VO Fresh

ATCA obs. of eROSITA tidal disruption events

2026-05-13T08:56:20Z

Description: We present a systematic analysis of the radio properties of an X-ray-selected sample of tidal disruption event (TDE) candidates discovered by the eROSITA telescope. We find radio sources coincident with half of the transient events (11 TDEs), with eight radio sources showing statistically significant variability over a 6 month period. We model the radio spectra of six sources with sufficiently bright radio emission and find the sources show radio spectra consistent with optically thin synchrotron emission and radio outflow minimum radii of 10^16^-10^17^cm, velocities 0.01c-0.05c, and energies 10^48^-10^51^erg. On comparison with the radio properties of an optically selected TDE sample at similar late times, we find no significant difference in the radio luminosity range or radio detection rate. We find a tentative positive trend with peak radio and X-ray luminosity, but require further observations to determine if this is real or due to observational bias due to the large range in distances of the events. Interestingly, none of the X-ray-selected events show late-rising radio emission, compared to 45% of radio-detected sources of an optically selected sample that showed late-rising radio emission. We propose that this may indicate that many TDEs launch radio outflows at or near peak X-ray luminosity, which can be significantly delayed from peak optical luminosity. This study presents the first systematic analysis of the radio properties of an X-ray-selected sample of TDEs, and gives insight into the possible link between the physical processes that power X-ray and radio emission in TDEs.
Author(s): Goodwin A.J.; Burn M.; Anderson G.E.; Miller-Jones J.C.A.; Grotova I.,Baldini P.; Liu Z.; Malyali A.; Rau A.; Salvato M.
IVOA id: ivo://cds.vizier/j/apjs/278/36

Deep UNCOVER-ALMA Legacy high-Z survey (DUALZ)

2026-05-13T08:47:11Z

Description: We present the survey design and initial results of the Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 9 program of DUALZ, which aims to establish a joint ALMA and JWST public legacy field targeting the massive galaxy cluster A2744. DUALZ features a contiguous 4'x6' ALMA 30GHz-wide mosaic in Band 6, covering areas of {mu}>2 down to a sensitivity of {sigma}=32.7{mu}Jy. Through a blind search, we identified 69 dust continuum sources at a signal-to-noise ratio (SNR) >~5.0 with median redshift and intrinsic 1.2mm flux of z=2.30 and S_1.2mm_^int^=0.24mJy. Of these, 27 have been spectroscopically confirmed, leveraged by the latest NIRSpec observations, while photometric redshifts are also constrained by the comprehensive Hubble Space Telescope (HST), NIRCam, and ALMA data sets for the remaining sources. With priors, we further identify a [CII]158{mu}m line emitter at z=6.3254+/-0.0004, confirmed by the latest NIRSpec spectroscopy. The NIRCam counterparts of the 1.2mm continuum exhibit undisturbed morphologies, denoted either by disk or spheroid, implying the triggers for the faint millimeter emission are less catastrophic than mergers. We have identified eight HST-dark galaxies (F150W>27mag, F150W-F444W>2.3) and two JWST-dark (F444W>30mag) galaxy candidates among the ALMA continuum sources. The former includes face-on disk galaxies, hinting that substantial dust obscuration does not always result from inclination. We also detect a marginal dust emission from an X-ray-detected galaxy at zspec=10.07, suggesting an active coevolution of the central black hole and its host. We assess the infrared luminosity function up to z~10 and find it is consistent with predictions from galaxy formation models.
Author(s): Fujimoto S.; Bezanson R.; Labbe I.; Brammer G.; Price S.H.; Wang B.,Weaver J.R.; Fudamoto Y.; Oesch P.A.; Williams C.C.; Dayal P.,Feldmann R.; Greene J.E.; Leja J.; Whitaker K.E.; Zitrin A.; Cutler S.E.,Furtak L.J.; Pan R.; Chemerynska I.; Kokorev V.; Miller T.B.; Atek H.,van Dokkum P.; Juneau S.; Kassin S.; Khullar G.; Marchesini D.; Maseda M.,Nelson E.J.; Setton D.J.; Smit R.
IVOA id: ivo://cds.vizier/j/apjs/278/45

Planet masses, radii, and orbits from K2 mission

2026-05-13T07:19:15Z

Description: We report the masses, sizes, and orbital properties of 86 planets orbiting 55 stars observed by NASA's K2 Mission with follow-up Doppler measurements by the HIRES spectrometer at the W. M. Keck Observatory and the Automated Planet Finder at Lick Observatory. Eighty-one of the planets were discovered from their transits in the K2 photometry, while five were found based on subsequent Doppler measurements of transiting planet-host stars. The sizes of the transiting planets range from Earth-size to larger than Jupiter (1-3R_{Earth}_ is typical), while the orbital periods range from less than a day to a few months. For 32 of the planets, the Doppler signal was detected with significance greater than 5{sigma} (51 were detected with >3{sigma} significance). An important characteristic of this catalog is the use of uniform analysis procedures to determine stellar and planetary properties. This includes the transit search and fitting procedures applied to the K2 photometry, the Doppler fitting techniques applied to the radial velocities (RVs), and the spectral modeling to determine bulk stellar parameters. Such a uniform treatment will make the catalog useful for statistical studies of the masses, densities, and system architectures of exoplanetary systems. This work also serves as a data release for all previously unpublished RVs and associated stellar activity indicators obtained by our team for these systems, along with derived stellar and planet parameters.
Author(s): Howard A.W.; Sinukoff E.; Blunt S.; Petigura E.A.; Crossfield I.J.M.,Isaacson H.; Kosiarek M.; Rubenzahl R.A.; Brewer J.M.; Fulton B.J.,Dressing C.D.; Hirsch L.A.; Knutson H.; Livingston J.H.; Mills S.M.,Roy A.; Weiss L.M.; Benneke B.; Ciardi D.R.; Christiansen J.L.,Cochran W.D.; Crepp J.R.; Gonzales E.; Hansen B.M.S.; Hardegree-Ullman K.,Howell S.B.; Lepine S.; Martinez A.O.; Rogers L.A.; Schlieder J.E.,Werner M.; Polanski A.S.; Angelo I.; Beard C.; Behmard A.; Bouma L.G.,Brinkman C.L.; Chontos A.; Dai F.; Dalba P.A.; Giacalone S.,Grunblatt S.K.; Hill M.L.; Kane S.R.; Lubin J.; Mayo A.W.; Mocnik T.,Murphy J.M.A.; Rice M.; Rosenthal L.J.; Tyler D.; Van Zandt J.; Yee S.W.
IVOA id: ivo://cds.vizier/j/apjs/278/52

Reconstruction of Cepheid radial velocity curves

2026-05-13T06:59:48Z

Description: Radial velocity (RV) curves of Cepheids are essential for studying their pulsation properties and also for measuring their distance via the parallax-of-pulsation method. Although precise RV curves are available for hundreds of Cepheids, it is still not possible to predict the complete RV curve from other observables such as their pulsation period or metallicity. This paper aims to develop the first method of reconstructing the shape of the RV curves of short-period fundamental-mode Cepheids, based exclusively on their pulsation period and the morphology of their V-band light curves (LCs). We compiled a dataset of high-quality spectroscopic and photometric measurements from the literature for 81 short-period fundamental-mode Galactic Cepheids up to a pulsation period of 8 days, enabling the precise determination of the Fourier parameters and their uncertainties. By performing a detailed comparative analysis of their shapes, we investigated correlations between LC and RV Fourier parameters and used these relations to reconstruct the RV curves. We further assessed the accuracy of these reconstructions by examining potential metallicity effects with an additional dataset of 24 metal-poor Cepheids. For pulsation periods between 3.5 and 7.0 days, we found tight correlations between different combinations of LC and RV Fourier parameters up to order 7. In particular, we discovered that the ratios R_21_(RV)/R_21_(LC) and R_31_(RV)/R_31_(LC) are tightly correlated with the pulsation period. These relationships enable the reconstruction of RV curves of Cepheids with their LC. The reconstructed curve has an uncertainty of about 0.60km/s relative to the Fourier fit of true spectroscopic RV measurements. For individual Cepheids, the reconstructed RV curves integrated along the pulsation cycle (i.e. the linear radius variations) are accurate to less than 1% and precise to within 4.16% in comparison to the integrated true spectroscopic RV curves. Last, our sample of metal-poor Cepheids shows a good agreement with the empirical relations calibrated on Galactic pulsators, indicating that the method of reconstruction is weakly dependent on metallicity. For the first time, we present a method of reconstructing the shape of the RV curves of Cepheids using solely the V-band LC and the pulsation period. This approach provides a valuable tool for the reconstruction of RV curves for extragalactic Cepheids through photometric data alone. It opens the road to a purely photometric parallax-of-pulsation method in the context of photometric surveys, such as the Vera Rubin Telescope. Further calibration in different photometric bands and for a larger metallicity baseline will be useful to improve the method.
Author(s): Hocde V.; Moskalik P.; Nardetto N.; Kervella P.; Pilecki B.; Smolec R.,PietrzyNski G.; Gieren W.; Hajdu G.; Gallenne A.; Bailleul M.C.; Bras G.,Wielgorski P.; Breuval L.; Merand A.; Rathour R.S.; Espinoza-Arancibia F.,Kiviaho W.; Apostolova B.; Sivkova K.
IVOA id: ivo://cds.vizier/j/a+a/709/a151

