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Okay, let's begin. Hi, everybody, and
welcome to this PSM two session. Today

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we're going to be talking about dark
sectors. And our first talk is from Brian,

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who will give us the theoretical
background to this, all of the talks today

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will be 15 minutes, they'll have a three
minute time for questions afterwards. And

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if we have a little time left over at the
end, we can discuss with all the panelists

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then. So I'm fine, feel free to get
started.

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Thanks very much for inviting me. And
thanks to the organizers for organizing

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this wonderful online meeting. So I have
the tall task of giving an overview of

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hidden sector theory in 15 minutes. So
let's get started. So the reason why we

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believe in the existence of hidden sectors
and why all of the impressive searches

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that you're seeing presented this
conference are taking place is because of

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a bunch of things that we don't
understand, that can't be explained by the

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standard model. These are of course,
questions of dark matter. The origins of

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the matter antimatter asymmetry, and also
neutrino oscillations. And in each of

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these cases, the evidence is pointing
towards new particles and interactions

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that are very weakly coupled with the
standard model. And also where the new

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particles and forces responsible for this
phenomena could happen at really any mass

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scale ranging from Evie up to maybe the
guts scale and beyond for some of these

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interactions. And so it gives us a rich
array of kinds of theories that we should

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be trying to study in whatever experiments
we have. And as I'm sure you're all aware,

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there's a proliferation of theories of
hidden sectors and what they could do. So

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one of the pictures I tried to keep in
mind when trying to make sense of this

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really extensive set of interactions that
could be out there is to try and think

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about terms of the signatures, how can I
organize them and maybe group them into

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categories and I think tried to do that
here by adopting, perhaps an organization

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scheme that we've seen before and for
instance, tried to tackle Susie or there

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is a strong dynamics in terms of trying to
come up with what are the irreducible non

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logical features of the theory? And how
can we look for those. And the simplest

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place to start is a theory with a single
particle and some relatively well

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prescribed set of interactions. And these
are the things that have become sort of

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the canonical example so far kinetically,
mixed dark photon, singlet scalar that

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mixes the Higgs sterile neutrino and so
on.

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And for the most part, we have a pretty
good understanding of what these look like

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how we can look for them. And there's a
robust search program to look for those,

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we can then move beyond this single
particle and imagine what happens if I

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have say, two particles that I connect and
suddenly the array of signatures becomes

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much more vast because I have for
instance, a different possible production

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mechanism. From decay mechanism so for
instance, I could make dark Higgs is from

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the decay of a vector and then you know,
the the decay comes through the scalar

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mixing or vice versa. And so suddenly we
have a different range of production,

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cross sections, decay mechanisms,
lifetimes, and so on. And in many cases,

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more becomes a very different. So it's not
just like, Oh, I got different, a few

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different signatures, all of which will
look similar to the single particle cases.

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But in many cases, the single particle
signatures go away and I got some new

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ones. And this goes all the way up to a
more complicated code complete model,

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which could have, you know, a set of 10s
or hundreds of particles. And this could

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lead to very sophisticated things like
showers and things that reproduce features

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from the standard model. And so I think
what we want to do is March from the

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simpler examples that we've been looking
at towards these more complicated ones.

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And of course, There are many ways that we
can move forward. And I hope to talk about

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just three of these today, or at least you
touch on what I think some of the

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interesting directions are. And then
hopefully, those of you who are

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experimentalists looking for something to
do. If you're bored, you can follow some

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of the references or Google some of these
ideas and see what, what more we could be

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doing. And I've kind of grouped these
roughly under sort of non minimal

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couplings meaning coupling patterns that
deviate from the canonical examples of

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dark photon dark Higgs, etc. Non
thermodynamics So, this specifically is

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interesting from the point of view of dark
matter, but, you know, we have a well

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prescribed Dark Matter program at the
Elysee. And this is of course, predicated

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on a specific thermal history in a
specific way that those particles are

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making dark matter and if you change
those, then you change maybe the

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phenomenological signatures and coupling
ranges that are of interest. And then

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finally, what happens if we move to words
Non perturbative are many body signatures,

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right? Got lots of new states showing up
like confining sectors and dark showers.

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So let's start with the non minimal
couplings and your sense of what I mean.

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So if you think about dark photons, or
dark scalars, these couple, the same way

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as regular photons are the standard model
takes just time some small overall mixing

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factor. And as we will see some of the
talks to come. There's really impressive

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coverage that's beginning to take shape
for many of these signatures. And we

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haven't seen any evidence yet, so we're
just piling up more and more constraints.

