# The Ariel Target List: The Impact of TESS and the Potential for
Characterising Multiple Planets Within a System

Billy Edwards AIM, CEA, CNRS, Université Paris-Saclay, Université de Paris,
F-91191 Gif-sur-Yvette, France  Department of Physics and Astronomy,
University College London, Gower Street, London, WC1E 6BT, UK  Giovanna
Tinetti Department of Physics and Astronomy, University College London, Gower
Street, London, WC1E 6BT, UK

(Received December 28, 2021; Revised March 25, 2022; Accepted April 28, 2022)

###### Abstract

The ESA Ariel mission has been adopted for launch in 2029 and will conduct a
survey of around one thousand exoplanetary atmospheres during its primary
mission life. By providing homogeneous datasets, with a high SNR and wide
wavelength coverage, Ariel will unveil the atmospheric demographics of these
far-away worlds, helping to constrain planet formation and evolution processes
on a galactic scale. Ariel seeks to undertake a statistical survey of a
diverse population of planets and, therefore, the sample of planets from which
this selection can be made is of the utmost importance. While many suitable
targets have already been found, hundreds more will be discovered before the
mission is operational. Previous studies have used predictions of exoplanet
detections to forecast the available planet population by the launch date of
Ariel, with the most recent noting that the Transiting Exoplanet Survey
Satellite (TESS) alone should provide over a thousand potential targets. In
this work, we consider the planet candidates found to date by TESS to show
that, with the addition of already confirmed planets, Ariel will already have
a more than sufficient sample to choose its target list from once these
candidates are validated. We showcase the breadth of this population as well
as exploring, for the first time, the ability of Ariel to characterise
multiple planets within a single system. Comparative planetology of worlds
orbiting the same star, as well as across the wider population, will
undoubtedly revolutionise our understanding of planet formation and evolution.

††journal: AJ††thanks: Paris Region Fellow

##  1 Introduction

Ariel has been selected as the next ESA medium-class science mission and is
due for launch in 2029 (Tinetti et al., 2021). During its 4-year mission,
Ariel will observe 1000 exoplanet atmospheres, aiming to provide a diverse
catalogue of homogeneous datasets which allow for the large-scale demographics
of exoplanet atmospheres to be uncovered for the first time. The planets
studied will span a wide range of planetary and stellar parameters, allowing
Ariel to probe all corners of the exoplanet population, from temperate
terrestrials to ultra-hot Jupiters. Data from Ariel will reveal the chemical
fingerprints of gases and condensates in the planets’ atmospheres, including
the elemental composition and thermal structure.

Ariel will simultaneously provide spectral coverage from 0.5-7.8 $\mu m$, with
photometric bands covering the visible and spectrometers providing data at
wavelengths longer than 1.1 $\mu m$. The mission objective of Ariel is to
uncover the chemical diversity of exoplanet atmospheres, with the bulk of the
mission being dedicated to a survey constructed of three Tiers where the depth
to which the planet is studied increases with each tier.

The list of potential targets for Ariel has been rapidly evolving over recent
years and will continue to do so over the period until its launch. The
evolution is driven by the plethora of planet detection surveys, each bringing
unique parameter spaces to the fore and thus providing a multifarious
population from which to select atmospheric targets. Ground-based surveys
(e.g. Bakos et al., 2004; Pollacco et al., 2006; Wheatley et al., 2018) have
been instrumental in proving the success of the transit detection method,
providing a multitude of hot gaseous planets as well as cooler, rocky worlds,
while the Convection, Rotation and planetary Transits (CoRoT, Auvergne et al.,
2009) mission was the first to detect exoplanets from space. The Kepler
mission (Borucki et al., 2010) has provided the majority of known transiting
planets to date, with the extended mission bringing yet more with a focus on
brighter stars along the ecliptic (Howell et al., 2014). Finally, the
Transiting Exoplanet Survey Satellite (TESS, Ricker et al., 2014) has been
operational since July 2018 and has been predicted to find thousands of
planets (Sullivan et al., 2015; Barclay et al., 2018), many of which will be
suitable for atmospheric characterisation with Ariel and other facilities.

Here, we build upon other works which have explored the potential target list
for Ariel (Zingales et al., 2018; Edwards et al., 2019a). The most recent of
these, Edwards et al. (2019a), hereafter E19, was conducted as the TESS
mission launched and utilised the predictions of Barclay et al. (2018),
hereafter B18, in addition to the planets known at the time, to projected the
expected numbers of planets that could be studied during the mission’s primary
life. In the summer of 2020, TESS completed its primary 2-year mission and
moved into an extended operations, resurveying parts of the northern and
southern hemisphere, as well as covering the ecliptic plane. An updated study
of the TESS planet yield was published Barclay (2020), hereafter B20,
suggesting that the extended mission would discover hundreds of additional
worlds. Over the last few years, thousands of potential planet signals have
been found within TESS data (Guerrero et al., 2021) with 205 planets having
been subsequently confirmed to date111NASA Exoplanet Archive, accessed 26th
April 2022.

In this work, we compare the current TESS TOIs to the detections predicted by
B18 and B20, with a specific focus on those which are suitable for study with
Ariel. We explore not only the number of TOIs Ariel could study, but the
variety in their properties. In E19, a focus was placed upon Ariel’s
capabilities to study smaller, potential rocky worlds which could host
secondary atmospheres. Here we focus instead on the systems in which there are
multiple planets which are suitable for study with Ariel, highlighting the
mission’s great potential for comparative planetology within a single
planetary system as well as across the vast exoplanet population. Finally, we
discuss the efforts that are required to ensure a robust list of potential
target is chosen for observation with Ariel.

##  2 Construction of Catalogues

###  2.1 Currently-Known Planets and Those Predicted to be Found By TESS

The catalogue of currently-known targets was built in an identical fashion to
that of E19 although it was updated to include the detections that have
occurred in the intervening years. As described in E19, the catalogue is built
mainly from the NASA Exoplanet
Archive222https://exoplanetarchive.ipac.caltech.edu/ (Akeson et al., 2013).
Since E19, the NASA Exoplanet Archive has been updated to include a “Planetary
Systems Composite Data” table. The table ensures that as many planetary and
stellar properties as possible are reported for a system which can mean the
data is gathered from multiple studies. Both tables were accessed on 26th
April 2022. Where certain parameters were not available, we made further
attempts to infer them. These included inferring the stellar mass, radius or
temperature from Pecaut & Mamajek
(2013)333http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt.
If the mass had been measured in multiple studies, we took the value from the
latest work, assuming that to be the most accurate. If it had not been
measured, we estimated it using the relation from Chen & Kipping (2017). We
removed any planets which did not have reported uncertainties on the planet
radius. Having inferred as many parameters as possible, we also removed any
planets which did not have the information required by Ariel instrument
simulator, ArielRad (Mugnai et al., 2020). For the host star, these are the
star radius, temperature, log(g) and distance. For the planet, the radius,
mass, temperature and transit duration are needed. Having removed those with
insufficient information, the input population consisted of 3488 planets.

Similarly, the B18 sample was the same as that considered in E19, although the
phantom inflated planets that were identified within the sample by Mayorga &
Thorngren (2018) were removed, reducing the number of predicted planets to
4231. The yield from B20 was not considered in E19 but we include those
planets here as an additional means of bench-marking the performance of TESS.
These planets were treated in an identical way to those from B18 and the
performance of Ariel was modelled for 7603 of them in this study.

###  2.2 TESS Objects of Interest

We accessed the latest TOIs from both the NASA Exoplanet Archive and the NASA
ExoFOP-TESS site444https://tev.mit.edu/data/, splicing them together using the
TOI ID. Both lists were accessed on 26th April 2022. The TOI list contains
objects which have been flagged as false positives, such as eclipsing
binaries, or as previously known planets (Guerrero et al., 2021). We used the
“TOI Disposition” column to determine the current status of a target. We
filtered out known planets which were denoted by “KP”. However, we found that,
in the “Public Comments” column, references to know systems were still made.
Therefore, having made all comments lower case, we searched this column for
the following keywords to identify known planets: ‘corot’, ‘hat’, ‘hd’, ‘hip’,
‘gj’, ‘kelt’, ‘kepler’, ‘k2’, ‘known’, ‘lhs’, ‘mascara’, ‘ogle’, ‘qatar’
‘tres’, ‘wasp’ and ‘xo’. Furthermore, we searched this same column for ‘eb’ to
filter out those identified as eclipsing binaries as well as comments which
contained the phrase ‘v-shaped’. To avoid double counting planets in our
analysis, we removed those labelled “CP” in the “TOI Disposition” clumn as
these are denoting TOIs which have since gone on to be confirmed planets from
the TESS mission. Removing all those that were flagged by the above process,
resulted in 4192 remaining TOIs from the initial sample of 5637. Our
acceptance rate is consistent with the $\sim$25% false positive rate found by
Guerrero et al. (2021) for the prime mission.

As mentioned, ArielRad, the instrument simulator used to model the performance
of Ariel’s photometers and spectrometers (Mugnai et al., 2020), requires a
number of input parameters. Some of these were not given in the TOI list and
so these were inferred using the methods of E19. For instance, the planet mass
is obviously not given in the TOI list as it is only known after further
follow-up has been conducted. Hence, we used Forecaster (Chen & Kipping, 2017)
to estimate the mass. Additionally, we note that an estimate of the planet’s
temperature is given within the TOI list but we recalculate it to ensure
compatibility between these targets and the predicted targets from B18. Having
followed this procedure, 3697 TOIs had enough information to be fed into
ArielRad. From this point forward, we refer to these as TESS Planet Candidates
(TPCs).

##  3 Potential Candidates for Atmospheric Study with Ariel

Ariel aims to undertake a meticulous chemical survey, searching for trends in
atmospheric composition and unveiling the demographics of exoplanet
atmospheres. Planning of observations with Ariel is based around a tiered
approach which we briefly summarise here. Initially $\sim$1000 planets will be
studied with the resulting spectra providing a basic characterisation of the
atmosphere (presence of clouds, colour-colour diagrams etc.). From this
sample, around half will be studied in more depth, with additional time
dedicated to them to build up the SNR of the spectra. These Tier 2
observations will provide a more detailed view of the atmosphere, constraining
the trace gases, metallicity and elemental ratios of hydrogen-dominated
envelopes. The third Tier of Ariel will be devoted to studying the best
targets for atmospheric characterisation multiple times in search of temporal
variations in chemistry or cloud coverage. Finally, a fourth tier will provide
time to undertake observations which don’t neatly fit into the original three
tier process. Examples could include phase-curves or detailed studies of
smaller planets which may host secondary atmospheres.

Figure 1: Examples of the spectral binning used to define the science
requirements for Tier 1 (top) and 2 (bottom) of the Ariel survey. The
reduction in resolution for these Tiers is a result of post-processing and so,
for reference, the native spectral resolution at which all observations are
taken is also shown. The error bars were computed using ArielRad and the
atmospheric forward models computed using TauREx 3 (Al-Refaie et al., 2021b).
The top panel is a free chemistry model while the TauREx GGChem plugin has
been used for the bottom panel (Woitke et al., 2018; Al-Refaie et al., 2021a).
Random Gaussian scatter has been added to each spectra based on the magnitude
of the spectral uncertainties. Ariel’s instruments operate simultaneously and,
therefore, the complete wavelength coverage (0.5-7.8 $\mu$m) is provided in a
single observation.

The suitability of a planet for study with Ariel in each of these tiers is
defined by a set of science requirements. While the requirements for Tier 3
are set at the native resolution of Ariel’s instruments, Tiers 1 and 2 are set
on data with a reduced resolution. The data quality requirement for each Tier
is that, at the defined resolution, the expected SNR on the atmosphere of the
planet is greater than 7. Examples of the data for Tier 1 and 2 are shown in
Figure 1. While the ESA science requirements are based upon the resolutions
show in Figure 1, the datasets could be analysed with different spectral
binning if required as the reduction in resolution is accomplished during
post-processing. More detail on the observation strategy of Ariel can be found
in a number of studies (e.g. Tinetti et al., 2018, 2021).

In this work, the performance of the Ariel mission has been modelled using
ArielRad (Mugnai et al., 2020). ArielRad is an adapted version of the
instrument independent radiometric simulator
ExoRad555https://github.com/ExObsSim/ExoRad2-public and accounts for a wide
variety of noise sources including those arising from the detector (readout,
gain, dark current), the photon noise from the target star, zodiacal
background, instrument emission, and jitter noise. For each target, the
expected uncertainty on as single transit or eclipse observation is determined
at the native resolution of the instruments. It is assumed that Ariel observes
for 2.5 times the length of the transit or eclipse. These uncertainties are
then utilised to calculate the required number of observations to meet the
SNR$>$7 requirement in each tier. The post-processing steps include reducing
the resolution to those used for the Tier 1 and 2 requirements, generating
error bars which can be used for more detailed analyses (e.g. spectral
retrievals).

###  3.1 The Mission Candidate Sample

Having derived a list of targets which have all the parameters necessary for
an ArielRad simulation, we use this efficient simulator to determine the
number of observations required to reach the required signal-to-noise ratio in
each tier. The boundary of suitability will not be concrete, with some planets
being assessed on a case-by-case basis, but, to broadly understand the entire
population, we set upper limits of 5 observations to achieve Tier 1 goals and
20 for Tier 2. These limits were also used in E19. We use these requirements
to construct the Mission Candidate Sample (MCS), a list of all potential
targets for Ariel. Any planets which meet these requirements are henceforth
considered suitable for observation with Ariel.

We compare the numbers of potential Tier 1 and 2 targets from B18 and B20 to
the TPCs in Figure 2, showing the known population as well. From this we see
that the number of TPCs that are suitable for study with Ariel currently lies
between with the predictions of B18 and B20. The situation is as one would
expect given that TESS has finished its prime mission but has not yet
completed its first extended mission. Analysis of 2241 TPCs from the prime
mission by Guerrero et al. (2021) suggested the yield of targets which were
suitable for atmospheric characterisation had not been as high as expected and
our results suggest similar finding but that the extended mission has
increased the number beyond the original yield prediction. However, we note
that many TPCs may yet turn out to be false positives and the assumptions we
have taken, particularly on parameters such as the mass, will also affect the
final number of suitable targets.

The large number of TPCs is impressive given the effects stray light from the
Earth and Moon have had on TESS. Excessive contamination by these sources
caused Sectors 14-16 and 24-26 to be shifted northwards by around 30∘, leaving
a portion of the sky unobserved during the prime mission (Guerrero et al.,
2021). The gap this shift caused can be seen when comparing the sky locations
of the Tier 1 targets, which is shown in Figure 3. Nevertheless, during the
first three years of operation TESS has undoubtedly provided an enormous
number of planet candidates which could be suitable for atmospheric
characterisation. Additionally, the extended mission is covering the portions
of the sky missed previously due to stray light as well as the ecliptic plane,
leading to further detections, some of which may be suitable for study with
Ariel.

Figure 2: Planets suitable for study in Tier 1 (top) and Tier 2 (bottom). For
lines marked by “Known + B18” and “Known + B20”, we do not include any
confirmed detections made by TESS. “Known” and “Known + TPCs” both include
confirmed planets from the TESS mission.

Figure 3: Sky locations of potential Ariel Tier 1 targets. Top panel:
currently-known planets, second panel: Tier 1 targets from the predicted
targets of B18, third panel: Tier 1 targets from the predicted targets of B20,
bottom: potential Tier 1 targets from the current TPCs. The sky coverage of
Ariel, which offers large continuous viewing zones at the ecliptic poles, was
determined using the Terminus code (Edwards & Stotesbury, 2021). Ariel’s
continuous viewing zones have been heavily studied by the TESS mission,
leading to many candidates within them.

