Data Release Research Articles

Ionized Gas Outflows in the Galaxy and Mass Assembly (GAMA) Survey: Signatures of AGN Feedback in Low-mass Galaxies

Abstract We present a sample of 398 galaxies with ionized gas outflow signatures in their spectra from the Galaxy and Mass Assembly Survey Data Release 4, including 45 low-mass galaxies with stellar masses M * < 1010 M ⊙. We assemble our sample by systematically searching for the presence of a second velocity component in the [O iii]λλ4959, 5007 doublet emission line in 39,612 galaxies with redshifts z < 0.3. The host galaxies are classified using the Baldwin–Phillips–Terlevich diagram, with ~89% identified as active galactic nuclei (AGNs) and composites and 11% as star-forming (SF) galaxies. The outflows are typically faster in AGNs with a median velocity of 936 km s−1 compared to 655 km s−1 in the SF objects. Of particular interest are the 45 galaxies in the low-mass range, of which a third are classified as AGNs/composites. The outflows from the low-mass AGNs are also faster and more blueshifted compared to those in the low-mass SF galaxies. This indicates that black hole outflows can affect host galaxies in the low-mass range and that AGN feedback in galaxies with M * < 1010 M ⊙ should be considered in galaxy evolution models.

A novel Bayesian approach for decomposing the radio emission of quasars: II. Link between quasar radio emission and black hole mass

Abstract Whether the mass of supermassive black hole (MBH) is directly linked to the quasar radio luminosity remains a long-debated issue, and understanding the role of MBH in the evolution of quasars is pivotal to unveiling the mechanism of AGN feedback. In this work, based on a two-component Bayesian model, we examine how MBH affects the radio emission from quasars, separating the contributions from host galaxy star formation (SF) and AGN activity. By modelling the radio flux density distribution of Sloan Digital Sky Survey (SDSS) quasars from the LOFAR Two-metre Sky Survey Data Release 2, we find no correlation between MBH and SF rate (SFR) at any mass for quasars at a given redshift and bolometric luminosity. The same holds for AGN activity across most MBH values; however, quasars with the top 20 % most massive SMBHs are 2 to 3 times more likely to host strong radio jets than those with lower-mass SMBHs at similar redshift and luminosity. We suggest defining radio quasar populations by their AGN and SF contributions instead of radio loudness; our new definition unifies previously divergent observational results on the role of MBH in quasar radio emissions. We further demonstrate that this radio enhancement in quasars with the 20 % most massive SMBHs affects only the $\sim 5~{{\%}}$ most radio bright quasars at a given redshift and bolometric luminosity. We discuss possible physical origins of this radio excess in the most massive and radio-bright quasar population, which remains an interest for future study.

A multi-modal neuroimaging data release for Meige Syndrome and Facial Paralysis Research

The sharing of multimodal magnetic resonance imaging (MRI) data is of utmost importance in the field, as it enables a deeper understanding of facial nerve-related pathologies. However, there is a significant lack of multi-modal neuroimaging databases specifically focused on these conditions, which hampers our comprehensive knowledge of the neural foundations of facial paralysis. To address this critical gap and propel advancements in this area, we have released the Multimodal Neuroimaging Dataset of Meige Syndrome, Facial Paralysis, and Healthy Controls (MND-MFHC). This dataset includes detailed clinical assessments of 53 individuals with facial paralysis (FP), 31 patients with Meige syndrome (MS), and 102 healthy controls (HC). To promote open access, the BIDS-formatted data and associated quality control reports can be accessed through the Science Data Bank (SciDB). By sharing this comprehensive dataset, our aim is to facilitate further research and exploration into the intricate neural mechanisms underlying facial nerve-related pathologies.

Responsible research in health disparities using the Adolescent Brain Cognitive DevelopmentSM (ABCD) study.

