14:46:05  

14:46:05 >>

14:46:06  Shall we start?

14:46:15  OK.

14:46:19  Good afternoon.

14:46:21  Welcome to voices from

14:46:25  the community Town Hall.

14:46:28  My name is Joel Butler from Fermilab

14:46:31  and I'm DPF vice chairperson

14:46:33  and I will be your host.

14:46:39  We have an exciting agenda of 22 
talks, each of 3 minutes duration.
14:46:43  This is the last session of the day

14:46:45  of talks, panels, goals,

14:46:48  broad visions, regional plans

14:46:51 , plans from related fields

14:46:54  and thoughts from funding agencies.

14:46:58  These visions and goals are 
constructed by researchers
14:47:02  from all over the world working 
on many scales, large and small
14:47:06  in particle physics 
and related areas.
14:47:08  We are presenting here 
a representative sample
14:47:11  of these efforts demonstrating 
the vibrancy
14:47:13  of our field

14:47:13  and our commitment

14:47:16  to expanding its diversity

14:47:19  and equity. 

14:47:20 We hope you enjoy these brief talks

14:47:23  whose duration, we 
remind the speakers,
14:47:26  will be strictly enforced.

14:47:31  We will not be able to accept 
questions during this session
14:47:36  but the Slack channel plenary 
voices from the community
14:47:39  is available

14:47:43  for questions and discussions and 
we encourage the speakers to engage 
14:47:47 with you after the session. 

14:47:48 I think now we can go 
to the first speaker,
14:47:51  who is mainly

14:47:55  mainly Sanchez, who will be talking

14:48:00  about ANNIE and the future 
of hybrid neutrino detectors.
14:48:04  

14:48:04 >>

14:48:10  Can you hear me?

14:48:12  Can I share my video?

14:48:25  

14:48:25 >> Please go ahead

14:48:26  and try to share

14:48:28  your video.

14:48:31  

14:48:32 >>

14:48:33  I think that worked.

14:49:03  

14:49:03 >>

14:49:06  Hold on a second and we 
will advance to the next
14:49:09  slide.

14:49:17  

14:49:17 >>

14:49:20  Thank you for having me. 

14:49:22 I would like to talk to you about

14:49:25  ANNIE

14:49:28 . 

14:49:28 There is a broad community address 
in the development of these detect
14:49:32  as which by using

14:49:33  water-based liquid

14:49:34  synthesizer

14:49:36  or slow

14:49:40  scintillation

14:49:47  increasing the coverage of LACCD

14:49:49  detection capability.

14:49:53  Is a critical step toward

14:49:56  ANNIE, and neutrino experiment

14:49:58  set to take physics

14:50:00  data

14:50:03  on the neutrino bean and it 
will measure the neutron yield
14:50:07  using a target of 30 tons

14:50:08  of

14:50:09  (unknown term) loaded water

14:50:13 .

14:50:15  ANNIE is an R&D platform

14:50:17  for neutrino

14:50:21  detection technologies and we are 
currently deploying the first
14:50:23  step of five large area

14:50:25  detectors

14:50:27  which you can see on

14:50:28  this slide.

14:50:34  The experiment to a preliminary 
neutrino data in 2020 is expected to 
14:50:38 run from 2020 to 2022

14:50:40  whether unique mix of interesting 
physics goals
14:50:47  and R&D, it is an excellent 
opportunity to train and develop 
14:50:50 early career physicist. 

14:50:52 In the next phase

14:50:53 , (unknown term)

14:50:54  aided

14:50:54  by

14:50:56  word

14:50:57  allow

14:51:00  a better understanding of 
the final state neutron
14:51:02  energy spectrum

14:51:03  and additional

14:51:05  LA PPD would meet

14:51:06  multitrack feeding

14:51:07  in

14:51:10  multi-directions

14:51:13 . 

14:51:14 With this addition, ANY

14:51:17  could be the first step in 
a series of detectors using
14:51:20  technologies

14:51:23  and we believe it is a criminal step

14:51:25  toward

14:51:28  demonstrating the power of 
these hybrid detectors. 
14:51:31 It could be used as a

14:51:32  new generation of experiments

14:51:34  that are at the same time

14:51:35  observatories for low energy

14:51:37  neutrinos.

14:51:40  We hope to see support for 
this approach out of Snowmass
14:51:44  and if you are interested 
to work on this and no more
14:51:47 , reach out to us. 

14:51:49 Thank you.

14:51:53  

14:51:54 >>

14:51:59  The next speaker

14:52:01  is (Unknown name)

14:52:03  and he will be telling us about

14:52:05  determining

14:52:07  KV range superlight

14:52:09  dark matter using graphene

14:52:10  Joseph

14:52:12  injunction.

14:52:16  

14:52:16 >>

14:52:18  Can you hear my voice?

14:52:23  Good afternoon.

14:52:24  My name

14:52:26  is (Unknown name), the idea

14:52:28  I would like to share with you today

14:52:31  is

14:52:32  new dark matter direct 
detection matter
14:52:34  using the state of our

14:52:35  recognition

14:52:37  (inaudible)

14:52:39  technology or the GJ J

14:52:41  device

14:52:43 , which would enable us

14:52:45  to improve

14:52:46  KV

14:52:47  range

14:52:48 , dark

14:52:50  matter in the near future.

14:52:52  The working principle

14:52:53  of a GJ J

14:52:55  devices schematically depicted

14:52:59  in panel A of the left figure.

14:53:06  The energy interacts with the free 
electrons on the breaking layer
14:53:10  and raises the electron temperature.

14:53:11  And then the effect

14:53:12  can switch

14:53:14  the zero

14:53:14  voltage

14:53:15  to

14:53:17  resistive state

14:53:18  with an appropriate level

14:53:20  of current

14:53:20 .

14:53:24  It was recently demonstrated 
in the lab
14:53:27  that the devices are accurate 2.1

14:53:29  that the devices are accurate 
2.1 million electron
14:53:32  deposit

14:53:35 . 

14:53:35 This sensitivity can be translated

14:53:37  2.1 KV

14:53:40  in the language of 
the dark matter mass.
14:53:42  Inspired by

14:53:43  these low

14:53:45  energy thresholds that 
we have proposed,
14:53:48  novel and possibly tabletop

14:53:50  experiments to detect satellite

14:53:52  dark matter

14:53:55  superlight

14:53:56  dark matter.

14:53:59  The proposal is shown in panel B

14:54:01  in the left figure

14:54:02  and a bigger scale

14:54:04  detector

14:54:07  could be built by stacking 
up the single-layer units.
14:54:09  Interestingly,

14:54:12  the calculation involves 
capturing dark matter
14:54:15  floating in the three-dimensional 
space and free
14:54:17  electrons confined in

14:54:19  two-dimensional grapheme

14:54:21 .

14:54:24  It depends on the dark matter 
direction, the supposed
14:54:27  detector can readily

14:54:28  check the

14:54:30  directional dependence 
of the signal.
14:54:32  We study

14:54:33  the

14:54:39  are... 

14:54:39 Together with a one-year exposure.

14:54:41  The right figure

14:54:42  shows the result

14:54:42 .

14:54:44  We found that GJ J

14:54:46  dark matter

14:54:51  detector can improve the search 
limit of the dark matter mats might 
14:54:54 three orders of magnitude over 
the existing bounce represented
14:54:57  by the gray shaded area.

14:54:58  Encouraged by this result,

14:55:00  we are now preparing

14:55:01  for the first

14:55:02  KV

14:55:04  scale

14:55:05  using the

14:55:06  sample

14:55:07  devices

14:55:10  that are already fabricating.

14:55:11  Finally,

14:55:13  we are going to

14:55:17  use high energy applications

14:55:20 , low sensitivity of the JG G

14:55:23  devices,

14:55:28  on the neutrino background.

14:55:32  Thank you.

14:55:33  

14:55:33 >>

14:55:41  We will go on to the next talk.

14:55:43  The next speaker

14:55:44  will be

14:55:48  (Unknown name) and she looked

14:55:50  talk about searches for

14:55:53 ...

14:55:56  

14:55:56 >>

14:55:59  Hello, I hope you can hear me.

14:56:04  I work in

14:56:07  a university in Sweden

14:56:08  and

14:56:14  (unknown term).

14:56:18  It's about the searches for 
long-lived particles at the FCC.
14:56:21  What is the FCC

14:56:23 -

14:56:25 ee?

14:56:26  It is an electron

14:56:32  provider proposed as 
a possible first step
14:56:35  toward FC HH,

14:56:36  it will

14:56:39  occupy over 100 km

14:56:42  under the Geneva Lake at

14:56:44  CERN

14:56:45 .

14:56:51  It is proposed with 
a large energy range,
14:56:54  it will have different 
dedicated runs,
14:56:57  like

14:56:59  (unknown term) production of

14:57:01  (unknown term)

14:57:01  and also

14:57:02  even

14:57:03  (unknown term).

14:57:06  It will be mostly a precision

14:57:07  tool

14:57:10  but will also be much 
more because it also has
14:57:13  a large

14:57:14  (unknown term) potential. 

14:57:15 Every measurement

14:57:15  is

14:57:17  (inaudible),

14:57:21  any small deviation 
with respect to the
14:57:23  (unknown term)

14:57:24  is exciting but

14:57:25  you can

14:57:30 ... 

14:57:31 In particular what we want to propose

14:57:33  is

14:57:35  lonely particles are quite cool,

14:57:37  they appear in the BSM models

14:57:39 , they are quite fun

14:57:41  and at the

14:57:43  FCC we have a flak show

14:57:45  for this,

14:57:47  -- Flagship.

14:57:51  The heavy neutron (unknown term)

14:57:53  theory gives

14:57:54  like

14:57:56  matter

14:58:00 , to name a couple. 

