1. Overview of the Hartnell Astronomy Research Inquiry Deisgn Team: Anne Metevier, Jennifer Lotz, Pimol Moth, Lindsey Pollack, Candace Church EHR Meeting, 19 December 2005

2. Inquiry Goals Attitude-based Attitude-based Build students’ confidence Build students’ confidence Succeed in research setting Succeed in research setting Foster a sense of community Foster a sense of community Skills-based Skills-based Give students practice using research skills Give students practice using research skills Generating questions Generating questions Transforming observations via plotting, interpreting data Transforming observations via plotting, interpreting data Developing explanations from evidence Developing explanations from evidence Oral and written communication Oral and written communication Conveying specific scientific content is NOT a key goal!

3. Before the Inquiry Activity Before the Inquiry Activity ~2 days of background lectures on doppler shift, the distant universe, light and spectra ~2 days of background lectures on doppler shift, the distant universe, light and spectra Question-generating activity Question-generating activity Present unfamiliar image, have students write down questions about it Present unfamiliar image, have students write down questions about it

4. Inquiry Time Line 20 min. Short intro & stated goals 20 min. Short intro & stated goals 70 min. Starters, 3 rotations 70 min. Starters, 3 rotations 15 min. Gallery walk, form groups of 2-3 students 15 min. Gallery walk, form groups of 2-3 students 4 hrs. Investigations (split over 4 days) 4 hrs. Investigations (split over 4 days) 10 min.Thinking tools (as needed in individual groups) 10 min.Thinking tools (as needed in individual groups) 30 min.If two groups working on same starter, groups meet to discuss findings and approaches. 30 min.If two groups working on same starter, groups meet to discuss findings and approaches. 45 min. Poster preparation 45 min. Poster preparation 10 min.Sharing out (10 min/group) 10 min.Sharing out (10 min/group) 30 min. Synthesis 30 min. Synthesis Final abstracts due after synthesis. (two iterations -- about 90 min. of informal time) Final abstracts due after synthesis. (two iterations -- about 90 min. of informal time)

5. Starters 3 Posters 3 Posters Galaxy morphologies -- Hubble UDF image Galaxy morphologies -- Hubble UDF image Rotation curves -- Poster with DEEP data Rotation curves -- Poster with DEEP data AGNs -- “Mystery Galaxies” poster AGNs -- “Mystery Galaxies” poster

6. Research Inquiry Stations: Galaxy Morphologies Content Areas: Content Areas: Galaxy Classification -- looking at different types of data Galaxy Classification -- looking at different types of data Images, surface brightness profiles, contour maps, spectra Images, surface brightness profiles, contour maps, spectra Galaxy subcomponents: disks, bulges, spiral arms, bars Galaxy subcomponents: disks, bulges, spiral arms, bars Exponential and de Vaucouleurs surface brightness profiles Exponential and de Vaucouleurs surface brightness profiles Components not easily fit: spiral arms, bars, star forming clumps Components not easily fit: spiral arms, bars, star forming clumps Galaxy morphologies vs. redshift Galaxy morphologies vs. redshift Selection effects: apparent sizes, viewing angle Selection effects: apparent sizes, viewing angle Tools: Tools: Color images, contour maps Color images, contour maps Ellipse measurements, models, residuals Ellipse measurements, models, residuals Graphical analysis software for SB analysis Graphical analysis software for SB analysis Redshifts Redshifts Useful websites with sims of mergers, etc. Useful websites with sims of mergers, etc.

7. Research Inquiry Stations: Spectra & Rotation Curves Content Areas: Content Areas: 1D vs. 2D spectra 1D vs. 2D spectra Viewing angle Viewing angle Relationship between mass distribution and rotation curve shape Relationship between mass distribution and rotation curve shape Solid body, Keplerian rotation, dark matter Solid body, Keplerian rotation, dark matter Tools: Tools: 1D and 2D spectra of edge-on and face-on galaxies, inclined disk with slit at wrong PA, galaxies with broadened emission and absorption lines 1D and 2D spectra of edge-on and face-on galaxies, inclined disk with slit at wrong PA, galaxies with broadened emission and absorption lines Stellar and galaxy spectra for comparison Stellar and galaxy spectra for comparison Solid body rotation demonstrator (turntable) Solid body rotation demonstrator (turntable) Keplerian rotation demonstrator (Vortex) Keplerian rotation demonstrator (Vortex) Doppler effect demonstrator (Doppler ball) Doppler effect demonstrator (Doppler ball) Worksheet on planetary orbits Worksheet on planetary orbits

8. Research Inquiry Stations: AGN Content Areas: Content Areas: Classification Classification Viewing angle -- unification Viewing angle -- unification Field of view and wavelength observed (affects whether we see disk vs. jet, etc.) Field of view and wavelength observed (affects whether we see disk vs. jet, etc.) Inferring presence of black hole (measuring size, mass of central object) Inferring presence of black hole (measuring size, mass of central object) Constraints on what is producing light Constraints on what is producing light Shape -- not spherical Shape -- not spherical Processes -- can rule out fusion, radiation pressure Processes -- can rule out fusion, radiation pressure Tools: Tools: Many images (radio, X-ray, visible) Many images (radio, X-ray, visible) Spectra & SEDs of AGNS and “normal” galaxies for comparison Spectra & SEDs of AGNS and “normal” galaxies for comparison Shape of SED is power law, not blackbody Shape of SED is power law, not blackbody Broad lines in AGN spectrum --> mass estimate of central object Broad lines in AGN spectrum --> mass estimate of central object Light curves --> size of central object Light curves --> size of central object Football stadium thinking tool Football stadium thinking tool Calculating the mass of Mrk 335 Calculating the mass of Mrk 335