Postering for Fun and Very Little Profit
Guidelines for Poster
Presentations
Rick Pam
Undergrad Summer Research Program
Depts. Of Physics, Applied Physics,SLAC
Stanford University
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Why?
• Communicating results is essential. If you
don’t communicate, they didn’t happen.
• Papers, talks, posters, public lectures,
lawsuits, romantic poetry, ransom notes
• Poster ≠ published paper – NOT as much
detail.
• Poster allows real time interaction between
author and readers
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Design Considerations
• One main take-home message
• Title: short, reflect your message, get viewer’s
attention
• Consider your audience
• Design poster for stand-alone AND stand-beside
• Design in one large PowerPoint (or equiv) slide
• Design to generate real-time discussion--not too
much detail. Want viewer to engage with you as
you stand there.
• If more detail needed, have hard copies of a more
complete paper available to hand out.
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Sub-picometer resolution from a
low-cost wavelength meter
Adam Banfield, Sarah Anderson and Chad Hoyt
Bethel University, St. Paul, MN
Wavemeter
•Michelson interferometer
•One arm comprises retroreflecting
mirror on inexpensive air track cart
• ~3 pm accuracy determined by I2
spectroscopic measurement
Motivation
•Accurate, precise measurement
of laser diode wavelength
•Laser diodes will be used for
laser cooling and trapping
Magneto-Optical Trap
depiction: the ball in the
center is a million atoms
moving at only centimeters
per second
How it works: Because the
beams travel identical
pathlengths
the wavelengths are
proportional through the
ratio of counted fringes,
NR/NU:
reference
laser
retroreflector
Count
r
e
Next Steps
•Double-retroreflector on air
cart to increase fringe count
•Machined track & cart with
air through cart to stabilize
system
Results
Expected Δλ=0.85 pm,
measured through a 640
MHz beat frequency
LabView & GPIB automated
data acquisition
Special thanks to
Sarah Kaiser
for digital gating
circuit
Search for the sgoldstino Boson in e+e- Collisions
(student), (advisor), SLAC & Dept. of Physics, Stanford University
LOGO
We present an analysis for observing a hypothesized resonance at
214.3 MeV. This resonance corresponds to the production of a proposed
supersymmetric boson sgoldstino (P) in the e+ e-  P channel, which
needs to be isolated from the dominant background: e+ e- . The
isolation is performed by a series of simple cuts on the angular and mass
distributions of the decay products. In addition to this decay mode, there
are also other samples that can be useful as potential signals, including
the processes:
e+ e- , e+ e-  0, and e+ e-  .
The dominant background is the e+ e-  radiative, electromagnetic process. We must remove this background in order to identify the
aforementioned signals. We define two of the most important cut parameters below:
(2)  cos (): Angle that the photons make with the e+ e- propagation direction in the e+ e- center of mass frame
a)
Our estimated sensitivity is given by our figure of merit,
We observe many e+ e-   events (Note that all graphs are normalized):
Monte Carlo (MC) simulation and data agree for both rate and angular distribution
Figure 2:  Invariant Mass
which corresponds to how well the resonance can be observed over the background.
Our analysis places the optimal figures of merit for the 0 (135.0 MeV) and  (547.5 MeV)
channels at approximately 0.09  0.01, and 0.11  0.01, respectively, which demonstrates that we
currently lack adequate sensitivity to observe these resonances. Note that both the 0 and  have
cross sections of approximately 0.46 fb = 460 ab = 0.00046 pb.
Figure 10: Optimal Figures of Merit
In order for us to observe the
sgoldstino resonance clearly, i.e.
0.14
FOM >= 3, we need the
0.12
sgoldstino cross-section to be at
0.1
least 7.53 fb = 7530 ab = 0.00753
0.08
Pi0 FOM
pb, which falls roughly within the
Eta FOM
0.06
range set by Rubakov, from 1 pb 0.04
5 ab.
Figure 3:  cos() Distribution
Legend
Data
MC
Legend
Data
MC


e+
e-

b)
M(Note
 (GeV)
We observe many e+ e-    events
that all graphs are normalized) :
Monte Carlo (MC) simulation and data agree for both rate and angular distribution
0.02
cos()
0
0
0.2
0.4
0.6
0.8
1
cos(theta) of Photons in CM Frame
Figure 4:  Invariant Mass
Figure 5:  Invariant Mass
This following example demonstrates how we calculate the FOM of a   sample after making the
appropriate cuts that remove most of the e+ e-    events:
CUTS: |cos(Pi0 Decay Angle)| < 0.8, and |photons’ cos theta| < 0.8
Signals of events from a Monte Carlo simulation and Background events in the same mass region
are shown below with the aforementioned cuts performed on the data. The data has a luminosity of
35 fb-1, which is scaled up to 400 fb-1 with the appropriate scale factors. The value in parentheses is
the number of events within one standard deviation of the ’s invariant mass.
Legend
Data
MC
Figure 11: Background  Invariant Mass
M
(GeV)
Figure 6:  cos() Distribution
1
e+