14:58:02 There are two parameters

14:58:06  that you care about when you are 
talking about heavy load electrons, 
14:58:10 one is the (unknown term) and the 
other is the (unknown term).
14:58:13  You can have a large

14:58:15  (unknown term), a lonely particle,

14:58:18  it has great potential for 
a large phase of space
14:58:21  with

14:58:24  heavy neutron electrons but 
it's not the only thing.
14:58:29  SCC will have sensitivity for 
action like particles also known as
14:58:34  Alps that have a fun name but they 
are quite interesting and when you 
14:58:38 have small couplings and 
light particles, you have
14:58:45 You can also perform

14:58:49  searches and likely 
their many more motives 
14:58:51 we are listing

14:58:53  to get to know. 

14:58:55 This kind of searches 
for particles are a 
14:58:58 little bit more special 
and bring expire mental 
14:59:01 challenges especially 
for the construction 
14:59:03 because they don't 
detector the sign for 
14:59:05 the future.

14:59:07  We are looking forward 
to exploring this kind 
14:59:09 of opportunities in the 
future and we have a lot 
14:59:13 of intent and you can 
take in the QR code and 
14:59:17 go through it and if you 
want you can contact me 
14:59:21 and we would be happy 
to help you. 
14:59:23 Thank you. 

14:59:25 >>Thank you, the next 
speaker will be
14:59:27  David

14:59:28  who is going to tell 
us about testing
14:59:31  universality

14:59:31  and

14:59:35  pion decays. 

14:59:36 Go ahead, David.

14:59:37  >

14:59:38 >

14:59:44 Thank you Vern, I am 
David from the 
14:59:47 University of Washington 
excitedly know but an 
14:59:50 emergent project we are 
considering which is 
14:59:52 motivated by day-to-day 
driven hits of new 
14:59:55 physics and theoretical 
explanations that 
14:59:56 connect the physics 
scales that are not 
14:59:59 constrained by 
other data.
15:00:00  Let me remind you of 
some of the persistent 
15:00:03 tensions in the standard 
model with respect to 
15:00:06 data.

15:00:12  First experiment I 
spent my time on we are 
15:00:15 suited to release first 
results, Joanne, we 
15:00:17 promise. 

15:00:18 But also, there is a 
deviation from the 
15:00:21 standard model in the 
electron G -2 by few 
15:00:24 standard deviations 
from her recently. 
15:00:26 Next most recent 
computation of the CK on 
15:00:29 first Road unitary stuff 
by standard deviations 
15:00:31 you might ask why? 

15:00:33 As you know there are 
several noncompliant on 
15:00:36 the case on universe 
settle teen violations. 
15:00:38 There are models I can 
explain these effects 
15:00:41 individually, but also, 
the personality, that is 
15:00:43 a tough one, violation 
can connect them.
15:00:48  We will address these 
by 2 precision 
15:00:51 measurements that can be 
carried out with one 
15:00:53 central compact 
apparatus and this 
15:00:55 morning, I saw all 
challenge us to think 
15:00:58 big and think small and 
I think this project 
15:01:01 here satisfies a. 

15:01:02 as suggestedthat. 

15:01:04 By our experimental 
name, the first case- 
15:01:06  directly in the 
nuanced system.
15:01:14  Hi is the ratio of 
charged pie indicates 
15:01:17 from electrons versus 
muons the standard model 
15:01:19 theory is known to 
credible precision of 2 
15:01:22 parts intended the 4th 
in the PDG experimental 
15:01:25 quarter magnitude 
less precise. 
15:01:26 This provides a very big 
window for discovery 
15:01:29 when there is a 
well-known standard lot 
15:01:31 prediction and 
experimental far behind.
15:01:33  The 2nd experiment is 
by a beta decay, easily 
15:01:36 the most theoretically 
cleaned method to obtain 
15:01:39 BOD, pi Beta

15:01:41  is challenging though 
because the branching 
15:01:43 ratio is about 10 to the 
-8 we want to know there 
15:01:48 is a lot better. 

15:01:49 Even with the threefold 
improvement, however,
15:01:51  one can get an 
improvement in the 
15:01:54 diagonal ratio on the 
plot that you see there, 
15:01:57 the diagonal constraint 
in the D&D plane and is 
15:02:00 the first goal. 

15:02:02 The diagonal will help 
relieve the tension you 
15:02:04 see very clearly evident 
in that figure. 
15:02:07 The group of us that 
have formed so far have 
15:02:10 come from high 
beta experiments
15:02:14  and a collection of 
other precision physics 
15:02:16 experiments around 
the world. 
15:02:18 We will draw from our 
collective lessons 
15:02:20 learned to develop 
the next generation 
15:02:22 experiment. 

15:02:23 Essential to this is 
basically the idea of 
15:02:26 using

15:02:27  for pie very fast high 
rate capable and very 
15:02:30 deep calorimeter, liquid 
xenon seems like--
15:02:34  inside will be a 
pixelated tracking 
15:02:36 system and an active 
pixilated stopping 
15:02:38 detector for the charge 
stopping pion 
15:02:40 experiments. 

15:02:41 Appropriate pion 
beings do exist
15:02:43  and may need to be 
modified slightly but 
15:02:46 they are not out 
of the question
15:02:48  and in summary, it is 
basically a modern cost 
15:02:51 high impact relatively 
fast timeline, I want to 
15:02:54 thank you very much 
for your attention. 
15:02:57 >>Thank you David, 
we will now go on
15:03:00  to the next speaker

15:03:01  was Sebastian Ellis,

15:03:02  he is going to report

15:03:04  on a heterodyne 
protection
15:03:06  of axion

15:03:07  dark matter

15:03:09  with superconducting 
cavities.
15:03:11  >

15:03:12 >

15:03:22 Thank you. 

15:03:23 My name is Sebastian 
Ellis and I would like 
15:03:26 to briefly tell you 
about some new approach 
15:03:29 we have proposed to 
detect Axum dark matter 
15:03:32 using a superconducting 
radiofrequency cavity 
15:03:34 SOS cavity. 

15:03:35 The work was conducted 
with the listed offers 
15:03:38 and we have submitted an 
LOI and a CF to any of 5 
15:03:42 somatic areas. 

15:03:43 Axion's, if they exist, 
convert protons in the 
15:03:46 presence of a background 
magnetic field. 
15:03:48 This process is form the 
basis of acts on dark 
15:03:52 matter searches 
for decades. 
15:03:53 Our motivation

15:03:56  is that low mass 
axion's are difficult to 
15:03:58 approach because either 
one needs to build a 
15:04:01 large resonant cavity or 
to somehow dissociate 
15:04:04 the resident frequency 
from the cavity 
15:04:06 geometry, such as by 
using an LC resonator 
15:04:09 which unfortunately 
leads to suppression of 
15:04:11 the signal at low 
axiom masses.
15:04:13  The core of our 
proposed approach is to 
15:04:16 load and SRF cavity 
resident mode, so that 
15:04:18 the background magnetic 
field required for axiom 
15:04:21 conversion is 
oscillating as opposed 
15:04:23 to static. 

15:04:24 The signal frequency is 
then a combination of 
15:04:26 the loaded mode 
frequency in the axiom 
15:04:29 hence the heterodyne 
which can be matched to 
15:04:32 a frequency by small 
deformation of the 
15:04:34 cavity means. 

15:04:35 The proximity of the 
loaded and single modes 
15:04:38 means SRF cavities are 
ideal due to their large 
15:04:41 quality factors which 
are frequently greater 
15:04:43 than 10 to the 10.

15:04:47  The mega collaboration 
in the early 2000's, 
15:04:49 there is a prototype of 
a similar device to 
15:04:52 measure high-frequency 
gravitational waves and 
15:04:54 achieved mode isolation 
of 140 dB. 
15:04:56 Scanning an axiom mass 
requires careful control 
15:04:59 of the cavity geometry.

15:05:06  In this respect, the 
dark SRF collaboration 
15:05:08 and formula has recently 
demonstrated control of 
15:05:10 roughly 1 past the 
10th of the 10. 
15:05:13 These 2 experimental 
presidents form part of 
15:05:15 the basis for a 
theoretical reach 
15:05:18 calculations sown on the 
slide, in particular, 
15:05:20 acute cavity and quality 
factor that are pushing 
15:05:23 the boundary of what has 
been achieved in SRF 
15:05:26 cavities. 

15:05:27 Of particular note, as a 
potential sensitivity to 
15:05:30 the axiom in a mass range

15:05:32  with neither DM radio 
are sensitive as well as 
15:05:35 the sensitivity till 
dark matter across 
15:05:37 almost 9 orders 
of magnitude.
15:05:39  The sensitivity of a 
thermal device shows a – 
15:05:42 green line on the slide 
is enhanced with respect 
15:05:45 to a resonator due to 
the signal frequency be 
15:05:48 much larger your

15:05:52  than the axiom as shown 
on the bottom right and 
15:05:55 in practice, our 
approach is only 
15:05:58 formalized in the higher 
axiom that masses for 
15:06:00 mode isolation and 
cavity vibrations become 
15:06:02 dominant sources. 

15:06:03 For more details on the 
signal please see the 2 
15:06:07 archived links I have 
listed on the slide. 
15:06:10 Of course, continuing 
research and developers 
15:06:12 will be required on both 
cavity design and 
15:06:15 control to make this 
vision a reality and we 
15:06:18 welcome discussion from 
interested groups. 
15:06:20 Thank you for listening. 

15:06:21 >>Thank you. 

15:06:22 We will go on next 
to Marcella
15:06:25  and she is going to

15:06:31 , her talk is towards 
the future world 
15:06:34 exploration at the 
energy frontier. 
15:06:35 Marcella,? 

