VO Fresh

OFS Observatory Archive Registry

2026-07-10T08:57:23Z

Description: The publishing registry for the OFS Observatory Archive.
Author(s): AISAS LSO team
IVOA id: ivo://lso.dc/__system__/services/registry

Coronagraphic spectro-polarimetric data from the Coronal Multi-channel Polarimeter for Slovakia (CoMP-S) at the Lomnicky Peak Observatory (LSO)

2026-07-10T08:24:02Z

Description

CoMP-S (Coronal Multi-channel Polarimeter for Slovakia) is the
spectro-polarimeter installed at the ZEISS coronagraph at the LSO
(Lomnicky Peak Observatory). This spectro-polarimeter is using 4-stage
Lyot filter for observations of the prominent emission lines emitted
from the solar prominences and corona in the VIS and near-IR spectral
ranges.

Author(s)

The LSO Team

IVOA id

ivo://lso.dc/lso/q/epn_core

AMS-02 Spectral Results Catalog

2026-07-10T00:00:00Z

Description: The AMS02SPEC database table records the spectral results obtained with the Alpha Magnetic Spectrometer experiment on the International Space Station (AMS-02), 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

Swift-XRT Living Point Source Catalog (LSXPS)

2026-07-10T00:00:00Z

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

Gas-phase metallicity gradients in GOODS galaxies

2026-07-08T09:25:11Z

Description: We explore the relationships between the [O/H] gas-phase metallicity radial gradients and multiple galaxy properties for 238 star-forming galaxies at 0.6<z<2.6 selected from the CANDELS Ly{alpha} Emission at Reionization survey with stellar mass 8.5<logM*/M_{sun}_<10.5. The gradients cover the range from -0.11 to 0.22dex/kpc, with the median value close to 0. We reconstruct the nonparametric star formation histories (SFHs) of the galaxies with spectral energy distribution modeling using Prospector with more than 40 photometric bands from the Hubble Space Telescope, Spitzer, and ground-based facilities. In general, we find weak or no correlations between the metallicity gradients and most galaxy properties, including the mass-weighted age, recent star formation rate, dust attenuation, and morphology as quantified by both parametric and nonparametric diagnostics. We find a significant but moderate correlation between the gradients and the "evolutionary time," a temporal metric that characterizes the evolutionary status of a galaxy, with flatter gradients observed in more evolved galaxies. Also, there is evidence that galaxies with multiple star formation episodes in their SFHs tend to develop more negative gas-phase metallicity gradients (higher [O/H] at the center). We conclude that gas kinematics, e.g., radial inflows and outflows, is likely an important process in setting the gas-phase metallicity gradients, in addition to the evolution of the SFH radial profile. Since the gradients are largely independent of the galaxies' physical properties and only weakly dependent on their SFH, it would appear that the timescale of the gas kinematics is significantly shorter than the evolution of star formation.
Author(s): Cheng Y.; Giavalisco M.; Simons R.C.; Ji Z.; Stroupe D.; Cleri N.J.
IVOA id: ivo://cds.vizier/j/apj/964/94

Magnetic delta Scuti candidates

2026-07-08T06:45:00Z

Description: delta Scuti stars are pulsating stars constituting the delta Scuti instability strip in the Hertzsprung-Russell (HR) diagram, which consists of A and F stars of various evolutionary stages. They are in the transition region between high-mass hot stars and low-mass solar-like stars, making understanding their magnetic properties essential to painting a complete picture of magnetism across the HR diagram. Furthermore, discovering magnetic delta Scuti stars allows for magneto-asteroseismology, which can be used to determine the internal rotation profile, internal magnetic field strength, and the efficiency of mixing and transport processes more accurately than classical asteroseismology. To date, magnetic fields have been detected at the surface of 13 delta Scuti stars. However, the overall incidence rate of magnetism in these stars remains unknown. Fossil magnetic fields are detected in 10% of OBA stars. The goal of this work is to find out if it is the same for delta Scuti stars. We investigated the incidence rate of surface magnetic fields among delta Scuti stars using photometric data from the CoRoT space mission. We analyzed long-duration (~5 months) light curves of ~1750 delta Scuti stars to search for pulsations and rotational modulation - a photometric signature that indicates chemical or temperature spots at the stellar surface, usually caused by magnetic fields. We identified 147 rotational variables that we designate as magnetic candidates, thus potentially increasing the known population of magnetic delta Scuti stars drastically and suggesting an incidence rate of fossil magnetic fields in delta Scuti stars similar to the incidence rate in OBA stars in general. Our analysis also revealed a few delta Scuti-gamma Dor hybrid stars and four binary stars in the sample. We determined the rotation periods and projected rotation velocities of the magnetic candidates in order to select suitable targets for follow-up spectropolarimetric observations aimed at confirming and characterizing their magnetic fields.
Author(s): Paul G.; Neiner C.; Catala C.; Labadie-Bartz J.
IVOA id: ivo://cds.vizier/j/a+a/711/a128

Extended Orion Nebula HI 21cm emission maps

2026-07-08T06:42:46Z

Description: The Orion nebula is the nearest site of ongoing and recent high-mass star formation. It is a unique laboratory for studying the mass, energy, and momentum input from high-mass stars. We present 21-centimeter emission line observations that resolve for the first time the neutral atomic hydrogen (HI) gas in the extended Orion nebula (EON) at a resolution of one arcminute, which corresponds to a physical scale of 0.12 parsecs at the standard distance to the region. Our HI emission maps reveal an expanding shell that matches the EON contours delineated by recent observations of ionized carbon ([CII]) line emission. However, our combination of single-dish and interferometric HI observations suggests 100 solar masses of material for the front hemisphere of the shell, which is lower by roughly a factor of ten than the mass inferred from [CII] observations. This discrepancy suggests that the mass of the nearest wind-blown bubble has been overestimated, although we do not rule out the possibility that a significant amount of molecular hydrogen (H_2_) in the shell may account for part of the difference. Our extended 21cm line maps also reveal uncharted structures in and around the EON. They include a probable secondary bubble and a linear protrusion extending roughly four parsecs from the shell boundary. Our results illustrate the potential of HI interferometric observations to elucidate key aspects of the multiphase structure of star-forming regions and their connection to their surroundings.
Author(s): Soler J.D.; Beuther H.; Glover S.C.O.; Klessen R.S.; Ott J.; Rugel M.,Teh J.W.; Clark S.E.; Goldsmith P.; Hacar A.; Socci A.; Heyer M.; Lee M.-Y.,Murray C.E.; Seifried D.; Walch S.; Godard B.; Miville-Deschenes M.-A.
IVOA id: ivo://cds.vizier/j/a+a/711/a85

6 seismic solar analogs asteroseismologic data

2026-07-08T00:00:00Z

Description: Solar analogs, stars that closely match the fundamental properties of the Sun, provide key benchmarks for testing stellar structure and evolution across different ages and activity levels. Their detailed characterization helps place the Sun in context within the broader population of solar-like stars. This study presents the characterization of six seismic solar analogs observed by the NASA Kepler and K2 missions. Combining asteroseismic constraints from space-based photometry with high-resolution spectroscopy and Gaia astrometry, we derived their fundamental parameters and assessed their resemblance to the Sun. Global seismic properties and individual oscillation modes were extracted from the photometric light curves, while atmospheric parameters were obtained from data collected by the HERMES spectrograph at the Mercator telescope. Stellar modeling using seven independent stellar evolution codes yielded consistent masses, radii, and ages. These stars have masses between 0.91 and 1.04M_{sun}_, radii between 0.95 and 1.08R_{sun}_, and ages from about 1.8 to 9.1Gyr, with typical systematic uncertainties of +/-0.02M_{sun}_, +/-0.01R_{sun}_, and +/-0.7Gyr, respectively. One star, EPIC 206064678, exhibits properties very similar to those of the Sun, with M=1.016+/-0.033M_{sun}_, R=0.990+/-0.011R_{sun}_, and an age of 5.40+/-0.12Gyr. It can therefore be considered a close solar twin, although it is slightly older and more metal-rich (0.25+/-0.07dex). Four targets display binarity signatures and all exhibit very low chromospheric activity. This work broadens the sample of well-characterized seismic solar analogs towards a larger sample of metallicities and ages, providing new references for comparative stellar studies and future asteroseismic investigations.
Author(s): Garcia R.A.; Mathur S.; Hookway G.T.; Godoy-Rivera D.; Masseron T.,Betrisey J.; Buldgen G.; Lindsay C.; Metcalfe T.S.; Scutt O.J.; Stokholm A.,Beck P.G.; Benomar O.; Davies G.R.; Jimenez A.; Merc J.; Nielsen M.B.,Panetier E.; Perez Hernandez F.; Borg L.; Breton S.N.; Debacker L.,Escorza A.; Grossmann D.H.; Hamy A.; Liagre B.; Lund M.N.; Mathis S.,Palakkatharappil D.B.; Santos A.R.G.; Delsanti V.; Gonzalez-Cuesta L.,Fox V.; Proust N.
IVOA id: ivo://cds.vizier/j/a+a/710/a369

Spectroscopy of open cluster UBC 1052

2026-07-08T00:00:00Z

Description: Of the thousands of newly discovered open clusters (OCs) thanks to the exquisite precision of the Gaia mission data, only a small fraction has been observed with high-resolution spectroscopy. Particularly, the population of OCs in the inner disc at relatively high altitudes (Z) from the Galactic plane remains poorly studied. Few such high-|Z| inner-disc OCs have been detected, and most are sparse groupings of stars that still await confirmation as real OCs. We performed a detailed spectroscopic analysis of the high-|Z| inner-disc OC UBC 1052, an old cluster located at a cylindrical Galactocentric radius Rgc=6.1kpc, where it is one of a few OCs situated at a considerable altitude (Z=340pc). We used FLAMES/VLT to acquire high signal-to-noise ratio (S/N) UVES spectra of four red clump (RC) members (G~14 mag), from which we derived high-precision radial velocities and local thermodynamic equilibrium chemical abundances for 23 elements. A strict line-by-line differential analysis was carried out using a reference RC star and a solar analogue in the OC M 67, allowing us to derive very precise abundances for each star (a median precision in [X/H] of ~0.06dex). We also acquired GIRAFFE spectra for other candidate member stars and derived their radial velocities. We determine that UBC 1052 has an age of 2.25+/-0.25Gyr, a distance of 3.11+/-0.07kpc, an extinction of A_V_=1.23mag, and a mean radial velocity of 34.0+/-0.6km/s. We find that the four RC stars have fully compatible chemical abundances, thus confirming UBC 1052 as a real OC. It has [Fe/H]=+0.05+/-0.01dex, and with [X/H] dispersions among the four stars <0.03dex for 20 elements, we give conservative limits for chemical inhomogeneities at ~0.05dex for these species. UBC 1052 stands out as the oldest and highest-|Z| inner-disc OC studied at high resolution to date, being located in the poorly sampled inner Galactic region where old OCs and OCs with large maximum excursions from the plane are scarce. Its relatively low [Fe/H] at its Rgc suggests it is a rare candidate for an inward-migrated OC in the inner disc. Its detailed abundance pattern (e.g. [Ba/Zr] and [Nd/Y]) shows some interesting features that appear to be unique in the current census of OCs studied at high resolution, making it an interesting object for potential strong chemical-tagging searches for already dispersed member stars.
Author(s): Donada J.; Casamiquela L.; Anders F.; Balaguer-Nunez L.; Blanco-Cuaresma S.,Luri X.; Slumstrup D.; Jordi C.; Castro-Ginard A.; Carrera R.; Carrasco J.M.
IVOA id: ivo://cds.vizier/j/a+a/710/a381