Limb-brightened jet in 3C 84 images

2026-05-13T06:57:22Z

Description: Relativistic jets launched by active galactic nuclei are fundamental for understanding the physics of accreting supermassive black holes and their immediate environment, but the mechanisms that drive the jet launching remain uncertain. We investigate the sub-parsec jet of 3C 84 using multi-epoch multi-frequency very long baseline interferometry (VLBI) observations with the European VLBI Network and the Very Long Baseline Array at 22 and 43GHz. We analysed the evolution of the spectral index gradient in the core region to relate the observed structure to physical interpretations and to distinguish between competing jet-launching models. Furthermore, we examined the effect of the ambient medium and magnetic field configuration on the jet morphology and dynamics over time and explored their connection to a coinciding gamma-ray flare. Our spectral analysis reveals significant changes across three epochs, indicating dynamic activity between filamentary structures on sub-parsec scales, evolving magnetic fields, and a complex interaction with the surrounding medium, all of which shape the innermost jet and might affect its high-energy emission.
Author(s): Debbrecht L.C.; Paraschos G.F.; Ros E.; Krichbaum T.P.; Bach U.,Gurwell M.A.; Hodgson J.A.; Janssen M.; Kim J.-Y.; Lisakov M.M.,MacDonald N.R.; Nair D.G.; Oh J.; Zensus J.A.
IVOA id: ivo://cds.vizier/j/a+a/709/a192

Velocity dispersion evolution in Sco-Cen OB

2026-05-13T06:56:28Z

Description: We study how the stellar velocity dispersion within the Scorpius-Centaurus OB association (Sco-Cen) has evolved over approximately 20 million years, from its formation to the present day, by investigating 32 stellar clusters in Sco-Cen. Using data from the Gaia mission along with supplementary stellar radial velocities, we identified a surprising sequence of abrupt jumps and intervening plateaus in the evolution of velocity dispersion correlating with times of star formation bursts. We find that the association is almost isotropically expanding and that star formation propagated from inside-out with a speed of about 5-6km/s. We measure a present-day expansion rate of about 10-12pc/Myr and observe that younger star clusters within the association exhibit higher velocities compared to older ones. This result, along with the stepwise increase in velocity dispersion over time, suggests a structured and sequential star formation process rather than a random one. This phased evolution suggests that stellar feedback is the primary driver of Sco-Cen's star formation history, expansion, and eventual dispersal. Our findings emphasise the value of precisely characterising stellar populations within OB associations, particularly through the creation of detailed, high-resolution age maps.
Author(s): Grossschedl J.E.; Alves J.; Ratzenbock S.; Miret-Roig N.; Hutschenreuter S.,Posch L.; Hacar A.
IVOA id: ivo://cds.vizier/j/a+a/709/a181

PSR J1023+0038 Nov 14-15 2017 photon lists

2026-05-13T06:54:52Z

Description: Neutron stars in close binary systems have the potential to spin up to millisecond periods due to the accretion of matter and angular momentum from their low-mass companions. In later stages of this process, they sometimes start to swing between the accretion-powered and rotation-powered regimes, manifesting themselves as low-mass X-ray binaries and millisecond radio pulsars, respectively. Such systems are known as transitional millisecond pulsars. PSR J1023+0038 was the first one of this kind to be discovered and the first to show optical pulsations at the rotation frequency of the neutron star during a peculiar low accretion state. The optical pulse profile is characterized by a smooth double-peaked shape resembling thermal light curves of X-ray pulsars, but more likely emerging from re-emission of the pulsar wind energy by charged particles in the surrounding medium. Although the amplitudes of the peaks show strong variability, the overall structure of the pulse profile was observed to be fixed, with the optical pulsed fraction <~1 percent. Here, we report time-resolved observation of a dramatic violation of this permanence during our high temporal resolution observations of PSR J1023+0038 with the 6-m BTA telescope of the Special Astrophysical Observatory. On a timescale of a few seconds the pulse profile took a single-peaked, nearly sinusoidal shape, with synchronous magnification of the pulsed fraction up to ~5 percent. After spending ~220 seconds in this new regime, accompanied by flaring activity, the system returned to its normal state. We discuss a number of possible explanations of this peculiar behavior in the context of the physics and geometry of interactions between the pulsar wind and surrounding matter. However, a complete picture is yet to be revealed.
Author(s): Karpov S.V.; Tanashkin A.S.; Beskin G.M.; Plokhotnichenko V.L.,Shibanov Y.A.; Zyuzin D.A.
IVOA id: ivo://cds.vizier/j/a+a/709/a170

eROSITA detected cool stars TESS derived periods

2026-05-13T06:51:37Z

Description: The rotation-activity connection is the standard paradigm for interpreting chromospheric and coronal activity in late-type stars, namely, stars with outer convection zones. This paradigm states that activity increases with decreasing rotation period until a saturation limit is reached. By scaling rotation periods with the convective turnover time via the Rossby number, Ro, saturation is expected to occur at a universal value across all spectral types. In our paper, we systematically investigate the relationship between rotation and activity as measured though X-ray emission for a large sample of late-type stars to test the universal applicability of this paradigm. To this end, we utilized TESS short-cadence space photometry to determine the rotation periods for late-type stars identified in the eROSITA all-sky survey. This combined dataset provides rotation and X-ray measurements for 14004 stars, representing a sample size increase of more than an order of magnitude compared to previous studies. Our results show that F-type stars do not reach the "classical" saturation limit of LX/Lbol~10^-3^, instead exhibiting significantly lower LX/Lbol values. We find that the convective turnover times derived from this sample closely agree with theoretical computations, supporting the idea that Rossby number-activity relations hold for all late-type main sequence stars. The lower level of activity in earlier spectral types (e.g., F-type and late A-type stars) is a physical consequence of their short convective turnover times, which prevent them from rotating rapidly enough to ever reach the saturation regime. We demonstrate that a simple model incorporating our derived turnover times versus color can successfully reproduce he observed characteristics of the eROSITA X-ray activity distribution, as measured by the LX /Lbol ratio and Gaia BP-RP color.
Author(s): Schmitt J.H.M.M.; Schneider P.C.; Czesla S.; Freund S.; Robrade J.
IVOA id: ivo://cds.vizier/j/a+a/709/a180

Galactic diffuse H2 rotational lines with JWST

2026-05-13T06:50:13Z

Description: A statistically significant sampling of H_2_ rotational excitation in the diffuse interstellar medium (ISM) is essential to identify its dominant excitation mechanisms and assess the importance of H_2_ in the cooling of the gas and the regulation of thermal pressure. To expand upon the statistics provided by ancillary telescopes, we conduct a search for pure rotational H_2_ emission lines in all publicly available background observations obtained with the Medium Resolution Spectrometer (MRS) aboard the JWST. The sample consists of 276 background observations acquired over the past three years. Departing from the standard pipeline, each uncalibrated MRS background file is reprocessed, enabling the analysis of H_2_ pure rotational emission. Lines of sight likely associated with star-forming complexes are excluded in order to focus on emission from the diffuse ISM. The results are compared with FUSE absorption data and are analyzed in relation to the column densities of H and H_2_ and dust emission derived from HI4PI, Planck, and WISE data. This analysis reveals widespread H_2_ emission throughout the Galaxy. We report the first detections of the pure rotational S(4), S(5), and S(7) lines in the diffuse ISM. The S(1) line is detected along 84 lines of sight, corresponding to a detection rate of 41%. Its integrated intensity decreases steeply with Galactic latitude, spanning nearly two orders of magnitude in remarkable agreement with absorption measurements. The T34 and T35 excitation temperatures are correlated, and vary between 200 and ~1000K, showing an anticorrelation with the column density of H_2_ as expected from ancillary data. All lines of sight in the sample have undergone the H-H_2_ transition, at NH>~10^+20^cm^-2^, and are partly molecular with f_H2_>~0.1. Under these conditions, the cooling rate associated with the S(1) line, expressed per hydrogen atom, is found to be remarkably constant, with a characteristic value of ~4x10^-27^erg/s/H. This study demonstrates that the high sensitivity of the JWST enables measurements that both strengthen and complement those from absorption studies. Observations collected over just a fraction of JWST's lifetime have already yielded detections along dozens of lines of sight, significantly expanding the statistical sample of H_2_ rotational excitation in the diffuse ISM.
Author(s): Nigou E.; Godard B.; Guillard P.; Pineau des Forets G.,Miville-Deschenes M.A.; Lesaffre P.
IVOA id: ivo://cds.vizier/j/a+a/709/a152

J-PLUS DR3 stellar mass function SFR gal.

