1. A Survey of Starburst Galaxies An effort to help understand the starburst phenomenon and its importance to galaxy evolution Megan Sosey & Duilia deMello March 2, 2006

2. Starburst Galaxies
Galaxies going through active, ongoing star formation
The “burst” dominates the luminosity of the galaxy
Contain massive hot stars which dominate the galaxies energetics from the farUV to the near IR.
Emission-line spectra, blue optical colors and far-IR colors are commonly used in diagnostics and classification
Good laboratories for investigating the physical processes occurring in star-forming regions locally and in the early universe

3. Questions to be answered?
Do all galaxies go through starburst phase?
What are the mechanisms required to start and stop star-formation? Interaction? Environment?
Are starbursts the local analog of high-redshift star forming galaxies such as Lyman Break galaxies?
How much of the intergalactic medium is enriched by outflows from starbursts?
How is the SFR or stellar mass budget distributed amongst galaxies of different types and masses

4. Why is this study important?
The definition of starburst is not well constrained in the literature
The available data is highly uneven, some objects have been studied more extensively, and in more wavelengths than others
Multi-wavelength data is essential because galaxies appear different depending on the emission mechanism that dominates their radiation; It will help properly evaluate the overlap between the starburst population and high-redshift star-forming galaxies

5. Initial Project Goals
Produce a color selected sample of star-forming galaxies from the SDSS
Identify a set of physical conditions and the chronology of events which lead to the starburst
Build a multi-wavelength database using the VO which is accessible to the community and can evolve as new observations are made available

6. Sample Selection
Samples of starbursts derived from UV spectral observations exist in the literature
Atlas of UV-to-FIR magnitudes for 83 starburst galaxies (Wu+, 2002; Kinney 1993)
Common objects are selected from the SDSS
We determine the SDSS colors that these galaxies have and use color-color and color-magnitude diagrams to select all galaxies in the SDSS with similar colors, in order to derive a statistical sample

7. Sample Contamination
Biased against dusty galaxies that are IR luminous
The nature of the underlying source is unknown and could be an AGN
AGN’s themselves might bias the sample, so a comparison against known star-forming galaxies in the SDSS must be performed
Control samples of isolated galaxies, mergers and pairs taken from SDSS will be used for comparison

8. Final Sample There will be two main components
A magnitude limited sample
A distance limited sample based on redshifts taken from SDSS
Objects can be classified as a function of luminosity, stellar mass, metallicity and total gas
-our sample criteria should allow us to find more than 1,000 objects in the SDSS

9. Analyze AND manage the data?
The VO is an excellent resource for information and analysis
Interconnected tools provide an easy interface between available data and scientific analysis
The convenience of the internet allows a unique opportunity to create an evolving data warehouse, easily accessible to the community, and easy to update as new data is made available

10. Examining the Environment around starburst galaxies
Interactions may be important for triggering activity in galaxies
How is the star formation efficiency correlated with the environment where galaxies reside?
Investigate galaxy properties by comparing SFR, metallicity, stellar mass in low and high density environments

13. An example galaxy to show, links go directly to sdss explorer

19. NGC 3690
V=3033

20. NGC2798 v=1739
Interaction with
NGC2799 v=1673

21. NGC 3448 v=1350
1 companion at 3.9’
V=1493 (UGC6016)

22. NGC 4194 v=2506 no companion within one degree
at similar velocity

26. Preliminary Results
--- Mergers (Allam et al. 04) Karachentseva isolated galaxies