Currently, around 500 confirmed planets would meet Ariel’s Tier 1 requirements
in 5 observations or fewer and, based on our assumptions, over 1700 TPCs could
as well. Hence, even if half of these TPCs are false positives, it is likely
there will be a copious number of planets to choose between for study with
Ariel. Therefore, we now focus on the variety of targets that could be
studied. The histograms in Figures 4 and 5 highlight the range of Tier 1
targets that are available from the currently known population and the current
TPCs. When combining these together, it is appears that a wide parameter space
could be probed by Ariel. While the planets studied will generally have a
short period ($<$ 20 days), their temperatures will vary from 200 to 4000 K
and span radii from Earth-sized to super-inflated Jupiters. The stellar hosts
primarily have temperature between 4000 K and 7000 K, but cooler dwarfs, as
well as A-type stars, are also present. We note that some targets around
cooler or fainter stars have been deemed unsuitable for study due to the
brightness requirements of Ariel’s FGS channels which facilitate pointing of
the spacecraft. Whether these requirements were reached was assessed by using
ArielRad and those that failed to reach them are not included in our analysis.

In Tier 1, Ariel will attempt to study planets in every category of a five
dimensional parameter space. They will be classified by the planet’s radius,
density and temperature, as well as the host star’s temperature and
metallicity. However, as the TPCs do not have measured masses, and their
stellar metallicities are not listed in the TPC catalogue, we have to overlook
these parameters for now. Therefore, we classified the potential Tier 1
targets in a three dimensional parameter space using the classifications shown
in Table 1, with the bounds for the stellar types being set by using the
values from Pecaut & Mamajek
(2013)666http://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt.

Star Type | Temperature Bounds |  | Planet Type | Radius Bounds |  | Climate | Temperature Bounds
---|---|---|---|---|---|---|---
M | Ts $\leq$ 3890 K |  | Earth/Super-Earth | Rp $<$ 1.8 R⊕ |  | Warm | TP $\leq$500 K
K | 3890 K $<$ Ts $\leq$5330 K |  | Sub-Neptune | 1.8 R⊕ $<$ Rp $\leq$ 3.5 R⊕ |  | Very Warm | 500 K $<$ TP $\leq$ 1000 K
G | 5330 K $<$ Ts $\leq$ 5960 K |  | Neptune | 3.5 R⊕ $<$ Rp $\leq$ 6 R⊕ |  | Hot | 1000 K $<$ T${}_{\rm P}\leq$ 1500 K
F | 5960 K $<$ T${}_{\rm s}\leq$7300 K |  | Jupiter | 6 R⊕ $<$ Rp $\leq$ 16 R⊕ |  | Very Hot | 1500 K $<$ T${}_{\rm P}\leq$ 2500 K
A | 7300 K $<$ Ts |  | Inflated Jupiter | 16 R⊕ $<$ Rp $\leq$ 26 R⊕ |  | Ultra Hot | 2500 K $<$ T${}_{\rm P}\leq$ 4000 K
Table 1: Bounds used to categorise host stars in Figures 6 and 7.

Figure 4: Histograms of the properties of the planets within the potential
Ariel Tier 1 Catalogue. While the period of planets that can be studied are
general constraint to $<20$ days, in terms of planet temperature and radii the
targets will be highly diverse.

Figure 5: Histograms of the properties of the host stars within the potential
Ariel Tier 1 Catalogue. Ariel will probe planets around a range of stellar
types, out to around 1000 pc from the Earth. The host star could be as faint
as T${}_{\rm mag}\sim$14.

Figure 6: Temperature and radius distribution of known planets, including
those found by TESS, (left) and these known planets in addition to the current
TPCs (right), for M (top), K (middle) and G (bottom) stars, that are suitable
for Tier 1 study with Ariel.

Figure 7: Temperature and radius distribution of known planets, including
those found by TESS, (left) and these known planets in addition to the current
TPCs (right), for F (top) and A (bottom) stars, that are suitable for Tier 1
study with Ariel.

Figure 8: Temperature and radius distribution of known planets, including
those found by TESS, (left) and these known planets in addition to the current
TPCs (right), for worlds with radii smaller than 3 R⊕ that are suitable for
Tier 1 study with Ariel. Figure 9: An example Mission Reference Sample (MRS)
derived from currently-known planets and the TESS Planet Candidates (TPCs).
The observing campaign shown would require 21,958 hours of telescope time,
equivalent to 88.5% of Ariel’s available science time in the prime mission
life ($\sim$24,800 hours). We note that around 10% of time is expected to be
left for Tier 4 observations and complementary science. Figure 10: Sky
locations of the example MRS, indicated by stars, with the brightest 35
million stars from the Gaia database (Gaia Collaboration et al., 2016, 2018)
plotted in the background. The host stars are spread across the sky, but with
a lower density in the galactic plane. Transit searches here are harder due to
the dilution of sources, but this will also be true of Ariel observations and
thus targets in this plane may be less advantageous anyway.

In Figure 6 and 7, the distribution of the potential Ariel targets are shown.
In each plot, the left column shows the variety of planets available today,
which includes those confirmed to date using data from TESS. In the right
column, the known population has been combined with the TPCs. While we already
known of a diverse sample of planets suitable for atmospheric
characterisation, these plots highlight the impact TESS will have in
increasing this variety yet further still. Furthermore, TESS will provide
additional planets within each section of the parameter space to allow for
more through comparisons between planets with similar bulk characteristics. We
note that, in the right hand side of the Figures, false positives may still be
present and the removal of these may reduce the overall diversity. For
instance, signals indicative of planets with large radii on short periods have
a relatively high false positive rate and, therefore, the potential expansion
of the parameter space at the top right of each figure may not be real.

In E19, we explored the ability of Ariel to study smaller planets. As these
planets may have atmospheres which are not hydrogen-dominated (e.g. Owen & Wu,
2017; Fulton & Petigura, 2018), or indeed no atmosphere at all, it is likely
that a specialised observing plan will need to be devised to ensure they are
studied in an efficient and thorough manner. While we do not go into depth on
this here, in Figure 8 we show the radius versus temperature distribution of
small planets ($<3R_{\oplus}$), highlighting the large number of potential
targets as well as their diversity. Numerous parameters could affect the
capability for a small planet to retain it’s primordial envelope, including
the stellar irradiation and planet mass (e.g. Owen & Wu, 2017; Fulton &
Petigura, 2018; Rogers et al., 2021), and thus a wide range of targets will
need to be studied if we are to understand which planets retain hydrogen-
dominated envelopes, and which don’t, as well as the pathways to secondary
atmospheres. Hubble observations of Sub-Neptunes have had mixed levels of
success in detecting atmospheres (e.g. Kreidberg et al., 2014; Benneke et al.,
2019; Tsiaras et al., 2019; Guilluy et al., 2021) but spectroscopic
observations of rocky planets have yet to yield convincing atmospheric
detections (e.g. de Wit et al., 2018; Edwards et al., 2021; Libby-Roberts et
al., 2021; Mugnai et al., 2021b). The current lack of detailed atmospheric
constraints for these worlds has increased the interest of the community in
them. As such, a number of smaller planets will be studied as part of JWST’s
GTO and GO Cycle 1 programmes, with over half the planets observed being
smaller than 2.5 R⊕. JWST will provide data with a wider spectral coverage and
higher SNR than Hubble and, hopefully, these observations, and further
proposals in future cycles, will provide the first detections of atmospheres
around small, rocky worlds. Results from these studies will be crucial inputs
into Ariel’s strategy for observing smaller planets and the mission’s
potential for studying these worlds will be the subject of a focused
manuscript in the future.

###  3.2 An Example Mission Reference Sample

As in E19, we took the MCS, the list of potential Ariel targets, and created
an example Mission Reference Sample (MRS), a selection of planets that could
be observed in the prime mission life. In-keeping with previous works, we
adopted the approach of aiming to choose a very diverse, and as complete as
possible, combination of star/planet parameters while minimising the number of
repeated observations by selecting the planets around the brightest stars.
Again we classified planets using the bounds in Table 1 and ensure that, where
possible, at least 2 planets within each star type/planet temperature/planet
radius bin are contained within the MRS. We force 1000 planets to be observed
in Tier 1 as well as 50 in Tier 3, each of which is assumed to be revisited 5
times in search of variability. We then fill the remainder of the mission time
with Tier 2 observations, finding that, with the TOIs included in the sample,
600 planets could be observed in Tier 2 across the prime mission life under
these conditions. We note that nominally Ariel will have 10% of time its
science time dedicated to Tier 4 targets and complementary science programmes.

The distribution of the planetary radii and temperature of this example MRS is
shown in Figure 9, while the sky locations are given in Figure 10. Ariel
target stars will be spread across the entire sky, hopefully helping to
alleviate scheduling constraints (Morales et al., 2015, 2022). The MRS derived
here requires 21,944 hours, which is 88.5% of Ariel’s available science time
in the prime mission life ($\sim$24,800 hours), leaving sufficient time for
these other programmes. However, we also note that much of this Tier 4 time
may be dedicated to phase curves. Naturally such observations would acquire
transits and eclipses of the planets being studied and the planets which are
suitable for phase curves studies with Ariel are also likely to be excellent
targets for atmospheric spectroscopy in Tiers 1, 2 or 3. Therefore, this
overlap means that primary science can be acquired from these Tier 4
observations, blurring the distinction between the two programmes and
potentially opening up more time to conduct additional observations. In any
case, the outcome of this study in clear: assuming a large portion of the
planet candidates within the TOIs are true planets, will we already have a
surplus of targets for Ariel and the mission will be capable of studying 1000
atmospheres during the prime mission life.

The Ariel mission should carry enough fuel for a mission extension to be
possible. Hence we explored the impact on the number of planets which could be
studied if the additional operating time were granted. We find that a two year
extension would allow for 1400 planets to be studied in Tier 1 and 700 in Tier
2 across the entire mission life. Again we assumed roughly 10% of time was
dedicated to additional science observations. Such an extension would be an
increase of 57% in terms of science time and, from the currently derived
target list, would yield increases of 40% in the numbers of Tier 1 and 2
targets studied.

Figure 11: Known (left) and TPC (right) systems that host at least two worlds
that could be studied in Tier 1 with Ariel. Colours indicate the suitability
of characterisation (white: not suitable, light blue: Tier 1, dark blue: Tier
2) while the size of the circle reflects the planets radius. Those below the
dotted line were listed as having been discovered by TESS in the NASA
Exoplanet Archive.

##  4 Systems which contain Multiple Planets for Atmospheric Study with Ariel

While in general Ariel seeks to conduct comparative planetology across
hundreds of targets, comparing the atmospheres of multiple planets within a
single system could offer unique insights into their formation and evolution.
Therefore, we isolated systems which had multiple planets that could be
studied by Ariel, finding 31 known systems as shown in Figure 11. Within the
TPCs, 17 such systems were found but we note that many multi-planet systems
have already been confirmed with TESS (e.g. Huang et al., 2020; Günther et
al., 2019; Dawson et al., 2019; Leleu et al., 2021) and thus are included
within the known count. The large number of multiple planet systems that have
been validated highlights their value as laboratories to study formation
processes and, as TESS continues to provide additional data, one hopes further
multi-planet systems will be found.

We note there is disagreement between Lacedelli et al. (2021) and Weiss et al.
(2021) about the number of planets in the TOI-561 system (4 and 3 claimed,
respectively). As the NASA Archive lists all of these worlds, our methodology
of creating a catalogue leads to 5 planets being listed for the system. For a
study looking across the whole population, such an error should not affect the
overall statistics. Planets b and c are consistently recovered by both studies
and so the third planet found by Weiss et al. (2021) is the only controversial
world that is suitable for characterisation with Ariel within this system (the
outer planets found by Lacedelli et al. (2021) are deemed to take too much
time to be studied based on the limits imposed here). Nevertheless, this
example provides a warning that must be heeded as Ariel approaches launch and
as the target list is further refined. The change in parameters between the
TOI list and the confirmed catalogue is expected given the significant work
that goes into confirming the planetary nature of the signal and
characterising the system. However, it again provides an indication that one
must be careful in the conclusions drawn from the TPC list and only once these
systems are confirmed will we truly know there suitability for atmospheric
studies with Ariel.

In light of this, we provide a first look at Ariel’s capabilities to study
multiple planets within one system by taking a confirmed system as an example:
TOI-1130. The TOI-1130 system contains a warm Jupiter (R = 1.5RJ) on an 8.4
day orbit but, strangely, also contains an Neptune-sized world on a 4.1-day
orbit (Huang et al., 2020). Systems with hot Jupiters rarely host other short
period planets (Steffen et al., 2012), with any companions generally being at
much larger orbital distances (Schlaufman & Winn, 2016). Given the brightness
of TOI-1130 (K=8.351), these planets are ideal targets for atmospheric
characterisation with Ariel and constraining their chemistry may provide
indicators as to their formation history.

Models suggest that lower mass planets are incapable of accreting substantial
gaseous envelopes, instead preferentially accreting higher-metallicity solids
(e.g. Mordasini et al., 2012; Fortney et al., 2013). As the primordial
elemental abundances of giant, gaseous planets are expected to remain largely
unchanged, measuring these can provide insights into the formation mechanisms
of these planets. Studies of methane content of the gaseous planets within our
own Solar System are in agreement with the predictions of the core-accretion
scenario. By comparing the bulk characteristics of exoplanets to structural
evolution models, there is evidence that a exoplanet mass-metallicity trend is
likely but could differ for that seen in our own system (Thorngren et al.,
2016).

Furthermore, elemental ratios are expected to a key indicator of where in the
disc the planet formed. By constraining these ratios, such as that of carbon
to oxygen, one may be able to uncover the formation and migration mechanisms
governing the planet’s evolution to its current state (e.g. Öberg et al.,
2011; Turrini et al., 2018; Shibata et al., 2020). Shorter period planets,
which will form the bulk of the population studied by Ariel, are likely to
have formed far further out than they currently orbit, having migrated inwards
over time (e.g. Lin & Papaloizou, 1986; Tanaka et al., 2002). The C/O ratio
could be a tracer of whether the planet formed beyond the snow line; if the
planet was originally outside the snow line it should have preferentially
accreted carbon-rich gases leading to a high C/O ratio. Alternatively, if the
planet accreted most of its material from inside the snow line, it should be
more oxygen-rich and thus have a lower C/O ratio. However, modelling by
Turrini et al. (2021) suggests that other elemental ratios, such as S/O or
N/O, may provide a better opportunity to constrain where in the disc a planet
formed. Nevertheless, as the C/O ratio is the most widely discussed ratio we
stick to using it for this study.

We explored Ariel’s capability to constrain these two key parameters, the C/O
ratio and the metallicity, for the TOI-1130 system. We used the trend derived
in Thorngren et al. (2016) to model the metallicities of TOI-1130 b and c.
While Thorngren et al. (2016) found a trend between an exoplanet’s mass and
its metallicity, a stronger correlation was found when comparing the mass to
the planet-to-star metallicity ratio. Hence we utilised their best fit model
to this, which was

$\frac{Z_{P}}{Z_{S}}=9.7M_{P}^{-0.45}$ (1)

where the metallicity of the star is determined from

$Z_{S}=0.014\times 10^{[Fe/H]}$ (2)

While TOI-1130 appears to be a metal-rich star, the Fe/H has not yet been
measured, with current observations suggesting Fe/H $>$ 0.2 for the star Huang
et al. (2020). As in our case the value is a multiplicative term applied to
both planets, we use Fe/H = 0.2. Furthermore, we note that the mass of
TOI-1130 b has not yet been constrained, with only a 3$\sigma$ upper limit of
0.17 MJ placed upon it. Hence we utilised the relation from Chen & Kipping
(2017) to estimate the mass as 0.0407 MJ (12.935 M⊕). We also note that the
relation from Thorngren et al. (2016) did not extend to such small masses.
Therefore, the trend within the TOI-1130 system, and within the population of
Sub-Neptunes, may not reflect the one modelled here. However, we seek here
only to present a proof of concept and leave a detailed study for future work.

| TOI-1130
---|---
TS [K] | 4250†
RS [R⊙] | 0.684†
Fe/H | 0.2∗
| TOI-1130 b | TOI-1130 c
TP [K] | 780 | 650
RP [RJ] | 0.326† | 1.5†
MP [MJ] | 0.0407∗ | 0.974†
C/O | 0.5 | 0.85
log(met) | -0.041 | -0.662
Cloud Pressure [Pa] | 1e3 | 1e3
No. Transits | 20 | 3
Table 2: Input parameters for the retrieval study of the TOI-1130 system.
†denotes parameters taken from Huang et al. (2020). ∗denotes basic parameters
that have not been yet measured and have been selected based on assumptions
described in the text.

