VO Fresh

AMS-02 All Particle Rates Catalog

2026-08-07T00:00:00Z

Description: The AMS02RATES database table records the incident rates for all particle species obtained with the Alpha Magnetic Spectrometer (AMS-02) experiment on the International Space Station (ISS), a cosmic ray particle detector installed in May 2011. The experiment consists of several components, which collectively measure particle species, energy, geomagnetic rigidity, or veto off-axis particles and high-energy photons. The experiment covers the energy range of ~0.1 GeV - ~2 TeV. AMS-02 is the result of a collaboration between MIT, the University of Hawaii, CERN, NASA, the U.S. Department of Energy, and ESA. It was launched on the Space Shuttle Endeavor (STS-134) on May 16, 2011 and was installed three days later at which time science operations commenced. Operations were interrupted by in-flight servicing of the cooling pumps for the silicon tracker: servicing took place between November 2019 and January 2020, after which science operations were restored. It is anticipated to continue operations for as long as the ISS itself remains functional. The rate at which all particle species are observed within a one-second time integration period is recorded for each interval, corrected for the livetime fraction. Each integration period contains the livetime value, observed rate, and the position of the AMS-02 instrument in latitude, longitude, and radius from the Earth's center in the Earth Centered Earth Fixed (ECEF) frame of reference. This database table was first ingested by the HEASARC in July 2026. The AMS-02 team in collaboration with the HEASARC developed the FITS file structure for these data which were created by the HEASARC from daily particle rate data provided by the AMS collaboration. The data and the database table are updated periodically to reflect additional data as they become available. This is a service provided by NASA HEASARC .
Author(s): HEASARC
IVOA id: ivo://nasa.heasarc/ams02rates

AMS-02 Spectral Results Catalog

2026-08-07T00:00:00Z

Description: The AMS02SPEC database table records the spectral results obtained with the Alpha Magnetic Spectrometer (AMS-02) experiment on the International Space Station (ISS), a cosmic ray particle detector installed in May 2011. The experiment consists of several components, which collectively measure particle species, energy, geomagnetic rigidity, or veto off-axis particles and high-energy photons. The experiment covers the energy range of ~0.1 GeV - ~2 TeV. AMS-02 is the result of a collaboration between MIT, the University of Hawaii, CERN, NASA, the U.S. Department of Energy, and ESA. It was launched on the Space Shuttle Endeavor (STS-134) on May 16, 2011 and was installed three days later at which time science operations commenced. Operations were interrupted by in-flight servicing of the cooling pumps for the silicon tracker: servicing took place between November 2019 and January 2020, after which science operations were restored. It is anticipated to continue operations for as long as the ISS itself remains functional. This database table was first ingested by the HEASARC in June 2026. The AMS-02 team in collaboration with the HEASARC developed the FITS file structure for these data. The data have been published in a series of papers (see bibliographic references) and archived in FITS format at the HEASARC. The data and the database table are updated periodically to reflect additional data as they becomes available. This is a service provided by NASA HEASARC .
Author(s): HEASARC
IVOA id: ivo://nasa.heasarc/ams02spec

Chandra Source Catalog Stacked Observation Detections, v2.1.1

2026-08-07T00:00:00Z

Description: The Chandra Source Catalog's Stacked Observation Detections Table (CSCSTACK) includes 493,236 detections (855,402 total entries consisting of detections plus photometric upper limits) based on 10,034 stacks of X-ray observations. Exploiting the unique resolution and very low background of Chandra data, the limiting sensitivity of the catalog is enhanced significantly by stacking (co-adding) multiple observations of the same field prior to source detection. To minimize the impact of the variation in the Chandra point spread function (PSF) with off-axis angles, source detection is constrained to run on stacks of observations that have telescope pointings that are co-located within 60 arcseconds and that were obtained using the same instrument (ACIS or HRC-I). Formally, the observations are matched using a tree clustering algorithm with complete linkage. This means that the pointing direction of every observation in the stack is co-aligned with the pointing direction of every other observation in the stack within 60 arcseconds. The stacked-observation level allows composite properties to be reported from the co-added observations for detections that would otherwise not be visible or have poor S/N in individual observations, while for higher S/N detections the per-observation properties facilitate analysis of variable sources. CSCSTACK is related to the <a href="/W3Browse/chandra/csc.html">Chandra Source Catalog (CSC)</a> catalog, which is the definitive catalog of X-ray sources detected by the Chandra X-ray Observatory. The CSC contains 407,806 unique compact and extended X-ray sources. By combining Chandra's sub-arcsecond on-axis spatial resolution and low instrumental background with consistent data processing, the CSC delivers a wide variety of uniformly calibrated properties and science ready data products for detected sources over four decades of flux. Each identified distinct X-ray source on the sky is represented in the catalog by one or more "stack detection" entries -- one for each stack in which the source has been detected -- and a single "master source" entry. The individual stack entries record all of the properties about a detection extracted from a single stack, as well as associated file-based data products, which are stack-specific. If a source is detected in one or more stacked-observations, photometric upper limits that are useful for temporal variability analyses are calculated for any overlapping stacked- and individual-observations in which the source is not detected. This database table was ingested by the HEASARC in July 2026 and is based on a download of the online version of the "Stacked Observation Detections" Table v. 2.1.1, at the CXC using the CLI. Refer to <a href="https://cxc.harvard.edu/csc/cli/">https://cxc.harvard.edu/csc/cli/</a> for details. This is a service provided by NASA HEASARC .
Author(s): Evans, Civano
IVOA id: ivo://nasa.heasarc/cscstack

Swift-XRT Living Point Source Catalog (LSXPS)

2026-08-07T00:00:00Z

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

SOFIA FORCAST Galactic Center Source Catalog

2026-08-06T00:00:00Z

Description: The SOFIA FORCAST Galactic Center Source Catalog is a catalog of sources at 25 and 37 um located within all of the regions observed with the SOFIA/FORCAST instrument in the inner ~200 pc of the Galaxy. The majority of the observations were obtained as part of the SOFIA Cycle 7 Galactic Center Legacy program survey, which was designed to complement the Spitzer/MIPS 24 um catalog in regions saturated in the MIPS observations. Due to the wide variety of source types captured by the observations at 25 and 37 um, the FORCAST source catalog is not limited to unresolved point sources, nor does it treat all sources as if they are point-like sources. The catalog includes all detectable sources in the regions, resulting in a catalog of 950 sources, including point sources, compact sources, and extended sources.
Author(s): Hankins et al.
IVOA id: ivo://irsa.ipac/sofia/catalog/sfgc/sfgc

VarWISE Pure Catalog

2026-08-06T00:00:00Z

Description: The Near-Earth Object Wide-field Infrared Explorer (NEOWISE) mission provides a decade of all-sky time-series data at 3.4 and 4.6 µm and an unprecedented opportunity for the discovery and characterization of variable objects. VarWISE catalogs infrared-variable objects discovered within the NEOWISE single-exposure data. VarWISE employs unique methodologies, including the spatial clustering of apparitions and the adoption of novel machine learning-based variable detection (VARnet) and classification (XGBoost) to identify and characterize significant variability. The catalog includes a prediction of variable object type and best-fit period values for each object, if its variations are cyclical, along with other calculated parameters to characterize the nature of the variability. The VarWISE Pure Catalog, containing only variables of highest confidence, has 457,080 objects, 49.81% of which are new discoveries; the VarWISE Extended Catalog, containing all sources, has 1,918,082 objects, 82.02% of which are new.
Author(s): Paz et al.
IVOA id: ivo://irsa.ipac/wise/catalog/varwise/varwisepure

