185 research outputs found
Resurrection of Traditional Luminosity Evolution Models to Explain Faint Field Galaxies
We explore the nature of the evolution of faint field galaxies by assuming
that the local luminosity function is not well defined. We use a non-negative
least squares technique to derive a near optimal set of local luminosity
functions for different spectral types of galaxies by fitting to the observed
optical and near-infrared counts, B-R colors, and redshift distributions for
galaxies with 15 < B < 27. We report here the results of using only traditional
luminosity evolution (ie. the photometric evolution of stars in a galaxy over
time given reasonable assumptions of the form of the star formation history for
various galaxy types), and simple galaxy reddening and find excellent fits to
the observed data to B = 27. We conclude that models more exotic than
traditional luminosity evolution are not yet required to explain existing faint
field galaxy data and thus the need for contributions by mergers or new
populations of galaxies is at least 5x less than previously estimated.Comment: 9 pages + 1 table + 4 figures; uuencoded tar compressed postscript;
to be published in The Astrohysical Journal Letter
Lyman Alpha Emitting Galaxies at 2 < z < 3: Towards a Calibrated Probe of Dark Energy
The goal of this project was to establish the physical properties of Ly{alpha}#11;emitting galaxies from redshifts of 2 to 3 in order to better calibrate the use of LAEs as probes of the large scale structure of the universe for upcoming dark energy experiments, such as the Hobby Eberly Telescope Dark Energy Experiment (HETDEX). We have obtained narrow-band imaging of the Extended Chandra Deep Field South (ECDF-S) in two different narrow-band #12;filters centered at Ly{alpha}#11; at z=2.1 and 3.1. The resulting of samples of LAEs were used to determine the LAE luminosity function, equivalent width distribution and clustering properties (bias) of LAEs at these redshifts. While the results from the ECDF-S appear robust, they are based on a single field. To explore the effects of cosmic variance and galaxy environment on the physical properties of LAEs, we have also obtained narrow-band data at both redshifts (z = 2:1 and 3:1) in three additional #12;fields (SDSS 1030+-05, the Extended Hubble Deep Field South, and CW 1255+01). The narrow-band imaging data has been reduced and LAE catalogs are being generated. We have calculated preliminary luminosity functions, equivalent width distributions, and clustering properties. We have also obtained follow-up spectroscopy in the optical (using VLT/FORS) and in the near-infrared (using Magellan/MMIRS). Since individual LAEs have too little S/N to enable meaningful fits for stellar population parameters, our previous work has analyzed stacked Spectral Energy Distributions (SEDs). SED #12;fitting was performed on several subsets of LAEs selected by their rest-UV luminosity, UV spectral slope, Ly alpha luminosity, Equivalent Width, or rest-optical (IRAC) luminosity
Comparing Infrared Star-Formation Rate Indicators with Optically-Derived Quantities
We examine the UV reprocessing efficiencies of warm dust and polycyclic
aromatic hydrocarbons (PAHs) through an analysis of the mid- and far-infrared
surface luminosity densities of 85 nearby H-selected star-forming
galaxies detected by the volume-limited KPNO International Spectroscopic Survey
(KISS). Because H selection is not biased toward continuum-bright
objects, the KISS sample spans a wide range in stellar masses
(-), as well as H luminosity
(-), mid-infrared 8.0m luminosity
(-), and [Bw-R] color (-.1-2.2). We find that
mid-infrared polycyclic aromatic hydrocarbon (PAH) emission in the Spitzer IRAC
8.0m band correlates with star formation, and that the efficiency with
which galaxies reprocess UV energy into PAH emission depends on metallicity. We
also find that the relationship between far-infrared luminosity in the Spitzer
MIPS 24m band pass and H-measured star-formation rate varies from
galaxy to galaxy within our sample; we do not observe a metallicity dependence
in this relationship. We use optical colors and established mass-to-light
relationships to determine stellar masses for the KISS galaxies; we compare
these masses to those of nearby galaxies as a confirmation that the
volume-limited nature of KISS avoids strong biases. We also examine the
relationship between IRAC 3.6m luminosity and galaxy stellar mass, and
find a color-dependent correlation between the two.Comment: 15 pages, 10 figure
UVOT Measurements of Dust and Star Formation in the SMC and M33
When measuring star formation rates using ultraviolet light, correcting for
dust extinction is a critical step. However, with the variety of dust
extinction curves to choose from, the extinction correction is quite uncertain.
Here, we use Swift/UVOT to measure the extinction curve for star-forming
regions in the SMC and M33. We find that both the slope of the curve and the
strength of the 2175 Angstrom bump vary across both galaxies. In addition, as
part of our modeling, we derive a detailed recent star formation history for
each galaxy.Comment: 6 pages, 5 figures, conference proceedings from Swift: 10 years of
Discovery, held in Rome (2-5 Dec. 2014
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