HD 75149 multi-epoch spectra

2026-07-08T00:00:00Z

Description: Massive stars continuously enrich the surrounding interstellar medium by supplying it with stellar material driven by their powerful winds. B supergiant stars (BSGs) in particular are a type of massive star characterized by strong winds and notable photometric and spectroscopic variability. We aim to conduct a pilot study of the optical spectroscopic variability of the BSG HD 75149 between 2004 and 2025. Its extended temporal baseline and pronounced variability amplitude make it particularly well suited for investigating the physical origin of the observed short-term variability within a consistent hydrodynamical and radiative-transfer framework. We analyzed 25 nightly averaged optical spectra obtained with different instruments and telescopes, some of them with observations over several consecutive days. We measured the radial velocities (RVs) and equivalent widths (EWs) of 17 spectral lines (H, HeI, SiIII, NII, MgII, CII). We modeled the H{alpha} emission, absorption, and P-Cygni profiles using the ISOSCELES grid and the delta-slow hydrodynamic regime. H{alpha} shows variability in intervals of a few days, including P-Cygni changes, while metal lines show small RV amplitudes, consistent with pulsating oscillations. The largest variation in the mass-loss rate corresponds to an increase of a factor of 1.8 within four days. In contrast, the terminal velocity remains barely affected during the same time interval. The pronounced variation observed in hydrogen lines, in contrast with the variability of other lines, suggests that it is due to mass-loss rate episodes driven by a slow wind occurring on a timescale comparable to photometric variations. We found no evidence of a close binary companion in the sample used, but we cannot completely exclude the possibility of a wide or low-inclination companion.
Author(s): Chamoun-Contreras J.; Arcos C.; Machuca N.; Perez-Ramirez C.E.; Cidale L.S.,Cure M.; Araya I.; Turis-Gallo D.; Hadjara M.
IVOA id: ivo://cds.vizier/j/a+a/710/a383

OH/IR stars in the inner Galactic bulge. I.

2026-07-08T00:00:00Z

Description: Stars on the asymptotic giant branch (AGB) play important roles in a number of astronomical contexts. To quantify these roles, it is necessary to establish the mass-loss characteristics of stars as they evolve up and beyond the AGB. We used an equidistant sample of 77 AGB stars in the inner Galactic bulge, selected on the existence and strength of OH1612 MHz maser emission, to obtain information on the mass loss of O-rich AGB stars, and on its transformations in geometry and kinematics that occur at the tip of the AGB. Observations of circumstellar lines from several rotational transitions of 12CO, 13CO, and C18O were performed with the Atacama Large Millimeter/submillimeter Array (ALMA), and, for a sub-sample, with the Atacama Pathfinder EXperiment telescope (APEX). The ALMA observations also provide continuum data. Existing infrared photometry was used to estimate colours and produce stellar light curves. Based on mid-infrared colour, CO line, and near-infrared variability characteristics, the objects were divided into four categories of distinct stellar and/or circumstellar properties. Various circumstellar CO line characteristics are presented and compared between the categories, such as morphologies and extents of brightness distributions (BDs), line profiles (LPs), line intensity ratios, and kinematics. A majority of the objects form a homogenous group with sharply, centrally peaked BDs and LPs of the soft-parabola type, while the rest show extended and complex BDs and/or LPs with high-velocity wings. The C^18^O line and ALMA continuum detection rates vary significantly between the categories. CO line emission is also detected from interaction zones where the expanding circumstellar gas meets the interstellar medium. These data provide the foundation for more detailed studies, including radiative transfer analyses of the CO line and photometry data, on the evolution of stellar and circumstellar characteristics of O-rich stars on the upper AGB and beyond.
Author(s): Olofsson H.; Khouri T.; Muller S.; Unnikrishnan R.; Groenewegen M.A.T.,Blommaert J.A.D.L.; De Beck E.; Kastner J.H.; Maercker M.; Patel N.,Ryde N.; Sargent B.A.; Srinivasan S.; Vlemmings W.H.T.
IVOA id: ivo://cds.vizier/j/a+a/710/a390

RX Gru times of primary and secondary minima

2026-07-08T00:00:00Z

Description: We report the discovery of a new short-period pre-main-sequence eclipsing binary, RX Gru, orbited by a distant circumbinary companion. We characterized the system by analysing the photometric observations from the Solaris network, the Transiting Exoplanet Survey Satellite, and the Super Wide Angle Search for Planets survey, combined with the radial velocities from four high-resolution spectrographs: HARPS, FEROS, CHIRON, and HRS. We determined the age of the system from the observed parameters using two evolution codes, MESA and Cesam2k20. We obtained an age of ~28Myr, placing the two stars at the very end of the pre-main-sequence phase. We conclude that RX Gru consists of a tight inner binary composed of two twin components and an outer low-mass companion (a massive brown dwarf or a very low-mass star) in a relatively wide orbit, and we suggest that the system was formed via the dynamical unfolding mechanism coupled with the shared accretion of the circumbinary material by the binary components.
Author(s): Marcadon F.; Moharana A.; Pawar T.B.; Pawar G.; Helminiak K.G.,Marques J.P.; Konacki M.
IVOA id: ivo://cds.vizier/j/a+a/710/a394

Inclination of 221 Gaia DR3 non-single stars

2026-07-08T00:00:00Z

Description: Orbital inclination is crucial in determining the mass of the binary. The astrometric excess noise contain the orbital motion information, which can be used to constrain the inclination.We aim to constrain the orbital inclination of a binary system by combining radial velocity measurements with the astrometric excess noise from the Gaia DR3 solution. The astrometric excess noise is directly related to the orbital parameters.For a binary system with a radial velocity solution, it can be treated as a function of the orbital inclination. Using the Gaia nominal scanning law and the estimated centroid uncertainties,we simulate Gaia astrometric epoch observations to reproduce the expected excess noise. By sampling different inclinations and comparing the resulting simulated excess noise with the value reported in Gaia DR3, we can constrain the inclination to a specific interval. We have developed a method to constrain the orbital inclination within a specific range, enabling a more accurate determination of the binary mass, particularly for spectroscopic binaries. Internal and external validations demonstrate the robustness of the method, although certain limitations remain. It is most reliable for systems exhibiting a strong astrometric signal of binary motion, while caution is required when applying it to binaries with weak astrometric wobbles or poorly sampled orbits.
Author(s): Liao S.; Ding Y.; Wen S.; Qi Z.; Wu Q.
IVOA id: ivo://cds.vizier/j/a+a/710/a398

Pleiades cluster single members

2026-07-08T00:00:00Z

Description: Establishing a self-consistent age scale for stellar populations requires physically well-calibrated chronometers. Among these, lithium-based diagnostics, particularly the lithium depletion boundary (LDB), provide one of the most robust age constraints for stellar populations in the low-mass regime. However, their application is limited by heterogeneous temperature scales and astrophysical dispersion, especially among FGK stars, where rotation can significantly affect lithium abundances. As a first step towards a self-consistent age scale, our aim has been to formulate CHRONOS, the first version of a Bayesian hierarchical lithium-based age-dating model combined with a neural network trained on stellar evolutionary models. We implemented a Bayesian hierarchical model that jointly infers stellar effective temperatures, lithium abundances, and the global age of a stellar association. The theoretical LDB is provided by a pre-trained multilayer perceptron based on BT-Settl evolutionary models. The model incorporates a temperature-dependent transition between fully convective ultra-cool dwarfs (UCDs) and FGKM dwarf stars, together with a two-component FGK mixture to account for rotation-induced lithium enhancement. We applied the method to the Pleiades cluster and performed a validation using synthetic datasets. For the Pleiades cluster, CHRONOS yields a posterior age distribution centred at Age=124.53_-2.70_^+3.34^Myr, consistent with classical LDB estimates, while simultaneously constraining both global and stellar-level rotation parameters. This work demonstrates that lithium-based stellar chronology can be recast as a coherent hierarchical inference problem, providing a flexible and statistically robust framework for making age determinations for young (1-600Myr) stellar populations.
Author(s): Gonzalez-Ramirez L.; Barrado D.; Olivares J.; Berihuete A.; Sarro L.M.,Palmero F.J.
IVOA id: ivo://cds.vizier/j/a+a/710/a407

PHANGS-Halpha nearby star-forming galaxies

2026-07-08T00:00:00Z

Description: We present PHANGS-H{alpha}, a narrowband imaging survey that maps H{alpha} emission over a sample of 65 nearby massive star-forming galaxies. The data were obtained using the MPG-ESO 2.2-meter telescope at La Silla and the du Pont 2.5-meter telescope at Las Campanas Observatory, within the framework of the multi-wavelength cloud-scale (50-100pc) resolution mapping of molecular gas and star formation conducted by the Physics at High Angular resolution in Nearby GalaxieS (PHANGS) collaboration. PHANGS-H{alpha} complements the published PHANGS-ALMA, PHANGS-MUSE, PHANGS-HST, and PHANGS-JWST surveys, providing an anchor point for the photometric and astrometric calibration of these datasets, as well as samples of HII regions and star formation rate maps for the bulk of the PHANGS sample. We describe the observations, data processing, and calibration of the PHANGS-H{alpha} dataset, as well as the procedures used to derive emission-line fluxes from narrowband imaging. A subset of galaxies with available spectroscopic Ha mapping from the PHANGS-MUSE survey serves as the basis of a detailed comparison with the narrowband photometry presented here. This comparison informs a set of best practices for the processing of narrowband H{alpha} imaging, which we subsequently apply to the full dataset.
Author(s): Razza A.; Blanc G.A.; Groves B.; Congiu E.; Neumann J.; Pan H.-A.; Ho I-T.,Barnes A.T.; Belfiore F.; Boquien M.; Burton C.; Chevance M.; Egorov O.,Emsellem E.; Faesi C.; Glover S.C.O.; Grasha K.; Klessen R.S.; Kreckel K.,Leroy A.K.; McElroy R.; Pessa I.; Schinnerer E.; Tomicic N.; Amiri A.,Anand G.S.; Cao Y.; Dale D.A.; Dlamini S.; Li J.; Mendez-Delgado J.E.,Murphy E.J.; Pathak D.; Querejeta M.; Ramambason L.; Rosolowsky E.,Scheuermann F.; Ubeda L.; Williams T.G.
IVOA id: ivo://cds.vizier/j/a+a/710/a412

