VO Fresh

TCO Echelle Spectra of Hot Supergiants

2026-06-22T11:24:42Z

Description

Spectral Archive of Hot Galactic Supergiants (TCO Node)

This resource provides a digital archive of one-dimensional (1D) optical spectra of hot galactic supergiants, obtained at the Three College Observatory (TCO). The archive is integrated into the Kazakhstan National Virtual Observatory (KazVO) data services and optimized for the IVOA Simple Spectral Access Protocol (SSAP).

**Data Specification:**

* Data Type: Medium-resolution optical echelle spectra.
* File Format: FITS (Flexible Image Transport System).
* Data Representation: 1D merged (stitched) spectra.
* Flux Calibration: Relative intensity, normalized to the continuum.

**Observational Setup and Instrumentation:**

* Observatory: Three College Observatory (TCO), North Carolina, USA
* Telescope: 0.81-m Ritchey-Chretien telescope
* Instrument: Fiber-fed echelle spectrograph eShel
* Spectrograph Manufacturer: Shelyak Instruments

**Spectral Characteristics:**

* Spectral Range: Approximately 3900 - 7800 Angstroms (precise wavelength boundaries are frame-dependent and fixed within individual FITS headers).
* Spectral Resolution: R approx 12,000.
* Wavelength Calibration: Executed using a Thorium-Argon (ThAr) reference lamp spectrum.

**Data Reduction Pipeline:**

Primary and scientific data reduction was performed within the IRAF (Image Reduction and Analysis Facility) environment using standard echelle spectroscopy packages.

**Key Reduction Steps:**

1. Pre-processing: Bias frame subtraction.
2. Extraction: Localization and extraction of individual echelle orders.
3. Dispersion Relation: Wavelength calibration based on ThAr reference frames.
4. Order Merging: Stitching of discrete spectral orders into a continuous 1D array.
5. Kinematic Correction: Application of the heliocentric velocity correction (documented under the VHELIO FITS header keyword).
6. Continuum Normalization: Continuum flattening achieved via high-order polynomial fitting.

Author(s)

Danford, S.; Miroshnichenko, A.

IVOA id

ivo://fai.kz/tco_hot_supergiants/q/ssa

Study of TESS LCs RRc stars variation modes

2026-06-20T14:48:47Z

Description: Using two years of data from the TESS space telescope, we have investigated the time series of 633 overtone pulsating field RR Lyrae (RRc) stars. The majority of stars (82.8 per cent) contain additional frequencies beyond the main pulsation. In addition to the frequencies previously explained by the l = 8 and 9 non-radial modes, we have identified a group of stars where the additional frequencies may belong to the l = 10 non-radial modes. We found that stars with no additional frequencies are more common among stars with shorter periods, while stars with longer periods almost always show additional frequencies. The incidence rate and this period distribution both agree well with the predictions of recent theoretical models. The amplitude and phase of additional frequencies are varying in time. The frequencies of different non-radial modes appearing in a given star seem to vary on different time-scales. We have determined a 10.4 per cent incidence rate for the Blazhko effect. For several stars we have detected continuous annual-scale phase change without significant amplitude variation. This type of variation offers a plausible explanation for the 'phase jump' phenomenon reported in many RRc stars. The main pulsation frequency could show quasi-periodic phase and amplitude fluctuations. This fluctuation is clearly related to additional frequencies present in the star: stars with two non-radial modes show the strongest fluctuations, while stars with no such modes show no fluctuations at all. The summation of the phase fluctuation over time may explain the O-C variations that have long been known for many non-Blazhko RRc stars.
Author(s): Benko J.M.; Plachy E.; Netzel H.; Bodi A.; Molnar L.; Pal A.
IVOA id: ivo://cds.vizier/j/mnras/521/443

HECATE nearby galaxies stellar properties

2026-06-20T14:39:07Z

Description: We present the Heraklion Extragalactic Catalogue, or HECATE, an all-sky value-added galaxy catalogue, aiming to facilitate present and future multiwavelength and multimessenger studies in the local Universe. It contains 204 733 galaxies up to a redshift of 0.047 (D <~ 200 Mpc) , and it is >50 per cent complete in terms of the B-band luminosity density at distances in the 0-170 Mpc range. By incorporating and homogenizing data from astronomical data bases and multiwavelength surveys, the catalogue offers positions, sizes, distances, morphological classifications, star formation rates, stellar masses, metallicities, and nuclear activity classifications. This wealth of information can enable a wide range of applications, such as (i) demographic studies of extragalactic sources, (ii) initial characterization of transient events, and (iii) searches for electromagnetic counterparts of gravitational-wave events. The catalogue is publicly available to the community at a dedicated portal, which will also host future extensions in terms of the covered volume and data products.
Author(s): Kovlakas K.; Zezas A.; Andrews J.J.; Basu-Zych A.; Fragos T.,Hornschemeier A.; Kouroumpatzakis K.; Lehmer B.; Ptak A.
IVOA id: ivo://cds.vizier/j/mnras/506/1896

Optical spectra of 14 planetary nebula candidates

2026-06-19T11:48:22Z

Description: The Gaia DR3, released in June 2022, included low-resolution BP/RP (XP) spectra that have been exploited for the classification of various types of emission-line objects using machine-learning techniques. The Gaia Extended Stellar Parametrizer for Emission-Line Stars (ESP-ELS) algorithm identified 273 sources as potential planetary nebulae (PNe). We aim to analyze the PN sample produced by the ESP-ELS algorithm to investigate the true nature of the objects classified as PNe. We extracted all sources from the Gaia catalog classified as PNe by the ESP-ELS algorithm and filtered out 200 objects with secure classifications available in the literature. Of these, ~65% correspond to known Galactic or Magellanic compact PNe, and ~20% to D- or D'-type symbiotic systems. The XP spectra of the remaining sources were visually inspected, leading to a subset of 14 promising candidates showing strong emission features attributable to Halpha and [OIII]lambda5007. Although typical of PNe, such features are also consistent with D- or D'-type symbiotics, known to mimic compact PNe. We obtained spectroscopic follow-up observations for these objects with the 2SPOT facilities in Chile and France, complemented by an analysis of archival photometric data to further constrain their nature. We report the identification of nine bona-fide or likely D- or D'-type symbiotic systems, one planetary nebula in the LMC, one polar cataclysmic variable, and three possible Be stars in (or in the direction of) the SMC, within our sample of 14 objects.
Author(s): Mulato L.; Merc J.; Charbonnel S.; Garde O.; Le Du P.; Petit T.
IVOA id: ivo://cds.vizier/j/a+a/710/a298

