Data products of "The demographics of obscured AGN from X-ray spectroscopy guided by multiwavelength information"

In Laloux et al. (2022, in prep), we developed an approach to guide AGN X-ray spectroscopy with multi-wavelength data. The abstract of the paper is in the  additional notes. We extracted and fitted the X-ray spectra of 2965 AGN within the Chandra COSMOS Legacy survey.
Here, we release the data of our results:
- spectral_extraction_info.fits contains the information relative to the spectral extraction and is described and partially displayed in Table 2 of the original paper. The table contains the information of the 2965 sources and has 11 columns: ['ID', 'RA', 'Dec', 'RA_optical', 'DEC_optical', 'EEF', 'radius_src', 'cts057', 'cts_bkg', 'hard_flag', 'ID_L18']. They correspond to:
    (1) source ID;
    (2-3) X-ray position;
    (4-5) optical counterpart position;
    (6) EEF used for extraction in percent units;
    (7) source radius in arcsecond;
    (8) $0.5-7$keV net photon counts of the source;
    (9) the net photon counts of the background in all energy band;
    (10) flag indicating if the source is detected in the hard band (2-7keV);
    (11) source ID in Lanzuisi et al. (2018) if cross-matched.

- fit_info.fits contains the information relative to the X-ray spectroscopic analysis and is described and partially displayed in Table 6 of the original paper. The tables also contains 2965 sources and has 19 columns: ['ID', 'z', 'ztype', 'logLx', 'logLxlo', 'logLxhi', 'logNH', 'logNHlo', 'logNHhi', 'gamma', 'gammalo', 'gammahi', 'CT_candidate', '2-peaked', 'ID_Jin', 'logL6um', 'logL6umlo', 'logL6umhi', 'upperlimits']. They correspond to:
    (1) source ID;
    (2) redshift;
    (3) redshift type: spectroscopic, photometric or None;
    (4-6) X-ray 2-10keV logarithmic luminosity and its 1-$\sigma$ lower and upper limit;
    (7-9) logarithmic column density $N_{\rm H}$ and its 1-$\sigma$ lower and upper limit;
    (10-12) photon index $\Gamma$ and its 1-$\sigma$ lower and upper limit;
    (13) CTK candidate flag i.e. if the original spectroscopic fit includes more than 5\% of its posterior distribution in the CTK regime;
    (14) double-peaked flag (see definition in section \ref{compaLanzuisi_subsec});
    (15) source ID in the multiwavelength catalog Jin et al. (2018) if available;
    (16-18) logarithmic AGN $L_{6\mu m}$ from SED fitting and its 1-$\sigma$ lower and upper limit;
    (19) logarithmic AGN $L_{6\mu m}$ upper limit at 99 percentile if the SED fit is unconstrained.

- lgphi_chains.fits is the space density calculation product. It contains a (1000, 10, 7, 4)-shaped array. The first axis corresponds to the space density posterior distribution for each parameter grid cell. The second, third and fourth axis are the X-ray luminosity, column density and redshift grid cell numbers, respectively. The edges of the grid pixels in each of the three dimensions are log($L_X$)=(40.0, 41.0, 42.0, 42.5, 43.0, 43.5, 44.0, 44.5, 45.0, 46.0, 47.0) [log(erg s$^{-1}$)], $z$=(0.0, 0.5, 1.0, 1.5, 2.0, 2.5, 3.0, 6.0) and log($N_{\rm H}$)=(20.0, 22.0, 23.0, 24.0, 26.0) [log(cm$^{-2}$)].

- f_CTK_chains.fits is the product of our Compton-thick fraction estimation as a function of the redshift. It contains a (1000, 7)-shaped array. The first axis is the Compton-thick fraction and the second one is the redshift grid cell presented earlier.

- plot_scripts.py is a python script containing the functions used to open the lgphi_chains.fits and f_CTK_chains.fits files. It plots the space density (see figure 17) and Compton-thick fraction evolution (see figure 18) in the paper.