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And these usually come from the coupling
of the dark photons that are scalars to

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standard model particles that are easy to
access and experiments like coupling to

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electrons or coupling the top quarks. At
the same time as we continue to improve

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our exclusions there are anomalies and
hints of new things that continue to

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accrue. So for instance, new on G minus
two is a persistent discrepancy with the

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standard model. There are, of course, the
anomalies in electronic similar time. BDK

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is possible upon flavor stuff going on
there. The Koto anomaly is a new thing of

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the past year, and so on. And if we want
to try and accommodate one or more of

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these within the standard framework, this
is often excluded in the minimal case. And

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so the workaround for this is to just say,
well, let's just shut off this most

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important coupling that's often used to
constrain these new particles. And this

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can weaken the constraints on the models
and potentially open up the viability in

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terms of explaining some of these
examples. And we'll talk about one

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scenario, which is something that I've
worked on in terms of searches with a bar

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experiment, which is what I call
electrophilic scalar. So it's a scalar.

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The couple's masks unfortunately, just
like the Higgs, but a couple's

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predominantly to leptons, as opposed to

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And this was shown recently that it could
potentially, for instance, simultaneously

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explain the new g minus two and the Koto
anomaly. But if we look at this plot on

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the lower right, if you ignore the green
curve, which is what the experiment just

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recently did, actually, most of them
laundry minus two parameter space was open

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and really uncovered. And so what we did
was we did a search where the dominant

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production mode of this is not going to be
directly off of the electrons but off of

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final state radiation from towers, which
which it has the largest coupling and then

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it will decay and to save your lines or
electrons. And this requires doing a

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search at finite lifetime. So, we're sort
of having to bring in a lot of different

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interesting modules initially of hidden
sectors. And the short version is we

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didn't see anything, and we exclude this
whole green region which greatly

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eliminates the view on T minus two
parameter space below the top shot. And

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this is interesting both because it shows
the power that a single search can have to

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improve our sensitivity. But also the fact
that, you know, the sensitivity dies off

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as soon as the thing starts decaying into
Taos as well. And so if we have a

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completely tau philic scalar, there's a
lot of open parameter space. So this might

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be a zooming in for our attention, as you
know, are there ways that we can try and

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access this parameter space? So what are
some things that I think are open

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opportunities with respect to these non
mental couplings? Like I said, I think

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Catholic forces things a couple probably
to nuance as opposed to electrons are a

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major gap and possible explanation and
being rungy minus two particularly below

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the diamond threshold and at high masses.
So in the Atlas CMS range of interest, and

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also accent like particles, which are
particles that coupled predominantly to

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pairs of gauge bosons and photons,
electric boat, those odds include bonds

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and so you know, While we should continue
to press ahead on these minimal scenarios,

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we should also see if there's something
hiding in some of these other cases. What

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about if we changed the dynamics in the
early universe are we consider different

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types of ways of explaining Dark Matter
abundance. Until recently thermal freeze

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out which is the mechanism for explaining
the dark matter, abundance and rent models

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was the major way of thinking about how we
come about dark matter abundance. But as

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we know, we have not seen any positive
signals in wimps searches nor in you know,

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some searches for lighter versions of
thermal dark matter and indirect detection

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and direct detection, so on.

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And so we can wonder, well, is this the
actual way the dark matter is determined

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and the answer is maybe not. So as soon as
we have multiple component hidden sectors

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with mediators and dark matter particles
with different masses and couplings, we

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can actually get a very wide range of
subjects very creatively named, dark

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matter things. So there were so many
references here, I couldn't fit them on

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the slide. But if you just Google any of
these, I guarantee that things will pop

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up. But it's probably the easiest way. So
if you're ever bored and depressed, that

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we haven't found dark matter, just look up
some of these and get some sense of how

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rich, docile Dark Matter dynamics can be.
I'm going to talk about a variant which is

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pretty simple, but it's called freezin.
And it's a scenario where the dark matter

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is so weakly coupled, that it never comes
into equilibrium is never abundantly

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produced in the early universe. And in
these cases, dark matter is just produced

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from the decay of some scalar that carries
Standard Model charge, for instance, and

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you just accumulate Dark Matter slowly
over time. And as the temperature of the

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universe evolves, and as we go through
time, you make it and then at some point,

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you stop making it it just happened
amount, and you can calculate how much

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that amount is and it's roughly this given
by the bottom of screen and you can see

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that for kind of reasonable masses, you
get very tiny couplings or 10 to the minus

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eight. So this can be interesting
predictions along with particle

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signatures. And this is kind of come back
into vogue recently because it's

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relatively untested type of dark matter
scenario. I've become interested in AI

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recently because it turns out that this
same interaction, if you have two or more

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dark matter particles, can also give you
the matter antimatter asymmetry almost for

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free with similar kinds of couplings. But
over a much more constrained parameter

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space, it's actually quite testable. So
over here on the left shows the mass of

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this scalar, which carries Standard Model
charges and the lifetime and you can see

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that in order to get the bearings and do
the work, which is in these shaded

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regions, you actually have to have the
scalar be within kinematic range vhc. And

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in the lifetime range, it's also an
interest for different sector searches.

