Beam Size, Shape and Efficiencies for the ATNF Mopra Radio Telescope at 86–115 GHz

By Ned Ladd, C. Purcell, T. Wong, S. Robertson. Publications Astronomical Society of Australia, 2005

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In Astronomy and Astrophysics

Citations in the corpus

THE MAGELLANIC MOPRA ASSESSMENT (MAGMA). I. THE MOLECULAR CLOUD POPULATION OF THE LARGE MAGELLANIC CLOUD (2011, methodology): “The efficiencies we have assumed for CO are listed in Table 1, and represent the “extended beam” efficiencyηxb discussed by Ladd et al. (2005), which includes the effect of coupling to the inner error beam for sources larger than∼2′.”
FILAMENTARY ACCRETION FLOWS IN THE EMBEDDED SERPENS SOUTH PROTOCLUSTER (2013, methodology): “We then created uniformly gridded spectral cubes for each waveband using Gridzilla7, using a final pixel size of 15′′; Mopra’s spatial resolution is ∼40′′ at 3 mm (Ladd et al 2005).”
THE “NESSIE” NEBULA: CLUSTER FORMATION IN A FILAMENTARY INFRARED DARK CLOUD (2009, background): “To convert to main-beam brightness temperatures, one should divide the antenna temperatures by the main-beam efficiency of 0.49 (Ladd et al. 2005).”
The RMS survey : Galactic distribution of massive star formation (2013, methodology): “The reduced spectra were converted to the telescope-independent main-beam temperature scale (Tmb), assuming a main-beam efficiency (ηmb) of 0.65 (Urquhart et al. 2010b), 0.60 and 0.55 (Ladd et al. 2005) for the NH3, CS and CO observations, respectively.”
Spectral imaging of the Central Molecular Zone in multiple 3-mm molecular lines (2011, methodology): “However, the Mopra beam has substantial sidelobes (Ladd et al. 2005) so that the extended beam efficiency, appropriate for the extended emission we are mostlystudying here, is quite different (0.65 at 86 GHz).”
A Herschel [C ii] Galactic plane survey - I. The global distribution of ISM gas components (2013, methodology): “To convert from antenna to main-beam temperature scale, we used a main-beam efficiency of 0.42 (Ladd et al. 2005).”
Global collapse of molecular clouds as a formation mechanism for the most massive stars (2013, methodology): “The angular resolution of these 1 http://irsa.ipac.caltech.edu/data/SPITZER/GLIMPSE 3mm Mopra observation is ∼ 37′′ and the rms noise is 0.1 K on the T∗A scale (∼ 0.2 K on the Tmb scale because the beam efficiency factor is ∼ 2 at 93 GHz on Mopra - Ladd et al. 2005).”