We present a deep, high-resolution CO(4-3) IRAM-NOEMA observation of a main sequence, barred, spiral galaxy at z≈1.12, with an on-source integration time of ≈37 hours and a beam FWHM of ≈0.^''3. We use the molecular gas data in conjunction with the available deep multi-band JWST and HST imaging, covering restframe UV to near-IR wavelengths, to quantitatively study the gas flows in the disk plane of this cosmic noon barred spiral. We find that this target is a massive (log(M_baryons/M_⊙)≈10.96), baryon-dominated (f_dm(<R_e)=u^2_circ,dm(R_e)/u^2_circ(R_e)∼4%), gas-rich (f_gas=M_gas/(M_⋆+M_gas)≈40%) disk, hosting a long (a_bar≈4.2 kpc), strong (Q_b≈0.37), and fast (ℛ=R_CR/a_bar≈1.05) bar, which rotates at an angular speed of Ω_pattern≈ 50 km/s/kpc. This bar is driving molecular gas inflows with a net inflow rate of Ṁ∼30 M_⊙/yr, based on three estimates, which is of the same order as the galaxy-integrated star formation rate (SFR≈36 M_⊙/yr). We additionally identify evidence of a well-defined dust lane shock at the northwestern side of the bar, with gas motions parallel to this feature, in agreement with expectations for an established bar-driven flow. Our study highlights the possible role of bars as key drivers of galaxy evolution for a significant fraction of cosmic noon galaxies, offering a detailed picture of well-defined, bar-driven inflows in a high-z barred spiral.

We present a spatially resolved study of cold molecular gas and dust in ten main-sequence galaxies at z=1.1-1.6, using observations of CO(4-3), CO(3-2), [CI](1-0), and dust continuum from the NOEMA3D survey. We find widespread spatially extended molecular gas and dust, with sizes comparable to those of the stellar disk, in contrast to those of centrally dominated starburst galaxies at similar redshifts. Among the targeted molecular gas tracers, the CO line (J=3-2 or J=4-3) remains the most effective for mapping molecular gas distribution and kinematics. The spatially resolved correlations between different molecular gas tracers exhibit about twice the scatter as their galactic-integrated correlations, indicating that interstellar medium (ISM) conditions already deviate from global averages on scales of 3-6 kpc. This likely reflects the clumpy or inhomogeneous ISM in cosmic noon star-forming galaxies. Within our sample, both the molecular gas fraction and its depletion time are nearly constant across the galactic disks out to 2xRe, supporting a global linear Kennicutt-Schmidt law. These galaxies also have relatively small bulges, with bulge-to-total ratios between 6-24

Cosmic noon represents the prime epoch where today’s massive galaxies assembled most of their stellar masses, and it is an ideal period for observations with both the space-based James Webb Telescope (JWST) and ground-based near-IR integral-field unit (IFU) spectrographs. This work analyzes JWST NIRSpec Micro Shutter Array (MSA) and NIRCam Wide Field Slitless Spectroscopy (WFSS) observations of K20-ID7, a large spiral, star-forming (SF) galaxy at z = 2.224 with evidence of radial gas inflows. Leveraging ground-based IFU ERIS observations, we conducted a comprehensive and resolved study of the interstellar medium and stellar properties of this galaxy, covering the rest-frame optical to near-IR. Our analysis – using several emission-line diagnostics, resolved spectral energy distribution (SED) fitting of high-resolution imaging, and Pa β line detection in NIRCam WFSS data – reveals massive SF clumps ( M ★ ≃ (0.67 − 3.5) × 10 9 M ⊙ ) with star formation rates (SFRs) of 3 − 24 M ⊙ yr −1 , low dust attenuation ( A V ≃ 0.4), electron densities ( n e ≲ 300 cm −3 ), and ionization parameter (log( U ) ≃ −3.0). The central bulge is modestly massive ( M ★ = (7 ± 3)×10 9 M ⊙ ), heavily obscured ( A V = 6.43 ± 0.55), and likely formed most of its stellar mass in the past (SFR = 82 ± 42 M ⊙ yr −1 over the last ∼100 Myr). Yet, it continues to form stars at a lower rate (SFR = 12 ± 8 M ⊙ yr −1 over the last ∼10 Myr). We infer a relatively low sulfur abundance of log(S/O) ≃ −1.9, which may have implications for sulfur production via type I supernova explosions. Moreover, all distinct galaxy regions feature a metallicity of 12+log(O/H) ≈ 8.54, likely due – along with the enhanced N/O abundance (i.e., log(N/O) ≃ −1.0) – to dilution effects from radial inflows of metal-poor gas. Lastly, we find tentative evidence of a negative gradient in stellar age, suggesting possible inside-out growth for K20-ID7.

