr about 0.8 and 2yr before explosion, respectively, with a total CSM mass of ~2-4M_{sun}_. We show that the most recent mass-loss episode could explain the precursor for the year preceding the explosion. The SN ejecta mass is constrained to be ~5-30M_{sun}_ for an explosion energy of ~(3-10)x10^51^erg. We discuss eruptive massive stars (luminous blue variable, pulsational pair instability) and an extreme stellar merger with a compact object as possible progenitor channels.
Author(s): Hiramatsu D.; Matsumoto T.; Berger E.; Ransome C.; Villar V.A.; Gomez S.,Cendes Y.; De K.; Bostroem K.A.; Farah J.; Howell D.A.; McCully C.,Newsome M.; Padilla Gonzalez E.; Pellegrino C.; Suzuki A.; Terreran G.
IVOA id: ivo://cds.vizier/j/apj/964/181

r-band LCs of a doubly imaged lensed SDSS quasar

2026-08-20T09:20:44Z

Description: We analyze variability in 15-season optical lightcurves from the doubly imaged lensed quasar SDSS J165043.44+425149.3, comprising five seasons of monitoring data from the Maidanak Observatory (277 nights in total, including the two seasons of data previously presented in Vuissoz+ 2007A&A...464..845V), five seasons of overlapping data from the Mercator telescope (269 nights), and 12 seasons of monitoring data from the US Naval Observatory, Flagstaff Station at lower cadence (80 nights). We update the 2007 time-delay measurement for SDSS_J165043.44+425149.3 with these new data, finding a time delay of {Delta}t_AB_=-55.1_-3.7_^+4.0^days, with image A leading image B. We analyze the microlensing variability in these lightcurves using a Bayesian Monte Carlo technique to yield measurements of the size of the accretion disk at {lambda}_rest_=2420{AA}, finding a half-light radius of log(r1/2/cm)=16.19_-0.58_^+0.38^ assuming a 60{deg} inclination angle. This result is unchanged if we model 30% flux contamination from the broad-line region. We use the width of the MgII line in the existing Sloan Digital Sky Survey spectra to estimate the mass of this system's supermassive black hole, finding M_BH_=2.47x10^9^M_{sun}_. We confirm that the accretion disk size in this system, whose black hole mass is on the very high end of the MBH scale, is fully consistent with the existing quasar accretion disk size-black hole mass relation.
Author(s): Rivera A.B.; Morgan C.W.; Florence S.M.; Kniezewski K.; Millon M.,Courbin F.; Dahm S.E.; Vrba F.J.; Tilleman T.M.; Cornachione M.A.,Asfandiyarov I.M.; Ehgamberdiev S.A.; Burkhonov O.A.
IVOA id: ivo://cds.vizier/j/apj/964/173

HST photometry of SNe in nearby galaxies

2026-08-20T09:02:20Z

Description: Over recent decades, robotic (or highly automated) searches for supernovae (SNe) have discovered several thousand events, many of them in quite nearby galaxies (distances <30Mpc). Most of these SNe, including some of the best-studied events to date, were found before maximum brightness and have associated with them extensive follow-up photometry and spectroscopy. Some of these discoveries are so-called "SN impostors," thought to be superoutbursts of luminous blue variable stars, although possibly a new, weak class of massive-star explosions. We conducted a Snapshot program with the Hubble Space Telescope (HST) and obtained images of the sites of 31 SNe and four impostors, to acquire late-time photometry through two filters. The primary aim of this project was to reveal the origin of any lingering energy for each event, whether it is the result of radioactive decay or, in some cases, ongoing late-time interaction of the SN shock with preexisting circumstellar matter, or the presence of a light echo. Alternatively, lingering faint light at the SN position may arise from an underlying stellar population (e.g., a host star cluster, companion star, or a chance alignment). The results from this study complement and extend those from Snapshot programs by various investigators in previous HST cycles.
Author(s): Baer-Way R.; DeGraw A.; Zheng W.; Van Dyk S.D.; Filippenko A.V.; Fox O.D.,Brink T.G.; Kelly P.L.; Smith N.; Vasylyev S.S.; de Jaeger T.; Zhang K.,Stegman S.; Ross T.; Yunus S.
IVOA id: ivo://cds.vizier/j/apj/964/172

