Formaldehyde (HCHO) is a hazardous atmospheric pollutant; however, spatiotemporal discrepancies between tropospheric column density (CHCHO) and surface concentration (SHCHO) hinder the accurate derivation of surface concentrations from satellite observations. Based on 2.5 years of vertical profile measurements from 18 sites within China's hyperspectral remote sensing network, this study demonstrates that HCHO is predominantly enriched below 0.2 km. Its diurnal variation exhibits a midday-evening bimodal pattern driven by boundary layer dynamics, photochemistry, and anthropogenic emissions. Using Generalized Additive Models (GAMs), we identify the dominant drivers of CHCHO and SHCHO across urban, suburban, and background environments. CHCHO is consistently governed by regional photochemistry (31-52% contribution), whereas SHCHO is primarily controlled by anthropogenic emissions in urban areas (29%) and shifts toward photochemical dominance in suburban (42%) and background (51%) regions. Discrepancies in the response magnitudes of CHCHO and SHCHO to strong emissions and photochemical activity substantially weaken their correlation. By integrating vertical profiles with height-resolved GAMs, we further characterize altitude-dependent mechanisms governing column-to-surface conversion. HCHO below 0.2 km is regulated by local emissions and photochemistry, transitions to photochemical dominance in the middle layer, and becomes increasingly influenced by seasonal variability, large-scale meteorology, and biogenic activity in the upper layer (>1.0 km).

Abstract Single-pointing observations of 73 Planck cores from the Early Cold Core Catalogue with the Nanshan 26-m telescope are presented targeting the H2CO (11, 0–11, 1) 4.8 GHz (λ ~ 6 cm) absorption line. H2CO absorption has been detected in 51 sources (69.9%), with 24 (32.9%) also showing components with hyperfine structure (HFS). In these 51 detected cores, non-thermal velocity dispersion dominates over thermal line broadening (σTH/σNT < 1), with 96% exhibiting supersonic turbulence ($\mathcal {M} > 1$). A weak correlation between σNT and Tkin suggests that turbulence contributes to gas heating. A strong σNT – ortho-H2CO column density correlation highlights the importance of both turbulence and gravity. For the 24 sources with resolved HFS, the derived excitation temperatures ranges from 2.08 to 2.59 K (mean 2.37 K). Follow-up mapping of four high-S/N cores with regions of resolved HFS components reveals widespread gas with Tex ≈ 2.36–2.64 K. Cores with resolved HFS exhibit narrower line widths, lower Mach numbers, higher column densities, and larger optical depths, indicating dynamically quiescent gas in clouds moving towards early gravitational collapse. In contrast, non-HFS regions surrounding the HFS regions in these sources display broader lines and stronger non-thermal motions, suggesting a dynamically complex environment where gravity begins to influence the earliest stages of star formation.

The outer Galaxy presents an optimal setting for investigating molecular clouds and star formation in environments with low-metallicity. A total of 72 Galactic edge clouds were surveyed using the CO,(2--1) line with the IRAM,30,m telescope, leading to the identification of 112 CO clumps within molecular clouds with linear resolutions of 0.5--0.9,pc. The parameters such as size, mass, surface density, and velocity dispersion of these CO clumps, derived from CO,(2--1) observations, exhibit ranges of 0.6--3.4,pc, 34--8250,M_⊙, 12--1025,M_⊙,pc-2, and -1 , respectively. Over the galactocentric distance range of 14--23,kpc, no systematic variations are found in these parameters. The velocity dispersion--size relationship of the Galactic edge clumps is modeled as σ_̊m v,=,0.69(±0.03)R_ ̊m eff ^ 0.36( , indicating that turbulence is present within the Galactic edge clumps, similarly to observations in the inner Galactic disk clouds. Furthermore, the luminous mass--size relation of the Galactic edge clumps is described by M_̊m lum,=,196(±17)R_ ̊m eff ^ ,2.18,( , suggesting the average column density remains almost constant for clouds of different sizes. The virial parameters range from 0.6 to 15.3, with a median value of 2.8,±,0.6, suggesting that most clumps are gravitationally unbound. Furthermore, the virial parameters of our Galactic edge clumps show a decreasing trend with increasing galactocentric distances, described by an exponential relation α_̊m vir,=,33.0(±,10.4),e -R_ ̊m g /6.7( , consistent with previous results.

