>>
Shall we start?
OK.
Good afternoon.
Welcome to voices from
the community Town Hall.
My name is Joel Butler from Fermilab
and I'm DPF vice chairperson
and I will be your host.
We have an exciting agenda of 22 talks, each of 3 minutes duration.
This is the last session of the day
of talks, panels, goals,
broad visions, regional plans
, plans from related fields
and thoughts from funding agencies.
These visions and goals are constructed by researchers
from all over the world working on many scales, large and small
in particle physics and related areas.
We are presenting here a representative sample
of these efforts demonstrating the vibrancy
of our field
and our commitment
to expanding its diversity
and equity.
We hope you enjoy these brief talks
whose duration, we remind the speakers,
will be strictly enforced.
We will not be able to accept questions during this session
but the Slack channel plenary voices from the community
is available
for questions and discussions and we encourage the speakers to engage
with you after the session.
I think now we can go to the first speaker,
who is mainly
mainly Sanchez, who will be talking
about ANNIE and the future of hybrid neutrino detectors.
>>
Can you hear me?
Can I share my video?
>> Please go ahead
and try to share
your video.
>>
I think that worked.
>>
Hold on a second and we will advance to the next
slide.
>>
Thank you for having me.
I would like to talk to you about
ANNIE
.
There is a broad community address in the development of these detect
as which by using
water-based liquid
synthesizer
or slow
scintillation
increasing the coverage of LACCD
detection capability.
Is a critical step toward
ANNIE, and neutrino experiment
set to take physics
data
on the neutrino bean and it will measure the neutron yield
using a target of 30 tons
of
(unknown term) loaded water
.
ANNIE is an R&D platform
for neutrino
detection technologies and we are currently deploying the first
step of five large area
detectors
which you can see on
this slide.
The experiment to a preliminary neutrino data in 2020 is expected to
run from 2020 to 2022
whether unique mix of interesting physics goals
and R&D, it is an excellent opportunity to train and develop
early career physicist.
In the next phase
, (unknown term)
aided
by
word
allow
a better understanding of the final state neutron
energy spectrum
and additional
LA PPD would meet
multitrack feeding
in
multi-directions
.
With this addition, ANY
could be the first step in a series of detectors using
technologies
and we believe it is a criminal step
toward
demonstrating the power of these hybrid detectors.
It could be used as a
new generation of experiments
that are at the same time
observatories for low energy
neutrinos.
We hope to see support for this approach out of Snowmass
and if you are interested to work on this and no more
, reach out to us.
Thank you.
>>
The next speaker
is (Unknown name)
and he will be telling us about
determining
KV range superlight
dark matter using graphene
Joseph
injunction.
>>
Can you hear my voice?
Good afternoon.
My name
is (Unknown name), the idea
I would like to share with you today
is
new dark matter direct detection matter
using the state of our
recognition
(inaudible)
technology or the GJ J
device
, which would enable us
to improve
KV
range
, dark
matter in the near future.
The working principle
of a GJ J
devices schematically depicted
in panel A of the left figure.
The energy interacts with the free electrons on the breaking layer
and raises the electron temperature.
And then the effect
can switch
the zero
voltage
to
resistive state
with an appropriate level
of current
.
It was recently demonstrated in the lab
that the devices are accurate 2.1
that the devices are accurate 2.1 million electron
deposit
.
This sensitivity can be translated
2.1 KV
in the language of the dark matter mass.
Inspired by
these low
energy thresholds that we have proposed,
novel and possibly tabletop
experiments to detect satellite
dark matter
superlight
dark matter.
The proposal is shown in panel B
in the left figure
and a bigger scale
detector
could be built by stacking up the single-layer units.
Interestingly,
the calculation involves capturing dark matter
floating in the three-dimensional space and free
electrons confined in
two-dimensional grapheme
.
It depends on the dark matter direction, the supposed
detector can readily
check the
directional dependence of the signal.
We study
the
are...
Together with a one-year exposure.
The right figure
shows the result
.
We found that GJ J
dark matter
detector can improve the search limit of the dark matter mats might
three orders of magnitude over the existing bounce represented
by the gray shaded area.
Encouraged by this result,
we are now preparing
for the first
KV
scale
using the
sample
devices
that are already fabricating.
Finally,
we are going to
use high energy applications
, low sensitivity of the JG G
devices,
on the neutrino background.
Thank you.
>>
We will go on to the next talk.
The next speaker
will be
(Unknown name) and she looked
talk about searches for
...
>>
Hello, I hope you can hear me.
I work in
a university in Sweden
and
(unknown term).
It's about the searches for long-lived particles at the FCC.
What is the FCC
-
ee?
It is an electron
provider proposed as a possible first step
toward FC HH,
it will
occupy over 100 km
under the Geneva Lake at
CERN
.
It is proposed with a large energy range,
it will have different dedicated runs,
like
(unknown term) production of
(unknown term)
and also
even
(unknown term).
It will be mostly a precision
tool
but will also be much more because it also has
a large
(unknown term) potential.
Every measurement
is
(inaudible),
any small deviation with respect to the
(unknown term)
is exciting but
you can
...
In particular what we want to propose
is
lonely particles are quite cool,
they appear in the BSM models
, they are quite fun
and at the
FCC we have a flak show
for this,
-- Flagship.
The heavy neutron (unknown term)
theory gives
like
matter
, to name a couple.
There are two parameters
that you care about when you are talking about heavy load electrons,
one is the (unknown term) and the other is the (unknown term).
You can have a large
(unknown term), a lonely particle,
it has great potential for a large phase of space
with
heavy neutron electrons but it's not the only thing.