Gaia20fnr reduced spectra

2026-06-19T11:43:30Z

Description: The microlensing event Gaia20fnr is a long-duration, non-caustic-crossing binary-lens event located at high Galactic latitude. Triggered by a photometric rise detected by the Gaia space mission, the event was followed up with observations from multiple ground-based facilities and observed by four space telescopes: Gaia, NEOWISE, Swift, and TESS. We characterize the Gaia20fnr microlensing system by determining the physical and orbital properties of the binary lens, the nature of the luminous source, and the kinematics of both the source and the lens. We employed a binary-lens microlensing model including full Keplerian orbital motion and annual microlens parallax to fit the photometric data. The event is best explained by a K2 giant source at D_S_=3.10+/-0.10kpc lensed by a stellar binary composed of M_L,1_=0.46+/-0.06M_{sun}_ and M_L,2_=0.52+/-0.06M_{sun}_ at a distance of D_L_=0.54+/-0.05kpc. The light curve exhibits strong signatures of orbital motion and requires a full Keplerian model with a period of P=0.67+/-0.04yr and a radial-velocity semi-amplitude of K_1_=16.9+/-0.9km/s to be explained. Gaia20fnr is one of the few microlensing events for which a complete Keplerian binary-lens solution has been derived. The model can be tested with follow-up radial-velocity and high-resolution imaging observations as well as forthcoming Gaia DR4 and DR5 astrometric time-series data. Its long duration, multi-peak structure, and extensive coverage from both space- and ground-based facilities make it a benchmark for studying faint nearby low-mass binaries through microlensing.
Author(s): Wicker M.; Wyrzykowski L.; Hundertmark M.; Rybicki K.A.; Zielinski P.,Stonkute E.; Gromadzki M.; Maskoliunas M.; Ihanec N.; Ratajczak M.,Bachelet E.; Kruszynska K.; Dominik M.; Buckley D.A.H.; Gezer I.,Chene A.-N.; Mikolajczyk P.; Kotysz K.; Majumdar J.; Pakstiene E.,Zdanavicius J.; Cepas V.; Jonauskaite U.; Bozza V.; Cassan A.,Figuera Jaimes R.; Rabus M.; Rota P.; Street R.A.; Tsapras Y.,Wambsganss J.; Awiphan S.; Brincat S.M.; Budzik Z.; Davidson J.W. Jr.,Dymock R.; Galdies C.; Godunova V.; Hambsch F.-J.; Jablonska M.; Kowalik P.,Kvernadze T.; Larma M.; Makowska M.; Markus Y.; Merc J.; Michniewicz O.,Motylinski M.; Popowicz A.; Radziwonowicz M.; Reichart D.; Romanov F.D.,Simon A.O.; Trzcionkowski P.; Wrobel E.; Zejmo M.; Zola S.
IVOA id: ivo://cds.vizier/j/a+a/710/a294

NGC 2509 spellar param. and abundances

2026-06-19T11:32:22Z

Description: NGC 2509 is a distant (~2.5kpc) and little-studied open cluster located in the third Galactic quadrant. It is a moderately old cluster, whose age has not yet been precisely determined. The main-sequence stars in NGC 2509 follow a narrow distribution in the color-magnitude diagram, unlike other clusters of similar age. In addition, its chemical composition has never been investigated. To address these issues and characterize the cluster we performed moderate- and high-resolution spectroscopy with FLAMES@VLT of 132 stars, both dwarfs and giants, which represents a significant fraction (~73%) of likely members. We provide atmospheric stellar parameters and, for the first time, chemical abundances for 21 species with atomic numbers up to 60. In our analysis we followed two different methodologies, both of which will be used for the incoming WEAVE stellar surveys. We find an average radial velocity for NGC 2509 of 58.6+/-1.3km/s and a mild supersolar metallicity ([Fe/H]~0.1dex). This value is slightly higher than expected according to its galactocentric distance, but still compatible with the Galactic gradient. From the lithium content of the dwarfs and the isochrone-fitting method we obtain an age for NGC 2509 of 1.26+/-0.3Gyr. The reddening across the cluster field is negligible (A_V_=0.25+/-0.02mag). The cluster peculiar main sequence turnoff is due to a narrow distribution of the rotational velocities peaking at vsini~80km/s, with little dispersion. The chemical pattern of NGC 2509 follows the Galactic trends shown by other open clusters in the Galactic thin disk.
Author(s): Boeche C.; Alonso-Santiago J.; Bragaglia A.; Frasca A.; Vallenari A.,Kallimanis I.N.; Carrera R.; Bossini D.; Lucatello S.; D'Orazi V.; Costa G.
IVOA id: ivo://cds.vizier/j/a+a/710/a285

Wide sdB binaries parameters

2026-06-19T11:30:28Z

Description: Long-period binary systems containing a B-type hot subdwarf (sdB) and a main-sequence (MS) companion are thought to originate from binary interactions involving stable mass transfer from the red giant, the progenitor of the sdB, to the MS companion. However, despite the recent progress in modelling their population, some of their observed properties are not entirely understood. Because determining their orbits requires extended campaigns of high-resolution spectroscopic observations, only a limited number of long-period sdB binaries have been studied with completely determined orbital parameters. We aim to expand the current sample of long-period sdB binaries with fully determined orbital parameters through the analysis of high-resolution spectroscopic data. In addition, the atmospheric parameters of the cool companions are analysed. Increasing the number of well-characterised systems will provide valuable insights into their formation channels and main characteristics. A sample of 32 wide binary systems containing sdB stars was selected for the analysis of the radial velocity (RV) curves of both companions. The dataset consisted of high-resolution spectra obtained with the HERMES and UVES spectrographs. The orbital parameters were derived by simultaneously fitting Keplerian orbits to the RVs of the sdB and its companion. The atmospheric parameters of the cool companions were determined using the GSSP code, which analyses the master spectra of the systems with a grid of LTE atmospheric models. An additional sample of wide sdB binaries was built by cross-matching the Gaia NSS catalogue with literature catalogues of sdB candidates and spectroscopically confirmed sdB systems. The outcomes from both samples were compared with existing theoretical models to assess their consistency with current formation and evolutionary scenarios. We obtained complete orbital solutions for 32 wide sdB binaries. The orbital period distribution of the ground-based spectroscopic sample is in reasonable agreement with population-synthesis predictions, except for two outliers. The CMD further suggests that current models overpredict systems with the coolest companions, since the observed systems with BP-RP>0.3 are associated with companions hotter than 6000K. The observed period-mass ratio distribution is consistent with recent population synthesis predictions, and suggests that the unexplained second branch found in these models is mainly populated by old systems. Excluding the two long-period outliers, the data do not support a clear increase in eccentricity with orbital period, whereas the Gaia-based candidate sample shows discrepant behaviour, owing to selection effects and larger uncertainties.
Author(s): Molina F.; Vos J.; Bobrick A.; Vuckovic M.
IVOA id: ivo://cds.vizier/j/a+a/710/a280

