VO Fresh

Gaia-ESO HR15N Ba and Eu abundances

2026-09-20T16:20:57Z

Description: Neutron-capture element abundances encode the time-dependent interplay between slow (s-) and rapid (r-) nucleosynthetic processes and provide critical constraints on Galactic chemical evolution. In particular, barium and europium provide important tracers of s-process and r-process nucleosynthetic enrichment, respectively. Large spectroscopic surveys enable robust statistical studies of these elements; however, determining reliable elemental abundances at intermediate spectral resolution remains challenging. Our aim was to derive homogeneous and statistically well-characterised stellar parameters and chemical abundances of Ba and Eu (hereafter collectively referred to as stellar labels) for the Gaia-ESO Survey HR15N dataset. We applied The Cannon to 36263 FLAMES/GIRAFFE HR15N spectra (R~19200, lambda~6440-6815 Angstrom), using a model trained on 782 stars with high-quality reference stellar labels drawn from the Gaia-ESO DR5 homogenised catalogue. The model infers Teff, logg, [Fe/H], vsini, A(Ba), and A(Eu); its reliability was quantified through multi-dimensional quality flags for the labels and detection strength of the Ba and Eu features. The uncertainties in the inferred stellar labels were obtained by combining the model's internal label-covariance errors with signal-to-noise-dependent dispersions. Our final catalogue contains stellar parameters for 36263 spectra, with ~21000 and ~400 reliable Ba and Eu abundances, respectively, satisfying multiple flagging criteria. We obtained median uncertainties of ~38K in Teff, ~0.08dex in logg, ~0.04dex in [Fe/H], ~0.06dex in A(Ba), and ~0.02dex in A(Eu). External validation against the Gaia Benchmark Stars, GALAH DR4, and multiple open clusters shows good agreement across independent reference datasets. This study provides a comprehensive dataset of neutron-capture abundances in the Galactic disc observed with the Gaia-ESO HR15N set-up. The resulting catalogue includes newly determined Ba and Eu abundances that complement those available from previous analyses, thereby enabling well-characterised investigations of neutron-capture enrichment patterns in open clusters. The model framework can readily be adapted to upcoming wide-field spectroscopic surveys such as 4MOST, WEAVE, and WST.
Author(s): Das P.B.; Primas F.; De Silva G.; Guiglion G.; Zucker D.B.; Ness M.
IVOA id: ivo://cds.vizier/j/a+a/713/a148

SMC red giants CaII triplet metallicities

2026-09-18T10:53:14Z

Description: Taking advantage of the near-infrared calcium triplet lines, we determine metallicities for a sample of more than 3500 red giant stars in the field of the Small Magellanic Cloud. We find a median metallicity of [Fe/H]=-1.05_/-0.01dex with a negative metallicity gradient of -0.064+/-0.007dex/deg between 1.2{deg} and 6.0{deg} consistent with an outside-in evolution scenario. For the first time, we detect hints of a positive metallicity gradient within 1.2{deg}, likely reflecting radial migration or centralized chemical enrichment. Azimuthal metallicity asymmetries are detected, with flatter gradients in the eastern and southern quadrants and steeper ones in the north and west. They are consistent with tidal interaction effects from the Large Magellanic Cloud. Finally, in spite of a clear distance and velocity bifurcations in the east, they seem to share a common chemical origin, in agreement with other studies.
Author(s): Navabi M.; Carrera R.; Noel N.E.D.; De Leo M.
IVOA id: ivo://cds.vizier/j/mnras/544/3980

eta Car historical light curves

2026-09-18T09:10:56Z

Description: The large amount of ground-based photometric measurements of eta Carinae obtained since 1940 have remained problematic for quantitative modeling due to the blending of flux from the stellar core and the surrounding circumstellar nebula. In the era of the Hubble Space Telescope (HST), spatially resolved imaging and spectrophotometry have enabled disentanglement of these components, allowing recovery of the stellar core V-band brightness from ground-based observations. We isolate the V-band fluxes of the stellar core and nebula using 1999-2020 HST (Advanced Camera for Surveys and Space Telescope Imaging Spectrograph) observations, and use these to calibrate coeval ground-based photometry. The main finding is an orbital light curve with an amplitude of +/-0.2mag, many times higher than that modeled by ellipsoidal deformation of the primary. The observations suggest that Roche lobe overflow starts at -75 days before periastron in coincidence with the start of rising in the orbital light curve, and remains for 150 days. An expanding (and afterward dissipating) gas cloud reflecting the light from the primary would explain the observed large amplitude of the orbital light curve. A sharp periodic photometric peak occurs at ~-18 days from the periastron. It is followed by a broad minimum around the superior conjunction of the secondary (T0 + 5.2 days), which we interpret as a partial eclipse of the ejected material, in coincidence with the shallow minimum in X-rays, which also has been attributed to an eclipse.
Author(s): Damineli A.; Almeida L.A.; Jablonski F.J.; Fernandez-Lajus E.; Navarete F.,Martioli E.; Weigelt G.; Capobiango R.
IVOA id: ivo://cds.vizier/j/apj/1008/152

The Blue Jay JWST galaxy sample properties

2026-09-18T09:02:49Z

Description: We present the Blue Jay survey, a Cycle-1 JWST program aimed at studying the stellar and gas content of galaxies at Cosmic Noon. The survey consists of deep spectroscopy for 153 targets observed over two pointings in the COSMOS field using the NIRSpec micro-shutter assembly (MSA). We employ the three medium-resolution gratings G140M, G235M, and G395M, with exposure times of 13 hours, 3.2 hours, and 1.6 hours, respectively. We thus obtain full coverage of the 1-5 {mu}m range, corresponding to the entire rest-frame optical wavelength range, with a spectral resolution R~1000. Parallel observations provide deep, multi-band NIRCam imaging, which partially overlaps with the spectroscopic observations. The sample is carefully selected to provide a census of galaxies over the redshift range 1.7<z<3.5 above a redshift-dependent minimum stellar mass that ranges from 10^8.7^M_{sun}_ to 10^9.3^M_{sun}_. The selection ensures that the Blue Jay sample is representative of the entire galaxy population at these redshifts, without strong biases in color, star formation rate, or other properties. The sizes of massive galaxies at these redshifts are comparable to, or larger than the NIRSpec shutters, which requires custom strategies for designing and reducing the observations. Since the standard A-B nod subtraction leads to flux self-subtraction for large galaxies, we construct a master background from empty shutters and subtract it from each of the science spectra. This, in turn, allows for the use of shorter slitlets consisting of only two shutters per galaxy instead of the usual three, with a substantial increase in the multiplexing of the NIRSpec MSA. Another problem introduced by the small shutter size is the mismatch between the galaxy region probed by NIRSpec and that probed by photometric measurements. For this reason, we measure multi-band photometry using archival JWST and Hubble Space Telescope observations in two different ways: source photometry is measured in a large elliptical aperture encompassing the entire source, while box photometry is measured from the exact area in the sky where the NIRSpec 1D spectrum is extracted. This enables self-consistent fits of spectroscopic and photometric data. The Blue Jay dataset, which we publicly release, represents the ideal sample for studying the stellar populations, neutral gas, and ionized gas in Cosmic Noon galaxies, including star formation histories, quenching, outflows, metallicity, and dust attenuation.
Author(s): Belli S.; Bugiani L.; Park M.; Mendel J.T.; Davies R.L.; Khoram A.H.,Johnson B.D.; Leja J.; Tacchella S.; Brown V.; Conroy C.; Emami R.; Li Y.,Liboni C.; Maheson G.; Mathews E.P.; Naidu R.P.; Nelson E.J.,Terrazas B.A.; Weinberger R.
IVOA id: ivo://cds.vizier/j/a+a/713/a237

