VO Fresh

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

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

KPF RVs for TOI-2374: Planet in Neptunian ridge

2026-07-31T12:01:38Z

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

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

AMS-02 Spectral Results Catalog

2026-07-31T00:00:00Z

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

Chandra Source Catalog Stacked Observation Detections, v2.1.1

2026-07-31T00:00:00Z

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)

2026-07-31T00:00:00Z

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

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

Parkes transient database II. (PTD II)

2026-07-30T09:31:51Z

Description: We have reprocessed single-pulse candidates from the first four years (1997-2001) of the Parkes Multibeam receiver system observations, creating a new Parkes transient database (PTD II) that contains 165,592 single pulses from 363 known pulsars. Unlike previous databases, PTD II preserves the critical raw data segments of each detected pulse, enabling detailed analyses of emission physics while maintaining a compact size of only 1.5GB. The database employs an sqlite3 structure organising pulsar metadata, observation files, and pulse events with their raw data stored in binary format. We provide processing tools for extracting and analyzing single-pulse data, enabling fluence fitting and statistical analysis. Our pulsars exhibit diverse fluence distributions, such as log-normal, Gaussian, and unimodal. Temporal analyses reveal significant evolution in emission characteristics of several pulsars, including event-rate variations spanning 2 orders of magnitude in PSR J1602-5100 and PSR J0942-5552. Beyond supporting fundamental pulsar emission studies, the database serves as a valuable training resource for developing new single-pulse detection algorithms in the presence of radio-frequency interference.
Author(s): Yang X.; Zhang S.; Le-Yu Tang; Toomey L.; Wu X.
IVOA id: ivo://cds.vizier/j/apjs/280/58

The CLASS quasar catalog: coronal line activity

2026-07-30T08:52:23Z

Description: We conduct the first systematic survey of a total of 11 optical coronal lines (CLs) in the spectra of a large sample of low-redshift (z<0.8) Type 1 quasars observed by the Sloan Digital Sky Survey (SDSS). We find that strong CL emission is rare in SDSS even in Type 1 quasars; only 885 out of 19508 (4.5%) galaxies show at least one CL, with higher ionization potential lines (>100 eV) being even rarer. The [NeV]{lambda}3426 line, which constitutes the majority of detections, is strongly correlated with the bolometric luminosity. These findings suggest that the optical CLs are significantly suppressed in the majority of local active galactic nuclei (AGNs), possibly as a result of the presence of dust in the emitting regions. We find that the incidence of ionized outflows is significantly higher in CL emitters compared with non-CL emitters, possibly suggesting that dust destruction in outflows enhances CL emission in AGNs. Many CLs show line profiles that are broader than those of narrow lines, and are blueshifted relative to the lower ionization potential lines, suggesting outflows in the highly ionized gas. Given the limited number of detections, we do not find any statistically significant trends in detection statistics or line ratios with black hole mass, Eddington ratio, or AGN bolometric luminosity. The catalog is publicly available and can provide a useful database of the CL properties of low- redshift quasars that can be compared to the growing number of high-z AGNs discovered by JWST.
Author(s): Doan S.; Satyapal S.; Reefe M.; Sexton R.O.; Matzko W.; McKaig J.D.,Secrest N.J.; Cann J.M.; Laor A.; Canalizo G.
IVOA id: ivo://cds.vizier/j/apjs/280/57

Recognizing blazars from VLASS radio morphology

2026-07-30T07:57:57Z

Description: Blazars are radio-loud active galactic nuclei whose jets have a very small angle to our line of sight. Observationally, the radio emissions are mostly compact or compact-core with a one-sided jet. With 2.5" resolution at 3GHz, the Very Large Array Sky Survey (VLASS) enables us to resolve the structure of some blazar candidates in the sky north of decl. -40{deg}. We introduce an algorithm to classify radio sources as either blazar-like or non-blazar-like based on their morphology in the VLASS images. We apply our algorithm to three existing catalogs, including one of the known blazars (Roma-BzCAT) and two blazar candidates identified by Wide-field Infrared Survey Explorer colors and radio emission (WIBRaLS, KDEBLLACS). We show that in all three catalogs, there are objects with morphologies inconsistent with being blazars. Considering all the catalogs, more than 12% of the candidates are unlikely to be blazars, based on this analysis. Notably, we show that 3% of the Roma-BzCAT confirmed blazars could be a misclassification based on their VLASS morphology. The resulting table with all sources and their radio morphological classification is available online.
Author(s): Xie Z.-L.; Banados E.; Belladitta S.; Mazzucchelli C.; Schindler J.-T.,Davies F.; Venemans B.P.
IVOA id: ivo://cds.vizier/j/apj/964/98

Molecular bubble and YSOs in S Mon region

2026-07-30T07:23:06Z

Description: We identify a molecular bubble, and study the star formation and its feedback in the S Mon region, using multiple molecular lines, young stellar objects (YSOs), and infrared data. We revisit the distance to S Mon, ~722{\pm}9pc, using Gaia Data Release 3 parallaxes of the associated Class II YSOs. The bubble may be mainly driven by a massive binary system (namely 15 Mon), the primary of which is an O7V-type star. An outflow is detected in the shell of the bubble, suggesting ongoing star formation activities in the vicinity of the bubble. The total wind energy of the massive binary star is 3 orders of magnitude higher than the sum of the observed turbulent energy in the molecular gas and the kinetic energy of the bubble, indicating that stellar winds help to maintain the turbulence in the S Mon region and drive the bubble. We conclude that the stellar winds of massive stars have an impact on their surrounding environment.
Author(s): Liu D.; Xu Ye; Li Y.; Lin Z.; Hao C.; Yang W.; Li J.; Liu X.; Dong Y.,Bian S.; Kong D.
IVOA id: ivo://cds.vizier/j/apj/964/93

