The Submillimeter array (SMA) is an array of 8 antennas operating at millimeter and sub-millimeter frequencies on Maunakea, Hawaii. At present, the frequency coverage of the SMA is from 180 to 420 GHz. Here we describe the challenges and progress of the SMA in implementing the wideband upgrade: the wSMA project, that we are undertaking. The existing or legacy instrument at the SMA consists of 4 single polarization Double-Side-Band (DSB) receivers. They are housed in a single cryostat with an aging He-4 GM/JT cryocooler. At the heart of the wSMA upgrade is a new receiver cryostat, cooled by a Cryomech PT410-RM pulse tube. The cryostat houses two dual-polarized receiver cartridges equipped with DSB SIS mixers. New Local Oscillator (LO) subsystems, based on a Voltage-Controlled Oscillator (VCO), as well as new mixer control electronics and IF processing upgrades are being introduced. Since there are differences between the existing SMA instrumentation and the new wSMA receiver system, in terms of sky frequency coverage and the available modes of operation, there are significant challenges of operating the legacy systems and the new wSMA instruments in parallel during the transition period. As it will take several years to replace the instrumentation in all 8 antennas, a detailed plan has been laid out to integrate the new instrument hardware and software packages into the array. We will present the transition plan to full wSMA operation, and we will also describe the antenna infrastructure changes, focusing on repurposing existing equipment and optics. In this presentation we will also discuss the comprehensive installation plan, in which the new wSMA cryostat, together with its associated compressor, chiller, electronics, LO's, cartridges, vacuum system are to be installed into the existing receiver cabin space. Another aspect of the project is to upgrade the internal computer networking that will be a key element of the upgrade, allowing the access and control of the distributed microcontrollers used in the entire instrumentation. The wSMA upgrade is expected to enhance the SMA's capabilities, further improve its sensitivity, as well as widening the Intermediate Frequency (IF) bandwidth. The transition plan that we have drawn up ensures that the wSMA upgrade will be easy to operate and will reduce the maintenance requirements by the SMA technical staff.
The Submillimeter Array (SMA) is an array of 8 antennas operating at millimeter and submillimeter wavelengths on Maunakea, Hawaii, operated by the Smithsonian Astrophysical Observatory and Academia Sinica Institute of Astronomy and Astrophysics, Taiwan. Over the past several years, we have been preparing a major upgrade to the SMA that will replace the aging original receiver cryostats and receiver cartridges with all new cryostats and new 230 and 345 GHz receiver designs. This wideband upgrade (wSMA) will also include significantly increased instantaneous bandwidth, improved sensitivity, and greater capabilities for dual frequency observations. In this paper, we will describe the wSMA receiver upgrade and status, as well as the future upgrades that will be enabled by the deployment of the wSMA receivers.
We describe the distributed control system that we are developing for the Wideband frontend receiver system for Submillimeter Array (wSMA). This distributed control system is based on an array of Raspberry-Pi (RPi) modules, which is embedded in each subsystem. The RPis run the Linux operating system and they are integrated with Input/Output (I/O) circuits which carry out the control and monitoring functions. The distributed architecture gives rise to a low-cost and yet versatile and powerful setup, which can be built up gradually by adding subsystems, one at a time. In this paper, we will present, in more details, two RPi-controlled subsystems: the Local oscillator (LO) module and the scanning spectrometer.
We report on the upgraded One Degree Imager (ODI) at the WIYN 3.5 meter telescope at the Kitt Peak Observatory after the focal plane was expanded by an additional seventeen detectors in spring 2015. The now thirty Orthogonal Transfer Array CCD detectors provide a total field of view of 40’ x 48’ on the sky. The newly added detectors underwent a design revision to mitigate reduced charge transfer efficiency under low light conditions. We discuss the performance of the focal plane and challenges in the photometric calibration of the wide field of view, helped by the addition of telescope baffles. In a parallel project, we upgraded the instrument’s three filter arm mechanisms, where a degrading worm-gear mechanism was replaced by a chain drive that is operating faster and with high reliability. Three more filters, a u’ band and two narrow band filters were added to the instrument’s complement, with two additional narrow band filters currently in procurement (including an Hα filter). We review the lessons learned during nearly three years of operating the instrument in the observatory environment and discuss infrastructure upgrades that were driven by ODI’s needs.