The Seyfert 1 galaxy NGC 3783 hosts a multi-phase warm absorber (WA) that has been extensively studied in the X-ray band. High-resolution spectra from 2000–2001 revealed a complex outflow with multiple ionization and velocity components. Two decades later, new . The ranges of column densities and turbulent velocities remain broadly consistent with the WAs from 2000–2001, but the earlier data contained more low-ionization, high-velocity components. The total column density of all the outflows in 2024 is 1.5 times larger than in 2000-2001, which means that it has been replenished by fresh material. The dominant unresolved transition array (UTA) absorber (component B3) has increased its column density by a factor of three while maintaining a similar ionization parameter. The WAs in NGC 3783 have undergone significant structural and dynamical evolution over the past 24 years. and observations allow us to investigate the long-term evolution of these outflows. We performed joint spectral modelling of the and time-averaged spectra using the photoionization code within We derived the ionization parameter, column density, turbulent velocity, and outflow velocity for each absorption component, and investigated their thermal stability and absorption measure distribution (AMD) to characterize the physical and dynamical properties of the WA in NGC 3783 in 2024. We compared these results with the 2000–2001 epoch to assess long-term variability, stability, and possible changes in the absorber population. We identify eight WA components spanning łogxi = 1.08–3.38 and outflow velocities of 480–1230 km s -1

Abstract We analyze the high velocity cloud HVC 53.9+1.3 using the highly sensitive and high angular resolution HI data piggybackly recorded by the FAST Galactic Plane Pulsar Snapshot (GPPS) survey. Detailed sub-structures of the HVC are resolved, the densest peak of the HVC has a HI column density of N HI = 3.5 × 10 19 cm -2 , two orders lower than the main component of the Galactic HI disk. Using the Gaussian decomposition method, cold and warm phases of HI gas clouds are separated. Cold HI gas is found in a supersonic state with Mach number of M = 2.3, and tends to associate with high HI density, with cold cores surrounded by skins of warmer gas, while warmer gas are in subsonic state with M < 1.

Abstract Based on Insight-HXMT observations, we present a detailed timing analysis and spectral evolution of a complete main high state for Her X-1 in 2020 February. We determine an accurate local ephemeris using the Rmer delay measured from five eclipses. We report the spin period of the neutron star at P spin = 1.23765212 ± 0.00000026 s with a spin period derivative of P ̇ spin = − ( 1.18 ± 0.04 ) × 1 0 − 13 s s −1 . By combining the newly measured local values T ecl with those reported in the literature, we refine the orbital ephemeris of Her X-1, obtaining T ecl = 46359.871956 ± 0.000010 MJD and P orb = 1.7001674990 ± 0.0000000105 days, and then detect a continuous decrease in the orbital period with a rate of P ̇ orb = − ( 1.957 ± 0.335 ) × 1 0 − 11 day day − 1 . We also investigate the evolution of X-ray spectral parameters during the main high state. The hydrogen absorption column density N H increased monotonously during the phase, and the photon index kept nearly constant. The cyclotron absorption line was detected with a centroid energy around 38 keV, showing no significant evolution with luminosity. The spectral variations with the superorbital phase are discussed within the accretion disk precession scenario.

Abstract Acetone (CH3COCH3) is a ubiquitous interstellar molecule, and serves as an important tracer of hot core chemistry. We conducted a line survey of acetone and its precursor acetaldehyde (CH3CHO) towards 60 hot cores by using the ALMA 3 mm lines observations. We calculated the rotational temperatures and column densities of acetone using the XCLASS software. Acetone was detected in 15 hot cores with rotational temperatures ranging from 89 to 176 K. Its column densities range from (0.9-24) × 1016 cm−2. The spatial distributions of acetone exhibit similarities with those of acetaldehyde. The emissions of acetone are concentrated toward the hot core regions and generally exhibit a compact spatial distribution, whereas the emission of acetaldehyde shows a more extended spatial profile. Combined with previous studies, we found a moderately positive correlation between the column densities and rotational temperatures of acetone for the high-mass hot cores (r = 0.59). We also found a strong positive correlation between the column densities of acetone and acetaldehyde (r = 0.82), indicating a chemical relationship between them. By comparing these observational results with the three-phase model results, we found that the models overpredict the ratio of acetone to methanol relative to the observational data. This discrepancy suggests that current chemical networks may inadequately account for acetone destruction pathways or potential missing physical conditions in the model. Therefore, our large sample observations can provide constraints on chemical models and reinforce the role of acetone as a tracer of complex organic chemistry in warm, dense regions.