VarWISE Extended Catalog

2026-08-06T00:00:00Z

Description: The Near-Earth Object Wide-field Infrared Explorer (NEOWISE) mission provides a decade of all-sky time-series data at 3.4 and 4.6 µm and an unprecedented opportunity for the discovery and characterization of variable objects. VarWISE catalogs infrared-variable objects discovered within the NEOWISE single-exposure data. VarWISE employs unique methodologies, including the spatial clustering of apparitions and the adoption of novel machine learning-based variable detection (VARnet) and classification (XGBoost) to identify and characterize significant variability. The catalog includes a prediction of variable object type and best-fit period values for each object, if its variations are cyclical, along with other calculated parameters to characterize the nature of the variability. The VarWISE Pure Catalog, containing only variables of highest confidence, has 457,080 objects, 49.81% of which are new discoveries; the VarWISE Extended Catalog, containing all sources, has 1,918,082 objects, 82.02% of which are new.
Author(s): Paz et al.
IVOA id: ivo://irsa.ipac/wise/catalog/varwise/varwiseext

The SPHEREx Target List of Ice Sources (SPLICES)

2026-08-06T00:00:00Z

Description: The SPHEREx List of Ice Sources is a compilation of nearly nine million spatially isolated, IR-bright point sources likely to exhibit ice absorption features when observed by NASA's SPHEREx mission. Because of its well-defined and broad-based selection, based on bright all-sky broadband photometry, SPLICES targets are accessible to observatories all over the Earth for followup to characterize e.g., YSOs, protoplanetary disks, and other identified objects (variable sources, carbon stars) in concert with the multi-epoch SPHEREx 0.75-5.0 micron spectrophotometry.
Author(s): Ashby et al.
IVOA id: ivo://irsa.ipac/spherex/catalog/splices

Database of Molecules in Space

2026-08-06T00:00:00Z

Description: SpaceMol is a searchable database of molecular transitions detected in space. It includes spectroscopic data from three Herschel instruments (HIFI, SPIRE, and PACS) and two SOFIA instruments (EXES and GREAT). Together these instruments span a wide wavelength range, 5-670 um, covering MIR, FIR, and sub-mm wavelengths, and resolving powers of 1e3-1e7 that enable studies of a broad range of environments and phenomena: galaxies, dense and diffuse gas, supernova remnants, protostars, protoplanetary disks, debris disks, and the solar system; shocks, dynamics, structure, and chemistry. This is the first data drop of SpaceMol, containing data from the SOFIA/EXES, Herschel/HIFI and SPIRE instruments only. The next data drop is anticipated for Spring 2027.
Author(s): Rangwala et al.
IVOA id: ivo://irsa.ipac/spacemol/catalog/spacemol

Herschel PACS Point Source Catalogs 2: High Reliability 100 micron Catalog

2026-08-06T00:00:00Z

Description: The HPPSC2 project revisited all the photometric observations obtained by the PACS instrument on-board of the Herschel space observatory, using more advanced techniques than before, including machine learning techniques. HPPSC2 includes a high-reliability and a rejected source catalogue for each PACS passband, i.e., at 70, 100, and 160 um. With the high-reliability catalogue, completeness in all bands is improved, especially at 70 um. At the same time, while the number of high-reliability detections decreased, the number of sources matching with existing catalogues increased, suggesting that the purity is also higher than before.
Author(s): Marton et al.
IVOA id: ivo://irsa.ipac/herschel/catalog/hppsc2/hppsc2_bl

Herschel PACS Point Source Catalogs 2: Rejected Source 100 micron Catalog

2026-08-06T00:00:00Z

Description: The HPPSC2 project revisited all the photometric observations obtained by the PACS instrument on-board of the Herschel space observatory, using more advanced techniques than before, including machine learning techniques. HPPSC2 includes a high-reliability and a rejected source catalogue for each PACS passband, i.e., at 70, 100, and 160 um. With the high-reliability catalogue, completeness in all bands is improved, especially at 70 um. At the same time, while the number of high-reliability detections decreased, the number of sources matching with existing catalogues increased, suggesting that the purity is also higher than before.
Author(s): Marton et al.
IVOA id: ivo://irsa.ipac/herschel/catalog/hppsc2/hppsc2_blrej

Herschel PACS Point Source Catalogs 2: High Reliability 70 micron Catalog

2026-08-06T00:00:00Z

Description: The HPPSC2 project revisited all the photometric observations obtained by the PACS instrument on-board of the Herschel space observatory, using more advanced techniques than before, including machine learning techniques. HPPSC2 includes a high-reliability and a rejected source catalogue for each PACS passband, i.e., at 70, 100, and 160 um. With the high-reliability catalogue, completeness in all bands is improved, especially at 70 um. At the same time, while the number of high-reliability detections decreased, the number of sources matching with existing catalogues increased, suggesting that the purity is also higher than before.
Author(s): Marton et al.
IVOA id: ivo://irsa.ipac/herschel/catalog/hppsc2/hppsc2_bs

Herschel PACS Point Source Catalogs 2: Rejected Source 70 micron Catalog

2026-08-06T00:00:00Z

Description: The HPPSC2 project revisited all the photometric observations obtained by the PACS instrument on-board of the Herschel space observatory, using more advanced techniques than before, including machine learning techniques. HPPSC2 includes a high-reliability and a rejected source catalogue for each PACS passband, i.e., at 70, 100, and 160 um. With the high-reliability catalogue, completeness in all bands is improved, especially at 70 um. At the same time, while the number of high-reliability detections decreased, the number of sources matching with existing catalogues increased, suggesting that the purity is also higher than before.
Author(s): Marton et al.
IVOA id: ivo://irsa.ipac/herschel/catalog/hppsc2/hppsc2_bsrej

Herschel PACS Point Source Catalogs 2: High Reliability 160 micron Catalog

2026-08-06T00:00:00Z

Description: The HPPSC2 project revisited all the photometric observations obtained by the PACS instrument on-board of the Herschel space observatory, using more advanced techniques than before, including machine learning techniques. HPPSC2 includes a high-reliability and a rejected source catalogue for each PACS passband, i.e., at 70, 100, and 160 um. With the high-reliability catalogue, completeness in all bands is improved, especially at 70 um. At the same time, while the number of high-reliability detections decreased, the number of sources matching with existing catalogues increased, suggesting that the purity is also higher than before.
Author(s): Marton et al.
IVOA id: ivo://irsa.ipac/herschel/catalog/hppsc2/hppsc2_r

Herschel PACS Point Source Catalogs 2: Rejected Source 160 micron Catalog

2026-08-06T00:00:00Z

Description: The HPPSC2 project revisited all the photometric observations obtained by the PACS instrument on-board of the Herschel space observatory, using more advanced techniques than before, including machine learning techniques. HPPSC2 includes a high-reliability and a rejected source catalogue for each PACS passband, i.e., at 70, 100, and 160 um. With the high-reliability catalogue, completeness in all bands is improved, especially at 70 um. At the same time, while the number of high-reliability detections decreased, the number of sources matching with existing catalogues increased, suggesting that the purity is also higher than before.
Author(s): Marton et al.
IVOA id: ivo://irsa.ipac/herschel/catalog/hppsc2/hppsc2_rrej

DustPedia: A Definitive Study of Cosmic Dust in the Local Universe

2026-08-06T00:00:00Z

Description: The DustPedia project capitalizes on the legacy of the Herschel Space Observatory, using cutting-edge modelling techniques to study dust in the 875 DustPedia galaxies - representing the vast majority of extended galaxies within 3000 km/s that were observed by Herschel. This work requires a database of multiwavelength imagery and photometry that greatly exceeds the scope (in terms of wavelength coverage and number of galaxies) of any previous local-Universe survey.
Author(s): Clark et al.
IVOA id: ivo://irsa.ipac/herschel/images/dustpedia

