of each of these topical groups. But I
will refer you to the Energy Frontier Wiki
, and the Wiki page
s and the topical groups and the indico
meeting agendas. And we have a calendar so you can be aware of all the meetings
that take place on a week-by-week basis. And also, if you want to
be in touch by list or Slack channels, there's
a communication link down there
.
And also, we have high-level and bi-directional
communication with other Frontiers
which is very important to make sure we are in good communication
with other
Frontiers and important for this workshop. You can see the
other Frontiers listed have one or two liaisons.
But what emerged very quickly
in our Snowmass
activity, the renewed interest for the Mathew
on Collider. We have the
forum. You can see the conveners, which belong
to the EF, AF and
theory frontier. And here we have a
Wiki page which is newly created.
Please join activities if you have interested in the
Muon Collider studies.
And the Snowmass thrives on the
participation of Early Career physicists. And in Snowmass
, it's really an ideal environment for young physicist
s to get involved
, promote their work and think ahead. Because
this is the future of their career. And there's an
Early Career representation in the Energy Frontier.
This rotates every 3 months. And at the
moment, Grace Cummings and
Matt LeBlanc are in the Early Career. If you are Early
Career stage, get in touch with Grace and Matt. Especially
if you need guidance on how to get involved
with Energy Frontier decease. Grace
and Matt will help build bridges
between new collaborators. Please get in touch
. There are points of entry for Early Career
people within Snowmass. And Snowmass is
really our time
to innovate and set new directions without barriers
and constraints set by our collaborations
. We want to
explore the Te
V energy scale and beyond, trying to understand what should be in the next collider
, lepton-lepton, hadron-hadron
, lepton-hadron, and to do that, we need
to set some questions. And focusing on open questions to evaluate
existing ideas. How those existing ideas can
help us as steppingstones
towards addressing new questions. For example
, if HL-LHC result
welcomes how they can be useful to shape studies for future
colliders. And also, this is important to identify
new ideas, as I mentioned. And ultimately, we want
to study the merit of a
our different collider options.
This is in the context not only with the Energy Frontier, but also
with other Frontiers. A
bit of history, had the kick
off meeting last May, and then the
workshop in July with the panel where we asked some
big picture questions to distinguished physicists
. And the Zoom recording is available as linked there
. And the
scenario is changing very fast.
Since last -- since the beginning of Snowmass, or in just
a year, we probably have
the evidence. So, a breaking of a paradigm
in the lepton flavor sector. So, it's becoming even
more urgent now to see how we can probe
directly, or indirectly in the Energy Frontier the
underlying flavor structure of the standard model. So, you see here
two teasers, two
plots from
lepton flavor LHCb and the data-theory
theory. And this is the subject of the talk in the
afternoon session.
But this lists another point which is very important
. These results
, these possible evidence of breaking of the standard model
paradigm are coming at the moment from other frontier
s with physicists or
cosmological frontiers.
The energy frontier, even though it seems slow at start
is necessary to win the race to discover
new fundamental loads of physics. And the reach
is very broad. We need to test many observables
to pin down the origin of new physics. And
there's a new complementar
ity between
electroweak precisions and fits. Please join us
to understand the fundamental laws of physics. We
can do that with many machines. The debate is between
hadron colliders, lepton colliders,
circular versus linear colliders. And all have their pro
s and cons and many ideas. Hadron
colliders, of course, allow us to reach high energy scale
s. Can allow many multiple detectors
. Are affected by poor signal-to
-background ratio
and by pdf
access. Leptons are clearer
, and the large ratio
allows polarized beams, but limited
in the mass reach. Circular allows
higher luminosity, several interaction points,
but affected by
syncroton radiation. Linear
are easier to upgrade
, but are affected by a beams
thlalung. This is
the debate we are in. And towards the goal of trying to report, we
see some benchmark parameters for the various
accelerator options which are the main ones, say. But
this does not exclude that we should
go beyond those parameters if people
have time to explore other parameter spaces. So
, you see here for various options
, the energy study, the polarization
of the beams,
the limited velocity. And moving towards more of the organization
al part, we are very happy that we received a lot of
interest from national and international community. We
received 376 letters of
intent last fall. Of
which 268 pertained to Energy Frontier
alone. And many others are together with other
Frontiers. And this was a major effort of solicitation
of LOIs from topical
group conveners. And we are very
happy that committee is very much engaged. However,
if you haven't submitted the LOI
, no worries. You're still in time. Just let us know your ideas and your plans.
And you're very much welcome to join our effort. Briefly on the time
line going forward. So, between January
and June this year, we had a slowdown of
activities. At the end of June, we restarted our
activities. Mid-
July we had the D PF meeting with the
Snowmass Town
hall. And now we have this Energy Frontier
restart workshop. On September 24th, Snowmass
day. I'll give more details.