Coma Cluster DESI galaxies

2026-06-19T11:28:13Z

Description: We investigate the kinematic properties of the Coma galaxy cluster using a new, large, spectroscopic sample of member galaxies, from the Dark Energy Spectroscopic Instrument (DESI). By means of the MG-MAMPOSST code, which is based on the Jeans equation, we jointly reconstruct the total cluster mass profile and the velocity anisotropy profile. Assuming a Navarro-Frenk-White model, we estimate a virial mass of M200c=1.04^+0.07^_-0.08_(stat)+/-0.09(syst)x10^15^M_{sun}_, corresponding to r200c=2.07+/-0.05Mpc and a scale radius for the mass profile of rs=0.73^+0.30^_-0.24_ (stat) +/- 0.21 (syst) Mpc, which provides the tightest robust kinematic mass profile constraint to date. By separately considering the mass of the hot gas and the galaxy stellar mass, we further determined the dark matter mass profile, with M200c^DM^=8.6^+1.2^_-0.8_x10^14^M_{sun}_. We discuss the impact of the mass and galaxy number density parametrisations, the effect induced by different choices of the cluster's rest frame and of the radial range of the kinematic analysis, further comparing our results with previous estimates from the literature. The cluster dynamical state was also assessed, using the spatial and line-of-sight velocity distributions of the members. We also analysed the line-of-sight velocity distributions and anisotropy profiles of different galaxy populations, selected based on their colour (red sequence, green valley, and blue cloud). The orbits of green valley and blue cloud galaxies appear to be more radial in the centre and in the outskirts, respectively, with the latter predicting a higher cluster virial mass. This study provides new insights into the interplay between dynamical and intrinsic properties of galaxies in massive structures, which is fundamental to verify the tight connection between a galaxy's evolution and its environment.
Author(s): Pedratti S.; Pizzuti L.; Fossati M.; Biviano A.; Boselli A.; Ragagnin A.,Carlin A.
IVOA id: ivo://cds.vizier/j/a+a/710/a218

JWST Bullet Cluster redshifts and spectra

2026-06-19T11:25:42Z

Description: The Bullet Cluster (1E 0657-56), located at a redshift of 0.296, is among the best-known merging galaxy clusters and a key laboratory for dark matter studies. Although the mass distribution in the Bullet Cluster has been modelled using an increasing number of multiply imaged galaxies, only six systems had spectroscopic redshifts published prior to this work, which are essential for system confirmation and as lens model constraints. We present an updated gravitational lens model of the Bullet cluster, obtained by combining JWST NIRCam imaging and NIRSpec spectroscopy. Our lens model has been constrained on the basis of a catalogue of 135 secure multiple images from 27 background galaxies with spectroscopic redshifts, uniformly covering both subclusters and a wide redshift range of 0.9-6.7. We also provide a catalogue of 199 multiple image candidates. We modelled the cluster with the parametric lens modelling code Lenstool. We incorporated several large-scale halos, cluster member galaxies, intracluster gas, and group-scale halos surrounding the cluster core, motivated by spectroscopic studies of cluster member kinematics. We describe the main cluster component with a complex, elongated double-peaked distribution, along with the subcluster, modelled using a single large-scale halo coinciding closely with the brightest cluster galaxy at a projected separation of 4_-2_^+3^kpc. The uncertainty of the displacement has been improved three-fold thanks to the addition of JWST systems. The addition of group-scale substructures, roughly following the two axes of cluster assembly, improves the fit to the multiple image positions and provides a physically motivated alternative to a constant shear component. Our lens model shows the closest agreement with previous studies in aperture mass profiles at ~60kpc from the brightest cluster galaxies (BCGs), but exhibits significant differences in the detailed mass distribution as a result of different lens-modelling strategies and adopted constraints. The differences are reflected in small, but spatially coherent deviations between the new spectroscopic redshifts and redshifts predicted by earlier lens models.
Author(s): Rihtarsic G.; Bradac M.; Desprez G.; Harshan A.; Martis N.S.; Willott C.J.,Asada Y.; Sarrouh G.T.E.; Cornil-Baiotto C.; Biviano A.; Clowe D.,Gonzalez A.H.; Jones C.; Judez J.; Kim S.Y.; Lemaux B.C.; Lombardi M.,Marchesini D.; Markevitch M.; Markov V.; Noirot G.; Peter A.H.G.,Randall S.W.; Robertson A.; Sawicki M.; Tripodi R.
IVOA id: ivo://cds.vizier/j/a+a/710/a207

VVVX & APOGEE-2. YSOs catalog in Carina Nebula

2026-06-19T08:49:32Z

Description: We present a catalog of 652 young stellar objects (YSOs) in the Carina star-forming region. The catalog was constructed by combining near-infrared KS-band variability from the VISTA Variables in the Via Lactea eXtended survey and medium-resolution H-band spectroscopy from APOGEE-2, Sloan Digital Sky Survey IV (SDSS-IV). Variability analysis of 6.35 million sources identified 606 variable stars. The classification of the spectral lines by semisupervised K-means clustering of 704 stars, refined through comparison with known catalogs in literature and visual inspection of the spectra, was performed. Combined with KS variability, the final catalog contains three groups: Emission-line YSOs, Absorption-line YSOs, and Literature/Variable-identified YSOs. Cross validation with the Gaia DR3 proper motion and distance estimates supports Carina membership for 415 sources. The statistical characterization of YSO variability demonstrated that most Carina members (78%) exhibit variability patterns. Of these, 134 stars show emissions in their spectra, which is consistent with some accretion processes. Analysis of fundamental stellar parameters from StarHorse and Gaia DR3 reveals typical distributions of YSOs, dominated by low-mass (1-4M_{sun}_), solar-metallicity stars with temperatures between 4000 and 6000K. Only a small fraction (4%) of the sources are more massive than 4M_{sun}_, suggesting limited ongoing massive star formation in Carina. This well-characterized catalog also offers a robust training data set for machine learning applications aimed at predicting YSO behavior.
Author(s): Borissova J.; Kurtev R.; Escobar J.; Alonso-Garcia J.; Medina N.,Osses J.; Guo Z.; Lucas P.W.; Kuhn M.; Minniti D.; Covey K.R.; Saito R.K.,Forster F.
IVOA id: ivo://cds.vizier/j/aj/170/135

AMS-02 Spectral Results Catalog

2026-06-19T00:00:00Z

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)

