adsabs/AstroCLIMB huggingface dataset:
Paper: Learning Cosmology and Clustering with Cosmic Graphs
Authors: Pablo Villanueva-Domingo, Francisco Villaescusa-Navarro
Figure caption: Example of the GNN architecture with two graph blocks. The node, edge, and global features are input into the network and updated through the different message-passing layers. A final pooling step aggregates the information from all nodes to output target  y .
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: The panels from left to right show the comparisons of the Si, C, and Mg abundances (where possible) between this work (low-resolution spectra R = 1800) and literature (high-resolution spectra) for 26 stars from McEvoy et al. (2017). The black dashed lines represent a one-to-one correlation, while the gray dashed line represents a linear fit to the data (C and Si abundances).
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: Histogram of projected rotational velocities for our B-type stars in LAMOST DR5. The blue dashed lines are the mean values of ﹩v\sin \,i﹩ (104 km s−1). The yellow and green dashed lines indicate 15% and 85% of ﹩v\sin \,i﹩ (50 km s−1 and 160 km s−1), respectively.
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: The left panel shows the distribution of B-type stars from LAMOST for effective temperature vs. spectral types. The colors represent the number of stars in each bin. The right panel is similar but for surface gravity vs. luminosity class.
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: Abundance gradients in the Galactocentric distances (7 ≤ R  g  ≤14 kpc) for carbon and silicon. The black dashed lines represent the best-fitting result for radial gradient slopes. The distance of the Sun (⊙) is 8.33 kpc.
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: The distribution of 36BFL stars in microturbulence (ξ) from literature vs. surface gravity (log g). The dashed lines represent the best linear fit to the data.
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: The distribution of the C and Si abundances of B-type stars in LAMOST. The red and black histograms represent the C abundances of 93 B-type stars and Si abundances of 101 B-type stars in LAMOST, respectively. The red and black dashed lines represent the solar C and Si abundances from Asplund et al. (2009).
Paper: Chemical Composition of B-type Stars from LAMOST DR5
Authors: Zhicun Liu, Wenyuan Cui, Chao Liu, Sofya Alexeeva, Jianrong Shi, Gang Zhao
Figure caption: The C and Si abundance uncertainty that is estimated by summing the uncertainties from the stellar parameters (T eff, log g, ﹩v\sin \,i﹩ and metallicity) are shown as histogram.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: SFR–stellar-mass distributions for galaxies in our CLEAR sample. The shaded regions and contours show the distribution of sources with 1.1 < z < 2.3 from the 3D–HST+ parent catalog. The red-colored squares show the CLEAR sample studied here. The plots at the top and to the right show the distributions of the samples in ﹩\mathrm{log}{M}_{* }﹩ and log SFR using a histogram and kernel density estimator.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Redshift distribution of galaxies in the CLEAR 1.1 < z < 2.3 sample in this study. This sample is selected from the 3D-HST+ parent catalog with spectroscopic redshifts from the grism data in this redshift range and by requiring that all galaxies have S/N > 3 in [O II], Hβ, or [O III].
