The VMC survey - L. Type II Cepheids in the Magellanic Clouds: Period–luminosity relations in the near-infrared bands

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Volume 685 (May 2024)

A&A, 685 (2024) A41

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Table 14.

Coefficients of the PL and PW relations for T2Cs with slope calculated in the LMC and zero point calibrated with Galactic T2Cs through photometric parallaxes (top) and ABL (bottom).

Relation	α	σ_α	β_LMC	σ_{β_LMC}	n_T2Cs	μ_LMC	σ_{μ_LMC}	μ_SMC	σ_{μ_SMC}
	(mag)	(mag)	(mag dex⁻¹)	(mag dex⁻¹)		(mag)	(mag)	(mag)	(mag)
Photometric parallax

PLJ	−0.859	0.059	−2.156	0.024	21	18.52	0.06	19.06	0.07
PLK_s	−1.124	0.037	−2.348	0.019	21	18.53	0.04	19.05	0.04
PWG	−1.041	0.019	−2.436	0.022	1121	18.49	0.02	–	–
PWVK_s	−1.244	0.034	−2.475	0.017	21	18.53	0.04 ^(a)	19.01	0.04
PWJK_s	−1.291	0.032	−2.501	0.016	21	18.54	0.03	19.00	0.04

ABL

PLJ	−0.876	0.063	−2.156	0.024	21	18.54	0.06	19.08	0.08
PLK_s	−1.139	0.036	−2.348	0.019	21	18.55	0.04	19.07	0.04
PWG	−1.085	0.017	−2.436	0.022	1118	18.53	0.04	–	–
PWVK_s	−1.260	0.029	−2.475	0.017	21	18.54	0.03	19.02	0.04
PWJK_s	−1.325	0.026	−2.501	0.016	21	18.58	0.03	19.04	0.06

Notes. We note that the relations are: M_λ, 0 = α + β log P for PL(λ); $W_{λ_{1}, λ_{2}}^{0} = α + β$ $W_{\lambda_1,\lambda_2}^0 = \alpha + \beta$ log P for the PW(λ₁, λ₂).

^(a)

Same result as in Wielgórski et al. (2022). We note that the μ_SMC based on the PWG relation is not listed because in this case, the β_SMC (see Table 8) is not compatible with the β_LMC.

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