15:06:36 >>

15:06:37 Yes.

15:06:38  Hello.

15:06:43  I cannot see myself but 
I suppose that is good.
15:06:46  Thank you.

15:06:48  For many decades,

15:06:52  colitis of the industry 
frontier have opened 
15:06:55 windows to the unknown. 

15:06:57 And most recently 
from the discovery.
15:06:59  It is

15:07:00  now the time to think 
about what is next
15:07:03  at the frontier?

15:07:05  What discoveries 
may lie ahead?
15:07:11  Thinking about future 
collateral experiment we 
15:07:13 can brisk challenging 
questions such as what 
15:07:15 is the true nature of 
the exposure and are 
15:07:19 there more scales?

15:07:20  To such an extended 
scale of sector be 
15:07:23 connected to dark matter 
and dark sector.
15:07:25  And a fundamental 
role in the dynamics
15:07:28  of the transition

15:07:32  during their years. 

15:07:33 Moreover, the 
explanation of the matter
15:07:36  and

15:07:38  matter of symmetry in 
the universe can be 
15:07:41 intimately related with 
insistence of new 
15:07:43 particles at the reach

15:07:44  of present and future 
collectives.
15:07:48  We have just started 
to scratch the surface
15:07:51  of missions affixed 
properties. 
15:07:52 As you see

15:07:56  on the right-hand side 
of the slide, it was 
15:07:59 only a couple months ago 
that we stop blushed the 
15:08:03 explosion with any-- 
beyond the next 
15:08:05 generation. 

15:08:06 Future runs may help 
us understand if
15:08:08  the hex is composted

15:08:14  rather than the 
particle ultimately the 
15:08:16 measurements of the 
interactions will lead 
15:08:18 to deep understanding 
of the properties
15:08:20  of this new and very 
intriguing scale of 
15:08:23 particle. 

15:08:23 Future collider's of 
many different types
15:08:27  from a collider with 
an initiative beyond 2 
15:08:30 collider hex factory, 
will give us unique 
15:08:32 handles in systems of 
new particles both 
15:08:35 through their direct 
discovery of signals as 
15:08:37 well as their 
interactions with 
15:08:39 exposure

15:08:39  and other particles. 

15:08:41 Most interesting,

15:08:42  if they exist,

15:08:43  they can establish

15:08:45  and modify the strength

15:08:47  of the

15:08:50  transition and thereby, 
help explaining
15:08:51  Association

15:08:52  with

15:08:53  the mature

15:08:55  -

15:08:55 -

15:09:00  very tantalizing 
possibility. 
15:09:01 It is of great 
importance for the US to 
15:09:05 continue a strong 
participation in the 
15:09:07 global energy frontier 
efforts.
15:09:12  Strong physics 
motivation, coupled with 
15:09:14 unique expertise make 
it natural for the US 
15:09:17 scientists to play a 
leading role in the next 
15:09:20 measure energy frontier 
facilities. 
15:09:22 Including existing 
proposals as we know, 
15:09:24 such as FCC, CBC,

15:09:26  click and MCC. 

15:09:27 Regardless

15:09:28  of where in the world

15:09:31  they may be hostage. 

15:09:32 Thank you.

15:09:32  >

15:09:33 >

15:09:35 Thank you Marcella, we 
will go on to the next 
15:09:39 speaker.

15:09:43  Who is Philip Harris, 
he is going to talk on 
15:09:47 dark quests and long 
quest at 120 GV for the 
15:09:50 main projector. 

15:09:51 >>Hi, I am Philip

15:09:58  Parris from the IT and 
I'd like to tell you but 
15:10:02 the dark West 
experiment, Carquest is 
15:10:04 an idea of an experiment 
to look for dark sectors
15:10:07 , dark sectors to become 
a very popular topic 
15:10:10 over the past few years. 

15:10:13 And we know that if the 
coupling is sufficiently 
15:10:16 small, for light dark 
matter, you can actually 
15:10:19 get the right thermal 
intensity of dark 
15:10:21 matter. 

15:10:22 Not only that, a small 
cup lead could be giving 
15:10:25 a striking signature is 
often leads to long 
15:10:28 lived particles. 

15:10:29 For dark particles, we 
want to use the proton 
15:10:32 main projector formula 
and fire this on the 
15:10:35 target and then using 
uniquely compact
15:10:42  duct to search for a 
long of signatures that 
15:10:45 come from this 
proton feed. 
15:10:47 But the nice thing about 
this experiment is that 
15:10:50 it mostly already 
exists, is called the 
15:10:53 spin quest experiment 
and is used currently 
15:10:55 for nuclear physics. 

15:10:57 We propose a modest 
upgrade in this 
15:10:59 experiment by adding an 
EM calibre from the 
15:11:02 Phoenix experiment

15:11:04  at minus cost and this 
will give us access to 
15:11:07 normally displaced 
neurons but displaced 
15:11:09 electrons and displaced 
hadrons. 
15:11:10 You can see a wealth of 
signatures and all of 
15:11:14 this can be run in 20 
2324 before the PIP to 
15:11:18 upgrade. 

15:11:18 To give you an idea of 
our sensitivity, here on 
15:11:22 the bottom left, we 
have sensitivity
15:11:24  on dark photons and 
you can see we have 
15:11:27 comparable sensitivity 
to other experiments 
15:11:29 such as phaser and any 
62+ plus, within the 
15:11:32 similar time 
scales 2024. 
15:11:34 We are capable of 
running a broad range of
15:11:37 -- including Acxiom 
like particles
15:11:41  in elastic dark matter, 
dark photons and so on.
15:11:45  And, with our LOI, 
we need to actually
15:11:48  put

15:11:48  modules into the test

15:11:50 ing

15:11:51  and looking and say the 
performance of the data 
15:11:55 rates

15:11:59  are for the potential 
upgrade of dark quest 
15:12:02 and further, we aim to 
build the full 
15:12:04 simulations we can 
really confirm our 
15:12:07 sensitivity and prove 
many of the new 
15:12:09 interesting practices. 

15:12:10 Thank you. 

15:12:11 >>Thank you, Phil. 

15:12:13 We are going to go onto 
the next speaker
15:12:16  who is Marcel. 

15:12:17 He will offer 
perspective on a unified 
15:12:20 US particle physics 
program. 
15:12:21 >>Thank you very 
much Juel.
15:12:24  And thank you for 
giving me the 
15:12:27 opportunity to 
speak to this.
15:12:31  I would like to speak 
to a perspective on 
15:12:34 creating a future 
particle physics program 
15:12:36 and the US. 

15:12:38 In my opinion, a healthy 
vibrant particle physics 
15:12:40 program cannot 
be dominated
15:12:46  by only megaprojects, 
but really needs a 
15:12:48 balanced portfolio of 
small, medium, and large 
15:12:50 scale projects. 

15:12:52 And that means, I also 
think that the field 
15:12:55 should exploit all 
opportunities that it 
15:12:57 has to advance 
its science. 
15:12:59 I know that this source

15:13:00 , the world's 
most intense
15:13:02  nutrient source

15:13:04  is actually also 
the brightest
15:13:07  and the cleanest 
neutrino source in the 
15:13:10 world. 

15:13:10 Just

15:13:13  demonstrate the 
scientific capabilities 
15:13:14 through the world's 
first discovery
15:13:17  of elastic and neutrino 
scattering not just
15:13:19  forms

15:13:22  like in 2017, but 
actually twice
15:13:25  with the recent 
demonstration of sevens
15:13:27  in the ion targets.

15:13:30  The SNS is in 
the process
15:13:35  of a power upgrade and 
they will have 2.8 MW
15:13:38  proton driver in 2025.

15:13:43  In there I think will 
provide unique 
15:13:45 opportunities for the 
field for neutrino 
15:13:47 physics.

15:13:52  Furthermore, the 2nd 
dark station is being 
15:13:55 constructed. 

15:13:56 And that could also 
potentially provide 
15:13:58 space in the 2nd target 
station building to 
15:14:00 house future neutrino 
experiments.
15:14:02  Now, the SMS is not 
the only neutron and 
15:14:05 neutrino source

15:14:06 . 

15:14:07 The high flux isotope 
reactor also provides a 
15:14:10 continuous

15:14:10  and a well understood 
source of electron 
15:14:13 anti-neutrinos.

15:14:13  2 upgrades

15:14:15  are being considered.

15:14:20  In both upgrades 
provide an opportunity 
15:14:22 for fundamental physics 
experiments
15:14:23  that is even strongly 
supported by a recent
15:14:27  B section report. 

15:14:28 This particle 
physics program
15:14:29  can be expanded also

15:14:32  to study not 
only neutrinos,
15:14:35  also neutrons such as 
small-scale searches
15:14:37  for mirror neutron

15:14:39  oscillations.

15:14:47  There are 2 other 
projects that I would 
15:14:50 like to mention 
at the lab. 
15:14:52 What is the materials 
plasma exposure 
15:14:54 experiment facility that 
will measure materials 
15:14:56 up to 50 displacements 
per hour. 
15:14:58 Which could inform the 
target tree that is 
15:15:01 being considered for the 
intensity frontier 
15:15:03 program and also

15:15:10  the nuances spin 
residence facility is 
15:15:12 being considered that 
build 2×10 to the Nuance 
15:15:15 per 2nd that could be a 
terrific source of 
15:15:18 nuance for fundamental 
physics studies. 
15:15:20 So, my 3 minutes here 
really is an invitation
15:15:23  from Oak Ridge to the 
high-energy physics 
15:15:25 community to consider 
these resources to build 
15:15:28 this future program. 

15:15:29 And I would like to 
remind you, together, we 
15:15:32 are stronger than this. 

