We report ALMA and ACA observations of atomic carbon ([C1](1-0)) and dust continuum in 10 Enormous Lyα Nebulae hosting ultra-luminous Type-I QSOs at z=2.2-2.5, as part of the SUrvey of Protocluster ELANe Revealing CO/CI in the Lyα Detected CGM (SUPERCOLD-CGM). We detect [C1](1-0) and dust in all ten QSOs and five companion galaxies. We find that the QSOs and companions have higher gas densities and more intense radiation fields than Luminous Infrared galaxies and high-z main sequence galaxies, with the highest values found in the QSOs. By comparing molecular gas masses derived from [C1](1-0), CO(4-3) and dust continuum, we find that the QSOs and companions display a similar low CO conversion factor of α_ CO ∼ 0.8 M_[ K km/s pc^2]^-1. After tapering our data to low resolution, the [C1](1-0) flux increases for nine QSOs, hinting at the possibility of [C1](1-0) in the circum-galactic medium (CGM) on a scale of 16-40 kpc. However, the [C1](1-0) sensitivity is too low to confirm this for individual targets, except for a tentative (2.7σ) CGM detection in Q0050+0051 with M_ H_2 = (1.0 - 2.8)× 10^10 M_. The 3σ mass limits of molecular CGM for the remaining QSO fields are (0.2-1.4) × 10^10 M_. This translates into a baryon fraction of <0.4-3% in the molecular CGM relative to the total baryonic halo mass. Our sample also includes a radio-detected AGN, Q1416+2649, which shows [C1](1-0) and CO(4-3) luminosities an order of magnitude fainter for its far-infrared luminosity than other QSOs in our sample, possibly due to a lower molecular gas mass.

We present continuum observations from the Atacama Large Millimeter/submillimeter Array of 10 high-redshift (2.2 ≤ z ≤ 2.7) ultraluminous quasars (QSOs) and constrain the presence of hot, ionized, circumgalactic gas in a stacking analysis. We measure a Compton- y parameter profile with a peak value of (1.7 ± 1.1) × 10 ^−6 at a radius of ∼50 kpc. We compare our stacked observations to active galactic nucleus feedback wind models and generalized Navarro–Frenk–White pressure profile models to constrain the wind luminosity and halo mass of the stacked QSOs. Our observations constrain the observed average halo mass to M _500 < 1 × 10 ^13 M _⊙ and the average feedback wind power <1 × 10 ^12 L _⊙ , which is <1% of the bolometric luminosity of the quasar.

We report Atacama Large Millimeter/submillimeter Array and Atacama Compact Array observations of atomic carbon ([C I](1-0)) and dust continuum in 10 enormous Ly alpha nebulae hosting ultraluminous Type-I QSOs at z = 2.2-2.5, as part of the Survey of Protocluster ELANe Revealing CO/C I in the Ly alpha Detected CGM. We detect [C I](1-0) and dust in all 10 QSOs and five companion galaxies. We find that the QSOs and companions have higher gas densities and more intense radiation fields than Luminous Infrared galaxies and high-z main sequence galaxies, with the highest values found in the QSOs. By comparing molecular gas masses derived from [C I](1-0), CO(4-3), and dust continuum, we find that the QSOs and companions display a similar low CO conversion factor of alpha(CO) similar to 0.8 M-circle dot[Kkms-1pc(2)](-1). After tapering our data to low resolution, the [C I](1-0) flux increases for nine QSOs, hinting at the possibility of [C I](1-0) in the circumgalactic medium (CGM) on a scale of 16-40 kpc. However, the [C I](1-0) sensitivity is too low to confirm this for individual targets, except for a tentative (2.7 sigma) CGM detection in Q0050+0051 with M-H2 = (1.0-2.8) x 10(10)M(circle dot). The 3 sigma mass limits of molecular CGM for the remaining QSO fields are (0.2-1.4) x 10(10)M(circle dot). This translates into a baryon fraction of <0.4%-3% in the molecular CGM relative to the total baryonic halo mass. Our sample also includes a radio-detected active galactic nuclei, Q1416+2649, which shows [C I](1-0) and CO(4-3) luminosities an order of magnitude fainter for its far-infrared luminosity than other QSOs in our sample, possibly due to a lower molecular gas mass.