N(HI) in the local interstellar medium

2026-08-19T14:33:11Z

Description: Obtaining a complete census of gas in the local interstellar medium (LISM; <100pc) is challenging given the limited available tracers of the warm, partially ionized medium. Medium- to high-resolution UV absorption spectroscopy toward individual nearby stars is the primary method used, and incomplete spatial sampling of this complex medium makes a global map of the material difficult. Using HI column density measurements derived from HI Ly{alpha} spectroscopy toward 164 stars inside 100pc, we have generated 2D spatially interpolated N(HI) maps for different distance shells. Based on the area-weighted sky averages, we find that sight lines inside 10pc typically have log_10_(N(HI)/cm^-2^)~17.9. For greater distance shells, log_10_(N(HI)/cm^-2^) increases to 18.3 (10-20pc), then to 18.4 (20-70pc), and finally to 18.6 (70-100pc). This last increase is likely associated with the detection of the Local Bubble boundary, thus making the plateau of column density from 20 to 70pc notable and suggestive of the rarity of warm LISM material beyond ~10-20pc. We estimate that the uncertainties associated with N(HI) values inferred from the interpolated sky maps are approximately inversely correlated with the number of samples in each distance shell, and are in the range of 0.20-0.48dex, compared to the 0.01-0.30dex typically determined from direct Ly{alpha} observations. We discuss the impact of these uncertainties on interstellar medium corrections of extreme-UV and Ly{alpha} observations for nearby stars. Denser spatial sampling of the sky via UV absorption spectroscopy of nearby stars is required to improve the accuracy of these N(HI) estimates.
Author(s): Youngblood A.; France K.; Koskinen T.; Mason J.P.; Redfield S.; Wood B.E.,Bourrier V.; dos Santos L.; Johns-Krull C.; King G.W.; Linsky J.L.,Peacock S.
IVOA id: ivo://cds.vizier/j/aj/170/342

MDW Halpha Sky Survey DR1

2026-08-19T08:04:26Z

Description: The Mittelman-di Cicco-Walker (MDW) H{alpha} Sky Survey is an autonomously operated all-sky narrowband (3nm) H{alpha} imaging survey. The survey was founded by amateur astronomers, and the northern sky (decl. >=0{deg}) is presented here in its second stage of refinement for academic use. Each 3.6 deg^2^ MDW field has 12 20 minutes individual exposures with a pixel scale of 3.2", a typical point-spread function of 6", and a stack point-source depth of 16-17 mag. The northern MDW Survey Data Release 1 (DR1) includes calibrated mean and individual images, star-removed mean fields, and point-source catalogs for all images matched to Data Release 1 of the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS1) and the INT Galactic Plane Survey. (All DR1 components are available at https://mdw.astro.columbia.edu. The catalogs are also made available in the AAS Journals Zenodo repository: doi:10.5281/zenodo.17307324.) Our initial study of H{alpha} filament widths finds a typical FWHM of 30"-45" in the Lyra region. The matched catalogs (with a median match distance of ~0.5"), combined with our distinctive narrowband photometry, are also used to identify H{alpha} variable and excess sources. These initial studies highlight some of the many scientific uses of the MDW H{alpha} survey.
Author(s): Aftab N.; Zhang X.; Walker S.; Di Cicco D.; Mittelman D.R.; Gupta S.,Saydjari A.K.; Putman M.; Schiminovich D.
IVOA id: ivo://cds.vizier/j/aj/171/17

Optical variability of jetted AGN

2026-08-19T07:04:18Z

Description: The variability characteristics of jetted active galactic nuclei (AGNs) serve as a powerful diagnostic tool for probing the physical mechanisms underlying accretion processes and jet formation in supermassive black holes. We used the jetted AGNs detected by the Fermi Large Area Telescope to study the origins of optical variability of jetted AGNs. Our main findings are that (1) jetted AGNs with efficient accretion exhibit significantly greater optical variability amplitudes than jetted AGNs with inefficient accretion. This result indicates that standard thin accretion disks produce stronger optical variability than advection-dominated accretion flows (ADAFs). (2) There is a significant positive correlation between optical variability amplitudes and radio luminosity, gamma-ray luminosity, X-ray luminosity, the synchrotron peak frequency luminosity, the inverse Compton peak frequency luminosity, and Compton dominance for jetted AGNs with inefficient accretion. In contrast, no significant correlation is found for jetted AGNs with efficient accretion. These results indicate that relativistic jets mainly drive the optical variability in jetted AGNs with inefficient accretion. (3) In the effective accretion mode, the variability amplitudes of jetted AGNs are inversely correlated with the accretion rate. In contrast, these amplitudes in the ineffective accretion mode are positively correlated with the accretion rate. These results suggest that in addition to relativistic jets, accretion rates also play a significant role in the optical variability of jetted AGNs with ineffective accretion. The trend of the correlation between optical amplitude and accretion rate depends on the mode of accretion.
Author(s): Chen Y.; Gudagger Q.; Fan J.; Xiong D.; Yu X.; Zhong X.; Guo X.,Ding N.; Yi T.
IVOA id: ivo://cds.vizier/j/a+a/712/a191

