VO Fresh

Euclid Quick Release 2

2026-07-15T00:00:00Z

Description: The Euclid Galactic Bulge Survey (EGBS) took images with Euclid's VIS camera of 4.8 sq. deg. over nine adjoining fields. This dataset is an unprecedented deep, wide-field, high-resolution view of the inner bulge region of our Milky Way galaxy. The Q2 release contains calibrated images as well as photometry and astrometry catalogues of all stars in this field.
Author(s): Euclid Consortium
IVOA id: ivo://irsa.ipac/euclid/images/q2

Pulsation timing of two sdB binaries from TESS

2026-07-10T13:40:56Z

Description: Hot subdwarf B (sdB) stars are post-main-sequence stars of high temperature and gravity. Approximately 30% of sdBs exhibit stable pressure and/or gravity-mode pulsations, which can be used via the timing method to test for companion stars and determine their orbital solutions. We used short cadence data from the Transiting Exoplanet Survey Satellite (TESS) to search for previously undiscovered companions to sdBs. In this paper, we focus on searching for companions with orbital periods shorter than 13.5days which are detectable within one sector of TESS data (about 27days). The timing method requires that we derive pulsation frequencies in subsets of data significantly shorter than the periods we are searching for, which we set at 0.5-1.5day. We investigated ten sdB stars with previously detected p-mode pulsations for which at least one p-mode pulsation remains detectable with a signal-to-noise ratio >4 within data subsets of duration 0.5-1.5day. We find that two (TIC 202354658 and TIC 69298924) of these ten sdB stars likely have white-dwarf companions and set limits on companion masses for the other eight sdB stars.
Author(s): Otani T.; Baran A.S.; Spence L.C.; von Hippel T.; Lozano E.L.-,Clark J.M.
IVOA id: ivo://cds.vizier/j/aj/170/199

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

SHEDR3: All-sky molecular clouds extinction catalog

2026-07-10T08:46:00Z

Description: Although interstellar dust extinction serves as a powerful distance estimator, the solar system's location within the Galactic plane complicates distance determinations, especially for molecular clouds (MCs) at varying distances along the line of sight (LoS). The presence of complex extinction patterns along the LoS introduces degeneracies, resulting in less accurate distance measurements to overlapping MCs in crowded regions of the Galactic plane. In this study, we develop the CUSUM-based Jump-point Analysis for Distance Estimation (CU-JADE), a novel method designed to help mitigate these observational challenges. The key strengths of CU-JADE include: (1) sensitivity to detect abrupt jumps in Distance-A{lambda} (D-A) data sets, (2) minimal systematic errors as demonstrated on both mock and observed data, and (3) the ability to combine CUSUM analysis with multiwavelength data to improve the completeness of distance measurements for nearby gas structures, even for extinction values as low as {Delta}AV>=0.15mag. By combining CO survey data with a large sample of stars characterized by high-precision parallaxes and extinctions, we uncovered the multilayered molecular gas distribution in the high-latitude Cepheus region. We also determined accurate distances to MCs beyond the Cygnus Rift by analyzing the intricate structure of gas and extinction within the Galactic plane. Additionally, we constructed a full-sky 3D extinction map extending to 4kpc, which provides critical insights into dense interstellar medium components dominated by molecular hydrogen. These results advance our understanding of the spatial distribution and physical properties of MCs across the Milky Way.
Author(s): Zhang S.; Su Y.; Chen X.; Fang M.; Du F.; Zhang S.; Yan Q.-Z.; Liu X.,Zhang M.; Sun Y.; Yang Ji
IVOA id: ivo://cds.vizier/j/aj/170/185