An Improved Atlas of Full-Scan Spectra from ISO/SWS

2026-08-06T00:00:00Z

Description: This dataset contains an updated atlas of spectra from the Short-Wavelength Spectrometer (SWS) on the Infrared Space Observatory (ISO), which took spectra from 2.4 to 45 um. The updated atlas (Mizuno et al. 2025) contains 1035 spectra that were reprocessed starting from the "pws" files from the original atlas of Sloan et al. (2003).
Author(s): Mizuno et al.
IVOA id: ivo://irsa.ipac/iso/spectra/sws_atlas

Optical spectroscopy of WISPIT 2

2026-08-05T13:46:35Z

Description: WISPIT 2 is a young pre-main-sequence star hosting a multi-ringed transition disk and two directly imaged accreting protoplanets, the closest known analogue to PDS 70, yet its central star has no published optical spectrum. Population-synthesis models predict that stellar accretion can be strongly suppressed once two or more giant planets have formed, so characterising the atmospheric and accretion properties of such hosts is essential. We present the first optical spectrum of WISPIT 2 and use it to derive the host atmospheric parameters, test its youth spectroscopically, and constrain its stellar accretion state relative to PDS 70 and to the embedded planets. We analysed low-resolution HFOSC spectra (R about 1200 for Grism 7 and R about 2200 for Grism 8) from the 2-m Himalayan Chandra Telescope with iSpec, validating the pipeline at HFOSC resolution against Gaia FGK Benchmark Stars and K-type pre-main-sequence templates from the public Manara et al. library. The Halpha residual filling was measured relative to synthetic photospheric profiles and compared with the chromospheric-noise level of Manara et al. (2013A&A...551A.107M, Cat. J/A+A/551/A107). Halpha remains in net absorption but is partially filled in by emission. The weak residual filling, at 1.5-2.0 sigma, lies about 1dex below the chromospheric-noise level, consistent with chromospheric emission and no detectable accretion. We place a 95 percent upper limit of dM_acc_/dt<3.6x10^-11^M_{sun}_/yr, below even the lowest epoch of PDS 70 monitoring and implying a host-to-planet ratio (dM_star/dt)/(dM_2b_/dt)<18. We also measure Teff= 4551+/-150K and a first, low-resolution, model-dependent global metallicity [M/H]=-0.17+/- 0.16; the surface gravity and Li I equivalent width support the pre-main-sequence nature of the host. Both known double-protoplanet hosts, PDS 70 and WISPIT 2, therefore appear to show strongly suppressed or undetectable stellar accretion. Larger spectroscopic samples are needed to test whether this is common in multi-protoplanet transition disks.
Author(s): Swastik C.; Bestha M.; Sonith L.S.; Facchini S.; Sivarani T.; Banyal R.K.,Wahhaj Z.; Choudhary A.; Gopinathan M.; Saraf P.; Mallik A.; Navaneeth M.P.,Biswas S.; Khushbu K.
IVOA id: ivo://cds.vizier/j/a+a/712/l13

Abundances of 17000 M dwarfs in SDSS-V

2026-08-05T13:30:53Z

Description: The cool temperatures of M dwarf atmospheres enable complex molecular chemistry, making robust characterization of M dwarf compositions a long-standing challenge. Recent modifications to spectral synthesis pipelines have enabled more accurate modeling of M dwarf atmospheres, but these methods are too slow for characterizing more than a handful of stars at a time. Data-driven methods such as The Cannon are viable alternatives, and can harness the information content of many M dwarfs from large spectroscopic surveys. Here, we train The Cannon on M dwarfs with FGK binary companions from the Sloan Digital Sky Survey-V/Milky Way Mapper (SDSS-V/MWM), with spectra from the Apache Point Observatory Galactic Evolution Experiment. The FGK-M pairs are assumed to be chemically homogeneous and span -0.56<[Fe/H]<0.31dex. The resulting model is capable of inferring M dwarf Teff and elemental abundances for Fe, Mg, Al, Si, C, N, O, Ca, Ti, Cr, and Ni with median uncertainties of 13 K and 0.018-0.029 dex, respectively. We test the model by verifying that it reproduces the reported abundance values of M dwarfs in open clusters and benchmark M dwarf data sets, as well as the expected metallicity trends from stellar evolution. We apply the model to 16,590 M dwarfs in SDSS-V/MWM and provide their detailed abundances in our accompanying catalog.
Author(s): Behmard A.; Ness M.K.; Casey A.R.; Angus R.; Cunha K.; Souto D.; Lu Y.,Johnson J.A.
IVOA id: ivo://cds.vizier/j/apj/982/13

Late-type gal. ultra-deep HI radial profiles

2026-08-05T08:43:11Z

Description: Galaxy discs have a finite extent, yet how and where their neutral atomic hydrogen (HI) components end is not fully understood. The existence of a break in the HI disc at column densities of ~10^+19^cm^-2^ has been debated since early 21-cm observations of the spiral galaxy NGC 3198. We present the HI radial profiles of 16 star-forming, late-type galaxies from the MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters (MHONGOOSE) survey spanning a range of HI mass from 10^+7^M_{sun}_ to 10^+10^M_{sun}_. We probed via spectral stacking their HI discs down to inclination-corrected column densities of a few times 10^+17^cm^-2^ at kpc resolution. The HI radial profiles of high-mass (MHI>10^+9^M_{sun}_) galaxies are characterised by a inner plateau, followed by a knee at column densities of ~5x10^+20^cm^-2^, but no edges are unambiguously identified. The HI radial profiles of low-mass (MHI<10^+9^M_{sun}-) galaxies shows a steeper decline and also no edges. We found that the profiles are self-similar when normalised to the radius at which a mass surface density of 0.01M_{sun}_/pc^2^ is reached, in agreement with recent literature results, but we also found a possible correlation between the normalisation radius and the environment, suggesting that environment contributes to the shaping of the HI distribution in galaxies. The emerging picture is that the diverse morphology of the HI radial profiles is difficult to interpret, and future studies with a larger sample are necessary for quantifying the contribution of internal and external processes acting at different levels for different galaxies.
Author(s): Veronese S.; de Blok W.J.G.; Brinks E.; Kleiner D.; Kurapati S.; Healy J.,Maccagni F.M.
IVOA id: ivo://cds.vizier/j/a+a/712/a74

CO-dark gas in compact emission-line galaxies

2026-08-05T08:41:49Z

Description: Green Pea and Blueberry galaxies are compact, low-metallicity starbursts that provide nearby analogs of high-redshift star-forming systems. We investigate whether their weak CO emission reflects genuinely small molecular reservoirs or CO-dark gas where independent tracers are available. We compiled 60 strong [OIII]{lambda}5007 compact emission-line galaxies with partially overlapping gas-tracer coverage: ^12^CO(1-0) observations from the Delingha 13.7m telescope, HI 21cm data from Arecibo, GBT, and FAST (ten detections and 41 upper limits), and Herschel/PACS [CII] {lambda}158um data (five detections and four upper limits after excluding merger systems). Quantitative conclusions are drawn only from detected or physically constraining subsets. Molecular masses were estimated using a metallicity-dependent CO-to-H_2_ conversion factor and the [CII]-to-H_2_ calibration for low-metallicity dwarf galaxies. Two CO upper limits are deep enough to constrain the expected molecular reservoir. We also removed major mergers and examined the large-scale environment using the SDSS DR7 VoidFinder catalog. For the five [CII]-detected sources, we find M_H2_^[CII]^~10^9^.0-10^9.7^M_{sun}_ and a median molecular gas depletion time of {tau}_dep,H2_~0.16Gyr, shorter than the ~1Gyr typical of main-sequence galaxies. HI-detected sources have a median atomic depletion time of {tau}_dep,H_~2.6Gyr. The detected subsets show high gas fractions and short depletion times consistent with rapid gas cycling, but the [CII] result remains limited by small-number statistics. About 39% of the volume-matched sample lies in cosmic voids. CO alone misses a substantial fraction of the star-forming fuel in these low-metallicity starbursts. Combined HI, [CII], and deep CO constraints are needed to characterize their interstellar medium and CO-dark molecular component.
Author(s): Liu S.; Yin X.; Luo A.-L.; Zhang W.; Yan P.; Bo Q.
IVOA id: ivo://cds.vizier/j/a+a/712/a47

