adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: LME as a function of N gas, the threshold molecular gas column density of the dendrogram level (branch or trunk) at which the LME is measured. Errors in the LME are propagated analytically from the gas mass estimations. The color scheme refers to estimates of the protocluster SFRIR based on their infrared luminosity (see text).
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Molecular gas column density (N gas) maps and molecular gas column density error maps for each of the six regions with spectral index measurement. The first and third rows show the N gas maps. The second and fourth rows show the N gas error maps.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: (a) For each field, the left subpanel presents the ALMA-IMF Band 3 data, the middle subpanel shows the MGPS90 data, and the right subpanel shows the combined data. The color scale in the middle column goes from −3 × MAD↫ to the maximum value in the map, using a square-root color mapping. For the interferometric and combined images the color mapping follows the same rule, but the minimum and maximum between the two images are used for both plots. (b) From top to bottom: W51-E, W51-IRS2.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: For each field the left subpanel presents the ALMA-IMF Band 6 data, the middle subpanel shows the BGPS data, and the right subpanel shows the combined data. The color scale in the middle column goes from −3 × MAD↫ to the maximum value in the map, using a square-root color mapping. For the interferometric and combined images the color mapping follows the same rule, but the minimum and maximum between the two images are used for both plots.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: For each field, the top subpanel presents the Band 3 to Band 6 spectral index map, and the bottom subpanel presents the corresponding error map.
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: For each field, the panels show the difference α comb−α ALMA between the spectral index measurements using the combined images and the bsens-nobright interferometric images from the release of Ginsburg et al. (2022).
Paper: ALMA-IMF. VIII. Combination of Interferometric Continuum Images with Single-dish Surveys and Structural Analysis of Six Protoclusters
Authors: Daniel J. Díaz-González, Roberto Galván-Madrid, Adam Ginsburg, Frédérique Motte, Pierre Dell'Ova, Stanley Kurtz, Nichol Cunningham, Amelia M. Stutz, Fabien Louvet, Timea Csengeri, Manuel Fernández-López, Patricio Sanhueza, Thomas Nony, Rudy Rivera-Soto, Rodrigo H. Álvarez-Gutiérrez, Melanie Armante, Melisse Bonfand, Sylvain Bontemps, Antoine Gusdorf, Hong-Li Liu
Figure caption: Estimates of SFRIR as a function of Q 0 (top panel) and Q 0,M (bottom panel).
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: The variations of magnitude offsets between the SCR method and the XPSP method prior to the improvement as a function of the G BP − G RP color (upper panels) and G magnitude (lower panels) for all bands. The bands are marked in the top left corners; the color represents the number density of stars in each panel. Color bars are plotted in the bottom left corner of each panel. The gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: An example showing the variations of stellar flat-field fitting residuals in the SCR method as a function of the extinction E(G BP − G RP) for the J0410 band for 140 (1%) of the tiles. The tile IDs are marked in the bottom right corner of each panel. The gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Variations of magnitude offsets between the XPSP method before and after improvement as a function of G BP − G RP color for all bands. The bands are marked in the top left corners. The color represents the G magnitude of the stars; a color bar is plotted on the right. The gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Same as Figure A3 but after the Gaia XP improvements are applied. The gray dashed lines denote zero offsets.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Polynomial fits of the intrinsic colors with respect to T eff and [Fe/H] for the calibration stars used in the SCR method. The intrinsic colors include G BP − u, G BP − J0378, G BP − J0395, G BP − J0410, G BP − J0430, G BP − g, G BP − J0515, G RP − r, G RP − J0660, G RP − i, G RP − J0861, and G RP − z. The fit results after 3σ clipping are shown in the first column, with the red and blue curves representing results for [Fe/H] = 0 and = −1, respectively. The fitting residuals are labeled in red. In the second to sixth columns, residuals are plotted as functions of T eff, [Fe/H], position on the CCD (X, Y), and extinction ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩. The zero-residual lines are denoted by black dashed lines.