March 15, 2022 is deadline for contributed paper
s. End of May is the deadline for submission of
preliminary topical group reports. End of June
is the decline for preliminary frontier reports. This will
lead to the mid-July community summer
study in Seattle. And eventually end of September
we will have the final reports that will lead to a publication
of Snowmass
book and guide documents end of
October. A bit more details
on the upcoming plans for the Energy Frontier. As I mentioned, it's
Snowmass Day for all
Frontiers on September 24th. Energy Frontier will give
a short presentation together with other Frontier
s. But we will also have a plenary session and
the speakers will be career people, most
likely postdocs. So, they
give their perspective to
topical activities and highlights of
Early Career status. And then moving forward in winter
, we'll have probably a few one-day virtual workshop
s split by topic. For example
, standard model, Higgs, B S
M, et cetera. To check the progress towards the March
deadline for contributed papers and discuss overlap with
other frontiers. In the spring, we will have the workshop where
you contributed papers
towards the deadline for topical group reports
and converge on summary plots and the main messages we're
going to get across. And between March and July
, we will have circulations of preliminary
reports both at topical
group level and Energy Frontier level and then public read
ings to collect the feedback from the whole community, from all of you
, and improve our report. And
with this, I'll complete just showing the agenda of the workshop
. Here in blue you
see the plenary sessions. We have one right now
. We have one in the afternoon after the break
where we discuss physics
anomalies and progress instrumentation. And tomorrow, two session
s, one on theory needs and progress in
accelerators. And one on emerge
ing future collider ideas and progress instrumentation. And then
on Friday, we'll have three hours where we go through the highlight
s of topical groups. Highlights
of sessions, but also plans moving
forward from topical conveners. In green
, our parallel sessions arrange
ed by topical groups. But also are arranged together
with other Frontiers. One example
is tomorrow afternoon, a session on dark
matter and the other
one on -- together
with computational
frontier carry. And here in purple, we have several
unstructured discussion sessions. And the idea is to have the
brainstorming and exchanging of ideas for presentation
s. The first one today will be with community engage
ment frontier. We'll
discuss funding issues in
the Energy Frontier which is more and more pressing and how to better reach
out to government. And we have three unstructured sessions. Tuesday,
Wednesday and Thursday with the
Accelerator Frontier
. And very importantly, the last one on Friday afternoon to discuss
plans towards the final reports. How to present
results, for example, plots and tables. So, the agenda
is really structured to facilitate
discussion. So, please part in the discussion and
hopefully we'll be align
ed. And I don't need to go much in the summary.
Just very brief. We have a very
ambitious plan in the Energy Frontier. And we can accomplish these plans only
if you help us to do so within the Energy Frontier
. But also across other Frontiers.
We have restarted activities, which took off already last year
. But restarted full steam now.
We have a lot of enthusiasm. We hope this enthuse
enthusiasm is renewed now. The
structure of the organization continues as last
year. So, please get involved and
hopefully you will enjoy the workshop this week.
Thank you. MEENAKSHI: Thank you, Alessandro.
So, you have any questions or comments, please raise your
hand and I will call upon you.
Okay. I don't see any hands raise
ed in Zoom. So, the
next -- thank you, Alessandro
, very nice -- ALESSANDRO: Thank you. MEENAKSHI:
Summary of the schedule in advance. Next I'm going
to invite Laura Reina to give the
highlights from the Energy Frontier work which has
happened mostly during the
slowdown and pause. So, please begin
, Laura, any
time.
Laura, we don't hear you. If you are speak
ing.
LAURA: Sorry. I was muted. Can you see my screen?
MEENAKSHI: Yes, we see your screen.
Thank you. LAURA: Thank you. Moving on to the highlights from the Energy Frontier.
These will be structured as highlights from the
topical groups that after a brief
introduction that have been the soul and the backbone of the
Energy Frontier and accomplished an enormous amount of
work since they started being active
in spring 2020, I will
say. So, by the fall community meeting that we had in
October 2020, they had already
outlined a very rich program of physics
organized around some key questions that
has been our modus operandi
from the very beginning that I will use as introduction
to their highlights in this very short presentation. During the pause,
the topical groups have been there. They have not
been as active as they used to be
during the first part of Snowmass. But they have served
as a sort of reference and minimal
framework to reach all participants
in the community. Could refer to, people
could start to contribute or continue to contribute.
They're now back eager to present what their physics
plan is based on the work done in the
past and the contributions they have received so far and
help recruit new people to help with the work and to bring in
new ideas. So, as you have heard from Alessandro
, we have organized our work around the three main area
s of standard model,
electroweak, strong interactions and beyond
the standard model. And from the very beginning
we liked
the proposal as the goal to bring out the fundamental questions so which we would
like to find answers. And both in terms of
theoretical investigation and experimental investigations.
