VO Fresh

Cassini Scalar Helium MAG Calibrated Housekeeping Data Collection

2026-10-02T17:04:38Z

Description

This collection contains Cassini scalar helium (SHM) magnetometer
housekeeping data collected between 1999-08-18 and 2005-06-08.

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_shm_hkrate_asc/ppi/epn_core

Cassini MAG Calibrated Full Res. Data in RTN Coords. Collection

2026-10-02T17:04:30Z

Description

Cassini magnetic-field data in the highest time resolution available,
from the Fluxgate Magnetometer (FGM) instrument in RTN coordinates

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_full_rtn/ppi/epn_core

Cassini MAG Calibrated 1 Sec. Avg. Data in KSO Coords. Collection

2026-10-02T17:04:07Z

Description

This collection contains Cassini magnetic-field 1 second averages in
KSO coordinates, from the Fluxgate Magnetometer (FGM) instrument.

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_1sec_kso/ppi/epn_core

Cassini MAG Calibrated 1 Sec. Avg. Data in GSE Coords. Collection

2026-10-02T17:03:46Z

Description

This collection contains Cassini magnetic-field 1 second averages, in
GSE coordinates, from the Fluxgate Magnetometer (FGM) instrument.

Author(s)

In Sook Moon

IVOA id

ivo://pds-ppi/cassini_mag_cal_1sec_gse/ppi/epn_core

RR Lyrae variables in M3

2026-10-02T11:13:16Z

Description: We present a comprehensive photometric study of RR Lyrae stars in the M3 globular cluster, utilizing a vast data set of 3140 optical (UBVRI) CCD images spanning 35yr from astronomical data archives. We have successfully identified previously known 238 RR Lyrae stars from the photometric data, comprising 178 RRab, 49 RRc, and 11 RRd stars. Multiband periodogram was used to significantly improve the long-term periods of 65 percent of RR Lyrae stars in our sample, thanks to the unprecedentedly long temporal coverage of the observations. The light curve templates were used to obtain accurate and precise mean magnitudes and amplitudes of all RR Lyrae variables. We combined optical (UBVRI) and near-infrared (NIR, JHKs) photometry of RR Lyrae variables to investigate their location in the colour-magnitude diagrams as well as the pulsation properties such as period distributions, Bailey diagrams and amplitude ratios. The period-luminosity relations in R and I bands and Period-Wesenheit relations were derived after excluding outliers identified in CMDs. The Period-Wesenheit relations calibrated via the theoretically predicted relations were used to determine a distance modulus of {mu}=15.04+/-0.04(stats)+/-0.19(syst.)mag (using metal-independent WBV Wesenheit) and {mu}=15.03+/-0.04(stats)+/-0.17(syst.)mag (using metal-dependent WVI Wesenheit) {mu}=15.03+/-0.04(stats)+/-0.17(syst.). Our distance measurements are in excellent agreement with published distances to M3 in the literature. We also employed an artificial neural network based comparison of theoretical and observed light curves to determine physical parameters (mass, luminosity, and effective temperature) for 79 non-Blazhko RRab stars that agree with limited literature measurements.
Author(s): Kumar N.; Bhardwaj A.; Singh H.P.; Rejkuba M.; Marconi M.; Prugniel P.
IVOA id: ivo://cds.vizier/j/mnras/531/2976

