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Table B.4.

Star formation rates (SFRs) and total magnetic field strengths for the galaxy sample. Duplicate entries indicate different regions.

Galaxy SFR [M⊙ yr−1] B [μG] Inclination [°] log M★ [M⊙] sSFR [Gyr−1] ΣSFR [M⊙ yr−1 kpc−2]
M 82* 1.30 × 101a 305 81a 10.01a 1.27 –
NGC 253 3.00q 186 78b 10.47a 0.10 –
NGC 2146 2.00 × 101r 354 63c 10.72a 0.38 –
Equipartition magnetic field from Beck et al. 2019
M 31 3.90 × 10−1b 7.2 77d 10.73a 0.01 4.97 × 10−4
M 33 3.20 × 10−1b 8.15 52e 9.42a 0.12 4.08 × 10−3
M 51 2.70c 15.5 22f 10.47b 0.09 1.66 × 10−2
M 81 5.40 × 10−1b 7.2 59g 10.68a 0.01 1.20 × 10−3
M 83 4.17b 17.5 24h 10.41a 0.16 9.23 × 10−3
NGC 253 (disc) 4.90b 15.0 78b 10.47a 0.17 3.47 × 10−2
NGC 1097 5.01b 13.0 48.6i 10.72a 0.10 6.38 × 10−2
NGC 1365 1.41 × 101b 12.0 40j 10.75a 0.25 2.03 × 10−2
NGC 4254 5.01b 17.5 42k 10.52a 0.15 3.07 × 10−2
NGC 4449 (global disc) 4.30 × 10−1b 13.5 56.2l 9.03a 0.40 1.52 × 10−2
NGC 6946 6.17b 16.0 38m 10.50a 0.20 2.23 × 10−2
IC 342 (disc) 1.91b 13.0 31n 9.81a 0.30 1.99 × 10−3
Equipartition magnetic field from Lacki & Beck 2013
M 82 7.08b 240 81a 10.01a 0.69 3.60 × 101
NGC 253 (core/starburst) 4.90b 230 78b 10.47a 0.17 6.94 × 101
NGC 4945 1.45b 130 75o 10.14a 0.10 1.58 × 100
NGC 1068 3.24 × 101b 72 40p 10.71a 0.63 1.14 × 100
IC 342 (central starburst) 1.91b 110 31n 9.81a 0.30 1.20 × 100
NGC 2146 2.51 × 101b 190 63c 10.72a 0.48 2.96 × 101
NGC 3690 1.55 × 102b 130 – 11.04a 1.41 8.14 × 100
NGC 1808 7.94b 110 57z 10.29a 0.41 2.38 × 100
NGC 3079 7.41b 350 84aa 10.89a 0.10 6.52 × 101
Arp 220 West 1.10 × 102d 750 > 52q 9.30d 55.0 3.50 × 103
Arp 220 East 8.10 × 101d 720 31r 9.30d 40.5 2.58 × 103
Arp 193 8.00 × 101l 550 – 10.45e 2.84 9.94 × 102
Mrk 273 1.39 × 102k 770 78s 10.84e 2.01 1.73 × 103
Equipartition magnetic field from Chyży et al. 2011
IC 1613 2.82 × 10−3b 2.8 58t 8.03a 0.03 8.51 × 10−5
NGC 6822 1.40 × 10−2e 4.0 – 8.00c 0.14 1.01 × 10−3
IC 10 5.00 × 10−2f 9.7 – 7.93c 0.11 1.08 × 10−2
LMC 2.00 × 10−1g 4.3 35.8u 9.18c 0.13 6.82 × 10−3
SMC 5.00 × 10−2h 3.2 – 8.66c 0.58 1.18 × 10−4
NGC 4449 4.27 × 10−1b 9.3 56.2l 9.03a 2.34 1.11 × 10−2
NGC 1569 9.55 × 10−1b 14 63.2v 8.61a 0.40 2.76 × 10−1
Aquarius 1.41 × 10−4n < 4.5 – 6.02a 0.14 2.46 × 10−4
GR 8 2.40 × 10−3m < 3.6 – 6.81c 0.37 1.70 × 10−3
WLM 3.47 × 10−3b < 3.9 74w 7.31a 0.17 3.34 × 10−4
LGS 3 6.00 × 10−6p < 4.0 – 5.98c 0.01 1.47 × 10−5
SagDIG 9.00 × 10−4o < 4.1 – 6.26f 0.50 5.10 × 10−4
Sextans A 6.61 × 10−3b < 3.1 – 8.04a 0.06 5.01 × 10−4
Sextans B 1.91 × 10−3b < 2.8 – 7.37a 0.08 2.18 × 10−4
Leo A 2.95 × 10−4b < 4.4 – 6.45a 0.10 1.44 × 10−4
Pegasus 6.17 × 10−4i < 3.7 – 6.82c 0.09 2.96 × 10−4
Equipartition magnetic field from CHANGES survey
NGC 5775 5.28j 13e 85.8x 10.47g 0.26 9.41 × 10−3
NGC 4217 1.50j 9f 89ab 10.52g 0.046 3.60 × 10−3
NGC 4666 7.30j 12.3g 85ac 10.53g 0.21 8.90 × 10−3
NGC 4631 1.33j 9h 89y 10.05g 0.12 3.10 × 10−3