M
Legend
Data
MC


e-
2

Legend
Data
MC
Signals  0,  ,  P also have certain angular and mass distributions that give hints for
appropriate cuts
cos()

1
e-
e+

cos()
Figure 9:  Decay Angle Distribution

MC
2

Figure 12: Signal  Invariant Mass
(GeV)
Figure 7:  Decay Angle Distribution
Legend
Data
MC

Figure 8:  cos() Distribution
Legend

Data
8/27/2012
N signal
N signal  N bkgnd
(1) 0 ,  Decay Angle:
Angle that the decay products (photons) make in the rest frame of the 0 ,  with the direction of the 0 and  in the e+ e- COM frame
c)
Figure 1: HyperCP Dimuon Mass Distribution
QuickTime™ and a
TIFF (Uncompressed) decompressor
are needed to see this picture.
OPTIMIZING THE CUTS
UNDERSTANDING BACKGROUND EVENTS
INTRODUCTION
Supersymmetry (SUSY) is a proposed theory that solves a number of
unsatisfying features of the Standard Model, such as the Gauge Hierarchy
and Naturalness problems3. In addition to this, SUSY unifies the EM,
weak, and strong forces by making quantum corrections to vacuum loop
diagrams. Indeed, it is known that the three forces have interaction
strengths that vary, or “run”, as the length scale is changed. This is caused
by the fact that the vacuum in which these forces operate acts like a
dielectric, screening the forces by creating quantum loops that negate the
strengths of the forces.
In the Standard Model, while the interaction strengths do run, the
values never coincide at a single point, thus making unification impossible.
However, with the additional quantum corrections predicted by
supersymmetry, the three interaction strengths actually run to coincide at a
single point. These quantum corrections, which are essentially additional
quantum loops in the vacuum, involve the interactions of a new class
particles. These new particles have a one to one correspondence with
existing particles and are thus aptly named the superpartners of current
particles.
The particle we are interested in searching for, the sgoldstino (pseudo
scalar spin 0 boson), is the superpartner to the goldstino matter particle.
The goldstino itself is the longitudinal component of the gravitino, which is
a candidate for the Lightest Supersymmetric Particle, or LSP.
Recently, the HyperCP2 group reported seeing three  p+- events
with a dimuon mass of 214.3 MeV (see figure below), a rare occurrence
that is expected to only have a 0.8% probability of happening. In an attempt
to explain this, Rubakov predicted that this process could in fact occur in
two stages1, with the sgoldstino produced as an intermediate particle, as
shown in the following process:  p + X, X+ -. Other processes
where the sgoldstino might be observed include the following: K+  + 0
P, KL    P, KS    P, and the process most interesting to us, e+ e- 
P, and e+ e- e+ e- P, which might be observed in SLAC’s e+ e- collider.
LOGO
FOM (S/sqrt(S+B))
ABSTRACT
Stanford Linear Accelerator Center, Menlo Park, CA
Department of Physics, Stanford University, Stanford, CA
Legend
Data
MC