Enhanced magnetic activity after period gap

2026-10-02T10:36:26Z

Description: For low-mass stars (M<1.4M_{sun}_), the connection between stellar rotation and magnetic activity governs stellar spin-down, shapes the environments of their exoplanets, and provides an age-diagnostic via magneto-gyro-chronology. Recently, unexpected phenomena known as the intermediate rotation period gap and the rotational stalling have been discovered. These are likely due to internal angular momentum redistribution, and mark departures from a smooth spin-down evolution. These rotational features have been shown to cause enhanced magnetic activity on the photosphere, as measured by the photometric index from light curves (Sph), in both cluster and field stars. However, their influence on other magnetic activity proxies, and particularly in field stars, remains poorly understood. In this work, we study the impact of the intermediate-period gap on chromospheric magnetic activity as traced by the CaII infrared triplet (IRT) index. We target the stars observed by the Kepler mission, as this is the largest and most reliable sample of field stars with measured rotation periods sensitive to the gap. We calculate the CaII IRT index for the Kepler stars using the spectroscopic information from the Gaia mission data release three (DR3). We study the rotation-activity relation as a function of location on the Hertzsprung-Russell (HR) diagram and spectral type, finding that K dwarfs are more active than G dwarfs, which in turn are more active than F dwarfs. For main-sequence stars, we find that chromospheric magnetic activity is also enhanced after the intermediate- period gap, mirroring its effect on the photospheric Sph index. Our work reveals that the intermediate-period gap marks a genuine transition in stellar magnetic behavior, not only at the photosphere but also at the chromosphere. This highlights the need to account for its signatures across activity proxies, as well as its impact on exoplanet habitability and the age-rotation-activity relation.
Author(s): Godoy-Rivera D.; Mathur S.; Richey-Yowell T.; Santos A.R.G.; Garcia R.A.,Grossmann D.H.; Claytor Z.R.; Beck P.G.
IVOA id: ivo://cds.vizier/j/a+a/714/a124

V557 Mon photometry and spectra

2026-10-02T10:22:01Z

Description: The unstable mass accretion process in young stellar objects (YSOs) often triggers observable outbursts. These episodic accretion events play a critical role in stellar mass assembly during the pre-main-sequence phase. In this paper, we present observations of an eruptive young star in the Rosette Nebula, identified by the Gaia Science Alerts system using Gaia time-series data. We aim to investigate the evolution of the brightness and mass accretion rate of V557 Mon throughout its outburst and subsequent decline. In addition, we trace the evolution of the inner accretion disk during the outburst by monitoring molecular emission features. We compiled multi-band photometric time series from Gaia, ZTF, and several 1m-class ground-based telescopes and obtained optical and near-infrared spectra at multiple epochs covering the outburst and fading phases. Stellar parameters were derived from quiescent colour/spectra and spectral energy distribution (SED) fitting. We also measured the mass accretion rate and fit models to molecular emission bands. Since late 2024, V557 Mon has undergone a year-long outburst consistent with EXor variability. Based on quiescent photometry, V557 Mon has a spectral type of M1 with an extinction of AV=1.8+/-0.3mag, consistent with a 0.4-0.5M_{sun}_ star at an age of 2Myr. Our multi-epoch spectra and u-band photometry indicate a peak accretion rate of 6.3x10^^-7^M_{sun}_/yr during the outburst, roughly 70 times higher than in quiescence. We report the detection of hot water vapour emission bands, together with TiO, VO, and CO emission features. Using ExoMol models, we measured the inner-disk temperature changed from 3000K to 2000K during the fading phase of the outburst. We report a recent EXor outburst in a low-mass Class II YSO. Our observations reveal the transient formation of a hot molecular inner disk, traced by variable water vapour emission during the EXor event. A positive correlation is found between the molecular excitation temperature and the overall stellar brightness.
Author(s): Guo Z.; Osses J.; Fermiano V.; Zhou Y.; Fang M.; Herczeg G.; Carvalho A.,Elbakyan V.; Hillenbrand L.; Wang M.; Liu H.; Liu Y.; Briceno C.; Singh K.,Ivanov V.D.; Ninan J.; Giannini T.; Aliaga A.; Morris C.; Montesinos M.,Zhao H.; Contreras Pena C.; Jose J.; Chand T.; Chen W.-P.; Wang W.-H.,Huang Y.; Lopez C.; Fernandez-Schlosser P.; Correa-Herrera D.; Kurtev R.,Rodriguez V.; Lizana-Vidal C.; Borissova J.; Kuhn M.; Saito R.K.; Yadav R.K.
IVOA id: ivo://cds.vizier/j/a+a/714/a98

