Performances

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.

 

Last update: 27/02/2017 (Vincent Revéret)

 

Maj : 27/02/2017 (1786)

 

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