Proof of Lemma <ref>.
Assume that $p_{t}^{\texttt{cwg}} \leq q_{t}^{l}$, then according to the definition of $p_{t}^{\texttt{otg}}$ defined in Section <ref>, we have that $p_{t}^{\texttt{otg}} = q_{t}^{u}$. Compensation is provided only if $q^{\theta}_{t} \in [p_{t}^{\texttt{cwg}}, p_{t}^{\texttt{otg}}]$. Suppose that is the case, then we have that $F^{-1}((p_{t}^{\texttt{cwg}})^{+}) \leq \theta_{t} \leq F^{-1}(p_{t}^{\texttt{otg}}) = F^{-1}(q_{t}^{u}) = u_{t}$. The CwG policy would accept the candidate with ability $\theta_{t}$ since $\theta_{t} \geq F^{-1}((p_{t}^{\texttt{cwg}})^{+})$ where as the OTG would want to reject the candidate with ability $\theta_{t}$, because in the future it knows that it can select a candidate with ability at least $u_{t} \geq \theta_{t}$. Hence to persuade the OTG, we need to compensate it $u_{t} - \theta_{t} = F^{-1}(p_{t}^{\texttt{otg}}) - \theta_{t}$ and maximum compensation can hence be $F^{-1}(p_{t}^{\texttt{otg}}) - F^{-1}((p_{t}^{\texttt{cwg}})^{+})$. An analogous analysis can be done for the case when $p_{t}^{\texttt{cwg}} \geq q_{t}^{u}$ which follows similarly.


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The crosses $\times$ stand for the corresponding row/column not being allowed
to be colored. That there is in every part a fixed row/column (we always fix
the lowest row/rightest column) comes from the $-1$’s in the binomial
coefficients that we consider in the coefficient of $q^{N}$ in
$\zeta_{q}^{\mathrm{SZ}}(\mathbf{k})$.

###### Proof (of Lemma 4.10).

Considering the index of the first sum of the coefficient of $q^{N}$ in
$\zeta_{q}^{\mathrm{SZ}}(\mathbf{k})$, we get that it is just the number of
partitions of $N$ with exactly $r$ parts, every partition counted with the
respective multiplicity, given as the product of binomial coefficients we have
seen.

Now, given such a partition of $N$, the $j$-the part consists of $n_{j}$ rows,
why there are $\tbinom{n_{j}-1}{k_{j}}$ ways of marking $d_{j}$ of the rows of
the $j$-th part without the last one. Since those markings in every part are
independent of the markings in the other parts, this rows coloring gives a
multiplicity of

$\displaystyle\binom{n_{1}-1}{k_{1}}\cdots\binom{n_{r}-1}{k_{r}}$

of the given partition.

For the column markings we use similar arguments: Since the $j$-th part of the
Young diagram has length $m_{j}$ and the $(j+1)$-th has length $m_{j+1}$,
there are $m_{j}-m_{j+1}-1$ columns between the $j$-th and $(j+1)$-th corner,
counted from the right. Hence, with marking $d_{j}$ of them, we get an
additional factor $\tbinom{m_{j}-m_{j+1}-1}{d_{j}}$ for the multiplicity of
the given partition (for every $1\leq j\leq r$) and so exactly the coefficient
of $q^{N}$ of $\zeta_{q}^{\mathrm{SZ}}(\mathbf{k})$.∎

######  Remark 4.12.

By transposing Young diagrams together with the markings, we get a new
generating series of specific marked partitions. One can verify that this
generating series is the SZ-$q$MZV of SZ-dual index. Hence, using marked
partition, we deduce SZ-duality ([Bri, §4.2]).