So, in the
electroweak interaction area, of course, and beyond the standard model
physics are the key question that came out was
really around the origin
of the electroweak scale, finding the origin of the electroweak
scale. And these materialized in many studies from
the precision of the Higgs measurements to
constrain triviality physics. That
then gave direct input to
a group of electroweak fits explore
exploring the measure of the Higgs potential, the
couplings, the connection
between Higgs and flavor. As well as the impact and implications of
naturalness. This is focus points
that's then two-factored many focus points for
the BSM and topical group
s. BSM has evolved with
two main tracks. One more model-independent and
one more model-specific. And
both complementary to each other. Both are very rich
and interconnected in ideas. So
, models, as you know, they play
a special role to link high-level
theoretical ideas to consistent
phenomena in a consistent way. But the question is which models should we consider and how
to compare model and model parameter space
s in a consistent way. And are we Lee
leaving something out? Are there
alternatives that we need to consider? That's the point and
the place with the more model-independent and agnostic
way of addressing kicks in and becomes fundamental. Becomes
really important. In particular, in avoiding gaps
in coverage and explore
exploring ideas or characteristics that sometimes can be
hidden in the specificity of a given model
. Now, if we wanted
to talk about future colliders both
in the short-term and in the long-term
and we see a big portion is hadron colliders
, the study of interactions in different regimes becomes really
important. This is the focus of the groups
where the key question around which of the work
in the QCD group has been knew collie wait
nucleated has been at the fundamental level and the
applicable or practical level. They have gone over a broad range of question
s that we can summarize into
addressing
perturbative and noneffects. Precision
is definitely needed if we want this machine to
use it to the fullest potential of this machine
at the level. Which is what they can reach. This has been
been, indeed, the focus of the QC
D topical groups at -- that will be then reflect
ed in the highlights that I will give short
ly. So, finding answers to these very general
questions that we were able to
outline as the foundation of our physics program within the
Energy Frontier has brought a very interesting
discussion. More specific discussion. Because answer
s to these very general questions bring specific question
s. And they were both on the experimental side and
on the thee
theoretical side, of course. You want to
ask yourself, given this plan, which collider
and properties are better tailored to what we want to achieve?
Can we identify technologies that
will represent definitely a step forward? On the theoretical
side, the basic question, the most important question
is what do we need from
theory? Where is theory going to have the most impact? And how can
we strike the right balance of total
freedom of investigation and specific contribution to
specific problems that can bring
out the potential of this machine even more? Both of these
areas will be the topic of
several discussions and several parallel sessions that
we have set in place for these
restart workshops and we definitely need the contribution of everybody
interested in contributing to push them
forward and to really learn from these discussions at the next level. So,
coming to the highlights of the topical group
s. They are organized into three main areas.
So,
electroweak -- and BSM. Starting from the highlights
of the electroweak working groups, they have sort of a Venn Diagram
approach to illustrate both the specificity of each of
them and the overlaps of them. We have four. Four of them.
EF1, 2, 3 and 4. The first two
are about Higgs physics within and beyond the standard
model. So, coupling properties,
extended Higgs sectors and their interplay
. We have a topical group
on heavy flavors. So, top and bottom and charm
. And EF4 where all
electroweak physics comes
together in formulating strategies for
observable Higgs. So, to go to the highlights that they would
like to present to you, have to go briefly over
them. There are many more details in
these slides that you are welcome to read.
But we wanted to have these highlights thrown at you just that
you somehow show as a
preview of what is going to be discussed into the parallel sessions
and the instructor discussions that are the core of these work
shops, as a matter of fact. So, EF01
is standard model Higgs. Higgs boson property
ies and couplings. They had a series of fantastic
discussions during the preparation and the restart of these --
of our activities. And they're focused on the
topics that really are missing. So, they're top
ics for which we really need a lot of investigation.
So, light fermion
Yuka with a couples. The progress on the
inverse problem. So, how to
investigate the effect of new Higgs as a portal
of new physics will give us information
on the specific standard model, or through interaction
with the Higgs participates. And we can go from a
more general description in the peer research to the
more specific discussion in terms of models. So, utiliz
ing both these directions and informational, parameter
spaces from your team investigations is extremely important.
And, of course, the Holy Grail of
them all which is the measurement
of the Higgs coupling is one of the focuses. EF02
is beyond standard model Higgs. A lot of interaction with
EF01, a lot of the themes are the same.
Investigating Higgs and flavor, investigating
the Higgs and beyond. The effect
of global -- in limiting the possible
scale of the standard model and how does that happen on different machines has been
part of the discussion pre-slowdown.
And has been maintained as background to new ideas and
investigations that have been promoted individually
or together with the EF01 during the pause and are now
restarting full speed for the
future series of meetings
that they will advertise during their parallel session
s. So, that they're organized together with
EF01, EF03
and EF04. Coming to EF03
, top and heavy flavor physics. Of course, top physics
is an integral part, has a lot of
relevance for Higgs studies as well
. It's everywhere. This group is intimately related to the study
of the other electroweak
groups as well as to the study of Q
CD, EF05 in particular.
So, prospects for precision measure
ments is one of their highlights. They have developed a
rich program. Joined studies to
determine fundamental parameter by the top mass.
Or effective couplings saying which of the top is involved
as which we will hear in the next session, which is a parallel
session dedicated
to global feeds and EFTs. And
prospects for measuring other heavy flavor
s, bottom and
charm, fundamental to both investigation
s physics
and reaching future machines.
EF04 is where everything comes together. They have been extreme
ly active in putting this very difficult problem.
The extension of the
standard global model to include interactions. They have now a task force in place. A new effort
that has been spearheaded by six members want
ing to engage more and more people
in these complicated studies that
build on what the European strategy has brought
us, but can happen much more to that. And bring
us to something that is now under the attention of the
global community. For instance, in conjunction
with the similar efforts through the
L HC-EFT working groups and
more. Moving on to highlights from the QC
D topical groups. 5, 6 and 7
. They explore aspects
of both
perturbative in different regimes. And there's the highlights
, precision QCD.