SCC will have sensitivity for action like particles also known as
Alps that have a fun name but they are quite interesting and when you
have small couplings and light particles, you have
You can also perform
searches and likely their many more motives
we are listing
to get to know.
This kind of searches for particles are a
little bit more special and bring expire mental
challenges especially for the construction
because they don't detector the sign for
the future.
We are looking forward to exploring this kind
of opportunities in the future and we have a lot
of intent and you can take in the QR code and
go through it and if you want you can contact me
and we would be happy to help you.
Thank you.
>>Thank you, the next speaker will be
David
who is going to tell us about testing
universality
and
pion decays.
Go ahead, David.
>
Thank you Vern, I am David from the
University of Washington excitedly know but an
emergent project we are considering which is
motivated by day-to-day driven hits of new
physics and theoretical explanations that
connect the physics scales that are not
constrained by other data.
Let me remind you of some of the persistent
tensions in the standard model with respect to
data.
First experiment I spent my time on we are
suited to release first results, Joanne, we
promise.
But also, there is a deviation from the
standard model in the electron G -2 by few
standard deviations from her recently.
Next most recent computation of the CK on
first Road unitary stuff by standard deviations
you might ask why?
As you know there are several noncompliant on
the case on universe settle teen violations.
There are models I can explain these effects
individually, but also, the personality, that is
a tough one, violation can connect them.
We will address these by 2 precision
measurements that can be carried out with one
central compact apparatus and this
morning, I saw all challenge us to think
big and think small and I think this project
here satisfies a.
as suggestedthat.
By our experimental name, the first case-
directly in the nuanced system.
Hi is the ratio of charged pie indicates
from electrons versus muons the standard model
theory is known to credible precision of 2
parts intended the 4th in the PDG experimental
quarter magnitude less precise.
This provides a very big window for discovery
when there is a well-known standard lot
prediction and experimental far behind.
The 2nd experiment is by a beta decay, easily
the most theoretically cleaned method to obtain
BOD, pi Beta
is challenging though because the branching
ratio is about 10 to the -8 we want to know there
is a lot better.
Even with the threefold improvement, however,
one can get an improvement in the
diagonal ratio on the plot that you see there,
the diagonal constraint in the D&D plane and is
the first goal.
The diagonal will help relieve the tension you
see very clearly evident in that figure.
The group of us that have formed so far have
come from high beta experiments
and a collection of other precision physics
experiments around the world.
We will draw from our collective lessons
learned to develop the next generation
experiment.
Essential to this is basically the idea of
using
for pie very fast high rate capable and very
deep calorimeter, liquid xenon seems like--
inside will be a pixelated tracking
system and an active pixilated stopping
detector for the charge stopping pion
experiments.
Appropriate pion beings do exist
and may need to be modified slightly but
they are not out of the question
and in summary, it is basically a modern cost
high impact relatively fast timeline, I want to
thank you very much for your attention.
>>Thank you David, we will now go on
to the next speaker
was Sebastian Ellis,
he is going to report
on a heterodyne protection
of axion
dark matter
with superconducting cavities.
>
Thank you.
My name is Sebastian Ellis and I would like
to briefly tell you about some new approach
we have proposed to detect Axum dark matter
using a superconducting radiofrequency cavity
SOS cavity.
The work was conducted with the listed offers
and we have submitted an LOI and a CF to any of 5
somatic areas.
Axion's, if they exist, convert protons in the
presence of a background magnetic field.
This process is form the basis of acts on dark
matter searches for decades.
Our motivation
is that low mass axion's are difficult to
approach because either one needs to build a
large resonant cavity or to somehow dissociate
the resident frequency from the cavity
geometry, such as by using an LC resonator
which unfortunately leads to suppression of
the signal at low axiom masses.
The core of our proposed approach is to
load and SRF cavity resident mode, so that
the background magnetic field required for axiom
conversion is oscillating as opposed
to static.
The signal frequency is then a combination of
the loaded mode frequency in the axiom
hence the heterodyne which can be matched to
a frequency by small deformation of the
cavity means.
The proximity of the loaded and single modes
means SRF cavities are ideal due to their large
quality factors which are frequently greater
than 10 to the 10.
The mega collaboration in the early 2000's,
there is a prototype of a similar device to
measure high-frequency gravitational waves and
achieved mode isolation of 140 dB.
Scanning an axiom mass requires careful control
of the cavity geometry.
In this respect, the dark SRF collaboration
and formula has recently demonstrated control of
roughly 1 past the 10th of the 10.
These 2 experimental presidents form part of
the basis for a theoretical reach
calculations sown on the slide, in particular,
acute cavity and quality factor that are pushing
the boundary of what has been achieved in SRF
cavities.
Of particular note, as a potential sensitivity to
the axiom in a mass range
with neither DM radio are sensitive as well as
the sensitivity till dark matter across
almost 9 orders of magnitude.
The sensitivity of a thermal device shows a –
green line on the slide is enhanced with respect
to a resonator due to the signal frequency be
much larger your
than the axiom as shown on the bottom right and
in practice, our approach is only
formalized in the higher axiom that masses for
mode isolation and cavity vibrations become
dominant sources.
For more details on the signal please see the 2
archived links I have listed on the slide.
Of course, continuing research and developers
will be required on both cavity design and
control to make this vision a reality and we
welcome discussion from interested groups.
Thank you for listening.
>>Thank you.
We will go on next to Marcella
and she is going to
, her talk is towards the future world
exploration at the energy frontier.
Marcella,?
>>
Yes.
Hello.
I cannot see myself but I suppose that is good.
Thank you.
For many decades,
colitis of the industry frontier have opened
windows to the unknown.
And most recently from the discovery.
It is
now the time to think about what is next
at the frontier?
What discoveries may lie ahead?
