The ALMA interferometer has been at the forefront of astronomical discoveries. To keep this status, it is essential to start thinking of its future. ESO has launched an Expanding Horizons call due in 1 June 2027 to identify the next major ground-based astronomy facility. Hence reflection on ALMA2040 facility are underway and science pitches from all areas of astronomy have been collected. To be able to perform this science an increase of the sensitivity by a factor of ten is desirable, the full wavelengths range is requested. A factor of three increase in the resolution is sufficient for most projects, while good image quality is necessary. We have looked into different solutions with 200 to 300 identical or different size antennas, different fixed of movable baseline configurations, receivers enabling multi-frequency operations or wider RF or IF bandwidth. In the talk I will present the science topics we have identified so far, the technical requirements deduced and possible technical solutions. Coordination with the Asian and the North American and Chilean initiatives is essential. We would like to invite everybody to submit scientific and technical White Papers by September 2026 and to participate in shaping ALMA2040.

In this talk, I will talk the followings:

i) reviewing key specifications of legacy/WSU ALMA (e.g., sensitivity, image dynamic range, spectral dynamic range, polarization, etc) and science cases that benefit from or are limited by these specifications,

ii) technical bottleneck for these specifications, and

iii) personal view of ambitious specifications for ALMA2040.

I hope this will give an insight for the "top-level" requirement of ALMA2040 and stimulate interactions between science side and technical side.

The increasing volume, complexity, and scientific ambition of modern astronomical facilities require a paradigm shift in data analysis, particularly in preparation for the ALMA2040 era, where data processing and inference will become integral components of scientific capability. In this talk, I will discuss key challenges at the intersection of artificial intelligence, astrostatistics, and big data, arising from the ill-posed inverse problems that underpin astronomical imaging and inference, drawing on results developed within the ESO internal ALMA development study BRAIN.

I will highlight approaches based on Information Field Theory (IFT) and deep learning, including RESOLVE and DeepFocus, applied to ALMA interferometric data, demonstrating significant improvements in image fidelity, sensitivity to faint structures, completeness of recovered emission, and computational efficiency. These results illustrate the complementarity of probabilistic inference methods and data-driven approaches in addressing different aspects of the reconstruction problem. Recent joint analyses of ALMA and JWST data further demonstrate the ability of these techniques to access astrophysical information beyond the reach of conventional imaging methods.

In addition, building on the BRAIN study, I will briefly outline the upcoming MADIV initiative, which extends deep-learning approaches through more modern architectures such as Transformers. I will also present further applications of Information Field Theory enabled by support from the ESO Science Department and discuss future perspectives. These developments demonstrate how advanced methods applied to ALMA data can contribute to next-generation analysis pipelines. More broadly, I will discuss how AI- and statistics-driven methodologies will be essential to maximizing the scientific return of ALMA upgrades and future observatories in an increasingly data-intensive landscape.

Very long baseline radio interferometry (VLBI) with ground-based observatories is limited by the size of Earth, the geographic distribution of antennas, and the transparency of the atmosphere. We present the tentative design for a space-to-space VLBI program composed of two missions: Mimosa, a pathfinder, and Capella, a science-grade VLBI observatory. Capella comprises four small (500 kg) satellites in two orthogonal polar low Earth orbit planes. With single-band heterodyne receivers operating at frequencies around 690 GHz, the interferometer is able to achieve angular resolutions of approximately 7 µas. Capella has explicitly (with an observing frequency corresponding to ALMA Band 9) been designed to be complementary to ALMA and to enable common observations. A ALMA + Capella collaboration will be able to address a range of science cases, including: the shadows of supermassive black holes; the acceleration and collimation zones of plasma jets emitted from the vicinity of supermassive black holes; the chemical composition of accretion flows into active galactic nuclei through observations of molecular absorption lines; mapping supermassive binary black holes; the magnetic activity of stars; and nova eruptions of symbiotic binary stars – and, like any substantially new observing approach, has the potential for unexpected discoveries.