2026-06-19T00:00:00Z

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

VST ATLAS QSO survey I photometric study

2026-06-18T15:25:15Z

Description: We present the VST ATLAS Quasar Survey, consisting of ~1229000 quasar (QSO) candidates with 16 < g < 22.5 over ~4700 deg^2^. The catalogue is based on VST ATLAS+NEOWISE imaging surveys and aims to reach a QSO sky density of 130 deg^-2^ for z < 2.2 and ~30 deg-2 for z > 2.2. To guide our selection, we use X-ray/UV/optical/MIR data in the extended William Herschel Deep Field (WHDF) where we find a g < 22.5 broad-line QSO density of 269 +/- 67 deg^-2^, roughly consistent with the expected ~196 deg^-2^. We find that ~25 per cent of our QSOs are morphologically classed as optically extended. Overall, we find that in these deep data, MIR, UV, and X-ray selections are ~70-90 per cent complete while X-ray suffers less contamination than MIR and UV. MIR is however more sensitive than X-ray or UV to z > 2.2 QSOs at g < 22.5 and the S_X_(0.5-10keV) > 1*10^-14^ erg/cm^-2^/s^-1^ limit of eROSITA. We adjust the selection criteria from our previous 2QDES pilot survey and prioritize VST ATLAS candidates that show both UV and MIR excess, also selecting candidates initially classified as extended. We test our selections using data from DESI (which will be released in DR1) and 2dF to estimate the efficiency and completeness, and we use ANNz2 to determine photometric redshifts. Applying over the ~4700 deg^2^ ATLAS area gives us ~917000 z<2.2 QSO candidates of which 472 000 are likely to be z < 2.2 QSOs, implying a sky density of ~100 deg^-2^, which our WHDF analysis suggests will rise to at least 130 deg^-2^ when eROSITA X-ray candidates are included. At z > 2.2, we find ~310000 candidates, of which 169000 are likely to be QSOs for a sky density of ~36 deg^-2^.
Author(s): Eltvedt A.M.; Shanks T.; Metcalfe N.; Ansarinejad B.; Barrientos L.F.,Sharp R.; Malik U.; Murphy D.N.A.; Irwin M.; Wilson M.; Alexander D.M.,Kovacs A.; Garcia-Bellido J.; Ahlen S.; Brooks D.; De La Macorra A.,Font-Ribera A.; Gontcho A Gontcho S.; Honscheid K.; Meisner A.; Miquel R.,Nie J.; Tarle G.; Vargas-Magana M.; Zhou Z.
IVOA id: ivo://cds.vizier/j/mnras/521/3384

NS in binary systems kick velocities study

2026-06-18T15:12:34Z

Description: Understanding the natal kicks received by neutron stars (NSs) during formation is a critical component of modelling the evolution of massive binaries. Natal kicks are an integral input parameter for population synthesis codes, and have implications for the formation of double NS systems and their subsequent merger rates. However, many of the standard observational kick distributions that are used are obtained from samples created only from isolated NSs. Kick distributions derived in this way overestimate the intrinsic NS kick distribution. For NSs in binaries, we can only directly estimate the effect of the natal kick on the binary system, instead of the natal kick received by the NS itself. Here, for the first time, we present a binary kick distribution for NSs with low-mass companions. We compile a catalogue of 145 NSs in low-mass binaries with the best available constraints on proper motion, distance, and systemic radial velocity. For each binary, we use a three-dimensional approach to estimate its binary kick. We discuss the implications of these kicks on system formation, and provide a parametric model for the overall binary kick distribution, for use in future theoretical modelling work. We compare our results with other work on isolated NSs and NSs in binaries, finding that the NS kick distributions fit using only isolated pulsars underestimate the fraction of NSs that receive low kicks. We discuss the implications of our results on modelling double NS systems, and provide suggestions on how to use our results in future theoretical works.
Author(s): O'Doherty T.N.; Bahramian A.; Miller-Jones J.C.A.; Goodwin A.J.; Mandel I.,Willcox R.; Atri P.; Strader J.
IVOA id: ivo://cds.vizier/j/mnras/521/2504

Midtransit times & orbit parameters of WASP-19b

2026-06-18T11:20:38Z

Description: In this study, we present a comprehensive analysis of transit timing variations (TTVs) in the ultrashort-period gas giant WASP-19b, which orbits a G-type main-sequence star. Our analysis is based on a data set comprising 204 transit light curves (LCs) obtained from the Transiting Exoplanet Survey Satellite, the Exoplanet Transit Database, and the ExoClock project, supplemented by 18 publicly available LCs. Mid-transit times were extracted from these data, and an additional 98 mid-transit times compiled from the literature were incorporated, resulting in a combined data set spanning 14 yr. After excluding LCs significantly impacted by stellar activity, such as starspot anomalies, the final data set consisted of 252 high-quality mid-transit times. Initial inspection of the transit timing residuals using an apsidal precession model suggested the possible presence of an additional planetary companion. However, subsequent frequency analysis and sinusoidal model fitting indicate that the observed TTVs are more consistently explained by apsidal precession of WASP-19b's orbit. We also considered alternative mechanisms, including the Applegate mechanism and the Shklovskii effect. Our findings suggest that stellar magnetic activity, potentially linked to the Applegate mechanism, may also contribute to the observed timing variations. To further constrain the origin of the TTVs and assess the contributions of these mechanisms, continued high-precision photometric monitoring of the WASP-19 system is strongly recommended.
Author(s): Biswas S.; Jiang I.-G.; Yeh L.-C.; Liu H.-M.; Parthasarathy K.,Sariya D.P.; Bisht D.; Bisht M.S.; Raj A.
IVOA id: ivo://cds.vizier/j/aj/170/133

Habitable zones of exoplanet host stars

2026-06-18T07:39:17Z

Description: Stellar high-energy radiation is a key driver of atmospheric erosion and evolution in exoplanets, directly affecting their long-term habitability. We present a comprehensive study on stellar high-energy radiation and its impact on exoplanetary atmospheres, leveraging data from the eROSITA telescope array aboard the Spektrum Rotgen Gamma (SRG) satellite. Our sample consists of 3750 main-sequence stars identified by cross-matching with Gaia DR3. Utilizing X-ray spectral fit s from the eROSITA catalog, we computed X-ray (L_X_) and combined extreme-ultraviolet (EUV) luminosities (L_EUV_), derived from scaling relationships, which we us ed to derive soft X-ray flux (XUV) fluxes at the habitable zone (F_XUV,HZ_). We find that the majority of stars in our sample are significantly more XUV-active than the Sun, with habitable zone fluxes ranging from 10^0 to 10^5^erg/cm^2^/s. The ratio of L_XUV_/L_bol_ is found to be higher for cooler, magnetically active stars, highlighting their potentially hazardous nature for planetary atmospheres. Applying the energy-limited escape model, we computed atmospheric mass-loss rates for hypothetical Earth-like planets located at the habitable zone of each star. We also present local maps for distances up to 500pc of the average XUV flux, revealing "hazard zones" where stellar radiation could significantly influence planetary atmospheric evolution. This work demonstrates the power of X-ray surveys in constraining the high-energy environments of exoplanets and underscores the critical role of stellar activity in planetary habitability.
Author(s): Gatuzz E.; Rukdee S.; Freund S.; Kallman T.; Stelzer B.
IVOA id: ivo://cds.vizier/j/a+a/710/a273