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

Distant quiescent galaxies DJA data

2026-07-10T07:38:35Z

Description: Massive galaxies stopped forming stars surprisingly early in the history of the Universe. However, after quenching, the galaxies continued to grow in size across time, as established in the literature up to cosmic noon. We assemble one of the largest and most comprehensive multiwavelength photometric sample of massive quenched galaxies at z>3 from publicly available JWST observations, counting 137 quiescent candidates within ~825arcmin^2^ and redshift 3<=z<7 across the well-studied extragalactic fields GOODS, PRIMER, and CEERS. We modeled their surface brightness distribution across five bands mapping their UV-to-near-IR rest-frame wavelength with Sersic profiles, and derived their sizes, concentrations, and ellipticities. The size-mass relation is consistent with previous studies, showing a shallower slope at low redshift z{in}[3, 3.5] and a steeper slope at high redshift z>3.5. The size decreases with increasing redshift, in agreement with previous studies and we extend them up to zspec=4.9. Leveraging the large sample statistics, we robustly constrain the intrinsic scatter of the mass-size relation to ~0.3dex with no relevant dependence on the redshift and the filter used. At the population level, our multiwavelength modeling reveals that the size decreases with increasing observed wavelength, and the wavelength gradient decreases with increasing stellar mass. This result proves that in the near-IR bands, massive elliptical galaxies appear to be more compact. The Sersic index shows no significant dependence on wavelength, regardless of the stellar mass. Following a forward-backward Bayesian fit analysis to assess the significance of several parameters in predicting the size of our sample, we identified no significant secondary dependence of the size on the axis ratio q, Sersic index n, UVJ-colors, or environment. The combination of stellar mass and redshift is sufficient to predict the size of quiescent galaxies at z>3, albeit with a large scatter. This suggests that the commonly used parameters of a Sersic distribution cannot explain the large intrinsic scatter around the stellar mass-size relation, suggesting that other physical quantities need to be taken into account to break the degeneracy between evolution paths across the galaxy population.
Author(s): Scarpe G.; Valentino F.; Ito K.; Baker M. W.; Pensabene A.; Zhu P.
IVOA id: ivo://cds.vizier/j/a+a/711/a177

Ks-band images of 18 Seyfert galaxies

2026-07-10T07:36:00Z

Description: The high-resolution imaging of active galactic nuclei on sub-kiloparsec scales offers an important avenue for investigating their fueling. Observations in the near-infrared are especially valuable as they minimize the absorption by dust. However, the inferred nuclear morphology may depend on the method used to analyze the images. The aim of this study is to assess whether ground-based adaptive-optics observations of the cores of Seyfert 2 galaxies in the Ks-band provide advantages over HST observations at shorter wavelengths (V- and H-band). We also investigate whether a dedicated two-dimensional analysis is preferable to a one-dimensional approach. A sample of 18 Seyfert 2 galaxies was observed with the adaptive optics system in the Ks-band at the Large Binocular Telescope and compared to archival HST V- or H-band images. The analysis included two-dimensional modeling via GALFIT and the use of the unsharp masking technique. The results obtained in different filters are mutually consistent, indicating no clear advantage of using a redder filter. Using GALFIT and unsharp-masking in concert is preferable, as the two methods provide complementary strengths. We identify nuclear stellar rings in 8 of the 18 galaxies in our sample (44+-12%. This fraction is significantly higher than reported in previous studies, and about a factor of two higher than found in the most complete atlas of nuclear rings. The radii, size distribution, and inferred masses of the detected nuclear rings are similar to those observed in non-active galaxies. Low-luminosity active nuclei seem to have little, if any, impact on the formation and evolution of nuclear rings. The high incidence of nuclear stellar rings was unexpected and warrants further investigation. It can be tested using the large number of suitable archival HST images available. If confirmed, it would imply that nuclear stellar rings are considerably more common than previously recognized.
Author(s): Mackensen N.; Heidt J.; Pozo Nunez F.
IVOA id: ivo://cds.vizier/j/a+a/711/a169