The Adolescent Brain Cognitive DevelopmentSM (ABCD) Study is the largest longitudinal study on brain development and adolescent health in the United States. The study includes a sociodemographically diverse cohort of nearly 12,000 youth born 2005-2009, with an open science model of making data rapidly available to the scientific community. The ABCD Study® data has been used in over 1100 peer-reviewed publications since its first data release in 2018. The dataset contains a broad scope and comprehensive set of measures of youths' behavioral, health, and brain outcomes, as well as extensive contextual and environmental measures that map onto the social determinants of health (SDOH). Understanding the impact of SDOH on the developmental trajectories of youth will help to address early lifecourse health inequities that lead to disparities later in life. However, the open science model and extensive use of ABCD data highlight the need for guidance on appropriate, responsible, and equitable use of the data. Our conceptual framework integrates the National Institute on Minority Health and Health Disparities (NIMHD) Research Framework with strength-based and data equity perspectives. We use this framework to articulate best practices and methods for investigations that aim to identify the multilevel pathways by which structural and systemic inequities impact adolescent health trajectories. Using our conceptual model, we provide recommendations for equitable health disparities research using ABCD Study data. We identify over fifty ABCD measures that can encompass SDOH across five levels of influence: individual, interpersonal, school, community, and societal. We expand the societal level to acknowledge structural discrimination as the root cause of systemic and structural inequities resulting in health disparities among marginalized youth. We apply the methodological recommendations in an example data analysis using a multi-level approach that integrates strength-based and data equity perspectives to elucidate pathways by which social and structural inequities may influence cognitive decision making in youth. We conclude with recommendations for strengthening the utility of ABCD data for health disparities research now and in the future. Adolescence is a critical period of development with subsequent ramifications for health outcomes across the lifespan. Thus, understanding SDOH among diverse youth can inform prevention interventions before the emergence of health disparities in adulthood.

Study on the One-year Accuracy of Pulsar Time-scale

Abstract Determining accurate pulsar timing model parameters is essential for establishing TT(PT), a realization of Terrestrial Time(TT) based on a pulsar time-scale(PT). This study discusses the impact of different data spans on the accuracy of pulsar timing model parameters when determining pulsar timing model parameters. Using observations of PSR J0437-4715, J1909-3744, J1713+0747, and J1744-1134 from the second data release of the International Pulsar Timing Array (IPTA II, Version A), we compare the accuracy of the timing model parameters determined by these observations with different data spans. The results show for PSR J0437-4715, J1713+0747, and J1909-3744, the amplitude fluctuations of rotational frequency remain within $10^{-15}$, $10^{-14}$, and $10^{-14}$ Hz, respectively, when the data spans for determining pulsar timing model parameters exceed 13, 14, and 6 years. Additionally, the one-year accuracy of TT(PT) is crucial for its application in timekeeping. By comparing the frequency deviations of TT(PT) relative to TT(BIPM) under both ideal ($k_{r}$) and actual ($k_{p}$) conditions across different data spans, we find that when the data span reaches the duration above, the accuracy of TT(PT) surpasses that of TT(TAI) under ideal conditions, slightly inferior under actual conditions. This suggests with improved observational technologies, the accuracy of TT(PT) can be further enhanced.

Kinematics of Young Stellar Objects under Various Stellar Feedback

Based on the Gaia Data Release 3 and APOGEE data sets, we investigate the kinematic differences between young stellar objects (YSOs) and their parent clouds in five nearby star-forming regions. Overall, the one-dimensional velocity differences between Class II YSOs and their parent molecular cloud range from [0, 1.4] km s−1. In feedback environments dominated by outflows, massive stars, and supernova feedback, the corresponding velocity differences range from [0, 1.4], [0.1, 0.4], and [0.1, 1] km s−1, respectively. These results indicate that YSO kinematics are not significantly affected by these different types of feedback environments. Additionally, compared to the Class II YSOs, Class III YSOs have slightly larger velocities and dispersions.

HETDEX-LOFAR Spectroscopic Redshift Catalog∗ ∗Based on observations obtained with the Hobby–Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen.

We combine the power of blind integral field spectroscopy from the Hobby–Eberly Telescope (HET) Dark Energy Experiment (HETDEX) with sources detected by the Low Frequency Array (LOFAR) to construct the HETDEX-LOFAR Spectroscopic Redshift Catalog. Starting from the first data release of the LOFAR Two-metre Sky Survey, including a value-added catalog with photometric redshifts, we extracted 28,705 HETDEX spectra. Using an automatic classifying algorithm, we assigned each object a star, galaxy, or quasar label along with a velocity/redshift, with supplemental classifications coming from the continuum and emission-line catalogs of the internal, fourth data release from HETDEX (HDR4). We measured 9087 new redshifts; in combination with the value-added catalog, our final spectroscopic redshift sample is 9710 sources. This new catalog contains the highest substantial fraction of LOFAR galaxies with spectroscopic redshift information; it improves archival spectroscopic redshifts and facilitates research to determine the [O ii] emission properties of radio galaxies from 0.0 < z < 0.5, and the Lyα emission characteristics of both radio galaxies and quasars from 1.9 < z < 3.5. Additionally, by combining the unique properties of LOFAR and HETDEX, we are able to measure star formation rates (SFRs) and stellar masses. Using the Visible Integral-field Replicable Unit Spectrograph, we measure the emission lines of [O iii], [Ne iii], and [O ii] and evaluate line-ratio diagnostics to determine whether the emission from these galaxies is dominated by active galactic nuclei or star formation and fit a new SFR–L 150MHz relationship.