2026-05-13T06:31:48Z

Description: We derive the stellar mass function (SMF) of quiescent and star-forming galaxies at z<=0.2 using 12-band (five broad plus seven narrow) photometry from the Javalambre Photometric Local Universe Survey (J-PLUS) third data release (DR3) over 3284 deg2, where the narrow bands improve photometric-redshift and stellar property precision relative to purely broadband surveys. We selected ~890000 galaxies with r<=20mag and photometric redshifts in the range 0.05<=z<=0.20 over an effective area of 2881deg^2^, corresponding to a comoving volume of V=~1.6x10^8^Mpc^3^. Stellar masses and star formation rates were derived through spectral energy distribution (SED) fitting with the Code Investigating GALaxy Emission (CIGALE), and confronted with spectroscopic samples. Galaxies were classified as star-forming or quiescent based on their specific star formation rate (sSFR), adopting a threshold of log(sSFR[yr^-1^])=-10.2. We computed SMFs for both populations using the 1/Vmax method, applied completeness corrections, and fit a parametric single Schechter function. The SMFs derived from J-PLUS DR3 are well described by Schechter functions and agree with previous photometric and spectroscopic studies. The characteristic mass for quiescent galaxies, log(M*/M_{sun}_)=10.80, is higher by 0.4dex than that of star-forming galaxies. The faint-end slope is steeper for star-forming galaxies (alpha=-1.2) than for quiescent ones (aplha=-0.7). The quiescent fraction increases by 40% per dex in stellar mass, reaching fQ>.95 at log(M*/M_{sun}_)>11. Comparisons with the GAlaxy Evolution and Assembly (GAEA) semi-analytic model show an overabundance of simulated star-forming galaxies, particularly at intermediate masses. The SMFs and quiescent fraction from J-PLUS DR3 are consistent with the literature and provide valuable constraints for galaxy formation models. Quiescent galaxies represent 45% of the number density at log M*>9 but contribute 75% of the stellar mass density. This work lays the groundwork for studies of environmental quenching using J-PLUS. The inclusion of seven narrowband filters improves redshift precision by 20%, enabling more accurate SED fitting and galaxy classification. These methods and findings can be extended with J-PAS, which will provide deeper and higher-resolution photometry over a wider spectral range.
Author(s): Arizo-Borillo F.D.; Lopez-Sanjuan C.; Pintos-Castro I.,Fernandez-Ontiveros J.A.; Kuutma T.; Lumbreras-Calle A.,Hernan-Caballero A.; Dominguez-Sanchez H.; De Lucia G.; Fontanot F.,Diaz-Garcia L.A.; Vilchez J.M.; Rahna P.T.; Cenarro A.J.,Cristobal-Hornillos D.; Hernandez-Monteagudo C.; Marin-Franch A.; Moles M.,Varela J.; Vazquez Ramio H.; Alcaniz J.; Dupke R.A.; Ederoclite A.,Sodre L. Jr; Angulo R.E.
IVOA id: ivo://cds.vizier/j/a+a/709/a157

VLBI-based combined catalog of radio sources

2026-05-13T06:19:41Z

Description: The International Celestial Reference System (ICRS) is realized in the radio band by a catalog of radio source positions obtained by very long baseline interferometry (VLBI) measurements and called the International Celestial Reference Frame (ICRF). The current ICRF approved by the International Astronomical Union (IAU) at its XXXth general assembly in August 2018 is the ICRF3. Discussions are currently underway on the preparation of the next ICRF release, the ICRF4. In this paper, we investigate a possibility to improve the S/X version of the ICRF3 by constructing a combined catalog of radio source positions based in individual catalogs provided by VLBI analysis centers. This study is based on the analysis of the systematic errors of six most recent VLBI radio source catalogs using Vector Spherical Harmonics (VSH). In a first step, we determined the systematic differences between each input catalog and the S/X version of the ICRF3. These systematics were then applied to the input catalogs to transform them into the ICRF3 system. The average of these transformed catalogs is the combined catalog in the ICRF3 system (COMB1X). Applying the averaged systematics to the COMB1X catalog, we obtain the combined catalog in an independent system (COMB2X). The intercomparison of partial combinations allowed us to rescale the formal errors to make them more realistic. The two combined catalogs of radio source positions contain a few more sources than individual catalogs. The COMB1X catalog can be considered as an improvement of ICRF3 in terms of stochastic errors. The COMB2X catalog can be considered as an improvement of ICRF3 in terms of both stochastic and systematic errors. The COMB2X catalog reveals systematic error of a few tens of microarcseconds with respect to the ICRF3.
Author(s): Lambert S.; Malkin Z.
IVOA id: ivo://cds.vizier/j/a+a/709/a98

DESI observations of the Andromeda galaxy

2026-05-12T20:05:24Z

Description: We present Dark Energy Spectroscopic Instrument (DESI) observations of the inner halo of M31, which reveal the kinematics of a recent merger-a galactic immigration event-in exquisite detail. Of the 11416 sources studied in 3.75hr of on-sky exposure time, 7438 are M31 sources with well-measured radial velocities. The observations reveal intricate coherent kinematic structure in the positions and velocities of individual stars: streams, wedges, and chevrons. While hints of coherent structures have been previously detected in M31, this is the first time they have been seen with such detail and clarity in a galaxy beyond the Milky Way. We find clear kinematic evidence for shell structures in the Giant Stellar Stream, the Northeast Shelf, and Western Shelf regions. The kinematics are remarkably similar to the predictions of dynamical models constructed to explain the spatial morphology of the inner halo. The results are consistent with the interpretation that much of the substructure in the inner halo of M31 is produced by a single galactic immigration event 1-2Gyr ago. Significant numbers of metal-rich stars ([Fe/H]{>}-0.5) are present in all of the detected substructures, suggesting that the immigrating galaxy had an extended star formation history. We also investigate the ability of the shells and Giant Stellar Stream to constrain the gravitational potential of M31, and estimate the mass within a projected radius of 125kpc to be log_10_M_NFW_(<125kpc)/M_{sun}_=11.80_-0.10_^+0.12^. The results herald a new era in our ability to study stars on a galactic scale and the immigration histories of galaxies.
Author(s): Dey A.; Najita J.R.; Koposov S.E.; Josephy-Zack J.; Maxemin G.; Bell E.F.,Poppett C.; Patel E.; Beraldo Silva L. e; Raichoor A.; Schlegel D.,Lang D.; Meisner A.; Myers A.D.; Aguilar J.; Ahlen S.; Allende Prieto C.,Brooks D.; Cooper A.P.; Dawson K.S.; de la Macorra A.; Doel P.,Font-Ribera A.; Garcia-Bellido J.; Gontcho Gontcho S. A; Guy J.,Honscheid K.; Kehoe R.; Kisner T.; Kremin A.; Landriau M.; Le Guillou L.,Levi M.E.; Li T.S.; Martini P.; Miquel R.; Moustakas J.; Nie J.,Palanque-Delabrouille N.; Prada F.; Schlafly E.F.; Sharples R.M.,Tarle G.; Ting Y.-S.; Tyas L.; Valluri M.; Wechsler R.H.; Zou H.
IVOA id: ivo://cds.vizier/j/apj/944/1

AGB with UV-excess dusty envelopes

2026-05-12T20:02:37Z

Description: Roughly spherical envelopes around asymptotic giant branch (AGB) stars transform into the highly-asymmetric morphologies observed in planetary nebulae. The complex processes suffered in this metamorphosis are not yet completely understood. However, binarity emerges as a strong shaping factor, although the identification of binary companions in AGB stars is observationally challenging. The presence of ultraviolet (UV) excesses in AGB stars has been suggested as a potential indicator of binarity. In a first study, we characterised the properties of the gas component in the circumstellar envelopes surrounding a sample of 29 AGB stars with UV excesses. Now we intend to complement this information with an analysis of the dust component and compare the estimated parameters with those previously inferred from larger samples of AGB stars. We modelled the spectral energy distributions of the sample using dust radiative transfer models. In some cases, we complemented the analysis with Herschel/PACS radial surface brightness profiles. We derived mass-loss rates and gas-to-dust ratios, which are in the typical ranges for AGB stars. We found that the stellar and mass-loss parameters follow similar trends than those presented in the literature. There is an anticorrelation between the gas-to-dust ratio and the UV emission, although it is weaker than its correlations with pulsation and mass-loss. We also estimated the dust attenuation produced by the dust at UV wavelengths and describe its effects on the intrinsic UV emission. Stellar and mass-loss parameters of UV emitting AGB stars follow similar trends as found for larger samples of AGB stars. High-angular resolution observations are required to explore the dust forming regions and identify the presence of stellar companions. Circumstellar dust attenuation might play a dominant role in the observed UV emission, and needs to be accounted to estimate the intrinsic UV emission.
Author(s): Alonso-Hernandez J.; Sanchez Contreras C.; Sahai R.; Sanz-Forcada J.
IVOA id: ivo://cds.vizier/j/a+a/709/a143

