The Sloan Digital Sky Survey V (SDSS-V) Local Volume Mapper (LVM) is an ultra-wide field high spatial resolution IFU survey of the Milky Way, the Magellanic Clouds, and a sample of galaxies in the local volume. Observations are carried out with the LVM Instrument (LVM-I), a specially designed robotic telescope, instrument, and facility located at Las Campanas Observatory (LCO) in Chile. The LVM-I is hosted in a custom-built roll-off type enclosure that protects the hardware, allows for simultaneous observations towards different directions in the sky by the four LVM-I telescopes, provides a thermally controlled stable and clean environment for the LVM-I spectrographs, supplies all necessary utilities (e.g. power, communications, LN2 detector cooling) to the different LVM-I sub-systems, provides environmental telemetry and information, and integrates with the LVM-I control software to operate in an automated fashion. In this paper we discuss the design of the LVM-I enclosure, its construction, and an evaluation of its performance. The LVM-I was successfully integrated on-site and commissioned during the first half of 2023, with the enclosure design and performance meeting its requirements and allowing for the start of the SDSS-V LVM project science operations.
We describe the Sloan Digital Sky Survey Local Volume Mapper Instrument (LVM-I) construction, testing, and initial performance. The facility is designed to produce the first integral map of thousands of degrees of the Southern sky. The map will cover spectra from bluer than [O II] to 980 nm with a dispersion of over R = Δλ/λ > 4, 000 at Hα wavelength. Each spaxel will have a pitch of ∼35′′, and the survey will be conducted using four integral field units (IFUs) with an instantaneous field of view of 530 arcmin2. The LVM facility is designed to achieve the required sub-Rayleigh spectroscopy over large sky areas with outstanding spectrophotometric accuracy and precision. LVM-I is designed to produce this unique dataset using four siderostats on commercial mounts. The four beams are fed into 16-cm-diameter f/11.4 apochromatic objectives, and the sky is derotated with K mirrors. These telescopes produce an image of the field onto both guider cameras and a lenslet array. The array reimages the field at f/3.7 onto 107-micron-diameter fibers. Blue throughput is maximized with a short 18.5-m fiber run from the IFUs to the spectrographs. The fibers are reconfigured inside a splicing box to distribute the fibers from the four telescopes to three spectrographs. The spectrographs are near-copies of the Dark Energy Survey three-band f/1.7 spectrographs, which deliver sharp images over the entire chromatic range. Nine STA charge-coupled devices (CCDs), cooled with liquid-nitrogen dewars, are used for the survey. The LVM-I is controlled with custom Python software and distributed over various computers using power-over-ethernet networking. The system is housed in a custom enclosure with a roll-off roof to grant access to the sky. The enclosure allows all four telescopes to point all over the sky and measure the transmissivity of the atmosphere and the sky background. Some of the first-light data products are highlighted here.
We developed control software for an enclosure system of the SDSS-V Local Volume Mapper (LVM) which provides a contiguous 2,500 deg2 integral-field survey. The LVM enclosure, located at the Las Campanas Observatory in Chile, is a building that hosts the LVM instruments (LVM-I). The enclosure system consists of four main systems: 1) a roll-off dome, 2) building lights, 3) a Heating, Ventilation, and Air Conditioning (HVAC) system, and 4) a safety system. Two Programmable Logic Controllers (PLCs) as middleware software directly operate complex mechanisms of the dome and the HVAC via the Modbus protocol. The LVMECP is implemented by Python 3.9 following the SDSS software framework which adopted a protocol, called CLU, with message passing based on the RabbitMQ and Advanced Message Queuing Protocol (AMQP). Also, we applied asynchronous programming to our system to process multiple requests simultaneously. The Dome PLC system remotely sends commands for the operation of a roll-off dome and enclosure lights. The HVAC PLC system keeps track of changing environmental values of the HVAC system in real-time. This software provides observers with remote access by high-level commands.
We describe the on-sky performance of the robotic Focal Plane System (FPS) units that replace the fiber plug-plate systems at the Sloan and duPont telescopes for the SDSS-V survey. The first FPS was arrived at Apache Point in December 2021, and the second unit will be delivered to Las Campanas in spring 2022. Each FPS carries 500 zonal fiber positioners carrying three fibers: two science fibers for the BOSS and APOGEE spectrographs and a back-illuminated metrology fiber. The FPS enables the SDSS-V Milky Way and Black Hole Mapper surveys that will begin survey operations in 2022.
VERMILION is a VLTI visitor instrument project intended to extend the sensitivity and the spectral coverage of Optical Long Baseline Interferometry (OLBIn). It is based on a new concept of Fringe Tracker (VERMILIONFT) combined with a J band spectro-interferometer (VERMILION-J). The Fringe Tracker is the Adaptive Optics module specific to OLBIn that measures and corrects in real time the Optical Path Difference (OPD) perturbations introduced by the atmosphere and the interferometer, by providing a sensitivity gain of 2 to 3 magnitudes over all other state of the art fringe trackers. The J band spectro-interferometer will provide all interferometric measurements as a function of wavelength. In addition to a possible synergy with MATISSE, VERMILION-J, by observing at high spectral resolution many strong lines in J (Paβ-γ, HeII, TiO and other metallic monoxides), will cover several scientific topics, e.g. Exoplanets, YSOs, Binaries, Active Hot, Evolved stars, Asteroseismology, and also AGNs.
