Announcements Project Medley Outlines due Tuesday! – 1 page typed and double-spaced – What do you plan to do for your project? On-Campus Observing Moved.

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Presentation transcript:

Announcements Project Medley Outlines due Tuesday! – 1 page typed and double-spaced – What do you plan to do for your project? On-Campus Observing Moved (likely July 15, depending on weather forecasts).

Photometry of the Pleiades Tiffany Pewett

The Pleiades Well known star cluster near Taurus the Bull. Nearby, easy to study.

Goal of the Lab Use computer program (CLEA) to gather photometric data of several stars in the Pleiades star cluster. Use this data with Main Sequence Fitting to find the distance to the cluster.

Magnitudes Absolute Magnitude (M)- brightness of an object if it were only 10 parsecs away. Apparent Magnitude (m)- brightness of an object as viewed from Earth. Higher magnitude number = fainter object. 1 unit in magnitude = 2.5× brighter or fainter.

H-R Diagram Luminosity Temperature

H-R Diagram Luminosity Temperature

H-R Diagram Luminosity Temperature

CLEA Program Do not exit out of the program, it takes a while to set it back up. You MUST measure sky brightness (first table) before you can do anything else. Wall computers gather data for stars 1-8, front computers do Share these with people behind you once you have finished.

Exposure Times & Integrations Exposure time- how long the shutter remains open. – Want it open long enough to gather enough light from the star. Integrations- number of images taken which are then combined. – This reduces error by eliminating any light that doesn’t belong.

Gathering Star Data Use only 2 filters B (blue) and V (visible). Center the star in the circular aperture. Take 4 integrations for each star. Determine exposure time based on size of star.

Gathering Data

Determining Exposure Time

PLOT YOUR POINTS WHILE YOU WAIT.

Answer Questions Make sure you fully answer ALL questions on the front page of your lab!

Finding Distance M=absolute magnitude (mag. From 10 pc away) M=apparent magnitude (mag. Seen from Earth) Use M=0 on transparency to find m D(in pc)=10 × 10 (m-M)/5 – Remember you used M=0 – 1 parsec=3.26 lightyears