PNe using Gaia DR3 and O/H gradient

2026-06-17T14:04:30Z

Description: The spatial distribution of chemical elements in the Galactic disk provides key constraints on models of galaxy evolution. However, studies using planetary nebulae (PNe) as tracers have been historically limited by large uncertainties in their distances. To overcome the long-standing distance uncertainties, we recalibrated the H{alpha} surface brightness-radius relation from Frew et al. (2013MNRAS.431....2F, Cat. J/MNRAS/431/2) with Gaia DR3 parallaxes, deriving distances for 1130 PNe of which 415 have Bayesian distances based on Gaia DR3 parallaxes. The O/H radial gradient for 231 disk PNe is fitted considering three models: a single linear gradient and segmented linear fits with one or two breaks. The segmented fits indicate a change in slope near the solar radius (R~8kpc), with a flatter or slightly positive gradient inward and a steeper negative gradient outward. This feature may reflect changes in star formation efficiency driven by the Galactic bar or the corotation resonance of the spiral arms. The breaks in the metallicity radial gradients observed in this work may result from the superposition of distinct stellar populations associated with the thin and thick disks. The two-dimensional O/H distribution in the Galactic plane supports the adopted distances and reveals modest azimuthal asymmetry, with enhanced abundances near the bar at positive longitudes, and a bimodal abundance structure between the inner and outer solar regions. Our results provide new constraints on the chemical evolution of the Milky Way, the impact of non-axisymmetric structures, and the possible existence of distinct radial abundance regimes across the Galactic disk.
Author(s): Cavichia O.; Monteiro H.; Cervino M.; da Cunha-Silva A.R.; Maciel W.J.,Cardoso A.F.S.
IVOA id: ivo://cds.vizier/j/apj/1004/220

JCMT fluxes & transient statistics of M17 submm YSOs

2026-06-17T12:33:02Z

Description: We conducted a comprehensive analysis of young stellar object (YSO) variability at submillimeter and mid-infrared (mid-IR) wavelengths for the M17 H_II_ region using 3.5yr monitoring data from the James Clerk Maxwell Telescope (JCMT) Transient Survey at 450 and 850um and 9yr mid-IR monitoring data from the NEOWISE mission. Our study encompasses observations of 198 and 164 bright submillimeter peaks identified within the deep JCMT coadded maps at 450 and 850um, and 66 YSOs seen by NEOWISE W2 that were previously identified in mid-IR observations. We find one robust linear submillimeter variable, an intermediate mass protostar, with a 4% peak flux change in 3.5yr of JCMT monitoring that sets a lower limit of 16% luminosity increase for the source. At mid-IR wavelengths, our analysis reveals secular and stochastic variability in 22 YSOs, with the highest fraction of secular variability occurring at the earliest evolutionary stage. This mid-IR fractional variability as a function of evolutionary stage result is similar to what has previously been found for YSO variability within the Gould Belt and the intermediate-mass star formation region M17 SWex, though overall less variability is detected in M17 in submillimeter and mid-IR. We suspect that this lower detection of YSO variability is due to both the greater distance to M17 and the strong feedback from the H ii region. Our findings showcase the utility of multiwavelength observations to better capture the complex variability phenomena inherent to star formation processes and demonstrate the importance of years-long monitoring of a diverse selection of star-forming environments.
Author(s): Chen Z.; Johnstone D.; Contreras Pena C.; Lee J.-E.; Liu S.-Y.,Herczeg G.; Mairs S.; Park G.; Kim K.-T.; Kim M.-R.; Qiu K.; Wang Y.-T.,Zhang Xu; Reiter M.; The JCMT Transient Team
IVOA id: ivo://cds.vizier/j/aj/170/125

APO ACCELS. Ages, Li EW, & Prot for 166 accel. stars

2026-06-17T08:36:59Z

Description: Directly imaged substellar companions with well-constrained ages and masses serve as vital empirical benchmarks for planet formation and evolution models. Potential benchmark companions can be identified from astrometric accelerations of their host stars. We use Gaia DR3 and Hipparcos astrometry to identify 166 northern hemisphere stars with astrometric accelerations consistent with a substellar companion between 0.5" and 1". For this accelerating sample we identify young stars using Apache Point Observatory/ARCES spectra and TESS light curves. From spectroscopic screening of the sample, we measure ages for 24 stars with detectable amounts of lithium, place lower age limits on 135 stars with lithium nondetections, and measure ages from R'_HK_ for 34 stars. A total of 129 stars have TESS light curves, from which we measure ages for 20 stars with rotation rates <15days, and we identify three eclipsing binaries. We present median ages and confidence intervals of age posteriors for the entire sample and discuss how the overall age distribution of our sample compares to a uniform star formation rate in the solar neighborhood. We identify 47 stars with median ages <2Gyr, 31 stars with median ages <1Gyr, and 14 stars with median ages <0.5Gyr, making them high-priority targets for direct imaging follow-up.
Author(s): Peck A.E.; Nielsen E.L.; De Rosa R.J.; Thompson W.; Macintosh B.,Roberson W.; Smith A.J.R.W.; Klusmeyer J.; Abbas A.; Jackiewicz J.,Holtzman J.; Gallamore H.; Brinjikji M.; Patience J.; Nguyen J.S.,Madurowicz A.; Savransky D.
IVOA id: ivo://cds.vizier/j/aj/170/122

Fornax dwarfs galaxies properties from scaling

2026-06-17T08:35:41Z

Description: Dwarf galaxies are excellent cosmological probes, because their shallow potential wells make them very sensitive to the key processes that drive galaxy evolution, including baryonic feedback, tidal interactions, and ram pressure stripping. However, some of the key parameters of dwarf galaxies, which help trace the effects of these processes, are still debated, including the relationship between their sizes and masses. We re-examine the Fornax Cluster dwarf population from the point of view of isomass-radius-stellar mass relations (IRSMRs) using the Fornax Deep Survey Dwarf galaxy Catalogue, with the centrally located (among dwarfs) 3.63M_{sun}_/pc^2^ isodensity radius defining our fiducial relation. This relation is a powerful diagnostic tool for identifying dwarfs with unusual structure, as dwarf galaxies' remarkable monotonicity in light profile shapes, as a function of stellar mass, reduces the relation's scatter tremendously. By examining how different dwarf properties (colour, 10th nearest neighbour distance, etc.) correlate with distance from our fiducial relation, we find a significant population of structural outliers with comparatively lower central mass surface density and larger half-light-radii, residing in locally denser regions in the cluster, albeit with similar red colours. We propose that these faint, extended outliers likely formed through tidal disturbances, which make the dwarfs more diffuse, but with little mass-loss. Comparing these outliers with ultra-diffuse galaxies (UDGs), we find that the term UDG lacks discriminatory power; UDGs in the Fornax Cluster lie both on and off of IRSMRs defined at small radii, while IRSMR outliers with masses below ~10^7.5^M_{sun}_ are excluded from the UDG classification due to their small effective radii.
Author(s): Watkins A.E.; Salo H.; Kaviraj S.; Collins C.A.; Knapen J.H.; Venhola A.,Roman J.
IVOA id: ivo://cds.vizier/j/mnras/521/2012