###  4.3 BZ-model

For admissible
${\mathbf{k}}=\left(k_{1}+1,\\{1\\}^{d_{1}-1},\dots,k_{r}+1,\\{1\\}^{d_{r}-1}\right)$,
i.e., $k_{1},\dots,k_{r},d_{1},\dots,d_{r}\geq 1$, we compute

$\displaystyle\zeta_{q}^{\mathrm{BZ}}({\mathbf{k}})=\sum\limits_{\begin{subarray}{c}m_{1}>n_{1}>\dots>n_{d_{1}-1}>m_{2}>\dots\\\
>m_{r}>\dots>n_{d_{1}+\dots+d_{r}-r}>0\\\
j_{1},i_{1},\dots,i_{d_{1}-1},j_{2}\\\ \dots,i_{d_{1}+\dots+d_{r}-r}\geq
0\end{subarray}}$
$\displaystyle\binom{j_{1}}{k_{1}}\cdots\binom{j_{r}}{k_{r}}q^{m_{1}j_{1}+\dots+m_{r}j_{r}+n_{1}i_{1}+\dots+n_{d_{1}+\dots+d_{r}-r}i_{d_{1}+\dots+d_{r}-r}}.$

The coefficient of $q^{N}$ is the number of partitions of $N$, where some
(exactly $j_{1}\geq 0$) rows of the 1st, some (exactly $j_{2}\geq 0$) of the
$(d_{1}+1)$-th part in the Young diagram are marked and so on.

It is useful to avoid the partitions where some $j_{i}=0$ for clearness.
Hence, we introduce also markings of the columns of the Young diagrams as
follows:

######  Proposition 4.13 ([Bri, Prop. 4.19]).

The coefficient of $q^{N}$ in $\zeta_{q}^{\mathrm{BZ}}(\mathbf{k})$
corresponds to the number of partitions of $N$, where the corresponding Young
diagram is split up into $r$ sub-Young diagrams with at most
$d_{1},\dots,d_{r}$ parts each. We mark $k_{j}$ rows in the first part of sub-
Young diagram $j$ for each $1\leq j\leq r$. Furthermore, we mark all columns
containing corners and some of the others such that the number of colored
columns, only belonging to sub-Young diagram $j$, in total is $d_{j}$ for each
$1\leq j\leq r$.

###### Proof.

We obtain the split up into $r$ sub-Young diagrams by the first line of the
sum index of the coefficient of $q^{N}$. Also, the row markings are self-
explaining when looking at the summand of our coefficient of $q^{N}$.

The marked columns represent the indices (from right to left) of shape
$j_{\ell}$ and $i_{\ell}$. If a marked column is not the rightmost one of a
part, this corresponds to whether the corresponding multiplicity $i_{\ell}$ is
zero. In this case, there is no $n_{\ell}$-part in the partition, which is, on
the one hand, the reason for having exactly $d_{j}$ marked columns that belong
to sub-Young diagram $j$ for each $1\leq j\leq r$ and on the other hand, it is
the reason why we have at most (and not exact) $d_{i}$ parts in sub-Young
diagram $i$.∎

######  Example 4.14.

The following marked partition of $N=118$ has $r=2$ sub-Young diagrams and is
assigned to the index $\mathbf{k}=(3,1,1,1,3,1,1)$, i.e.,
$k_{1}=k_{2}=2,\,d_{1}=4,\,d_{2}=3$:

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Remark that $n_{3}$ occurs with multiplicity $i_{2}=0$, such as $n_{5}$ with
multiplicity $i_{5}=0$ which is the reason that the columns corresponding to
$n_{3}$ and $n_{5}$ respectively are marked but contain no corner of the Young
diagram.

The following statement is now equivalent to BZ-duality (see [Bri, §4.3]):

######  Theorem 4.15 ([Bri, 4.18]).

For all $r\geq 1$, $k_{1},\dots,k_{r},d_{1},\dots,d_{r}\geq 1$ and $N\geq 1$
we have:

$\displaystyle\sum\limits_{\begin{subarray}{c}m_{1}>n_{1}>\dots>n_{d_{1}-1}>m_{2}>\dots>m_{r}>\dots>n_{d_{1}+\dots+d_{r}-r}>0\\\
j_{1},i_{1},\dots,i_{d_{1}-1},j_{2},\dots,i_{d_{1}+\dots+d_{r}-r}\geq 0\\\
m_{1}j_{1}+\dots+m_{r}j_{r}+n_{1}i_{1}+\dots+n_{d_{1}+\dots+d_{r}-r}i_{d_{1}+\dots+d_{r}-r}=N\end{subarray}}\binom{j_{1}}{k_{1}}\cdots\binom{j_{r}}{k_{r}}$
$\displaystyle=\,$
$\displaystyle\sum\limits_{\begin{subarray}{c}m_{1}>n_{1}>\dots>n_{k_{r}-1}>m_{2}>\dots>m_{r}>\dots>n_{k_{r}+\dots+k_{1}-r}>0\\\
j_{1},i_{1},\dots,i_{k_{r}-1},j_{2},\dots,i_{k_{r}+\dots+k_{1}-r}\geq 0\\\
m_{1}j_{1}+\dots+m_{r}j_{r}+n_{1}i_{1}+\dots+n_{k_{r}+\dots+k_{1}-r}i_{k_{r}+\dots+k_{1}-r}=N\end{subarray}}\binom{j_{1}}{d_{r}}\cdots\binom{j_{r}}{d_{1}}$

Moreover, this is equivalent to the duality of Bradley–Zhao $q$MZVs.

###  4.4 Partition function, _q_ MZVs and conjugacy classes

When studying SZ-$q$MZVs and special values of them, we get a connection to
the partition numbers:

######  Lemma 4.16 ([Bri, Lem. 4.26]).

Let be $p_{N}$ the number of partitions of $N$, then

$\displaystyle\sum\limits_{r\geq
1}\zeta_{q}^{\mathrm{SZ}}(\\{1\\}^{r})=\sum\limits_{r\geq
1}\operatorname{g}\genfrac{(}{)}{0.0pt}{}{\\{1\\}^{r}}{\\{0\\}^{r}}=\sum\limits_{N\geq
1}p_{N}q^{N}.$

###### Proof.

The first equality is clear by the definition of bi-brackets. We consider now
the left side first:

$\displaystyle\sum\limits_{r\geq
0}\zeta_{q}^{\mathrm{SZ}}(\\{1\\}^{r})=\sum\limits_{r\geq
0}\sum\limits_{m_{1}>\dots>m_{r}>0}\frac{q^{m_{1}}}{1-q^{m_{1}}}\cdots\frac{q^{m_{r}}}{1-q^{m_{r}}}=\sum\limits_{r\geq
0}\sum\limits_{\begin{subarray}{c}m_{1}>\dots>m_{r}>0\\\
n_{1},\dots,n_{r}>0\end{subarray}}q^{m_{1}n_{1}+\dots+m_{r}n_{r}}.$

The coefficient of some $q^{N}$ here is the sum over all $r\in\mathbb{N}_{0}$,
where we sum the number of all partitions of $N$ with exact $r$ different
parts, i.e., the number of partitions of $N$, $p_{N}$.∎

The partition function also occurs in other contexts than $q$MZVs, namely when
considering equivalence classes of the symmetric group $\mathcal{S}_{n}$. For
more details, we refer to [FH, §4].

######  Lemma 4.17.

Partitions of $n\in\mathbb{N}$ and conjugacy classes of $\mathcal{S}_{n}$ are
in 1:1-correspondence. In particular, the number of conjugacy classes of
$\mathcal{S}_{n}$ is $p_{n}$.

###### Proof.

Write every $\sigma\in\mathcal{S}_{n}$ as union of cycles. The length of the
cycles form a partition of $n$. Since a conjugacy class $[\sigma]$ of
$\mathcal{S}_{n}$ is uniquely determined by the lengths of cycles of $\sigma$
\- conjugacy means only to rename the elements $1,\dots,n$, but not to change
the structure of $\sigma$ \- the claim follows.∎

######  Example 4.18.

The conjugacy class of $\sigma=(1\,4\,3)(2\,6)(5\,7)\in\mathcal{S}_{7}$
corresponds to the partition

$\displaystyle\ydiagram{3,2,2}\ \ \text{of }3+2+2=7.$

######  Remark 4.19.

Lemmas 4.16 and 4.17 give a remarkable connection between the number of
conjugacy classes of $\mathcal{S}_{n}$ and SZ-$q$MZVs. More precisely, fixing
$r$ and $n$, the coefficient of $q^{n}$ in
$\zeta_{q}^{\mathrm{SZ}}(\\{1\\}^{r})$ is the number of conjugacy classes of
$\mathcal{S}_{n}$ with cycles of exactly $r$ different lengths.

