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Online resources / data / computing
Guide to first draft: standards for draft preparation for all students in our group.
Guide to publication-quality figures: standards for figure preparation for all students in our group.
IDL code used in Zakamska & Greene 2014 and Yuan et al. 2016 to measure kinematics of [OIII] is now available. As input, it takes a list of fits files with SDSS spectra and their pipeline redshifts. An example list of the first 10 objects from the Yuan's sample is available here. The spectra from this list are bundled up here.
This paper was submitted to MNRAS on June 14, 2016. The full text of the paper is here, with data model for the catalogs presented on the last page of the paper.
Four electronic tables are available:
Full electronic tables from Zakamska et al. 2016 (MNRAS): far-infrared photometry and mid-infrared spectroscopy of type 2 quasars and red type 1 quasars. Herschel photometry of type 2 quasars from Petric et al. (in prep) will be publicly available at a later time. Herschel photometry of type 1 quasars is presented by Petric et al. 2015 and Spitzer spectroscopy of type 1 quasars is presented by Shi et al. 2007. Other data available on request.
From the paper by Hill and Zakamska 2014 -- reduced, stitched and calibrated Spitzer IRS data, along with measurements of emission features available HERE for a sample of 115 Ultraluminous Infrared Galaxies from the IRAS 1 Jy sample.
From Zakamska et al. 2003, a composite spectrum of type 2 AGN. The columns wv and flave are the wavelength and the average flux density. About half of these are above the quasar luminosity cutoff, and about half are below. The redshift was based on the [OII] emission line. The host galaxy is prominently detected, but the composite does not capture the wide range of the emission line equivalent widths. Therefore, this composite is not appropriate for calculating simulated colors of type 2 AGN; I suggest adding host galaxy, scattered light and emission lines from the next template in different proportions to get an idea of what the scatter of colors would be like. If you use this composite, please cite Zakamska et al. 2003.
From Zakamska and Greene 2014, host-galaxy-subtracted (pure emission line) 5 composites in bins of [OIII] width and 5 composites in bins of [OIII] luminosity. The first column is the rest-frame wavelength in A, then 5 templates in order of increasing value of width or luminosity. The host galaxy subtraction is not perfect, there are some residual features visible in the stacks, this is discussed in the paper. If you use these composites, please cite Zakamska and Greene 2014.
Lots of other data available; please feel free to contact me.