adsabs/AstroCLIMB huggingface dataset:
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the parameters used for the C34S (2–1) LOC + MCMC in Figure 4.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the CS (2–1) parameters used for the LOC + MCMC in Figure 7.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Top panel: SO (2, 3–1, 2) observations toward the L1544 dust peak in black and combined modeling results in red. Middle panel: 34SO (2, 3–1, 2) observations toward the L1544 dust peak in black and combined modeling results in red. Bottom panel: corner plot of the parameters used for the SO + 34SO nonextended model.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Top panel: CS (2–1) observations toward the L1544 dust peak in black and modeling results in red. Middle panel: same as the top panel but for C34S (2–1). Bottom panel: corner plot for the CS + C34S nonextended model.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the extended c-C3H2 (21,2–10,1) parameters used for the LOC + MCMC in Figure 13.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the c-C3H2 (21,2–10,1) parameters used for the LOC + MCMC in Figure 12.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the extended H2CO (21,2–11,1) parameters used for the LOC + MCMC in Figure 11.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the H2CO (21,2–11,1) parameters used for the LOC + MCMC in Figure 10.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the HCO+ (1–0) parameters used for the LOC + MCMC in Figure 9.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Corner plot of the SO (2, 3–1, 2) parameters used for the LOC + MCMC in Figure 8.
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: The model using the approach of E. Redaelli et al. (2022) is shown as a dashed–dotted blue line. Observations toward the L1544 dust peak are shown in black.
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The evolution of the individual fractions of the five primary particle species as a function of energy, obtained based on the three hadronic interaction models. The inner error bars represent the statistical uncertainties, while the outer error brackets represent the systematic uncertainties (see Section 5.1). The x-axis value of each point corresponds to the center of the energy bin; however, to improve visual clarity, they have been artificially shifted along the x-axis.
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The LCm−1 distributions in the energy range lg(E/eV) = [15.4–15.6] and lg(E/eV) = [15.6–15.8] for proton- (left) and Fe (right)-induced showers as predicted by the three hadronic interaction models. Bottom plots display the ratio between each pair of two distributions: EPOS-LHC–QGSjet-II-04 (red), EPOS-LHC–SIBYLL 2.3d (blue), and QGSjet-II-04–SIBYLL 2.3d (green).
Paper: High-sensitivity Molecular Line Observations toward the L1544 Prestellar Core Challenge Current Models 
Authors: J. Ferrer Asensio, S. S. Jensen, S. Spezzano, P. Caselli, F. O. Alves, O. Sipilä, E. Redaelli
Figure caption: Top panel: HCO+ (1–0) observations toward the L1544 dust peak in black and HCO+ + HC17O+ extended modeling results as a dashed–dotted blue line. Middle panel: HC17O+ (1–0) observations toward the L1544 dust peak in black and combined modeling results as a dashed–dotted blue line. Bottom panel: corner plot of the parameters used for the HCO+ + HC17O+ extended model.
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The Nμ distributions in the energy range lg(E/eV) = [15.4–15.6] and lg(E/eV) = [15.6–15.8] for proton- (left) and Fe (right)-induced showers as predicted by the three hadronic interaction models. Bottom plots display the ratio between each pair of two distributions: EPOS-LHC–QGSjet-II-04 (red), EPOS-LHC–SIBYLL 2.3d (blue), and QGSjet-II-04–SIBYLL 2.3d (green).
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The ﹩{N}_{e}^{-1}﹩ distributions in the energy range lg(E/eV) = [15.4–15.6] and lg(E/eV) = [15.6–15.8] for proton- (left) and Si (right)-induced showers as predicted by the three hadronic interaction models. Bottom plots display the ratio between each pair of two distributions: EPOS-LHC–QGSjet-II-04 (red), EPOS-LHC–SIBYLL 2.3d (blue), and QGSjet-II-04–SIBYLL 2.3d (green).