The current work presents a fiber coupling tip-tilt controller developed for a three-telescope experimental prototype of an Astronomical Fiber-Based Near-Infrared Heterodyne Interferometer. It is based on a commercial magneto-mechanical compact-disk laser-beam actuator on which the fiber-ferrule is mounted. The actuator is driven by a two-axis controller electronics board which was developed by us based on digital processing in a dsPIC33EP device with analog periphery, which reads the quad-photodiode signals amplified by 109, and drives the actuator with two high-current outputs. While this realizes the very fine and relatively fast (up to 100 Hz) fiber-position control in the telescope focus, as a basis to this, a relatively coarse and slow auto-guiding is given by an amateur guiding camera. During first optical bench testing we obtained an average coupled power increase of up to 50% under certain perturbations.
Recent results for the cross-correlation signal of a newly proposed balanced correlation receiver at 1.5 μm pointed towards a possible bypassing of the standard quantum limit for the receiver noise-temperature hν⁄k in cross-correlation by a factor of 4-6. The only radiation source strong enough for a clear hot-cold measurement was a heavily attenuated fiber-coupled superluminant LED (SLED), because a multi-mode fiber-coupled thermal halogen lamp was difficult to control in polarization due to its weakness when coupled to a single-mode fiber. This peculiarity left some doubts regarding a possible “strange” quantum-mechanical behavior of the signal light from the SLED. Here we want to present the concept for more convincing measurements using a true thermal signal source.
A semi-classical theory was re-derived in a consistent form for properly comparing direct and heterodyne detection as a function of wavelength. Plots are shown for example cases. We show that heterodyne should be better than direct detection for wavelengths longer than 3 microns, even with a bandwidth disadvantage, since direct detection is more sensitive to ambient temperature background than heterodyne detection. For interferometry the advantage of heterodyne is more pronounced in this case due to the smaller beam filling factors. When we include even the effect of surpassing the noise temperature quantum limit with a novel correlation receiver architecture (see paper 10701-94), the advantage of heterodyne detection becomes irrefutable.
KEYWORDS: Receivers, Signal to noise ratio, Heterodyning, Interference (communication), Photodiodes, Sensors, Signal detection, Optical correlators, Temperature metrology, Electroluminescence
We present concept and first experimental lab results for a novel heterodyne correlation receiver architecture and demonstrate that it can surpass the standard quantum limit (SQL) for the noise temperature by “correlating out” the local oscillator shot noise made uncorrelated at both receivers due to replacing the laser shot noise by individual beam splitter noise. It is based on two balanced receivers, comprising in total of 4 mixers, and uses an 8-bit digitization FPGA-based 1GHz bandwidth digital correlation between the two receivers. The demonstrated prototype was built for 1550 nm using InGaAs balanced photodiodes. We present here a summary of the results described in detail in a paper accepted at IEEEAccess journal. The extra-sensitivity would lead to heterodyne being better than direct detection for wavelengths beyond 3 microns. We propose therefore this receiver architecture as a building block in a heterodyne technology to be developed for the future Planet Formation Imager Infrared Interferometer (PFI). This paper is a reduced version of a paper accepted at IEEE Access a week before the conference [1].
We present the concept and experimental development of a low-cost near-infrared heterodyne interferometer prototype based on commercial 1.55 μm fiber components. As the most crucial component of it we characterized a novel sub-shot noise correlation detection system. We are upgrading to a Reconfigurable Open Architecture Computing Hardware, 2nd Generation (ROACH-2) board with the capacity of four parallel 1.25 GHz bandwidth digitization, so that phase closure measurements will be possible. We extended the stabilization of the local oscillator phase between the telescopes to cover the whole acoustic range. For the telescope to single-mode fiber coupling under atmospheric perturbation, we developed a fiber actuator lock-loop for small telescopes and good seeing, and tested an adaptive optics approach for mediocre seeing and/or larger telescopes. We constructed also a frequency comb based laser synthesizer system to include tests on multi-frequency band measurements towards ultra-broad band dispersed" heterodyne detection systems finally useful for the Planet Formation Imager (PFI).
We present concept and first experimental lab results for a low-cost near-infrared heterodyne interferometer based on commercial 1.55μm fiber components with relative phase-stabilization between both telescopes. After a demonstration with 14”-telescopes, the concept should be upgradable to larger numbers of mid- or large-class telescopes. Given that the employed fiber phase stabilization scheme should enable the operation of long baselines, we discuss the applicability of this concept for long-baseline, high telescope number systems (scalability of the concept) and mid-infrared wavelengths. This could finally result in contributions to the design of the large infrared Planet Formation Imager which is being proposed currently.
We are presenting first experimental results for subsystems of a low-cost near-infrared heterodyne interferometer concept based on commercial 1.55μm fiber-components with relative phase-stabilization between both telescopes, a shot noise limited heterodyne scheme with ambient temperature operated photodiodes, an ultra-coherent fiber laser, and a ROACH-based correlator. After we worked on a first demonstration with two 14” amateur telescopes on Betelgeuse, the concept should be upgradable to connect mid- or large-class telescopes, also given that the employed fiber phase stabilization scheme will enable the operation of long baselines.
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