Starburst History -- Connecting the Dots
Starburst history in individual galaxies must be consistent with the statistics
of galaxies in bursting, quiescent star formation, or non-star-forming states.
This investigation of 0<z<3 galaxies determines whether the individual and
collective histories are consistent, and whether galaxies can be traced evolving
over time using mass, specific star formation rate, and/or morphology.
Cosmic Star Formation History
Synthesis analysis:
the star formation density history of the universe over 0<z<2 using GALEX UV,
Far IR, and optical redshifts (photo and spectroscopic). Using the largest
sample possible, subdivide SF History by galaxy properties: stellar mass, gas
mass, star formation rate, specific star formation rate, SED, morphology, SF
radius, stellar radius, recent starburst history, local galaxy density,
extinction, SF mode [starburst, quiescent], presence of companions, etc.
Star
Formation and Dust Reprocessing
A central and
controversial question in galaxy evolution is the balance of energy emitted in
the UV/optical and the Far IR/sub-mm bands. It has implications both for the
history of star formation and how this history depends on the modality of star
formation, quiescent or violent. We will use IRAS and GALEX to determine the
joint FIR/UV luminosity function in the local universe and the corresponding
star formation rate. This investigation will be extended to z ~ 1 using the
deepest Galex imaging data together with far-IR data from Spitzer and a
combination of photometric and spectroscopic redshifts (DEEP2, CDF-S, NOAO-DWFS,
COSMOS).
Intergalactic Medium
Emission:
GALEX deep images and spectroscopy provide the first opportunity to search for
emission from the Intergalatic Medium in the low redshift universe with
unprecedented sensitivity. This search will require new analysis tools designed
to perform
unbiased and targeted (w/priors) searches for Lyman alpha emission from the IGM
either through direct detection or cross-correlation with group, filamentary, UV
luminous objects, and other structures with 3-d distributions determined from
redshift surveys. Compare IGM to the local UV luminosity density.
Absorption:
GALEX spectroscopy of QSOs is yielding many Lyman Limit absorption systems. This
project will explore the spatial distribution of LL systems and its relationship
to the large scale structure traced by star forming galaxies.