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And so we got, for instance, cares of lung
lip particles, each of which decays to a

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single standard model particle plus mad.
And so this is, could be a clear signature

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of both the dark matter production as well
as a matter antimatter asymmetry coming in

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one bundle. And this is the only way the
freezing could happen. For instance,

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instead of having a TV scale Meteor, we
could have a low mass and the leader like

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a dark photon, there's recently been a lot
of theoretical work that's been going into

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calculating what's going on in the early
universe plasma effects that are relevant

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at those scales. And this has been opening
up some parameter space for Dark Matter

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also in the kind of K 10s of k v to
hundreds of k v scale, the producer very

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different mechanism, predicting new
signals inferences, direct detection

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experiments, astrophysical probes,
cosmology and so on. So by tricking our

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our prejudice or our views of what Dark
Matter could be and how its produced we

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also expand our range of phenomenological
probes. Within the last couple of minutes,

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I want to touch briefly on the non
perturbative in many body signatures,

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which is Not gonna be super extensive
because this is still a relatively

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emerging field. But in these scenarios,
you might consider our hidden sectors

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where the dark matter carries some charge
under a dark confining force, and so it

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undergoes apart on shower, and then hunter
ization much like you see. And in these

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scenarios, the dark hadrons can decay
properly or long lived. And because we

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don't know anything about this dark,
confining forest, the shower properties

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are unknown. And they could range anywhere
between the jet like features like we see

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in the bottom left, or we could end up
with something that's very kind of

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isotopic radiation patterns that you see
on the right. Then, of course, there's an

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open question about well, if I change the
knobs of the theory, do I move smoothly

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from the picture on the left to the right,
you know, do it go through some

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interesting intermediate phase? And this
is hard to answer theoretically because of

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the non perturbative nature. So, you know,
this is a new area of experimental study.

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There's, as far as I'm aware, one public
was often seen So we know that Atlas is

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working on

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a search for similar kinds of models,
these so called a virgin jets with long

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lift, two K's of these dark hadron. So
this shows that it is feasible. And it's

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interesting and that we need to do better
to understand it for theoretically and in

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terms of experimental sensitivity. And
just in the past month, there's been

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several papers that have come out that
have investigated for instance, new events

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shape variables that are kind of like
thrust, or they're based on something

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called the energy movers distance that can
distinguish a digest sample from isotropic

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distributions that have different numbers
of particles per events ranging from 10 to

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50. And you see that they're all separated
from one another, as well as new

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applications of jet substructure variables
like energy correlation functions that can

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be used to distinguish QED showers from
these dark showers. This is very much an

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early stages and so it's a great
opportunity for new theory and

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experimental development. So I'm out of
time So we'll leave it here. I think that

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to the sector's there's been a really
impressive development and search program

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for them. And we still have a lot of
interesting things to look at the LFC has

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a really important role to play and
testing, particularly sort of Hidden

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Valley scenarios or scenarios where you
have a heavier mediator relative to other

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lower energy experiments. And stay tuned
because we have three great talks that are

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going to show just some of the exciting
results from these efforts.

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Thanks a lot, Brian. That was both a
fascinating talk and on time to within

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plus or minus one second. So I have any
questions from the attendees, the other

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speakers, use the raise your hand option
zoom will be able to unmute you.

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Go ahead, Mary.

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was wondering if you could say a few more
words about the energy movers distance and

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what it is exactly. This new variable?

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Yeah, so I was not involved in this. So
I've only kind of glanced at the paper.

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But I think the rough idea is, so it's
based on something called the Earthmovers

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distance, which is a problem in computer
science, which is that if I have two

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distributions of masses in space, and you
can ask what's the minimal way that I can

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rearrange math so that I moved from
pattern age to pattern B. What this

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variable does is it compares a particular
event which has some distribution in phi

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and pseudo rapidity. And then it asks if
this were a purely isotopic event, I can

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compare those two pictures and what's the
minimum amount of energy that I have to

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expend to change one to the other. And the
paper goes into great detail of how they

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define exactly the waiting and the metric
of this but the rough idea is that if it's

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already isotopic, you don't have to
rearrange the events at all. And so it has

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a very small energy movers distance
whereas if it's a diner Like then you have

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to expend a lot of this normalized.

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interest, just for my understanding on
this plot as well. I was curious about it

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to the end in this case is the number of
initial particles you have creating the

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energy distributions you're looking at,
or?

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Yeah, so this was a, I picked this one
because it kind of showed the the most

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distinguishing power even though it's
perhaps a little bit of an artificial

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setup, we're basically out there saying,
I'm not going to go into the details of

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the model, I'm just going to generate
events that have kind of isotropic ish

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distributions of say, 50 particles
compared to say QC D digest events. And

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the remarkable thing is that so if for
instance, you showed the corresponding

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plot for thrust, which if you look at the
paper, it's there or some other events,

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shape variables, it's hard to distinguish
the 1025 and 50. You can distinguish maybe

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the From QC dB, you can't tell them apart.
Whereas this is really sensitive to like

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how many particles Do I need to rearrange?

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testing? we maybe have time for one more
question for Brian. What else hustler?

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Okay, in that case, thanks again. This was
very interesting. And let's move on to our

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next speaker, which I believe is
Constantine