He abundances in galactic O-type stars

2026-07-10T07:34:36Z

Description: The presence of massive O-type stars with surfaces enriched by CNO-cycle products has been known since the early 1980s. For many years, internal rotational mixing was assumed to be the dominant mechanism responsible for this chemical contamination. However, accumulating evidence suggests that binary interaction may play an equally important, if not dominant, role. We aim to carry out a large-scale investigation of surface helium (He) abundances in Galactic O-type stars, based on the results from the analysis of high-quality spectroscopic data from the IACOB project. We perform a homogeneous spectroscopic analysis of 318 Galactic O-type stars with the iacob-broad and fastwind/iacob-gbat tools, deriving rotational velocities, atmospheric parameters, and He abundances. We also account for the influence of binarity, and parameter degeneracies on the abundance determinations. We present homogeneously determined surface He abundances (YHe=N(He)/N(H)) for the so far largest, statistically significant sample of Galactic O-type stars. About 60% of the stars show He abundances consistent with the cosmic abundance standard of YHe=0.098+/-0.002. For another 18% of the stars, we obtain anomalously low He abundance estimates, reaching values down to 0.07. These unusual He abundances might be a consequence of flux contamination of the analyzed spectra by a faint companion. The remaining 22% display clear He enrichment (YHe>0.13). We provide observational evidence indicating that most of these He-enriched stars are likely the products of binary interaction.Our study highlights how large spectroscopic surveys are gradually opening robust observational avenues to identify the products of massive binary interaction. It also emphasizes the need for caution when interpreting the spectroscopic properties of apparently single O-type stars. A significant fraction may in fact be the outcome of binary evolution rather than isolated stellar birth.
Author(s): Simon-Diaz S.; Holgado G.; Martinez-Sebastian C.; Carretero-Castrillo M.,Jin H.; Urbaneja M.A.; Gamen R.; Puls J.; de Burgos A.; Garcia M.,Herrero A.; Keszthelyi Z.; Langer N.; Najarro F.; Paredes J.M.; Ribo M.
IVOA id: ivo://cds.vizier/j/a+a/711/a151

Anti-mass-segregated open clusters in MW

2026-07-10T07:25:59Z

Description: Mass segregation, defined as the preferential concentration of massive stars towards cluster centres, is a well-established outcome of two-body relaxation in star clusters. It is not yet established whether the inverse configuration, in which massive stars are preferentially dispersed to large radii, can survive over dynamical timescales on a population scale. We investigate whether anti-mass-segregated open clusters exist as a statistically significant, dynamically stable population in the Milky Way. We used 2800 open clusters from the Gaia DR3 catalogue and identified mass segregation using two independent diagnostics: the minimum spanning tree ratio (Lambda_MSR_) and the centre-of-mass distance ratio (Lambda_CC_), evaluated for the five and ten most massive members. We further performed direct N-body simulations to test the dynamical stability of anti-segregated configurations. We identify 706 anti-mass-segregated clusters (25.2% of the sample). Compared to the normal population, these systems are systematically more extended (+20% in the half-mass radius), dynamically younger (~39% in dynamical age) and have longer relaxation timescales (+25%). The mass excess of anti-segregated clusters relative to normal clusters increases monotonically with dynamical age, reaching +109% at tau=5-10. Direct N-body simulations confirm that anti-segregated configurations remain stable over multiple relaxation timescales, while mass-segregated and random clusters develop strong positive segregation. Anti-mass segregation is a dynamically stable structural state that likely reflects primordial cluster conditions. The prevalence of this configuration provides indirect constraints on the central mass content of open clusters, as massive central black holes would rapidly disrupt the anti-segregated state.
Author(s): Zhang S.; Huang L.; Zhao W.; Chi H.; Chen J.
IVOA id: ivo://cds.vizier/j/a+a/711/a138

SPHERE infrared survey for exoplanets. V.