JADES galaxies at z>8 in GOODS-N & GOODS-S

2026-07-30T06:49:31Z

Description: We present a catalog of 717 candidate galaxies at z>8 selected from 125 square arcmin of NIRCam imaging as part of the JWST Advanced Deep Extragalactic Survey (JADES). We combine the full JADES imaging data set with data from the JWST Extragalactic Medium Survey and First Reionization Epoch Spectroscopic COmplete Survey (FRESCO) along with extremely deep existing observations from Hubble Space Telescope (HST)/Advanced Camera for Surveys (ACS) for a final filter set that includes 15 JWST/NIRCam filters and five HST/ACS filters. The high-redshift galaxy candidates were selected from their estimated photometric redshifts calculated using a template-fitting approach, followed by visual inspection from seven independent reviewers. We explore these candidates in detail, highlighting interesting resolved or extended sources, sources with very red long-wavelength slopes, and our highest-redshift candidates, which extend to zphot ~18. Over 93% of the sources are newly identified from our deep JADES imaging, including 31 new galaxy candidates at zphot>12. We also investigate potential contamination by stellar objects, and do not find strong evidence from spectral energy distribution fitting that these faint high-redshift galaxy candidates are low-mass stars. Using 42 sources in our sample with measured spectroscopic redshifts from NIRSpec and FRESCO, we find excellent agreement to our photometric redshift estimates, with no catastrophic outliers and an average difference of <{Delta}z=zphot-zspec>=0.26. These sources comprise one of the most robust samples for probing the early buildup of galaxies within the first few hundred million years of the Universe's history.
Author(s): Hainline K.N.; Johnson B.D.; Robertson B.; Tacchella S.; Helton J.M.,Sun F.; Eisenstein D.J.; Simmonds C.; Topping M.W.; Whitler L.,Willmer C.N.A.; Rieke M.; Suess K.A.; Hviding R.E.; Cameron A.J.,Alberts S.; Baker W.M.; Baum S.; Bhatawdekar R.; Bonaventura N.,Boyett K.; Bunker A.J.; Carniani S.; Charlot S.; Chevallard J.; Chen Z.,Curti M.; Curtis-Lake E.; D'Eugenio F.; Egami E.; Endsley R.; Hausen R.,Ji Z.; Looser T.J.; Lyu J.; Maiolino R.; Nelson E.; Puskas D.; Rawle T.,Sandles L.; Saxena A.; Smit R.; Stark D.P.; Williams C.C.; Willott C.,Witstok J.
IVOA id: ivo://cds.vizier/j/apj/964/71

MAGIC DL5 Light Curves

2026-07-29T13:25:46.339000Z

Description

MAGIC DL5 release of light curves for an increasing subset
        	    of published results. The dataset contains high-level products derived from
        	    MAGIC observations and is continuously updated as new analyses are released.

Author(s)

MAGIC Collaboration

IVOA id

ivo://magictelescope/dl5_lc

Secondary standards J and K MKO photometry

2026-07-29T06:05:42Z

Description: We present precise J- and K-band photometric measurements for 128 near-infrared (NIR) secondary standard stars, located in the 19 United Kingdom Infrared Telescope/Maunakea Observatories (UKIRT/MKO) primary faint standard fields. The data were collected over more than 50 nights, covering a decade of observations between 2008 and 2018 at the ESO La Silla Observatory, using the New Technology Telescope equipped with the SOFI NIR camera. Presented magnitudes are calibrated onto the MKO photometric system. The J- and K-band magnitudes range from 10 to 15.8 mag, with median values of J=13.5mag and K=13mag. The selection process ensured high photometric quality, with a precision better than 0.01 mag for all stars. The catalog excludes stars with close neighbors, high proper motion, or variable stars. Using these fields for standardization can improve the precision and accuracy of photometric calibrations without increasing the observational time cost.
Author(s): Gorski M.; Pietrzynski G.; Karczmarek P.; Hajdu G.; Kicia M.,Kaluszynski M.; Eimer J.R.; Smee S.A.; Zgirski B.; Wielgorski P.,Narloch W.
IVOA id: ivo://cds.vizier/j/apjs/282/44

NETS. III. Activity & RV from NEID of 41 systems

2026-07-28T14:09:47Z

Description: The NEID Earth Twin Survey (NETS) has been delivering a rich set of precise radial velocity (RV) measurements for 41 bright, nearby main-sequence stars. Here, we describe the status of the survey after 3yr on sky, and we present the full set of RV measurements and accompanying stellar activity indicators. We discuss intermediate survey diagnostics, including calibration of the known RV zero-point offset introduced following the Contreras fire in 2022 and the identification of an undiagnosed and previously unknown zero-point offset in 2021. An analysis of our data set using RVSearch demonstrates that for these target stars, NEID is independently sensitive to nearly all known planets with periods shorter than the NETS observing baseline. We also highlight a number of newly detected RV signals, which present exciting opportunities for future investigations.
Author(s): Gupta A.F.; Fitzmaurice E.; Mahadevan S.; Robertson P.; Luhn J.K.,Wright J.T.; Logsdon S.E.; Krolikowski D.M.; Paredes L.A.; Bender C.F.,Giovinazzi M.R.; Lin A.S.J.; Blake C.H.; Canas C.I.; Ford E.B.,Halverson S.; Kanodia S.; McElwain M.W.; Monson A.; Ninan J.P.,Rajagopal J.; Roy A.; Schwab C.; Stefansson G.; Terrien R.C.
IVOA id: ivo://cds.vizier/j/aj/170/264