Thinking about future collateral experiment we
can brisk challenging questions such as what
is the true nature of the exposure and are
there more scales?
To such an extended scale of sector be
connected to dark matter and dark sector.
And a fundamental role in the dynamics
of the transition
during their years.
Moreover, the explanation of the matter
and
matter of symmetry in the universe can be
intimately related with insistence of new
particles at the reach
of present and future collectives.
We have just started to scratch the surface
of missions affixed properties.
As you see
on the right-hand side of the slide, it was
only a couple months ago that we stop blushed the
explosion with any-- beyond the next
generation.
Future runs may help us understand if
the hex is composted
rather than the particle ultimately the
measurements of the interactions will lead
to deep understanding of the properties
of this new and very intriguing scale of
particle.
Future collider's of many different types
from a collider with an initiative beyond 2
collider hex factory, will give us unique
handles in systems of new particles both
through their direct discovery of signals as
well as their interactions with
exposure
and other particles.
Most interesting,
if they exist,
they can establish
and modify the strength
of the
transition and thereby, help explaining
Association
with
the mature
-
very tantalizing possibility.
It is of great importance for the US to
continue a strong participation in the
global energy frontier efforts.
Strong physics motivation, coupled with
unique expertise make it natural for the US
scientists to play a leading role in the next
measure energy frontier facilities.
Including existing proposals as we know,
such as FCC, CBC,
click and MCC.
Regardless
of where in the world
they may be hostage.
Thank you.
>
Thank you Marcella, we will go on to the next
speaker.
Who is Philip Harris, he is going to talk on
dark quests and long quest at 120 GV for the
main projector.
>>Hi, I am Philip
Parris from the IT and I'd like to tell you but
the dark West experiment, Carquest is
an idea of an experiment to look for dark sectors
, dark sectors to become a very popular topic
over the past few years.
And we know that if the coupling is sufficiently
small, for light dark matter, you can actually
get the right thermal intensity of dark
matter.
Not only that, a small cup lead could be giving
a striking signature is often leads to long
lived particles.
For dark particles, we want to use the proton
main projector formula and fire this on the
target and then using uniquely compact
duct to search for a long of signatures that
come from this proton feed.
But the nice thing about this experiment is that
it mostly already exists, is called the
spin quest experiment and is used currently
for nuclear physics.
We propose a modest upgrade in this
experiment by adding an EM calibre from the
Phoenix experiment
at minus cost and this will give us access to
normally displaced neurons but displaced
electrons and displaced hadrons.
You can see a wealth of signatures and all of
this can be run in 20 2324 before the PIP to
upgrade.
To give you an idea of our sensitivity, here on
the bottom left, we have sensitivity
on dark photons and you can see we have
comparable sensitivity to other experiments
such as phaser and any 62+ plus, within the
similar time scales 2024.
We are capable of running a broad range of
-- including Acxiom like particles
in elastic dark matter, dark photons and so on.
And, with our LOI, we need to actually
put
modules into the test
ing
and looking and say the performance of the data
rates
are for the potential upgrade of dark quest
and further, we aim to build the full
simulations we can really confirm our
sensitivity and prove many of the new
interesting practices.
Thank you.
>>Thank you, Phil.
We are going to go onto the next speaker
who is Marcel.
He will offer perspective on a unified
US particle physics program.
>>Thank you very much Juel.
And thank you for giving me the
opportunity to speak to this.
I would like to speak to a perspective on
creating a future particle physics program
and the US.
In my opinion, a healthy vibrant particle physics
program cannot be dominated
by only megaprojects, but really needs a
balanced portfolio of small, medium, and large
scale projects.
And that means, I also think that the field
should exploit all opportunities that it
has to advance its science.
I know that this source
, the world's most intense
nutrient source
is actually also the brightest
and the cleanest neutrino source in the
world.
Just
demonstrate the scientific capabilities
through the world's first discovery
of elastic and neutrino scattering not just
forms
like in 2017, but actually twice
with the recent demonstration of sevens
in the ion targets.
The SNS is in the process
of a power upgrade and they will have 2.8 MW
proton driver in 2025.
In there I think will provide unique
opportunities for the field for neutrino
physics.
Furthermore, the 2nd dark station is being
constructed.
And that could also potentially provide
space in the 2nd target station building to
house future neutrino experiments.
Now, the SMS is not the only neutron and
neutrino source
.
The high flux isotope reactor also provides a
continuous
and a well understood source of electron
anti-neutrinos.
2 upgrades
are being considered.
In both upgrades provide an opportunity
for fundamental physics experiments
that is even strongly supported by a recent
B section report.
This particle physics program
can be expanded also
to study not only neutrinos,
also neutrons such as small-scale searches
for mirror neutron
oscillations.
There are 2 other projects that I would
like to mention at the lab.
What is the materials plasma exposure
experiment facility that will measure materials
up to 50 displacements per hour.
Which could inform the target tree that is
being considered for the intensity frontier
program and also
the nuances spin residence facility is
being considered that build 2×10 to the Nuance
per 2nd that could be a terrific source of
nuance for fundamental physics studies.
So, my 3 minutes here really is an invitation
from Oak Ridge to the high-energy physics
community to consider these resources to build
this future program.
And I would like to remind you, together, we
are stronger than this.
Thank you very much.
>>Thank you Marcel.
Next speaker will be Ryan ignored,
and he will
tell us the culture change is necessary and
it requires strategic planning.
Ryan, go ahead.
>>
Thank you for organizing this and they could to
The evidence is then,
racism permeates society
and the community.
The evidence is that black people and persons of color
are minority ice by
policies and we are
disenfranchise.