Four new brown dwarf discoveries

2026-05-12T20:02:35Z

Description: We present four newly validated transiting brown dwarfs identified through TESS photometry and confirmed with high-precision radial velocity measurements obtained from the FEROS and PLATOSpec spectrographs. Notably, three of these companions exhibit orbital periods exceeding 100 days, thereby expanding the sample of long-period transiting brown dwarfs from four to seven systems. The host stars of long-period brown dwarfs show mild subsolar metallicity. These discoveries highlight the expansion of the metal-poor, long-period distribution and help us better understand the brown dwarf desert. In our comparative analysis of eccentricity and metallicity demographics, we utilize catalogues of long-period giant planets, brown dwarfs, and low-mass stellar companions. After accounting for tidal influences, the eccentricity distribution aligns with that of low-mass stellar binaries, presenting a different profile than that observed within the giant planet population. Additionally, the metallicity of the host stars reveals a noteworthy trend: short-period transiting brown dwarfs are predominantly associated with metal-rich stars, whereas long-period brown dwarfs are more often found around metal-poor stars, demonstrating statistical similarities to low-mass stellar hosts. This trend has also been previously observed in studies of hot and cold Jupiters and points to a period-coded mixture of channels. A natural explanation is that most brown dwarfs originate from fragmentation at wider separations, with long-period systems retaining this stellar-like imprint, while only those embedded in massive, long-lived, metal-rich protoplanetary discs are efficiently delivered and stabilised to short orbits.
Author(s): Subjak J.; Brahm R.; Liptak J.; Eberhardt J.; Tala Pinto M.; Casewell S.L.,Henning T.; Hesse K.; Trifonov T.; Jordan A.; Rojas F.I.; Vitkova M.,Salinas H.; Boyle G.; Suc V.; Antonucci L.; Bernacki K.; Briceno C.,Collins K.A.; Fernandez Fernandez J.; Gill S.; Janik J.; Law N.; Mann A.W.,McCormac J.; Popowicz A.; Sebastian D.; Skarka M.; Vaclavik J.; Vanzi L.,West R.G.; Wilkin F.P.; Ziegler C.
IVOA id: ivo://cds.vizier/j/a+a/709/a130

Rotational velocities of 2558 stars

2026-05-12T16:23:52Z

Description: A general catalogue of rotational velocities of 2558 stars has been compiled on the basis of published data. All the vsini values are reduced to the Slettebak system. The spectral classes of 1913 stars are in the MK system and of most of the others in the HD system. The catalogue is sufficiently complete for O5-G5 stars brighter than 5.5m.
Author(s): Boyarchuk A.A.; Kopylov I.M.
IVOA id: ivo://cds.vizier/j/other/izkry/31.44

HD 161098 RVs and activity indicators

2026-05-12T16:14:55Z

Description: The development of refined instruments and techniques for a detailed analysis of the radial velocities (RVs) of stars other than the Sun allows the presence of planetary signals of amplitude below 1m/s to be investigated. Long-term RV surveys allow the detection of Earth-like and super-Earth-like planets in the habitable zones of Sun-like stars, prime targets for future missions for the atmospheric characterization of exoplanets. We present the analysis of the nearby G8 V-type star HD 161098 (V=7.68mag, d=29.75pc). We searched for terrestrial planets in the habitable zone. We combined historical datasets with new data collected in an ongoing blind search program with HARPS, HARPS-N, and ESPRESSO. We utilized recently developed tools to extract RVs and to deal with the analysis of stellar activity. We performed a joint analysis of RVs and activity indicators to separate the planetary signals from those related to activity. We detected two sub-m/s1 signals that we claim as candidate planets. We are not able to confirm their nature with certainty. Candidate HD 161098 b has an orbital period of 72.578_-0.060_^+0.059^d and a minimum mass of 3.63+/-0.59M_{Earth}_. HD 161098 c has an orbital period of 682.5_-9.9_^+9.5^d and a minimum mass of 7.8_-1.4_^+1.5^M_{Earth}_. If confirmed, candidate HD 161098 c would reside in the optimistic habitable zone of the star. We find a magnetic cycle of 4090_-130_^+140^d period and a rotation period of 28.22_-0.35_^+0.30^d. Our analysis sets the stage for future observing campaigns of the star, finalized for the confirmation of our results. We are entering the sub-m/s era at long orbital periods with a combination of stellar activity treatment and long-term campaigns.
Author(s): Nari N.; Suarez Mascareno A.; Gonzalez Hernandez J.I.; Stefanov A.K.,Rebolo R.; Mestre J.M.; Dumusque X.; Cretignier M.; Passegger V.M.,Mignon L.; Manni F.; De Amorim R.G.S.B.
IVOA id: ivo://cds.vizier/j/a+a/709/a123

z~1 star-forming galaxies Tully-Fisher relation

2026-05-12T15:59:35Z

Description: Extending local kinematic studies to earlier cosmic times is valuable to understand how galaxies evolve in relation to their dark matter haloes. In a series of papers on lensed kinematics, we seek to combine the sensitivity of 3D forward modelling to low signal-to-noise ratio outskirts with the enhanced spatial resolution provided by cluster lensing. In this first paper, we (i) present and validate our methodology, which directly constrains the source parameters by incorporating lensing deflections into the GalPaK3D forward-modelling algorithm, and (ii) investigate the evolution of the stellar-mass and baryonic-mass Tully-Fisher relations (sTFR and bTFR) since z~1 as a demonstration. We define a robust sample of strongly lensed star-forming galaxies (SFGs) from the MUSE Lensing Cluster survey, spanning magnifications mu=1.4-12.4 and stellar masses M*=10^8.1^-10^10.3^M__{sun}_. Using a series of mock galaxies representative of our sample, we find that our method is significantly more reliable at recovering morpho-kinematic properties than approaches that ignore differential magnification, even for relatively modest magnifications (mu<6). Restricting the analysis to 95 rotationally supported SFGs with well-constrained velocities, we find a significant evolution of the sTFR zero-point ({Delta}b^sTFR^=-0.42^+0.05^_-0.05_dex in stellar mass) but no detectable evolution of the bTFR zero-point ({Delta}b^bTFR^=0.00^+0.06^_-0.06_dex in baryonic mass) relative to z~0. Our results are consistent with a mild evolution of the stellar-to-halo mass ratio and support the view that the sTFR has evolved only weakly over the past ~8Gyr, aside from shifts driven by the redshift dependence of halo-defining quantities such as the critical density and overdensity. The absence of detectable evolution in the bTFR zero-point suggests that the increasing contribution of cold gas mass at higher redshift fully compensates the evolution observed in the stellar component alone.
Author(s): Jeanneau A.; Richard J.; Bouche N.F.; Krajnovic D.; Ciocan B.-I.,Freundlich J.; Epinat B.; Contini T.
IVOA id: ivo://cds.vizier/j/a+a/709/a120

UNCOVER survey: redshift cat. from JWST sp. in A2744

2026-05-12T15:41:22Z

Description: We present the design and observations of low-resolution JWST/NIRSpec PRISM spectroscopy from the Ultradeep NIRSpec and NIRCam ObserVations before the Epoch of Reionization (UNCOVER) Cycle 1 JWST Treasury program. Targets are selected using JWST/NIRCam photometry from UNCOVER and other programs, and cover a wide range of categories and redshifts to ensure the legacy value of the survey. These categories include the first galaxies at z>~10, faint galaxies during the Epoch of Reionization (z~6-8), high-redshift active galactic nuclei (z>=6), Population III star candidates, distant quiescent and dusty galaxies (1<~z<~6), and filler galaxies sampling redshift-color-magnitude space from z~0.1-13. Seven NIRSpec microshutter array masks across the extended A2744 cluster were observed, along with NIRCam parallel imaging in nine filters (F090W, F115W, F150W, F200W, F277W, F356W, F410M, F444W, and F480M) over a total area of ~26arcmin2, overlapping existing Hubble Space Telescope coverage from programs including the Hubble Frontier Fields and BUFFALO. We successfully observed 553 objects down to m_F444W_~30 AB, and by leveraging mask overlaps, we reach total on-target exposure times ranging from 2.4 to 16.7hr. We demonstrate the success rate and distribution of the confirmed redshifts, and also highlight the rich information revealed by these ultradeep spectra for a subset of our targets. An updated lens model of A2744 is also presented, including 14 additional spectroscopic redshifts and finding a total cluster mass of M_SL_=(2.1+/-0.3)x10^15^M_{sun}_.
Author(s): Price S.H.; Bezanson R.; Labbe I.; Furtak L.J.; de Graaff A.; Greene J.E.,Kokorev V.; Setton D.J.; Suess K.A.; Brammer G.; Cutler S.E.; Leja J.,Pan R.; Wang B.; Weaver J.R.; Whitaker K.E.; Atek H.; Burgasser A.J.,Chemerynska I.; Dayal P.; Feldmann R.; Forster Schreiber N.M.,Fudamoto Y.; Fujimoto S.; Glazebrook K.; Goulding A.D.; Khullar G.,Kriek M.; Marchesini D.; Maseda M.V.; Miller T.B.; Muzzin A.,Nanayakkara T.; Nelson E.; Oesch P.A.; Shipley H.; Smit R.; Taylor E.N.,van Dokkum P.; Williams C.C.; Zitrin A.
IVOA id: ivo://cds.vizier/j/apj/982/51