VESTIGE XXI. HII regions in perturbed galaxies

2026-08-05T08:25:43Z

Description: We use narrow-band Halpha+[NII] imaging data gathered during the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE), a blind survey of the Virgo cluster carried out with MegaCam at the Canada-French-Hawaii telescope (CFHT), to identify [HII] regions in 385 galaxies showing ionised gas emission. After excluding objects where the emission is not associated to star formation and edge-on systems, we identify 76645 [HII] regions in 322 star-forming galaxies and study their physical properties for those above the completeness limit of the survey (L(Halpha)>=10^37^erg/s, 34358 regions). The present work is focused on perturbed cluster galaxies, identified as those having a reduced amount of atomic hydrogen when compared to similar objects in the field. We derive composite luminosity functions, diameter and electron density distributions, and several scaling relations, and compare them to those already derived for gas-rich, unperturbed systems identified during the VESTIGE survey. The analysis shows that the statistical and physical properties of HI gas-deficient cluster galaxies are different from those of unperturbed systems, with perturbed objects having a steeper faint-end slope and a brighter characteristic Halpha luminosity than gas-rich galaxies. The difference in the two distributions comes principally from the outer disc (outside the effective radius). Perturbed and unperturbed systems share a similar HII size distribution, while gas-poor objects hosts higher electron density regions than HI-rich systems. The analysis of the scaling relations indicates that perturbed objects have, on average, a lower number of HII regions per unit stellar mass and disc surface than unperturbed systems, with differences increasing with the HI-deficiency parameter, principally in the outer disc where HII regions are less present in gas-poor systems. This systematic difference is also observed in the Halpha luminosity of the first ranked and first three ranked HII regions, which is reduced in HI-deficient systems with respect to gas-rich objects. All these differences can be explained in the framework of galaxy evolution in rich environments, where their hydrodynamic interaction with the surrounding intracluster medium (ram pressure) removes the gas outside-in quenching the star formation activity in the outer disc once the atomic hydrogen is removed.
Author(s): Boselli A.; Fossati M.; Roehlly Y.; Boquien M.; Braine J.; Cote P.,Cuillandre J.C.; Epinat B.; Ferrarese L.; Gwyn S.; Hensler G.
IVOA id: ivo://cds.vizier/j/a+a/712/a46

KPF RVs for TOI-2374: Planet in Neptunian ridge

2026-08-05T00:00:00Z

Description: The "Neptunian ridge" is a recently identified peak in the frequency of planets with sizes between that of Neptune and Saturn orbiting their host stars with periods between 3 and 6days. These planets may have formed similarly to their larger, hot Jupiter counterparts in the "3 day pileup," through a dynamically excited migration pathway. The distribution of stellar obliquities in hot Neptune systems may therefore provide a vital clue as to their origin. We report a new stellar obliquity measurement for TOI-2374b, a planet in the Neptunian ridge (P=4.31days, R_p_=7.5R_{Earth}_). We observed a spectroscopic transit of TOI-2374b with the Keck Planet Finder, detecting the Rossiter-McLaughlin (RM) anomaly with an amplitude of 3m/s, and measured a sky-projected obliquity of {lambda}=81{deg}_-22{deg}_^+23{deg}^, indicating an orbit significantly misaligned with the spin axis of its host star. A reloaded RM analysis of the cross-correlation functions confirms this misalignment, measuring {lambda}=65{deg}_-24{deg}_^+32{deg}^. Additionally, we measured a stellar rotation period of P_rot_=26.4_-0.8_^+0.9^days with photometry from the Tierras observatory, allowing us to deduce the three-dimensional stellar obliquity of {psi}=85.9{deg}_-9.2{deg}_^+8.6{deg}^. TOI-2374b joins a growing number of hot Neptunes on polar orbits. The high frequency of misaligned orbits for Neptunian ridge and desert planets, compared with their longer period counterparts, is reminiscent of patterns seen for the giant planets and may suggest a similar formation mechanism.
Author(s): Yee S.W.; Tamburo P.; Stefansson G.; Garcia-Mejia J.; Charbonneau D.,Barkaoui K.; Collins K.A.; Schwarz R.P.; Narita N.; Fukui A.; Howard A.W.,Isaacson H.; Fulton B.J.; Dai F.
IVOA id: ivo://cds.vizier/j/aj/170/275

Validation of Gaia EDR3 parallaxes

2026-08-04T14:26:04Z

Description: We construct from Gaia eDR3 an extensive catalogue of spatially resolved binary stars within ~1kpc of the Sun, with projected separations ranging from a few AU to 1pc. We estimate the probability that each pair is a chance alignment empirically, using the Gaia catalogue itself to calculate the rate of chance alignments as a function of observables. The catalogue contains 1.3 (1.1) million binaries with >90% (>99%) probability of being bound, including 16000 white dwarf-main-sequence (WD+MS) binaries and 1400 WD+WD binaries. We make the full catalogue publicly available, as well as the queries and code to produce it. We then use this sample to calibrate the published Gaia DR3 parallax uncertainties, making use of the binary components' near-identical parallaxes. We show that these uncertainties are generally reliable for faint stars (G>=18), but are underestimated significantly for brighter stars. The underestimates are generally <=30% for isolated sources with well-behaved astrometry, but are larger (up to ~80%) for apparently well-behaved sources with a companion within <=4", and much larger for sources with poor astrometric fits. We provide an empirical fitting function to inflate published {sigma}p values for isolated sources. The public catalogue offers wide ranging follow-up opportunities: from calibrating spectroscopic surveys, to precisely constraining ages of field stars, to the masses and the initial-final mass relation of WDs, to dynamically probing the Galactic tidal field.
Author(s): El-Badry K.; Rix H.-W.; Heintz T.M.
IVOA id: ivo://cds.vizier/j/mnras/506/2269

VLBI images of UGC 2369S

2026-08-04T08:10:04Z

Description: UGC 2369S is a luminous infrared galaxy (LIRG) undergoing a late-stage merger in a triple system, where the heavily obscured northern core is suspected to host an active galactic nucleus (AGN). However, severe dust and gas obscuration makes definitive confirmation challenging. We aim to provide direct observational evidence for the buried AGN through high-resolution radio imaging, while investigating the AGN accretion and feedback properties within this merger-driven gas-rich environment. We analyzed archival European VLBI Network (1.6GHz) and Very Long Baseline Array (1.7 and 5GHz) data of UGC 2369S. Through high-resolution imaging and visibility-domain Gaussian modeling, we characterized the morphology and intensity of its milliarcsecond-scale radio emission. A compact radio component is detected in the northern core, exhibiting high brightness temperatures (Tb>10^7^K) and a flat radio spectrum (alpha=-0.45), which confirms the presence of an obscured AGN. The sub-Eddington accretion rate ({lambda}_Edd_~2.7x10^-4^) indicates that it falls within the radiatively inefficient accretion flow state. We provide direct imaging evidence for an AGN in the northern core of UGC 2369S, revealing a deeply buried, jet-emitting low-luminosity AGN enshrouded by a Compton-thick gas cocoon. This demonstrates that VLBI is a uniquely effective tool for disentangling nuclear accretion and feedback processes within the heavily obscured environments of multiple-merger systems.
Author(s): Xu W.; Frey S.; Cui L.; Gabanyi K.E.
IVOA id: ivo://cds.vizier/j/a+a/712/a67