This remark should be the motivation for the following theorem:

######  Theorem 4.20 ([Bri, Thm. 4.30]).

Let $K$ be a finite field with $c$ elements. Then we have

$\displaystyle\mathrm{G}_{K}:=\sum\limits_{n\geq
0}a_{n,K}q^{n}=\sum\limits_{r\geq
0}(c-1)^{r}\zeta_{q}^{\mathrm{OOZ}}(\\{1\\}^{r}),$

where $a_{n,K}$ is the number of conjugacy classes of $\text{GL}(n,K)$ and
with $a_{0,K}:=1$ for every field $K$.

The proof can be visualized with marked partitions. For details and connected
results about several representations of the numbers $a_{n,K}$, we refer to
[Bri, §4.6].

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University of Cologne, Department of Mathematics and Computer Sciences

Weyertal 86-90, 50931 Cologne, Germany

E-mail address<EMAIL_ADDRESS>


Peel et al. SatHub

385 Astronomy and Satellite Constellations: Pathways Forward

10.1017/xxxxx

# Summary of SatHub, and the current observational status of satellite
constellations

Mike W. Peel1,2 Siegfried Eggl1,3 Meredith Rawls1,4 Michelle Dadighat1,5 Piero
Benvenuti1,6 Federico di Vruno1,7 Connie Walker1,5<EMAIL_ADDRESS>1\. IAU
Centre for the Protection of the Dark and Quiet Sky from Satellite
Constellation Interference, France.  2\. Imperial College London, Blackett
Lab, Prince Consort Road, London SW7 2AZ, UK.  3\. Department of Aerospace
Engineering/Department of Astronomy, University of Illinois at Urbana-
Champaign, Illinois, USA.  4\. Department of Astronomy/DiRAC/Vera C. Rubin
Observatory, University of Washington, Seattle, Washington, USA.  5\. NSFs
NOIRLab, Tucson, Arizona, USA.  6\. Emeritus, Department of Astronomy,
University of Padova, Italy.  7\. SKA Observatory, Jodrell Bank, Macclesfield
SK11 9FT, United Kingdom.

###### Abstract

SatHub is one of the four hubs of the IAU Centre for the Protection of the
Dark and Quiet Sky from Satellite Constellation Interference (CPS). It focuses
on observations, data analysis, software, and training materials to improve
our understanding of the impact of satellite constellations on astronomy and
observers worldwide. As a preface to more in-depth IAUS385 sessions, we gave a
summary of some recent work by SatHub members and the current status of
satellite constellations, including optical and radio observations. We shared
how the audience can join or get more involved, e.g., via the CPS Slack for
asynchronous collaboration. We also touched on what a future with hundreds of
thousands of constellation satellites might look like.

###### keywords:

SatHub, satellites

††editors: P. Grimley, eds.

##  1 Introduction

SatHub is part of the International Astronomical Union (IAU) Centre for the
Protection of the Dark and Quiet Sky from Satellite Constellation Interference
(CPS). It is a public, community driven, coordinated hub focused on the
collection and analysis of artificial satellite observations, as well as
carrying out training and outreach related to satellite constellations. It was
formed following the recommendations from SATCON2 (Rawls et al.,, 2021), and
adopted the outline structure established in that report, see Fig. 1. SatHub
is still under construction, and has built-in flexibility to change and evolve
based on community feedback and needs.

Figure 1: SatHub outline from the SATCON2 Observations Working Group (Rawls et
al.,, 2021).