Baryonic Faber-Jackson relation

2026-07-08T00:00:00Z

Description: The baryonic Faber-Jackson relation (BFJR) links the baryonic mass of pressure-supported systems to their mean velocity dispersion. For elliptical galaxies, the BFJR is thought to be a projection of the fundamental plane (FP), which includes the stellar half-mass radius as a third variable. We study the BFJR and FP across eight orders of magnitude in baryonic mass, encompassing galaxy groups, ellipticals, dwarf ellipticals, and dwarf spheroidals. We compile and homogenize data for 1400 pressure-supported systems and measure their mean internal baryonic acceleration <gbar>. We find that the properties of the BFJR and FP systematically depend on the internal acceleration of the sampled systems, with a transition around the acceleration scale a0~=~1.2x10^-10m/s^2^. For low-acceleration systems with <gbar> < 0.6a0 (dwarf galaxies and galaxy groups), the BFJR relation takes the form log10(Mbar/M_{sun}_)=(4.19+/-0.10)log10(siglos/(km/s))+2.55+/-0.16 with an orthogonal intrinsic scatter of 0.11+/-0.01 dex. The FP expected from the Newtonian virial theorem is followed by high-acceleration systems (massive ellipticals with <gbar> >= 6a0), whereas low-acceleration systems deviate from the FP at both low masses (dwarf galaxies) and high masses (galaxy groups). Our results generally agree with the expectations of MOND: high-acceleration systems follow the Newtonian virial theorem in which a radial variable explicitly appears (the FP), while low-acceleration systems follow the MOND virial theorem in which the radial dependence disappears (the BFJR). On average, the MOND external field effect seems to play a secondary role in dwarf galaxies in galaxy groups and clusters.
Author(s): Tian; Y.; Lelli; F.; Pawlowski; M.S.; McGaugh; S.; Duann; Y.; Chae; K.-H.,Di Teodoro; E.; Haubner; K.; Kuo; M.H.; Ko; C.-M.
IVOA id: ivo://cds.vizier/j/a+a/710/l39

Euclid (Q1). Census of dwarf galaxies

2026-07-08T00:00:00Z

Description: The Euclid Q1 fields were selected for calibration purposes in cosmology and are therefore relatively devoid of nearby galaxies. However, this is precisely what makes them interesting fields in which to search for dwarf galaxies in local density environments. We take advantage of the unprecedented depth, spatial resolution, and field of view of the Euclid Quick Release (Q1) to build a census of dwarf galaxies in these regions. We have identified dwarf galaxies in a representative sample of 25 contiguous tiles in the Euclid Deep Field North (EDF-N), covering a total area of 14.25 square degrees. The dwarf galaxy candidates were identified using a semi-automatic detection method, based on properties measured by the Euclid pipeline and released as part of the catalogue produced by the MERge Processing Function (MER PF) pipeline. A selection cut in surface brightness and magnitude was used to produce an initial dwarf candidate catalogue, followed by a cut in morphology (removing background spirals) and I_E-H_E colour (removing red ellipticals). This catalogue was then visually classified to produce a final sample of dwarf candidates, including their morphology, number of nuclei, globular cluster (GC) richness, and presence of a blue compact centre. We identified 2674 dwarf candidates, corresponding to 188 dwarfs per square degree. The visual classification of the dwarfs reveals a slightly uneven morphological mix of 58% ellipticals and 42% irregulars, with very few potentially GC-rich (1.0%) and nucleated (4.0%) candidates but a noticeable fraction (6.9%) of dwarfs with blue compact centres. The distance distribution of 388 (15%) of the dwarf candidates with spectroscopic redshifts peaks at about 400Mpc. Their stellar mass distribution confirms our selection effectively identifies dwarfs while minimising contamination. The most prominent dwarf overdensities are dominated by dEs, while dIs are more evenly distributed across the field of view. This work highlights Euclid's remarkable ability to detect and characterise dwarf galaxies across diverse masses, distances, and environments. Description: Table A.1 lists the entire sample of dwarf galaxy candidates with their morphological and visual properties, ordered by increasing RA. Table A.2 lists the Photometric and structural properties of the dwarf galaxy candidates ordered by increasing RA. Table A.3. lists the aperture magnitudes and extinction corrections (EC) of the dwarf galaxy candidates for the Euclid I_E, Y_E, J_E and H_E photometric bands. The dwarf galaxy candidates are ordered by increasing RA or equivalently Euclid ID. Table A.4. lists the stellar mass estimates obtained via the reference SED fitting setup and all available photometric bands assuming z=0.1 or z=0.05 respectively. The dwarf galaxy candidates are ordered by increasing RA or equivalently Euclid ID. Table A.5. lists the stellar mass estimates obtained via the reference SED fitting setup and all available photometric bands for dwarf galaxy candidates with spectroscopic redshifts available. The dwarf galaxy candidates are ordered by increasing RA or equivalently Euclid ID.
Author(s): Euclid Collaboration; Marleau F.R.; Habas R.; Carollo D.; Tortora C.,Duc P.-A.; Sola E.; Saifollahi T.; Fugenschuh M.; Walmsley M.; Zoller R.,Ferre-Mateu A.; Cantiello M.; Urbano M.; Saremi E.; Ragusa R.; Laureijs R.,Hilker M.; Muller O.; Poulain M.; Peletier R.F.; Sprenger S.J.; Marchal O.,Aghanim N.; Altieri B.; Amara A.; Andreon S.; Auricchio N.; Aussel H.,Baccigalupi C.; Baldi M.; Balestra A.; Bardelli S.; Basset A.; Battaglia P.,Bender R.; Biviano A.; Bonchi A.; Bonino D.; Branchini E.; Brescia M.,Brinchmann J.; 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.; Corcione L.; Courbin F.; Courtois H.M.; Cropper M.,Cuillandre J.-C.; Da Silva A.; Degaudenzi H.; De Lucia G.; Di Giorgio A.M.,Dolding C.; Dole H.; Dubath F.; Dupac X.; Dusini S.; Escoffier S.,Fabricius M.; Farina M.; Faustini F.; Ferriol S.; Fosalba P.; Fotopoulou S.,Frailis M.; Franceschi E.; Franzetti P.; Fumana M.; Galeotta S.; George K.,Gillis B.; Giocoli C.; Granett B.R.; Grazian A.; Grupp F.; Gwyn S.,Haugan S.V.H.; Hoar J.; Hoekstra H.; Holmes W.; Hormuth F.; Hornstrup A.,Hudelot P.; Jahnke K.; Jhabvala M.; Joachimi B.; Keihanen E.; Kermiche S.,Kiessling A.; Kubik B.; Kummel M.; Kunz M.; Kurki-Suonio H.; Lahav O.,Le Boulc'h Q.; 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.,Marcin S.; Marggraf O.; Martinelli M.; Martinet N.; Marulli F.; Massey R.,Maurogordato S.; McCracken H.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.; Nightingale J.W.,Padilla C.; Paltani S.; Pasian F.; Pedersen K.; Percival W.J.; Pettorino V.,Pires S.; Polenta G.; Poncet M.; Popa L.A.; Pozzetti L.; Raison F.; Rebolo R.,Renzi A.; Rhodes J.; Riccio G.; Romelli E.; Roncarelli M.; Rossetti E.,Rusholme B.; Saglia R.; Sakr Z.; Sanchez A.G.; Sapone D.; Sartoris B.,Sauvage M.; Schewtschenko J.A.; Schirmer M.; Schneider P.; Scodeggio M.,Secroun A.; Seidel G.; Seiffert M.; Serrano S.; Simon P.; Sirignano C.,Sirri G.; Skottfelt J.; Stanco L.; Steinwagner J.; Tallada-Crespi P.,Tavagnacco D.; Taylor A.N.; Teplitz H.I.; Tereno I.; 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.; Cappi A.; Di Ferdinando D.; Escartin Vigo J.A.; Gabarra L.,Huertas-Company M.; Martin-Fleitas J.; Matthew S.; Mauri N.; Metcalf R.B.,Pontinen M.; Scottez V.; Sereno M.; Tenti M.; Viel M.; Wiesmann M.; Akrami Y.,Andika I.T.; Anselmi S.; Archidiacono M.; Atrio-Barandela F.; Bertacca D.,Bethermin M.; Blanchard A.; Borgani S.; Brown M.L.; Bruton S.; Buitrago F.,Calabro A.; Camacho Quevedo B.; Caro F.; Carvalho C.S.; Castro T.; Cogato F.,Conseil S.; Cooray A.R.; Davini S.; De Paolis F.; Desprez G.; Diaz-Sanchez A.,Di Domizio S.; Diego J.M.; Dimauro P.; Enia A.; Franco A.; Ganga K.,Garcia-Bellido J.; Gasparetto T.; Gaztanaga E.; Gianotti F.; Gozaliasl G.,Guidi M.; Gutierrez C.M.; Hall A.; Hernandez-Monteagudo C.; Hildebrandt H.,Kajava J.J.E.; Kang Y.; Kansal V.; Karagiannis D.; Kiiveri K.,Kirkpatrick C.C.; Kruk S.; Legrand L.; Lepori F.; Leroy G.; Lesci G.F.,Lesgourgues J.; Liaudat T.I.; Liu S.J.; Macias-Perez J.; Mannucci F.,Maoli R.; Martins C.J.A.P.; Maurin L.; Miluzio M.; Monaco P.; Moretti C.,Morgante G.; Navarro-Alsina A.; Nicastro L.; Paterson K.; Patrizii L.,Potter D.; Quai S.; Radovich M.; Rocci P.-F.; Sacquegna S.; Sahlen M.,Sanders D.B.; Sarpa E.; Schultheis M.; Sciotti D.; Sellentin E.; Tanidis K.,Tao C.; Testera G.; Teyssier R.; Tosi S.; Troja A.; Tucci M.; Venhola A.,Vergani D.; Verza G.; Scott D.
IVOA id: ivo://cds.vizier/j/a+a/711/a10

large-scale 3D extinction mapping

2026-07-08T00:00:00Z

Description: Three-dimensional extinction mapping of the Milky Way faces a fundamental trade-off: Gaia's precise astrometry and photometry enable high-resolution mapping but only to limited distances due to visible-wavelength extinction, while infrared surveys like 2MASS penetrate deeper into the Galactic plane but provide poor distance constraints, especially in the solar neighbourhood. Many studies have cross-matched these surveys in order to provide more wavelength coverage and therefore better extinction estimates. This comes at a cost as the cross-matching limits depth to the visible survey's reach, as highly extinguished stars detected in infrared lack visible counterparts. We develop PyRedLine as an evolution of the REDLINE method, enabling simultaneous exploitation of multiple surveys without cross-matching. Our goal is to achieve both high spatial resolution at short distances through Gaia and extended reach into the Galactic plane through 2MASS, with target resolution of ~100pc within several kpc. PyRedLine compares statistical distributions of observed stellar properties (colours, parallaxes, absolute magnitudes) against predictions from the Besancon Galaxy Model reddened by parameterised extinction profiles. Using Bayesian inference with MCMC sampling, we independently determine extinction along each LOS by fitting model predictions to Gaia DR3 and 2MASS observations simultaneously, then assemble these profiles into three-dimensional maps. Validation with synthetic data confirms reliable structure detection to ~8kpc. We successfully map the Galactic plane from 240{deg}<=l<=303{deg} and |b|<=5{deg} at 15' resolution. The resulting map reveals extinction to 13kpc with up to 42pc resolution. We recover known structures including the Vela molecular complex and Carina arm tangent, achieving significantly finer resolution at short distances compared to REDLINE while maintaining comparable depth. We detect distant features potentially associated with the Perseus arm that remain undetected in other surveys.
Author(s): Deforet B.; Montillaud J.; Robin A.C.; Marshall D.J.
IVOA id: ivo://cds.vizier/j/a+a/710/a344