Microlensing Events in Five Years of Photometry from the Zwicky Transient Facility

Microlensing has a unique advantage for detecting dark objects in the Milky Way, such as free-floating planets, neutron stars, and stellar-mass black holes. Most microlensing surveys focus on the Galactic bulge, where higher stellar density leads to a higher event rate. However, microlensing events in the Galactic plane have closer lenses and longer timescales, which leads to a greater chance of measuring microlens parallax, providing an additional constraint on the mass of the lens. This work searches for microlensing events in Zwicky Transient Facility (ZTF) Data Release 17 from 2018 to 2023 in the Galactic plane region. We find 124 high-confidence microlensing events and 54 possible events, all available online (see footnote 11). Thus, with 2 yr of additional ZTF data in DR17, we have more than doubled the number of microlensing events (60) found in the previous 3 yr DR5 search. In the event selection, we use the efficient EventFinder algorithm to detect microlensing signals, which could be used for large data sets such as future ZTF data releases or data from the Rubin Observatory Legacy Survey of Space and Time. Using detection efficiencies of ZTF fields obtained from catalog-level simulations, we calculate the mean Einstein timescale to be 〈t E〉 = 51.7 ± 3.3 days, smaller than previous results of the Galactic plane but within 1.5σ. We also calculate optical depths and event rates, although some caution is needed due to the use of visual inspection when creating our final sample. Spectroscopy of three possible candidates confirms their microlensing nature.

A Compilation of Optical Starlight Polarization Catalogs

Polarimetry of stars at optical and near-infrared wavelengths is an invaluable tool for tracing interstellar dust and magnetic fields. Recent studies have demonstrated the power of combining stellar polarimetry with distances from the Gaia mission, in order to gain accurate, 3D information on the properties of the interstellar magnetic field and the dust distribution. However, access to optical polarization data is limited, as observations are conducted by different investigators, with different instruments, and are made available in many separate publications. To enable a more widespread accessibility of optical polarimetry for studies of the interstellar medium, we compile a new catalog of stellar polarization measurements. The data are gathered from 81 separate publications spanning two decades since the previous, widely used agglomeration of catalogs by C. Heiles. The compilation contains a total of 55,742 measurements of stellar polarization. We combine this database with stellar distances based on the Gaia Early Data Release 3, thereby providing polarization and distance data for 42,482 unique stars. We provide two separate data products: an extended catalog (containing all polarization measurements) and a unique source catalog (containing a subset of sources excluding duplicate measurements). We propose the use of a common tabular format for the publication of stellar polarization catalogs to facilitate accessibility and increase discoverability in the future.

Assessing the detection of the Yarkovsky effect using the Gaia DR3 and FPR catalogues

Aims. The primary objective of this study was to use the newest Gaia Focused Product Release (FPR) catalogue, which contains ultra-precise asteroid astrometry spanning 66 months, to detect the Yarkovsky effect. This non-gravitational acceleration affects the orbits of small asteroids. Moreover, we examined close approaches of near-Earth asteroids by comparing orbits calculated based on Gaia data. Methods. We used the conventional least-squares orbit computation method, which is available in the OrbFit software (version developed at the MPC). We used the latest Gaia FPR, complemented by data from the Minor Planet Center and radar astrometry from the Jet Propulsion Laboratory. We fitted the orbital parameters for 446 eear-Earth asteroids, including the additional non-gravitational transverse acceleration, to model the Yarkovsky effect. Furthermore, we compared the results obtained using different datasets: the Gaia FPR, and the previous Gaia Data Release 3 (DR3). Results. We detected a robust Yarkovsky effect in 43 NEAs. As expected, we found an improvement in the orbital element uncertainty and in the signal-to-noise ratio of the Yarkovsky effect detections when we used the current Gaia FPR with twice the observing arc compared to the Gaia DR3 catalogue. We also found nine additional reliable detections of the Yarkovsky effect based on the new Gaia FPR catalogue. Conclusions. It can be important to include the Yarkovsky effect in the force model to reliably estimate close-approach distances of near-Earth asteroids. Several of the detected Yarkovsky drifts already have a signal-to-noise ratio greater than 10, which is high enough for their Yarkovsky effect to be included in their reliable long-term orbital evolution, close approach, and Earth-impact analysis. The final Gaia catalogue may provide a much higher number of detections with a high signal-to-noise ratio of the Yarkovsky effect. This would allow us to include the effect more broadly in routine close-approach and impact analyses of these objects.