To understand how massive galaxies at high z coevolve with enormous reservoirs of halo gas, it is essential to study the coldest phase of the circumgalactic medium (CGM), which directly relates to stellar growth. The SUPERCOLD-CGM survey is the first statistical survey of cold molecular gas on CGM scales. We present Atacama Large Millimeter Array and Atacama Compact Array observations of CO(4-3) and continuum emission from 10 enormous Ly & alpha; nebulae (ELANe) around ultraluminous type I quasi-stellar objects (QSOs) at z & SIM; 2. We detect CO(4-3) in 100% of our targets, with 60% showing extended CO on scales of 15-100 kpc. Q1228+3128 reveals the most extended CO(4-3) reservoir of & SIM;100 kpc and is the only radio-loud target in our sample. The CO reservoir is located along the radio axis, which could indicate a link between the inner radio jet and cold halo gas. For the other five radio-quiet ELANe, four of them show extended CO(4-3) predominantly in the direction of their companions. These extended CO(4-3) reservoirs identify enrichment of the CGM and may potentially contribute to widespread star formation. However, there is no evidence from CO(4-3) for diffuse molecular gas spread across the full extent of the Ly & alpha; nebulae. One target in our sample (Q0107) shows significant evidence for a massive CO disk associated with the QSO. Moreover, 70% of our QSO fields contain at least one CO companion, two of which reveal extended CO emission outside the ELANe. Our results provide insight into roles of both the cold CGM and companions in driving the early evolution of massive galaxies.

We investigate the resolved kinematics of the molecular gas, as traced by the Atacama Large Millimeter/submillimeter Array in CO (2−1), of 25 cluster member galaxies across three different clusters at a redshift of z ∼ 1.6. This is the first large-scale analysis of the molecular gas kinematics of cluster galaxies at this redshift. By separately estimating the rotation curve of the approaching and receding sides of each galaxy via kinematic modeling, we quantify the difference in total circular velocity to characterize the overall kinematic asymmetry of each galaxy. 3/14 of the galaxies in our sample that we are able to model have similar degrees of asymmetry as that observed in galaxies in the field at similar redshift based on observations of mainly ionized gas. However, this leaves 11/14 galaxies in our sample with significantly higher asymmetry, and some of these galaxies have degrees of asymmetry of up to ∼50 times higher than field galaxies observed at similar redshift. Some of these extreme cases also have one-sided tail-like morphology seen in the molecular gas, supporting a scenario of tidal and/or ram pressure interaction. Such stark differences in the kinematic asymmetry in clusters versus the field suggest the evolutionary influence of dense environments, established as being a major driver of galaxy evolution at low redshift, is also active in the high-redshift universe.

We present testing of a 180GHz prototype filter bank spectrometer and report on designs for larger channeled millimeter-wave filter banks at 50-183 GHz. This technology will be utilized in the development of a novel low-SWaP-C microwave sounding sensor. It works by amplifying the broadband signal with an LNA then channelizing with the millimeter-wave filter bank. Each channel of the filter bank is detected by a separate diode. The sensor system enabled by the millimeter-wave filter bank has a great potential for measuring 3D atmospheric water vapor and temperature by detecting the 183 GHz water line. We will report here our progress in utilizing the sensor for on the ground detections of humidity and preliminary designs for the use of the sensor on a small satellite. Satellite based microwave radiometers are the most important driver of global weather forecasting. Current sensors rely on high-Swap-C LO/mixer/RF components. We will demonstrate that the maturation and adoptions of our novel sensor system would greatly improve weather forecasting. The prototype millimeter-wave filter banks were fabricated using a micro milling CNC with a tolerance of 5-microns and is a waveguide coupled to five spectrometer channels. The spectrometer channels are resonant with a tuned center frequency. We tested a single channel prototype to determine sensitivity. Testing was performed by driving a VNA extender with a signal generator to input a sweeping signal into the prototype.

