The High-Resolution Infrared Spectrograph for Exoplanet Characterization (HISPEC) is a new instrument for the W. M. Keck Observatory that enables R similar to 100,000 spectroscopy simultaneously across the y, J, H, and K astronomical bands (0.98-2.5 mu m). The fiber delivery subsystem of HISPEC is responsible for routing science and calibration light throughout the observatory efficiently. It consists of high-performance single mode fibers, a photonic lantern, mechanical and MEMS-based fiber switchers that allow for the reconfiguration of light paths. To efficiently cover this large wavelength range, a silica fiber is used for the y&J bands and the 1x3 photonic lantern while a ZBLAN fiber is used for the H&K bands. The HK fiber is a custom design by Le Verre Fluore. The fibers route the science light from the focal point of the adaptive optics system to spectrographs in the basement similar to 65 m away, hence, the fibers must be very efficient. To calibrate the instrument, several mechanical fiber switchers can be used to direct calibration light to the spectrograph or the front of the optical train. Some switchers must make over 800 cycles annually, while maintaining sub-3% coupling losses between fibers with core sizes of 4.4 mu m. To achieve this, extensive testing was conducted, in which throughput and dust accumulation were monitored to determine how these parameters are impacted by switch preparation procedures and ambient environmental conditions. We developed systems to automatically and remotely clean and image fiber end faces in situ. We have created a protocol that allows us to achieve thousands of switch connections reliably. Additionally, through the 25,000+ switch cycles ran during testing, we identified shortcomings in the design of these mechanical fiber switchers which will be remedied for the final instrument. In this paper, we describe the detailed design of the fiber delivery subsystem for HISPEC and outline several innovative solutions and summarize our de-risking activities to date.

We measure the photon arrival timing jitter of three superconducting Microwave Kinetic Inductance Detectors (MKIDs) within a large array of 20,440 pixels, spanning resonating frequencies from 4 to 8 GHz. We analyze arrival time distributions for photon number n = 1 and n = 2 events and find the distribution full-width at half-maximum ranging from 132 to 796 ns across the three detectors. In combination with nearly zero dark counts and multiplexed readout schemes, sub-microsecond jitter can be leveraged for high-time resolved astronomy, quantum, and bio-physics applications. The measured system jitter serves as an upper limit for MKIDs, with optimized performance likely reaching tens of nanoseconds. We discuss how to improve upon the detector and readout performance.

MagAO-X is the coronagraphic extreme adaptive optics system for the 6.5 m Magellan Clay Telescope. We report the results of commissioning the first phase of MagAO-X. Components now available for routine observations include: the > 2 kHz high-order control loop consisting of a 97 actuator woofer deformable mirror (DM), a 2040 actuator tweeter DM, and a modulated pyramid wavefront sensor (WFS); classical Lyot coronagraphs with integrated low-order (LO) WFS and control using a third 97-actuator non-common path correcting (NCPC) DM; broad band imaging in g, r, i, and z filters with two EMCCDs; simultaneous differential imaging in Ha; and integral field spectroscopy with the VIS-X module. Early science results include the discovery of an Ha jet, images of accreting protoplanets at H alpha, images of young extrasolar giant planets in the optical, discovery of new white dwarf companions, resolved images of evolved stars, and high-contrast images of circumstellar disks in scattered light in g-band (500 nm). We have commenced an upgrade program, called "Phase II", to enable high-contrast observations at the smallest inner working angles possible. These upgrades include a new 952 actuator NCPC DM to enable coronagraphic wavefront control; phase induced amplitude apodization coronagraphs; new fast cameras for LOWFS and Lyot-LOWFS; and real-time computer upgrades. We will report the status of these upgrades and results of first on-sky testing in March-May 2024.

Building large, cryogenic MKID arrays requires processing highly-multiplexed, wideband readout signals in real time; a task that has previously required large, heavy, and power-intensive custom electronics. In this work, we present the third-generation UVOIR MKID readout system (Gen3) which is capable of reading out twice as many detectors with a fifth the weight and power and an order of magnitude less volume and cost-per-pixel as compared to the previous system. Gen3 leverages the Xilinx RFSoC4x2 platform to read out 2048, 1 MHz MKID channels per board. The system takes a modern approach to FPGA design using Vitis High-Level Synthesis (HLS) to specify signal processing blocks in C/C++, Vivado ML Intelligent Design Runs (IDR) to inform implementation stragety and close timing, and Python Productivity for ZYNQ (PYNQ) to simplify interacting with and programming the FPGA using Python. This design suite and tool flow allows general users to contribute to and maintain the design and positions Gen3 to rapidly migrate to future platforms as they become available. In this work, we describe the system requirements, design, and implementation. We also provide performance characterization details and show that the system achieves detector-limited resolving power in the case of few readout tones and minimal degradation with all 2048 tones. Planned upgrades and future work are also discussed. The Gen3 MKID readout system is fully open-source and is expected to facilitate future array scaling to megapixel-sized formats and increase the feasibility of deploying UVOIR MKIDs in space.