Dark galaxies are small, dark matter-dominated haloes whose gas remains in hydrostatic and thermal equilibrium and has never formed stars. These systems are of particular interest because they represent a strong prediction of the Lambda cold dark matter ( łcdm ) model. As of today, only a few dark galaxy candidates have been detected so far, the most intriguing of which being Cloud-9. Using several state-of-the-art hydrodynamical simulations, we aim to predict the abundance of dark galaxies within our Local Group, characterise their physical properties, and provide guidance for their potential observational detection. We analyse Local Group simulations with constrained initial conditions, each run with different codes, implementing different baryonic physics, feedback prescriptions, and employing two distinct values of star-formation density threshold, n_ th =0.13 and 10, cm^ -3 , to select samples of dark and bright galaxies harboured in haloes of similar mass. We demonstrate that dark galaxies exist in all such simulations, though their number is larger in simulations that use a higher, more realistic n_̊m th. These galaxies, whose gas remains diffuse and never forms stars, predominantly inhabit less-concentrated, higher-spin dark matter haloes than their luminous counterparts. Dark galaxies are typically found in low-density regions at the outskirts of the Local Group. Their formation and evolution across redshift indicate that both the dark matter and gas densities in the surroundings of dark galaxies were consistently lower than those found around bright galaxies, making them less susceptible to interactions, mergers, or gas inflows. We estimate that up to eight dark galaxies should be detectable in ̋Isc emission within 2.5,̊m Mpc of the Milky Way, with the FAST radio telescope, accounting for its sky coverage and minimum ̋Isc mass and column density. Current hydrodynamical simulations of galaxies, combined with upcoming ̋Isc surveys, will offer a direct and powerful test of łcdm through their ability to predict and measure properties of dark galaxies within and beyond the Local Group.

Abstract We use constrained idealized simulations of the Large Magellanic Cloud (LMC)/Milky Way interaction to determine if the size of the LMC’s gaseous halo (Corona) can be used to distinguish between first and second passage models—an orbital trajectory for the LMC in which it has just recently approached the Milky Way for the first time (first passage) or one in which it has had a previous pericenter (second passage). Using live circumgalactic gas particles combined with analytic dark matter potentials evolved to follow previously published orbital trajectories, we find that the first passage model is able to reproduce the observed velocity profile and column density profile of the present day LMC Corona. On the other hand, in a second passage scenario, the longer interaction time leads to the velocities and column densities around the LMC at the present day being significantly lower than observations. Based on this observed velocity profile, recent works have found that the LMC’s Corona has been truncated to 17–20 kpc, and we find truncation radii of 16.6 ± 0.5 kpc and 5 . 7 − 2.2 + 1.8 kpc for the first and second passage models, respectively. Thus, based on the gas properties of the LMC’s circumgalactic medium at the present day, a second passage trajectory is strongly disfavored.

Abstract We utilize James Webb Space Telescope/Mid Infrared Instrument (JWST/MIRI) Integral Field Unit observations from the Galaxy Activity, Torus and Outflow Survey to investigate the diverse range of ionized outflow rates of obscured active galactic nuclei (AGN) with similar bolometric luminosity and explore potential associations with AGN feedback. We explore spatial correlations between ionized emission potentially associated with fast shocks ([Fe II ] 5.34 μ m ) and the excitation of H 2 . We further constrain our investigation to the inner 400 pc (the nuclear and circumnuclear regions r < 200 pc), and estimate the excitation temperature and column density of H 2 assuming local thermodynamic equilibrium and using the S(1)–S(8) rotational H 2 emission lines visible to JWST/MIRI spectroscopy. We report the molecular gas temperature of the deprojected 400 pc nuclear region to correlate with the ionized mass outflow rate. We also observe a stronger degree of spatial correlation between [Fe II ] 5.34 μ m emission and H 2 gas temperature. We observe regions of enhanced [Fe II ] 5.34 μ m /[Ar II ] 6.99 μ m spatially coincident with the ionization cones of objects with higher ionized outflow rates and [Fe II ] 5.34 μ m /[Ar II ] 6.99 μ m in the deprojected 400 pc nuclear region to scale positively with both the ionized outflow rate and the estimated molecular gas temperature. We do not observe the estimated jet cavity power within the central 400 pc as strongly correlated with the ionized mass outflow rate or molecular gas temperature of the nuclear region. We take the preceding observations to suggest a higher degree of interaction between AGN outflows and the circumnuclear disk.