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Histograms of the difference in zero-points between the SCR method and the SL method (blue), the SCR method and the XPSP method (red), and the SCR method and the improved XPSP method (green). The bands are marked in the top right corner of each panel. The Gaussian fitting results are plotted as gray, orange, and black dashed curves, respectively. The sigma values are marked in the top left corner of each panel with the same colors.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Correlation plots of the zero-point offsets between the SCR method and J-PLUS DR3 magnitudes for each of the two bands considered. For each panel, the correlation coefficients are marked in the bottom right corners, with a restriction that the correlation coefficient is more than 0.5. The linear fitting lines are shown as red lines for panels where the correlation coefficient is more than 0.8, and the slopes of the line are marked in the top left corners. The black dashed lines denote y = x in each panel.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Left panel: spatial variations of the zero-point offsets in the r band of J-PLUS DR3. Middle panel: spatial variations of the systematic errors in the r PS1 band of PS1. Right panel: correlation plot between the zero-point offsets in the systematic errors in the r PS1 band of PS1 and the r band of J-PLUS DR3. The black dashed line denotes y = x in this panel.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Spatial variations of the difference between the SCR and J-PLUS zero-points in each tile. The bands are marked in each panel, and a color bar is shown on the right. To clearly shown the spatial structure, the results for the J0430, g, J0515, r, J0660, i, J0861, and z bands are expanded three times.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: Variations of the magnitude offsets as a function of G magnitude (left column) and intrinsic color ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ (right column). From top to bottom, the u, J0378, J0395, J0410, J0430, g, J0515, r, J0660, i, J0861, and z bands are shown. The black dashed lines denote the zero-residual lines.
Paper: J-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Haibo Yuan, C. López-Sanjuan, Yang Huang, Bowen Huang, Timothy C. Beers, Shuai Xu, Yuanchang Wang, Lin Yang, Jailson Alcaniz, Carlos Andrés Galarza, Raul E. Angulo De La Fuente, A. J. Cenarro, David Cristóbal-Hornillos, Renato A. Dupke, Alessandro Ederoclite, Carlos Hernández-Monteagudo, Antonio Marín-Franch, Mariano Moles, Laerte Sodré, Héctor Vázquez Ramió, Jesús Varela López
Figure caption: A flowchart illustrating the use of the SCR and improved XPSP methods in this work.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Different colors are used for different sources. Left: the variation of the intrinsic luminosity of the soft excess with N H. Right: the variation of the intrinsic luminosity of primary continuum with N H. These plots indicate that there is no correlation between the intrinsic luminosities and N H in long-term observations for different sources.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Left: the number distribution of reduced χ 2 (﹩{\chi }_{\mathrm{red}}^{2}={\chi }^{2}﹩/dof) obtained from the X-ray spectral fitting with the powerlaw+powerlaw model on 21 “bare” AGNs. Right: the number distribution of hydrogen column density N H obtained from the X-ray spectral fitting of data of 21 “bare” AGNs with the composite model.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: The confidence contours between the photon index (Γ) of primary continuum and soft excess are shown for 1H 0419–577 (MJD 52,635; top left), 3C 382 (MJD 54,584; top middle), 3C 390.3 (MJD 53,286; top right), Ark 564 (MJD 55,705; bottom left), Mrk 1018 (MJD 55,174; bottom middle), and IRAS 13224–3809 (MJD 52,019); bottom right). The red, green, and blue contours represent the 1σ, 2σ, and 3σ levels, respectively.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: The variation of the spectral indices is plotted in the left panel. The variation between the normalized luminosity of soft excess (L SE/L Edd) and corresponding spectral slope (ΓSE) is plotted in the middle panel. The right panel shows the variation of the normalized luminosity of primary continuum (L PC/L Edd) and spectral slope (ΓPC). The red dotted line represents the linear correlation of corresponding parameters.
