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     -preparing and
presenting at your best-

                     Malika Bell
                    Summer, 2006
           Why Posters?
 Enables your individual input to a
  conference or meeting
 Share your work

 Network

 Get feedback on your research

 Develop your experience communicating
  in the scientific/technological world
 Get travel award for a conference
  (travel free!!!)
      Relevant to Audience – Do You
          Know Your Audience?

Organized,                               Presentation
   and           A Successful
 Logically          Poster
       Visually               Demonstrates Enthusiasm
    Appealing, But             – The Presenter and the
    Not Too Busy                  Poster By Itself -
     What Goes on a Poster
   Minimal Words
   Introduction
   Abstract (optional)
   Methods
   Results
   Discussion or Summary
   Acknowledgements
   Your Style
               Standard Flow


•Show them
your story
•Visuals rather
than words
•What if you’re
not there to
present it?
Keep it Interesting
Preparing YOUR Poster
                       Prioritize Information

  Design Your Layout

      Use Oral           Get Details From
    Presentation         the Conference
         Font and Poster Size

 Can you read it from 4 feet away?
 Suggestions
                                   What size should
    •   Basic font and symbols     my poster be?

    •   Titles: 90 pt
    •   Sub titles: 72 pt
    •   Other poster content: 18-20pt
    •   NEVER smaller than 14 point
   Ask conference people about size
    Setting Up the Poster Slide
•   Create a New PPT File - choose "blank
    presentation" upon opening program, or use "File"
    menu and choose "New..."
•   Page Setup - choose "Page Setup..." in "File" menu
•   Page Setup Dialog Box - set as below...

Page Settings
      48" = 4 feet
                                                 don't worry
      36" = 3 feet
 Looking at Your Poster Slide

                            Notice that you are
 This one                   only looking at a 11%
 slide is                   zoom of your poster
 3' X 4'

You Now Have a Presentation with 1 Very Big
                 Slide !!
                            Stellar Population Evolution in Early-type Galaxies
                       J.M.Holt, Dept. of Physics, University of California, Santa Cruz

                Abstract                            Hertzsprung-Russell diagram                                 Findings                                Conclusions
Galaxies are complex systems that contain                                                             Galaxies at z~1 are brighter              •The Size vs. Magnitude plot at left
stars and gas. The easiest galaxies to                                                                             Size vs. Magnitude           shows that galaxies at high redshift
model are early-type galaxies, which have                                                                                                       are brighter by about 1.5 mag. This
elliptical shapes, smooth images, and are                                                                                                       means that 7 billion years ago
gas-poor. In this project, high-resolution                                                                                                      galaxies were four times more
images of galaxies taken with the Hubble                                                                                                        luminous than today.
Space Telescope are used to estimate how                                                                                                        •A Single stellar population model
much early-type galaxies have changed in                                                                                                        (lower left) shows that galaxies
the last 7 billion years. This corresponds to                                                                                                   formed their stars around 9.5 billion
the last half age of the Universe. As one                                                                                                       years ago. This means that at the
looks back in space and time, stellar                                                                                                           epoch that we observe them the
populations of galaxies should be younger                                                                                                       stellar populations were about 2.5
and should contain more short-lived,                                                                                                            billion years old.
luminous stars that have since disappeared.
The total amount of light emitted by an
object over its area is called “the surface
brightness,” a quantity that for galaxies is
independent of the distance but evolves with
time. Surface brightnesses for a small                                                                    Best fit is at z=1.65
sample of early-type galaxies will be                                                                                                             Acknowledgements
measured, and the expectation is that in the                                                                  Single Stellar Population Model   I would like to thank Prof. Sandy
past, these surface brightness were higher                                                                                                      Faber for sharing her expertise,
than at present.                                                                                                                                Dr. Christopher Willmer donating
                                                  The Hertzsprung-Russell diagram is a plot of                                                  his time and talents to explain
                                                  stellar luminosity vs. temperature. The diagram                                               every step. Thanks to Ben
                                                  above shows the evolutionary track of a star. The                                             Weiner for help with population
                   Goals                          most massive stars have the most fuel but they                                                models and everyone at CfAO.
•Compare young galaxies to present day            also use it up faster. Thus, they leave the main                                              This work has been funded by
galaxies.                                         sequence sooner than lower mass stars and                                                     the National Science Foundation
•Verify that galaxies in the past were brighter   eventually burn themselves out. This means that                                               under Grant No. AST 00-71198.
than present day galaxies.                        high surface brightness in a galaxy is a good
                                                  indicator that its stellar population is young. I
•Model how the stellar populations in galaxies    compared the surface brightness of local galaxies
change with time.                                 to that of galaxies at very large distances when
•Find out when galaxies formed their stars.       their stellar populations were younger.
               Vinya Agluba, Smithsonian Astrophysical Observatory, Submillimeter Array, Hilo, HI

SMA Optics Layout                                                                                                                                                                 Second Trial
                                                                                      Since it would be hard for us to look for
                                                                                      the laser beam propagated on the sub
                                                                                                                                                                                                                Instead of positioning the laser
                                                                                      reflector, a video camera is installed on
                                                                                                                                                                                                                170mm high from the 4-5-6 plate, the
                                                                                      the vertex of the reflector.
                                                                                                                                                                                                                laser is placed such that the laser
                                                                                                                                                                                                                beam strikes the center of mirrors M4
                                                                                                                                                                                                                and M6. Crosshairs are placed
                                                                                                                                                                                                                across the mirrors to show the center
                                                                                                                                                                                                                of the mirrors.