Both of the aspects of QCD
, even the physics of near future
and far future hadron colliders is at the percent level. They have been
engaged in all these fronts from
precision determination of stronger
programmers, the strong coupling constant
to the Monte Carlo, to
quantifying and taking into
account non-perturbative effect
s. And as well as functions together with E
F06. Or if you want QC
D strong interaction like jets in different
regimes and in conjunction with EF07. As we were say
ing, hadron
-- parton distribution functions are
one of the parts of EF06. They are specifically
looking at QCD
with hadronic structure and QCD. They have added
two more highlights which is both the
analysis and study of QCD in high-density regimes and
that is becoming increasingly
relevant with the HL-LH
C, the FCC-h
hh and the L
HeC. And one they have with another frontier
, the nonperturbtive models of
hadron and hadron
speckoscopy. They are working with other groups
as well as other frontiers that you are invited if you wanted to join
or participate or be updated on their physics Langerhans. And
finally, among the QCD E
F07, EF07, heavy ions
is a topical group
that is an interfacer between
particle and nuclear physics. And because of that, living
through the very exciting times of the EIC. Because of
that, has had to have a sort of
slightly different schedule with respect to the other groups. So, it
doesn't -- it didn't
really lead through the pause that we have had for the
past 6 months in the Snowmass community
exercise because of its own time frame
work. They also participate
ed to other planning processes. They have push
ed forward during this time. And they have contributed
really important studies at the
interface with particle physics colliders. So
, basically, the complementary of heavy
-ion studies with heavy flavor studies,
jet studies, electrical
physics and even studies as
planned for future colliders in particle physics
. They have dedicated parallel sessions and joint sessions with a
topical group at this meeting.
And everybody interested in knowing about their studies and
joining their studies is invited. Moving on to BSM
topical groups. As I outlined at the begin
ning, the approach has been both to contribute
to studies in the
QCD section, but also to develop
two main leads. One
oriented toward model-specific explorations and the
other towards more general explorations. And as
we all know, in this context, all models
models, all general explorations are particular -- have a
particular focus on one question. Which is the question of dark matter
, about dark matter, the
origin and the nature of dark matter. And that's the reason for the existence of --
within the Energy Frontier of a specific group on dark matter
colliders that has had a lot of overlaps with about other
EF08 and EF09 as well as
with other frontiers, in particular the
cosmic frontier. And by now has come
up with really strong and important highlights
that will be briefly overviewed here. So, specific exploration
s. Of course, it involves
going through several very promising and
at the same time quite representative models. And
finding reasons to either explore them
in conjunction or single them
out for specific physics reasons. They have
had a huge
activity during the pre-pause time.
And kept that going during the pause at a much slower pace. But enough
to keep connection and cohesiveness
among the people working at that. Before the pause, they
had to review with dedicated meet
ings and parallel activities all the different scenarios that they want
ed to explore. And they're now coming out after the
pause with specific recommendations they have planned
for their Monte Carlo needs. They will discuss in the months
to come finalizing their plots and tables
and scenarios so that they wanted to propose
for future colliders investigations. So
, at the same time their activity is complement
ed and in conjunctions with the activity of EF
09 which is a more generic exploration
of B SM physics
with future colliders in mind and with avoiding gaps in coverage
, they have take an different approach of optimize
ing searches at future colliders in classes of
new particles that they wanted
to explore and not miss. That
could be new heavy bosons, new fermion
s. As well as focusing on searches or particles that we haven't
thought of so far with characterric
s or properties that we haven't considered. So
, exotic searches or searches
as a prototype
example. And they will inform specific scenarios
both at the theoretical and experimental
level. So, in this context
, we -- the work of EF
10 has tried to talk to both the
EF topical groups, 8 and 9 and
beyond EF at the
cosmic frontier. They have been very, very active before the pause that they have
decided to use the slowdown period to connect to
other activities in this very
rich and very vital scenario that is the scenario
of dark matter searches and dark matter
-- dark matter physics community. So, at
this meeting that we present results from
activities on Dark Showers in
conjunction with EF09. Or studies
of W
IMPs and
and colliders.
And they have been represented by younger members of the community
which is very welcome. In particular to engage them more
and more in this Snowmass effort. And they are recruiting
more people interested in the topic. So, we invite you to
participate to their sessions. So, one last
thing that we would like to advertise as one of the
activities, not of a specific topical group,
but of a forum that has been forming within the
Energy Frontier during, as a matter of fact,
the pause in particular is the Muon
Collider forum. This was started together with other initiative
s around the world that are summarized in our
backup slide. And has been started,
as I was saying, really when the pause was starting. So
, in January 2021. So, they haven't really
paused. But they had four meetings during this time
and an upcoming one on September 21
st to which we are all invited. They will have dedicated
sessions during this workshop as well as
unstructured discussions in which they will take time to
both present the physics highlights. So, how
this machine responds to the main
key question presented in the introduction to this
talk as well as, of course, as a new technology
highlights on accelerators and detectors.