2026-07-10T07:21:53Z

Description: Unbiased surveys of large stellar samples are the prime means through which the prevalence of exoplanets can be derived, and crucial constraints to planet formation models can be set.Direct imaging (DI) is ideally positioned to probe the outer regions (5-300au) of planetary systems, providing complementary information to techniques such as transits and radial velocities. We present the full sample of the SpHere INfrared survey for Exoplanets (SHINE), the second largest DI campaign to date. SHINE observed 460 stars between 2015 and 2023 thanks to the guaranteed time observations (GTO) allocated by ESO to the SPHERE consortium at VLT. The goal of this paper is to homogeneously derive the stellar properties of the targets and to define a subsample of young single hosts to be used as a starting point for the final statistical analysis of the survey. Stellar ages were determined based on kinematic indicators (such as the membership to young moving groups), age diagnostics (lithium abundance, rotation, and activity), and isochrone fitting. A thorough vetting for binarity was undertaken combining astrometric, spectroscopic, and imaging data. A subsample of 333 stars, covering a large extent of stellar ages and masses, was constructed. Selection criteria, global features, as well as the properties of individual stars are reported and discussed.
Author(s): Squicciarini V.; Desidera S.; Chauvin G.; Kiefer F.; D'Orazi V.,Fontanive C.; Vigan A.; Nardiello D.; Messina S.; Albert D.; Bergeon S.,Beuzit J.-L.; Biller B.; Boccaletti A.; Bonavita M.; Bonnefoy M.,Brandner W.; Cantalloube F.; Cheetham A.; Delorme P.; Dominik C.; Feldt M.,Galicher R.; Gratton R.; Hagelberg J.; Henning T.; Janson M.; Lagadec E.,Lagrange A.-M.; Langlois M.; Lazzoni C.; Le Coroller H.; Ligi R.,Maire A.-L.; Marleau G.-D.; Menard F.; Mesa D.; Meunier N.; Meyer M.,Mordasini C.; Moutou C.; Mueller A.; Perrot C.; Samland M.; Schmid H.M.,Schmidt T.; Sissa E.; Turatto M.; Udry S.; Zurlo A.; Abe L.; Antichi J.,Baruffolo A.; Baudoz P.; Baudrand J.; Bazzon A.; Blanchard P.; Bohn A.J.,Carbillet M.; Carle M.; Cascone E.; Charton J.; Claudi R.; Costille A.,De Caprio V.; Delboulbe A.; Dohlen K.; Engler N.; Fantinel D.; Feautrier P.,Fusco T.; Gigan P.; Girard J.H.; Giro E.; Gisler D.; Glueck L.; Gry C.,Hubin N.; Hugot E.; Jaquet M.; Kasper M.; Le Mignant D.; Llored M.,Madec F.; Magnard Y.; Martinez P.; Maurel D.; Moeller-Nilsson O.,Mouillet D.; Moulin T.; Origne A.; Pavlov A.; Perret D.; Petit C.; Pragt J.,Puget P.; Rabou P.; Ramos J.; Rigal F.; Rochat S.; Roelfsema R.; Rousset G.,Roux A.; Salasnich B.; Sauvage J.-F.; Sevin A.; Soenke C.; Stadler E.,Suarez M.; Wahhaj Z.; Weber L.; Wildi F.
IVOA id: ivo://cds.vizier/j/a+a/711/a136

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

Distance results for the Galactic Ring Survey

2026-07-09T18:36:31Z

Description: Knowledge about the distribution of CO emission in the Milky Way is essential to understand the impact of Galactic environment on the formation and evolution of structures in the interstellar medium. However, currently our insight about the fraction of CO in spiral arm and interarm regions is still limited by large uncertainties in assumed rotation curve models or distance determination techniques. In this work we use the Bayesian approach from Reid et al. (2016ApJ...823...77R) and Reid et al. (2019ApJ...885..131R) that is based on our presently most precise knowledge about the structure and kinematics of the Milky Way to obtain the current best assessment of the Galactic distribution of ^13^CO from the Galactic Ring Survey (GRS). We performed two different distance estimates that either included (Run A) or excluded (Run B) a model for Galactic features, such as spiral arms or spurs. We also include a prior for the solution of kinematic distance ambiguity that was determined from a compilation of literature distances and an assumed size-linewidth relationship. Even though the two distance runs show strong differences due to the prior for Galactic features for Run A and larger uncertainties due to kinematic distances in Run B, the majority of their distance results are consistent with each other within the uncertainties. We find that the fraction of ^13^CO emission associated with spiral arm features varies between 76% to 84% between the two distance runs. The vertical distribution of the gas is concentrated around the Galactic midplane showing full-width at half-maximum values of ~75pc. We do not find any significant difference between gas emission properties associated with spiral arm and interarm features. In particular the distribution of velocity dispersion values of gas emission in spurs and spiral arms is very similar. We detect a trend of higher velocity dispersion values with increasing heliocentric distance, which we however attribute to beam averaging effects caused by differences in spatial resolution. We argue that the true distribution of the gas emission is likely more similar to a combination of the two discussed distance results, and highlight the importance of using complementary distance estimations to safeguard against the pitfalls of any single approach. We conclude that the methodology presented in this work is a good approach for distance determinations of gas emission features in Galactic plane surveys.
Author(s): Riener M.; Kainulainen J.; Henshaw J.D.; Beuther H.
IVOA id: ivo://cds.vizier/j/a+a/640/a72