Abstract We report the discovery of two broad-line X-ray active galactic nuclei (AGNs) ( cid_414 and cid_947 ) at z ∼ 3 identified in the JWST Cycle 3 COSMOS-3D program using NIRCam F444W grism spectroscopy. Both exhibit prominent He i λ 10830 +Pa γ emission and absorption, indicative of circumnuclear dense gas that is traced in these systems. Complementary UV and optical spectroscopy in the COSMOS field provides Ly α , Si iv , and C iv measurements. Both sources are detected in MIRI F1000W, and cid_414 is also detected in F2100W, indicating hot dust emission. The two AGNs show distinct black hole and obscuration properties. The source cid_414 displays little red dot (LRD)-like, V-shaped spectral energy distribution with a turnover near the Balmer 4000 Å break and a narrow Ly α line with log L Ly α = 42.49 ± 0.01 erg s − 1 , with no additional metal lines detected. In contrast, cid_947 exhibits a higher He i λ 10830 absorption column density, larger X-ray–inferred N H , lower intrinsic 2–10 keV luminosity, and strong blueshifted features in He i , Si iv , and C iv absorption with velocity offsets exceeding 5000 km s −1 . Photoionization modeling implies gas densities of ∼10 9−10 cm −3 and sizes comparable to the broad-line region, consistent with dense gas envelopes predicted for LRDs. Together with previous detections of He i λ 10830 absorption in compact LRDs, these results suggest that dense circumnuclear gas is likely prevalent at high redshift and may regulate obscuration and black hole–host coevolution across AGN types.

Abstract High velocity clouds supply the Milky Way with gas that sustains star formation over cosmic timescales. Precise distance measurements are therefore essential to quantify their mass inflow rates and gauge their exact contribution to the Galaxy’s gas supply. We use a sample of 594 SDSS-V BOSS stellar spectra within 10° of the high-velocity Smith Cloud (SC) to trace Na I absorption and dust extinction as functions of distance. By fitting interstellar-medium-corrected MaStar templates to each spectrum, we isolate residual equivalent widths and extinction and then compare trends in the SC region to a same-latitude control field. Stars beyond 1 kpc toward the SC exhibit a significant Na I equivalent width excess (>0.2 Å, >3 σ ) relative to the control. Two-component linear fits of Na I equivalent width and A V against both low and high-velocity H I column densities show that the low-velocity component is strongly correlated with both quantities, while the high-velocity term is marginally significant in extinction and Na I , consistent with a patchy, low dust-to-gas ratio. Given that the excess Na I begins at distances <2 kpc uniquely in the direction of the SC, and previous estimates of the SC place it at 12.4 ± 1.3 kpc, further investigation of its distance is warranted.

We extended the radio K-band spectroscopic survey for organics in southern hemisphere dense cores by observing seven sources using NASA's Deep Space Network 70 m antenna in Canberra, Australia, over the frequency range 18 to 25 GHz. Molecular column densities of NH_3, c-C_3H_2, HC_3N, HC_5N, CCS, C_3S, and c-C_3HD were derived for each source assuming local thermodynamic equilibrium. The resulting column density ratios were compared with predictions of a state-of-the art astrochemical model to constrain the C/O ratio and chemical age of each source. Most cores have similar C/O ratios of 0.5 - 0.7, much different from the best studied TMC-1 dense core, which is characterized by a high C/O ratio of ∼ 1.4. The chemical ages of the cores are also similar and fall between 0.6 and 5 Myr. The less dense cores tend to have the oldest chemical ages, as might be expected given that chemical timescales scale with density. Our results showcase the synergistic approach of combining radio observations using the DSS-43 antenna with state-of-the-art astrochemical models to study the chemical composition of southern hemisphere dense cores, enabling constraints to be placed on their C/O ratios and chemical ages, which remain largely unexplored.