SatHub is co-led by three people: Meredith Rawls (University of Washington,
WA, USA; remote attendee of IAUS385); Mike Peel (Imperial College London, UK;
in-person attendee); and Siegfried Eggl (University of Illinois at Urbana-
Champaign, USA; in-person attendee). In addition, Michelle Dadighat (NOIRLab,
in-person attendee) is a software engineer working on SatHub software
development.

##  2 Software development

A central part of the work of SatHub involves software development to make it
easier to identify, avoid, and remove satellites from astronomical
observations across the electromagnetic spectrum. Software development is
actively underway, and we have marked in the section below where things are
already working well / up-and-running as “done”; in development as
“developing”; and still in need of doing as “to be done”.

###  2.1 Data repository and exchange

One of the primary purposes of SatHub is to serve as a Hub for Data Exchange
from brightness measurements. This will be a central place where data can be
deposited and exchanged with others. Such a system needs to be publicly
available, easily accessible, user-friendly, and well documented.

The repository will enable the submission and retrieval of satellite
brightness measurements (made visually by eye, observed with optical
telescopes, etc.; developing); collections of optical/near-IR images with
satellite streaks (developing); spectra contaminated with reflected solar
spectrum (to be done); and radio data affected by satellite interference (to
be done).

We already welcome contributions from everyone who is willing to share
observing campaign plans and data. We aim to have easy-to-use interfaces for
both professional and amateur astronomers to upload and download satellite-
affected images (developing). Software developers/contributors are welcome to
contact us to help with this work!

###  2.2 Orbital solutions portal

A critical need for astronomy is high accuracy predictions of where satellites
will be seen from any observatory around the world, which we aim to enable
through the Orbital Solution Portal. This will provide public, standardised
access to orbital solutions of artificial satellites. NOIRlab has recently
hired a software developer (Michelle Dadighat) to work with SatHub on this and
other tools.

The portal will convert general perturbation-style two-line element (“TLE”)
solutions to on-sky positions, with automatic synchronisation with
complementary services and databases (done). It is updated every 8 hours for
Starlink satellites, with others updated every 24 hours (due to the
availability of published TLEs). It will include error bars with all orbital
solutions (developing), and have built-in robustness by using multiple backend
systems to provide TLEs and position predictions
(CelesTrak111https://celestrak.org/, Privateer222https://www.privateer.com/,
etc.; developing). Ultimately it will include the full history of all TLEs, so
positions can be predicted for any satellite at any time, which is critical
when analysing archival and long-duration survey data (to be done; funding
applied for).

At present we have a prototype SatChecker that does some of
this333https://satchecker.readthedocs.io. We welcome contributions to this
work. In particular, we need industry to cooperate and share the highest
accuracy orbital information about their satellites in a timely, regular
manner. We also need astronomers to check that orbits are accurate by
observing and measuring satellites, and reporting inaccuracies back to us and
to industry.

###  2.3 Other software tools

In addition to the two key tools above, we are also working on other tools, as
described in the SATCON2 report (Rawls et al.,, 2021). We aim to make sure
that all software tools have user-friendly documentation, support, and are
actively maintained (developing). In addition, we plan to have a standard test
suite supporting a wide range of instrument and satellite signature properties
to support software development (to be done).

We encourage contributions to open-source software development, particularly
through the tools developed within CPS. We also want to test the software with
data from many different telescopes and cameras. We are looking for funding to
work on software development.

In addition to software developed within CPS, we are also seeking to
understand existing tools and their availability, so that we can reduce
duplication and avoid recreating what already exists. SatHub is running a
software survey444https://forms.gle/FzkT1FekoVb2Fxqi6, with one submission per
tool requested. Tools inputted into this survey before and during IAUS385 were
then discussed and worked on at the SatHub hackathon on the last day of the
symposium.

##  3 Real-time collaboration

SatHub is working on establishing communication and collaboration across the
astronomy community about satellite constellations in an open and
collaborative way. We mostly do this through the IAU CPS Slack, which all
members of CPS can access, with the main #sathub channel and a host of sub-
channels on specific topics (for example, #sathub_optical_observing).