Gaia EDR3 white dwarfs Ca abundances

2026-10-02T10:12:12Z

Description: White dwarf (WD) atmospheric metal pollution provides strong evidence for the presence of remnant planetary material, and it can be used as an indirect tracer of outer planetary systems. We analyze whether the presence of a wide stellar companion affects the occurrence of outer planetary systems by comparing the incidence of calcium pollution in hydrogen-atmosphere WDs in wide binaries and in apparently single stars. We constructed two sample pairs: a large homogeneous SDSS low-resolution spectroscopic set (4844 single WDs; 322 WDs in wide binaries) and a smaller high-resolution sample (83 single WDs; 34 WDs in wide binaries). For each WD, we measured calcium abundances or upper limits and computed detectability-corrected cumulative pollution fractions that account for variations in effective temperature, signal-to-noise ratio, and spectral resolution. In the SDSS-based samples, we find pollution fractions below ~1%, defined as the fraction of white dwarfs with detected Ca relative to the total number of white dwarfs, for both single WDs and WDs in wide binaries. After correcting for detectability, the cumulative abundance distributions of the two populations are statistically consistent. The same conclusion was obtained for the higher-resolution samples, despite their different raw detection fractions. Our results indicate no statistically significant difference in the occurrence rate of remnant outer planetary systems between single stars and stars with wide (~200au) companions, within the current uncertainties. These uncertainties are significant because the samples contain only a small number of polluted WDs. The corrected detectability cumulative fraction approach used here provides a framework for comparing samples with different detection sensitivities and can be extended to larger spectroscopic datasets. Such samples will be required to determine whether wide stellar companions affect the survival and delivery of planetary material and to search for more subtle trends, for example, as a function of companion separation.
Author(s): Lizana-Vidal C.; Aguilera-Gomez C.; Rogers L.K.; Bonsor A.,Munoz-Arriagada M.I.; Dufour P.; Bravo-Parra C.; Salugova E.
IVOA id: ivo://cds.vizier/j/a+a/714/a64

On the rotation period of the O giant xi Per

2026-10-02T10:07:44Z

Description: OB stars exhibit line profile variability, often over timescales associated with rotation, notably in their ultraviolet wind-sensitive lines in which "discrete absorption components" recur cyclically. We searched for periodicity in spectral regions of the O7.5III(n)((f)) star xi Persei that are formed very close to the star and are least likely to be affected by doublet overlap or irregular transient phenomena. We identified the low-velocity wind region probed by the NIV lambda 1718{AA} line as the most uncontaminated spectral region for which a large and homogeneous dataset is available: 307 International Ultraviolet Explorer (IUE) spectra over 12 years, and 11 STIS (onboard the Hubble Space Telescope) spectra taken 21 years later. We also studied 322 time-resolved HeII lambda 4686{AA} spectra. We searched for periodicities in high-precision space photometry (MOST, BRITE, and TESS), covering 13 years. We also reconsidered X-ray studies with Chandra. A CLEAN analysis and subsequent weighted least-squares fit of the flux in this region resulted in a unique period of 2.040514+/-0.000020d, interpreted as due to rotation. The phase of maximum flux in the NIV, SiIV, Halpha, and HeII line profiles, and X-ray variability studies, coincide. We also found this period with low amplitude in the photometric data, albeit with large intrinsic scatter, and with a deviating maximum phase. Given the coherent periodic behaviour of several observables probing the region of the wind nearest the stellar surface, we propose that xi Per has an as-yet undetected weak global surface magnetic field. We excluded a rotation period of ~4d based on stellar parameters. The sinusoidal behaviour suggested that only one magnetic pole is visible, implying an inclination of i~51deg, and therefore, beta<~90-i=39deg for the magnetic obliquity. We present a conceptual framework within which weak wind confinement by a global magnetic field can create a small magnetospheric disc, while allowing the formation of more classic `corotating interaction regions' at higher magnetic latitudes. The periodic variations are then understood to result from the changing projected area of the magnetospheric disc as a function of rotational phase, both along the line of sight and off the stellar limb.
Author(s): Henrichs H.F.; Sudnik N.; David-Uraz A.
IVOA id: ivo://cds.vizier/j/a+a/714/a63

