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Table 2.

Literature compilation of slopes from resolved molecular KS relations.

Reference Index (N) Scale αCO Fitting method
(M pc−2/(K km s−1))
VERTICO 0.97 ± 0.07 720 pc 4.35 Least Trimmed Squares
Querejeta et al. (2021) 0.97 ± 0.06 (a) ∼1 − 2 kpc 4.35 × Z−1.6 Bisector Ordinary Least Squares (OLS)
Pessa et al. (2021) 1.06 ± 0.01 100 pc 4.35 × Z−1.6 OLS
Sánchez et al. (2021) 0.95 ± 0.21 ∼kpc 4.3 OLS
Ellison et al. (2021a) 0.86 ± 0.01 ∼kpc 4.3 Orthogonal Distance Regression (ODR)
Morselli et al. (2020) 0.80 ± 0.12 500 pc 4.3 OLS
Lin et al. (2019) 1.05 ± 0.01 ∼kpc 4.3 ODR
Usero et al. (2015) 1.01 ± 0.08 ∼1 − 2 kpc 4.4 Total Least Squares
Leroy et al. (2013) 1.00 ± 0.15 ∼kpc 4.35 Monte Carlo fitting
Schruba et al. (2011) 1.0 ± 0.1 ∼0.2–2 kpc 4.35 Bisector OLS
Genzel et al. (2010) 1.17 ± 0.09 > kpc 4.35 (b) Not specified
Daddi et al. (2010) 1.31 ± 0.09 > kpc 3.6 (c) Not specified
Blanc et al. (2009) 0.82 ± 0.05 ∼750 pc 6.0 (d) Monte Carlo fitting
Bigiel et al. (2008) 1.0 ± 0.02 ∼750 pc 4.35 Bisector OLS
Kennicutt (2007) 1.37 ± 0.03 ∼500 pc 6.0 (d) Bivariate Least Squares

Notes. The αCO factors correspond to the CO (1-0) transition.

(a)

Querejeta et al. (2021) report a range of values between 0.90 − 1.43 for the slopes, which is due to the choice of αCO conversion factor.

(b)

Genzel et al. (2010) employ a conversion factor of 4.35 for star-forming galaxies (SFGs) and 1.36 for submillimeter galaxies (SMGs).

(c)

Daddi et al. (2010) use a conversion factor of 3.6 for z = 0.5 − 2.5 normal galaxies, 4.6 for local spirals, and 0.8 for local ULIRGs and distant SMGs.

(d)

Blanc et al. (2009) and Kennicutt (2007) adopt the conversion factor derived in Bloemen et al. (1986), with XCO = 2.8 × 1020 cm−2 (K km s−1)−1.

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