When the reality is acknowledged by groups in the scientific community
responses have included a reinvigoration
of diversity initiatives, creating committees and generating solutions
before consulting the main excerpts
-- experts.
It can be dangerous for the purported
beneficiaries
, and for enabling a sustained effort
that goes beyond
a few initiatives
or committees.
Therefore,
we make multiple recommendations which are detailed in our Snowmass
, linked at the top of the slide.
These include things
that many of us are familiar with our
design of science experiments like becoming familiar with the problem
space and state-of-the-art
processes, partnering with experts
and strategic planning.
These also include
some newly framed elements like constructive and compassionate
conflict and shared leadership.
Imagine we are pursuing a new
understanding of some aspect of the universe,
what are
the processes we go through to design the experiment and build
collaboration?
What actions or strategies do we avoid?
How do we prioritize
approaches to those challenges?
We establish clear and measurable goals and write down requirements to
achieve those goals and then we grind,
periodically revisiting the strategy until the goal is a disk
accomplished.
Now imagine
this effort is creating a just research environment
because it is a fundamental issue in our community
and the right thing is to do something about it.
If we consider the challenge urgent,
it means we have to deal with the tension between
triage
and acting
on research
elements while also planning all of the elements coherently.
We recommend that we as a community access the creativity and discipline
were using science efforts and apply it to work
for justice in the scientific community.
This includes using strategic planning and partnering with experts
to get to a more equitable
decision-making
process than we have now.
Examining what we've done in the past and updating
those methods.
In some ways this work is similar to our work in scientific
efforts,
we need to establish new
knowledge, if we want something different we need new approaches and
solutions and an appropriate plan.
Now we've spent a lot of our time
imagining what our future of understanding the universe looks like
, we need strategic planning to carry out
our
future imagination of justice.
>>
Thank you, Brian.
The next
speaker is Kelly who will talk about Snowmass as a path toward
cultural change and the role of collaborations.
>>
My name is Kelly and I speak on behalf of a group of folks from the
neutrino and dark matter experiment communities.
As we have heard, inequities and marginalisation of
identity groups continue to plague our society as a whole and physics
in particular.
The evidence is striking.
75% of undergrad women in physics report
experiencing sexual harassment
and the number of undergrad physics
degrees awarded to black students in the US has stagnated or declined
.
Our subfield
is a unique situation since many of us belong to
multi-hundred or thousand person collaborations which continue to
grow.
Our collaborations radically expand the sites we can pursue
and introduce new challenges,
they bring together people from a wide variety of backgrounds.
Since they play
such a large role in the day-to-day experiences of many scientists in our
field, every collaboration should be grappling with the issues of equity
and justice with the same energy with which we pursue our science.
As Brian asserted, we must not
approach this uninformed, we must draw on the results from
reports and community calls to action like those listed at the
bottom of the slide.
This can and should
be urgently happening in all collaborations,
independent of the Snowmass process.
Collaborations can't do it alone.
We often lack the resources, the institutional infrastructure
or political standing required for meaningful change.
For example many collaborations have instituted codes of conduct
but
struggle to enforce them
when the parties come from different
institutions or different countries with different sets of regulations.
Solutions to these crosscutting issues will
necessarily come from working together with funding agencies,
national labs,
universities and professional societies
and this is the power of the Snowmass process
– it is a chance for us as a community
to describe the future we want to see for our field
and start planning for the changes that will bring us closer to that
future.
For this reason, the resulting P5 report
should include recommendations to put it on a path toward a more
equitable and just community.
These recommendations, informed by strategic planning
and expertise in appropriate discipline should support
and empower collaborations to pursue justice, as we do our science
because
this problem of inequity in our field will not solve
itself.
We must face it head on, every day,
into the future,
both in our collaborations and as a community.
Thank you.
>>
Thank you, Kelly.
We will now move on to
Sven
who will talk about gas TPCs with directional sensitivity to dark
matter, neutrinos and BSM physics.
>> I'd like to talk you
about Cygnus,
the proposal to build directional
detectors searching forward neutrinos, dark matter and BSM
physics.
It's been demonstrated that that gas correction
chambers with high definition charge readouts can
detect
, shown on the top left seen in 3D
,
electronic readouts and to die
2D with optical readouts.
We can have fine readout
segmentation,
and
low enough that the diffusion scale
is smaller than
the report went.
This enables not only directionality but particle
identification as shown here,
very low energies in the KV range,
electron
look very
different in the resolution.
This allows
us to open the door
to large experiments
and directionality.
The directionality is key for penetrating
neutrino flow and distinguishing neutrinos from other sources such as
the sun and the oath from the
dark matter is coming from a different direction.
To get sensing our exposure, to build a multi-
science underground Observatory,
this effort
has now
been
built
an international
effort receiving its first funding in Europe and Australia.
Up what I would like to emphasize is the long-term goal
, a nice long-term research
project here that allows you to do new physics measurement for every
factor of 10 in exposure,
we have released a design paper which is on the archive,
but many other measurements are possible,
very small
, should be able to
observe the (unknown term) effect,
scaling up from 1 to 10 m³
should
detect
elastic neutrino scattering is
in the neutrino beam could be
the one shown here or the SMS
.
Going up to 10 m³
as shown on the plot on the right, you should be able to
set the world's strongest limits.
For
every order of magnitude increase in exposure, new physics becomes
possible.
We take this to a
scale
facility at room temperature, lower cost,
this should be able to detect free
neutrinos
, revealing the physics of the heat
generation of the earth.
For Snowmass many
proposals related to this was submitted,
many of them address beyond the standard model
aspects of it, searches for new particles,
and unfortunately this slide
doesn't show this
,
but the main
message is there are many unexplored ideas
for Snowmass
and we
invite you to join this exciting
effort
, we plan
a workshop
this fall,
the cosmic neutrino
implementation for
frontiers exploring this further.