NETS. IV. RVs of confirmed planet HD 190360 d

2026-07-28T14:04:19Z

Description: We present the confirmation of HD 190360 d, a warm (P=88.690_-0.049_^+0.051^days), low-mass (m.sin(i)=10.23_-0.80_^+0.81^M_{Earth}) planet orbiting the nearby (d=16.0pc), Sun-like (G7) star HD 190360. We detect HD 190360 d at high statistical significance even though its radial velocity (RV) semiamplitude is only K=1.48+/-0.11m/s. Such low-amplitude signals are often challenging to confirm due to potential confusion with low-amplitude stellar signals. The HD 190360 system previously had two known planets: the 1.7M_J_ (true mass) HD 190360 b on a 7.9yr orbit and the 21M_{Earth}_ (minimum mass) HD 190360 c on a 17.1days orbit. Here, we present an in-depth analysis of the HD 190360 planetary system that comprises more than 30yr of RV measurements and absolute astrometry from the Hipparcos and Gaia spacecraft. Our analysis uses more than 1400 RVs, including nearly 100 from NEID. The proper motion anomaly as measured by these two astrometric missions solves for the dynamical mass of HD 190360 b and contributes to our understanding of the overall system architecture, while the long baseline of RVs enables the robust characterization of HD 190360 c and confirms the discovery of HD 190360 d.
Author(s): Giovinazzi M.R.; Fitzmaurice E.; Gupta A.F.; Robertson P.; Mahadevan S.,Ford E.B.; Alvarado-Montes J.A.; Bender C.F.; Blake C.H.; Dong J.,Fernandes R.B.; Halverson S.; Han Te; Kanodia S.; Krolikowski D.M.,Logsdon S.E.; Ninan J.P.; Roy A.; Schwab C.; Stefansson G.; Terrien R.C.,Wright J.T.
IVOA id: ivo://cds.vizier/j/aj/171/286

SMGPS Local Void HI galaxy catalogue

2026-07-28T13:47:07Z

Description: The Local Void is one of the nearest large voids, located at a distance of 23Mpc. It lies largely behind the Galactic Bulge and is therefore extremely difficult to observe. We use HI 21cm emission observations from the SARAO MeerKAT Galactic Plane Survey (SMGPS) to study the Local Void and its surroundings over the Galactic longitude range 329deg<l<55deg, Galactic latitude |b|<1.5deg, and redshift cz<7500km/s. We have detected 291 galaxies of median rms sensitivity 0.44 mJy per beam per 44 km/s channel. We find 17 galaxies deep inside the Void, 96 at the border of the Void, while the remaining 178 galaxies are in average density environments. The extent of the Void is ~58Mpc. It is severely underdense for the longitude range 350deg<l<35deg up to redshift z<4500km/s. The galaxies in the Void tend to have HI masses that are lower (by approximately 0.25dex) than their average density counterparts. We find several potential candidates for small groups of galaxies, of which two groups (with 3 members and 5 members) in the Void show signs of filamentary substructure within the Void.
Author(s): Kurapati S.; Kraan-korteweg R.C.; Pisano D.J.; Chen H.; Rajohnson S.H.A.,Steyn N.; Frank B.; Serra P.; Goedhart S.; Camilo F.
IVOA id: ivo://cds.vizier/j/mnras/528/542

Catalog of outbursts of neutron star LMXBs

2026-07-28T11:19:32Z

Description: Many X-ray binaries (XRBs) are transiently accreting. Having statistics on their recurrence times is helpful to address questions related to binary evolution and populations, as well as the physics of binary systems. We compile a catalog of known outbursts of 87 transient neutron stars (identified through bursts or pulsations) and low-mass XRBs until mid-2025. Most outbursts are taken from the literature, but we also identify some outbursts from public X-ray monitoring lightcurves. We find 109 outbursts not previously identified in the literature; most are from the frequent transients GRS 1747-312 and the Rapid Burster MXB 1730-335, though we suspect that two outbursts from Liller 1 may be from another transient besides the Rapid Burster. We also find new outbursts for 10 other systems, and verify substantial quiescent intervals for XMM J174457-2850.3, XMMU J174716.1-281048, and AX J1754.2-2754. Outburst detection has been relatively efficient since 1996 for outbursts above F_X_(2-10keV)=3x10^-10^erg/cm^2^/s. While several systems have many known outbursts, 40 of the 87 systems we track have zero or one recorded outburst between 1996 and 2023. This suggests that many faint Galactic center XRBs may be neutron star XRBs, though we cannot completely rule out the proposition that most neutron star XRBs undergo frequent outbursts below all-sky monitor detection limits.
Author(s): Heinke C.O.; Zheng J.; Maccarone T.J.; Degenaar N.; Bahramian A.,Sivakoff G.R.; Toor S.
IVOA id: ivo://cds.vizier/j/apjs/279/57