Rate coefficients of OCS by He

2026-07-09T18:27:55Z

Description: In typical molecular clouds, analyzing the physic-chemical conditions with non-LTE models requires the knowledge of the collisional rate coefficients of the detected molecule with the most common colliders in the interstellar medium (ISM), e.g., H_2_, He, and H. The OCS molecule has been widely observed in the ISM. However, the collision data available for this species were calculated using a potential energy surface (PES) that shows differences with more recent surfaces. The main goal of this work is to report a new set of rate coefficients for the collisional of OCS with He based on a new PES computed at a high level of theory. A large set of ab initio energies calculated using the coupled cluster with single, double, and perturbative triple excitations (CCSD(T)) method at the completed basis set limit for the OCS+He complex is employed to develop an analytical PES. This surface is used in close-coupling calculations, and a new set of collisional rate coefficients for OCS by He is computed. The de-excitation rate coefficients are compared with previously available data. Furthermore, a |{DELTA}j|=1 propensity rule was observed. Finally, a set of rate coefficients for the lower thirty-nine rotational states of OCS are reported, which is the largest set determined up to date for this collision.
Author(s): Denis-Apizar O.; Guerra C.; Zarate X.
IVOA id: ivo://cds.vizier/j/a+a/680/a113

C-MetaLL survey. IX. Cepheid data

2026-07-09T18:25:11Z

Description: The C-MetaLL project has provided homogeneous spectroscopic abundances of 290 Classical Cepheids (DCEPs) for which we have the intensity-averaged magnitudes in multiple optical and near-infrared (NIR) bands, periods, pulsation modes, and Gaia parallaxes corrected for individual zero-point (ZP) biases. Our goal is to derive updated period-Wesenheit-metallicity (PWZ) relations using the largest and most homogeneous metallicity sample ever used for such analyses, covering a range of -1.3<[Fe/H]<+0.3dex, and to assess the metallicity dependence of these relations. We computed several optical and NIR Wesenheit magnitudes adopting both Cardelli et al. and Fitzpatrick reddening laws, and transformed Johnson-Cousins Wesenheit magnitudes into their HST equivalents using empirical relations. Using 275 DCEPs with reliable parallaxes, we applied a robust photometric parallax technique, which simultaneously fits all parameters --- including the global ZP counter-correction to Gaia parallaxes --- and handles outliers via a Cauchy likelihood to account for the sample's excess variance. We find a stronger metallicity dependence (gamma~-0.5mag/dex in optical, ~-0.4mag/dex in NIR) than recent literature reports. Gaia parallax ZP counter-correction epsilon varies smoothly across bands, with an average value of ~10 muas, aligning with previous determinations. Applying our PWZ relations to ~4500 LMC Cepheids yields distances generally consistent within 1 sigma with geometric estimates. The choice of reddening law has a small impact, while using only fundamental-mode pulsators significantly increases the uncertainties. Including alpha-element corrections increases abs(gamma) and reduces epsilon. However, we find 1 sigma consistency gamma values with the literature, particularly for the Wesenheit magnitude in the HST bands, by restricting the sample to brighter (i.e. closer) objects, or by including only pulsators with -0.7<[Fe/H]<0.2dex. Our results hint at a large gamma or a non-linear dependence on metallicity of DCEP luminosities at the metal-poor end, which is difficult to quantify with the precision of parallaxes of the present dataset.
Author(s): Ripepi V.; Trentin E.; Catanzaro G.; Marconi M.; Bhardwaj A.; Clementini G.,Cusano F.; De Somma G.; Molinaro R.; Sicignano T.; Storm J.
IVOA id: ivo://cds.vizier/j/a+a/708/a216