Galaxies of Euclid (Q1)

2026-07-08T00:00:00Z

Description: We present three catalogues of candidate active galactic nuclei (AGN) in the Euclid Quick Release (Q1) fields. For each Euclid source we collect multi-wavelength photometric and spectroscopic information from surveys such as the Galaxy Evolution Explorer (GALEX), Gaia, Dark Energy Survey (DES), Wide-field Infrared Survey Explorer (WISE), Spitzer, Dark Energy Spectroscopic Instrument (DESI), and Sloan Digital Sky Survey (SDSS), including spectroscopic redshifts from public compilations when available. We investigate the AGN content of the Q1 fields using multiple selection methods. Applying Euclid colours and WISE-AllWISE cuts, we identify 292222 and 65131 candidates, respectively. We compile a high-purity QSO catalogue based on Gaia DR3 information, containing 1971 candidates. Using spectroscopic information from DESI, we perform broad-line and narrow-line AGN selections, yielding 4392 AGN candidates across the Q1 fields. We investigate and refine the Euclid Q1 probabilistic random forest QSO population, selecting a refined sample of 180666 candidates. Additionally, we perform SED fitting on sources with available z_spec_ and, utilizing the derived AGN fraction, identify 7766 AGN candidates. To improve selection purity, we define two new colour criteria (JH_IeY and IeH_gz), finding 313714 and 267513 candidates, respectively, across the Q1 fields. We find a total of 229779 AGN candidates equivalent to an AGN surface density of 3641 deg^{-2} for 18<Ie<=24.5, and a subsample of 30422 candidates corresponding to an AGN surface density of 482 deg^{-2} when limiting the depth to 18<Ie<=22. The AGN surface densities recove
Author(s): Euclid Collaboration: Matamoro Zatarain T.; Fotopoulou S.; Ricci F.,Bolzonella M.; La Franca F.; Viitanen A.; Zamorani G.; Taylor M.B.,Mezcua M.; Laloux B.; Bongiorno A.; Jahnke K.; Stevens G.; Shaw R.A.,Bisigello L.; Roster W.; Fu Y.; Margalef-Bentabol B.; La Marca A.,Tarsitano F.; Feltre A.; Calhau J.; Lopez Lopez X.; Scialpi M.; Salvato M.,Allevato V.; Siudek M.; Saulder C.; Vergani D.; Bremer M.N.; Wang L.,Giulietti M.; Alexander D.M.; Sluse D.; Shankar F.; Spinoglio L.; Scott D.,Shirley R.; Landt H.; Selwood M.; Toba Y.; Dayal P.; Aghanim N.; Altieri B.,Amara A.; Andreon S.; Auricchio N.; Aussel H.; Baccigalupi C.; Baldi M.,Bardelli S.; Basset A.; Battaglia P.; Biviano A.; Bonchi A.; Branchini E.,Brescia M.; Brinchmann J.; Camera S.; Canas-Herrera G.; Capobianco V.,Carbone C.; Carretero J.; Casas S.; Castander F.J.; Castellano M.,Castignani G.; Cavuoti S.; Chambers K.C.; Cimatti A.; Colodro-Conde C.,Congedo G.; Conselice C.J.; Conversi L.; Copin Y.; Courbin F.,Courtois H.M.; Cropper M.; Da Silva A.; Degaudenzi H.; De Lucia G.,Di Giorgio A.M.; Dolding C.; Dole H.; Dubath F.; Duncan C.A.J.; Dupac X.,Dusini S.; Ealet A.; Escoffier S.; Fabricius M.; Farina M.; Farinelli R.,Faustini F.; Ferriol S.; Finelli F.; Fourmanoit N.; Frailis M.,Franceschi E.; Galeotta S.; George K.; Gillis B.; Giocoli C.,Gomez-Alvarez P.; Gracia-Carpio J.; Granett B.R.; Grazian A.; Grupp F.,Gwyn S.; Haugan S.V.H.; Hoekstra H.; Holmes W.; Hook I.M.; Hormuth F.,Hornstrup A.; Hudelot P.; Jhabvala M.; Keihaenen E.; Kermiche S.,Kiessling A.; Kubik B.; Kuemmel M.; Kunz M.; Kurki-Suonio H.; Le Boulc'h Q.,Le Brun A.M.C.; Le Mignant D.; Liebing P.; 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.,Masters D.C.; Maurogordato S.; 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.; Nightingale J.W.,Padilla C.; Paltani S.; Pasian F.; Pedersen K.; Percival W.J.; Pettorino V.,Pires S.; Polenta G.; Poncet M.; Popa L.A.; Pozzetti L.; Raison F.,Rebolo R.; Renzi A.; Rhodes J.; Riccio G.; Romelli E.; Roncarelli M.,Rossetti E.; Rottgering H.J.A.; Rusholme B.; Saglia R.; Sakr Z.,Sanchez A.G.; Sapone D.; Sartoris B.; Schewtschenko J.A.; Schneider P.,Schrabback T.; Scodeggio M.; Secroun A.; Seidel G.; Seiffert M.; Serrano S.,Simon P.; Sirignano C.; Sirri G.; Skottfelt J.; Stanco L.; Steinwagner J.,Tallada-Crespi P.; Taylor A.N.; Tereno I.; 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.,Zerbi F.M.; Zinchenko I.A.; Zucca E.; Ballardini M.; Bozzo E.; Burigana C.,Cabanac R.; Cappi A.; Di Ferdinando D.; Escartin Vigo J.A.; Fabbian G.,Gabarra L.; Martin-Fleitas J.; Matthew S.; 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.; Anselmi S.,Archidiacono M.; Atrio-Barandela F.; Benoist C.; Benson K.; Bertacca D.,Bethermin M.; Blanchard A.; Blot L.; Boehringer H.; Brown M.L.; Bruton S.,Calabro A.; Camacho Quevedo B.; Caro F.; Carvalho C.S.; Castro T.,Cogato F.; Contini T.; Cooray A.R.; Cucciati O.; Davini S.; De Paolis F.,Desprez G.; Diaz-Sanchez A.; Diaz J.J.; Di Domizio S.; Diego J.M.,Duc P.-A.; Enia A.; Fang Y.; Ferrari A.G.; Finoguenov A.; Fontana A.,Fontanot F.; Franco A.; Ganga K.; Garcia-Bellido J.; Gasparetto T.,Gautard V.; Gaztanaga E.; Giacomini F.; Gianotti F.; Gozaliasl G.,Gregorio A.; Guidi M.; Gutierrez C.M.; Hall A.; Hartley W.G.; Hemmati S.,Hernandez-Monteagudo C.; Hildebrandt H.; Hjorth J.; Kajava J.J.E.; Kang Y.,Kansal V.; Karagiannis D.; Kiiveri K.; Kirkpatrick C.C.; Kruk S.,Legrand L.; Lembo M.; Lepori F.; Leroy G.; Lesci G.F.; Lesgourgues J.,Leuzzi L.; Liaudat T.I.; Loureiro A.; Macias-Perez J.; Maggio G.,Magliocchetti M.; Magnier E.A.; Mannucci F.; Maoli R.; Martins C.J.A.P.,Maurin L.; Miluzio M.; Monaco P.; Moretti C.; Morgante G.; Murray C.,Naidoo K.; Navarro-Alsina A.; Nesseris S.; Passalacqua F.; Paterson K.,Patrizii L.; Pisani A.; Potter D.; Quai S.; Radovich M.; Rocci P.-F.,Rodighiero G.; Sacquegna S.; Sahlen M.; Sanders D.B.; Sarpa E.,Schneider A.; Schultheis M.; Sciotti D.; Sellentin E.; Shulevski A.,Smith L.C.; Stanford S.A.; Tanidis K.; Testera G.; Teyssier R.; Tosi S.,Troja A.; Tucci M.; Valieri C.; Venhola A.; Verza G.; Vielzeuf P.,Walton N.A.; Soubrie E.
IVOA id: ivo://cds.vizier/j/a+a/711/a20