We present observational evidence of three massive, accreting black holes in the z = 5.0167 galaxy J0148-4214 from JWST/NIRSpec-IFU spectroscopy. The black holes are revealed through broad H α emission (FWHM = 430–2920 km/s) without a forbidden-line counterpart in the bright [O III ] doublet. Channel maps of the asymmetric central H α profile isolate two spatially distinct broad-line regions (BLRs), separated by 190 ± 40 pc, while a third BLR is found in the galaxy outskirts with a projected separation of 1.7 kpc. We discuss whether this emission could be due to supernovae, shocks, winds, or massive stars, but find the BLR origin most likely. Using single-epoch virial relations, we estimated black hole masses of log( M • / M ⊙ ) = 7.9 ± 0.4 (primary), 5.8 ± 0.5 (secondary), and 6.3 ± 0.5 (third off-nuclear). We argue that the two central black holes will likely rapidly merge, with a simple dynamical friction time estimate of the order of ≲700 Myr. Assuming that the third off-nuclear black hole is also in the process of sinking towards the centre, it will likely lead to a second merger, and we investigated the detection probability of such mergers with LISA. Alternatively, the third black hole may be the result of a previous central three-body interaction or a gravitational recoil, where our observations would provide evidence that such black holes may retain their accretion discs and BLRs even in the aftermath of such extreme dynamical interactions. The possible discovery of a black hole triplet at high redshifts, together with other recent results on distant black hole pairs, indicates that multiple massive black hole systems were likely common in the early Universe. Our results highlight the importance of IFU observations for the detection of massive black hole multiplets in distant galaxies, the progenitors of massive black hole mergers that may be detected with next-generation gravitational wave observatories.

Ultrafast outflows (UFOs) are thought to be a driving mechanism of large-scale winds driven by active galactic nuclei (AGN), which cause significant galactic feedback through quenching star formation and regulating supermassive black hole growth. We present James Webb Space Telescope (JWST) Mid-Infrared Instrument Medium-Resolution Spectrometer observations of two nearby ultraluminous infrared galaxies, F11119+3257 and F05189-2524, with nuclear X-ray detected UFOs and kiloparsec-scale outflow. These galaxies show remarkably similar mid-infrared continuum and emission line features, notably including a high-velocity v _90 ∼ 4000 km s ^−1 outflow detected in highly ionized neon emission lines, e.g., [Ne VI ]. In F05189-2524, we see a slightly slower biconical outflow extending up to ∼2 kpc in the same neon emission lines. Both sources show evidence of AGN-driven radiative feedback through a deficit of rotational molecular hydrogen lines in the nuclear region, <1 kpc from the central quasar, but no clear evidence of any molecular gas entrained in the quasar-driven outflow. Energetic analysis shows that the warm ionized gas in both of these sources contributes minimally (∼0.1%–5%) to the momentum outflow rate of these sources and leaves the conclusions of previous literature unchanged: the energetics of these sources are broadly consistent with a momentum-conserving outflow.