A 6-meter diameter paraboloidal primary reflector is combined                                                         The DS9 program is used to measure
with a 350 mm diameter hyperboloidal sub reflector. Mirrors M3                                                        the amount of displacement of the
through M6 form a beam waveguide which directs the beam                                                               laser beam on the sub reflector from
from the antenna vertically downward into the receiver optics                                                         the center as the antenna moves from
assembly.                                                                                                             different elevation.
The goal of this project is to assemble a portable setup that
would align the sub reflector and the beam waveguide mirrors.

  Align                 Reduce                    Achieve
  Mirrors               Losses                    Maximum                                                                                                                              Antenna elevation: 15°                    Antenna elevation: 85°

                      -due to: beam
                                                                                      First Trial                                                                                 Looking again at the sub reflector, the laser beam is off the center
                      truncation, distortion at   230GHz – 0.7-0.8                                                                                                                at an antenna elevation of 15°. But as the antenna elevation
                      focusing mirrors, and       345GHz – 0.55-0.65                                             M4
                                                                                                                                                                                  increases, the laser beam disappears as shown in the picture
                      absorption and                                                                                                                                              above with an elevation of 85°. This proves that the laser beam
                                                  690GHz – 0.4                                                         One end of the dual laser is placed
                      reflection at windows
                                                                                                                       right on the focal point of mirror M4,                     does not pass through the focal point (the laser beam was higher
                      and mirrors
                                                                                                                       which is 170mm high from the 4-5-6                         than 170mm) and thus, beam truncation could have occurred.
                                                                                                                       plate to assure that the laser beam

Methods                                                                                                 170mm          passes this critical point.

To align the mirrors, a dual beam laser is used. Because there
are visible red beams at each end of the laser that are aligned to
                                                                                                                                                                                                                   A portable setup is built to align the
each other, it feasible to place this laser between mirrors M4 and
                                                                                                                                                                                                                   mirrors of the Submillimeter Array
M5 since there is a lot of space for the laser and a focal point is
                                                                                                                                                                                                                   optics. It must be noted that the
located. The mount for the laser is kinematic, it can be adjusted
                                                                                                                                                                                                                   laser beam should pass through
by its x-y-z axis and angle.                                                                                                                                                                               170mm
                                                                                                                                                                                                                   the focal point of mirror M4 so
                                                                                                                                                                                                                   there would be no beam truncation
                                 Mirror M4 is an ellipsoidal mirror.                    Antenna elevation: 20°                        Antenna elevation: 70°
                                                                                                                                                                                                                   that would occur. To assure the
                                 If the laser beam strikes this                                                                                                                                                    170mm height, targets like shown
                                 mirror, the beam would disperse.                      Looking on the sub reflector, the laser beam is off the center and
                                                                                       as the elevation of the antenna changes, it moved by 1-3 pixels.                                                            on the picture on the left could be
                                 So, an aperture stop is placed                                                                                                                                                    placed on both ends of the laser
                                 after M4 to block the dispersion                      The laser beam on the sub reflector is still dispersed even
                                                                                       though an aperture stop is already placed because the mirror M3                                                             and one target is positioned right
                                 and still have a fine beam going                                                                                                                                                  where the focal point is located.
                                 to the sub reflector.                                 is too dusty that it had contributed to the dispersion of the laser

                                      •Rob Christensen, Research Supervisor                                                         This project is supported by the National Science Foundation Science and
                                      •SMA Staff                                                                                    Technology Center for Adaptive Optics, managed by the University of California at
                                      •Sarah Anderson, Malika Bell and Lisa Hunter, Center for Adaptive Optics                      Santa Cruz under cooperative agreement No. AST - 9876783.
                                      •University of Hawaii - Manoa
Presenting Your Poster
              Prepare and
               Rehearse 3-5 Minute
              Don’t Ramble
              Avoid Reading
              Enhance What is
               Already Written
              Dress to Impress
              Bring Resume or
               Business Cards
Your Poster at SACNAS
              You never know who
               you will meet!
              We’ll be there to
               support you
              Lots of graduate
               school and industry
               representative to
              You will be judged
              Winner $500
                    Poster Making Timeline
                                           For Mainland
   July 24
  Weekly         July 27
  Meeting      Mini Poster
               Outline Due

                               July 31
                              Go Over
                             Mini Poster
                              Outlines           Aug 10
                                                Work on
                                              Final Posters
                                               Due at End
                                                 of Day
        Mini Poster Outline
 Due for next weeks meeting
 Sketch out the topics you’ll cover

 Determine what existing slides you’ll
  use (from your mini talk)
 Play around with formatting so we
  can answer questions next week

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