Gaia DR3 [Fe/H] from LAMOST DR10

2026-10-02T10:03:52Z

Description: Gaia DR3 provides astrophysical parameters for hundreds of millions of stars but the [M/H] from its GSP-Phot module suffer from systematic bias. In this paper, we estimate stellar metallicities from Gaia DR3 data, using the homogeneous spectroscopic iron abundances [Fe/H] of LAMOST DR10 as training labels. We have cross-matched LAMOST DR10 [Fe/H] with Gaia DR3 and trained a gradient-boosted decision-tree regressor (XGBoost) on 1.20 million AFGK stars, using only Gaia-derived inputs and proxies. We validated the estimates on held-out LAMOST stars, on GALAH DR4 and APOGEE DR17, and on 46 open clusters, and applied the model to measure the radial metallicity gradient of the disk of the Milky Way. On the held-out test set, the model reaches a mean absolute error of 0.052dex and R^2^=0.94 with negligible bias, against 0.242dex for GSP-Phot on the same stars. The estimates transfer well to external surveys with a mean absolute error of 0.066dex (GALAH) and 0.068dex (APOGEE). For open clusters, the median difference between our estimated [Fe/H] and [Fe/H] from spectroscopy surveys is 0.041dex which is smaller than both GSP-Phot (0.248dex) and previous work on an APOGEE-trained XG-Boost model (0.067dex). When we applied our model to the disk, it recovers a broken thin disk radial gradient (inner +0.119, outer -0.058dex/kpc with a break near 5.9kpc) and an open-cluster gradient of -0.066dex/kpc, both in agreement with previous high-resolution spectroscopy works. Our estimated [Fe/H] values are accurate to 0.05dex to 0.07dex for AFGK stars within the range [Fe/H]>~-2.5; below this limit the predictions should be treated as lower bounds. The catalogue and the trained model are publicly available on Zenodo. These estimates are suitable for chemical studies of the Milky Way.
Author(s): Srivastava D.; Niedzielski A.; Smiljanic R.
IVOA id: ivo://cds.vizier/j/a+a/714/a59

Optical spectra of HD 14134

2026-10-02T09:52:35Z

Description: The post-main sequence (MS) evolution of massive stars encompasses phases in which the stars display high variability. One such class of objects are the blue supergiants which may be in either the pre- or post-red supergiant phase of their evolution. Their variability patterns might provide constraints for a proper classification of the objects. Teh study aims to characterise the observed variability of the B supergiant HD14134 and to investigate the imprint of a time-variable wind on the brightness variation of the star and its impact on the detectability of pulsation signals. Spectroscopic data were collected over a 5-month period and combined with photometry from TESS. Stellar parameters were derived from modelling of the time-averaged spectrum with CMFGEN and the SED and were confirmed with stellar evolution models computed with MESA. The light curves and radial velocity curves of selected lines were analysed to determine pulsation signals. The wind variability and its imprint on the stellar brightness were investigated from an analysis of the Halpha line. Predictions of mode excitations were computed with the GYRE pulsation code and compared to the frequencies determined from the observations. A g-mode with a period of ~19.2d and its harmonics are consistently detected in all data sets. The spectra unveil strong, non-periodic wind variability and 3 frequency signals were identified as due to this wind variability. The stellar parameters and age derived for HD14134 together with the absence of radial pulsations classify the star as a post-MS object evolving towards the red-supergiant stage, questioning its classification as alpha Cyg variable. The results reinforce that simultaneous long-term spectroscopic and photometric monitoring is indispensable for reliable frequency detections and for disentangling of variabilities imprinted by a time-variable wind from those imposed by pulsations.
Author(s): Guha S.; Kraus M.; Sanchez Arias J.P.; Nemeth P.; Kaminski K.
IVOA id: ivo://cds.vizier/j/a+a/714/a46

AMS-02 All Particle Rates Catalog

2026-10-02T00:00:00Z

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

2026-10-02T00:00:00Z

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

2026-10-02T00:00:00Z

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)