Blue horizontal-branch stars from SkyMapper colors

2026-05-12T14:15:55Z

Description: Blue horizontal-branch (BHB) stars are ideal tracers for mapping the structure of the Galactic stellar halo. Traditionally, BHB sample stars are built from large-scale spectroscopic surveys utilizing their spectral features; however, the resulting sample sizes have been quite limited. In this paper, we construct a catalog of BHB stars based on synthetic colors (u-v)0 and (g-i)0 in SkyMapper photometric systems, which are convolved from Gaia XP spectra. A total of 49,733 BHB stars are selected from nearly the entire sky (excluding regions of low Galactic latitudes |b|<=8{deg} with heavy reddening), with a completeness and purity exceeding 90%. Using member stars of globular clusters with precise distance determinations, we carefully calibrate the relationship between the g-band absolute magnitude and (g-i)0, achieving a precision of 0.11mag, which corresponds to a 5% uncertainty in distance. This relation is applied to derive distances for all BHB stars in the constructed sample. Given the current capabilities of Gaia XP observations, the constructed BHB sample is primarily located within 20 kpc, enabling detailed mapping of the inner stellar halo. To extend this depth to the outer halo or even the edge of our Galaxy, we explore the potential of the Chinese Space Station Telescope (CSST) and its broadband photometry for detecting BHB stars. Using mock data from synthetic spectra, we find that it is feasible to distinguish BHB stars from blue stragglers stars using CSST near-ultraviolet band (u) photometry. Thanks to the deep limiting magnitude of CSST, its data will provide a groundbreaking perspective on our Galaxy, particularly regarding the outer halo, in an unprecedented volume.
Author(s): Hu G.; Huang Y.; Cui W.; Wang T.; Xiao K.; Shi R.; Ju J.; Huang B.; Li C.,Liu Z.; Wang X.; Luo C.
IVOA id: ivo://cds.vizier/j/apjs/278/62

Supermassive BH with accretion rates in AGN. XIV.

2026-05-12T13:23:04Z

Description: We report the results of a long-duration high-cadence reverberation mapping campaign of a second batch of 11 PG quasars using the 2.2m telescope at the Calar Alto Observatory. This follows a similar earlier study of another sample of 15 objects reported by Hu+ (2021, J/ApJS/253/20). Among the 11 PG quasars, eight objects have the H{beta} time lags measured for the first time, while the other three objects were observed in previous campaigns but only had highly uncertain H{beta}-lag measurements. Long-term light curves are presented of photometric V-band, spectroscopic 5100{AA} continuum, and the H{beta} emission line, lasting for ~3-6yr with a cadence of ~6-14d. Accurate H{beta} time lags ranging from ~20 to 150 days in the rest frame are obtained. The estimated virial masses of the central supermassive black holes range from ~(3-300)x10^7^M_{sun}_. Combining these results with those reported in Hu+ (2021), we now have 26 PG quasars, with representative properties, having reliable H{beta} time-lag measurements from our long-duration high-cadence campaign. A tentative fit to the relation between the H{beta} time lag and the continuum luminosity for these 26 objects gives a slope of 0.53.
Author(s): Hu C.; Yao Z.-H.; Chen Y.-J.; Songsheng Y.-Y.; Wang Y.-L.; Yang S.,Zhang H.; Guo W.-J.; Du Pu; Li Y.-R.; Xiao M.; Liu J.-R.; Bai H.-R.,Fang F.-N.; Fu Y.-X.; Peng Y.-C.; Zhai S.; Bai J.-M.; Ho L.C.,Brotherton M.S.; Aceituno J.; Winkler H.; Wang J.-M.,SEAMBH collaboration
IVOA id: ivo://cds.vizier/j/apjs/278/61

SEAMBH in AGNs. XIII. Mrk142 GMOS and LJT spectra

2026-05-12T12:33:38Z

Description: We performed a rigorous reverberation-mapping analysis of the broad-line region (BLR) in a highly accreting (L/L_Edd_=0.74-3.4) active galactic nucleus, Markarian 142 (Mrk 142), for the first time using concurrent observations of the inner accretion disk and the BLR to determine a time lag for the H{beta}{lambda}4861 emission relative to the ultraviolet (UV) continuum variations. We used continuum data taken with the Niel Gehrels Swift Observatory in the UVW2 band, and the Las Cumbres Observatory, Dan Zowada Memorial Observatory, and Liverpool Telescope in the g band, as part of the broader Mrk 142 multiwavelength monitoring campaign in 2019. We obtained new spectroscopic observations covering the H{beta} broad emission line in the optical from the Gemini North Telescope and the Lijiang 2.4m Telescope for a total of 102 epochs (over a period of 8 months) contemporaneous to the continuum data. Our primary result states a UV-to-H{beta} time lag of 8.68_-0.72_^+0.75^ days in Mrk 142 obtained from light-curve analysis with a Python-based running optimal average algorithm. We placed our new measurements for Mrk 142 on the optical and UV radius-luminosity relations for NGC 5548 to understand the nature of the continuum driver. The positions of Mrk 142 on the scaling relations suggest that UV is closer to the "true" driving continuum than the optical. Furthermore, we obtain log(M_{bullet}_/M_{sun}_)=6.32+/-0.29 assuming UV as the primary driving continuum.
Author(s): Khatu V.C.; Gallagher S.C.; Horne K.; Cackett E.M.; Hu C.; Pasquini S.,Hall P.; Wang J.-M.; Bian W.-H.; Li Y.-R.; Bai J.-M.; Chen Y.-J.; Du Pu,Goad M.; Jiang B.-W.; Li S.-S.; Songsheng Y.-Y.; Wang C.; Xiao M.; Yu Z.
IVOA id: ivo://cds.vizier/j/apj/958/127

Astro-COLIBRI Simple Cone Search

2026-05-12T09:13:16.577000Z

Description: IVOA-compliant Simple Cone Search service for Astro-COLIBRI. Retrieving all transient events from the past year.
IVOA id: ivo://astrocolibri/conesearch

Hubble Missing Globular Cluster Survey. III.

2026-05-12T07:59:47Z

Description: The Hubble Missing Globular Cluster Survey (MGCS) has taken one of the last opportunities to complete the census of Galactic globular clusters (GCs) started by past Hubble Space Telescope (HST) programs, securing high-resolution data for 34 GCs never observed before by HST. The previous papers of the series have highlighted the astrometric and photometric potential of the project by analyzing a subsample of targets. We present, and release to the community, the official astro-photometric catalogs of the MGCS for all GCs imaged by this project. We describe the data reduction using state-of-the-art techniques designed for HST. We discuss the photometric calibration and show, for the first time, the synergy with the Gaia catalog to ensure homogeneous photometry across our data set. We compute artificial-star tests that can be used to assess systematics and the completeness level of our data. We combined HST and Gaia data to refine the absolute proper motions of our GCs, reaching a precision ~3 times better than that of Gaia alone. We used these new proper motions to update (and to determine for the first time for six systems) the associations between GCs and their putative galaxy progenitors. This work continues decades-long efforts of large Treasury programs in sharing precise and accurate atlases to the community for studying GCs across a wide range of scientific endeavors.
Author(s): Libralato M.; Bellini A.; Massari D.; Bellazzini M.; Aguado-Agelet F.,Cassisi S.; Ceccarelli E.; Dalessandro E.; Dodd E.; Ferraro F.R.,Gallart C.; Lanzoni B.; Monelli M.; Mucciarelli A.; Pancino E.; Pascale R.,Rosignoli L.; Salaris M.; Saracino S.; Zerbinati C.
IVOA id: ivo://cds.vizier/j/a+a/709/a140

TOI-1710 HARPS-N radial velocity curve

2026-05-12T07:53:19Z

Description: The obliquity between a planet's orbital axis and its host star's spin axis provides crucial insights into planetary formation and migration. Planets with scaled semi-major axes (a/R*) large enough to be unaffected by tidal alterations (tidally detached), offer a unique opportunity to study the original obliquity in which the system formed. We therefore observed TOI-1710 b (a/R*~36) in-transit using HARPS-N + GIANO-B, collecting high-precision radial velocities to measure the Rossiter-McLaughlin (RM) effect. Spectral analysis of the H{alpha} and HeI triple lines was also pursued to evaluate atmospheric photoevaporation. Using our knowledge of the star rotation period (21.5+/-0.2d), we estimated a true obliquity of psi=149^+11^_-10_deg, which indicates a retrograde motion and places TOI-1710 b among the most misaligned systems -- and the only one known orbiting a cool star in retrograde motion. The strong misalignment favours a high-eccentricity migration (HEM) origin for this low-density super-Neptune planet in the savanna region, challenging previous findings that claimed a minor role of HEM in this period-radius(-density) domain. Moreover, the strong misalignment and lack of a detected close stellar companion suggests a purely planetary post-migration misalignment, likely due to planet-planet scattering followed by planet-planet Kozai-Lidov oscillations and tidal circularisation.
Author(s): Mantovan G.; Malavolta L.; Lanza A.F.; Marzari F.; Naponiello L.; Biazzo K.,Cosentino R.; D'Arpa M.C.; Desidera S.; Guilluy G.; Nardiello D.,Sozzetti A.; Vissapragada S.; Aloisi R.; Benatti S.; Borsato L.; Claudi R.,Jenkins S.; Nascimbeni V.; Piotto G.; Zingales T.
IVOA id: ivo://cds.vizier/j/a+a/709/l15