Mining Double-line Spectroscopic Candidates in the LAMOST Medium-resolution Spectroscopic Survey Using a Human–AI Hybrid Method

We utilize a hybrid approach that integrates the traditional cross-correlation function (CCF) and machine learning to detect spectroscopic multiple star systems, specifically focusing on double-line spectroscopic binaries (SB2s). Based on the ninth data release (DR9) of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST), which includes a medium-resolution survey (MRS) containing 29,920,588 spectra, we identify 27,164 double-line and 3124 triple-line spectra, corresponding to 7096 SB2 candidates and 1903 triple-line spectroscopic binary (SB3) candidates, respectively, representing about 1% of the selected data set from LAMOST-MRS DR9. Notably, 70.1% of the SB2 candidates and 89.6% of the SB3 candidates are newly identified. Compared to using only the traditional CCF technique, our method significantly improves the efficiency of detecting SB2s, saving time on visual inspections by a factor of 4.

Development and early life stress sensitivity of the rat cortical microstructural similarity network.

Network models derived from neuroimaging have revolutionized our understanding of human brain development but need translation into animal models to interrogate their underlying mechanisms. Rats provide a valuable model due to their complex behaviors and biological similarities to humans; however, in vivo models of individual-level brain networks remain underdeveloped. In this study, we present a novel computational pipeline to construct such networks from in vivo rat structural neuroimaging data. Our findings highlight the dynamic development and experiential sensitivity of fronto-hippocampal systems in rats, offering a reference for cross-species comparisons and mechanistic insights into brain architecture. To support broader research efforts, we include an open release of code and data for rat MIND similarity network analysis.

The Redshift-space Momentum Power Spectrum. III. Measuring the Growth Rate from the SDSSv Survey Using the Auto- and Cross-power Spectrum of the Galaxy Density and Momentum Fields

The large-scale structure of the Universe and its evolution over time contains an abundance of cosmological information. One way to unlock this is by measuring the density and momentum power spectrum from the positions and peculiar velocities of galaxies and fitting the cosmological parameters from these power spectra. In this paper, we will explore the cross-power spectrum between the density and momentum fields of galaxies. We derive the estimator of the density–momentum cross-power spectrum multipoles. The growth rate of the large-scale structure, f σ 8, is measured from fitting the combined density monopole, momentum monopole, and cross-dipole power spectrum. The estimators and models of the power spectrum as well as our fitting method have been tested using mock catalogs; we find that they perform well in recovering the fiducial values of the cosmological parameters of the simulations, and we also find that the errors of the parameters can be largely reduced by including the cross-power spectrum in the fit. We measure the autodensity, automomentum, and cross-power spectrum using the Sloan Digital Sky Survey Data Release 14 peculiar velocity catalog. The fit result of the growth rate f σ 8 is fσ8=0.413−0.058+0.050 at effective redshift z eff = 0.073, and our measurement is consistent with the prediction of the Lambda cold dark matter cosmological model, assuming general relativity.

The Impact of Void-finding Algorithms on Galaxy Classification

We explore how the definition of a void influences the conclusions drawn about the impact of the void environment on galactic properties using two void-finding algorithms in the Void Analysis Software Toolkit: Voronoi Voids (V 2 ), a Python implementation of ZOnes Bordering On Voidness (ZOBOV); and VoidFinder, an algorithm that grows and merges spherical void regions. Using the Sloan Digital Sky Survey Data Release 7, we find that galaxies found in VoidFinder voids tend to be bluer and fainter and to have higher (specific) star formation rates than galaxies in denser regions. Conversely, galaxies found in V 2 voids show less significant differences when compared to galaxies in denser regions, less consistent with the large-scale environmental effects on galaxy properties expected from both simulations and previous observations. These results align with previous simulation results that show V 2 -identified voids “leak” into the dense walls between voids because their boundaries extend up to the density maxima in the walls. As a result, when using ZOBOV-based void-finders, galaxies likely to be part of wall regions are instead classified as void galaxies, a misclassification that can be critical to our understanding of galaxy evolution.