Starless and pre-stellar cores sulfur depletion

2026-06-17T08:29:00Z

Description: Sulfur is one of the most abundant elements in the Universe, yet the sulfur budget inferred from the observed sulfur-bearing molecules in dense cores is significantly lower than expected. Starless and pre-stellar cores represent the earliest stages of star formation, thus providing an ideal laboratory to study the physical and chemical processes that cause sulfur depletion. We aim to constrain the sulfur chemistry in dense cores by measuring the abundances of different sulfur-bearing molecules and examining how these abundances reflect core evolution and environmental effects. We observed nine cores in the Taurus Molecular Cloud, targeting 13 sulfur-bearing molecules, including CS, CCS, C_3_S, OCS, SO, SO_2_, H_2_CS, and various isotopologs. The molecular abundances and six abundance ratios were then compared to three evolutionary tracers: H_2_ column density, N_2_D+/N_2_H+, and the CO depletion factor. We also compared the observed abundances with 0D chemical models with different initial sulfur abundances. We observe substantial variations in the abundances of individual sulfur-bearing molecules across the cores. L1517B exhibits consistently low abundances and a high depletion factor, whereas L1495B shows high abundances in oxygen-bearing species compared to the other cores within the L1495 filament. Ratios that probe the balance between carbon- and oxygen-bearing sulfur species (CCS/^34^SO and C^34^S/^34^SO) decrease with increasing H_2_ column density and N_2_D+/N_2_H+ ratio. In contrast, individual molecules and other ratios show weak or no correlation with the evolutionary tracers. The 0D chemical models reproduce the abundances of some molecules, such as OCS, H_2_CS, and HDCS, reasonably well but cannot simultaneously account for all observed species. This difference is most evident between the carbon- and oxygen-bearing molecules. The observed variations in sulfur abundances between the different cores and the lack of clear correlations with three standard evolutionary tracers indicate that a single evolutionary parameter cannot describe the sulfur chemistry. Instead, it is strongly influenced by local environmental factors. Reproducing the full sample of sulfur-bearing molecules would require improved chemical networks and models that account for the core's physical structure.
Author(s): Schoeller L.; Spezzano S.; Sipilae O.; Makarenko E.I.; Caselli P.,Bunn H.A.; Jensen S.S.
IVOA id: ivo://cds.vizier/j/a+a/710/a251

Super-Nyquist freq. in Kepler delta Scuti stars

2026-06-17T08:26:19Z

Description: Pressure-mode frequencies in {delta} Scuti stars may exceed the Nyquist limit of Kepler long-cadence photometry and appear as reflected Nyquist aliases at lower frequencies. We performed a systematic survey of 1838 Kepler {delta} Scuti stars using a sliding Lomb-Scargle periodogram analysis, and identified 15265 confirmed super-Nyquist frequencies in 1309 stars among 259883 extracted frequencies. The catalog gives the identified super-Nyquist frequencies, their inferred real frequencies above the Nyquist limit, and the diagnostic quantities used for their classification. The full set of extracted frequencies is provided as reference material for future asteroseismic studies.
Author(s): Mo Y.; Zong W.; Wang X.; Murphy S.; Yang Z.; Fu J.-N.; Charpinet S.,Ma X.-Y.
IVOA id: ivo://cds.vizier/j/a+a/710/a245

Symbiotic star candidates in inner Galactic disk

2026-06-17T08:23:44Z

Description: The origin of the highly ionized iron emission (FeXXV at 6.7keV) characterizing the Galactic ridge X-ray emission (GRXE) remains a fundamental puzzle in high-energy astrophysics. Although the GRXE continuum is largely resolved into discrete populations of cataclysmic variables and coronally active stars, these sources exhibit Fe XXV equivalent widths significantly lower than that of the total GRXE, leaving the intense iron line emission unexplained. In this work, we cross-correlated the XMM-Newton survey of the inner Galactic disk with Gaia DR3 astrometry to identify and characterize hard X-ray sources (>2keV) with reliable stellar counterparts. We selected 107 X-ray sources located within the red giant branch of the color-magnitude diagram, many of which are verified long-period variables. These sources exhibit high X-ray luminosities (Lx~10^31^-10^33^erg/s), significantly exceeding the typical coronal saturation levels of single giants. Their X-ray spectra are notably harder than those of quiescent stellar coronae, with plasma temperatures reaching up to kT ~6keV and a prominent emission feature at ~6.7keV. The combination of high Lx, hard spectra, and intense FeXXV emission identifies this population as accretion-powered binaries associated with late-type giants. Our analysis demonstrates that this population contributes ~20% of the total GRXE continuum and ~40% of its iron line emission, providing a key component to resolving the Galactic X-ray background puzzle.
Author(s): Bao T.; Ponti G.; Xu X.-J.; Morris M.R.; Levin B.; Mori K.; Mandel S.,Locatelli N.; Munoz-Darias T.; Casares J.; Torres M.A.P.
IVOA id: ivo://cds.vizier/j/a+a/710/a243

Galaxy Zoo barred galaxies properties with MaNGA

2026-06-17T08:22:10Z

Description: We study the bar pattern speeds and corotation radii of 225 barred galaxies, using integral field unit data from MaNGA and the Tremaine-Weinberg method. Our sample, which is divided between strongly and weakly barred galaxies identified via Galaxy Zoo, is the largest that this method has been applied to. We find lower pattern speeds for strongly barred galaxies than for weakly barred galaxies. As simulations show that the pattern speed decreases as the bar exchanges angular momentum with its host, these results suggest that strong bars are more evolved than weak bars. Interestingly, the corotation radius is not different between weakly and strongly barred galaxies, despite being proportional to bar length. We also find that the corotation radius is significantly different between quenching and star-forming galaxies. Additionally, we find that strongly barred galaxies have significantly lower values for R, the ratio between the corotation radius and the bar radius, than weakly barred galaxies, despite a big overlap in both distributions. This ratio classifies bars into ultrafast bars (R< 1.0; 11 per cent of our sample), fast bars (1.0 <R< 1.4; 27 per cent), and slow bars (R> 1.4; 62 per cent). Simulations show that R is correlated with the bar formation mechanism, so our results suggest that strong bars are more likely to be formed by different mechanisms than weak bars. Finally, we find a lower fraction of ultrafast bars than most other studies, which decreases the recently claimed tension with Lambda cold dark matter. However, the median value of R is still lower than what is predicted by simulations.
Author(s): Geron T.; Smethurst R.J.; Lintott C.; Kruk S.; Masters K.L.; Simmons B.,Mantha K.B.; Walmsley M.; Garma-Oehmichen L.; Drory N.; Lane R.R.
IVOA id: ivo://cds.vizier/j/mnras/521/1775