Figure 12: Constraints on the main carbon and oxygen bearing species from our
retrievals for TOI-1130 b (red) and c (blue). The solid lines show the best-
fit model while the 1$\sigma$ uncertainties are highlighted by the filled
regions. The input values are given by the dotted lines. While the H2O and CO
abundances are well constrained, the CO2 profile is less so, as is CH4 in the
upper atmosphere. Increasing the number of observations might improve our
knowledge of these molecules and thus elemental ratios such as C/O. Ariel
probes from the cloud-deck at 1e3 Pa up to roughly 1e1. Figure 13: Posterior
distributions for our retrievals of TOI-1130 b and c. For the assumed
atmospheric metallicities and C/O ratios, Ariel would be able to distinguish
between them and thus uncover a mass-metallicity trend in the system as well
as inferring differences in their formation.

As well as modelling differing planet metallicities, we imposed different C/O
ratios for the planets. We based these on the modelling in Turrini et al.
(2018), assuming a ratio of 0.5 and 0.85 for planets b and c respectively. We
then modelled the spectra for these planets assuming equilibrium chemistry
using the ACE package (Agúndez et al., 2012; Venot & Agúndez, 2015) which is a
plugin for the TauREx 3.1 retrieval code (Al-Refaie et al., 2021b, a). We
assumed isothermal temperature-pressure profiles and introduced a grey cloud
deck at 5e2 Pa (0.005 Bar) and 1e3 Pa (0.01 Bar) for TOI-1130 b and c,
respectively, to produce spectral features in the HST WFC3 band which are
equivalent in size to those seen in similar planets studied with this
instrument (e.g. Guilluy et al., 2021). We generated the error bars using
ArielRad, assuming 20 observations for TOI-1130 b and 3 for TOI-1130 c, and
our inputs are summarised in Table 2.

We find that, in the case presented here, the atmospheric constituents of
TOI-1130 b and c would generally be well constrained as shown in Figures 13
and 12. We find that the metallicities of these planets could be distinguished
(Figure 13), providing evidence for a mass-metallicity trend in the system if
one should exist. Additionally, for the assumed C/O ratios, the solutions can
be distinguished but less convincing than the metallicities. From Figure 12 we
note that CH4 and CO2 are less well constrained than H2O and CO. Modelling a
greater number of observations of TOI-1130 c in particular might help further
distinguish the C/O ratios. However, we leave an in-depth analysis of this to
a future detailed study of comparative planetology within multi-planet systems
with Ariel, aiming here to only motivate the idea with a simple example and
set forth the best systems with which to conduct such a study.

##  5 Discussion, Conclusions and Future Work

The Ariel target list, in the forms of an MCS and MRS, will continue to evolve
as new systems are found, the instrument performance is refined, and the
observing strategy is adjusted to maximise the science yield of the mission.
We have shown here that TESS has already provided a plethora of planet
candidates which are suitable for study with Ariel and, when combined with the
currently-known population, its success will mean that the MCS could contain
2000 planets.

Figure 14: The transit spectroscopic metric, used by the TESS Atmospheric
Characterisation Working Group (ACWG) to classify the suitability of
atmospheres for characterisation (TSM, Kempton et al., 2018), for TESS Planet
Candidates (TPCs) that are potential targets for Ariel’s Tier 1 and Tier 2
surveys. In Tier 1, Ariel will be capable of observing planets with far lower
TSMs that the statistical sample considered in Kempton et al. (2018)
(TSM$>$90), with some planets which have TSM$\sim$40 still being considered
suitable for the mission. We note that the metric was designed only for JWST
NIRISS and, therefore, is not a robust method for assessing the suitability
for study with Ariel.

While the majority of these candidates still require confirmation, the
continued persistence and devotion of those involved in following up these
potential planetary signals, as well as the further extension to the TESS
mission, will ensure a large and diverse population of planets are available
for Ariel to characterise. The metrics derived in Kempton et al. (2018) are
being widely used to direct the TESS follow-up of potential atmospheric
targets. In Figure 14, one can see the number of Ariel observations needed to
reach the Tier 1 and Tier 2 requirements plotted against the Transit
Spectroscopy Metric (TSM) from Kempton et al. (2018) for the TPCs analysed
here. Over-plotted are the suggested quartiles for larger planets from Kempton
et al. (2018), with the scaling factor removed. Kempton et al. (2018)
suggested that the cut-off TSM for a statistical sample of gaseous planets
should be placed at around 90, a value often quoted and benchmarked against in
TESS discovery papers. While this value seems applicable to Ariel Tier 2, we
suggest that the boundary should be lower for Tier 1, with Ariel being capable
of potentially studying planets with a TSM$\sim$40 or above. However, we note
that this metric was designed specifically for JWST NIRISS and thus utilises
the star’s magnitude in the J band. If one takes two stars which have the same
J band magnitude but different temperatures, the stellar flux at longer
wavelengths will be greater for the cooler star. Therefore, as Ariel’s science
requirements are driven by the performance at longer wavelengths (1.95-7.8
$\mu$m), its use in this context may not be valid and the performance for
planets around cooler stars may be under-represented with respect to those
around hotter ones. Hence, we recommend the use of ArielRad (Mugnai et al.,
2020) to truly assess the suitability of a target for study.

In addition to the multitude of TESS discoveries, the sustained analysis of
Kepler/K2 data (e.g. Castro-González et al., 2022; de Leon et al., 2021;
Valizadegan et al., 2021; Zink et al., 2021), ongoing ground-based surveys
(e.g. Wheatley et al., 2018; Sebastian et al., 2021), and ESA’s PLATO mission
(Rauer et al., 2016) will also add to the population of exoplanets from which
the Ariel sample will be derived. Moreover, other space-based facilities, such
as CHEOPS (Benz et al., 2021) and Twinkle (Edwards et al., 2019b), can be
expected to find a handful of targets by searching for transits of planets
detected by radial velocity (e.g. Delrez et al., 2021) or conducting
observations of systems with transiting worlds in the search of additional
bodies (e.g. Bonfanti et al., 2021).

Such an overabundance of potential targets is undoubtedly beneficial, yet it
offers many challenges. While much of the final MRS will be selected based
upon which targets occupy the most sparsely-populated regions of parameter
space or are best placed to answer key questions on the nature of exoplanet
atmospheres, prioritisation may also be based upon how well-characterised the
planets bulk parameters and host star are. If we are to seek trends between
atmospheric composition and the bulk characteristics of planets, we must first
know both of these. While Ariel will give us the former, the latter knowledge
must generally be acquired before launch to ensure the sample of planets
selected allows for these comparisons to be drawn. The key parameters needed
include the stellar metallicity and the planet’s mass and transit ephemerides.

Luckily, a large cohort of researchers777The Ariel consortium is currently
composed of over 500 scientists. are working to ensure this is the case. For
instance, stellar parameters such as age and metallicity must be known and
work is underway to homogeneously derive such parameters (Brucalassi et al.,
2021; Danielski et al., 2021; Magrini et al., 2022). Furthermore, the
ephemerides of the potential planets must be well known to ensure efficient
scheduling. Here again, work is underway to refine the periods of these worlds
using citizen science, with thousands of light curves being observed by
amateur facilities as part of the ExoClock project (Kokori et al., 2021a, b)
and by secondary school students through the ORBYTS programme (e.g. Edwards et
al., 2021). Planets with non-linear ephemerides, such as those within multi-
planet systems that experience transit timing variations (TTVs) due to the
gravitational interaction of the planets, will require particular care and
attention (e.g. Dawson et al., 2019; Kipping et al., 2019; Ducrot et al.,
2020). By highlighting these key systems in Figure 11, and continuing to
update this list, we hope to motivate such follow-up in a timely manner.

Accurately knowing the planet’s mass is also useful, particularly for smaller
or cloudier worlds (Changeat et al., 2020b; Batalha et al., 2019). Several
studies have explored the time need to provide radial velocity measurements
necessary to constrain planet masses for Ariel (e.g. Barnes & Haswell, 2021;
Demangeon et al., submitted) and the ongoing work of radial velocity teams,
both within the Ariel consortium and outside of it (e.g. Lillo-Box et al.,
2020; Chontos et al., 2021; Nielsen et al., 2020; Kaye et al., 2022; Van Eylen
et al., 2021), are ensuring that the best targets for atmospheric
characterisation are followed-up. Nevertheless, it may not be possible to
conduct detailed follow-up of all the TPCs which may be of interest to the
Ariel mission.

The formation of the Ariel MRS will also need to account for the knowledge
gained through previous spectroscopic studies of exoplanetary atmospheres.
Ground-based and space-based spectroscopy are constantly providing new
insights into exoplanetary atmospheres. High-resolution spectroscopy from the
ground is becoming ever-more fruitful (e.g. Pino et al., 2020; Tabernero et
al., 2021; Giacobbe et al., 2021; Wardenier et al., 2021). At lower
resolutions, transit and eclipse studies with ground-based facilities and
Hubble continue to deliver new views of atmospheres (e.g. McGruder et al.,
2020; Braam et al., 2021; Saba et al., 2021; Yip et al., 2021), with a recent
focus on smaller planets (e.g. de Wit et al., 2018; Benneke et al., 2019;
Tsiaras et al., 2019; Diamond-Lowe et al., 2020; Edwards et al., 2021;
Gressier et al., 2021), and findings from these studies will further our
understanding of exoplanetary atmospheres.

Through its GTO and Cycle 1 GO programmes, a significant amount of time has
been attributed for JWST to study exoplanets via transit and eclipse
spectroscopy. The high precision data that will be acquired, on top of a wider
wavelength coverage with respect to current space-based instruments, will
unlocking new avenues for exoplanet characterisation (e.g. Changeat et al.,
2021b; Phillips et al., 2021; Pidhorodetska et al., 2021). The lessons learned
from these studies, particularly those of smaller worlds, will influence the
choices made to ensure the scientific yield of Ariel is maximised.

While thus far we assumed 1000 planets would be studied in Tier 1, this is by
no means fixed. We varied the number of Tier 1 planets studied, experimenting
with the impact this would have on the number of targets that could be
observed in Tier 2. Assuming that at least 500 planets are required in Tier 2,
it could be possible to study around 1350 planets from the list derived here
during the primary mission life. Reducing the required number of Tier 1
targets increases the time available for Tier 2 but the returns are quickly
diminishing. The optimal strategy, purely from an efficiency perspective,
occurs when the change in the gradient is sharpest. From Figure 15, this is
currently at around 1050 Tier 1 planets, which corresponds to 595 Tier 2
targets if one assumes 10% of Ariel science time is reserved for Tier 4 and
complementary science. These numbers are based on a four-year primary mission
life but if a two year extension were granted, and the time utilised to extend
the observing strategy of the primary mission life, we could potential study a
far greater number of worlds. However, the results from the primary mission
may suggest alternative lines of inquiry. The tiering system of Ariel has been
designed to account for our general lack of knowledge around the properties of
exoplanet atmospheres and their correlation with the bulk characteristics of a
system. Given the primary mission will provide us with the first demographical
study of exoplanet atmospheres, the extended mission could then be utilised to
study specific populations of interest. The strategy could involve delving
deep into trends uncovered in the prime mission, giving extra time to targets
or correlations which weren’t fully explored, conducting more time intensive
observations or pursuing observing strategies that are high risk/high reward.

Figure 15: The relationship between the number of Tier 1 and Tier 2 planets
that can be observed during the prime mission life. The red region is
forbidden: by their very definition one cannot observe more targets in Tier 2
than in Tier 1. We also show what could be achieved with a 2 year mission
extension. In all cases, 50 planets are assumed to be studied in Tier 3 and
10% of Ariel’s science time is left for Tier 4 observations and complementary
science programmes.

In reality, the Ariel Mission Consortium (AMC) and the Ariel Science Team
(AST) will decide the observing plan of Ariel based upon the scientific yield
which is dependent upon a number of parameters, many of which are qualitative
in nature. Studies of the impact of altering the number of planets in each
Tier will be required, with population-level studies needed to ascertain the
science loss/gain from adopting different strategies (e.g. Changeat et al.,
2020a; Mugnai et al., 2021a). While not discussed here, Ariel has a fourth
Tier to account for targets or observations which do not fit into the main
structure of the survey. Much of this time might be dedicated to exoplanet
phase curves, observing a planet throughout its entire orbit (e.g. Stevenson
et al., 2017; Changeat et al., 2021a; Dang et al., 2021; May et al., 2021),
and studies are underway to find the best targets for phase curve studies with
Ariel (Charnay et al., 2021; Moses et al., 2021). Additionally, this time
could be utilised to observe small, rocky worlds which may host secondary
atmospheres, as outlined in E19. Further in-depth studies of Ariel’s
capabilities across specific populations will be needed (e.g. Encrenaz et al.,
2021; Ito et al., 2021) to provide meaningful constraints on the potential
science yield. These studies, alongside community engagement, will act as
guides for the AMC and AST as they construct an ideal MCS. The final MCS will
be endorsed by the AST and reviewed under the responsibility of the ESA
Advisory Structure before launch. More details on this procedure can be found
in the Ariel Science Management Plan.

The confirmed planets and TESS planet candidates that are considered potential
targets for Ariel using the methodology described here are given in Tables 3
and 4. To guide the studies described above, and facilitate engagement with
the wider community, an Ariel Target List website, which will be maintained by
the AMC, is being constructed (Al-Refaie, in prep). The site will allow users
to keep track of all the planets that are potential viable targets for Ariel,
motivating further preliminary follow-up as well as theoretical studies into
Ariel’s capabilities. Through this collaborative platform, we hope to ensure
the Ariel mission delivers datasets of value to the entire extrasolar
community and that their interests are reflected in the final observing
strategy.

## Acknowledgements

BE is a Laureate of the Paris Region fellowship programme which is supported
by the Ile-de-France Region and has received funding under the Horizon 2020
innovation framework programme and the Marie Sklodowska-Curie grant agreement
no. 945298. This project has also received funding from the European Research
Council (ERC) under the European Union’s Horizon 2020 research and innovation
programme (grant agreement No 758892, ExoAI) and from the Science and
Technology Funding Council (STFC) grant ST/S002634/1.

We acknowledge the availability and support from the High Performance
Computing (HPC) platform DIRAC, which provided the computing resources
necessary to perform this work. The research conducted here has made use of
the NASA Exoplanet Archive, which is operated by the California Institute of
Technology, under contract with the National Aeronautics and Space
Administration under the Exoplanet Exploration Program. Additionally, this
paper relied upon data products from by the TESS mission, funding for which is
provided by the NASA’s Science Mission Directorate. We acknowledge the use of
public TOI Release data from pipelines at the TESS Science Office and at the
TESS Science Processing Operations Center.

We thank the Ariel Science Team, and many members of the Ariel consortium, for
their feedback on this manuscript throughout its development. We are also
indebted to Lorenzo V. Mugnai for his ongoing efforts to develop and maintain
the ArielRad tool, which facilitated this work. Finally, we thank the referee
for their insightful comments and suggestions which led us to refine many
aspects of the work and improve the overall quality of the study.

Software: ArielRad (v2.4.16, Mugnai et al., 2020), TauREx3 (Al-Refaie et al.,
2021b), TauREx3 ACE plug-in (Al-Refaie et al., 2021a; Venot & Agúndez, 2015),
Astropy (Astropy Collaboration et al., 2018), h5py (Collette, 2013),
Matplotlib (Hunter, 2007), Multinest (Feroz et al., 2009; Buchner et al.,
2014), Pandas (Wes McKinney, 2010; pandas development team, 2020), Numpy
(Oliphant, 2006), SciPy (Virtanen et al., 2020), corner (Foreman-Mackey,
2016).

Linelists: H2O (Polyansky et al., 2018), CH4 (Yurchenko & Tennyson, 2014), CO
(Li et al., 2015), CO2 (Rothman et al., 2010), CIA (Abel et al., 2011;
Fletcher et al., 2018; Abel et al., 2012).