So, please join the discussion. So, I would
like to conclude by reminding that what has been
the main spirit of the Energy Frontier? And
what we have been wanting to
stress and around which we have
informed these restart workshops is the
synergy between topical group
and other frontier. And in the plot, you can see the
overlap between electroweak, BSM, and
QCD and other parts of the group is the other
Snowmass frontier. From the computation
al to the ray processes,
cosmic frontier, chain of frontier, and last but not last
, the neutrino frontier. And if we have a
look back at our program, you cansee that
most of the spirit of this workshop
has been cross-breeding and talking to
each other So, starting from the plenary talks. Some
of which have been dedicated to speakers that are
mainly active in other frontiers
, the instrumentation frontier, the
accelerator frontier. We have a plenary discussion with the
theory frontier. And the joint sessions among topical
groups and informed instructor discussion with other frontier
. The accelerator frontier, the
community engagement frontier and the computational frontier
. One last instructor discussion section we would
like to bring strongly your attention to is the last one.
The one we're gonna have on Friday where we all
come together to really plan
and discuss how we want to present the results
. This is a discussion of themes. And how we want the themes to make
it to plots and tables. So, please participate
to these joint discussion and
sessions and bring your contribution now and in the month
s to come to the success of the
physics program of the Energy Frontier.
Thank you. MEENAKSHI: Thank you, Laura, for
a very extensive quick summary
of all the work which has been going on during the
slowdown. Any questions
or comments for Laura? Please
raise your hand.
Okay. So, there is one raise
ed hand. Please go ahead
. >> Yes, hello. Hi. So
, I'm -- I'm wondering whether anybody in this
forum is -- is
considering the need of
analysis preservation and reuse?
Specifically but not only for the Higgs sites. It's not so
obvious to bring everything together in a coherent picture
and actually arrive at
the global field where
all the experimental data is already bringing the
results together is not so easy. And when looking at
the more distant future, incorporating maybe also
-- it's also other experiment
s, other colliders. With the
way the results of the research is really
, really important.
LAURA: Yeah. >> In the long-term, is anybody really
considering this? LAURA: Yeah. This is a big problem. And this is an important one
. And definitely will need to be discussed. So
, from the point of view of of course not lose
ing memory of what has been done, a lot of the working groups, all
of them, I would say, started their work up from review
ing what was going on with the European strategy. And building on that
that. But I think that your question goes even
farther than that. Is really not losing
track of analysis and work that has been done within
also the experimental community. And I think that we're
all aware of that and
if it would be good also, and I think during this meeting
we have a discussion planned to
ensure that -- to try
to address this problem. But more specific
discussions are welcomed
and requested, definitely Snowmass, as you say, is a place
where this discussion should
happen. >> Thanks. I think Alessandro
wants to comment as
well. ALESSANDRO: Yes, thank you. I just wanted to point out that we have a
session on Tuesday. The session with the computational
frontier which is shown there in green on
Tuesday afternoon, 1 to 2:30. And
I think that could actually be a good place to bring this up.
Because although it's not computational,
but data preservation is part of the data storage. And the
formatting for the future. So, I think it's a
very important topic. And maybe that's a good
place to bring this up. So, I'll keep that in mind
and hopefully you can join the discussion too. >> Yes
, I'm planning to -- we have already been discussing a
white paper for Snowmass. Particularly on these issues. But
it's very little discussed in the physics
Corp. And there has to be more communication in
my mind. So, this
may be useful. ALESSANDRO: Let's put that in the list of
things you want to discuss in that session.
Thank you. LAURA: Thank you. MEENAKSHI: Thank you. And I think we
will move on to the
-- thank you, Laura. And move on to the next speaker which is John Stupak
. And he's going to give us a summary of the
progress made from Monte Carlo productions and future plan
s and effort. Thank you. Please go ahead
, John. Yep. We see your
slides. JOHN: Okay. Thank you,
Meenakshi. So, I'm going to try to keep this quick and to the point
and give you the -- the status
on production of background Monte Carlo samples on behalf of
several people whose names you'll see in a
minute. So, Alessandro
kind of went over this background already. So, I won't
go into any detail. I'll just say we have
a Wiki here where you can go to find any information
on -- related to the stuff I'm gonna talk about today. It's
not super well-populated at the moment. But we're
gonna add more information to it.
And here's -- so, the back story is
that the Monte Carlo Production Task Force came up with a
plan for production of Monte Carlo sample
s. That plan is being carried bout
I the Monte Carlo production
team who consists of the folks
here. For reasons, we have lost
about half of these folks to
attrition. We had to pause, things come
up and people have to refocus their efforts.
There's really just two people who active
ly have their hands on code and developing things. And we
really need additional purpose power to develop
this workflow and validate the samples. I have a link here. If
you have any spare time, please click this link. And, of course, I
do value everyone's contributions who have been contribute
ing so far. Whether they're actively contributing with
their hands on code, or providing technical
expertise and attending meetings. Everyone's efforts
are very welcome. These are the colliders and energies
we plan to support as a -- for the community
. We have, you know, the circular machines, the linear machine
s, we've got the Mathew
Muon Collider there. EH,
we want to support everything that the community has an
interest in. This is what the current plan is. We
plan to produce these hh samples that
I had listed on that table proactively. Mean
ing you don't necessarily have to request them, we're going to
go ahead and produce them no matter what because
we're pretty confident they're needed. The e
e, eh
and mu-
mu-mu samples will only be requested on demand. So far
we have no requests for these samples. So, if no one asked
for it, it's not gonna get produc
ed. If you need those samples, that's fine, let us
know at the link here. And we would be happy to help you.