Here we describe the principles behind the design, construction, and implementation of a vector near-field beam scanner for the antennas of the Submillimeter Array. The Submillimeter Array (SMA) is a radio interferometer array operating at frequencies ranging from 200 { 700 GHz at the summit of Maunakea in Hawaii. A set of 4 receivers cover the key atmospheric windows over which the SMA operates. Each receiver insert is equipped with an ambient optical insert, which is pre-aligned in the lab prior to installation at the summit. However, as a result of receiver upgrades and problems, some receiver inserts may no longer be matched to the original optics inserts. Since the SMA is used extensively in dual-receiver observations, such beam mis-alignments lead to a relative pointing error between a pair of receivers during the observation. In order to address this issue, we have designed a near-field beam scanner which can be used to map out the receiver beam of each antenna. The setup employs the existing radio references available in each antenna for the vector beam measurement. We have successfully used this scanner to improve the on-sky co-alignment of receiver beams. In this presentation, we will describe the system and operational aspect of this in-situ radio frequency alignment technique.
The ALMA North America Prototype Antenna was awarded to the Smithsonian Astrophysical Observatory (SAO) in 2011. SAO and the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), SAO’s main partner for this project, are working jointly to relocate the antenna to Greenland to carry out millimeter and submillimeter VLBI observations. This paper presents the work carried out on upgrading the antenna to enable operation in the Arctic climate by the GLT Team to make this challenging project possible, with an emphasis on the unexpected telescope components that had to be either redesigned or changed. Five-years of inactivity, with the antenna laying idle in the desert of New Mexico, coupled with the extreme weather conditions of the selected site in Greenland have it necessary to significantly refurbish the antenna. We found that many components did need to be replaced, such as the antenna support cone, the azimuth bearing, the carbon fiber quadrupod, the hexapod, the HVAC, the tiltmeters, the antenna electronic enclosures housing servo and other drive components, and the cables. We selected Vertex, the original antenna manufacturer, for the main design work, which is in progress. The next coming months will see the major antenna components and subsystems shipped to a site of the US East Coast for test-fitting the major antenna components, which have been retrofitted. The following step will be to ship the components to Greenland to carry out VLBI
The Submillmeter Array (SMA) consists of 8 6-meter telescopes on the summit of Mauna Kea. The array has been
designed to operate from the summit of Mauna Kea and from 3 remote facilities: Hilo, Hawaii, Cambridge,
Massachusetts and Taipei, Taiwan. The SMA provides high-resolution scientific observations in most of the major
atmospheric windows from 180 to 700 GHz. Each telescope can house up to 8 receivers in a single cryostat and can
operate with one or two receiver bands simultaneously. The array being a fully operational observatory, the demand for
science time is extremely high. As a result specific time frames have been set-aside during both the day and night for
engineering activities. This ensures that the proper amount of time can be spent on maintaining existing equipment or
upgrading the system to provide high quality scientific output during nighttime observations. This paper describes the
methods employed at the SMA to optimize engineering development of the telescopes and systems such that the time
available for scientific observations is not compromised. It will also examine some of the tools used to monitor the SMA
during engineering and science observations both at the site and remote facilities.
The eSMA ("expanded SMA") combines the SMA, JCMT and CSO into a single facility, providing enhanced sensitivity
and spatial resolution owing to the increased collecting area at the longest baselines. Until ALMA early
science observing (2011), the eSMA will be the facility capable of the highest angular resolution observations at
345 GHz. The gain in sensitivity and resolution will bring new insights in a variety of fields, such as protoplanetary/
transition disks, high-mass star formation, solar system bodies, nearby and high-z galaxies. Therefore the
eSMA is an important facility to prepare the grounds for ALMA and train scientists in the techniques.
