High-resolution, high-sensitivity, ground-based solar spectropolarimetry with a new fast imaging polarimeter - I. Prototype characterization

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Volume 590 (June 2016)

A&A, 590 (2016) A89

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Table 1

Approximate values of the main, detector-related properties for eight state-of-the-art, full-Stokes, ground-based, solar polarimeters working in the visible part of the spectrum.

Polarimeter	Pixel area	Detector	Frame rate	Ro. noise	ADC	Duty	Mod.	Dual	WB
	[μm²]	area [px²]	[fps]	[e⁻ rms]	[bits]	cycle [%]	freq. [Hz]	beam	channel

IBIS	6.8 × 6.8	1024 × 1024	2.86	20	12	3^a	0.42	Yes	Yes
VIP	16 × 16	512 × 512	29	5.4	16	100	7.25	Yes	Yes
CRISP	16 × 16	1024 × 1024	37	20	12	70	9.25	Yes	Yes
DLSP*	12 × 12	488 × 652	50	50	14	100	12.5	Yes	No
SPINOR*	16 × 16	512 × 1024	100	40	12	100	12.5	Yes	No
FSP	48 × 48	264 × 264	400^b	4.9	14	98.6	100	No	No
FSPII^c	36 × 36	1024 × 1024	400	5	16	95	100	Yes	Optional^d
ZIMPOL-3*^e	22.5 × 90	1252 × 144	1.47	6	16	1.5^a	≥1000	No	No

Notes. Instruments indicated with * operate in spectrograph mode, while the others are used in filtergraph mode. FSP has been tested in both modes. See the text for details.

^(a)

Computed for an exposure time of 10 ms.

^(b)

The FSP camera can achieve a frame rate of 1100 fps using a special readout mode. However, we consider the maximum to be 400 fps because it is the value used during the observations presented here and in Paper II. Such value is also the expected maximum frame rate for FSPII.

^(c)

Currently under development, we listed the expected values. See Sect. 7.

^(d)

The camera noise is less critical in the WB channel due to the higher flux, thus, it can be implemented with e.g. a fast commercial CMOS camera.

^(e)

Even though the CCD55-30 sensor used has frame transfer architecture, the ability of reading while integrating is not implemented resulting in an overhead readout time of about 0.66 s.

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