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Metallicity vs. R 23 for the CLEAR sample derived by comparing the observed [O II], Hβ, and [O III] line fluxes to MAPPINGS V photoionization models. The data points show the mode of the posterior likelihoods on metallicity. The error bars denote the inter-68th percentiles derived from the HDIs; arrows show 1σ limits. The curves denote various calibrations in the literature (Maiolino et al. 2008; Curti et al. 2017; Strom et al. 2018; Kewley et al. 2019b); the solid-thick line is our fit to the CLEAR results (see Equation (3)). The left panel shows the CLEAR galaxies colored by redshift. The right panel shows the CLEAR galaxies colored by ionization, ﹩\mathrm{log}q﹩. While there is a trend between R 23 and metallicity, there is an additional dependence on ionization q. The ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ values are derived using the line fluxes in R 23, which causes the apparently “tight” scatter data points relative to their error bars. To illustrate this, we show example error ellipses for a fiducial galaxy with 12 + log(O/H) = 8.8. These illustrate the covariance between R 23 and ﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩ lies in the direction of the relation.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: The stellar-mass, gas-phase-metallicity relation (MZR) for CLEAR galaxies at 1.1 < z < 2.3. The top plot shows the MZR with the CLEAR galaxies color-coded by redshift. Large squares show medians in bins of stellar mass. Error bars show the scatter in each bin. The red and blue solid lines show fits to the CLEAR galaxies. The gray shaded region shows the distribution for SDSS galaxies derived using our analysis (identical to that applied to CLEAR). The black solid curve shows our quadratic fit to the SDSS galaxies (Equation (5) and Table 2). The dotted lines show the MZR relation at z = 0.07, 0.7, and 2.2 derived by Maiolino et al. (2008). The histogram and curve along the top of the panel shows the distribution of stellar mass in the z ∼ 1.3 (blue) and z ∼ 1.8 CLEAR samples. The bottom panels show the MZR with galaxies color-coded by specific SFR (bottom left; log sSFR ) and nebular ionization (bottom right; ﹩\mathrm{log}q﹩).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Top panel: distribution of O 32 as a function of R 23 for galaxies in the CLEAR sample (colored squares) compared to those from SDSS (using a kernel density estimator, KDE, gray shaded region; the contours contain 50% and 80% of the SDSS sample). For clarity, the plot only shows CLEAR galaxies with S/N > 3 in [O II], [O III], and Hβ, color-coded by redshift. The data have been corrected for dust attenuation (see Section 4). The CLEAR galaxies reside in the upper end of the SDSS distribution. The panels to the top and right show the 1D distributions from a KDE. Bottom panels: the distribution of the CLEAR and SDSS R 23 vs. O 32 distributions compared to predictions from photoionization models considered here. In this work we adopt the MAPPINGS V models (Kewley et al. 2019b) as these are the most current at the time of this writing, and they best cover the line ratios spanned by the observed galaxies.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: One-dimensional G102 + G141 spectral stacks of galaxies in the sample (1.1 < z < 2.3), divided in four bins of stellar mass. The spectra have been shifted to the rest-frame, and stacked as described in the text. The solid lines show the weighted mean of each stack and the shaded region shows standard deviation of the population (NB: this the dispersion of the objects in the stack, and not the error on the mean). The locations of prominent emission features are labeled. The stacked spectra illustrate the effects of the instrumental resolution on the emission features. The data also show that the relative strength of emission features depends on stellar mass, with galaxies with lower stellar masses having stronger emission lines, and stronger [O III] compared to [O II] and Hβ.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Gallery of HST RGB images (using ACS F775W, WFC3 F105W, and F160W imaging), grism spectra, and derived constraints on the gas-phase metallicity (﹩12+\mathrm{log}﹩ O/H) and ionization (﹩\mathrm{log}q﹩). The figure includes galaxies in the CLEAR GOODS-N pointings with redshift 1.2 < z < 1.5 such that the spectra contain [O II], Hβ, [O III], and Hα+[N II]. Each row shows one galaxy. The leftmost panel shows the RGB image. The scale bar corresponds to 1″. The middle panel shows the 1D, G102 (blue), and G141 (red) extracted spectra; prominent emission features are indicated. The rightmost two panels adjacent to each spectrum show the posterior on the gas-phase metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩) and ionization parameter (﹩\mathrm{log}q﹩) derived by comparing the [O II], Hβ, and [O III] line fluxes against the MAPPINGS V photoionization models. The solid and dashed vertical lines show the mode and 68% range derived for the HDI (Bailer-Jones et al. 2018). The galaxies are sorted as a function of decreasing stellar mass (top to bottom).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption:  O 32 vs. ionization for the CLEAR sample, derived by comparing the observed [O II], Hβ, and [O III] line fluxes to the MAPPINGS V photoionization models. The left panel shows CLEAR galaxies color-coded by redshift. The right panel shows the CLEAR galaxies color-coded by R 23 value. In each panel, the top axis shows the corresponding dimensionless ionization parameter (U = q/c). The dashed line shows the linear relation calibrated by Strom et al. (2018) using independent photoionization modeling for z ∼ 2.3 galaxies. The solid line shows a linear fit to the CLEAR galaxies derived from a Bayesian method. The shaded gray region shows 400 random draws from the posterior of the linear fit. The O 32 ratio correlates with ionization parameter. There is a secondary dependence on R 23 (which translates to a dependence on gas-phase metallicity).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Examples of model fits to the broadband photometry and HST grism data for two example galaxies at z  ∼ 1.5 in the GOODS-N CLEAR fields (GN 19659 is also shown in Figure 7). The fitting procedure uses the method of Estrada-Carpenter et al. (2020, and V. Estrada-Carpenter et al., in preparation). The top row of each set of panels shows the broadband photometry (green dots) from the CLEAR 3DHST+ catalog, and the G102 (blue) and G141 (red) spectra along with a best-fit stellar population model (black line). The model fits currently exclude emission lines (though the emission features are prominent in the data for these galaxies). The lower set of panels for each galaxy shows the posteriors for the stellar mass (﹩\mathrm{log}M/{M}_{\odot }﹩), dust attenuation (A(V)/mag), and specific SFR (log sSFR/yr−1), where the vertical line shows the median, and the shaded region shows the 16th–84th percentile range of the HDI.