Thank you.
>>
The next speaker is Matthew
, he will tell us about searching for Millie charged particles with
center later based detectors.
>>
Millie charged particles are well motivated through kinetic mixing
between the standard model
and a possible dark sector.
Coladas and neutrino saucers but general-purpose detectors
typically they will be sensitive as the interaction probability goes to
the charge of the particle squared.
How can we find such signatures?
The idea is to use a long center later bar
,
and beam them to detect small
charged particles
and you can see on the left ear.
The expected single from Millie charged particles traveling through
the back tractor
detector
and each part must be capable of
detecting a single scintillation photon
.
The design is important because backgrounds can be
rejected
,
coming with a small 50 ms window.
This design is easy to scale and adapt
and this has been used
at a variety of societies,
facilities,
to detect
neutrino
sources
...
You can see the sensitivity curves for detections on the right-hand side
in blue and purple
.
There is a possibility for detecting
...
How do we know such a detection design work
?
In 2018 a small prototype
was installed at CERN,
this rants
successfully
characterizing
backgrounds as well as setting the first limits in Millie charged
particles at the hadron Collider.
You can see the results of this on the right-hand side in red.
This was published
, the data was also used to provide
important lessons to guide
future detectors
.
Summarizing
for Snowmass,
the idea is we want to use the data from the demonstration
to update protections for full-scale
detectives with consideration of the backgrounds
as well as a fully calibrated SA simulation.
And important lessons for
detectors
, for example,
we have observed that three layers was not enough
, for layers was required.
This is timely
as a collaboration has recently saved
received
funding, this is an important intermediate step
.
And the input
will because equal for that
project.
In conclusion,
scintillation
base detection over the next few years,
it will be an exciting time
for the
potential discovery of Millie charged
physics.
>>
Thank you,
the next
speaker will talk about
measurement
of the fine structure constant as test of the standard model.
the community for paying attention.
>>
h
ello this is from
Berkeley, the fine structure concept
designs the strength of the electromagnetic
interaction and therefore underlies most
of the physics
that we are familiar with.
The most precise measurements of the fine
structure constant are based on 2 effects, one
is the anomaly which has precision off 1/4
part per billion and the other is measuring
the ratio of the plan constant with the
particle mass and combining that with the
Richter constant.
This has so far been the most precise measurement
of the fine structure constant that our 2018
results of being over 137 or 35999046.
The power of such measurements
or about the standard physics is shown on the
right-hand side of the slide that shows
all the terms that enter the prediction of
the fine structure constant at the current
expert mental position.
And you will see it's not only the first 5
orders of quantum electrodynamics can we a
nation but also the existence of the neuron
and hydrants features and about sending a at
the current accuracy.
The goal of our project is to improve the
accuracy
to the fine structure constant measure by more
than a model of magnitude and this would
for the first time reveal for example, the
existence of the low energy experiment, this
would get very close depending on other
auxiliary
measurements that are needed and importantly,
on a remeasurement of the neuron's magnetic
moments that is being prepared by Jerry
Gabriels.
The key to our improved experiment, the
experiment
itself by measuring the recoil velocity of an
atom that has scattered a photon and as you can
imagine, this velocity depends
on the normality's speckled patterns.
Our approach is to take the control over the
spatial structure
of the laser beam to an unprecedented level and
then experiment shown on the left is essentially
a massive vacuum chamber that has been optimized
to provide a nearly perfect conditions and
propagation in the middle.
The recoil velocity will be measured in an atomic
and you can see the space-time diagrams of
the atomic trajectories of the graphs at the
bottom of the page.
If everything works fine we hope to get a 10 to
20 part result on the fine structure constant
in 3 years, this would amount to a broad and
deep test of the standard model, lots of
pieces of the standard model have to be right
in order for the comparison of the
electrons momentum to check out and is also
brought a sensitive search for dark matter
candidates.
Thank you very much for your attention.
>>
Thank you.
The next speaker will be Harvey Newman, he is
going to tell us about future information and
communication technologies, for the
LAC and beyond the limit.
Harvey, go ahead.
>>Hello everyone, I am Harvey Newman from
Caltech, I'd love to give a perspective on
coming revolutions in information
and communication technologies.
Both because
they shape the way we actually do research
and also
how the environment will change.
And also, because it represents
opportunities for future planning
some of which
may not have already been realized.
On the front of semiconductors there
have been struggles
to go beyond
and feature the roadmaps that go down
below the 1 m level around 2030
,
and so there has been arriving tied
on new technologies
on the unseen laws which can maintain the
progress and the capability increase
which is really driver of progress and also
unlike other fields the industry is already
grappling with the fact that there are
continuing to progress that will have to
undergo these transitions.
Among the technologies
are photonics which have surface waves
or
things other than electrons that carry
signals and overcome the energy speed barriers
which we are familiar with and we actually
build into some of our detecting designs and so
this is an opportunity to go beyond them.
And also, our range of new methods that have
tested technologies, materials using surfaces
which are structured which enable you to
shape and direct
form white fronts and change beams and use
freedoms such as
momentum.
Optical communication that we use every day
also in experiments completely change and
so, multicore farmers using
fibers
fibers using photons
will come to the forefront very soon.
These are the opportunities, and I
think, and future planning,
it is important to realize that some of the
barriers we have built into our designs
will probably be bypassed and replaced,
so these when these emerge we should take
advantage of them was a pause from the system
point of view, 60 wireless is already
being formed
for the standard, which will take another 10
years.
There is been a new generation of wireless
every 10 years.