Table 3: Currently-known exoplanets which are considered here to be potential targets for Ariel. The list will continue to evolve as surveys discover more planets. Planet Name | Tier | Method | Planet Name | Tier | Method | Planet Name | Tier | Method
---|---|---|---|---|---|---|---|---
55 Cnc e | 2 | Transit | HAT-P-30 b | 3 | Eclipse | HATS-29 b | 1 | Eclipse
AU Mic b | 3 | Transit | HAT-P-31 b | 1 | Eclipse | HATS-3 b | 2 | Eclipse
AU Mic c | 2 | Transit | HAT-P-32 b | 3 | Eclipse | HATS-30 b | 2 | Eclipse
CoRoT-1 b | 1 | Eclipse | HAT-P-33 b | 3 | Eclipse | HATS-31 b | 2 | Eclipse
CoRoT-11 b | 1 | Eclipse | HAT-P-34 b | 2 | Eclipse | HATS-33 b | 2 | Eclipse
CoRoT-2 b | 3 | Eclipse | HAT-P-35 b | 2 | Eclipse | HATS-34 b | 1 | Eclipse
DS Tuc A b | 1 | Eclipse | HAT-P-36 b | 2 | Eclipse | HATS-35 b | 2 | Eclipse
EPIC 211945201 b | 1 | Transit | HAT-P-37 b | 1 | Eclipse | HATS-37 A b | 2 | Transit
EPIC 246851721 b | 1 | Eclipse | HAT-P-38 b | 1 | Transit | HATS-38 b | 1 | Transit
G 9-40 b | 1 | Transit | HAT-P-39 b | 2 | Eclipse | HATS-42 b | 1 | Eclipse
GJ 1132 b | 2 | Transit | HAT-P-4 b | 3 | Eclipse | HATS-43 b | 2 | Transit
GJ 1214 b | 3 | Transit | HAT-P-40 b | 2 | Eclipse | HATS-46 b | 1 | Transit
GJ 1252 b | 1 | Transit | HAT-P-41 b | 3 | Eclipse | HATS-47 b | 1 | Transit
GJ 3470 b | 3 | Transit | HAT-P-42 b | 2 | Eclipse | HATS-48 A b | 1 | Transit
GJ 3473 b | 1 | Transit | HAT-P-44 b | 2 | Transit | HATS-5 b | 2 | Transit
GJ 357 b | 2 | Transit | HAT-P-45 b | 3 | Eclipse | HATS-51 b | 2 | Eclipse
GJ 367 b | 2 | Transit | HAT-P-46 b | 2 | Eclipse | HATS-52 b | 2 | Eclipse
GJ 3929 b | 2 | Transit | HAT-P-49 b | 3 | Eclipse | HATS-56 b | 2 | Eclipse
GJ 436 b | 3 | Transit | HAT-P-5 b | 2 | Eclipse | HATS-57 b | 2 | Eclipse
GJ 486 b | 2 | Transit | HAT-P-50 b | 2 | Eclipse | HATS-58 A b | 2 | Eclipse
GJ 9827 b | 1 | Transit | HAT-P-51 b | 2 | Transit | HATS-6 b | 1 | Transit
GJ 9827 c | 1 | Transit | HAT-P-53 b | 1 | Eclipse | HATS-60 b | 1 | Eclipse
GJ 9827 d | 1 | Transit | HAT-P-54 b | 1 | Eclipse | HATS-62 b | 1 | Transit
GPX-1 b | 2 | Eclipse | HAT-P-56 b | 2 | Eclipse | HATS-65 b | 2 | Eclipse
HAT-P-1 b | 3 | Eclipse | HAT-P-57 b | 3 | Eclipse | HATS-67 b | 1 | Eclipse
HAT-P-11 b | 2 | Transit | HAT-P-58 b | 2 | Transit | HATS-68 b | 1 | Eclipse
HAT-P-12 b | 2 | Transit | HAT-P-59 b | 2 | Eclipse | HATS-7 b | 1 | Transit
HAT-P-13 b | 3 | Eclipse | HAT-P-6 b | 3 | Eclipse | HATS-72 b | 2 | Transit
HAT-P-14 b | 2 | Eclipse | HAT-P-60 b | 3 | Eclipse | HATS-9 b | 1 | Eclipse
HAT-P-15 b | 1 | Eclipse | HAT-P-62 b | 2 | Eclipse | HD 106315 c | 1 | Transit
HAT-P-16 b | 3 | Eclipse | HAT-P-64 b | 2 | Eclipse | HD 108236 c | 1 | Transit
HAT-P-17 b | 2 | Transit | HAT-P-65 b | 2 | Eclipse | HD 108236 d | 1 | Transit
HAT-P-18 b | 2 | Transit | HAT-P-66 b | 1 | Eclipse | HD 108236 e | 1 | Transit
HAT-P-19 b | 2 | Transit | HAT-P-67 b | 3 | Transit | HD 110082 b | 1 | Transit
HAT-P-2 b | 2 | Eclipse | HAT-P-68 b | 2 | Eclipse | HD 136352 c | 2 | Transit
HAT-P-20 b | 2 | Eclipse | HAT-P-69 b | 3 | Eclipse | HD 1397 b | 3 | Eclipse
HAT-P-21 b | 2 | Eclipse | HAT-P-7 b | 3 | Eclipse | HD 149026 b | 3 | Eclipse
HAT-P-22 b | 3 | Eclipse | HAT-P-70 b | 3 | Eclipse | HD 152843 b | 1 | Transit
HAT-P-23 b | 2 | Eclipse | HAT-P-8 b | 3 | Eclipse | HD 152843 c | 2 | Transit
HAT-P-24 b | 2 | Eclipse | HAT-P-9 b | 2 | Eclipse | HD 17156 b | 2 | Eclipse
HAT-P-25 b | 1 | Eclipse | HATS-1 b | 2 | Eclipse | HD 183579 b | 2 | Transit
HAT-P-26 b | 2 | Transit | HATS-18 b | 2 | Eclipse | HD 189733 b | 3 | Eclipse
HAT-P-27 b | 2 | Eclipse | HATS-2 b | 2 | Eclipse | HD 191939 b | 2 | Transit
HAT-P-28 b | 1 | Eclipse | HATS-23 b | 2 | Eclipse | HD 191939 c | 2 | Transit
HAT-P-29 b | 1 | Eclipse | HATS-24 b | 2 | Eclipse | HD 191939 d | 2 | Transit
HAT-P-3 b | 2 | Eclipse | HATS-26 b | 2 | Eclipse | HD 202772 A b | 3 | Eclipse
HD 209458 b | 3 | Eclipse | KELT-11 b | 3 | Transit | LTT 1445 A c | 2 | Transit
HD 219666 b | 2 | Transit | KELT-12 b | 3 | Eclipse | LTT 3780 b | 1 | Transit
HD 221416 b | 2 | Transit | KELT-14 b | 3 | Eclipse | LTT 3780 c | 1 | Transit
HD 2685 b | 3 | Eclipse | KELT-15 b | 3 | Eclipse | LTT 9779 b | 2 | Eclipse
HD 332231 b | 3 | Transit | KELT-16 b | 3 | Eclipse | MASCARA-1 b | 3 | Eclipse
HD 63433 b | 2 | Transit | KELT-17 b | 3 | Eclipse | MASCARA-4 b | 3 | Eclipse
HD 63433 c | 2 | Transit | KELT-18 b | 3 | Eclipse | NGTS-10 b | 2 | Eclipse
HD 63935 b | 1 | Transit | KELT-19 A b | 3 | Eclipse | NGTS-12 b | 2 | Transit
HD 63935 c | 1 | Transit | KELT-2 A b | 3 | Eclipse | NGTS-2 b | 2 | Eclipse
HD 73583 b | 2 | Transit | KELT-20 b | 3 | Eclipse | NGTS-5 b | 2 | Transit
HD 89345 b | 2 | Transit | KELT-21 b | 3 | Eclipse | NGTS-6 b | 2 | Eclipse
HD 97658 b | 1 | Transit | KELT-23 A b | 3 | Eclipse | Qatar-1 b | 2 | Eclipse
HIP 41378 e | 1 | Transit | KELT-24 b | 3 | Eclipse | Qatar-10 b | 2 | Eclipse
HIP 41378 f | 2 | Transit | KELT-3 b | 3 | Eclipse | Qatar-2 b | 3 | Eclipse
HIP 65 A b | 3 | Eclipse | KELT-4 A b | 3 | Eclipse | Qatar-4 b | 2 | Eclipse
HIP 67522 b | 2 | Transit | KELT-6 b | 2 | Eclipse | Qatar-5 b | 1 | Eclipse
HR 858 b | 2 | Transit | KELT-7 b | 3 | Eclipse | Qatar-6 b | 2 | Eclipse
K2-107 b | 1 | Eclipse | KELT-8 b | 3 | Eclipse | Qatar-7 b | 2 | Eclipse
K2-121 b | 1 | Transit | KELT-9 b | 3 | Eclipse | Qatar-8 b | 2 | Eclipse
K2-136 c | 1 | Transit | KOI-13 b | 3 | Eclipse | Qatar-9 b | 2 | Eclipse
K2-138 f | 2 | Transit | KOI-94 d | 1 | Transit | TIC 257060897 b | 2 | Eclipse
K2-139 b | 1 | Transit | KOI-94 e | 1 | Transit | TOI-1064 c | 2 | Transit
K2-141 c | 3 | Transit | KPS-1 b | 2 | Eclipse | TOI-1130 b | 2 | Transit
K2-19 b | 1 | Transit | Kepler-105 b | 1 | Transit | TOI-1130 c | 3 | Transit
K2-198 b | 1 | Transit | Kepler-12 b | 2 | Transit | TOI-1201 b | 1 | Transit
K2-232 b | 2 | Transit | Kepler-1314 b | 1 | Transit | TOI-1227 b | 2 | Transit
K2-237 b | 3 | Eclipse | Kepler-16 b | 1 | Transit | TOI-1231 b | 2 | Transit
K2-238 b | 1 | Eclipse | Kepler-18 d | 1 | Transit | TOI-125 c | 1 | Transit
K2-24 b | 1 | Transit | Kepler-25 c | 1 | Transit | TOI-1259 A b | 2 | Transit
K2-24 c | 2 | Transit | Kepler-33 c | 1 | Transit | TOI-1268 b | 2 | Transit
K2-260 b | 2 | Eclipse | Kepler-444 b | 1 | Transit | TOI-1296 b | 2 | Transit
K2-261 b | 2 | Transit | Kepler-444 c | 1 | Transit | TOI-1333 b | 3 | Eclipse
K2-266 b | 1 | Transit | Kepler-444 e | 1 | Transit | TOI-1411 b | 1 | Transit
K2-266 d | 1 | Transit | Kepler-447 b | 2 | Eclipse | TOI-1431 b | 3 | Eclipse
K2-287 b | 1 | Transit | Kepler-468 b | 1 | Transit | TOI-1478 b | 2 | Eclipse
K2-289 b | 1 | Transit | Kepler-6 b | 1 | Eclipse | TOI-150.01 | 2 | Eclipse
K2-29 b | 2 | Eclipse | Kepler-7 b | 1 | Transit | TOI-1518 b | 3 | Eclipse
K2-295 b | 1 | Transit | L 98-59 b | 2 | Transit | TOI-157 b | 2 | Eclipse
K2-31 b | 3 | Eclipse | L 98-59 c | 2 | Transit | TOI-1601 b | 2 | Eclipse
K2-32 b | 2 | Transit | L 98-59 d | 2 | Transit | TOI-163 b | 2 | Eclipse
K2-32 d | 1 | Transit | LHS 1140 c | 1 | Transit | TOI-1670 c | 1 | Transit
K2-329 b | 1 | Transit | LHS 1478 b | 1 | Transit | TOI-1685 b | 1 | Transit
K2-34 b | 2 | Eclipse | LHS 1678 b | 1 | Transit | TOI-169 b | 1 | Eclipse
K2-36 c | 1 | Transit | LHS 3844 b | 2 | Transit | TOI-1728 b | 2 | Transit
K2-406 b | 2 | Transit | LP 714-47 b | 1 | Transit | TOI-1759 b | 1 | Transit
K2-52 b | 1 | Eclipse | LP 791-18 b | 1 | Transit | TOI-178 d | 2 | Transit
KELT-1 b | 3 | Eclipse | LP 791-18 c | 1 | Transit | TOI-178 e | 1 | Transit
KELT-10 b | 3 | Eclipse | LTT 1445 A b | 2 | Transit | TOI-178 g | 2 | Transit
TOI-1789 b | 3 | Eclipse | TRAPPIST-1 e | 1 | Transit | WASP-15 b | 3 | Eclipse
TOI-1807 b | 1 | Transit | TRAPPIST-1 f | 1 | Transit | WASP-151 b | 2 | Transit
TOI-1842 b | 2 | Transit | TRAPPIST-1 g | 1 | Transit | WASP-153 b | 2 | Transit
TOI-1899 b | 1 | Transit | TRAPPIST-1 h | 1 | Transit | WASP-156 b | 1 | Transit
TOI-201 b | 2 | Transit | TrES-1 b | 2 | Eclipse | WASP-159 b | 1 | Eclipse
TOI-2076 b | 2 | Transit | TrES-2 b | 3 | Eclipse | WASP-16 b | 2 | Eclipse
TOI-2076 c | 2 | Transit | TrES-3 b | 3 | Eclipse | WASP-160 B b | 2 | Transit
TOI-2076 d | 2 | Transit | TrES-4 b | 2 | Eclipse | WASP-161 b | 2 | Eclipse
TOI-2109 b | 3 | Eclipse | TrES-5 b | 2 | Eclipse | WASP-163 b | 2 | Eclipse
TOI-216.01 | 1 | Transit | V1298 Tau b | 2 | Transit | WASP-164 b | 2 | Eclipse
TOI-216.02 | 2 | Transit | V1298 Tau c | 1 | Transit | WASP-165 b | 1 | Eclipse
TOI-2337 b | 1 | Eclipse | V1298 Tau d | 2 | Transit | WASP-166 b | 2 | Transit
TOI-2427 b | 1 | Transit | V1298 Tau e | 2 | Transit | WASP-167 b | 3 | Eclipse
TOI-257 b | 2 | Transit | WASP-1 b | 2 | Eclipse | WASP-168 b | 2 | Transit
TOI-2669 b | 2 | Eclipse | WASP-10 b | 2 | Eclipse | WASP-169 b | 1 | Eclipse
TOI-269 b | 1 | Transit | WASP-100 b | 3 | Eclipse | WASP-17 b | 3 | Transit
TOI-270 b | 1 | Transit | WASP-101 b | 3 | Eclipse | WASP-170 b | 2 | Eclipse
TOI-270 c | 2 | Transit | WASP-103 b | 3 | Eclipse | WASP-172 b | 2 | Transit
TOI-270 d | 2 | Transit | WASP-104 b | 2 | Eclipse | WASP-173 A b | 3 | Eclipse
TOI-421 b | 1 | Transit | WASP-107 b | 3 | Transit | WASP-174 b | 2 | Transit
TOI-421 c | 2 | Transit | WASP-11 b | 2 | Eclipse | WASP-176 b | 2 | Eclipse
TOI-431 b | 1 | Transit | WASP-110 b | 2 | Transit | WASP-177 b | 3 | Transit
TOI-431 d | 2 | Transit | WASP-113 b | 2 | Eclipse | WASP-178 b | 3 | Eclipse
TOI-4329 b | 2 | Eclipse | WASP-114 b | 2 | Eclipse | WASP-18 b | 3 | Eclipse
TOI-451 c | 1 | Transit | WASP-117 b | 2 | Transit | WASP-180 A b | 2 | Eclipse
TOI-451 d | 1 | Transit | WASP-118 b | 2 | Eclipse | WASP-181 b | 2 | Transit
TOI-481 b | 2 | Eclipse | WASP-119 b | 2 | Eclipse | WASP-182 b | 2 | Transit
TOI-530 b | 1 | Transit | WASP-12 b | 3 | Eclipse | WASP-183 b | 2 | Transit
TOI-540 b | 2 | Transit | WASP-120 b | 2 | Eclipse | WASP-185 b | 2 | Eclipse
TOI-544 b | 1 | Transit | WASP-121 b | 3 | Eclipse | WASP-186 b | 2 | Eclipse
TOI-559 b | 2 | Eclipse | WASP-123 b | 3 | Eclipse | WASP-187 b | 3 | Eclipse
TOI-561 b | 1 | Transit | WASP-124 b | 1 | Eclipse | WASP-189 b | 3 | Eclipse
TOI-561 c | 2 | Transit | WASP-126 b | 2 | Eclipse | WASP-19 b | 3 | Eclipse
TOI-561 f | 1 | Transit | WASP-127 b | 3 | Transit | WASP-192 b | 1 | Eclipse
TOI-564 b | 2 | Eclipse | WASP-13 b | 3 | Eclipse | WASP-2 b | 2 | Eclipse
TOI-620 b | 2 | Transit | WASP-131 b | 3 | Transit | WASP-20 b | 3 | Transit
TOI-628 b | 3 | Eclipse | WASP-132 b | 2 | Transit | WASP-21 b | 2 | Transit
TOI-640 b | 3 | Eclipse | WASP-133 b | 1 | Eclipse | WASP-22 b | 2 | Eclipse
TOI-674 b | 2 | Transit | WASP-135 b | 2 | Eclipse | WASP-23 b | 2 | Eclipse
TOI-677 b | 2 | Eclipse | WASP-136 b | 3 | Eclipse | WASP-24 b | 2 | Eclipse
TOI-700 c | 1 | Transit | WASP-138 b | 2 | Eclipse | WASP-25 b | 2 | Eclipse
TOI-776 b | 1 | Transit | WASP-139 b | 2 | Transit | WASP-26 b | 2 | Eclipse
TOI-776 c | 1 | Transit | WASP-14 b | 3 | Eclipse | WASP-28 b | 2 | Eclipse
TOI-905 b | 2 | Eclipse | WASP-140 b | 3 | Eclipse | WASP-29 b | 2 | Transit
TOI-954 b | 2 | Transit | WASP-141 b | 1 | Eclipse | WASP-3 b | 3 | Eclipse
TRAPPIST-1 b | 2 | Transit | WASP-142 b | 1 | Eclipse | WASP-31 b | 2 | Eclipse
TRAPPIST-1 c | 2 | Transit | WASP-145 A b | 2 | Eclipse | WASP-32 b | 2 | Eclipse
TRAPPIST-1 d | 2 | Transit | WASP-147 b | 2 | Transit | WASP-33 b | 3 | Eclipse
WASP-34 b | 2 | Eclipse | WASP-62 b | 3 | Eclipse | WASP-85 A b | 3 | Eclipse
WASP-35 b | 3 | Eclipse | WASP-63 b | 2 | Transit | WASP-87 b | 3 | Eclipse
WASP-36 b | 2 | Eclipse | WASP-64 b | 2 | Eclipse | WASP-88 b | 2 | Eclipse
WASP-37 b | 1 | Eclipse | WASP-65 b | 2 | Eclipse | WASP-89 b | 1 | Eclipse
WASP-38 b | 3 | Eclipse | WASP-66 b | 2 | Eclipse | WASP-90 b | 2 | Eclipse
WASP-39 b | 3 | Transit | WASP-67 b | 2 | Transit | WASP-91 b | 2 | Eclipse
WASP-4 b | 3 | Eclipse | WASP-68 b | 2 | Eclipse | WASP-92 b | 2 | Eclipse
WASP-41 b | 2 | Eclipse | WASP-69 b | 3 | Transit | WASP-93 b | 2 | Eclipse
WASP-42 b | 2 | Transit | WASP-7 b | 3 | Eclipse | WASP-94 A b | 3 | Eclipse
WASP-43 b | 3 | Eclipse | WASP-70 A b | 2 | Eclipse | WASP-95 b | 3 | Eclipse
WASP-44 b | 1 | Eclipse | WASP-71 b | 2 | Eclipse | WASP-96 b | 1 | Eclipse
WASP-45 b | 1 | Eclipse | WASP-72 b | 2 | Eclipse | WASP-97 b | 3 | Eclipse
WASP-46 b | 2 | Eclipse | WASP-73 b | 2 | Eclipse | WASP-98 b | 1 | Eclipse
WASP-47 b | 2 | Eclipse | WASP-74 b | 3 | Eclipse | WASP-99 b | 2 | Eclipse
WASP-48 b | 2 | Eclipse | WASP-75 b | 2 | Eclipse | Wolf 503 b | 1 | Transit
WASP-49 b | 2 | Eclipse | WASP-76 b | 3 | Eclipse | XO-1 b | 2 | Eclipse
WASP-5 b | 2 | Eclipse | WASP-77 A b | 3 | Eclipse | XO-2 N b | 2 | Eclipse
WASP-50 b | 2 | Eclipse | WASP-78 b | 2 | Eclipse | XO-3 b | 3 | Eclipse
WASP-52 b | 3 | Eclipse | WASP-79 b | 3 | Eclipse | XO-4 b | 2 | Eclipse
WASP-53 b | 2 | Eclipse | WASP-8 b | 2 | Eclipse | XO-5 b | 2 | Eclipse
WASP-54 b | 3 | Eclipse | WASP-80 b | 3 | Eclipse | XO-6 b | 3 | Eclipse
WASP-55 b | 2 | Eclipse | WASP-81 b | 2 | Eclipse | XO-7 b | 3 | Eclipse
WASP-58 b | 2 | Eclipse | WASP-82 b | 3 | Eclipse | pi Men c | 2 | Transit
WASP-6 b | 2 | Eclipse | WASP-83 b | 2 | Transit |  |  |
WASP-61 b | 2 | Eclipse | WASP-84 b | 2 | Transit |  |  |