Euclid Q1. Little red dots properties

2026-07-08T00:00:00Z

Description: Recent observations with the James Webb Space Telescope (JWST) have revealed an interesting population of sources with a compact morphology and a characteristic v-shaped continuum, namely blue at a rest frame {lambda}<4000{AA} and red at longer wavelengths. The nature of these sources, which are called little red dots (LRDs), is still highly debated because it is unclear whether they host active galactic nuclei (AGNs) and their number seems to drop drastically at z<4. We took advantage of the 63deg^2^ covered by the quick Euclid Quick Data Release (Q1) to extend the search for LRDs to brighter magnitudes and lower redshifts than what was possible with JWST. This is fundamental for a broader view of the evolution of this peculiar galaxy population. The selection was performed by fitting the available photometric data (Euclid, the Spitzer Infrared Array Camera (IRAC), and ground-based griz data) with two power laws to retrieve the rest-frame optical and UV slopes consistently over a wide redshift range (i.e. z<7.6). We then excluded extended objects and possible line emitters and inspected the data visually to remove any imaging artefacts. The final selection included 3341 LRD candidates from z=0.33 to z=3.6, 29 of which were also detected in IRAC. The resulting rest-frame UV luminosity function, in contrast with previous JWST studies, shows that the number density of LRD candidates increases from high redshift to z=1.5-2.5 and decreases at even lower redshifts. The subsample of more robust LRD candidates that are also detected with IRAC show a weaker evolution, however, which is affected by low statistics and limited by the IRAC resolution. The comparison with previous quasar UV luminosity functions shows that LRDs are not the dominant AGN population at z<4 and M_UV_<-21. Follow-up studies of these LRD candidates are pivotal to confirm their nature, probe their physical properties, and determine whether they are compatible with JWST sources because the different spatial resolution and wavelength coverage of Euclid and JWST might select different samples of compact sources.
Author(s): Euclid Collaboration; Bisigello L.; Rodighiero G.; Fotopoulou S.,Ricci F.; Jahnke K.; Feltre A.; Allevato V.; Shankar F.; Cassata P.,Dalla Bonta E.; Gandolfi G.; Girardi G.; Giulietti M.; Grazian A.,Lovell C.; Maiolino R.; Matamoro Zatarain T.; Mezcua M.; Prandoni I.,Roberts D.; Roster W.; Salvato M.; Siudek M.; Tarsitano F.; Toba Y.,Vietri A.; Wang L.; Zamorani G.; Baes M.; Belladitta S.; Nersesian A.,Spinoglio L.; Lopez Lopez X.; Aghanim N.; Altieri B.; Amara A.,Andreon S.; Auricchio N.; Aussel H.; Baccigalupi C.; Baldi M.,Balestra A.; Bardelli S.; Basset A.; Battaglia P.; Bender R.; Biviano A.,Bonchi A.; Branchini E.; Brescia M.; Brinchmann J.; 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.,Courbin F.; Courtois H.M.; Cropper M.; Da Silva A.; Degaudenzi H.,De Lucia G.; Di Giorgio A.M.; Dolding C.; Dole H.; Dubath F.,Duncan C.A.J.; Dupac X.; Dusini S.; Ealet A.; Escoffier S.; Farina M.,Farinelli R.; Faustini F.; Ferriol S.; Finelli F.; Frailis M.,Franceschi E.; Galeotta S.; George K.; Gillard W.; Gillis B.; Giocoli C.,Gomez-Alvarez P.; Gracia-Carpio J.; Granett B.R.; Grupp F.; Gwyn S.,Haugan S.V.H.; Hoekstra H.; Holmes W.; Hook I.M.; Hormuth F.,Hornstrup A.; Hudelot P.; Jhabvala M.; Keihaenen E.; Kermiche S.,Kiessling A.; Kubik B.; Kuemmel M.; Kunz M.; Kurki-Suonio H.,Le Boulc'h Q.; Le Brun A.M.C.; Le Mignant D.; Liebing P.; 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.; Maurogordato S.; 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.,Nightingale J.W.; Padilla C.; Paltani S.; Pasian F.; Pedersen K.,Percival W.J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.; Popa L.A.,Pozzetti L.; Raison F.; Rebolo R.; Renzi A.; Rhodes J.; Riccio G.,Romelli E.; Roncarelli M.; Rossetti E.; Rottgering H.J.A.; Rusholme B.,Saglia R.; Sakr Z.; Sapone D.; Sartoris B.; Schewtschenko J.A.,Schirmer M.; Schneider P.; Schrabback T.; Scodeggio M.; Secroun A.,Seidel G.; Serrano S.; Simon P.; Sirignano C.; Sirri G.; 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.; Verdoes Kleijn G.; Veropalumbo A.; Wang Y.,Weller J.; Zacchei A.; Zerbi F.M.; Zinchenko I.A.; Zucca E.,Ballardini M.; Bolzonella M.; Bozzo E.; Burigana C.; Cabanac R.; Cappi A.,Di Ferdinando D.; Escartin Vigo J.A.; Gabarra L.; Huertas-Company M.,Martin-Fleitas J.; Matthew S.; Maturi M.; Mauri N.; Pezzotta A.,Poentinen M.; Porciani C.; Risso I.; Scottez V.; Sereno M.; Tenti M.,Viel M.; Wiesmann M.; Akrami Y.; Andika I.T.; Anselmi S.; Archidiacono M.,Atrio-Barandela F.; Benoist C.; Benson K.; Bertacca D.; Bethermin M.,Blanchard A.; Blot L.; Brown M.L.; Bruton S.; Calabro A.; Caro F.,Carvalho C.S.; Castro T.; Charles Y.; Cogato F.; Contini T.; Cooray A.R.,Cucciati O.; Davini S.; De Paolis F.; Desprez G.; Diaz-Sanchez A.,Diaz J.; Di Domizio S.; Diego J.M.; Enia A.; Fang Y.; Ferrari A.G.,Ferreira P.G.; Finoguenov A.; Fontana A.; Fontanot F.; Franco A.,Ganga K.; Garcia-Bellido J.; Gasparetto T.; Gautard V.; Gaztanaga E.,Giacomini F.; Gianotti F.; Gozaliasl G.; Guidi M.; Gutierrez C.M.,Hall A.; Hartley W.G.; Hemmati S.; Hernandez-Monteagudo C.,Hildebrandt H.; Hjorth J.; Kajava J.E.; Kang Y.; Kansal V.,Karagiannis D.; Kiiveri K.; Kirkpatrick C.; Kruk S.; Le Graet J.,Legrand L.; Lembo M.; Lepori F.; Leroy G.; Lesci G.F.; Lesgourgues J.,Leuzzi L.; Liaudat T.I.; Loureiro A.; Macias-Perez J.; Maggio G.,Magliocchetti M.; Magnier E.A.; Mancini C.; Mannucci F.; Maoli R.,Martins C.J.A.P.; Maurin L.; Miluzio M.; Monaco P.; Moretti C.,Morgante G.; Nadathur S.; Naidoo K.; Navarro-Alsina A.; Nesseris S.,Passalacqua F.; Paterson K.; Patrizii L.; Pisani A.; Potter D.; Quai S.,Radovich M.; Rocci P.-F.; Sacquegna S.; Sahlen M.; Sanders D.B.; Sarpa E.,Scarlata C.; Schaye J.; Schneider A.; Sciotti D.; Sellentin E.,Shulevski A.; Smith L.C.; Tanidis K.; Tao C.; Testera G.; Teyssier R.,Tosi S.; Troja A.; Tucci M.; Valieri C.; Venhola A.; Vergani D.; Verza G.,Vielzeuf P.; Viitanen A.; Walton N.A.; Weaver J.R.; Soubrie E.; Scott D.
IVOA id: ivo://cds.vizier/j/a+a/711/a24

Euclid Q1. Photometric studies of known transients

2026-07-08T00:00:00Z

Description: We report on serendipitous Euclid observations of previously known transients, using the Euclid Q1 data release. By cross-matching with the Transient Name Server (TNS) we identify 164 transients that coincide with the data release. Although the Euclid Q1 release only includes single- epoch data, we are able to make Euclid photometric measurements at the location of 161 of these transients. Euclid obtained deep photometric measurements or upper limits of these transients in the IE, YE, JE, and HE bands at various phases of the transient light-curves, including before, during, and after the observations of ground-based transient surveys. Approximately 70% of known transients reported in the six months before the Euclid observation date and with discovery magnitude brighter than 24 were detected in Euclid IE images. Our observations include one of the earliest near-infrared detections of a Type Ia supernova (SN 2024pvw) 15 days prior to its peak brightness, and the late-phase (435.9 days post peak) observations of the enigmatic core-collapse SN 2023aew. Euclid deep photometry provides valuable information on the nature of these transients such as their progenitor systems and power sources, with late time observations being a uniquely powerful contribution. In addition, Euclid is able to detect the host galaxies of some transients that were previously classed as hostless. The Q1 data demonstrate the power of the Euclid data even with only single-epoch observations available, as will be the case for much larger areas of sky in the Euclid Wide Survey.
Author(s): Duffy C.; Cappellaro E.; Botticella M.T.; Hook I.M.; Poidevin F.,Moriya T.J.; Chrimes A.A.; Petrecca V.; Paterson K.; Goobar A.; Galbany L.,Kotak R.; Gall C.; Gutierrez C.M.; Tao C.; Izzo L.; Aghanim N.; Altieri B.,Amara A.; Andreon S.; Auricchio N.; Baccigalupi C.; Baldi M.; Balestra A.,Bardelli S.; Basset A.; Battaglia P.; Biviano A.; Bonchi A.; Branchini E.,Brescia M.; Brinchmann J.; Camera S.; Capobianco V.; Carbone C.,Carretero J.; Casas R.; Casas S.; 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.; Di Giorgio A.M.; Dolding C.; Dole H.; Dubath F.; Duncan C.A.J.,Dupac X.; Dusini S.; Ealet A.; Escoffier S.; Farina M.; Faustini F.,Ferriol S.; Fotopoulou S.; Frailis M.; Franzetti P.; Galeotta S.; George K.,Gillis B.; Giocoli C.; Gomez-Alvarez P.; Grazian A.; Grupp F.; Gwyn S.,Haugan S.V.H.; Hoar J.; Hoekstra H.; Holmes W.; Hormuth F.; Hornstrup A.,Hudelot P.; Jahnke K.; Jhabvala M.; Keihanen E.; Kermiche S.; Kubik B.,Kuijken K.; Kummel M.; Kunz M.; Kurki-Suonio H.; Le Boulc'h Q.,Le Brun A.M.C.; Le Mignant D.; Liebing P.; Ligori S.; Lilje P.B.,Lindholm V.; Lloro I.; Maino D.; Maiorano E.; Mansutti O.; Marcin S.,Marggraf O.; Martinelli M.; Martinet N.; Marulli F.; Massey R.,Medinaceli E.; Melchior M.; Mellier Y.; Meneghetti M.; Merlin E.; Meylan G.,Moresco M.; Morris P.W.; Moscardini L.; Neissner C.; Nichol R.C.,Niemi S.-M.; Nightingale J.W.; Padilla C.; Paltani S.; Pasian F.,Pedersen K.; Percival W.J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.,Popa L.A.; Raison F.; Rebolo R.; Renzi A.; Rhodes J.; Riccio G.; Romelli E.,Roncarelli M.; Saglia R.; Sakr Z.; Sapone D.; Sartoris B.,Schewtschenko J.A.; 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.; Tereno I.,Toledo-Moreo R.; Torradeflot F.; Tutusaus I.; Valenziano L.; Vassallo T.,Verdoes Kleijn G.; Wang Y.; Weller J.; Zacchei A.; Zamorani G.; Zerbi F.M.,Zucca E.; Burigana C.; Cabanac R.; Gabarra L.; Scottez V.; Scott D.,Sullivan M.
IVOA id: ivo://cds.vizier/j/a+a/711/a38

