presenting at your best-
Enables your individual input to a
conference or meeting
Share your work
Get feedback on your research
Develop your experience communicating
in the scientific/technological world
Get travel award for a conference
Relevant to Audience – Do You
Know Your Audience?
and A Successful
Visually Demonstrates Enthusiasm
Appealing, But – The Presenter and the
Not Too Busy Poster By Itself -
What Goes on a Poster
Discussion or Summary
•What if you’re
not there to
Keep it Interesting
Preparing YOUR Poster
Design Your Layout
Use Oral Get Details From
Presentation the Conference
Font and Poster Size
Can you read it from 4 feet away?
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...
48" = 4 feet
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
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.
MIRROR ALIGNMENT USING DUAL BEAM LASER
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
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
Rehearse 3-5 Minute
Enhance What is
Dress to Impress
Bring Resume or
Your Poster at SACNAS
You never know who
you will meet!
We’ll be there to
Lots of graduate
school and industry
You will be judged
Poster Making Timeline
Weekly July 27
Meeting Mini Poster
Outlines Aug 10
Due at End
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