We present NOEMA3D, a unique high-resolution study of purely molecular gas kinematics at z ∼ 1.1 to 1.6, providing a dedicated view of cold gas dynamics at the late stages of the peak epoch of cosmic star formation. Using deep (gtrsim 20 hr on source per target) IRAM-NOEMA CO observations of 10 massive (10.45 < log(M^*/M_⊙) < 11.43) ) main-sequence galaxies, complemented by high-resolution JWST imaging, we resolve the molecular gas kinematics and morphology on kiloparsec scales. We find that all galaxies exhibit ordered rotation with moderate intrinsic turbulence (median σ_0 ∼ 32 ± 10 km/s, median V_c/σ_0 ∼ 8.6 ± 2.9), consistent with dynamically turbulent disks at late cosmic noon. After modeling the axisymmetric rotation with the forward-modeling code DysmalPy, we reveal spatially coherent velocity residuals in all but one more inclined system. The inferred in-plane non circular motions reach amplitudes of ∼ 50-100 km/s, significantly larger than typically observed in local disk galaxies. Interpreting these non-circular motions as radial flows we find that the velocity residuals spatially coincide with non-axisymmetric structures – spiral arms and bars – demonstrating a direct link between galaxy morphology and gas transport at z ∼ 1-2. In spiral galaxies, the residual velocity patterns are typically dominated by inflows, while barred systems display an apparent inflow-outflow pattern, characteristic of in-plane bar-driven gas motions. We further find that the inferred molecular gas inflow rates are substantial, with a typical net inflow rate of the order of the star formation rate ( Ṁ∼ -50 M_⊙/yr). This implies that spiral arms and bars at cosmic noon are highly efficient at funneling cold gas toward galaxy centers, perhaps driving the buildup of bulges and feeding central star forming regions and supermassive black holes.

MICADO is the designated ELT first light instrument, a near-infrared imager working at the diffraction limit of the telescope thanks to a SCAO and an MCAO mode. Since summer 2024, MICADO is in its AIT phase and all MICADO partners are currently integrating their subsystems. The MICADO SCAO module will follow three successive AIT phases in France: the beta flat configuration, the flat configuration and the final configuration. In this contribution I will first present the progress made in the AIT of the beta flat configuration and its closed loop results. I will then present the performed and on-going tasks for the flat and final configurations (manufacturing, delivery and integration of several SCAO subsystems and pieces of software) and the results obtained so far in the flat configuration. I will then conclude with the expected following steps of the SCAO module AIT in Garching.

We present Northern Extended Millimeter Array observations of the CO (2-1) molecular gas kinematics in the nearby Compton-thick Seyfert 2 galaxy NGC 3079, with an angular resolution of 0 .'' 5 (similar to 40 pc). To interpret the observed CO (2-1) kinematics, we model the rotating disk using two software tools, 3D-Barolo and DysmalPy, to generate mock 3D data cubes. Both models indicate, in addition to the rotating disk, the presence of a spatially unresolved nuclear component characterized by high velocity dispersion. Analysis of the visibility data reveals that the blueshifted, high-velocity component is spatially offset from the continuum peak by 0 .'' 17 (similar to 14 pc) and exhibits line-of-sight velocities of v - vsys = -350 to -450 km s-1, which we interpret as a nuclear molecular outflow. We calculate a molecular gas mass outflow rate of 8.82 M circle dot yr-1, with a kinetic power ( Eout ) of 3.8 & times;1041 erg s-1 and a momentum rate ( pout ) of 2.05 & times; 1034 Dyne. The momentum rate exceeds the AGN radiation momentum rate by a factor of similar to 15, suggesting an energy-driven outflow. Furthermore, we argue that the derived kinetic power of the nuclear molecular outflow favors a jet-powered scenario that explains the slowdown and brightening of the parsec-scale radio source observed with the Very Long Baseline Array.

We targeted with deep NOEMA observations the [CII]158μm emission of three JWST-discovered AGN at z>6. Two of them have the typical features of Little Red Dots (LRDs), while the third one is a blue, extended, Type I AGN. We do not significantly detect [CII] emission or dust continuum in any of the targets, even after stacking. The resulting [CII] luminosity upper limits, log (L_[CII]/L_⊙)<7.77-8.1, lie ∼2σ below the values expected from the [CII]-SFR relation, and we explore different scenarios to explain the lack of [CII]. We obtained upper limits on the gas masses of log (M_gas/M_⊙)<9.26-9.59 corresponding to log( M_dust/M_⊙)<5.68-6.55 assuming a metallicity dependent dust to gas ratio. Using the continuum non-detections (rms ∼ 16-25 μJy) together with JWST/MIRI constraints, we performed a revised SED-fitting decomposition, resulting in stellar masses up to ∼ 2 dex lower than previously reported, and implying 0.03≲ M_BH/M_*≲0.7. For the two LRDs, the SED is well reproduced by stellar emission in the rest-frame UV, while the rising rest-frame optical slope, flattening toward the near-infrared, is consistent with emission from a Type I AGN partially obscured along the polar direction with E(B-V)_ polar≃ 1, in agreement with attenuation derived from the broad lines Balmer decrement. This decomposition demonstrates that a relatively standard AGN configuration can reproduce the SEDs of the two LRDs, without invoking more exotic scenarios. Finally, we investigate the positions of the three sources in the IRX-β_UV plane, finding that they lie in a parameter space where galaxies are typically characterized by patchy dust distributions. Our analysis highlights the importance of millimeter constraints to characterize the different physical properties of high-z AGN.

