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Online resources / data / computing

Writing guide

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.

Computing in our group / at JHU CAS

Astro5 is available for CAS (Center for Astrophysical Sciences) members and students. It is particularly beneficial to those working on SDSS data.

Kinematic decomposition and non-parametric measurements of emission lines

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. The code calls dl_detail.dat, where the first column is redshift and the second is the dimensionless combination D_L H/c (luminosity distance times Hubble constant divided by speed of light) pre-computed for H=70 km/sec, Omega_M=0.3 and Omega_Lambda=0.7.

Spectroscopic identification of type 2 quasars at z<1 in SDSS-III/BOSS -- by Yuan, Strauss and Zakamska

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:
-- The catalog of 2920 spectra of type 2 quasars by Yuan et al. in FITS and tbl formats;
-- Kinematic decomposition of the [OIII]5007 line and double-peaked candidates in the Yuan et al. sample in FITS and tbl formats;
-- Kinematic decomposition of the [OIII]5007 line and double-peaked candidates in the Reyes et al. 2008 / Zakamska and Greene 2014 sample in FITS and tbl formats (if you use this catalog please cite Yuan et al. 2016, Zakamska and Greene 2014, and Reyes et al. 2008 papers);
-- Composite spectrum of the Yuan et al. type 2 quasars in FITS and tbl formats.
Please let me know if you discover any problems with the data tables.

Star formation rates in quasar hosts

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.

Ultraluminous infrared galaxies

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.

Optically selected type 2 quasars

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.