The Submillimeter Array

By P. Ho, J. Moran, K. Lo. Astronomical Telescopes and Instrumentation, 2004

515 citations recorded by the source corpus.

The Submillimeter Array, a collaborative project of the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, has begun operation on Mauna Kea in Hawaii. The array comprises a total of eight 6 m telescopes, which will cover the frequency range of 180-900 GHz. All eight telescopes have been deployed and are operational. First scientific results utilizing the three receiver bands at 230, 345, and 690 GHz have been obtained and are presented in the accompanying Letters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/afaf19e21d3d3309144dfebc29824f00b74a4b56

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Citations in the corpus

• FRAGMENTATION AT THE EARLIEST PHASE OF MASSIVE STAR FORMATION (2009, background): “A detailed description of the SMA is given in Ho et al. (2004).”
• Luminous Infrared Galaxies with the Submillimeter Array. I. Survey Overview and the Central Gas to Dust Ratio (2008, methodology): “Observations with the Submillimeter Array (SMA: Ho et al. 2004) were obtained be- tween 2005 May 16 and 2007 May 2.”
• DISPERSION OF MAGNETIC FIELDS IN MOLECULAR CLOUDS. II. (2008, methodology): “The SMA receiver system has two sidebands, each with a bandwidth of ∼ 2 GHz.”
• A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE (2009, methodology): “The GM Aur disk was observed with the 8-element (each with a 6 m diameter) Submillimeter Array (SMA; Ho et al. 2004) in the very extended (68-509m baselines) and compact (16-70m baselines) configurations on 2005 November 5 and 26, respectively.”
• A millimeter Continuum Size–Luminosity Relationship for Protoplanetary Disks (2017, methodology): “Sample A sample of 50 nearby (d ≤ 200 pc) disk targets was collated from the archived catalog of ∼340 GHz (880µm) continuum measurements made with the Submillimeter Array (SMA; Ho et al. 2004), since the 2004 start of science operations.”
• THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, methodology): “TW Hya was observed at 345GHz (870 µm) with the Submillimeter Array (SMA; Ho et al. 2004) on 8 occasions in 2006-2010 in the compact (C), extended (E), and very extended (V) array configurations, providing baseline lengths of 16-70m, 28-226m, and 68-509m, respectively.”
• Imaging the Disk around TW Hydrae with the Submillimeter Array (2004, background): “The Submillimeter Array (SMA)1 , now nearing completion on Mauna Kea, is an ideal instrument for making these observations (Ho et al. 2004).”
• Hierarchical fragmentation and differential star formation in the Galactic ‘Snake’: infrared dark cloud G11.11−0.12 (2014, background): “The Submillimeter Array2 (SMA; Ho et al. 2004) was pointed towards G11.”
• THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, unknown): “We observed 52 new targets with the Submillimeter Array (SMA; Ho et al. 2004) in its compact configuration (8-70m baselines) over six tracks from 2012 November to 2013 February.”
• EVIDENCE FOR DUST CLEARING THROUGH RESOLVED SUBMILLIMETER IMAGING (2008, methodology): “Dust emission measurements of LkHα 330 were acquired with the Submillimeter Array (SMA)1 (Ho et al. 2004) on 2006 November 11 and 19 using the very extended configuration of seven of the 6 meter diameter antennas, which provided baselines ranging in length from 80 to 590 meters.”
• PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, methodology): “A sample of 9 disks was observed with the very extended (V) configuration of the Submillimeter Array interferometer (SMA; Ho et al. 2004) at Mauna Kea, Hawaii.”
• RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, methodology): “We have constructed a sample of 12 nearby transition disks with high angular resolution 880µm continuum data using new and archival observations with the SMA interferometer (Ho et al. 2004).”
• GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, methodology): “First, we give results from a large, multi-semester program with the Submillimeter Array (SMA; Ho et al. 2004) that comprises over 160 hours of on-source integration time and provides sub-arcsecond, spatially-resolved 880µm images of 30 Herschel lens candidates (some of the SMA data 35…”
• PROSAC: A Submillimeter Array Survey of Low-Mass Protostars. I. Overview of Program: Envelopes, Disks, Outflows, and Hot Cores (2007, background): “479 (Ho et al. 2004), however, a new window has opened up, allowing for detailed studies of the radial variations of both the physical /dynamical and chemical structure of protostellar cores.”
• Evidence for a Population of High-Redshift Submillimeter Galaxies from Interferometric Imaging (2007, methodology): “In this work, we present high–resolution 890 µm interferometric imaging by the Submillimeter Array (SMA: Ho et al. 2004) of a flux–limited sample of sources selected at 1.1 mm by the AzTEC Camera (Wilson et al. 2007) on the JCMT, in a survey of a section of the COSMOS field (Scott et al. 2007).”
• PROSAC: a submillimeter array survey of low-mass protostars - II. The mass evolution of envelopes, disks, and stars from the class 0 through I stages (2009, methodology): “Our data consist of line and continuum observations of 10 Class 0 sources and 9 Class I sources observed as part of the Submillimeter Array (SMA; Ho et al. 2004)1 key project, Protostellar Submillimeter Array Campaign (PROSAC; Jørgensen et al. 2007a).”
• High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, methodology): “Interferometric observations of 24 young star/disk systems were conducted with the Submillimeter Array (SMA; Ho et al. 2004) on the summit of Mauna Kea, Hawaii.”