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The distributions of the age parameter in the energy range lg(E/eV) = [15.4–15.6] and lg(E/eV) = [15.6–15.8] for He- (left) and Fe (right)-induced showers as predicted by the three hadronic interaction models. Bottom plots display the ratio between each pair of two distributions: EPOS-LHC–QGSjet-II-04 (red), EPOS-LHC–SIBYLL 2.3d (blue), and QGSjet-II-04–SIBYLL 2.3d (green).
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The distributions of PCA0 for proton-induced showers (left) and PCA1 for iron-induced showers (right) in the energy range lg(E/eV) = [15.4–15.6] and lg(E/eV) = [15.6–15.8] for three hadronic interaction models. Bottom plots display the ratio between each pair of two distributions: EPOS-LHC–QGSjet-II-04 (red), EPOS-LHC–SIBYLL 2.3d (blue), and QGSjet-II-04–SIBYLL 2.3d (green).
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The 2D PCA0 vs. PCA1 distributions for proton- and iron-induced showers in the energy interval lg(E/eV) = [15.6–15.8] based on the EPOS-LHC model. The size of the squares reflects the number of events in each bin.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Measurements and fits for the nine 0.8 < z < 1.0 samples defined in Figure 3 and Table 1. The top-left, top-right, and bottom-left panels show the projected 2PCFs of the low-, intermediate-, and high-stellar-mass samples, respectively. Filled circles mark the measurements. Solid curves and shaded regions mark the median and 1σ bounds of the posterior model distribution, respectively. For illustrative purposes, measurements are staggered in rp. Vertical offsets of −1 dex and +1 dex are applied to the lowest and highest [O II] luminosity samples in each panel, respectively. The subpanel below each main panel shows the residual of the model relative to the measurement, normalized by the measurement uncertainty. The shaded region represents the ±1σ bounds. Bottom right: measurements of the number densities are shown as filled circles, with 10% uncertainties assumed. Open circles and error bars mark the median and 1σ bounds of the posterior model distribution, respectively. For illustrative purposes, horizontal offsets are added between the measurement and fit of a given sample and between samples.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Model constraints from the low-redshift (0.8 < z < 1.0) samples. From left to right, the model relations are (top row) the occupation fraction of central ELGs, the median ﹩{\mathrm{log}}\,\,{M}_{* }﹩ of centrals, the scatter in ﹩{\mathrm{log}}\,\,{M}_{* }﹩ of centrals, (middle row) the median ﹩{\mathrm{log}}\,\,{L}_{[{\rm{OII}}]}﹩ of centrals, the scatter in ﹩{\mathrm{log}}\,\,{L}_{[{\rm{OII}}]}﹩ of centrals, the normalization for the conditional stellar mass function of satellites, (bottom row) the low-mass slope for the conditional stellar mass function of satellites, the median ﹩{\mathrm{log}}\,\,{L}_{[{\rm{OII}}]}﹩ of satellites, and the scatter in ﹩{\mathrm{log}}\,\,{L}_{[{\rm{OII}}]}﹩ of satellites. Solid lines indicate the median solution. Dark and light shaded regions mark the 1σ and 2σ bounds, respectively. Panels for μx, μy, and μy,sat also include gray shaded regions that mark the central 95% range spanned by the sample data. Panels for the constraints on central galaxies have thicker outlines.
Paper: Cosmic-Ray Mass Composition around the Knee via Principal Component Analysis
Authors: Nicusor Arsene
Figure caption: The evolution of ﹩\langle \mathrm{ln}(A)\rangle ﹩ as a function of energy, obtained using the PCA method based on the three hadronic interaction models. For comparison, we also plotted the evolution of ﹩\langle \mathrm{ln}(A)\rangle ﹩ as a function of energy derived solely from the LCm parameter based on the KASCADE experimental data (N. Arsene 2023), as well as recent results from the LHAASO−KM2A experiment (Z. Cao et al. 2024). These results are further compared with the predictions of four data-driven and astrophysical models: GSF (H. P. Dembinski et al. 2018), Horandel (J. R. Hoerandel 2003), Gaisser H3a (T. K. Gaisser et al. 2013), and GST (T. Stanev et al. 2014).