Detections of protoplanets are rare and protoplanetary disk features mischaracterized as planets are common. PDS 70 is one of only two stars known to host multiple confirmed protoplanets, PDS 70 b and c, and repeat detections of a third point-like source in the system suggest the presence of third inner planet. However, previous observations of this third source are insufficient to distinguish whether it is a planet or a concentrated dust clump in Keplerian motion. Our observations with VLTI/GRAVITY+ did not re-detect this point-like source, suggesting that it is, in fact, a dust clump and not a planet. These observations demonstrate how the angular resolving power of VLTI/GRAVITY+ can be used to distinguish between protoplanets and protoplanetary disk features.

We present new James Webb Space Telescope Mid-Infrared Instrument Medium-Resolution Spectrometer observations of the nearby ultraluminous infrared galaxy F10565+2448. These integral field spectroscopic data reveal an unresolved nuclear outflow in both warm-ionized and warm-molecular gas phases as well as a resolved blueshifted kiloparsec-scale warm-molecular outflow. The unresolved warm-ionized outflow has a mean projected velocity up to -520 km s(-1), while the unresolved warm-molecular outflow is slower at -150 km s(-1). For the resolved warm-molecular outflow, the projected mean velocity (-280 < v(50) < -110 km s(-1)) is only slightly faster than the velocity of the disk (-70 < v(50) < 120 km s(-1)) and, as such, likely does not exceed the estimated escape velocity of greater than or similar to 300 km s(-1). The warm-molecular outflow is slightly hotter (507 +/- 25 K) than the disk (329 +/- 5 K), and displays areas of higher temperature and lower column density that may indicate a shock front, which we explore using the [Fe II] 5.34 mu m/Pf alpha shock diagnostic. Analysis of the polycyclic aromatic hydrocarbon features reveals trends of ionization and grain size that first decrease with radius up to 1 kpc before increasing up to 3 kpc. These results bolster the picture of F10565+2448 being an active galactic nucleus (AGN)-starburst composite where both star formation and AGN-powered phenomena are required to explain the outflow energetics.

We report the direct imaging discovery of a third exoplanet in the β Pictoris system. We detect β Pictoris d in non-coronagraphic observations obtained with VLT/ERIS as well as multi-epoch archival datasets from JWST/NIRCam and VLT/SPHERE. Astrometric measurements over an 11-year baseline demonstrate that it is consistent with a gravitationally-bound source with orbital motion. Joint multi-planet orbit fits of all three planets in the system yield a semi-major axis of 26.0^+2.2_-6.1 au and inclination 89.0^+0.7_-0.6 deg for planet d. β Pictoris d has a larger orbital semi-major axis than the other known planets in the system, but is coplanar with the inner two planets, and its orbit is consistent with sculpting the inner edge of the debris disk. β Pictoris d has a contrast of ΔL^'=12.11±0.15 mag, with colors and luminosity that closely match those of 51 Eri b, another exoplanet in the β Pictoris moving group. Its VLT/ERIS and JWST/NIRCam colors are distinct from those of free-floating planetary-mass objects of a similar age and temperature. Its red F410M-F444W color indicates strong CO_2 absorption in its atmosphere and suggests significant enhancement in metals compared to free-floating objects. From the ATMO hot-start evolutionary models, we estimate an effective temperature of 600^+45_-60 K and mass of 2.4±0.6 M_ Jup, which also closely matches similar estimates for 51 Eri b. β Pictoris d is among the lowest-mass exoplanets imaged from the ground. This discovery highlights the deep sensitivity achievable with ground-based imaging in the mid-infrared and the discovery potential of future high-contrast observations with the Extremely Large Telescope.