MW-MC Bridge young stellar members

2026-07-09T16:50:11Z

Description: The interaction between the LMC and SMC (the Clouds) has resulted in prominent tidal features, including an extended bridge of gas and stars connecting the two galaxies. This Bridge has likely formed during the most recent interaction between the Clouds, about 150-250Myr ago. While some young stars observed in the Bridge have formed in-situ from the tidally stripped gas, stellar populations may also have been drawn out of the SMC during the tidal interaction. We aim to identify a clean sample of likely Bridge stars in the region between the LMC and SMC using Gaia DR3 astrometric and photometric data combined with machine-learning techniques. We use the dimensionality-reduction algorithm UMAP to construct a training sample of young stars in the outskirts of the SMC and LMC. A neural network trained on this sample is then applied to Gaia sources in the inter-Cloud region to classify the stars and identify candidate Bridge members. We present and characterise a new sample of young candidate Bridge stars, selected from Gaia DR3. We investigate its spatial distribution, kinematic properties and colour-magnitude diagram and validate it using existing Bridge samples. The young stellar Bridge aligns well with HI gas, clusters, and Cepheid samples, apart from a small offset near the LMC outer disc. We measure a Bridge length of ~15kpc and the stars are travelling from the SMC to the LMC at a median tangential velocity of ~114km/s. This implies a crossing time of ~125Myr, which is within the timeframe of the last interaction of the Clouds and therefore supports tidal stripping as a possible formation scenario of the Bridge.
Author(s): Schoelch M.; Jimenez-Arranz O.; Romero-Gomez M.; Luri X.
IVOA id: ivo://cds.vizier/j/a+a/711/a55

Gaia GSP-Spec catalogue

2026-07-09T16:47:23Z

Description: The Gaia/DR3 GSP-Spec module has published the atmospheric parameters of up to 5.6 million stars, thanks to the analysis of their Radial Velocity Spectrometer spectra. By combining these spectroscopic parameters with Gaia parallax and photometric measurements, a large catalogue of interstellar colour excesses and extinctions, complemented with stellar luminosities, radii and masses is constructed, without relying on any stellar evolution or structure models. This catalogue also contains their associated uncertainties estimated from Monte-Carlo realisations, for about 4.6 million stars. A system of quality flags based on the GSP-Spec quality parameters, the achieved numerical precision, and the Gaia astrometric quality is presented. Adopting these flags, we defined a sub-sample of high-accuracy and precision parameters of more than 1.5 million stars. The impact of possible GSP-Spec parameter inaccuracies on the derived extinctions, luminosities, radii and masses are also explored, revealing that the mass is the most affected quantity. The validations of the radii and masses, by comparison with interferometric and asteroseismic data, confirm their high-quality, even when the targets suffer from large interstellar extinction. We also emphasize that they are fully compatible and homogeneous with the GSP-Spec parameters. This allows to avoid systematics and biases that could be hidden when combining data from different (and potentially) heterogeneous catalogues. Some example applications of this catalogue are finally presented: (i) exoplanet radii and masses, (ii) present day mass distribution functions, (iii) identification of Galactic populations from their mass distribution, and (iv) Galactic halo accreted star luminosities and masses confirming their merger epochs.
Author(s): de Laverny P.; Recio-Blanco A.; Navarrete C.; Palicio P.A.; Spitoni E.
IVOA id: ivo://cds.vizier/j/a+a/711/a54