First NenuFAR pulsar catalog

2026-09-18T08:43:32Z

Description: The radio frequency range below 100 MHz has been unexplored until recently for extended pulsar population studies. We present the first low-frequency pulsar census of the northern sky with the NenuFAR radio telescope (10-85 MHz), performed during its commissioning and early science phase in 2019-2021. Our programme was conceived as the first stepping stone of a future pulsar key science project, aimed at preparing for targeted studies on pulsars of peculiar interest (mode switching, drifting subpulses, and polarised emission), exploring pulsar spectra and pulse-shape evolution below the expected turn-over, and investigating dispersion and scattering due to the interstellar and heliospheric plasma. We observed all known pulsars observable from the Nancay Radio Observatory in France, i.e. with a declination above -20{deg} and dispersion measures (DMs) up to 100pc/cm^-3^. At the time of the sample selection, 576 pulsars fulfilled these criteria in the ATNF pulsar catalogue. We complemented this sample with 69 additional LOTAAS/LOFAR pulsars, yielding 645 observed pulsars. We used the 56 mini-arrays available in the NenuFAR core (i.e. 1064 antennas), corresponding to ~58% of the nominal collecting area. Targets were observed for between 25 and 180 minutes, depending on their elevation and nature (regular or millisecond pulsars). We detected 182 pulsars in the frequency range 10-85MHz, 89 of which had never been seen before in this range. We detected 13 millisecond pulsars, ten of which are new detections below 100MHz. We measured new DMs, scattering indices, duty cycles, and calibrated fluxes for all of them. The typical minimum detectable pulse was 1-2mJy for MSPs and 5-10mJy for the regular population. We release full-band phasograms for all targets, with frequency-resolved pulse profiles where the pulsar was bright enough.
Author(s): Bondonneau L.; Griessmeier J.-M.; Theureau G.; Cognard I.; Jankowski F.,Kondratiev V.; Kravtsov I.; Petri J.; Possenti A.; Ulyanov O.,Zakharenko V.; Brionne M.; Cecconi B.; Corbel S.; Girard J.N.,Konovalenko O.; Tokarsky P.; Zarka P.
IVOA id: ivo://cds.vizier/j/a+a/713/a224

Gaia FGK benchmark stars. n-capture abundances

2026-09-18T08:30:13Z

Description: In the current era, in which an unprecedented wealth of data are available for the study of the Milky Way, Gaia benchmark stars (GBSs) have become an established reference and calibration sample. Studies of stellar structure and evolution and of the chemical history of our Galaxy generally rely on large spectroscopic surveys and their output catalogs. In this context, deriving precise and accurate stellar parameters and chemical abundances is of paramount importance. This study provides the determination of neutron-capture element abundances and extends the set of chemical abundances available for the third GBS release (GBSv3). Based on the compilation of high-resolution spectra assembled for GBSv3 and consistent with the spectral analysis adopted for the chemical abundances of GBSv3, we used the public iSpec code to derive heavy element abundances. We inferred homogeneous abundances of neutron-capture elements (Y, Zr, Mo, Ba, La, Ce, Pr, Nd, and Eu) across the GBSv3 sample using an in-depth line assessment tailored to different groups identified through a clustering algorithm that accounts for the diversity in stellar parameters and metallicities. This approach addresses key challenges in the spectral analysis of these elements, including the paucity of usable lines, weak line strengths, saturation effects, and sensitivity to atomic data. The assessment yielded reliable measurements, establishing an extended and robust reference scale in good agreement with the literature. This compilation of neutron-capture abundances is based on the GBS sample's robust and accurate atmospheric parameters and the analysis of a large sample of stellar spectra per star, which provides a reliable and homogeneous spectral analysis. It also supports the use of chemical abundances as precise tracers of the Milky Way's star formation history and chemical evolution and constitutes a legacy sample for the calibration of current and future spectroscopic surveys.
Author(s): Vitali S.; Jofre P.; Casamiquela L.; Soubiran C.; Heiter U.,Aguilera-Gomez C.; Barrios-Lopez D.; Blanco-Cuaresma S.; Escorza A.,Hernandez-Araya I.; Signor T.; Sinclair-Wentworth H.; Worley C.
IVOA id: ivo://cds.vizier/j/a+a/713/a219

AMS-02 All Particle Rates Catalog

2026-09-18T00:00:00Z

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

2026-09-18T00:00:00Z

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

2026-09-18T00:00:00Z

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)

2026-09-18T00:00:00Z

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

Reddening maps of the Magellanic Clouds

2026-09-17T08:13:18Z

Description: Robust reddening maps of the Large and Small Magellanic Clouds (LMC and SMC) are crucial for a wide range of astrophysical studies, including the calibration of the cosmic distance ladder, investigations of stellar populations in low-metallicity environments, and the characterization of interstellar dust properties. We aim to construct reddening maps of the Magellanic Clouds using spectral energy distribution (SED) fitting and to investigate the impact of different stellar atmosphere models on the resulting maps. We combined optical (ugriz) photometry from the SMASH survey with near-infrared (YJKs) photometry from the VMC survey for red giant branch (RGB) stars. We matched the observed SEDs to synthetic photometry derived from three atmosphere model grids. Our maps cover 34.5deg^2^ of the LMC and 24.5deg^2^ of the SMC at 4-arcmin resolution. We find mean reddening values of E(B-V)=0.076 +/-0.022mag for the LMC and 0.058+/-0.024mag for the SMC. We find that employing different atmospheric models results in differences of up to 0.03 mag in the mean reddening. Canonical RV values for the Magellanic Clouds (3.41 for LMC and 2.74 for SMC; Gordon et al., 2003ApJ...594..279G) provide results consistent with previous studies. We confirm a higher and more structured reddening in the LMC compared to the SMC, with 30 Doradus standing out as the dominant high-reddening region. Our results show that the absolute reddening scale depends on the choice of stellar atmosphere models, while the relative spatial structure of the reddening maps remains stable.
Author(s): Netzel H.; Pietrzynski G.; Gorski M.; Kervella P.; Hajdu G.,Kudritzki R.; Chini R.; Kiviaho W.; Zgirski B.; Wielgorski P.,Graczyk D.; Gieren W.
IVOA id: ivo://cds.vizier/j/a+a/713/a201