15:15:34 Thank you very much. 

15:15:36 >>Thank you Marcel. 

15:15:37 Next speaker will 
be Ryan ignored,
15:15:39  and he will

15:15:43  tell us the culture 
change is necessary and 
15:15:46 it requires strategic 
planning.
15:15:47  Ryan, go ahead.

15:15:48  

15:15:48 >>

15:15:50 Thank you for organizing 
this and they could to 
15:16:00 The evidence is then,

15:16:02  racism permeates society

15:16:07  and the community. 

15:16:08 The evidence is that black 
people and persons of color
15:16:11  are minority ice by

15:16:14  policies and we are

15:16:16  disenfranchise.

15:16:20  When the reality is acknowledged by 
groups in the scientific community
15:16:23  responses have included 
a reinvigoration
15:16:28  of diversity initiatives, creating 
committees and generating solutions
15:16:31  before consulting the main excerpts

15:16:34  -- experts.

15:16:37  It can be dangerous 
for the purported
15:16:39  beneficiaries

15:16:42 , and for enabling a sustained effort

15:16:44  that goes beyond

15:16:45  a few initiatives

15:16:46  or committees.

15:16:47  Therefore,

15:16:52  we make multiple recommendations 
which are detailed in our Snowmass
15:16:56 , linked at the top of the slide.

15:16:59  These include things

15:17:01  that many of us are 
familiar with our
15:17:06  design of science experiments like 
becoming familiar with the problem 
15:17:09 space and state-of-the-art

15:17:10  processes, partnering with experts

15:17:12  and strategic planning.

15:17:13  These also include

15:17:17  some newly framed elements like 
constructive and compassionate
15:17:19  conflict and shared leadership.

15:17:21  Imagine we are pursuing a new

15:17:24  understanding of some 
aspect of the universe,
15:17:26  what are

15:17:30  the processes we go through to 
design the experiment and build 
15:17:34 collaboration? 

15:17:34 What actions or strategies 
do we avoid?
15:17:36  How do we prioritize

15:17:37  approaches to those challenges?

15:17:43  We establish clear and measurable 
goals and write down requirements to 
15:17:46 achieve those goals 
and then we grind,
15:17:49  periodically revisiting the 
strategy until the goal is a disk
15:17:53  accomplished.

15:17:54  Now imagine

15:17:57  this effort is creating a 
just research environment
15:18:00  because it is a fundamental 
issue in our community
15:18:03  and the right thing is 
to do something about it.
15:18:06  If we consider the challenge urgent,

15:18:08  it means we have to deal 
with the tension between
15:18:11  triage

15:18:12  and acting

15:18:13  on research

15:18:17  elements while also planning 
all of the elements coherently.
15:18:22  We recommend that we as a community 
access the creativity and discipline
15:18:26  were using science efforts 
and apply it to work
15:18:29  for justice in the 
scientific community.
15:18:32  This includes using strategic 
planning and partnering with experts
15:18:35  to get to a more equitable

15:18:37  decision-making

15:18:38  process than we have now.

15:18:40  Examining what we've done 
in the past and updating
15:18:43  those methods.

15:18:45  In some ways this work is similar 
to our work in scientific
15:18:48  efforts,

15:18:49  we need to establish new

15:18:55  knowledge, if we want something 
different we need new approaches and 
15:18:58 solutions and an appropriate plan. 

15:19:00 Now we've spent a lot of our time

15:19:02  imagining what our future of 
understanding the universe looks like
15:19:05 , we need strategic 
planning to carry out
15:19:08  our

15:19:09  future imagination of justice.

15:19:12  

15:19:12 >>

15:19:14  Thank you, Brian.

15:19:15  The next

15:19:21  speaker is Kelly who will talk 
about Snowmass as a path toward 
15:19:24 cultural change and the 
role of collaborations.
15:19:26  

15:19:27 >>

15:19:31  My name is Kelly and I speak on 
behalf of a group of folks from the 
15:19:36 neutrino and dark matter 
experiment communities.
15:19:38  As we have heard, inequities 
and marginalisation of
15:19:43  identity groups continue to plague 
our society as a whole and physics 
15:19:46 in particular.

15:19:47  The evidence is striking. 

15:19:48 75% of undergrad women 
in physics report
15:19:51  experiencing sexual harassment

15:19:52  and the number of undergrad physics

15:19:56  degrees awarded to black students 
in the US has stagnated or declined
15:20:00 . 

15:20:00 Our subfield

15:20:02  is a unique situation since 
many of us belong to
15:20:08  multi-hundred or thousand person 
collaborations which continue to 
15:20:10 grow.

15:20:11  Our collaborations radically 
expand the sites we can pursue
15:20:13  and introduce new challenges,

15:20:18  they bring together people from 
a wide variety of backgrounds. 
15:20:21 Since they play

15:20:24  such a large role in the day-to-day 
experiences of many scientists in our 
15:20:27 field, every collaboration should be 
grappling with the issues of equity 
15:20:31 and justice with the same energy 
with which we pursue our science. 
15:20:34 As Brian asserted, we must not

15:20:36  approach this uninformed, we 
must draw on the results from
15:20:41  reports and community calls to 
action like those listed at the 
15:20:45 bottom of the slide. 

15:20:46 This can and should

15:20:47  be urgently happening 
in all collaborations,
15:20:49  independent of the Snowmass process.

15:20:52  Collaborations can't do it alone.

15:20:56  We often lack the resources, the 
institutional infrastructure
15:20:59  or political standing required 
for meaningful change.
15:21:04  For example many collaborations 
have instituted codes of conduct
15:21:07  but

15:21:07  struggle to enforce them

15:21:09  when the parties come from different

15:21:13  institutions or different countries 
with different sets of regulations.
15:21:16  Solutions to these crosscutting 
issues will
15:21:20  necessarily come from working 
together with funding agencies, 
15:21:23 national labs,

15:21:23  universities and professional 
societies
15:21:26  and this is the power 
of the Snowmass process
15:21:28  – it is a chance for 
us as a community
15:21:31  to describe the future we 
want to see for our field
15:21:36  and start planning for the changes 
that will bring us closer to that 
15:21:39 future. 

15:21:40 For this reason, the 
resulting P5 report
15:21:42  should include recommendations 
to put it on a path toward a more
15:21:46  equitable and just community.

15:21:47  These recommendations, informed 
by strategic planning
15:21:50  and expertise in appropriate 
discipline should support
15:21:55  and empower collaborations to 
pursue justice, as we do our science 
15:21:58 because

15:21:59  this problem of inequity 
in our field will not solve
15:22:02  itself.

15:22:02  We must face it head on, every day,

15:22:05  into the future,

15:22:07  both in our collaborations 
and as a community.
15:22:10  Thank you.

15:22:10  

15:22:11 >>

15:22:12  Thank you, Kelly.

15:22:14  We will now move on to

15:22:16  Sven

15:22:24  who will talk about gas TPCs with 
directional sensitivity to dark 
15:22:27 matter, neutrinos and BSM physics. 

15:22:29 >> I'd like to talk you

15:22:31  about Cygnus,

15:22:33  the proposal to build directional

15:22:38  detectors searching forward 
neutrinos, dark matter and BSM 
15:22:41 physics.

15:22:41  It's been demonstrated 
that that gas correction
15:22:45  chambers with high definition 
charge readouts can
15:22:47  detect

15:22:49 , shown on the top left seen in 3D

15:22:52 ,

15:22:52  electronic readouts and to die

15:22:56  2D with optical readouts.

15:22:57  We can have fine readout

15:22:59  segmentation,

15:23:01  and

15:23:03  low enough that the diffusion scale

15:23:05  is smaller than

15:23:07  the report went.

15:23:10  This enables not only 
directionality but particle 
15:23:12 identification as shown here,

15:23:16  very low energies in the KV range,

15:23:18  electron

15:23:18  look very

15:23:20  different in the resolution.

15:23:21  This allows

15:23:23  us to open the door

15:23:25  to large experiments

15:23:27  and directionality.

15:23:31  The directionality is 
key for penetrating
15:23:36  neutrino flow and distinguishing 
neutrinos from other sources such as 
15:23:39 the sun and the oath from the

15:23:41  dark matter is coming from 
a different direction.
15:23:47  To get sensing our exposure, 
to build a multi-
15:23:50 science underground Observatory,

15:23:51  this effort

15:23:52  has now

15:23:52  been

15:23:54  built

15:23:58  an international

15:24:04  effort receiving its first funding 
in Europe and Australia.
15:24:07  Up what I would like to emphasize 
is the long-term goal
15:24:10 , a nice long-term research

15:24:16  project here that allows you to do 
new physics measurement for every 
15:24:19 factor of 10 in exposure,

15:24:22  we have released a design paper 
which is on the archive,
15:24:25  but many other measurements 
are possible,
15:24:27  very small

15:24:29 , should be able to

15:24:32  observe the (unknown term) effect,

15:24:35  scaling up from 1 to 10 m³

15:24:37  should

15:24:38  detect

15:24:41  elastic neutrino scattering is

15:24:43  in the neutrino beam could be

15:24:45  the one shown here or the SMS

15:24:47 .

15:24:48  Going up to 10 m³

15:24:52  as shown on the plot on the 
right, you should be able to
15:24:56  set the world's strongest limits.

15:24:58  For

15:25:03  every order of magnitude increase 
in exposure, new physics becomes 
15:25:06 possible. 

15:25:06 We take this to a

15:25:08  scale

15:25:10  facility at room temperature, 
lower cost,
15:25:12  this should be able to detect free

15:25:14  neutrinos

15:25:16 , revealing the physics of the heat

15:25:19  generation of the earth. 