The geometric distances of active galactic nuclei (AGNs) are challenging to measure because of their exceptionally compact structure, yet vast cosmic distances. A combination of spectroastrometry and reverberation mapping (SARM) of broad-line regions (BLRs) constitutes a novel means to probe the geometric distance of AGNs, which has recently become practically feasible owing to successful interferometric observations with the Very Large Telescope Interferometer/GRAVITY. Here, we perform SARM analysis of four nearby quasars: Mrk 509, PDS 456, 3C 273, and NGC 3783. Results for the former two are reported for the first time, and the latter two are revisited using our improved BLR dynamical modeling that includes the radial-dependent responsivity of BLRs. This allows us to self-consistently account for the emissivity weighting of the BLR in spectroastrometry and responsivity weighting in reverberation mapping. We obtain angular-diameter distances of the four quasars, from which we derive a Hubble constant of H 0 = 6 9 − 10 + 12 km s − 1 Mpc − 1 . Although this constitutes a large uncertainty for a measurement of H 0 , it is anticipated that the precision will improve to a competitive level once a greater number of AGNs are accessible following the upgrade of GRAVITY in the near future. From SARM analysis, the black hole masses of the four quasars are also measured with the statistical uncertainty ranging from 0.06 to 0.23 dex, consistent with the correlations between black hole masses and properties of the host bulges.

Context. The Enhanced Resolution Imager and Spectrograph (ERIS) is the new adaptive optics (AO) assisted infrared instrument at the Very Large Telescope (VLT). Its refurbished integral field spectrograph (IFS) SPIFFIER leverages a new AO module, enabling high-contrast imaging applications and giving access to the orbital and atmospheric characterisation of super-Jovian exoplanets. Aims. We tested the detection limits of ERIS, and demonstrate its scientific potential by exploring the atmospheric composition of the young super-Jovian AF Lep b. Additionally, we improved its orbital solution by measuring its radial velocity relative to its host star. Methods. We present new spectroscopic observations of AF Lep b in K-band at R similar to 11 000 obtained with ERIS/SPIFFIER at the VLT. We reduced the data using the standard pipeline together with a custom wavelength calibration routine, and removed the stellar point spread function using principal component analysis along the spectral axis. We computed molecular maps by cross-correlating the residuals with molecular spectral templates and measured the radial velocity of the planet relative to the star. Furthermore, we computed contrast grids for molecular mapping by injecting fake planets. Results. We detect a strong signal from H2O and CO but not from CH4 or CO2. This result corroborates the hypothesis of chemical disequilibrium in the atmosphere of AF Lep b. Our measurement of the RV of the planet yields Delta v(R, P star) = 7.8 +/- 1.7 km s(-1). This enables us to disentangle the degeneracy of the orbital solution; specifically, the correct longitude of the ascending node is Omega = 248(-0.7)(+0.4) deg and the argument of periapsis is omega = 109(-21)(+13) deg. Our detection limits reach a contrast of Delta K = 11.5 mag at 0 ''.12 for the spectral templates of H2O and CO, significantly extending the parameter space available to moderately high spectral resolution towards small angular separation. Conclusions. Our results demonstrate the competitiveness of the new ERIS/SPIFFIER instrument for the orbital and atmospheric characterisation of exoplanets at high contrast and small angular separation.

Observations have suggested that galactic outflows contain substantial amounts of dense and clumpy molecular gas, creating favourable conditions for igniting star formation. Indeed, theoretical models and hydrodynamical simulations have suggested that stars could form within galactic outflows, representing a new mode of star-formation that differs significantly from the typical star formation in star forming discs. In this paper, we examine 12 local galaxies with powerful Active Galactic Nuclei and high star-formation rate using spectroscopic data from the X-shooter spectrograph at the Very Large Telescope. We investigate the excitation mechanism and physical properties of these outflows via spatially resolved diagnostic diagrams (along with tests to rule out contribution by shocks and external photoionisation). Out of the seven galaxies with clearly detected outflows, we find robust evidence for star formation within the outflow of one galaxy (IRAS 20551-4250), with two additional galaxies showing tentative signs (IRAS 13120-5453 and F13229-2934). Therefore, our findings support previous results that star formation inside outflows can be a relatively common phenomenon among these active galaxies and may have played an important role in the formation and evolution of the spheroidal component of galaxies.