M3W. I. DIB characteristics

2026-09-17T08:12:14Z

Description: Multiplicity is ubiquitous among massive stars and our knowledge of its processes is constrained by the limited sample of well-determined orbits, hampering progress across astronomical fields ranging from the initial mass function to gravitational-wave sources. The immediate goal of Multiplicity of Massive stars in the Milky Way (hereafter, M3W) is to significantly increase the number of massive multiple systems with accurately determined orbits and masses. With that information in hand, we are equipped to address issues such as multiplicity statistics, the mass function in clusters and the field, the properties of binaries with compact companions and gravitational-wave progenitors, the origin and characteristics of runaways and their 3D motions, the use of apsidal motion as a probe of stellar interiors, and the mass discrepancy between different methods (i.e. evolutionary, spectroscopic, and Keplerian). In this first paper, we present the project, describe the data and tools we plan to use, along with an explanation of how to apply the UNWIND tool for disentangling and analysing the very massive twin binary system GLS 11 448. We describe different issues related to massive-star multiplicity that will be analysed in the series. At the start, GLS 11 448 has been chosen as the first object to be analysed for three reasons: the extreme high mass of its components, the difficulties associated with its high extinction that can be addressed with our technique, and its status as an standard star for the interstellar medium (ISM). We present a new orbital solution for GLS 11 448 using UNWIND to obtain, for the first time, disentangled spectra for the full 3820-11000{AA} range for an OB spectroscopic binary. Having derived the stellar parameters, we have the ability to explain how UNWIND makes new stellar lines available for the study of O stars. The Aa and Ab components of GLS 11 448, both classified as O3.5 II(f*), are the two most massive O stars ever detected according to the evolutionary masses of 70+/-10M_{sun}_ and 76+/-11M_{sun}_ determined in this paper. We also report the first-ever detection of the interstellar HeI {lambda}10 830 triplet in absorption in an OB-star sightline. As a byproduct of the interstellar-medium model derived for UNWIND using GLS 11 448 and five other standard stars, we present the most detailed diffuse-interstellar-band (DIB) library ever built, with a total of 631 DIBs in the 4000-17100{AA} range, 37 of which have been fitted with multiple-Gaussian profiles and 116 had never been identified before.
Author(s): Maiz Apellaniz J.; Gamen R.C.; Holgado G.; Rosu S.; Arias J.I.,Simon-Diaz S.; Pellerin A.; Abdul-Masih M.; Madero Fuentes E.,Molina-Calzada J.A.; Barba R.H.
IVOA id: ivo://cds.vizier/j/a+a/713/a177

The WISE catalog of Galactic H II regions. v3.0

2026-09-16T12:26:34Z

Description: The WISE Catalog of Galactic HII Regions is a catalog of HII regions and candidates, compiled from Widefield Infrared Survey Explorer (WISE) 12um and 22um data. It was created by Loren Anderson, Thomas Bania, Dana Balser, Virginia Cunningham, Trey Wenger, Brittany Johnstone, and William Armentrout, with help from numerous students at West Virginia University.
Author(s): Anderson L.D.; Bania T.M.; Balser D.S.; Cunningham V.; Wenger T.V.,Johnstone B.M. and Armentrout W.P.
IVOA id: ivo://cds.vizier/ii/392

gr8stars. II.

2026-09-16T11:29:09Z

Description: Many areas of astrophysics, including exoplanetary studies, rely on precise and accurate stellar parameters. This demands that uncertainties on these parameters truly reflect all biases and systematics. Within this second work of the gr8stars collaboration, we take a set of 585 bright FGK type dwarfs with high resolution, high signal-to-noise ratio spectra from the SOPHIE (Spectrographe pour l'Observation des Phenomenes des Interieurs stellaires et des Exoplanetes) spectrograph. We determine stellar effective temperature, surface gravity, and metallicity using five different spectroscopic methods for each star, with an additional method used for comparisons. We find a typical scatter of 76K in Teff, 0.14dex in logg, and 0.07dex in [Fe/H]. These deviations are significantly larger than the average precision error on these parameters. We furthermore use isochrone fitting to determine mass, radius, and age for all 585 stars, using input from all results. We use the radii determined by SED (Spectral Energy Distribution) fitting in the first gr8stars paper as a comparison to our isochronal radii from this work, in addition to comparing the isochronal logg to spectroscopic logg. The scatter in mass and radius from the use of different spectroscopic methods is investigated and propagated to exoplanetary parameters. The induced fractional uncertainties in planetary radius (<~3 per cent) and mass (<~5 per cent) are found to be below those typically found in the literature. We estimate a lower limit on planetary equilibrium temperature fractional uncertainty of ~4 per cent, a noise floor that is currently not sufficiently represented in the literature.
Author(s): Freckelton A.V.; Mortier A.; Bedell M.; Cretignier M.; Kolecki J.R.,Korn A.J.; Sousa S.G.; Tsantaki M.; Brewer J.M.; Buchhave L.A.; Davies G.R.,Gonzalez Hernandez J.I.; Morrell S.; Nielsen M.B.; Passegger V.M.,Quirrenbach A.; Roy A.; Santos N.C.; Suarez Mascareno A.; Watson C.A.,Zhao L.L.
IVOA id: ivo://cds.vizier/j/mnras/549/g1070