13 planets and brown dwarfs astrometry

2026-08-19T06:59:55Z

Description: Over the past decade, advances in high-contrast imaging instrumentation, coupled with extreme adaptive optics systems, have enabled the discovery of tens of planets and brown dwarfs orbiting at wide separations from their host stars (a>~10au). The existence of companions at these separations challenges current planet-formation paradigms, highlighting the importance of high- contrast imaging as the only technique capable of directly probing this region of planetary systems. In this paper, we present a survey of thirteen planets and brown dwarfs observed with VLT/SPHERE between June 2023 and July 2025. These data provide updated photometry in the 1.0-1.7um range and new high-precision astrometry, enabling tighter constraints on their orbital properties. We used the IRDIS subsystem to acquire dual-band H2H3 images ({lambda}_H2_=1.593um, {lambda}_H3_=1.667um) for all companions in our sample. For the three objects located within the IFS field of view (GQ Lup B, PZ Tel B, and HD 984 B), we additionally obtained low-resolution (R~50) near-infrared (0.96-1.34um) spectra. We combined our new astrometric measurements with those available in the literature to derive updated orbital solutions. The orbital fitting was performed using the orbitize! Python package. For CT Cha b, HIP 78530 B, HIP 64892 B, and RX J1609.5-2105 b, this work provides the first orbital solutions to date. We derived new photometry for all objects, which, when compared with field dwarfs in color-magnitude diagrams, indicates spectral types ranging from mid-M to mid-L. For the companions observed with IFS, their spectra are best matched by those of M6-M8.5 field dwarfs. Our updated orbital fits provide tighter constraints for nearly all companions and are consistent with non-circular orbits in all cases, potentially disfavoring core-accretion formation within their circumstellar disks.
Author(s): Bernardi A.; Zurlo A.; Lazzoni C.; Desidera S.; Mesa D.; Perez S.,Nogueira P.H.; Barbato D.; Dasgupta A.
IVOA id: ivo://cds.vizier/j/a+a/712/a190

SN 2024gy photometry and polarimetry

2026-08-18T15:15:53Z

Description: Type Ia supernovae (SNe Ia) are well-known standardisable candles, and are one of the main ways to measure the distance to their host galaxies. However, extinction due to interstellar dust causes objects to appear fainter and redder. Correcting for this requires estimating the amount of intervening material and how the extinction changes as a function of wavelength. We present and analyse optical and near-infrared data of the well-observed SN 2024gy and use these to compare different extinction estimation techniques, making use of photometric, spectroscopic, and polarimetric data. SN 2024gy is a normal SN Ia with high velocity (HV) components in SiII_{lambda}6355_ (phase<-10-days) and a particularly strong HV feature in the CaII near-infrared triplet (up to peak). Modelling SN 2024gy with TARDIS shows better matches with a double-detonation scenario compared to a delayed-detonation scenario due to a better match to the CaII HV component. A measurement of the stable Ni/Fe ratio however favours a delayed-detonation scenario. Host extinction estimates range from E(B-V)_host_=0.12+/-0.02mag (narrow interstellar absorption lines) to E(B-V)_host_=0.24+/-0.06mag (Lira law) with a mean of E(B-V)_host_=0.22+/-0.04mag, assuming R_V_=3.1. The spread between different methods highlights the challenge of accurately estimating the amount of extinction light suffers before being observed.
Author(s): Terwel J.H.; Maguire K.; O'Donnell C.; Pursiainen M.; Casasbuenas A.,Thiim Gadeberg J.; Godson B.; Harvey L.; Nobre Hauptmann B.; Koivisto N.,Liu C.; Shenoy S.; Grund Sorensen S.; Diaz Teodori M.A.; Guldberg Theil A.,Turkki M.; Alburai A.; Anderson J.; de Boer T.; Mueller Bravo T.; Burgaz U.,Chambers K.C.; Chen T.-W.; Duarte J.; Galbany L.; Gromadzki M.; Inserra C.,Johansson J.; Kim Y.-L.; Lowe T.; Magnier E.; Santos R.P.; Sollerman J.,Wainscoat R.; Young D.R.; Chen T.X.; Graham M.J.; Kasliwal M.M.,Masci F.J.; Purdum J.N.; Belkhodja I.
IVOA id: ivo://cds.vizier/j/a+a/712/a173