And this will also change
the way we enter communicate
with universities that harkens
directing how we handle
systems
of entities which are mobile
and overlapping ensembles of objects
on mobile scales.
This again will be revolutionary.
Finally, I wanted to say, when you look at
our roadmaps which go up several years, we also
thought back to what is the timing from first
ideas to products and it's typically about 15
years.
We should have a flexible view, keep a
watch on all these technologies, and
ongoing revolutions and use them in our
experiments and our future planning, thank
you.
>>
Thank you Harvey.
The next speaker is Mariana and she will
tell us about
atomic clocks and precision spectroscopy
measurements for dark matter and dark sector
searches surges.
Go ahead.
>>
Thank you so much.
This project isn't a collaboration of 7
countries and about 30 people.
And the identity of atomic and
nuclear clocks to search
for physics be a standard model comes
through the extraordinary
improvements
in the precision of the clocks.
As you can see, in the graph, on the left-hand
side, the blue line, that is a program
progressive micro meant crop
clocks, about 16 fraction percentage in
the optimal clocks which are based on particle
frequency however, are now 10 to the -18 and
approved by 4 orders of magnitude in recent
15 years or so.
And we really don't know how far this will go.
There is no technical reason why it can
continue improving clocks by more orders of
magnitude.
And just to put things into perspective, as a
fraction of precision of clocks at 10 to the -18,
means that this clock, the model is one 2nd.
In this progress enables
various studies of physics beyond the
standard model in clocks, and it all
started from the question of the
fundamental constant because the fundamental
constant such as a fine structure constant was
measuring actually changes with time or
space.
Then so do automatic frequencies or nuclear
frequencies and still do all the call
frequencies and you can detect them by looking
at ratios of the clocks.
And that recently was realized dark matter
also fundamental constants.
Either transient or
Austro literary.
There many new projects now
which already have new results, looking for
dark matter clocks
the equivalence principle, searches the
violation and also proposal to do rotation
of detection
and recent proposals of quantum sensors such as
clocks would actually act for
multi-messenger astronomy.
There also later projects which don't
specifically have clocks on other precision
experiments such as searches for new force
mediators.
And, the motivation for all of those experiments
besides extraordinary precision of clocks is
that a number, many of these theories
propose to solve various problems of the
standard model, actually remove those fields and
we have now an opportunity
to really reach those experiments
by several orders of magnitude by building
clocks which have the highest
sensitivity and fact.
In fact, this project is a part of the developing
field of precision of the Potomac there are 30
letters of interests
of atomic physics communities and our goal
for this normal process is to redevelop particle
particle physics collaborations and hope
it brought interest in those experiments and to
have
strong collaboration to actually fully realize
the potential.
They could so much for your pension
attention.
>>Thank you.
The next speaker is Francesco Giovanni
and he will talk about 3D proton tomography at
the IC TMD distributions.
You can start now.
>>
Thanks, hello everyone, today I will present
this one slide about tri-mental description on
colitis and I will be happy to motivate future
studies and mass communicate about
TMD
functions.
My work is a basic name
ongoing project in collaboration
with the Citigroup and Muniz city in Italy.
And we know that
they represent a co-sector
of the electronic colitis studies.
And we know that without
this next generation of colliding machines, it
will be possible to study
to perform its systematic study
,
in particular from the TMT point of view, which
actually presents one of the most challenging and
the less known sector of the interactions.
With the aim of fulfilling the need for
affects of models,
the terminology, we provide systematic
framework
, which allow us to calculate at the end of
this approach and polarize
TMD
function
and
we know that the information
distribution and mainly in large, in reach,
our knowledge,
and our knowledge coming from the standard
one dimension description at the end
of standard functioning and can be used
to
mention autographing studies
in particular, the axle acts.
So
my work may be referred to
the first paper in collaboration
with my colleagues
and here as an example
on the right block, on the right
lower corner of the slides, I present
to possible
combinations
of this distribution,
the density on the left
and the density on the right, there is a
functional process.
We see here the plot of oscillation on these 2
densities, along
the trances momentum plane, they move it to
the left one in response to the density of
finding polarizing and not polarizing in this
case,
the other one is on the right, we have
the one which corresponds
that gives us the probability of finding
a secondary
polarizer
in this case, again proton, and this is just
an example to show
to see,
how
it's enough to predict things
in the behaviour
of the densities, taking into account the
polarization out of the aim 2nd one
and after our calculation
,
and distinguishing function, we will perform
the distinguishing function and provide
support
to physics.
Thanks.
>
Thank you, the next speaker will be Richard
Tomlin, who will talk about colliding elastic
PPE
scattering to test
P violation are
-
go ahead, Richard.
>>
I'm Richard from
Cornell,
and you heard
in the earlier talk, about the pronounced
closing lab
in Germany, the stock described in application
.
The goal is
to detect
violation or parity violation
in seemingly
proton proton
proton neuron scattering.
Lien and Wolfenstein
have independently proposed
semi strong symmetry breaking mechanisms
going beyond the standard model.
The goal will be to improve symmetry
violation
upper limits by more than one order of
magnitude's, approaching
one part per thousand.
The method suppose it is proton neurons
gathering, detection chambers at the
intersection point of a single ring providing
beam storage ring,
protons travel in one direction, pseudo-frozen
neurons in the other.
This fixes the spin states of both
particles.
Being a storage ring, the centre of masses is
moving only slowly
so both scattered energies lie in the
narrow range, for example, from 40 to 65
kinetic energy.
The scattered particles will flow
tracking chambers.
Some will undergo nuclear scatters
in the tracking chamber plates, this will
provide
efficiency of 1%
analysing power of 0.4,
.
Finally, I turned to the anticipated
performance.
The storage ring luminosity will be 0.6
in hurst Miller binds per 2nd.