Photometric filter characteristics derived from the SVO Filter Profile Service "Carlos Rodrigo"

2026-06-16T14:59:57Z

Description

This table provides photometric filter characteristics derived from the SVO Filter Profile Service "Carlos Rodrigo" https://svo2.cab.inta-csic.es/svo/theory/fps/.
Each row corresponds to a single photometric filter and contains basic bandpass information.

Exposing these data through TAP enables ADQL queries joining filter data with photometric datasets. 

The table contains a selected subset of filters used in the published light-curve collections. 
The full transmission curves can be retrieved from the FPS using the fps_url column.

These data are republished with permission from the SVO SVO Filter Profile Service "Carlos Rodrigo".
If this table contributes to your research, please acknowledge the original service and cite the following references:

* Rodrigo, C., Cruz, P., Aguilar, J.F., et al. 2024, :bibcode:`2024A&A...689A..93R`; 
* The SVO Filter Profile Service. Rodrigo, C., Solano, E., Bayo, A., 2012, :bibcode:`2012ivoa.rept.1015R`;
* The SVO Filter Profile Service. Rodrigo, C., Solano, E., 2020, :bibcode:`2020sea..confE.182R`.

The SVO Filter Profile Service is funded by MCIN/AEI/10.13039/501100011033/ through grant PID2023-146210NB-I00.

Author(s)

Rodrigo, C.; Solano, E.

IVOA id

ivo://astro.upjs/filters/q/main

Filter Profiles

2026-06-16T14:59:57Z

Description

This table provides photometric filter characteristics derived from the SVO Filter Profile Service "Carlos Rodrigo" https://svo2.cab.inta-csic.es/svo/theory/fps/.
Each row corresponds to a single photometric filter and contains basic bandpass information.

Exposing these data through TAP enables ADQL queries joining filter data with photometric datasets. 

The table contains a selected subset of filters used in the published light-curve collections. 
The full transmission curves can be retrieved from the FPS using the fps_url column.

These data are republished with permission from the SVO SVO Filter Profile Service "Carlos Rodrigo".
If this table contributes to your research, please acknowledge the original service and cite the following references:

* Rodrigo, C., Cruz, P., Aguilar, J.F., et al. 2024, :bibcode:`2024A&A...689A..93R`; 
* The SVO Filter Profile Service. Rodrigo, C., Solano, E., Bayo, A., 2012, :bibcode:`2012ivoa.rept.1015R`;
* The SVO Filter Profile Service. Rodrigo, C., Solano, E., 2020, :bibcode:`2020sea..confE.182R`.

The SVO Filter Profile Service is funded by MCIN/AEI/10.13039/501100011033/ through grant PID2023-146210NB-I00.

Author(s)

Rodrigo, C.; Solano, E.

IVOA id

ivo://astro.upjs/filters/q/q

EGPM. III. HPF RVs & activity of young giant planets

2026-06-16T08:32:27Z

Description: We present statistical results from the Epoch of Giant Planet Migration RV planet search program. This survey was designed to measure the occurrence rate of giant planets interior to the water ice line of young Sun-like stars, compare this to the prevalence of giant planets at older ages, and provide constraints on the timescale and dominant inward migration mechanism of giant planets. Our final sample amounts to 85 single young (20-200Myr) G and K dwarfs that we target across a 4yr time baseline with the near-infrared Habitable-zone Planet Finder spectrograph at McDonald Observatory's Hobby- Eberly Telescope. As part of this survey, we discovered the young hot Jupiter HS Psc b. We characterize survey detection completeness with realistic injection-recovery tests and measure an occurrence rate of 1.9_-1.4_^+2.6^% for intermediate-age giant planets (0.3M_J_<Msin(i)<13M_J_) within 2.5AU. This is lower than the field age occurrence rate for the same planet masses and separations and favors an increase in the prevalence of giant planets over time from ~100Myr to several Gyr, although our results cannot rule out a constant rate. A decaying planet occurrence rate is, however, strongly excluded. This suggests that giant planets located inside the water ice line originate from a combination of in situ formation or early migration coupled with longer-term inward scattering. The completeness-corrected prevalence of young hot Jupiters in our sample is 1.5_-1.1_^+2.2^% -similar to the rate for field stars-and the 95% upper limit for young brown dwarfs within 5000 days is <3.6% .
Author(s): Tran Q.H.; Bowler B.P.; Cochran W.D.; Bender C.F.; Halverson S.,Mahadevan S.; Ninan J.P.; Robertson P.; Roy A.; Stefansson G.,Terrien R.C.
IVOA id: ivo://cds.vizier/j/aj/170/103

NGC 346 VIHa photometry

2026-06-16T06:43:44Z

Description: We studied the properties of star formation and the characteristics of young stars in a quiet region located beyond the outskirts of the prominent star-forming cluster NGC 346 in the Small Magellanic Cloud (SMC). Utilising observations from the Hubble Space Telescope across the broad V and I bands, as well as the narrow Halpha band, we identified populations with ages of roughly 10, 60, 400Myr and of 5Gyr through isochrone comparison. We successfully identified 137 bona fide pre-main sequence (PMS) candidates exhibiting Halpha excess with a significance level of 5 sigma, accompanied by a Halpha line emission equivalent width exceeding 20{AA}. Physical parameters for these PMS stars were determined, including mass, age, accretion luminosity, and mass accretion rate. Most PMS stars have an age around 16 Myr and an average mass of 0.80+/-0.16M_{sun{_. The median mass accretion rate for all 137 PMS stars is estimated to be about 8.0x10^-9^M_{sun}_/yr. While this rate is lower than that observed in the NGC 346 cluster itself, it is comparable with those measured for PMS stars in low-density star-forming regions in the SMC, despite the absence of apparent clustering and nebulosity. Furthermore, our analysis reveals that the ratios of accreting and non-accreting PMS stars to non-PMS stars and their mass accretion rate correlate with their distance from a group of hot massive stars in the vicinity. This suggests that the ultraviolet radiation emitted by these massive stars might erode the circumstellar discs of nearby PMS stars. Lastly, the overlap between our studied region and observations from the James Webb Space Telescope reveals that some of the identified PMS stars display near-infrared excess.
Author(s): Dik C.; De Marchi G.
IVOA id: ivo://cds.vizier/j/a+a/710/a246