JWST light curves & transit depths of HAT-P-26b

2026-08-18T14:13:27Z

Description: We present the James Webb Space Telescope (JWST) transmission spectrum of the exoplanet HAT-P-26 b (18.6M_{Earth}_, 6.33R_{Earth}_), based on a single transit observed with the JWST NIRSpec G395H grating. We detect water vapor (ln(B)=4.1), carbon dioxide (ln(B)=85.6), and sulfur dioxide (ln(B)=13.5) with high confidence, along with marginal indications for hydrogen sulfide and carbon monoxide (ln(B)<0.5). The detection of SO_2_ in a warm super-Neptune-sized exoplanet (R_P_~6R_{Earth}_) bridges the gap between previous detections in hot Jupiters and sub-Neptunes, highlighting the role of disequilibrium photochemistry across a broad range of exoplanet atmospheres, including those cooler than 1000 K. Our precise measurements of carbon, oxygen, and sulfur indicate an atmospheric metallicity of ~10x solar and a subsolar C/O ratio. Retrieved molecular abundances are consistent within 2{sigma} with predictions from self-consistent models including photochemistry. The elevated CO2 abundance and possible H2S signal may also reflect sensitivities to the thermal structure, cloud properties, or additional disequilibrium processes such as vertical mixing. We compare the SO_2_ abundance in HAT-P-26 b with that of 10 other JWST-observed giant exoplanets, and find a correlation with atmospheric metallicity. The trend is consistent with the prediction from I. J. M. Crossfield, showing a steep rise in SO_2_ abundance at low metallicities, and a more gradual increase beyond 30x solar. This work is part of a series of studies by our JWST Telescope Scientist Team (JWST-TST), in which we use Guaranteed Time Observations to perform Deep Reconnaissance of Exoplanet Atmospheres through Multi-instrument Spectroscopy (DREAMS).
Author(s): Gressier A.; Batalha N.E.; Wogan N.; Alderson L.; Doud D.; Espinoza N.,MacDonald R.J.; Wakeford H.R.; Valenti J.A.; Lewis N.K.; Seager S.,Stevenson K.B.; Allen N.H.; Canas C.I.; Challener R.C.; Glidden A.,Huang J.; Lin Z.; Louie D.R.; Maguire C.; Mullens E.; Sotzen K.,Valentine D.; Clampin M.; Pueyo L.; van der Marel R.P.; Mountain C.M.
IVOA id: ivo://cds.vizier/j/aj/170/292

The eXtended Catalogue of Spectroscopic Binary Orbits

2026-08-18T14:05:52Z

Description: SBX originated from the migration of the SB9 catalogue, a project undertaken as part of Simon Alexandre's Master's thesis in Data Science at ULB in 2024/2025. This effort involved transferring the catalogue into a robust relational SQL database with well-defined constraints to guarantee data consistency and facilitate advanced querying capabilities. Enriched with high-precision astrometric data from Gaia DR3 and other external sources, SBX offers significantly improved completeness and accuracy in the positions and motions of astronomical objects. Today, the database is maintained by Simon Alexandre and Thibault Merle. A modern web interface, featuring intuitive search functions, orbital visualisations, and comprehensive data download options, has been developed to enhance accessibility and usability. The first release of SBX is online since 2025-06-24.
Author(s): Merle; T.; Jorissen; A.; Alexandre; S.; Desuter; J.; Loup; C.; Tokovinin; A.,Traven; G.; Van der Swaelmen; M.; Van Eck; S.; Van de Steene; G.,Southworth; J.; Sadowski; G.
IVOA id: ivo://cds.vizier/b/sbx

Hidden Monsters with SPHEREx. I.

2026-08-18T13:30:14Z

Description: Heavily reddened quasars (HRQs) are luminous, dust-obscured broad-line quasars thought to trace a short-lived phase of intense black hole growth and feedback. Previous studies have been limited by small sample sizes, which restricted robust statistical analyses of their properties. We expand the census of the most luminous HRQs to enable population-level studies, aiming to connect their spectral energy distributions (SEDs) to other luminous quasar populations and place them in the context of an evolutionary sequence for massive galaxy and black hole formation. We assembled multi-wavelength broadband photometry for the brightest (K_AB_<18mag) HRQ candidates and selected active galactic nucleus (AGN) candidates with red near-IR colours of (J-K)_AB_>1.6. We employed SPX spectrophotometry to confirm the HRQs and determine redshifts. Detailed SED fitting allowed us to compare these HRQs to other luminous quasar populations, including a control sample of hyper-luminous, unobscured unWISE-Gaia (Quaia) quasars, as well as luminous hot dust-obscured galaxies (hot DOGs). We confirm 76 new HRQs with redshifts of 1.5<z_sys_<3.9, dust-corrected optical continuum luminosities of log_10_({lambda}L_{lambda}(3000{AA}_[erg/s])>47.0, and line-of-sight extinctions of 0.4<E(B-V)<1.6 (A_V_~1-5mag). This more than doubles the number of confirmed HRQs at z_sys_>1.5 including the first 7 HRQs ever identified at z>3. A UV excess consistent with scattered quasar emission is detected in 76 per cent of SPX HRQs. We conclusively demonstrate that HRQs are hot-dust poor compared to blue quasars of similar luminosities and redshifts. We find that the 6um continuum luminosities of HRQs are systematically lower at fixed 3000{AA}, continuum luminosity relative to blue Quaia quasars, suggesting that HRQs are deficient in both hot and warm dust components. This combination of depleted torus-scale dust reservoirs and higher luminosities compared to hot DOGs and blue quasars supports a scenario in which HRQs represent a blow-out phase, when strong feedback has begun to clear the central regions of obscuring material.
Author(s): Stepney M.; Banerji M.; Bauer F.E.; Assef R.J.; Li G.
IVOA id: ivo://cds.vizier/j/a+a/712/a183

MiMO: 1232 Gaia DR3 open clusters param. & mass funct.