15:25:21 For Snowmass many

15:25:22  proposals related to 
this was submitted,
15:25:25  many of them address beyond 
the standard model
15:25:28  aspects of it, searches 
for new particles,
15:25:31  and unfortunately this slide

15:25:32  doesn't show this

15:25:33 ,

15:25:34  but the main

15:25:37  message is there are 
many unexplored ideas
15:25:39  for Snowmass

15:25:39  and we

15:25:42  invite you to join this exciting

15:25:44  effort

15:25:45 , we plan

15:25:46  a workshop

15:25:47  this fall,

15:25:48  the cosmic neutrino

15:25:49  implementation for

15:25:52  frontiers exploring this further.

15:25:53  Thank you.

15:25:55  

15:25:55 >>

15:25:57  The next speaker is Matthew

15:26:03 , he will tell us about searching 
for Millie charged particles with 
15:26:06 center later based detectors.

15:26:07  

15:26:08 >>

15:26:12  Millie charged particles are well 
motivated through kinetic mixing
15:26:14  between the standard model

15:26:16  and a possible dark sector.

15:26:21  Coladas and neutrino saucers 
but general-purpose detectors
15:26:27  typically they will be sensitive as 
the interaction probability goes to 
15:26:30 the charge of the particle squared. 

15:26:32 How can we find such signatures? 

15:26:34 The idea is to use a 
long center later bar
15:26:37 ,

15:26:37  and beam them to detect small

15:26:40  charged particles

15:26:43  and you can see on the left ear.

15:26:48  The expected single from Millie 
charged particles traveling through 
15:26:50 the back tractor

15:26:51  detector

15:26:53  and each part must be capable of

15:26:56  detecting a single 
scintillation photon
15:26:57 .

15:27:00  The design is important 
because backgrounds can be
15:27:02  rejected

15:27:03 ,

15:27:06  coming with a small 50 ms window.

15:27:08  This design is easy 
to scale and adapt
15:27:10  and this has been used

15:27:13  at a variety of societies,

15:27:16  facilities,

15:27:17  to detect

15:27:18  neutrino

15:27:19  sources

15:27:24 ... 

15:27:24 You can see the sensitivity curves 
for detections on the right-hand side
15:27:28  in blue and purple

15:27:29 . 

15:27:30 There is a possibility for detecting

15:27:34 ... 

15:27:35 How do we know such a 
detection design work
15:27:38 ? 

15:27:38 In 2018 a small prototype

15:27:40  was installed at CERN,

15:27:42  this rants

15:27:42  successfully

15:27:45  characterizing

15:27:50  backgrounds as well as setting the 
first limits in Millie charged 
15:27:53 particles at the hadron Collider.

15:27:55  You can see the results of this 
on the right-hand side in red.
15:27:59  This was published

15:28:00 , the data was also used to provide

15:28:02  important lessons to guide

15:28:03  future detectors

15:28:06 . 

15:28:06 Summarizing

15:28:07  for Snowmass,

15:28:10  the idea is we want to use the 
data from the demonstration
15:28:14  to update protections for full-scale

15:28:15  detectives with consideration 
of the backgrounds
15:28:19  as well as a fully calibrated 
SA simulation.
15:28:22  And important lessons for

15:28:24  detectors

15:28:26 , for example,

15:28:29  we have observed that three 
layers was not enough
15:28:32 , for layers was required.

15:28:34  This is timely

15:28:36  as a collaboration 
has recently saved
15:28:38  received

15:28:41  funding, this is an important 
intermediate step
15:28:43 .

15:28:45  And the input

15:28:47  will because equal for that

15:28:49  project. 

15:28:50 In conclusion,

15:28:51  scintillation

15:28:54  base detection over 
the next few years,
15:28:56  it will be an exciting time

15:28:57  for the

15:28:59  potential discovery 
of Millie charged
15:29:00  physics.

15:29:03  

15:29:03 >>

15:29:05  Thank you,

15:29:06  the next

15:29:07  speaker will talk about

15:29:08  measurement

15:29:13  of the fine structure constant 
as test of the standard model.
15:29:15 the community for 
paying attention.
15:29:16  

15:29:17 >>

15:29:21  h

15:29:21 ello this is from

15:29:24  Berkeley, the fine 
structure concept 
15:29:25 designs the strength of 
the electromagnetic 
15:29:27 interaction and 
therefore underlies most 
15:29:29 of the physics

15:29:31  that we are familiar 
with. 
15:29:33 The most precise 
measurements of the fine 
15:29:36 structure constant are 
based on 2 effects, one 
15:29:38 is the anomaly which 
has precision off 1/4
15:29:45  part per billion and 
the other is measuring 
15:29:48 the ratio of the plan 
constant with the 
15:29:50 particle mass and 
combining that with the 
15:29:53 Richter constant. 

15:29:54 This has so far been the 
most precise measurement
15:29:58  of the fine structure 
constant that our 2018 
15:30:01 results of being over 
137 or 35999046.
15:30:03  The power of such 
measurements
15:30:06  or about the standard 
physics is shown on the 
15:30:09 right-hand side of 
the slide that shows
15:30:17  all the terms that 
enter the prediction of 
15:30:19 the fine structure 
constant at the current 
15:30:22 expert mental position. 

15:30:23 And you will see it's 
not only the first 5 
15:30:27 orders of quantum 
electrodynamics can we a 
15:30:29 nation but also the 
existence of the neuron 
15:30:32 and hydrants features 
and about sending a at 
15:30:35 the current accuracy. 

15:30:36 The goal of our project 
is to improve the 
15:30:39 accuracy

15:30:40  to the fine structure 
constant measure by more 
15:30:42 than a model of 
magnitude and this would 
15:30:45 for the first time 
reveal for example, the 
15:30:48 existence of the low 
energy experiment, this 
15:30:51 would get very close 
depending on other 
15:30:53 auxiliary

15:30:54  measurements that are 
needed and importantly, 
15:30:56 on a remeasurement of 
the neuron's magnetic 
15:30:58 moments that is being 
prepared by Jerry 
15:31:01 Gabriels. 

15:31:02 The key to our improved 
experiment, the 
15:31:04 experiment

15:31:07  itself by measuring the 
recoil velocity of an 
15:31:10 atom that has scattered 
a photon and as you can 
15:31:13 imagine, this velocity 
depends
15:31:16  on the normality's 
speckled patterns. 
15:31:18 Our approach is to take 
the control over the 
15:31:21 spatial structure

15:31:28  of the laser beam to an 
unprecedented level and 
15:31:31 then experiment shown on 
the left is essentially 
15:31:34 a massive vacuum chamber 
that has been optimized 
15:31:36 to provide a nearly 
perfect conditions and 
15:31:39 propagation in 
the middle. 
15:31:40 The recoil velocity will 
be measured in an atomic
15:31:43  and you can see the 
space-time diagrams of 
15:31:46 the atomic trajectories 
of the graphs at the 
15:31:49 bottom of the page. 

15:31:51 If everything works fine 
we hope to get a 10 to 
15:31:55 20 part result on the 
fine structure constant
15:32:00  in 3 years, this would 
amount to a broad and 
15:32:03 deep test of the 
standard model, lots of 
15:32:06 pieces of the standard 
model have to be right 
15:32:09 in order for the 
comparison of the 
15:32:12 electrons momentum to 
check out and is also 
15:32:15 brought a sensitive 
search for dark matter 
15:32:17 candidates. 

15:32:18 Thank you very much 
for your attention. 
15:32:20 >>

15:32:21 Thank you. 

15:32:22 The next speaker will be 
Harvey Newman, he is 
15:32:25 going to tell us about 
future information and 
15:32:28 communication 
technologies, for the 
15:32:29 LAC and beyond 
the limit. 
15:32:31 Harvey, go ahead. 

15:32:32 >>Hello everyone, I am 
Harvey Newman from 
15:32:35 Caltech, I'd love to 
give a perspective on 
15:32:38 coming revolutions 
in information
15:32:39  and communication 
technologies. 
15:32:40 Both because

15:32:41  they shape the way we 
actually do research
15:32:44  and also

15:32:47  how the environment 
will change. 
15:32:49 And also, because 
it represents
15:32:51  opportunities for 
future planning
15:32:52  some of which

15:32:53  may not have already 
been realized.
15:32:58  On the front of 
semiconductors there 
15:33:00 have been struggles

15:33:01  to go beyond

15:33:03  and feature the 
roadmaps that go down 
15:33:05 below the 1 m level 
around 2030
15:33:08 ,

15:33:09  and so there has 
been arriving tied
15:33:11  on new technologies

15:33:14  on the unseen laws 
which can maintain the 
15:33:17 progress and the 
capability increase
15:33:21  which is really driver 
of progress and also
15:33:27  unlike other fields the 
industry is already 
15:33:29 grappling with the fact 
that there are 
15:33:32 continuing to progress 
that will have to
15:33:34  undergo these 
transitions.
15:33:36  Among the technologies

15:33:40  are photonics which 
have surface waves
15:33:42  or

15:33:51  things other than 
electrons that carry 
15:33:53 signals and overcome the 
energy speed barriers 
15:33:55 which we are familiar 
with and we actually 
15:33:58 build into some of our 
detecting designs and so 
15:34:01 this is an opportunity 
to go beyond them. 
15:34:04 And also, our range of 
new methods that have 
15:34:07 tested technologies, 
materials using surfaces
15:34:09  which are structured 
which enable you to 
15:34:11 shape and direct

15:34:12  form white fronts and 
change beams and use 
15:34:15 freedoms such as

15:34:18  momentum. 