Euclid Q1. Secondary nuclei in ET galaxies

2026-07-08T00:00:00Z

Description: Massive early-type galaxies (ETGs; M>10^11^M_{sun}_) are believed to form primarily through mergers of less massive progenitors, which leave behind numerous traces of violent formation histories, such as stellar streams and shells. A particularly striking signature of these mergers is the formation of supermassive black hole (SMBH) binaries, which can create depleted stellar cores through interactions with stars on radial orbits -- a process known as core scouring. The secondary SMBH in such systems may still carry a dense stellar envelope and thereby remain observable for some time as a secondary nucleus while it sinks towards the shared gravitational potential of the merged galaxy. Direct observations of secondary nuclei on sub-kiloparsec scales remain rare, with only a few notable cases, such as NGC5419. Investigating such features and building up statistics requires both high spatial resolution and wide-field coverage, a capability uniquely provided by Euclid. In this study, we leverage Euclid's Q1 Early Release data to systematically search for secondary nuclei in ETGs. We present a preliminary sample of 666 candidate systems distributed over 504 hosts (some of which contain multiple secondary nuclei). The vast majority of these fall at separations of 3 kpc to 15 kpc, indicative of normal mergers. However, 44 fall at projected separations of less than 2 kpc. We argue that this most interesting subset of secondary nucleus candidates -- those at very close angular separations -- are unlikely to be a consequence of chance alignments. We show that their stellar masses are mostly too large for them to be globular clusters and that a significant subset are unresolved even at Euclid's spatial resolution, rendering them too small to be dwarf galaxies. These objects may represent the highest-density nuclei of a previously merged galaxy currently sinking into the centre of the new common gravitational potential, and thus they likely host a secondary SMBH. We also demonstrate that convolutional neural networks offer a viable avenue to detect multiple nuclei in the 30 times larger sky coverage of the future Euclid DR1. Finally, we argue that our method can detect the remnants of a recoil event from two merged SMBHs, as two of our secondary nuclei candidates are unresolved at the Euclid spatial resolution, occur at projected physical separations of less than 2kpc, and occur in hosts of M>10^11^M_{sun}_, which makes them viable candidates.
Author(s): Fabricius M.; Saglia R.; Balzer F.; Ecker L.R.; Thomas J.; Bender R.,Gracia-Carpio J.; Magliocchetti M.; Marggraf O.; Rawlings A.; Sorce J.G.,Voggel K.; Wang L.; van der Wel A.; Altieri B.; Amara A.; Andreon S.,Auricchio N.; Baccigalupi C.; Baldi M.; Balestra A.; Bardelli S.,Biviano A.; Branchini E.; Brescia M.; Brinchmann J.; Camera S.,Canas-Herrera G.; Capobianco V.; Carbone C.; Carretero J.; Castellano M.,Castignani G.; Cavuoti S.; Chambers K.C.; Cimatti A.; Colodro-Conde C.,Congedo G.; Conselice C.J.; Conversi L.; Copin Y.; Courbin F.,Courtois H.M.; Cropper M.; Degaudenzi H.; De Lucia G.; Dolding C.; Dole H.,Dubath F.; Dupac X.; Dusini S.; Escoffier S.; Farina M.; Farinelli R.,Ferriol S.; Finelli F.; Frailis M.; Franceschi E.; Fumana M.; Galeotta S.,George K.; Gillis B.; Giocoli C.; Grazian A.; Grupp F.; Haugan S.V.H.,Hoar J.; Hoekstra H.; Holmes W.; Hook I.M.; Hormuth F.; Hornstrup A.,Jahnke K.; Jhabvala M.; Joachimi B.; Keihaenen E.; Kermiche S.,Kiessling A.; Kubik B.; Kuijken K.; 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.; 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.,Niemi S.-M.; Padilla C.; Paltani S.; Pasian F.; Pedersen K.; Percival W.J.,Pettorino V.; Pires S.; Polenta G.; Poncet M.; Popa L.A.; Pozzetti L.,Raison F.; Renzi A.; Rhodes J.; Riccio G.; Romelli E.; Roncarelli M.,Rottgering H.J.A.; Sakr Z.; Sanchez A.G.; 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.; Starck J.-L.,Steinwagner J.; Tallada-Crespi P.; Taylor A.N.; Teplitz H.I.; Tereno I.,Tessore N.; Toft S.; Toledo-Moreo R.; Torradeflot F.; Tutusaus I.,Valenziano L.; Valiviita J.; Vassallo T.; Verdoes Kleijn G.; Veropalumbo A.,Wang Y.; Weller J.; Wetzstein M.; Zacchei A.; Zamorani G.; Zinchenko I.A.,Zucca E.; Huertas-Company M.; Scottez V.; Siudek M.
IVOA id: ivo://cds.vizier/j/a+a/711/a39

X-ray point-like sources of Euclid (Q1)

2026-07-08T00:00:00Z

Description: To better understand the role of active galactic nuclei (AGN) in galaxy evolution, it is crucial to work with a complete and pure AGN sample. X-ray surveys are key to this, but identifying their counterparts (CTPs) at other wavelengths remains challenging due to their larger positional uncertainties and limited availability of deeper, uniform ancillary data. Euclid is revolutionising this effort, offering extensive coverage of nearly the entire extragalactic sky, particularly in the near-infrared bands, where AGN are more easily detected. With the first Euclid Quick Data Release (Q1), we validated methods for identifying and classifying Euclid CTPs to known point-like sources from major X-ray surveys, including XMM- Newton, Chandra, and eROSITA. Using Bayesian statistics, combined with machine learning (ML), as incorporated in the algorithm NWAY, we identify the CTPs to 11286 X-ray sources from the three X-ray telescopes. For the large majority of 10194 sources, the association is unique, with the remaining ~10% of multi-CTP cases equally split between XMM-Newton and eROSITA. Six per cent of the Euclid CTPs are detected in more than one X-ray survey. ML is then used to distinguish between Galactic (8%) and extragalactic (92%) sources. We computed photo-zs using deep learning for the 9259 sources detected in the 10th data release of the DESI Legacy Survey, reaching an accuracy and a fraction of outliers of roughly 5%. Based on their X-ray luminosities, all CTPs identified as extragalactic are classified as AGN, most of which appear as type I AGN according to their hardness ratios. With this paper, we release our catalogue, which includes identifiers, basic X-ray properties, the reliability of the associations, and additional property extensions such as Galactic/extragalactic classifications and photometric/spectroscopic redshifts. We also provide probabilities for sub-selecting the sample based on purity and completeness, allowing users to tailor the sample according to their specific needs.
Author(s): Euclid Collaboration: Roster W.; Salvato M.; Buchner J.; Shirley R.,Lusso E.; Landt H.; Zamorani G.; Siudek M.; Laloux B.; Matamoro Zatarain T.,Ricci F.; Fotopoulou S.; Ferre-Mateu A.; Lopez Lopez X.; Aghanim N.,Altieri B.; Amara A.; Andreon S.; Auricchio N.; Aussel H.; Baccigalupi C.,Baldi M.; Balestra A.; Bardelli S.; Battaglia P.; Biviano A.; Bonchi A.,Branchini E.; Brescia M.; Brinchmann J.; 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.; Courbin F.,Courtois H.M.; Cropper M.; Da Silva A.; Degaudenzi H.; De Lucia G.,Di Giorgio A.M.; Dolding C.; Dole H.; Dubath F.; Duncan C.A.J.; Dupac X.,Dusini S.; Escoffier S.; Fabricius M.; Farina M.; Farinelli R.; Faustini F.,Ferriol S.; Finelli F.; Fosalba P.; Fourmanoit N.; Frailis M.,Franceschi E.; Galeotta S.; George K.; Gillis B.; Giocoli C.,Gracia-Carpio J.; Granett B.R.; Grazian A.; Grupp F.; Gwyn S.,Haugan S.V.H.; Holmes W.; Hook I.M.; Hormuth F.; Hornstrup A.; Hudelot P.,Jahnke K.; Jhabvala M.; Keihaenen E.; Kermiche S.; Kiessling A.; Kubik B.,Kuemmel M.; Kunz M.; Kurki-Suonio H.; Le Boulc'h Q.; 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.; Marcin S.; Marggraf O.; Martinelli M.,Martinet N.; Marulli F.; Massey R.; Masters D.C.; 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.,Nightingale J.W.; Padilla C.; Paltani S.; Pasian F.; Pedersen K.,Percival W.J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.; Popa L.A.,Pozzetti L.; Raison F.; Rebolo R.; Renzi A.; Rhodes J.; Riccio G.,Romelli E.; Roncarelli M.; Saglia R.; Sakr Z.; Sanchez A.G.; Sapone D.,Sartoris B.; Schewtschenko J.A.; Schirmer M.; Schneider P.; Schrabback T.,Secroun A.; Seidel G.; Seiffert M.; Serrano S.; Simon P.; Sirignano C.,Sirri G.; Stanco L.; Steinwagner J.; Tallada-Crespi P.; Tavagnacco D.,Taylor A.N.; Tereno I.; 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.; Zerbi F.M.; Zinchenko I.A.,Zucca E.; Allevato V.; Ballardini M.; Bolzonella M.; Bozzo E.; Burigana C.,Cabanac R.; Cappi A.; Di Ferdinando D.; Escartin Vigo J.A.; Gabarra L.,Huertas-Company M.; Martin-Fleitas J.; Matthew S.; 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.; Anselmi S.,Archidiacono M.; Atrio-Barandela F.; Benoist C.; Benson K.; Bertacca D.,Bethermin M.; Bisigello L.; Blanchard A.; Blot L.; Boehringer H.,Brown M.L.; Bruton S.; Calabro A.; Caro F.; Carvalho C.S.; Castro T.,Cogato F.; Cooray A.R.; Cucciati O.; Davini S.; De Paolis F.; Desprez G.,Diaz-Sanchez A.; Diaz J.J.; Di Domizio S.; Diego J.M.; Enia A.; Fang Y.,Ferrari A.G.; Finoguenov A.; Fontana A.; Franco A.; Ganga K.,Garcia-Bellido J.; Gasparetto T.; Gautard V.; Gaztanaga E.; Giacomini F.,Gianotti F.; Gozaliasl G.; Guidi M.; Gutierrez C.M.; Hall A.; Hartley W.G.,Hemmati S.; Hernandez-Monteagudo C.; Hildebrandt H.; Hjorth J.,Kajava J.J.E.; Kang Y.; Kansal V.; Karagiannis D.; Kiiveri K.,Kirkpatrick C.C.; Kruk S.; Le Graet J.; Legrand L.; Lembo M.; Lepori F.,Leroy G.; Lesci G.F.; Lesgourgues J.; Leuzzi L.; Liaudat T.I.; Loureiro A.,Macias-Perez J.; Maggio G.; Magliocchetti M.; Mannucci F.; Maoli R.,Martins C.J.A.P.; Maurin L.; Miluzio M.; Monaco P.; Moretti C.; Morgante G.,Naidoo K.; Navarro-Alsina A.; Nesseris S.; Passalacqua F.; Paterson K.,Patrizii L.; Pisani A.; Potter D.; Quai S.; Radovich M.; Sacquegna S.,Sahlen M.; Sanders D.B.; Sarpa E.; Schneider A.
IVOA id: ivo://cds.vizier/j/a+a/711/a16

