&lt;title&gt;345-GHz facility SIS receiver for the JCMT&lt;/title&gt;

Cunningham, C. T.; Avery, L. W.; Bergeron, C. R.; Claude, S.; Feldman, P. A.; Fletcher, J. R.; Gao, J. R.; Hayward, R. H.; Jegers, J.; Klapwijk, T. M.; MacLeod, J. M.; Matheson, D. N.; Mirza, Akhmad; Redman, R. O.; Stadt, H. van de; Taada, E. R.; Wade, James B.; Yeung, K.

doi:10.1117/12.317416

Cited by 8 publications

(1 citation statement)

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“…In the continuum, SCUBA (1998 -2005) forged the path for SCUBA-2 (2011 to present), and in the heterodyne, the 16-element 345 GHz HARP (2007 to present) replaced the single-element RxB3 receiver. 27 In Figure 7, the left-hand plot shows the cumulative sky coverage of SCUBA and SCUBA-2 is plotted. The coverage is in square degrees of sky and is presented on a logarithmic scale.…”

Section: Sky Coverage With Wide-field Array Instrumentsmentioning

confidence: 99%

Setting the standard: 25 years of operating the JCMT

et al. 2014

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The James Clerk Maxwell Telescope (JCMT) is the largest single-dish submillimetre telescope in the world, and throughout its lifetime the volume and impact of its science output have steadily increased. A key factor for this continuing productivity is an ever-evolving approach to optimising operations, data acquisition, and science product pipelines and archives. The JCMT was one of the first common-user telescopes to adopt flexible scheduling in 2003, and its impact over a decade of observing will be presented. The introduction of an advanced data-reduction pipeline played an integral role, both for fast real-time reduction during observing, and for sciencegrade reduction in support of individual projects, legacy surveys, and the JCMT Science Archive. More recently, these foundations have facilitated the commencement of remote observing in addition to traditional on-site operations to further increase on-sky science time. The contribution of highly-trained and engaged operators, support and technical staff to efficient operations will be described. The long-term returns of this evolution are presented here, noting they were achieved in face of external pressures for leaner operating budgets and reduced staffing levels. In an era when visiting observers are being phased out of many observatories, we argue that maintaining a critical level of observer participation is vital to improving and maintaining scientific productivity and facility longevity.

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Section: Sky Coverage With Wide-field Array Instrumentsmentioning

confidence: 99%

Setting the standard: 25 years of operating the JCMT

et al. 2014

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Star-like activity from a very young ‘isolated planet’

Greaves

Holland

Pound

2003

Monthly Notices of the Royal Astronomical Society

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The discovery of isolated bodies of planetary mass has challenged the paradigm that planets form only as companions to stars. To determine whether ‘isolated planets’, brown dwarfs and stars can have a common origin, we have made deep submillimetre observations of part of the ρ Oph B star formation region. Spectroscopy of the 9‐Jupiter‐mass core Oph B‐11 has revealed carbon monoxide line wings such as those of a protostar. Moreover, the estimated mass of outflowing gas lies on the force versus core‐mass relation for protostars and protobrown dwarfs. This is evidence for a common process that can form any object between planetary and stellar masses in a molecular cloud. In a submillimetre continuum map, six compact cores in ρ Oph B were found to have masses presently below the deuterium‐burning limit, extending the core mass function down to 0.01 M⊙ with the approximate form dN/dM∝M−3/2. If these lowest‐mass cores are not transient and can collapse under gravity, then isolated planets should be very common in ρ Oph in the future, as is the case in the Orion star formation region. In fact, the isolated planetary objects that may form from these cores would outnumber the massive planets that have been found as companions to stars.

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