2026-08-18T12:45:53Z

Description: We present a homogeneous catalog of 1232 open clusters with precisely determined ages, metallicities, distances, extinctions, and stellar mass function (MF) slopes, derived from Gaia DR3 data. The parameters are inferred using the Mixture Model for Open clusters (MiMO), a novel Bayesian framework for modeling clusters in the color-magnitude diagram. By explicitly accounting for field-star contamination as a model component, MiMO removes the conventional need for stringent membership preselection, allowing for a more complete inclusion of member stars, and thereby enhancing both precision and robustness. Our results broadly agree with existing catalogs but offer improved precision. For each cluster, we provide the best-fit age, metallicity, distance, extinction, and MF slope, along with their full likelihood chains and photometric membership probabilities for individual stars. We further identify an "MF Prime" subsample of 163 clusters with high- quality data, for which the MF estimates are considered most reliable. The catalog and an open-source implementation of MiMO are made publicly available to the community.
Author(s): Li Lu; Shao Z.; Li Z.; Fu X.
IVOA id: ivo://cds.vizier/j/aj/170/288

2min TESS data vetting with Exominer++

2026-08-18T08:45:31Z

Description: We present ExoMiner++, an enhanced deep learning model that builds on the success of ExoMiner to improve transit signal classification in 2-minute TESS data. ExoMiner++ incorporates additional diagnostic inputs, including periodogram, flux trend, difference image, unfolded flux, and spacecraft attitude control data, all of which are crucial for effectively distinguishing transit signals from more challenging sources of false positives (FPs). To further enhance performance, we leverage multisource training by combining high-quality labeled data from the Kepler space telescope with TESS data. This approach mitigates the impact of TESS's noisier and more ambiguous labels. ExoMiner++ achieves high accuracy across various classification and ranking metrics, significantly narrowing the search space for follow-up investigations to confirm new planets. To serve the exoplanet community, we introduce a new TESS catalog containing ExoMiner++ classifications and confidence scores for each transit signal. Among the 147,568 unlabeled TCEs, ExoMiner++ identifies 7330 as planet candidates (PCs), with the remainder classified as FPs. These 7330 PCs correspond to 1868 existing TESS Objects of Interest (TOIs), 69 Community TESS Objects of Interest (CTOIs), and 50 newly introduced CTOIs. 1797 out of the 2506 TOIs previously labeled as PCs in ExoFOP are classified as PCs by ExoMiner++. This reduction in plausible candidates, combined with the excellent ranking quality of ExoMiner++, allows the follow-up efforts to be focused on the most likely candidates, increasing the overall planet yield.
Author(s): Valizadegan H.; Martinho M.J.S.; Jenkins J.M.; Twicken J.D.,Caldwell D.A.; Maynard P.; Wei H.; Zhong W.; Yates C.; Donald S.,Collins K.A.; Latham D.; Barkaoui K.; Calkins M.L.; Carden K.; Chazov N.,Esquerdo G.A.; Guillot T.; Krushinsky V.; Nowak G.; Rackham B.V.,Triaud A.; Schwarz R.P.; Stephens D.; Stockdale C.; Watkins C.N.,Wilkin F.P.
IVOA id: ivo://cds.vizier/j/aj/170/287