A catalogue of TeV pulsar environments

2026-08-04T08:08:46Z

Description: Pulsars and their environments represent a major class of Galactic gamma-ray sources. Their complex evolution, shaped by the interactions of the pulsar outflow with both the supernova remnant (SNR) and the surrounding interstellar medium (ISM), produces diverse morphological and spectral characteristics observable from radio to PeV energies. This work aims to collect and homogenize data from all major operating TeV observatories, presenting the first comprehensive catalogue of TeV gamma-ray properties of pulsar environments, and facilitating systematic studies of the evolution of PWNe and pulsar halos. The catalogue is created from information regarding all gamma-ray sources that have been classified as pulsar-associated sources in published results from H.E.S.S., MAGIC, VERITAS, HAWC, and LHAASO. For each source, the observed gamma-ray properties are cross-matched with pulsar properties from the ATNF catalogue and Fermi-LAT pulsar catalogue. This information is then used to predict the surface brightness for powerful pulsars around which no PWN has been detected yet. The final catalogue comprises all currently known TeV sources associated with pulsars, as seen by different instruments, spanning all evolutionary stages. The sample consists of 128 gamma-ray sources, connected to 66 different pulsars. It reflects that the TeV-detected population is dominated by young and energetic pulsars located near the Galactic plane, but includes a growing number of middle-aged systems detected as extended halos. Only a weak correlation is found between TeV luminosity and pulsar characteristic age, indicating that TeV evolution is driven by environmental and transport effects rather than by spin-down age alone. Additionally, 5 pulsars which should host a PWN detectable by CTAO are identified as prime targets for future observation to improve our understanding of properties inhibiting the formation of a TeV nebula. This publicly available catalogue provides a uniform foundation for future population studies and for constraining models of particle transport and energy losses in pulsar environments.
Author(s): Wach T.; Linden T.; Mitchell A.M.W.; Spencer S.T.
IVOA id: ivo://cds.vizier/j/a+a/712/a60

Galaxy groups within voids

2026-08-04T08:03:49Z

Description: Despite cosmic voids being vast and almost empty, galaxy aggregations do exist within them, although they are much sparser than in denser regions like walls, filaments and clusters. The internal matter distribution within voids might have an impact on the properties and evolution of void galaxies. In this work, we aim to identify and characterise a sample of galaxy groups within voids in the local Universe (z<0.08), taking into account the peculiarities of these vast and empty structures. The void galaxies used in this study are selected from a well-defined void galaxy sample, from which the parent sample of the Calar Alto Void Integral-field Treasury surveY (CAVITY) legacy project was drawn. To identify galaxy groups, we applied a fiends-of-friends (FoF) like group finder algorithm to the selected sample, ensuring a certain degree of gravitational binding among group members. The same algorithm has been applied to identify a control sample of groups not in clusters nor voids, referred as NCNV groups. The catalogue of groups consists on 1367 physically bound groups, with a total of 3040 galaxies, plus 14672 galaxy singlets. Most of the galaxies in voids are singlets (59%), in contrast, most of the NCNV galaxies in the control sample are in groups (60%). To consider the dynamical stage of the groups we used the parameters harmonic radius (R_H_), radial velocity dispersion (sigma_v_r^2^), dimensionless crossing time (H0tc), and group virial mass (Mvir). We also used the total optical (r-band) luminosity, L_r, to estimate the mass-to-light ratio (M/L) of the groups. We studied the relations of void properties and these parameters with the group richness. Galaxy groups can be found in any void in the local Universe, with no dependency of group richness on the density of voids. The densest groups in the studied sample of voids are composed of six galaxies, therefore, voids generally contain small groups, in comparison to denser structures such as filaments, walls, and galaxy clusters. Galaxy groups within voids are typically loose groups, in an early stage of their evolution.
Author(s): Argudo-Fernandez M.; Torres-Rios G.; Vasquez-Bustos P.; Verley S.; Perez I.,Duarte Puertas S.; Jimenez A.; Garcia-Benito R.; Zurita A.,Alcazar-Laynez M.; Bidaran B.; Conrado A.; Espada D.; Florido E.,Gonzalez Delgado R.; Hernandez-Sanchez M.; del Moral-Castro I.; Roman J.,Sanchez-Menguiano L.; Subramanian S.; Villalba-Gonzalez P.
IVOA id: ivo://cds.vizier/j/a+a/712/a55

The Subaru Deep Field (SDF) v1

2026-08-04T06:38:44Z

Description: The Subaru Deep Field (SDF) project is an ultra deep survey which aims to explore the universe as deep as possible, and as early as possible with Subaru in both visible and near-infrared. In the SDF project, we attempted to take the deepest imaging data among those having a single Suprime-Cam's FOV. The survey goes as deep as the HDF, while it can cover far wider area than the HDF. We believe that this SDF project will provide our community the pride to say that "Subaru could expand our knowledge to such a deep universe." The project guarantees both quality and quantity of the data as well as a plenty of fascinate scientific goals. Although the observational approach is conservative that widespread popularity in current studies of distant universe, the proposed survey based on a large amount of the observational time of an 8m telescope would be a milestone of these deep surveys. It is not too much to say that this project is the "Power Play" of Subaru and the project should be carried out as the observatory key project. The major goal of this survey project is to search and study for the highest redshift (z>6) galaxy population. In this project, we will carry out a couple of different approaches to search them. One is to detect continuum dropout galaxies using deep multi broad-band imaging and the other is the deep narrow-band imaging for a high-z population as having only the Lyα emission feature. This is the first systematic survey to carry on the combination of these two attempts. In addition, this proposed survey will produce our own large sample for galaxies at z=4-6 as well as the nearby (z<1.5) galaxy sample down to M *+3. Whole the sample and following careful reduction enable us to quantify the galaxy evolution from z=0 to z=5 with derived fundamental tools such as luminosity function and correlation function. For these scientific goals, we propose as the first step of our survey project to take a deep imaging with Suprime-Cam on B, V, RC, i', z' bands as well as two narrow-bands. The subsequent step is the following-up spectroscopy observation with FOCAS for detected dropouts, Lyα emitters and so on. The NIR imaging and follow-up spectroscopy would definitely make the field more valuable. This optical imaging data of a single Suprime-Cam' FOV (34' x 27') will be the deepest of all the previous/forthcoming data taken with Suprime-Cam which is an unique instrument of Subaru.
Author(s): SDF project team
IVOA id: ivo://jvo/subaru/sdf/v1

Gaia RVS stellar labels and GSE Chemodynamics

2026-08-03T09:33:41Z

Description: We present a comprehensive data-driven spectroscopic analysis of 357415 red giant stars using Gaia DR3 Radial Velocity Spectrometer (RVS) spectra (8460-8700 Angstrom; R~11500), aimed at deriving homogeneous stellar parameters and elemental abundances (collectively referred to as stellar labels). We employ The Cannon (Ness et al., 2015ApJ...808...16N, Cat. J/ApJ/808/16; Casey et al., arXiv:1603.03040), a generative model based on 2747 giants in common with GALactic Archaeology with HERMES (GALAH) DR4, adopting GALAH labels (R~28000) for training. The resulting model predicts 11 stellar labels for RVS giants: effective temperature (Teff), surface gravity (logg), projected rotational velocity (vsini), and abundances of [Fe/H], [Ca/Fe], [Si/Fe], [Ni/Fe], [Ti/Fe], as well as the neutron-capture elements [Zr/Fe], [Ce/Fe], and [Nd/Fe]. Building on these results, we develop a probabilistic framework to chemically identify debris from the Gaia- Sausage-Enceladus (GSE) accretion event. A logistic regression classifier, optimised via Markov chain Monte Carlo sampling and trained on a small reference sample of GSE members and comparison stars, identifies stars with high GSE membership probabilities based solely on their chemical abundances, with the resulting candidates exhibiting distinctive abundance-ratio patterns, including [Ca/Ti], [Ti/Ce], and [Nd/Zr]. Applying independent kinematic constraints yields a robust sample of GSE candidates, demonstrating that the characteristic chemical signatures remain consistent after applying these constraints. This work demonstrates the potential of data-driven analysis techniques to extract detailed chemical information from medium-resolution spectra and establishes a framework for tracing Galactic accretion events using chemical abundances.
Author(s): Das P.B.; Zucker D.B.; Mura-Guzman A.; Borsato N.W.; De Silva G.M.,Buder S.; Feuillet D.; Nordlander T.; Ness M.; Martell S.L.; Kos J.,Bland-Hawthorn J.; Freeman K.C.; Casey A.R.; Lewis G.F.; Stello D.,de Grijs R.; GALAH Collaboration
IVOA id: ivo://cds.vizier/j/mnras/550/g1142