We present spectroscopic data for 16,369 stellar targets within and/or toward 38 dwarf spheroidal galaxies and faint star clusters within the Milky Way halo environment. All spectra come from observations with the multiobject, fiber-fed echelle spectrographs M2FS at the Magellan/Clay telescope or Hectochelle at the MMT, reaching a typical limiting magnitude G less than or similar to 21. Data products include processed spectra from all observations and catalogs listing estimates-derived from template model fitting-of line-of-sight velocity (median uncertainty 1.4 km s(-1)) effective temperature (255 K), (base-10 logarithm of) surface gravity (0.59 dex in cgs units), [Fe/H] (0.4 dex) and [Mg/Fe] (0.27 dex) abundance ratios. The sample contains multiepoch measurements for 3720 sources, with up to 15 epochs per source, enabling studies of intrinsic spectroscopic variability. The sample contains 6087 likely red giant stars (based on surface gravity), and 4492 likely members (based on line-of-sight velocity and Gaia-measured proper motion) of the target systems. The number of member stars per individual target system ranges from a few, for the faintest systems, to similar to 850 for the most luminous. For most systems, our new samples extend over wider fields than have previously been observed; of the likely members in our samples, 820 lie beyond 2 times the projected half-light radius of their host system, and 42 lie beyond 5 R-half.

The ultrafaint dwarf galaxy Reticulum II was enriched by a single rare and prolific r -process event. The r -process content of Reticulum II thus provides a unique opportunity to study metal mixing in a relic first galaxy. Using multi-object high-resolution spectroscopy with VLT/GIRAFFE and Magellan/M2FS, we identify 32 clear spectroscopic member stars and measure abundances of Mg, Ca, Fe, and Ba where possible. We find 72 − 12 + 10 % of the stars are r -process-enhanced, with a mean [ Ba / H ] = − 1.68 ± 0.07 and unresolved intrinsic dispersion σ [Ba/H] <0.20. The homogeneous r -process abundances imply that Ret II’s metals are well mixed by the time the r -enhanced stars form, which simulations have shown requires at least 100 Myr of metal mixing in between bursts of star formation to homogenize. This is the first direct evidence of bursty star formation in an ultrafaint dwarf galaxy. The homogeneous dilution prefers a prompt and high-yield r -process site, such as collapsar disk winds or prompt neutron star mergers. We also find evidence from [Ba/H] and [Mg/Ca] that the r -enhanced stars in Ret II formed in the absence of substantial pristine gas accretion, perhaps indicating that ≈70% of Ret II stars formed after reionization.

We used high-resolution spectra acquired with the Magellan Telescope to measure radial and rotational velocities of approximately 200 stars in the Galactic globular cluster NGC 3201. The surveyed sample includes blue straggler stars (BSSs) and reference stars in different evolutionary stages (main-sequence turnoff, subgiant, red giant, and asymptotic giant branches). The average radial velocity value (〈V r 〉 = 494.5 ± 0.5 km s−1) confirms a large systemic velocity for this cluster and was used to distinguish 33 residual field interlopers. The final sample of member stars has 67 BSSs and 114 reference stars. Similarly to what is found in other clusters, the totality of the reference stars has negligible rotation (< 20 km s−1), while the BSS rotational velocity distribution shows a long tail extending up to ∼200 km s−1, with 19 BSSs (out of 67) spinning faster than 40 km s−1. This sets the percentage of fast-rotating BSSs to ∼28%. Such a percentage is roughly comparable to that measured in other loose systems (ω Centauri, M4, and M55) and significantly larger than that measured in high-density clusters (as 47 Tucanae, NGC 6397, NGC 6752, and M30). This evidence supports a scenario where recent BSS formation (mainly from the evolution of binary systems) is occurring in low-density environments. We also find that the BSS rotational velocity tends to decrease for decreasing luminosity and surface temperature, similarly to what is observed in main-sequence stars. Hence, further investigations are needed to understand the impact of BSS internal structure on the observed rotational velocities.