Table 4: TESS planet candidates which are considered here to be potential targets for Ariel. The list will continue to evolve as TESS discovers more potential planets. TOI | Tier | Method | TOI | Tier | Method | TOI | Tier | Method | TOI | Tier | Method
---|---|---|---|---|---|---|---|---|---|---|---
139.01 | 1 | Transit | 375.01 | 1 | Eclipse | 603.01 | 2 | Transit | 778.01 | 3 | Eclipse
145.01 | 1 | Transit | 376.01 | 1 | Transit | 610.01 | 1 | Transit | 783.01 | 1 | Transit
148.01 | 1 | Transit | 383.01 | 1 | Transit | 611.01 | 1 | Transit | 784.01 | 1 | Transit
153.01 | 1 | Transit | 392.01 | 3 | Eclipse | 614.01 | 1 | Eclipse | 790.01 | 1 | Transit
155.01 | 1 | Transit | 393.01 | 1 | Transit | 615.01 | 3 | Eclipse | 791.01 | 1 | Transit
159.01 | 3 | Eclipse | 399.01 | 1 | Transit | 618.01 | 1 | Transit | 802.01 | 1 | Transit
166.01 | 2 | Transit | 406.01 | 1 | Transit | 620.01 | 1 | Transit | 811.01 | 1 | Transit
170.01 | 1 | Eclipse | 412.01 | 3 | Eclipse | 621.01 | 3 | Eclipse | 812.01 | 1 | Transit
171.01 | 2 | Eclipse | 422.01 | 1 | Transit | 622.01 | 3 | Transit | 815.01 | 1 | Transit
172.01 | 1 | Transit | 424.01 | 1 | Transit | 623.01 | 2 | Transit | 821.01 | 1 | Transit
173.01 | 2 | Transit | 431.01 | 2 | Transit | 627.01 | 3 | Eclipse | 823.01 | 1 | Transit
174.04 | 1 | Transit | 431.02 | 1 | Transit | 628.01 | 3 | Eclipse | 829.01 | 1 | Transit
176.01 | 2 | Transit | 432.01 | 1 | Eclipse | 629.01 | 2 | Transit | 836.02 | 1 | Transit
177.01 | 2 | Transit | 435.01 | 1 | Transit | 633.01 | 2 | Transit | 841.01 | 1 | Transit
179.01 | 2 | Transit | 438.01 | 1 | Transit | 634.01 | 1 | Transit | 842.01 | 1 | Transit
181.01 | 2 | Transit | 444.01 | 2 | Transit | 635.01 | 1 | Transit | 845.01 | 2 | Eclipse
198.01 | 1 | Transit | 445.01 | 3 | Eclipse | 638.01 | 1 | Transit | 846.01 | 1 | Transit
199.01 | 2 | Transit | 450.01 | 3 | Transit | 640.01 | 3 | Eclipse | 847.01 | 2 | Eclipse
213.01 | 1 | Transit | 456.01 | 3 | Eclipse | 642.01 | 2 | Eclipse | 852.01 | 1 | Transit
214.01 | 1 | Transit | 459.01 | 1 | Eclipse | 643.01 | 2 | Transit | 853.01 | 2 | Eclipse
217.01 | 2 | Transit | 462.01 | 1 | Transit | 645.01 | 2 | Eclipse | 856.01 | 1 | Eclipse
233.01 | 1 | Transit | 469.01 | 2 | Transit | 649.01 | 3 | Eclipse | 857.01 | 2 | Eclipse
238.01 | 1 | Transit | 470.01 | 1 | Transit | 658.01 | 2 | Transit | 858.01 | 2 | Eclipse
242.01 | 2 | Eclipse | 475.01 | 1 | Transit | 659.01 | 2 | Eclipse | 859.01 | 1 | Transit
243.01 | 1 | Eclipse | 476.01 | 3 | Eclipse | 672.01 | 2 | Transit | 880.01 | 2 | Transit
245.01 | 1 | Transit | 478.01 | 3 | Eclipse | 682.01 | 1 | Transit | 880.02 | 2 | Transit
260.01 | 1 | Transit | 480.01 | 1 | Transit | 689.01 | 3 | Transit | 882.01 | 1 | Eclipse
261.01 | 1 | Transit | 486.01 | 2 | Transit | 691.01 | 1 | Transit | 883.01 | 2 | Transit
268.01 | 1 | Transit | 493.01 | 1 | Transit | 694.01 | 2 | Transit | 885.01 | 2 | Eclipse
275.01 | 3 | Eclipse | 523.01 | 2 | Transit | 696.01 | 1 | Transit | 887.01 | 2 | Eclipse
277.01 | 2 | Transit | 525.01 | 1 | Transit | 696.02 | 1 | Transit | 892.01 | 2 | Transit
278.01 | 1 | Transit | 526.01 | 2 | Transit | 696.03 | 1 | Transit | 899.01 | 1 | Transit
287.01 | 2 | Eclipse | 528.01 | 1 | Transit | 716.01 | 1 | Transit | 902.01 | 1 | Transit
302.01 | 1 | Transit | 532.01 | 1 | Transit | 735.01 | 1 | Transit | 907.01 | 2 | Eclipse
310.01 | 1 | Transit | 544.01 | 1 | Transit | 738.01 | 1 | Transit | 909.01 | 2 | Transit
317.01 | 1 | Eclipse | 552.01 | 1 | Transit | 741.01 | 2 | Transit | 910.01 | 2 | Transit
322.01 | 3 | Eclipse | 559.01 | 2 | Transit | 742.01 | 1 | Transit | 911.01 | 3 | Eclipse
326.01 | 2 | Eclipse | 560.01 | 2 | Transit | 746.01 | 1 | Transit | 912.01 | 1 | Transit
330.01 | 1 | Transit | 560.02 | 2 | Transit | 759.01 | 1 | Eclipse | 913.01 | 1 | Transit
341.01 | 1 | Transit | 575.01 | 2 | Eclipse | 761.01 | 1 | Transit | 926.01 | 1 | Transit
344.01 | 1 | Transit | 577.01 | 2 | Eclipse | 762.01 | 2 | Transit | 931.01 | 2 | Eclipse
351.01 | 1 | Transit | 579.01 | 2 | Eclipse | 763.01 | 1 | Transit | 933.01 | 1 | Transit
352.01 | 2 | Eclipse | 585.01 | 3 | Eclipse | 771.01 | 1 | Transit | 934.01 | 1 | Transit
354.01 | 2 | Eclipse | 587.01 | 3 | Eclipse | 772.01 | 2 | Transit | 939.01 | 2 | Transit
360.01 | 2 | Eclipse | 599.01 | 3 | Eclipse | 776.02 | 1 | Transit | 941.01 | 1 | Transit
368.01 | 3 | Eclipse | 601.01 | 1 | Eclipse | 777.01 | 2 | Transit | 943.01 | 2 | Transit
947.01 | 2 | Eclipse | 1111.01 | 2 | Eclipse | 1285.01 | 1 | Transit | 1415.01 | 1 | Transit
948.01 | 1 | Transit | 1113.01 | 3 | Transit | 1288.01 | 2 | Transit | 1416.01 | 1 | Transit
950.01 | 2 | Eclipse | 1119.01 | 2 | Eclipse | 1292.01 | 3 | Eclipse | 1420.01 | 2 | Transit
954.01 | 2 | Eclipse | 1120.01 | 2 | Eclipse | 1294.01 | 1 | Transit | 1423.01 | 2 | Transit
961.01 | 3 | Eclipse | 1123.01 | 3 | Eclipse | 1295.01 | 2 | Eclipse | 1424.01 | 1 | Transit
963.01 | 2 | Transit | 1126.01 | 1 | Transit | 1297.01 | 2 | Eclipse | 1431.01 | 3 | Eclipse
965.01 | 1 | Transit | 1130.01 | 3 | Transit | 1303.01 | 3 | Eclipse | 1434.01 | 1 | Transit
966.01 | 3 | Eclipse | 1130.02 | 1 | Transit | 1306.01 | 2 | Eclipse | 1438.01 | 1 | Transit
969.01 | 1 | Transit | 1133.01 | 1 | Transit | 1310.01 | 2 | Eclipse | 1448.01 | 1 | Transit
978.01 | 2 | Transit | 1135.01 | 2 | Transit | 1312.01 | 2 | Transit | 1449.01 | 2 | Transit
985.01 | 3 | Eclipse | 1136.01 | 2 | Transit | 1313.01 | 2 | Transit | 1449.02 | 1 | Transit
987.01 | 2 | Eclipse | 1136.02 | 1 | Transit | 1314.01 | 1 | Eclipse | 1454.01 | 2 | Eclipse
990.01 | 2 | Transit | 1136.03 | 1 | Transit | 1317.01 | 3 | Eclipse | 1460.01 | 3 | Eclipse
991.01 | 2 | Eclipse | 1143.01 | 2 | Eclipse | 1319.01 | 2 | Transit | 1461.01 | 2 | Eclipse
996.01 | 2 | Eclipse | 1158.01 | 3 | Eclipse | 1321.01 | 2 | Eclipse | 1467.01 | 1 | Transit
1007.01 | 2 | Eclipse | 1166.01 | 1 | Transit | 1325.01 | 2 | Transit | 1468.01 | 1 | Transit
1015.01 | 2 | Eclipse | 1168.01 | 3 | Eclipse | 1329.01 | 1 | Transit | 1468.02 | 1 | Transit
1017.01 | 3 | Eclipse | 1170.01 | 1 | Eclipse | 1331.01 | 2 | Eclipse | 1471.01 | 2 | Transit
1018.01 | 3 | Eclipse | 1171.01 | 1 | Eclipse | 1333.01 | 3 | Eclipse | 1472.01 | 1 | Transit
1019.01 | 3 | Eclipse | 1173.01 | 2 | Transit | 1343.01 | 1 | Transit | 1473.01 | 1 | Transit
1022.01 | 1 | Transit | 1176.01 | 2 | Transit | 1345.01 | 1 | Eclipse | 1474.01 | 1 | Transit
1027.01 | 1 | Transit | 1180.01 | 1 | Transit | 1350.01 | 2 | Eclipse | 1478.01 | 2 | Transit
1027.02 | 1 | Transit | 1181.01 | 3 | Eclipse | 1352.01 | 2 | Eclipse | 1482.01 | 2 | Eclipse
1028.01 | 2 | Transit | 1182.01 | 2 | Eclipse | 1353.01 | 1 | Transit | 1483.01 | 1 | Transit
1036.01 | 1 | Transit | 1184.01 | 1 | Transit | 1355.01 | 3 | Eclipse | 1484.01 | 1 | Eclipse
1047.01 | 2 | Transit | 1185.01 | 1 | Transit | 1359.01 | 2 | Eclipse | 1486.01 | 1 | Transit
1053.01 | 2 | Eclipse | 1186.01 | 3 | Eclipse | 1361.01 | 2 | Eclipse | 1489.01 | 1 | Eclipse
1058.01 | 2 | Eclipse | 1193.01 | 3 | Eclipse | 1362.01 | 2 | Eclipse | 1490.01 | 2 | Eclipse
1059.01 | 2 | Eclipse | 1194.01 | 2 | Transit | 1364.01 | 1 | Eclipse | 1492.01 | 1 | Transit
1064.01 | 1 | Transit | 1195.01 | 1 | Eclipse | 1367.01 | 1 | Transit | 1493.01 | 3 | Eclipse
1075.01 | 1 | Transit | 1196.01 | 2 | Eclipse | 1369.01 | 2 | Transit | 1496.01 | 3 | Transit
1077.01 | 1 | Eclipse | 1197.01 | 2 | Eclipse | 1370.01 | 2 | Transit | 1501.01 | 3 | Eclipse
1080.01 | 1 | Transit | 1199.01 | 2 | Eclipse | 1371.01 | 3 | Eclipse | 1507.01 | 2 | Eclipse
1081.01 | 2 | Transit | 1224.01 | 1 | Transit | 1381.01 | 1 | Transit | 1508.01 | 1 | Eclipse
1083.01 | 1 | Transit | 1232.01 | 1 | Transit | 1382.01 | 3 | Eclipse | 1511.01 | 3 | Eclipse
1086.01 | 1 | Eclipse | 1234.01 | 1 | Transit | 1383.01 | 2 | Eclipse | 1516.01 | 3 | Eclipse
1087.01 | 1 | Eclipse | 1239.01 | 1 | Transit | 1384.01 | 1 | Eclipse | 1518.01 | 3 | Eclipse
1088.01 | 1 | Transit | 1246.01 | 1 | Transit | 1387.01 | 1 | Transit | 1519.01 | 2 | Transit
1090.01 | 3 | Eclipse | 1248.01 | 1 | Transit | 1391.01 | 1 | Transit | 1521.01 | 3 | Eclipse
1091.01 | 3 | Eclipse | 1250.01 | 2 | Transit | 1394.01 | 2 | Transit | 1522.01 | 1 | Transit
1094.01 | 1 | Eclipse | 1264.01 | 2 | Transit | 1396.01 | 2 | Transit | 1527.01 | 2 | Eclipse
1095.01 | 2 | Eclipse | 1270.01 | 1 | Eclipse | 1397.01 | 2 | Transit | 1531.01 | 3 | Eclipse
1099.01 | 2 | Transit | 1272.01 | 1 | Transit | 1399.01 | 1 | Transit | 1532.01 | 2 | Transit
1101.01 | 2 | Eclipse | 1274.01 | 2 | Transit | 1400.01 | 1 | Transit | 1535.01 | 2 | Eclipse
1102.01 | 1 | Transit | 1275.01 | 1 | Transit | 1401.01 | 3 | Eclipse | 1538.01 | 2 | Transit
1107.01 | 2 | Eclipse | 1276.01 | 2 | Transit | 1410.01 | 1 | Transit | 1541.01 | 2 | Eclipse
1108.01 | 2 | Eclipse | 1279.01 | 2 | Transit | 1411.01 | 1 | Transit | 1548.01 | 1 | Transit
1110.01 | 2 | Eclipse | 1280.01 | 1 | Transit | 1412.01 | 2 | Transit | 1549.01 | 2 | Eclipse
1550.01 | 2 | Eclipse | 1694.01 | 2 | Transit | 1852.01 | 1 | Transit | 2045.01 | 2 | Transit
1553.01 | 2 | Eclipse | 1697.01 | 1 | Transit | 1853.01 | 1 | Transit | 2046.01 | 3 | Eclipse
1555.01 | 2 | Eclipse | 1702.01 | 1 | Transit | 1854.01 | 1 | Transit | 2047.01 | 2 | Eclipse