Abundances in 8 nearby young clusters

2026-05-12T07:52:25Z

Description: We conducted a homogeneous chemical analysis of pre-main sequence stars with effective temperatures ranging from ~3000K to ~5500K in eight nearby star-forming regions (SFRs): Chamaeleon I, eta Chamaeleonis, Lupus, Orion OB1a, Orion OB1b, sigma Orionis, Taurus, and Corona-Australis. Our study aims to: 1) derive the lithium abundance (A(Li)) and highlight the impact of veiling correction on both A(Li) and age determination; 2) perform the iron (Fe) and barium (Ba) abundance analysis in regions with scarce previous measurements; 3) investigate the possible Ba enhancement. The analyzed data were obtained as part of the PENELLOPE Large Program using the ESPRESSO, UVES, and X-Shooter instruments. We measured the equivalent width of the lithium line (EWLi) at {lambda}=6707.8{AA}, from which A(Li) is derived using the curves of growth method. The Fe and Ba abundances have been measured through spectral synthesis analysis. Using the EAGLES code, we derived an upper limit on the age of the eight SFRs. Our findings underscore the necessity of veiling corrections on EWLi, which can shift A(Li) and age estimates by up to ~0.7dex and ~20Myr, respectively. Accounting for veiling, the A(Li) distributions peak in a range between 3.3 and 3.8dex for most clusters, and the upper age limit is approximately 5Myr for all SFRs. We successfully measured the mean iron and barium abundances in Lupus, Taurus, Cha I, and eta Cha, showing slightly sub-solar iron abundance, and a clear Ba overabundance, with [Ba/H] values reaching up to 0.75 dex.
Author(s): Carini R.; Biazzo K.; Frasca A.; Manara C.F.; Alcala J.M.; Abraham P.,Campbell-White J.; Claes R.; Fang M.; Gangi M.; Gameiro J.F.; Kospal A.,Mauco K.; Mendigutia I.; Nisini B.; Robberto M.; Robinson C.E.,Schneider C.; Siwak M.; Sperling T.; Tychoniec L.; Venuti L.
IVOA id: ivo://cds.vizier/j/a+a/709/a144

HC_9N {nu}_19 overtones in IRC +10216

2026-05-12T07:49:56Z

Description: The sub-milliKelvin sensitivity achieved in the Q-band (31-50GHz) line survey of IRC+10216 obtained with the Yebes 40m telescope reveals the presence of several new vibrational HC_9_N overtones (nu_19_>=2) beyond the already reported nu_19_=1. The newly found series of rotational lines appears in seven groups with rotational constants (B) between 291.252 and 293.465MHz, with integer quantum numbers from J_up_=54 to 81 and upper-level excitation energies up to ~600K, well above what is typical of lines found in the outer part of this circumstellar envelope. All evidence, especially the spectral splitting of the l-doubling components and the spacing between B values, unambiguously points toward rotational lines within nu_19_=2-8 that appear surprisingly strong, possibly due to very efficient infrared pumping and slow decay via the nu_19_ mode. The detection of nu_19_=5, 6, 7, and 8 has been possible thanks to collapsed l-doubling components to a single or only two spectral features per rotational transition. To obtain a correct determination of the abundance of HC_9_N in IRC+10216 one has to take into account that about ~70% is estimated to be in the vibrationally excited nu_19_ states.
Author(s): Pardo J.R.; Cernicharo J.; Fonfria J.P.; Cabezas C.; Agundez M.; Tercero B.,Marcelino N.; de Vicente P.; Velilla-Prieto L.; Guelin M.
IVOA id: ivo://cds.vizier/j/a+a/709/l13

Einstein Probe TAP Service

2026-05-11T12:47:38.567000Z

Description: Einstein Probe Observation Schedule and Plans accessed via Table Access Protocol.
IVOA id: ivo://einsteinprobe/tap

The eXtended Catalogue of Spectroscopic Binary Orbits (SBX)

2026-05-10T09:10:39.999000Z

Description: The SBX TAP service provides programmatic access to the eXtended Catalogue of Spectroscopic Binary Orbits (SBX), the successor of the SB9 catalogue, a curated and continuously updated database of orbital solutions for spectroscopic binary stars.
IVOA id: ivo://astro.ulb.ac.be/sbx-tap

LBT spectra of 16 stars

2026-05-08T16:01:32Z

Description: The diffuse interstellar bands (DIBs) at 9577 and 9632{AA} are attributed to electronic transitions of the C60+ fullerene ion; thus, its column density in molecular clouds may be inferred. A comparison with the column density of the neutral C60 fullerene makes it possible to determine local physical conditions in the clouds. We aim to detect absorption lines of neutral C60 in the visible spectra of stars toward interstellar clouds. We searched for the {gamma}0, A0, and A1 absorption bands of C60 near 6070{AA}, 4024{AA}, and 3980{AA} using the Potsdam Echelle Polarimetric and Spectroscopic Instrument at the Large Binocular Telescope. We measured spectra toward eight background stars including BD+31 643. None of the {gamma}0, A0, and A1 absorption bands of C60 were detected in our spectra. Toward BD+31 643, we determine an upper limit of (14+/-11)x10^12^cm^-2^ for the column density of C60, and values in the range of 10^12^-10^14^cm^-2^ toward other stars. Using literature data for C60+, we derive upper limits of 0.8-3.8 for the C60:C60+ column density ratios. The non-detection of the {gamma}0 absorption band toward BD+31 643 is in conflict with a measurement employing infrared (IR) emission bands of C60. The discrepancy may indicate that free C60 molecules are not the source of the observed IR emission bands toward the star and that the IR emission arises from C60 molecules in dust grains instead. Alternatively, the oscillator strength of the {gamma}0 band may not be well constrained from the laboratory measurements.
Author(s): Rouille G.; Gredel R.
IVOA id: ivo://cds.vizier/j/a+a/709/a104

Milky Way as seen by classical Cepheids. I. WISE

2026-05-07T13:53:31Z

Description: Classical Cepheids are the archetype of the standard candle, thanks to the period-luminosity relation, which allows us to measure their intrinsic brightness. They are also relatively young and bright, potentially making them excellent tracers of the young stellar population that is responsible for shaping the visible aspect of our Galaxy. However, being observers embedded in the dusty interstellar medium of the Galaxy, deriving reliable photometric distances to classical Cepheids of the Milky Way is a challenge. The typical approach is to use "reddening-free" indices, such as Wesenheit magnitudes, to obviate the need for an extinction correction. However, this approach could lead to unknown systematics-especially toward the inner Galaxy-as its assumption of a universal total-to-selective extinction ratio is not satisfied, particularly in lines of sight where the extinction is high and crosses spiral arms. We instead estimate new distances for 3424 Cepheids based on mid-IR photometry from the Wide-field Infrared Survey Explorer, which suffers minimally from extinction, and by adopting a 3D extinction map to calculate the necessary (albeit small) extinction corrections. We show that our distances are consistent with Gaia's parallaxes for the subset with relative parallax errors smaller than 10%, verifying that our mean distance errors are of the order of 6% and that the mean parallax zero-point for this subsample is 7{mu}as.
Author(s): Skowron D.M.; Drimmel R.; Khanna S.; Spagna A.; Poggio E.; Ramos P.
IVOA id: ivo://cds.vizier/j/apjs/278/57