The dense central regions of tidally disrupted galaxies can survive as ultracompact dwarfs (UCDs) that hide among the luminous globular clusters (GCs) in the halo of massive galaxies. An exciting confirmation of this model is the detection of overmassive black holes in the centers of some UCDs, which also lead to elevated dynamical mass-to-light ratios (M/L dyn). Here we present new high-resolution spectroscopic observations of 321 luminous GC candidates in the massive galaxy NGC 5128/Centaurus A. Using these data we confirm 27 new luminous GCs, and measure velocity dispersions for 57 luminous GCs (with g-band luminosities between 2.5 × 105 and 2.5 × 107 L ⊙), of which 48 are new measurements. Combining these data with size measurements from Gaia, we determine the M/L dyn for all 57 luminous GCs. We see a clear bimodality in the M/L dyn distribution, with a population of normal GCs with mean M/L dyn = 1.51 ± 0.31, and a second population of ∼20 GCs with elevated mean M/L dyn = 2.68 ± 0.22. We show that black holes with masses ∼4%–18% of the luminous GCs can explain the elevated mass-to-light ratios. Hence, it is plausible that the NGC 5128 sources with elevated M/L dyn are mostly stripped galaxy nuclei that contain massive central black holes, though future high spatial resolution observations are necessary to confirm this hypothesis for individual sources. We also present a detailed discussion of an extreme outlier, VHH81-01, one of the largest and most massive GC in NGC 5128, making it an exceptionally strong candidate to be a tidally stripped nucleus.

IFUM (Integral Field Units for Magellan) consists of three IFUs at the Nasmyth-East focus of the Magellan/Clay telescope. Each IFU consists of a Barlow lens, a lenslet array, a set of fiber assemblies that feed a pair of fiber shoes that allow the fibers to be used with the twin spectrographs of M2FS (the 'Michigan/Magellan Fiber System'). The IFUs are optimized for excellent seeing conditions (the 'HR' IFU with 864 fibers with 75µm diameter cores), standard seeing conditions ('STD', 552 fibers, 150µm) and extended (low surface brightness) targets ('LSB', 360 fibers, 260µm). The Barlow lenses magnify the field at the lenslet arrays which deliver to each fiber images the telescope entrance pupil (the primary mirror) at f/3.5—as defined by the marginal rays of the pupil image—that becomes an f/3.3 output beam at the spectrographs. The fiber assemblies consist of 'sky-end' fiber mounts that are aligned with the lenslet arrays to high precision and 'spectrograph-end' fiber mounts that maintain the fibers at the focal surfaces of the spectrographs within the fiber shoes. The fibers can be aligned within the shoes with slits that deliver spectral resolutions ranging from ℛ = 1200 to 40000. Movable focal-plane masks on each IFU enable spectroscopy of faint sources near much brighter point sources (e.g. AGN or young stellar objects). IFUM can be used with a deployable ADC on the Magellan/Clay guider; a separate deployable mirror on the guider allows onboard calibration light sources to illuminate any of the IFUM IFUs. Initial commissioning data are presented.

MagAO-X is a visible to near-IR AO system that will enable a suite of instruments to perform high-contrast, high-resolution science. During its "Phase II" plan a 10-kilopixel Microwave Kinetic Inductance Detector (MKID) IFU will be deployed as a science camera behind MagAO-X. MKIDs are photon-counting detectors with energy resolution up to 30. The photon counting capability and readout allow for microsecond time resolution with no associated read noise. As a consequence of the high readout rate the MKID camera can be used as a Focal Plane Wavefront Sensor (FPWFS) allowing real-time speckle control while simultaneously taking science observations. With the high resolution and contrasts delivered by MagAO-X the MKID camera will aim to directly image and characterize exoplanets in the near-IR. The camera's IR filters can also be replaced with visible filters that will allow for further characterization and the potential for exploration of the inner regions of circumstellar disks.

Superconducting devices represent a class of breakthrough technologies enabling detection and manipulation of quantum signals [1] – [3] . Many thousands of interconnected superconducting devices are needed to support quantum error correction for quantum computing and mega-pixel-scale scientific cameras for single-photon-sensing applications [4] – [6] . With each device requiring up to 1 MHz of bandwidth, full readout systems must perform analysis on multi-gigahertz, ultra-wideband signals in real time [7] .

The Pathways to Discovery in Astronomy and Astrophysics for the 2020s decadal survey highlighted the ability of the coming generation of 30-meter-class telescopes “to detect, image, and characterize temperate rocky planets around low-mass stars, measure their atmospheric compositions including searches for oxygen.” However, many of the technologies required to reach the challenging contrast ratios associated with this science case are not yet available, and targeted preparatory science must be carried out well in advance of these observations. In this paper, we draw from the example of NASA’s Exoplanet Exploration Program and propose a preliminary version of a “Technology Gap List” and “Science Gap List” for the ground-based imaging of rocky planets around the nearest stars with extremely large ground-based telescopes. These lists can be used to prioritize precursor technical demonstrations and observations with current and near-term high contrast instrumentation, so that the community is ready to exploit the collecting area of extremely large telescopes.