Here we propose two ideas for the ALMA2040; (1) THz observations with the ACA, and (2) longer baselines with ALMA together with a large single-dish telescope (i.e., AtLAST/LST). About (1), the ALMA site is possible to observe at THz frequency (three atmospheric windows at 1000 - 1500 GHz or 200 - 300 micron), and this frequency range is very important for the dust studies, since the cold dust temperature peaks around this frequency. On the other hand, it is difficult to observe, and quite challenging to install THz receivers on all the ALMA antennas from the beginning. ACA can be the good test-bed to install the THz receivers and study the cold dust as a precursor. About (2), now the ALMA is producing many long baseline scientific data, which are changing our understandings, such as planet formation and galaxy formation. ALMA observations with longer baseline will provide more detail information on these topics, but sensitivity can be the issue, since such detail structures have very low intensity. Combine with a large single-dish telescope, such as AtLAST/LST, and ALMA longer baseline antennas at >20 km, it is possible to obtain high sensitivity long baseline images that cannot be obtained with the current ALMA. We will present these two ideas in this presentation.

The ALMA 2040 vision highlights the need for an order-of-magnitude improvement in spectral line sensitivity, motivating consideration of both increased collecting area and expanded array functionality. In this context, a large-aperture (∼50 m) submillimeter single-dish telescope can play several complementary roles when combined with ALMA in a heterogeneous configuration.

Such a facility would serve as (1) a wide-field surveyor enabling efficient mapping with wide field of view and large instantaneous bandwidth, (2) a zero- and short-spacing sampler to recover extended emission and improve imaging fidelity, and (3) a high-sensitivity element contributing to interferometric and VLBI observations. From a technical standpoint, baselines including a large dish substantially enhance the fringe sensitivity, leading to not only improved imaging sensitivity but also accurate complex gain and bandpass calibration.

This concept builds on the experience of the Nobeyama "Rainbow" interferometer, where a heterogeneous array combining the 45 m telescope and the millimeter array was successfully used for studies on proto-planetary disks and high-redshift galaxies. Extending such an approach to ALMA may provide a useful pathway toward improving sensitivity and expanding its scientific capabilities.

Photonic-electronic convergence devices will be a key foundation for computing and communication infrastructures in the 2040s. As electronic scaling faces limits in energy efficiency, bandwidth, latency, and thermal management, deeper integration of photonics and electronics will become essential. This talk presents a long-term vision for such devices, covering optical interconnects, heterogeneous integration, advanced packaging, and device architectures for AI, sensing, and data-centric systems. It also discusses how co-design across materials, circuits, modules, and systems can enable ultra-low-power processing and high-capacity communication. Looking toward the 2040s, photonic-electronic convergence will drive new computing paradigms and sustainable digital infrastructure.

Millimeter and submillimeter interferometers such as ALMA rely on coherent frequency reference signals distributed across antenna arrays with extremely high phase stability. Toward ALMA2040 and beyond, demands on reference signal quality will intensify as receiver bandwidths and array scales grow. This talk presents a photonic approach to reference signal generation based on high-precision optical modulation.

The key technology is a Mach-Zehnder modulator (MZM) with active trimming, which compensates structural imbalance caused by fabrication imperfections. By controlling the extinction ratio to exceed 50 dB — far beyond the 20 dB typical of conventional devices — a spectrally pure optical two-tone signal can be generated. When detected by a high-speed photodetector, this yields a millimeter-wave reference tone whose spectral purity is decoupled from the frequency response of the modulator itself, enabling stable broadband LO signal synthesis over fiber. The same platform supports optical single-sideband modulation for frequency-agile reference generation.

This precise modulation technique also underpins IEC-standardized measurement methods for qualifying optical modulators and photodetectors — the core components of any photonic LO distribution network — ensuring reliable characterization across international supply chains. We discuss how these capabilities address ALMA2040-class system requirements and outline prospects for collaboration within the East Asian radio astronomy community.

Since there is currently no agreed specification for the ALMA 2040 upgrade, we propose target parameters: scaling the array to 256 antennas (4X compared with current 66), expanding the total science bandwidth to 256 GHz (64 GHz per polarization per sideband, representing 4X WSU), and achieving 10 kHz final spectral resolution. To address this, we present a hybrid FPGA-GPU correlator strawman design. In this design, digitization and coarse channelization are performed using FPGAs at each antenna, while fine channelization and cross-correlation are executed on GPUs.