15:34:18 Optical communication 
that we use every day
15:34:24  also in experiments 
completely change and 
15:34:26 so, multicore 
farmers using
15:34:28  fibers

15:34:33  fibers using photons

15:34:35  will come to the 
forefront very soon.
15:34:40  These are the 
opportunities, and I 
15:34:42 think, and future 
planning,
15:34:44  it is important to 
realize that some of the 
15:34:47 barriers we have built 
into our designs
15:34:49  will probably be 
bypassed and replaced, 
15:34:51 so these when these 
emerge we should take 
15:34:54 advantage of them was a 
pause from the system 
15:34:57 point of view, 60 
wireless is already 
15:35:00 being formed

15:35:00  for the standard, which 
will take another 10 
15:35:03 years. 

15:35:04 There is been a new 
generation of wireless
15:35:07  every 10 years. 

15:35:08 And this will also change

15:35:10  the way we enter 
communicate
15:35:12  with universities 
that harkens
15:35:14  directing how we handle

15:35:15  systems

15:35:18  of entities which 
are mobile
15:35:21  and overlapping 
ensembles of objects
15:35:30  on mobile scales. 

15:35:32 This again will be 
revolutionary. 
15:35:34 Finally, I wanted to 
say, when you look at 
15:35:37 our roadmaps which go up 
several years, we also 
15:35:40 thought back to what is 
the timing from first 
15:35:43 ideas to products and 
it's typically about 15 
15:35:46 years. 

15:35:46 We should have a 
flexible view, keep a 
15:35:49 watch on all these 
technologies, and 
15:35:51 ongoing revolutions 
and use them in our 
15:35:54 experiments and our 
future planning, thank 
15:35:56 you. 

15:35:57 >>

15:35:57 Thank you Harvey. 

15:35:59 The next speaker is 
Mariana and she will 
15:36:02 tell us about

15:36:04  atomic clocks and 
precision spectroscopy 
15:36:06 measurements for dark 
matter and dark sector 
15:36:08 searches surges. 

15:36:09 Go ahead. 

15:36:10 >>

15:36:14 Thank you so much. 

15:36:15 This project isn't a 
collaboration of 7 
15:36:18 countries and about 
30 people. 
15:36:19 And the identity 
of atomic and
15:36:22  nuclear clocks to search

15:36:23  for physics be a 
standard model comes 
15:36:26 through the 
extraordinary 
15:36:27 improvements

15:36:32  in the precision 
of the clocks. 
15:36:34 As you can see, in the 
graph, on the left-hand 
15:36:38 side, the blue line, 
that is a program 
15:36:40 progressive micro 
meant crop
15:36:47  clocks, about 16 
fraction percentage in 
15:36:49 the optimal clocks which 
are based on particle 
15:36:52 frequency however, are 
now 10 to the -18 and 
15:36:55 approved by 4 orders 
of magnitude in recent
15:37:00  15 years or so. 

15:37:01 And we really don't know 
how far this will go. 
15:37:05 There is no technical 
reason why it can 
15:37:08 continue improving 
clocks by more orders of 
15:37:10 magnitude. 

15:37:11 And just to put things 
into perspective, as a 
15:37:14 fraction of precision of 
clocks at 10 to the -18, 
15:37:17 means that this clock, 
the model is one 2nd. 
15:37:21 In this progress enables

15:37:22  various studies of 
physics beyond the 
15:37:25 standard model in 
clocks, and it all 
15:37:27 started from the 
question of the 
15:37:29 fundamental constant 
because the fundamental 
15:37:31 constant such as a fine 
structure constant was 
15:37:34 measuring actually 
changes with time or 
15:37:36 space. 

15:37:36 Then so do automatic 
frequencies or nuclear 
15:37:39 frequencies and still 
do all the call
15:37:41  frequencies and you can 
detect them by looking 
15:37:44 at ratios of the clocks. 

15:37:46 And that recently was 
realized dark matter
15:37:49  also fundamental 
constants. 
15:37:50 Either transient or

15:37:52  Austro literary. 

15:37:53 There many new 
projects now
15:37:56  which already have new 
results, looking for 
15:37:58 dark matter clocks

15:38:05  the equivalence 
principle, searches the 
15:38:07 violation and also 
proposal to do rotation 
15:38:10 of detection

15:38:10  and recent proposals of 
quantum sensors such as 
15:38:13 clocks would actually 
act for
15:38:15  multi-messenger 
astronomy.
15:38:23  There also later 
projects which don't 
15:38:25 specifically have clocks 
on other precision 
15:38:27 experiments such as 
searches for new force 
15:38:29 mediators.

15:38:33  And, the motivation for 
all of those experiments 
15:38:36 besides extraordinary 
precision of clocks is 
15:38:38 that a number, many 
of these theories
15:38:40  propose to solve 
various problems of the 
15:38:43 standard model, actually 
remove those fields and 
15:38:45 we have now an 
opportunity
15:38:47  to really reach 
those experiments
15:38:50  by several orders of 
magnitude by building 
15:38:52 clocks which have 
the highest
15:38:56  sensitivity and fact. 

15:38:57 In fact, this project is 
a part of the developing 
15:39:01 field of precision of 
the Potomac there are 30 
15:39:04 letters of interests

15:39:08  of atomic physics 
communities and our goal 
15:39:10 for this normal process 
is to redevelop particle 
15:39:13 particle physics 
collaborations and hope 
15:39:15 it brought interest in 
those experiments and to 
15:39:18 have

15:39:19  strong collaboration to 
actually fully realize 
15:39:21 the potential. 

15:39:22 They could so much 
for your pension
15:39:25  attention. 

15:39:26 >>Thank you.

15:39:30  The next speaker is 
Francesco Giovanni
15:39:35  and he will talk about 
3D proton tomography at 
15:39:39 the IC TMD distributions.

15:39:41  You can start now.

15:39:42  

15:39:42 >>

15:39:46 Thanks, hello everyone, 
today I will present 
15:39:48 this one slide about 
tri-mental description on
15:39:52  colitis and I will be 
happy to motivate future 
15:39:55 studies and mass 
communicate about
15:39:57  TMD

15:39:58  functions.

15:40:00  My work is a basic name

15:40:03  ongoing project 
in collaboration
15:40:07  with the Citigroup and 
Muniz city in Italy. 
15:40:10 And we know that

15:40:11  they represent 
a co-sector
15:40:14  of the electronic 
colitis studies. 
15:40:16 And we know that without

15:40:20  this next generation of 
colliding machines, it 
15:40:22 will be possible to study

15:40:24  to perform its 
systematic study
15:40:26 ,

15:40:29  in particular from the 
TMT point of view, which 
15:40:32 actually presents one of 
the most challenging and 
15:40:35 the less known sector 
of the interactions.
15:40:39  With the aim of 
fulfilling the need for 
15:40:42 affects of models,

15:40:43  the terminology, we 
provide systematic 
15:40:44 framework

15:40:46 , which allow us to 
calculate at the end of 
15:40:49 this approach 
and polarize
15:40:51  TMD

15:40:51  function

15:40:52  and

15:40:56  we know that 
the information
15:41:01  distribution and mainly 
in large, in reach,
15:41:03  our knowledge,

15:41:08  and our knowledge 
coming from the standard 
15:41:10 one dimension 
description at the end 
15:41:12 of standard functioning 
and can be used
15:41:15  to

15:41:18  mention autographing 
studies
15:41:21  in particular, 
the axle acts.
15:41:23  So

15:41:27  my work may 
be referred to
15:41:29  the first paper 
in collaboration
15:41:31  with my colleagues

15:41:32  and here as an example

15:41:35  on the right block, 
on the right
15:41:39  lower corner of the 
slides, I present
15:41:42  to possible

15:41:42  combinations

15:41:44  of this distribution,

15:41:46  the density on the left

15:41:49  and the density on the 
right, there is a 
15:41:52 functional process.

15:41:55  We see here the plot of 
oscillation on these 2 
15:41:59 densities, along

15:42:02  the trances momentum 
plane, they move it to 
15:42:04 the left one in response 
to the density of 
15:42:08 finding polarizing and 
not polarizing in this 
15:42:10 case,

15:42:11  the other one is on 
the right, we have
15:42:15  the one which 
corresponds
15:42:17  that gives us the 
probability of finding
15:42:19  a secondary

15:42:20  polarizer

15:42:25  in this case, again 
proton, and this is just 
15:42:28 an example to show

15:42:29  to see,

15:42:30  how

15:42:32  it's enough to 
predict things
15:42:34  in the behaviour

15:42:39  of the densities, 
taking into account the 
15:42:42 polarization out 
of the aim 2nd one
15:42:44  and after our 
calculation
15:42:45 ,

15:42:47  and distinguishing 
function, we will perform
15:42:52  the distinguishing 
function and provide 
15:42:53 support

15:42:54  to physics.

15:42:55  Thanks.

15:42:56  >

15:42:56 >

15:43:00 Thank you, the next 
speaker will be Richard 
15:43:02 Tomlin, who will talk 
about colliding elastic 
15:43:05 PPE

15:43:05  scattering to test

15:43:07  P violation are

15:43:08 -

15:43:08 -

15:43:10  go ahead, Richard.

15:43:11  

15:43:11 >>

15:43:13 I'm Richard from

15:43:14  Cornell,

15:43:16  and you heard

15:43:20  in the earlier talk, 
about the pronounced
15:43:22  closing lab

15:43:24  in Germany, the stock 
described in application
15:43:27 .

15:43:27  The goal is

15:43:28  to detect

15:43:32  violation or parity 
violation
15:43:33  in seemingly

15:43:35  proton proton

15:43:37  proton neuron 
scattering.
15:43:40  Lien and Wolfenstein

15:43:45  have independently 
proposed
15:43:51  semi strong symmetry 
breaking mechanisms 
15:43:52 going beyond the 
standard model.
15:43:54  The goal will be to 
improve symmetry 
15:43:57 violation

15:43:58  upper limits by more 
than one order of 
15:44:01 magnitude's, approaching

15:44:02  one part per thousand.