But otherwise, we're not gonna do it
if no one needs it. The OSG has been
very generous and is helping us out a lot with
this production. They offered -- they set up this
really nice machine, a dead
dedicated machine, Snow connect. If you have
heard of OSG connects, it's
relatively familiar to you. It's very similar to those. It's
an interactive login node, batch submission
and a lot of storage. So, this is a really nice machine. We're gonna use
it to produce the Monte Carlo for everyone to use
. But these resources can also be used
by anyone for any Snowmass use case. The OSG
would be very happy to see us using this and
burning CPU cycles that they can report to their funding agencies.
So, they would be very happy for us to use this.
It's better than my local tier 3. I love using this
machine. I use it every chance I get. If you don't have an
account yet, you can request one here. There's
documentation here. And we are using
Slack for user support and discussion. So
, please, feel free to use these resources
. A few words on what we're not going to do.
We are not going to be producing any signal
Monte Carlo. Signal Monte Carlo's not really -- is specialized and
it doesn't require a ton of resources. So, we think
people can generally handle single Monte Carlo production
do signal production Monte Carlo on their own. But you can use the resources to generate
your signal Monte Carlo if you need to. And we are not
going to produce any full sim samples. The
reason for in is all of the future
collider groups are allowing people to do studies
with their existing full sim samples. They
make minor and reasonable impositions. Like if you are
going to use their Monte Carlo, attend a meeting of theirs
every now and then and present your work so they get
to scrutinize it to some degree. If you want to do
some study and you require
the accuracy of full sim, you should be talking to the
future collider study groups. Unless -- if
they don't have something you need, you can talk to us and
we can see about getting it produced. But because using
full sim Monte Carlo from a foreign experiment is
tricky, there's a bit of a learning curve
, we did organize a series of Monte Carlo tutorials for
each of these, you know, future colliders that you see
here. ILC actually did a few
tutorials. One was sort of a general
wizard tutorial and they did an analysis
walk through. But the other experiments have also done a
nice tutorial. If you want to use any of this full sim
and you are confused how to get started, these would be a good
resource. So, what are we gonna do
? We're gonna produce a whole bunch of Monte Carlo
with Delphes fast simulation
. It's widely-used, well known, fast
and accurate enough for most Snowmass studies.
And there are detectors cards that have been blessed by all
of these future collider study groups already. So, we can
just go ahead and use those blessed cards and
generate the Monte Carlo. That's what the plan is
. Now since we're focused initially
on hadron colliders, because as I said, that's where
we know we're definitely going to end up producing some Monte Carlo
. So, I'll go into some detail on the strategy there
. You know, when you're talking about a hundred
TeV collider, the cross sections for even what
we consider rare processes like
triBoson production, these become large. And we have
to worry about a whole wide range of backgrounds. And we're try
ing to anticipate all the different kinds of studies that people might want to do
. So, we have to be really
inclusive and try to generate as many standard model
backgrounds as possible. And that requires some organization in order to keep thing
s sensible and limit the number of samples we're producing. So
, we're following a similar strategy that we follow
ed in 2013. And here is sort of the way we've
categorized different standard
model processes. We've grouped them into groups of
processes that have similar cross sections so we
can just generate one
sample and we'll get a significant number of events for all of the
processes we've lumped together. The B here basic
ally means a beauson, photon
, WZ, and sometimes Higgs. We have Boson
, try-Boson,
di-Boson. And LL is a lepton
, that's off shell dileptons
. LLB is
offshelf leptons plus a beauson. Single top
, single top plus a beau
Boson.
We veto the on-
shell propagators to geep all of the processes
orthogonal to one another. In 2013, we took each of these
samples that's listed here and sliced it in HT and had
, you know, so four to six slices
in HT for each of these samples. Which
obviously blew up the total number of samples and
the, you know, the organization became
a little bit trickier. So, we would like to
not have to do that. And so, the plan this time instead of slice
ing an HT, we want to use something called
a bias function that can bias the generation of the
matrix at events at matrix element level
to large HT. And we think we can solve the problem that way and
just have one sample per process group here
. And in 2013 what we
did was we treated all the on-shells residences
at stable at matrix element level and
then decayed them democratically using bridge
. By "Democratly," basic
ally equal branching ratio
to hadrons, and enhance
our statistics and final states with lots of leptons. Bridge is kind
of an old product although this point and we want to move
to something more modern. We want to use madspan
to replace that functionality. I'm talking about bias
ing things in terms of lepton multiplicity
and in terms of HT. So
the way we did previously and the way we will again recover
our physical distributions is via the use of an event wait. So,
there will be one event wait calculated in the file
. You will have to apply that event wait
and you will recover physical distributions.