We also have a SatHub GitHub organisation555https://github.com/iausathub,
which anyone can use to share open-source code, and we encourage documentation
that follows “Write the Docs”666https://www.writethedocs.org/ best practices
(developing). We plan to have a website that will direct to new and existing
resources (to be done).

We offer a paper review process, which provides free peer reviews within two
weeks for satellite-related papers. The aim is to provide feedback from peers
who are also working on satellites within CPS, to ensure accuracy and
connections between publications produced by different groups. The reviews are
carried out by CPS members, for CPS members, and while being a member is not
strictly required to use this service, we encourage everyone interested in the
topic to join CPS. Papers that have gone through this peer review process can
include CPS as an affiliation and acknowledgement. A recent example of a paper
that has gone through the process is Mallama et al., (2023). We are currently
working on documenting the process, to be published soon on the CPS website.

##  4 Potential impact at radio frequencies

As well as optical reflections, satellites actively transmit at radio
frequencies. We don’t yet have a complete picture of the impact that radio
transmissions from satellite constellations will have across the full
frequency range used by radio astronomy, and we need observations to assess
actual impact. Various talks at IAUS385 covered this topic, and are described
later in this Proceeding.

Satellite constellations actively transmit at radio frequencies to provide
internet connectivity services. This is currently at $\sim$10–20 GHz
(12.7–14.7 GHz for Starlink, others use different frequencies), various
satellite constellations are looking at using higher frequencies for higher
bandwidth in the near future ($\sim$40–200 GHz). Typically there are also
octaves of radio emission at, e.g., 2$\times$ the base frequency (or even 3,
5, 10$\times$ etc.), which can also impact radio astronomy since the main
signals are so bright. In addition, telescopes are not only sensitive to the
direction they are observing, but also to other directions through sidelobes
(reflections from different parts of the telescope other than the main
mirror). If these couple to satellite transmissions, this can be a concern,
particularly for CMB experiments who are mapping large angular scale emission
and could see interference over large parts of the sky away from the satellite
positions. This can be seen in data from the QUIJOTE MFI instrument (Rubiño-
Martín et al.,, 2010, 2023, Génova-Santos in prep.) in 2012 observing at 10–14
GHz (Fig. 2), where geostationary satellites appear as bright as the Sun, and
sidelobes were also initially visible—these were later avoided by adding
additional baffles around the telescope aperture.

Figure 2: QUIJOTE local map of the radio sky above Tenerife, with relevant
features highlighted. Geostationary satellites appear as a band across the
sky, similar in brightness to the Sun (top of the image), and also appearing
in telescope sidelobes in the bottom half of the image.

At lower frequencies ($\sim$100-200 MHz), unintended emission has been
observed by LOFAR (Di Vruno et al.,, 2023) and SKA low (Grigg et al.,, 2023).
This emission comes from the electronics on board the satellites, and was not
foreseen by the satellite operators before being detected by radio telescopes.

The types of detectors used in radio telescopes, particularly at high
frequencies, can make it difficult to filter out satellite emission.
Radiometers require FPGAs rather than broad-band detectors to be able to
excise frequencies affected by interference - and these are much more
expensive than simple detectors. At high frequencies ($>$30 GHz),
superconducting detectors like Transition Edge Sensors (TESs) and Kinetic
Inductance Devices (KIDs) are inherently broad-band and can only have optical
filters to remove unwanted emissions - mainly high and low-pass filters that
define the overall bandwidth. In such systems, interference can only be
removed by flagging the time-ordered data.

Figure 3: Observations of Starlink with a satellite dish in 2022,
demonstrating broad bandwidth and high variability, courtesy of F. Di Vruno.

In addition, satellite emission can be highly variable (see Fig. 3), both
because of their high angular velocities, and because they can be changing
transmission direction, e.g., using phased arrays. It is important to
accurately know satellite positions, otherwise such emission could be mis-
identified as transient astronomical signals.