1556.01 | 2 | Eclipse | 1703.01 | 2 | Eclipse | 1858.01 | 2 | Eclipse | 2057.01 | 2 | Transit
1566.01 | 1 | Transit | 1708.01 | 2 | Transit | 1859.01 | 1 | Transit | 2058.01 | 2 | Eclipse
1568.01 | 3 | Eclipse | 1709.01 | 2 | Eclipse | 1860.01 | 1 | Transit | 2062.01 | 1 | Eclipse
1569.01 | 1 | Eclipse | 1710.01 | 2 | Transit | 1861.01 | 1 | Transit | 2066.01 | 3 | Eclipse
1570.01 | 2 | Transit | 1712.01 | 2 | Eclipse | 1873.01 | 1 | Transit | 2072.01 | 1 | Transit
1575.01 | 3 | Eclipse | 1717.01 | 3 | Eclipse | 1883.01 | 1 | Transit | 2076.01 | 2 | Transit
1577.01 | 2 | Transit | 1718.01 | 2 | Transit | 1884.01 | 1 | Transit | 2076.02 | 2 | Transit
1578.01 | 3 | Eclipse | 1722.01 | 1 | Transit | 1886.01 | 1 | Transit | 2079.01 | 1 | Transit
1585.01 | 1 | Eclipse | 1724.01 | 1 | Transit | 1890.01 | 1 | Transit | 2079.02 | 1 | Transit
1586.01 | 2 | Eclipse | 1730.01 | 1 | Transit | 1898.01 | 2 | Transit | 2099.01 | 1 | Transit
1588.01 | 2 | Eclipse | 1730.03 | 1 | Transit | 1938.01 | 2 | Transit | 2106.01 | 2 | Transit
1592.01 | 1 | Transit | 1758.01 | 1 | Transit | 1944.01 | 3 | Eclipse | 2107.01 | 2 | Eclipse
1593.01 | 1 | Eclipse | 1759.01 | 2 | Transit | 1945.01 | 1 | Eclipse | 2108.01 | 3 | Eclipse
1594.01 | 1 | Eclipse | 1765.01 | 1 | Transit | 1949.01 | 3 | Eclipse | 2114.01 | 2 | Eclipse
1596.01 | 2 | Eclipse | 1768.01 | 1 | Transit | 1951.01 | 3 | Eclipse | 2117.01 | 1 | Transit
1597.01 | 1 | Transit | 1774.01 | 1 | Transit | 1952.01 | 2 | Transit | 2119.01 | 3 | Transit
1600.01 | 2 | Eclipse | 1775.01 | 2 | Transit | 1954.01 | 2 | Transit | 2123.01 | 2 | Transit
1601.01 | 2 | Eclipse | 1786.01 | 2 | Eclipse | 1955.01 | 2 | Transit | 2133.01 | 1 | Transit
1603.01 | 2 | Eclipse | 1788.01 | 2 | Transit | 1956.01 | 1 | Transit | 2134.01 | 2 | Transit
1604.01 | 3 | Eclipse | 1792.01 | 2 | Transit | 1963.01 | 2 | Eclipse | 2136.01 | 1 | Transit
1605.01 | 2 | Transit | 1797.01 | 1 | Transit | 1968.01 | 2 | Eclipse | 2141.01 | 1 | Transit
1606.01 | 1 | Transit | 1801.01 | 1 | Transit | 1969.01 | 1 | Transit | 2143.01 | 2 | Eclipse
1608.01 | 3 | Eclipse | 1803.01 | 1 | Transit | 1970.01 | 2 | Eclipse | 2145.01 | 2 | Eclipse
1613.01 | 1 | Transit | 1806.01 | 1 | Transit | 1980.01 | 2 | Eclipse | 2146.01 | 2 | Eclipse
1615.01 | 3 | Eclipse | 1807.01 | 1 | Transit | 1982.01 | 2 | Transit | 2147.01 | 1 | Transit
1622.01 | 2 | Transit | 1811.01 | 2 | Transit | 1991.01 | 2 | Eclipse | 2150.01 | 1 | Transit
1623.01 | 1 | Transit | 1815.01 | 3 | Eclipse | 1994.01 | 2 | Eclipse | 2152.01 | 3 | Eclipse
1634.01 | 1 | Transit | 1818.01 | 1 | Transit | 1995.01 | 1 | Eclipse | 2154.01 | 2 | Eclipse
1635.01 | 2 | Transit | 1820.01 | 2 | Transit | 1996.01 | 3 | Eclipse | 2155.01 | 1 | Eclipse
1637.01 | 2 | Eclipse | 1822.01 | 2 | Eclipse | 1998.01 | 1 | Transit | 2157.01 | 2 | Eclipse
1638.01 | 2 | Eclipse | 1823.01 | 2 | Transit | 2000.01 | 2 | Transit | 2158.01 | 2 | Transit
1639.01 | 1 | Transit | 1824.01 | 1 | Transit | 2001.01 | 3 | Eclipse | 2159.01 | 2 | Transit
1640.01 | 1 | Transit | 1825.01 | 1 | Transit | 2005.01 | 1 | Transit | 2169.01 | 1 | Transit
1641.01 | 1 | Eclipse | 1827.01 | 2 | Transit | 2013.01 | 1 | Transit | 2171.01 | 2 | Eclipse
1647.01 | 2 | Eclipse | 1828.01 | 1 | Transit | 2015.01 | 1 | Transit | 2183.01 | 3 | Eclipse
1649.01 | 3 | Eclipse | 1830.01 | 3 | Eclipse | 2016.01 | 1 | Transit | 2190.01 | 1 | Eclipse
1655.01 | 1 | Transit | 1832.01 | 1 | Transit | 2016.02 | 1 | Transit | 2192.01 | 1 | Transit
1658.01 | 1 | Eclipse | 1835.01 | 2 | Transit | 2018.01 | 2 | Transit | 2194.01 | 2 | Transit
1662.01 | 3 | Eclipse | 1836.01 | 2 | Transit | 2019.01 | 1 | Transit | 2195.01 | 2 | Transit
1663.01 | 2 | Eclipse | 1837.01 | 1 | Transit | 2023.01 | 1 | Transit | 2200.01 | 1 | Transit
1668.01 | 1 | Transit | 1843.01 | 1 | Transit | 2025.01 | 1 | Transit | 2203.01 | 2 | Eclipse
1671.01 | 1 | Eclipse | 1845.01 | 1 | Transit | 2030.01 | 2 | Eclipse | 2207.01 | 1 | Transit
1673.01 | 1 | Transit | 1848.01 | 1 | Transit | 2031.01 | 2 | Transit | 2212.01 | 1 | Transit
1683.01 | 1 | Transit | 1849.01 | 1 | Transit | 2033.01 | 1 | Transit | 2215.01 | 1 | Transit
1691.01 | 1 | Transit | 1850.01 | 2 | Eclipse | 2040.01 | 2 | Transit | 2217.01 | 1 | Transit
2222.01 | 1 | Eclipse | 2404.02 | 1 | Transit | 2554.01 | 2 | Eclipse | 2668.01 | 1 | Transit
2223.01 | 1 | Transit | 2407.01 | 1 | Transit | 2556.01 | 1 | Transit | 2672.01 | 1 | Eclipse
2226.01 | 1 | Transit | 2408.01 | 1 | Transit | 2557.01 | 2 | Eclipse | 2677.01 | 2 | Eclipse
2234.01 | 1 | Eclipse | 2413.01 | 1 | Transit | 2558.01 | 1 | Transit | 2679.01 | 1 | Transit
2236.01 | 2 | Eclipse | 2418.01 | 2 | Transit | 2560.01 | 1 | Transit | 2692.01 | 1 | Transit
2241.01 | 2 | Eclipse | 2420.01 | 1 | Eclipse | 2561.01 | 2 | Eclipse | 2700.01 | 1 | Transit
2244.01 | 2 | Eclipse | 2421.01 | 2 | Eclipse | 2562.01 | 1 | Transit | 2710.01 | 1 | Transit
2247.01 | 2 | Eclipse | 2422.01 | 3 | Transit | 2563.01 | 1 | Transit | 2711.01 | 1 | Transit
2248.01 | 1 | Transit | 2424.01 | 2 | Eclipse | 2564.01 | 1 | Transit | 2714.01 | 1 | Transit
2249.01 | 2 | Eclipse | 2425.01 | 1 | Transit | 2566.01 | 1 | Transit | 2716.01 | 1 | Transit
2274.01 | 1 | Transit | 2427.01 | 1 | Transit | 2567.01 | 1 | Transit | 2718.01 | 1 | Transit
2283.01 | 1 | Transit | 2429.01 | 1 | Transit | 2568.01 | 1 | Eclipse | 2721.01 | 1 | Transit
2300.02 | 1 | Transit | 2431.01 | 2 | Eclipse | 2569.01 | 1 | Transit | 2724.01 | 2 | Eclipse
2303.01 | 1 | Eclipse | 2443.01 | 2 | Transit | 2570.01 | 2 | Eclipse | 2728.01 | 1 | Eclipse
2308.01 | 1 | Transit | 2446.01 | 1 | Transit | 2571.01 | 2 | Transit | 2729.01 | 2 | Transit
2312.01 | 1 | Transit | 2449.01 | 3 | Transit | 2576.01 | 2 | Transit | 2735.01 | 2 | Transit
2313.01 | 1 | Transit | 2450.01 | 1 | Transit | 2578.01 | 2 | Eclipse | 2741.01 | 2 | Eclipse
2316.01 | 2 | Eclipse | 2463.01 | 2 | Eclipse | 2580.01 | 3 | Eclipse | 2745.01 | 3 | Eclipse
2325.01 | 1 | Transit | 2469.01 | 3 | Eclipse | 2581.01 | 1 | Transit | 2746.01 | 1 | Transit
2328.01 | 1 | Transit | 2473.01 | 3 | Eclipse | 2582.01 | 1 | Transit | 2749.01 | 2 | Eclipse
2329.01 | 1 | Transit | 2476.01 | 1 | Eclipse | 2583.01 | 1 | Eclipse | 2751.01 | 1 | Transit
2331.01 | 1 | Transit | 2484.01 | 1 | Transit | 2586.01 | 1 | Transit | 2757.01 | 1 | Eclipse
2332.01 | 1 | Transit | 2485.01 | 1 | Transit | 2587.01 | 1 | Transit | 2758.01 | 1 | Transit
2336.01 | 2 | Transit | 2486.01 | 1 | Transit | 2589.01 | 1 | Transit | 2762.01 | 1 | Transit
2337.01 | 2 | Eclipse | 2489.01 | 2 | Eclipse | 2591.01 | 2 | Eclipse | 2766.01 | 2 | Eclipse
2338.01 | 1 | Transit | 2491.01 | 2 | Eclipse | 2594.01 | 1 | Eclipse | 2767.01 | 1 | Eclipse
2346.01 | 2 | Eclipse | 2492.01 | 2 | Eclipse | 2596.01 | 1 | Transit | 2768.01 | 1 | Transit
2350.01 | 1 | Transit | 2494.01 | 2 | Transit | 2597.01 | 1 | Eclipse | 2778.01 | 2 | Eclipse
2357.01 | 1 | Transit | 2497.01 | 2 | Transit | 2598.01 | 2 | Eclipse | 2783.01 | 3 | Eclipse
2359.01 | 2 | Eclipse | 2500.01 | 1 | Eclipse | 2600.01 | 2 | Eclipse | 2784.01 | 1 | Eclipse
2361.01 | 1 | Transit | 2504.01 | 1 | Eclipse | 2602.01 | 2 | Eclipse | 2786.01 | 1 | Eclipse
2363.01 | 1 | Transit | 2511.01 | 1 | Eclipse | 2614.01 | 2 | Eclipse | 2790.01 | 2 | Eclipse
2364.01 | 2 | Transit | 2516.01 | 3 | Eclipse | 2615.01 | 1 | Transit | 2797.01 | 1 | Transit
2366.01 | 1 | Transit | 2521.01 | 1 | Transit | 2616.01 | 1 | Transit | 2798.01 | 1 | Eclipse
2368.01 | 2 | Transit | 2524.01 | 1 | Transit | 2619.01 | 1 | Transit | 2799.01 | 2 | Eclipse
2369.01 | 1 | Transit | 2526.01 | 2 | Transit | 2621.01 | 1 | Eclipse | 2800.01 | 1 | Transit
2371.01 | 1 | Transit | 2527.01 | 1 | Eclipse | 2622.01 | 1 | Eclipse | 2803.01 | 2 | Eclipse
2374.01 | 2 | Transit | 2528.01 | 1 | Transit | 2624.01 | 1 | Transit | 2809.01 | 1 | Transit
2378.01 | 1 | Transit | 2531.01 | 1 | Transit | 2626.01 | 2 | Transit | 2813.01 | 1 | Transit
2383.01 | 2 | Eclipse | 2532.01 | 1 | Transit | 2631.01 | 1 | Transit | 2814.01 | 2 | Eclipse
2384.01 | 1 | Transit | 2533.01 | 1 | Transit | 2636.01 | 2 | Eclipse | 2816.01 | 2 | Transit
2385.01 | 1 | Transit | 2535.01 | 1 | Transit | 2645.01 | 3 | Eclipse | 2817.01 | 1 | Transit
2391.01 | 1 | Eclipse | 2540.01 | 2 | Transit | 2646.01 | 1 | Eclipse | 2818.01 | 2 | Eclipse
2395.01 | 1 | Transit | 2540.02 | 2 | Transit | 2647.01 | 1 | Eclipse | 2819.01 | 2 | Eclipse
2397.01 | 1 | Transit | 2543.01 | 1 | Transit | 2649.01 | 1 | Transit | 2820.01 | 1 | Transit
2398.01 | 1 | Transit | 2546.01 | 1 | Eclipse | 2654.01 | 1 | Transit | 2834.01 | 2 | Transit
2401.01 | 3 | Eclipse | 2550.01 | 1 | Transit | 2659.01 | 2 | Eclipse | 2835.01 | 1 | Eclipse
2402.01 | 1 | Transit | 2553.01 | 1 | Transit | 2665.01 | 1 | Transit | 2836.01 | 2 | Transit
2840.01 | 2 | Eclipse | 3037.01 | 1 | Eclipse | 3177.01 | 2 | Transit | 3304.01 | 1 | Transit
2841.01 | 1 | Eclipse | 3039.01 | 1 | Eclipse | 3179.01 | 1 | Eclipse | 3305.01 | 1 | Transit
2842.01 | 1 | Transit | 3040.01 | 1 | Transit | 3181.01 | 1 | Transit | 3306.01 | 1 | Transit
2847.01 | 2 | Transit | 3041.01 | 2 | Eclipse | 3184.01 | 1 | Transit | 3307.01 | 1 | Transit
2856.01 | 1 | Eclipse | 3045.01 | 2 | Eclipse | 3185.01 | 1 | Eclipse | 3309.01 | 2 | Transit