CAMIRA clusters in the eFEDS field

2026-06-16T06:42:38Z

Description: This is the second paper in a series exploring the X-ray properties of galaxy clusters optically selected by the Subaru Hyper Suprime-Cam (HSC) survey, using data from the SRG/eROSITA Final Equatorial-Depth Survey (eFEDS). We aim to investigate scaling relations between observable cluster properties and mass, and to study the radial X-ray profiles of a large sample of optically selected clusters. We analyze a sample of 997 CAMIRA clusters with richness N>15 and redshifts of 0.1<z<1.3. Using bolometric luminosities derived from count rates and a weak-lensing mass calibration, we study the L-M and N-M scaling relations through stacking analysis, while accounting for selection effects and redshift evolution. We also compare clusters with and without X-ray counterparts in the eFEDS catalog in terms of their scaling relations and surface brightness profiles. The best-fit L-M slope (1.56^+0.14^_-0.12_) is slightly steeper than the self-similar prediction, yet remains consistent with our previous findings. The N-M slope (0.766^+0.070^_-0.060_) broadly agrees with theoretical expectations and other optical samples. The data do not require any additional redshift evolution beyond the standard self-similar scaling, although current constraints on evolution remain weak. X-ray detected clusters exhibit a marginally steeper L-M slope, higher central surface brightness, and more centrally concentrated X-ray profiles than undetected systems. Our results highlight systematic differences in the X-ray properties between optically and X-ray selected cluster samples. This study extends scaling relation analyses into lower mass and luminosity regimes, demonstrating the value of combining deep X-ray and optical surveys like eROSITA and Subaru HSC.
Author(s): Nguyen-Dang N.T.; Ota N.; Okabe N.; Oguri M.; Mitsuishi I.; Reiprich T.H.,Pacaud F.; Bulbul E.; Sanders J.S.; Brueggen M.; Liu A.; Tsujita Y.,Chiu I.; Ghirardini V.; Grandis S.; Klein M.; Migkas K.; Miyatake H.,Miyazaki S.; Ramos-Ceja M.E.
IVOA id: ivo://cds.vizier/j/a+a/710/a202

Reconstruction of annual solar irradiance

2026-06-16T06:41:06Z

Description: Solar irradiance measurements are limited, spanning only the last few decades, requiring reconstructions to assess solar variability on longer timescales and its impact on Earth's climate. We present the first physics-based reconstruction of total solar irradiance (TSI) at annual resolution over the last three millennia. The reconstruction is obtained by extending the SATIRE-T model beyond the telescopic era using recently published, annually resolved sunspot number series derived from cosmogenic isotope records. This yields a continuous, physics-based TSI record extending from the satellite era back over the last three millennia, with an annual resolution throughout the pre-telescopic period. Over this full interval, the reconstructed TSI exhibits a maximum difference of 1.04_-0.2_^+0.14^ W/m^2^, defined as the difference between the maximum and minimum of the 50-year running mean values.
Author(s): Temaj D.; Krivova N.A.; Solanki S.K.; Usoskin I.G.; Chatzistergos T.
IVOA id: ivo://cds.vizier/j/a+a/710/l24

The X-ray ExSeSS source sample from 2SXPS

2026-06-15T07:07:38Z

Description: We present the Extragalactic Serendipitous Swift Survey (ExSeSS), providing a new well-defined sample constructed from the observations performed using the Swift X-ray Telescope. The ExSeSS sample consists of 79342 sources detected in the medium (1-2 keV), hard (2-10 keV), or total (0.3-10 keV) energy bands, covering 2086.6 deg^2^ of sky across a flux range of f_0.3-10 keV_ ~ 10^-15^ - 10^-10^ erg/s/cm^2^. Using the new ExSeSS sample we present measurements of the differential number counts of X-ray sources as a function of 2-10 keV flux that trace the population of Active Galactic Nuclei (AGNs) in a previously unexplored regime. We find that taking the line-of-sight absorption column density into account has an effect on the differential number count measurements and is vital to obtain agreement with previous results. In the hard band, we obtain a good agreement between the ExSeSS measurements and previous, higher energy data from NuSTAR and Swift/BAT when taking into account the varying column density of the ExSeSS sample as well as the X-ray spectral parameters of each of the samples we are comparing to. We also find discrepancies between the ExSeSS measurements and AGN population synthesis models, indicating a change in the properties of the AGN population over this flux range that is not fully described by current models at these energies, hinting at a larger, moderately obscured population at low redshifts (z <~ 0.2) that the models are not currently taking into account.
Author(s): Delaney J.N.; Aird J.; Evans P.A.; Barlow-Hall C.; Osborne J.P.,Watson M.G.
IVOA id: ivo://cds.vizier/j/mnras/521/1620

Bar strengths of galaxies

2026-06-15T07:06:51Z

Description: The 'Triangal' galaxy evolution schema is used to assess whether the Tuning Fork (bar strength) or the van den Bergh Trident and ATLAS Comb (spiral strength) offer greater evolutionary insight. A new catalogue of quantitative bar strengths (measured by the bar-to-total luminosity ratio, P), refined galaxy morphologies, and dust bin classifications is presented. It contains 137 galaxies with spheroid stellar masses, obtained from multicomponent decompositions, and directly measured black hole masses, M_bb_. By placing these galaxies within the M_bb_-(M_*,sph_, M_*,gal_) parameter space, an evolutionary reference frame reflecting integrated growth is established. Galaxies with varying bar strengths, and double bars, are observed to not occupy preferred locations, highlighting that bars are products of secular evolution - and can be transient or recurrent phenomena - and that they track neither hierarchical mass assembly nor galaxy speciation. In contrast, three physically distinct formation channels for S0/a galaxies are identified: (primeval S0)-to-S transitions; faded spiral galaxies; and, most commonly, wet-major-merger-built dust-rich S0 galaxies (on the 'green mountain'). Galaxies with particularly strong spirals appear on the right-hand side of the spiral galaxy distribution. Furthermore, a 'Dust Attrition/Retention' sequence places S0 (and compact massive ES,b) galaxies with dusty nuclear discs between the dust-poor and dust-rich S0 galaxies, and a 'Disc Down-sizing' sequence is revealed, in which E galaxies with dusty nuclear discs - potentially formed through 'damp' mergers - bridge the ES,e (ellicular) galaxies with intermediate-scale stellar discs and the dust-poor pure E galaxies. Extensive historical context is provided, and, finally, suspected biases in precision cosmology stemming from neglected precision galaxy morphology are discussed.
Author(s): Graham A.W.
IVOA id: ivo://cds.vizier/j/mnras/549/g782