Detection and characterization of giant planets with Gaia astrometry

ABSTRACT Astrometric observations with Gaia are expected to play a valuable role in future exoplanet surveys. With current data from Gaia’s third data release (DR3), we are sensitive to periods from less than 1 yr to more than 4 yr but, unlike radial velocity (R.V.) are not as restricted by the orbital inclination of a potential planet. The presence and potential properties of a companion affect the primary’s renormalized unit weight error (RUWE) making this a valuable quantity in the search for exoplanets. Using this value and the fitted astrometric tracks from Gaia, we use Bayesian inference to constrain the mass and orbital parameters of companions in known systems. Combining this with R.V. measurements, we show it is possible to independently measure mass and inclination and suggest HD 66141 b is a possible brown dwarf with maximum mass 23.9$^{+7.2}_{-6.4}$ $\mathrm{ M}_{\mathrm{J}}$. We show how this method may be applied to directly imaged planets in the future, using $\beta$-Pictoris c as an example but note that the host star is bright and active, making it difficult to draw clear conclusions. We show how the next Gaia data release, which will include epoch astrometry, will allow us to accurately constrain orbital parameters from astrometric data alone, revolutionizing future searches for exoplanets. Combining predicted observational limits on planet mass with theoretical distributions, we estimate the probability that a star with a given RUWE will host a detectable planet, which will be highly valuable in planning future surveys.

Constraining dark energy with the integrated Sachs-Wolfe effect

We use the integrated Sachs-Wolfe (ISW) effect, by now detectable at ∼5σ within the context of Λ cold dark matter (ΛCDM) cosmologies, to place strong constraints on dynamical dark energy theories. Working within an effective field theory (EFT) framework for dark energy we find that including ISW constraints from galaxy–cosmic microwave background (CMB) cross-correlations significantly strengthens existing large-scale structure constraints, yielding bounds consistent with ΛCDM and approximately reducing the viable parameter space by ∼70%. This is a direct consequence of O(1) changes induced in these cross-correlations by otherwise viable dark energy models, which we discuss in detail. We compute constraints by adapting the ΛCDM ISW likelihood from Stölzner [] for dynamical dark energy models using galaxy data from 2 MASS, wide-field infrared survey explorer (WISE) × SuperCOSMOS, Sloan Digital Sky Survey Data Release 12, the catalog of photometric quasars and NRAO Very Large Array Sky Survey, CMB data from Planck 18, and baryon acoustic oscillation and redshift space distortion large-scale structure measurements from BOSS and 6dF. We show constraints both in terms of EFT-inspired αi and phenomenological μ/Σ parametrizations. Furthermore we discuss the approximations involved and related aspects of bias modeling in detail and highlight what these constraints imply for the underlying dark energy theories. Published by the American Physical Society 2024

Dietary inflammatory index and its associations with cardiovascular diseases and cancer: Evidence form NHANES 2017-2018 and Mendelian randomization analysis.

Cardiovascular diseases (CVDs) and cancer are significant global causes of mortality. However, the link between diets that promote inflammation and various subtypes of CVDs and cancers remains unclear. Utilizing the dataset from the 2017-2018 National Health and Nutrition Examination Survey (NHANES) data release cycle, our study encompassed 3538 adult participants within the age range of 20 to 80 years. The dietary questionnaire information was utilized to calculate dietary inflammatory index (DII) scores. Logistic regression analysis was employed to validate the association between the DII and CVDs, as well as overall cancer and special type cancer. Mediation analysis was conducted to evaluate the relationship between DII and the aforementioned diseases, with hemoglobin serving as the potential mediator. Mendelian randomization (MR) analysis externally validated hemoglobin's causal link to these diseases. Patients with the highest quartile levels of DII scores demonstrated an elevated prevalence of congestive heart failure (CHF), stroke, overall cancer and some specific types of cancers. The logistic regression analysis revealed a correlation between DII and CHF (OR = 1.197, p = 0.002), stroke (OR = 1.205, p < 0.001), as well as breast cancer (OR = 1.306, p = 0.004). The pro-inflammatory diet also resulted in lower hemoglobin levels (p < 0.001). Mediation analyses found a role for hemoglobin in the relationship of DII and CVDs. Both CVDs and cancer risk were positively correlated with the DII in our study. Hemoglobin emerged as a potential mediator in the intricate relationship between DII and CHF, as well as stroke.