2866.01 | 1 | Transit | 3053.01 | 2 | Transit | 3187.01 | 1 | Eclipse | 3314.01 | 2 | Eclipse
2870.01 | 2 | Eclipse | 3054.01 | 1 | Eclipse | 3192.01 | 2 | Eclipse | 3315.01 | 1 | Transit
2876.01 | 1 | Transit | 3056.01 | 1 | Eclipse | 3194.01 | 1 | Transit | 3321.01 | 2 | Eclipse
2886.01 | 3 | Eclipse | 3058.01 | 2 | Eclipse | 3195.01 | 1 | Eclipse | 3322.01 | 1 | Eclipse
2892.01 | 1 | Transit | 3065.01 | 1 | Transit | 3196.01 | 1 | Transit | 3326.01 | 1 | Eclipse
2896.01 | 1 | Eclipse | 3066.01 | 1 | Transit | 3198.01 | 1 | Eclipse | 3329.01 | 2 | Transit
2901.01 | 2 | Eclipse | 3070.01 | 1 | Eclipse | 3203.01 | 1 | Transit | 3330.01 | 1 | Eclipse
2906.01 | 1 | Transit | 3073.01 | 1 | Transit | 3206.01 | 1 | Eclipse | 3331.01 | 2 | Eclipse
2912.01 | 1 | Transit | 3077.01 | 1 | Transit | 3208.01 | 1 | Transit | 3334.01 | 1 | Eclipse
2913.01 | 1 | Transit | 3082.01 | 1 | Transit | 3210.01 | 2 | Eclipse | 3341.01 | 1 | Transit
2916.01 | 1 | Transit | 3089.01 | 1 | Transit | 3212.01 | 2 | Transit | 3342.01 | 1 | Transit
2919.01 | 1 | Transit | 3091.01 | 2 | Eclipse | 3214.01 | 1 | Eclipse | 3344.01 | 3 | Eclipse
2920.01 | 1 | Eclipse | 3095.01 | 1 | Transit | 3228.01 | 1 | Eclipse | 3345.01 | 1 | Eclipse
2921.01 | 1 | Transit | 3097.01 | 1 | Transit | 3231.01 | 1 | Eclipse | 3351.01 | 2 | Eclipse
2927.01 | 1 | Eclipse | 3098.01 | 2 | Eclipse | 3233.01 | 1 | Eclipse | 3353.01 | 1 | Transit
2929.01 | 1 | Transit | 3099.01 | 1 | Transit | 3237.01 | 1 | Eclipse | 3358.01 | 1 | Transit
2937.01 | 1 | Eclipse | 3106.01 | 1 | Eclipse | 3240.01 | 1 | Transit | 3362.01 | 1 | Transit
2938.01 | 2 | Transit | 3107.01 | 2 | Eclipse | 3241.01 | 2 | Eclipse | 3364.01 | 2 | Transit
2941.01 | 2 | Eclipse | 3114.01 | 1 | Transit | 3242.01 | 1 | Eclipse | 3365.01 | 2 | Transit
2943.01 | 2 | Eclipse | 3118.01 | 1 | Eclipse | 3244.01 | 1 | Eclipse | 3371.01 | 1 | Transit
2946.01 | 2 | Transit | 3122.01 | 1 | Transit | 3245.01 | 1 | Eclipse | 3374.01 | 2 | Eclipse
2950.01 | 1 | Transit | 3126.01 | 2 | Eclipse | 3248.01 | 1 | Transit | 3388.01 | 1 | Eclipse
2952.01 | 1 | Transit | 3127.01 | 2 | Eclipse | 3250.01 | 1 | Transit | 3397.01 | 1 | Transit
2955.01 | 1 | Eclipse | 3129.01 | 2 | Eclipse | 3252.01 | 1 | Transit | 3398.01 | 1 | Transit
2956.01 | 1 | Transit | 3130.01 | 2 | Eclipse | 3253.01 | 1 | Transit | 3400.01 | 2 | Eclipse
2958.01 | 2 | Transit | 3134.01 | 1 | Eclipse | 3255.01 | 1 | Transit | 3401.01 | 1 | Transit
2962.01 | 1 | Eclipse | 3135.01 | 2 | Transit | 3259.01 | 1 | Transit | 3404.01 | 1 | Transit
2964.01 | 1 | Transit | 3136.01 | 2 | Eclipse | 3266.01 | 1 | Transit | 3407.01 | 1 | Eclipse
2974.01 | 1 | Eclipse | 3138.01 | 1 | Transit | 3268.01 | 1 | Transit | 3417.01 | 1 | Transit
2975.01 | 1 | Eclipse | 3145.01 | 2 | Eclipse | 3271.01 | 2 | Eclipse | 3422.01 | 1 | Eclipse
2981.01 | 1 | Transit | 3146.01 | 2 | Eclipse | 3273.01 | 2 | Transit | 3433.01 | 1 | Transit
2984.01 | 2 | Transit | 3151.01 | 1 | Eclipse | 3274.01 | 1 | Transit | 3436.01 | 1 | Eclipse
2989.01 | 2 | Transit | 3155.01 | 2 | Eclipse | 3275.01 | 1 | Transit | 3437.01 | 1 | Transit
2991.01 | 1 | Transit | 3156.01 | 2 | Eclipse | 3276.01 | 1 | Transit | 3443.01 | 1 | Eclipse
2992.01 | 1 | Eclipse | 3160.01 | 1 | Eclipse | 3277.01 | 2 | Eclipse | 3444.01 | 2 | Eclipse
2995.01 | 1 | Eclipse | 3161.01 | 1 | Eclipse | 3281.01 | 1 | Transit | 3445.01 | 2 | Eclipse
2997.01 | 2 | Eclipse | 3162.01 | 1 | Eclipse | 3283.01 | 1 | Eclipse | 3447.01 | 1 | Transit
3001.01 | 1 | Eclipse | 3163.01 | 1 | Eclipse | 3285.01 | 1 | Eclipse | 3451.01 | 1 | Transit
3004.01 | 1 | Eclipse | 3164.01 | 1 | Eclipse | 3288.01 | 2 | Eclipse | 3456.01 | 1 | Transit
3006.01 | 1 | Eclipse | 3167.01 | 1 | Eclipse | 3290.01 | 1 | Transit | 3458.01 | 2 | Transit
3010.01 | 1 | Eclipse | 3168.01 | 1 | Transit | 3294.01 | 2 | Eclipse | 3460.01 | 3 | Eclipse
3017.01 | 1 | Eclipse | 3174.01 | 1 | Eclipse | 3296.01 | 1 | Transit | 3464.01 | 1 | Transit
3023.01 | 2 | Eclipse | 3176.01 | 1 | Transit | 3298.01 | 1 | Eclipse | 3466.01 | 2 | Eclipse
3468.01 | 1 | Transit | 3566.01 | 1 | Eclipse | 3683.01 | 1 | Eclipse | 3790.01 | 2 | Transit
3469.01 | 2 | Eclipse | 3568.01 | 1 | Transit | 3686.01 | 2 | Eclipse | 3791.01 | 1 | Eclipse
3471.01 | 1 | Transit | 3569.01 | 2 | Eclipse | 3688.01 | 2 | Transit | 3796.01 | 2 | Transit
3472.01 | 2 | Eclipse | 3571.01 | 2 | Eclipse | 3691.01 | 1 | Transit | 3797.01 | 1 | Transit
3474.01 | 2 | Eclipse | 3573.01 | 1 | Transit | 3693.01 | 2 | Transit | 3798.01 | 1 | Transit
3475.01 | 1 | Eclipse | 3576.01 | 1 | Transit | 3698.01 | 1 | Eclipse | 3799.01 | 1 | Transit
3476.01 | 1 | Eclipse | 3580.01 | 2 | Transit | 3699.01 | 1 | Eclipse | 3801.01 | 1 | Transit
3478.01 | 2 | Eclipse | 3585.01 | 1 | Transit | 3700.01 | 1 | Transit | 3805.01 | 1 | Transit
3484.01 | 2 | Eclipse | 3586.01 | 2 | Transit | 3703.01 | 2 | Eclipse | 3809.01 | 1 | Transit
3489.01 | 2 | Eclipse | 3587.01 | 2 | Eclipse | 3704.01 | 1 | Transit | 3812.01 | 2 | Transit
3490.01 | 1 | Transit | 3589.01 | 2 | Eclipse | 3705.01 | 1 | Eclipse | 3815.01 | 2 | Eclipse
3491.01 | 3 | Eclipse | 3593.01 | 2 | Transit | 3708.01 | 2 | Transit | 3822.01 | 2 | Transit
3492.01 | 2 | Eclipse | 3595.01 | 2 | Transit | 3713.01 | 1 | Transit | 3826.01 | 1 | Eclipse
3493.01 | 1 | Transit | 3597.01 | 2 | Transit | 3714.01 | 2 | Transit | 3827.01 | 1 | Transit
3494.01 | 1 | Transit | 3599.01 | 1 | Transit | 3715.01 | 3 | Eclipse | 3829.01 | 1 | Transit
3498.01 | 1 | Transit | 3600.01 | 1 | Eclipse | 3719.01 | 2 | Eclipse | 3835.01 | 2 | Eclipse
3503.01 | 2 | Eclipse | 3602.01 | 2 | Eclipse | 3720.01 | 1 | Eclipse | 3837.01 | 1 | Transit
3504.01 | 2 | Eclipse | 3605.01 | 2 | Eclipse | 3721.01 | 1 | Transit | 3842.01 | 2 | Transit
3505.01 | 1 | Transit | 3613.01 | 1 | Transit | 3726.01 | 1 | Eclipse | 3845.01 | 1 | Eclipse
3506.01 | 1 | Transit | 3616.01 | 1 | Eclipse | 3727.01 | 1 | Transit | 3847.01 | 1 | Transit
3507.01 | 1 | Transit | 3618.01 | 1 | Transit | 3731.01 | 1 | Transit | 3849.01 | 2 | Eclipse
3508.01 | 2 | Eclipse | 3619.01 | 1 | Eclipse | 3732.01 | 1 | Eclipse | 3850.01 | 1 | Transit
3510.01 | 1 | Transit | 3625.01 | 1 | Eclipse | 3733.01 | 2 | Eclipse | 3855.01 | 1 | Transit
3511.01 | 2 | Eclipse | 3626.01 | 1 | Transit | 3735.01 | 2 | Transit | 3856.01 | 2 | Eclipse
3514.01 | 2 | Eclipse | 3628.01 | 2 | Transit | 3737.01 | 2 | Eclipse | 3857.01 | 1 | Transit
3515.01 | 1 | Transit | 3629.01 | 2 | Transit | 3738.01 | 1 | Transit | 3862.01 | 1 | Transit
3519.01 | 1 | Eclipse | 3630.01 | 1 | Transit | 3741.01 | 2 | Eclipse | 3868.01 | 1 | Transit
3522.01 | 1 | Transit | 3632.01 | 1 | Eclipse | 3745.01 | 1 | Transit | 3870.01 | 1 | Transit
3523.01 | 2 | Eclipse | 3633.01 | 1 | Eclipse | 3746.01 | 1 | Transit | 3871.01 | 1 | Transit
3524.01 | 1 | Transit | 3635.01 | 1 | Eclipse | 3749.01 | 1 | Eclipse | 3872.01 | 1 | Transit
3525.01 | 1 | Eclipse | 3636.01 | 1 | Eclipse | 3750.01 | 1 | Transit | 3877.01 | 1 | Transit
3526.01 | 1 | Eclipse | 3639.01 | 1 | Transit | 3751.01 | 1 | Transit | 3881.01 | 1 | Transit
3527.01 | 1 | Eclipse | 3640.01 | 1 | Eclipse | 3754.01 | 1 | Eclipse | 3883.01 | 2 | Transit
3529.01 | 1 | Eclipse | 3642.01 | 1 | Transit | 3755.01 | 1 | Transit | 3884.01 | 2 | Transit
3531.01 | 3 | Eclipse | 3645.01 | 1 | Transit | 3756.01 | 1 | Transit | 3889.01 | 2 | Transit
3539.01 | 1 | Transit | 3646.01 | 2 | Eclipse | 3758.01 | 2 | Eclipse | 3892.01 | 2 | Transit
3542.01 | 1 | Eclipse | 3652.01 | 2 | Eclipse | 3763.01 | 2 | Eclipse | 3894.01 | 2 | Eclipse
3543.01 | 2 | Eclipse | 3662.01 | 1 | Transit | 3764.01 | 1 | Eclipse | 3905.01 | 1 | Transit
3545.01 | 2 | Eclipse | 3664.01 | 1 | Transit | 3765.01 | 2 | Eclipse | 3907.01 | 1 | Transit
3546.01 | 1 | Transit | 3666.01 | 2 | Eclipse | 3767.01 | 2 | Eclipse | 3909.01 | 1 | Eclipse
3548.01 | 3 | Eclipse | 3668.01 | 2 | Eclipse | 3768.01 | 1 | Eclipse | 3910.01 | 2 | Transit
3551.01 | 1 | Eclipse | 3670.01 | 1 | Transit | 3769.01 | 2 | Transit | 3912.01 | 2 | Eclipse
3553.01 | 1 | Eclipse | 3673.01 | 1 | Eclipse | 3772.01 | 1 | Transit | 3913.01 | 1 | Transit
3559.01 | 1 | Eclipse | 3675.01 | 1 | Transit | 3780.01 | 2 | Eclipse | 3914.01 | 2 | Transit
3560.01 | 1 | Transit | 3677.01 | 2 | Eclipse | 3781.01 | 1 | Transit | 3915.01 | 2 | Transit
3563.01 | 1 | Transit | 3678.01 | 2 | Eclipse | 3785.01 | 1 | Transit | 3921.01 | 2 | Transit
3564.01 | 2 | Eclipse | 3679.01 | 1 | Transit | 3786.01 | 1 | Eclipse | 3924.01 | 1 | Eclipse
3565.01 | 1 | Transit | 3682.01 | 2 | Eclipse | 3788.01 | 2 | Eclipse | 3926.01 | 1 | Transit
3927.01 | 1 | Eclipse | 4087.01 | 2 | Eclipse | 4274.01 | 2 | Eclipse | 4487.01 | 2 | Eclipse
3929.01 | 2 | Eclipse | 4088.01 | 1 | Eclipse | 4279.01 | 2 | Eclipse | 4491.01 | 1 | Transit
3932.01 | 1 | Eclipse | 4103.01 | 2 | Transit | 4280.01 | 1 | Transit | 4492.01 | 3 | Eclipse
3937.01 | 2 | Eclipse | 4104.01 | 1 | Eclipse | 4283.01 | 2 | Eclipse | 4495.01 | 1 | Transit
3939.01 | 2 | Transit | 4116.01 | 1 | Eclipse | 4289.01 | 2 | Eclipse | 4504.01 | 1 | Transit
3940.01 | 2 | Transit | 4121.01 | 2 | Eclipse | 4293.01 | 2 | Eclipse | 4505.01 | 2 | Eclipse
3948.01 | 1 | Transit | 4124.01 | 2 | Eclipse | 4324.01 | 1 | Transit | 4507.01 | 1 | Transit