2026-10-02T00:00:00Z

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

ESDC Multi-mission Data Services TAP

2026-10-01T13:29:33.182000Z

Description: The ESDC Multi-mission Data Services (EMDS) TAP service provides unified access to metadata across multiple ESDC Science Archives, supporting interoperability, standardised data discovery, and long-term service sustainability. The service implements the IVOA Table Access Protocol (TAP) standard and enables access to metadata exposed through both mission-specific data models and the IVOA Observation Core Components (ObsCore) data model. The archives currently accessible through the EMDS TAP service include Einstein Probe, EXOSAT, ISO, Cheops, Smile, Ulysses, and Proba-3.
IVOA id: ivo://esavo/emds/tap

J-PAS-E2DR (October, 2026)

2026-10-01T08:30:00Z

Description: J-PAS E2DR Extended Early Data Release (October, 2026) HiPS catalogue. J-PAS is a 57-band photometric optical survey, observing the Northern Hemisphere from the dedicated JST250 telescope and the JPCam instrument at the Observatorio Astrofísico de Javalambre (OAJ, Teruel, Spain). . Please include the following in any published material that makes use of this data: "Based on observations made with the JST250 telescope and JPCam camera of the J-PAS Survey at the Observatorio Astrofísico de Javalambre, in Teruel, owned, managed and operated by the Centro de Estudios de Física del Cosmos de Aragón."
Author(s): Centro de Estudios de Física del Cosmos de Aragón (CEFCA)
IVOA id: ivo://cefca/j-pas/j-pas-e2dr

Dust in II Zw 096

2026-10-01T08:23:46Z

Description: Galaxy mergers drive intense radiation environments that fundamentally alter interstellar dust properties through photo-destruction and thermal processing. The luminous infrared galaxy II Zw 096 presents several distinctive regions, including starburst clumps and a proposed buried AGN in region D1, making it an ideal laboratory for studying dust evolution under extreme conditions. This work aims to determine the carbonaceous dust properties across II Zw 096 by characterizing the spatial variations in carbonaceous feature ratios and investigate how intense radiation fields process carbonaceous dust grains, using the relationship between dust processing signatures and traditional radiation field diagnostics. Using JWST NIRSpec IFU and MIRI MRS, carbonaceous features were observed and analyzed using the Continuum and Feature Extraction tool (CAFE) with 61 carbonaceous features from the PDRs4all project and new absorption features for ice and crystalline silicates. We analyze spatial variations in carbonaceous feature ratios at multiple resolutions (0.281", 0.787" and 0.961") to trace dust composition and grain size distribution. The 3.4/3.3 um ratio probes aliphatic versus aromatic content, while the 11.3/3.3um ratio diagnoses grain size distribution. The 3.4/3.3um ratio spans between 0.056-0.148, with the lowest values near the proposed AGN (D1) and starburst clumps (C0, D0), indicating preferential destruction of C-H bonds connected to aliphatic structures in highly irradiated environments. The 11.3/3.3 um ratio varies from 0.334 up to ~2.348 in D1. Both PAH ratios show no clear correlation with [NeIII]/[NeII], suggesting ionization diagnostics either break down in extreme merger environments, or as an effect of tracing different ISM phases and radiation-field regimes in this highly obscured merger environment. We detect water ice (3.1um), CO_2_ ice (4.27um), and crystalline silicates (11.1um) with spatial distributions anti-correlating with carbonaceous processing signatures. Spatial resolution critically affects dust diagnostics: the 3.4/3.3um dynamic range doubles when increasing the resolution from 0.961" to 0.281", demonstrating that apparent uniformity at low resolution masks significant variations in compact regions undergoing intense dust processing. Multiple coherent diagnostics point to intense dust processing, such as photodestruction of the smallest nanograins and aromatisation, consistent with a buried AGN in D1, though definitive confirmation remains elusive.
Author(s): Olander G.; Schirmer T.; Aalto S.; del Palacio S.; Diaz-Santos T.; Inami H.,Armus L.; Buiten V.; Knudsen K.K.; Konig S.; Lai T.S.-Y.; Lenkic L.,Linden S.T.; Nyman G.; Riesco C.; van der Werf P.; Vlemmings W.,Sameera W.M.C.; Wethers C.
IVOA id: ivo://cds.vizier/j/a+a/714/a43