Observational data of GRBs

2026-07-08T00:00:00Z

Description: Gamma-ray burst (GRB) prompt and afterglow emission, as well as kilonova (KN) emission, are the expected electromagnetic (EM) counterparts of binary neutron star (BNS) and neutron star-black hole (NSBH) mergers. Only one BNS merger (GW170817) detected on the basis of gravitational waves (GWs) has a confirmed association with EM counterparts. Without a GW signal, the ejecta parameters from a KN can be used to infer the progenitor properties. We aim to infer the KN ejecta parameters and the progenitor properties by modeling merger-driven GRBs with a claim of KN, good data, and robust redshift measurements. We modeled the afterglow and KN, performing a Bayesian analysis, within the Nuclear physics and Multi-Messenger Astrophysics (NMMA) framework. The KN emission is modeled with the radiative transfer code POSSIS and for the afterglow, we used the afterglowpy library. In contrast to previous approaches, our methodology simultaneously models both the afterglow and KN. We find that all GRBs in our sample have a KN, but we were unable to confirm or exclude its presence in GRB 150101B. A BNS progenitor is favored for GRB 160821B, GRB 170817A/AT2017gfo, GRB 211211A, and GRB 230307A. For GRB 150101B and GRB 191019A, we found a slight preference for the NSBH scenario; however, a BNS is also a viable possibility. For KN emission, we see that the median wind mass <Mwind>=0.027^+0.046^_-0.019_M_{sun}_ is higher than the dynamical <Mdyn>=0.012^+0.007^_-0.006_M_{sun}_. We find that Mwind and the collimation-corrected kinetic energy of the jet can be attributed as log(Mwind)=-20.23+0.38log(E0,J). We confirm the results of numerical simulations that the mass-weighted tidal deformability increases with decrease in the chirp mass. Our results exemplify and reinforce that EM modeling is the only feasible pathway to investigate binary mergers in absence of GW observations. In this work, we present for the first time the binary progenitor properties of a sizable sample of merger-driven GRBs.
Author(s): Singh P.; Stratta G.; Rossi A.; Pang P.T.H.; Bulla M.; Ragosta F.,De Rosa A.; Kann D.A.; Cogato F.
IVOA id: ivo://cds.vizier/j/a+a/710/a350

Transit survey of 121 TESS M3-M6 dwarfs

2026-07-08T00:00:00Z

Description: As the most favorable hosts for small transiting planets, M-dwarf stars can be very useful in detecting these objects. A newly accessible discovery space has recently opened up thanks to mid-to-late M-dwarfs characterized by sufficient TESS multisector coverage thanks to new Cycle 6+ observations. This paper presents a systematic transit survey of 121 "newly enabled" M3-M6 dwarfs (Teff=2700-3400K) over a period of P=0.5-100d. These surveyed stars only recently crossed the multisector TESS detection threshold via Cycle 6+ coverage. The sample was selected from 498312 TIC M-dwarfs via a nine-step funnel. The pipeline combines a transit least squares approach (TLS) with a signal validation cascade, TRICERATOPS vetting, Gaia data release 3 (DR3) verification, and three empirical signal reliability tests. The pipeline validation achieved 100% recovery (16/16 planets) on ten known systems with zero false positives. The survey identified 20 transit-like signals across 16 systems, none of which had been characterized by any prior TESS object of interest (TOI) designations. The reliability framework classified two as tier 1 (high robustness), seven as tier 2 (moderate), and ten as tier 3 (noise-susceptible), while one monotransit was excluded. For nine out of 16 hosts, the candidate SDE sits at or below the measurable noise floor. Of the remaining seven, the floor lies below SDE_in,_=7 and the candidates end up exceeding it. The global false alarm rate is 17.4% (21/121; Wilson 95% CI: [11.6%, 25.1%]). The survey quantifies TLS sensitivity limits on active M3-M6 dwarfs with sparse TESS coverage. The two tier 1 candidates are priorities for RV confirmation. The ten tier 3 candidates require additional TESS sectors to establish a signal persistence, while nine systems call for high-resolution imaging to confirm their classification.
Author(s): Tschudi Y.
IVOA id: ivo://cds.vizier/j/a+a/710/a352

DeepDive + DJA QG catalog

2026-07-08T00:00:00Z

Description: We present the DeepDive program, in which we obtained deep (1-3 hours) JWST/NIRSpec G235M/F170LP spectra for ten primary massive (log(Mstar/Msun)=10.8-11.5) quiescent galaxies at z~3-4. A novel reduction procedure was used to extend the nominal wavelength coverage of G235M beyond Halpha and [NII] at z~4, revealing weak, narrow Halpha lines indicative of low star formation rates (SFR~ 0-5 Msun yr-1). Two out of ten primary targets have broad Halpha lines, indicating the presence of active galactic nuclei. We also conducted an archival search of quiescent galaxies observed with NIRSpec gratings in the DAWN JWST Archive, which provides a statistical context for interpreting the DeepDive targets. This archival search provided a spectroscopic sample of 126 quiescent galaxies spanning 1<z<5, selected by high Dn4000, UVJ color, or low specific star formation rate (more than one dex lower than that of the star formation main sequence), and covering more than an order of magnitude in stellar mass. This sample allowed us to revisit the sample from the different selections, finding ~90% overlap between these criteria. The total sample of 136 quiescent galaxies constructed in this study shows that those at z~3-5, including the DeepDive targets, typically exhibit weaker 4000AA breaks and bluer colors than their lower-redshift counterparts, indicating generally younger stellar populations. Stacked spectra of sources grouped by the Dn4000 index reveal faint iron and magnesium absorption line features in the stellar continuum even for the low Dn4000 (Dn4000<1.35) subsample at high redshift (z~3). In addition, higher Dn4000 subsamples show fainter nebular emission lines. These results demonstrate that medium-resolution NIRSpec spectroscopy is essential for robustly characterizing the diversity and evolution of early quiescent galaxies. The large sample constructed in this paper will allow a statistical census of the properties of quiescent galaxies at high redshift to be obtained. All photometric and spectroscopic data from this study have been made publicly available.
Author(s): Ito K.; Valentino F.; Brammer G.; Hamadouche M.L.; Whitaker K.E.,Kokorev V.; Zhu P.; Kakimoto T.; Wu P.-F.; Antwi-Danso J.; Baker W.M.,Ceverino D.; Faisst A.L.; Farcy M.; Fujimoto S.; Gallazzi A.; Gillman S.,Gottumukkala R.; Heintz K.E.; Hirschmann M.; Jespersen C.K.; Kubo M.,Lee M.; Magdis G.; Onodera M.; Shimakawa R.; Tanaka M.; Toft S.; Weaver J.R.
IVOA id: ivo://cds.vizier/j/a+a/710/a364

KiDS grav. lenses obscured by foreground light

2026-07-08T00:00:00Z

Description: Many lensing images are often obscured by foreground light from the central galaxies, making them challenging to detect. To address the limitations of previous lens search efforts, particularly for samples with smaller RE or faint lensed images, we developed a composite CNN framework that utilizes both U-Net and ResNet architectures for feature extraction and classification. We propose a hybrid search method that combines U-Net and ResNet architectures to enhance the detection of the foreground galaxy-obscured lenses. Our approach consists of two main stages: first, the U-Net model separates the foreground galaxy light from potential lensing signals, creating residual images that highlight the lensing features. Next, the ResNet module performs binary classification on these residual images to determine the presence of lensing signals. We evaluated the hybrid search method with real observational data to demonstrate its effectiveness, achieving a recall of 71.5% and a 4.5% false positive rate at a confidence threshold of 0.6. By applying this method to over 638398 galaxy samples from the Kilo-Degree Survey Data Release 4 and conducting thorough inspections, we identified 88 Class A, 322 Class B, and 1758 Class C candidates. This hybrid approach significantly enhances the completeness of existing strong gravitational lensing searches and shows great potential for improving future astronomical surveys.
Author(s): Liu S.; Li R.; Jia J.; Li H.; Chen L.; Cao X.; He Z.; Busillo V.,Napolitano N.N.; Tortora C.; Zhong F.; Su H.; Feng H.; Dong Y.; Li R.,Gao L.
IVOA id: ivo://cds.vizier/j/a+a/710/a366

SN 2021lwz light curves

2026-07-08T00:00:00Z

Description: Current large-scale, high-cadence surveys, such as the Zwicky Transient Facility (ZTF), provide detections of new and rare types of transients and supernovae (SNe) whose physical origins are not well understood. We aim to investigate the nature of SN 2021lwz at a redshift z=0.065, an over-luminous SN with an absolute magnitude of Mg~-20.1 AB that falls in the lower range of superluminous supernovae (SLSNe) luminosities and was discovered in a faint dwarf galaxy with an absolute magnitude of Mg~-14.5 AB. We studied SN 2021lwz using optical spectroscopy and photometry and by imaging linear polarimetry obtained during several follow-up campaigns. All the data were used to analyse and model the evolution of the explosion. Comparisons with other SNe of well-known or rarer types were investigated. SN 2021lwz belongs to the rare class of rapidly evolving transients. The bolometric light curve rises in about seven days to a peak luminosity of about 5x10^43^erg/s, at a rate of 0.2mag/day close to the peak. Spectroscopy modelling reveals more similarities with a normal Type Ic-like SN than with an SLSN before peak, showing slightly broadened lines after peak. Light curve modelling shows that the Arnett model of the bolometric light curve using a radioactive source (56 Ni) is not able to reasonably explain the light curve evolution. A magnetar model seems more appropriate, suggesting that the explosion of low ejecta mass (Mej~0.24 solar mass) took place in a low-mass (M~10^6.66^ solar mass) dwarf galaxy of specific star formation rate about ten times larger than typical star-forming galaxies. SN 2021lwz is an uncommon transient showing many similarities with several classes of transients, including rare transients. It may be an interesting example of how differences in ejecta mass and engine parameters could produce a wide range of engine-driven stripped-envelope SNe.
Author(s): Poidevin F.; West S.L.; Omand C.M.B.; Koenyves-Toth R.; Schulze S.; Yan L.,Kangas T.; Perez-Fournon I.; Geier S.; Sollerman J.; Pessi P.J.,Gutierrez C.M.; Chen T.-W.; Hinds K-Ryan; Marques-Chaves R.; Shirley R.,Jimenez Angel C.; Lunnan R.; Perley D.A.; Sarin N.; Yao Y.; Dekany R.,Purdum J.; Wold A.; Laher R.R.; Graham M.J.; Kasliwal M.M.; Jegou Du Laz T.
IVOA id: ivo://cds.vizier/j/a+a/710/a367

Srg C Region CII datacubes

2026-07-08T00:00:00Z

Description: Sagittarius C (Sgr C) is a massive, relatively quiescent complex at the western edge of the Galaxy's Central Molecular Zone (CMZ). While the Sgr B2 region has been extensively studied, Sgr C has received comparatively less attention. We aim to characterize the kinematics and physical state of the gas in Sgr C using spatially and velocity-resolved [CII] 158 microns emission. This line traces the multi-phase interstellar medium, providing a crucial complement to molecular, infrared, and radio observations. We present a fully sampled 74x47 pc map of the [CII] line toward Sgr C, observed with SOFIA. The data feature a 0.55 pc spatial and 1km/s spectral resolution. These observations are analyzed in conjunction with ancillary maps of the CO(2-1) transition and its isotopologues from the APEX telescope. [CII] emission is widespread, showing a continuous structure extending from Sgr A to Sgr C with complex morphology. The bulk emission arises at negative radial velocities, consistent with Galactic rotation. The most prominent feature is the giant Sgr C HII region, where [CII] reveals an expanding, ring-like shell interpreted as a photo-dissociation region (PDR). Kinematic modelling yields an expansion velocity of 23km/s and a dynamical age of about 0.13Myr. Our analysis suggests that stellar winds from known massive stars are insufficient to power the observed expansion, pointing toward alternative drivers like a buried supernova. Finally, we find a striking spatial association between this shell and a non-thermal radio filament, indicating that the shell's expansion has triggered high-mass star formation at its edge.
Author(s): Riquelme-Vasquez D.; Guesten R.; Morris M.R.; Harris A.I.,Requena-Torres M.A.; Morales E.F.E.; Stutzki J.; Simon R.; Risacher C.,Higgins R.
IVOA id: ivo://cds.vizier/j/a+a/710/a309

