Do spiral arms enhance star formation efficiency? | Astronomy & Astrophysics (A&A)

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Volume 687 (July 2024)

A&A, 687 (2024) A293

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Table 1.

Arm/interarm contrast measurements.

	Σ_⋆	Σ_mol	Σ_SFR	SFE
Nominal contrasts	$1 . 28_{- 0.26}^{+ 0.49}$ $1.28_{-0.26}^{+0.49}$	$2 . 22_{- 0.96}^{+ 2.19}$ $2.22_{-0.96}^{+2.19}$	$2 . 56_{- 1.61}^{+ 4.59}$ $2.56_{-1.61}^{+4.59}$	$1 . 16_{- 0.58}^{+ 1.23}$ $1.16_{-0.58}^{+1.23}$

Contrasts from MUSE	$1 . 21_{- 0.29}^{+ 0.46}$ $1.21_{-0.29}^{+0.46}$	$2 . 28_{- 0.96}^{+ 2.12}$ $2.28_{-0.96}^{+2.12}$	$2 . 72_{- 1.57}^{+ 4.55}$ $2.72_{-1.57}^{+4.55}$	$1 . 21_{- 0.54}^{+ 0.93}$ $1.21_{-0.54}^{+0.93}$

Low resolution (1.5 kpc)	$1 . 15_{- 0.21}^{+ 0.48}$ $1.15_{-0.21}^{+0.48}$	$1 . 49_{- 0.49}^{+ 1.35}$ $1.49_{-0.49}^{+1.35}$	$1 . 50_{- 0.57}^{+ 2.20}$ $1.50_{-0.57}^{+2.20}$	$1 . 04_{- 0.31}^{+ 0.56}$ $1.04_{-0.31}^{+0.56}$

Narrow masks	$1 . 28_{- 0.24}^{+ 0.53}$ $1.28_{-0.24}^{+0.53}$	$2 . 53_{- 1.02}^{+ 2.83}$ $2.53_{-1.02}^{+2.83}$	$3 . 11_{- 1.97}^{+ 5.45}$ $3.11_{-1.97}^{+5.45}$	$1 . 21_{- 0.59}^{+ 1.23}$ $1.21_{-0.59}^{+1.23}$

Thinner radial bins (250 pc)	$1 . 27_{- 0.25}^{+ 0.47}$ $1.27_{-0.25}^{+0.47}$	$2 . 25_{- 1.10}^{+ 2.48}$ $2.25_{-1.10}^{+2.48}$	$2 . 54_{- 1.56}^{+ 4.92}$ $2.54_{-1.56}^{+4.92}$	$1 . 15_{- 0.61}^{+ 1.33}$ $1.15_{-0.61}^{+1.33}$

Wider radial bins (1000 pc)	$1 . 27_{- 0.29}^{+ 0.49}$ $1.27_{-0.29}^{+0.49}$	$2 . 14_{- 0.81}^{+ 2.48}$ $2.14_{-0.81}^{+2.48}$	$2 . 34_{- 1.34}^{+ 4.56}$ $2.34_{-1.34}^{+4.56}$	$1 . 14_{- 0.51}^{+ 1.09}$ $1.14_{-0.51}^{+1.09}$

Perpendicular bins along spiral arms	$1 . 34_{- 0.32}^{+ 0.68}$ $1.34_{-0.32}^{+0.68}$	$2 . 31_{- 1.13}^{+ 2.94}$ $2.31_{-1.13}^{+2.94}$	$2 . 64_{- 1.74}^{+ 7.30}$ $2.64_{-1.74}^{+7.30}$	$1 . 16_{- 0.63}^{+ 1.62}$ $1.16_{-0.63}^{+1.62}$

Perpendicular bins with adjacent interarm	$1 . 14_{- 0.18}^{+ 0.27}$ $1.14_{-0.18}^{+0.27}$	$2 . 19_{- 1.24}^{+ 3.37}$ $2.19_{-1.24}^{+3.37}$	$2 . 76_{- 1.78}^{+ 6.13}$ $2.76_{-1.78}^{+6.13}$	$1 . 17_{- 0.73}^{+ 1.91}$ $1.17_{-0.73}^{+1.91}$