M-type AGB stars wind and dust models

2026-09-16T08:46:41Z

Description: Mass loss from asymptotic giant branch (AGB) stars is the result of a complex interplay between pulsation, atmospheric dynamics, dust formation, and radiative acceleration. Pulsation periods are a key input in dynamical atmosphere and wind models, and different prescriptions for assigning periods based on stellar parameters may lead to systematic differences in the predicted wind properties. To better constrain this critical parameter, we investigate how the choice of pulsation period affects the wind properties of dynamical atmosphere and wind models of M-type AGB stars by comparing models based on an empirical period-luminosity (P-L) relation with corresponding ones adopting a period-mean density relation derived from 3D pulsation models. We analyse two grids of DARWIN models covering a range of current stellar masses, luminosities, and effective temperatures. For each grid, pulsation periods are assigned using either the P-L relation or the period-mean density relation, allowing for a direct comparison of the resulting dynamical structures and wind properties for pairs of models differing by period only. Independent of the adopted period prescription, the time-averaged wind properties correlate strongly with L*/M*. The pulsation period affects the atmospheric dynamics through changes in the relative timing of shock propagation and dust formation, affecting both wind formation and the resulting wind properties. Shorter periods favour the onset of a wind, and models differing only in pulsation period can exhibit significantly different wind properties. The period-mean density relation provides a physically motivated alternative to the empirical P-L relation by accounting for stellar parameters beyond luminosity, and enables a more direct comparison between DARWIN models and observed Mira variables.
Author(s): Siderud E.; Eriksson K.; Hoefner S.; Ahmad A.
IVOA id: ivo://cds.vizier/j/a+a/713/a210

Revisiting TOI-4438 and TOI-442

2026-09-16T08:45:28Z

Description: We present a comprehensive re-analysis of two star-planet systems: TOI-4438, an M3.5V star hosting a mini-Neptune in a 7.4-day orbit, and TOI-442, an M1V star with a 4-day period planet located within the hot Neptune desert. Both systems were originally identified as transiting planet candidates by the Transiting Exoplanet Survey Satellite (TESS) and subsequently validated through the radial velocity (RV) method. Our work incorporates new TESS transit data and high-resolution spectroscopy from the SPIRou near-infrared (nIR) spectropolarimeter. We detect a persistent and relatively strong Zeeman signature in TOI-442, while TOI-4438 exhibits weaker and intermittent magnetic activity, and we infer the stellar rotation periods of both stars from the variability of the longitudinal magnetic field. We jointly fit photometry and RV models for each system. For TOI-4438 b we combine archival CARMENES data with 81 SPIRou observations and five TESS sectors. This yields a refined planetary mass of Mp=4.11^+0.40^_-0.38_M_{Earth}_ and a radius of Rp=2.40^+0.09^_-0.10_R_{Earth}_, consistent with the previous estimate within 1.1 sigma while improving by 53% the precision on the mass and 22% on the radius. For TOI-442 b, we add 29 SPIRou RV measurements to an extensive archival dataset, significantly extending the temporal baseline. Incorporating this with a new TESS sector, we tighten the constraints on the planetary mass to Mp=28.38^+0.77^_-0.73_M_{Earth}_ and radius to Rp=4.25^+0.10^_-0.08_R_{Earth}_, which agrees to the previous values within 1.5 sigma and improves the precisions by 46% and 67% respectively. We find no clear signs of additional planets in the currently available RV data, although we detect a single-transit event in the TOI-4438 light curve. We compare various RV models and find that those accounting for stellar variability-induced signals yield improved constraints on the planetary parameters.
Author(s): Serrano Bell J.; Hebrard G.; Martioli E.; Diaz R.F.; de Almeida L.,Lorenzo-Oliveira D.; Salmi A.; Dorn C.; Valatsou M.; Carmona A.,Ould-Elhkim M.; Arnold L.; Artigau E.; Boisse I.; Bonfils X.; Cadieux C.,Chakir Z.; Cook N.J.; Delfosse X.; Donati J.-F.; Doyon R.; Heidari N.,Jenkins J.M.; Kiefer F.; Lafrance S.; L'Heureux A.; Moutou C.,Morneau J.; Vandelac X.
IVOA id: ivo://cds.vizier/j/a+a/713/a166

Galactic plane WR stars at 1.3GHz

2026-09-16T08:39:59Z

Description: Massive stars, including Wolf-Rayet stars (WR), are found mainly in binary systems. These systems are known to emit both thermal emission from stellar winds and sometimes non-thermal emission produced by relativistic electrons accelerated in the wind-wind interaction region. We intend to provide the most complete census of radio emission from WR stars in the Galactic plane, using the SARAO Meerkat Galactic Plane Survey (SMGPS) complemented by the MeerKAT Galactic Center Survey (MGCS). Our main motivation is to identify hints of synchrotron radio emission indicative of particle-accelerating colliding-wind binaries (PACWB). We compiled an input catalogue of 428 WR stars positionally covered by the SMGPS and the MGCS. Using the Survey data, we measured the radio emission at 1.3GHz for detected WR stars, and we measured the upper limits for objects located in sufficiently low radio background regions. For detected objects, we searched for a radio excess by comparing the measured fluxes to two different evaluators of the thermal emission from massive star winds. We detected 23 targets and determined the upper limits for 279 WR stars. Among the detected objects, 15 display a (significant or potential) radio excess that cannot be explained by unresolved circumstellar emission of any kind. Removing already known PACWBs, we report on the identification of 12 potential new PACWB candidates. Our study led to the compilation of the most extensive catalogue of Galactic WR radio (snapshot) emission to date, based on a homogeneous data set covering the Galactic plane. The low detection rate indicates either a low occurrence rate of synchrotron emission or substantial attenuation by turnover processes, certainly dominated by free-free absorption from the WR wind material. Our results open the door for dedicated follow-up observations to ascertain the nature of the identified radio excesses.
Author(s): Tasseroul M.; De Becker M.; Benaglia P.; Tej A.
IVOA id: ivo://cds.vizier/j/a+a/713/a154

