2147, from ∆m = 0 at the diffraction limit of 0.06′′ to ∆m = 3.7 at 0.15′′.

The contrast increases more gradually past 0.15′′, reaching ∆m = 5 by 1′′.

TOI-6019 was observed on December 24, 2022, with the Speckle Polarimeter (SPP), a facility instrument on the 2.5-m telescope at the Caucasian Observatory of the Sternberg Astronomical Institute (SAI) of Lomonosov Moscow State University.

A low-noise CMOS detector, Hamamatsu ORCA–quest (Strakhov et al. 2023) was used.

TOI-2147 was observed on October 27, 2020, with a previous, EMCCD–based version of the instrument (Safonov et al. 2017).

In both cases, the atmospheric dispersion compensator was active, which allowed using the Ic band.

The respective angular resolution was 0.083′′.

The pixel scale was 20.6 mas/pixel.

The power spectrum of TOI-6019 was estimated from 5200 frames with 23 ms exposure time.

For TOI-2147, 4000 frames with 60 ms exposure were accumulated.

The long–exposure atmospheric seeing was 0.65′′ and 1.05′′, respectively, for TOI-6019 and TOI-2147.

For TOI-6019, we detected a stellar companion at a separation 977 ± 7 mas and a position angle PA=285.5 ± 0.5◦, with a magnitude difference is 6.6 ± 0.3 mag.

The detection limits are ∆Ic = 4.2 and 7.2 mag at distances 0.25 and 1.0′′ from the star, respectively.

For TOI-2147, we did not detect any stellar companions; the detection limits are ∆Ic = 4.5 and 5.8 mag at distances 0.25 and 1.0′′ from the star, respectively.
2.4.

High-resolution spectroscopy 2.4.1.

TRES We obtained reconnaissance spectra with the Tillinghast Reflector Echelle Spectrograph (TRES, Furész et al. (2008)) on the 1.5 m Tillinghast Reflector telescope at the Fred Lawrence Whipple Observatory (FLWO) on Mount Hopkins in Arizona.

TRES is a fiber-fed, optical spectrograph with a resolving power of R = 44,000 covering a wavelength range between 390 and 910 nm.

TOI-2147 was observed twice: on November 19, 2020 and December 2, 2020.

TOI-6019 was observed on December 24, 2022 and January 1, 2023.

All the spectra were visually inspected to check for composite spectra and then a multi-order spectral analysis was performed, following procedures outlined in Buchhave et al. (2010) and Quinn et al. (2012).

We found no signs of composite spectra or larger RV variations indicative of an eclipsing binary.

The differences in the RVs obtained at opposite quadratures are ∼52 m/s and ∼95 m/s with errors ∼35 m/s and ∼22 m/s for TOI-2147 and TOI-6019, respectively.
2.4.2.

MaHPS We confirmed the planetary nature of the two candidates and measured their masses using the Manfred Hirt Planet finder Spectrograph (MaHPS, Kellermann et al. 2015, 2016) installed at the 2.1 m telescope of the Wendelstein Observatory in the Bavarian Alps in Germany.

This spectrograph consists of the stabilized, fiber-fed, high-resolution (R ∼60, 000), optical (385 − 885 nm), echelle spectrograph FOCES (Pfeiffer et al. 1998), and a Menlo Systems Astro Frequency Comb as a wavelength calibration source.

TOI-2147 was observed between the 26th of January, 2023, and the 14th of December 2025, collecting a total of 136 spectra on 57 nights.

For TOI-6019, we collected 93 spectra (38 nights) between the 14th of July 2024 and the 18th of November 2025.

With V-band magnitudes of 11.1 and 10.8, both stars are close Article number, page 4 of 14
to the limit for precise RV work with MaHPS (Ehrhardt et al. 2024).