3952.01 | 2 | Eclipse | 4127.01 | 1 | Transit | 4327.01 | 1 | Transit | 4515.01 | 2 | Transit
3955.01 | 1 | Eclipse | 4129.01 | 1 | Transit | 4329.01 | 2 | Eclipse | 4527.01 | 2 | Transit
3958.01 | 1 | Transit | 4131.01 | 1 | Transit | 4330.01 | 3 | Eclipse | 4529.01 | 1 | Transit
3960.01 | 1 | Transit | 4137.01 | 2 | Eclipse | 4335.01 | 2 | Eclipse | 4537.01 | 1 | Transit
3962.01 | 1 | Eclipse | 4140.01 | 2 | Transit | 4336.01 | 1 | Transit | 4546.01 | 2 | Eclipse
3965.01 | 1 | Eclipse | 4144.01 | 2 | Transit | 4339.01 | 2 | Transit | 4548.01 | 1 | Transit
3972.01 | 2 | Transit | 4149.01 | 1 | Transit | 4341.01 | 1 | Transit | 4552.01 | 1 | Transit
3974.01 | 1 | Transit | 4153.01 | 2 | Eclipse | 4377.01 | 2 | Eclipse | 4553.01 | 2 | Transit
3976.01 | 1 | Transit | 4160.01 | 1 | Transit | 4379.01 | 2 | Eclipse | 4557.01 | 1 | Transit
3977.01 | 2 | Transit | 4162.01 | 2 | Eclipse | 4381.01 | 3 | Eclipse | 4564.01 | 2 | Transit
3984.01 | 1 | Transit | 4168.01 | 1 | Transit | 4384.01 | 1 | Transit | 4576.01 | 1 | Transit
3986.01 | 1 | Eclipse | 4170.01 | 2 | Eclipse | 4385.01 | 1 | Eclipse | 4596.01 | 1 | Transit
3988.01 | 1 | Eclipse | 4173.01 | 1 | Transit | 4386.01 | 1 | Transit | 4597.01 | 3 | Eclipse
3991.01 | 1 | Eclipse | 4176.01 | 3 | Eclipse | 4387.01 | 2 | Eclipse | 4598.01 | 1 | Transit
3998.01 | 2 | Eclipse | 4177.01 | 2 | Eclipse | 4394.01 | 1 | Eclipse | 4599.01 | 2 | Transit
4000.01 | 2 | Eclipse | 4180.01 | 1 | Transit | 4395.01 | 1 | Transit | 4599.02 | 3 | Transit
4003.01 | 1 | Transit | 4188.01 | 2 | Transit | 4399.01 | 1 | Transit | 4600.01 | 1 | Transit
4007.01 | 2 | Transit | 4193.01 | 1 | Transit | 4400.01 | 2 | Eclipse | 4602.01 | 1 | Transit
4010.01 | 1 | Transit | 4196.01 | 2 | Eclipse | 4406.01 | 1 | Transit | 4605.01 | 2 | Transit
4010.02 | 1 | Transit | 4197.01 | 2 | Transit | 4409.01 | 1 | Transit | 4609.01 | 3 | Eclipse
4012.01 | 2 | Transit | 4198.01 | 1 | Transit | 4412.01 | 1 | Transit | 4615.01 | 2 | Eclipse
4013.01 | 1 | Eclipse | 4199.01 | 2 | Eclipse | 4416.01 | 2 | Eclipse | 4617.01 | 2 | Eclipse
4014.01 | 1 | Transit | 4201.01 | 2 | Transit | 4417.01 | 1 | Transit | 4626.01 | 1 | Transit
4015.01 | 2 | Eclipse | 4204.01 | 1 | Transit | 4422.01 | 2 | Eclipse | 4635.01 | 2 | Transit
4029.01 | 1 | Transit | 4205.01 | 1 | Transit | 4423.01 | 1 | Transit | 4641.01 | 2 | Transit
4034.01 | 2 | Eclipse | 4207.01 | 1 | Eclipse | 4425.01 | 2 | Transit | 4642.01 | 1 | Transit
4041.01 | 2 | Transit | 4209.01 | 1 | Eclipse | 4427.01 | 2 | Transit | 4645.01 | 3 | Eclipse
4043.01 | 1 | Transit | 4214.01 | 2 | Eclipse | 4429.01 | 1 | Transit | 4646.01 | 2 | Transit
4044.01 | 1 | Transit | 4223.01 | 1 | Transit | 4436.01 | 3 | Eclipse | 4650.01 | 1 | Transit
4056.01 | 1 | Transit | 4224.01 | 1 | Eclipse | 4438.01 | 1 | Transit | 4652.01 | 1 | Transit
4059.01 | 1 | Transit | 4236.01 | 2 | Eclipse | 4441.01 | 2 | Eclipse | 4655.01 | 1 | Transit
4066.01 | 1 | Transit | 4243.01 | 1 | Eclipse | 4443.01 | 1 | Transit | 4660.01 | 2 | Eclipse
4067.01 | 1 | Transit | 4245.01 | 1 | Transit | 4447.01 | 1 | Transit | 4663.01 | 1 | Transit
4069.01 | 1 | Transit | 4246.01 | 1 | Transit | 4451.01 | 1 | Transit | 4664.01 | 1 | Transit
4074.01 | 1 | Eclipse | 4247.01 | 1 | Eclipse | 4458.01 | 1 | Eclipse | 4666.01 | 2 | Transit
4077.01 | 1 | Transit | 4248.01 | 1 | Eclipse | 4461.01 | 2 | Transit | 4672.01 | 1 | Eclipse
4079.01 | 2 | Eclipse | 4252.01 | 1 | Transit | 4462.01 | 1 | Eclipse | 4702.01 | 1 | Eclipse
4080.01 | 1 | Transit | 4254.01 | 1 | Eclipse | 4468.01 | 1 | Transit | 4707.01 | 1 | Eclipse
4082.01 | 1 | Transit | 4262.01 | 2 | Transit | 4477.01 | 2 | Eclipse | 4719.01 | 1 | Transit
4085.01 | 2 | Transit | 4266.01 | 1 | Eclipse | 4478.01 | 1 | Transit | 4721.01 | 1 | Transit
4086.01 | 1 | Transit | 4273.01 | 1 | Eclipse | 4481.01 | 2 | Transit | 4726.01 | 2 | Transit
4728.01 | 1 | Transit | 4961.01 | 2 | Transit | 5124.01 | 1 | Eclipse | 5269.01 | 1 | Transit
4730.01 | 1 | Transit | 4968.01 | 1 | Eclipse | 5126.01 | 1 | Transit | 5270.01 | 1 | Eclipse
4738.01 | 1 | Eclipse | 4970.01 | 1 | Transit | 5128.01 | 2 | Transit | 5276.01 | 1 | Eclipse
4739.01 | 2 | Eclipse | 4977.01 | 1 | Transit | 5143.01 | 2 | Transit | 5285.01 | 1 | Transit
4749.01 | 2 | Eclipse | 4979.01 | 1 | Transit | 5148.01 | 2 | Eclipse | 5287.01 | 2 | Eclipse
4764.01 | 1 | Transit | 4981.01 | 2 | Eclipse | 5149.01 | 1 | Eclipse | 5288.01 | 2 | Transit
4766.01 | 2 | Eclipse | 4987.01 | 2 | Eclipse | 5150.01 | 2 | Eclipse | 5291.01 | 1 | Transit
4768.01 | 2 | Eclipse | 4994.01 | 1 | Transit | 5153.01 | 1 | Transit | 5293.01 | 2 | Transit
4770.01 | 1 | Eclipse | 4998.01 | 1 | Transit | 5169.01 | 1 | Transit | 5295.01 | 1 | Transit
4771.01 | 1 | Transit | 4999.01 | 1 | Transit | 5172.01 | 1 | Transit | 5296.01 | 2 | Transit
4772.01 | 1 | Transit | 5001.01 | 1 | Transit | 5174.01 | 1 | Transit | 5298.01 | 1 | Transit
4773.01 | 1 | Eclipse | 5003.01 | 1 | Transit | 5179.01 | 1 | Eclipse | 5299.01 | 1 | Eclipse
4775.01 | 2 | Eclipse | 5004.01 | 1 | Transit | 5180.01 | 1 | Eclipse | 5300.01 | 2 | Transit
4776.01 | 1 | Transit | 5005.01 | 1 | Transit | 5181.01 | 1 | Eclipse | 5302.01 | 1 | Transit
4787.01 | 1 | Transit | 5007.01 | 1 | Transit | 5185.01 | 1 | Eclipse | 5305.01 | 1 | Transit
4791.01 | 2 | Eclipse | 5008.01 | 1 | Transit | 5186.01 | 2 | Eclipse | 5307.01 | 1 | Transit
4792.01 | 1 | Transit | 5009.01 | 1 | Eclipse | 5189.01 | 1 | Transit | 5308.01 | 2 | Eclipse
4794.01 | 1 | Eclipse | 5015.01 | 2 | Eclipse | 5190.01 | 1 | Transit | 5310.01 | 1 | Transit
4798.01 | 1 | Transit | 5022.01 | 1 | Eclipse | 5191.01 | 2 | Eclipse | 5313.01 | 1 | Transit
4811.01 | 2 | Eclipse | 5025.01 | 1 | Eclipse | 5195.01 | 1 | Eclipse | 5314.01 | 1 | Transit
4822.01 | 1 | Eclipse | 5026.01 | 1 | Transit | 5198.01 | 1 | Eclipse | 5319.01 | 1 | Transit
4823.01 | 2 | Eclipse | 5028.01 | 1 | Eclipse | 5204.01 | 1 | Eclipse | 5321.01 | 1 | Eclipse
4831.01 | 1 | Eclipse | 5029.01 | 2 | Transit | 5205.01 | 2 | Transit | 5322.01 | 2 | Eclipse
4841.01 | 1 | Transit | 5038.01 | 2 | Eclipse | 5207.01 | 1 | Transit | 5323.01 | 1 | Eclipse
4844.01 | 1 | Transit | 5043.01 | 2 | Eclipse | 5208.01 | 1 | Transit | 5324.01 | 1 | Transit
4852.01 | 1 | Transit | 5047.01 | 2 | Transit | 5209.01 | 2 | Transit | 5326.01 | 1 | Transit
4860.01 | 2 | Transit | 5048.01 | 1 | Eclipse | 5210.01 | 2 | Transit | 5327.01 | 2 | Transit
4871.01 | 1 | Eclipse | 5049.01 | 1 | Transit | 5211.01 | 1 | Eclipse | 5328.01 | 2 | Eclipse
4877.01 | 1 | Transit | 5051.01 | 2 | Eclipse | 5217.01 | 1 | Eclipse | 5330.01 | 1 | Transit
4882.01 | 1 | Transit | 5052.01 | 2 | Eclipse | 5226.01 | 2 | Eclipse | 5331.01 | 1 | Transit
4887.01 | 1 | Transit | 5053.01 | 1 | Transit | 5227.01 | 1 | Transit | 5334.01 | 1 | Transit
4890.01 | 2 | Eclipse | 5056.01 | 1 | Transit | 5231.01 | 1 | Eclipse | 5337.01 | 1 | Eclipse
4903.01 | 1 | Transit | 5057.01 | 2 | Eclipse | 5232.01 | 1 | Eclipse | 5338.01 | 1 | Eclipse
4909.01 | 2 | Eclipse | 5059.01 | 2 | Transit | 5235.01 | 1 | Transit | 5339.01 | 1 | Transit
4914.01 | 1 | Transit | 5060.01 | 1 | Eclipse | 5237.01 | 1 | Eclipse | 5340.01 | 1 | Eclipse
4917.01 | 2 | Transit | 5070.01 | 1 | Transit | 5240.01 | 1 | Eclipse | 5341.01 | 1 | Transit
4928.01 | 1 | Eclipse | 5075.01 | 1 | Transit | 5241.01 | 1 | Transit | 5342.01 | 1 | Eclipse
4929.01 | 1 | Transit | 5076.01 | 1 | Transit | 5242.01 | 1 | Transit | 5344.01 | 1 | Transit
4934.01 | 1 | Eclipse | 5079.01 | 1 | Transit | 5246.01 | 1 | Eclipse | 5349.01 | 1 | Transit
4935.01 | 1 | Transit | 5082.01 | 2 | Transit | 5248.01 | 1 | Eclipse | 5350.01 | 2 | Transit
4938.01 | 2 | Transit | 5088.01 | 2 | Transit | 5250.01 | 1 | Eclipse | 5354.01 | 1 | Transit
4941.01 | 1 | Transit | 5091.01 | 2 | Eclipse | 5251.01 | 1 | Eclipse | 5355.01 | 1 | Transit
4946.01 | 1 | Eclipse | 5092.01 | 1 | Transit | 5254.01 | 1 | Eclipse | 5357.01 | 1 | Transit
4947.01 | 1 | Eclipse | 5099.01 | 2 | Transit | 5259.01 | 1 | Transit | 5364.01 | 1 | Eclipse
4949.01 | 2 | Eclipse | 5100.01 | 2 | Eclipse | 5261.01 | 1 | Transit | 5368.01 | 1 | Eclipse
4950.01 | 1 | Transit | 5108.01 | 1 | Transit | 5263.01 | 1 | Eclipse | 5371.01 | 2 | Eclipse
4951.01 | 1 | Transit | 5109.01 | 1 | Eclipse | 5264.01 | 2 | Eclipse | 5375.01 | 2 | Transit
4960.01 | 2 | Eclipse | 5120.01 | 2 | Transit | 5266.01 | 1 | Eclipse | 5378.01 | 1 | Eclipse
5379.01 | 2 | Eclipse | 5404.01 | 1 | Transit | 5448.01 | 1 | Transit | 5505.01 | 1 | Transit
5383.01 | 2 | Transit | 5410.01 | 1 | Transit | 5472.01 | 1 | Transit | 5507.01 | 1 | Transit
5385.01 | 2 | Eclipse | 5412.01 | 2 | Eclipse | 5477.01 | 1 | Transit | 5510.01 | 2 | Eclipse
5386.01 | 2 | Eclipse | 5416.01 | 1 | Transit | 5483.01 | 1 | Eclipse | 5511.01 | 1 | Transit
5387.01 | 1 | Transit | 5417.01 | 1 | Eclipse | 5486.01 | 1 | Transit | 5512.01 | 1 | Transit
5388.01 | 1 | Transit | 5422.01 | 1 | Transit | 5496.01 | 1 | Transit | 5514.01 | 1 | Transit
5398.01 | 2 | Transit | 5427.01 | 2 | Eclipse | 5498.01 | 1 | Transit | 5518.01 | 2 | Transit
5398.02 | 1 | Transit | 5432.01 | 1 | Eclipse | 5499.01 | 1 | Transit | 5540.01 | 3 | Eclipse
5401.01 | 3 | Eclipse | 5438.01 | 1 | Transit | 5500.01 | 2 | Eclipse |  |  |

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