32 naked-eye stars seismic characterisation

2026-08-03T08:47:24Z

Description: The Transiting Exoplanet Survey Satellite (TESS) is conducting a nearly full-sky survey, enabling the photometric characterisation of millions of stars. The forthcoming PLAnetary Transits and Oscillations of stars mission (PLATO) will provide long-duration, high-precision photometry of tens of thousands of bright stars to be characterised through asteroseismology. The TESS Luminaries Sample is a catalogue of 196 bright naked-eye (V<6) main-sequence (MS) and sub-giant (SG) stars exhibiting solar-like oscillations. Among them, the subset located within the PLATO Long-duration Observation Phase (LOP) fields constitutes an exceptional set of targets that will be observable by PLATO from the earliest phases of the mission, making them ideal calibrators during commissioning and the first months of science operations. This paper aims to provide an in-depth asteroseismic characterisation of 32 Luminaries stars that fall within the PLATO LOP fields of view. Individual mode parameters were extracted using three independent seismic pipelines, one of which was similar to the algorithms used in the official PLATO pipeline. The Peirce criterion and a Z-score were applied to identify the optimal combination of data calibration, observing cadence, and fitting pipeline for each star. We analyse 32 MS and SG stars up to TESS Sector 88, with individual mode frequencies derived for the first time for 26 of them. For all stars, we derived large and small separations, the asymptotic phase term epsilon, radial mode amplitudes, and mean linewidths per order. Comparisons with previous Kepler observations reveal consistent trends in the seismic parameters, confirming the robustness of our analysis based on TESS data. In sub-giants, mixed-mode identification differs in the three pipelines, revealing extraction inconsistencies requiring longer datasets to improve our mode identifications. These results demonstrate the capability of TESS to deliver high-quality asteroseismic observations for MS and SG stars. The Luminaries stars located in the PLATO LOP fields constitute a unique sample that will play a crucial role in validating, calibrating, and optimising PLATO's seismic performance from the earliest stages of the mission.
Author(s): Panetier E.; Hookway G.T.; Corsaro E.; Breton S.N.; Garcia R.A.; Liagre B.,Lund M.N.; Nielsen M.B.; Palakkatharappil D.B.; Debacker L.; Gosmain J.,Chaumard M.; Chontos A.; Grundahl F.; Mathur S.; Santos A.R.G.
IVOA id: ivo://cds.vizier/j/a+a/712/a33

KQ Pup radial velocities

2026-08-03T08:46:01Z

Description: The majority of massive stars are part of binary systems and may interact with their companions during their evolution. This has important consequences for systems in which one star evolves into a red supergiant (RSG). However, not many RSGs have been found in binary systems, and only a few have constrained orbital parameters. We aim to better characterize and constrain the properties of some of the known RSGs in binaries. We were inspired to do so by recent observations where these RSGs transitioned to an earlier spectral type, likely following a major interaction event with their companions. We searched the available TESS photometry for eclipsing companions. We focused on the best candidate, the VV Cephei-type RSG binary KQ Pup, which is made up of an RSG, KQ Pup A, and a B-type companion, KQ Pup B and has an orbital period of 26 years. For this system, we have enough data to constrain the system properties. We used archival photometry and UV spectroscopy along with newly acquired optical spectra and interferometric data from VLTI-GRAVITY. Using TESS light curves, we discovered eclipses with a period of 17.2596d associated with KQ Pup B, making it a binary. We refer to the two components as KQ Pup Ba and Bb. Meanwhile, the detection of the hydrogen Br{gamma} line with VLTI-GRAVITY enabled us to track the orbital motion of the Ba+Bb pair relative to A and thus determine the astrometric orbit of A+B. The dynamical masses agree with independent estimates from asteroseismology and evolutionary models. The results give a mass of ~10M_{sun}_ for the RSG KQ Pup A and ~14M_{sun}_ for the sum of the hot components Ba+Bb. The observed properties of the system are compatible with a coeval hierarchical triple star, where we constrained the mass of KQ Pup Bb to be >~1.2M_{sun}_. We determined an orbital parallax of {pi}=1.24^+0.05^_-0.04_mas based on the detailed orbital model of the system, which is the first such parallax measurement for an RSG, and the value is consistent with Gaia DR3. KQ Pup represents a unique demonstration of mass transfer in a wide, eccentric RSG system. The variability of Balmer emission lines and the detection of Br{gamma} are a strong signature of accretion to the Ba+Bb pair near periastron. With the RSG filling its Roche lobe by only ~70% at periastron ({phi}_A+B_~0), the mass transfer is instead driven by accretion from its extended atmosphere via the wind Roche-lobe overflow. The accretion disk is formed already by {phi}_A+B_~0.95, while TESS light curves also begin to show a signature of occultations by the circumbinary disk, similar to young stellar objects. Through apastron ({phi}_A+B_~0.5), Balmer emissions weaken and indicate a decaying disk. Overall, using TESS, we discovered that several previously assumed RSG binaries host eclipsing inner systems, corresponding to ~10% of all known Galactic RSG binaries. This suggests that many of the other RSG binaries may also be hierarchical triples.
Author(s): Jadlovsky D.; Molnar L.; Ercolino A.; Bernini-Peron M.; Merand A.,Krticka J.; Wang L.; Adam R.Z.; Baade D.; Bayo A.; Gonzalez-Tora G.,Granzer T.; Henry G/W/; Janik J.; Kolar J.; Kravchenko K.; Langer N.,Oskinova L.M.; Pauli D.; Ramachandran V.; Rubio A.C.; Sander A.A.C.,Strassmeier K.G.; Weber M.; Wittkowski M.; Brahm R.; Schaffenroth V.,Vanzi L.; Skarka M.
IVOA id: ivo://cds.vizier/j/a+a/712/a30