MgII line profiles & refined param. of FGKM stars

2026-07-28T10:27:13Z

Description: The MgII h&k emission lines (2803, 2796{AA}) are a useful tool for understanding stellar chromospheres and transition regions due to their intrinsic brightness, relatively low interstellar medium (ISM) absorption interference, and abundance of archival spectra available. Similar to other optically thick chromospheric emission lines such as HI Ly{alpha}, MgII emissions commonly present with a self-reversed line core, the depth and shape of which vary from star to star. We explore the relationship between self-reversal and the stellar atmosphere by investigating the extent to which fundamental stellar parameters affect self-reversal. We present a search for correlations between photospheric parameters such as effective temperature, surface gravity, and metallicity with the MgII k self-reversal depth for a group of 135 FGKM main-sequence stars with high-resolution near-ultraviolet spectra from the Hubble Space Telescope. We modeled the observed MgII k line profiles to correct for ISM attenuation and recover the depth of the emission line's self-reversal in relation to the intensity of the line. We used the PHOENIX atmosphere code to homogeneously determine the stellar parameters by computing a suite of stellar atmosphere models that include a chromosphere and transition region, and using archival photometry to guide the models of each star. We quantify the sensitivity of the visible and near-infrared photometry to chromospheric and photospheric parameters. We find weak trends between MgII k self-reversal depth and age, rotation period, MgII luminosity, temperature, and mass. All stars in our sample older than ~2Gyr or rotating slower than ~10days exhibit self-reversal.
Author(s): Taylor A.; Dunn A.; Peacock S.; Youngblood A.; Redfield S.
IVOA id: ivo://cds.vizier/j/apj/964/80

Gas-phase mass-metallicity relation for LEGA-C gal.

2026-07-28T10:15:24Z

Description: The massive end of the gas-phase mass-metallicity relation (MZR) is a sensitive probe of active galactic nuclei (AGN) feedback that is a crucial but highly uncertain component of galaxy evolution models. In this paper, we extend the z~0.7 MZR by ~0.5dex up to log(M*/M_{sun}_)~11.1. We use extremely deep VLT VIMOS spectra from the Large Early Galaxy Astrophysics Census (LEGA-C) survey to measure metallicities for 145 galaxies. The LEGA-C MZR matches the normalization of the z~0.8 DEEP2 MZR where they overlap, so we combine the two to create an MZR spanning from 9.3 to 11.1 log(M*/M_{sun}_). The LEGA-C+DEEP2 MZR at z~0.7 is offset to slightly lower metallicities (0.05-0.13 dex) than the z~0 MZR, but it otherwise mirrors the established power-law rise at low/intermediate stellar masses and asymptotic flattening at high stellar masses. We compare the LEGA-C+DEEP2 MZR to the MZR from two cosmological simulations (IllustrisTNG and SIMBA), which predict qualitatively different metallicity trends for high-mass galaxies. This comparison highlights that our extended MZR provides a crucial observational constraint for galaxy evolution models in a mass regime where the MZR is very sensitive to choices about the implementation of AGN feedback.
Author(s): Lewis Z.J.; Andrews B.H.; Bezanson R.; Maseda M.; Bell E.F.; Dave R.,D'Eugenio F.; Franx M.; Gallazzi A.; de Graaff A.; Kaushal Y.,Nersesian A.; Newman J.A.; van der Wel A.; Wu P.-F.
IVOA id: ivo://cds.vizier/j/apj/964/59

Li-rich stars with GALAH, Gaia and GALEX data

2026-07-28T09:11:06Z

Description: Stellar models predict that lithium (Li) inside a star is destroyed during the first dredge-up phase, yet 1.2% of red giant stars are Li-rich. We aim to uncover possible origins of this population, by analyzing 1099 Li-rich giants (A(Li)>=1.5) in GALAH DR3. To expose peculiar traits of Li-rich stars, we construct a reference sample of Li-normal (doppelganger) stars with matched evolutionary state and fiducial iron-peak and alpha-process abundances ([Fe/H] and [Mg/Fe]). Comparing Li-rich and doppelganger spectra reveals systematic differences in the H{alpha} and Ca-triplet line profiles associated with the velocity broadening measurement. We also find twice as many Li-rich stars appear to be fast rotators (2% with vbroad >~20km/s) compared to doppelgangers. On average, Li-rich stars have higher abundances than their doppelgangers, for a subset of elements, and Li-rich stars at the base of RGB have higher mean s-process abundances (>=0.05dex for Ba, Y, Zr), relative to their doppelgangers. External mass-transfer from intermediate-mass AGB companions could explain this signature. Additional companion analysis excludes binaries with mass ratios >~0.5 at >~7au. Finally, we confirm a prevalence of Li-rich stars on the red clump that increases with lithium, which supports an evolutionary state mechanism for Li-enhancement. Multiple culprits, including binary spin-up and mass-transfer, are therefore likely mechanisms of Li-enrichment.
Author(s): Sayeed M.; Ness M.K.; Montet B.T.; Cantiello M.; Casey A.R.; Buder S.,Bedell M.; Breivik K.; Metzger B.D.; Martell S.L.; McGee-Gold L.
IVOA id: ivo://cds.vizier/j/apj/964/42