This will produce 100 million clean evens per
year.
A clean, I mean 2 unambiguous single tracks
detected in time coincidence.
Most will be cold in here, except for centre
These events will provide accurate,
independent
measurements are
over
, more than 1 million of these events
will have one or the other particle, nuclear scattering in the
dragging chambers.
These polarization measurements are
sensitive to symmetry
violations, 10,000 events will have both particles of nuclear scattering
,
these are particularly sensitive to symmetry violation
.
For these events both
initial and states are known
, and final state
polarizations will have been measured.
These events
lead us to expect
to be able to reduce
the upper limits
on symmetry violation that I mentioned before.
Thank you.
>>
Thank you.
For selecting me to talk.
I'll talk to you about
Max has to bore water a breakthrough tax attack matter and
neutrinos.
We have started to form a collaboration with the institutions
you see on the upper right.
White is metastable water?
You think of super heating or super cooling,
we are focusing on super cooling,
which has never been used in HDP
.
The idea here is to establish a new technology
that can be used to drive discovery in the 21st-century like
the bubble chamber did
a long time ago.
In our prototype we have looked at
supercooled water
and we call this the snowball
chamber, analogous to the bubble chamber and the cloud chamber,
liquid to solid
transition and the technology is scalable for modularity.
We consider it ideal for low mass dark matter
due to several advantages I will get into now.
Water has hydrogen and oxygen and if you have the ability to
distinguish between them,
that will lead to good signal background discrimination.
We also show on the right sensitivity
to the spin independent
proton interactions.
In existing literature for supercooled water
and atmospheric science and chemistry
we find that the highest threshold reported, worst case,
is of water
tens of AV.
That should enable incredibly low mass dark matter sensitivity
and because we are dealing with individual protons with the hydrogen,
atoms, this unprecedented sensitivity
,
it should be possible to have the neutrino floor not being a serious
issue.
The neutrino floor would be lower for the snowball chamber.
The other potential here is nuclear recall
directionality from a gas detector,
together
with the bulk target
you get from a liquid
detector.
We are currently gathering
preliminary evidence of this
and the idea is this directionality comes from the intense hydrogen
bonding that is present in water.
At the left you see our preliminary
evidence that water is sensitive to nuclear recoils, which has never been
demonstrated before for super calling
cooling
.
In the future in order to precisely calibrate
the energy threshold we need to go to a place like
a tunnel to calibrate
but
in California it is indicative of at least one KV threshold
but large uncertainty.
We can look at the different images and how snowballs form
in order to be able to stink to
distinguish between backgrounds and non-dark background
and hybrid detectors like
water
(inaudible) detectors.
>>
Thank you,
we will go on to our next speaker,
who will talk about
a deci Hz
gravitational wave lunar Observatory for cosmology.
>>
Thank you to the organizers for the
invitation.
I am at Vanderbilt
University and a member of the
(inaudible) collaboration
.
I will be sharing this idea of a next-generation gravitational wave
experiment
that has great synergy with the scientific goals we are discussing
at Snowmass, the possibility of a joint
OAE.
As mentioned by
the exciting talk this morning,
what is the next experiment
after
While we have the concept idea of extending
a lie go like
detector, there is a fundamental limitation on earth due to seismic
noise,
we cannot go below 5 Hz with a conventional design.
With space missions we can go to Millie hertz,
but the one-
point one range, this is a sweet
frequency spot
for the most powerful sources in the universe and our
crucial for understanding primordial black holes and duck
Matic candidates.
This makes the case for
building a detector on the moon.
One of the major developments has been NASA's
Artemis program, the program released last month by NASA has
accelerated the process of sounding
sending to astronauts by 2024
with payloads.
One of the strategies for Artemis is to observe the universe from
a unique
location in the natural vacuum on the surface of the moon, the wider
seismic activity and no environmental effects make
the moon
the natural location and using a conventional design
with existing projects, a detector on the moon
can achieve much if not
all of the sites we have explored
.
In the plot on the left, that is the design of what a gravitational
wave detector on the Moon's surface would look like.
The plot on the right is essentially the science case, the outermost
circle
is microwave background and different shades are how far
in the universe the experiment can survey
.
The conventional sources of gravitational waves
we already know exist can be served up to
70% of the observable volume,
this makes it a further reach than any other experiment
.
The frequency sensitivity is ideal for type I supernova
, we can temporarily constrain
the silence in directions five and 10, dark matter candidates
if they exist, we can
survey up to 30% of the entire universe and all this will
complement the Largo detector on earth as well as telescopes
allowing multi-mesh and Joe
observations
.
Similar has been submitted to NASA
and if you are interested in this effort, please reach out.
Thank you.
>>
Thank you.
The next speaker will be
talking about
testing as IDM
with realistic galaxy formation simulations.
>>
Hello, everybody, thanks for the Emmett
invitation.
Today
I want to talk with you and share my excitement
about how we can use simulations of dwarf galaxies,
galaxy smaller than the Milky Way as a tool to constrain dark matter
with the
various telescopes
poised to launch in the next 10 years we are entering an exciting
time where constraints on dark matter from all scales
will become available.
My work looks toward that future.
Now is the prime time to use cosmological galaxy information
simulation
to predict which observables dose Observatory should be looking for
and how to interpret them.
That said the project I would like to highlight,
being conducted with my collaborators listed on the slide,
and I will draw your attention
to
1 of them, we will answer the following question – can dwarf galaxy
formation simulations predict an observable
that favors one dark matter model?
In astronomy CDM
is the most favored
paradigm but I will start with the assumption
that there is no good reason to favor cold dark matter
when you consider baryons.