OJ 287 polarisation in radio, mm and optical

2026-07-07T18:33:13Z

Description: OJ 287 is a bright blazar with century-long observations, and one of the strongest candidates to host a supermassive black hole binary. Its polarisation behaviour between 2015 and 2017 (MJD 57300-58000) contains several interesting events that we re-contextualise in this study. We collected optical photometric and polarimetric data from several telescopes and obtained high-cadence light curves from this period. In the radio band, we collected mm-wavelength polarisation data from the AMAPOLA program. We combined these with existing multifrequency polarimetric radio results and the results of very-long-baseline-interferometry imaging with the Global mm-VLBI Array at 86GHz. In December 2015, an optical flare was seen according to the general relativistic binary black hole model. We suggest that the overall activity near the accretion disk and the jet base during this time may be connected to the onset of a new moving component K seen in the jet in March 2017. With the additional optical data, we find a fast polarisation angle rotation of ~210{deg} coinciding with the December 2015 flare, hinting at a possible link between these events. Based on the 86-GHz images, we calculated a new speed of 0.12mas/yr for K, which places it inside the core at the time of the 2015 flare. This speed also supports the scenario where the passage of K through the quasi-stationary feature S1 could have been the trigger for the very-high-energy gamma-ray flare of OJ 287 seen in February 2017. With the mm-polarisation data, we established that these bands follow the cm-band data but show a difference during the time of K passing through S1. This indicates that the mm-bands trace the substructures of the jet still unresolved in the cm-bands.
Author(s): Jormanainen J.; Hovatta T.; Lindfors E.; Berdyugin A.; Chamani W.,Fallah Ramazani V.; Jermak H.; Jorstad S.G.; Laehteenmaeki A.; McCall C.,Nilsson K.; Smith P.; Steele I.A.; Tammi J.; Tornikoski M.; Wierda F.
IVOA id: ivo://cds.vizier/j/a+a/694/a206

OFS Observatory Archive TAP service

2026-07-07T11:10:18Z

Description

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

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

Author(s)

AISAS LSO team

IVOA id

ivo://lso.dc/tap

Magellanic Cloud tip of the red giant branch

2026-07-07T07:20:24Z

Description: We have calibrated the tip of the red giant branch (TRGB) using our recent catalogue of homogeneous globular cluster (GC) distances. The GC distances were determined via a global joint fit to optical period-Wesenheit relations of their member RR Lyrae stars and type-II Cepheids, anchored by trigonometric parallaxes; all data were taken from the ESA Gaia mission's (early) third data release (GDR3). Using I-band measurements of 48 GCs from P. Stetson's database, we determined M_I,0_=-3.948^+0.037^_-0.034_mag (1.6% in distance). Calibrating the TRGB using Gaia's homogeneous, space-based RP photometry of 53 GCs, we found M_RP,0_=-3.807^+0.041^_-0.035_mag (1.8%). The stated uncertainties include statistical and systematic effects, including the correlated nature of the GC distances. The robustness of our calibrations was evaluated via tests against small-number statistics and analysis choices. Within the (small) uncertainties, no significant metallicity effect is detected in our sample of old, low-metallicity GCs. We measured approximately 2% distances to the Large and Small Magellanic Clouds, 18.447^+0.036^_-0.042_mag (48.9+/-0.9kpc) and 18.898^+0.049^_-0.054_mag (60.2+/-1.4kpc), respectively, using a single photometric system: RP (spectro-)photometry from GDR3. Our new TRGB distances, whose absolute scale derives from Gaia parallaxes, are fully independent of the well-known detached eclipsing binary (DEB) distances and agree with them to within the uncertainties. Combining our new TRGB and existing DEB distances, we illustrate how additional constraints can be incorporated into the Local Distance Network and obtain H0=73.52+/-0.80km/s/Mpc. Expected improvement thanks to the upcoming fourth Gaia data release are discussed.
Author(s): Cruz Reyes M.; Anderson R.I.; Lengen B.
IVOA id: ivo://cds.vizier/j/a+a/708/l8

Gaia XP asteroseismic parameters

2026-07-07T06:45:58Z

Description: Red giants are key tracers of stellar evolution and Galactic structure, and their asteroseismic properties - particularly the large frequency separation ({DELTA}{nu}), the frequency of maximum oscillation power ({nu}max), and the dipole-mode period spacing ({DELTA}{PI}1) - provide direct insight into their internal structure, masses, and evolutionary states. Until now, seismic inferences on large stellar samples have relied primarily on high-quality light curves from missions such as Kepler and TESS or on moderate-resolution spectroscopy (LAMOST : R~1800 and APOGEE : R~22500) that clearly preserve information correlated with these seismic quantities. With Gaia XP spectra (R~15-85), the possibility arises to obtain asteroseismic measurements of orders of magnitude more stars, despite the much lower spectral resolution. Our goal is to assess whether XP spectra retain enough information to enable reliable seismic inference for red giants. We developed hybrid convolutional neural network (CNN) - long short-term memory (LSTM) models trained on red giants with seismic parameters measured from Kepler photometry. The networks learn the subtle spectral signatures - imprinted through global stellar properties - that correlate with {DELTA}{nu}, {nu}max, and {DELTA}{PI}1. The models recover all three global asteroseismic parameters from Gaia XP spectra with accuracies comparable to results based on moderate-resolution surveys such as LAMOST, demonstrating that even low-resolution spectrophotometry carries sufficient information for seismic prediction. Saliency analysis reveals wavelength regions most strongly associated with seismic sensitivity and highlights the physically distinct spectral behavior between RGB and RC stars. Applying our models to Gaia DR3 yielded seismic predictions for more than 2.5 million bright red giants, which allows for population-level asteroseismic studies on an unprecedented scale. We also identified a small subset of low-{DELTA}{nu} red clump candidates that show unusual spectral-seismic correlations, offering new avenues for investigating evolved stellar populations.
Author(s): Barman R.; Bhattacharya S.; Hanasoge S.M.; Dhanpal S.
IVOA id: ivo://cds.vizier/j/a+a/711/a121

Predicted spectral type of white dwarf

2026-07-06T07:25:39Z

Description: The latest Gaia data release provides astrometric measurements for 1.8 billion sources and low-resolution spectra for 220 million, including approximately 100 000 white dwarfs. Although useful for pre-classification, Gaia spectra lack the resolution required for accurate spectral typing and reliable parameter determination, motivating dedicated spectroscopic follow-up observations. We assess the reliability of machine-learning spectral classifications derived from Gaia spectra through comparison with medium-resolution spectroscopy.We determine the nature of objects classified as "massive helium-rich (DB)" white dwarfs by automated methods, and characterise the properties of warm and hot DQ (carbon-dominated) white dwarfs, as well as magnetic and metal-polluted objects. We observed 255 white dwarfs along the Gaia B and Q branches with the Gran Telescopio Canarias equipped with the OSIRIS instrument (R~1000). Spectral types were assigned through visual inspection and compared with machine-learning classifications applied to Gaia spectra. For objects labelled as "massive DBs", we independently determined their atmospheric spectral composition. Magnetic white dwarfs were identified via Zeeman splitting, and first-order magnetic field strengths were estimated when possible. Machine-learning classifications are highly accurate (>90% for spectral types included in their training sets), despite the low resolution of Gaia spectra. We determine the true nature of objects classified as "massive DBs" to be largely composed of magnetic white dwarfs and warm DQs, with only 5 of 112 observed objects (4.46%) confirmed as genuine DBs. Warm DQs are found along the Gaia Q branch and exhibit unusually high tangential velocities. We provide spectral classifications for 255 white dwarfs and demonstrate that Random Forest algorithms reliably classify low-resolution Gaia spectra for the main spectral types. We also determine the nature of objects classified as "massive DBs" and identify a large population of magnetic white dwarfs and carbon-rich objects. Several rare subtypes are identified, including 2 DAB, 1 DBAZ, 1 DZAB, 2 DZBA, 14 DAH, 1 DAQ, 1 DQZA, 4 hot and 29 warm DQ stars, along with 63 magnetic white dwarfs. The location and kinematics of warm DQs are consistent with previous studies, supporting their proposed origin as merger remnants.
Author(s): Garcia-Zamora E.M.; Torres S.; Rebassa-Mansergas A.; Ferrer-Burjachs A.
IVOA id: ivo://cds.vizier/j/a+a/711/a70

149 FXTs detected with BeppoSAX-WFC

2026-07-06T07:23:24Z

Description: We performed a search for fast X-ray transients (FXTs), defined for the purposes of this work as transients with durations of longer than one second and shorter than one day. We used data from the Wide Field Camera (WFC) instrument on board the BeppoSAX X-ray observatory collected between June 1996 and April 2002. The WFC sensitivity ranged from 10^-9^erg/s/cm^2^ (2-10keV), for a timescale of 10s, to a few times 10^-11^erg/s/cm^2^,, for a timescale of 10^5^s. The WFC location accuracy was 0.7-4.9 arcmin at a 68% confidence. We focused our search on gamma-ray bursts (GRBs), X-ray flashes (XRFs), and X-ray flares from high-mass X-ray binaries and stellar flares. Overall, 149 FXTs were detected. 63 of these are new to the literature. 38 flares were identified with 22 nearby stars. Three stars in the sample have never been seen flaring before in X-rays or optical (NLTT 51688, GR Dra and UCAC4 255-003783). We find that the MeV transient GRO J1753+57 is most likely the same object as GR Dra, rather than an active galactic nucleus (AGN) as previously thought. Eleven flares were detected from known high-mass X-ray binaries with irregular wind accretion. 100 GRBs were identified. Of these, 24 had not been published before. We classified 38% of the X-ray detected GRBs as XRFs with a relatively high X-ray-to-gamma-ray flux ratio. The gamma rays were measured with the BeppoSAX Gamma Ray Burst Monitor. The duration and spectral hardness distribution of all FXTs are bimodal, separating the group roughly in transients that are either shorter or longer than 1 ksec and with relatively hard and soft spectra, respectively. We identified the "short" FXTs as GRBs and XRFs and the "long" FXTs as flares from nearby late-type stars and X-ray binaries. The BeppoSAX-WFC FXT sample is found to be consistent with the one observed by Einstein Probe when the sensitivity of the two instruments is taken into account. These results suggest that the bulk of the population of faints events disclosed by Einstein Probe could represent the extension of a similar population to lower luminosities.
Author(s): in 't Zand J.J.M.; Guidorzi C.; Heise J.; Amati L.; Kuulkers E.,Frontera F.; Gianfanga G.; Piro L.
IVOA id: ivo://cds.vizier/j/a+a/711/a60