15:44:11  The method suppose 
it is proton neurons 
15:44:13 gathering, detection 
chambers at the 
15:44:15 intersection point of a 
single ring providing 
15:44:17 beam storage ring,

15:44:21  protons travel in one 
direction, pseudo-frozen 
15:44:23 neurons in the other. 

15:44:25 This fixes the spin 
states of both
15:44:28  particles. 

15:44:28 Being a storage ring, 
the centre of masses is 
15:44:31 moving only slowly

15:44:34  so both scattered 
energies lie in the 
15:44:37 narrow range, for 
example, from 40 to 65
15:44:40  kinetic energy. 

15:44:41 The scattered particles 
will flow
15:44:45  tracking chambers. 

15:44:46 Some will undergo 
nuclear scatters
15:44:49  in the tracking chamber 
plates, this will 
15:44:51 provide

15:44:53  efficiency of 1%

15:44:56  analysing power of 0.4,

15:44:58 .

15:45:01  Finally, I turned 
to the anticipated 
15:45:03 performance.

15:45:04  The storage ring 
luminosity will be 0.6
15:45:06  in hurst Miller 
binds per 2nd.
15:45:11  This will produce 100 
million clean evens per 
15:45:14 year.

15:45:15  A clean, I mean 2 
unambiguous single tracks
15:45:18  detected in time 
coincidence.
15:45:28  Most will be cold in 
here, except for centre 
15:45:36 These events will provide accurate,

15:45:37  independent

15:45:39  measurements are

15:45:39  over

15:45:44 , more than 1 million of these events

15:45:50  will have one or the other 
particle, nuclear scattering in the 
15:45:53 dragging chambers. 

15:45:54 These polarization measurements are

15:45:55  sensitive to symmetry

15:45:59  violations, 10,000 events will have 
both particles of nuclear scattering
15:46:02 ,

15:46:04  these are particularly sensitive 
to symmetry violation
15:46:07 . 

15:46:07 For these events both

15:46:09  initial and states are known

15:46:11 , and final state

15:46:14  polarizations will 
have been measured.
15:46:16  These events

15:46:17  lead us to expect

15:46:19  to be able to reduce

15:46:21  the upper limits

15:46:24  on symmetry violation 
that I mentioned before.
15:46:27  Thank you.

15:46:30  

15:46:30 >>

15:46:52  Thank you.

15:46:58  For selecting me to talk. 

15:47:00 I'll talk to you about

15:47:04  Max has to bore water a 
breakthrough tax attack matter and
15:47:07  neutrinos.

15:47:12  We have started to form a 
collaboration with the institutions 
15:47:15 you see on the upper right. 

15:47:17 White is metastable water?

15:47:19  You think of super heating 
or super cooling,
15:47:21  we are focusing on super cooling,

15:47:24  which has never been used in HDP

15:47:26 .

15:47:28  The idea here is to establish 
a new technology
15:47:32  that can be used to drive discovery 
in the 21st-century like
15:47:36  the bubble chamber did

15:47:39  a long time ago. 

15:47:40 In our prototype we have looked at

15:47:42  supercooled water

15:47:44  and we call this the snowball

15:47:49  chamber, analogous to the bubble 
chamber and the cloud chamber, 
15:47:52 liquid to solid

15:47:54  transition and the technology 
is scalable for modularity.
15:47:58  We consider it ideal for 
low mass dark matter
15:48:01  due to several advantages 
I will get into now.
15:48:08  Water has hydrogen and oxygen and 
if you have the ability to 
15:48:11 distinguish between them,

15:48:12  that will lead to good signal 
background discrimination.
15:48:14  We also show on the 
right sensitivity
15:48:17  to the spin independent

15:48:19  proton interactions.

15:48:22  In existing literature 
for supercooled water
15:48:25  and atmospheric science 
and chemistry
15:48:29  we find that the highest threshold 
reported, worst case,
15:48:32  is of water

15:48:33  tens of AV.

15:48:37  That should enable incredibly 
low mass dark matter sensitivity
15:48:41  and because we are dealing with 
individual protons with the hydrogen,
15:48:46  atoms, this unprecedented 
sensitivity
15:48:47 ,

15:48:53  it should be possible to have the 
neutrino floor not being a serious 
15:48:57 issue. 

15:48:57 The neutrino floor would be lower 
for the snowball chamber.
15:49:00  The other potential 
here is nuclear recall
15:49:04  directionality from a gas detector,

15:49:06  together

15:49:07  with the bulk target

15:49:09  you get from a liquid

15:49:11  detector. 

15:49:12 We are currently gathering

15:49:13  preliminary evidence of this

15:49:18  and the idea is this directionality 
comes from the intense hydrogen 
15:49:21 bonding that is present in water.

15:49:23  At the left you see our preliminary

15:49:28  evidence that water is sensitive to 
nuclear recoils, which has never been 
15:49:32 demonstrated before for super calling

15:49:33  cooling

15:49:35 .

15:49:38  In the future in order 
to precisely calibrate
15:49:41  the energy threshold we 
need to go to a place like
15:49:44  a tunnel to calibrate

15:49:45  but

15:49:49  in California it is indicative 
of at least one KV threshold
15:49:53  but large uncertainty.

15:49:55  We can look at the different 
images and how snowballs form
15:49:58  in order to be able to stink to

15:50:02  distinguish between backgrounds 
and non-dark background
15:50:06  and hybrid detectors like

15:50:07  water

15:50:11  (inaudible) detectors.

15:50:12  

15:50:13 >>

15:50:14  Thank you,

15:50:17  we will go on to our next speaker,

15:50:23  who will talk about

15:50:24  a deci Hz

15:50:29  gravitational wave lunar 
Observatory for cosmology.
15:50:31  

15:50:31 >>

15:50:34  Thank you to the organizers for the

15:50:36  invitation.

15:50:37  I am at Vanderbilt

15:50:39  University and a member of the

15:50:41  (inaudible) collaboration

15:50:42 .

15:50:47  I will be sharing this idea of a 
next-generation gravitational wave
15:50:50  experiment

15:50:53  that has great synergy with the 
scientific goals we are discussing 
15:50:56 at Snowmass, the possibility 
of a joint
15:50:58  OAE.

15:50:59  As mentioned by

15:51:02  the exciting talk this morning,

15:51:05  what is the next experiment

15:51:06  after

15:51:13  While we have the concept 
idea of extending
15:51:16  a lie go like

15:51:21  detector, there is a fundamental 
limitation on earth due to seismic 
15:51:24 noise,

15:51:25  we cannot go below 5 Hz with 
a conventional design.
15:51:28  With space missions we 
can go to Millie hertz,
15:51:31  but the one-

15:51:33 point one range, this is a sweet

15:51:35  frequency spot

15:51:38  for the most powerful sources 
in the universe and our
15:51:43  crucial for understanding 
primordial black holes and duck 
15:51:46 Matic candidates. 

15:51:47 This makes the case for

15:51:48  building a detector on the moon.

15:51:50  One of the major developments 
has been NASA's
15:51:56  Artemis program, the program 
released last month by NASA has 
15:51:59 accelerated the process of sounding

15:52:01  sending to astronauts by 2024

15:52:03  with payloads.

15:52:08  One of the strategies for Artemis 
is to observe the universe from
15:52:12  a unique

15:52:14  location in the natural vacuum on 
the surface of the moon, the wider
15:52:18  seismic activity and no 
environmental effects make
15:52:20  the moon

15:52:23  the natural location and 
using a conventional design
15:52:27  with existing projects, 
a detector on the moon
15:52:29  can achieve much if not

15:52:31  all of the sites we have explored

15:52:33 .

15:52:38  In the plot on the left, that is 
the design of what a gravitational 
15:52:42 wave detector on the Moon's 
surface would look like. 
15:52:44 The plot on the right is essentially 
the science case, the outermost 
15:52:48 circle

15:52:48  is microwave background and 
different shades are how far
15:52:51  in the universe the 
experiment can survey
15:52:55 . 

15:52:55 The conventional sources 
of gravitational waves
15:52:58  we already know exist 
can be served up to
15:53:01  70% of the observable volume,

15:53:04  this makes it a further reach 
than any other experiment
15:53:07 .

15:53:10  The frequency sensitivity is 
ideal for type I supernova
15:53:14 , we can temporarily constrain

15:53:18  the silence in directions five 
and 10, dark matter candidates
15:53:21  if they exist, we can

15:53:27  survey up to 30% of the entire 
universe and all this will 
15:53:31 complement the Largo detector 
on earth as well as telescopes
15:53:34  allowing multi-mesh and Joe

15:53:35  observations

15:53:37 .

15:53:40  Similar has been submitted to NASA

15:53:44  and if you are interested in 
this effort, please reach out.
15:53:47  Thank you. 

15:53:48 >>

15:53:48  Thank you.

15:53:49  The next speaker will be

15:53:52  talking about

15:53:56  testing as IDM

15:54:00  with realistic galaxy 
formation simulations.
15:54:02  

15:54:02 >>

15:54:06  Hello, everybody, thanks 
for the Emmett
15:54:08  invitation.

15:54:11  Today

15:54:13  I want to talk with you 
and share my excitement
15:54:17  about how we can use simulations 
of dwarf galaxies,
15:54:22  galaxy smaller than the Milky Way 
as a tool to constrain dark matter
15:54:26  with the

15:54:26  various telescopes

15:54:30  poised to launch in the next 10 
years we are entering an exciting
15:54:34  time where constraints on 
dark matter from all scales
15:54:37  will become available.

15:54:38  My work looks toward that future.

