Institute of research into the fundamental laws of the Universe

This table sums up the estimated on-sky performance of ArTéMiS (2013-2016) and P-ArTéMiS (2009)

 

Instrument	Central Wavelength (µm)	Instantaneous FOV	Beam FWHM (arcsec)	Pixel size (arcsec)	Per pixel NEFDa (mJy/beam, 1σ, 1s)	Relative imaging speedb
ArTéMiS/APEX	350 (2014) 350 (2016) 450 (2016)	4.1' x 2.3' 4.1' x 2.3' 4.1' x 2.3'	8 8 10	3.9 3.9 3.9	600 1000 600	5 1.8 1.5
P-ArTéMiS/APEX	450 (2009)	1.5' x 1.5'	10	6	2000	0.3
SABOCA	350	1.2'c	8	12	200	1
SHARC-2	350	2.6' x 1.0'	8.5	4.8	1000	1.5
SCUBA-2	450	7.4 'x 7.4'	7.5	6.2	(500)	(10)d
LABOCA	870	11.4'c	18.2	30	120	50

 

(a) NEFD performance per detector pixel measured “outside” the atmosphere (i.e. taking into account the proper background load on the detectors but not the limited transmission of the atmosphere).

 

(b) Imaging speed relative to SABOCA at 350 μm on APEX for mapping cold dust emission. This is defined as the speed at which areas of the sky can be imaged (at full resolution) to a given equivalent surface brightness sensitivity. The wavelength normalization assumes a dust temperature Td = 15 K and a dust emissivity index β = 1.5 (local Universe), equivalent to Td = 48 K, β = 1.5 at a redshift z = 2.2 typical of submillimeter galaxies (high-z Universe).

 

(c) The field of views of SABOCA and LABOCA are not instantaneously sampled: observing a minimum of 16 positions is required to obtain a fully-sampled image.

(d) Under PWV ≤ 0.6 mm which occurs ∼ 20% of the winter time at Mauna Kea.