Under this architecture, each antenna performs real digitization across four streams using future high-speed Analog-to-Digital Converters (ADCs) operating at 128 GS/s. Coarse-channelized data (8-bit real + 8-bit imaginary) is streamed to the central correlator facility via high-speed optical links. The aggregate data rate of this 16-bit complex data from the 256-antenna array exceeds 1.05 Pbps (131 TB/s)—corresponding to 4.096 Tbps (512 GB/s) per antenna—leveraging the roadmap of 1.6/3.2 Tbps Ethernet and scaling to 6.4/12.8 Tbps beyond 2040. At the central facility, the massive corner-turning bottleneck is resolved using NVLink technology, which is projected to reach dozens of TB/s per GPU by 2040 using co-packaged optics (CPO) (compared with 3.6 TB/s per GPU for NVLink 6 in the 2026 Rubin era). Fine channelization (FFTs) and cross-correlations are executed on a compact, highly energy-efficient GPU cluster. The cross-correlation across 32,640 baselines requires a total of 50 PetaFLOPS, which translates to a modest 50 TeraFLOPS per GPU when distributed across 1024 GPUs. This processing requirement is highly feasible with modern and future GPU architectures, demonstrating that the computational and data transport requirements for ALMA 2040 can be efficiently met using emerging commercially available hardware architectures.

Millimeter and Sub-millimeter radio astronomy heterodyne receivers are dominated by the superconductor-based devices for decades. Among the existing ALMA bands, only the lowest ones, i.e. Band 1 and 2, are so-called HEMT-based receivers where cryogenic semiconductor amplifiers are employed as the first device in the receiver front-end. Thanks to the increasing demands in quantum computing and other applications, the interests in cryogenic semiconductor technologies grow rapidly in the commercial communities. Will the radio astronomy community benefit from these advanced semiconductor technologies? The talk will summarize the development in the past years and try to provide a projection on the cryogenic semiconductor noise performance for the next decades.

600 – 720 and 780 – 950 GHz are the highest-frequency atmospheric window for Llano de Chajnantor site where the ALMA AOS located. With the strong influence by the water vapor of the atmosphere, these two bands are with very limited observable period during very dry and cold weather condition. The idea of band-combining of the two bands with waveguide diplexer is to promote the efficiency of observation on these two frequency bands. Based on the ultra-wideband waveguide diplexer developed, it is possible to combine the waveguide bands up to 1.7. for 600 – 950 GHz, using WR-1.2 waveguide could provide TE10 single mode propagation from 600 -960 GHz, for which band combining of 600 – 720 GHz and 780 – 950 GHz is possible. With the configuration of feedhorn – diplexer, lower band (600 – 720 GHz) and higher band (780 – 950 GHz) could be separated by sharing the same feed.

The main technical challenging to realize this receiver approach is the low-loss waveguide components fabrication for < 600 GHz. Dry-etching process on silicon with gold-plating surface finish could be the initial solution for diplexer, waveguide OMT, quadrature hybrid. A further study of superconducting thin-film coating on metallic waveguide components is required.

My team has been studying structures and magnetic fields in star-forming regions using ALMA. In this talk, I will first introduce recent results obtained by my team members on young stellar objects. I will then discuss the ALMA capabilities that we would like to see developed to advance studies of structures and magnetic fields in star formation.

To understand the underlying processes of star formation, a multi-wavelength and multi-scale observational study of IRAS 11332-6258 hosting 6.7 GHz methanol maser is carried out. The IRAS source is associated with the bright-rimmed cloud BRC 68 and notably lacks detectable radio continuum peak emission. The Spitzer 4.5 micron image reveals an Extended Green Object toward IRAS 11332-6258, suggesting the presence of a young massive protostar driving energetic outflow activity. To investigate the dynamical processes governing mass accretion and fragmentation, the ALMA-QUARKS continuum and line data are employed. The 1.3 mm continuum map reveals some compact continuum sources, nearly 50% of which satisfy the condition for massive star formation. Their spatial distribution indicates two distinct groups of sources, referred to as the northern group (NG) and southern group (SG). Among the detected continuum sources, one particularly intriguing object in the NG appears to host a forming massive protostar that is driving a powerful bipolar molecular outflow while also exhibiting signatures of channeled gas inflow. I will present results derived from a variety of molecular line tracers observed with ALMA and discuss their implications for fragmentation, mass accretion, outflow activity, and the formation of massive stars in IRAS 11332-6258.

Water, a fundamental ingredient for life, plays a key role in the earliest stages of star formation. In both gaseous and solid forms, H₂O regulates thermal balance, drives chemical evolution, and traces dynamical processes in protostellar environments.

