adsabs/AstroCLIMB huggingface dataset:
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: AGN spectral classification tests and outputs, detailed in Section 4. Top-left panel: the OHNO diagram (B. E. Backhaus et al. 2022) for AGN identification using line ratios available in this redshift and observed wavelength regime. Top-right panel: star formation rate (SFR) distribution inferred by scaling each object’s L6μm to L24μm with the ratio from an Sc galaxy template from M. Polletta et al. (2007), and then scaling this luminosity to an SFR following the G. H. Rieke et al. (2009) relation. We show the K. E. Whitaker et al. (2012) main-sequence value and 1σ spread as a black line and shaded region to compare with our HSC×DESI samples’ distribution. Bottom-left panel: sandplot representation of the distribution of the probability of the object being a Type I AGN given its HSC+WISE photometry, split by final classification. The total number of objects in each bin is written above the bars. It shows a correlation between the abundance of the BL spectroscopic classification with the photometric probability they were Type I, and its converse for the NL objects. Bottom-right panel: i magnitude sandplot distribution as a function of spectroscopic classification. As in the left panel, the total number in each bin is above the bars. We note how the brightest end of the distribution is dominated by BL AGNs, while the dimmest objects are mostly NL AGNs, LWISE-selected AGNs, and unclassified objects.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: The projected two-point cross-correlation between DESI LRGs and our HSC×DESI AGN (sub)samples for the three HSC–DESI overlap fields in the z ∈ 0.5–1.0 redshift bin. The open symbols are the per-bin inverse-variance-weighted average correlation function across fields. The 1σ uncertainties are taken from the square root of the diagonal of the jackknife covariance matrix for the sample. The dashed lines represent the fitted DM halo model to each field. We fit points for physical scales rp > 1 h−1 Mpc, while the gray region contains the interior points excluded from the fit. We note the departure from the DM model on these small scales, as expected for the one-halo term we do not model. The dotted–dashed black line represents the full AGN sample average best-fit linear DM model, and is repeated across all panels as a reference line for ease of comparison. (From left to right, starting at the top) the cross-correlation of the full, BL, NL, and LWISE-selected samples of AGNs across the three overlap fields. Next, the cross-correlation of blue (β ≤ −1) BL, and red (β > −1) BL and the NL + LWISE-selected samples of AGNs with the DESI LRGs. Symbols used for each (sub)sample here match those in Figure 12.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Summary of recovered halo masses (Mh) from the spectroscopic AGN cross-correlations, and in comparison with our result from the photometric cross-correlation from R. Córdova Rosado et al. (2024). Left: the ﹩{\mathrm{log}}\langle {M}_{h}\rangle ﹩ for each of our spectroscopic samples, as a function of the median L6μm of the sample. We highlight the difference between the inferred Mh of the blue (β ≤ −1) BL and NL + LWISE-selected AGNs (the two opaque symbols), where the former are in DM halos that are 5.5× more massive than the latter, at 2.8σ statistical significance. The values represented here are also found in Table 3, and the symbols for each (sub)sample here match those in Figure 11. Right: the ﹩{\mathrm{log}}\langle {M}_{h}\rangle ﹩ results from R. Córdova Rosado et al. (2024) with the uncertainty from the full covariance matrix estimation (open symbols), overlaid on the analogous spectroscopic sample from this analysis (symbol shapes are shared). We note the <1σ shifts in the average inferred halo mass between each of the analogous photometric and spectroscopic samples, suggesting that systematic biases in our redshifts that would affect the inferred Mh are subdominant to statistical uncertainties.
Paper: Cross-correlation of Luminous Red Galaxies with ML-selected Active Galactic Nuclei in HSC-SSP. II. AGN Classification and Clustering with DESI Spectroscopy
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Nickolas Kokron, Michael A. Strauss, ChangHoon Hahn, Grayson C. Petter, Ryan C. Hickox, Raphael E. Hviding
Figure caption: Example HSC×DESI AGN spectra and PyQSOFit fits to the continua and emission lines, following the procedure described in Section 3.1. The three spectra are chosen to be representative of an unobscured (β ≤ −1) BL AGN (top), a reddened (β > −1) BL AGN (middle), and an obscured NL AGN (bottom). The key emission lines we fit (as defined in Section 3.1) are highlighted with dotted vertical lines, where the spectra are presented in their rest-frame wavelength in units of fλ. The DESI target ID’s and redshift are shown in the top-left corner of each panel, and their R.A., decl. coordinates are (from top to bottom): (178﹩\mathop{.}\limits^{^\circ }﹩6969, −0﹩\mathop{.}\limits^{^\circ }﹩1721), (182﹩\mathop{.}\limits^{^\circ }﹩3379, −1﹩\mathop{.}\limits^{^\circ }﹩1214), (219﹩\mathop{.}\limits^{^\circ }﹩6499, −0﹩\mathop{.}\limits^{^\circ }﹩1611). The components to the spectral fits such as the continuum model and the emission-line model are shown as red and blue lines, respectively. These showcase the impressive spectral resolution from DESI.