K2-312 (HD 80653) RVs and activity index

2026-09-16T08:34:26Z

Description: The architecture of planetary systems hosting ultra-short-period (USP) planets is a key diagnostic for understanding formation and migration scenarios. The presence of outer giant companions in these systems is of particular interest to test theories regarding dynamical effects and pebble accretion. We present an extended radial velocity (RV) monitoring of the bright star K2-312=HD 80653, known to host a rocky USP super-Earth (Pb=0.720d). Previous studies identified a long-term trend and subsequently a Keplerian signal due to an outer highly eccentric giant planet, K2-312 c. We aim to refine the orbital parameters of K2-312 c by precisely monitoring its periastron passage and to model the formation and dynamical evolution of the system. We analyzed a set of 237 HARPS-N high-resolution spectra, extending the observation baseline of previous literature by almost 4 years. We performed a joint analysis of the RVs together with K2 and TESS photometry to refine the ephemerides and properties of the two planets. To account for stellar activity, we coupled the Keplerian models with a Gaussian processes regression. K2-312 c is a cold Jupiter on a wide orbit (orbital period refined to Pc=871.32d), with a minimum mass of Mc*sini~5M_{Jup}_ and a refined eccentricity of e_c_~0.85. It is among the most eccentric cold Jupiters known in multi-planet systems, and the only one that is highly eccentric and has a USP planet companion. Our simulations suggest that planet-planet scattering between two giant planets could have driven K2-312 c to its current high eccentricity, ejected the other giant, and still allowed for the survival of K2-312 b. The extended observation baseline further allowed us to identify the stellar rotation period and a long activity cycle, while a new K2 reduction improved the significance of the secondary eclipse detection for K2-312 b.
Author(s): Naponiello L.; Poretti E.; Rice K.; Bonomo A.S.; Malavolta L.; Stalport M.,Vanderburg A.; Ziegler C.; Affer L.; Cecconi M.; Collier Cameron A.,Cosentino R.; Damasso M.; Dumusque X.; Eschen Y.N.E.; Ghedina A.,Latham D.W.; Lopez-Morales M.; Lu T.; Massa A.; Mortier A.; Nicholson B.A.,Palethorpe L.; Pepe F.A.; Sozzetti A.; Udry S.; Wilson T.G.
IVOA id: ivo://cds.vizier/j/a+a/713/a140

Orion B cores maps physical properties

2026-09-16T08:14:08Z

Description: Pre-stellar cores are the sites of the earliest stages of star formation. Dust continuum observations are often used to identify and characterize their properties yet only a small fraction of them was observed and studied in terms of their composition and dynamical status. Pre-stellar cores are often analysed as being analogous to template objects such as L1544 in Taurus, which could create an observational bias if this template is not representative of all possible prestellar cores. We explore the chemical diversity of prestellar cores and protostellar cores residing in the Orion B giant molecular cloud selected on their dust continuum emission to provide an unbiased view of their line emission properties and how they vary as function of the core parameters and environment. We make use of the large scale maps of Orion B in 25 molecular lines from which we extract information for a sample of 1001 cores selected using positions extracted from Herschel dust continuum observations. The main properties of the core sample are derived using the Principal Component Analysis and additional maps of physical parameters: column density N_H2_, far-ultraviolet (FUV) radiation field G0 and mean volume gas density n. Additional high spectral resolution observations of C^18^O(1-0) serve to evaluate the dynamical status of cores. The average line width of the cores is larger than what is typically expected for prestellar cores of closer star forming regions, which suggests that cores in Orion B are subjected to stronger turbulence affecting their stability. The first factor of the PCA analysis explaining the variation of the detected line intensities is the core column density of molecular gas. The second factor explains how the core chemical composition is strictly linked to their environment, which can be traced by the ratio of the external FUV radiation field over the core volume density, G0/n. Cold and shielded cores exhibit strong emission of N_2_H^+^, CH_3_OH and deuterated species, whereas cores exposed to radiation are devoid of typical core tracers, but exhibit emission of ^12^CN, HCO^+^ and HCN. The third factor explaining the core chemical diversity is the mean density along the core line of sight, which is also associated with freeze-out and fractionation signatures. Pre-stellar cores selected based on their dust emission exhibit a wide range of line emission patterns, which can be related to their intrinsic properties (column density N_H2_, mean volume density n) and environment (presence or lack of FUV). The key parameter that distinguishes cores of different emission patterns is G0/n.
Author(s): Mazurek H.J.; Gerin M.; Gratier P.; Pety J.; Bron E.; Roueff E.; Roueff A.,Beslic I.; Einig L.; Orkisz J. H.; Palud P.; Santa-Maria M. G.; Segal L.,Zakardjian A.; Bardeau S.; Chainais P.; Coude S.; Demyk K.,de Souza Magalhaes V.; Goicoechea J.R.; Hughes A.; Languignon D.,Levrier F.; Le Petit F.; C.L. Dariusz C.; Liszt H.S.; Peretto N.,Sievers A.; Thouvenin P.-A.
IVOA id: ivo://cds.vizier/j/a+a/713/a137

J1030 field radio heavily obscured AGN

2026-09-15T17:43:34Z

Description: Models of supermassive black holes (SMBHs) and galaxy coevolution, simulations, and recent JWST observations suggest that the population of heavily obscured, Compton-thick (CTK) active galactic nuclei (AGNs) at high redshift might be underestimated by X-ray surveys. To retrieve a complete census of SMBHs it is therefore necessary to identify new and complementary methods to select these sources, for example by exploiting the radio band as radio waves are almost unaffected by obscuration. We aim to test the effectiveness of radio selection to discover heavily obscured AGNs, particularly at high z, and, in turn, measure their abundance for the first time from a radio perspective. We considered the radio sources detected in the J1030 field, which is one of the fields with the deepest combination of 1.4GHz radio and X-ray observations publicly available. We defined a radio excess parameter as the ratio between the star formation rate (SFR) that would correspond to the observed radio luminosity and the one directly derived from the spectral-energy-distribution (SED) fitting, REX=SFR_1.4GHz_/SFR^corr^_SED_. We then selected sources with REX>8.5 as radio- excess AGNs; this corresponds to a 3{sigma} excess above the median value (REX~1). In this way, we find 145 radio-excess sources falling in the Chandra X-ray image footprint but without X-ray detection. From the deep X-ray upper limits, we estimated a lower limit to the obscuration of each radio- excess AGN, finding on average log(N_H_/m{cm^-2^)>23.7. A CTK AGN scenario is also supported by the results of the X-ray stacking analysis performed on sources at z>1.5, which revealed X-ray luminosities and hardness ratios compatible with very highly obscured AGNs. Finally, we computed the number density of these radio-selected CTK AGNs. While at z~2 the radio number density agrees well with the CTK AGN predictions of different population synthesis models, at z~3 the radio selection returns a CTK AGN number density ~2-3 times larger than what is predicted by the CXB models and X-ray observations. This result supports the effectiveness of radio emission in selecting the most obscured sources, unraveling a population of AGNs potentially missed by X-ray surveys at z>3; this paves the way to a synergistic use of the future radio and X-ray facilities such as the Square Kilometer Array Observatory (SKAO), NewAthena, and the Advanced X-ray Imager Satellite (AXIS).
Author(s): Mazzolari G.; Gilli R.; Mignoli M.; Brusa M.; Prandoni I.; Vito F.,Delvecchio I.; Lanzuisi G.; Peca A.; Comastri A.; Marchesi S.; Chiaberge M.,Brienza M.; Vignali C.; Signorini M.; D'Amato Q.; Gentile F.; Iwasawa K.,Norman C.; Traina A.; Loiacono F.; Baldini P.; Annunziatella M.; Decarli R.
IVOA id: ivo://cds.vizier/j/a+a/713/a139