Stanford Physics/AP/SLAC Undergrad Summer
cos()
M (GeV)
Ndata = 1.23457 * 109
Nbackground raw = 11106 (627)
Nbackground scaled = 126926 (7166)
Efficiency = 9 * 10-4 %
Scaling Factor: (400 fb-1 /35 fb-1) = 11.4
N signal
N signal  N bkgnd
M (GeV)
Ngenerated = 100000
Nsignal raw = 7609 (5435)
Nsignal scaled = 14 (10)
Efficiency = 7.5%
Scaling Factor: (0.46 fb * 400 fb-1) / 100,000 = 0.00184
= 10 / (sqrt (10+7166)) = 0.118
FUTURE WORK
We would like to analyze the system with a higher luminosity (currently looking with only 0.35
fb-1), and look at how additional cuts on other parameters might improve the FOM. Finally, we
can look into the e+ e- + -  channel and perform a similar signal and background analysis.
Like the current analysis, we expect the dominant background to be coming from
Research
5 radiative
electromagnetic processes.
cos()
REFERENCES
[1] D.S. Gorbunov, V.A. Rubakov, “On sgoldstino interpretation of HyperCP events,” arXiv:hep-ph/0509147
[2] H. Park et al. [HyperCP Collaboration], Phys. Rev. Lett 94, 021801 (2005).
[3] J. Feng, “Supersymmetry for Astrophysicists,” 2007 SLAC Summer Institute Lecture
Readability
• Poster is an art form but don’t get cute
• 18 pt font minimum (this is 32 pt)
• Smaller for captions (24 pt) /
This is 18 pt
• Title should be readable from distance
• Serif fonts easier to read than sans serif.
Times Roman is ok default; Arial for titles
• Use color to aid understanding, not entertain
• Minimize equations/derivations (see next
slide, lower left)
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Gravitational Wave Detection using Pulsar Timing Arrays
{Name}, Physics Class of 2009, Advisor {Name}
Wave Generation
PSR J0437-4715
August 29, 2008
In the weak field approximation to General Relativity, Einstein’s field equations
can be linearized to produce wave solutions. This gravitational radiation has
been indirectly shown to exist but has not been directly observed.
PSR J0613-0200
According to GR, the waves would be composed of two polarizations -- each a
quadrupole metric tensor perturbation -- rotated 45˚ from one another.
PSR J1713+0747
Figure 3. Logarithmic plot of strain amplitude versus frequency, showing the types of waves predicted to
be produced by certain phenomena. The sensitivity regions of the major detection efforts are also shown.
PSR J1824-2452
Observation
Figure 1. Schematic showing the plus and cross polarizations of a gravitational
wave, and their quadrupole signature.
Gravitational waves are produced by the changing quadrupole mass
moment of the source, according to the equations below:
One of the proposed methods for detecting gravitational waves is to analyze their effect on pulsar
signals. A passing wave will effect the time of arrival (TOA) to Earth of the pulsar’s pulses in a
periodic manner. The TOA residuals from an array of pulsars can be analyzed to reconstruct
information about the source of the gravitational waves. Thus an array can be used a telescope to
study otherwise unobservable objects.
The plots on the right show the effect of gravitational waves generated by the binary 3C 66B on the
pulsar array shown below. The parameters for the binary (Jenet et al. 2004) used in these calculations
are not reasonable, but are useful for demonstrative purposes. The binary is estimated to be
composed of two ~10 billion solar mass black holes orbiting each other with a period of 1 year and
eccentricity of 0.3. The binary is approximately 80 Mpc from Earth. The points in the plots are
simulated residuals with characteristic noise.
PSR J1909-3744
PSR J1939+2134
PSR J2129-5721
Conclusions
Figure 2. Artist’s rendering of the inspiral of a white dwarf binary, and its emission of
gravitational radiation.
Figure 4. Aitoff plot showing the positions on the sky of the seven pulsars in the array used for
these simulations. The larger the circle, the more accurately timed the pulsar is.
Acknowledgements: Figure 1: Kostas Kokkotas, Presentation, Aristotle University of Thessaloniki; Figure 2: NASA website; Figure 3: Richard N. Manchester, Presentation; Figure 4: Steve Healey; Equations: Hugo Wahlquist,
1987.
Although the effects of this particular wave could be easily seen, more
realistic wave amplitudes are still at least an order of magnitude from
being detected. Pulsars are being timed to greater and greater accuracies,
however, and the prospects for detection in the next decade using this
method are promising.
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Content
• Break into sections:
–
–
–
–
–
–
8/27/2012
Abstract
Statement of the problem or question investigated
description of the method used (iff relevant)
Results, including data/plots
Conclusions
If this is a work in progress, next steps or future
directions
Stanford Physics/AP/SLAC Undergrad Summer Research
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Abstract
• Full summary of the work
– What you did
– The Result(s)
• Based on Title and Abstract, viewer decides
whether to continue
• Next slide – good abstract, title font good,
other font too small
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Don’t Forget
• Acknowledgments
• References
• Contact info
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Printing
•
•
•
•
•
Design in one full-size PowerPoint/Keynote slide
Standard poster size is 36” x 42” (inches)
BUT our poster boards are 30”x40”
Use printer in your group if they have one
Printer in Varian 240 (next to Rick’s office)has
24” roll; size your poster for 22” x 34”
• Convert slide to pdf, then print from the PC next
to the printer.
• V240 printer instructions:
www.stanford.edu/dept/physics/academics/summer/poster_printing_instructions.html
8/27/2012
Stanford Physics/AP/SLAC Undergrad Summer Research
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Resources/References
Some material in this presentation is adapted from
1. Prof. Steven Block (Depts. of Biology, Applied Physics):
Block, S.M (1996). Do’s and Don’ts of Poster Presentation, Biophysical Journal 71(6), 3527-29. :
http://www.stanford.edu/group/blocklab/dos%20and%20donts%20of%20poster%20presentation.pdf
(some of this is dated but the main ideas are still good)
2. VPUE Poster Presentation info: http://www.stanford.edu/dept/undergrad/cgibin/drupal_ual/OO_research_opps_SURPSResources.html
A random sampling of web resources [search "designing poster presentations“]
– UW/NASA: poster recommendations
http://www.waspacegrant.org/posterdesign.html
– UCSF: Detailed PowerPoint instructions:
http://nurseweb.ucsf.edu/conf/cripc/posterppt.pdf
– Penn State: Samples and Templates http://www.writing.engr.psu.edu/posters.html
– DOE guidebook for general writing and presentations
http://educationlink.labworks.org/media/guidebook.pdf.
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