LCOGT LCs of the variable AGN 6dFGS gJ022550.0-060145

2026-07-28T08:18:43Z

Description: We use LCOGT observations (MJD 59434-59600) with a total exposure time of ~50hr and a median cadence of 0.5d to measure the interband time delays (with respect to u) in the g, r, and i continua of a highly variable active galactic nucleus (AGN), 6dFGS gJ022550.0-060145. We also calculate the expected time delays of the X-ray reprocessing of a static Shakura-Sunyaev disk according to the source's luminosity and virial black hole mass; the two parameters are measured from the optical spectrum of our spectroscopic observation via the Lijiang 2.4m telescope. It is found that the ratio of the measured time delays to the predicted ones is 2.6_-1.3_^+1.3^. With optical light curves (MJD53650-59880) from our new LCOGT and archival Zwicky Transient Facility, Pan-STARRS, Catalina Sky Survey, and ATLAS observations, and Wide-field Infrared Survey Explorer (WISE) data (MJD 55214-59055), we also measured time delays between WISE W1/W2 and the optical emission. W1 and W2 have time delays (with respect to V), 9.6_-1.6_^+2.9^x10^2^d and 1.18_-0.10_^+0.13^x10^3^d in the rest frame, respectively; hence, the dusty torus of 6dFGS gJ022550.0-060145 should be compact. The time delays of the W1 and W2 bands are higher than the dusty torus size-luminosity relationship of Lyu+ (2019ApJ...886...33L). By comparing the infrared and optical variability amplitude, we find that the dust-covering factors of the W1 and W2 emission regions are 0.7 and 0.6, respectively. Future broad emission-line reverberation mapping of this target and the results of this work enable us to determine the sizes of the AGN main components simultaneously.
Author(s): Li D.; Sun M.; Wang J.; Wu J.; Zhang Z.
IVOA id: ivo://cds.vizier/j/apj/964/37

ALMA-LEGUS. I. Molecular gas in NGC1313 and NGC7793

2026-07-28T08:09:39Z

Description: We present a comparative study of the molecular gas in two galaxies from the Legacy ExtraGalactic UV Survey (LEGUS) sample: barred spiral NGC 1313 and flocculent spiral NGC 7793. These two galaxies have similar masses, metallicities, and star formation rates, but NGC 1313 is forming significantly more massive star clusters than NGC 7793, especially young massive clusters (<10Myr, >10^4^M_{sun}_). Using Atacama Large Millimeter/submillimeter Array (ALMA) CO(2-1) observations of the two galaxies with the same sensitivity and resolution (13pc), we directly compare the molecular gas in these two similar galaxies to determine the physical conditions responsible for their large disparity in cluster formation. By fitting size-line width relations for the clouds in each galaxy, we find that NGC 1313 has a higher intercept than NGC 7793, implying that its clouds have higher kinetic energies at a given size scale. NGC 1313 also has more clouds near virial equilibrium than NGC 7793, which may be connected to its higher rate of massive cluster formation. However, these virially bound clouds do not show a stronger correlation with young clusters than with the general cloud population. We find surprisingly small differences between the distributions of molecular cloud populations in the two galaxies, though the largest of those differences is that NGC 1313 has higher surface densities and lower freefall times.
Author(s): Finn M.K.; Johnson K.E.; Indebetouw R.; Costa A.H.; Adamo A.; Aloisi A.,Bittle L.; Calzetti D.; Dale D.A.; Dobbs C.L.; Donovan Meyer J.,Elmegreen B.G.; Elmegreen D.M.; Fumagalli M.; Gallagher J.S.; Grasha K.,Grebel E.K.; Kennicutt R.C.; Krumholz M.R.; Lee J.C.; Messa M.; Nair P.,Sabbi E.; Smith L.J.; Thilker D.A.; Whitmore B.C.; Wofford A.
IVOA id: ivo://cds.vizier/j/apj/964/12

Extreme variability quasars. II. SDSS sp. fitting

2026-07-28T07:55:28Z

Description: We previously built a sample of 14,012 extremely variable quasars (EVQs) based on Sloan Digital Sky Survey (SDSS) and Pan-STARRS1 photometric observations. In this work we present the spectral fitting to their SDSS spectra and study the spectral variation in 1259 EVQs with multiepoch SDSS spectra (after prudently excluding spectra with potentially unreliable spectroscopic photometry). We find a clear "bluer-when-brighter" trend in EVQs, consistent with previous findings of normal quasars and active galactic nuclei. We detect significant intrinsic Baldwin effect (iBeff, i.e., smaller line equivalent width at higher continuum flux in individual active galactic nuclei) in the broad MgII and CIV lines of EVQs. Meanwhile, no systematical iBeff is found for the broad H{beta} line, which could be attributed to strong host contamination at longer wavelengths. Remarkably, by comparing the iBeff slope of EVQs with archived changing-look quasars, we show that the changing-look quasars identified in the literature are most likely a biased (due to its definition) subpopulation of EVQs, rather than a distinct population of quasars. We also found no significant broad line breathing of H{beta}, MgII, or CIV, suggesting the broad line breathing in quasars may disappear at longer timescales (~3000days).
Author(s): Ren W.; Wang J.; Cai Z.; Hu X.
IVOA id: ivo://cds.vizier/j/apj/963/7