##  5 Observing campaigns

SatHub runs observing campaigns for specific high-importance satellite
constellation launches, such as a the launch of a new type or generation of
satellite. A strength of SatHub is our ability to recruit observers from
across the globe with a wide variety of expertise to assemble a more complete
picture of how a satellite or constellation of satellites is affecting the
sky.

###  5.1 BlueWalker3

AST BlueWalker 3 is a prototype satellite that was launched in 2022 to test
direct connectivity between satellites and unmodified mobile phones. To do
this, it uses a 64 m2 phased array that was folded on launch and deployed in
orbit. Already bright after launch, the satellite became one of the brightest
objects in the sky once unfolded (Fig. 4), and is also large enough to be
imaged from the ground (Fig. 5 777https://www.astrobin.com/tffts1/
888https://noirlab.edu/public/images/ann23027b/ ). The launch vehicle adapter
was also bright, and initially untracked with public TLEs. In addition, we
demonstrated that the position accuracy decays between releases of TLEs,
highlighting the importance of regularly releasing updated TLEs.

Figure 4: Brightness of BW3 over time, from Nandakumar et al., (2023). The
first dashed vertical line shows the point where BW3’s phased array was
deployed and the satellite became exceptionally bright. Figure 5: Image of
BlueWalker 3 in orbit by M. Tzukran (CC-BY-4.0)

The observing campaign was published in Nature (Nandakumar et al.,, 2023),
with an online
announcement999https://noirlab.edu/public/announcements/ann23027/. The
announcement included a video of BW3, as well as Starlink satellites, as they
transited the sky—showing how bright BW3 was compared with Starlink satellites
and nearby stars.101010https://noirlab.edu/public/videos/ann23027a/

###  5.2 Ongoing

Starlink started launching its Generation 2 mini satellites in 2023. These
have optical mitigations using Bragg
mirrors111111https://api.starlink.com/public-
files/BrightnessMitigationBestPracticesSatelliteOperators.pdf, and CPS seeks
to quantify how well these mitigations have worked. Early observations
indicate mixed results so far, with some satellites being faint, but some
remaining bright. This is concerning as the full Generation 2 satellites will
be bigger than the minis (which were downsized to fit into the Falcon 9
launcher), and potentially will be correspondingly brighter. The results of
the observing campaign are planned to be published in early 2024.

Observations are also continuing of BlueWalker 3, using SCUBA2/JCMT to observe
the satellite (and also the International Space Station) at submm wavelengths,
to see how thermally bright the satellites are. The observations were recently
approved, and will start shortly; if successful these will lead to future
observations of smaller satellites such as Starlink and OneWeb.

We are also preparing for other observing campaigns in the future, for
example, of the Amazon Kuiper satellites. Participation in, and ideas for,
observing campaigns are very welcome.

##  6 Get involved

SatHub needs the help of everyone interested in the impact of satellite
constellations on astronomy. We are seeking sky observers, data analysts,
software developers, industry experts, students, and others to help with this
work. Additionally, as the satellite population changes, the evolving impacts
that this will have on astronomy require ongoing observer-operator dialogs.
Information in SatHub will be public, open, and accessible to support real-
time collaboration. We aim to join innovation with existing solutions,
prioritize ease of use, and enable coordination among multiple stakeholders.

To contribute to SatHub, first of all, join CPS! After that, join the SatHub
channel at the CPS Slack, which is where most of the discussions take place.
Please also share your observations, experience, relevant code and work plans
with us, and contribute to open-source software and documentation development!
There are no requirements, prerequisites, or fees for membership—you just have
to follow our collaboration
agreement121212https://docs.google.com/forms/d/e/1FAIpQLSe6w5rZhxvF0ozGe1dMssLTolua1Apq1_QjJ8aLWprGUGQGog/viewform
and our code of conduct131313https://tinyurl.com/IAUCPSCoC. You can apply for
membership at https://cps.iau.org/.

## Acknowledgements

MP, SE, MD acknowledge travel funding from IAU CPS to attend IAUS385.

