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Table 3

Magnetic field estimates and physical parameters for our sample of LG dwarfs and comparison dwarfs.

Galaxy name Btota SFRb H   i massc Total massd S60 μme vrotf σvg
μG M⊙ yr-1 106M⊙ 106M⊙ mJy km s-1 km s-1
Aquarius  < 4.5 ± 1.2 4.6  ×  10-5 2.7 5.4 139 13 6.6
GR 8  < 3.6 ± 0.9 7.0  ×  10-4 9.6 7.6 20 21 11.0
IC 1613 2.8 ± 0.7 3.0  ×  10-3 58 795 1420 37 8.5
NGC 6822 4.0 ± 1.0 2.1  ×  10-2 140 1640 47 600 51 8.0
WLM  < 3.9 ± 0.9 1.0  ×  10-3 63 150 320 23 8.0
IC 10 9.7 ± 2.0 6.0  ×  10-2 98 1580 31 200 47 8.0
LGS 3  < 4.0 ± 1.0 2.5  ×  10-6 0.2 13 75 18 9.0
SagDIG  < 4.1 ± 1.1 6.7  ×  10-5 8.6 9.6 94 14 7.5
Sextans A  < 3.1 ± 0.8 2.0  ×  10-3 54 395 503 33 8.0
Sextans B  < 2.8 ± 0.6 2.0  ×  10-3 44 885 246 38 18.0
Leo A  < 4.4 ± 1.2 3.2  ×  10-5 7.6 11 90 18 9.3
Pegasus  < 3.7 ± 0.9 3.0  ×  10-4 3.4 58 55 17 8.6
LMC 4.3 ± 1.0 2.6  ×  10-1 500 20 000 8.29  ×  107 72 14.1
SMC 3.2 ± 1.0 4.6  ×  10-2 420 2400 7.45  ×  106 60 25.0
NGC 4449 9.3 ± 2.0 4.7  ×  10-1 2500 70 000 36 000 40 20.0
NGC 1569 14 ± 3.0 3.2  ×  10-1 130 297 54 400 42 21.3

References. 

(a)

this paper and for LMC – Gaensler et al. (2005), SMC – Mao et al. (2008), NGC 4449 – estimation based on 4.86 GHz data (Chyży et al. 2000), NGC 1569 – Kepley et al. (2010);

(b)

Woo et al. (2008), if not available – Hunter & Elmegreen (2004), for Aquarius and LGS 3 estimated from infrared emission;

(c)

Woo et al. (2008); NGC 1569 – Still & Israel (2002); NGC 4449 – Hunter et al. (1999);

(d)

Mateo (1998);

(e)

IRAS (Helou & Walker 1995; Moshir et al. 1990);

(f)

estimated rotational velocity defined as the maximum of rotational velocity and 2 times the galaxy velocity dispersion – Woo et al. (2008), for NGC 4449 – Valdez-Gutiérrez (2002);

(g)

velocity dispersion of ISM estimated from H i: Mateo (1998); LMC – Prevot et al. (1989); SMC – Staveley-Smith et al. (1997); NGC 1569 – Stil & Israel (2002); for NGC 4449 – Hunter et al. (1999).

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