Online resources, computing, datasets

Guides for graduate students

Guide to first draft: standards for paper preparation for all students in our group.

Guide to publication-quality figures: standards for figure preparation for all students in our group.

Guide to asking questions at presentations

Garland -- advice for speakers, it's a classic that never gets old.

Software developed in our group:

Q3DFIT, custom software for scientific analysis of integral field unit (IFU) spectroscopy of quasars and their host galaxies (PI D.Wylezalek, CoPIs N.Zakamska and S.Veilleux, software lead D.Rupke, 2022), specifically targeted at high-contrast analysis of quasar host galaxies with the James Webb Space Telescope. Papers that explain and use the code inlude: Veilleux et al. 2023 on outflow in XID 2028 and Vayner et al. 2023 on ionization in SDSS J1652.

Hsiang-Chih Hwang's Github with tools for download and analysis of WISE light curves (2020) and measurements of eccentricities of wide binaries (2022)

Vedant Chandra's pipeline for the analysis of white dwarf spectra (2021) and for high-precision radial velocity measurements of white dwarfs and red dwarfs (2024).

Nadia Zakamska's Github page. Currently available: (1) a first-principles filter convolution code; (2) a code to calculate the cyclotron spectrum from homogeneous thermal plasma in uniform magnetic field (2022); (3) a code to calculate the spectropolarimetric properties of quasar emission lines scattered by axisymmetric outflows (Zakamska and Alexandroff 2023).

Self-contained data tables

If you use the data, please reference the paper(s) the data came from, as indicated.

2021: Variability, periodicity, and contact binaries in WISE, Petrosky et al.

FITS catalog of WISE periodic and aperiodic variables, accompanything this paper; data model for the FITS file is shown in the paper.

2019: Mid-infrared spectroscopic evidence for AGN heating warm molecular gas, Lambrides et al.

The stacked Spitzer spectra and spectral feature measurements

2016: 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.

2016: 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.

2016: 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.

2014: Ultraluminous infrared galaxies

From the paper by Hill and Zakamska 2014 -- reduced, stitched and calibrated Spitzer IRS data, along with measurements of emission features for a sample of 115 Ultraluminous Infrared Galaxies from the IRAS 1 Jy sample.

Download this file which contains two directories:
-- Directory "tables", with six files tab*_final.dat containing all the data for all the tables in the paper. Every file has a header describing the contents of the table (also explained in the text of the paper).
-- Directory "spitzer_spectra" with 115 data files for Spitzer spectra of the 115 objects presented in the paper. The files are named in accordance with the object identifications shown in Table 1, except the sign of the declination is replaced by a letter ('m' for 'minus' or negative declination, 'p' for 'plus' or positive declination). All files are of the same size and in the same format. The pointing of the Spitzer observation and the names and units of the data columns are shown in the header of each data file.

If you use these data, please reference the paper.

2003, 2014: 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.