Stellar rotation in open clusters

2026-07-09T16:33:29Z

Description: Stellar rotation is a fundamental ingredient in shaping the evolution of stars and it can also be used to trace past stellar interactions. Yet, systematic studies of stellar rotation in large samples of stars belonging to different populations have only recently been made possible, thanks to spectroscopic surveys. We profit from the catalogue of rotational broadening and rotation periods released with Gaia DR3. We focus on open clusters to study the rotational behaviour of several interesting populations including, among others, blue stragglers and extended main sequence turnoffs (eMSTO). We use literature lists of almost a million member stars in several thousand open clusters in the Milky Way. We collect properties of stars and clusters from large surveys, including Gaia, and from various literature sources. We include a comprehensive collection of known variables and binary stars from various databases. We manually select (exotic) stellar populations from the color-magnitude diagrams of individual clusters and study their rotational properties. Our catalogue contains more than 44000 rotationally characterised stars, almost 57000 variables (excluding binaries) and more than 22000 binary stars. We find several interesting results, including a few hundred new blue stragglers, several fast rotating red giants, and we increase the number of clusters with an eMSTO to 96. We discover that most clusters more massive than 10^3^M_{sun}_ display an eMSTO. We present a new parametrization of the number of blue stragglers as a function of cluster mass and age. We find that the percentage of binary stars in the equal-mass binary sequence and in the main sequence are similar. Conclusions: We present the first large-scale statistical exploration of stellar rotation in open clusters, which already yielded new interesting results and which can be used as the basis for several detailed follow-up studies.
Author(s): Pancino E.; Reggiani E.; Marinoni S.; Marrese P.M.; Alvarez Garay D.,Avdeeva A.; Echeveste M.; Leitinger E.; Nedhath S.; Rani S.; Sanna N.,Saracino S.; Steinbauer L.; Turchi A.; Jadhav V.V.; Kamann S.; Rainer M.
IVOA id: ivo://cds.vizier/j/a+a/711/a67

Scaling K2. VIII. Sub-Neptunes & M dwarfs

2026-07-09T12:44:06Z

Description: We uniformly combined data from the NASA Kepler and K2 missions to compute planet occurrence rates across the entire FGK and M-dwarf stellar range. The K2 mission, driven by targets selected by guest observers, monitored nine times more M dwarfs than the Kepler mission. Combined, Kepler and K2 observed 130 short-period (P=1-40days) Earth to Neptune-sized candidate planets orbiting M dwarfs. K2 observed 3.5 times more of these planets than Kepler for host stars below 3700K. Our planet occurrence rates show that short-period sub-Neptunes peak at 3750_-97_^+153^K and drop for cooler M dwarfs. A peak near this location was predicted by pebble accretion planet formation models and confirmed here by observations for the first time. Super-Earths continue to increase in occurrence toward cooler stars and show no clear evidence of a peak in the host star range considered here (3200-6900K). Our observations provide critical input to further refine planet formation models. We strongly recommend further study of mid-to-late M dwarfs with TESS and soon the Nancy Grace Roman Space Telescope and PLATO to identify additional small planet trends.
Author(s): Hardegree-Ullman K.K.; Bergsten G.J.; Christiansen J.L.; Zink J.K.,Bhure S.; Boley K.M.; Fernandes R.B.; Giacalone S.; Karpoor P.R.
IVOA id: ivo://cds.vizier/j/aj/170/183

Sub-Neptunes obliquities & Marroon-X TOI-1759 RVs

2026-07-08T12:43:51Z

Description: We present the Rossiter-McLaughlin measurement of the sub-Neptune TOI-1759A b with MAROON-X. A joint analysis with MuSCAT3 photometry and nine additional TESS transits produces a sky-projected obliquity of |{lambda}|=4{deg}+/-18{deg}. We also derive a true obliquity of {psi}=24{deg}+/-12{deg} making this planet consistent with full alignment albeit to <1{sigma}. With a period of 18.85days and an a/R* of 40, TOI-1759A b is the longest period single sub-Neptune to have a measured obliquity. It joins a growing number of smaller planets which have had this measurement made and, along with K2-25 b, is the only single, aligned sub-Neptune known to date. We also provide an overview of the emerging distribution of obliquity measurements for planets with R<8R_{Earth}_. We find that these types of planets tend toward alignment, especially the sub-Neptunes and super-Earths, implying a dynamically cool formation history. The majority of misaligned planets in this category have 4<R<=8R_{Earth}_ and are more likely to be isolated than planets rather than in compact systems. We find this result to be significant at the 3{sigma} level, consistent with previous studies. In addition, we conduct injection and recovery testing on available archival radial velocity data to put limits on the presence of massive companions in these systems. Current archival data is insufficient for most systems to have detected a giant planet.
Author(s): Polanski A.S.; Crossfield I.J.M.; Seifahrt A.; Bean J.L.; Brande J.,Collins K.A.; Coria D.R.; Fukui A.; Narita N.; Sturmer J.; Giacalone S.,Kasper D.
IVOA id: ivo://cds.vizier/j/aj/170/182