Nominal – Grand design spirals	$1 . 34_{- 0.33}^{+ 0.57}$ $1.34_{-0.33}^{+0.57}$	$2 . 73_{- 1.36}^{+ 3.06}$ $2.73_{-1.36}^{+3.06}$	$3 . 12_{- 2.08}^{+ 6.74}$ $3.12_{-2.08}^{+6.74}$	$1 . 16_{- 0.57}^{+ 1.56}$ $1.16_{-0.57}^{+1.56}$
Nominal – Rest of spirals	$1 . 23_{- 0.19}^{+ 0.30}$ $1.23_{-0.19}^{+0.30}$	$1 . 90_{- 0.78}^{+ 1.04}$ $1.90_{-0.78}^{+1.04}$	$2 . 00_{- 1.14}^{+ 3.15}$ $2.00_{-1.14}^{+3.15}$	$1 . 17_{- 0.58}^{+ 1.06}$ $1.17_{-0.58}^{+1.06}$

Nominal – High M_⋆	$1 . 34_{- 0.34}^{+ 0.49}$ $1.34_{-0.34}^{+0.49}$	$2 . 70_{- 1.34}^{+ 3.09}$ $2.70_{-1.34}^{+3.09}$	$3 . 14_{- 2.14}^{+ 6.91}$ $3.14_{-2.14}^{+6.91}$	$1 . 17_{- 0.61}^{+ 1.51}$ $1.17_{-0.61}^{+1.51}$
Nominal – Low M_⋆	$1 . 24_{- 0.19}^{+ 0.39}$ $1.24_{-0.19}^{+0.39}$	$1 . 80_{- 0.68}^{+ 1.24}$ $1.80_{-0.68}^{+1.24}$	$1 . 85_{- 0.95}^{+ 3.18}$ $1.85_{-0.95}^{+3.18}$	$1 . 13_{- 0.54}^{+ 1.21}$ $1.13_{-0.54}^{+1.21}$

Nominal – High SFR	$1 . 33_{- 0.30}^{+ 0.51}$ $1.33_{-0.30}^{+0.51}$	$2 . 46_{- 1.15}^{+ 2.73}$ $2.46_{-1.15}^{+2.73}$	$3 . 07_{- 2.17}^{+ 5.28}$ $3.07_{-2.17}^{+5.28}$	$1 . 18_{- 0.60}^{+ 1.54}$ $1.18_{-0.60}^{+1.54}$
Nominal – Low SFR	$1 . 19_{- 0.20}^{+ 0.44}$ $1.19_{-0.20}^{+0.44}$	$2 . 02_{- 0.90}^{+ 2.00}$ $2.02_{-0.90}^{+2.00}$	$2 . 13_{- 1.17}^{+ 3.99}$ $2.13_{-1.17}^{+3.99}$	$1 . 11_{- 0.53}^{+ 1.00}$ $1.11_{-0.53}^{+1.00}$

Nominal – High ΔMS	$1 . 41_{- 0.34}^{+ 0.48}$ $1.41_{-0.34}^{+0.48}$	$2 . 32_{- 1.02}^{+ 2.92}$ $2.32_{-1.02}^{+2.92}$	$3 . 05_{- 2.10}^{+ 5.33}$ $3.05_{-2.10}^{+5.33}$	$1 . 23_{- 0.64}^{+ 1.57}$ $1.23_{-0.64}^{+1.57}$
Nominal – Low ΔMS	$1 . 17_{- 0.19}^{+ 0.39}$ $1.17_{-0.19}^{+0.39}$	$2 . 06_{- 0.93}^{+ 1.99}$ $2.06_{-0.93}^{+1.99}$	$2 . 16_{- 1.25}^{+ 3.84}$ $2.16_{-1.25}^{+3.84}$	$1 . 09_{- 0.53}^{+ 0.85}$ $1.09_{-0.53}^{+0.85}$

Notes. Arm/interarm contrasts in the surface density of stellar mass, molecular gas, star formation rates, and SFE (median and 16th–84th percentile range, measured on galactocentric rings of 500 pc width). The nominal contrasts rely on the masks from Querejeta et al. (2021), while the narrow masks refer to those introduced here in Sect. 2.6.2. The two alternative sampling schemes based on perpendicular bins are explained in Appendix F (Fig. F.1). Low and high M_⋆ refer to the bottom or top 50% of stellar masses in the sample (threshold 3.4 × 10¹⁰ M_⊙); analogously for SFRs (threshold 2.3 M_⊙ yr⁻¹) and ΔMS (threshold 0.234 dex).

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