Hot Rocks Survey I: A possible shallow eclipse for LHS 1478 b

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Volume 695 (March 2025)

A&A, 695 (2025) A171

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Table 3

Inter-model comparison for the light-curve fitting.

Pipeline	n_clip	Model	BIC	$χ_{r e d}^{2}$ ${\chi _{red}^2}$	RMS	f_p/f_*
	100	L	–9561	1.44	714	138 ±53
`Frida`		EL	–9554	1.44	714	128 ± 56
		GP	–9546	1.43	713	110 ± 63

	150	L	–8984	1.44	713	138 ±52
		EL	–8977	1.44	714	124 ± 57
		GP	–8969	1.43	713	111 ±65

	200	L	–8400	1.45	715	139 ±53

	100	L	–9442	1.51	774	125 ± 56
`Eureka!`		LPOS	–9303	1.47	762	112 ± 59
		GP	–9325	1.64	806	110 ± 67

	150	L	–8877	1.50	772	124 ± 56
		LPOS	–8891	1.46	759	107 ± 59
		GP	–8852	1.62	801	109 ± 70

	200	L	–8307	1.51	772	127 ± 60
		LPOS	–8327	1.45	756	107 ± 59

`juliet^(*)`	150	EL	–8880	1.35	784	$101_{- 59}^{+ 80}$ ${101_{ - 59}^{ + 80}}$
		LGP	–8880	1.34	782	$107_{- 61}^{+ 69}$ ${107_{ - 61}^{ + 69}}$
		EGP	–8874	1.34	782	$106_{- 61}^{+ 69}$ $106_{ - 61}^{ + 69}$

Notes. We fit the observation 1 light curve obtained through different data reduction pipelines with their respective fitting routines. The different functions explored to model the systematics are: L, a first order polynomial; EL, a first order polynomial with an exponential term; GP, a Gaussian process (squared exponential kernel for Frida and Matern32 kernel for Eureka!; LPOS, and a first order polynomial with centroid position decorrelation; LGP, a first order polynomial and a GP (Matern32 kernel); EGP, an exponential and a GP (Matern32 kernel). The BIC is computed using BIC= –2 · log(L) + k · log(N), where log(L) is the maximum log-likelihood for each fit, k is the number of free parameters and N is the number of integrations in the light curve. The final f_p/f_* value quoted in the paper and in Figure 2 is highlighted in pink. nclip are the integrations discarded at the start of the light curve.^(*) This fit was performed on the light curve reduced independently with the transitspectroscopy pipeline.

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