Abstract We report Giant Metrewave Radio Telescope (GMRT) H i 21 cm imaging of NGC 4141, the host galaxy of FRB 20250316A at z = 0.0063. Our GMRT H i 21 cm images have spatial resolutions, at z ≈ 0.0063, of ≈0.48–8.0 kpc, and provide evidence for (i) a companion galaxy, LEDA 2582852, to the southwest, (ii) a nearby (27 kpc distant) H i cloud to the southwest, (iii) disturbances in the H i distributions of both NGC 4141 and LEDA 2582852, and (iv) high H i column densities in the southwestern outskirts of NGC 4141. A Sloan Digital Sky Survey spectrum yields a low metallicity and a high star formation rate (SFR) surface density in the southwestern disk of NGC 4141, and an H α -based SFR estimate that is significantly higher than that at the same location from the Galaxy Evolution Explorer near-ultraviolet image, indicating a recent burst of star formation. The total SFR of NGC 4141 is also found to be higher via the H α line than from the 1.4 GHz radio continuum. The above evidence indicates that NGC 4141 has recently (within the last ≈3 Myr) acquired metal-poor gas, via either a merger or accretion, that resulted in the southwestern starburst and that may also have triggered large-scale star-formation activity in NGC 4141, resulting in the formation of the stellar progenitor of FRB 20250316A and the other transients. Our highest-resolution (480 pc) GMRT H i 21 cm image finds no H i 21 cm emission from the location of FRB 20250316A or the nearby star-forming region, suggesting that most of the H i here has been either ionized or converted into the molecular phase. Our nondetection of continuum emission at the location of FRB 20250316A yields the 3 σ upper limit νL 1.38 GHz < 4.4 × 10 34 erg s −1 on the 1.38 GHz radio luminosity of a putative persistent radio source associated with FRB 20250316A, one of the strongest constraints on the radio luminosity of such an associated persistent radio source.

Abstract NGC 4051 is a nearby (16.7 Mpc), Narrow Line Seyfert 1 galaxy (NLS1), which has a low black hole mass of 10 6 M ⊙ . It is also known for its rapid X-ray variability, on timescales of kiloseconds, and has a complex, multicomponent wind in both the soft X-ray and Fe K bands. Here we present the first high-resolution XRISM Resolve spectrum of NGC 4051, which was captured in a historically bright state for a 150 ks exposure. XRISM resolves two blueshifted Fe K shell absorption troughs in the mean spectrum, which can be ascribed to H-like iron and arises from two outflow components with outflow velocities of 0.025 c and 0.04 c . A time-dependent spectral analysis shows that the iron K absorption is variable on timescales of less than a day, increasing in velocity over the duration of the observation. The velocity changes may be explained either by the passage of two separate transiting absorbers, of different velocities, or by a single accelerating outflow of approximately constant column density. In the latter case, the wind acceleration is likely to be too large to be caused by radiation pressure, and instead, magnetic driving is favored to accelerate the wind up to 0.04 c . The outflow can originate from an accretion disk wind, whose kinetic power is sub-Eddington, in contrast to recent examples of winds from powerful, luminous quasars observed by XRISM.

ABSTRACT It has recently been suggested that the typical separation between cores in molecular clouds dominated by turbulence is determined by the sonic scale, the size scale at which the turbulent velocity dispersion equals the sound speed. In this work, we test this hypothesis using a suite of non self-gravitating, purely hydrodynamic turbulent simulations with Mach numbers $\mathcal {M}=$ 2, 4, and 8, and three turbulent forcing wavenumbers ($k_{\rm for}=2,4$, and 8). Dense cores are identified through dendrogram analysis of column density maps, and their separations are compared to the sonic scale measured from velocity structure functions. We find no statistical correlation between the core separation and the sonic scale nor the driving scale. Instead, for each run, the core separation spans the entire range of values between the resolution and the injection scale, and peaks at a scale apparently dependent on the resolution, even when the sonic scale has converged. This could be the consequence of the distribution of core separations being given by the distribution of travelling shock-compressed layers. Our results indicate that the mean separation between the smallest density structures in non-self-gravitating, supersonically turbulent flow is determined in simulations by the global sonic Mach number and the resolution, with no limit imposed by the sonic scale. This finding calls into question the use of the sonic scale as a predictive quantity in star formation theories and cautions against interpreting observational core spacings as evidence for universal turbulent fragmentation physics.

FEASTS and MHONGOOSE: H I Column Density Distribution at z = 0 for NHI > 1017.8​​​​​​ cm−2

