J/A+A/712/A147 RV measurements of TOI-1272 and TOI-1694 (Mancini+, 2026)
The GAPS Programme at TNG LXXIV. A reanalysis of the planetary systems TOI-1272
and TOI-1694 with HARPS-N and retraction of the planetary interpretation of
TOI-1272 c.
Mancini L., Naponiello L., Damasso M., Biazzo K., Bonomo A.S., Lanza A.F.,
Lillo-Box J., Pinamonti M., Cosentino R., Bignamini A., Boschin W.,
Fiorenzano A., Giacobbe P., Manni F., Rainer M., Scandariato G., Sozzetti A.
<Astron. Astrophys. 712, A147 (2026)>
=2026A&A...712A.147M 2026A&A...712A.147M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, K-type ; Radial velocities ; Optical
Keywords: method: data analysis - techniques: photometry -
techniques: radial velocities - stars: individual: TOI-1694 -
stars: individual: TOI-1272
Abstract:
Hot Neptunes are close-in exoplanets that occupy a sparsely populated
region of parameter space known as the "hot-Neptune desert". Their
presence in this extreme environment is puzzling as it implies a
complex history involving intense stellar radiation, atmospheric loss,
and unique migration patterns, different from Neptunes at larger
orbital periods.
We are running an observational programme conceived to enlarge the
number of close-in Neptune-sized planets, with well-measured physical
and orbital parameters, with the aim of contributing to obtaining a
statistically significant sample needed to clarify what the formation
and migration pathways of this class of exoplanets are.
We used currently available TESS photometry, along with new (HARPS-N)
and archival (HIRES) high-precision radial-velocity measurements, to
review the main properties of the planetary systems TOI-1272 and
TOI-1694 by means of joint-fit analyses that, in the case of TOI-1272,
included Gaussian-process regressions for carefully modelling stellar
activity.
Our final estimates of the parameters of the two systems are
consistent with previous measurements but have smaller uncertainties.
We identified the radial-velocity variation of TOI-1272 found in the
HIRES data as stellar activity rather than planetary in nature and,
therefore, rejected the non-transiting planet TOI-1272c. This opens up
the possibility that TOI-1272b's eccentricity is the result of
high-eccentricity migration. The larger number of data at our disposal
also allowed us to point out that both TOI-1694b and TOI-1694c move on
slightly eccentric orbits. The current orbital architecture of
TOI-1694 suggests a history of migration driven by both disc and
dynamical interactions.
Description:
Radial-velocity measurements and corresponding activity indices of the
stars TOI-1272 and TOI-1694. Data were obtained with
Objects:
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RA (2000) DE Designation(s)
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13 16 47.19 +49 51 39.7 TOI-1272 = 2MASS J13164717+4951399
06 30 59.57 +66 21 38.4 TOI-1694 = 2MASS J06305955+6621384
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
toi-1272.dat 111 94 Radial velocities of TOI-1272
toi-1694.dat 111 89 Radial velocities of TOI-1694
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Byte-by-byte Description of file: toi-1272.dat toi-1694.dat
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Bytes Format Units Label Explanations
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1- 13 F13.5 d BJD Barycentric Julian date for the midpoint of
observation, TDB
15- 18 I4 s Texp Exposure time
20- 28 F9.2 m/s RV Radial velocity
30- 34 F5.2 m/s e_RV Uncertainty of the radial velocity measurement
36- 40 F5.2 --- S/N Signal to noise ratio of the measurement
42- 47 F6.4 m/s FWHM FWHM of the cross-correlation function
49- 54 F6.4 m/s e_FWHM Uncertainty of the FWHM
56- 61 F6.3 m/s Contrast Contrast of the cross-correlation function
63- 67 F5.3 m/s e_Contrast Uncertainty of the Contrast
69- 75 F7.4 m/s BIS Bisector span of the cross-correlation
function
77- 82 F6.4 m/s e_BIS Uncertainty of the bisector span
84- 89 F6.4 --- Halpha Halpha index
90- 96 F7.4 --- e_Halpha Uncertainty of the Halpha index
97-104 F8.4 [-] log(R'HK) log(R'_HK) index
106-111 F6.4 [-] e_log(R'HK) Error of the log(R'_HK) index
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Acknowledgements:
Luigi Mancini, lmancini(at)roma2.infn.it
License: CC-BY-4.0
(End) Patricia Vannier [CDS] 01-Jul-2026