Baryons as
an astronomer after many pesky galaxies that live in
dark matter halides,
halos,
in particular
I am looking at small dwarf galaxies
and modeling
those baryons.
What I'm showing you on this slide,
when you consider
different dark matter paradigms from CDM
to warm dark matter
and you include those pesky galaxies, there is no way to
differentiate between those models.
All of them solve these challenges I have listed.
The models become virtual belief
virtually indistinguishable,
I aim to leverage state-of-the-art simulations that push the agitations
and you have what is computationally possible.
To look for the smoking gun that distinguishes in particular
as IBM from CDM
in the presence of
galaxies.
In particular the observables we are looking for
are listed on the slide and these are directly testable
by the great observatories I mentioned previously.
And with this we hope to guide future observations and provide a
theoretical background
for strong new constraints on dark matter soon to come from
low dwarf galaxy astrophysics.
Thank you.
>>
Thanks so much.
Our next speaker will be telling us about superconducting qubit advantage
for dark matter, squad.
>>
I am a graduate
at the University of Chicago.
Today I am going to talk about the search for low mass
dark matter candidates, these candidates include axion's and
photons would potentially convert
into a quantile flight of the same energy as the dark matter mass
and we attempt
to capture the light in a microwave clarity and read it out.
To enable the dark matter such as in the mass or frequency range of
3-30 GHz, we present
to techniques that utilize superconducting
quantum
bit first, reduce the background count
by a factor of 1300
as compared to the current technology, and second, boost the
signal rate by at least a factor of 10 using
stimulating
...
To sense the electric field of the
dark matter
, and this is a quantum non-demolition
interaction, meaning the photon is not observed
during the measurement
and this allows us
to make multiple measurements of the same photon
to mitigate the effect of a readout
error
in any usual measurement.
In the top left figure we see that
with more measurements the availability of erroneous readout
is suppressed exponentially.
This results in a background rate 1300 times smaller than the
conventional readout strategies.
With this improved sensitivity we can take photon search and exclude
the
region of parameter space as shown on the bottom left whether Y
accesses the hidden photon mixing angle and the X axis is the
dark matter.
It's mass
.
Only eight seconds of integration time,
enabled by the cubit
-based sensing technique we have developed.
Moving onto the signal part of we start the cavity in a non-
space, we can enhance the capability of the dark
cavity
matter in the cavity.
We harness the non-
linearity of the cubit
and use machine learning tools to generate
optimal control pulses while some Italian sleep
simultaneously including the
state in the cavity.
As you can see on the right,
eight
stages
, and with future dark matter surges we can
include and rates greater than 10.
We are starting to see this enhancement initializing the cavity
close to 0
versus an equal to one state.
A cubit technology makes future dark matter surges possible by
enhancing the dark matter signal and reducing the detected noise.
This work is an example of the type of cross disciplinary research we are
fostering it Snowmass planning exercises and we look forward to
working with everyone here.
Thank you, and for more information,
it can be accessed by the QR code on the top right.
>> Thank you.
Our next speaker will be talking about the initiative for dark matter
in Europe and beyond.
>>
Thank you for inviting me here.
mass function and multiple scattering, and
they will point back to a common origin.
Here I'm talking about something slightly
different, still about dark matter.
It's initiative for dark matter that has started
but also means to go beyond because of
course, dark matter has no boundaries.
I think we all agree the best region defined dark
matter is the one you can use more techniques
and ideas, and explore it.
And it's amazing how many different things
we've seen also this community also the whole
mass that there are so many possibilities here.
With this in mind, the ones on the top right,
coming from different fields, so
astrophysics, accelerator
for now,
met at the
conference that was set up
by the accelerator, nuclear and particle
physics communities
in Europe.
And
we realized we were ask each other questions
will kind of assumptions are you using, how are
you using this technique and what is your
statistical and obviously how does your
finding affect my findings ?
we realized there was no common platform for this
kind of discussion or resources.
On issues again, we started developing it as
initiative.
This is how the initiative was formed.
We have 3
connected objectives, the first one is to
collect dark matter resources in our own
matter, one page contribution from the
community that will have dark matter resources.
We also want to facilitate
that participate in cross community
collaborations
and it means we are
preventing existing community efforts is
that we want to try and facilitate
them talking to each other.
And then finally something we will hear
on the last day of the community planning team
to help develop a story, a common dark matter
story for different audiences.
It's often one gets one side of the story but
how can we reach, for example, the general
public and give them the breath of perspective
that dark matter
probes were off.
I DMU is still taking shape, it is something
that has started rolling in a couple of months
ago with the help of a task force that was put
in place but,
the ground state is that we want to be a
service to the community with an organization.
The first step would be reaching out to the
communities
towards a kickoff meeting in Spring 2021.
If you want to see how this develops, you can
go to the link at the top left and then sign
up and sign up about 300 people
that when this kickoff meeting happens.
Thank you very much for your attention.
>>Thank you for that talk.
That was the last talk in the session,
I'd like to thank all of the speakers
for what I think was an extraordinarily
interesting
session, I really think
some
of the comments by previous speakers of
what the community should do, they should be
relaxed about it because I think these
things
word demonstrate in the session.
I want to remind you,
the audience you can engage with the speakers
who I hope will stay around
and discuss things on Slack with them, before
we close the session, we will organize
the committee probably has some announcements
and I will turn it over to then to close the
session.
>>
Thank you Jule, for the last session, we have a
special thank you to Louis who really helped
bring the session together.
The organizers want to thank everyone who
participated in today's opening day of the CPN
and just a reminder that tomorrow will be
entirely parallel breakouts which will be
held in a number of Zoom rooms and we will be
sending out the connection details to
those rooms later tonight, they are going
to go to the same way you seen the connection