Euclid accretion properties of X-ray AGN

2026-08-18T08:03:15Z

Description: The Euclid Quick Data Release (Q1) is a powerful dataset to study active galactic nuclei (AGN) and their host galaxies. Deriving their physical properties through multi-component spectral energy distribution (SED) fitting is a challenging task for AGN, but it is greatly aided by the Euclid near-infrared photometry. Here we present a new method of quantifying the reliability of SED-derived parameters, such as AGN bolometric and monochromatic luminosities, host's stellar mass (M*), star-formation rate (SFR), and specific star-formation rate (sSFR), by using mock SEDs of AGN built by combining observed SEDs of QSOs and galaxies. We applied this methodology to the ~1 million Q1 AGN candidates, constructing a catalogue of AGN and host galaxy properties, alongside their respective reliability values. With a reliability threshold at 0.5, we find 88% of sources to have robust stellar masses and 76% to have reliable AGN luminosities. Moreover, through SED fitting we also measured the AGN fraction (fAGN) of the total mid-infrared flux and we used its lower-limit to select AGN. A f_AGN,ow_>0.075 threshold yields 85% completeness and purity. Comparable to colour-colour AGN selections, this method has the advantage of being less affected by redshift evolution and exploring fainter magnitudes. Additionally, by comparing the AGN and host galaxy parameters across different identification methods, we find that the probed range in stellar mass and AGN luminosity can be quite different. This highlights the importance of combining different approaches and accounting for their selection biases when studying AGN and their role in galaxy evolution. Finally, for the X-ray detected sample, we present the X-ray to mid-IR luminosity relation, and the correlation between stellar mass and bolometric luminosity as a function of redshift, in good agreement with previous results.
Author(s): Euclid Coll.; Laloux B.; Bongiorno A.; Salvato M.; Allevato V.; Mezcua M.,Roster W.; Matamoro Zatarain T.; Paltani S.; Shirley R.; Tarsitano F.,Saulder C.; Fotopoulou S.; Andonie C.; Buchner J.; La Franca F.; Le Brun V.,Ricci F.; Scott D.; Shankar F.; Siudek M.; Sorce J.G.; Spinoglio L.,Toba Y.; Viitanen A.; Wang L.; Zamorani G.; Andreon S.; Auricchio N.,Baccigalupi C.; Baldi M.; Balestra A.; Bardelli S.; Battaglia P.,Biviano A.; Branchini E.; Brescia M.; Camera S.; Canas-Herrera G.,Capobianco V.; Carbone C.; Carretero J.; Casas S.; Castellano M.,Castignani G.; Cavuoti S.; Chambers K.C.; Cimatti A.; Colodro-Conde C.,Congedo G.; Conselice C.J.; Conversi L.; Copin Y.; Costille A.; Courbin F.,Courtois H.M.; Cropper M.; Da Silva A.; Degaudenzi H.; De Lucia G.; Dole H.,Dubath F.; Duncan C.A.J.; Dupac X.; Escoffier S.; Fabricius M.; Farina M.,Farinelli R.; Ferriol S.; Finelli F.; Fosalba P.; Fourmanoit N.; Frailis M.,Franceschi E.; Fumana M.; Galeotta S.; George K.; Gillis B.; Giocoli C.,Gracia-Carpio J.; Grazian A.; Grupp F.; Gwyn S.; Haugan S.V.H.; Hoekstra H.,Holmes W.; Hormuth F.; Hornstrup A.; Jahnke K.; Jhabvala M.; Joachimi B.,Kermiche S.; Kiessling A.; Kubik B.; Kuemmel M.; Kunz M.; Kurki-Suonio H.,Le Brun A.M.C.; Ligori S.; Lilje P.B.; Lindholm V.; Lloro I.; Mainetti G.,Maino D.; Maiorano E.; Mansutti O.; Marcin S.; Marggraf O.; Martinelli M.,Martinet N.; Marulli F.; Massey R.J.; Medinaceli E.; Mei S.; Mellier Y.,Meneghetti M.; Merlin E.; Meylan G.; Mora A.; Moresco M.; Moscardini L.,Nakajima R.; Neissner C.; Nichol R.C.; Niemi S.-M.; Padilla C.; Pasian F.,Pedersen K.; Percival W.J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.,Popa L.A.; Pozzetti L.; Racca G.D.; Raison F.; Renzi A.; Rhodes J.,Riccio G.; Romelli E.; Roncarelli M.; Saglia R.; Sakr Z.; Sapone D.,Sartoris B.; Schneider P.; Schrabback T.; Scodeggio M.; Secroun A.,Seidel G.; Serrano S.; Sihvola E.; Simon P.; Sirignano C.; Sirri G.,Steinwagner J.; Tallada-Crespi P.; Taylor A.N.; Tereno I.; Tessore N.,Toft S.; Toledo-Moreo R.; Torradeflot F.; Tutusaus I.; Valenziano L.,Valiviita J.; Vassallo T.; Veropalumbo A.; Wang Y.; Weller J.; Zacchei A.,Zucca E.; Ballardini M.; Bolzonella M.; Bozzo E.; Burigana C.; Cabanac R.,Calabrese M.; Cappi A.; Castro T.; Escartin Vigo J.A.; Gabarra L.,Garcia-Bellido J.; Maoli R.; Martin-Fleitas J.; Maturi M.; Mauri N.,Metcalf R.B.; Pezzotta A.; Poentinen M.; Porciani C.; Risso I.; Scottez V.,Sereno M.; Tenti M.; Viel M.; Wiesmann M.; Akrami Y.; Andika I.T.,Angora G.; Anselmi S.; Archidiacono M.; Atrio-Barandela F.; Bazzanini L.,Bertacca D.; Bethermin M.; Bisigello L.; Blanchard A.; Blot L.; Bonici M.,Brown M.L.; Bruton S.; Calabro A.; Camacho Quevedo B.; Caro F.,Carvalho C.S.; Cogato F.; Conseil S.; Cooray A.R.; Davini S.; De Paolis F.,Desprez G.; Diaz-Sanchez A.; Di Domizio S.; Diego J.M.; Elkhashab M.Y.,Enia A.; Fang Y.; Finoguenov A.; Fontanot F.; Franco A.; Gasparetto T.,Gaztanaga E.; Giacomini F.; Gianotti F.; Gozaliasl G.; Guidi M.,Gutierrez C.M.; Hall A.; Hernandez-Monteagudo C.; Hildebrandt H.; Hjorth J.,Hunt L.K.; Kajava J.J.E.; Kang Y.; Kansal V.; Karagiannis D.; Kiiveri K.,Kim J.; Kirkpatrick C.C.; Kruk S.; Lattanzi M.; Legrand L.; Lepori F.,Leroy G.; Lesci G.F.; Lesgourgues J.; Leuzzi L.; Liaudat T.I.; Liu S.J.,Lopez Lopez X.; Macias-Perez J.; Magliocchetti M.; Magnier E.A.; Mancini C.,Manjon-Garcia A.; Mannucci F.; Martins C.J.A.P.; Maurin L.; Miluzio M.,Monaco P.; Montoro A.; Moretti C.; Morgante G.; Murray C.; Nadathur S.,Naidoo K.; Natoli P.; Navarro-Alsina A.; Nesseris S.; Paoletti D.,Passalacqua F.; Paterson K.; Pisani A.; Potter D.; Pratt G.W.; Quai S.,Radovich M.; Rodighiero G.; Rojas K.; Sacquegna S.; Sahlen M.; Sanders D.B.,Sarpa E.; Schneider A.; Sciotti D.; Sellentin E.; Smith L.C.; Tanidis K.,Tao C.; Testera G.; Teyssier R.; Tosi S.; Troja A.; Tucci M.; Venhola A.,Vergani D.; Verza G.; Vielzeuf P.; Vinciguerra S.; Walton N.A.
IVOA id: ivo://cds.vizier/j/a+a/712/a182