We analyze JWST/MIRI integral-field spectroscopy (5–28 μm) of gas-phase H₂O in five protostars from the JWST Cycle 1 Investigating Protostellar Accretion (IPA) program, spanning masses of 0.1–12 M☉ and luminosities of 0.1–10,000 L☉. In the most luminous sources, HOPS 370 and IRAS 20126, H₂O is detected in the fundamental rovibrational (010–000) band at 5–8 μm. These sources exhibit spatially extended emission and blueshifted absorption associated with bipolar outflows, features largely absent in lower-luminosity protostars. This contrast suggests that radiative excitation dominates water emission in high-luminosity systems.

We extend the analysis to thirteen young protostars from the JWST Cycle 3 High Angular Resolution Observations of Stellar Emergence in Filamentary Environments (HEFE) program. Combining both samples reveals a clear increase in H₂O feature strength with protostellar luminosity, highlighting radiative pumping as a key excitation mechanism. Complementary ALMA observations of H₂¹⁸O transitions will provide constraints on the cold-water reservoir, enabling a multi-temperature view of the protostellar water budget.

Jets and winds are ubiquitous in young stars, particularly powerful in the youngest protostars. Recent high-resolution JWST observations have revealed a nested flow structure in many protostars: fast, highly collimated ionic jets (opening angle ~ 5-10°, velocities ≥ 150 km/s) surrounded by a slower (10–20 km/s), wide-angled (≥ 20-30°) molecular wind traced by H2. A few protostars instead show fast (>40 km/s), highly collimated (<20°) molecular jets, whose origin remains unclear and is actively debated.

We investigate why these sources deviate from the rest of the sample using JWST NIRSpec/IFU and MIRI/MRS observations of 15 Class 0 protostars in the Orion molecular cloud obtained as part of two JWST GO programs, High Angular Resolution observations of Stellar Emergence in Filamentary Environments (HEFE) and Investigating Protostellar Accretion(IPA). Three protostar, HOPS-60, HOPS-88 and HOPS-370, in our sample stand out as they exhibit fast, collimated H2 jets. We characterize their morphology by measuring opening angle and maximum launch radius using hysteresis thresholding method. We compare their protostellar, disk, and envelope properties with the rest of the sample and analyze outflow kinematics and energetics using rotational and position velocity diagrams to determine whether these molecular-jet sources are intrinsically distinct. We present our results and discuss their implications for jet launching and the transition to molecular jet phases in young protostars.

ALMA has revolutionized our understanding of molecular gas in nearby galaxies. By enabling observations of multiple molecular transitions, it has become possible to characterize the physical conditions of star-forming molecular gas in unprecedented detail. Recent studies have examined dense gas, shocked gas, and molecular environments affected by high-energy radiation and particles. In this talk, I will review major scientific advances achieved with ALMA, discuss the new opportunities offered by WSU, and consider the scientific opportunities that could be realized through the ALMA 2040 development program.

Molecular hydrogen is the dominant baryonic component of galaxies, yet it remains essentially unconstrained in the first billion years of cosmic history. At very high redshift, conventional tracers such as CO, dust continuum, and even [C II] become increasingly uncertain because of low metallicity and rapidly evolving interstellar-medium conditions.

A remarkable opportunity arises from the H2 0-0 S(0) rotational transition at 28.2 um. This line is redshifted into ALMA Bands 10, 9, and 8 over the redshift range z~10-27, making ALMA the only existing or foreseeable facility capable of directly probing warm (100-300 K) molecular hydrogen that traces the bulk of the molecular gas mass throughout the Cosmic Dawn era. No other planned observatory offers comparable access to this parameter space.

In this talk, I will use the z = 14.18 galaxy JADES-GS-z14-0, among the most distant galaxies with a detected [O III] 88 um emission line, as a case study to evaluate the current capabilities and limitations of ALMA Band-9 observations of warm H2. I will argue that increasing the total collecting area, potentially through the addition of one or more large-aperture single dishes, would dramatically expand ALMA’s unique discovery space by improving both line sensitivity and high-frequency phase calibration. With such capabilities, ALMA2040 could transform direct observations of warm H2 from exploratory experiments into a major new probe of galaxy formation during Cosmic Dawn.