Tidal tails from NGC7492 along Sgr stream

2026-10-01T08:22:09Z

Description: The formation, extension, and morphology of extra-tidal stars around globular clusters depend on the internal kinematics of the host cluster and the influence of the Galactic potential. Tracing the kinematics of faint tidal tails sheds light on their formation and contribution to the Milky Way halo assembly. NGC 7492 is an outer halo globular cluster with conflicting evidence regarding the presence of tidal tails. If present, the tails are expected to be faint and embedded in the Sagittarius tidal stream, located at a similar heliocentric distance but having different kinematics. We carried out a GIRAFFE spectroscopic follow-up of ten fields at the expected location of tidal tails associated with NGC 7492 to obtain the radial velocity component. Gaia parallaxes were used to remove foreground contaminants, while only loose constraints on Gaia proper motion were applied to select the targets. From the high-resolution spectra, radial velocities and metallicities were derived for more than 700 stars, from the red giant branch down to the upper main sequence. Cluster and extra-tidal stars were identified based on their proper motions, radial velocities, and metallicities. This population extends over at least ~1.8deg from the cluster center, confirming the tidal tails previously detected only photometrically. The extra-tidal stars are located at positions consistent with spray-particle models for the cluster's disruption. The Sagittarius stream is also clearly identified through its distinct proper motion distribution, radial velocities and more metal-rich population. Despite the low spatial density of extra-tidal stars, the kinematic signature of the cluster is clearly detected, confirming the presence of tidal tails overlapping on the sky with the Sagittarius stream, though the two structures are physically unrelated. The present spectroscopic dataset provides a robust basis for future studies aimed at extending the characterization of the tails, both in extension and limiting magnitude.
Author(s): Navarrete C.; Rojas-Arriagada A.; Piatti A.E.; Carballo-Bello J.A.,Sbordone L.; Kundu R.; Belokurov V.; Koposov S.E.; Vitral E.; Boldrini P.,Palicio P.A.
IVOA id: ivo://cds.vizier/j/a+a/714/a39

LINCC Frameworks - Hugging Face - mmu_cfa_seccsn

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_cfa_seccsn

LINCC Frameworks - Hugging Face - mmu_cfa_snii

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_cfa_snii

LINCC Frameworks - Hugging Face - mmu_chandra_spectra

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_chandra_spectra

LINCC Frameworks - Hugging Face - mmu_csp_csp

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_csp_csp

LINCC Frameworks - Hugging Face - mmu_des_y3_sne_ia

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_des_y3_sne_ia

LINCC Frameworks - Hugging Face - mmu_desi_edr_sv3

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_desi_edr_sv3

LINCC Frameworks - Hugging Face - mmu_desi_provabgs

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_desi_provabgs

LINCC Frameworks - Hugging Face - mmu_euclid_q1

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_euclid_q1

LINCC Frameworks - Hugging Face - mmu_foundation

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_foundation

LINCC Frameworks - Hugging Face - mmu_gaia_gaia

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_gaia_gaia

LINCC Frameworks - Hugging Face - mmu_gz10

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_gz10

LINCC Frameworks - Hugging Face - mmu_hsc_pdr3_dud

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_hsc_pdr3_dud

LINCC Frameworks - Hugging Face - mmu_hsc_pdr3_wide_21

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_hsc_pdr3_wide_21

LINCC Frameworks - Hugging Face - mmu_jwst_ceers

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_ceers

LINCC Frameworks - Hugging Face - mmu_jwst_ceers_full_grizli

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_ceers_full_grizli

LINCC Frameworks - Hugging Face - mmu_jwst_gdn

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_gdn

LINCC Frameworks - Hugging Face - mmu_jwst_gdn_grizli

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_gdn_grizli

LINCC Frameworks - Hugging Face - mmu_jwst_gds

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_gds

LINCC Frameworks - Hugging Face - mmu_jwst_gds_grizli

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_gds_grizli

LINCC Frameworks - Hugging Face - mmu_jwst_ngdeep

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_ngdeep

LINCC Frameworks - Hugging Face - mmu_jwst_ngdeep_grizli

2026-09-30T18:46:46Z

Description
Author(s): LINCC Frameworks
IVOA id: ivo://data.lsdb/hf_mmu/mmu_jwst_ngdeep_grizli