A(Li) and stellar parameters of near MS stars

2026-07-27T13:29:17Z

Description: We investigate the distribution of the lithium abundances, A(Li), of metal-poor dwarf and subgiant stars within the limits 5500 K < Teff < 6700 K, -6.0 < [Fe/H] < -1.5, and log g ~> 3.5 (a superset of parameters first adopted by Spite and Spite), using literature data for some 200 stars. We address the problem of the several methods that yield Teff differences up to 350 K, and hence uncertainties of 0.3 dex in [Fe/H] and A(Li), by anchoring Teff to the infrared flux method. We seek to understand the behaviour of A(Li) as a function of [Fe/H] - small dispersion at highest [Fe/H], 'meltdown' at intermediate values (i.e. large spread in Li below the Spite Plateau), and extreme variations at lowest [Fe/H]. Decreasing A(Li) is accompanied by increasing dispersion. Insofar as [Fe/H] increases as the Universe ages, the behaviour of A(Li) reflects chaotic star formation involving destruction of primordial Li, which settles to the classic Spite Plateau, with A(Li) ~ 2.3, by the time the Galactic halo reaches [Fe/H] ~ -3.0. We consider three phases: (1) first star formation in C-rich environments ([C/Fe] > 2.3), with depleted Li; (2) silicates-dominated star formation and destruction of primordial Li during pre-main-sequence evolution; and (3) materials from these two phases co-existing and coalescing to form C-rich stars with A(Li) below the Spite Plateau, leading to a toy model with the potential to explain the 'meltdown'. We comment on the results of Mucciarelli et al. on the Lower RGB, and the suggestion of Aguado et al. (2019ApJ...874L..21A) favouring a lower primordial lithium abundance than generally accepted.
Author(s): Norris J.E.; Yong D.; Frebel A.; Ryan S.G.
IVOA id: ivo://cds.vizier/j/mnras/522/1358

Kinematic groups in USco with GaiaEDR3

2026-07-27T13:23:56Z

Description: The improved astrometry precision of Gaia-eDR3 allows us to perform a detailed study of the Upper Scorpius OB association and revisit its spatial, kinematic, and age substructure. We achieve this by combining clustering techniques and complementing with age estimations based on Gaia photometry. Our census retrieves 3661 candidate members for Upper Scorpius with contamination ~9 per cent. We also extract an astrometrically clean sample of 3004 sources with contamination ~6 per cent. We show that Upper Scorpius can be divided into at least three main kinematic groups. We systematically investigate and characterize the Upper Scorpius' internal structure, revealing that at least ~34 per cent of its stellar populations are contained in seven spatial substructures, with well defined boundaries, kinematics, and relative ages with suggested names: {pi} Scorpii (20^+/-2^_+/-1_ Myr), {alpha} Scorpii (14^+/-2^_+/-1_ Myr), {delta} Scorpii (9^+/-2^_+/-1_ Myr), {beta} Scorpii (8^+/-1^_+/-1_ Myr), {omega} Scorpii (8^+/-1^_+/-1_ Myr), v Scorpii (7^+/-1^_+/-1_ Myr), after their brightest member, and the well known {rho} Ophiuchi (4^+/-1^_+/-1_ Myr). We find a clear correlation in (1) density-age, providing an empirical expansion law to be tested in other associations, and (2) tangential velocity-age, providing constrains on the dynamics of these substructures and the position of potential past triggering events. We estimate the time at which four potential supernovae events occurred in Upper Scorpius. Based on these findings, we tie together previous work on the region and suggest a star formation history with unprecedented temporal resolution.
Author(s): Briceno-Morales G.; Chaname J.
IVOA id: ivo://cds.vizier/j/mnras/522/1288

MaNGA galaxy kinematic properties from RCs fit

2026-07-27T13:06:45Z

Description: We present a catalogue of dynamical properties for 2368 late-type galaxies from the MaNGA survey. The latter complements the catalogue of photometric properties for the same sample based on deep optical dark energy sky instrument legacy imaging survey (DESI) photometry processed with AUTOPROF . Rotation curves (RCs), extracted by model-fitting H {alpha} velocity maps from the MaNGA Data Analysis Pipeline, extend out to 1.4 (1.9) R_e_ for the primary (secondary) MaNGA samples, respectively. The RCs and ancillary MaNGA Pipe3D data products were used to construct various fundamental galaxy scaling relations that are also compared uniformly with similar relations from numerical investigation of a hundred astrophysical object (NIHAO) zoom-in simulations. Simulated NIHAO galaxies were found to broadly reproduce the observed MaNGA galaxy population for log(M*/M_{sun}_) > 8.5. Some discrepancies remain, such as those pertaining to central stellar densities and the diversity of RCs due to strong feedback schemes. Also presented are spatially resolved scatters for the velocity-size-stellar mass (VRM*) structural relations using MaNGA and NIHAO samples. The scatter for these relations in the galaxian interiors is a consequence of the diversity of inner RC shapes, while scatter in the outskirts is dictated by the large range of stellar surface densities, which is itself driven by sporadic star formation. The detailed, spatially resolved scatter analysis highlights the complex interplay between local and global astrophysical processes and provides a strong constraint to numerical simulations.
Author(s): Arora N.; Courteau S.; Stone C.; Maccio A.V.
IVOA id: ivo://cds.vizier/j/mnras/522/1208

MUSE/HST z measure of galaxies in RXJ0437+00

2026-07-27T12:56:42Z

Description: We present the first strong-gravitational-lensing analysis of the galaxy cluster RX J0437.1+0043 (RXJ0437; z = 0.285). Newly obtained, deep MUSE observations, Keck/MOSFIRE near-infrared spectroscopy, and Hubble Space Telescope SNAPshot imaging reveal 13 multiply imaged background galaxies, three of them (at z = 1.98, 2.97, and 6.02, respectively) in hyperbolic umbilic (H-U) lensing configurations. The H-U images are located only 20-50 kpc from the cluster centre, i.e. at distances well inside the Einstein radius where images from other lens configurations are demagnified and often unobservable. Extremely rare (only one H-U lens was known previously) these systems are able to constrain the inner slope of the mass distribution - and unlike radial arcs, the presence of H-U configurations is not biased towards shallow cores. The galaxies lensed by RXJ0437 are magnified by factors ranging from 30 to 300 and (in the case of H-U systems) stretched nearly isotropically. Taking advantage of this extreme magnification, we demonstrate how the source galaxies in H-U systems can be used to probe for small-scale (10^9^M_{sun}_) substructures, providing additional insight into the nature of dark matter.
Author(s): Lagattuta D.J.; Richard J.; Ebeling H.; Basto Q.; Cerny C.; Edge A.,Jauzac M.; Mahler G.; Massey R.
IVOA id: ivo://cds.vizier/j/mnras/522/1091