Solar System bodies cross-matches catalog

2026-08-17T11:38:30Z

Description: In this paper I will describe a new software package developed using the Java programming language, aimed to compute the positions of any Solar System body (among asteroids, comets, planets, and satellites) to help to perform cross-matches of them in observations taken from earth- and space-based observatories. The space telescopes supported are Hubble, James Webb, Euclid, XMM-Newton, Spitzer, Herschel, Gaia, Kepler, Chandra, and TESS, although the flexibility of the software allows to support any other mission without the need to change a single line of code. The orbital elements can be selected among the asteroid database from the Lowell observatory (completed with the cometpro database of comets maintained by the LTE), and the JPL database of minor bodies. The software does not depend on external tools, and performs its own numerical integration of minor bodies. The dynamical model implemented for the Solar System includes the gravity effects of all major bodies, including the Earth, Moon, and Pluto as individual bodies, 16 perturbing asteroids as in other tools, the General Relativity effects, the oblateness of the Sun, Earth, and Moon, and the non-gravitational forces for both comets and asteroids. A complete set of web services allow to compute the cross-matches (that are later to be confirmed, for instance by visual inspection of the images) and also ephemerides of specific bodies. The code is highly optimized and follows the highest standards in terms of software quality and documentation.
Author(s): Alonso-Albi; T.
IVOA id: ivo://cds.vizier/j/other/ac/52.968

172 TESS planet candidates passing LEO-Vetting

2026-08-17T09:15:24Z

Description: The Transiting Exoplanet Survey Satellite (TESS) has identified several thousand planet candidates orbiting a wide variety of stars, and has provided an exciting opportunity for demographic studies. However, current TESS planet searches require significant manual inspection efforts to identify planets among the enormous number of detected transit-like signatures, which limits the scope of such searches. Demographic studies also require a detailed understanding of the relationship between observed and true exoplanet populations, a task for which current TESS planet catalogs are rendered unsuitable by the subjectivity of vetting by eye. We present LEO-Vetter, a publicly available and fully automated exoplanet vetting system designed after the Kepler Robovetter, which is capable of efficiently producing catalogs of promising planet candidates and making statistically robust TESS demographic studies possible. LEO-Vetter implements flux- and pixel-level tests against noise/systematic false positives and astrophysical false positives. The vetter achieves high completeness (91%) and high reliability against noise/systematic false alarms (97%) based on its performance on simulated data. We demonstrate the usefulness of the vetter by searching ~200,000 M dwarf light curves, and reducing ~20,000 transit-like detections down to 172 uniformly vetted planet candidates. LEO-Vetter facilitates analyses that would otherwise be impractical to perform on all possible signals due to time constraints or computational limitations. Users will be able to efficiently produce their own TESS planet catalog starting with transit-like detections, as well as have the framework needed to characterize their catalog's completeness and reliability for occurrence rates.
Author(s): Kunimoto M.; Bryson S.; Jaffee D.; Rowe J.F.; Daylan T.; Giacalone S.,Lissauer J.J.; Matesic M.R.B.; Mullally S.E.; Eschen Y.N.E.
IVOA id: ivo://cds.vizier/j/aj/170/280