Hierarchical mass cascade in W43-MM1

2026-09-15T17:42:04Z

Description: The gravoturbulent fragmentation of the interstellar medium is expected to create a hierarchical cascade of cloud structures, crossing the scales from core to disk. We aim to predict how the currently observed top-heavy core mass function (CMF) in the massive protocluster W43-MM1 evolves due to core subfragmentation. We used the getsf algorithm to extract sources in five ALMA images of W43-MM1 at 3mm, with a spatial resolution ranging from 14kau to 270au. Then, we applied FAMILY, a graph-theory-based analysis tool, to create and characterize networks of nested sources in W43-MM1. We compared the hierarchical fragmentation cascade of W43-MM1 to those measured in the NGC 2264 protocluster and in synthetic images of an Orion-like protocluster simulated by magneto-hydrodynamical calculations. Assuming self-similarity, we measured a small fractality index of F3D=1.19+/-0.10 in W43-MM1, which means that, on average, a cloud structure fragments into only 1.19 fragments each time the physical scale decreases by a factor of two. In line with values measured above the core scale in the NGC 2264 and synthetic protoclusters, the W43-MM1 fractality index increases by about 30% at larger scales. We also estimate an imbalanced mass partition between siblings, with two-thirds of the mass of siblings at a given scale belonging to the dominant sibling. The mass transfer efficiency, computed from one physical scale to another, is high and corresponds to a core formation efficiency (CFE) from 2400 au cores to 200au seeds of ~16%. Based on the fractality and efficiency values measured in W43-MM1, the gravoturbulent model by Thomasson predicts that its fragmentation below ~14kau is not driven by turbulence but by gravity. Using these parameters and the measured mass partition, we demonstrate that the seed mass function, from which the initial mass function (IMF) emerges, has a high-mass end that remains top-heavy. Therefore, based on our current assumptions, core subfragmentation in W43-MM1, and perhaps more broadly in massive Galactic protoclusters, plays a minimal role in shaping the high-mass slope of the IMF.
Author(s): Motte F.; Le Nestour N.; Veyry R.; Brouillet N.; Nony T.; Thomasson B.,Louvet F.; Joncour I.; Moraux E.; Men'shchikov A.; Yoo T.; Ginsburg A.,Gusdorf A.; Stutz A.M.; Galvan-Madrid R.; Csengeri T.,Alvarez-Gutierrez R.H.; Armante M.; Bernard Y.; Bonfand M.; Chevalier S.,Cunningham N.; Dell'Ova P.; Gonzalez M.; Koley A.; Olguin F.A.; Panda D.,Pouteau Y.; Salinas J.; Sanhueza P.; Sandoval-Garrido N.A.,Valeille-Manet M.
IVOA id: ivo://cds.vizier/j/a+a/713/a105

Silicate and Carbonaceous collisions

2026-09-15T07:15:20Z

Description: Observations have revealed the presence of silicate and carbonaceous material in interstellar grains, however, these components are generally assumed to belong to distinct dust populations. While some dust models do incorporate mixed silicate-carbonaceous grains, there is little evidence to support grain mixing mechanisms. In this work, we use atomistic simulations to investigate collisions between silicate and carbonaceous nanograins at velocities representative of a range of astrophysical environments. Our overall objective is to determine how collision velocity governs the interactions between silicate and carbonaceous nanograins. We aim to: i) identify collisional regimes capable of producing mixed silicate-carbonaceous grains and/or chemically complex molecular species; and ii) quantify fragmentation threshold velocities related to dust destruction. We performed molecular dynamics simulations employing a machine-learning force field to model head-on collisions between silicate and carbonaceous nanograins of comparable masses. Collision velocities span 1 to 11km/s . For all collisions, we tracked the extent of grain-grain mixing and the formation of molecular fragments. We identified four velocity regimes: 1) <~1.5km/s, where grains bounce off one another; 2) ~1.5-3.5km/s, where sticking between the grains starts to occur; 3) ~3.5-7.5km/s, where grains tend to aggregate and form inter-grain chemical bonds, yielding stable mixed grains; and 4) >~7.5km/s, where fragmentation dominates. The latter regime produces CO as the main product, along with hydrocarbons, complex organic molecules, molecular silicates, and mixed carbonaceous-silicate clusters. The fragmentation threshold velocity for these collisions is approximately 7.5km/s. We show that collision velocities govern both the physical and chemical outcomes of silicate-carbonaceous nanograin interactions. In the fragmentation regime, collisions provide a viable pathway for generating mixed grains and a wide range of molecular species, many of which have been observationally detected. Here, we provide a simple credible mechanism linking the physics of grain processing with observed complex interstellar chemistry.
Author(s): Kyriazis l.; Rimola A.; Bromley S.T.
IVOA id: ivo://cds.vizier/j/a+a/713/a125

INT survey of local dwarf gal. VIII. LPV stars

2026-09-14T14:57:26Z

Description: We present a comprehensive catalog, in the Sloan i and Harris V filters, of long-period variable (LPV) stars in the spheroidal dwarf satellites of the Andromeda galaxy based on a dedicated survey for variable stars in Local Group dwarf systems. Using photometric time-series data obtained with the Wide Field Camera on the 2.5m Isaac Newton Telescope, we identify approximately 2800 LPV candidates across 17 Andromeda satellites, spanning a broad range in luminosity and variability amplitude. This study is accompanied by a public data release that includes two comprehensive catalogs, a catalog of the complete stellar populations for each galaxy, and a separate catalog listing all identified LPV candidates. Both are available through CDS/VizieR and provide a valuable resource for investigating quenching timescales, stellar mass distributions, and the effects of mass loss and dust production in dwarf galaxies. We derive updated structural parameters, including newly measured half-light radii, and determine distance moduli using the tip of the red giant branch method with Sobel filter edge detection, yielding values between 23.38{\pm}0.06 and 25.35{\pm}0.06mag.
Author(s): Abdollahi H.; Javadi A.; van Loon J.T.; McDonald I.; Abdollahi M.,Saremi E.; Khosroshahi H.G.; Molnar L.; Mahani H.
IVOA id: ivo://cds.vizier/j/apj/1000/69

Warm Jupiter migration pathways. I. Radial veloc.