Astrometric Calibration of MagAO-X with Updated Solutions for HD 165054 Field Stars

Abstract MagAO-X is a recently commissioned extreme adaptive optics instrument for the Magellan Clay 6.5 m telescope at Las Campanas Observatory in Chile. MagAO-X had first light in 2019 and subsequent commissioning observations in 2022 and 2023. An essential step for the commissioning of any new instrument is the calibration of the conversion of detector coordinates to angular sky coordinates, which we accomplish with observations of HD 165054. The background stars adjacent to HD 165054 in Baade’s Window are in a fortuitous configuration for the astrometric calibration of natural-guide-star high-contrast imaging instruments. We extend past work to connect these stars’ positions to absolute astrometry for HD 165054 itself using Gaia Data Release 3 data, and bootstrap the creation of an astrometric solution for our new high-contrast imaging instrument. Through Markov Chain Monte Carlo analysis of the historical data and position measurements from MagAO-X, we obtain updated astrometric parameters for the seven background stars and an astrometric calibration of the MagAO-X science cameras.

The impact on astrometry by solar-wind effect in pulsar timing

Abstract Astrometry of pulsars, particularly their distances, serves as a critical input for various astrophysical experiments using pulsars. Pulsar timing is a primary approach for determining a pulsar’s position, parallax, and distance. In this paper, we explore the influence of the solar wind on astrometric measurements obtained through pulsar timing, focusing on its potential to affect the accuracy of these parameters. Using both theoretical calculation and mock-data simulations, we demonstrate a significant correlation between the pulsar position, annual parallax and the solar-wind density parameters. This correlation strongly depends on the pulsar’s ecliptic latitude. We show that fixing solar-wind density to an arbitrary value in the timing analysis can introduce significant bias in the estimated pulsar position and parallax, and its significance is highly dependent on the ecliptic latitude of the pulsar and the timing precision of the data. For pulsars with favourable ecliptic latitude and timing precision, the astrometric and solar-wind parameters can be measured jointly with other timing parameters using single-frequency data. The parameter correlation can be mitigated by using multi-frequency data, which also significantly improves the measurement precision of these parameters; this is particularly important for pulsars at a medium or high ecliptic latitude. Additionally, for a selection of pulsars we reprocess their EPTA Data Release 2 data to include modelling of solar-wind effect in the timing analysis. This delivers significant measurements of both parallax and solar-wind density, the latter of which are consistent with those obtained at low-frequency band. In the future, combining pulsar timing data at gigahertz and lower frequencies will probably deliver the most robust and precise measurements of astrometry and solar wind properties in pulsar timing.

The reliability of gas-phase metallicities immediately adjacent to non-star-forming spaxels in MaNGA

Abstract In this work, we use gas phase metallicities calculated from the Sloan Digital Sky Survey (SDSS) Mapping Nearby Galaxies at Apache Point (MaNGA) Data Release 17 (DR17) to assess the extent of potential biases in spaxels which are spatially adjacent to spaxels identified as non-star forming (non-SF) on a BPT diagram. We identify a sample of ∼21, 000 such spaxels with calculable metallicities from the full metallicity catalogue (∼1.57 million), representing a small fraction (∼1.3 per cent) of the full metallicity sample. ∼23 per cent of all galaxies with at least one spaxel with a calculable metallicity also contain at least one spaxel with a calculated metallicity adjacent to a non-SF spaxel, with a typical galaxy hosting 9 non-SF-adjacent spaxels. From our suite of 6 different metallicity calibrations, we find that only the metallicity calibrations based entirely on the [N ii]6584/Hα ratio are affected, showing systematic offsets to higher metallicities by up to ∼0.04 dex if they are located adjacent to a non-SF flagged spaxel, relative to a radially matched control sample. The inclusion of additional diagnostic diagrams (based on [O i]6300 &amp;/or [S ii]6717 + 6731) is insufficient to remove the observed offset in the [N ii]6584/Hα based calibrations. Using a stricter diagnostic line on the BPT diagram removes ∼94 per cent of identified bordering spaxels with metallicities for all metallicity calibrations, and removes the residual offset to higher metallicity values seen in [N ii]6584/Hα calibrations. If science cases demand an exceptionally clean metallicity sample, we recommend either a stricter BPT cut, and/or a non-[N ii]6584/Hα based metallicity calibration.