Spectroscopic redshift survey of the Coma cluster

2026-05-07T07:47:31Z

Description: We study the physical properties of weak-lensing subhalos in the Coma cluster of galaxies using data from galaxy redshift surveys. The data include 12,989 galaxies with measured spectroscopic redshifts (2184 from our MMT/Hectospec observations and 10,807 from the literature). The r-band magnitude limit at which the differential spectroscopic completeness drops below 50% is 20.2mag, which is spatially uniform in a region of 4.5deg2 where the weak-lensing map of Okabe+ 2014ApJ...784...90O exists. We identify 1337 member galaxies in this field and use them to understand the nature of 32 subhalos detected in a weak-lensing analysis. We use Gaussian mixture modeling (GMM) in the line-of-sight velocity domain to measure the mean velocity, the velocity dispersion, and the number of subhalo galaxies by mitigating contamination from interloping galaxies. Using subhalo properties calculated with the GMM, we find no significant difference in the redshift space distribution between the cluster member galaxies and subhalos. We find that the weak-lensing mass shows strong correlations with the number of subhalo member galaxies, velocity dispersion, and dynamical mass of subhalos with power-law slopes of 0.54_-0.15_^+0.16^, 0.93_-0.32_^+0.35^, and 0.50_-0.18^+0.31^, respectively. The slope of the mass-velocity dispersion relation of the weak-lensing subhalos appears shallower than that of galaxy clusters, galaxy groups, and individual galaxies. These results suggest that the combination of redshift surveys with weak-lensing maps can be a powerful tool for better understanding the nature of subhalos in clusters.
Author(s): Kang W.; Hwang Ho S.; Okabe N.; Park C.
IVOA id: ivo://cds.vizier/j/apjs/278/51

CL-AGN from the DESI. II. Stat. properties from DR1

2026-05-07T07:34:22Z

Description: We present the identification of changing-look active galactic nuclei (CL-AGNs) from the Dark Energy Spectroscopic Instrument First Data Release and Sloan Digital Sky Survey Data Release 16 at z<=0.9. To confirm the CL-AGNs, we utilize spectral flux calibration assessment via an [OIII]-based calibration, pseudophotometry examination, and visual inspection. This rigorous selection process allows us to compile a statistical catalog of 561 CL-AGNs, encompassing 527 H{beta}, 149 H{alpha}, and 129 MgII CL behaviors. In this sample, we find (1) a 283:278 ratio of turn-on to turn-off CL-AGNs. (2) The median Eddington ratio for CL-AGNs in the dim state is approximately {lambda}Edd~0.01. (3) A strong correlation between the change in the luminosity of the broad emission lines (BELs) and variation in the continuum luminosity, with MgII and H{beta} displaying similar responses during CL phases. (4) The Baldwin-Phillips-Terlevich diagram for CL-AGNs shows no statistical difference from the general AGN catalog. (5) Five CL-AGNs are associated with asymmetrical mid-infrared flares, possibly linked to tidal disruption events. Given the large CL-AGN sample and the stochastic sampling of spectra, we propose that some CL phenomena are inherently due to typical AGN variability during low accretion rates, particularly for CL phenomenon only occurring on one BEL. Finally, we introduce a monotonically dimming CL phase for objects characterized by a gradual decline over decades in the light curve and the complete disappearance of entire BELs in faint spectra, indicative of a real transition in the accretion disk.
Author(s): Guo W.-J.; Zou Hu; Greenwell C.L.; Alexander D.M.; Fawcett V.A.; Pan Z.,Siudek M.; Aguilar J.N.; Ahlen S.; Brooks D.; Claybaugh T.; Dawson K.,de la Macorra A.; Doel P.; Font-Ribera A.; Gaztanaga E.,Gontcho Gontcho S. A; Gutierrez G.; Kehoe R.; Kisner T.; Landriau M.,Le Guillou L.; Manera M.; Meisner A.; Miquel R.; Moustakas J.; Prada F.,Rossi G.; Sanchez E.; Schubnell M.; Sprayberry D.; Sui J.; Tarle G.,Weaver B.A.; Xiao Y.-A.; Zou S.
IVOA id: ivo://cds.vizier/j/apjs/278/28

WD-MS binaries SEDs

2026-05-07T06:54:46Z

Description: Understanding the demographics of white dwarf-main sequence (WDMS) binaries is key to uncovering the formation of various stellar exotica and refining the details of binary stellar evolution. Despite several dedicated efforts to identify unresolved WD-MS binaries, their population remains incomplete, even within a 100pc volume-limited sample. This study aims to identify WD-MS binaries hidden within the main sequence of the optical color-magnitude diagram (CMD), improving the completeness of WD-MS binaries within a volume-limited sample of 100pc. We use NUV-optical CMDs to distinguish unresolved WD-MS binaries from the rest of the populations. High- precision astrometric and photometric data from Gaia DR3 and NUV data from GALEX GR6/7 are combined to construct CMDs. Using the binary spectral energy distribution (SED) fitting algorithm within the Virtual Observatory SED Analyzer (VOSA) tool, we estimate stellar parameters such as effective temperature, bolometric luminosity, and radii. The WD masses are determined using white dwarf evolutionary models. As we use the sources which are detected only in NUV band of GALEX, this study directly complements to majority of the previous studies. We identify 347 WDMS binary candidates within 100pc, with 188 newly reported. Our method predominantly identifies binaries having cooler WDs (<=10000K) compared to previous studies. The WD masses range from ~0.2 and 1.3M_{sun}_ , and most MS companions are of M spectral type.
Author(s): Nayak P.K.
IVOA id: ivo://cds.vizier/j/a+a/709/a114

Pleiades, Hyades, Blanco 1 rot. periods

2026-05-07T05:45:51Z

Description: We use photometric data from the TESS space observatory and optical catalogs of stars in the Pleiades, Hyades, and Blanco 1 open clusters that contain 2226, 790, and 752 sources selected based on Gaia data. Using various statistical periodicity estimation methods, such as SNR and PDM, and taking into account the TESS angular resolution (1 pixel=21"), we have determined the periods for 635, 222, and 98 stars in the Pleiades, the Hyades, and Blanco 1, respectively. The search for periodic signals was limited to 13 days, since the light curve duration in one TESS sector is about 27 days, while the use of several successive sectors is made difficult by the zero-point offset of the instrumental flux between them. Supplementing our results by information from the VizieR database, we have found that the periods were estimated for 1290 (58%), 584 (74%), and 250 (33%) stars in the Pleiades, the Hyades, and Blanco 1, respectively. Among them, for 44, 28, and 12 sources in these clusters the periods have been determined for the first time. Thus, in this paper we present the most complete catalog of periods of stars in these clusters.
Author(s): Gorbachev Mark A.; Khamitov I.M.; Bikmaev I.F.; Suslikov M.V.; Gumerov R.I.,Akhmetkhanova A.E.; Nikolaeva E.A.
IVOA id: ivo://cds.vizier/j/other/astl/51.498

Wave breaking predictions for hot Jupiters

2026-05-06T08:59:36Z

Description: Tidal interactions shape the evolution of close-in giant planets, and internal-gravity-wave breaking offers an efficient pathway for dynamical-tide dissipation, though its population-wide impact remains poorly constrained. We aim to quantify wave-breaking tidal dissipation for 550 hot Jupiters, accounting for stellar-parameter uncertainties, and to identify the most promising systems for detecting orbital decay through transit timing. Stellar masses, radii, and ages were homogeneously redetermined from spectroscopic and photometric data using isochrone fitting. For each system, these parameters were propagated through a dedicated MESA model grid to calculate the tidal quality factor, wave-breaking probability, orbital decay rate, and transit- timing diagnostics. Long-term orbital evolution was modelled to predict planetary destruction timescales. Wave breaking is predicted to be largely inactive in pre-intermediate-age main sequence (IAMS) stars. For hosts with masses <1.2M_{sun}_, it becomes effective after the IAMS, while in more massive stars it begins between the IAMS and the terminal-age main sequence (TAMS). The tidal quality factor for systems undergoing wave breaking peaks between 10^6 and 10^7, consistent with population-level inferences. About 43 % of planets, mostly with periods <3.5d, are expected to inspiral on the main sequence, providing a physical explanation for the observed tendency of hot Jupiters to orbit younger stars. A further 41 % inspiral during post-main- sequence evolution within the stages considered. Roche-limit disruption dominates overall, with engulfment occurring mainly for planets with periods > 5-6d. Systems with periods <1d, that could in principle experience the strongest tidal forcing, are unlikely to trigger wave breaking, leaving planets on stable orbits. Conversely, the most rapidly inspiralling systems with high wave-breaking probability may display measurable orbital-period shortening only over multi-decade baselines, eluding immediate detection. By contrast, the demographic imprint of wave breaking on occurrence rates should emerge more readily, with the first signs already visible in current population statistics.
Author(s): Golonka J.; Maciejewski G.
IVOA id: ivo://cds.vizier/j/a+a/709/a60