2026-09-14T14:05:09Z

Description: Giant planets are expected to predominantly form beyond the water-ice line and occasionally undergo inward migration. Unlike hot Jupiters, which can result from high-eccentricity tidal migration, warm Jupiters between 0.1 and 1au (~10-365days) are in many ways more challenging to explain because they reside outside the tidal influence of their host stars. Warm Jupiters should therefore preserve traces of their origins as their eccentricities are directly related to their past interactions. We analyze the eccentricities of 200 warm Jupiters orbiting 194 Sunlike host stars (with FGKM spectral types) using 18,587 radial velocity (RV) measurements across 40 high-resolution spectrographs. RVs are compiled from the literature and are supplemented with 540 new observations from MINERVA-Australis at Mount Kent Observatory and the Habitable-zone Planet Finder spectrograph at McDonald Observatory's Hobby-Eberly Telescope, which are timed to improve eccentricity constraints by sampling orbits near periastron passage. The overarching goal of this program is to establish the relative importance of giant planet migration channels through the largest homogeneous analysis of warm Jupiter orbital properties to date. In particular, we evaluate and compare the impact of different system architectures and host star characteristics on the population-level eccentricity distributions of warm Jupiters. Here, we present the target sample, observations, orbit-fitting procedure, and parameter summary statistics of our survey. All orbit fit solutions, parameter posterior chains, and merged RV tables for each system are made publicly available.
Author(s): Morgan M.; Bowler B.P.; Tran Q.H.; Wittenmyer R.A.; Wright D.J.; Zhou G.,Fairnington T.R.
IVOA id: ivo://cds.vizier/j/apjs/280/76

AGN selection and demographics from SMILES

2026-09-14T14:02:26Z

Description: Understanding the coevolution of supermassive black holes and their host systems requires a comprehensive census of active galactic nuclei (AGNs) behavior across a wide range of redshift, luminosity, obscuration level, and galaxy properties. We report significant progress with JWST toward this goal from the Systematic Mid-infrared Instrument Legacy Extragalactic Survey (SMILES). Based on comprehensive spectral energy distribution (SED) analysis of 3273 MIRI-detected sources, we identify 217 AGN candidates over a survey area of ~34arcmin2, including a primary sample of 111 AGNs in normal massive galaxies (M*>10^9.5^M_{sun}_) at z~0-4, an extended sample of 86 AGN candidates in low-mass galaxies (M*<10^9.5^M_{sun}_), and a high-z sample of 20 AGN candidates at z~4-8.4. Notably, about 80% of our MIRI-selected AGN candidates are new discoveries despite the extensive pre-JWST AGN searches. Even among the massive galaxies where the previous AGN search is believed to be thorough, 34% of the MIRI AGN identifications are new, highlighting the impact of obscuration on previous selections. By combining our results with the efforts at other wavelengths, we build the most complete AGN sample to date and examine the relative performance of different selection techniques. We find the obscured AGN fraction increases from L_AGN,bol_~10^10^L_{sun}_ to 10^11^L_{sun}_ and then drops toward higher luminosity. Additionally, the obscured AGN fraction gradually increases from z~0 to z~4 with most high-z AGNs obscured. We discuss how AGN obscuration, intrinsic SED variations, galaxy contamination, survey depth, and selection techniques complicate the construction of a complete AGN sample.
Author(s): Lyu J.; Alberts S.; Rieke G.H.; Shivaei I.; Perez-Gonzalez P.G.; Sun F.,Hainline K.N.; Baum S.; Bonaventura N.; Bunker A.J.; Egami E.,Eisenstein D.J.; Florian M.; Ji Z.; Johnson B.D.; Morrison J.; Rieke M.,Robertson B.; Rujopakarn W.; Tacchella S.; Scholtz J.; Willmer C.N.A.
IVOA id: ivo://cds.vizier/j/apj/966/229

MUSE UDF. V. Mass-metallicities at z~1-2

2026-09-14T14:02:24Z

Description: Using more than 100 galaxies in the MUSE Ultra Deep Field with spectroscopy from the Hubble Space Telescope's (HST) WFC3 and the Very Large Telescope's Multi Unit Spectroscopic Explorer (MUSE), we extend the gas-phase mass-metallicity relation (MZR) at z~1-2 down to stellar masses of M*~10^7.5^M_{sun}_. The sample reaches 6 times lower in stellar mass and star formation rate (SFR) than previous HST studies at these redshifts, and we find that galaxy metallicities decrease to log(O/H)+12~7.8+/-0.1 (15% solar) at log(M*/M_{sun}_)~7.5, without evidence of a turnover in the shape of the MZR at low masses. We validate our strong-line metallicities using the direct method for sources with [OIII]{lambda}4363 and [OIII]{lambda}1666 detections, and find excellent agreement between the techniques. The [OIII]{lambda}1666-based metallicities double existing measurements with a signal-to-noise ratio >=5 for unlensed sources at z>1, validating the strong-line calibrations up to z~2.5. We confirm that the MZR resides ~0.3dex lower in metallicity than local galaxies and is consistent with the fundamental metallicity relation if the low-mass slope varies with SFR. At lower redshifts (z~0.5) our sample reaches ~0.5dex lower in SFR than current calibrations and we find enhanced metallicities that are consistent with extrapolating the MZR to lower SFRs. Finally, we detect only an ~0.1dex difference in the metallicities of galaxies in groups versus isolated environments. These results are based on robust calibrations and reach the lowest masses and SFRs that are accessible with HST, providing a critical foundation for studies with the Webb and Roman Space Telescopes.
Author(s): Revalski M.; Rafelski M.; Henry A.; Fossati M.; Fumagalli M.; Dutta R.,Pirzkal N.; Beckett A.; Arrigoni Battaia F.; Dayal P.; D'Odorico V.,Lusso E.; Nedkova K.V.; Prichard L.J.; Papovich C.; Peroux C.
IVOA id: ivo://cds.vizier/j/apj/966/228