So, again, here's the proposed workflow
that we wanted to use. We wanted to use Mad
Graph where we would generate up
to 4 partons at the level
. Pp goes to tt, or tt
+ j, or tt + two jets. We would
then use MadSpin to perform a
series of 1 to N decays of these
heavy resonances. That takes our tt + jj final state
all the way to an 8 parton final state. By
using madSpin we are able to generate
an 8 parton final state in the amount of time it would take to
generate basically a 4 parton final state.
So, saves a lot of CPU. And use Pyth
ia for showering and hadronnization, and
Delph ess for detector
simulation. This is the proposed workflow.
Now let me talk about the statuses Things. I
wanted to do had
Ht bias. This is from 2013 where we had a
sample in four different Ht slices
that when combined together gives a smoothly falling
Ht distribution. This time, rather than slicing, we want
to bias the generation in Ht. What I did is
I generated a
diboson in black with no bias. And then in
red and blue, I diced
the sample to large Ht or large Ht squared in
the case of blue. We have enhanced our statistics
at high Wpt in the red and
blue. But when I apply the event wait that
Madgraph calculates,
they turn into the green and yellow distribution. Which if
I zoom in, does match the unbiased
distribution. But we have far smaller error bars on
the Monte Carlo and green than the yellow and
black. We have decreased the
statistical uncertainty. And here's
the Wa distribution as
well. It gets corrected with
this event weight. This is a bit of a work in progress. It seem
s to be working here. But we need more validation of
this before we feel it's really ready to deploy wide scale
. On MadSpin. If you're
unfamiliar with MadSpin, it does a
series of one to
two decays and have the
finite width effects. But the devil is in the
details. Madspin can only do one to two decay
s. We cannot go Higgs to
four fermions in the mode. What
the authors did was developed another
mode specifically for decaying scalers like the
Higgs where it allows you to decay to 4 fermion
s. But unfortunately, you can't
combine these different modes of operation in a single job.
We have to choose if we wanted to decay tops, W
s and Zs with their spin-correlations
, or decay to 4 fermions. But
we can't do both in a single sample
. The answer is fairly obvious, generate
a separate Higgs StratoQLly from a top, a W
or a Z and then use the appropriate mode in
both cases. The only problem is what to do with sample
s like VH or ttH. We have both
particles that we want to decay with spin correlations,
and the Higgs which we want to decay to 4 fermion
s. There's another wrinkle
because we also want to use MadSpin
to enhance our rare decays. I'm using the
term "rare" here very
loosely to even
include W and Z decays to leptons. So, I'm working with
Olivier, one of the madgraph authors to
develop this capability in madspin.
His initial idea only worked for
WZ and
top decase. On the left, it's
raw Monte Carlo events. And this red sample is what you get
, you know, with -- this is t
tbar, so, this is, you know, the raw
lepton multiplicity distribution in red. What
I did artificially in green is artificial
artificially biased to high lepton multiplicity, right?
We see this green distribution shifting to the right.
But then when you apply the Monte Carlo event
wait
that madspin calculated,
go from these to these distributions. And the green
distribution perfectly matches the nominal lepton
multiplicity distribution. So, we had figured
something out that worked for W/Z
s and top decays, but not for
Higgs. Olivier
has something to work out, but August vacations got in the
way of things and I need to come back to that. But it's something we're
working on.
MEENAKSHI: John, could you wrap up
. JOHN: Sorry, yeah. So, here's, again, the proposed workflow
. It was madgraph with an H
t bias, followed by mad
spin with the bias, followed by Pyth
Pythia and Delphes.
To get things for today, we had a
simpler workflow, replaced this
blob here with Pythia. We're generate
ing up to four partons with
madgraph, decaying them with Pythia so we have no
spin correlations and doing detector simulation
with Delphes. This is not validated yet
. We just put the finishing touches on some grid pack
s on Friday and we have let the grid churn over the weekend
to produce some Monte Carlo for today. So, these samples
are imperfect. We're never gonna be able to populate
the tails of the distributions with this simple strategy.
So, we need to do better. But we need more person power to help
us with that. So, please, if you're interested in getting involved with this
, please, you know, click the link here and volunteer. Or
volunteer your student or postdoc.
So, Andrew
has been submitting and monitoring jobs over the weekend using this
Snowmass Monte Carlo
framework that he developed.
We're running at 13 and 100 T
eV with the F CC
Delphes card for both.
It will be available here soon. It's in a temporary location and we have to
transfer it over to its permanent home. And we're working on easy
ier web access for that. But we have some event
s here for these processes. All of the ones I mentioned
except for the, you know, the
gluon fusion Higgs sample which will be available soon
. But we have something like 8 terabytes of data
that we produced this weekend and people can take a look at.
Again, it's not validated. So
, we're crowd sourcing this and need help validating this. If you
want to help validate and help develop new
Monte Carlo techniques, whatever. Please click this link
and let us know. And then here's my summary
. The two most important things are that we need volunteers. And
if you need more info on anything I said, here is the
link to the Wiki which
should have the info. MEENAKSHI: Thank you, John, for
a very nice overview and the progress on the Monte Carlo
generations. Thank you very much to you and your team. At this point
, I would like to see if anyone has any questions or comments?