Perseus cluster LOFAR sub-80MHz LBA images

2026-05-06T08:17:11Z

Description: The Perseus cluster is a nearby cool-core galaxy cluster that hosts an archetypal radio mini-halo. Recent Low Frequency Array (LOFAR) High Band Antenna (HBA) observations at 120-168MHz have revealed the presence of a giant radio halo within the cluster with a size of 1.1Mpc enveloping the mini-halo. By exploring the spectral properties of the radio emission at low frequencies, we can gain deeper insights into the nature of this emission and improve our understanding of its origin. Here we present LOFAR Low Band Antenna (LBA) images of the cluster between 30.0-57.7MHz, with a resolution of 19.2"x15.0" and a r.m.s. noise of 3.7mJy/beam . In our images, we detect both the mini-halo and giant radio halo. We measured the spectral indices between 44 and 144 MHz of the mini-halo and giant radio halo to be -1.34+/-0.10, and -1.01+/-0.11, respectively. An alternative and more direct measurement of the spectrum of the giant radio halo results in a spectral index of -1.28+/-0.15. The discrepancy between both values is caused by the poor ionospheric conditions. In addition, we study two X-ray 'ghost cavities' in the cluster. These cavities are thought to have been produced by an older outburst from the central AGN 3C 84. We measure a spectral index between 44 and 144MHz for the radio plasma in these cavities of -1.86+/-0.12 and -1.90+/-0.12 for the northwest and southern ghost cavities, respectively. Furthermore, by including VLA 352MHz data, we find that the spectrum steepens at higher frequencies. These results are consistent with the ghost cavities being filled with old and aged radio plasma. We also detect the tailed radio galaxies NGC 1265 and IC 310. In our analysis, these sources show signs of spectral steepening along their tails.
Author(s): Groeneveld C.; van Weeren R.J.; Gendron-Marsolais M.-L.; Osinga E.,Botteon A.; de Gasperin F.; Cianfaglione M.; di Gennaro G.; Brunetti G.,Cassano R.
IVOA id: ivo://cds.vizier/j/a+a/709/a64

0446+11 15GHz VLBA images in Stokes I, Q, U

2026-05-06T08:14:56Z

Description: The physical mechanisms driving neutrino and electromagnetic flares in blazars remain poorly understood. We investigate a prominent multimessenger flare in the quasar PKS 0446+11 to identify the processes responsible for its high-energy emission. We analyzed the IceCube-240105A high-energy neutrino event together with contemporaneous observations in the gamma-ray, X-ray, optical, and radio bands. We modeled the on- and off-flare spectral energy distributions (SEDs) within a single-zone leptohadronic framework. Multi-epoch VLBA observations from the MOJAVE program provide parsec-scale polarization data that complement the multiwavelength light curves. No significant time delay was detected between the neutrino arrival and the flares in different energy bands. This is consistent with an extremely small jet viewing angle below 1 deg, inferred from the parsec-scale polarization structure. The flare can be reproduced by the injection of a proton population and an increase in the Doppler factor from 18 to 24. We also detected an approximately 90 deg rotation of the EVPA in the parsec-scale core during the initial phase of the flare, indicating the emergence of a shock formed by the change in the bulk plasma speed. Our comprehensive multimessenger analysis demonstrates that the extreme beaming and subdegree viewing angle of this distant blazar can account for the observed neutrino and electromagnetic activity. These findings strengthen the case for blazars as efficient accelerators of hadrons and significant contributors to the observed high-energy neutrino flux.
Author(s): Kovalev Y.Y.; Aller M.F.; Erkenov A.K.; Gomez J.L.; Homan D.C.,Kivokurtseva P.I.; Kovalev Yu.A.; Lister M.L.; de la Parra P.V.,Plavin A.V.; Popkov A.V.; Pushkarev A.B.; Readhead A.C.S.,Shablovinskaia E.; Sotnikova Yu.V.; Spiridonova O.I.; Troitsky S.V.,Vlasyuk V.V.
IVOA id: ivo://cds.vizier/j/a+a/709/a50

3C 84 jet images

2026-05-06T08:11:05Z

Description: The location of gamma-ray creation and emission within extra-galactic jets is a matter of active debate. One particularly well-suited source to pinpoint the location is the nearby, bright radio galaxy 3C 84, harbouring a powerful jet. Here we investigate the origin of gamma-rays measured during a recent gamma-ray flare, by analysing the linear polarisation signal of close-in-time very long baseline interferometry (VLBI) observations at centimetre and millimetre wavelengths. While 3C 84 is overall almost unpolarised, we find that close-in-time to the gamma-ray flare peak regions at parsec-scale distances from the central engine shows a fractional linear polarisation increase. Under the physically well-motivated assumption of a causal relation between this polarisation enhancement and the gamma-ray flare, and combined with insights from concurrent X-ray polarisation measurements, the gamma-rays being created in this region is a physically motivated scenario, in a process consistent with synchrotron self-Compton.
Author(s): Paraschos G.F.; Liodakis I.; Jorstad S.; Kovalev Y.Y.; Chakraborty S.,Marin F.; Ehlert S.R.; Traianou E.; Debbrecht L.C.; Agudo I.; Barnouin T.,Casey J.J.; Di Gesu L.; Kaaret P.; Kim D.E.; Kislat F.; Ratheesh A.,Saade M.L.; Tombesi F.; Marscher A.; Gomez J.-L.; Pushkarev A.B.,Savolainen T.; Myserlis I.; Gurwell M.; Keating G.; Rao R.; Kang S.,Lee S.-S.; Kim S.; Yeon Cheong W.; Jeong H.-W.; Song C.; Li S.; Nam M.-S.,Alvarez-Ortega D.; Casadio C.; Chen C.-T.; Costa E.; Churazov E.,Ferrazzoli R.; Galanti G.; Khabibullin I.; O'Dell S.L.; Pacciani L.,Roncadelli M.; Roberts O.J.; Soffitta P.; Swartz D.A.; Tavecchio F.,Weisskopf M.C.; Zhuravleva I.
IVOA id: ivo://cds.vizier/j/a+a/709/a92

Extended cluster radio sources catalog

2026-05-06T00:00:00Z

Description: The radio jets of radio galaxies in galaxy clusters are often bent due to the ram pressure of the intracluster medium. Most studies of bent radio tails initially identified tailed sources and then attempted to characterise their environments. In this paper we take an alternative approach, by starting with a well-defined sample of galaxy clusters and subsequently identifying tailed radio sources in these known environments. Our sample consists of 81 galaxy clusters from the Planck ESZ cluster sample. We present a catalogue of 127 extended cluster radio sources, including brightest cluster galaxies, obtained by visually inspecting Karl G. Jansky Very Large Array (1-2 GHz) observations. We have determined the bending angle of 109 well-structured sources, and classified them accordingly: 84 narrow-angle tailed sources (NATs), 16 wide-angle tailed sources (WATs), and 9 non-bent radio sources (i.e. with bending angles of less than 15{deg}). We find a negative correlation between the bending angle and the distance to the cluster centre (impact radius), and we observe that NATs generally have smaller impact radii than the regular galaxy population and WATs. We present a phase-space diagram of tailed radio galaxy velocities and impact radii and find that NATs have a significant excess in the high-velocity and low-impact radius region of phase space, indicating they undergo the largest amount of ram pressure bending. We compared the results from our sample with those for jellyfish galaxies, and suggest that the mechanism responsible for bending the radio tails is similar to the stripping of gas in jellyfish galaxies, although tailed radio galaxies are more concentrated in the centre of the phase space. Finally, we find that NATs and WATs have the same occurrence ratio in merging and relaxed clusters. However, their distribution in the phase-space is significantly different. We report an excess of NATs in the high-velocity and low-impact-radius phase-space region in merging clusters, and an excess of NATs in relaxed clusters in the low-velocity and low-impact-radius region.
Author(s): van der Jagt S.; Osinga E.; van Weeren R.J.; Miley G.K.; Roberts I.D.,Botteon A.; Ignesti A.
IVOA id: ivo://cds.vizier/j/a+a/699/a66

1782 Mira variables candidates with VVV survey

2026-05-06T00:00:00Z

Description: The properties of the Milky Way's nuclear stellar disc give crucial information on the epoch of bar formation. Mira variables are promising bright candidates to study the nuclear stellar disc, and through their period-age relation dissect its star formation history. We report on a sample of 1782 Mira variable candidates across the central 3*3 deg^2^ of the Galaxy using the multi-epoch infrared VISTA Variables in Via Lactea (VVV) survey. We describe the algorithms employed to select candidate variable stars and then model their light curves using periodogram and Gaussian process methods. By combining with WISE, 2MASS, and other archival photometry, we model the multiband light curves to refine the periods and inspect the amplitude variation between different photometric bands. The infrared brightness of the Mira variables means many are too bright and missed by VVV. However, our sample follows a well-defined selection function as expected from artificial star tests. The multiband photometry is modelled using stellar models with circumstellar dust that characterize the mass-loss rates. We demonstrate how ~>90 per cent of our sample is consistent with O-rich chemistry. Comparison to period-luminosity relations demonstrates that the bulk of the short period stars are situated at the Galactic Centre distance. Many of the longer period variables are very dusty, falling significantly under the O-rich Magellanic Cloud and solar neighbourhood period-luminosity relations and exhibit high mass-loss rates of ~2.5*10^-5^M_{sun}_yr^-1^. The period distribution appears consistent with the nuclear stellar disc forming ~> 8 Gyr ago, although it is not possible to disentangle the relative contributions of the nuclear stellar disc and the contaminating bulge.
Author(s): Sanders J.L.; Matsunaga N.; Kawata D.; Smith L.C.; Minniti D.; Lucas P.W.
IVOA id: ivo://cds.vizier/j/mnras/517/257