Circumstellar emission of Cepheids across the instability strip: Mid-infrared observations with VLTI/MATISSE

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Volume 694 (February 2025)

A&A, 694 (2025) A101

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Table 3

Cepheid ephemeris, fluxes, and angular diameters of the star sample.

Star	P₀ (day)	T₀ (MJD)	$\dot{P}$ $\[\dot{P}\]$ (s/yr)	ϕ_MATISSE	$θ_{LD}^{SPIPS} (m a s)$ $\[\theta_{\text {LD }}^{\text {SPIPS}}(\mathrm{mas})\]$	θ_UD(L)(mas)	F_L (Jy)	F_N (Jy)
X Sgr	7.012	56926.825	+0.29 ± 0.01	0.04	1.35 ± 0.03	1.33 ± 0.03	20.1 ± 6.9	4.1 ± 1.2
U Aql	7.023	56935.587	+0.17 ± 0.04	0.88	0.73 ± 0.03	0.71 ± 0.03	7.7 ± 2.7	1.1 ± 0.3
η Aql	7.177	56975.775	+0.25 ± 0.01	0.58	1.80 ± 0.04	1.78 ± 0.04	46.7 ± 6.8	7.5 ± 1.8
β Dor	9.842	50275.770	+0.85 ± 0.11	0.15	1.87 ± 0.04	1.85 ± 0.04	51.9 ± 13.1	7.6 ± 2.3
ζ Gem	10.149	48708.059	−3.12 ± 0.04	0.60	1.61 ± 0.03	1.59 ± 0.03	36.9 ± 2.2	5.1 ± 0.5
TT Aql	13.754	48310.561	−0.70 ± 0.11	0.03	0.76 ± 0.03	0.74 ± 0.03	8.1 ± 0.2	1.4 ± 0.4
T Mon	27.029	43783.986	+14.49 ± 0.78	0.03	0.87 ± 0.04	0.85 ± 0.04	11.7 ± 2.9	2.0 ± 0.6
U Car	38.791	56886.190	+97.85 ± 2.03	0.22	0.83 ± 0.03	0.82 ± 0.03	12.8 ± 0.5	2.6 ± 1.2

Notes. For X Sgr, U Aql, η Aql, and U Car, we chose the pulsation period P₀ and the reference epoch at maximum light T₀ from Gaia DR3. For β Dor, ζ Gem, TT Aql, and T Mon, we adopted the SPIPS values. We used an independent rate of the period change $\dot{P}$ $\[\dot{P}\]$ derived by Csörnyei et al. (2022), except for β Dor, for which we adopted the SPIPS value. These data were used to derive the pulsation phase at the epoch of the MATISSE observations ϕ_MATISSE, and the corresponding LD diameter $θ_{L D}^{S P I P S}$ $\[\theta_{\mathrm{LD}}^{\mathrm{SPIPS}}\]$ of each star. The UD diameter in the L band was derived using the tables from Claret & Bloemen (2011).

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