Over the last two years, and especially since November 2006, there has been substantial progress toward
making the eSMA into a working interferometer. In particular, (i) new 345-GHz receivers, that match the
capabilities of the SMA system, were installed at the JCMT and CSO; (ii) numerous tests have been performed
for receiver, correlator and baseline calibrations in order to determine and take into account the effects arising
from the differences between the three types of antennas; (iii) First fringes at 345 GHz were obtained on August
30 2007, and the array has entered the science-verification stage.
We report on the characteristics of the eSMA and its measured performance at 230 GHz and that expected
at 345 GHz. We also present the results of the commissioning and some initial science-verification observations,
including the first absorption measurement of the C/CO ratio in a galaxy at z=0.89, located along the line of sight to the lensed quasar PKS 1830-211, and on the imaging of the vibrationally excited HCN line towards
IRC+10216.
Atmospheric water vapor causes significant undesired phase fluctuations for the SMA interferometer, particularly in its highest frequency observing band of 690 GHz. One proposed solution to this atmospheric effect is to observe simultaneously at two separate frequency bands of 230 and 690 GHz. Although the phase fluctuations have a smaller magnitude at the lower frequency, they can be measured more accurately and on shorter timescales due to the greater sensitivity of the array to celestial point source calibrators at this frequency. In theory, we can measure the atmospheric phase fluctuations in the 230 GHz band, scale them appropriately with frequency, and apply them to the data in 690 band during the post-observation calibration process. The ultimate limit to this atmospheric phase calibration scheme will be set by the instrumental phase stability of the IF and LO systems. We describe the methodology and initial results of the phase stability characterization of the IF and LO systems.
The holography program to measure and set the surfaces of the antennas of the Submillmeter Array (SMA) has been very successful, with the best antenna meeting the stringent 12 μm rms specification. The surfaces of the 6-meter diameter antennas
of the 8 element array have been set to accuracies of 12-25 μm, and are under constant improvement. This allows efficient operation in the 660 GHz band, currently the highest frequency band of observations. The system used to make routine near-field holographic measurements at 232.4 GHz -- the primary method of obtaining surface error maps -- is now fully integrated into the SMA. The measurements are carried out remotely from Cambridge. A sequence of upto 4 rounds of measurements and adjustments is needed to achieve the design specification of 12 μm rms starting typically from 65 μm rms. The last sets of adjustments incorporate corrections for panel flexures, allowed by the 4 points of adjustment for most of the panels, and the high spatial resolution (~ 8 cm) of the surface error maps. Repeat measurements indicate a surface stability time scale of ~ 1 year including antenna transport between stations. Celestial holography to characterize gravitational deformations and careful efficiency measurements to validate the holographic measurements are in progress.
Efficient operation of a submillimeter interferometer requires remote (preferably automated) control of mechanically tuned local oscillators, phase-lock loops, mixers, optics, calibration vanes and cryostats. The present control system for these aspects of the Submillimeter Array (SMA) will be described. Distributed processing forms the underlying architecture. In each antenna cabin, a serial network of up to ten independent 80C196 microcontroller boards attaches to the real-time PowerPC computer (running LynxOS). A multi-threaded, gcc-compiled program on the PowerPC accepts top-level requests via remote procedure calls (RPC), subsequently dispatches tuning commands to the relevant microcontrollers, and regularly reports the system status to optical-fiber-based reflective memory for common access by the telescope monitor and error reporting system. All serial communication occurs asynchronously via encoded, variable-length packets. The microcontrollers respond to the requested commands and queries by accessing non-volatile, rewriteable lookup-tables (when appropriate) and executing embedded software that operates additional electronic devices (DACs, ADCs, etc.). Since various receiver hardware components require linear or rotary motion, each microcontroller also implements a position servo via a one-millisecond interrupt service routine which drives a DC-motor/encoder combination that remains standard across each subsystem.
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