Stellar properties of M3/M13 HB stars with UVIT

2026-07-27T12:53:30Z

Description: We present a far-ultraviolet (FUV) study of hot stellar populations in the second parameter pair globular clusters (GCs) M3 and M13, as a part of the GC UVIT Legacy Survey programme (GlobULeS). We use observations made with F148W and F169M filters of the Ultraviolet Imaging Telescope (UVIT) onboard AstroSat along with ground-based data (UBVRI filters), Hubble Space Telescope(HST) GC catalogue, and Gaia EDR3 catalogue. Based on the FUV-optical colour-magnitude diagrams, we classify the sources into the horizontal branch (HB) stars, post-HB stars, and hot white dwarfs (WDs) in both the GCs. The comparison of synthetic and observed colours of the observed HB stars suggests that the mass-loss at the red giant branch and He spread in both clusters have a simultaneous effect on the different HB distributions detected in M3 and M13, such that HB stars of M13 require a larger spread in He (0.247-0.310) than those of M3 (Y = 0.252-0.266). The evolutionary status of HB stars, post-HB stars, and WDs are studied using SED fit parameters and theoretical evolutionary tracks on the H-R diagram. We found that the observed post-HB stars have evolved from zero-age HB (ZAHB) stars of the mass range of 0.48-0.55 M_{sun}_ in M3 and M13. We detect 24 WD candidates in each cluster having log(Lbol/L_{sun}_) in the range of -0.8 to +0.6 and log(Teff/K) in the range of 4.2-5.0. Placing the WDs on the H-R diagram and comparing them with models, it is found that M13 has a population of low-mass WDs, probably originating from binary evolution.
Author(s): Kumar R.; Pradhan A.C.; Sahu S.; Subramaniam A.; Piridi S.; Cassisi S.,Ojha D.K.
IVOA id: ivo://cds.vizier/j/mnras/522/847

JWST properties of high-z HST-dark galaxies

2026-07-27T12:48:47Z

Description: Over the last few years, both Atacama Large Millimeter/submillimeter Array (ALMA) and Spitzer observations have revealed a population of likely massive galaxies at z > 3 that was too faint to be detected inHubble Space Telescope (HST) rest-frame ultraviolet imaging. However, due to the very limited photometry for individual galaxies, the true nature of these so-called HST-dark galaxies has remained elusive. Here, we present the first sample of such galaxies observed with very deep, high-resolution NIRCam imaging from the Early Release Science programme CEERS. 30 HST-dark sources are selected based on their red colours across 1.6-4.4 {mu}m. Their physical properties are derived from 12-band multiwavelength photometry, including ancillary HST imaging. We find that these galaxies are generally heavily dust-obscured (A_V_ ~2 mag), massive (logM/M_{sun}_) ~10), star-forming sources at z ~ 2-8 with an observed surface density of ~0.8 arcmin^-2^. This suggests that an important fraction of massive galaxies may have been missing from our cosmic census at z > 3 all the way into the Epoch of Reionization. The HST-dark sources lie on the main sequence of galaxies and add an obscured star formation rate density of 3.2^+1.8^_-1.3_ * 10^-3^M_{sun}_/yr/Mpc^3^ at z ~ 7, showing likely presence of dust in the Epoch of Reionization. Our analysis shows the unique power of JWST to reveal this previously missing galaxy population and to provide a more complete census of galaxies at z = 2-8 based on rest-frame optical imaging.
Author(s): Barrufet L.; Oesch P.A.; Weibel A.; Brammer G.; Bezanson R.; Bouwens R.,Fudamoto Y.; Gonzalez V.; Gottumukkala R.; Illingworth G.; Heintz K.E.,Holden B.; Labbe I.; Magee D.; Naidu R.P.; Nelson E.; Stefanon M.; Smit R.,Van Dokkum P.; Weaver J.R.; Williams C.C.
IVOA id: ivo://cds.vizier/j/mnras/522/449

HST colors of ESO 137-001 tail stars

2026-07-27T12:46:00Z

Description: We present the results from the HST WFC3 and ACS data on an archetypal galaxy undergoing ram pressure stripping (RPS), ESO 137-001, in the nearby cluster Abell 3627. ESO 137-001 is known to host a prominent stripped tail detected in many bands from X-rays, H {alpha} to CO. The HST data reveal significant features indicative of RPS such as asymmetric dust distribution and surface brightness as well as many blue young star complexes in the tail. We study the correlation between the blue young star complexes from HST, H II regions from H {alpha} (MUSE), and dense molecular clouds from CO (ALMA). The correlation between the HST blue star clusters and the H II regions is very good, while their correlation with the dense CO clumps are typically not good, presumably due in part to evolutionary effects. In comparison to the STARBURST99 + CLOUDY model, many blue regions are found to be young (<10 Myr) and the total star formation (SF) rate in the tail is 0.3-0.6 M_{sun}_/yr for sources measured with ages less than 100 Myr, about 40 per cent of the SF rate in the galaxy. We trace SF over at least 100 Myr and give a full picture of the recent SF history in the tail. We also demonstrate the importance of including nebular emissions and a nebular to stellar extinction correction factor when comparing the model to the broad-band data. Our work on ESO 137-001 demonstrates the importance of HST data for constraining the SF history in stripped tails.
Author(s): Waldron W.; Sun M.; Luo R.; Laudari S.; Chatzikos M.; Sivanandam S.,Kenney J.D.P.; Jachym P.; Voit G.M.; Donahue M.; Fossati M.
IVOA id: ivo://cds.vizier/j/mnras/522/173