15:54:44  Now is the prime time to use 
cosmological galaxy information 
15:54:47 simulation

15:54:48  to predict which observables dose 
Observatory should be looking for
15:54:51  and how to interpret them.

15:54:53  That said the project I 
would like to highlight,
15:54:57  being conducted with my 
collaborators listed on the slide,
15:55:00  and I will draw your attention

15:55:02  to

15:55:07  1 of them, we will answer the 
following question – can dwarf galaxy
15:55:11  formation simulations 
predict an observable
15:55:13  that favors one dark matter model?

15:55:16  In astronomy CDM

15:55:17  is the most favored

15:55:19  paradigm but I will start 
with the assumption
15:55:23  that there is no good reason 
to favor cold dark matter
15:55:26  when you consider baryons.

15:55:28  Baryons as

15:55:31  an astronomer after many 
pesky galaxies that live in
15:55:33  dark matter halides,

15:55:35  halos,

15:55:38  in particular

15:55:41  I am looking at small dwarf galaxies

15:55:43  and modeling

15:55:44  those baryons.

15:55:47  What I'm showing you on this slide,

15:55:49  when you consider

15:55:52  different dark matter 
paradigms from CDM
15:55:53  to warm dark matter

15:55:59  and you include those pesky 
galaxies, there is no way to 
15:56:03 differentiate between those models.

15:56:04  All of them solve these 
challenges I have listed.
15:56:07  The models become virtual belief

15:56:10  virtually indistinguishable,

15:56:14  I aim to leverage state-of-the-art 
simulations that push the agitations
15:56:19  and you have what is 
computationally possible.
15:56:22  To look for the smoking gun that 
distinguishes in particular
15:56:25  as IBM from CDM

15:56:27  in the presence of

15:56:30  galaxies. 

15:56:31 In particular the observables 
we are looking for
15:56:33  are listed on the slide and 
these are directly testable
15:56:37  by the great observatories 
I mentioned previously.
15:56:42  And with this we hope to guide 
future observations and provide a 
15:56:46 theoretical background

15:56:46  for strong new constraints on 
dark matter soon to come from
15:56:49  low dwarf galaxy astrophysics.

15:56:51  Thank you.

15:56:53  

15:56:53 >>

15:56:55  Thanks so much.

15:57:01  Our next speaker will be telling us 
about superconducting qubit advantage 
15:57:04 for dark matter, squad.

15:57:06  

15:57:06 >>

15:57:09  I am a graduate

15:57:14  at the University of Chicago. 

15:57:16 Today I am going to talk about 
the search for low mass
15:57:20  dark matter candidates, these 
candidates include axion's and 
15:57:23 photons would potentially convert

15:57:26  into a quantile flight of the same 
energy as the dark matter mass
15:57:29  and we attempt

15:57:31  to capture the light in a microwave 
clarity and read it out.
15:57:36  To enable the dark matter such as 
in the mass or frequency range of
15:57:40  3-30 GHz, we present

15:57:42  to techniques that utilize 
superconducting
15:57:43  quantum

15:57:46  bit first, reduce 
the background count
15:57:48  by a factor of 1300

15:57:53  as compared to the current 
technology, and second, boost the 
15:57:55 signal rate by at least 
a factor of 10 using
15:57:58  stimulating

15:57:59  ...

15:58:02  To sense the electric field of the

15:58:04  dark matter

15:58:06 , and this is a quantum 
non-demolition
15:58:09  interaction, meaning the 
photon is not observed
15:58:11  during the measurement

15:58:12  and this allows us

15:58:14  to make multiple measurements 
of the same photon
15:58:17  to mitigate the effect of a readout

15:58:19  error

15:58:19  in any usual measurement.

15:58:21  In the top left figure we see that

15:58:25  with more measurements the 
availability of erroneous readout
15:58:28  is suppressed exponentially.

15:58:34  This results in a background rate 
1300 times smaller than the 
15:58:37 conventional readout strategies.

15:58:39  With this improved sensitivity we 
can take photon search and exclude
15:58:43  the

15:58:46  region of parameter space as shown 
on the bottom left whether Y 
15:58:50 accesses the hidden photon mixing 
angle and the X axis is the
15:58:53  dark matter. 

15:58:54 It's mass

15:58:56 . 

15:58:56 Only eight seconds 
of integration time,
15:58:58  enabled by the cubit

15:59:00 -based sensing technique 
we have developed.
15:59:04  Moving onto the signal part of 
we start the cavity in a non-
15:59:08 space, we can enhance the 
capability of the dark
15:59:11  cavity

15:59:11  matter in the cavity.

15:59:13  We harness the non-

15:59:14 linearity of the cubit

15:59:17  and use machine learning 
tools to generate
15:59:20  optimal control pulses 
while some Italian sleep
15:59:25  simultaneously including the

15:59:27  state in the cavity.

15:59:28  As you can see on the right,

15:59:31  eight

15:59:32  stages

15:59:35 , and with future dark 
matter surges we can
15:59:39  include and rates greater than 10.

15:59:44  We are starting to see this 
enhancement initializing the cavity 
15:59:47 close to 0

15:59:47  versus an equal to one state.

15:59:54  A cubit technology makes future 
dark matter surges possible by 
15:59:57 enhancing the dark matter signal 
and reducing the detected noise.
16:00:01  This work is an example of the type 
of cross disciplinary research we are 
16:00:06 fostering it Snowmass planning 
exercises and we look forward to 
16:00:09 working with everyone here. 

16:00:10 Thank you, and for more information,

16:00:12  it can be accessed by the 
QR code on the top right.
16:00:16  

16:00:16 >> Thank you.

16:00:21  Our next speaker will be talking 
about the initiative for dark matter 
16:00:25 in Europe and beyond. 

16:00:26 >>

16:00:27  Thank you for inviting me here.

16:00:30 mass function and 
multiple scattering, and 
16:00:32 they will point back 
to a common origin.
16:00:36 Here I'm talking about 
something slightly 
16:00:38 different, still about 
dark matter. 
16:00:40 It's initiative for dark 
matter that has started
16:00:48  but also means to go 
beyond because of 
16:00:51 course, dark matter 
has no boundaries. 
16:00:53 I think we all agree the 
best region defined dark 
16:00:57 matter is the one you 
can use more techniques 
16:01:00 and ideas, and 
explore it. 
16:01:02 And it's amazing how 
many different things 
16:01:04 we've seen also this 
community also the whole 
16:01:07 mass that there are so 
many possibilities here. 
16:01:10 With this in mind, the 
ones on the top right, 
16:01:13 coming from different 
fields, so
16:01:15  astrophysics, 
accelerator
16:01:16  for now,

16:01:16  met at the

16:01:18  conference that 
was set up
16:01:22  by the accelerator, 
nuclear and particle 
16:01:24 physics communities

16:01:25  in Europe. 

16:01:26 And

16:01:33  we realized we were ask 
each other questions 
16:01:36 will kind of assumptions 
are you using, how are 
16:01:40 you using this technique 
and what is your 
16:01:42 statistical and 
obviously how does your 
16:01:44 finding affect 
my findings ? 
16:01:46 we realized there was no 
common platform for this 
16:01:49 kind of discussion 
or resources. 
16:01:51 On issues again, we 
started developing it as 
16:01:54 initiative. 

16:01:54 This is how the 
initiative was formed.
16:01:57  We have 3

16:02:01  connected objectives, 
the first one is to 
16:02:03 collect dark matter 
resources in our own 
16:02:06 matter, one page 
contribution from the 
16:02:08 community that will have 
dark matter resources.
16:02:10  We also want 
to facilitate
16:02:13  that participate 
in cross community 
16:02:14 collaborations

16:02:15  and it means we are

16:02:19  preventing existing 
community efforts is 
16:02:20 that we want to try 
and facilitate
16:02:23  them talking 
to each other.
16:02:25  And then finally 
something we will hear
16:02:30  on the last day of the 
community planning team 
16:02:34 to help develop a story, 
a common dark matter 
16:02:37 story for different 
audiences. 
16:02:38 It's often one gets one 
side of the story but 
16:02:42 how can we reach, for 
example, the general 
16:02:44 public and give them the 
breath of perspective 
16:02:47 that dark matter

16:02:48  probes were off.

16:02:54  I DMU is still taking 
shape, it is something 
16:02:57 that has started rolling 
in a couple of months 
16:03:00 ago with the help of a 
task force that was put 
16:03:04 in place but,

16:03:05  the ground state is 
that we want to be a 
16:03:08 service to the community 
with an organization.
16:03:11  The first step would 
be reaching out to the 
16:03:14 communities

16:03:18  towards a kickoff 
meeting in Spring 2021. 
16:03:20 If you want to see how 
this develops, you can 
16:03:24 go to the link at the 
top left and then sign 
16:03:28 up and sign up 
about 300 people
16:03:30  that when this kickoff 
meeting happens. 
16:03:32 Thank you very much 
for your attention. 
16:03:35 >>Thank you for 
that talk.
16:03:37  That was the last 
talk in the session,
16:03:40  I'd like to thank 
all of the speakers
16:03:44  for what I think was 
an extraordinarily
16:03:47  interesting

16:03:48  session, I really think

16:03:49  some

16:03:55  of the comments by 
previous speakers of 
16:03:58 what the community 
should do, they should be
16:04:01  relaxed about it 
because I think these 
16:04:03 things

16:04:04  word demonstrate 
in the session. 
16:04:05 I want to remind you,

16:04:09  the audience you can 
engage with the speakers 
16:04:12 who I hope will 
stay around
16:04:15  and discuss things on 
Slack with them, before 
16:04:18 we close the session, 
we will organize
16:04:20  the committee probably 
has some announcements 
16:04:22 and I will turn it over 
to then to close the