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Gallery of individual 1D G102 + G141 spectra for the sample of 40 galaxies in CLEAR with 1.1 < z < 2.3 in the stellar-mass range ﹩9.6\lt \mathrm{log}{M}_{* }/{M}_{\odot }\lt 9.9﹩ with S/N > 3 in at least one of [O II] λ3726,3729, [O III] λ λ4959, 5008, and Hβ λ4861. The spectra have been shifted to the rest-frame to illustrate common spectral features. The color scale changes with spectroscopic redshift (the gray shading of each spectrum indicates the uncertainty). For galaxies with z ≲ 1.6, the data cover Hα λ6563 (which is blended with [N II] λ λ6584, 6584 at the resolution of the G141 grism).
Paper: CLEAR: The Ionization and Chemical-enrichment Properties of Galaxies at 1.1 < z < 2.3
Authors: Casey Papovich, Raymond C. Simons, Vicente Estrada-Carpenter, Jasleen Matharu, Ivelina Momcheva, Jonathan R. Trump, Bren E. Backhaus, Gabriel Brammer, Nikko J. Cleri, Steven L. Finkelstein, Mauro Giavalisco, Zhiyuan Ji, Intae Jung, Lisa J. Kewley, David C. Nicholls, Norbert Pirzkal, Marc Rafelski, Benjamin Weiner
Figure caption: Same as Figure 7, but showing example galaxies with spectroscopic redshifts 1.3 < z < 1.9 in the CLEAR GOODS-S pointings. The galaxies are sorted as a function of decreasing stellar mass (top to bottom).
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: Left: the 2.0–5.0 keV NuSTAR and Swift spectra, obs5 (left) and obs6 (right), of Mrk 590 fitted with an absorbed power law and the rest of the energy band (0.6–50.0 keV) extrapolated. The broadband residuals from the fit show no soft excess and only Fe emission-line complex around 6.4 keV similar to the two Suzaku observations. The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: Left: the 2.0–5.0  keV Suzaku spectra, obs3 (left) and obs4 (right), of Mrk 590 fitted with an absorbed power law and the rest of the energy band (0.6–50.0  keV) extrapolated. The broadband residuals from the fit show no soft excess and only Fe emission-line complex around 6.4 keV for the two Suzaku observations. The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: Left: the 2.0–5.0 keV XMM-Newton spectra, obs1 (left) and obs2 (right), of Mrk 590 fitted with an absorbed power law and the rest of the energy band (0.3–10.0 keV) extrapolated. The broadband residuals from the fit show the presence of soft excess and an Fe emission line for the two XMM-Newton observations. The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The 0.001–10.0 keV NuSTAR FPM and Swift XRT and UVOT data of Mrk 590 fitted with an absorbed relxill and MyTorus model. The data, the residuals, and the theoretical model are shown for obs5 (left) and obs6 (right). The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: Same as Figure 11, but for obs7 (left) and obs8 (right). The broadband residuals from the fit show no soft excess and only Fe emission-line complex around 6.4 keV similar to the two Suzaku observations. The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The 0.001–10.0  keV XMM-Newton EPIC-pn and OM data of Mrk 590 fitted with an absorbed relxill and MyTorus model. The data, the residuals, and the theoretical model are shown for obs1 (left) and obs2 (right). The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: The 0.6–50.0 keV Suzaku XIS and PIN data of Mrk 590 fitted with an absorbed relxill and MyTorus model. The data, the residuals, and the theoretical model are shown for obs3 (left) and obs4 (right). The X-axis represents observed-frame energy.