MaNGA DynPop. VII. Circular velocity curves

2026-08-03T07:26:34Z

Description: We derive circular velocity curves (CVCs) from stellar dynamical models for ~6000 nearby galaxies in the final data release of the Sloan Digital Sky Survey-IV MaNGA survey with integral-field spectroscopy, exploring connections between the inner gravitational potential (traced by CVC amplitude/shape) and galaxy properties. The maximum circular velocity (V_circ_^max^) and circular velocity at the half-light radius (V_circ_(Re^maj^)) both scale linearly with the stellar second velocity moment {sigma}_e_^2^=<V^2^+{sigma}^2^> within the half-light isophote, following V_circ_^max^~1.72{sigma}_e_ (7% error) and V_circ_(Re^maj^)~1.62{sigma}_e_ (7% error). CVC shapes (rising, flat, declining) correlate strongly with structural and stellar population properties: declining curves dominate in massive, early-type, bulge-dominated galaxies with old, metal-rich stars and early quenching, while rising CVCs prevail in disk-dominated systems with younger stellar populations and ongoing star formation. Using a unified bulge-disk-halo model, we predict CVC shapes with minimal bias, identifying three governing parameters: bulge-to-total mass ratio (B/T), dark matter fraction within Re, and bulge Sersic index. The distribution of CVC shapes across the mass-size plane reflects evolutionary pathways driven by (i) in situ star formation (spurring bulge growth) and (ii) dry mergers. This establishes CVC morphology as a diagnostic for galaxy evolution, linking dynamical signatures to structural and stellar population histories.
Author(s): Zhu K.; Cappellari M.; Mao S.; Lu S.; Li R.; Shi Y.; Simon D.A.; Fu Y.,Wang X.
IVOA id: ivo://cds.vizier/j/apjs/280/55

Young stellar group around Sh 2-295

2026-07-31T12:13:46Z

Description: Star formation is governed by multiple physical processes, making it inherently complicated. One excellent example is the Canis Major OB1/R1 association, whose complex history of star formation is related to different episodes. Three supernova (SN) events potentially altered the environment and impacted star formation and stellar evolution. Prior investigations revealed two stellar groups of different ages associated with GU CMa and Z CMa. This work focusses on identifying the low-mass young stellar population near FZ CMa, located between these two groups and spatially related to the HII region Sh 2-295. Our main goal is to verify whether this group is age-mixed and characterise its physical properties. We analysed multi-object spectroscopic data acquired with Gemini/GMOS to search for typical features of T Tauri stars (TTs) and to determine their spectral types. Lithium absorption line ({lambda} 6708{AA}) was used as a youth indicator, while H{alpha} emission was investigated to probe accretion activity. We also derived ages based on optical photometry from Gaia DR3 and compared the projected spatial distribution to diffuse infrared emission. We identified 29 TTs, including six new members of the association and three classical TTs. The equivalent width of the LiI absorption line suggests an age of 8.1^+2.1^_-3.8_Myr, while optical photometric data indicate stellar ages ranging from ~1 to 14Myr. Younger stars are concentrated around Sh 2-295, whereas the older ones are more widely dispersed. We increased the number of known TTs related to the CMa association. Our results support a scenario of multiple star formation episodes, including a younger group that may have been triggered by the expansion of Sh 2-295. The influence of SN events appears limited in this context.
Author(s): Correa-Rodrigues J.V.; Gregorio-Hetem J.
IVOA id: ivo://cds.vizier/j/a+a/707/a241

HD 4614 RVs from HIRES, APF, Hamilton & NEID

2026-07-31T08:41:54Z

Description: Given the vast number of stars that exist within binary systems, it remains important to explore the effect of binary star environments on the formation and evolution of exoplanetary systems. Nearby binaries provide opportunities to characterize their properties and orbits through a combination of radial velocities, astrometry, and direct imaging. Eta Cassiopeiae is a bright, well-known binary system for which recent observations have provided greatly improved stellar masses and orbital parameters. We present additional radial velocity data that are used to perform an injection-recovery analysis for potential planetary signatures. We further provide a detailed dynamical study that explores the viability of planetary orbits throughout the system. Our combined analysis shows that giant planets are significantly ruled out for the system, and indeed no planetary orbits are viable beyond ~8AU of the primary star. However, terrestrial planets may yet exist within the habitable zone where orbits can remain long-term stable. We discuss the implications of these results, highlighting the effect of wide binary companions on giant planet formation, and the consequences for occurrence rates and planetary habitability.
Author(s): Kane S.R.; Li Z.; Hill M.L.; D'Angiolillo S.; Fulton B.J.; Howard A.W.
IVOA id: ivo://cds.vizier/j/aj/170/270

HELP DR1 photometry of extragalactic field sources

2026-07-30T15:45:59Z

Description: We present the Herschel Extragalactic Legacy Project (HELP). This project collates, curates, homogenizes, and creates derived data products for most of the premium multiwavelength extragalactic data sets. The sky boundaries for the first data release cover 1270 deg^2^ defined by the Herschel SPIRE extragalactic survey fields; notably the Herschel Multi-tiered Extragalactic Survey (HerMES) and the Herschel Atlas survey (H-ATLAS). Here, we describe the motivation and principal elements in the design of the project. Guiding principles are transparent or 'open' methodologies with care for reproducibility and identification of provenance. A key element of the design focuses around the homogenization of calibration, meta data, and the provision of information required to define the selection of the data for statistical analysis. We apply probabilistic methods that extract information directly from the images at long wavelengths, exploiting the prior information available at shorter wavelengths and providing full posterior distributions rather than maximum-likelihood estimates and associated uncertainties as in traditional catalogues. With this project definition paper, we provide full access to the first data release of HELP; Data Release 1 (DR1), including a monolithic map of the largest SPIRE extragalactic field at 385 deg^2^ and 18 million measurements of PACS and SPIRE fluxes. We also provide tools to access and analyse the full HELP data base. This new data set includes far-infrared photometry, photometric redshifts, and derived physical properties estimated from modelling the spectral energy distributions over the full HELP sky. All the software and data presented is publicly available.
Author(s): Shirley R.; Duncan K.; Campos-Varillas M.C.; Hurley P.D.; Malek K.,Roehlly Y.; Smith M.W.L.; Aussel H.; Bakx T.; Buat V.; Burgarella D.,Christopher N.; Duivenvoorden S.; Eales S.; Efstathiou A.,Gonzalez Solares E.A.; Griffin M.; Jarvis M.; Faro B.L.; Marchetti L.,McCheyne I.; Papadopoulos A.; Penner K.; Pons E.; Prescott M.; Rigby E.,Rottgering H.; Saxena A.; Scudder J.; Vaccari M.; Wang L. and Oliver S.J.
IVOA id: ivo://cds.vizier/vii/299

PHANGS-ALMA GMC clustering

2026-07-30T12:39:05Z

Description: The spatial distribution of giant molecular clouds (GMCs) at sub-kiloparsec scales encodes information about cloud formation and evolution. However, we still lack a general quantitative characterisation of molecular gas structure at this scale. We aim to provide a quantitative description of molecular gas structure at 150-1000pc for a typical star-forming main sequence galaxy. We analyse how GMCs cluster together and how CO emission is spatially correlated with bright GMCs using a sample of 8984 GMCs from 40 galaxies observed by PHANGS-ALMA. We homogenized our data to a common spatial resolution of 150pc and a mass sensitivity of 2.5M_{sun}_/pc^2^ to remove observational bias. We then calculated the nearest neighbour distances, neighbour number density, and two-point correlation functions (2PCFs) for the catalogued GMCs in each galaxy. When analysing the 2PCFs, we generated several control samples that reflect different null hypotheses on large spatial scales. We stacked integrated intensity CO emission profiles around the position of catalogued GMCs to probe the gas distribution on scales between the observational resolution and the typical GMC-GMC spacing. Our measurements of cloud spacing and the number of neighbours show that GMC clustering follows the large-scale gas distribution. Once we accounted for this contribution, the peak excess clustering relative to the null hypothesis in the 2PCF dropped from 1+{imega}~2.3 to 1.3, with the power-law slope flattened from -0.25 to 0. Stacks of CO intensity around local maxima show a strong clustering signal on scales smaller than the typical GMC-GMC separation. We show that this is largely the same signal captured by the "GMC size" measured by CPROPS, with an additional ~20% of the flux in an extended component beyond 500 pc. We find that our stacked profiles can be fit with a double Gaussian function plus a constant offset. The broad Gaussian component accounts for 70% of the over-density power above the constant background and is stronger around massive and gravitationally bound GMCs. Our measurements yield a general statistical description of the structure of CO emission from ~150pc to galactic scales that can serve as a benchmark for simulations of molecular cloud formation and destruction in galaxy disks. Our results indicate that galactic structure exerts a strong influence on the GMC distribution in galaxy disks and that the formation of massive gravitationally bound GMCs is related to strong local gas clustering.
Author(s): He H.; Leroy A.K.; Rosolowsky E.; Hughes A.; Sun J.; Machado J.; Bigiel F.,Barnes A.; Bazzi Z.; Cao Y.; Chevance M.; Colombo D.; Glover S.C.O.,Henshaw J.D.; Koch E.W.; Meidt S.E.; Pan H.; Saito T.; Sarbadhicary S.K.,Schinnerer E.; Smith R.J.; Usero A.; Weinberg D.H.; Williams T.G.
IVOA id: ivo://cds.vizier/j/a+a/712/a24