I see Michael,
please go ahead, Michael. >>
Yes. So, John didn't say anything
about the E plus, E minus resources.
But I would just like to say that the
ILC team even last fall set up a
web page with a great deal of simulation data at
all of the relevant energies, 250, 500
, 350 and 1
TeV together with tutorials and some
documentation. And I think there are several groups that are using
this now who are new to the plus and minus studies.
But I encourage other people who would like to do studies
in E plus and E minus to visit this page
. All the standard model backgrounds are there so you don't
have to do that. It's -- this page is at the
level of Delphis
. But let me just say, linear, circular
, all the E plus and E minus machine
s are basically looking at the same physics. There it is.
We really encourage you to
use all the simulation data that is here. A lot of interesting
studies can be done. If you have questions, please feel free
to write to me by email and I can get you connected to the right people
. If you want to do full simulation, I can also get you connected
to the people that can help you with that. So, it's
there. Please use it. And hopefully we can do some
something studies
. JOHN: Thank you for that reminder, yes. The ILC was really fantastic in
putting together great documentation. So, it should be easy for
people to jump in. >> Yeah, I'll put the URL
in the chat.
MEENAKSHI: Thank you, John and Michael. So, next
hand that's raised is Marc-Andre
. Please go ahead. >> Hello
, this is Marc-
Andrey speaking. I have a question about the Monte Carlo samples
. Is there a way to access the card files
, because if you want people to generate the
single Monte Carlo samples, they need to be able to access the background settings
so they can make sure things are generated consistently from the
PDFs used to all the other nitty gritty details
. I think it would be very good to have access to the card files
. And at least glancing through the
Wiki page, I was unable to find
them. JOHN: Yeah, the page I need to update with the
latest stuff going on. We have been focused on getting it
produced first. But if all that nitty gritty info
is available at the link here at the bottom of this slide which shows
exactly how we're installing things. And then there's, you know, the
one -- the cards. The one non-default
card we're using right now is in that directory
. >> Thank you. JOHN: If anything is unclear, though
, please let me know and I'll make sure to add that. >>
Thanks. MEENAKSHI: Thank you, John
and Marc-Andre. So, next
is Jeff. >> Yeah. Hi, thanks, John, for the talk
and all the hard work from everybody
in the task force. It's great to see. My question is basically along the
lines of Marc-Andres about try
ing to coordinate different settings between people who are going to be
generating signal Monte Carlo and what the -- how the background
samples would be produced. So, maybe one thing
that I guess hasn't been talked about is whether a pile-
up is included in these background
samples and how people generating
signal might include those. And maybe to ask if it's possible that
we could avoid sort of mismatch
es in
Delphis card
parameter settings by sending the Monte Carlo
task force a grid pack or something like that and they
handle the Delphis
part of the workflow. JOHN: That's something we've talked
a little bit about inside the task force. We want to make it easy to
generate signal. But so far we have focused on getting the
background stuff generated.
We have to the quite figured out if we're going to support if people give
us a grid pack, we run it. I don't see how
we can't do that. Once you have the grid pack
, it's pretty easy to turn the crank and let it run. But we
will make sure everyone has the info they need
to produce equivalent
signal Monte Carlo. On the pile-up question, we're using
the official FCC-hh card. The
approach they took was they do not
explicitly overlay pile
up events on the hard scatter events
. They have parameterized
the performance of the detectiver in the presence of pile-up and fed
that into the card. We're implicit I taking
into accountthe degradation
of performance. What people have to do is use the same
blessed FCC-hh card
with Delph es and they
should be fine. >> Great. Yeah. That help
s clarify things for me. MEENAKSHI: Thank you. I think
the last question would be from Sergo
. >> Thanks, Meenakshi. I wanted
to comment in line what's been previously said. But in
regards to the Muon collider. John has
said there haven't been a lot of requests. I know a fair
amount of people are actually generating private samples
both in full sim
and -- but we
do have links to the hands-on tutorial. We have
material on how to generate those samples. And also, I encourage
people who are new and interested
in engaging in simulation to contact
us. Laura had our contact information on the slides
slides, I believe. Or a pointer to a
Wiki where you can find all the information. So, reach out to us and
we'll be able to get you going with simulation
or, you know, help you to simulate samples you
need. JOHN: Yeah. Just to clarify. When I say we haven't gotten
any requests, I mean, the Monte Carlo production team
. That's completely separate from, you know, what the Mu
on Collider folks might be hearing
from people interested in that,
or ILC folks are hearing from folks interested in
the ILC. I drew a hard line on ee
and eh samples. Because the Muo
n Collider is in a unique position and playing
a catchup to the other ideas, I didn't draw a hard
line on Muon. If there's something with the
Muon
colliders that come
up in the future and we can help, let us know. MEENAKSHI: Thank you very much
, John, for this detailed presentation. And with
this, I'm gonna close the first plenary
and we thank all the speakers for
today's talk. Alessandro, Laura and John
. And for a nice summary of the work going on
in the last few months during the
slowdown or pause of the Snowmass
. And the next session is going
to be on discussion on global EF
T fits. For that session, I'm gonna hand it
over to
Alberto and others to convene it. We are running a bit late