ReveaLLAGN 0: JWST MIRI obs. of NGC4594 and NGC1052

2026-09-14T14:02:23Z

Description: We present the first results from the Revealing Low-Luminosity Active Galactic Nuclei (ReveaLLAGN) survey, a JWST survey of seven nearby LLAGNs. We focus on two observations with the Mid-Infrared Instrument (MIRI)'s Medium-Resolution Spectrometer of the nuclei of NGC 1052 and Sombrero (NGC 4594/M104). We also compare these data to public JWST data of higher-luminosity AGNs, NGC 7319 and NGC 7469. JWST clearly separates the AGN spectrum from the galaxy light even in Sombrero, the faintest target in our survey; the AGN components have very red spectra. We find that the emission-line widths in both NGC 1052 and Sombrero increase with increasing ionization potential, with FWHM>1000km/s for lines with ionization potential >~50eV. These lines are also significantly blueshifted in both LLAGNs. The high-ionization-potential lines in NGC 7319 show neither broad widths nor significant blueshifts. Many of the lower-ionization-potential emission lines in Sombrero show significant blue wings extending >1000km/s. These features and the emission-line maps in both galaxies are consistent with outflows along the jet direction. Sombrero has the lowest-luminosity high-ionization-potential lines ([NeV] and [OIV]) ever measured in the mid-infrared, but the relative strengths of these lines are consistent with higher-luminosity AGNs. On the other hand, the [NeV] emission is much weaker relative to the [NeIII] and [NeII] lines of higher-luminosity AGNs. These initial results show the great promise that JWST holds for identifying and studying the physical nature of LLAGNs.
Author(s): Goold K.; Seth A.; Molina M.; Ohlson D.; Runnoe J.C.; Boker T.,Davis T.A.; Dumont A.; Eracleous M.; Fernandez-Ontiveros J.A.; Gallo E.,Goulding A.D.; Greene J.E.; Ho L.C.; Markoff S.B.; Neumayer N.,Plotkin R.M.; Prieto A.; Satyapal S.; van de Ven G.; Walsh J.L.; Yuan F.,Feldmeier-Krause A.; Gultekin K.; Honig S.; Kirkpatrick A.,Lutzgendorf N.; Reines A.E.; Strader J.; Trump J.R.; Voggel K.T.
IVOA id: ivo://cds.vizier/j/apj/966/204

NGVS. III. Surface brightness fluctuation dist.

2026-09-14T14:02:22Z

Description: The surface brightness fluctuation (SBF) method is a robust and efficient way of measuring distances to galaxies containing evolved stellar populations. Although many recent applications of the method have used space-based imaging, SBF remains a powerful technique for ground-based telescopes. Deep, wide-field imaging surveys with subarcsecond seeing enable SBF measurements for numerous nearby galaxies. Using a preliminary calibration, Cantiello+ 2018ApJ...856..126C presented SBF distances for 89 bright, mainly early-type galaxies observed in the Next Generation Virgo Cluster Survey. Here we present a refined calibration and SBF distances for 278 galaxies extending several magnitudes fainter than in previous work. The derived distances have uncertainties of 5%-12% depending on the properties of the individual galaxies, and our sample is more than 3 times larger than any previous SBF study of this region. Virgo has a famously complex structure with numerous subclusters, clouds, and groups; we associate individual galaxies with the various substructures and map their three-dimensional spatial distribution. Curiously, subcluster A, centered around M87, appears to have two peaks in distance: the main peak at ~16.5Mpc, and a smaller one at ~19.4Mpc. Subclusters B and C have distances of ~15.8Mpc. The W and W' groups form a filament-like structure, extending more than 15Mpc behind the cluster with a commensurate velocity increase of ~1000km/s along its length. These measurements are a valuable resource for future studies of the relationship between galaxy properties and local environment within a dynamic and evolving region.
Author(s): Cantiello M.; Blakeslee J.P.; Ferrarese L.; Cote P.; Raimondo G.,Cuillandre J.-C.; Durrell P.R.; Gwyn S.; Hazra N.; Peng E.W.,Roediger J.C.; Sanchez-Janssen R.; Kurzner M.
IVOA id: ivo://cds.vizier/j/apj/966/145

Catalog of eccentric eclipsing binaries from TESS

2026-09-14T11:50:22Z

Description: Eccentric eclipsing binaries (EEBs) are the ideal objects to constrain the tidal theory. During the 2yr mission, TESS 2min cadence mode obtained high-precision photometry of more than 200,000 objects distributed over almost the entire sky. Among these objects, we identify 368 EEBs, including 23 newly discovered systems, through a detailed analysis of periods, light-curve shapes, and eclipses. We have also adopted the two recent TESS-based eclipsing binary catalogs, bringing our sample size to 514. The eccentricity, argument of periastron, absolute magnitude, and intrinsic color are determined for these EEBs. We find the absolute magnitude MG of EEBs has a span of at least 20mag. Stars as low as 0.15M_{sun}_ and as high as 30M_{sun}_ can have an eccentric orbit. Based on the parameters of Gaia Radial Velocity Spectrometer spectra, we find four EEBs contain evolved components, namely, TIC146039664, TIC141809359, TIC428249301, and TIC294261093. Overall, more luminous EEBs have a shorter circularization period. There are peculiarities in the eccentricity distribution of the brightest and faintest EEBs (M_G_<1 and M_G_>5). The former may not have a strict cutoff circularization period, while the latter may still have an eccentric orbit at periods shorter than 1day.
Author(s): Tang Y.; Chen X.; Gai N.; Wang S.; Li Z.; Li Z.; Li K.; Wang Y.
IVOA id: ivo://cds.vizier/j/aj/170/356

NGVS. XXXVII. RR Lyrae stars out to 300kpc

2026-09-14T07:22:13Z

Description: RR Lyrae stars are standard candles with characteristic photometric variability and serve as powerful tracers of Galactic structure, substructure, accretion history, and dark matter content. Here we report the discovery of distant RR Lyrae stars, including some of the most distant stars known in the Milky Way halo, with Galactocentric distances of ~300kpc. We use time-series u*g'i'z' Canada-France-Hawaii Telescope/MegaCam photometry from the Next Generation Virgo Cluster Survey (NGVS). We use a template light-curve fitting method based on empirical Sloan Digital Sky Survey Stripe 82 RR Lyrae data to identify RR Lyrae candidates in the NGVS data set. We eliminate several hundred suspected quasars and identify 180 RR Lyrae candidates with heliocentric distances of ~20-300kpc. The halo stellar density distribution is consistent with an r^-4.09{\pm}0.10^ power-law radial profile over most of this distance range with no signs of a break. The distribution of ab-type RR Lyrae in a period-amplitude plot (Bailey diagram) suggests that the mean metallicity of the halo decreases outward. Compared to other recent RR Lyrae surveys, like Pan-STARRS1, the High Cadence Transient Survey, and the Dark Energy Survey, our NGVS study has better single-epoch photometric precision and a comparable number of epochs but smaller sky coverage. At large distances, our RR Lyrae sample appears to be relatively pure and complete, with well-measured periods and amplitudes. These newly discovered distant RR Lyrae stars are important additions to the few secure stellar tracers beyond 150 kpc in the Milky Way halo.
Author(s): Feng Y.; Guhathakurta P.; Peng E.W.; Gwyn S.D.J.; Ferrarese L.; Cote P.,Cuillandre J.-C.; Munsell J.; Talukdar M.
IVOA id: ivo://cds.vizier/j/apj/966/159