3C 279 is an archetypal blazar with a prominent radio jet that show broadband flux density variability across the entire electromagnetic spectrum. We use an ultra-high angular resolution technique – global Very Long Baseline Interferometry (VLBI) at 1.3 mm (230 GHz) – to resolve the innermost jet of 3C 279 in order to study its fine-scale morphology close to the jet base where highly variableγ-ray emission is thought to originate, according to various models. The source was observed during four days in April 2017 with the Event Horizon Telescope at 230 GHz, including the phased Atacama Large Millimeter/submillimeter Array (ALMA), at an angular resolution of ∼20 μas (at a redshift ofz = 0.536 this corresponds to ∼0.13 pc ∼ 1700 Schwarzschild radii with a black hole massMBH = 8 × 108 M⊙). Imaging and model-fitting techniques were applied to the data to parameterize the fine-scale source structure and its variation. We find a multicomponent inner jet morphology with the northernmost component elongated perpendicular to the direction of the jet, as imaged at longer wavelengths. The elongated nuclear structure is consistent on all four observing days and across different imaging methods and model-fitting techniques, and therefore appears robust. Owing to its compactness and brightness, we associate the northern nuclear structure as the VLBI “core”. This morphology can be interpreted as either a broad resolved jet base or a spatially bent jet. We also find significant day-to-day variations in the closure phases, which appear most pronounced on the triangles with the longest baselines. Our analysis shows that this variation is related to a systematic change of the source structure. Two inner jet components move non-radially at apparent speeds of ∼15 cand ∼20 c(∼1.3 and ∼1.7 μas day−1, respectively), which more strongly supports the scenario of traveling shocks or instabilities in a bent, possibly rotating jet. The observed apparent speeds are also coincident with the 3C 279 large-scale jet kinematics observed at longer (cm) wavelengths, suggesting no significant jet acceleration between the 1.3 mm core and the outer jet. The intrinsic brightness temperature of the jet components are ≲1010K, a magnitude or more lower than typical values seen at ≥7 mm wavelengths. The low brightness temperature and morphological complexity suggest that the core region of 3C 279 becomes optically thin at short (mm) wavelengths.

The Event Horizon Telescope (EHT) is a very long baseline interferometry (VLBI) array that comprises millimeter- and submillimeter-wavelength telescopes separated by distances comparable to the diameter of the Earth. At a nominal operating wavelength of 1.3 mm, EHT angular resolution (lambda/D) is 25 micro-as, which is sufficient to resolve nearby supermassive black hole candidates on spatial and temporal scales that correspond to their event horizons. With this capability, the EHT scientific goals are to probe general relativistic effects in the strong-field regime and to study accretion and relativistic jet formation near the black hole boundary. In this Letter we describe the system design of the EHT, detail the technology and instrumentation that enable observations, and provide measures of its performance. Meeting the EHT science objectives has required several key developments that have facilitated the robust extension of the VLBI technique to EHT observing wavelengths and the production of instrumentation that can be deployed on a heterogeneous array of existing telescopes and facilities. To meet sensitivity requirements, high-bandwidth digital systems were developed that process data at rates of 64 gigabit/s, exceeding those of currently operating cm-wavelength VLBI arrays by more than an order of magnitude. Associated improvements include the development of phasing systems at array facilities, new receiver installation at several sites, and the deployment of hydrogen maser frequency standards to ensure coherent data capture across the array. These efforts led to the coordination and execution of the first Global EHT observations in 2017 April, and to event-horizon-scale imaging of the supermassive black hole candidate in M87.

The Event Horizon Telescope (EHT) is a very-long-baseline interferometry (VLBI) experiment that aims to observe supermassive black holes with an angular resolution that is comparable to the event horizon scale. The South Pole occupies an important position in the array, greatly increasing its north-south extent and therefore its resolution. The South Pole Telescope (SPT) is a 10-meter diameter, millimeter-wavelength telescope equipped for bolometric observations of the cosmic microwave background. To enable VLBI observations with the SPT we have constructed a coherent signal chain suitable for the South Pole environment. The dual-frequency receiver incorporates state-of-the-art SIS mixers and is installed in the SPT receiver cabin. The VLBI signal chain also includes a recording system and reference frequency generator tied to a hydrogen maser. Here we describe the SPT VLBI system design in detail and present both the lab measurements and on-sky results.