Since the start of operations, ALMA has revolutionized our view of the high-redshift Universe. Its unprecedented sensitivity and angular resolution have revealed massive molecular gas reservoirs at the peak epoch of cosmic star formation, mapped dust-obscured star formation in distant galaxies, and resolved the kinematics of systems far into the Epoch of Reionization. These observations have transformed our understanding of how galaxies assemble, form stars, and build their structures across cosmic time. The forthcoming WSU will further expand ALMA’s discovery space through substantially increased bandwidth and observing efficiency. For studies of high-redshift galaxies, the WSU will enable more efficient redshift determinations, simultaneous multi-line diagnostics of the interstellar medium, and large statistical surveys that probe fainter and more representative galaxy populations in the early Universe. Looking ahead, the 2030s and 2040s will see powerful synergies between ALMA and next-generation facilities. In particular, ngVLA will provide sensitive measurements of low-J molecular gas tracers, while PRIMA will probe dust and far-infrared cooling lines, together offering a comprehensive view of galaxy evolution. In this talk, I will discuss how these developments serve as key science drivers for ALMA2040 and beyond to address the next frontier of high-redshift galaxy science.

Accretion flow around black holes (BH) or neutron stars (NS) emit high energy radiations with varying spectral and temporal properties. Observed temporal variations (Mauche 2002) point to the existence of a mechanism, dictated by the flow dynamics and not by the stellar surface or magnetic fields, that is common in both types of compact objects. For accretion, such a generalized flow configuration has been proposed (Bhattacharjee 2018; Bhattacharjee and Chakrabarti 2019), where an advective sub-Keplerian disk, along with the standard disk, could explain various spectral and temporal variabilities, especially for wind-dominated sources such as Cir X-1. Presence of ultra-relativistic jets around BH and NS, strongly favored a common ejection mechanism (Fender et al., 2004), as well, yet remains less explored.

We perform Smoothed Particle Hydrodynamics simulations of accretion-ejection around NS, in presence of cooling and viscosity. We find shock mediated jets and outflows, dynamically connecting the accretion and ejection branches. We compute synthetic observables, and compare with recent radio observations of Cir X-1 (Cowie et al. 2025). Furthermore, the results provide possible explanations for multi-wavelength observational features such as complex radio/X-Ray luminosity correlations across soft/hard states and jet quenching (e.g. 4U 1820−30, Ser X-1, GX 5-1).

We would like to present the first [NIII] 57 um observation at high redshift. The target A1689-zD1 is a gravitationally-lensed sub-L* galaxy at z=7.13. The new emission line in this work, [NIII] 57 um, provides us with a precise nitrogen-to-oxygen abundance ratio (N/O) by being combined with [OIII] emission lines. Unfortunately, the [NIII] 57 um line was not detected; however, this non-detection results in a stringent N/O upper limit at almost the solar value. This low abundance ratio demonstrates that A1689-zD1 is not a nitrogen-rich emitter recently found with JWST rest-frame UV spectroscopy. Importantly, [NIII] 57 um and rest-frame UV emission lines trace different ionized regions in terms of the electron density. ALMA [NIII] 57 observations shed light on the nitrogen abundance in normal star-forming regions at high redshift, which is complementary to very dense, highly ionized regions traced by JWST.

More than 6000 exoplanets have been discovered to date, and many are thought to begin forming during the earliest stages of star formation, when protostellar disks have just emerged and are still growing. The formation and early evolution of these disks therefore set the initial conditions for planet formation. Theoretically, disk formation is strongly regulated by microphysical processes, including non-ideal magnetohydrodynamic (MHD) effects that control magnetic flux transport and angular momentum redistribution. Subsequent planet formation within disks is further shaped by dust aerodynamics. In this presentation, I will discuss possible observational experiments to test non-ideal MHD effects and dust physics in protostellar disks.

Millimeter polarization is a unique probe of dust properties in protoplanetary disks. Before ALMA, polarized emission from disks had rarely been detected because of the low polarization fraction (~1%) and the need for high sensitivity. ALMA opened this field by detecting and spatially resolving polarized emission, enabling studies of dust self-scattering and grain alignment in the disk environments. In this talk, I will discuss why disk polarization should be an important science case for ALMA 2040. Protoplanetary disks commonly show rings, gaps, asymmetries, and other substructures, so high angular resolution is essential for interpreting polarization patterns and connecting them to dust growth and planet formation. However, extending polarization studies from a small number of the brightest disks to statistically meaningful samples still requires substantially higher sensitivity. Future ALMA capabilities combining sensitivity, angular resolution, broad frequency coverage, and accurate polarization calibration will be crucial for making millimeter polarization a general diagnostic of dust evolution in planet-forming disks.