Paper: The Origin of the Vanishing Soft X-Ray Excess in the Changing-look Active Galactic Nucleus Mrk 590
Authors: Ritesh Ghosh, Sibasish Laha, Kunal Deshmukh, Varun Bhalerao, Gulab C. Dewangan, Ritaban Chatterjee
Figure caption: Same as Figure 15, but for obs7 (left) and obs8 (right). The X-axis represents observed-frame energy.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: The z phot and M 1450 distributions of candidates selected by each process, after the initial selection. The candidates satisfying DL criteria (the blue circles), a combination of DL, BIC, and visual inspection (the black diamonds), and all the selection criteria (the pink squares) are marked. The total completeness function as a function of z and M 1450 is expressed as a two-dimensional histogram. This function has a value from 0 to 1, indicating the fraction of quasar SED models satisfying preselection, the DL, and BIC selections in a bin with Δz = 0.05 and ΔM 1450 = 0.1. The side panel shows the normalized M 1450 histogram.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: Quasar LFs at z ∼ 5. The binned LF from our work is marked with hot pink pentagons. The rebinned LF of quasars in Yang et al. (2016) and K20 are shown in the orange squares and the green diamonds, respectively. The pink solid (dashed–dotted) line represents our parametric LF without (with) K20. These binned and parametric LFs from our work are similar to those of the recently reported LFs (K20; N20; Shen et al. 2020) at M 1450 < −23.5. The empty pentagon and star points indicate the bins not used for obtaining a parametric quasar LF in this work and N20, respectively, considering potentially high galaxy contamination. Contrary to several works, binned LFs of Boutsia et al. (2018) and Giallongo et al. (2019) show a high number density at the faint end.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: Color–color diagrams in riz (left) and riy (right). The green and red histograms indicate the number densities of i-band-selected point sources with i <25 mag and quasar models. The 1,599 DL-selected candidates are marked with gray dots. The stars indicate the confirmed quasar or promising candidates reported in Shin et al. (2020), while the pentagons represent the 35 quasar candidates used for constructing the parametric LF. These stars and pentagons are color-coded by their photometric redshifts. The dotted, dashed, and solid lines correspond to the loose, best, and tight color selection criteria, respectively. Color cuts used in N20 are marked with the navy lines in the riy color space.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: The SED-fitting results of one quasar (HSC J021844–044824) and one medium-band-selected quasar (IMS J160732+544750) in Shin et al. (2020). For a given object, we show the results with the seven HSC-SSP filters (left) and ten filters at least (right) consisting of HSC-SSP, near-infrared, and medium-band filters in Shin et al. (2020). The dark gray and the light gray lines show the best-fit quasar SED model and star SED model, respectively. The measured fluxes by HSC-SSP and near-infrared filters (red), and medium-band filters (green) are marked with points. The blue open circles with arrows indicate the detection limit in the case of nondetection.
Paper: The Quasar Luminosity Function at z ∼ 5 via Deep Learning and Bayesian Information Criterion
Authors: Suhyun Shin, Myungshin Im, Yongjung Kim
Figure caption: The i-band normalized SEDs of the galaxies at z ∼ 5 (LBG) and quasars at z ∼ 5 (QSO). The light red and green solid lines in the left and middle panels show the SED of each object in the QSO and LBG samples, respectively. The red and green solid lines correspond to the mean fluxes of the QSO and LBG objects. The pink thick line in the right panel represents the mean fluxes of model quasars at z ∼ 5. The error bars with the solid lines indicate a 68% range of normalized fluxes.