This work presents an experimental methodology for the quantification of unburned methane (CH 4 ) flow in laboratory-scale air assisted flares. The approach relies on the use of a mid-infrared hyperspectral Fourier Transform Infrared (FTIR) imaging system operated in absorption mode, in combination with a gas capture setup that ensures complete extraction of combustion products. The extracted gases are directed through a T-shaped tube with an extended optical path, where their transmittance spectra are recorded and fitted to a radiative transfer model to retrieve CH 4 column densities. The core of the method is a calibration procedure that establishes a relationship between these column densities and mass flow rates by releasing known CH 4 flows through the burner and measuring the corresponding column densities in the tube. The methodology is applied to assess the performance in terms of the CH 4 destruction and removal efficiency (DRE CH 4 ) of a flare under different levels of air assistance and crosswind. The results reveal a critical threshold beyond which CH 4 emissions increase significantly due to partial flame extinction, thus lowering the DRE CH 4 , and demonstrate the method’s ability to resolve temporal variations in combustion efficiency with a time resolution of 10 s. Although developed in a controlled laboratory setting, the proposed technique provides a reliable framework for studying combustion instability and validating field-deployable remote sensing technologies. Its implementation can contribute to improving flare performance assessment and to the mitigation of methane emissions from industrial combustion sources. • A method is presented to quantify unburned methane in lab-scale flare systems. • FTIR system with methane filter to improve sensitivity and reduce noise. • A calibration process converts methane column density into mass flow rate. • Temporal resolution allows real-time monitoring of flame instabilities. • Method is suitable to calibrate and validate field detection techniques.

Most observational studies of galactic-scale magnetic fields using Faraday rotation rely on estimates of thermal electron densities in galaxies and their radial variations. However, the spatial distribution of electrons in the interstellar medium (ISM) is not clearly known. In this study, we propose and utilize collisionally-excited doublet emission line ratios of [S ii] λλ 6716, 6731 Å to estimate the electron densities (ne ). To map their distribution in the galaxies, we employ IFU spectroscopic observations from the SDSS MaNGA survey, utilising data products from the MaNGA Data Analysis Pipeline (DAP). We present a spatially resolved analysis of 66 face-on galaxies (inclination, i ≤ 15°), including 46 star-forming galaxies (SFGs) and 20 Non-SFGs. Azimuthally averaged radial profiles of ne are obtained. We found that both SFGs and Non-SFGs exhibit ne gradients, with higher densities of ne (S ii) = 52.87 ± 8.32 cm-3 and 99.39 ± 24.37 cm-3, respectively, in the inner disk region (r/R e ≤ 1.5), which decreases to ne (S ii) = 20.92 ± 4.2 cm-3 in SFGs and 34.64 ± 11.24 cm-3 in Non-SFGs, in the outer disk region (r/R e > 1.5). We have also analysed these sources with Pipe3D fluxes. We translated ne to electron column densities (Ne ) by assuming a typical disk of thickness 1 kpc and note that Ne ∼ 1022 cm-2 at ∼14 kpc in the disk outer region. We have also discussed the profiles obtained using [O ii] λλ 3726, 3729 Å doublet. These electron density estimates at different radii provide valuable insights for resolving ambiguities in current and future studies of magnetic fields in galaxies.

Context . Outflows and jets are defining characteristics in protostellar evolution, intimately linked to accretion. Understanding their properties and origins is essential for probing the earliest phases of star formation. Aims . This study characterizes the physical and kinematic properties within the innermost 500 au region of the L1527 bipolar outflow, a class 0/I low-mass protostar, as part of the JWST Observations of Young protoStars (JOYS) program. Methods . We obtained spectroscopic observations using the JWST MIRI/MRS instrument across 5-28 μm at 0.2-1.0″ spatial resolution. We identified emission lines from molecular and ionized species and analyzed their spatial morphology using line-integrated intensity maps. We derived gas temperatures and column densities from excitation diagram analysis of H 2 rotational lines and compared results with shock models. Results . The observations reveal extended molecular hydrogen emission tracing the bipolar outflow, with the H 2 gas temperatures distributed into warm (~550 K) and hot (~2500 K) components, likely originating from moderate-velocity J -type shocks and some UV irradiation. We detect forbidden atomic and ionized emission lines of [Ni II ], [Ar II ], [Ne II ], [Ne III ], [S I ], and [Fe II ] showing spatially extended morphology. Double-peaked emission profiles were seen in [Ar II ], [Ne III ], and [Fe II ] in the eastern region, suggesting that the high-velocity component traces a fast, highly ionized jet. A radial velocity map derived from [Ne II ] emission shows the eastern region to be redshifted and the western region blueshifted, contrary to earlier interpretations. Conclusions . The analysis of the MIRI/MRS observations reveals molecular, atomic, and ionized emission lines in this low-mass protostar connected with active outflow signatures. The most striking feature discovered is a poorly collimated high-velocity ionized jet, embedded within a broader, wide-angle molecular outflow likely driven by a disk wind. The coexistence of these components supports a stratified outflow structure and suggests that L1527 exhibits jet-launching characteristics atypical of its early evolutionary stage.