Protoplanetary disks form around young stars when dense molecular cloud cores collapse. An outer shroud of gas and dust, known as the envelope, surrounds and feeds both the young star and the forming disk. The observations of protostellar systems show a break in the radial profile of specific angular momentum (and in the rotational velocity) at the envelope-disk transition. In this talk, I will present our results based on both theoretical and observational grounds, which show the existence of a distinct transition zone at the envelope-disk interface, through which infalling gas motions from the envelope transform into Keplerian motions within the disk. We name this transition zone as ENDTRANZ (Envelope Disk Transition Zone). To determine the physics of the ENDTRANZ, we first employ global MHD disk simulations of gravitational collapse starting from a prestellar core. Our simulations reveal that the transition from the envelope to the Keplerian disk gradually unfolds through a jump across a finite thickness in the radial profile of specific angular momentum. This jump serves as a kinematical tracer for the angular momentum redistribution within ENDTRANZ and suggests how the internal torques drive the disk evolution. We also, for the first time, identify a similar jump in the radial profile of the specific angular momentum at the envelope-disk transition of class 0/I protostar L1527 IRS, using ALMA Large Program eDisk (Embedded Disks in Planet Formation) observations. This observed jump confirms the existence of an ENDTRANZ in L1527 IRS. Our results offer insights into the observable imprints of mass and angular momentum redistribution during star–disk formation.

Planet-forming disks display substructures, gaps, rings, spirals, and asymmetries, which are

widely interpreted as signposts of embedded planets. High-contrast direct imaging is a powerful

tool for resolving these features, yet conventional angular differential imaging suffers from

self-subtraction artifacts that can obscure genuine disk structure. Near-simultaneous reference

differential imaging via the star-hopping technique offers a robust alternative, recovering

high-fidelity total-intensity images free from these biases.

We present high-resolution Ks-band total- and polarized-intensity observations of the HD

163296 protoplanetary disk with SPHERE/VLT using the star-hopping strategy. This structured

disk, suspected to harbor one or more protoplanets from prior kinematic studies, is analyzed

through radiative-transfer modeling with a two-zone geometry and two grain populations,

simultaneously fit to near-infrared and archival ALMA submillimeter data, tracing both disk

surface and midplane layers. From the well-resolved inner disk, we constrain the scattering

phase function and polarized fraction within an aggregate-dust framework. We further perform a

multi-epoch search for potential embedded planetary companions and apply inverse

polarimetric mapping as an independent probe of point sources within the disk.

During star formation, materials are transported from envelopes to disks, where planet formation takes place. Along this journey, which ranges from thousands of au to a few au, chemical reactions between gas and grains enrich the compositions of these materials and, at the same time, regulate the tracers that we can probe throughout the evolution. On this subject, ALMA has made paradigm-defining discoveries, from asymmetric infall and late infall in protostellar and protoplanetary disks, to complex molecules detected in envelopes and disks, and to the substructures leading to planet formation. However, the orders of magnitude difference in spatial scale still poses a great challenge observationally to probe the envelope scale at the same sensitivity as that for the disk scale. A substantial increase in short-baseline sensitivity will overcome this limitation, which is essential to depict a complete picture of a co-evolving system with an envelope and disks. In this talk, I will use ALMA data to demonstrate the current limitations and show why short-baseline capability is needed in ALMA2040.

The next frontier in astrochemistry is no longer the detection of individual complex organic molecules, but the reconstruction of chemical networks that connect molecular clouds, protostellar envelopes, planet-forming disks, and ultimately the ingredients of the Solar System. While ALMA has been transformative, current observations remain limited to the brightest species and nearby benchmark sources, leaving the emergence and diversity of chemical complexity largely unexplored. I will present a science case for ALMA2040 centered on a comprehensive census of prebiotic chemistry across Galactic environments. Substantial gains in sensitivity, combined with broad instantaneous spectral coverage and high angular resolution, would enable simultaneous detection of large populations of chemically related species, isotopologues, and reaction intermediates. Such capabilities would further enable direct measurements of molecular inventories, isotopic fractionation, and chemical inheritance from molecular clouds to planetary system. By tracing the emergence and inheritance of complex organic matter across evolutionary stages, ALMA2040 could determine whether the chemical pathways leading towards prebiotic molecules are ubiquitous in the Galaxy and establish the link between interstellar chemistry and the origins of life.