## References

  * Di Vruno et al., (2023) Di Vruno, F., Winkel, B., Bassa, C. G., Józsa, G. I. G., Brentjens, M. A., Jessner, A., & Garrington, S. 2023, Unintended electromagnetic radiation from Starlink satellites detected with LOFAR between 110 and 188 MHz.  Astronomy & Astrophysics, 676, A75.
  * Grigg et al., (2023) Grigg, D., Tingay, S. J., Sokolowski, M., Wayth, R. B., Indermuehle, B., & Prabu, S. 2023, Detection of intended and unintended emissions from Starlink satellites in the SKA-Low frequency range, at the SKA-Low site, with an SKA-Low station analogue.  Astronomy & Astrophysics, 678, L6.
  * Mallama et al., (2023) Mallama, A., Hornig, A., Cole, R. E., Harrington, S., Respler, J., Lee, R., & Worley, A. 2023, Assessment of Brightness Mitigation Practices for Starlink Satellites.  arXiv e-prints,, arXiv:2309.14152.
  * Nandakumar et al., (2023) Nandakumar, S., Eggl, S., Tregloan-Reed, J., Adam, C., Anderson-Baldwin, J., Bannister, M. T., Battle, A., Benkhaldoun, Z., Campbell, T., Colque, J. P., Damke, G., Plauchu Frayn, I., Ghachoui, M., Guillen, P. F., Kaeouach, A. E., Krantz, H. R., Langbroek, M., Rattenbury, N., Reddy, V., Ridden-Harper, R., Young, B., Unda-Sanzana, E., Watson, A. M., Walker, C. E., Barentine, J. C., Benvenuti, P., Di Vruno, F., Peel, M. W., Rawls, M. L., Bassa, C., Flores-Quintana, C., García, P., Kim, S., Longa-Peña, P., Ortiz, E., Otarola, ., Romero-Colmenares, M., Sanhueza, P., Siringo, G., & Soto, M. 2023, The high optical brightness of the BlueWalker 3 satellite.  Nature, August 2023.
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  * Rubiño-Martín et al., (2023) Rubiño-Martín, J. A., Guidi, F., Génova-Santos, R. T., Harper, S. E., Herranz, D., Hoyland, R. J., Lasenby, A. N., Poidevin, F., Rebolo, R., Ruiz-Granados, B., Vansyngel, F., Vielva, P., Watson, R. A., Artal, E., Ashdown, M., Barreiro, R. B., Bilbao-Ahedo, J. D., Casas, F. J., Casaponsa, B., Cepeda-Arroita, R., de la Hoz, E., Dickinson, C., Fernández-Cobos, R., Fernández-Torreiro, M., González-González, R., Hernández-Monteagudo, C., López-Caniego, M., López-Caraballo, C., Martínez-González, E., Peel, M. W., Peláez-Santos, A. E., Perrott, Y., Piccirillo, L., Razavi-Ghods, N., Scott, P., Titterington, D., Tramonte, D., & Vignaga, R. 2023, QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20 GHz with the multifrequency instrument.  MNRAS, 519(3), 3383–3431.
  * Rubiño-Martín et al., (2010) Rubiño-Martín, J. A., Rebolo, R., Tucci, M., Génova-Santos, R., Hildebrandt, S. R., Hoyland, R., Herreros, J. M., Gómez-Reñasco, F., Caraballo, C. L., Martínez-González, E., Vielva, P., Herranz, D., Casas, F. J., Artal, E., Aja, B., Fuente, L. d., Cano, J. L., Villa, E., Mediavilla, A., Pascual, J. P., Piccirillo, L., Maffei, B., Pisano, G., Watson, R. A., Davis, R., Davies, R., Battye, R., Saunders, R., Grainge, K., Scott, P., Hobson, M., Lasenby, A., Murga, G., Gómez, C., Gómez, A., Ariño, J., Sanquirce, R., Pan, J., Vizcargüenaga, A., & Etxeita, B.  The QUIJOTE CMB Experiment.  In Highlights of Spanish Astrophysics V 2010,, volume 14 of Astrophysics and Space Science Proceedings, 127.