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Footprint of the 20 One-Percent Survey rosettes in blue (Mollweide projection). The Galactic plane is shown in green. The inset image shows the angular distribution of spectroscopically confirmed ELGs within one rosette; the galaxies observed in the highly complete annulus are highlighted in blue.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Selection boundaries for the nine samples within each redshift group as a function of ﹩{\mathrm{log}}\,{L}_{\,\rm{[OII]}\,}﹩ and ﹩{\mathrm{log}}\,{M}_{* }﹩. The horizontal error bars illustrate the 0.5 dex measurement scatter in stellar mass as quantified in Appendix A with respect to COSMOS2020. Left, middle, and right panels correspond to redshift ranges 0.8 < z < 1.0, 1.0 < z < 1.2, and 1.2 < z < 1.6, respectively.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Same as Figure 4 but for the 1.2 < z < 1.6 high-redshift samples.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Number density of spectroscopically confirmed ELGs in the DESI One-Percent Survey. Only galaxies within rosette annuli (Figure 1) are included. Colored regions mark the redshift ranges considered in this work.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Same as Figure 4 but for the 1.0 < z < 1.2 intermediate-redshift samples.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Derived quantities of each sample. From top to bottom, the rows are the galaxy bias, the median halo mass of centrals, the satellite fraction, and the median halo mass of satellites. Halo masses are in units of h−1 M⊙. Each panel contains all luminosity and redshift samples at fixed stellar mass. Data points are colored according to the binning in stellar mass and [O II] luminosity in Figure 3. From low to high, redshifts are marked as filled circles, filled stars, and open squares.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Results from an alternative parameterization of the Ac–Mh relation. For illustrative purposes, only constraints for the intermediate-redshift samples are shown. Left panels show the occupation fraction of central ELGs (top) and median ﹩{\mathrm{log}}\,{L}_{[{\rm{OII}}]}﹩ of centrals (bottom), formatted as in Figure 7. The right panel shows the mean occupation functions of the intermediate-stellar-mass samples, formatted as in Figure 10. All other constraints are largely unchanged.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Mean occupation functions of each sample. Each row contains one redshift group. Solid lines and shaded regions show the median and 1σ bounds of the mean occupation functions for centrals, respectively. Dashed lines mark the same but for satellites. For clarity, uncertainties are included only for the middle [O II] luminosity samples. Error bars for other samples within a panel are roughly the same magnitude. [O II] luminosities are given in erg s−1.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Comparison between aperture corrections. Each row contains one redshift group. Left column: equivalent-width-corrected (“EW-corrected”) [O II] luminosity vs. r-band-corrected (“r-corrected”) [O II] luminosity. Shaded squares and color bar give the number of galaxies in each 2D bin. The one-to-one (black dashed) line traces the median (red solid) within 1 standard deviation and ∼0.1 dex, suggesting consistency in the central value. Middle column: distribution of r-corrected ﹩{\mathrm{log}}\,{L}_{[{\rm{OII}}]}﹩ at fixed EW-corrected ﹩{\mathrm{log}}\,{L}_{[{\rm{OII}}]}﹩. Right column: distribution of EW-corrected ﹩{\mathrm{log}}\,{L}_{[{\rm{OII}}]}﹩ at fixed r-corrected ﹩{\mathrm{log}}\,{L}_{[{\rm{OII}}]}﹩ (reverse of middle column).
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Comparison of ELG properties reported by DESI (via FASTSPECFIT) and COSMOS2020 (via EAZY). Left: DESI stellar masses have a notable offset and scatter with respect to COSMOS2020. The 2σ bounds highlight that the DESI stellar mass distribution is skewed, especially at low stellar masses. Middle: COSMOS2020-inferred [O II] luminosities as a function of DESI-measured [O II] luminosities. Right: star formation rate estimates from COSMOS2020 as a function of DESI [O II] luminosity.