leading to orbits with periods of years. Consequently, continuous HCI
astrometric follow-up over the years is essential to refine our understanding
of these systems and unravel their dynamics. One example of such an approach
and successful results is given for $\eta$ Tel system, in Chapter 3. The
analysis of $\eta$ Tel underscores its significance in achieving a
comprehensive understanding of the system when integrated with extensive
observations spanning nearly two decades.

However, it is crucial to acknowledge an important aspect. The orbital fitting
for widely separated systems lacking thorough orbital coverage from HCI
observations is highly sensitive to the precision of astrometric measurements.
The initial “raw” results obtained for $\eta$ Tel B were deemed physically
implausible due to higher eccentricities obtained for the companion, which
would cause instability and disruption in the closer-in debris disk.
Fortunately, the $\eta$ Tel system’s constraints allowed for a more refined
assessment of possible orbits in this work. It’s worth noting that these
priors may not be achievable for all HCI systems. Thus, the study underscores
the significance of obtaining more precise astrometric measurements to derive
more physically meaningful orbital results.

The importance of robust astrometric measurements for HCI companions becomes
even more pronounced, particularly in the case of multiplanetary systems like
HR 8799, $\beta$ Pic, or even PDS 70 with its two protoplanets. The impact of
dynamical analysis is not limited to orbital properties; it also extends to
crucial aspects such as mass retrieval. In subsection 1.2.4, particularly in
the discussion of remarkable systems observed via HCI, it becomes apparent
that planetary masses, even when derived from various studies, exhibit
considerable uncertainty. The spectrum of masses for each exoplanetary
companion discussed in that section spans both dynamical masses and masses
calculated from luminosity-age evolutionary models. The latter derivation also
highlights the importance of robust photometric retrieval, as was done to
$\eta$ Tel B. In my analysis of the companion, however, I only assumed the
mass derived from the orbit fitting.

####  4.1.3 How can one deduct the formation scenario for multiple systems?

I tentatively answer this question in the specific cases of HBC 494 (Chapter
2) and $\eta$ Tel (Chapter 3) components. The only way to link formation
scenarios from early YSO stages to mature systems is through simulations.
While simulations play a pivotal role in this process, observations alone can
also offer insights.

In environments with specific conditions, discerning a formation scenario
becomes plausible. In the cases of HBC 494 and $\eta$ Tel components, the
proposed scenario suggests rotational disk fragmentation rather than direct
collapsing. This conclusion is drawn from the orbital alignment—quasi-
coplanarity of HBC 494 N and S inferred from similar inclinations and PAs
between the components of the system, and quasi-coplanarity between $\eta$ Tel
B and the debris disk inferred from the inclinations. Therefore, observations
of multiple systems in different stages may serve as a control test,
establishing a connection between (sub)stellar formation and their subsequent
evolution.

Alternative methods of detecting the formation scenario, such as observing
regions of protoplanetary disks susceptible to gravitational instability (GI),
can also provide useful insights. However, discovering the formation scenario
without unveiling the gas/dust dynamics between YSOs (as in the case of HBC
494) or in more evolved systems with (nearly) depleted gas, such as in the
case of $\eta$ Tel, remains challenging.

####  4.1.4 Is it possible to search for satellites orbiting substellar
companions via HCI?

The answer to this question is yes. The deep analysis done for $\eta$ Tel B
surroundings in Chapter 3 was heavily inspired by the notable satellite
candidate unveiled through SPHERE observations around DH Tau B (Lazzoni et
al.,, 2020), yet to be confirmed. Although we pushed to the limits of one of
the best modern high-contrast imagers (SPHERE) till the moment, the non-
detection of a satellite or structure surrounding $\eta$ Tel B does not
completely discard the possibility of an orbiting unresolved source. It just
provides deeper contrasts showing limitations that HCI observations may
overcome to possibly find objects surrounding $\eta$ Tel B. I highlight that
no blind detection will necessarily be proven successful, and $\eta$ Tel B’s
surroundings can be indeed empty. But, as an HCI explorer/researcher, part of
the journey is to sail through seas of the unknown.

To tackle the problem for $\eta$ Tel and other systems but with the same
instrument, better PSF models need to be created, which can be provided by
different observing strategies and cadence of models’ creation. Alternatively,
the next generation of ground-based high-contrast imagers, boasting improved
resolving power and enhanced Adaptive Optics (AO), or space-based high-
contrast imagers like the James Webb Space Telescope, may provide noteworthy
increase in sensitivity and/or resolution in the coming years and decades (see
Currie et al.,, 2023 for an updated review of the next generation instruments
dedicated to HCI). Indeed, the future of HCI is promising.

During the course of my PhD, I, as PI, got three successful observing
proposals using SPHERE proposals to detect satellites/structures around 15
promising substellar companions, including $\eta$ Tel. Using the star-hopping
(a Reference-star differential imaging observing strategy; (Wahhaj et al.,,
2021), I plan to observe these substellar companions, obtaining a quasi-
simultaneous model of the instrumental PSF. This approach involves alternating
between our target and a reference star until the end of the sequence,
minimizing turbulence and improving efficiency in retrieving features. Star-
hopping enhances data quality by providing multiple PSFs compared to standard
IRDIS observations. Additionally, the negative fake companion technique, also
used in Chapter 3, will be applied in post-processing to create models of the
companion from the reference star. Subsequently, these models will be
subtracted from the data, and a following analysis of the residuals will be
performed for further insights. This approach is thus, one example of how HCI
can be performed and optimized for the search of companions’ companions.

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