SB1s properties from GaiaDR3/TESS/ASAS-SN

2026-07-27T12:10:42Z

Description: Gaia Data Release 3 (DR3) provides >181000 radial velocity (RV) solutions for single-lined spectroscopic binaries (SB1s) that can be used to search for non-interacting compact object + star binary candidates by selecting systems with large mass functions. We selected 234 such systems and identified 115 systems with good RV solutions in DR3. We used light curves from the All-Sky Automated Survey for SuperNovae (ASAS-SN) and the Transiting Exoplanet Survey Satellite (TESS) to identify and remove 31 eclipsing binaries to produce a catalogue of 80 compact object + star candidates, including 38 ellipsoidal variables. The positions of these candidates on Gaia and Two Micron All-Sky Survey (2MASS) colour-magnitude diagrams (CMDs) suggest that many of these systems are binaries with luminous companions. We compared the periods and eccentricities of detached eclipsing binaries in Gaia DR3 and ASAS-SN, and found that ~11 per cent and ~60 per cent of the binaries had different periods and eccentricities. We also compared RV solutions for 311 binaries in both Gaia DR3 and the Ninth Catalogue of Spectroscopic Binary Orbits (SB9), and found similar results. We do not identify any strong candidates for non-interacting compact object + star binaries.
Author(s): Jayasinghe T.; Rowan D.M.; Thompson T.A.; Kochanek C.S.; Stanek K.Z.
IVOA id: ivo://cds.vizier/j/mnras/521/5927

Properties and asymmetries of QSOs host galaxies

2026-07-27T11:26:36Z

Description: How does the host galaxy morphology influence a central quasar or vice versa? We address this question by measuring the asymmetries of 2424 SDSS quasar hosts at 0.2 < z < 0.8 using broad-band (grizy) images from the Hyper Suprime-Cam Subaru Strategic Program. Control galaxies (without quasars) are selected by matching the redshifts and stellar masses of the quasar hosts. A two-step pipeline is run to decompose the PSF and Sersic components and then measure asymmetry indices (ACAS, Aouter, and Ashape) of each quasar host and control galaxy. We find a mild correlation between host asymmetry and AGN bolometric luminosity (Lbol) for the full sample (spearman correlation of 0.37) while a stronger trend is evident at the highest luminosities (L_bol_>45). This then manifests itself into quasar hosts being more asymmetric, on average, when they harbour a more massive and highly accreting black hole. The merger fraction also positively correlates with Lbol and reaches up to 35 per cent for the most luminous. Compared to control galaxies, quasar hosts are marginally more asymmetric (excess of 0.017 in median at 9.4{sigma} level) and the merger fractions are similar (~16.5 per cent). We quantify the dependence of asymmetry on optical band that demonstrates that mergers are more likely to be identified with the bluer bands and the correlation between Lbol and asymmetry is also stronger in such bands. We stress that the band dependence, indicative of a changing stellar population, is an important factor in considering the influence of mergers on AGN activity.
Author(s): Tang S.; Silverman J.D.; Yesuf H.M.; Ding X.; Li J.; Bottrell C.,Goulding A.; Omori K.C.; Toba Y.; Kawaguchi T.
IVOA id: ivo://cds.vizier/j/mnras/521/5272

Andromeda XXV new member stars kinematics

2026-07-27T10:01:31Z

Description: Andromeda (And) XXV has previously been reported as a dwarf spheroidal galaxy (dSph) with little-to-no dark matter. However, the uncertainties on this result were significant. In this study, we nearly double the number of member stars and re-derive the kinematics and mass of And XXV. We find that And XXV has a systemic velocity of v_r_ = -107.7 +/- 1.0 km/s and a velocity dispersion of {sigma}_v_ = 3.7^+1.2^_-1.1_ km/s. With this updated velocity dispersion and a new literature measurement of the radial surface brightness profile, we derive a mass contained within the half-light radius of M(r < r_h_) = 4.79^+3.0^_-2.9_ * 10^6^ M_{sun}_. This mass corresponds to a mass-to-light ratio of [M/L]_rh_ = 25^+17^_-16_ M_{sun}_/L_{sun}_, demonstrating that And XXV is most-likely dark matter dominated. We also measure the metallicity of And XXV to be [Fe/H] = -1.9 +/- 0.1 dex, which is in agreement with previous results. Finally, we extend the analysis of And XXV to include mass modelling using GravSphere. We find that And XXV has a low central dark matter density, {rho}_DM_(150 pc) = 2.3^+1.4^_-1.1_ * 10^7^ M_{sun}_ kpc^-3^, which makes And XXV a clear outlier when compared to other local group dSphs of the similar stellar mass. In a companion paper, we will explore whether some combination of dark matter cusp-core transformations and/or tides can explain And XXV's low density.
Author(s): Charles E.J.E.; Collins M.L.M.; Rich R.M.; Read J.I.; Kim S.Y.; Ibata R.A.,Martin N.F.; Chapman S.C.; Balbinot E.; Weisz D.R.
IVOA id: ivo://cds.vizier/j/mnras/521/3527