APOGEE: M dwarfs metallicity & planet parameters

2026-07-08T11:43:04Z

Description: One important property in studying the exoplanet population is the host star metallicity ([M/H]). In this study, we derived stellar metallicities and oxygen abundances for 48 M dwarf stars using the near-infrared high-resolution spectra from the SDSS APOGEE survey and synthetic spectra computed in LTE. We also investigated the exoplanetary radii distribution for a larger sample of 246 exoplanets orbiting 188 M dwarf stars. The [M/H] versus [O/M] distribution obtained indicates that our sample is composed mainly of thin disk stars, which follow the behavior of the low-alpha sequence in the Milky Way thin disk. Small planets with radii smaller than 3R_{Earth}_ were found around stars with a range of metallicities (-0.6<[M/H]<+0.3), while larger planets of the sample orbit only stars with [M/H]>=0.0. These results indicate that while small planets can form in different environments, larger planets preferentially form in metal-rich protoplanetary disks. Exoplanets with P_orb_<4.3days orbit on average more metal-rich stars than planets with longer periods. This threshold is smaller than that found for FGK stars (8-10days) and might be related to M dwarfs having a smaller dust sublimation radius. The distribution of exoplanets with R_p_>4R_{Earth}_ shows a concentration at orbital periods between 2 and 5days, which may result from inward orbital migration. There is also a different behavior between single-detected exoplanets and planets from multiplanetary systems, with the latter being found on average around more metal-poor stars, and with planetary radii roughly up to 3R_{Earth}_.
Author(s): Wanderley F.; Cunha K.; Souto D.; Smith V.V.; Daflon S.
IVOA id: ivo://cds.vizier/j/aj/170/177

2MASS & Gaia DR3 phot. of YSOs in three clusters

2026-07-08T09:39:56Z

Description: The outer Galaxy presents a distinctive environment for investigating star formation. This study develops a novel approach to identify true cluster members based on unsupervised clustering using astrometry with significant uncertainties. As a proof of concept, we analyze three outer Galactic young stellar object (YSO) clusters at different distances and densities within 65<l<265, each known to contain >100 members based on the Star Formation in Outer Galaxy (SFOG; E. Winston et al. (2020) catalog. The 618 YSO clusters in the SFOG data set were based on 2D clustering. In this contribution, we apply the Hierarchical Density-Based Spatial Clustering of Applications with Noise (HDBSCAN*) algorithm to the precise Gaia DR3 astrometry to assign YSO cluster membership. A Monte Carlo simulation coupled with the HDBSCAN* (HDBSCAN-MC algorithm) addresses YSO astrometric uncertainties through 5D clustering. We introduce the Generation Of cLuster anD FIeld STar (GOLDFIST) simulation to enable robust membership determination, performing an unsupervised clustering analysis in higher-dimensional feature space while accommodating measurement errors. In this study, we extended our approach to distant outer galaxy YSOs and clusters with larger astrometric uncertainties. The results include the discovery of new members in the previously identified clusters. We also analyze the known stars in the clusters and confirm their membership. The derived membership probabilities are included in the provided cluster catalogs. The more accurately predicted simulation distance estimates closely agree, within uncertainty limits, with the median distance estimates derived from Gaia data, and are compared with the kinematic distances from the Wide- field Infrared Survey Explorer H ii survey.
Author(s): Patel V.; Hora J.L.; Ashby M.L.N.; Vig S.
IVOA id: ivo://cds.vizier/j/aj/170/172

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

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

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

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

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

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

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

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

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

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

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

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

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