Paper: Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess
Authors: Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Figure caption: Distribution of sources with respect to redshift (z) and mass of central black holes (M BH) is shown in the left and right histograms, respectively.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Performance test with empirical statistics–based mock galaxy sample for the photometric redshift estimation of galaxies in the CSST wide-field multiband imaging survey. (a) The results for only the simplest SED model (SFH = τ, –CEH, DAL = Cal+00) employed in this work. We consider six different choices of efr (target sampling efficiency) as shown by the different symbols. For each efr, we consider eight cases with the number of live points (nlive), which determines the effective sampling resolution, equal to 10, 15, 20, 25, 50, 100, 200, and 400, respectively. The relations between the computation time (in s/object/CPU, by employing one core of a 2.2 GHz CPU) and the performance metrics σ NMAD (top panels), BIA (middle panels), and OLF (bottom panels) are shown. The results for the two cases with (left panels) and without (right panels) observational noise in the mock data are shown. In general, a larger value of nlive and a smaller value of efr lead to better quality of redshift estimation, but with the cost of longer running time. (b) The results for six different SED models with increasing complexity. Only the results with efr = 0.1 are shown. In general, more complicated SED models require longer running time. They also lead to worse quality of photometric redshift estimation, which is likely due to more severe parameter degeneracies. Actually, for the last four more complicated SED models with the DAL of Salim et al. (2018), the number of free parameters is greater than the number of photometric data points (seven for the CSST imaging survey), as shown in Table 1.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: The results of photometric redshift estimation with (right panels) and without (left panels) noise, for the analysis of the empirical statistics–based (top panels) and hydrodynamical simulation–based (bottom panels) mock galaxy samples. The error from imperfect SED modeling will only present for the analysis of the hydrodynamical simulation–based mock galaxy sample. The photometric redshifts (z phot) are estimated by employing the τ model of SFH without consideration of metallicity evolution and the Calzetti et al. (2000) model of DAL. The red solid line indicates the identity while the red dashed lines indicate the outlier limits, i.e., ﹩\left|{z}_{\mathrm{phot}}-{z}_{\mathrm{true}}\right|/(1+{z}_{\mathrm{true}})\gt 0.15﹩. Here, we show the results obtained with the MultiNest runtime parameters efr and nlive equal to 0.1 and 50, respectively. In general, the observational noise is the more important source of error for the photometric redshift estimation of galaxies, though the contribution from imperfect SED modeling is also very important.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Performance test of Bayesian evidence estimation with empirical statistics–based mock galaxy sample for CSST imaging survey. The relations between the computation time (in seconds per object by employing a single 2.2 GHz CPU core) and the value of the natural logarithm of Bayesian evidence (as computed with Equation (31)) and its error (bottom panels) for the whole galaxy sample are shown. The results for two versions of Bayesian evidence with (top panels) or without (middle panels) importance sampling are shown. (a) The results for only the simplest SED model (SFH = τ, –CEH, DAL = Cal+00) employed in this work. We consider six different choices of efr (target sampling efficiency) as shown by the different symbols. The results for seven cases with nlive equal to 15, 20, 25, 50, 100, 200, or 400 are shown. The left panels show the results with noisy data while the right panels show the results with noise-free data. (b) The results for six different SED models with increasing complexity. Only the results with efr = 0.1 are shown. The value of Bayesian evidence clearly decreases with the increase of complexity of the SED model.
Paper: BayeSED-GALAXIES. I. Performance Test for Simultaneous Photometric Redshift and Stellar Population Parameter Estimation of Galaxies in the CSST Wide-field Multiband Imaging Survey
Authors: Yunkun Han, Lulu Fan, Xian Zhong Zheng, Jin-Ming Bai, Zhanwen Han
Figure caption: Same as Figure 4, but for the SFR estimation. The quality of SFR estimation, in terms of σ NMAD, BIA, and OLF, is slightly better than that of stellar mass estimation, but even more sensitive to the selection of SED models. In the case with noise, for the four most complicated SED models used in this work, the σ NMAD, bias, and OLF of SFR estimation significantly increase with nlive. This is an even clearer indication of overfitting to the noise in the data. In general, more complicated SED models lead to worse quality of SFR estimation.