Notes. SFR tracers used: FUV+WISE4 (hybrid, ∼100 Myr), UV+IR (hybrid), GALEX FUV (∼100 Myr), CMD–SFH (resolved stars), FIR (10–100 Myr), IR/TIR (8–1000 μm), radio 1.4 GHz (non-thermal, ∼100 Myr). Magnetic field strengths are synchrotron equipartition values. Inclinations are in degrees; “—” = not available/meaningful.

SFR methods by superscript:a (Förster Schreiber et al. 2003) IR/TIR (8–1000 μm);b (Leroy et al. 2019) FUV+WISE4 hybrid;c (Eufrasio et al. 2017) UV+IR hybrid;d (Varenius et al. 2016) radio 1.4 GHz;e (Efremova et al. 2011) GALEX FUV;f (Yin et al. 2010) IR/TIR;g (Harris & Zaritsky 2009) CMD-based SFH (HST);h (Wilke et al. 2004) FIR;i (Hunter et al. 2012) GALEX FUV;j (Wiegert et al. 2015) FUV+WISE4 hybrid;k (Cicone et al. 2014) IR/TIR;l (Modica et al. 2012) Radio+IR composite;m (Ott et al. 2012) GALEX FUV;n (Leroy et al. 2021) FUV+WISE4 hybrid;o (Tang et al. 2016) CMD-based SFH (HST);p (Miller et al. 2001) CMD-based SFH (HST/WFPC2);q (Bolatto et al. 2013) IR/TIR;r (Gorski et al. 2018) IR/TIR.

Btot superscripts: a (Lopez-Rodriguez 2023);b (Beck et al. 2019);c (Lacki & Beck 2013);d (Chyży et al. 2011);e (Heald et al. 2022);f (Stein et al. 2020);g (Stein et al. 2019);h (Mora-Partiarroyo et al. 2019).

Inclination superscripts: a (Achtermann & Lacy 1995); b (Pence 1980); c (Della Ceca et al. 1999); d (McConnachie et al. 2005); e (Kam et al. 2015); f (Colombo et al. 2014); g (Karachentsev et al. 2013); h (Tilanus & Allen 1993); i (Lang et al. 2020); j (Jorsater & van Moorsel 1995); k (Phookun et al. 1993); l (Bajaja et al. 1994); m (Boomsma et al. 2008); n (Crosthwaite et al. 2000); o (Henkel et al. 2018); p (Schinnerer et al. 2000); q (Sakamoto et al. 2021); r (Scoville et al. 2015); s (Schmelz et al. 1987); t (Lake & Skillman 1989); u (Olsen & Salyk 2002); v (Sánchez-Cruces et al. 2022); w (Read et al. 2016); x (Irwin 1994); y (Mora-Partiarroyo et al. 2019); z (Dahlem et al. 1990); aa (Israel et al. 1998); ab (Stein et al. 2020); ac (Stein et al. 2019).

log M★ superscripts: a (Leroy et al. 2021); b (Wei et al. 2021); c (McConnachie 2012); d (Sakamoto et al. 1999); e (Vivian et al. 2012); f (Kirby et al. 2017); g (Leroy et al. 2019).

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