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![UKT14 imaging of the starburst galaxy M82 at 800 μm (a) and at 450 μm (b). The higher angular resolution afforded by the 450 μm observations revealed the double-peaked central structure for the first time at submillimetre wavelengths. Adapted from Hughes et al. [45,46].](publication/317932866/figure/fig3/AS:1165382954033161@1654860356771/UKT14-imaging-of-the-starburst-galaxy-M82-at-800mm-a-and-at-450mm-b-The-higher.jpeg)
UKT14 imaging of the starburst galaxy M82 at 800 μm (a) and at 450 μm (b). The higher angular resolution afforded by the 450 μm observations revealed the double-peaked central structure for the first time at submillimetre wavelengths. Adapted from Hughes et al. [45,46].
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The James Clerk Maxwell Telescope (JCMT) has been the world's most successful single dish telescope at submillimetre wavelengths since it began operations in 1987. From the pioneering days of single-element photometers and mixers, through the first modest imaging arrays, leading to the state-of-the-art widefield camera SCUBA-2 and the spectrometer...
Citations
... [15]) and the huge impact it has made-and will continue to make-toward our understanding of dust-obscured star formation in the distant (z > 1) Universe. The success of ALMA builds on the huge progress made by earlier long-wavelength telescopes, including (far-)infrared satellites such as the Spitzer [16] and Herschel [17] space telescopes, radio interferometers like the Karl G. Jansky Very Large Array (VLA [18,19]), single-dish submillimetre telescopes such as the James Clerk Maxwell Telescope (JCMT; [20]), the IRAM 30-metre telescope [21], the Atacama Submillimetre Telescope Experiment (ASTE; [22]), the Atacama Pathfinder EXperiment (APEX; [23]), and the South Pole Telescope (SPT; [24]), and earlier (sub-)millimetre interferometers such as the Submillimetre Array (SMA; [25]) and the Plateau de Bure interferometer (PdBI; [26] now succeeded by the NOrthern Extended Millimetre Array, NOEMA). These facilities have already revolutionized our view of high-redshift dusty star formation, from discovering submillimetre galaxies (SMGs) in the first extragalactic surveys with single-dish submillimetre telescopes, to quantifying the relative contribution of dusty star formation over much of cosmic time. ...
The Atacama Large Millimetre/submillimetre Array (ALMA) is currently in the process of transforming our view of star-forming galaxies in the distant (
z
≳
1
) universe. Before ALMA, most of what we knew about dust-obscured star formation in distant galaxies was limited to the brightest submillimetre sources-the so-called submillimetre galaxies (SMGs)-and even the information on those sources was sparse, with resolved (i.e. sub-galactic) observations of the obscured star formation and gas reservoirs typically restricted to the most extreme and/or strongly lensed sources. Starting with the beginning of early science operations in 2011, the last 9 years of ALMA observations have ushered in a new era for studies of high-redshift star formation. With its long baselines, ALMA has allowed observations of distant dust-obscured star formation with angular resolutions comparable to-or even far surpassing-the best current optical telescopes. With its bandwidth and frequency coverage, it has provided an unprecedented look at the associated molecular and atomic gas in these distant galaxies through targeted follow-up and serendipitous detections/blind line scans. Finally, with its leap in sensitivity compared to previous (sub-)millimetre arrays, it has enabled the detection of these powerful dust/gas tracers much further down the luminosity function through both statistical studies of colour/mass-selected galaxy populations and dedicated deep fields. We review the main advances ALMA has helped bring about in our understanding of the dust and gas properties of high-redshift (
z
≳
1
) star-forming galaxies during these first 9 years of its science operations, and we highlight the interesting questions that may be answered by ALMA in the years to come.
Scientists are increasingly relying on astronomical and remote sensing technologies to gain deeper insights into the Earth and the universe. In these fields, the optical spectrum analyzer (OSA) or spectrometer plays a pivotal role. This Review offers a comprehensive overview of the fundamental principles, key parameters, and applications of various branches of traditional OSAs, including prisms, gratings, interferometers, tunable filters, and reconstructive spectrometers. We specifically focus on their latest major applications in astronomy and remote sensing. Additionally, we present a mathematical model of the generalized reconstructive spectrometer and provide a summary of its principles pertaining to spectral mapping, reconstruction, and imaging. Despite its limited aperture and étendue, the reconstructive spectrometer holds great potential for future use in astronomy and remote sensing due to its compact size and exceptional ultrahigh spectral resolution.
The James Clerk Maxwell Telescope (JCMT) is the largest single dish telescope in the world focused on sub-millimeter astronomy - and it remains at the forefront of sub-millimeter discovery space. JCMT continues itspush for higher efficiency and greater science impact with a switch to fully remote operation. This switch toremote operations occurred on November 1st 2019. The switch to remote operations should be recognized to bepart of a decade long process involving incremental changes leading to Extended Observing - observing beyondthe classical night shift - and eventually to full remote operations. The success of Remote Observing is indicatedin the number of productive hours and continued low fault rate from before and after the switch.