SRG/eROSITA All-Sky Survey DR2

2026-08-17T08:51:16Z

Description: The eROSITA telescope array on board the Spektrum-Roentgen-Gamma (SRG) mission began its all-sky survey program in December 2019, scanning the sky at an approximately six-month cadence. Here, we present new catalogues of point-like and extended X-ray sources derived from the first three completed eROSITA all-sky surveys (eRASS:3), covering the western Galactic hemisphere, which Germany's eROSITA consortium holds proprietary rights for. We describe the observational strategy, data processing, and analysis pipelines. We also characterise the resulting X-ray source populations. The eRASS:3 main catalogue contains nearly two million sources, including 1,911,744 point-like and 63,796 extended sources, detected in the 0.2-2.3keV energy band, eROSITA's most sensitive energy window. This volume has doubled the X-ray source content of eRASS1 and provides a comprehensive census of X-ray-emitting objects across diverse astrophysical classes. We also released a secondary hard catalogue of nearly 15000 sources detected in the harder 2.3-5.0keV energy band. In addition, we released six catalogues, three for the main sample and three for the hard sample, in which we identify and classify the optical and infrared counterparts of eRASS:3 point-like sources. This approach delivers a homogeneous, high-quality identification of mostly extragalactic X-ray emitters; for example, we estimate that approximately 88% of the 1.4 million counterparts identified within the footprints of the Legacy Survey Imaging for DESI are extragalactic sources. This work has enabled the generation of samples optimised for completeness and purity, while expanding the discovery space for rare populations. The second data release (DR2) of the SRG/eROSITA all-sky survey is a catalogue-only release, comprising the catalogues presented in this work together with an updated version of the eROSITA upper flux limit server.
Author(s): Ramos-Ceja M.E.; Lamer G.; Salvato M.; Merloni A.; Sanders J.S.,Georgakakis A.; Liu T.; Bulbul E.; Buchner J.; Dennerl K.; Freyberg M.J.,Friedrich S.; Kreykenbohm I.; Maitra C.; Nandra K.; Predehl P.,Reiprich T.H.; Robrade J.; Schwope A.; Shirley R.; Stelzer B.; Stewart I.,Seppi R.; Starck H.; Tubin-Arenas D.; Traulsen I.; Artis E.; Aydar C.,Baldini P.; Balzer F.; Becker W.; Bennedik M.M.; Bornemann W.; Brueggen M.,Brink J.; Brusa M.; Burwitz V.; Canal i Saguer M.; Clerc N.; Comparat J.,Coriat M.; Correa-Rodrigues J.V.; Czesla S.; Dauner L.; Dietl J.; Ding Z.,Ducci L.; Dwelly T.; Fiorino L.; Freund S.; Friedrich P.; Gaida R.,Gatuzz E.; Guida S.T.; Haemmerich S.; Haberl F.; Hartner G.,Hernandez-Diaz S.; Igo Z.; Ilic N.; Kaltenbrunner D.M.; Khokhriakova A.,Kink W.; Kirsch C.; Kluge M.; Krippendorf S.; Krumpe M.; Kulkarni S.,Kurpas J.; Kyritsis E.; Laktionov R.; Liu A.; Lorenz M.; Malavasi N.,Mayer M.G.F.; Meidinger N.; Mistele T.; Mueller S.; Munoz-Giraldo D.,Nguyen-Dang N.T.; Ni Q.; Ok S.; Ota N.; Puehlhofer G.; Pacaud F.; Pandya A.,Perinati E.; Pommranz C.; Ponti G.; Poppenhaeger K.; Pradeep K.G.; Rau A.,Roster W.; Rukdee S.; Saeedi S.; Santangelo A.; Sasaki M.; Sheth S.,Shreeram S.; Sommer M.; Srivastava A.; Suleimanov V.; Truemper J.,Vasilas N.; Veronica A.; Webb N.; Weber P.; Wilms J.; Yeung M.C.H.,Zangrandi F.; Zelmer S.; Zhang X.; Zhang Y.; Zheng X.
IVOA id: ivo://cds.vizier/j/a+a/712/a171