Chemical composition in low-mass galaxies

2026-07-30T12:36:53Z

Description: We present Very Large Telescope/Xshooter spectrophotometric observations of eleven low-redshift (z<0.085) compact star-forming galaxies (the high O 32 sample). These galaxies are characterised by extremely high emission-line ratios, [O III]5007/[O II]3727, ranging from 11 to 42. Galaxies with such high ratios are promising candidates for leaking large amounts of Lyman continuum radiation. They are characterised by low oxygen abundances, 12+log(O/H)=7.5-8.0, and low stellar masses, M*~10^6^-10^8^M_{sun}. We used strong emission lines of various ions in all spectra to derive helium and oxygen abundances and N/O, Ne/O, S/O, Cl/O, Ar/O, and Fe/O abundance ratios. We also derived macroscopic velocity dispersions, sigma(lambda), from various emission lines of different ions. We find that sigma(4861) of the Hbeta emission line increases with increasing stellar mass and decreasing O 32 ratio. In contrast, sigma(lambda)/sigma(4861) ratios for various lines are close to unity. Exceptions are the sigma(lambda)/sigma(4861) of two lines, HeII 4686 and HeI 10830, which are considerably higher than unity, and those of four lines, [OII] 3726, 3729, [SII] 6717, and 6731, for which sigma(lambda)/sigma(4861) is lower than unity. The HeII 4686 and He I 10830 lines are likely produced in the inner parts of HII regions and are broadened by dynamical processes generated by massive stars, and, in the case of the HeI 10830 emission line, by radiative scattering. Emission in the [OII] and [SII] lines is produced mainly in the outer and likely more quieter parts of HII regions.
Author(s): Izotov Y.I.; Guseva N.G.; Schaerer D.; Amorin R.O
IVOA id: ivo://cds.vizier/j/a+a/712/a19

JWST COSMOS-3D [OIII] census and luminosity func.

2026-07-30T12:34:39Z

Description: We present a catalogue of spectroscopically-selected [OIII]+Hbeta emitters at 6.75<z<9.05 and the resulting [OIII] 5008{AA} Luminosity Function (LF) in the COSMOS field. We leverage the 0.33deg^2^ covered by COSMOS-3D using NIRCam/WFSS F444W to perform the largest spectroscopic search for [OIII] emitters at 6.75<z<9.05. We present our catalogue of 249 [OIII] emitters and their associated completeness function. The inferred constraints on the [OIII] LF enable us to characterise the knee of the [OIII] 5008{AA} LF, resulting in improved [OIII] 5008{AA} LF constraints at z~7, 8. Notably, we find evidence for a decline of the [OIII] luminosity density between z~6-8, which could be expected if the metallicity of [OIII] emitters, as well as the cosmic star-formation rate density, is declining at these redshifts. We find that theoretical models that reproduce the z~7,8 [OIII] 5008{AA} LF do not reproduce well the [OIII] equivalent width distribution, pointing to potential challenges in the modelling of [OIII] and other nebular lines in the early Universe. Finally, we provide the first constraints on the cosmic variance of [OIII] emitters, estimating at 15% the fractional uncertainty for the z~7,8 [OIII] 5008{AA} LF in the 0.33deg^2^ field. This estimate is in good agreement with that inferred from clustering, and shows that the [OIII] 5008{AA} LF derived from smaller extragalactic legacy fields is strongly affected by cosmic variance. Our results highlight the fundamental role that wide-area JWST slitless surveys play to map the galaxy large-scale structure down into the reionisation era, serving as a springboard for a variety of science cases.
Author(s): Meyer R.A.; Wang F.; Kakiichi K.; Brammer G.; Champagne J.; Jurk K.; Li Z.,Li Z.; Musin M.; Satyavolu S.; Schindler J.-T.; Shuntov M.; Xu Y.; Zou S.,Bian F.; Casey C.; Egami E.; Fan X.; Jiang D.; Laporte N.; Liu W.,Oesch P.A.; Tasca L.; Yang J.; Zhang Z.; Akins H.; Cai Z.; Coulter D.A.,Huang J.; Li M.; Liu W.; Liang Y.; Jin B.; Jin X.; Kartaltepe J.,Koekemoer A.M.; Matharu J.; Pudoka M.; Tee W.-L.; Witten C.; Zhang H.,Zhu Y.
IVOA id: ivo://cds.vizier/j/a+a/712/a16

Chemo-dynamical complexity of omega Centauri

2026-07-30T12:33:15Z

Description: The origin of omega Centauri remains one of the key open problems in stellar dynamics and chemical evolution. Its large abundance spreads and multiple populations suggest a formation history more complex than that of a typical globular cluster. Aims. We investigate whether the chemical sub-populations identified in APOGEE DR17 also exhibit distinct spatial and kinematic signatures, and what constraints these provide on the formation pathways of omega Cen. We analyse a sample of APOGEE DR17 red-giant stars using a Gaussian Mixture Model in an eight-dimensional chemical-abundance space. The resulting chemical components are combined with Gaia proper motions and APOGEE line-of-sight velocities to derive intrinsic mean velocities and velocity dispersions in all three observable directions. We measure both global kinematic quantities and radial profiles for each chemically defined group, extending from the inner regions to ~4 half-light radii. The Gaussian Mixture Model identifies five chemical components, which, when examined through their radial cumulative distributions, naturally group into two broader families characterised by lower and higher aluminium enrichment. The two families differ significantly in their spatial and kinematic properties: the Al-rich stars are more centrally concentrated and exhibit stronger radial anisotropy than the Al-poor stars, which remain closer to isotropy over the radial range probed. Despite these significant differences (>2{sigma}), the two populations share a common rotation pattern, with comparable intrinsic rotation amplitudes and rotation-axis inclinations within the uncertainties (~0.5km/s). Both families span a wide range in metallicity, indicating that they do not simply correspond to a first- and second-generation dichotomy, but rather trace chemically and dynamically complex substructures within omega Cen. This work represents the first chemo-dynamical study of omega Cen linking detailed chemical tagging to internal kinematics from the inner regions to the cluster outskirts, and provides a key benchmark for models of its formation. A formation path involving both hierarchical assembly within a dwarf-galaxy potential and centrally concentrated, chemically enriched star formation offers a natural explanation for the observed chemo-dynamical complexity. Extending this approach to larger fields of view and to more numerous, fainter stars will be essential to robustly uncover the origin of this uniquely complex system.
Author(s): Pagnini G.; Bianchini P.; Di Matteo P.; Mastrobuono-Battisti A.
IVOA id: ivo://cds.vizier/j/a+a/712/a6

Splatalogue CASA SLAP2

2026-07-30T10:53:48Z

Description: These are spectral lines from the splatalogue that come with casa
Author(s): Brogan, C.; Remijan, A. J.; Markwick-Kemper, A.
IVOA id: ivo://org.gavo.dc/casa_lines/q/q